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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Bergamini%2C+P&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Bergamini%2C+P&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Bergamini%2C+P&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> </ul> </nav> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.00191">arXiv:2412.00191</a> <span> [<a href="https://arxiv.org/pdf/2412.00191">pdf</a>, <a href="https://arxiv.org/format/2412.00191">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Euclid preparation: TBD. The impact of line-of-sight projections on the covariance between galaxy cluster multi-wavelength observable properties -- insights from hydrodynamic simulations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Ragagnin%2C+A">A. Ragagnin</a>, <a href="/search/astro-ph?searchtype=author&query=Saro%2C+A">A. Saro</a>, <a href="/search/astro-ph?searchtype=author&query=Andreon%2C+S">S. Andreon</a>, <a href="/search/astro-ph?searchtype=author&query=Biviano%2C+A">A. Biviano</a>, <a href="/search/astro-ph?searchtype=author&query=Dolag%2C+K">K. Dolag</a>, <a href="/search/astro-ph?searchtype=author&query=Ettori%2C+S">S. Ettori</a>, <a href="/search/astro-ph?searchtype=author&query=Giocoli%2C+C">C. Giocoli</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+A+M+C+L">A. M. C. Le Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Mamon%2C+G+A">G. A. Mamon</a>, <a href="/search/astro-ph?searchtype=author&query=Maughan%2C+B+J">B. J. Maughan</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">M. Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Moscardini%2C+L">L. Moscardini</a>, <a href="/search/astro-ph?searchtype=author&query=Pacaud%2C+F">F. Pacaud</a>, <a href="/search/astro-ph?searchtype=author&query=Pratt%2C+G+W">G. W. Pratt</a>, <a href="/search/astro-ph?searchtype=author&query=Sereno%2C+M">M. Sereno</a>, <a href="/search/astro-ph?searchtype=author&query=Borgani%2C+S">S. Borgani</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">F. Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Castignani%2C+G">G. Castignani</a>, <a href="/search/astro-ph?searchtype=author&query=De+Petris%2C+M">M. De Petris</a>, <a href="/search/astro-ph?searchtype=author&query=Eckert%2C+D">D. Eckert</a>, <a href="/search/astro-ph?searchtype=author&query=Lesci%2C+G+F">G. F. Lesci</a>, <a href="/search/astro-ph?searchtype=author&query=Macias-Perez%2C+J">J. Macias-Perez</a>, <a href="/search/astro-ph?searchtype=author&query=Maturi%2C+M">M. Maturi</a>, <a href="/search/astro-ph?searchtype=author&query=Amara%2C+A">A. Amara</a> , et al. (218 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.00191v1-abstract-short" style="display: inline;"> Cluster cosmology can benefit from combining multi-wavelength studies, which can benefit from characterising the correlation coefficients between different mass-observable relations. In this work, we aim to provide information on the scatter, the skewness, and the covariance of various mass-observable relations in galaxy clusters in cosmological hydrodynamic simulations. This information will help… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.00191v1-abstract-full').style.display = 'inline'; document.getElementById('2412.00191v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.00191v1-abstract-full" style="display: none;"> Cluster cosmology can benefit from combining multi-wavelength studies, which can benefit from characterising the correlation coefficients between different mass-observable relations. In this work, we aim to provide information on the scatter, the skewness, and the covariance of various mass-observable relations in galaxy clusters in cosmological hydrodynamic simulations. This information will help future analyses to better tackle accretion histories and projection effects and model mass observable relations for cosmology studies.We identify galaxy clusters in Magneticum Box2b simulations with mass $M_{\rm 200c}>10^{14} {\rm M}_\odot$ at redshift $z=0.24$ and $z=0.90$. Our analysis includes \Euclid-derived properties such as richness, stellar mass, lensing mass, and concentration. Additionally, we investigate complementary multi-wavelength data, including X-ray luminosity, integrated Compton-$y$ parameter, gas mass, and temperature. The impact of projection effects on mass-observable residuals and correlations is