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</a> </li> <li> <a href="/search/?searchtype=author&query=Kocevski%2C+D&start=200" class="pagination-link " aria-label="Page 5" aria-current="page">5 </a> </li> <li> <a href="/search/?searchtype=author&query=Kocevski%2C+D&start=250" class="pagination-link " aria-label="Page 6" aria-current="page">6 </a> </li> <li> <a href="/search/?searchtype=author&query=Kocevski%2C+D&start=300" class="pagination-link " aria-label="Page 7" aria-current="page">7 </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/2502.02637">arXiv:2502.02637</a> <span> [<a href="https://arxiv.org/pdf/2502.02637">pdf</a>, <a href="https://arxiv.org/format/2502.02637">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"> Ultra High-Redshift or Closer-by, Dust-Obscured Galaxies? Deciphering the Nature of Faint, Previously Missed F200W-Dropouts in CEERS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gandolfi%2C+G">G. Gandolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Rodighiero%2C+G">G. Rodighiero</a>, <a href="/search/astro-ph?searchtype=author&query=Bisigello%2C+L">L. Bisigello</a>, <a href="/search/astro-ph?searchtype=author&query=Grazian%2C+A">A. Grazian</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=Dickinson%2C+M">M. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Merlin%2C+E">E. Merlin</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=Papovich%2C+C">C. Papovich</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchetti%2C+A">A. Bianchetti</a>, <a href="/search/astro-ph?searchtype=author&query=Ba%C3%B1ados%2C+E">E. Ba帽ados</a>, <a href="/search/astro-ph?searchtype=author&query=Benotto%2C+P">P. Benotto</a>, <a href="/search/astro-ph?searchtype=author&query=Buitrago%2C+F">F. Buitrago</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">E. Daddi</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=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=Haro%2C+P+A">P. Arrabal Haro</a>, <a href="/search/astro-ph?searchtype=author&query=Lapi%2C+A">A. Lapi</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=Lyu%2C+Y">Y. Lyu</a>, <a href="/search/astro-ph?searchtype=author&query=Massardi%2C+M">M. Massardi</a>, <a href="/search/astro-ph?searchtype=author&query=Pacucci%2C+F">F. Pacucci</a> , et al. (19 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="2502.02637v1-abstract-short" style="display: inline;"> The James Webb Space Telescope (JWST) is revolutionizing our understanding of the Universe by unveiling faint, near-infrared dropouts previously beyond our reach, ranging from exceptionally dusty sources to galaxies up to redshift $z \sim 14$. In this paper, we identify F200W-dropout objects in the Cosmic Evolution Early Release Science (CEERS) survey which are absent from existing catalogs. Our s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.02637v1-abstract-full').style.display = 'inline'; document.getElementById('2502.02637v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.02637v1-abstract-full" style="display: none;"> The James Webb Space Telescope (JWST) is revolutionizing our understanding of the Universe by unveiling faint, near-infrared dropouts previously beyond our reach, ranging from exceptionally dusty sources to galaxies up to redshift $z \sim 14$. In this paper, we identify F200W-dropout objects in the Cosmic Evolution Early Release Science (CEERS) survey which are absent from existing catalogs. Our selection method can effectively identify obscured low-mass ($\log \text{M}_* \leq 9$) objects at $z \leq 6$, massive dust-rich sources up to $z \sim 12$, and ultra-high-redshift ($z > 15$) candidates. Primarily relying on NIRCam photometry from the latest CEERS data release and supplementing with Mid-Infrared/(sub-)mm data when available, our analysis pipeline combines multiple SED-fitting codes, star formation histories, and CosMix - a novel tool for astronomical stacking. Our work highlights three $2<z<3$ dusty dwarf galaxies which have larger masses compared to the typical dusty dwarfs previously identified in CEERS. Additionally, we reveal five faint sources with significant probability of lying above $z>15$, with best-fit masses compatible with $螞$CDM and a standard baryons-to-star conversion efficiency. Their bi-modal redshift probability distributions suggest they could also be $z<1.5$ dwarf galaxies with extreme dust extinction. We also identify a strong line emitter galaxy at $z \sim 5$ mimicking the near-infrared emission of a $z \sim 13$ galaxy. Our sample holds promising candidates for future follow-ups. Confirming ultra high-redshift galaxies or lower-z dusty dwarfs will offer valuable insights into early galaxy formation, evolution with their central black holes and the nature of dark matter, and/or cosmic dust production mechanisms in low-mass galaxies, and will help us to understand degeneracies and contamination in high-z object searches. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.02637v1-abstract-full').style.display = 'none'; document.getElementById('2502.02637v1-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 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">Submitted to Astronomy & 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/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/2412.01887">arXiv:2412.01887</a> <span> [<a href="https://arxiv.org/pdf/2412.01887">pdf</a>, <a href="https://arxiv.org/format/2412.01887">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 Comprehensive Photometric Selection of `Little Red Dots' in MIRI Fields: An IR-Bright LRD at $z=3.1386$ with Warm Dust Emission </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=Leung%2C+G+C+K">Gene C. K. Leung</a>, <a href="/search/astro-ph?searchtype=author&query=Cullen%2C+F">Fergus Cullen</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=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=Illingworth%2C+G">Garth Illingworth</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=McLure%2C+R+J">Ross J. McLure</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+G">Guang Yang</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="2412.01887v1-abstract-short" style="display: inline;"> JWST has revealed a population of compact `Little Red Dots' (LRDs) at $z\gtrsim4$, with red rest-frame optical and blue UV colors. These objects are likely compact dusty starbursts or heavily reddened AGNs, playing a pivotal role in early black hole growth, dust production, and stellar assembly. We introduce a new photometric selection to identify LRDs over a broad range in redshifts and rest-fram… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.01887v1-abstract-full').style.display = 'inline'; document.getElementById('2412.01887v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.01887v1-abstract-full" style="display: none;"> JWST has revealed a population of compact `Little Red Dots' (LRDs) at $z\gtrsim4$, with red rest-frame optical and blue UV colors. These objects are likely compact dusty starbursts or heavily reddened AGNs, playing a pivotal role in early black hole growth, dust production, and stellar assembly. We introduce a new photometric selection to identify LRDs over a broad range in redshifts and rest-frame UV-to-NIR colors enabling a more complete census of the population. This method identifies 248 LRDs with F444W$<27$ mag over 263 arcmin$^2$ in the JADES, PRIMER-COSMOS, and UDS fields with MIRI coverage, increasing the number density by $\times$1.7 compared to previous samples, suggesting that previous census were underestimated. Most LRDs are detected in MIRI/F770W but only 7% (17) are detected in F1800W. We use MIRI-based rest-frame [1$-$3 $渭$m] colors to trace dust emission. F1800W-detected LRDs have a median [1$-$3 $渭$m]$=1.5$ mag, with a broad scatter indicative of diverse dust emission properties. About 20% exhibit [1$-$3 $渭$m]$<1$ mag colors consistent with negligible dust emission, but the majority show significant dust emission at 3 $渭$m (f$^{\rm dust}_{3渭m}\lesssim0.8$) from the galaxy ISM or a hot-dust-deficient AGN torus. A correlation between bluer UV-to-NIR colors and stronger IR emission suggests that the bluest LRDs may resemble unobscured QSOs. We report a LRD at $z_{\rm spec}=3.1386$, detected in MIRI, Spitzer/MIPS, and Herschel/PACS. Its IR SED rises steeply at $位_{\rm rest}>6~渭$m and peaks near $\sim40~渭$m, providing the first direct evidence of warm dust emission (T$=50-100$ K) in a LRD. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.01887v1-abstract-full').style.display = 'none'; document.getElementById('2412.01887v1-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">The new photometric selection is shown in Figure 1. The mid-IR detected LRD is in Figure 11</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/2410.23959">arXiv:2410.23959</a> <span> [<a href="https://arxiv.org/pdf/2410.23959">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> <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"> CEERS: Forging the First Dust -- Transition from Stellar to ISM Grain Growth in the Early Universe </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Burgarella%2C+D">Denis Burgarella</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=Theul%C3%A9%2C+P">Patrice Theul茅</a>, <a href="/search/astro-ph?searchtype=author&query=Zavala%2C+J">Jorge Zavala</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=Boquien%2C+M">M茅d茅ric Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N">Nikko Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Dewachter%2C+T">Tim Dewachter</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=Fern%C3%A1ndez%2C+V">Vital Fern谩ndez</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=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=Grogin%2C+N">Norman 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=Kartaltepe%2C+J+S">Jeyhan S. Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=Kewley%2C+L">Lisa 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">Dale 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=Long%2C+A">Arianna Long</a>, <a href="/search/astro-ph?searchtype=author&query=Lotz%2C+J">Jennifer Lotz</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="2410.23959v1-abstract-short" style="display: inline;"> We investigate the coevolution of metals and dust for 173 galaxies at 4.0<z<11.4 observed with JWST/NIRSpec. We use the code CIGALE that integrates photometric and spectroscopic data. Our analysis reveals a critical transition at Mstar = 10^8.5 MSun, from galaxies dominated by supernovae and AGB stardust, to those dominated by grain growth. This implies a two-mode building of dust mass, supported… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.23959v1-abstract-full').style.display = 'inline'; document.getElementById('2410.23959v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.23959v1-abstract-full" style="display: none;"> We investigate the coevolution of metals and dust for 173 galaxies at 4.0<z<11.4 observed with JWST/NIRSpec. We use the code CIGALE that integrates photometric and spectroscopic data. Our analysis reveals a critical transition at Mstar = 10^8.5 MSun, from galaxies dominated by supernovae and AGB stardust, to those dominated by grain growth. This implies a two-mode building of dust mass, supported by model predictions. The detection of stardust galaxies provides a natural and inherent explanation to the excess of UV-bright galaxies at z>10 by JWST. Besides, we observe that the metallicity of galaxies at z>8 presents a metal-to-stellar mass ratio larger than a few 10^-3, above a floor. This suggests a very fast rise of metals at high redshift, impacting the tentative detections of population III objects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.23959v1-abstract-full').style.display = 'none'; document.getElementById('2410.23959v1-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 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">This paper is submitted. It contains a main paper with 5 figures and 2 tables, plus supplementary materials</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/2410.03980">arXiv:2410.03980</a> <span> [<a href="https://arxiv.org/pdf/2410.03980">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Time-Domain And MultiMessenger Astrophysics Communications Science Analysis Group Report </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kennea%2C+J+A">Jamie A. Kennea</a>, <a href="/search/astro-ph?searchtype=author&query=Racusin%2C+J+L">Judith L. Racusin</a>, <a href="/search/astro-ph?searchtype=author&query=Burns%2C+E">Eric Burns</a>, <a href="/search/astro-ph?searchtype=author&query=Grefenstettte%2C+B+W">Brian W. Grefenstettte</a>, <a href="/search/astro-ph?searchtype=author&query=Hounsell%2C+R+A">Rebekah A. Hounsell</a>, <a href="/search/astro-ph?searchtype=author&query=Hui%2C+C+M">C. Michelle Hui</a>, <a href="/search/astro-ph?searchtype=author&query=Kocevski%2C+D">Daniel Kocevski</a>, <a href="/search/astro-ph?searchtype=author&query=Lazio%2C+T+J+W">T. Joseph W. Lazio</a>, <a href="/search/astro-ph?searchtype=author&query=Lesage%2C+S">Stephen Lesage</a>, <a href="/search/astro-ph?searchtype=author&query=Pritchard%2C+T+A">Tyler A. Pritchard</a>, <a href="/search/astro-ph?searchtype=author&query=Tohuvavohu%2C+A">Aaron Tohuvavohu</a>, <a href="/search/astro-ph?searchtype=author&query=Tomsick%2C+J+A">John A. Tomsick</a>, <a href="/search/astro-ph?searchtype=author&query=Traore%2C+D">David Traore</a>, <a href="/search/astro-ph?searchtype=author&query=Wilson-Hodge%2C+C+A">Colleen A. Wilson-Hodge</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="2410.03980v1-abstract-short" style="display: inline;"> The Time-Domain And MultiMessenger (TDAMM) Communications Science Analysis Group (TDAMMCommSAG) was formulated to describe the unique technical challenges of communicating rapidly to and from NASA astrophysics missions studying the most variable, transient, and extreme objects in the Universe. This report describes the study of if and how the transition from current NASA-operated space and ground… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.03980v1-abstract-full').style.display = 'inline'; document.getElementById('2410.03980v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.03980v1-abstract-full" style="display: none;"> The Time-Domain And MultiMessenger (TDAMM) Communications Science Analysis Group (TDAMMCommSAG) was formulated to describe the unique technical challenges of communicating rapidly to and from NASA astrophysics missions studying the most variable, transient, and extreme objects in the Universe. This report describes the study of if and how the transition from current NASA-operated space and ground relays to commercial services will adequately serve these missions. Depending on the individual mission requirements and Concept of Operations (ConOps), TDAMM missions may utilize a rapid low-rate demand access service, a low-rate continuous contact service, low-latency downlink upon demand, or a higher-latency but regular relay service. The specific implementations can vary via space relay or direct to Earth, but requires flexibility and adaptability using modern software infrastructure. The study team reviewed the current state of NASA communications services and future commercial and NASA communications services under study and in development. We explored the communications capabilities driving from the behavior of the astrophysical objects themselves. