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<button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Cleri%2C+N+J&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Cleri%2C+N+J&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Cleri%2C+N+J&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> </ul> </nav> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2503.02059">arXiv:2503.02059</a> <span> [<a href="https://arxiv.org/pdf/2503.02059">pdf</a>, <a href="https://arxiv.org/format/2503.02059">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> A confirmed deficit of hot and cold dust emission in the most luminous Little Red Dots </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Setton%2C+D+J">David J. Setton</a>, <a href="/search/astro-ph?searchtype=author&query=Greene%2C+J+E">Jenny E. Greene</a>, <a href="/search/astro-ph?searchtype=author&query=Spilker%2C+J+S">Justin S. Spilker</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+C+C">Christina C. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Labbe%2C+I">Ivo Labbe</a>, <a href="/search/astro-ph?searchtype=author&query=Ma%2C+Y">Yilun Ma</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+B">Bingjie Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Whitaker%2C+K+E">Katherine E. Whitaker</a>, <a href="/search/astro-ph?searchtype=author&query=Leja%2C+J">Joel Leja</a>, <a href="/search/astro-ph?searchtype=author&query=de+Graaff%2C+A">Anna de Graaff</a>, <a href="/search/astro-ph?searchtype=author&query=Alberts%2C+S">Stacey Alberts</a>, <a href="/search/astro-ph?searchtype=author&query=Bezanson%2C+R">Rachel Bezanson</a>, <a href="/search/astro-ph?searchtype=author&query=Boogaard%2C+L+A">Leindert A. Boogaard</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">Gabriel Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Cutler%2C+S+E">Sam E. Cutler</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Cooper%2C+O+R">Olivia R. Cooper</a>, <a href="/search/astro-ph?searchtype=author&query=Dayal%2C+P">Pratika Dayal</a>, <a href="/search/astro-ph?searchtype=author&query=Fujimoto%2C+S">Seiji Fujimoto</a>, <a href="/search/astro-ph?searchtype=author&query=Furtak%2C+L+J">Lukas J. Furtak</a>, <a href="/search/astro-ph?searchtype=author&query=Goulding%2C+A+D">Andy D. Goulding</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">Michaela Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Kokorev%2C+V">Vasily Kokorev</a>, <a href="/search/astro-ph?searchtype=author&query=Maseda%2C+M+V">Michael V. Maseda</a>, <a href="/search/astro-ph?searchtype=author&query=McConachie%2C+I">Ian McConachie</a> , et al. (11 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2503.02059v1-abstract-short" style="display: inline;"> Luminous broad H$伪$ emission and red rest-optical SEDs are the hallmark of compact Little Red Dots (LRDs), implying highly attenuated dusty starbursts and/or obscured active galactic nuclei. However, the lack of observed FIR emission has proved difficult to reconcile with the implied attenuated luminosity in these models. Here, we utilize deep new ALMA imaging, new and existing JWST/MIRI imaging,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2503.02059v1-abstract-full').style.display = 'inline'; document.getElementById('2503.02059v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2503.02059v1-abstract-full" style="display: none;"> Luminous broad H$伪$ emission and red rest-optical SEDs are the hallmark of compact Little Red Dots (LRDs), implying highly attenuated dusty starbursts and/or obscured active galactic nuclei. However, the lack of observed FIR emission has proved difficult to reconcile with the implied attenuated luminosity in these models. Here, we utilize deep new ALMA imaging, new and existing JWST/MIRI imaging, and archival Spitzer/Herschel imaging of two of the rest-optically brightest LRDs ($z=3.1$ and $z=4.47$) to place the strongest constraints on the IR luminosity in LRDs to date. The detections at $位_\mathrm{rest}=1-4 \ 渭$m imply flat slopes in the rest-IR, ruling out a contribution from hot ($T\gtrsim500$ K) dust. Similarly, FIR non-detections rule out any appreciable cold ($T\lesssim75$ K) dust component. Assuming energy balance, these observations are inconsistent with the typical FIR dust emission of dusty starbursts and quasar torii, which usually show a mixture of cold and hot dust. Additionally, our [$\mathrm{C}_{II}$] non-detections rule out typical dusty starbursts. We compute empirical maximum IR SEDs and find that both LRDs must have $\log(L_\mathrm{IR}/L_\odot) \lesssim 12.2$ at the $3蟽$ level. These limits are in tension with the predictions of rest-optical spectrophotometric fits, be they galaxy only, AGN only, or composite. It is unlikely that LRDs are highly dust-reddened intrinsically blue sources with a dust temperature distribution that conspires to avoid current observing facilities. Rather, we favor an intrinsically redder LRD SED model that alleviates the need for strong dust attenuation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2503.02059v1-abstract-full').style.display = 'none'; document.getElementById('2503.02059v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 March, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 5 figures, 3 tables. Submitted to ApJ Letters. Comments welcome!</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.03519">arXiv:2502.03519</a> <span> [<a href="https://arxiv.org/pdf/2502.03519">pdf</a>, <a href="https://arxiv.org/format/2502.03519">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Emission-Line Diagnostics at z>4: [OIII]位4363/H纬 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Backhaus%2C+B+E">Bren E. Backhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Trump%2C+J+R">Jonathan R. Trump</a>, <a href="/search/astro-ph?searchtype=author&query=Kirkpatrick%2C+A">Allison Kirkpatrick</a>, <a href="/search/astro-ph?searchtype=author&query=Simons%2C+R+C">Raymond C. Simons</a>, <a href="/search/astro-ph?searchtype=author&query=Haro%2C+P+A">Pablo Arrabal Haro</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M+B">Micaela B. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+M">Madisyn Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Calabr%C3%B2%2C+A">Antonello Calabr貌</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+K">Kelcey Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">Michaela Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J+S">Jeyhan S. Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Llerena%2C+M">Mario Llerena</a>, <a href="/search/astro-ph?searchtype=author&query=Pacucci%2C+F">Fabio Pacucci</a>, <a href="/search/astro-ph?searchtype=author&query=Pirzkal%2C+N">Nor Pirzkal</a>, <a href="/search/astro-ph?searchtype=author&query=Papovich%2C+C">Casey Papovich</a>, <a href="/search/astro-ph?searchtype=author&query=Wilkins%2C+S+M">Stephen M. Wilkins</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2502.03519v1-abstract-short" style="display: inline;"> We use JWST Near-Infrared Spectrograph (NIRSpec) observations from the the Cosmic Evolution Early Release survey (CEERS), GLASS-JWST ERS (GLASS), and JWST Advanced Deep Extragalactic Survey (JADES) to measure rest-frame optical emission-line ratios of 90 galaxies at z>4. The stacked spectra of galaxies with and without a broad-line feature reveal a difference in the [OIII]$位$ 4363 and H$纬$ ratios.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.03519v1-abstract-full').style.display = 'inline'; document.getElementById('2502.03519v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.03519v1-abstract-full" style="display: none;"> We use JWST Near-Infrared Spectrograph (NIRSpec) observations from the the Cosmic Evolution Early Release survey (CEERS), GLASS-JWST ERS (GLASS), and JWST Advanced Deep Extragalactic Survey (JADES) to measure rest-frame optical emission-line ratios of 90 galaxies at z>4. The stacked spectra of galaxies with and without a broad-line feature reveal a difference in the [OIII]$位$ 4363 and H$纬$ ratios. This motivated our investigation of the [OIII]/H$纬$ vs [NeIII]/[OII] diagram. We define two AGN/SF classification lines based on 1869 SDSS galaxies at z$\sim$0. After applying a redshift correction to the AGN/SF lines we find 76.8% of BLAGN continue to land in the AGN region of the diagnostic largely due to the [NeIII]/[OII] ratio. However, 40.2% of non-BLAGN land in the AGN region as well, this could be due to star forming galaxies having harder ionization of there are narrow line AGN which are not accounted for. This indicates the potential of the [NeIII]/[OII] ratio to continue classifying galaxies to z$\sim$6. We further inspect galaxies without broad emission lines in each region of [OIII]/H纬vs [NeIII]/[OII] diagram and found that they have slightly stronger CIII]$位$1908 fluxes and equivalent width when landing in the BLAGN region. However, the cause of this higher ionization is unclear. Additionally, we find that BLAGN are characterized by a higher ionization (at constant electron temperature) compared to non-broad line galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.03519v1-abstract-full').style.display = 'none'; document.getElementById('2502.03519v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 8 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.04085">arXiv:2501.04085</a> <span> [<a href="https://arxiv.org/pdf/2501.04085">pdf</a>, <a href="https://arxiv.org/format/2501.04085">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The Cosmic Evolution Early Release Science Survey (CEERS) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M+B">Micaela B. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Haro%2C+P+A">Pablo Arrabal Haro</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+H+C">Henry C. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J+S">Jeyhan S. Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=Kocevski%2C+D+D">Dale D. Kocevski</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Lotz%2C+J+M">Jennifer M. Lotz</a>, <a href="/search/astro-ph?searchtype=author&query=Papovich%2C+C">Casey Papovich</a>, <a href="/search/astro-ph?searchtype=author&query=Perez-Gonzalez%2C+P+G">Pablo G. Perez-Gonzalez</a>, <a href="/search/astro-ph?searchtype=author&query=Pirzkal%2C+N">Nor Pirzkal</a>, <a href="/search/astro-ph?searchtype=author&query=Somerville%2C+R+S">Rachel S. Somerville</a>, <a href="/search/astro-ph?searchtype=author&query=Trump%2C+J+R">Jonathan R. Trump</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+G">Guang Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Yung%2C+L+Y+A">L. Y. Aaron Yung</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">Adriano Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Grazian%2C+A">Andrea Grazian</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">Norman A. Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Kewley%2C+L+J">Lisa J. Kewley</a>, <a href="/search/astro-ph?searchtype=author&query=Kirkpatrick%2C+A">Allison Kirkpatrick</a>, <a href="/search/astro-ph?searchtype=author&query=Larson%2C+R+L">Rebecca L. Larson</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">Laura Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Ravindranath%2C+S">Swara Ravindranath</a>, <a href="/search/astro-ph?searchtype=author&query=Wilkins%2C+S+M">Stephen M. Wilkins</a> , et al. (74 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2501.04085v1-abstract-short" style="display: inline;"> We present the Cosmic Evolution Early Release Science (CEERS) Survey, a 77.2 hour Director's Discretionary Early Release Science Program. CEERS demonstrates, tests, and validates efficient extragalactic surveys using coordinated, overlapping parallel observations with the JWST instrument suite, including NIRCam and MIRI imaging, NIRSpec low (R~100) and medium (R~1000) resolution spectroscopy, and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.04085v1-abstract-full').style.display = 'inline'; document.getElementById('2501.04085v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.04085v1-abstract-full" style="display: none;"> We present the Cosmic Evolution Early Release Science (CEERS) Survey, a 77.2 hour Director's Discretionary Early Release Science Program. CEERS demonstrates, tests, and validates efficient extragalactic surveys using coordinated, overlapping parallel observations with the JWST instrument suite, including NIRCam and MIRI imaging, NIRSpec low (R~100) and medium (R~1000) resolution spectroscopy, and NIRCam slitless grism (R~1500) spectroscopy. CEERS targets the Hubble Space Telescope-observed region of the Extended Groth Strip (EGS) field, supported by a rich set of multiwavelength data. CEERS facilitated immediate community science in both of the extragalactic core JWST science drivers ``First Light" and ``Galaxy Assembly," including: 1) The discovery and characterization of large samples of galaxies at z >~ 10 from ~90 arcmin^2 of NIRCam imaging, constraining their abundance and physical nature; 2) Deep spectra of >1000 galaxies, including dozens of galaxies at 6<z<10, enabling redshift measurements and constraints on the physical conditions of star-formation and black hole growth via line diagnostics; 3) Quantifying the first bulge, bar and disk structures at z>3; and 4) Characterizing galaxy mid-IR emission with MIRI to study dust-obscured star-formation and supermassive black hole growth at z~1-3. As a legacy product for the community, the CEERS team has provided several data releases, accompanied by detailed notes on the data reduction procedures and notebooks to aid in reproducibility. In addition to an overview of the survey and quality of the data, we provide science highlights from the first two years with CEERS data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.04085v1-abstract-full').style.display = 'none'; document.getElementById('2501.04085v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">38 pages, 13 figures, 6 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.01358">arXiv:2412.01358</a> <span> [<a href="https://arxiv.org/pdf/2412.01358">pdf</a>, <a href="https://arxiv.org/format/2412.01358">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The ionizing photon production efficiency of star-forming galaxies at $z\sim 4-10$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Llerena%2C+M">M. Llerena</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+L">L. Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Mascia%2C+S">S. Mascia</a>, <a href="/search/astro-ph?searchtype=author&query=Amor%C3%ADn%2C+R">R. Amor铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Calabr%C3%B2%2C+A">A. Calabr貌</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">N. J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Giavalisco%2C+M">M. Giavalisco</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">N. A. Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N+P">N. P. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">M. Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">A. M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Nanayakkara%2C+T">T. Nanayakkara</a>, <a href="/search/astro-ph?searchtype=author&query=Pacucci%2C+F">F. Pacucci</a>, <a href="/search/astro-ph?searchtype=author&query=Shen%2C+L">L. Shen</a>, <a href="/search/astro-ph?searchtype=author&query=Wilkins%2C+S+M">S. M. Wilkins</a>, <a href="/search/astro-ph?searchtype=author&query=Yoon%2C+I">I. Yoon</a>, <a href="/search/astro-ph?searchtype=author&query=Yung%2C+L+Y+A">L. Y. A. Yung</a>, <a href="/search/astro-ph?searchtype=author&query=Bhatawdekar%2C+R">R. Bhatawdekar</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+R+A">R. A. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+X">X. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Haro%2C+P+A">P. Arrabal Haro</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M+B">M. B. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">S. L. Finkelstein</a> , et al. (4 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.01358v1-abstract-short" style="display: inline;"> Investigating the ionizing emission of star-forming galaxies is critical to understanding their contribution to reionization and their impact on the surrounding environment. The number of ionizing photons available to reionize the intergalactic medium (IGM) depends not only on the abundance of galaxies but also on their efficiency in producing ionizing photons ($尉_{ion}$). We aim to estimate the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.01358v1-abstract-full').style.display = 'inline'; document.getElementById('2412.01358v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.01358v1-abstract-full" style="display: none;"> Investigating the ionizing emission of star-forming galaxies is critical to understanding their contribution to reionization and their impact on the surrounding environment. The number of ionizing photons available to reionize the intergalactic medium (IGM) depends not only on the abundance of galaxies but also on their efficiency in producing ionizing photons ($尉_{ion}$). We aim to estimate the $尉_{ion}$ using Balmer lines in a sample of 731 galaxies at $4\leq z \leq 10$ selected from different JWST surveys. We used the available HST and JWST photometry to perform a SED fitting in the sample to determine their physical properties. We used the BAGPIPES code and assumed a delayed exponential model for the star formation history. We used the NIRSpec spectra from prism or grating configurations to estimate Balmer luminosities and then constrained $尉_{ion}$ values after dust correction. We find a mean value of 10$^{25.23}$Hz erg$^{-1}$ for $尉_{ion}$ in the sample with an observed scatter of 0.42dex. We find an increase in the median values of $尉_{ion}$ which confirms the redshift evolution of $尉_{ion}$ found in other works. Regarding the relation with physical properties, we find a decrease of $尉_{ion}$ with increasing stellar mass, indicating that low-mass galaxies are efficient producers of ionizing photons. We also find an increase of $尉_{ion}$ with increasing specific star formation rate (sSFR) and increasing UV absolute magnitude, which indicates that faint galaxies and with high sSFR are also efficient producers. We also investigated the relation of $尉_{ion}$ with the EW([OIII]$位$5007) and find that galaxies with the higher EW([OIII]) are the more efficient producers of ionizing photons. Similarly, we find that galaxies with higher O32 ratios and lower gas-phase metallicities (based on the R23 calibration) show higher $尉_{ion}$ values. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.01358v1-abstract-full').style.display = 'none'; document.getElementById('2412.01358v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to A&A. Comments are welcome</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.12005">arXiv:2411.12005</a> <span> [<a href="https://arxiv.org/pdf/2411.12005">pdf</a>, <a href="https://arxiv.org/format/2411.12005">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Exploring the Nature of Little Red Dots: Constraints on AGN and Stellar Contributions from PRIMER MIRI Imaging </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Leung%2C+G+C+K">Gene C. K. Leung</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Gonz%C3%A1lez%2C+P+G">Pablo G. P茅rez-Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Morales%2C+A+M">Alexa M. Morales</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+A+J">Anthony J. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=Barro%2C+G">Guillermo Barro</a>, <a href="/search/astro-ph?searchtype=author&query=Kocevski%2C+D+D">Dale D. Kocevski</a>, <a href="/search/astro-ph?searchtype=author&query=Akins%2C+H+B">Hollis B. Akins</a>, <a href="/search/astro-ph?searchtype=author&query=Carnall%2C+A+C">Adam C. Carnall</a>, <a href="/search/astro-ph?searchtype=author&query=Ortiz%2C+%C3%93+A+C">脫scar A. Ch谩vez Ortiz</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Cullen%2C+F">Fergus Cullen</a>, <a href="/search/astro-ph?searchtype=author&query=Donnan%2C+C+T">Callum T. Donnan</a>, <a href="/search/astro-ph?searchtype=author&query=Dunlop%2C+J+S">James S. Dunlop</a>, <a href="/search/astro-ph?searchtype=author&query=Ellis%2C+R+S">Richard S. Ellis</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">Norman A. Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">Michaela Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Kokorev%2C+V">Vasily Kokorev</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+R+A">Ray A. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=McLeod%2C+D+J">Derek J. McLeod</a>, <a href="/search/astro-ph?searchtype=author&query=Papovich%2C+C">Casey Papovich</a>, <a href="/search/astro-ph?searchtype=author&query=Yung%2C+L+Y+A">L. Y. Aaron Yung</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.12005v2-abstract-short" style="display: inline;"> JWST has revealed a large population of compact, red galaxies at $z>4$ known as Little Red Dots (LRDs). We analyze the spectral energy distributions (SEDs) of 95 LRDs from the JWST PRIMER survey with complete photometric coverage from $1-18\ 渭$m using NIRCam and MIRI imaging, representing the most extensive SED analysis on a large LRD sample with long-wavelength MIRI data. We examine SED models in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.12005v2-abstract-full').style.display = 'inline'; document.getElementById('2411.12005v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.12005v2-abstract-full" style="display: none;"> JWST has revealed a large population of compact, red galaxies at $z>4$ known as Little Red Dots (LRDs). We analyze the spectral energy distributions (SEDs) of 95 LRDs from the JWST PRIMER survey with complete photometric coverage from $1-18\ 渭$m using NIRCam and MIRI imaging, representing the most extensive SED analysis on a large LRD sample with long-wavelength MIRI data. We examine SED models in which either galaxy or active galactic nucleus (AGN) emission dominates the rest-frame UV or optical continuum, extracting physical properties to explore each scenario's implications. In the galaxy-only model, we find massive, dusty stellar populations alongside unobscured, low-mass components, hinting at inhomogeneous obscuration. The AGN-only model indicates dusty, luminous AGNs with low hot dust fractions compared to typical quasars. A hybrid AGN and galaxy model suggests low-mass, unobscured galaxies in the UV, with stellar mass estimates spanning $\sim$2 dex across the different models, underscoring the need for caution in interpreting LRD stellar masses. With MIRI photometry, the galaxy-only model produces stellar masses within cosmological limits, but extremely high stellar mass densities are inferred. The hybrid model infers highly overmassive black holes exceeding those in recently reported high-redshift AGNs, hinting at a partial AGN contribution to the rest-optical continuum or widespread super-Eddington accretion. Our findings highlight the extreme conditions required for both AGN or galaxy dominated scenarios in LRDs, supporting a mixed contribution to the red continuum, or novel scenarios to explain the observed emission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.12005v2-abstract-full').style.display = 'none'; document.getElementById('2411.12005v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 10 figures, submitted to ApJ. Machine-readable form of Table 2 available at: https://github.com/geneckleung/lrd_primer_miri</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.08100">arXiv:2411.08100</a> <span> [<a href="https://arxiv.org/pdf/2411.08100">pdf</a>, <a href="https://arxiv.org/format/2411.08100">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ad9909">10.3847/1538-4357/ad9909 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Unveiling the Dark Side of UV/Optical Bright Galaxies: Optically Thick Dust Absorption </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+Y">Yingjie Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Giavalisco%2C+M">Mauro Giavalisco</a>, <a href="/search/astro-ph?searchtype=author&query=Backhaus%2C+B+E">Bren E. Backhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Bhatawdekar%2C+R">Rachana Bhatawdekar</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Costantin%2C+L">Luca Costantin</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">Emanuele Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">Michaela Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">Benne W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+R+A">Ray A. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Pacucci%2C+F">Fabio Pacucci</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Gonz%C3%A1lez%2C+P+G">Pablo G. P茅rez-Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Rodighiero%2C+G">Giulia Rodighiero</a>, <a href="/search/astro-ph?searchtype=author&query=Seill%C3%A9%2C+L">Lise-Marie Seill茅</a>, <a href="/search/astro-ph?searchtype=author&query=Whitaker%2C+K+E">Katherine E. Whitaker</a>, <a href="/search/astro-ph?searchtype=author&query=Yung%2C+L+Y+A">L. Y. Aaron Yung</a>, <a href="/search/astro-ph?searchtype=author&query=Haro%2C+P+A">Pablo Arrabal Haro</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M+B">Micaela B. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J+S">Jeyhan S. Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=Papovich%2C+C">Casey Papovich</a>, <a href="/search/astro-ph?searchtype=author&query=Pirzkal%2C+N">Nor Pirzkal</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.08100v1-abstract-short" style="display: inline;"> Over the past decades, a population of galaxies invisible in optical/near-infrared, but bright at longer wavelengths, have been identified through color selections. These so-called optically faint/dark galaxies are considered to be massive quiescent galaxies or highly dust-attenuated galaxies. Having the entire galaxy obscured by dust, however, is likely an extreme case of the much more common occ… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.08100v1-abstract-full').style.display = 'inline'; document.getElementById('2411.08100v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.08100v1-abstract-full" style="display: none;"> Over the past decades, a population of galaxies invisible in optical/near-infrared, but bright at longer wavelengths, have been identified through color selections. These so-called optically faint/dark galaxies are considered to be massive quiescent galaxies or highly dust-attenuated galaxies. Having the entire galaxy obscured by dust, however, is likely an extreme case of the much more common occurrence of optically thin and thick absorption coexisting in the same system. With the power of JWST imaging, we are able to spatially resolve massive galaxies at z~3, accurately model their spectral energy distributions, and identify candidate optically thick substructures. We target galaxies with log(M*/Msun)>10.3 and 2.5<z<3.5, and get 486 galaxies in CEERS and PRIMER fields. Based on excess NIR luminosity, we identify 162 galaxies (~33\% of the parent sample) as candidate hosts of optically thick substructures. We then carry out spatially resolved SED modeling to explore the physical properties of those dark substructures and estimate the amount of optically thick obscuration. We find that optically thick dust is ubiquitous in normal massive galaxies with a wide variety of SFR and morphology. 