then examined. At intermediate redshift ($z=0.24$), projection effects impact lensing concentration, richness, and gas mass the most in terms of scatter and skewness of log-residuals of scaling relations. The contribution of projection effects can be significant enough to boost a spurious hot- vs. cold-baryons correlation and consequently hide underlying correlations due to halo accretion histories. At high redshift ($z=0.9$), the richness has a much lower scatter (of log-residuals), and the quantity that is most impacted by projection effects is the lensing mass. Lensing concentration reconstruction, in particular, is affected by deviations of the reduced-shear profile shape from the one derived by an NFW profile rather than interlopers in the line of sight. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.00191v1-abstract-full').style.display = 'none'; document.getElementById('2412.00191v1-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, 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">26 pages, 22 figures, submitted to A&A, replied to referee comments</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.18763">arXiv:2410.18763</a> <span> [<a href="https://arxiv.org/pdf/2410.18763">pdf</a>, <a href="https://arxiv.org/format/2410.18763">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 dual nature of GHZ9: coexisting AGN and star formation activity in a remote X-ray source at z=10.145 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+L">Lorenzo Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">Marco Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">Laura Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Vignali%2C+C">Cristian Vignali</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">Roberto Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">Adriano Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Santini%2C+P">Paola Santini</a>, <a href="/search/astro-ph?searchtype=author&query=Treu%2C+T">Tommaso Treu</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=Llerena%2C+M">Mario Llerena</a>, <a href="/search/astro-ph?searchtype=author&query=Piconcelli%2C+E">Enrico Piconcelli</a>, <a href="/search/astro-ph?searchtype=author&query=Zappacosta%2C+L">Luca Zappacosta</a>, <a href="/search/astro-ph?searchtype=author&query=Mascia%2C+S">Sara Mascia</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">Pietro Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Bakx%2C+T+J+L+C">Tom J. L. C. Bakx</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Glazebrook%2C+K">Karl Glazebrook</a>, <a href="/search/astro-ph?searchtype=author&query=Henry%2C+A">Alaina Henry</a>, <a href="/search/astro-ph?searchtype=author&query=Leethochawalit%2C+N">Nicha Leethochawalit</a>, <a href="/search/astro-ph?searchtype=author&query=Mazzolari%2C+G">Giovanni Mazzolari</a>, <a href="/search/astro-ph?searchtype=author&query=Merlin%2C+E">Emiliano Merlin</a>, <a href="/search/astro-ph?searchtype=author&query=Morishita%2C+T">Takahiro Morishita</a>, <a href="/search/astro-ph?searchtype=author&query=Nanayakkara%2C+T">Themiya Nanayakkara</a>, <a href="/search/astro-ph?searchtype=author&query=Paris%2C+D">Diego Paris</a>, <a href="/search/astro-ph?searchtype=author&query=Puccetti%2C+S">Simonetta Puccetti</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="2410.18763v1-abstract-short" style="display: inline;"> We present JWST/NIRSpec PRISM spectroscopic characterization of GHZ9 at z= 10.145 $\pm$ 0.010, currently the most distant source detected by the Chandra X-ray Observatory. The spectrum reveals several UV high-ionization lines, including CII, SiIV, [NIV], CIV, HeII, OIII], NIII], and CIII]. The prominent rest-frame equivalent widths (EW(CIV)$\simeq$65A, EW(HeII)$\simeq$18A, EW(CIII])$\simeq$48A) sh… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.18763v1-abstract-full').style.display = 'inline'; document.getElementById('2410.18763v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.18763v1-abstract-full" style="display: none;"> We present JWST/NIRSpec PRISM spectroscopic characterization of GHZ9 at z= 10.145 $\pm$ 0.010, currently the most distant source detected by the Chandra X-ray Observatory. The spectrum reveals several UV high-ionization lines, including CII, SiIV, [NIV], CIV, HeII, OIII], NIII], and CIII]. The prominent rest-frame equivalent widths (EW(CIV)$\simeq$65A, EW(HeII)$\simeq$18A, EW(CIII])$\simeq$48A) show