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.03980v1-abstract-full').style.display = 'none'; document.getElementById('2410.03980v1-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 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 page, 1 figure</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.00286">arXiv:2410.00286</a> <span> [<a href="https://arxiv.org/pdf/2410.00286">pdf</a>, <a href="https://arxiv.org/format/2410.00286">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Applications">stat.AP</span> </div> </div> <p class="title is-5 mathjax"> Fermi-GBM Team Analysis on The Ravasio Line </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Burns%2C+E">Eric Burns</a>, <a href="/search/astro-ph?searchtype=author&query=Lesage%2C+S">Stephen Lesage</a>, <a href="/search/astro-ph?searchtype=author&query=Goldstein%2C+A">Adam Goldstein</a>, <a href="/search/astro-ph?searchtype=author&query=Briggs%2C+M+S">Michael S. Briggs</a>, <a href="/search/astro-ph?searchtype=author&query=Veres%2C+P">Peter Veres</a>, <a href="/search/astro-ph?searchtype=author&query=Bala%2C+S">Suman Bala</a>, <a href="/search/astro-ph?searchtype=author&query=de+Barra%2C+C">Cuan de Barra</a>, <a href="/search/astro-ph?searchtype=author&query=Bissaldi%2C+E">Elisabetta Bissaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Cleveland%2C+W+H">William H Cleveland</a>, <a href="/search/astro-ph?searchtype=author&query=Giles%2C+M+M">Misty M Giles</a>, <a href="/search/astro-ph?searchtype=author&query=Godwin%2C+M">Matthew Godwin</a>, <a href="/search/astro-ph?searchtype=author&query=Hristov%2C+B+A">Boyan A. Hristov</a>, <a href="/search/astro-ph?searchtype=author&query=Hui%2C+C+M">C. Michelle Hui</a>, <a href="/search/astro-ph?searchtype=author&query=Kocevski%2C+D">Daniel Kocevski</a>, <a href="/search/astro-ph?searchtype=author&query=Mailyan%2C+B">Bagrat Mailyan</a>, <a href="/search/astro-ph?searchtype=author&query=Malacaria%2C+C">Christian Malacaria</a>, <a href="/search/astro-ph?searchtype=author&query=McBreen%2C+S">Sheila McBreen</a>, <a href="/search/astro-ph?searchtype=author&query=Preece%2C+R">Robert Preece</a>, <a href="/search/astro-ph?searchtype=author&query=Roberts%2C+O+J">Oliver J. Roberts</a>, <a href="/search/astro-ph?searchtype=author&query=Scotton%2C+L">Lorenzo Scotton</a>, <a href="/search/astro-ph?searchtype=author&query=von+Kienlin%2C+A">A. von Kienlin</a>, <a href="/search/astro-ph?searchtype=author&query=Wilson-Hodge%2C+C+A">Colleen A. Wilson-Hodge</a>, <a href="/search/astro-ph?searchtype=author&query=Wood%2C+J">Joshua Wood</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="2410.00286v1-abstract-short" style="display: inline;"> The prompt spectra of gamma-ray bursts are known to follow broadband continuum behavior over decades in energy. GRB 221009A, given the moniker the brightest of all time (BOAT), is the brightest gamma-ray burst identified in half a century of observations, and was first identified by the Fermi Gamma-ray Burst Monitor (GBM). On behalf of the Fermi-GBM Team, Lesage et al. (2023) described the initial… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.00286v1-abstract-full').style.display = 'inline'; document.getElementById('2410.00286v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.00286v1-abstract-full" style="display: none;"> The prompt spectra of gamma-ray bursts are known to follow broadband continuum behavior over decades in energy. GRB 221009A, given the moniker the brightest of all time (BOAT), is the brightest gamma-ray burst identified in half a century of observations, and was first identified by the Fermi Gamma-ray Burst Monitor (GBM). On behalf of the Fermi-GBM Team, Lesage et al. (2023) described the initial GBM analysis. Ravasio et al. (2024) report the identification of a spectral line in part of the prompt emission of this burst, which they describe as evolving over 80 s from $\sim$12 MeV to 6 MeV. We report a GBM Team analysis on the Ravasio Line: 1) We cannot identify an instrumental effect that could have produced this signal, and 2) our method of calculating the statistical significance of the line shows it easily exceeds the 5$蟽$ discovery threshold. We additionally comment on the claim of the line beginning at earlier time intervals, up to 37 MeV, as reported in Zhang et al. (2024). We find that it is reasonable to utilize these measurements for characterization of the line evolution, with caution. We encourage theoretical studies exploring this newly discovered gamma-ray burst spectral feature, unless any rigorous alternative explanation unrelated to the emission from GRB 221009A is identified. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.00286v1-abstract-full').style.display = 'none'; document.getElementById('2410.00286v1-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 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.19205">arXiv:2409.19205</a> <span> [<a href="https://arxiv.org/pdf/2409.19205">pdf</a>, <a href="https://arxiv.org/format/2409.19205">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 Search for $z=5$ H$伪$ and H$尾+$[O III] Dual-Line Emitting Galaxies in the JWST CEERS Field: Implications for the AGN Abundance </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Guo%2C+J">Jingsong Guo</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=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=Bagley%2C+M+B">Micaela B. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=McGrath%2C+E+J">Elizabeth J. McGrath</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="2409.19205v1-abstract-short" style="display: inline;"> The James Webb Space Telescope (JWST) has enabled us to uncover faint galaxies and active galactic nuclei (AGNs) in the early universe. Taking advantage of the unique filter combination used in the Cosmic Evolution Early Release Science Survey (CEERS) program, we perform an extensive photometric search of galaxies emitting strong H$尾+$[O III] and H$伪$ lines. The redshift range of the galaxies is l… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.19205v1-abstract-full').style.display = 'inline'; document.getElementById('2409.19205v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.19205v1-abstract-full" style="display: none;"> The James Webb Space Telescope (JWST) has enabled us to uncover faint galaxies and active galactic nuclei (AGNs) in the early universe. Taking advantage of the unique filter combination used in the Cosmic Evolution Early Release Science Survey (CEERS) program, we perform an extensive photometric search of galaxies emitting strong H$尾+$[O III] and H$伪$ lines. The redshift range of the galaxies is limited to $5.03\leq z\leq 5.26$ by requiring photometric excesses in NIRCam's F277W and F410M images. A total of 261 H$尾+$[O III] and H$伪$ dual-line emitters are found over the absolute UV magnitude $-22\lesssim M_{\mathrm{UV}}\lesssim -17$, with a mean rest-frame equivalent width of 1010 A for H$尾+$[O III] and 1040 A for H$伪$. This population accounts for $\sim 40\%$ of the Lyman break galaxies at this redshift range. Intriguingly, there are 58 objects (22% of the whole sample) that exhibit compact morphology at the rest-UV or optical wavelength. With an assumption that these compact dual-line emitters are dominated by AGN, their AGN bolometric luminosities are in the range of $2\times 10^{43} \lesssim L_{\rm bol}/({\rm erg~s}^{-1})\lesssim 3\times 10^{44}$. Their number density is two orders of magnitude higher than the extrapolation from the UV-selected luminous quasars, which is in good agreement with previous JWST studies of broad-line AGNs, requiring a $\sim 10\%$ of the AGN duty cycle. Moreover, our dual-line emitter sample reaches the faint end of the H$伪$ and [O III] luminosity functions down to $\lesssim 10^{42}~{\rm erg~s}^{-1}$. Spectroscopic follow-up observations are planned in an approved JWST Cycle 3 program, in which we aim to confirm their nature, characterize their black hole activity, and construct their mass distribution at $10^6\lesssim M_{\rm BH}/M_\odot \lesssim 10^8$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.19205v1-abstract-full').style.display = 'none'; document.getElementById('2409.19205v1-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> 27 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">24 pages, 16 figures, 5 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/2409.13047">arXiv:2409.13047</a> <span> [<a href="https://arxiv.org/pdf/2409.13047">pdf</a>, <a href="https://arxiv.org/format/2409.13047">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The Case for Super-Eddington Accretion: Connecting Weak X-ray and UV Line Emission in JWST Broad-Line AGN During the First Gyr of Cosmic Time </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lambrides%2C+E">Erini Lambrides</a>, <a href="/search/astro-ph?searchtype=author&query=Garofali%2C+K">Kristen Garofali</a>, <a href="/search/astro-ph?searchtype=author&query=Larson%2C+R">Rebecca Larson</a>, <a href="/search/astro-ph?searchtype=author&query=Ptak%2C+A">Andrew Ptak</a>, <a href="/search/astro-ph?searchtype=author&query=Chiaberge%2C+M">Marco Chiaberge</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=Hutchison%2C+T+A">Taylor A. Hutchison</a>, <a href="/search/astro-ph?searchtype=author&query=Norman%2C+C">Colin Norman</a>, <a href="/search/astro-ph?searchtype=author&query=McKinney%2C+J">Jed McKinney</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=Berg%2C+D+A">Danielle A. Berg</a>, <a href="/search/astro-ph?searchtype=author&query=Chisholm%2C+J">John Chisholm</a>, <a href="/search/astro-ph?searchtype=author&query=Civano%2C+F">Francesca Civano</a>, <a href="/search/astro-ph?searchtype=author&query=Cloonan%2C+A+P">Aidan P. Cloonan</a>, <a href="/search/astro-ph?searchtype=author&query=Endsley%2C+R">Ryan Endsley</a>, <a href="/search/astro-ph?searchtype=author&query=Faisst%2C+A+L">Andreas L. Faisst</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">Roberto Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Gillman%2C+S">Steven Gillman</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=Kokorev%2C+V">Vasily Kokorev</a>, <a href="/search/astro-ph?searchtype=author&query=Pacucci%2C+F">Fabio Pacucci</a>, <a href="/search/astro-ph?searchtype=author&query=Richardson%2C+C+T">Chris T. Richardson</a>, <a href="/search/astro-ph?searchtype=author&query=Stiavelli%2C+M">Massimo Stiavelli</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="2409.13047v1-abstract-short" style="display: inline;"> A multitude of JWST studies reveal a surprising over-abundance of over-massive accreting super-massive blackholes (SMBHs) -- leading to a deepening tension between theory and observation in the first billion years of cosmic time. Across X-ray to infrared wavelengths, models built off of pre-JWST predictions fail to easily reproduce observed AGN signatures (or lack thereof), driving uncertainty aro… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.13047v1-abstract-full').style.display = 'inline'; document.getElementById('2409.13047v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.13047v1-abstract-full" style="display: none;"> A multitude of JWST studies reveal a surprising over-abundance of over-massive accreting super-massive blackholes (SMBHs) -- leading to a deepening tension between theory and observation in the first billion years of cosmic time. Across X-ray to infrared wavelengths, models built off of pre-JWST predictions fail to easily reproduce observed AGN signatures (or lack thereof), driving uncertainty around the true nature of these sources. Using a sample of JWST AGN identified via their broadened Halpha emission and covered by the deepest X-ray surveys, we find neither any measurable X-ray emission nor any detection of high-ionization emission lines frequently associated with accreting SMBHs. We propose that these sources are accreting at or beyond the Eddington limit, which reduces the need for efficient production of heavy SMBH seeds at cosmic dawn. Using a theoretical model of super-Eddington accretion, we can produce the observed relative dearth of both X-ray and ultraviolet emission, as well as the high Balmer decrements, without the need for significant dust attenuation. This work indicates that super-Eddington accretion is easily achieved through-out the early Universe, and further study is required to determine what environments are required to trigger this mode of black hole growth. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.13047v1-abstract-full').style.display = 'none'; document.getElementById('2409.13047v1-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 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">Submitted</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/2409.04580">arXiv:2409.04580</a> <span> [<a href="https://arxiv.org/pdf/2409.04580">pdf</a>, <a href="https://arxiv.org/format/2409.04580">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> GRB 221009A: the B.O.A.T Burst that Shines in Gamma Rays </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Axelsson%2C+M">M. Axelsson</a>, <a href="/search/astro-ph?searchtype=author&query=Ajello%2C+M">M. Ajello</a>, <a href="/search/astro-ph?searchtype=author&query=Arimoto%2C+M">M. Arimoto</a>, <a href="/search/astro-ph?searchtype=author&query=Baldini%2C+L">L. Baldini</a>, <a href="/search/astro-ph?searchtype=author&query=Ballet%2C+J">J. Ballet</a>, <a href="/search/astro-ph?searchtype=author&query=Baring%2C+M+G">M. G. Baring</a>, <a href="/search/astro-ph?searchtype=author&query=Bartolini%2C+C">C. Bartolini</a>, <a href="/search/astro-ph?searchtype=author&query=Bastieri%2C+D">D. Bastieri</a>, <a href="/search/astro-ph?searchtype=author&query=Gonzalez%2C+J+B">J. Becerra Gonzalez</a>, <a href="/search/astro-ph?searchtype=author&query=Bellazzini%2C+R">R. Bellazzini</a>, <a href="/search/astro-ph?searchtype=author&query=Berenji%2C+B">B. Berenji</a>, <a href="/search/astro-ph?searchtype=author&query=Bissaldi%2C+E">E. Bissaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Blandford%2C+R+D">R. D. Blandford</a>, <a href="/search/astro-ph?searchtype=author&query=Bonino%2C+R">R. Bonino</a>, <a href="/search/astro-ph?searchtype=author&query=Bruel%2C+P">P. Bruel</a>, <a href="/search/astro-ph?searchtype=author&query=Buson%2C+S">S. Buson</a>, <a href="/search/astro-ph?searchtype=author&query=Cameron%2C+R+A">R. A. Cameron</a>, <a href="/search/astro-ph?searchtype=author&query=Caputo%2C+R">R. Caputo</a>, <a href="/search/astro-ph?searchtype=author&query=Caraveo%2C+P+A">P. A. Caraveo</a>, <a href="/search/astro-ph?searchtype=author&query=Cavazzuti%2C+E">E. Cavazzuti</a>, <a href="/search/astro-ph?searchtype=author&query=Cheung%2C+C+C">C. C. Cheung</a>, <a href="/search/astro-ph?searchtype=author&query=Chiaro%2C+G">G. Chiaro</a>, <a href="/search/astro-ph?searchtype=author&query=Cibrario%2C+N">N. Cibrario</a>, <a href="/search/astro-ph?searchtype=author&query=Ciprini%2C+S">S. Ciprini</a>, <a href="/search/astro-ph?searchtype=author&query=Cozzolongo%2C+G">G. Cozzolongo</a> , et al. (129 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="2409.04580v1-abstract-short" style="display: inline;"> We present a complete analysis of Fermi Large Area Telescope (LAT) data of GRB 221009A, the brightest Gamma-Ray Burst (GRB) ever detected. The burst emission above 30 MeV detected by the LAT preceded by 1 s the low-energy (< 10 MeV) pulse that triggered the Fermi Gamma-Ray Burst Monitor (GBM), as has been observed in other GRBs. The prompt phase of GRB 221009A lasted a few hundred seconds. It was… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.04580v1-abstract-full').style.display = 'inline'; document.getElementById('2409.04580v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.04580v1-abstract-full" style="display: none;"> We present a complete analysis of Fermi Large Area Telescope (LAT) data of GRB 221009A, the brightest Gamma-Ray Burst (GRB) ever detected. The burst emission above 30 MeV detected by the LAT preceded by 1 s the low-energy (< 10 MeV) pulse that triggered the Fermi Gamma-Ray Burst Monitor (GBM), as has been observed in other GRBs. The prompt phase of GRB 221009A lasted a few hundred seconds. It was so bright that we identify a Bad Time Interval (BTI) of 64 seconds caused by the extremely high flux of hard X-rays and soft gamma rays, during which the event reconstruction efficiency was poor and the dead time fraction quite high. The late-time emission decayed as a power law, but the extrapolation of the late-time emission during the first 450 seconds suggests that the afterglow started during the prompt emission. We also found that high-energy events observed by the LAT are incompatible with synchrotron origin, and, during the prompt emission, are more likely related to an extra component identified as synchrotron self-Compton (SSC). A remarkable 400 GeV photon, detected by the LAT 33 ks after the GBM trigger and directionally consistent with the location of GRB 221009A, is hard to explain as a product of SSC or TeV electromagnetic cascades, and the process responsible for its origin is uncertain. Because of its proximity and energetic nature, GRB 221009A is an extremely rare event. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.04580v1-abstract-full').style.display = 'none'; document.getElementById('2409.04580v1-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 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">60 pages, 38 figures, 9 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/2409.00169">arXiv:2409.00169</a> <span> [<a href="https://arxiv.org/pdf/2409.00169">pdf</a>, <a href="https://arxiv.org/format/2409.00169">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/10.1051/0004-6361/202451409">10.1051/0004-6361/202451409 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> ASTRODEEP-JWST: NIRCam-HST multiband photometry and redshifts for half a million sources in six extragalactic deep fields </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Merlin%2C+E">E. Merlin</a>, <a href="/search/astro-ph?searchtype=author&query=Santini%2C+P">P. Santini</a>, <a href="/search/astro-ph?searchtype=author&query=Paris%2C+D">D. Paris</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">A. Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Treu%2C+T">T. Treu</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=Dunlop%2C+J+S">J. S. Dunlop</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=Boyett%2C+K">K. Boyett</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=Correnti%2C+M">M. Correnti</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=Donnan%2C+C+T">C. T. Donnan</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=Fortuni%2C+F">F. Fortuni</a>, <a href="/search/astro-ph?searchtype=author&query=Giavalisco%2C+M">M. Giavalisco</a>, <a href="/search/astro-ph?searchtype=author&query=Glazebrook%2C+K">K. Glazebrook</a>, <a href="/search/astro-ph?searchtype=author&query=Grazian%2C+A">A. Grazian</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">N. 