10-20\% of the stellar mass/SFR are unaccounted for in our selected galaxies, and the fraction is insensitive to stellar mass or SFR. The dark substructures are generally dustier than the rest of the galaxies and are irregularly distributed, arguing against an obscured AGN as the source of the NIR excess. A correlation between the obscured luminosity and the presence of a recent starburst in the past <100 Myr is also observed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.08100v1-abstract-full').style.display = 'none'; document.getElementById('2411.08100v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 18 figures, submitted to ApJ, responses to the referee report sent</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal, 2025, Volume 979, Issue 1, id.71 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.03424">arXiv:2411.03424</a> <span> [<a href="https://arxiv.org/pdf/2411.03424">pdf</a>, <a href="https://arxiv.org/format/2411.03424">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Little Red Dots at an Inflection Point: Ubiquitous "V-Shaped" Turnover Consistently Occurs at the Balmer Limit </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Setton%2C+D+J">David J. Setton</a>, <a href="/search/astro-ph?searchtype=author&query=Greene%2C+J+E">Jenny E. Greene</a>, <a href="/search/astro-ph?searchtype=author&query=de+Graaff%2C+A">Anna de Graaff</a>, <a href="/search/astro-ph?searchtype=author&query=Ma%2C+Y">Yilun Ma</a>, <a href="/search/astro-ph?searchtype=author&query=Leja%2C+J">Joel Leja</a>, <a href="/search/astro-ph?searchtype=author&query=Matthee%2C+J">Jorryt Matthee</a>, <a href="/search/astro-ph?searchtype=author&query=Bezanson%2C+R">Rachel Bezanson</a>, <a href="/search/astro-ph?searchtype=author&query=Boogaard%2C+L+A">Leindert A. Boogaard</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Katz%2C+H">Harley Katz</a>, <a href="/search/astro-ph?searchtype=author&query=Labbe%2C+I">Ivo Labbe</a>, <a href="/search/astro-ph?searchtype=author&query=Maseda%2C+M+V">Michael V. Maseda</a>, <a href="/search/astro-ph?searchtype=author&query=McConachie%2C+I">Ian McConachie</a>, <a href="/search/astro-ph?searchtype=author&query=Miller%2C+T+B">Tim B. Miller</a>, <a href="/search/astro-ph?searchtype=author&query=Price%2C+S+H">Sedona H. Price</a>, <a href="/search/astro-ph?searchtype=author&query=Suess%2C+K+A">Katherine A. Suess</a>, <a href="/search/astro-ph?searchtype=author&query=van+Dokkum%2C+P">Pieter van Dokkum</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+B">Bingjie Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Weibel%2C+A">Andrea Weibel</a>, <a href="/search/astro-ph?searchtype=author&query=Whitaker%2C+K+E">Katherine E. Whitaker</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+C+C">Christina C. Williams</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.03424v1-abstract-short" style="display: inline;"> Among the most puzzling early discoveries of JWST are "Little Red Dots" -- compact red sources that host broad Balmer emission lines and, in many cases, exhibit a "V shaped" change in slope in the rest-optical. The physical properties of Little Red Dots currently have order-of-magnitude uncertainties, because models to explain the continuum of these sources differ immensely. Here, we leverage the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.03424v1-abstract-full').style.display = 'inline'; document.getElementById('2411.03424v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.03424v1-abstract-full" style="display: none;"> Among the most puzzling early discoveries of JWST are "Little Red Dots" -- compact red sources that host broad Balmer emission lines and, in many cases, exhibit a "V shaped" change in slope in the rest-optical. The physical properties of Little Red Dots currently have order-of-magnitude uncertainties, because models to explain the continuum of these sources differ immensely. Here, we leverage the complete selection of red sources in the RUBIES program, supplemented with public PRISM spectra, to study the origin of this "V shape". By fitting a broken power law with a flexible inflection point, we find that a large fraction (20/44, nearly all spatially unresolved) of extremely red H$伪$ emitters at $2<z<6$ exhibit a strong change in slope, and that all strong inflections appear associated with the Balmer limit ($0.3645$ $渭$m). Using a simple model of a reddened AGN with an unobscured scattered light component, we demonstrate that the observed "V shape" in Little Red Dots is unlikely to occur at any specific wavelength if the entire continuum is dominated by light from a power law AGN continuum. In contrast, models with an intrinsic feature at the Balmer limit, such as those that are dominated by evolved stellar populations in the rest-UV-to-optical, can produce the observed spectral shapes, provided that a reddened component picks up sufficiently redward of the break. While no model can comfortably explain the full Little Red Dot spectral energy distribution, the common inflection location suggests that it is most likely a single component that consistently dominates the rest-UV-to-optical in Little Red Dots, and that this component is associated with $T\sim10^4$ K hydrogen due to the clear preference for a break at H$_\infty$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.03424v1-abstract-full').style.display = 'none'; document.getElementById('2411.03424v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 5 figures. Submitted to ApJ, comments welcome!</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.23349">arXiv:2410.23349</a> <span> [<a href="https://arxiv.org/pdf/2410.23349">pdf</a>, <a href="https://arxiv.org/format/2410.23349">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/adb28d">10.3847/2041-8213/adb28d <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> NGDEEP: The Star Formation and Ionization Properties of Galaxies at $1.7 < z < 3.4$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shen%2C+L">Lu Shen</a>, <a href="/search/astro-ph?searchtype=author&query=Papovich%2C+C">Casey Papovich</a>, <a href="/search/astro-ph?searchtype=author&query=Matharu%2C+J">Jasleen Matharu</a>, <a href="/search/astro-ph?searchtype=author&query=Pirzkal%2C+N">Nor Pirzkal</a>, <a href="/search/astro-ph?searchtype=author&query=Hu%2C+W">Weida Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Berg%2C+D+A">Danielle A. Berg</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M+B">Micaela B. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Backhaus%2C+B+E">Bren E. Backhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N+P">Nimish P. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Huertas-Company%2C+M">Marc Huertas-Company</a>, <a href="/search/astro-ph?searchtype=author&query=Hutchison%2C+T+A">Taylor A. Hutchison</a>, <a href="/search/astro-ph?searchtype=author&query=Giavalisco%2C+M">Mauro Giavalisco</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">Norman A. Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Jaskot%2C+A+E">Anne E. Jaskot</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+I">Intae Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J+S">Jeyhan S. Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Lotz%2C+J+M">Jennifer M. Lotz</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Gonz%C3%A1lez%2C+P+G">Pablo G. P茅rez-Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Rothberg%2C+B">Barry Rothberg</a>, <a href="/search/astro-ph?searchtype=author&query=Simons%2C+R+C">Raymond C. Simons</a>, <a href="/search/astro-ph?searchtype=author&query=Vanderhoof%2C+B+N">Brittany N. Vanderhoof</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.23349v2-abstract-short" style="display: inline;"> We use JWST/NIRISS slitless spectroscopy from the Next Generation Deep Extragalactic Exploratory Public (NGDEEP) Survey to investigate the physical condition of star-forming galaxies at $1.7 < z < 3.4$. At these redshifts, the deep NGDEEP NIRISS slitless spectroscopy covers the [O II]$位位$3726,3729, [O III]$位位$4959,5007, H$尾$ and H$伪$ emission features for galaxies with stellar masses… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.23349v2-abstract-full').style.display = 'inline'; document.getElementById('2410.23349v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.23349v2-abstract-full" style="display: none;"> We use JWST/NIRISS slitless spectroscopy from the Next Generation Deep Extragalactic Exploratory Public (NGDEEP) Survey to investigate the physical condition of star-forming galaxies at $1.7 < z < 3.4$. At these redshifts, the deep NGDEEP NIRISS slitless spectroscopy covers the [O II]$位位$3726,3729, [O III]$位位$4959,5007, H$尾$ and H$伪$ emission features for galaxies with stellar masses $\log(\mathrm{M_\ast/M_\odot}) \gtrsim 7$, nearly a factor of a hundred lower than previous studies. We focus on the [O III]/[O II] (O$_{32}$) ratio which is primarily sensitive to the ionization state and with a secondary dependence on the gas-phase metallicity of the interstellar medium. We find significant ($\gtrsim5蟽$) correlations between the O$_{32}$ ratio and galaxy properties as O$_{32}$ increases with decreasing stellar mass, decreasing star formation rate (SFR), increasing specific SFR (sSFR$\equiv \mathrm{SFR}/M_*$), and increasing equivalent width (EW) of H$尾$ and H$伪$. These trends suggest a tight connection between the ionization parameter and these galaxy properties. Galaxies at $z\sim2-3$ exhibit a higher O$_{32}$ than local normal galaxies with the same stellar masses and SFRs, indicating that they have a higher ionization parameter and lower metallicity than local normal galaxies. In addition, we observe a mild evolutionary trend in the O$_{32}$ -- EW(H$尾$) relation from $z\sim0$ to $z\gtrsim5$, where higher redshift galaxies show increased O$_{32}$ and EW, with possibly higher O$_{32}$ at fixed EW. We argue that both the enhanced recent star formation activity and the higher star formation surface density may contribute to the increase in O$_{32}$ and the ionization parameter. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.23349v2-abstract-full').style.display = 'none'; document.getElementById('2410.23349v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">31 pages, 12 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.10954">arXiv:2410.10954</a> <span> [<a href="https://arxiv.org/pdf/2410.10954">pdf</a>, <a href="https://arxiv.org/format/2410.10954">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202452604">10.1051/0004-6361/202452604 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spectroscopic confirmation of a dust-obscured, metal-rich dwarf galaxy at z~5 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bisigello%2C+L">L. Bisigello</a>, <a href="/search/astro-ph?searchtype=author&query=Gandolfi%2C+G">G. Gandolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Feltre%2C+A">A. Feltre</a>, <a href="/search/astro-ph?searchtype=author&query=Haro%2C+P+A">P. Arrabal Haro</a>, <a href="/search/astro-ph?searchtype=author&query=Calabr%C3%B2%2C+A">A. Calabr貌</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">N. J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Costantin%2C+L">L. Costantin</a>, <a href="/search/astro-ph?searchtype=author&query=Girardi%2C+G">G. Girardi</a>, <a href="/search/astro-ph?searchtype=author&query=Giulietti%2C+M">M. Giulietti</a>, <a href="/search/astro-ph?searchtype=author&query=Grazian%2C+A">A. Grazian</a>, <a href="/search/astro-ph?searchtype=author&query=Gruppioni%2C+C">C. Gruppioni</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N+P">N. P. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">B. W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Llerena%2C+M">M. Llerena</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+R+A">R. A. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Pacucci%2C+F">F. Pacucci</a>, <a href="/search/astro-ph?searchtype=author&query=Prandoni%2C+I">I. Prandoni</a>, <a href="/search/astro-ph?searchtype=author&query=Rodighiero%2C+G">G. Rodighiero</a>, <a href="/search/astro-ph?searchtype=author&query=Seill%C3%A9%2C+L+-">L. -M. Seill茅</a>, <a href="/search/astro-ph?searchtype=author&query=Wilkins%2C+S+M">S. M. Wilkins</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M">M. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson.%2C+M">M. Dickinson.</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">S. L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J">J. Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">A. M. Koekemoer</a> , et al. (2 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.10954v2-abstract-short" style="display: inline;"> We present the first spectroscopic confirmation of a dust-obscured dwarf galaxy, CEERS-14821. The analysis is performed combining JWST NIRCam broad-band photometry and NIRSpec/PRISM spectroscopic data. From the detection of multiple rest-frame optical lines, we derive that CEERS-14821 is located at $z=4.883\pm0.003$. Moreover, from a secure detection of the $H_伪$ and $H_尾$ we derived that the gala… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.10954v2-abstract-full').style.display = 'inline'; document.getElementById('2410.10954v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.10954v2-abstract-full" style="display: none;"> We present the first spectroscopic confirmation of a dust-obscured dwarf galaxy, CEERS-14821. The analysis is performed combining JWST NIRCam broad-band photometry and NIRSpec/PRISM spectroscopic data. From the detection of multiple rest-frame optical lines, we derive that CEERS-14821 is located at $z=4.883\pm0.003$. Moreover, from a secure detection of the $H_伪$ and $H_尾$ we derived that the galaxy has a dust extinction ranging from Av=2.2 to Av=3.3, depending on the assumed reddening law. This value is extremely large given that we estimated a low stellar mass around log(M/Mo)=8.0-8.2. Moreover, using different metallicity tracers, we verify that the galaxy is also metal-rich, with 12+log(O/H)>8.3. This is well above the expectation from both the mass-metallicity relation and the fundamental mass-metalliticy relation. CEERS-14821 is going through a burst of star formation, there are no indications of a strong contribution from an active galactic nuclei (f(AGN)<0.5 with respect to the total dust luminosity). Based on the rest-frame optical images, this source has a size compatible with galaxies of similar stellar mass and redshift. Finally, with the current data, it seems that there are galaxies closely interacting with CEERS-14821. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.10954v2-abstract-full').style.display = 'none'; document.getElementById('2410.10954v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 12 figures. Accepted by A&A on the 13th of December 2024</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 693, L18 (2025) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.08387">arXiv:2410.08387</a> <span> [<a href="https://arxiv.org/pdf/2410.08387">pdf</a>, <a href="https://arxiv.org/format/2410.08387">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> RUBIES: JWST/NIRSpec resolves evolutionary phases of dusty star-forming galaxies at $z\sim2$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cooper%2C+O+R">Olivia R. Cooper</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">Gabriel Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Heintz%2C+K+E">Kasper E. Heintz</a>, <a href="/search/astro-ph?searchtype=author&query=Toft%2C+S">Sune Toft</a>, <a href="/search/astro-ph?searchtype=author&query=Casey%2C+C+M">Caitlin M. Casey</a>, <a href="/search/astro-ph?searchtype=author&query=Setton%2C+D+J">David J. Setton</a>, <a href="/search/astro-ph?searchtype=author&query=de+Graaff%2C+A">Anna de Graaff</a>, <a href="/search/astro-ph?searchtype=author&query=Boogaard%2C+L">Leindert Boogaard</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Gillman%2C+S">Steven Gillman</a>, <a href="/search/astro-ph?searchtype=author&query=Gottumukkala%2C+R">Rashmi Gottumukkala</a>, <a href="/search/astro-ph?searchtype=author&query=Greene%2C+J+E">Jenny E. Greene</a>, <a href="/search/astro-ph?searchtype=author&query=Gullberg%2C+B">Bitten Gullberg</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">Michaela Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Hviding%2C+R+E">Raphael E. Hviding</a>, <a href="/search/astro-ph?searchtype=author&query=Lambrides%2C+E">Erini Lambrides</a>, <a href="/search/astro-ph?searchtype=author&query=Leja%2C+J">Joel Leja</a>, <a href="/search/astro-ph?searchtype=author&query=Long%2C+A+S">Arianna S. Long</a>, <a href="/search/astro-ph?searchtype=author&query=Manning%2C+S+M">Sinclaire M. Manning</a>, <a href="/search/astro-ph?searchtype=author&query=Maseda%2C+M+V">Michael V. Maseda</a>, <a href="/search/astro-ph?searchtype=author&query=McConachie%2C+I">Ian McConachie</a>, <a href="/search/astro-ph?searchtype=author&query=McKinney%2C+J">Jed McKinney</a>, <a href="/search/astro-ph?searchtype=author&query=Narayanan%2C+D">Desika Narayanan</a>, <a href="/search/astro-ph?searchtype=author&query=Price%2C+S+H">Sedona H. Price</a>, <a href="/search/astro-ph?searchtype=author&query=Strait%2C+V">Victoria Strait</a> , et al. (2 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.08387v1-abstract-short" style="display: inline;"> The dearth of high quality spectroscopy of dusty star-forming galaxies (DSFGs) -- the main drivers of the assembly of dust and stellar mass at the peak of activity in the Universe -- greatly hinders our ability to interpret their physical processes and evolutionary pathways. We present JWST/NIRSpec observations from RUBIES of four submillimeter-selected, ALMA-detected DSFGs at cosmic noon,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.08387v1-abstract-full').style.display = 'inline'; document.getElementById('2410.08387v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.08387v1-abstract-full" style="display: none;"> The dearth of high quality spectroscopy of dusty star-forming galaxies (DSFGs) -- the main drivers of the assembly of dust and stellar mass at the peak of activity in the Universe -- greatly hinders our ability to interpret their physical processes and evolutionary pathways. We present JWST/NIRSpec observations from RUBIES of four submillimeter-selected, ALMA-detected DSFGs at cosmic noon, $z\sim2.3-2.7$. While photometry uniformly suggests vigorous ongoing star formation for the entire sample in line with canonical DSFGs, the spectra differ: one source has spectroscopic evidence of an evolved stellar population, indicating a recent transition to a post-starburst phase, while the remainder show strong spectroscopic signatures of ongoing starbursts. All four galaxies are infrared-luminous (log$_{10}$$L_{\rm{IR}}$/L$_{\rm \odot}$ $>12.4$), massive (log$_{10}\,M_\star$/M$_{\rm \odot}$ $>11$), and very dust-obscured ($A_V\sim3-4$ ABmag). Leveraging detections of multiple Balmer and Paschen lines, we derive an optical attenuation curve consistent with Calzetti overall, yet an optical extinction ratio $R_V\sim2.5$, potentially indicating smaller dust grains or differences in star-dust geometry. This case study provides some of the first detailed spectroscopic evidence that the DSFGs encompass a heterogeneous sample spanning a range of star formation properties and evolutionary stages, and illustrates the advantages of synergistic JWST and ALMA analysis of DSFGs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.08387v1-abstract-full').style.display = 'none'; document.getElementById('2410.08387v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 4 figures; submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.07340">arXiv:2410.07340</a> <span> [<a href="https://arxiv.org/pdf/2410.07340">pdf</a>, <a href="https://arxiv.org/format/2410.07340">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Here There Be (Dusty) Monsters: High Redshift AGN are Dustier Than Their Hosts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+M">Madisyn Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Simons%2C+R+C">Raymond C. Simons</a>, <a href="/search/astro-ph?searchtype=author&query=Trump%2C+J+R">Jonathan R. Trump</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+A+J">Anthony J. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=Backhaus%2C+B">Bren Backhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+K">Kelcey Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Buat%2C+V">V茅ronique Buat</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">Michaela Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">Benne W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Kocevski%2C+D+D">Dale D. Kocevski</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+R+A">Ray A. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Pacucci%2C+F">Fabio Pacucci</a>, <a href="/search/astro-ph?searchtype=author&query=Seill%C3%A9%2C+L">Lise-Marie Seill茅</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.07340v1-abstract-short" style="display: inline;"> JWST spectroscopy has discovered a population of $z \gtrsim 3.5$ galaxies with broad Balmer emission lines, and narrow forbidden lines, that are consistent with hosting active galactic nuclei (AGN). Many of these systems, now known as ``little red dots" (LRDs), are compact and have unique colors that are very red in the optical/near-infrared and blue in the ultraviolet. The relative contribution o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.07340v1-abstract-full').style.display = 'inline'; document.getElementById('2410.07340v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.07340v1-abstract-full" style="display: none;"> JWST spectroscopy has discovered a population of $z \gtrsim 3.5$ galaxies with broad Balmer emission lines, and narrow forbidden lines, that are consistent with hosting active galactic nuclei (AGN). Many of these systems, now known as ``little red dots" (LRDs), are compact and have unique colors that are very red in the optical/near-infrared and blue in the ultraviolet. The relative contribution of galaxy starlight and AGN to these systems remains uncertain, especially for the galaxies with unusual blue+red spectral energy distributions. In this work, we use Balmer decrements to measure the independent dust attenuation of the broad and narrow emission-line components of a sample of 29 broad-line AGN identified from three public JWST spectroscopy surveys: CEERS, JADES, and RUBIES. Stacking the narrow components from the spectra of 25 sources with broad H$\rm伪$ and no broad H$\rm尾$ results in a median narrow H$\rm伪$/H$\rm尾$ = $2.47^{+0.05}_{-0.05}$ (consistent with $A_{v} = 0$) and broad H$\rm伪$/H$\rm尾$ $> 8.85$ ($A_{v} > 3.63$). The narrow and broad Balmer decrements imply little-to-no attenuation of the narrow emission lines, which are consistent with being powered by star formation and located on larger physical scales. Meanwhile, the lower limit in broad H$\rm伪$/H$\rm尾$ decrement, with broad H$\rm尾$ undetected in the stacked spectrum of 25 broad-H$\rm伪$ AGN, implies significant dust attenuation of the broad-line emitting region that is presumably associated with the central AGN. Our results indicate that these systems, on average, are consistent with heavily dust-attenuated AGN powering the red parts of their SED while their blue UV emission is powered by unattenuated star formation in the host galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.07340v1-abstract-full').style.display = 'none'; document.getElementById('2410.07340v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">4 figures, 3 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.03784">arXiv:2410.03784</a> <span> [<a href="https://arxiv.org/pdf/2410.03784">pdf</a>, <a href="https://arxiv.org/format/2410.03784">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Emission-Line Ratios and Ionization Conditions of CEERS Star-Forming Galaxies with JWST/NIRSpec </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gupta%2C+A+R">Ansh R. Gupta</a>, <a href="/search/astro-ph?searchtype=author&query=Kirkpatrick%2C+A">Allison Kirkpatrick</a>, <a href="/search/astro-ph?searchtype=author&query=Fernandez%2C+V">Vital Fernandez</a>, <a href="/search/astro-ph?searchtype=author&query=Haro%2C+P+A">Pablo Arrabal Haro</a>, <a href="/search/astro-ph?searchtype=author&query=Backhaus%2C+B+E">Bren E. Backhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">Norman A. Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.03784v1-abstract-short" style="display: inline;"> Galaxy emission-line fluxes can be analyzed to determine star formation rates (SFR) and ISM ionization. Here, we investigate rest-frame optical emission lines of 71 star-forming galaxies at redshift 0.7 < z < 7 from the Cosmic Evolution Early Release Science (CEERS) survey using JWST/NIRSpec. We use H$伪$ line fluxes to measure SFRs. We combine these with HST CANDELS stellar mass estimates to deter… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.03784v1-abstract-full').style.display = 'inline'; document.getElementById('2410.03784v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.03784v1-abstract-full" style="display: none;"> Galaxy emission-line fluxes can be analyzed to determine star formation rates (SFR) and ISM ionization. Here, we investigate rest-frame optical emission lines of 71 star-forming galaxies at redshift 0.7 < z < 7 from the Cosmic Evolution Early Release Science (CEERS) survey using JWST/NIRSpec. We use H$伪$ line fluxes to measure SFRs. We combine these with HST CANDELS stellar mass estimates to determine the redshift evolution of specific SFR (sSFR) and compare our sample with the star-forming galaxy main sequence. We create [O III]$位$5008/H$尾$ versus [Ne III]$位$3870/[O II]$位$3728 line ratio diagrams and correlate these ratios with sSFR and the distance of each galaxy from the main sequence (excess sSFR). We find a modest correlation between the line ratios and sSFR, which is consistent with previous work analyzing similar samples. However, we find a weak correlation between the line ratios and excess sSFR. Taken together, our results suggest that sSFR is the parameter that governs ionization conditions rather than SFR or a galaxy's distance from the main sequence. These measurements reveal a rich diversity of ISM conditions and physical galaxy properties throughout cosmic time. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.03784v1-abstract-full').style.display = 'none'; document.getElementById('2410.03784v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, 1 figure. Submitted to Research Notes of the American Astronomical Society</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.06772">arXiv:2409.06772</a> <span> [<a href="https://arxiv.org/pdf/2409.06772">pdf</a>, <a href="https://arxiv.org/format/2409.06772">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Broad-Line AGN at $3.5<z<6$: The Black Hole Mass Function and a Connection with Little Red Dots </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+A+J">Anthony J. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Kocevski%2C+D+D">Dale D. Kocevski</a>, <a href="/search/astro-ph?searchtype=author&query=Jeon%2C+J">Junehyoung Jeon</a>, <a href="/search/astro-ph?searchtype=author&query=Bromm%2C+V">Volker Bromm</a>, <a href="/search/astro-ph?searchtype=author&query=Amorin%2C+R+O">Ricardo O. Amorin</a>, <a href="/search/astro-ph?searchtype=author&query=Haro%2C+P+A">Pablo Arrabal Haro</a>, <a href="/search/astro-ph?searchtype=author&query=Backhaus%2C+B+E">Bren E. Backhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M+B">Micaela B. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Ba%C3%B1ados%2C+E">Eduardo Ba帽ados</a>, <a href="/search/astro-ph?searchtype=author&query=Bhatawdekar%2C+R">Rachana Bhatawdekar</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+M">Madisyn Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Calabro%2C+A">Antonello Calabro</a>, <a href="/search/astro-ph?searchtype=author&query=Ortiz%2C+O+A+C">Oscar A. Chavez Ortiz</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+Y">Yingjie Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+J+W">Justin W. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+K">Kelcey Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Donnan%2C+C">Callum Donnan</a>, <a href="/search/astro-ph?searchtype=author&query=Dunlop%2C+J+S">James S. Dunlop</a>, <a href="/search/astro-ph?searchtype=author&query=Ellis%2C+R+S">Richard S. Ellis</a>, <a href="/search/astro-ph?searchtype=author&query=Fernandez%2C+V">Vital Fernandez</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">Adriano Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Fujimoto%2C+S">Seiji Fujimoto</a> , et al. (26 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.06772v1-abstract-short" style="display: inline;"> We present a sample of 50 H-alpha detected broad-line active galactic nuclei (BLAGN) at redshifts 3.5<z<6.8 using data from the CEERS and RUBIES surveys. We select these sources directly from JWST/NIRSpec G395M/F290LP spectra. We use a multi-step pre-selection and a Bayesian fitting procedure to ensure a high-quality sample of sources with broad Balmer lines and narrow forbidden lines. We compute… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.06772v1-abstract-full').style.display = 'inline'; document.getElementById('2409.06772v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.06772v1-abstract-full" style="display: none;"> We present a sample of 50 H-alpha detected broad-line active galactic nuclei (BLAGN) at redshifts 3.5<z<6.8 using data from the CEERS and RUBIES surveys. We select these sources directly from JWST/NIRSpec G395M/F290LP spectra. We use a multi-step pre-selection and a Bayesian fitting procedure to ensure a high-quality sample of sources with broad Balmer lines and narrow forbidden lines. We compute rest-frame ultraviolet and optical spectral slopes for these objects, and determine that 10 BLAGN in our sample are also little red dots (LRDs). These LRD BLAGN, when examined in aggregate, show broader H-alpha line profiles and a higher fraction of broad-to-narrow component H-alpha emission than non-LRD BLAGN. Moreover, we find that ~66% of these objects are intrinsically reddened (beta (optical)>0), independent of the contributions of emission lines to the broadband photometry. We construct the black hole (BH) mass function at 3.5<z<6 after computing robust observational and line detection completeness corrections. This BH mass function shows broad agreement with both recent JWST/NIRSpec and JWST/NIRCam WFSS based BH mass functions, though we extend these earlier results to log(M(BH)/M(sun)) < 7. The derived BH mass function is consistent with a variety of theoretical models, indicating that the observed abundance of black holes in the early universe is not discrepant with physically-motivated predictions. The BH mass function shape resembles a largely featureless power-law, suggesting that any signature from black-hole seeding has been lost by redshift z~5-6. Finally, we compute the BLAGN UV luminosity function and find good agreement with JWST-detected BLAGN samples from recent works, finding that BLAGN hosts constitute <10% of the total observed UV luminosity at all but the brightest luminosities. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.06772v1-abstract-full').style.display = 'none'; document.getElementById('2409.06772v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 14 figures, 4 tables. Submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.05948">arXiv:2409.05948</a> <span> [<a href="https://arxiv.org/pdf/2409.05948">pdf</a>, <a href="https://arxiv.org/format/2409.05948">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> RUBIES: a complete census of the bright and red distant Universe with JWST/NIRSpec </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=de+Graaff%2C+A">Anna de Graaff</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">Gabriel Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Weibel%2C+A">Andrea Weibel</a>, <a href="/search/astro-ph?searchtype=author&query=Lewis%2C+Z">Zach Lewis</a>, <a href="/search/astro-ph?searchtype=author&query=Maseda%2C+M+V">Michael V. Maseda</a>, <a href="/search/astro-ph?searchtype=author&query=Oesch%2C+P+A">Pascal A. Oesch</a>, <a href="/search/astro-ph?searchtype=author&query=Bezanson%2C+R">Rachel Bezanson</a>, <a href="/search/astro-ph?searchtype=author&query=Boogaard%2C+L+A">Leindert A. Boogaard</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Cooper%2C+O+R">Olivia R. Cooper</a>, <a href="/search/astro-ph?searchtype=author&query=Gottumukkala%2C+R">Rashmi Gottumukkala</a>, <a href="/search/astro-ph?searchtype=author&query=Greene%2C+J+E">Jenny E. Greene</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">Michaela Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Hviding%2C+R+E">Raphael E. Hviding</a>, <a href="/search/astro-ph?searchtype=author&query=Katz%2C+H">Harley Katz</a>, <a href="/search/astro-ph?searchtype=author&query=Labb%C3%A9%2C+I">Ivo Labb茅</a>, <a href="/search/astro-ph?searchtype=author&query=Leja%2C+J">Joel Leja</a>, <a href="/search/astro-ph?searchtype=author&query=Matthee%2C+J">Jorryt Matthee</a>, <a href="/search/astro-ph?searchtype=author&query=McConachie%2C+I">Ian McConachie</a>, <a href="/search/astro-ph?searchtype=author&query=Miller%2C+T+B">Tim B. Miller</a>, <a href="/search/astro-ph?searchtype=author&query=Naidu%2C+R+P">Rohan P. Naidu</a>, <a href="/search/astro-ph?searchtype=author&query=Price%2C+S+H">Sedona H. Price</a>, <a href="/search/astro-ph?searchtype=author&query=Rix%2C+H">Hans-Walter Rix</a>, <a href="/search/astro-ph?searchtype=author&query=Setton%2C+D+J">David J. Setton</a>, <a href="/search/astro-ph?searchtype=author&query=Suess%2C+K+A">Katherine A. Suess</a> , et al. (3 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.05948v2-abstract-short" style="display: inline;"> We present the Red Unknowns: Bright Infrared Extragalactic Survey (RUBIES), providing JWST/NIRSpec spectroscopy of red sources selected across ~150 arcmin$^2$ from public JWST/NIRCam imaging in the UDS and EGS fields. RUBIES novel observing strategy offers a well-quantified selection function: the survey is optimised to reach high (>70%) completeness for bright and red (F150W-F444W>2) sources that… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.05948v2-abstract-full').style.display = 'inline'; document.getElementById('2409.05948v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.05948v2-abstract-full" style="display: none;"> We present the Red Unknowns: Bright Infrared Extragalactic Survey (RUBIES), providing JWST/NIRSpec spectroscopy of red sources selected across ~150 arcmin$^2$ from public JWST/NIRCam imaging in the UDS and EGS fields. RUBIES novel observing strategy offers a well-quantified selection function: the survey is optimised to reach high (>70%) completeness for bright and red (F150W-F444W>2) sources that are very rare. To place these rare sources in context, we simultaneously observe a reference sample of the 2<z<7 galaxy population, sampling sources at a rate that is inversely proportional to their number density in the 3D space of F444W magnitude, F150W-F444W colour, and photometric redshift. In total, RUBIES observes ~3000 targets across $1<z_{phot}<10$ with both the PRISM and G395M dispersers, and ~1500 targets at $z_{phot}>3$ using only the G395M disperser. The RUBIES data reveal a highly diverse population of red sources that span a broad redshift range ($z_{spec}\sim1-9$), with photometric redshift scatter and outlier fraction that are 3 times higher than for similarly bright sources that are less red. This diversity is not apparent from the photometric SEDs. Only spectroscopy reveals that the SEDs encompass a mixture of galaxies with dust-obscured star formation, extreme line emission, a lack of star formation indicating early quenching, and luminous active galactic nuclei. As a first demonstration of our broader selection function we compare the stellar masses and rest-frame U-V colours of the red sources and our reference sample: red sources are typically more massive ($M_*\sim10^{10-11.5} M_\odot$) across all redshifts. However, we find that the most massive systems span a wide range in U-V colour. We describe our data reduction procedure and data quality, and publicly release the reduced RUBIES data and vetted spectroscopic redshifts of the first half of the survey through the DJA. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.05948v2-abstract-full').style.display = 'none'; document.getElementById('2409.05948v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 March, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 16 figures; accepted for publication in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.03829">arXiv:2409.03829</a> <span> [<a href="https://arxiv.org/pdf/2409.03829">pdf</a>, <a href="https://arxiv.org/format/2409.03829">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> RUBIES Reveals a Massive Quiescent Galaxy at z=7.3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Weibel%2C+A">Andrea Weibel</a>, <a href="/search/astro-ph?searchtype=author&query=de+Graaff%2C+A">Anna de Graaff</a>, <a href="/search/astro-ph?searchtype=author&query=Setton%2C+D+J">David J. Setton</a>, <a href="/search/astro-ph?searchtype=author&query=Miller%2C+T+B">Tim B. Miller</a>, <a href="/search/astro-ph?searchtype=author&query=Oesch%2C+P+A">Pascal A. Oesch</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">Gabriel Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Lagos%2C+C+D+P">Claudia D. P. Lagos</a>, <a href="/search/astro-ph?searchtype=author&query=Whitaker%2C+K+E">Katherine E. Whitaker</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+C+C">Christina C. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Baggen%2C+J+F+W">Josephine F. W. Baggen</a>, <a href="/search/astro-ph?searchtype=author&query=Bezanson%2C+R">Rachel Bezanson</a>, <a href="/search/astro-ph?searchtype=author&query=Boogaard%2C+L+A">Leindert A. Boogaard</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Greene%2C+J+E">Jenny E. Greene</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">Michaela Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Hviding%2C+R+E">Raphael E. Hviding</a>, <a href="/search/astro-ph?searchtype=author&query=Kuruvanthodi%2C+A">Adarsh Kuruvanthodi</a>, <a href="/search/astro-ph?searchtype=author&query=Labb%C3%A9%2C+I">Ivo Labb茅</a>, <a href="/search/astro-ph?searchtype=author&query=Leja%2C+J">Joel Leja</a>, <a href="/search/astro-ph?searchtype=author&query=Maseda%2C+M+V">Michael V. Maseda</a>, <a href="/search/astro-ph?searchtype=author&query=Matthee%2C+J">Jorryt Matthee</a>, <a href="/search/astro-ph?searchtype=author&query=McConachie%2C+I">Ian McConachie</a>, <a href="/search/astro-ph?searchtype=author&query=Naidu%2C+R+P">Rohan P. Naidu</a>, <a href="/search/astro-ph?searchtype=author&query=Roberts-Borsani%2C+G">Guido Roberts-Borsani</a>, <a href="/search/astro-ph?searchtype=author&query=Schaerer%2C+D">Daniel Schaerer</a> , et al. (4 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.03829v2-abstract-short" style="display: inline;"> We report the spectroscopic discovery of a massive quiescent galaxy at $z_{\rm spec}=7.29\pm0.01$, just $\sim700\,$Myr after the Big Bang. RUBIES-UDS-QG-z7 was selected from public JWST/NIRCam and MIRI imaging from the PRIMER survey and observed with JWST/NIRSpec as part of RUBIES. The NIRSpec/PRISM spectrum reveals one of the strongest Balmer breaks observed thus far at $z>6$, no emission lines,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.03829v2-abstract-full').style.display = 'inline'; document.getElementById('2409.03829v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.03829v2-abstract-full" style="display: none;"> We report the spectroscopic discovery of a massive quiescent galaxy at $z_{\rm spec}=7.29\pm0.01$, just $\sim700\,$Myr after the Big Bang. RUBIES-UDS-QG-z7 was selected from public JWST/NIRCam and MIRI imaging from the PRIMER survey and observed with JWST/NIRSpec as part of RUBIES. The NIRSpec/PRISM spectrum reveals one of the strongest Balmer breaks observed thus far at $z>6$, no emission lines, but tentative Balmer and Ca absorption features, as well as a Lyman break. Simultaneous modeling of the NIRSpec/PRISM spectrum and NIRCam and MIRI photometry (spanning $0.9-18\,渭m$) shows that the galaxy formed a stellar mass of log$(M_*/M_\odot)=10.23^{+0.04}_{-0.04}$ before $z\sim8$, and ceased forming stars $50-100\,$Myr prior to the time of observation, resulting in $\log(\rm{sSFR/Gyr}^{-1})<-1$. We measure a small physical size of $209_{-24}^{+33}\,{\rm pc}$, which implies a high stellar mass surface density within the effective radius of $\log(危_{*,\rm e}/M_\odot\,kpc^{-2})=10.85_{-0.12}^{+0.11}$ comparable to the highest densities measured in quiescent galaxies at $z\sim2-5$. The 3D stellar mass density profile of RUBIES-UDS-QG-z7 is remarkably similar to the central densities of local massive ellipticals, suggesting that at least some of their cores may have already been in place at $z>7$. The discovery of RUBIES-UDS-QG-z7 has strong implications for galaxy formation models: the estimated number density of quiescent galaxies at $z\sim7$ is $>100\times$ larger than predicted from any model to date, indicating that quiescent galaxies have formed earlier than previously expected. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.03829v2-abstract-full').style.display = 'none'; document.getElementById('2409.03829v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 8 figures, accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.03189">arXiv:2408.03189</a> <span> [<a href="https://arxiv.org/pdf/2408.03189">pdf</a>, <a href="https://arxiv.org/format/2408.03189">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> 21 Balmer Jump Street: The Nebular Continuum at High Redshift and Implications for the Bright Galaxy Problem, UV Continuum Slopes, and Early Stellar Populations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Katz%2C+H">Harley Katz</a>, <a href="/search/astro-ph?searchtype=author&query=Cameron%2C+A+J">Alex J. Cameron</a>, <a href="/search/astro-ph?searchtype=author&query=Saxena%2C+A">Aayush Saxena</a>, <a href="/search/astro-ph?searchtype=author&query=Barrufet%2C+L">Laia Barrufet</a>, <a href="/search/astro-ph?searchtype=author&query=Choustikov%2C+N">Nicholas Choustikov</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=de+Graaff%2C+A">Anna de Graaff</a>, <a href="/search/astro-ph?searchtype=author&query=Ellis%2C+R+S">Richard S. Ellis</a>, <a href="/search/astro-ph?searchtype=author&query=Fosbury%2C+R+A+E">Robert A. E. Fosbury</a>, <a href="/search/astro-ph?searchtype=author&query=Heintz%2C+K+E">Kasper E. Heintz</a>, <a href="/search/astro-ph?searchtype=author&query=Maseda%2C+M">Michael Maseda</a>, <a href="/search/astro-ph?searchtype=author&query=Matthee%2C+J">Jorryt Matthee</a>, <a href="/search/astro-ph?searchtype=author&query=McConchie%2C+I">Ian McConchie</a>, <a href="/search/astro-ph?searchtype=author&query=Oesch%2C+P+A">Pascal A. Oesch</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.03189v2-abstract-short" style="display: inline;"> We study, from both a theoretical and observational perspective, the physical origin and spectroscopic impact of extreme nebular emission in high-redshift galaxies. The nebular continuum, which can appear during extreme starbursts, is of particular importance as it tends to redden UV slopes and has a significant contribution to the UV luminosities of galaxies. Furthermore, its shape can be used to… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.03189v2-abstract-full').style.display = 'inline'; document.getElementById('2408.03189v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.03189v2-abstract-full" style="display: none;"> We study, from both a theoretical and observational perspective, the physical origin and spectroscopic impact of extreme nebular emission in high-redshift galaxies. The nebular continuum, which can appear during extreme starbursts, is of particular importance as it tends to redden UV slopes and has a significant contribution to the UV luminosities of galaxies. Furthermore, its shape can be used to infer the gas density and temperature of the ISM. First, we provide a theoretical background, showing how different stellar populations (SPS models, IMFs, and stellar temperatures) and nebular conditions impact observed galaxy spectra. We demonstrate that, for systems with strong nebular continuum emission, 1) UV fluxes can increase by up to 0.7~magnitudes (or more in the case of hot/massive stars) above the stellar continuum, which may help reconcile the surprising abundance of bright high-redshift galaxies and the elevated UV luminosity density at $z>10$, 2) at high gas densities, UV slopes can redden from $尾\lesssim-2.5$ to $尾\sim-1$, 3) observational measurements of $尉_{ion}$ are grossly underestimated, and 4) UV downturns from two-photon emission can masquerade as DLAs. Second, we present a dataset of 58 galaxies observed with NIRSpec on JWST at $2.5<z<9.0$ that are selected to have strong nebular continuum emission via the detection of the Balmer jump. Five of the 58 spectra are consistent with being dominated by nebular emission, exhibiting both a Balmer jump and a UV downturn consistent with two-photon emission. For some galaxies, this may imply the presence of hot massive stars and a top-heavy IMF. We conclude by exploring the properties of spectroscopically confirmed $z>10$ galaxies, finding that UV slopes and UV downturns are in some cases redder or steeper than expected from SPS models, which may hint at more exotic (e.g. hotter/more massive stars or AGN) ionizing sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.03189v2-abstract-full').style.display = 'none'; document.getElementById('2408.03189v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">26 pages, 18 figures, submitted to The Open Journal of Astrophysics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.21279">arXiv:2407.21279</a> <span> [<a href="https://arxiv.org/pdf/2407.21279">pdf</a>, <a href="https://arxiv.org/format/2407.21279">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> CEERS Key Paper. IX. Identifying Galaxy Mergers in CEERS NIRCam Images Using Random Forests and Convolutional Neural Networks </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rose%2C+C">Caitlin Rose</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J+S">Jeyhan S. Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=Snyder%2C+G+F">Gregory F. Snyder</a>, <a href="/search/astro-ph?searchtype=author&query=Huertas-Company%2C+M">Marc Huertas-Company</a>, <a href="/search/astro-ph?searchtype=author&query=Yung%2C+L+Y+A">L. Y. Aaron Yung</a>, <a href="/search/astro-ph?searchtype=author&query=Haro%2C+P+A">Pablo Arrabal Haro</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M+B">Micaela B. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Bisigello%2C+L">Laura Bisigello</a>, <a href="/search/astro-ph?searchtype=author&query=Calabr%C3%B2%2C+A">Antonello Calabr貌</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+H+C">Henry C. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">Adriano Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Grazian%2C+A">Andrea Grazian</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">Norman A. Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">Benne W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Iyer%2C+K+G">Kartheik G. Iyer</a>, <a href="/search/astro-ph?searchtype=author&query=Kewley%2C+L+J">Lisa J. Kewley</a>, <a href="/search/astro-ph?searchtype=author&query=Kirkpatrick%2C+A">Allison Kirkpatrick</a>, <a href="/search/astro-ph?searchtype=author&query=Kocevski%2C+D+D">Dale D. Kocevski</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Lotz%2C+J+M">Jennifer M. Lotz</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+R+A">Ray A. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Napolitan%2C+L">Lorenzo Napolitan</a> , et al. (10 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.21279v1-abstract-short" style="display: inline;"> A crucial yet challenging task in galaxy evolution studies is the identification of distant merging galaxies, a task which suffers from a variety of issues ranging from telescope sensitivities and limitations to the inherently chaotic morphologies of young galaxies. In this paper, we use random forests and convolutional neural networks to identify high-redshift JWST CEERS galaxy mergers. We train… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.21279v1-abstract-full').style.display = 'inline'; document.getElementById('2407.21279v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.21279v1-abstract-full" style="display: none;"> A crucial yet challenging task in galaxy evolution studies is the identification of distant merging galaxies, a task which suffers from a variety of issues ranging from telescope sensitivities and limitations to the inherently chaotic morphologies of young galaxies. In this paper, we use random forests and convolutional neural networks to identify high-redshift JWST CEERS galaxy mergers. We train these algorithms on simulated $3<z<5$ CEERS galaxies created from the IllustrisTNG subhalo morphologies and the Santa Cruz SAM lightcone. We apply our models to observed CEERS galaxies at $3<z<5$. We find that our models correctly classify $\sim60-70\%$ of simulated merging and non-merging galaxies; better performance on the merger class comes at the expense of misclassifying more non-mergers. We could achieve more accurate classifications, as well as test for the dependency on physical parameters such as gas fraction, mass ratio, and relative orbits, by curating larger training sets. When applied to real CEERS galaxies using visual classifications as ground truth, the random forests correctly classified $40-60\%$ of mergers and non-mergers at $3<z<4$, but tended to classify most objects as non-mergers at $4<z<5$ (misclassifying $\sim70\%$ of visually-classified mergers). On the other hand, the CNNs tended to classify most objects as mergers across all redshifts (misclassifying $80-90\%$ of visually-classified non-mergers). We investigate what features the models find most useful, as well as characteristics of false positives and false negatives, and also calculate merger rates derived from the identifications made by the models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.21279v1-abstract-full').style.display = 'none'; document.getElementById('2407.21279v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 14 figures, submitted to ApJL</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.01473">arXiv:2405.01473</a> <span> [<a href="https://arxiv.org/pdf/2405.01473">pdf</a>, <a href="https://arxiv.org/format/2405.01473">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/ad55f7">10.3847/2041-8213/ad55f7 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> RUBIES: Evolved Stellar Populations with Extended Formation Histories at $z \sim 7-8$ in Candidate Massive Galaxies Identified with JWST/NIRSpec </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wang%2C+B">Bingjie Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Leja%2C+J">Joel Leja</a>, <a href="/search/astro-ph?searchtype=author&query=de+Graaff%2C+A">Anna de Graaff</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G+B">Gabriel B. Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Weibel%2C+A">Andrea Weibel</a>, <a href="/search/astro-ph?searchtype=author&query=van+Dokkum%2C+P">Pieter van Dokkum</a>, <a href="/search/astro-ph?searchtype=author&query=Baggen%2C+J+F+W">Josephine F. W. Baggen</a>, <a href="/search/astro-ph?searchtype=author&query=Suess%2C+K+A">Katherine A. Suess</a>, <a href="/search/astro-ph?searchtype=author&query=Greene%2C+J+E">Jenny E. Greene</a>, <a href="/search/astro-ph?searchtype=author&query=Bezanson%2C+R">Rachel Bezanson</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">Michaela Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Labbe%2C+I">Ivo Labbe</a>, <a href="/search/astro-ph?searchtype=author&query=Matthee%2C+J">Jorryt Matthee</a>, <a href="/search/astro-ph?searchtype=author&query=McConachie%2C+I">Ian McConachie</a>, <a href="/search/astro-ph?searchtype=author&query=Naidu%2C+R+P">Rohan P. Naidu</a>, <a href="/search/astro-ph?searchtype=author&query=Nelson%2C+E">Erica Nelson</a>, <a href="/search/astro-ph?searchtype=author&query=Oesch%2C+P+A">Pascal A. Oesch</a>, <a href="/search/astro-ph?searchtype=author&query=Setton%2C+D+J">David J. Setton</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+C+C">Christina C. Williams</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.01473v2-abstract-short" style="display: inline;"> The identification of red, apparently massive galaxies at $z>7$ in early JWST photometry suggests a strongly accelerated timeline compared to standard models of galaxy growth. A major uncertainty in the interpretation is whether the red colors are caused by evolved stellar populations, dust, or other effects such as emission lines or AGN. Here we show that three of the massive galaxy candidates at… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.01473v2-abstract-full').style.display = 'inline'; document.getElementById('2405.01473v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.01473v2-abstract-full" style="display: none;"> The identification of red, apparently massive galaxies at $z>7$ in early JWST photometry suggests a strongly accelerated timeline compared to standard models of galaxy growth. A major uncertainty in the interpretation is whether the red colors are caused by evolved stellar populations, dust, or other effects such as emission lines or AGN. Here we show that three of the massive galaxy candidates at $z=6.7-8.4$ have prominent Balmer breaks in JWST/NIRSpec spectroscopy from the RUBIES program. The Balmer breaks demonstrate unambiguously that stellar emission dominates at $位_{\rm rest} = 0.4\,渭$m, and require formation histories extending hundreds of Myr into the past in galaxies only 600--800 Myr after the Big Bang. Two of the three galaxies also show broad Balmer lines, with H$尾$ FWHM $>2500~{\rm km\,s^{-1}}$, suggesting that dust-reddened AGN contribute to, or even dominate, the SEDs of these galaxies at $位_{\rm rest}\gtrsim 0.6\,渭$m. All three galaxies have relatively narrow [O III] lines, seemingly ruling out a high-mass interpretation if the lines arise in dynamically-relaxed, inclined disks. Yet, the inferred masses also remain highly uncertain. We model the high-quality spectra using Prospector to decompose the continuum into stellar and AGN components, and explore limiting cases in stellar/AGN contribution. This produces a wide range of possible stellar masses, spanning $M_\star \sim 10^9 - 10^{11}\,{\rm M_{\odot}}$. Nevertheless, all fits suggest a very early and rapid formation, most of which follow with a truncation in star formation. Potential origins and evolutionary tracks for these objects are discussed, from the cores of massive galaxies to low-mass galaxies with over-massive black holes. Intriguingly, we find all of these explanations to be incomplete; deeper and redder data are needed to understand the physics of these systems. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.01473v2-abstract-full').style.display = 'none'; document.getElementById('2405.01473v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJL; 20 pages, 10 figures, 1 table</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal Letters, 969, L13 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.09659">arXiv:2404.09659</a> <span> [<a href="https://arxiv.org/pdf/2404.09659">pdf</a>, <a href="https://arxiv.org/format/2404.09659">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202450373">10.1051/0004-6361/202450373 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Physical properties of strong 1 < z < 3 Balmer and Paschen lines emitters observed with JWST </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Seill%C3%A9%2C+L+-">L. -M. Seill茅</a>, <a href="/search/astro-ph?searchtype=author&query=Buat%2C+V">V. Buat</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez%2C+V">V. Fern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Boquien%2C+M">M. Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Roehlly%2C+Y">Y. Roehlly</a>, <a href="/search/astro-ph?searchtype=author&query=Boselli%2C+A">A. Boselli</a>, <a href="/search/astro-ph?searchtype=author&query=Calabr%C3%B2%2C+A">A. Calabr貌</a>, <a href="/search/astro-ph?searchtype=author&query=Amor%C3%ADn%2C+R+O">R. O. Amor铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Backhaus%2C+B+E">B. E. Backhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Burgarella%2C+D">D. Burgarella</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">N. J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">M. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N+P">N. P. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">B. W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">A. M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+L">L. Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Pacucci%2C+F">F. Pacucci</a>, <a href="/search/astro-ph?searchtype=author&query=Robertson%2C+C">C. Robertson</a>, <a href="/search/astro-ph?searchtype=author&query=Yung%2C+L+Y+A">L. Y. A. Yung</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.09659v3-abstract-short" style="display: inline;"> The ultraviolet continuum traces young stars while the near-infrared unveils older stellar populations and dust-obscured regions. Balmer emission lines provide insights on gas properties and young stellar objects but are highly affected by dust attenuation. The near-infrared Paschen lines suffer less dust attenuation and can be used to measure star formation rates (SFRs) in star-forming regions ob… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.09659v3-abstract-full').style.display = 'inline'; document.getElementById('2404.09659v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.09659v3-abstract-full" style="display: none;"> The ultraviolet continuum traces young stars while the near-infrared unveils older stellar populations and dust-obscured regions. Balmer emission lines provide insights on gas properties and young stellar objects but are highly affected by dust attenuation. The near-infrared Paschen lines suffer less dust attenuation and can be used to measure star formation rates (SFRs) in star-forming regions obscured by dust clouds. We select 13 sources between redshifts 1 and 3 observed with HST, JWST/NIRCam and NIRSpec based on the availability of at least one Balmer and one Paschen line with S/N > 5. With a newly-developed version of CIGALE, we fit their hydrogen line equivalent widths (EWs) and photometric data. We assess the impacts of the removal of spectroscopic data by comparing the quality of the fits of the spectro-photometric data to those with photometric data only. We compare the single (BC03) vs binary (BPASS) stellar populations models in the fitting process of spectro-photometric data. We derive the differential attenuation and explore different attenuation recipes by fitting spectro-photometric data with BC03. For each stellar model and for each input dataset (with and without EWs), we quantify the deviation on the SFRs and stellar masses from the "standard" choice. On average, the SFRs are overestimated and the stellar masses are underestimated when EWs are not included as input data. We find a major contribution of the H$伪$ emission line to the broadband photometric measurements of our sources, and a trend of increasing contribution with specific SFR. Using the BPASS models has a significant impact on the derived SFRs and stellar masses. We show that a flexible attenuation recipe provides more accurate estimates of the dust attenuation parameters, especially the differential attenuation which agrees with the original value of Charlot & Fall (2000). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.09659v3-abstract-full').style.display = 'none'; document.getElementById('2404.09659v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted in Astronomy & Astrophysics, 19 pages, 15 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 689, A102 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.05683">arXiv:2404.05683</a> <span> [<a href="https://arxiv.org/pdf/2404.05683">pdf</a>, <a href="https://arxiv.org/format/2404.05683">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Efficient formation of a massive quiescent galaxy at redshift 4.9 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=de+Graaff%2C+A">Anna de Graaff</a>, <a href="/search/astro-ph?searchtype=author&query=Setton%2C+D+J">David J. Setton</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">Gabriel Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Cutler%2C+S">Sam Cutler</a>, <a href="/search/astro-ph?searchtype=author&query=Suess%2C+K+A">Katherine A. Suess</a>, <a href="/search/astro-ph?searchtype=author&query=Labbe%2C+I">Ivo Labbe</a>, <a href="/search/astro-ph?searchtype=author&query=Leja%2C+J">Joel Leja</a>, <a href="/search/astro-ph?searchtype=author&query=Weibel%2C+A">Andrea Weibel</a>, <a href="/search/astro-ph?searchtype=author&query=Maseda%2C+M+V">Michael V. Maseda</a>, <a href="/search/astro-ph?searchtype=author&query=Whitaker%2C+K+E">Katherine E. Whitaker</a>, <a href="/search/astro-ph?searchtype=author&query=Bezanson%2C+R">Rachel Bezanson</a>, <a href="/search/astro-ph?searchtype=author&query=Boogaard%2C+L+A">Leindert A. Boogaard</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=De+Lucia%2C+G">Gabriella De Lucia</a>, <a href="/search/astro-ph?searchtype=author&query=Franx%2C+M">Marijn Franx</a>, <a href="/search/astro-ph?searchtype=author&query=Greene%2C+J+E">Jenny E. Greene</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">Michaela Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Matthee%2C+J">Jorryt Matthee</a>, <a href="/search/astro-ph?searchtype=author&query=McConachie%2C+I">Ian McConachie</a>, <a href="/search/astro-ph?searchtype=author&query=Naidu%2C+R+P">Rohan P. Naidu</a>, <a href="/search/astro-ph?searchtype=author&query=Oesch%2C+P+A">Pascal A. Oesch</a>, <a href="/search/astro-ph?searchtype=author&query=Price%2C+S+H">Sedona H. Price</a>, <a href="/search/astro-ph?searchtype=author&query=Rix%2C+H">Hans-Walter Rix</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">Francesco Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+B">Bingjie Wang</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.05683v3-abstract-short" style="display: inline;"> Within the established framework of structure formation, galaxies start as systems of low stellar mass and gradually grow into far more massive galaxies. The existence of massive galaxies in the first billion years of the Universe, suggested by recent observations, appears to challenge this model, as such galaxies would require highly efficient conversion of baryons into stars. An even greater cha… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.05683v3-abstract-full').style.display = 'inline'; document.getElementById('2404.05683v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.05683v3-abstract-full" style="display: none;"> Within the established framework of structure formation, galaxies start as systems of low stellar mass and gradually grow into far more massive galaxies. The existence of massive galaxies in the first billion years of the Universe, suggested by recent observations, appears to challenge this model, as such galaxies would require highly efficient conversion of baryons into stars. An even greater challenge in this epoch is the existence of massive galaxies that have already ceased forming stars. However, robust detections of early massive quiescent galaxies have been challenging due to the coarse wavelength sampling of photometric surveys. Here we report the spectroscopic confirmation with the James Webb Space Telescope of the quiescent galaxy RUBIES-EGS-QG-1 at redshift $z=4.90$, 1.2 billion years after the Big Bang. Deep stellar absorption features in the spectrum reveal that the galaxy's stellar mass of $10^{11}\,M_\odot$, corroborated by the mass implied by its gas kinematics, formed in a short $200\,$Myr burst of star formation, after which star formation activity dropped rapidly and persistently. According to current galaxy formation models, systems with such rapid stellar mass growth and early quenching are too rare to plausibly occur in the small area probed spectroscopically with JWST. Instead, the discovery of RUBIES-EGS-QG-1 implies that early massive quiescent galaxies can be quenched earlier or exhaust gas available for star formation more efficiently than currently assumed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.05683v3-abstract-full').style.display = 'none'; document.getElementById('2404.05683v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.03576">arXiv:2404.03576</a> <span> [<a href="https://arxiv.org/pdf/2404.03576">pdf</a>, <a href="https://arxiv.org/ps/2404.03576">ps</a>, <a href="https://arxiv.org/format/2404.03576">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The Rise of Faint, Red AGN at $z>4$: A Sample of Little Red Dots in the JWST Extragalactic Legacy Fields </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kocevski%2C+D+D">Dale D. Kocevski</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Barro%2C+G">Guillermo Barro</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+A+J">Anthony J. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=Calabr%C3%B2%2C+A">Antonello Calabr貌</a>, <a href="/search/astro-ph?searchtype=author&query=Laloux%2C+B">Brivael Laloux</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+J">Johannes Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Trump%2C+J+R">Jonathan R. Trump</a>, <a href="/search/astro-ph?searchtype=author&query=Leung%2C+G+C+K">Gene C. K. Leung</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+G">Guang Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Gonz%C3%A1lez%2C+P+G">Pablo G. P茅rez-Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Pacucci%2C+F">Fabio Pacucci</a>, <a href="/search/astro-ph?searchtype=author&query=Inayoshi%2C+K">Kohei Inayoshi</a>, <a href="/search/astro-ph?searchtype=author&query=Somerville%2C+R+S">Rachel S. Somerville</a>, <a href="/search/astro-ph?searchtype=author&query=McGrath%2C+E+J">Elizabeth J. McGrath</a>, <a href="/search/astro-ph?searchtype=author&query=Akins%2C+H+B">Hollis B. Akins</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M+B">Micaela B. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Bisigello%2C+L">Laura Bisigello</a>, <a href="/search/astro-ph?searchtype=author&query=Bowler%2C+R+A+A">Rebecca A. A. Bowler</a>, <a href="/search/astro-ph?searchtype=author&query=Carnall%2C+A">Adam Carnall</a>, <a href="/search/astro-ph?searchtype=author&query=Casey%2C+C+M">Caitlin M. Casey</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+Y">Yingjie Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Costantin%2C+L">Luca Costantin</a> , et al. (32 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.03576v3-abstract-short" style="display: inline;"> We present a sample of 341 "little red dots" (LRDs) spanning the redshift range $z\sim2-11$ using data from the CEERS, PRIMER, JADES, UNCOVER and NGDEEP surveys. Unlike past use of color indices to identify LRDs, we employ continuum slope fitting using shifting bandpasses to sample the same rest-frame emission blueward and redward of the Balmer break. This enables the detection of LRDs over a wide… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03576v3-abstract-full').style.display = 'inline'; document.getElementById('2404.03576v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.03576v3-abstract-full" style="display: none;"> We present a sample of 341 "little red dots" (LRDs) spanning the redshift range $z\sim2-11$ using data from the CEERS, PRIMER, JADES, UNCOVER and NGDEEP surveys. Unlike past use of color indices to identify LRDs, we employ continuum slope fitting using shifting bandpasses to sample the same rest-frame emission blueward and redward of the Balmer break. This enables the detection of LRDs over a wider redshift range and with less contamination from galaxies with strong breaks that otherwise lack a rising red continuum. The redshift distribution of our sample increases at $z<8$ and then undergoes a rapid decline at $z\sim4.5$, which may tie the emergence of these sources to the inside-out growth that galaxies experience during this epoch. We find that LRDs are $\sim1$ dex more numerous than X-ray and UV selected AGN at z~5-7. Within our sample, we have identified the first two X-ray detected LRDs. An X-ray spectral analysis confirms that these AGN are moderately obscured with $\log\,(N_{\rm H}/{\rm cm}^{2}$) of $23.3^{+0.4}_{-1.3}$ and $22.72^{+0.13}_{-0.16}$. Our analysis reveals that reddened AGN emission dominates their rest-optical light, while the rest-UV originates from their host galaxies. We also present NIRSpec observations from the RUBIES survey of 17 LRDs that show broad emission lines consistent with AGN activity. The confirmed AGN fraction of our sample is 71\% for sources with F444W<26.5. In addition, we find three LRDs with blue-shifted Balmer absorption features in their spectra, suggesting an outflow of high-density, low-ionization gas from near the central engine of these faint, red AGN. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03576v3-abstract-full').style.display = 'none'; document.getElementById('2404.03576v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">32 pages, 28 figures, accepted or publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.10491">arXiv:2403.10491</a> <span> [<a href="https://arxiv.org/pdf/2403.10491">pdf</a>, <a href="https://arxiv.org/format/2403.10491">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1038/s41550-024-02397-3">10.1038/s41550-024-02397-3 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A luminous and young galaxy at z=12.33 revealed by a JWST/MIRI detection of H伪 and [OIII] </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zavala%2C+J+A">Jorge A. Zavala</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">Marco Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Akins%2C+H+B">Hollis B. Akins</a>, <a href="/search/astro-ph?searchtype=author&query=Bakx%2C+T+J+L+C">Tom J. L. C. Bakx</a>, <a href="/search/astro-ph?searchtype=author&query=Burgarella%2C+D">Denis Burgarella</a>, <a href="/search/astro-ph?searchtype=author&query=Casey%2C+C+M">Caitlin M. Casey</a>, <a href="/search/astro-ph?searchtype=author&query=Ortiz%2C+%C3%93+A+C">脫scar A. Ch谩vez Ortiz</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Mitsuhashi%2C+I">Ikki Mitsuhashi</a>, <a href="/search/astro-ph?searchtype=author&query=Nakajima%2C+K">Kimihiko Nakajima</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Gonz%C3%A1lez%2C+P+G">Pablo G. P茅rez-Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Haro%2C+P+A">Pablo Arrabal Haro</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">Pietro Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Buat%2C+V">Veronique Buat</a>, <a href="/search/astro-ph?searchtype=author&query=Backhaus%2C+B">Bren Backhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Calabr%C3%B2%2C+A">Antonello Calabr貌</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Arenas%2C+D">David Fern谩ndez-Arenas</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">Adriano Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Franco%2C+M">Maximilien Franco</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">Claudio Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Giavalisco%2C+M">Mauro Giavalisco</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">Norman A. Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N">Nimish Hathi</a> , et al. (15 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.10491v2-abstract-short" style="display: inline;"> The James Webb Space Telescope (JWST) has discovered a surprising population of bright galaxies in the very early universe (<500 Myrs after the Big Bang) that is hard to explain with conventional galaxy formation models and whose physical properties remain to be fully understood. Insight into their internal physics is best captured through nebular lines but, at these early epochs, the brightest of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.10491v2-abstract-full').style.display = 'inline'; document.getElementById('2403.10491v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.10491v2-abstract-full" style="display: none;"> The James Webb Space Telescope (JWST) has discovered a surprising population of bright galaxies in the very early universe (<500 Myrs after the Big Bang) that is hard to explain with conventional galaxy formation models and whose physical properties remain to be fully understood. Insight into their internal physics is best captured through nebular lines but, at these early epochs, the brightest of these spectral features are redshifted into the mid-infrared and remain elusive. Using the JWST Mid-Infrared Instrument, MIRI, here we present the first detection of H伪 and doubly-ionized oxygen ([OIII]5007AA) at z>10. These detections place the bright galaxy GHZ2/GLASS-z12 at z=12.33+/-0.04, making it the most distant astronomical object with direct spectroscopic detection of these lines. These observations provide key insights into the conditions of this primeval, luminous galaxy, which shows hard ionizing conditions rarely seen in the local Universe likely driven by compact and young (~30Myr) burst of star formation. Its oxygen-to-hydrogen abundance is close to a tenth of the solar value, indicating a rapid metal enrichment. This study confirms the unique conditions of this remarkably bright and distant galaxy and the huge potential of mid-IR observations to characterize these objects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.10491v2-abstract-full').style.display = 'none'; document.getElementById('2403.10491v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published in Nature Astronomy on 30 October 2024 (this represents the authors' submitted version)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.05362">arXiv:2403.05362</a> <span> [<a href="https://arxiv.org/pdf/2403.05362">pdf</a>, <a href="https://arxiv.org/format/2403.05362">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202449904">10.1051/0004-6361/202449904 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Physical properties of extreme emission-line galaxies at $z\sim 4-9$ from the JWST CEERS survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Llerena%2C+M">M. Llerena</a>, <a href="/search/astro-ph?searchtype=author&query=Amor%C3%ADn%2C+R">R. Amor铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Haro%2C+P+A">P. Arrabal Haro</a>, <a href="/search/astro-ph?searchtype=author&query=Backhaus%2C+B+E">B. E. Backhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M+B">M. B. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Calabr%C3%B2%2C+A">A. Calabr貌</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">N. J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+K">K. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">M. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">S. L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Gawiser%2C+E">E. Gawiser</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">N. A. Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N+P">N. P. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">M. Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J+S">J. S. Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">A. M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=McGrath%2C+E+J">E. J. McGrath</a>, <a href="/search/astro-ph?searchtype=author&query=Mobasher%2C+B">B. Mobasher</a>, <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+L">L. Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Papovich%2C+C">C. Papovich</a>, <a href="/search/astro-ph?searchtype=author&query=Pirzkal%2C+N">N. Pirzkal</a>, <a href="/search/astro-ph?searchtype=author&query=Trump%2C+J+R">J. R. Trump</a>, <a href="/search/astro-ph?searchtype=author&query=Wilkins%2C+S+M">S. M. Wilkins</a>, <a href="/search/astro-ph?searchtype=author&query=Yung%2C+L+Y+A">L. Y. A. Yung</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.05362v2-abstract-short" style="display: inline;"> Extreme emission line galaxies (EELGs) are typically characterized by high equivalent widths (EWs) which are driven by elevated specific star formation rates (sSFR) in low-mass galaxies with subsolar metallicities and little dust. Such extreme systems are rare in the local universe, but the number density of EELGs increases with redshift. Such starburst galaxies are currently presumed to be the ma… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.05362v2-abstract-full').style.display = 'inline'; document.getElementById('2403.05362v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.05362v2-abstract-full" style="display: none;"> Extreme emission line galaxies (EELGs) are typically characterized by high equivalent widths (EWs) which are driven by elevated specific star formation rates (sSFR) in low-mass galaxies with subsolar metallicities and little dust. Such extreme systems are rare in the local universe, but the number density of EELGs increases with redshift. Such starburst galaxies are currently presumed to be the main drivers of hydrogen reionization over 5.5<z<15, which serves to motivate many of the searches for high-z EELGs. We aim to characterize the physical properties of a sample of ~730 EELGs at 4<z<9 photometrically selected from the CEERS survey using JWST/NIRCam. We validate our method and demonstrate the main physical properties of a subset of EELGs using NIRSpec spectra. We create synthetic NIRCam observations of EELGs using empirical templates based on ~2000 local metal-poor starbursts to select EELGs based on color-color criteria. We study their properties based on SED fitting and flux excess from emission lines in the photometric filters. Our sample has a mean stellar mass of $10^{7.84}$Msun with high sSFRs with a mean value of $10^{-7.03}$ yr$^{-1}$. We consider a delayed-$蟿$ model for the star formation history and find our sample of EELGs are young with a mean value of the time after the onset of star formation of 45Myr. We find that they have similar line ratios to local metal-poor starbursts with high log([OIII]/H$尾$)>0.4-1 which indicates that star formation may be the dominant source of ionization. Based on the photometric fluxes, we find an increase of EW([OIII]+H$尾$) with sSFR and $危_{SFR}$, and a decrease with age and stellar mass. The sample of EELGs can reach $危_{SFR}>$10Msun yr$^{-1}$kpc$^{-2}$ which indicate they are strong candidates of LyC leakers. Another indirect indicator is the high values of O32>5 that can be reached for some galaxies in the sample. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.05362v2-abstract-full').style.display = 'none'; document.getElementById('2403.05362v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A. We updated the manuscript following referee's suggestions</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 691, A59 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.02304">arXiv:2403.02304</a> <span> [<a href="https://arxiv.org/pdf/2403.02304">pdf</a>, <a href="https://arxiv.org/format/2403.02304">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> RUBIES: JWST/NIRSpec Confirmation of an Infrared-luminous, Broad-line Little Red Dot with an Ionized Outflow </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wang%2C+B">Bingjie Wang</a>, <a href="/search/astro-ph?searchtype=author&query=de+Graaff%2C+A">Anna de Graaff</a>, <a href="/search/astro-ph?searchtype=author&query=Davies%2C+R+L">Rebecca L. Davies</a>, <a href="/search/astro-ph?searchtype=author&query=Greene%2C+J+E">Jenny E. Greene</a>, <a href="/search/astro-ph?searchtype=author&query=Leja%2C+J">Joel Leja</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G+B">Gabriel B. Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Goulding%2C+A+D">Andy D. Goulding</a>, <a href="/search/astro-ph?searchtype=author&query=Miller%2C+T+B">Tim B. Miller</a>, <a href="/search/astro-ph?searchtype=author&query=Suess%2C+K+A">Katherine A. Suess</a>, <a href="/search/astro-ph?searchtype=author&query=Weibel%2C+A">Andrea Weibel</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+C+C">Christina C. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Bezanson%2C+R">Rachel Bezanson</a>, <a href="/search/astro-ph?searchtype=author&query=Boogaard%2C+L+A">Leindert A. Boogaard</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">Michaela Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Katz%2C+H">Harley Katz</a>, <a href="/search/astro-ph?searchtype=author&query=Labbe%2C+I">Ivo Labbe</a>, <a href="/search/astro-ph?searchtype=author&query=Maseda%2C+M+V">Michael V. Maseda</a>, <a href="/search/astro-ph?searchtype=author&query=Matthee%2C+J">Jorryt Matthee</a>, <a href="/search/astro-ph?searchtype=author&query=McConachie%2C+I">Ian McConachie</a>, <a href="/search/astro-ph?searchtype=author&query=Naidu%2C+R+P">Rohan P. Naidu</a>, <a href="/search/astro-ph?searchtype=author&query=Oesch%2C+P+A">Pascal A. Oesch</a>, <a href="/search/astro-ph?searchtype=author&query=Rix%2C+H">Hans-Walter Rix</a>, <a href="/search/astro-ph?searchtype=author&query=Setton%2C+D+J">David J. Setton</a>, <a href="/search/astro-ph?searchtype=author&query=Whitaker%2C+K+E">Katherine E. Whitaker</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.02304v4-abstract-short" style="display: inline;"> The JWST discovery of ``little red dots'' (LRDs) is reshaping our picture of the early Universe, yet the physical mechanisms driving their compact size and UV-optical colors remain elusive. Here we report an unusually bright LRD ($z=3.1$) observed as part of the RUBIES program. This LRD exhibits broad emission lines (FWHM $\sim4000$km/s), a blue UV continuum, a clear Balmer break and a red continu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.02304v4-abstract-full').style.display = 'inline'; document.getElementById('2403.02304v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.02304v4-abstract-full" style="display: none;"> The JWST discovery of ``little red dots'' (LRDs) is reshaping our picture of the early Universe, yet the physical mechanisms driving their compact size and UV-optical colors remain elusive. Here we report an unusually bright LRD ($z=3.1$) observed as part of the RUBIES program. This LRD exhibits broad emission lines (FWHM $\sim4000$km/s), a blue UV continuum, a clear Balmer break and a red continuum sampled out to rest 4 $渭$m with MIRI. We develop a new joint galaxy and AGN model within the Prospector Bayesian inference framework and perform spectrophotometric modeling using NIRCam, MIRI, and NIRSpec/Prism observations. Our fiducial model reveals a $M_*\sim 10^9M_\odot$ galaxy alongside a dust-reddened AGN driving the optical emission. Explaining the rest-frame optical color as a reddened AGN requires $A_{\rm v}\gtrsim3$, suggesting that a great majority of the accretion disk energy is re-radiated as dust emission. Yet despite clear AGN signatures, we find a surprising lack of hot torus emission, which implies that either the dust emission in this object must be cold, or the red continuum must instead be driven by a massive, evolved stellar population of the host galaxy -- seemingly inconsistent with the high EW broad lines (H$伪$ EW $\sim800$脜). The widths and luminosities of Pa$尾$, Pa$未$, Pa$纬$, and H$伪$ imply a modest black hole mass of $M_{\rm BH}\sim10^8M_\odot$. Additionally, we identify a narrow blue-shifted HeI absorption in G395M spectra, signaling an ionized outflow with kinetic energy up to $\sim1$\% the luminosity of the AGN. The low redshift of RUBIES-BLAGN-1 combined with the depth and richness of the JWST imaging and spectroscopic observations provide a unique opportunity to build a physical model for these so-far mysterious LRDs, which may prove to be a crucial phase in the early formation of massive galaxies and their supermassive black holes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.02304v4-abstract-full').style.display = 'none'; document.getElementById('2403.02304v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 March, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ; 24 pages, 9 figures, 5 tables. Code implementing the joint galaxy and AGN model is made publicly available online as a part of Prospector; the model used in this work corresponds to the state of the Git repository at commit 1cce164 https://github.com/bd-j/prospector/pull/366</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.17829">arXiv:2402.17829</a> <span> [<a href="https://arxiv.org/pdf/2402.17829">pdf</a>, <a href="https://arxiv.org/format/2402.17829">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202449768">10.1051/0004-6361/202449768 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The evolution of the SFR and Sigma-SFR of galaxies in cosmic morning (4 < z < 10) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Calabr%C3%B2%2C+A">A. Calabr貌</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Santini%2C+P">P. Santini</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrara%2C+A">A. Ferrara</a>, <a href="/search/astro-ph?searchtype=author&query=Llerena%2C+M">M. Llerena</a>, <a href="/search/astro-ph?searchtype=author&query=Mascia%2C+S">S. Mascia</a>, <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+L">L. Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Yung%2C+L+Y+A">L. Y. A. Yung</a>, <a href="/search/astro-ph?searchtype=author&query=Bisigello%2C+L">L. Bisigello</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">N. J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Dekel%2C+A">A. Dekel</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">M. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Franco%2C+M">M. Franco</a>, <a href="/search/astro-ph?searchtype=author&query=Giavalisco%2C+M">M. Giavalisco</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">M. Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">B. W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">A. M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+R+A">R. A. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Pacucci%2C+F">F. Pacucci</a>, <a href="/search/astro-ph?searchtype=author&query=Pirzkal%2C+N">N. Pirzkal</a>, <a href="/search/astro-ph?searchtype=author&query=Roberts-Borsani%2C+G">G. Roberts-Borsani</a>, <a href="/search/astro-ph?searchtype=author&query=Seill%C3%A9%2C+L+M">L. M. Seill茅</a>, <a href="/search/astro-ph?searchtype=author&query=Tacchella%2C+S">S. Tacchella</a>, <a href="/search/astro-ph?searchtype=author&query=Wilkins%2C+S">S. Wilkins</a> , et al. (6 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2402.17829v2-abstract-short" style="display: inline;"> The galaxy integrated star-formation rate (SFR) surface density ($危_{\rm SFR}$) has been proposed as a valuable diagnostic of the mass accumulation in galaxies as being more tightly related to the physics of star-formation (SF) and stellar feedback than other SF indicators. In this paper, we assemble a statistical sample of 230 galaxies observed with JWST in the GLASS and CEERS spectroscopic surve… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.17829v2-abstract-full').style.display = 'inline'; document.getElementById('2402.17829v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.17829v2-abstract-full" style="display: none;"> The galaxy integrated star-formation rate (SFR) surface density ($危_{\rm SFR}$) has been proposed as a valuable diagnostic of the mass accumulation in galaxies as being more tightly related to the physics of star-formation (SF) and stellar feedback than other SF indicators. In this paper, we assemble a statistical sample of 230 galaxies observed with JWST in the GLASS and CEERS spectroscopic surveys to estimate Balmer line based dust attenuations and SFRs, and UV rest-frame effective radii. We study the evolution of galaxy SFR and $危_{\rm SFR}$ in the first 1.5 Billion years of our Universe, finding that $危_{\rm SFR}$ is mildly increasing with redshift with a linear slope of $0.16 \pm 0.06$. We also explore the dependence of SFR and $危_{\rm SFR}$ on stellar mass, showing that a SF 'Main-Sequence' and a $危_{\rm SFR}$ `Main-Sequence' are in place out to z=10, with a similar slope compared to the same relations at lower redshifts. We find that the specific SFR (sSFR) and $危_{\rm SFR}$ are correlated with the [OIII]5007/[OII]3727 ratio and with indirect estimates of the escape fraction of Lyman continuum photons, hence they likely play an important role in the evolution of ionization conditions and in the escape of ionizing radiation. We also search for spectral outflow signatures in a subset of galaxies observed at high resolution, finding an outflow incidence of $2/11$ ($=20\%^{32\%}_{9\%}$) at $z<6$, but no evidence at $z>6$ ($<26\%$). Finally, we find a positive correlation between A$_V$ and $危_{\rm SFR}$, and a flat trend as a function of sSFR, indicating that there is no evidence of a drop of A$_V$ in extremely star-forming galaxies between z=4 and 10. This might be at odds with a dust-clearing outflow scenario, which might instead take place at redshifts $z\geq 10$, as suggested by some theoretical models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.17829v2-abstract-full').style.display = 'none'; document.getElementById('2402.17829v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A ; 19 pages, 9 figures, 1 table. Compared to the previous version, we have corrected a typo in Fig. 5 (the x and y axis labels were inverted)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 690, A290 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.11220">arXiv:2402.11220</a> <span> [<a href="https://arxiv.org/pdf/2402.11220">pdf</a>, <a href="https://arxiv.org/format/2402.11220">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202449644">10.1051/0004-6361/202449644 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Peering into cosmic reionization: the Ly$伪$ visibility evolution from galaxies at $z$ = 4.5-8.5 with JWST </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+L">L. Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Santini%2C+P">P. Santini</a>, <a href="/search/astro-ph?searchtype=author&query=Calabr%C3%B2%2C+A">A. Calabr貌</a>, <a href="/search/astro-ph?searchtype=author&query=Mascia%2C+S">S. Mascia</a>, <a href="/search/astro-ph?searchtype=author&query=Llerena%2C+M">M. Llerena</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">M. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">S. L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Amorin%2C+R">R. Amorin</a>, <a href="/search/astro-ph?searchtype=author&query=Haro%2C+P+A">P. Arrabal Haro</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M">M. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Bhatawdekar%2C+R">R. Bhatawdekar</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">N. J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+K">K. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Gardner%2C+J+P">J. P. Gardner</a>, <a href="/search/astro-ph?searchtype=author&query=Gawiser%2C+E">E. Gawiser</a>, <a href="/search/astro-ph?searchtype=author&query=Giavalisco%2C+M">M. Giavalisco</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N">N. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Hu%2C+W">W. Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+I">I. Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J+S">J. S. Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">A. M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Merlin%2C+E">E. Merlin</a>, <a href="/search/astro-ph?searchtype=author&query=Mobasher%2C+B">B. Mobasher</a> , et al. (6 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2402.11220v1-abstract-short" style="display: inline;"> The resonant scattering interaction between Ly$伪$ photons and neutral hydrogen implies that a partially neutral IGM can significantly impact the detectability of Ly$伪$ emission in galaxies. The redshift evolution of the Ly$伪$ equivalent width distribution of galaxies thus offers a key probe of the degree of ionization during the Epoch of Reionization (EoR). Previous in-depth investigations at $z$… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.11220v1-abstract-full').style.display = 'inline'; document.getElementById('2402.11220v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.11220v1-abstract-full" style="display: none;"> The resonant scattering interaction between Ly$伪$ photons and neutral hydrogen implies that a partially neutral IGM can significantly impact the detectability of Ly$伪$ emission in galaxies. The redshift evolution of the Ly$伪$ equivalent width distribution of galaxies thus offers a key probe of the degree of ionization during the Epoch of Reionization (EoR). Previous in-depth investigations at $z$ $\geq$ 7 were limited by ground-based instrument capabilities. We present an extensive study of Ly$伪$ emission from galaxies at 4 < $z$ < 8.5, observed from the CEERS and JADES surveys in the JWST NIRSpec/PRISM configuration. The sample consists of 235 galaxies, among which we identify 65 as Ly$伪$ emitters. We first measure Ly$伪$ escape fractions from Balmer lines, and explore the correlations with the inferred galaxies' physical properties, which are similar to those found at lower redshift. We also investigate the possible connection between the escape of Ly$伪$ photons and the inferred escape fractions of LyC photons obtained from indirect indicators. We then analyze the redshift evolution of the Ly$伪$ emitter fraction, finding lower average values at $z$ = 5 and 6 compared to ground-based observations. At $z$ = 7 we find a very large difference in Ly$伪$ visibility between the EGS and GOODS-South fields, possibly due to the presence of early reionized regions in the EGS. Such large variance is also expected in the Cosmic Dawn II radiation-hydrodynamical simulation. Our findings suggest a scenario in which the ending phase of the EoR is characterized by $\sim$ 1 pMpc ionized bubbles around a high fraction of moderately bright galaxies. Finally, we characterize such two ionized regions found in the EGS at $z$ = 7.18 and $z$ = 7.49 by estimating the radius of the ionized bubble that each of the spectroscopically-confirmed members could have created. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.11220v1-abstract-full').style.display = 'none'; document.getElementById('2402.11220v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 688, A106 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.12402">arXiv:2401.12402</a> <span> [<a href="https://arxiv.org/pdf/2401.12402">pdf</a>, <a href="https://arxiv.org/format/2401.12402">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Characterizing the Average Interstellar Medium Conditions of Galaxies at $z\sim$ 5.6-9 with UV and Optical Nebular Lines </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hu%2C+W">Weida Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Papovich%2C+C">Casey Papovich</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Kennicutt%2C+R">Robert Kennicutt</a>, <a href="/search/astro-ph?searchtype=author&query=Shen%2C+L">Lu Shen</a>, <a href="/search/astro-ph?searchtype=author&query=Amor%C3%ADn%2C+R+O">Ricardo O. Amor铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Haro%2C+P+A">Pablo Arrabal Haro</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M+B">Micaela B. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Bhatawdekar%2C+R">Rachana Bhatawdekar</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+J+W">Justin W. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Dekel%2C+A">Avishai Dekel</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Vega%2C+A">Alexander de la Vega</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">Norman A. Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N+P">Nimish P. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">Michaela Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">Benne W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Hutchison%2C+T+A">Taylor A. Hutchison</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+I">Intae Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J+S">Jeyhan S. Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+R+A">Ray A. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Llerena%2C+M">Mario Llerena</a>, <a href="/search/astro-ph?searchtype=author&query=Mascia%2C+S">S. Mascia</a> , et al. (8 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.12402v1-abstract-short" style="display: inline;"> Ultraviolet (UV; rest-frame $\sim1200-2000$ A) spectra provide a wealth of diagnostics to characterize fundamental galaxy properties, such as their chemical enrichment, the nature of their stellar populations, and their amount of Lyman-continuum (LyC) radiation. In this work, we leverage publicly released JWST data to construct the rest-frame UV-to-optical composite spectrum of a sample of 63 gala… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.12402v1-abstract-full').style.display = 'inline'; document.getElementById('2401.12402v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.12402v1-abstract-full" style="display: none;"> Ultraviolet (UV; rest-frame $\sim1200-2000$ A) spectra provide a wealth of diagnostics to characterize fundamental galaxy properties, such as their chemical enrichment, the nature of their stellar populations, and their amount of Lyman-continuum (LyC) radiation. In this work, we leverage publicly released JWST data to construct the rest-frame UV-to-optical composite spectrum of a sample of 63 galaxies at $5.6<z<9$, spanning the wavelength range from 1500 to 5200 A. Based on the composite spectrum, we derive an average dust attenuation $E(B-V)_\mathrm{gas}=0.16^{+0.10}_{-0.11}$ from \hb/\hg, electron density $n_e = 570^{+510}_{-290}$ cm$^{-3}$ from the [O II] doublet ratio, electron temperature $T_e = 17000^{+1500}_{-1500}$ K from the [O III] $\lambda4363$/ [O III] $\lambda5007$ ratio, and an ionization parameter $\log(U)=-2.18^{+0.03}_{-0.03}$ from the [O III]/[O II] ratio. Using a direct $T_e$ method, we calculate an oxygen abundance $12+\log\mathrm{(O/H)}=7.67\pm0.08$ and the carbon-to-oxygen (C/O) abundance ratio $\log\mathrm{(C/O)}=-0.87^{+0.13}_{-0.10}$. This C/O ratio is smaller than compared to $z=0$ and $z=2$ - 4 star-forming galaxies, albeit with moderate significance. This indicates the reionization-era galaxies might be undergoing a rapid build-up of stellar mass with high specific star-formation rates. A UV diagnostic based on the ratios of C III] $位\lambda1907,1909$/He II $\lambda1640$ versus O III] $\lambda1666$/He II $\lambda1640$ suggests that the star formation is the dominant source of ionization, similar to the local extreme dwarf galaxies and $z\sim2$ - 4 He II-detected galaxies. The [O III]/[O II] and C IV/C III] ratios of the composite spectrum are marginally larger than the criteria used to select galaxies as LyC leakers, suggesting that some of the galaxies in our sample are strong contributors to the reionizing radiation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.12402v1-abstract-full').style.display = 'none'; document.getElementById('2401.12402v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 7 figures, 4 tables. Submitted. Comments are welcome</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.12319">arXiv:2401.12319</a> <span> [<a href="https://arxiv.org/pdf/2401.12319">pdf</a>, <a href="https://arxiv.org/format/2401.12319">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ad234a">10.3847/1538-4357/ad234a <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Exploring the Gas-Phase Metallicity Gradients of Star-forming Galaxies at Cosmic Noon </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+Y">Yingjie Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Giavalisco%2C+M">Mauro Giavalisco</a>, <a href="/search/astro-ph?searchtype=author&query=Simons%2C+R+C">Raymond C. Simons</a>, <a href="/search/astro-ph?searchtype=author&query=Ji%2C+Z">Zhiyuan Ji</a>, <a href="/search/astro-ph?searchtype=author&query=Stroupe%2C+D">Darren Stroupe</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.12319v1-abstract-short" style="display: inline;"> We explore the relationships between the [O/H] gas-phase metallicity radial gradients and multiple galaxy properties for 238 star-forming galaxies at 0.6<z<2.6 selected from the CANDELS Ly$伪$ Emission at Reionization (CLEAR) survey with stellar mass 8.5 < log $M_{*}/M_{\odot}$ < 10.5. The gradients cover the range from -0.11 to 0.22 dex kpc$^{-1}$, with the median value close to zero. We reconstru… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.12319v1-abstract-full').style.display = 'inline'; document.getElementById('2401.12319v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.12319v1-abstract-full" style="display: none;"> We explore the relationships between the [O/H] gas-phase metallicity radial gradients and multiple galaxy properties for 238 star-forming galaxies at 0.6<z<2.6 selected from the CANDELS Ly$伪$ Emission at Reionization (CLEAR) survey with stellar mass 8.5 < log $M_{*}/M_{\odot}$ < 10.5. The gradients cover the range from -0.11 to 0.22 dex kpc$^{-1}$, with the median value close to zero. We reconstruct the nonparametric star-formation histories (SFHs) of the galaxies with spectral energy distribution modeling using Prospector with more than 40 photometric bands from HST, Spitzer and ground-based facilities. In general, we find weak or no correlations between the metallicity gradients and most galaxy properties, including the mass-weighted age, recent star formation rate, dust attenuation, and morphology as quantified by both parametric and non-parametric diagnostics. We find a significant but moderate correlation between the gradients and the 'evolutionary time', a temporal metric that characterizes the evolutionary status of a galaxy, with flatter gradients observed in more evolved galaxies. Also, there is evidence that galaxies with multiple star-formation episodes in their SFHs tend to develop more negative gas-phase metallicity gradients (higher [O/H] at the center). We conclude that gas kinematics, e.g. radial inflows and outflows, is likely an important process in setting the gas-phase metallicity gradients, in addition to the evolution of the SFH radial profile. Since the gradients are largely independent on the galaxies' physical properties, and only weakly dependent on their SFH, it would appear that the timescale of the gas kinematics is significantly shorter than the evolution of star formation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.12319v1-abstract-full').style.display = 'none'; document.getElementById('2401.12319v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 21 figures, accepted for publication in APJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal, 2024, Volume 964, Issue 1, id.94, 17 pp </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.10152">arXiv:2312.10152</a> <span> [<a href="https://arxiv.org/pdf/2312.10152">pdf</a>, <a href="https://arxiv.org/format/2312.10152">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> CEERS: Increasing Scatter along the Star-Forming Main Sequence Indicates Early Galaxies Form in Bursts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cole%2C+J+W">Justin W. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Papovich%2C+C">Casey Papovich</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M+B">Micaela B. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Iyer%2C+K+G">Kartheik G. Iyer</a>, <a href="/search/astro-ph?searchtype=author&query=Yung%2C+L+Y+A">L. Y. Aaron Yung</a>, <a href="/search/astro-ph?searchtype=author&query=Ciesla%2C+L">Laure Ciesla</a>, <a href="/search/astro-ph?searchtype=author&query=Amorin%2C+R+O">Ricardo O. Amorin</a>, <a href="/search/astro-ph?searchtype=author&query=Haro%2C+P+A">Pablo Arrabal Haro</a>, <a href="/search/astro-ph?searchtype=author&query=Bhatawdekar%2C+R">Rachana Bhatawdekar</a>, <a href="/search/astro-ph?searchtype=author&query=Calabro%2C+A">Antonello Calabro</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Vega%2C+A">Alexander de la Vega</a>, <a href="/search/astro-ph?searchtype=author&query=Dekel%2C+A">Avishai Dekel</a>, <a href="/search/astro-ph?searchtype=author&query=Endsley%2C+R">Ryan Endsley</a>, <a href="/search/astro-ph?searchtype=author&query=Gawiser%2C+E">Eric Gawiser</a>, <a href="/search/astro-ph?searchtype=author&query=Giavalisco%2C+M">Mauro Giavalisco</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N+P">Nimish P. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">Michaela Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">Benne W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J+S">Jeyhan S. Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+R+A">Ray A. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Mascia%2C+S">Sara Mascia</a> , et al. (7 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.10152v1-abstract-short" style="display: inline;"> We present the star-formation-rate -- stellar-mass (SFR-M$_\ast$) relation for galaxies in the CEERS survey at $4.5\leq z\leq 12$. We model the \jwst\ and \hst\ rest-UV and rest-optical photometry of galaxies with flexible star-formation histories (SFHs) using \bagpipes. We consider SFRs averaged from the SFHs over 10~Myr (\sfrten) and 100~Myr (\sfrcen), where the photometry probes SFRs on these t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.10152v1-abstract-full').style.display = 'inline'; document.getElementById('2312.10152v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.10152v1-abstract-full" style="display: none;"> We present the star-formation-rate -- stellar-mass (SFR-M$_\ast$) relation for galaxies in the CEERS survey at $4.5\leq z\leq 12$. We model the \jwst\ and \hst\ rest-UV and rest-optical photometry of galaxies with flexible star-formation histories (SFHs) using \bagpipes. We consider SFRs averaged from the SFHs over 10~Myr (\sfrten) and 100~Myr (\sfrcen), where the photometry probes SFRs on these timescales, effectively tracing nebular emission lines in the rest-optical (on $\sim10$~Myr timescales) and the UV/optical continuum (on $\sim100$ Myr timescales). We measure the slope, normalization and intrinsic scatter of the SFR-M$_\ast$ relation, taking into account the uncertainty and the covariance of galaxy SFRs and $M_\ast$. From $z\sim 5-9$ there is larger scatter in the $\sfrten-M_\ast$ relation, with $蟽(\log \sfrcen)=0.4$~dex, compared to the $\sfrcen-M_\ast$ relation, with $蟽(\log \sfrten)=0.1$~dex. This scatter increases with redshift and increasing stellar mass, at least out to $z\sim 7$. These results can be explained if galaxies at higher redshift experience an increase in star-formation variability and form primarily in short, active periods, followed by a lull in star formation (i.e. ``napping'' phases). We see a significant trend in the ratio $R_\mathrm{SFR}=\log(\sfrten/\sfrcen)$ in which, on average, $R_\mathrm{SFR}$ decreases with increasing stellar mass and increasing redshift. This yields a star-formation ``duty cycle'' of $\sim40\%$ for galaxies with $\log M_\ast/M_\odot\geq 9.3$, at $z\sim5$, declining to $\sim20\%$ at $z\sim9$. Galaxies also experience longer lulls in star formation at higher redshift and at higher stellar mass, such that galaxies transition from periods of higher SFR variability at $z\gtrsim~6$ to smoother SFR evolution at $z\lesssim~4.5$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.10152v1-abstract-full').style.display = 'none'; document.getElementById('2312.10152v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 12 figures, 2 Appendix figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.09972">arXiv:2312.09972</a> <span> [<a href="https://arxiv.org/pdf/2312.09972">pdf</a>, <a href="https://arxiv.org/format/2312.09972">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The Next Generation Deep Extragalactic Exploratory Public Near-Infrared Slitless Survey Epoch 1 (NGDEEP-NISS1): Extra-Galactic Star-formation and Active Galactic Nuclei at 0.5 < z < 3.6 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pirzkal%2C+N">Nor Pirzkal</a>, <a href="/search/astro-ph?searchtype=author&query=Rothberg%2C+B">Barry Rothberg</a>, <a href="/search/astro-ph?searchtype=author&query=Papovich%2C+C">Casey Papovich</a>, <a href="/search/astro-ph?searchtype=author&query=Shen%2C+L">Lu Shen</a>, <a href="/search/astro-ph?searchtype=author&query=Leung%2C+G+C+K">Gene C. K. Leung</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M+B">Micaela B. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Vanderhoof%2C+B+N">Brittany N. Vanderhoof</a>, <a href="/search/astro-ph?searchtype=author&query=Lotz%2C+J+M">Jennifer M. Lotz</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N+P">Nimish P. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+Y">Yingjie Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">Norman A. Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Yung%2C+L+Y+A">L. Y. Aaron Yung</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+H+C">Henry C. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Gardner%2C+J+P">Jonathan P. Gardner</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+I">Intae Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J+S">Jeyhan S. Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=Ryan%2C+R">Russell Ryan</a>, <a href="/search/astro-ph?searchtype=author&query=Simons%2C+R+C">Raymond C. Simons</a>, <a href="/search/astro-ph?searchtype=author&query=Ravindranath%2C+S">Swara Ravindranath</a>, <a href="/search/astro-ph?searchtype=author&query=Berg%2C+D+A">Danielle A. Berg</a>, <a href="/search/astro-ph?searchtype=author&query=Backhaus%2C+B+E">Bren E. Backhaus</a> , et al. (26 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.09972v4-abstract-short" style="display: inline;"> The Next Generation Deep Extragalactic Exploratory Public (NGDEEP) survey program was designed specifically to include Near Infrared Slitless Spectroscopic observations (NGDEEP-NISS) to detect multiple emission lines in as many galaxies as possible and across a wide redshift range using the Near Infrared Imager and Slitless Spectrograph (NIRISS). We present early results obtained from the the firs… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.09972v4-abstract-full').style.display = 'inline'; document.getElementById('2312.09972v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.09972v4-abstract-full" style="display: none;"> The Next Generation Deep Extragalactic Exploratory Public (NGDEEP) survey program was designed specifically to include Near Infrared Slitless Spectroscopic observations (NGDEEP-NISS) to detect multiple emission lines in as many galaxies as possible and across a wide redshift range using the Near Infrared Imager and Slitless Spectrograph (NIRISS). We present early results obtained from the the first set of observations (Epoch 1, 50$\%$ of the allocated orbits) of this program (NGDEEP-NISS1). Using a set of independently developed calibration files designed to deal with a complex combination of overlapping spectra, multiple position angles, and multiple cross filters and grisms, in conjunction with a robust and proven algorithm for quantifying contamination from overlapping dispersed spectra, NGDEEP-NISS1 has achieved a 3$蟽$ sensitivity limit of 2 $\times$ 10$^{-18}$ erg/s/cm$^2$. We demonstrate the power of deep wide field slitless spectroscopy (WFSS) to characterize the star-formation rates, and metallicity ([OIII]/H$尾$), and dust content, of galaxies at $1<z<3.5$. The latter showing intriguing initial results on the applicability and assumptions made regarding the use of Case B recombination. Further, we identify the presence of active galactic nuclei (AGN) and infer the mass of their supermassive black holes (SMBHs) using broadened restframe MgII and H$尾$ emission lines. The spectroscopic results are then compared with the physical properties of galaxies extrapolated from fitting spectral energy distribution (SED) models to photometry alone. The results clearly demonstrate the unique power and efficiency of WFSS at near-infrared wavelengths over other methods to determine the properties of galaxies across a broad range of redshifts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.09972v4-abstract-full').style.display = 'none'; document.getElementById('2312.09972v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">33 pages, 28 Figures, Accepted (ApJ)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.07799">arXiv:2312.07799</a> <span> [<a href="https://arxiv.org/pdf/2312.07799">pdf</a>, <a href="https://arxiv.org/format/2312.07799">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> A Census from JWST of Extreme Emission Line Galaxies Spanning the Epoch of Reionization in CEERS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Davis%2C+K">Kelcey Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Trump%2C+J+R">Jonathan R. Trump</a>, <a href="/search/astro-ph?searchtype=author&query=Simons%2C+R+C">Raymond C. Simons</a>, <a href="/search/astro-ph?searchtype=author&query=Mcgrath%2C+E+J">Elizabeth J. Mcgrath</a>, <a href="/search/astro-ph?searchtype=author&query=Wilkins%2C+S+M">Stephen M. Wilkins</a>, <a href="/search/astro-ph?searchtype=author&query=Haro%2C+P+A">Pablo Arrabal Haro</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M+B">Micaela B. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%81ndez%2C+V">Vital Fern脕ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Amor%C3%8Dn%2C+R+O">Ricardo O. Amor脥n</a>, <a href="/search/astro-ph?searchtype=author&query=Backhaus%2C+B+E">Bren E. Backhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Llerena%2C+M">Mario Llerena</a>, <a href="/search/astro-ph?searchtype=author&query=Brunker%2C+S+W">Samantha W. Brunker</a>, <a href="/search/astro-ph?searchtype=author&query=Barro%2C+G">Guillermo Barro</a>, <a href="/search/astro-ph?searchtype=author&query=Bisigello%2C+L">Laura Bisigello</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+M">Madisyn Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Costantin%2C+L">Luca Costantin</a>, <a href="/search/astro-ph?searchtype=author&query=De+La+Vega%2C+A">Alexander De La Vega</a>, <a href="/search/astro-ph?searchtype=author&query=Dekel%2C+A">Avishai Dekel</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N+P">Nimish P. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">Michaela Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J+S">Jeyhan S. Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a> , et al. (7 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.07799v1-abstract-short" style="display: inline;"> We present a sample of 1165 extreme emission-line galaxies (EELGs) at 4<z<9 selected using James Webb Space Telescope (JWST) NIRCam photometry in the Cosmic Evolution Early Release Science (CEERS) program. We use a simple method to photometrically identify EELGs with Hb + [OIII] (combined) or Ha emission of observed-frame equivalent width EW >5000 AA. JWST/NIRSpec spectroscopic observations of a s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.07799v1-abstract-full').style.display = 'inline'; document.getElementById('2312.07799v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.07799v1-abstract-full" style="display: none;"> We present a sample of 1165 extreme emission-line galaxies (EELGs) at 4<z<9 selected using James Webb Space Telescope (JWST) NIRCam photometry in the Cosmic Evolution Early Release Science (CEERS) program. We use a simple method to photometrically identify EELGs with Hb + [OIII] (combined) or Ha emission of observed-frame equivalent width EW >5000 AA. JWST/NIRSpec spectroscopic observations of a subset (34) of the photometrically selected EELGs validate our selection method: all spectroscopically observed EELGs confirm our photometric identification of extreme emission, including some cases where the SED-derived photometric redshifts are incorrect. We find that the medium-band F410M filter in CEERS is particularly efficient at identifying EELGs, both in terms of including emission lines in the filter and in correctly identifying the continuum between Hb + [OIII] and Ha in the neighboring broad-band filters. We present examples of EELGs that could be incorrectly classified at ultra-high redshift (z>12) as a result of extreme Hb + [OIII] emission blended across the reddest photometric filters. We compare the EELGs to the broader (sub-extreme) galaxy population in the same redshift range and find that they are consistent with being the bluer, high equivalent width tail of a broader population of emission-line galaxies. The highest-EW EELGs tend to have more compact emission-line sizes than continuum sizes, suggesting that active galactic nuclei are responsible for at least some of the most extreme EELGs. Photometrically inferred emission-line ratios are consistent with ISM conditions with high ionization and moderately low metallicity, consistent with previous spectroscopic studies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.07799v1-abstract-full').style.display = 'none'; document.getElementById('2312.07799v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 25 figures, submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.14804">arXiv:2311.14804</a> <span> [<a href="https://arxiv.org/pdf/2311.14804">pdf</a>, <a href="https://arxiv.org/format/2311.14804">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Evidence for a Shallow Evolution in the Volume Densities of Massive Galaxies at $z=4$ to $8$ from CEERS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chworowsky%2C+K">Katherine Chworowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Boylan-Kolchin%2C+M">Michael Boylan-Kolchin</a>, <a href="/search/astro-ph?searchtype=author&query=McGrath%2C+E+J">Elizabeth J. McGrath</a>, <a href="/search/astro-ph?searchtype=author&query=Iyer%2C+K+G">Kartheik G. Iyer</a>, <a href="/search/astro-ph?searchtype=author&query=Papovich%2C+C">Casey Papovich</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+A+J">Anthony J. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=Yung%2C+L+Y+A">L. Y. Aaron Yung</a>, <a href="/search/astro-ph?searchtype=author&query=Haro%2C+P+A">Pablo Arrabal Haro</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M+B">Micaela B. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Backhaus%2C+B+E">Bren E. Backhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Bhatawdekar%2C+R">Rachana Bhatawdekar</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+Y">Yingjie Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+J+W">Justin W. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Cooper%2C+M+C">M. C. Cooper</a>, <a href="/search/astro-ph?searchtype=author&query=Costantin%2C+L">Luca Costantin</a>, <a href="/search/astro-ph?searchtype=author&query=Dekel%2C+A">Avishai Dekel</a>, <a href="/search/astro-ph?searchtype=author&query=Franco%2C+M">Maximilien Franco</a>, <a href="/search/astro-ph?searchtype=author&query=Fujimoto%2C+S">Seiji Fujimoto</a>, <a href="/search/astro-ph?searchtype=author&query=Hayward%2C+C+C">Christopher C. Hayward</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">Benne W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Huertas-Company%2C+M">Marc Huertas-Company</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">Michaela Hirschmann</a> , et al. (14 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.14804v1-abstract-short" style="display: inline;"> We analyze the evolution of massive (log$_{10}$ [$M_\star/M_\odot$] $>10$) galaxies at $z \sim$ 4--8 selected from the JWST Cosmic Evolution Early Release Science (CEERS) survey. We infer the physical properties of all galaxies in the CEERS NIRCam imaging through spectral energy distribution (SED) fitting with dense basis to select a sample of high redshift massive galaxies. Where available we inc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.14804v1-abstract-full').style.display = 'inline'; document.getElementById('2311.14804v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.14804v1-abstract-full" style="display: none;"> We analyze the evolution of massive (log$_{10}$ [$M_\star/M_\odot$] $>10$) galaxies at $z \sim$ 4--8 selected from the JWST Cosmic Evolution Early Release Science (CEERS) survey. We infer the physical properties of all galaxies in the CEERS NIRCam imaging through spectral energy distribution (SED) fitting with dense basis to select a sample of high redshift massive galaxies. Where available we include constraints from additional CEERS observing modes, including 18 sources with MIRI photometric coverage, and 28 sources with spectroscopic confirmations from NIRSpec or NIRCam wide-field slitless spectroscopy. We sample the recovered posteriors in stellar mass from SED fitting to infer the volume densities of massive galaxies across cosmic time, taking into consideration the potential for sample contamination by active galactic nuclei (AGN). We find that the evolving abundance of massive galaxies tracks expectations based on a constant baryon conversion efficiency in dark matter halos for $z \sim$ 1--4. At higher redshifts, we observe an excess abundance of massive galaxies relative to this simple model. These higher abundances can be explained by modest changes to star formation physics and/or the efficiencies with which star formation occurs in massive dark matter halos, and are not in tension with modern cosmology. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.14804v1-abstract-full').style.display = 'none'; document.getElementById('2311.14804v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 10 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.04294">arXiv:2311.04294</a> <span> [<a href="https://arxiv.org/pdf/2311.04294">pdf</a>, <a href="https://arxiv.org/format/2311.04294">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Rest-Frame UV Colors for Faint Galaxies at $z \sim 9-16$ with the \textit{JWST} NGDEEP Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Morales%2C+A+M">Alexa M. Morales</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Leung%2C+G+C+K">Gene C. K. Leung</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M+B">Micaela B. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Dave%2C+R">Romeel Dave</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+H+C">Henry C. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N+P">Nimish P. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+E">Ewan Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Papovich%2C+C">Casey Papovich</a>, <a href="/search/astro-ph?searchtype=author&query=Perez-Gonzalez%2C+P+G">Pablo G. Perez-Gonzalez</a>, <a href="/search/astro-ph?searchtype=author&query=Pirzkal%2C+N">Nor Pirzkal</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+B">Britton Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Wilkins%2C+S+M">Stephen M. Wilkins</a>, <a href="/search/astro-ph?searchtype=author&query=Yung%2C+L+Y+A">L. Y. Aaron Yung</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.04294v1-abstract-short" style="display: inline;"> We present measurements of the rest-frame UV spectral slope, $尾$, for a sample of 36 faint star-forming galaxies at z ~ 9-16 discovered in one of the deepest JWST NIRCam surveys to date, the Next Generation Deep Extragalactic Exploratory Public (NGDEEP) Survey. We use robust photometric measurements for UV-faint galaxies (down to $M_{UV}$ ~ -16), originally published in Leung+23, and measure value… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.04294v1-abstract-full').style.display = 'inline'; document.getElementById('2311.04294v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.04294v1-abstract-full" style="display: none;"> We present measurements of the rest-frame UV spectral slope, $尾$, for a sample of 36 faint star-forming galaxies at z ~ 9-16 discovered in one of the deepest JWST NIRCam surveys to date, the Next Generation Deep Extragalactic Exploratory Public (NGDEEP) Survey. We use robust photometric measurements for UV-faint galaxies (down to $M_{UV}$ ~ -16), originally published in Leung+23, and measure values of the UV spectral slope via photometric power-law fitting to both the observed photometry and to stellar population models obtained through spectral energy distribution (SED) fitting with Bagpipes. We obtain a median and 68% confidence interval for $尾$ from photometric power-law fitting of $尾_{PL} = -2.7^{+0.5}_{-0.5}$ and from SED-fitting, $尾_{SED} = -2.3^{+0.2}_{-0.1}$ for the full sample. We show that when only 2-3 photometric detections are available, SED-fitting has a lower scatter and reduced biases than photometric power-law fitting. We quantify this bias and find that after correction, the median $尾_{SED,corr} = -2.5^{+0.2}_{-0.2}$. We measure physical properties for our galaxies with Bagpipes and find that our faint ($M_{UV} = -18.1^{+0.7}_{-0.9}$) sample is low mass (${log}[M_{\ast}/M_\odot] = 7.7^{+0.5}_{-0.5}$), fairly dust-poor ($A_{v} = 0.1^{+0.2}_{-0.1}$ mag), and modestly young (${log[age]} = 7.8^{+0.2}_{-0.8}$ yr) with a median star formation rate of $\mathrm{log(SFR)} = -0.3^{+0.4}_{-0.4} M_\odot{/yr}$. We find no strong evidence for ultra-blue UV spectral slopes ($尾$ ~ -3) within our sample, as would be expected for exotically metal-poor ($Z/Z_{\odot}$ < 10$^{-3}$) stellar populations with very high LyC escape fractions. Our observations are consistent with model predictions that galaxies of these stellar masses at z~9-16 should have only modestly low metallicities ($Z/Z_{\odot}$ ~ 0.1--0.2). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.04294v1-abstract-full').style.display = 'none'; document.getElementById('2311.04294v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 8 figures, 3 tables, submitted to ApjL</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.04279">arXiv:2311.04279</a> <span> [<a href="https://arxiv.org/pdf/2311.04279">pdf</a>, <a href="https://arxiv.org/format/2311.04279">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The Complete CEERS Early Universe Galaxy Sample: A Surprisingly Slow Evolution of the Space Density of Bright Galaxies at z ~ 8.5-14.5 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Leung%2C+G+C+K">Gene C. K. Leung</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M+B">Micaela B. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+H+C">Henry C. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Papovich%2C+C">Casey Papovich</a>, <a href="/search/astro-ph?searchtype=author&query=Akins%2C+H+B">Hollis B. Akins</a>, <a href="/search/astro-ph?searchtype=author&query=Haro%2C+P+A">Pablo Arrabal Haro</a>, <a href="/search/astro-ph?searchtype=author&query=Dave%2C+R">Romeel Dave</a>, <a href="/search/astro-ph?searchtype=author&query=Dekel%2C+A">Avishai Dekel</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J+S">Jeyhan S. Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=Kocevski%2C+D+D">Dale D. Kocevski</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Pirzkal%2C+N">Norbert Pirzkal</a>, <a href="/search/astro-ph?searchtype=author&query=Somerville%2C+R+S">Rachel S. Somerville</a>, <a href="/search/astro-ph?searchtype=author&query=Yung%2C+L+Y+A">L. Y. Aaron Yung</a>, <a href="/search/astro-ph?searchtype=author&query=Amorin%2C+R">Ricardo Amorin</a>, <a href="/search/astro-ph?searchtype=author&query=Backhaus%2C+B+E">Bren E. Backhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Behroozi%2C+P">Peter Behroozi</a>, <a href="/search/astro-ph?searchtype=author&query=Bisigello%2C+L">Laura Bisigello</a>, <a href="/search/astro-ph?searchtype=author&query=Bromm%2C+V">Volker Bromm</a>, <a href="/search/astro-ph?searchtype=author&query=Casey%2C+C+M">Caitlin M. Casey</a>, <a href="/search/astro-ph?searchtype=author&query=Ortiz%2C+O+A+C">Oscar A. Chavez Ortiz</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+Y">Yingjie Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Chworowsky%2C+K">Katherine Chworowsky</a> , et al. (30 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.04279v1-abstract-short" style="display: inline;"> We present a sample of 88 candidate z~8.5-14.5 galaxies selected from the completed NIRCam imaging from the Cosmic Evolution Early Release Science (CEERS) survey. These data cover ~90 arcmin^2 (10 NIRCam pointings) in six broad-band and one medium-band imaging filter. With this sample we confirm at higher confidence early JWST conclusions that bright galaxies in this epoch are more abundant than p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.04279v1-abstract-full').style.display = 'inline'; document.getElementById('2311.04279v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.04279v1-abstract-full" style="display: none;"> We present a sample of 88 candidate z~8.5-14.5 galaxies selected from the completed NIRCam imaging from the Cosmic Evolution Early Release Science (CEERS) survey. These data cover ~90 arcmin^2 (10 NIRCam pointings) in six broad-band and one medium-band imaging filter. With this sample we confirm at higher confidence early JWST conclusions that bright galaxies in this epoch are more abundant than predicted by most theoretical models. We construct the rest-frame ultraviolet luminosity functions at z~9, 11 and 14, and show that the space density of bright (M_UV=-20) galaxies changes only modestly from z~14 to z~9, compared to a steeper increase from z~8 to z~4. While our candidates are photometrically selected, spectroscopic followup has now confirmed 13 of them, with only one significant interloper, implying that the fidelity of this sample is high. Successfully explaining the evidence for a flatter evolution in the number densities of UV-bright z>10 galaxies may thus require changes to the dominant physical processes regulating star formation. While our results indicate that significant variations of dust attenuation with redshift are unlikely to be the dominant factor at these high redshifts, they are consistent with predictions from models which naturally have enhanced star-formation efficiency and/or stochasticity. An evolving stellar initial mass function could also bring model predictions into better agreement with our results. Deep spectroscopic followup of a large sample of early galaxies can distinguish between these competing scenarios. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.04279v1-abstract-full').style.display = 'none'; document.getElementById('2311.04279v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to ApJL. Main paper is 33 pages, 13 figures, 5 tables. Two appendices with additional figures and tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.13745">arXiv:2310.13745</a> <span> [<a href="https://arxiv.org/pdf/2310.13745">pdf</a>, <a href="https://arxiv.org/format/2310.13745">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> NGDEEP Epoch 1: Spatially Resolved H$伪$ Observations of Disk and Bulge Growth in Star-Forming Galaxies at $z \sim$ 0.6-2.2 from JWST NIRISS Slitless Spectroscopy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shen%2C+L">Lu Shen</a>, <a href="/search/astro-ph?searchtype=author&query=Papovich%2C+C">Casey Papovich</a>, <a href="/search/astro-ph?searchtype=author&query=Matharu%2C+J">Jasleen Matharu</a>, <a href="/search/astro-ph?searchtype=author&query=Pirzkal%2C+N">Nor Pirzkal</a>, <a href="/search/astro-ph?searchtype=author&query=Hu%2C+W">Weida Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Backhaus%2C+B+E">Bren E. Backhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M+B">Micaela B. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+Y">Yingjie Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Huertas-Company%2C+M">Marc Huertas-Company</a>, <a href="/search/astro-ph?searchtype=author&query=Giavalisco%2C+M">Mauro Giavalisco</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">Norman A. Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+I">Intae Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J+S">Jeyhan S. Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Lotz%2C+J+M">Jennifer M. Lotz</a>, <a href="/search/astro-ph?searchtype=author&query=Maseda%2C+M+V">Michael V. Maseda</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Gonz%C3%A1lez%2C+P+G">Pablo G. P茅rez-Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Rothberg%2C+B">Barry Rothberg</a>, <a href="/search/astro-ph?searchtype=author&query=Simons%2C+R+C">Raymond C. Simons</a>, <a href="/search/astro-ph?searchtype=author&query=Tacchella%2C+S">Sandro Tacchella</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+C+C">Christina C. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Yung%2C+L+Y+A">L. Y. Aaron Yung</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.13745v2-abstract-short" style="display: inline;"> We study the H$伪$ equivalent width, EW(H$伪$), maps of 19 galaxies at $0.6 < z < 2.2$ in the Hubble Ultra Deep Field (HUDF) derived from NIRISS slitless spectroscopy as part of the Next Generation Deep Extragalactic Exploratory Public (NGDEEP) Survey. Our galaxies mostly lie on the star-formation main sequence with a stellar mass range of $\mathrm{10^9 - 10^{11} M_\odot}$, characterized as "typical… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.13745v2-abstract-full').style.display = 'inline'; document.getElementById('2310.13745v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.13745v2-abstract-full" style="display: none;"> We study the H$伪$ equivalent width, EW(H$伪$), maps of 19 galaxies at $0.6 < z < 2.2$ in the Hubble Ultra Deep Field (HUDF) derived from NIRISS slitless spectroscopy as part of the Next Generation Deep Extragalactic Exploratory Public (NGDEEP) Survey. Our galaxies mostly lie on the star-formation main sequence with a stellar mass range of $\mathrm{10^9 - 10^{11} M_\odot}$, characterized as "typical" star-forming galaxies at these redshifts. Leveraging deep HST and JWST broad-band images, spanning 0.4-4.8 $渭$m, we perform spatially-resolved fitting of the spectral energy distributions (SEDs) for these galaxies and construct specific star formation rate (sSFR) and stellar-mass-weighted age maps with a spatial resolution of $\sim$1 kpc. The pixel-to-pixel EW(H$伪$) increases with increasing sSFR and with decreasing age. The average trends are slightly different from the relations derived from integrated fluxes of galaxies from the literature, suggesting complex evolutionary trends within galaxies. We quantify the radial profiles of EW(H$伪$), sSFR, and age. The majority (84%) of galaxies show positive EW(H$伪$) gradients in line with the inside-out quenching scenario. A few galaxies (16%) show inverse (and flat) trends possibly due to merging or starbursts. We compare the distributions of EW(H$伪$) and sSFR to the star formation history models (SFHs) as a function of galactocentric radius. We argue that the central regions of galaxies have experienced, at least one, rapid star-formation episodes, which leads to the formation of the bulge, while their outer regions (e.g., disks) grow via more smoothly varying SFHs. These results demonstrate the ability to study resolved star formation in distant galaxies with JWST NIRISS. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.13745v2-abstract-full').style.display = 'none'; document.getElementById('2310.13745v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 12 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.02219">arXiv:2309.02219</a> <span> [<a href="https://arxiv.org/pdf/2309.02219">pdf</a>, <a href="https://arxiv.org/format/2309.02219">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> New insight on the nature of cosmic reionizers from the CEERS survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mascia%2C+S">S. Mascia</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Calabr%C3%B2%2C+A">A. Calabr貌</a>, <a href="/search/astro-ph?searchtype=author&query=Santini%2C+P">P. Santini</a>, <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+L">L. Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Haro%2C+P+A">P. Arrabal Haro</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">M. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Ocvirk%2C+P">P. Ocvirk</a>, <a href="/search/astro-ph?searchtype=author&query=Lewis%2C+J+S+W">J. S. W. Lewis</a>, <a href="/search/astro-ph?searchtype=author&query=Amor%C3%ADn%2C+R">R. Amor铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M">M. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+R+N+J">R. N. J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Costantin%2C+L">L. Costantin</a>, <a href="/search/astro-ph?searchtype=author&query=Dekel%2C+A">A. Dekel</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">S. L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">A. Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Giavalisco%2C+M">M. Giavalisco</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">N. A. Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N+P">N. P. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">M. Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">B. W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+I">I. Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J+S">J. S. Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">A. M. Koekemoer</a> , et al. (7 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.02219v1-abstract-short" style="display: inline;"> The Epoch of Reionization (EoR) began when galaxies grew in abundance and luminosity, so their escaping Lyman continuum (LyC) radiation started ionizing the surrounding neutral intergalactic medium (IGM). Despite significant recent progress, the nature and role of cosmic reionizers are still unclear: in order to define them, it would be necessary to directly measure their LyC escape fraction (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.02219v1-abstract-full').style.display = 'inline'; document.getElementById('2309.02219v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.02219v1-abstract-full" style="display: none;"> The Epoch of Reionization (EoR) began when galaxies grew in abundance and luminosity, so their escaping Lyman continuum (LyC) radiation started ionizing the surrounding neutral intergalactic medium (IGM). Despite significant recent progress, the nature and role of cosmic reionizers are still unclear: in order to define them, it would be necessary to directly measure their LyC escape fraction ($f_{esc}$). However, this is impossible during the EoR due to the opacity of the IGM. Consequently, many efforts at low and intermediate redshift have been made to determine measurable indirect indicators in high-redshift galaxies so that their $f_{esc}$ can be predicted. This work presents the analysis of the indirect indicators of 62 spectroscopically confirmed star-forming galaxies at $6 \leq z \leq 9$ from the Cosmic Evolution Early Release Science (CEERS) survey, combined with 12 sources with public data from other JWST-ERS campaigns. From the NIRCam and NIRSpec observations, we measured their physical and spectroscopic properties. We discovered that on average $6<z<9$ star-forming galaxies are compact in the rest-frame UV ($r_e \sim $ 0.4 kpc), are blue sources (UV-$尾$ slope $\sim $ -2.17), and have a predicted $f_{esc}$ of about 0.13. A comparison of our results to models and predictions as well as an estimation of the ionizing budget suggests that low-mass galaxies with UV magnitudes fainter than $M_{1500} = -18$ that we currently do not characterize with JWST observations probably played a key role in the process of reionization. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.02219v1-abstract-full').style.display = 'none'; document.getElementById('2309.02219v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 11 figures, submitted to A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.09750">arXiv:2308.09750</a> <span> [<a href="https://arxiv.org/pdf/2308.09750">pdf</a>, <a href="https://arxiv.org/format/2308.09750">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> CEERS Key Paper VII: JWST/MIRI Reveals a Faint Population of Galaxies at Cosmic Noon Unseen by Spitzer </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kirkpatrick%2C+A">Allison Kirkpatrick</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+G">Guang Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Bail%2C+A+L">Aurelien Le Bail</a>, <a href="/search/astro-ph?searchtype=author&query=Troiani%2C+G">Greg Troiani</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Elbaz%2C+D">David Elbaz</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N+P">Nimish P. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">Michaela Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">Benne W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Kocevski%2C+D+D">Dale D. Kocevski</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+R+A">Ray A. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=McKinney%2C+J">Jed McKinney</a>, <a href="/search/astro-ph?searchtype=author&query=Papovich%2C+C">Casey Papovich</a>, <a href="/search/astro-ph?searchtype=author&query=Perez-Gonzalez%2C+P+G">Pablo G. Perez-Gonzalez</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Vega%2C+A">Alexander de la Vega</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M+B">Micaela B. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">Emanuele Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+H+C">Henry C. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">Adriano Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Grazian%2C+A">Andrea Grazian</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">Norman A. Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Haro%2C+P+A">Pablo Arrabal Haro</a> , et al. (11 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2308.09750v1-abstract-short" style="display: inline;"> The Cosmic Evolution Early Release Science (CEERS) program observed the Extended Groth Strip with the Mid-Infrared Instrument (MIRI) on the James Webb Space Telescope (JWST) in 2022. In this paper, we discuss the four MIRI pointings that observed with longer wavelength filters, including F770W, F1000W, F1280W, F1500W, F1800W, and F2100W. We compare the MIRI galaxies with the Spitzer/MIPS 24$渭$m po… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.09750v1-abstract-full').style.display = 'inline'; document.getElementById('2308.09750v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.09750v1-abstract-full" style="display: none;"> The Cosmic Evolution Early Release Science (CEERS) program observed the Extended Groth Strip with the Mid-Infrared Instrument (MIRI) on the James Webb Space Telescope (JWST) in 2022. In this paper, we discuss the four MIRI pointings that observed with longer wavelength filters, including F770W, F1000W, F1280W, F1500W, F1800W, and F2100W. We compare the MIRI galaxies with the Spitzer/MIPS 24$渭$m population in the EGS field. We find that MIRI can observe an order of magnitude deeper than MIPS in significantly shorter integration times, attributable to JWST's much larger aperture and MIRI's improved sensitivity. MIRI is exceptionally good at finding faint ($L_{\rm IR}<10^{10} L_\odot$) galaxies at $z\sim1-2$. We find that a significant portion of MIRI galaxies are "mid-IR weak"--they have strong near-IR emission and relatively weaker mid-IR emission, and most of the star formation is unobscured. We present new IR templates that capture how the mid-IR to near-IR emission changes with increasing infrared luminosity. We present two color-color diagrams to separate mid-IR weak galaxies and active galactic nuclei (AGN) from dusty star-forming galaxies and find that these color diagrams are most effective when used in conjunction with each other. We present the first number counts of 10$渭$m sources and find that there are $\lesssim10$ IR AGN per MIRI pointing, possibly due to the difficulty of distinguishing AGN from intrinsically mid-IR weak galaxies (due to low metallicities or low dust content). We conclude that MIRI is most effective at observing moderate luminosity ($L_{\rm IR}=10^9-10^{10}L_\odot$) galaxies at $z=1-2$, and that photometry alone is not effective at identifying AGN within this faint population. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.09750v1-abstract-full').style.display = 'none'; document.getElementById('2308.09750v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 10 figures. Resubmitted to ApJS after revision</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.09503">arXiv:2307.09503</a> <span> [<a href="https://arxiv.org/pdf/2307.09503">pdf</a>, <a href="https://arxiv.org/format/2307.09503">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> CEERS Key Paper VIII: Emission Line Ratios from NIRSpec and NIRCam Wide-Field Slitless Spectroscopy at z>2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Backhaus%2C+B+E">Bren E. Backhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Trump%2C+J+R">Jonathan R. Trump</a>, <a href="/search/astro-ph?searchtype=author&query=Pirzkal%2C+N">Nor Pirzkal</a>, <a href="/search/astro-ph?searchtype=author&query=Barro%2C+G">Guillermo Barro</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Haro%2C+P+A">Pablo Arrabal Haro</a>, <a href="/search/astro-ph?searchtype=author&query=Simons%2C+R+C">Raymond C. Simons</a>, <a href="/search/astro-ph?searchtype=author&query=Wessner%2C+J">Jessica Wessner</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">Michaela Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M+B">Micaela B. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Nicholls%2C+D+C">David C. Nicholls</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J+S">Jeyhan S. Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=Papovich%2C+C">Casey Papovich</a>, <a href="/search/astro-ph?searchtype=author&query=Kocevski%2C+D+D">Dale D. Kocevski</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Bisigello%2C+L">Laura Bisigello</a>, <a href="/search/astro-ph?searchtype=author&query=Jaskot%2C+A+E">Anne E. Jaskot</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+R+A">Ray A. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+I">Intae Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Wilkins%2C+S+M">Stephen M. Wilkins</a>, <a href="/search/astro-ph?searchtype=author&query=Yung%2C+L+Y+A">L. Y. Aaron Yung</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+H+C">Henry C. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">Adriano Fontana</a> , et al. (15 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.09503v3-abstract-short" style="display: inline;"> We use James Webb Space Telescope Near-Infrared Camera Wide Field Slitless Spectroscopy (NIRCam WFSS) and Near-Infrared spectrograph (NIRSpec) in the Cosmic Evolution Early Release survey (CEERS) to measure rest-frame optical emission-line of 155 galaxies at z>2. The blind NIRCam grism observations include a sample of galaxies with bright emission lines that were not observed on the NIRSpec masks.