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> , 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="2409.00169v3-abstract-short" style="display: inline;"> We present a set of photometric catalogs primarily aimed at providing the community with a comprehensive database for the study of galaxy populations in the high redshift Universe. The set gathers data from eight JWST NIRCam observational programs, targeting the Abell 2744 (GLASS-JWST, UNCOVER, DDT2756 and GO3990), EGS (CEERS), COSMOS and UDS (PRIMER), and GOODS North and South (JADES and NGDEEP)… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.00169v3-abstract-full').style.display = 'inline'; document.getElementById('2409.00169v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.00169v3-abstract-full" style="display: none;"> We present a set of photometric catalogs primarily aimed at providing the community with a comprehensive database for the study of galaxy populations in the high redshift Universe. The set gathers data from eight JWST NIRCam observational programs, targeting the Abell 2744 (GLASS-JWST, UNCOVER, DDT2756 and GO3990), EGS (CEERS), COSMOS and UDS (PRIMER), and GOODS North and South (JADES and NGDEEP) deep fields, for a total area of $\sim$0.2 sq. degrees. Photometric estimates are obtained by means of well-established techniques, including tailored improvements designed to enhance the performance on the specific dataset. We also include new measurements from HST archival data, thus collecting 16 bands spanning from 0.44 to 4.44 $渭$m. A grand total of $\sim$530 thousand sources is detected on stacks of NIRCam 3.56 and 4.44 $渭$m mosaics. We assess the photometric accuracy by comparing fluxes and colors against archival catalogs. We also provide photometric redshift estimates, statistically validated against a large set of robust spectroscopic data. The catalogs are publicly available on the Astrodeep website. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.00169v3-abstract-full').style.display = 'none'; document.getElementById('2409.00169v3-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 August, 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, 16 figures; accepted for publication on Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 691, A240 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.11890">arXiv:2408.11890</a> <span> [<a href="https://arxiv.org/pdf/2408.11890">pdf</a>, <a href="https://arxiv.org/format/2408.11890">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</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/10.3847/2515-5172/ad7262">10.3847/2515-5172/ad7262 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Sizes and Stellar Masses of the Little Red Dots Imply Immense Stellar Densities </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Guia%2C+C+A">Carl Audric Guia</a>, <a href="/search/astro-ph?searchtype=author&query=Pacucci%2C+F">Fabio Pacucci</a>, <a href="/search/astro-ph?searchtype=author&query=Kocevski%2C+D+D">Dale D. Kocevski</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="2408.11890v1-abstract-short" style="display: inline;"> The ``Little Red Dots'' (LRDs) are red and compact galaxies detected in JWST deep fields, mainly in the redshift range $z=4-8$. Given their compactness and the inferred stellar masses in the hypothesis that LRDs are starburst galaxies, the implied stellar densities are immense. This Research Note uses an extensive catalog of LRDs from the PRIMER and the COSMOS-Web surveys to investigate these dens… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.11890v1-abstract-full').style.display = 'inline'; document.getElementById('2408.11890v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.11890v1-abstract-full" style="display: none;"> The ``Little Red Dots'' (LRDs) are red and compact galaxies detected in JWST deep fields, mainly in the redshift range $z=4-8$. Given their compactness and the inferred stellar masses in the hypothesis that LRDs are starburst galaxies, the implied stellar densities are immense. This Research Note uses an extensive catalog of LRDs from the PRIMER and the COSMOS-Web surveys to investigate these densities. We find a median (upper limit) on the effective radius of $80$ pc, which leads to median (lower limit) values of the core density of $\sim 10^4 \, \rm M_\odot \, pc^{-3}$, and individual densities as high as $\sim 10^8 \, \rm M_\odot \, pc^{-3}$, which is $\sim 10$ times higher than the density necessary for runaway collisions to take place. For $\sim 35\%$ of the LRDs investigated, the lower limits are higher than the highest stellar densities observed in any system in any redshift range. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.11890v1-abstract-full').style.display = 'none'; document.getElementById('2408.11890v1-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">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">Accepted on Research Notes of the AAS. This is a concise note (3 pages, 1 figure) regarding the inferred stellar densities for 475 LRDs from the PRIMER and the COSMOS-Web surveys</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Res. Notes AAS, 2024, 8 207 </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/2406.10341">arXiv:2406.10341</a> <span> [<a href="https://arxiv.org/pdf/2406.10341">pdf</a>, <a href="https://arxiv.org/format/2406.10341">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"> COSMOS-Web: The over-abundance and physical nature of "little red dots"--Implications for early galaxy and SMBH assembly </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Akins%2C+H+B">Hollis B. Akins</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=Lambrides%2C+E">Erini Lambrides</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+N">Natalie Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Andika%2C+I+T">Irham T. Andika</a>, <a href="/search/astro-ph?searchtype=author&query=Brinch%2C+M">Malte Brinch</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=Cooper%2C+O">Olivia Cooper</a>, <a href="/search/astro-ph?searchtype=author&query=Ding%2C+X">Xuheng Ding</a>, <a href="/search/astro-ph?searchtype=author&query=Drakos%2C+N+E">Nicole E. Drakos</a>, <a href="/search/astro-ph?searchtype=author&query=Faisst%2C+A">Andreas Faisst</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=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=Gentile%2C+F">Fabrizio Gentile</a>, <a href="/search/astro-ph?searchtype=author&query=Gillman%2C+S">Steven Gillman</a>, <a href="/search/astro-ph?searchtype=author&query=Gozaliasl%2C+G">Ghassem Gozaliasl</a>, <a href="/search/astro-ph?searchtype=author&query=Harish%2C+S">Santosh Harish</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=Hirschmann%2C+M">Michaela Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Ilbert%2C+O">Olivier Ilbert</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=Kokorev%2C+V">Vasily Kokorev</a> , et al. (16 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="2406.10341v1-abstract-short" style="display: inline;"> JWST has revealed a population of compact and extremely red galaxies at $z>4$, which likely host active galactic nuclei (AGN). We present a sample of 434 ``little red dots'' (LRDs), selected from the 0.54 deg$^2$ COSMOS-Web survey. We fit galaxy and AGN SED models to derive redshifts and physical properties; the sample spans $z\sim5$-$9$ after removing brown dwarf contaminants. We consider two ext… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.10341v1-abstract-full').style.display = 'inline'; document.getElementById('2406.10341v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.10341v1-abstract-full" style="display: none;"> JWST has revealed a population of compact and extremely red galaxies at $z>4$, which likely host active galactic nuclei (AGN). We present a sample of 434 ``little red dots'' (LRDs), selected from the 0.54 deg$^2$ COSMOS-Web survey. We fit galaxy and AGN SED models to derive redshifts and physical properties; the sample spans $z\sim5$-$9$ after removing brown dwarf contaminants. We consider two extreme physical scenarios: either LRDs are all AGN, and their continuum emission is dominated by the accretion disk, or they are all compact star-forming galaxies, and their continuum is dominated by stars. If LRDs are AGN-dominated, our sample exhibits bolometric luminosities $\sim10^{45-47}$ erg\,s$^{-1}$, spanning the gap between JWST AGN in the literature and bright, rare quasars. We derive a bolometric luminosity function (LF) $\sim100$ times the (UV-selected) quasar LF, implying a non-evolving black hole accretion density of $\sim10^{-4}$ M$_\odot$ yr$^{-1}$ Mpc$^{-3}$ from $z\sim2$-$9$. By contrast, if LRDs are dominated by star formation, we derive stellar masses $\sim10^{8.5-10}\,M_\odot$. MIRI/F770W is key to deriving accurate stellar masses; without it, we derive a mass function inconsistent with $螞$CDM. The median stellar mass profile is broadly consistent with the maximal stellar mass surface densities seen in the nearby universe, though the most massive $\sim50$\% of objects exceed this limit, requiring substantial AGN contribution to the continuum. Nevertheless, stacking all available X-ray, mid-IR, far-IR/sub-mm, and radio data yields non-detections. Whether dominated by dusty AGN, compact star-formation, or both, the high masses/luminosities and remarkable abundance of LRDs implies a dominant mode of early galaxy/SMBH growth. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.10341v1-abstract-full').style.display = 'none'; document.getElementById('2406.10341v1-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> 14 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">27 pages, 13 figures. Submitted to ApJ, comments welcome! Data access at https://github.com/hollisakins/akins24_cw</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.10752">arXiv:2405.10752</a> <span> [<a href="https://arxiv.org/pdf/2405.10752">pdf</a>, <a href="https://arxiv.org/format/2405.10752">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> </div> <p class="title is-5 mathjax"> Constraining possible $纬$-ray burst emission from GW230529 using Swift-BAT and Fermi-GBM </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ronchini%2C+S">Samuele Ronchini</a>, <a href="/search/astro-ph?searchtype=author&query=Bala%2C+S">Suman Bala</a>, <a href="/search/astro-ph?searchtype=author&query=Wood%2C+J">Joshua Wood</a>, <a href="/search/astro-ph?searchtype=author&query=Delaunay%2C+J">James Delaunay</a>, <a href="/search/astro-ph?searchtype=author&query=Dichiara%2C+S">Simone Dichiara</a>, <a href="/search/astro-ph?searchtype=author&query=Kennea%2C+J+A">Jamie A. Kennea</a>, <a href="/search/astro-ph?searchtype=author&query=Parsotan%2C+T">Tyler Parsotan</a>, <a href="/search/astro-ph?searchtype=author&query=Raman%2C+G">Gayathri Raman</a>, <a href="/search/astro-ph?searchtype=author&query=Tohuvavohu%2C+A">Aaron Tohuvavohu</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">Naresh Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Bhat%2C+N+P">Narayana P. Bhat</a>, <a href="/search/astro-ph?searchtype=author&query=Biscoveanu%2C+S">Sylvia Biscoveanu</a>, <a href="/search/astro-ph?searchtype=author&query=Bissaldi%2C+E">Elisabetta Bissaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Burns%2C+E">Eric Burns</a>, <a href="/search/astro-ph?searchtype=author&query=Campana%2C+S">Sergio Campana</a>, <a href="/search/astro-ph?searchtype=author&query=Chandra%2C+K">Koustav Chandra</a>, <a href="/search/astro-ph?searchtype=author&query=Cleveland%2C+W+H">William H. Cleveland</a>, <a href="/search/astro-ph?searchtype=author&query=Dalessi%2C+S">Sarah Dalessi</a>, <a href="/search/astro-ph?searchtype=author&query=De+Pasquale%2C+M">Massimiliano De Pasquale</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Bellido%2C+J">Juan Garc铆a-Bellido</a>, <a href="/search/astro-ph?searchtype=author&query=Gasbarra%2C+C">Claudio Gasbarra</a>, <a href="/search/astro-ph?searchtype=author&query=Giles%2C+M+M">Misty M. Giles</a>, <a href="/search/astro-ph?searchtype=author&query=Gupta%2C+I">Ish Gupta</a>, <a href="/search/astro-ph?searchtype=author&query=Hartmann%2C+D">Dieter Hartmann</a>, <a href="/search/astro-ph?searchtype=author&query=Hristov%2C+B+A">Boyan A. Hristov</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="2405.10752v1-abstract-short" style="display: inline;"> GW230529 is the first compact binary coalescence detected by the LIGO-Virgo-KAGRA collaboration with at least one component mass confidently in the lower mass-gap, corresponding to the range 3-5$M_{\odot}$. If interpreted as a neutron star-black hole merger, this event has the most symmetric mass ratio detected so far and therefore has a relatively high probability of producing electromagnetic (EM… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.10752v1-abstract-full').style.display = 'inline'; document.getElementById('2405.10752v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.10752v1-abstract-full" style="display: none;"> GW230529 is the first compact binary coalescence detected by the LIGO-Virgo-KAGRA collaboration with at least one component mass confidently in the lower mass-gap, corresponding to the range 3-5$M_{\odot}$. If interpreted as a neutron star-black hole merger, this event has the most symmetric mass ratio detected so far and therefore has a relatively high probability of producing electromagnetic (EM) emission. However, no EM counterpart has been reported. At the merger time $t_0$, Swift-BAT and Fermi-GBM together covered 100$\%$ of the sky. Performing a targeted search in a time window $[t_0-20 \text{s},t_0+20 \text{s}]$, we report no detection by the Swift-BAT and the Fermi-GBM instruments. Combining the position-dependent $纬-$ray flux upper limits and the gravitational-wave posterior distribution of luminosity distance, sky localization and inclination angle of the binary, we derive constraints on the characteristic luminosity and structure of the jet possibly launched during the merger. Assuming a top-hat jet structure, we exclude at 90$\%$ credibility the presence of a jet which has at the same time an on-axis isotropic luminosity $\gtrsim 10^{48}$ erg s$^{-1}$, in the bolometric band 1 keV-10 MeV, and a jet opening angle $\gtrsim 15$ deg. Similar constraints are derived testing other assumptions about the jet structure profile. Excluding GRB 170817A, the luminosity upper limits derived here are below the luminosity of any GRB observed so far. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.10752v1-abstract-full').style.display = 'none'; document.getElementById('2405.10752v1-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 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">18 pages, 1 table, 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/2404.11808">arXiv:2404.11808</a> <span> [<a href="https://arxiv.org/pdf/2404.11808">pdf</a>, <a href="https://arxiv.org/format/2404.11808">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Future Perspectives for Gamma-ray Burst Detection from Space </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bozzo%2C+E">Enrico Bozzo</a>, <a href="/search/astro-ph?searchtype=author&query=Amati%2C+L">Lorenzo Amati</a>, <a href="/search/astro-ph?searchtype=author&query=Baumgartner%2C+W">Wayne Baumgartner</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+T">Tzu-Ching Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Cordier%2C+B">Bertrand Cordier</a>, <a href="/search/astro-ph?searchtype=author&query=De+Angelis%2C+N">Nicolas De Angelis</a>, <a href="/search/astro-ph?searchtype=author&query=Doi%2C+A">Akihiro Doi</a>, <a href="/search/astro-ph?searchtype=author&query=Feroci%2C+M">Marco Feroci</a>, <a href="/search/astro-ph?searchtype=author&query=Froning%2C+C">Cynthia Froning</a>, <a href="/search/astro-ph?searchtype=author&query=Gaskin%2C+J">Jessica Gaskin</a>, <a href="/search/astro-ph?searchtype=author&query=Goldstein%2C+A">Adam Goldstein</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%B6tz%2C+D">Diego G枚tz</a>, <a href="/search/astro-ph?searchtype=author&query=Grove%2C+J+E">Jon E. Grove</a>, <a href="/search/astro-ph?searchtype=author&query=Guiriec%2C+S">Sylvain Guiriec</a>, <a href="/search/astro-ph?searchtype=author&query=Hernanz%2C+M">Margarita Hernanz</a>, <a href="/search/astro-ph?searchtype=author&query=Hui%2C+C+M">C. Michelle Hui</a>, <a href="/search/astro-ph?searchtype=author&query=Jenke%2C+P">Peter Jenke</a>, <a href="/search/astro-ph?searchtype=author&query=Kocevski%2C+D">Daniel Kocevski</a>, <a href="/search/astro-ph?searchtype=author&query=Kole%2C+M">Merlin Kole</a>, <a href="/search/astro-ph?searchtype=author&query=Kouveliotou%2C+C">Chryssa Kouveliotou</a>, <a href="/search/astro-ph?searchtype=author&query=Maccarone%2C+T">Thomas Maccarone</a>, <a href="/search/astro-ph?searchtype=author&query=McConnell%2C+M+L">Mark L. McConnell</a>, <a href="/search/astro-ph?searchtype=author&query=Matsuhara%2C+H">Hideo Matsuhara</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Brien%2C+P">Paul O'Brien</a>, <a href="/search/astro-ph?searchtype=author&query=Produit%2C+N">Nicolas Produit</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="2404.11808v1-abstract-short" style="display: inline;"> Since their first discovery in the late 1960s, Gamma-ray bursts have attracted an exponentially growing interest from the international community due to their central role in the most highly debated open questions of the modern research of astronomy, astrophysics, cosmology, and fundamental physics. These range from the intimate nuclear composition of high density material within the core of ultra… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.11808v1-abstract-full').style.display = 'inline'; document.getElementById('2404.11808v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.11808v1-abstract-full" style="display: none;"> Since their first discovery in the late 1960s, Gamma-ray bursts have attracted an exponentially growing interest from the international community due to their central role in the most highly debated open questions of the modern research of astronomy, astrophysics, cosmology, and fundamental physics. These range from the intimate nuclear composition of high density material within the core of ultra-dense neuron stars, to stellar evolution via the collapse of massive stars, the production and propagation of gravitational waves, as well as the exploration of the early Universe by unveiling first stars and galaxies (assessing also their evolution and cosmic re-ionization). GRBs have stimulated in the past $\sim$50 years the development of cutting-edge technological instruments for observations of high energy celestial sources from space, leading to the launch and successful operations of many different scientific missions (several of them still in data taking mode nowadays). In this review, we provide a brief description of the GRB-dedicated missions from space being designed and developed for the future. The list of these projects, not meant to be exhaustive, shall serve as a reference to interested readers to understand what is likely to come next to lead the further development of GRB research and associated phenomenology. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.11808v1-abstract-full').style.display = 'none'; document.getElementById('2404.11808v1-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 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 for publication on Universe. Invited review, contribution to the Universe Special Issue "Recent Advances in Gamma Ray Astrophysics and Future Perspectives", P. Romano eds. (https://www.mdpi.com/journal/universe/special_issues/7299902Z97)</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/2402.07994">arXiv:2402.07994</a> <span> [<a href="https://arxiv.org/pdf/2402.07994">pdf</a>, <a href="https://arxiv.org/format/2402.07994">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Historical Fermi All-Sky Variability Analysis of Galactic Flares </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Joffre%2C+S+D">Scott D. Joffre</a>, <a href="/search/astro-ph?searchtype=author&query=Torres-Alb%C3%A0%2C+N">N煤ria Torres-Alb脿</a>, <a href="/search/astro-ph?searchtype=author&query=Ajello%2C+M">Marco Ajello</a>, <a href="/search/astro-ph?searchtype=author&query=Kocevski%2C+D">Daniel Kocevski</a>, <a href="/search/astro-ph?searchtype=author&query=Buehler%2C+R">Rolf Buehler</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="2402.07994v2-abstract-short" style="display: inline;"> The Fermi All-sky Variability Analysis (FAVA) provides a photometric alternative for identifying week-long gamma-ray flares across the entire sky while being independent of any diffuse Galactic or isotropic emission model. We reviewed 779 weeks of Fermi-LAT data analyzed by FAVA to estimate the rate and origin of Galactic gamma-ray flares, and to search for new variable Galactic gamma-ray transien… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.07994v2-abstract-full').style.display = 'inline'; document.getElementById('2402.07994v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.07994v2-abstract-full" style="display: none;"> The Fermi All-sky Variability Analysis (FAVA) provides a photometric alternative for identifying week-long gamma-ray flares across the entire sky while being independent of any diffuse Galactic or isotropic emission model. We reviewed 779 weeks of Fermi-LAT data analyzed by FAVA to estimate the rate and origin of Galactic gamma-ray flares, and to search for new variable Galactic gamma-ray transients. We report an estimated yearly rate of ~8.5 Galactic gamma-ray flares/year with ~1 flare/year coming from unknown sources. Out of the known gamma-ray sources that are spatially coincident with these detected flares, we report gamma-ray flares for six of them for the first time. All six are classified as pulsars, or a source of unknown nature but which positionally overlaps with known supernova remnants or pulsar wind nebulae. This potentially means these sites are tentative candidates to be the second known site of a variable gamma-ray pulsar wind nebula (PWN), after the famous Crab Nebula's PWN. Additionally, we identify 9 unassociated flares that are unlikely to have originated from known gamma-ray sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.07994v2-abstract-full').style.display = 'none'; document.getElementById('2402.07994v2-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> 28 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 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 ApJ Feb. 28 2024. Minor edits in Section 4 and 5 for clarity. 26 pages, 6 figures, 5 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/2401.11826">arXiv:2401.11826</a> <span> [<a href="https://arxiv.org/pdf/2401.11826">pdf</a>, <a href="https://arxiv.org/format/2401.11826">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Tracing the rise of supermassive black holes: A panchromatic search for faint, unobscured quasars at z > 6 with COSMOS-Web and other surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Andika%2C+I+T">Irham T. Andika</a>, <a href="/search/astro-ph?searchtype=author&query=Jahnke%2C+K">Knud Jahnke</a>, <a href="/search/astro-ph?searchtype=author&query=Onoue%2C+M">Masafusa Onoue</a>, <a href="/search/astro-ph?searchtype=author&query=Silverman%2C+J+D">John D. Silverman</a>, <a href="/search/astro-ph?searchtype=author&query=Fitriana%2C+I+K">Itsna K. Fitriana</a>, <a href="/search/astro-ph?searchtype=author&query=Bongiorno%2C+A">Angela Bongiorno</a>, <a href="/search/astro-ph?searchtype=author&query=Brinch%2C+M">Malte Brinch</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=Faisst%2C+A">Andreas Faisst</a>, <a href="/search/astro-ph?searchtype=author&query=Gillman%2C+S">Steven Gillman</a>, <a href="/search/astro-ph?searchtype=author&query=Gozaliasl%2C+G">Ghassem Gozaliasl</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=Hirschmann%2C+M">Michaela Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Kocevski%2C+D">Dale 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=Kokorev%2C+V">Vasily Kokorev</a>, <a href="/search/astro-ph?searchtype=author&query=Lambrides%2C+E">Erini Lambrides</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+M+M">Minju M. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Rich%2C+R+M">R. Michael Rich</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">Benny Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Urry%2C+C+M">C. Megan Urry</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=Vijayan%2C+A+P">Aswin P. Vijayan</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="2401.11826v2-abstract-short" style="display: inline;"> We report the identification of 64 new candidates of compact galaxies, potentially hosting faint quasars with bolometric luminosities of $L_\mathrm{bol} = 10^{43}$--10$^{46}$ erg s$^{-1}$, residing in the reionization epoch within the redshift range of $6 \lesssim z \lesssim 8$. These candidates were selected by harnessing the rich multiband datasets provided by the emerging JWST-driven extragalac… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.11826v2-abstract-full').style.display = 'inline'; document.getElementById('2401.11826v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.11826v2-abstract-full" style="display: none;"> We report the identification of 64 new candidates of compact galaxies, potentially hosting faint quasars with bolometric luminosities of $L_\mathrm{bol} = 10^{43}$--10$^{46}$ erg s$^{-1}$, residing in the reionization epoch within the redshift range of $6 \lesssim z \lesssim 8$. These candidates were selected by harnessing the rich multiband datasets provided by the emerging JWST-driven extragalactic surveys, focusing on COSMOS-Web, as well as JADES, UNCOVER, CEERS, and PRIMER. Our search strategy includes two stages: applying stringent photometric cuts to catalog-level data and detailed spectral energy distribution fitting. These techniques effectively isolate the quasar candidates while mitigating contamination from low-redshift interlopers, such as brown dwarfs and nearby galaxies. The selected candidates indicate physical traits compatible with low-luminosity active galactic nuclei, likely hosting $\approx10^5$--$10^7~M_\odot$ supermassive black holes (SMBHs) living in galaxies with stellar masses of $\approx10^8$--$10^{10}~M_\odot$. The SMBHs selected in this study, on average, exhibit an elevated mass compared to their hosts, with the mass ratio distribution slightly higher than those of galaxies in the local Universe. As with other high-$z$ studies, this is at least in part due to the selection method for these quasars. An extensive Monte Carlo analysis provides compelling evidence that heavy black hole seeds from the direct collapse scenario appear to be the preferred pathway to mature this specific subset of SMBHs by $z\approx7$. This work underscores the significance of further spectroscopic observations, as the quasar candidates presented here offer exceptional opportunities to delve into the nature of the earliest galaxies and SMBHs that formed during cosmic infancy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.11826v2-abstract-full').style.display = 'none'; document.getElementById('2401.11826v2-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 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 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">Accepted for publication in the Astronomy & Astrophysics journal. 19 pages, 10 figures, and 4 tables. We welcome comments from the reader</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/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/2310.15232">arXiv:2310.15232</a> <span> [<a href="https://arxiv.org/pdf/2310.15232">pdf</a>, <a href="https://arxiv.org/format/2310.15232">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"> Galaxies Going Bananas: Inferring the 3D Geometry of High-Redshift Galaxies with JWST-CEERS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pandya%2C+V">Viraj Pandya</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+H">Haowen Zhang</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=Iyer%2C+K+G">Kartheik G. Iyer</a>, <a href="/search/astro-ph?searchtype=author&query=McGrath%2C+E">Elizabeth McGrath</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=Kuemmel%2C+M">Martin Kuemmel</a>, <a href="/search/astro-ph?searchtype=author&query=Hartley%2C+W+G">William G. Hartley</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=Primack%2C+J">Joel Primack</a>, <a href="/search/astro-ph?searchtype=author&query=Dekel%2C+A">Avishai Dekel</a>, <a href="/search/astro-ph?searchtype=author&query=Faber%2C+S+M">Sandra M. Faber</a>, <a href="/search/astro-ph?searchtype=author&query=Koo%2C+D+C">David C. Koo</a>, <a href="/search/astro-ph?searchtype=author&query=Bryan%2C+G+L">Greg L. Bryan</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=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=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=Bertin%2C+E">Emmanuel Bertin</a>, <a href="/search/astro-ph?searchtype=author&query=Costantin%2C+L">Luca Costantin</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> , et al. (31 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="2310.15232v2-abstract-short" style="display: inline;"> The 3D geometry of high-redshift galaxies remains poorly understood. We build a differentiable Bayesian model and use Hamiltonian Monte Carlo to efficiently and robustly infer the 3D shapes of star-forming galaxies in JWST-CEERS observations with $\log M_*/M_{\odot}=9.0-10.5$ at $z=0.5-8.0$. We reproduce previous results from HST-CANDELS in a fraction of the computing time and constrain the mean e… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.15232v2-abstract-full').style.display = 'inline'; document.getElementById('2310.15232v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.15232v2-abstract-full" style="display: none;"> The 3D geometry of high-redshift galaxies remains poorly understood. We build a differentiable Bayesian model and use Hamiltonian Monte Carlo to efficiently and robustly infer the 3D shapes of star-forming galaxies in JWST-CEERS observations with $\log M_*/M_{\odot}=9.0-10.5$ at $z=0.5-8.0$. We reproduce previous results from HST-CANDELS in a fraction of the computing time and constrain the mean ellipticity, triaxiality, size and covariances with samples as small as $\sim50$ galaxies. We find high 3D ellipticities for all mass-redshift bins suggesting oblate (disky) or prolate (elongated) geometries. We break that degeneracy by constraining the mean triaxiality to be $\sim1$ for $\log M_*/M_{\odot}=9.0-9.5$ dwarfs at $z>1$ (favoring the prolate scenario), with significantly lower triaxialities for higher masses and lower redshifts indicating the emergence of disks. The prolate population traces out a ``banana'' in the projected $b/a-\log a$ diagram with an excess of low $b/a$, large $\log a$ galaxies. The dwarf prolate fraction rises from $\sim25\%$ at $z=0.5-1.0$ to $\sim50-80\%$ at $z=3-8$. If these are disks, they cannot be axisymmetric but instead must be unusually oval (triaxial) unlike local circular disks. We simultaneously constrain the 3D size-mass relation and its dependence on 3D geometry. High-probability prolate and oblate candidates show remarkably similar S茅rsic indices ($n\sim1$), non-parametric morphological properties and specific star formation rates. Both tend to be visually classified as disks or irregular but edge-on oblate candidates show more dust attenuation. We discuss selection effects, follow-up prospects and theoretical implications. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.15232v2-abstract-full').style.display = 'none'; document.getElementById('2310.15232v2-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 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 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">Accepted version to appear in ApJ, main body is 36 pages of which ~half are full-page 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/2308.13666">arXiv:2308.13666</a> <span> [<a href="https://arxiv.org/pdf/2308.13666">pdf</a>, <a href="https://arxiv.org/format/2308.13666">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> A Joint Fermi-GBM and Swift-BAT Analysis of Gravitational-Wave Candidates from the Third Gravitational-wave Observing Run </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fletcher%2C+C">C. Fletcher</a>, <a href="/search/astro-ph?searchtype=author&query=Wood%2C+J">J. Wood</a>, <a href="/search/astro-ph?searchtype=author&query=Hamburg%2C+R">R. Hamburg</a>, <a href="/search/astro-ph?searchtype=author&query=Veres%2C+P">P. Veres</a>, <a href="/search/astro-ph?searchtype=author&query=Hui%2C+C+M">C. M. Hui</a>, <a href="/search/astro-ph?searchtype=author&query=Bissaldi%2C+E">E. Bissaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Briggs%2C+M+S">M. S. Briggs</a>, <a href="/search/astro-ph?searchtype=author&query=Burns%2C+E">E. Burns</a>, <a href="/search/astro-ph?searchtype=author&query=Cleveland%2C+W+H">W. H. Cleveland</a>, <a href="/search/astro-ph?searchtype=author&query=Giles%2C+M+M">M. M. Giles</a>, <a href="/search/astro-ph?searchtype=author&query=Goldstein%2C+A">A. Goldstein</a>, <a href="/search/astro-ph?searchtype=author&query=Hristov%2C+B+A">B. A. Hristov</a>, <a href="/search/astro-ph?searchtype=author&query=Kocevski%2C+D">D. Kocevski</a>, <a href="/search/astro-ph?searchtype=author&query=Lesage%2C+S">S. Lesage</a>, <a href="/search/astro-ph?searchtype=author&query=Mailyan%2C+B">B. Mailyan</a>, <a href="/search/astro-ph?searchtype=author&query=Malacaria%2C+C">C. Malacaria</a>, <a href="/search/astro-ph?searchtype=author&query=Poolakkil%2C+S">S. Poolakkil</a>, <a href="/search/astro-ph?searchtype=author&query=von+Kienlin%2C+A">A. von Kienlin</a>, <a href="/search/astro-ph?searchtype=author&query=Wilson-Hodge%2C+C+A">C. A. Wilson-Hodge</a>, <a href="/search/astro-ph?searchtype=author&query=Team%2C+T+F+G+B+M">The Fermi Gamma-ray Burst Monitor Team</a>, <a href="/search/astro-ph?searchtype=author&query=Crnogor%C4%8Devi%C4%87%2C+M">M. Crnogor膷evi膰</a>, <a href="/search/astro-ph?searchtype=author&query=DeLaunay%2C+J">J. DeLaunay</a>, <a href="/search/astro-ph?searchtype=author&query=Tohuvavohu%2C+A">A. Tohuvavohu</a>, <a href="/search/astro-ph?searchtype=author&query=Caputo%2C+R">R. Caputo</a>, <a href="/search/astro-ph?searchtype=author&query=Cenko%2C+S+B">S. B. Cenko</a> , et al. (1674 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="2308.13666v1-abstract-short" style="display: inline;"> We present Fermi Gamma-ray Burst Monitor (Fermi-GBM) and Swift Burst Alert Telescope (Swift-BAT) searches for gamma-ray/X-ray counterparts to gravitational wave (GW) candidate events identified during the third observing run of the Advanced LIGO and Advanced Virgo detectors. Using Fermi-GBM on-board triggers and sub-threshold gamma-ray burst (GRB) candidates found in the Fermi-GBM ground analyses,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.13666v1-abstract-full').style.display = 'inline'; document.getElementById('2308.13666v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.13666v1-abstract-full" style="display: none;"> We present Fermi Gamma-ray Burst Monitor (Fermi-GBM) and Swift Burst Alert Telescope (Swift-BAT) searches for gamma-ray/X-ray counterparts to gravitational wave (GW) candidate events identified during the third observing run of the Advanced LIGO and Advanced Virgo detectors. Using Fermi-GBM on-board triggers and sub-threshold gamma-ray burst (GRB) candidates found in the Fermi-GBM ground analyses, the Targeted Search and the Untargeted Search, we investigate whether there are any coincident GRBs associated with the GWs. We also search the Swift-BAT rate data around the GW times to determine whether a GRB counterpart is present. No counterparts are found. Using both the Fermi-GBM Targeted Search and the Swift-BAT search, we calculate flux upper limits and present joint upper limits on the gamma-ray luminosity of each GW. Given these limits, we constrain theoretical models for the emission of gamma-rays from binary black hole mergers. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.13666v1-abstract-full').style.display = 'none'; document.getElementById('2308.13666v1-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 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.12709">arXiv:2308.12709</a> <span> [<a href="https://arxiv.org/pdf/2308.12709">pdf</a>, <a href="https://arxiv.org/format/2308.12709">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</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/10.22323/1.444.1547">10.22323/1.444.1547 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Fermi-LAT Light Curve Repository: A resource for the time-domain and multi-messenger communities </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Valverde%2C+J">Janeth Valverde</a>, <a href="/search/astro-ph?searchtype=author&query=Kocevski%2C+D">D. Kocevski</a>, <a href="/search/astro-ph?searchtype=author&query=Negro%2C+M">M. Negro</a>, <a href="/search/astro-ph?searchtype=author&query=Garrappa%2C+S">S. Garrappa</a>, <a href="/search/astro-ph?searchtype=author&query=Brill%2C+A">A. Brill</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="2308.12709v1-abstract-short" style="display: inline;"> For over 15 years the Fermi Large Area Telescope (Fermi-LAT) has been monitoring the entire high-energy gamma-ray sky, providing the best sampled 0.1 -- $>1$ TeV photons to this day. As a result, the Fermi-LAT has been serving the time-domain and multi-messenger community as the main source of gamma-ray activity alerts. All of this makes the Fermi-LAT a key instrument towards understanding the und… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.12709v1-abstract-full').style.display = 'inline'; document.getElementById('2308.12709v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.12709v1-abstract-full" style="display: none;"> For over 15 years the Fermi Large Area Telescope (Fermi-LAT) has been monitoring the entire high-energy gamma-ray sky, providing the best sampled 0.1 -- $>1$ TeV photons to this day. As a result, the Fermi-LAT has been serving the time-domain and multi-messenger community as the main source of gamma-ray activity alerts. All of this makes the Fermi-LAT a key instrument towards understanding the underlying physics behind the most extreme objects in the universe. However, generating mission-long LAT light curves can be very computationally expensive. The Fermi-LAT light curve repository (LCR) tackles this issue. The LCR is a public library of gamma-ray light curves for 1525 Fermi-LAT sources deemed variable in the 4FGL-DR2 catalog. The repository consists of light curves on timescales of days, weeks, and months, generated through a full-likelihood unbinned analysis of the source and surrounding region, providing flux and photon index measurements for each time interval. Hosted at NASA's FSSC, the library provides users with access to this continually updated light curve data, further serving as a resource to the time-domain and multi-messenger communities. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.12709v1-abstract-full').style.display = 'none'; document.getElementById('2308.12709v1-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 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">Proceedings for the 38th International Cosmic Ray Conference (ICRC2023)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> PoS(ICRC2023)1547 </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/2307.14509">arXiv:2307.14509</a> <span> [<a href="https://arxiv.org/pdf/2307.14509">pdf</a>, <a href="https://arxiv.org/format/2307.14509">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> <p class="title is-5 mathjax"> CEERS MIRI Imaging: Data Reduction and Quality Assessment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yang%2C+G">Guang Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Papovich%2C+C">Casey Papovich</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M">Micaela Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+H">Henry Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S">Steven Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A">Anton Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Gonz%C3%A1lez%2C+P">Pablo 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=Bisigello%2C+L">Laura Bisigello</a>, <a href="/search/astro-ph?searchtype=author&query=Caputi%2C+K">Karina Caputi</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+Y">Yingjie Cheng</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=Fontana%2C+A">Adriano Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Gardner%2C+J">Jonathan Gardner</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">Norman Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Harish%2C+S">Santosh Harish</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B">Benne Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Iani%2C+E">Edoardo Iani</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J">Jeyhan Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=Kewley%2C+L">Lisa 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">Dale Kocevski</a>, <a href="/search/astro-ph?searchtype=author&query=Kokorev%2C+V">Vasily Kokorev</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="2307.14509v2-abstract-short" style="display: inline;"> The Cosmic Evolution Early Release Science Survey (CEERS), targeting the Extended Groth Strip extragalactic field, is one of the JWST Director's Discretionary Early Release Science programs. To date, all observations have been executed and include NIRCam/MIRI imaging and NIRSpec/NIRCam spectroscopic exposures. Here, we discuss the MIRI imaging, which includes eight pointings, four of which provide… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.14509v2-abstract-full').style.display = 'inline'; document.getElementById('2307.14509v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.14509v2-abstract-full" style="display: none;"> The Cosmic Evolution Early Release Science Survey (CEERS), targeting the Extended Groth Strip extragalactic field, is one of the JWST Director's Discretionary Early Release Science programs. To date, all observations have been executed and include NIRCam/MIRI imaging and NIRSpec/NIRCam spectroscopic exposures. Here, we discuss the MIRI imaging, which includes eight pointings, four of which provide deep imaging with the bluer bands (F560W, F770W) and four with contiguous wavelength coverage in F1000W, F1280W, F1500W, and F1800W, where two of these also include coverage in F770W and F2100W. We present a summary of the data, the data quality, and data reduction. The data reduction is based on the JWST Calibration Pipeline combined with custom modifications and additional steps designed to enhance the output quality, including improvements in astrometry and the removal of detector artifacts. We estimate the image depth of the reduced mosaics, and show that these generally agree with expectations from the Exposure Time Calculator. We compare the MIRI F560W and F770W flux densities for bright sources to measurements from Spitzer/IRAC Ch3 (5.8 $渭$m) and Ch4 (8.0 $渭$m), and we find that they agree with systematic differences of $<0.1$ mag. For the redder MIRI bands, we assess their quality by studying the spectral energy distributions (SEDs) of Galactic stars. The SEDs are consistent with the expected Rayleigh-Jeans law with a deviation $\sim 0.03$ mag, indicating that the MIRI colors are reliable. We also discuss all publicly released data products (images and source catalogs), which are available on the CEERS website (https://ceers.github.io/). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.14509v2-abstract-full').style.display = 'none'; document.getElementById('2307.14509v2-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 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 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">17 pages, 11 figures, and 4 tables. ApJL in press</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/2306.06244">arXiv:2306.06244</a> <span> [<a href="https://arxiv.org/pdf/2306.06244">pdf</a>, <a href="https://arxiv.org/format/2306.06244">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: The Faint-End of the Luminosity Function at $z \sim$ 9-12 from Ultra-Deep JWST 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=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=Ferguson%2C+H+C">Henry C. Ferguson</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=Perez-Gonzalez%2C+P+G">Pablo G. Perez-Gonzalez</a>, <a href="/search/astro-ph?searchtype=author&query=Morales%2C+A">Alexa Morales</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=Yang%2C+G">Guang Yang</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=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=Fujimoto%2C+S">Seiji Fujimoto</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=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=Berg%2C+D+A">Danielle A. Berg</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=Castellano%2C+M">Marco Castellano</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=Dickinson%2C+M">Mark Dickinson</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=Hutchison%2C+T+A">Taylor A. Hutchison</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="2306.06244v1-abstract-short" style="display: inline;"> We present a robust sample of very high-redshift galaxy candidates from the first epoch of {\it JWST}/NIRCam imaging from the Next Generation Extragalactic Exploratory Deep (NGDEEP) Survey. The NGDEEP NIRCam imaging in the Hubble Ultra Deep Field Parallel Field 2 (HUDF-Par2) reaches $m=30.4$ (5$蟽$, point-source) in F277W, making it the deepest public {\it JWST} GO imaging dataset to date. We descr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.06244v1-abstract-full').style.display = 'inline'; document.getElementById('2306.06244v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.06244v1-abstract-full" style="display: none;"> We present a robust sample of very high-redshift galaxy candidates from the first epoch of {\it JWST}/NIRCam imaging from the Next Generation Extragalactic Exploratory Deep (NGDEEP) Survey. The NGDEEP NIRCam imaging in the Hubble Ultra Deep Field Parallel Field 2 (HUDF-Par2) reaches $m=30.4$ (5$蟽$, point-source) in F277W, making it the deepest public {\it JWST} GO imaging dataset to date. We describe our detailed data reduction process of the six-filter broad-band {\it JWST}/NIRCam imaging, incorporating custom corrections for systematic effects to produce high-quality calibrated images. Using robust photometric redshift selection criteria, we identify a sample of 38 $z \gtrsim 9$ galaxy candidates. These objects span a redshift range of $z=8.5-15.8$, and apparent magnitudes of $m_\mathrm{F277W} = 27-30.5$ AB mag, reaching $\sim 1.5$ mag deeper than previous public {\it JWST} imaging surveys. We calculate the rest-frame ultraviolet (UV) luminosity function at $z \sim$ 9 and 11, and present a new measurement of the luminosity function faint-end slope at $z \sim 11$. There is no significant evolution in the faint-end slope and number density from $z=9$ to 11. Comparing our results with theoretical predictions, we find that some models produce better agreement at the faint end than the bright end. These results will help to constrain how stellar feedback impacts star formation at these early epochs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.06244v1-abstract-full').style.display = 'none'; document.getElementById('2306.06244v1-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 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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. 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/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/2305.12262">arXiv:2305.12262</a> <span> [<a href="https://arxiv.org/pdf/2305.12262">pdf</a>, <a href="https://arxiv.org/format/2305.12262">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</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/ace82d">10.3847/2041-8213/ace82d <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Extreme Variability in a Long Duration Gamma-ray Burst Associated with a Kilonova </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Veres%2C+P">P. Veres</a>, <a href="/search/astro-ph?searchtype=author&query=Bhat%2C+P+N">P. N. Bhat</a>, <a href="/search/astro-ph?searchtype=author&query=Burns%2C+E">E. Burns</a>, <a href="/search/astro-ph?searchtype=author&query=Hamburg%2C+R">R. Hamburg</a>, <a href="/search/astro-ph?searchtype=author&query=Fraija%2C+N">N. Fraija</a>, <a href="/search/astro-ph?searchtype=author&query=Kocevski%2C+D">D. Kocevski</a>, <a href="/search/astro-ph?searchtype=author&query=Preece%2C+R">R. Preece</a>, <a href="/search/astro-ph?searchtype=author&query=Poolakkil%2C+S">S. Poolakkil</a>, <a href="/search/astro-ph?searchtype=author&query=Christensen%2C+N">N. Christensen</a>, <a href="/search/astro-ph?searchtype=author&query=Bizouard%2C+M+A">M. A. Bizouard</a>, <a href="/search/astro-ph?searchtype=author&query=Canton%2C+T+D">T. Dal Canton</a>, <a href="/search/astro-ph?searchtype=author&query=Bala%2C+S">S. Bala</a>, <a href="/search/astro-ph?searchtype=author&query=Bissaldi%2C+E">E. Bissaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Briggs%2C+M+S">M. S. Briggs</a>, <a href="/search/astro-ph?searchtype=author&query=Cleveland%2C+W">W. Cleveland</a>, <a href="/search/astro-ph?searchtype=author&query=Goldstein%2C+A">A. Goldstein</a>, <a href="/search/astro-ph?searchtype=author&query=Hristov%2C+B+A">B. A. Hristov</a>, <a href="/search/astro-ph?searchtype=author&query=Hui%2C+C+M">C. M. Hui</a>, <a href="/search/astro-ph?searchtype=author&query=Lesage%2C+S">S. Lesage</a>, <a href="/search/astro-ph?searchtype=author&query=Mailyan%2C+B">B. Mailyan</a>, <a href="/search/astro-ph?searchtype=author&query=Roberts%2C+O+J">O. J. Roberts</a>, <a href="/search/astro-ph?searchtype=author&query=Wilson-Hodge%2C+C+A">C. A. Wilson-Hodge</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="2305.12262v1-abstract-short" style="display: inline;"> The recent discovery of a kilonova from the long duration gamma-ray burst, GRB 211211A, challenges classification schemes based on temporal information alone. Gamma-ray properties of GRB 211211A reveal an extreme event, which stands out among both short and long GRBs. We find very short variations (few ms) in the lightcurve of GRB 211211A and estimate ~1000 for the Lorentz factor of the outflow. W… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.12262v1-abstract-full').style.display = 'inline'; document.getElementById('2305.12262v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.12262v1-abstract-full" style="display: none;"> The recent discovery of a kilonova from the long duration gamma-ray burst, GRB 211211A, challenges classification schemes based on temporal information alone. Gamma-ray properties of GRB 211211A reveal an extreme event, which stands out among both short and long GRBs. We find very short variations (few ms) in the lightcurve of GRB 211211A and estimate ~1000 for the Lorentz factor of the outflow. We discuss the relevance of the short variations in identifying similar long GRBs resulting from compact mergers. Our findings indicate that in future gravitational wave follow-up campaigns, some long duration GRBs should be treated as possible strong gravitational wave counterparts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.12262v1-abstract-full').style.display = 'none'; document.getElementById('2305.12262v1-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 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">10 pages 5 figures, submitted to AAS journals</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJL 954 L5 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.05692">arXiv:2305.05692</a> <span> [<a href="https://arxiv.org/pdf/2305.05692">pdf</a>, <a href="https://arxiv.org/format/2305.05692">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="High Energy Astrophysical Phenomena">astro-ph.HE</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/10.1093/mnras/stad1300">10.1093/mnras/stad1300 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Obscured AGN enhancement in galaxy pairs at cosmic noon: evidence from a probabilistic treatment of photometric redshifts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dougherty%2C+S+L">Sean L. Dougherty</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+C+M">C. M. Harrison</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=Rosario%2C+D+J">D. J. Rosario</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="2305.05692v1-abstract-short" style="display: inline;"> Observations of the nearby universe reveal an increasing fraction of active galactic nuclei (AGN) with decreasing projected separation for close galaxy pairs, relative to control galaxies. This implies galaxy interactions play a role in enhancing AGN activity. However, the picture at higher redshift is less established, partly due to limited spectroscopic redshifts. We combine spectroscopic survey… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.05692v1-abstract-full').style.display = 'inline'; document.getElementById('2305.05692v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.05692v1-abstract-full" style="display: none;"> Observations of the nearby universe reveal an increasing fraction of active galactic nuclei (AGN) with decreasing projected separation for close galaxy pairs, relative to control galaxies. This implies galaxy interactions play a role in enhancing AGN activity. However, the picture at higher redshift is less established, partly due to limited spectroscopic redshifts. We combine spectroscopic surveys with photometric redshift probability distribution functions for galaxies in the CANDELS and COSMOS surveys, to produce the largest ever sample of galaxy pairs used in an AGN fraction calculation for cosmic noon ($0.5<z<3$). We present a new technique for assessing galaxy pair probability (based on line-of-sight velocities +/-1000 km/s) from photometric redshift posterior convolutions and use these to produce weighted AGN fractions. Over projected separations 5-100kpc we find no evidence for enhancement, relative to isolated control galaxies, of X-ray (L_X > 10^42 erg/s) or infrared-selected AGN in major (mass ratios up to 4:1) or minor (4:1 to 10:1) galaxy pairs. However, defining the most obscured AGN as those detected in the infrared but not in X-rays, we observe a trend of increasing obscured AGN enhancement at decreasing separations. The peak enhancement, relative to isolated controls, is a factor of 2.08+/-0.61 for separations <25kpc. Our simulations with mock data, indicates this could be a lower limit of the true enhancement. If confirmed with improved infrared imaging (e.g., with JWST) and redshifts (e.g., with forthcoming multi-object spectrograph surveys), this would suggest that galaxy interactions play a role in enhancing the most obscured black hole growth at cosmic noon. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.05692v1-abstract-full').style.display = 'none'; document.getElementById('2305.05692v1-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 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">Accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.04662">arXiv:2305.04662</a> <span> [<a href="https://arxiv.org/pdf/2305.04662">pdf</a>, <a href="https://arxiv.org/format/2305.04662">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 NIRCam Selection of Quiescent Galaxies at 3 < z < 6 in CEERS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Long%2C+A+S">Arianna S. Long</a>, <a href="/search/astro-ph?searchtype=author&query=Antwi-Danso%2C+J">Jacqueline Antwi-Danso</a>, <a href="/search/astro-ph?searchtype=author&query=Lambrides%2C+E+L">Erini L. Lambrides</a>, <a href="/search/astro-ph?searchtype=author&query=Lovell%2C+C+C">Christopher C. Lovell</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=Valentino%2C+F">Francesco Valentino</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=Casey%2C+C+M">Caitlin M. Casey</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=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=Chworowsky%2C+K">Katherine Chworowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Cooper%2C+M+C">Michael 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=Cooray%2C+A+R">Asantha R. Cooray</a>, <a href="/search/astro-ph?searchtype=author&query=Croton%2C+D">Darren Croton</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=Franco%2C+M">Maximilien Franco</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+K+M+L">Katriona M. L. Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">Michaela Hirschmann</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> , 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="2305.04662v2-abstract-short" style="display: inline;"> Substantial populations of massive quiescent galaxies at $z\ge3$ challenge our understanding of rapid galaxy growth and quenching over short timescales. In order to piece together this evolutionary puzzle, more statistical samples of these objects are required. Established techniques for identifying massive quiescent galaxies are increasingly inefficient and unconstrained at $z>3$. As a result, st… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.04662v2-abstract-full').style.display = 'inline'; document.getElementById('2305.04662v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.04662v2-abstract-full" style="display: none;"> Substantial populations of massive quiescent galaxies at $z\ge3$ challenge our understanding of rapid galaxy growth and quenching over short timescales. In order to piece together this evolutionary puzzle, more statistical samples of these objects are required. Established techniques for identifying massive quiescent galaxies are increasingly inefficient and unconstrained at $z>3$. As a result, studies report that as much as 70\% of quiescent galaxies at $z>3$ may be missed from existing surveys. In this work, we propose a new empirical color selection technique designed to select massive quiescent galaxies at $3\lesssim z \lesssim 6$ using JWST NIRCam imaging data. We use empirically-constrained galaxy SED templates to define a region in the $F277W-F444W$ vs. $F150W-F277W$ color plane that captures quiescent galaxies at $z>3$. We apply this color selection criteria to the Cosmic Evolution Early Release Science (CEERS) Survey and identify 44 candidate $z\gtrsim3$ quiescent galaxies. Over half of these sources are newly discovered and, on average, exhibit specific star formation rates of post-starburst galaxies. We derive volume density estimates of $n\sim1-4\times10^{-5}$\,Mpc$^{-3}$ at $3< z <5$, finding excellent agreement with existing reports on similar populations in the CEERS field. Thanks to NIRCam's wavelength coverage and sensitivity, this technique provides an efficient tool to search for large samples of these rare galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.04662v2-abstract-full').style.display = 'none'; document.getElementById('2305.04662v2-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 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 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">12 pages, 4 figures, 2 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/2304.12347">arXiv:2304.12347</a> <span> [<a href="https://arxiv.org/pdf/2304.12347">pdf</a>, <a href="https://arxiv.org/format/2304.12347">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"> Two massive, compact, and dust-obscured candidate $z\sim 8$ galaxies discovered by JWST </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Akins%2C+H+B">Hollis B. Akins</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=Allen%2C+N">Natalie Allen</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=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Franco%2C+M">Maximilien Franco</a>, <a href="/search/astro-ph?searchtype=author&query=Harish%2C+S">Santosh Harish</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=Ilbert%2C+O">Olivier Ilbert</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=Liu%2C+D">Daizhong Liu</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=McCracken%2C+H+J">Henry Joy McCracken</a>, <a href="/search/astro-ph?searchtype=author&query=Paquereau%2C+L">Louise Paquereau</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=Rhodes%2C+J">Jason Rhodes</a>, <a href="/search/astro-ph?searchtype=author&query=Robertson%2C+B+E">Brant E. Robertson</a>, <a href="/search/astro-ph?searchtype=author&query=Shuntov%2C+M">Marko Shuntov</a>, <a href="/search/astro-ph?searchtype=author&query=Toft%2C+S">Sune Toft</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+G">Guang Yang</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> , et al. (34 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="2304.12347v1-abstract-short" style="display: inline;"> We present a search for extremely red, dust-obscured, $z>7$ galaxies with $\textit{JWST}$/NIRCam+MIRI imaging over the first 20 arcmin$^2$ of publicly-available Cycle 1 data from the COSMOS-Web, CEERS, and PRIMER surveys. Based on their red color in F277W$-$F444W ($\sim 2.5$ mag) and detection in MIRI/F770W ($\sim 25$ mag), we identify two galaxies$\unicode{x2014}$COS-z8M1 and CEERS-z7M1… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.12347v1-abstract-full').style.display = 'inline'; document.getElementById('2304.12347v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.12347v1-abstract-full" style="display: none;"> We present a search for extremely red, dust-obscured, $z>7$ galaxies with $\textit{JWST}$/NIRCam+MIRI imaging over the first 20 arcmin$^2$ of publicly-available Cycle 1 data from the COSMOS-Web, CEERS, and PRIMER surveys. Based on their red color in F277W$-$F444W ($\sim 2.5$ mag) and detection in MIRI/F770W ($\sim 25$ mag), we identify two galaxies$\unicode{x2014}$COS-z8M1 and CEERS-z7M1$\unicode{x2014}$which have best-fit photometric redshifts of $z=8.5^{+0.3}_{-0.4}$ and $z=7.6^{+0.1}_{-0.1}$, respectively. We perform SED fitting with a variety of codes (including BAGPIPES, PROSPECTOR, BEAGLE, and CIGALE), and find a $>95\%$ probability that these indeed lie at $z>7$. Both sources are compact ($R_{\rm eff} \lesssim 200$ pc), highly obscured ($A_V \sim 1.5$$\unicode{x2013}$$2.5$), and, at our best-fit redshift estimates, likely have strong [OIII]+H$尾$ emission contributing to their $4.4\,渭$m photometry. We estimate stellar masses of $\sim 10^{10}~M_\odot$ for both sources; by virtue of detection in MIRI at $7.7\,渭$m, these measurements are robust to the inclusion of bright emission lines, for example, from an AGN. We identify a marginal (2.9$蟽$) ALMA detection at 2 mm within $0.5''$ of COS-z8M1, which if real, would suggest a remarkably high IR luminosity of $\sim 10^{12} L_\odot$. These two galaxies, if confirmed at $z\sim 8$, would be extreme in their stellar and dust masses, and may be representative of a substantial population of modestly dust-obscured galaxies at cosmic dawn. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.12347v1-abstract-full').style.display = 'none'; document.getElementById('2304.12347v1-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 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">23 pages, 8 figures, submitted to ApJL, 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/2303.15431">arXiv:2303.15431</a> <span> [<a href="https://arxiv.org/pdf/2303.15431">pdf</a>, <a href="https://arxiv.org/format/2303.15431">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/10.1038/s41586-023-06521-7">10.1038/s41586-023-06521-7 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Confirmation and refutation of very luminous galaxies in the early universe </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=Kartaltepe%2C+J+S">Jeyhan S. Kartaltepe</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=Burgarella%2C+D">Denis Burgarella</a>, <a href="/search/astro-ph?searchtype=author&query=Carnall%2C+A">Adam Carnall</a>, <a href="/search/astro-ph?searchtype=author&query=Cullen%2C+F">Fergus Cullen</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=Fern%C3%A1ndez%2C+V">Vital Fern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Fujimoto%2C+S">Seiji Fujimoto</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+I">Intae Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Krips%2C+M">Melanie Krips</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=Papovich%2C+C">Casey Papovich</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=Amor%C3%ADn%2C+R+O">Ricardo O. Amor铆n</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=Buat%2C+V">V茅ronique Buat</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=Chworowsky%2C+K">Katherine Chworowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+S+H">Seth H. Cohen</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=Giavalisco%2C+M">Mauro Giavalisco</a>, <a href="/search/astro-ph?searchtype=author&query=Huertas-Company%2C+M">Marc Huertas-Company</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="2303.15431v3-abstract-short" style="display: inline;"> During the first 500 million years of cosmic history, the first stars and galaxies formed, seeding the Universe with heavy elements and eventually reionizing the intergalactic medium. Observations with JWST have uncovered a surprisingly high abundance of candidates for early star-forming galaxies, with distances (redshifts, $z$), estimated from multi-band photometry, as large as $z\approx 16$, far… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.15431v3-abstract-full').style.display = 'inline'; document.getElementById('2303.15431v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.15431v3-abstract-full" style="display: none;"> During the first 500 million years of cosmic history, the first stars and galaxies formed, seeding the Universe with heavy elements and eventually reionizing the intergalactic medium. Observations with JWST have uncovered a surprisingly high abundance of candidates for early star-forming galaxies, with distances (redshifts, $z$), estimated from multi-band photometry, as large as $z\approx 16$, far beyond pre-JWST limits. While generally robust, such photometric redshifts can suffer from degeneracies and occasionally catastrophic errors. Spectroscopic measurement is required to validate these sources and to reliably quantify physical properties that can constrain galaxy formation models and cosmology. Here we present JWST spectroscopy that confirms redshifts for two very luminous galaxies with $z > 11$, but also demonstrates that another candidate with suggested $z\approx 16$ instead has $z = 4.9$, with an unusual combination of nebular line emission and dust reddening that mimics the colors expected for much more distant objects. These results reinforce evidence for the early, rapid formation of remarkably luminous galaxies, while also highlighting the necessity of spectroscopic verification. The large abundance of bright, early galaxies may indicate shortcomings in current galaxy formation models, or deviation from physical properties (such as the stellar initial mass function) that are generally believed to hold at later times. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.15431v3-abstract-full').style.display = 'none'; document.getElementById('2303.15431v3-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 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 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">Accelerated Article Preview (AAP) version published in Nature</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.14172">arXiv:2303.14172</a> <span> [<a href="https://arxiv.org/pdf/2303.14172">pdf</a>, <a href="https://arxiv.org/format/2303.14172">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</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/ace5b4">10.3847/2041-8213/ace5b4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Fermi-GBM Discovery of GRB 221009A: An Extraordinarily Bright GRB from Onset to Afterglow </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lesage%2C+S">S. Lesage</a>, <a href="/search/astro-ph?searchtype=author&query=Veres%2C+P">P. Veres</a>, <a href="/search/astro-ph?searchtype=author&query=Briggs%2C+M+S">M. S. Briggs</a>, <a href="/search/astro-ph?searchtype=author&query=Goldstein%2C+A">A. Goldstein</a>, <a href="/search/astro-ph?searchtype=author&query=Kocevski%2C+D">D. Kocevski</a>, <a href="/search/astro-ph?searchtype=author&query=Burns%2C+E">E. Burns</a>, <a href="/search/astro-ph?searchtype=author&query=Wilson-Hodge%2C+C+A">C. A. Wilson-Hodge</a>, <a href="/search/astro-ph?searchtype=author&query=Bhat%2C+P+N">P. N. Bhat</a>, <a href="/search/astro-ph?searchtype=author&query=Huppenkothen%2C+D">D. Huppenkothen</a>, <a href="/search/astro-ph?searchtype=author&query=Fryer%2C+C+L">C. L. Fryer</a>, <a href="/search/astro-ph?searchtype=author&query=Hamburg%2C+R">R. Hamburg</a>, <a href="/search/astro-ph?searchtype=author&query=Racusin%2C+J">J. Racusin</a>, <a href="/search/astro-ph?searchtype=author&query=Bissaldi%2C+E">E. Bissaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Cleveland%2C+W+H">W. H. Cleveland</a>, <a href="/search/astro-ph?searchtype=author&query=Dalessi%2C+S">S. Dalessi</a>, <a href="/search/astro-ph?searchtype=author&query=Fletcher%2C+C">C. Fletcher</a>, <a href="/search/astro-ph?searchtype=author&query=Giles%2C+M+M">M. M. Giles</a>, <a href="/search/astro-ph?searchtype=author&query=Hristov%2C+B+A">B. A. Hristov</a>, <a href="/search/astro-ph?searchtype=author&query=Hui%2C+C+M">C. M. Hui</a>, <a href="/search/astro-ph?searchtype=author&query=Mailyan%2C+B">B. Mailyan</a>, <a href="/search/astro-ph?searchtype=author&query=Malacaria%2C+C">C. Malacaria</a>, <a href="/search/astro-ph?searchtype=author&query=Poolakkil%2C+S">S. Poolakkil</a>, <a href="/search/astro-ph?searchtype=author&query=Roberts%2C+O+J">O. J. Roberts</a>, <a href="/search/astro-ph?searchtype=author&query=von+Kienlin%2C+A">A. von Kienlin</a>, <a href="/search/astro-ph?searchtype=author&query=Wood%2C+J">J. Wood</a> , et al. (115 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="2303.14172v2-abstract-short" style="display: inline;"> We report the discovery of GRB 221009A, the highest flux gamma-ray burst ever observed by the Fermi Gamma-ray Burst Monitor (GBM). This GRB has continuous prompt emission lasting more than 600 seconds which smoothly transitions to afterglow visible in the GBM energy range (8 keV--40 MeV), and total energetics higher than any other burst in the GBM sample. By using a variety of new and existing ana… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.14172v2-abstract-full').style.display = 'inline'; document.getElementById('2303.14172v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.14172v2-abstract-full" style="display: none;"> We report the discovery of GRB 221009A, the highest flux gamma-ray burst ever observed by the Fermi Gamma-ray Burst Monitor (GBM). This GRB has continuous prompt emission lasting more than 600 seconds which smoothly transitions to afterglow visible in the GBM energy range (8 keV--40 MeV), and total energetics higher than any other burst in the GBM sample. By using a variety of new and existing analysis techniques we probe the spectral and temporal evolution of GRB 221009A. We find no emission prior to the GBM trigger time (t0; 2022 October 9 at 13:16:59.99 UTC), indicating that this is the time of prompt emission onset. The triggering pulse exhibits distinct spectral and temporal properties suggestive of the thermal, photospheric emission of shock-breakout, with significant emission up to $\sim$15 MeV. We characterize the onset of external shock at t0+600 s and find evidence of a plateau region in the early-afterglow phase which transitions to a slope consistent with Swift-XRT afterglow measurements. We place the total energetics of GRB 221009A in context with the rest of the GBM sample and find that this GRB has the highest total isotropic-equivalent energy ($\textrm{E}_{纬,\textrm{iso}}=1.0\times10^{55}$ erg) and second highest isotropic-equivalent luminosity ($\textrm{L}_{纬,\textrm{iso}}=9.9\times10^{53}$ erg/s) based on redshift of z = 0.151. These extreme energetics are what allowed us to observe the continuously emitting central engine of GBM from the beginning of the prompt emission phase through the onset of early afterglow. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.14172v2-abstract-full').style.display = 'none'; document.getElementById('2303.14172v2-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 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 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 7 figures - accepted for publication in 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/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/2303.08918">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/2302.14037">arXiv:2302.14037</a> <span> [<a href="https://arxiv.org/pdf/2302.14037">pdf</a>, <a href="https://arxiv.org/format/2302.14037">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</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/acc39c">10.3847/2041-8213/acc39c <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> GRB 221009A, The BOAT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Burns%2C+E">Eric Burns</a>, <a href="/search/astro-ph?searchtype=author&query=Svinkin%2C+D">Dmitry Svinkin</a>, <a href="/search/astro-ph?searchtype=author&query=Fenimore%2C+E">Edward Fenimore</a>, <a href="/search/astro-ph?searchtype=author&query=Kann%2C+D+A">D. Alexander Kann</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez%2C+J+F+A">Jos茅 Feliciano Ag眉铆 Fern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Frederiks%2C+D">Dmitry Frederiks</a>, <a href="/search/astro-ph?searchtype=author&query=Hamburg%2C+R">Rachel Hamburg</a>, <a href="/search/astro-ph?searchtype=author&query=Lesage%2C+S">Stephen Lesage</a>, <a href="/search/astro-ph?searchtype=author&query=Temiraev%2C+Y">Yuri Temiraev</a>, <a href="/search/astro-ph?searchtype=author&query=Tsvetkova%2C+A">Anastasia Tsvetkova</a>, <a href="/search/astro-ph?searchtype=author&query=Bissaldi%2C+E">Elisabetta Bissaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Briggs%2C+M+S">Michael S. Briggs</a>, <a href="/search/astro-ph?searchtype=author&query=Fletcher%2C+C">Cori Fletcher</a>, <a href="/search/astro-ph?searchtype=author&query=Goldstein%2C+A">Adam Goldstein</a>, <a href="/search/astro-ph?searchtype=author&query=Hui%2C+C+M">C. Michelle Hui</a>, <a href="/search/astro-ph?searchtype=author&query=Hristov%2C+B+A">Boyan A. Hristov</a>, <a href="/search/astro-ph?searchtype=author&query=Kocevski%2C+D">Daniel Kocevski</a>, <a href="/search/astro-ph?searchtype=author&query=Lysenko%2C+A+L">Alexandra L. Lysenko</a>, <a href="/search/astro-ph?searchtype=author&query=Mailyan%2C+B">Bagrat Mailyan</a>, <a href="/search/astro-ph?searchtype=author&query=Racusin%2C+J">Judith Racusin</a>, <a href="/search/astro-ph?searchtype=author&query=Ridnaia%2C+A">Anna Ridnaia</a>, <a href="/search/astro-ph?searchtype=author&query=Roberts%2C+O+J">Oliver J. Roberts</a>, <a href="/search/astro-ph?searchtype=author&query=Ulanov%2C+M">Mikhail Ulanov</a>, <a href="/search/astro-ph?searchtype=author&query=Veres%2C+P">Peter Veres</a>, <a href="/search/astro-ph?searchtype=author&query=Wilson-Hodge%2C+C+A">Colleen A. Wilson-Hodge</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="2302.14037v3-abstract-short" style="display: inline;"> GRB 221009A has been referred to as the Brightest Of All Time (the BOAT). We investigate the veracity of this statement by comparing it with a half century of prompt gamma-ray burst observations. This burst is the brightest ever detected by the measures of peak flux and fluence. Unexpectedly, GRB 221009A has the highest isotropic-equivalent total energy ever identified, while the peak luminosity i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.14037v3-abstract-full').style.display = 'inline'; document.getElementById('2302.14037v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.14037v3-abstract-full" style="display: none;"> GRB 221009A has been referred to as the Brightest Of All Time (the BOAT). We investigate the veracity of this statement by comparing it with a half century of prompt gamma-ray burst observations. This burst is the brightest ever detected by the measures of peak flux and fluence. Unexpectedly, GRB 221009A has the highest isotropic-equivalent total energy ever identified, while the peak luminosity is at the $\sim99$th percentile of the known distribution. We explore how such a burst can be powered and discuss potential implications for ultra-long and high-redshift gamma-ray bursts. By geometric extrapolation of the total fluence and peak flux distributions GRB 221009A appears to be a once in 10,000 year event. Thus, while it almost certainly not the BOAT over all of cosmic history, it may be the brightest gamma-ray burst since human civilization began. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.14037v3-abstract-full').style.display = 'none'; document.getElementById('2302.14037v3-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 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 February, 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">Version accepted to ApJL. Also adds proper acknowledgements</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.05466">arXiv:2302.05466</a> <span> [<a href="https://arxiv.org/pdf/2302.05466">pdf</a>, <a href="https://arxiv.org/format/2302.05466">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 (NGDEEP) Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M+B">Micaela B. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Pirzkal%2C+N">Nor Pirzkal</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=Papovich%2C+C">Casey Papovich</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=Lotz%2C+J+M">Jennifer M. Lotz</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=Ferguson%2C+H+C">Henry C. Ferguson</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=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=Kocevski%2C+D+D">Dale D. Kocevski</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=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=Castellano%2C+M">Marco Castellano</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=Chworowsky%2C+K">Katherine Chworowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Cox%2C+I+G">Isabella G. Cox</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=Davis%2C+K">Kelcey Davis</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=Fontana%2C+A">Adriano Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Fujimoto%2C+S">Seiji Fujimoto</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="2302.05466v1-abstract-short" style="display: inline;"> We present the Next Generation Deep Extragalactic Exploratory Public (NGDEEP) Survey, a deep slitless spectroscopic and imaging Cycle 1 JWST treasury survey designed to constrain feedback mechanisms in low-mass galaxies across cosmic time. NGDEEP targets the Hubble Ultra Deep Field (HUDF) with NIRISS slitless spectroscopy (f~1.2e-18 erg/s/cm^2, 5sigma) to measure metallicities and star-formation r… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.05466v1-abstract-full').style.display = 'inline'; document.getElementById('2302.05466v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.05466v1-abstract-full" style="display: none;"> We present the Next Generation Deep Extragalactic Exploratory Public (NGDEEP) Survey, a deep slitless spectroscopic and imaging Cycle 1 JWST treasury survey designed to constrain feedback mechanisms in low-mass galaxies across cosmic time. NGDEEP targets the Hubble Ultra Deep Field (HUDF) with NIRISS slitless spectroscopy (f~1.2e-18 erg/s/cm^2, 5sigma) to measure metallicities and star-formation rates (SFRs) for low-mass galaxies through the peak of the cosmic SFR density (0.5<z<4). In parallel, NGDEEP targets the HUDF-Par2 parallel field with NIRCam (m=30.6-30.9, 5sigma) to discover galaxies to z>12, constraining the slope of the faint-end of the rest-ultraviolet luminosity function. NGDEEP overlaps with the deepest HST ACS optical imaging in the sky: F435W in the HUDF (m=29.6), and F814W in HUDF-Par2 (m=30), making this a premier HST+JWST Deep Field. As a treasury survey, NGDEEP data is public immediately, and we will rapidly release data products and catalogs in the spirit of previous deep field initiatives. In this paper we present the NGDEEP survey design, summarize the science goals, and detail plans for the public release of NGDEEP reduced data products. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.05466v1-abstract-full').style.display = 'none'; document.getElementById('2302.05466v1-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 February, 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">21 pages, 9 figures, submitted to AAS Journals</span> </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/2301.09482">arXiv:2301.09482</a> <span> [<a href="https://arxiv.org/pdf/2301.09482">pdf</a>, <a href="https://arxiv.org/format/2301.09482">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 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/acd2d9">10.3847/2041-8213/acd2d9 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CEERS Spectroscopic Confirmation of NIRCam-Selected z > 8 Galaxy Candidates with JWST/NIRSpec: Initial Characterization of their Properties </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fujimoto%2C+S">Seiji Fujimoto</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=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=Larson%2C+R+L">Rebecca L. Larson</a>, <a href="/search/astro-ph?searchtype=author&query=Burgarella%2C+D">Denis Burgarella</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=Behroozi%2C+P">Peter Behroozi</a>, <a href="/search/astro-ph?searchtype=author&query=Chworowsky%2C+K">Katherine Chworowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">Michaela Hirschmann</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=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=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=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=Grogin%2C+N+A">Norman A. Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Grazian%2C+A">Andrea Grazian</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=Kocevski%2C+D+D">Dale D. Kocevski</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=Pentericci%2C+L">Laura Pentericci</a> , et al. (16 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="2301.09482v2-abstract-short" style="display: inline;"> We present JWST NIRSpec spectroscopy for 11 galaxy candidates with photometric redshifts of $z\simeq9-13$ and $M_{\rm\,UV} \in[-21,-18]$ newly identified in NIRCam images in the Cosmic Evolution Early Release Science (CEERS) Survey. We confirm emission line redshifts for 7 galaxies at $z=7.762-8.998$ using spectra at $\sim1-5渭$m either with the NIRSpec prism or its three medium resolution gratings… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.09482v2-abstract-full').style.display = 'inline'; document.getElementById('2301.09482v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.09482v2-abstract-full" style="display: none;"> We present JWST NIRSpec spectroscopy for 11 galaxy candidates with photometric redshifts of $z\simeq9-13$ and $M_{\rm\,UV} \in[-21,-18]$ newly identified in NIRCam images in the Cosmic Evolution Early Release Science (CEERS) Survey. We confirm emission line redshifts for 7 galaxies at $z=7.762-8.998$ using spectra at $\sim1-5渭$m either with the NIRSpec prism or its three medium resolution gratings. For $z\simeq9$ photometric candidates, we achieve a high confirmation rate of $\simeq$90\%, which validates the classical dropout selection from NIRCam photometry. No robust emission lines are identified in three galaxy candidates at $z>10$, where the strong [OIII] and H$尾$ lines would be redshifted beyond the wavelength range observed by NIRSpec, and the Lyman-$伪$ continuum break is not detected with the current sensitivity. Compared with HST-selected bright galaxies ($M_{\rm\,UV}\simeq-22$) that are similarly spectroscopically confirmed at $z\gtrsim8$, these NIRCam-selected galaxies are characterized by lower star formation rates (SFR$\simeq4\,M_{\odot}$~yr$^{-1}$) and lower stellar masses ($\simeq10^{8}\,M_{\odot}$), but with higher [OIII]+H$尾$ equivalent widths ($\simeq$1100$脜$), and elevated production efficiency of ionizing photons ($\log(尉_{\rm\,ion}/{\rm\,Hz\,erg}^{-1})\simeq25.8$) induced by young stellar populations ($<10$~Myrs) accounting for $\simeq20\%$ of the galaxy mass, highlighting the key contribution of faint galaxies to cosmic reionization. Taking advantage of the homogeneous selection and sensitivity, we also investigate metallicity and ISM conditions with empirical calibrations using the [OIII]/H$尾$ ratio. We find that galaxies at $z\sim8-9$ have higher SFRs and lower metallicities than galaxies at similar stellar masses at $z\sim2-6$, which is generally consistent with the current galaxy formation and evolution models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.09482v2-abstract-full').style.display = 'none'; document.getElementById('2301.09482v2-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 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 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">24 pages, 12 figures, 2 tables. ApJL Focus Issue in press</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/2301.01607">arXiv:2301.01607</a> <span> [<a href="https://arxiv.org/pdf/2301.01607">pdf</a>, <a href="https://arxiv.org/format/2301.01607">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</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/acbb6a">10.3847/1538-4365/acbb6a <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Fermi-LAT Light Curve Repository </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abdollahi%2C+S">S. Abdollahi</a>, <a href="/search/astro-ph?searchtype=author&query=Ajello%2C+M">M. Ajello</a>, <a href="/search/astro-ph?searchtype=author&query=Baldini%2C+L">L. Baldini</a>, <a href="/search/astro-ph?searchtype=author&query=Ballet%2C+J">J. Ballet</a>, <a href="/search/astro-ph?searchtype=author&query=Bastieri%2C+D">D. Bastieri</a>, <a href="/search/astro-ph?searchtype=author&query=Gonzalez%2C+J+B">J. Becerra Gonzalez</a>, <a href="/search/astro-ph?searchtype=author&query=Bellazzini%2C+R">R. Bellazzini</a>, <a href="/search/astro-ph?searchtype=author&query=Berretta%2C+A">A. Berretta</a>, <a href="/search/astro-ph?searchtype=author&query=Bissaldi%2C+E">E. Bissaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Bonino%2C+R">R. Bonino</a>, <a href="/search/astro-ph?searchtype=author&query=Brill%2C+A">A. Brill</a>, <a href="/search/astro-ph?searchtype=author&query=Bruel%2C+P">P. Bruel</a>, <a href="/search/astro-ph?searchtype=author&query=Burns%2C+E">E. Burns</a>, <a href="/search/astro-ph?searchtype=author&query=Buson%2C+S">S. Buson</a>, <a href="/search/astro-ph?searchtype=author&query=Cameron%2C+A">A. Cameron</a>, <a href="/search/astro-ph?searchtype=author&query=Caputo%2C+R">R. Caputo</a>, <a href="/search/astro-ph?searchtype=author&query=Caraveo%2C+P+A">P. A. Caraveo</a>, <a href="/search/astro-ph?searchtype=author&query=Cibrario%2C+N">N. Cibrario</a>, <a href="/search/astro-ph?searchtype=author&query=Ciprini%2C+S">S. Ciprini</a>, <a href="/search/astro-ph?searchtype=author&query=Orestano%2C+P+C">P. Cristarella Orestano</a>, <a href="/search/astro-ph?searchtype=author&query=Crnogorcevic%2C+M">M. Crnogorcevic</a>, <a href="/search/astro-ph?searchtype=author&query=Cutini%2C+S">S. Cutini</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Ammando%2C+F">F. D'Ammando</a>, <a href="/search/astro-ph?searchtype=author&query=De+Gaetano%2C+S">S. De Gaetano</a>, <a href="/search/astro-ph?searchtype=author&query=Digel%2C+S+W">S. W. Digel</a> , et al. (88 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="2301.01607v2-abstract-short" style="display: inline;"> The Fermi Large Area Telescope (LAT) light curve repository (LCR) is a publicly available, continually updated library of gamma-ray light curves of variable Fermi-LAT sources generated over multiple timescales. The Fermi-LAT LCR aims to provide publication-quality light curves binned on timescales of 3 days, 7 days, and 30 days for 1525 sources deemed variable in the source catalog of the first 10… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.01607v2-abstract-full').style.display = 'inline'; document.getElementById('2301.01607v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.01607v2-abstract-full" style="display: none;"> The Fermi Large Area Telescope (LAT) light curve repository (LCR) is a publicly available, continually updated library of gamma-ray light curves of variable Fermi-LAT sources generated over multiple timescales. The Fermi-LAT LCR aims to provide publication-quality light curves binned on timescales of 3 days, 7 days, and 30 days for 1525 sources deemed variable in the source catalog of the first 10 years of Fermi-LAT observations. The repository consists of light curves generated through full likelihood analyses that model the sources and the surrounding region, providing fluxes and photon indices for each time bin. The LCR is intended as a resource for the time-domain and multi-messenger communities by allowing users to quickly search LAT data to identify correlated variability and flaring emission episodes from gamma-ray sources. We describe the sample selection and analysis employed by the LCR and provide an overview of the associated data access portal. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.01607v2-abstract-full').style.display = 'none'; document.getElementById('2301.01607v2-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> 14 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 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">Accepted for publication in ApJ Supplement Series</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/2212.07095">arXiv:2212.07095</a> <span> [<a href="https://arxiv.org/pdf/2212.07095">pdf</a>, <a href="https://arxiv.org/format/2212.07095">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</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/acc581">10.3847/1538-4357/acc581 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Temporal and Spectral Evolution of Gamma-ray Burst Broad Pulses: Identification of High Latitude Emission in the Prompt Emission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tak%2C+D">Donggeun Tak</a>, <a href="/search/astro-ph?searchtype=author&query=Uhm%2C+Z+L">Z. Lucas Uhm</a>, <a href="/search/astro-ph?searchtype=author&query=Racusin%2C+J">Judith Racusin</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+B">Bing Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Guiriec%2C+S">Sylvain Guiriec</a>, <a href="/search/astro-ph?searchtype=author&query=Kocevski%2C+D">Daniel Kocevski</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+B">Bin-Bin Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=McEnery%2C+J">Julie McEnery</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="2212.07095v2-abstract-short" style="display: inline;"> We perform a detailed analysis on broad pulses in bright Gamma-ray bursts (GRBs) to understand the evolution of GRB broad pulses. Using the temporal and spectral properties, we test the high latitude emission (HLE) scenario in the decaying phase of broad pulses. The HLE originates from the curvature effect of a relativistic spherical jet, where higher latitude photons are delayed and softer than t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.07095v2-abstract-full').style.display = 'inline'; document.getElementById('2212.07095v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.07095v2-abstract-full" style="display: none;"> We perform a detailed analysis on broad pulses in bright Gamma-ray bursts (GRBs) to understand the evolution of GRB broad pulses. Using the temporal and spectral properties, we test the high latitude emission (HLE) scenario in the decaying phase of broad pulses. The HLE originates from the curvature effect of a relativistic spherical jet, where higher latitude photons are delayed and softer than the observer's line-of-sight emission. The signature of HLE has not yet been identified undisputedly during the prompt emission of GRBs. The HLE theory predicts a specific relation, F$_{谓, E_{p}}$ $\propto$ E$_{p}\!^{2}$, between the peak energy $E_{p}$ in $谓$F$_谓$ spectra and the spectral flux F$_谓$ measured at $E_{p}$, F$_{谓, E_{p}}$. We search for evidence of this relation in 2157 GRBs detected by the Gamma-ray Burst Monitor (GBM) on board the Fermi Gamma-ray Space Telescope (Fermi) from the years 2008 to 2017. After imposing unbiased selection criteria in order to minimize contamination in a signal by background and overlaps of pulses, we build a sample of 32 broad pulses in 32 GRBs. We perform a time-resolved spectral analysis on each of these 32 broad pulses and find that the evolution of 18 pulses (56%) is clearly consistent with the HLE relation. For the 18 broad pulses, the exponent $未$ in the relation of F$_{谓, E_{p}}$ $\propto$ E$_{p}\!^未$ is distributed as a Gaussian function with median and width of 1.99 and 0.34, respectively. This result provides constraint on the emission radius of GRBs with the HLE signature. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.07095v2-abstract-full').style.display = 'none'; document.getElementById('2212.07095v2-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 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 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">30 pages, 36 figures, accepted 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/2212.07094">arXiv:2212.07094</a> <span> [<a href="https://arxiv.org/pdf/2212.07094">pdf</a>, <a href="https://arxiv.org/ps/2212.07094">ps</a>, <a href="https://arxiv.org/format/2212.07094">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Evidence of high latitude emission in the prompt phase of GRBs: How far from the central engine are the GRBs produced? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Uhm%2C+Z+L">Z. Lucas Uhm</a>, <a href="/search/astro-ph?searchtype=author&query=Tak%2C+D">Donggeun Tak</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+B">Bing Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Racusin%2C+J">Judith Racusin</a>, <a href="/search/astro-ph?searchtype=author&query=Kocevski%2C+D">Daniel Kocevski</a>, <a href="/search/astro-ph?searchtype=author&query=Guiriec%2C+S">Sylvain Guiriec</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+B">Bin-Bin Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=McEnery%2C+J">Julie McEnery</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="2212.07094v2-abstract-short" style="display: inline;"> The physical mechanism of gamma-ray bursts (GRBs) remains elusive. One of the difficulties in nailing down their physical mechanism comes from the fact that there has been no clear observational evidence on how far from the central engine the prompt gamma-rays of GRBs are emitted while the competing physical mechanisms predict different characteristic distances. Here we present a simple study addr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.07094v2-abstract-full').style.display = 'inline'; document.getElementById('2212.07094v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.07094v2-abstract-full" style="display: none;"> The physical mechanism of gamma-ray bursts (GRBs) remains elusive. One of the difficulties in nailing down their physical mechanism comes from the fact that there has been no clear observational evidence on how far from the central engine the prompt gamma-rays of GRBs are emitted while the competing physical mechanisms predict different characteristic distances. Here we present a simple study addressing this question by making use of the "high-latitude emission" (HLE). We show that our detailed numerical modeling exhibits a clear signature of HLE in the decaying phase of "broad pulses" of GRBs. We show that the HLE can emerge as a prominent spectral break in $F_谓$ spectra and dominate the peak of $谓F_谓$ spectra even while the "line-of-sight emission" (LoSE) is still ongoing, hence providing a new view of HLE emergence. We remark that this "HLE break" could be hidden in some broad pulses, depending on the proximity between the peak energies of the LoSE and the HLE. Also, we present three examples of Fermi-GBM GRBs with broad pulses that exhibit the HLE signature. We show that their gamma-ray emitting region should be located at $\sim 10^{16}$ cm from the central engine, which disfavors the photosphere models and small-radii internal shock models but favors magnetic dissipation models with a large emission radius. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.07094v2-abstract-full').style.display = 'none'; document.getElementById('2212.07094v2-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 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">8 pages, 4 figures, submitted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.16537">arXiv:2211.16537</a> <span> [<a href="https://arxiv.org/pdf/2211.16537">pdf</a>, <a href="https://arxiv.org/format/2211.16537">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</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/s41550-022-01820-x">10.1038/s41550-022-01820-x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Birth of a Relativistic Jet Following the Disruption of a Star by a Cosmological Black Hole </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pasham%2C+D+R">Dheeraj R. Pasham</a>, <a href="/search/astro-ph?searchtype=author&query=Lucchini%2C+M">Matteo Lucchini</a>, <a href="/search/astro-ph?searchtype=author&query=Laskar%2C+T">Tanmoy Laskar</a>, <a href="/search/astro-ph?searchtype=author&query=Gompertz%2C+B+P">Benjamin P. Gompertz</a>, <a href="/search/astro-ph?searchtype=author&query=Srivastav%2C+S">Shubham Srivastav</a>, <a href="/search/astro-ph?searchtype=author&query=Nicholl%2C+M">Matt Nicholl</a>, <a href="/search/astro-ph?searchtype=author&query=Smartt%2C+S+J">Stephen J. Smartt</a>, <a href="/search/astro-ph?searchtype=author&query=Miller-Jones%2C+J+C+A">James C. A. Miller-Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+K+D">Kate D. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Fender%2C+R">Rob Fender</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+G+P">Graham P. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Fulton%2C+M+D">Michael D. Fulton</a>, <a href="/search/astro-ph?searchtype=author&query=Dewangan%2C+G">Gulab Dewangan</a>, <a href="/search/astro-ph?searchtype=author&query=Gendreau%2C+K">Keith Gendreau</a>, <a href="/search/astro-ph?searchtype=author&query=Coughlin%2C+E+R">Eric R. Coughlin</a>, <a href="/search/astro-ph?searchtype=author&query=Rhodes%2C+L">Lauren Rhodes</a>, <a href="/search/astro-ph?searchtype=author&query=Horesh%2C+A">Assaf Horesh</a>, <a href="/search/astro-ph?searchtype=author&query=van+Velzen%2C+S">Sjoert van Velzen</a>, <a href="/search/astro-ph?searchtype=author&query=Sfaradi%2C+I">Itai Sfaradi</a>, <a href="/search/astro-ph?searchtype=author&query=Guolo%2C+M">Muryel Guolo</a>, <a href="/search/astro-ph?searchtype=author&query=Segura%2C+N+C">N. Castro Segura</a>, <a href="/search/astro-ph?searchtype=author&query=Aamer%2C+A">Aysha Aamer</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J+P">Joseph P. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Arcavi%2C+I">Iair Arcavi</a>, <a href="/search/astro-ph?searchtype=author&query=Brennan%2C+S+J">Sean J. Brennan</a> , et al. (41 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="2211.16537v1-abstract-short" style="display: inline;"> A black hole can launch a powerful relativistic jet after it tidally disrupts a star. If this jet fortuitously aligns with our line of sight, the overall brightness is Doppler boosted by several orders of magnitude. Consequently, such on-axis relativistic tidal disruption events (TDEs) have the potential to unveil cosmological (redshift $z>$1) quiescent black holes and are ideal test beds to under… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.16537v1-abstract-full').style.display = 'inline'; document.getElementById('2211.16537v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.16537v1-abstract-full" style="display: none;"> A black hole can launch a powerful relativistic jet after it tidally disrupts a star. If this jet fortuitously aligns with our line of sight, the overall brightness is Doppler boosted by several orders of magnitude. Consequently, such on-axis relativistic tidal disruption events (TDEs) have the potential to unveil cosmological (redshift $z>$1) quiescent black holes and are ideal test beds to understand the radiative mechanisms operating in super-Eddington jets. Here, we present multi-wavelength (X-ray, UV, optical, and radio) observations of the optically discovered transient \target at $z=1.193$. Its unusual X-ray properties, including a peak observed luminosity of $\gtrsim$10$^{48}$ erg s$^{-1}$, systematic variability on timescales as short as 1000 seconds, and overall duration lasting more than 30 days in the rest-frame are traits associated with relativistic TDEs. The X-ray to radio spectral energy distributions spanning 5-50 days after discovery can be explained as synchrotron emission from a relativistic jet (radio), synchrotron self-Compton (X-rays), and thermal emission similar to that seen in low-redshift TDEs (UV/optical). Our modeling implies a beamed, highly relativistic jet akin to blazars but requires extreme matter-domination, i.e, high ratio of electron-to-magnetic field energy densities in the jet, and challenges our theoretical understanding of jets. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.16537v1-abstract-full').style.display = 'none'; document.getElementById('2211.16537v1-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 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">To appear in Nature Astronomy on 30th November 2022. Also see here for an animation explaining the result: https://youtu.be/MQHdSbxuznY</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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