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.09503v3-abstract-full').style.display = 'inline'; document.getElementById('2307.09503v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.09503v3-abstract-full" style="display: none;"> We use James Webb Space Telescope Near-Infrared Camera Wide Field Slitless Spectroscopy (NIRCam WFSS) and Near-Infrared spectrograph (NIRSpec) in the Cosmic Evolution Early Release survey (CEERS) to measure rest-frame optical emission-line of 155 galaxies at z>2. The blind NIRCam grism observations include a sample of galaxies with bright emission lines that were not observed on the NIRSpec masks. We study the changes of the Ha, [OIII]/Hb, and [NeIII]/[OII] emission lines in terms of redshift by comparing to lower redshift SDSS and CLEAR samples. We find a significant (>3$蟽$) correlation between [OIII]/Hb with redshift, while [NeIII]/[OII] has a marginal (2$蟽$) correlation with redshift. We compare [OIII]/Hb and [NeIII]/[OII] to stellar mass and Hb SFR. We find that both emission-line ratios have a correlation with Hb SFR and an anti-correlation with stellar mass across the redshifts 0<z<9. Comparison with MAPPINGS~V models indicates that these trends are consistent with lower metallicity and higher ionization in low-mass and high-SFR galaxies. We additionally compare to IllustriousTNG predictions and find that they effectively describe the highest [OIII]/Hb ratios observed in our sample, without the need to invoke MAPPINGS models with significant shock ionizionation components. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.09503v3-abstract-full').style.display = 'none'; document.getElementById('2307.09503v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 11 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.14418">arXiv:2305.14418</a> <span> [<a href="https://arxiv.org/pdf/2305.14418">pdf</a>, <a href="https://arxiv.org/format/2305.14418">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Extremely red galaxies at $z=5-9$ with MIRI and NIRSpec: dusty galaxies or obscured AGNs? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Barro%2C+G">Guillermo Barro</a>, <a href="/search/astro-ph?searchtype=author&query=Perez-Gonzalez%2C+P+G">Pablo G. Perez-Gonzalez</a>, <a href="/search/astro-ph?searchtype=author&query=Kocevski%2C+D+D">Dale D. Kocevski</a>, <a href="/search/astro-ph?searchtype=author&query=McGrath%2C+E+J">Elizabeth J. McGrath</a>, <a href="/search/astro-ph?searchtype=author&query=Trump%2C+J+R">Jonathan R. Trump</a>, <a href="/search/astro-ph?searchtype=author&query=Simons%2C+R+C">Raymond C. Simons</a>, <a href="/search/astro-ph?searchtype=author&query=Somerville%2C+R+S">Rachel S. Somerville</a>, <a href="/search/astro-ph?searchtype=author&query=Yung%2C+L+Y+A">L. Y. Aaron Yung</a>, <a href="/search/astro-ph?searchtype=author&query=Haro%2C+P+A">Pablo Arrabal Haro</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M+B">Michaela B. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Costantin%2C+L">Luca Costantin</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+K">Kelcey Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steve L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Giavalisco%2C+M">Mauro Giavalisco</a>, <a href="/search/astro-ph?searchtype=author&query=Gomez-Guijarro%2C+C">Carlos Gomez-Guijarro</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N+P">Nimish P. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">Michaela Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Akins%2C+H+B">Hollis B. Akins</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">Benne W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Huertas-Company%2C+M">Marc Huertas-Company</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+R+A">Ray A. Lucas</a>, <a href="/search/astro-ph?searchtype=author&query=Papovich%2C+C">Casey Papovich</a>, <a href="/search/astro-ph?searchtype=author&query=Seille%2C+L">Lise-Marie Seille</a> , et al. (5 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2305.14418v1-abstract-short" style="display: inline;"> We study a new population of extremely red objects (EROs) recently discovered by JWST based on their NIRCam colors F277W$-$F444W $>1.5$ mag. We find 37 EROs in the CEERS field with F444W $<28$ mag and photometric redshifts between $5<z<7$, with median $z=6.9^{+1.0}_{-1.6}$. Surprisingly, despite their red long-wavelength colors, these EROs have blue short-wavelength colors (F150W$-$F200W$\sim$0 ma… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.14418v1-abstract-full').style.display = 'inline'; document.getElementById('2305.14418v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.14418v1-abstract-full" style="display: none;"> We study a new population of extremely red objects (EROs) recently discovered by JWST based on their NIRCam colors F277W$-$F444W $>1.5$ mag. We find 37 EROs in the CEERS field with F444W $<28$ mag and photometric redshifts between $5<z<7$, with median $z=6.9^{+1.0}_{-1.6}$. Surprisingly, despite their red long-wavelength colors, these EROs have blue short-wavelength colors (F150W$-$F200W$\sim$0 mag) indicative of bimodal SEDs with a red, steep slope in the rest-frame optical, and a blue, flat slope in the rest-frame UV. Moreover, all these EROs are unresolved, point-like sources in all NIRCam bands. We analyze the spectral energy distributions of 8 of them with MIRI and NIRSpec observations using stellar population models and AGN templates. We find that a dusty galaxy or an obscured AGN provide similarly good SED fits but different stellar properties: massive and dusty, log M/M_sun$\sim$10 and A$_{\rm V}\gtrsim3$ mag, or low mass and obscuration, log M/M_sun$\sim$7.5 and A$_{\rm V}\sim0$ mag, hosting an obscured QSO. SED modeling does not favor either scenario, but their unresolved sizes are more suggestive of an AGN. If any EROs are confirmed to have log M/M_sun$\gtrsim10.5$, it would increase pre-JWST number densities at $z>7$ by up to a factor $\sim$60. Similarly, if they are OSOs with luminosities in the L$_{\rm bol}>10^{46-47}$ erg s$^{-1}$ range, their number would exceed that of bright blue QSOs by more than two orders of magnitude. Additional photometry at mid-IR wavelengths will reveal the true nature of the red continuum emission in these EROs and will place this puzzling population in the right context of galaxy evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.14418v1-abstract-full').style.display = 'none'; document.getElementById('2305.14418v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">26 pages, 10 figures, submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.04953">arXiv:2305.04953</a> <span> [<a href="https://arxiv.org/pdf/2305.04953">pdf</a>, <a href="https://arxiv.org/format/2305.04953">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/acd4be">10.3847/1538-4357/acd4be <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CLEAR: The Morphological Evolution of Galaxies in the Green Valley </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Estrada-Carpenter%2C+V">Vicente Estrada-Carpenter</a>, <a href="/search/astro-ph?searchtype=author&query=Papovich%2C+C">Casey Papovich</a>, <a href="/search/astro-ph?searchtype=author&query=Momcheva%2C+I">Ivelina Momcheva</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">Gabriel Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Simons%2C+R+C">Raymond C. Simons</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Giavalisco%2C+M">Mauro Giavalisco</a>, <a href="/search/astro-ph?searchtype=author&query=Matharu%2C+J">Jasleen Matharu</a>, <a href="/search/astro-ph?searchtype=author&query=Trump%2C+J+R">Jonathan R. Trump</a>, <a href="/search/astro-ph?searchtype=author&query=Weiner%2C+B">Benjamin Weiner</a>, <a href="/search/astro-ph?searchtype=author&query=Ji%2C+Z">Zhiyuan Ji</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2305.04953v1-abstract-short" style="display: inline;"> Quiescent galaxies having more compact morphologies than star-forming galaxies has been a consistent result in the field of galaxy evolution. What is not clear is at what point this divergence happens, i.e. when do quiescent galaxies become compact, and how big of a role does the progenitor effect play in this result? Here we aim to model the morphological and star-formation histories of high reds… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.04953v1-abstract-full').style.display = 'inline'; document.getElementById('2305.04953v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.04953v1-abstract-full" style="display: none;"> Quiescent galaxies having more compact morphologies than star-forming galaxies has been a consistent result in the field of galaxy evolution. What is not clear is at what point this divergence happens, i.e. when do quiescent galaxies become compact, and how big of a role does the progenitor effect play in this result? Here we aim to model the morphological and star-formation histories of high redshift (0.8 $<$ z $<$ 1.65) massive galaxies (log(M/M$\odot$) $>$ 10.2) with stellar population fits using HST/WFC3 G102 and G141 grism spectra plus photometry from the CLEAR (CANDELS Lyman-alpha Emission at Reionization) survey, constraining the star-formation histories for a sample of $\sim$ 400 massive galaxies using flexible star-formation histories. We develop a novel approach to classifying galaxies by their formation activity in a way that highlights the green valley population, by modeling the specific star-formation rate distributions as a function of redshift and deriving the probability that a galaxy is quiescent (PQ). Using PQ and our flexible star-formation histories we outline the evolutionary paths of our galaxies in relation to stellar mass, Sersic index, $R_{eff}$, and stellar mass surface density. We find that galaxies show no appreciable stellar mass growth after entering the green valley (a net decrease of 4$\%$) while their stellar mass surface densities increase by $\sim$ 0.25 dex. Therefore galaxies are becoming compact during the green valley and this is due to increases in Sersic index and decreases in $R_{eff}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.04953v1-abstract-full').style.display = 'none'; document.getElementById('2305.04953v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 10 figures, submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.05385">arXiv:2304.05385</a> <span> [<a href="https://arxiv.org/pdf/2304.05385">pdf</a>, <a href="https://arxiv.org/format/2304.05385">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> CEERS: Diversity of Lyman-Alpha Emitters during the Epoch of Reionization </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jung%2C+I">Intae Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Haro%2C+P+A">Pablo Arrabal Haro</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+H+C">Henry C. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Hutchison%2C+T+A">Taylor A. Hutchison</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J+S">Jeyhan S. Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=Larson%2C+R+L">Rebecca L. Larson</a>, <a href="/search/astro-ph?searchtype=author&query=Simons%2C+R+C">Raymond C. Simons</a>, <a href="/search/astro-ph?searchtype=author&query=Papovich%2C+C">Casey Papovich</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+H">Hyunbae Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">Laura Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Trump%2C+J+R">Jonathan R. Trump</a>, <a href="/search/astro-ph?searchtype=author&query=Amorin%2C+R+O">Ricardo O. Amorin</a>, <a href="/search/astro-ph?searchtype=author&query=Backhaus%2C+B+E">Bren E. Backhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Casey%2C+C+M">Caitlin M. Casey</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+Y">Yingjie Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Cooper%2C+M+C">M. C. Cooper</a>, <a href="/search/astro-ph?searchtype=author&query=Cooper%2C+O+R">Olivia R. Cooper</a>, <a href="/search/astro-ph?searchtype=author&query=Gardner%2C+J+P">Jonathan P. Gardner</a>, <a href="/search/astro-ph?searchtype=author&query=Gawiser%2C+E">Eric Gawiser</a>, <a href="/search/astro-ph?searchtype=author&query=Grazian%2C+A">Andrea Grazian</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N+P">Nimish P. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">Michaela Hirschmann</a> , et al. (7 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.05385v1-abstract-short" style="display: inline;"> We analyze rest-frame ultraviolet to optical spectra of three $z\simeq7.47$ - $7.75$ galaxies whose Ly$伪$-emission lines were previously detected with Keck/MOSFIRE observations, using the JWST/NIRSpec observations from the Cosmic Evolution Early Release Science (CEERS) survey. From NIRSpec data, we confirm the systemic redshifts of these Ly$伪$ emitters, and emission-line ratio diagnostics indicate… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.05385v1-abstract-full').style.display = 'inline'; document.getElementById('2304.05385v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.05385v1-abstract-full" style="display: none;"> We analyze rest-frame ultraviolet to optical spectra of three $z\simeq7.47$ - $7.75$ galaxies whose Ly$伪$-emission lines were previously detected with Keck/MOSFIRE observations, using the JWST/NIRSpec observations from the Cosmic Evolution Early Release Science (CEERS) survey. From NIRSpec data, we confirm the systemic redshifts of these Ly$伪$ emitters, and emission-line ratio diagnostics indicate these galaxies were highly ionized and metal poor. We investigate Ly$伪$ line properties, including the line flux, velocity offset, and spatial extension. For the one galaxy where we have both NIRSpec and MOSFIRE measurements, we find a significant offset in their flux measurements ($\sim5\times$ greater in MOSFIRE) and a marginal difference in the velocity shifts. The simplest interpretation is that the Ly$伪$ emission is extended and not entirely encompassed by the NIRSpec slit. The cross-dispersion profiles in NIRSpec reveal that Ly$伪$ in one galaxy is significantly more extended than the non-resonant emission lines. We also compute the expected sizes of ionized bubbles that can be generated by the Ly$伪$ sources, discussing viable scenarios for the creation of sizable ionized bubbles ($>$1 physical Mpc). The source with the highest-ionization condition is possibly capable of ionizing its own bubble, while the other two do not appear to be capable of ionizing such a large region, requiring additional sources of ionizing photons. Therefore, the fact that we detect Ly$伪$ from these galaxies suggests diverse scenarios on escape of Ly$伪$ during the epoch of reionization. High spectral resolution spectra with JWST/NIRSpec will be extremely useful for constraining the physics of patchy reionization. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.05385v1-abstract-full').style.display = 'none'; document.getElementById('2304.05385v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to ApJ (18 pages, 7 figures, 2 tables)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.05378">arXiv:2304.05378</a> <span> [<a href="https://arxiv.org/pdf/2304.05378">pdf</a>, <a href="https://arxiv.org/format/2304.05378">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/acdd54">10.3847/2041-8213/acdd54 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spectroscopic Confirmation of CEERS NIRCam-selected Galaxies at $\boldsymbol{z \simeq 8-10}$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Haro%2C+P+A">Pablo Arrabal Haro</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Fujimoto%2C+S">Seiji Fujimoto</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez%2C+V">Vital Fern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J+S">Jeyhan S. Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+I">Intae Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+J+W">Justin W. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Burgarella%2C+D">Denis Burgarella</a>, <a href="/search/astro-ph?searchtype=author&query=Chworowsky%2C+K">Katherine Chworowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Hutchison%2C+T+A">Taylor A. Hutchison</a>, <a href="/search/astro-ph?searchtype=author&query=Morales%2C+A+M">Alexa M. Morales</a>, <a href="/search/astro-ph?searchtype=author&query=Papovich%2C+C">Casey Papovich</a>, <a href="/search/astro-ph?searchtype=author&query=Simons%2C+R+C">Raymond C. Simons</a>, <a href="/search/astro-ph?searchtype=author&query=Amor%C3%ADn%2C+R+O">Ricardo O. Amor铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Backhaus%2C+B+E">Bren E. Backhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M+B">Micaela B. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Bisigello%2C+L">Laura Bisigello</a>, <a href="/search/astro-ph?searchtype=author&query=Calabr%C3%B2%2C+A">Antonello Calabr貌</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">Marco Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Dav%C3%A9%2C+R">Romeel Dav茅</a>, <a href="/search/astro-ph?searchtype=author&query=Dekel%2C+A">Avishai Dekel</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+H+C">Henry C. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">Adriano Fontana</a> , et al. (23 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.05378v2-abstract-short" style="display: inline;"> We present JWST/NIRSpec prism spectroscopy of seven galaxies selected from the Cosmic Evolution Early Release Science Survey (CEERS) NIRCam imaging with photometric redshifts z_phot>8. We measure emission line redshifts of z=7.65 and 8.64 for two galaxies, and z=9.77(+0.37,-0.29) and 10.01(+0.14,-0.19) for two others via the detection of continuum breaks consistent with Lyman-alpha opacity from a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.05378v2-abstract-full').style.display = 'inline'; document.getElementById('2304.05378v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.05378v2-abstract-full" style="display: none;"> We present JWST/NIRSpec prism spectroscopy of seven galaxies selected from the Cosmic Evolution Early Release Science Survey (CEERS) NIRCam imaging with photometric redshifts z_phot>8. We measure emission line redshifts of z=7.65 and 8.64 for two galaxies, and z=9.77(+0.37,-0.29) and 10.01(+0.14,-0.19) for two others via the detection of continuum breaks consistent with Lyman-alpha opacity from a mostly neutral intergalactic medium. The presence (absense) of strong breaks (strong emission lines) give high confidence that these two galaxies are at z>9.6, but the break-derived redshifts have large uncertainties given the low spectral resolution and relatively low signal-to-noise of the CEERS NIRSpec prism data. The two z~10 sources are relatively luminous (M_UV<-20), with blue continua (-2.3<beta<-1.9) and low dust attenuation (A_V=0.15(+0.3,-0.1)); and at least one of them has high stellar mass for a galaxy at that redshift (log(M_*/M_sol)=9.3(+0.2,-0.3)). Considered together with spectroscopic observations of other CEERS NIRCam-selected high-z galaxy candidates in the literature, we find a high rate of redshift confirmation and low rate of confirmed interlopers (8.3%). Ten out of 34 z>8 candidates with CEERS NIRSpec spectroscopy do not have secure redshifts, but the absence of emission lines in their spectra is consistent with redshifts z>9.6. We find that z>8 photometric redshifts are generally in agreement (within uncertainties) with the spectroscopic values. However, the photometric redshifts tend to be slightly overestimated (average Delta(z)=0.50+/-0.12), suggesting that current templates do not fully describe the spectra of very high-z sources. Overall, our results solidifies photometric evidence for a high space density of bright galaxies at z>8 compared to theoretical model predictions, and further disfavors an accelerated decline in the integrated UV luminosity density at z>8. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.05378v2-abstract-full').style.display = 'none'; document.getElementById('2304.05378v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published in ApJL. 19 pages, 9 figures, 7 tables. File with Table 6 included in source .tar file</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys. J. Lett. 951, L22 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.11736">arXiv:2303.11736</a> <span> [<a href="https://arxiv.org/pdf/2303.11736">pdf</a>, <a href="https://arxiv.org/format/2303.11736">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/acd639">10.3847/2041-8213/acd639 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CEERS Key Paper VI: JWST/MIRI Uncovers a Large Population of Obscured AGN at High Redshifts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yang%2C+G">G. Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Caputi%2C+K+I">K. I. Caputi</a>, <a href="/search/astro-ph?searchtype=author&query=Papovich%2C+C">C. Papovich</a>, <a href="/search/astro-ph?searchtype=author&query=Haro%2C+P+A">P. Arrabal Haro</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M+B">M. B. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Behroozi%2C+P">P. Behroozi</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">E. F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Bisigello%2C+L">L. Bisigello</a>, <a href="/search/astro-ph?searchtype=author&query=Buat%2C+V">V. Buat</a>, <a href="/search/astro-ph?searchtype=author&query=Burgarella%2C+D">D. Burgarella</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+Y">Y. Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">N. J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Dave%2C+R">R. Dave</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">M. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Elbaz%2C+D">D. Elbaz</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+H+C">H. C. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">S. L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">N. A. Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N+P">N. P. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">M. Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">B. W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Huertas-Company%2C+M">M. Huertas-Company</a>, <a href="/search/astro-ph?searchtype=author&query=Hutchison%2C+T">T. Hutchison</a>, <a href="/search/astro-ph?searchtype=author&query=Iani%2C+E">E. Iani</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J+S">J. S. Kartaltepe</a> , et al. (13 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.11736v2-abstract-short" style="display: inline;"> Mid-infrared observations are powerful in identifying heavily obscured Active Galactic Nuclei (AGN) which have weak emission in other wavelengths. Data from the Mid-Infrared Instrument (MIRI) onboard JWST provides an excellent opportunity to perform such studies. We take advantage of the MIRI imaging data from the Cosmic Evolution Early Release Science Survey (CEERS) to investigate the AGN populat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.11736v2-abstract-full').style.display = 'inline'; document.getElementById('2303.11736v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.11736v2-abstract-full" style="display: none;"> Mid-infrared observations are powerful in identifying heavily obscured Active Galactic Nuclei (AGN) which have weak emission in other wavelengths. Data from the Mid-Infrared Instrument (MIRI) onboard JWST provides an excellent opportunity to perform such studies. We take advantage of the MIRI imaging data from the Cosmic Evolution Early Release Science Survey (CEERS) to investigate the AGN population in the distant universe. We estimate the source properties of MIRI-selected objects by utilizing spectral energy distribution (SED) modelling, and classify them into star-forming galaxies (SF), SF-AGN mixed objects, and AGN. The source numbers of these types are 418, 111, and 31, respectively, from 4 MIRI pointings covering $\sim 9$ arcmin$^2$. The sample spans a redshift range of $\approx 0$--5. We derive the median SEDs for all three source types, respectively, and publicly release them. The median MIRI SED of AGN is similar to the typical SEDs of hot dust-obscured galaxies and Seyfert 2s, for which the mid-IR SEDs are dominantly from AGN-heated hot dust. Based on our SED-fit results, we estimate the black-hole accretion density (BHAD; i.e., total BH growth rate per comoving volume) as a function of redshift. At $z<3$, the resulting BHAD agrees with the X-ray measurements in general. At $z>3$, we identify a total of 27 AGN and SF-AGN mixed objects, leading to that our high-$z$ BHAD is substantially higher than the X-ray results ($\sim 0.5$ dex at $z \approx 3$--5). This difference indicates MIRI can identify a large population of heavily obscured AGN missed by X-ray surveys at high redshifts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.11736v2-abstract-full').style.display = 'none'; document.getElementById('2303.11736v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">ApJL in press, as part of the CEERS Focus Issue. 13 pages and 7 figures (median SEDs in Fig. 5 are available upon request)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.09570">arXiv:2303.09570</a> <span> [<a href="https://arxiv.org/pdf/2303.09570">pdf</a>, <a href="https://arxiv.org/format/2303.09570">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/acc517">10.3847/1538-4365/acc517 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CLEAR: Survey Overview, Data Analysis and Products </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Simons%2C+R+C">Raymond C. Simons</a>, <a href="/search/astro-ph?searchtype=author&query=Papovich%2C+C">Casey Papovich</a>, <a href="/search/astro-ph?searchtype=author&query=Momcheva%2C+I+G">Ivelina G. Momcheva</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">Gabriel Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Estrada-Carpenter%2C+V">Vicente Estrada-Carpenter</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Gosmeyer%2C+C+M">Catherine M. Gosmeyer</a>, <a href="/search/astro-ph?searchtype=author&query=Matharu%2C+J">Jasleen Matharu</a>, <a href="/search/astro-ph?searchtype=author&query=Trump%2C+J+R">Jonathan R. Trump</a>, <a href="/search/astro-ph?searchtype=author&query=Backhaus%2C+B+E">Bren E. Backhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+Y">Yingjie Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+H+C">Henry C. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Finlator%2C+K">Kristian Finlator</a>, <a href="/search/astro-ph?searchtype=author&query=Giavalisco%2C+M">Mauro Giavalisco</a>, <a href="/search/astro-ph?searchtype=author&query=Ji%2C+Z">Zhiyuan Ji</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+I">Intae Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Lotz%2C+J+M">Jennifer M. Lotz</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Brien%2C+R">Rosalia O'Brien</a>, <a href="/search/astro-ph?searchtype=author&query=Skelton%2C+R+E">Rosalind E. Skelton</a>, <a href="/search/astro-ph?searchtype=author&query=Tilvi%2C+V">Vithal Tilvi</a>, <a href="/search/astro-ph?searchtype=author&query=Weiner%2C+B">Benjamin Weiner</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.09570v1-abstract-short" style="display: inline;"> We present an overview of the CANDELS Lyman-a Emission At Reionization (CLEAR) survey. CLEAR is a 130 orbit program of the Hubble Space Telescope using the Wide Field Camera 3 (WFC3) IR G102 grism. CLEAR targets 12 pointings divided between the GOODS-N and GOODS-S fields of the Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey (CANDELS). Combined with existing spectroscopic data from other… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.09570v1-abstract-full').style.display = 'inline'; document.getElementById('2303.09570v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.09570v1-abstract-full" style="display: none;"> We present an overview of the CANDELS Lyman-a Emission At Reionization (CLEAR) survey. CLEAR is a 130 orbit program of the Hubble Space Telescope using the Wide Field Camera 3 (WFC3) IR G102 grism. CLEAR targets 12 pointings divided between the GOODS-N and GOODS-S fields of the Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey (CANDELS). Combined with existing spectroscopic data from other programs, the full CLEAR dataset includes spectroscopic imaging of these fields over 0.8-1.7 um. In this Paper, we describe the CLEAR survey, the survey strategy, the data acquisition, reduction, processing, and science products and catalogs released alongside this paper. The catalogs include emission line fluxes and redshifts derived from the combination of the photometry and grism spectroscopy for 6048 galaxies, primarily ranging from 0.2 < z < 3. We also provide an overview of CLEAR science goals and results. In conjunction with this Paper we provide links to electronic versions of the data products, including 1D + 2D extracted spectra and emission line maps. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.09570v1-abstract-full').style.display = 'none'; document.getElementById('2303.09570v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted in ApJS. 29 pages, 14 figures. The data products (1D + 2D spectra, emission line maps) and catalogs (photometric and spectroscopic catalogs of GOODS-N and GOODS-S) are available at https://archive.stsci.edu/hlsp/clear</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.08918">arXiv:2303.08918</a> <span> [<a href="https://arxiv.org/pdf/2303.08918">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/ace619">10.3847/2041-8213/ace619 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A CEERS Discovery of an Accreting Supermassive Black Hole 570 Myr after the Big Bang: Identifying a Progenitor of Massive z > 6 Quasars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Larson%2C+R+L">Rebecca L. Larson</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Kocevski%2C+D+D">Dale D. Kocevski</a>, <a href="/search/astro-ph?searchtype=author&query=Hutchison%2C+T+A">Taylor A. Hutchison</a>, <a href="/search/astro-ph?searchtype=author&query=Trump%2C+J+R">Jonathan R. Trump</a>, <a href="/search/astro-ph?searchtype=author&query=Haro%2C+P+A">Pablo Arrabal Haro</a>, <a href="/search/astro-ph?searchtype=author&query=Bromm%2C+V">Volker Bromm</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Fujimoto%2C+S">Seiji Fujimoto</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J+S">Jeyhan S. Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Papovich%2C+C">Casey Papovich</a>, <a href="/search/astro-ph?searchtype=author&query=Pirzkal%2C+N">Nor Pirzkal</a>, <a href="/search/astro-ph?searchtype=author&query=Tacchella%2C+S">Sandro Tacchella</a>, <a href="/search/astro-ph?searchtype=author&query=Zavala%2C+J+A">Jorge A. Zavala</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M">Micaela Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Behroozi%2C+P">Peter Behroozi</a>, <a href="/search/astro-ph?searchtype=author&query=Champagne%2C+J+B">Jaclyn B. Champagne</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+J+W">Justin W. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+I">Intae Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Morales%2C+A+M">Alexa M. Morales</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+G">Guang Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+H">Haowen Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Zitrin%2C+A">Adi Zitrin</a> , et al. (27 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.08918v2-abstract-short" style="display: inline;"> We report the discovery of an accreting supermassive black hole at z=8.679, in CEERS_1019, a galaxy previously discovered via a Ly$伪$-break by Hubble and with a Ly$伪$ redshift from Keck. As part of the Cosmic Evolution Early Release Science (CEERS) survey, we observed this source with JWST/NIRSpec spectroscopy, MIRI and NIRCam imaging, and NIRCam/WFSS slitless spectroscopy. The NIRSpec spectra unc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.08918v2-abstract-full').style.display = 'inline'; document.getElementById('2303.08918v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.08918v2-abstract-full" style="display: none;"> We report the discovery of an accreting supermassive black hole at z=8.679, in CEERS_1019, a galaxy previously discovered via a Ly$伪$-break by Hubble and with a Ly$伪$ redshift from Keck. As part of the Cosmic Evolution Early Release Science (CEERS) survey, we observed this source with JWST/NIRSpec spectroscopy, MIRI and NIRCam imaging, and NIRCam/WFSS slitless spectroscopy. The NIRSpec spectra uncover many emission lines, and the strong [O III] emission line confirms the ground-based Ly$伪$ redshift. We detect a significant broad (FWHM~1200 km/s) component in the H$尾$ emission line, which we conclude originates in the broad-line region of an active galactic nucleus (AGN), as the lack of a broad component in the forbidden lines rejects an outflow origin. This hypothesis is supported by the presence of high-ionization lines, as well as a spatial point-source component embedded within a smoother surface brightness profile. The mass of the black hole is log($M_{BH}/M_{\odot})=6.95{\pm}0.37$, and we estimate that it is accreting at 1.2 ($\pm$0.5) x the Eddington limit. The 1-8 $渭$m photometric spectral energy distribution (SED) from NIRCam and MIRI shows a continuum dominated by starlight and constrains the host galaxy to be massive (log M/M$_{\odot}$~9.5) and highly star-forming (SFR~30 M$_{\odot}$ yr$^{-1}$). Ratios of the strong emission lines show that the gas in this galaxy is metal-poor (Z/Z$_{\odot}$~0.1), dense (n$_{e}$~10$^{3}$ cm$^{-3}$), and highly ionized (log U~-2.1), consistent with the general galaxy population observed with JWST at high redshifts. We use this presently highest-redshift AGN discovery to place constraints on black hole seeding models and find that a combination of either super-Eddington accretion from stellar seeds or Eddington accretion from massive black hole seeds is required to form this object by the observed epoch. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.08918v2-abstract-full').style.display = 'none'; document.getElementById('2303.08918v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">26 pages, 14 figures, 6 tables, published in ApJL</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal Letters, 2023, Volume 953, Issue 2, id.L29, 26 pp </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.00012">arXiv:2302.00012</a> <span> [<a href="https://arxiv.org/pdf/2302.00012">pdf</a>, <a href="https://arxiv.org/ps/2302.00012">ps</a>, <a href="https://arxiv.org/format/2302.00012">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Hidden Little Monsters: Spectroscopic Identification of Low-Mass, Broad-Line AGN at $z>5$ with CEERS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kocevski%2C+D+D">Dale D. Kocevski</a>, <a href="/search/astro-ph?searchtype=author&query=Onoue%2C+M">Masafusa Onoue</a>, <a href="/search/astro-ph?searchtype=author&query=Inayoshi%2C+K">Kohei Inayoshi</a>, <a href="/search/astro-ph?searchtype=author&query=Trump%2C+J+R">Jonathan R. Trump</a>, <a href="/search/astro-ph?searchtype=author&query=Haro%2C+P+A">Pablo Arrabal Haro</a>, <a href="/search/astro-ph?searchtype=author&query=Grazian%2C+A">Andrea Grazian</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J+S">Jeyhan S. Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">Michaela Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Fujimoto%2C+S">Seiji Fujimoto</a>, <a href="/search/astro-ph?searchtype=author&query=Juneau%2C+S">Stephanie Juneau</a>, <a href="/search/astro-ph?searchtype=author&query=Amorin%2C+R+O">Ricardo O. Amorin</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M+B">Micaela B. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Barro%2C+G">Guillermo Barro</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Bisigello%2C+L">Laura Bisigello</a>, <a href="/search/astro-ph?searchtype=author&query=Calabro%2C+A">Antonello Calabro</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Cooper%2C+M+C">M. C. Cooper</a>, <a href="/search/astro-ph?searchtype=author&query=Ding%2C+X">Xuheng Ding</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">Norman A. Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Ho%2C+L+C">Luis C. Ho</a>, <a href="/search/astro-ph?searchtype=author&query=Inoue%2C+A+K">Akio K. Inoue</a>, <a href="/search/astro-ph?searchtype=author&query=Jiang%2C+L">Linhua Jiang</a> , et al. (12 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.00012v1-abstract-short" style="display: inline;"> We report on the discovery of two low-luminosity, broad-line AGN at $z>5$ identified using JWST NIRSpec spectroscopy from the CEERS Survey. We detect broad H$伪$ emission from both sources, with FWHM of $2038\pm286$ and $1807\pm207$ km s$^{-1}$, resulting in black hole (BH) masses that are 1-2 dex below that of existing samples of luminous quasars at $z>5$. The first source, CEERS 1670 at… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.00012v1-abstract-full').style.display = 'inline'; document.getElementById('2302.00012v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.00012v1-abstract-full" style="display: none;"> We report on the discovery of two low-luminosity, broad-line AGN at $z>5$ identified using JWST NIRSpec spectroscopy from the CEERS Survey. We detect broad H$伪$ emission from both sources, with FWHM of $2038\pm286$ and $1807\pm207$ km s$^{-1}$, resulting in black hole (BH) masses that are 1-2 dex below that of existing samples of luminous quasars at $z>5$. The first source, CEERS 1670 at $z=5.242$, is 2-3 dex fainter than known quasars at similar redshifts and was previously identified as a candidate low-luminosity AGN based on its rest-frame optical SED. We measure a BH mass of $M_{\rm BH}=1.3\pm0.4\times 10^{7}~M_{\odot}$, confirming that this AGN is powered by the least-massive BH known in the universe at the end of cosmic reionization. The second source, CEERS 3210 at $z=5.624$, is inferred to be a heavily obscured, broad-line AGN caught in a transition phase between a dust-obscured starburst and an unobscured quasar. We estimate its BH mass to be $M_{\rm BH}\simeq 0.9-4.7 \times 10^{7}~M_{\odot}$, depending on the level of dust obscuration assumed. We derive host stellar masses, $M_\star$, allowing us to place constraints on the BH-galaxy mass relationship in the lowest mass range yet probed in the early universe. The $M_{\rm BH}/M_\star$ ratio for CEERS 1670, in particular, is consistent with or higher than the empirical relationship seen in massive galaxies at $z=0$. We examine the emission-line ratios of both sources and find that their location on the BPT and OHNO diagrams is consistent with model predictions for low-metallicity AGN with $Z/Z_\odot \simeq 0.2-0.4$. The spectroscopic identification of low-luminosity, broad-line AGN at $z>5$ with $M_{\rm BH}\simeq 10^{7}~M_{\odot}$ demonstrates the capability of JWST to push BH masses closer to the range predicted for the BH seed population and provides a unique opportunity to study the early stages of BH-galaxy assembly. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.00012v1-abstract-full').style.display = 'none'; document.getElementById('2302.00012v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 8 figures, submitted to ApJL</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.07745">arXiv:2301.07745</a> <span> [<a href="https://arxiv.org/pdf/2301.07745">pdf</a>, <a href="https://arxiv.org/format/2301.07745">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/acde55">10.3847/1538-4357/acde55 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Using [Ne V]/[Ne III] to Understand the Nature of Extreme-Ionization Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Olivier%2C+G+M">Grace M. Olivier</a>, <a href="/search/astro-ph?searchtype=author&query=Hutchison%2C+T+A">Taylor A. Hutchison</a>, <a href="/search/astro-ph?searchtype=author&query=Papovich%2C+C">Casey Papovich</a>, <a href="/search/astro-ph?searchtype=author&query=Trump%2C+J+R">Jonathan R. Trump</a>, <a href="/search/astro-ph?searchtype=author&query=Amorin%2C+R+O">Ricardo O. Amorin</a>, <a href="/search/astro-ph?searchtype=author&query=Backhaus%2C+B+E">Bren E. Backhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Berg%2C+D+A">Danielle A. Berg</a>, <a href="/search/astro-ph?searchtype=author&query=Fernandez%2C+V">Vital Fernandez</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Fujimoto%2C+S">Seiji Fujimoto</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">Michaela Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J+S">Jeyhan S. Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=Kocevski%2C+D+D">Dale D. Kocevski</a>, <a href="/search/astro-ph?searchtype=author&query=Simons%2C+R+C">Raymond C. Simons</a>, <a href="/search/astro-ph?searchtype=author&query=Wilkins%2C+S+M">Stephen M. Wilkins</a>, <a href="/search/astro-ph?searchtype=author&query=Yung%2C+L+Y+A">L. Y. Aaron Yung</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2301.07745v2-abstract-short" style="display: inline;"> Spectroscopic studies of extreme-ionization galaxies (EIGs) are critical to our understanding of exotic systems throughout cosmic time. These EIGs exhibit spectral features requiring >54.42 eV photons: the energy needed to fully ionize helium into He2+ and emit He II recombination lines. They are likely key contributors to reionization, and they can also probe exotic stellar populations or accreti… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.07745v2-abstract-full').style.display = 'inline'; document.getElementById('2301.07745v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.07745v2-abstract-full" style="display: none;"> Spectroscopic studies of extreme-ionization galaxies (EIGs) are critical to our understanding of exotic systems throughout cosmic time. These EIGs exhibit spectral features requiring >54.42 eV photons: the energy needed to fully ionize helium into He2+ and emit He II recombination lines. They are likely key contributors to reionization, and they can also probe exotic stellar populations or accretion onto massive black holes. To facilitate the use of EIGs as probes of high ionization, we focus on ratios constructed from strong rest-frame UV/optical emission lines, specifically [O III] 5008, H-beta, [Ne III] 3870, [O II] 3727,3729, and [Ne V] 3427. These lines probe the relative intensity at energies of 35.12, 13.62, 40.96, 13.62 eV, and 97.12, respectively, covering a wider range of ionization than traced by other common rest-frame UV/optical techniques. We use ratios of these lines ([Ne V]/[Ne III] = Ne53 and [Ne III]/[O II]), which are closely separated in wavelength, and mitigates effects of dust attenuation and uncertainties in flux calibration. We make predictions from photoionization models constructed from Cloudy that use a broad range of stellar populations and black hole accretion models to explore the sensitivity of these line ratios to changes in the ionizing spectrum. We compare our models to observations from the Hubble Space Telescope and James Webb Space Telescope of galaxies with strong high-ionization emission lines at z ~ 0, z ~ 2, and z ~ 7. We show that the Ne53 ratio can separate galaxies with ionization from 'normal' stellar populations from those with AGN and even 'exotic' Population III models. We introduce new selection methods to identify galaxies with photoionization driven by Population III stars or intermediate-mass black hole accretion disks that could be identified in upcoming high-redshift spectroscopic surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.07745v2-abstract-full').style.display = 'none'; document.getElementById('2301.07745v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 5 figures, 1 table. Accepted in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.00027">arXiv:2301.00027</a> <span> [<a href="https://arxiv.org/pdf/2301.00027">pdf</a>, <a href="https://arxiv.org/format/2301.00027">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/acc948">10.3847/2041-8213/acc948 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CEERS Key Paper IV: Galaxies at $4 < z < 9$ are Bluer than They Appear -- Characterizing Galaxy Stellar Populations from Rest-Frame $\sim 1$ micron Imaging </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Papovich%2C+C">Casey Papovich</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+J">Justin Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+G">Guang Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Barro%2C+G">Guillermo Barro</a>, <a href="/search/astro-ph?searchtype=author&query=Buat%2C+V">V茅ronique Buat</a>, <a href="/search/astro-ph?searchtype=author&query=Burgarella%2C+D">Denis Burgarella</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Gonz%C3%A1lez%2C+P+G">Pablo G. P茅rez-Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Santini%2C+P">Paola Santini</a>, <a href="/search/astro-ph?searchtype=author&query=Seill%C3%A9%2C+L">Lise-Marie Seill茅</a>, <a href="/search/astro-ph?searchtype=author&query=Shen%2C+L">Lu Shen</a>, <a href="/search/astro-ph?searchtype=author&query=Haro%2C+P+A">Pablo Arrabal Haro</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M+B">Micaela B. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Bisigello%2C+L">Laura Bisigello</a>, <a href="/search/astro-ph?searchtype=author&query=Calabr%C3%B2%2C+A">Antonello Calabr貌</a>, <a href="/search/astro-ph?searchtype=author&query=Casey%2C+C+M">Caitlin M. Casey</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">Marco Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Chworowsky%2C+K">Katherine Chworowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Cooper%2C+M+C">M. C. Cooper</a>, <a href="/search/astro-ph?searchtype=author&query=Costantin%2C+L">Luca Costantin</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+H+C">Henry C. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">Adriano Fontana</a> , et al. (24 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2301.00027v2-abstract-short" style="display: inline;"> We present results from the Cosmic Evolution Early Release Survey (CEERS) on the stellar-population parameters for 28 galaxies with redshifts $4<z<9$ using imaging data from the James Webb Space Telescope (JWST) Mid-Infrared Instrument (MIRI) combined with data from the Hubble Space Telescope and the Spitzer Space Telescope. The JWST/MIRI 5.6 and 7.7 $渭$m data extend the coverage of the rest-frame… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.00027v2-abstract-full').style.display = 'inline'; document.getElementById('2301.00027v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.00027v2-abstract-full" style="display: none;"> We present results from the Cosmic Evolution Early Release Survey (CEERS) on the stellar-population parameters for 28 galaxies with redshifts $4<z<9$ using imaging data from the James Webb Space Telescope (JWST) Mid-Infrared Instrument (MIRI) combined with data from the Hubble Space Telescope and the Spitzer Space Telescope. The JWST/MIRI 5.6 and 7.7 $渭$m data extend the coverage of the rest-frame spectral-energy distribution (SED) to nearly 1 micron for galaxies in this redshift range. By modeling the galaxies' SEDs the MIRI data show that the galaxies have, on average, rest-frame UV (1600 脜) $-$ $I$-band colors 0.4 mag bluer than derived when using photometry that lacks MIRI. Therefore, the galaxies have lower (stellar)-mass-to-light ratios. The MIRI data reduce the stellar masses by $\langle 螖\log M_\ast\rangle=0.25$ dex at $4<z<6$ (a factor of 1.8) and 0.37 dex at $6<z<9$ (a factor of 2.3). This also reduces the star-formation rates (SFRs) by $\langle 螖\log\mathrm{SFR} \rangle=0.14$ dex at $4<z<6$ and 0.27 dex at $6<z<9$. The MIRI data also improve constraints on the allowable stellar mass formed in early star-formation. We model this using a star-formation history that includes both a "burst' at $z_f=100$ and a slowly varying ("delayed-$蟿$") model. The MIRI data reduce the allowable stellar mass by 0.6 dex at $4<z< 6$ and by $\approx$1 dex at $6<z<9$. Applying these results globally, this reduces the cosmic stellar-mass density by an order of magnitude in the early universe ($z\approx9$). Therefore, observations of rest-frame $\gtrsim$1 $渭$m are paramount for constraining the stellar-mass build-up in galaxies at very high-redshifts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.00027v2-abstract-full').style.display = 'none'; document.getElementById('2301.00027v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Updated with accepted ApJ version. Part of the CEERS Focus Issue. 27 pages, many figures (4 Figure Sets, available upon reasonable request)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.09850">arXiv:2212.09850</a> <span> [<a href="https://arxiv.org/pdf/2212.09850">pdf</a>, <a href="https://arxiv.org/format/2212.09850">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> New $z > 7$ Lyman-alpha Emitters in EGS: Evidence of an Extended Ionized Structure at $z \sim 7.7$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jung%2C+I">Intae Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Larson%2C+R+L">Rebecca L. Larson</a>, <a href="/search/astro-ph?searchtype=author&query=Hutchison%2C+T+A">Taylor A. Hutchison</a>, <a href="/search/astro-ph?searchtype=author&query=Straughn%2C+A+N">Amber N. Straughn</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M+B">Micaela B. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">Marco Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Cooper%2C+M+C">M. C. Cooper</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+H+C">Henry C. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">Benne W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J+S">Jeyhan S. Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Seonwoo Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Papovich%2C+C">Casey Papovich</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+H">Hyunbae Park</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">Laura Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Perez-Gonzalez%2C+P+G">Pablo G. Perez-Gonzalez</a>, <a href="/search/astro-ph?searchtype=author&query=Song%2C+M">Mimi Song</a>, <a href="/search/astro-ph?searchtype=author&query=Tacchella%2C+S">Sandro Tacchella</a>, <a href="/search/astro-ph?searchtype=author&query=Weiner%2C+B+J">Benjamin J. Weiner</a>, <a href="/search/astro-ph?searchtype=author&query=Willmer%2C+C+N+A">Christopher N. A. Willmer</a>, <a href="/search/astro-ph?searchtype=author&query=Zavala%2C+J+A">Jorge A. Zavala</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2212.09850v1-abstract-short" style="display: inline;"> We perform a ground-based near-infrared spectroscopic survey using the Keck/MOSFIRE spectrograph to target Ly$伪$ emission at $7.0<z<8.2$ from 61 galaxies to trace the ionization state of the intergalactic medium (IGM). We cover a total effective sky area of $\sim10^\prime\times10^\prime$ in the Extended Groth Strip field of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey. From o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.09850v1-abstract-full').style.display = 'inline'; document.getElementById('2212.09850v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.09850v1-abstract-full" style="display: none;"> We perform a ground-based near-infrared spectroscopic survey using the Keck/MOSFIRE spectrograph to target Ly$伪$ emission at $7.0<z<8.2$ from 61 galaxies to trace the ionization state of the intergalactic medium (IGM). We cover a total effective sky area of $\sim10^\prime\times10^\prime$ in the Extended Groth Strip field of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey. From our observations, we detect Ly$伪$ emission at a $>$4$蟽$ level in eight $z>7$ galaxies, which include additional members of the known $z\sim7.7$ Ly$伪$-emitter (LAE) cluster (Tilvi et al. 2020). With the addition of these newly-discovered $z\sim7.7$ LAEs, this is currently the largest measured LAE cluster at $z>7$. The unusually-high Ly$伪$ detection rate at $z\sim7.7$ in this field suggests significantly stronger Ly$伪$ emission from the clustered LAEs than from the rest of our targets. We estimate the ionized bubble sizes around these LAEs and conclude that the LAEs are clustered within an extended ionized structure created by overlapping ionized bubbles which allow the easier escape of Ly$伪$ from galaxies. It is remarkable that the brightest object in the cluster has the lowest measured redshift of the Ly$伪$ line, being placed in front of the other LAEs in the line-of-sight direction. This suggests that we are witnessing the enhanced IGM transmission of Ly$伪$ from galaxies on the rear side of an ionized area. This could be a consequence of Ly$伪$ radiative transfer: Ly$伪$ close to the central velocity is substantially scattered by the IGM while Ly$伪$ from the rear-side galaxies is significantly redshifted to where it has a clear path. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.09850v1-abstract-full').style.display = 'none'; document.getElementById('2212.09850v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to ApJ (17 pages, 8 figures, 4 tables)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.05792">arXiv:2211.05792</a> <span> [<a href="https://arxiv.org/pdf/2211.05792">pdf</a>, <a href="https://arxiv.org/format/2211.05792">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/acade4">10.3847/2041-8213/acade4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CEERS Key Paper I: An Early Look into the First 500 Myr of Galaxy Formation with JWST </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M+B">Micaela B. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+H+C">Henry C. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Wilkins%2C+S+M">Stephen M. Wilkins</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J+S">Jeyhan S. Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=Papovich%2C+C">Casey Papovich</a>, <a href="/search/astro-ph?searchtype=author&query=Yung%2C+L+Y+A">L. Y. Aaron Yung</a>, <a href="/search/astro-ph?searchtype=author&query=Haro%2C+P+A">Pablo Arrabal Haro</a>, <a href="/search/astro-ph?searchtype=author&query=Behroozi%2C+P">Peter Behroozi</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Kocevski%2C+D+D">Dale D. Kocevski</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Larson%2C+R+L">Rebecca L. Larson</a>, <a href="/search/astro-ph?searchtype=author&query=Bail%2C+A+L">Aurelien Le Bail</a>, <a href="/search/astro-ph?searchtype=author&query=Morales%2C+A+M">Alexa M. Morales</a>, <a href="/search/astro-ph?searchtype=author&query=Perez-Gonzalez%2C+P+G">Pablo G. Perez-Gonzalez</a>, <a href="/search/astro-ph?searchtype=author&query=Burgarella%2C+D">Denis Burgarella</a>, <a href="/search/astro-ph?searchtype=author&query=Dave%2C+R">Romeel Dave</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">Michaela Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Somerville%2C+R+S">Rachel S. Somerville</a>, <a href="/search/astro-ph?searchtype=author&query=Wuyts%2C+S">Stijn Wuyts</a>, <a href="/search/astro-ph?searchtype=author&query=Bromm%2C+V">Volker Bromm</a>, <a href="/search/astro-ph?searchtype=author&query=Casey%2C+C+M">Caitlin M. Casey</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">Adriano Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Fujimoto%2C+S">Seiji Fujimoto</a> , et al. (42 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2211.05792v2-abstract-short" style="display: inline;"> We present an investigation into the first 500 Myr of galaxy evolution from the Cosmic Evolution Early Release Science (CEERS) survey. CEERS, one of 13 JWST ERS programs, targets galaxy formation from z~0.5 to z>10 using several imaging and spectroscopic modes. We make use of the first epoch of CEERS NIRCam imaging, spanning 35.5 sq. arcmin, to search for candidate galaxies at z>9. Following a det… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.05792v2-abstract-full').style.display = 'inline'; document.getElementById('2211.05792v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.05792v2-abstract-full" style="display: none;"> We present an investigation into the first 500 Myr of galaxy evolution from the Cosmic Evolution Early Release Science (CEERS) survey. CEERS, one of 13 JWST ERS programs, targets galaxy formation from z~0.5 to z>10 using several imaging and spectroscopic modes. We make use of the first epoch of CEERS NIRCam imaging, spanning 35.5 sq. arcmin, to search for candidate galaxies at z>9. Following a detailed data reduction process implementing several custom steps to produce high-quality reduced images, we perform multi-band photometry across seven NIRCam broad and medium-band (and six Hubble broadband) filters focusing on robust colors and accurate total fluxes. We measure photometric redshifts and devise a robust set of selection criteria to identify a sample of 26 galaxy candidates at z~9-16. These objects are compact with a median half-light radius of ~0.5 kpc. We present an early estimate of the z~11 rest-frame ultraviolet (UV) luminosity function, finding that the number density of galaxies at M_UV ~ -20 appears to evolve very little from z~9 to z~11. We also find that the abundance (surface density [arcmin^-2]) of our candidates exceeds nearly all theoretical predictions. We explore potential implications, including that at z>10 star formation may be dominated by top-heavy initial mass functions, which would result in an increased ratio of UV light per unit halo mass, though a complete lack of dust attenuation and/or changing star-formation physics may also play a role. While spectroscopic confirmation of these sources is urgently required, our results suggest that the deeper views to come with JWST should yield prolific samples of ultra-high-redshift galaxies with which to further explore these conclusions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.05792v2-abstract-full').style.display = 'none'; document.getElementById('2211.05792v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Replaced with published version</span> </p> </li> 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