the presence of a hard radiation field, while the analysis of line ratio diagnostics suggest this galaxy hosts both AGN and star-formation activity. GHZ9 is nitrogen-enriched (6--9.5 times solar), carbon-poor (0.2--0.65 times solar), metal-poor (Z = 0.01--0.1 Z$_{\odot}$), and compact ($<$ 106 pc), similarly to GNz11, GHZ2, and recently discovered N-enhanced high redshift objects. We exploited the newly available JWST/NIRSpec and NIRCam dataset to perform an independent analysis of the Chandra data confirming that GHZ9 is the most likely JWST source associated to X-ray emission at 0.5-7 keV. Assuming a spectral index $螕$ = 2.3 (1.8), we estimate a black hole (BH) mass of 1.60 $\pm$ 0.31 (0.48 $\pm$ 0.09) $\times$ 10$^8$M$_{\odot}$, which is consistent either with Eddington-accretion onto heavy ($\geq$ 10$^6$ M$_{\odot}$) BH seeds formed at z=18, or super-Eddington accretion onto a light seed of $\sim$ 10$^2-10^4$ M$_{\odot}$ at z = 25. The corresponding BH-to-stellar mass ratio M$_{BH}$/M$_{star}$= 0.33$\pm$0.22 (0.10$\pm$0.07), with a stringent limit $>$0.02, implies an accelerated growth of the BH mass with respect to the stellar mass. GHZ9 is the ideal target to constrain the early phases of AGN-galaxy coevolution with future multi-frequency observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.18763v1-abstract-full').style.display = 'none'; document.getElementById('2410.18763v1-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 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">Submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.10967">arXiv:2410.10967</a> <span> [<a href="https://arxiv.org/pdf/2410.10967">pdf</a>, <a href="https://arxiv.org/format/2410.10967">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"> Seven wonders of Cosmic Dawn: JWST confirms a high abundance of galaxies and AGNs at z $\simeq$ 9-11 in the GLASS field </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+L">L. Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Haro%2C+P+A">P. Arrabal Haro</a>, <a href="/search/astro-ph?searchtype=author&query=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=Bergamini%2C+P">P. Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Calabro%2C+A">A. Calabro</a>, <a href="/search/astro-ph?searchtype=author&query=Mascia%2C+S">S. Mascia</a>, <a href="/search/astro-ph?searchtype=author&query=Morishita%2C+T">T. Morishita</a>, <a href="/search/astro-ph?searchtype=author&query=Roberts-Borsani%2C+G">G. Roberts-Borsani</a>, <a href="/search/astro-ph?searchtype=author&query=Santini%2C+P">P. Santini</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Vulcani%2C+B">B. Vulcani</a>, <a href="/search/astro-ph?searchtype=author&query=Zakharova%2C+D">D. Zakharova</a>, <a href="/search/astro-ph?searchtype=author&query=Bakx%2C+T">T. Bakx</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">M. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Leethochawalit%2C+N">N. Leethochawalit</a>, <a href="/search/astro-ph?searchtype=author&query=Llerena%2C+M">M. Llerena</a>, <a href="/search/astro-ph?searchtype=author&query=Merlin%2C+E">E. Merlin</a>, <a href="/search/astro-ph?searchtype=author&query=Paris%2C+D">D. Paris</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas-Ruiz%2C+S">S. Rojas-Ruiz</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+X">X. Wang</a> , et al. (2 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.10967v1-abstract-short" style="display: inline;"> We present JWST/NIRSpec PRISM follow-up of candidate galaxies at z=9-11 selected from deep JWST/NIRCam photometry in GLASS-JWST Early Release Science data. We spectroscopically confirm six sources with secure redshifts at z = 9.52-10.43, each showing multiple emission lines. An additional object is likely at z = 10.66, based on its Lya-break and a single emission feature, while one source is a low… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.10967v1-abstract-full').style.display = 'inline'; document.getElementById('2410.10967v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.10967v1-abstract-full" style="display: none;"> We present JWST/NIRSpec PRISM follow-up of candidate galaxies at z=9-11 selected from deep JWST/NIRCam photometry in GLASS-JWST Early Release Science data. We spectroscopically confirm six sources with secure redshifts at z = 9.52-10.43, each showing multiple emission lines. An additional object is likely at z = 10.66, based on its Lya-break and a single emission feature, while one source is a lower redshift interloper. The sample includes the first JWST-detected candidate at z=10, GHZ1/GLASS-z10, which we confirm at z = 9.875, and the X-ray detected AGN GHZ9 confirmed at z = 10.145. Three objects in our sample, including GHZ9, have EW(CIII])>20A and occupy a region compatible with AGN emission in the EW(CIII]) vs CIV/CIII] diagram. The spectroscopic sample confirms a high abundance of galaxies at z > 9. We measure a number density of z=10 galaxies in the GLASS-JWST ERS field that is a factor of >3 higher than other JWST-based estimates at demagnified rest-frame magnitudes of -21 < Muv < -19. We find that the positions of these galaxies in redshift and angular space are not consistent with all of them being part of a unique progenitor of present-day galaxy clusters. The high density of objects in the GLASS region can be explained either by clustering on large scales or by a superposition of different forming structures of which we observe only the brightest members. By considering all the spectroscopic z=10 sources in the Abell-2744 field, we identify two potential galaxy proto-clusters centered around GHZ9 and JD1, with relative separations between their members of 1-2 pMpc. The potential AGN nature of three of the sources in our sample lends support to a scenario in which the high abundance of bright sources determined by JWST surveys at cosmic dawn may be affected by AGN contribution to their UV luminosity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.10967v1-abstract-full').style.display = 'none'; document.getElementById('2410.10967v1-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 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">Submitted to A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.01883">arXiv:2410.01883</a> <span> [<a href="https://arxiv.org/pdf/2410.01883">pdf</a>, <a href="https://arxiv.org/format/2410.01883">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> The next step in galaxy cluster strong lensing: modeling the surface brightness of multiply-imaged sources </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Acebron%2C+A">Ana Acebron</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">Claudio Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Suyu%2C+S+H">Sherry H. Suyu</a>, <a href="/search/astro-ph?searchtype=author&query=Angora%2C+G">Giuseppe Angora</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">Pietro Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Caminha%2C+G+B">Gabriel B. Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Ertl%2C+S">Sebastian Ertl</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">Amata Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">Mario Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">Piero Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+H">Han Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Bolamperti%2C+A">Andrea Bolamperti</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">Massimo Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Schuldt%2C+S">Stefan Schuldt</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">Eros Vanzella</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="2410.01883v1-abstract-short" style="display: inline;"> Overcoming both modeling and computational challenges, we present, for the first time, the extended surface-brightness distribution model of a strongly-lensed source in a complex galaxy-cluster-scale system. We exploit the high-resolution Hubble Space Telescope (HST) imaging and extensive Multi Unit Spectroscopic Explorer spectroscopy to build an extended strong-lensing model, in a full multi-plan… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.01883v1-abstract-full').style.display = 'inline'; document.getElementById('2410.01883v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.01883v1-abstract-full" style="display: none;"> Overcoming both modeling and computational challenges, we present, for the first time, the extended surface-brightness distribution model of a strongly-lensed source in a complex galaxy-cluster-scale system. We exploit the high-resolution Hubble Space Telescope (HST) imaging and extensive Multi Unit Spectroscopic Explorer spectroscopy to build an extended strong-lensing model, in a full multi-plane formalism, of SDSS J1029+2623, a lens cluster at $z = 0.588$ with three multiple images of a background quasar ($z = 2.1992$). Going beyond typical cluster strong-lensing modeling techniques, we include as observables both the positions of 26 pointlike multiple images from seven background sources, spanning a wide redshift range between 1.02 and 5.06, and the extended surface-brightness distribution of the strongly-lensed quasar host galaxy, over $\sim78000$ HST pixels. In addition, we model the light distribution of seven objects, angularly close to the strongly-lensed quasar host, over $\sim9300$ HST pixels. Our extended lens model reproduces well both the observed intensity and morphology of the quasar host galaxy in the HST F160W band (with a 0''.03 pixel scale). The reconstructed source shows a single, compact, and smooth surface-brightness distribution, for which we estimate an intrinsic magnitude of 23.3 $\pm$ 0.1 in the F160W band and a half-light radius of (2.39 $\pm$ 0.03) kpc. The increased number of observables enables the accurate determination of the total mass of line-of-sight halos lying angularly close to the extended arc. This work paves the way for a new generation of galaxy cluster strong-lens models, where additional, complementary lensing observables are directly incorporated as model constraints. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.01883v1-abstract-full').style.display = 'none'; document.getElementById('2410.01883v1-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 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">19 pages, 9 Figures, 2 Tables. Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.10980">arXiv:2408.10980</a> <span> [<a href="https://arxiv.org/pdf/2408.10980">pdf</a>, <a href="https://arxiv.org/format/2408.10980">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"> Accelerated Emergence of Evolved Galaxies in Early Overdensities at $z\sim5.7$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Morishita%2C+T">Takahiro Morishita</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Z">Zhaoran Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Stiavelli%2C+M">Massimo Stiavelli</a>, <a href="/search/astro-ph?searchtype=author&query=Treu%2C+T">Tommaso Treu</a>, <a href="/search/astro-ph?searchtype=author&query=Trenti%2C+M">Michele Trenti</a>, <a href="/search/astro-ph?searchtype=author&query=Chartab%2C+N">Nima Chartab</a>, <a href="/search/astro-ph?searchtype=author&query=Roberts-Borsani%2C+G">Guido Roberts-Borsani</a>, <a href="/search/astro-ph?searchtype=author&query=Vulcani%2C+B">Benedetta Vulcani</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">Pietro Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">Marco Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">Claudio Grillo</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="2408.10980v1-abstract-short" style="display: inline;"> We report the identification of two galaxy overdensities at $z\sim5.7$ in the sightline of the galaxy cluster Abell 2744. These overdensities consist of 25 and 17 member galaxies, spectroscopically confirmed with JWST NIRSpec/MSA and NIRCam/WFSS. Each overdensity has a total stellar mass of $\sim2\times10^{10} M_\odot$ and a star formation rate of $\sim200 M_\odot$/yr within a central region of ra… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.10980v1-abstract-full').style.display = 'inline'; document.getElementById('2408.10980v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.10980v1-abstract-full" style="display: none;"> We report the identification of two galaxy overdensities at $z\sim5.7$ in the sightline of the galaxy cluster Abell 2744. These overdensities consist of 25 and 17 member galaxies, spectroscopically confirmed with JWST NIRSpec/MSA and NIRCam/WFSS. Each overdensity has a total stellar mass of $\sim2\times10^{10} M_\odot$ and a star formation rate of $\sim200 M_\odot$/yr within a central region of radius $R=2$ Mpc (physical). The sensitive PRISM spectra allow us to identify six galaxies that show weak Ha+[NII] emissions within the overdensities ($27\pm6\%$), whereas the fraction of such galaxies is found significantly lower ($6\pm2\%$) in field samples of the equivalent redshift range. These weak emission line galaxies, dubbed as wELGs, exhibit a strong continuum break at $4000$AA rest-frame, a characteristic feature of evolved stellar populations. The high observed fraction of wELGs in the two overdensities is consistent with the idea that high-density environments are an ideal site where galaxies can accelerate their evolutionary pace compared to field analogs. Our study pinpoints an early onset of environmental effects, already important within one billion years after the Big Bang, and provides a complementary perspective on the emergence of quenched, massive galaxies at lower redshifts. Potential contributions from black hole accretion feedback to the reduction of star formation activity are discussed, but the connection to the local environments remains unclear. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.10980v1-abstract-full').style.display = 'none'; document.getElementById('2408.10980v1-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 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">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/2407.20331">arXiv:2407.20331</a> <span> [<a href="https://arxiv.org/pdf/2407.20331">pdf</a>, <a href="https://arxiv.org/format/2407.20331">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"> Anatomy of a z=6 Lyman-伪 emitter down to parsec scales: extreme UV slopes, metal-poor regions and possibly leaking star clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Messa%2C+M">Matteo Messa</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Loiacono%2C+F">F. Loiacono</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">P. Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+B">B. Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Willott%2C+C">C. Willott</a>, <a href="/search/astro-ph?searchtype=author&query=Windhorst%2C+R+A">R. A. Windhorst</a>, <a href="/search/astro-ph?searchtype=author&query=Yan%2C+H">H. Yan</a>, <a href="/search/astro-ph?searchtype=author&query=Angora%2C+G">G. Angora</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Adamo%2C+A">A. Adamo</a>, <a href="/search/astro-ph?searchtype=author&query=Annibali%2C+F">F. Annibali</a>, <a href="/search/astro-ph?searchtype=author&query=Bolamperti%2C+A">A. Bolamperti</a>, <a href="/search/astro-ph?searchtype=author&query=Brada%C4%8D%2C+M">M. Brada膷</a>, <a href="/search/astro-ph?searchtype=author&query=Bradley%2C+L+D">L. D. Bradley</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">F. Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Claeyssens%2C+A">A. Claeyssens</a>, <a href="/search/astro-ph?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C+J">C. J. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Silva%2C+J+C+J">J. C. J. D'Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">M. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Frye%2C+B+L">B. L. Frye</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">N. A. Grogin</a> , et al. (9 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="2407.20331v1-abstract-short" style="display: inline;"> We present a detailed JWST/NIRSpec and NIRCam analysis of a gravitationally-lensed galaxy ($\rm 渭=17-21$) at redshift 6.14 magnified by the Hubble Frontier Field galaxy cluster MACS J0416. The target galaxy is overall a typical compact and UV-faint ($\rm M_{UV}=-17.8$) Lyman-$伪$ emitter; yet, the large magnification allows the detailed characterisation of structures on sub-galactic (down to few pa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.20331v1-abstract-full').style.display = 'inline'; document.getElementById('2407.20331v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.20331v1-abstract-full" style="display: none;"> We present a detailed JWST/NIRSpec and NIRCam analysis of a gravitationally-lensed galaxy ($\rm 渭=17-21$) at redshift 6.14 magnified by the Hubble Frontier Field galaxy cluster MACS J0416. The target galaxy is overall a typical compact and UV-faint ($\rm M_{UV}=-17.8$) Lyman-$伪$ emitter; yet, the large magnification allows the detailed characterisation of structures on sub-galactic (down to few parsec) scales. Prominent optical $\rm H伪$, $\rm H尾$ and [OIII]$位\lambda4959,5007$ lines are spatially resolved with the high spectral resolution grating (G395H, R~2700), with large equivalent widths, EW($\rm H尾$+[OIII])$\gtrsim1000$ 脜, and elevated ionising photon production efficiencies $\rm log(尉_{ion}/erg^{-1}Hz)=25.2-25.7$. NIRCam deep imaging reveals the presence of compact rest-UV bright regions along with individual star clusters of sizes $\rm R_{eff}=3-8~pc$ and masses $\rm M\sim2\cdot10^5-5\cdot10^{6}~M_\odot$ These clusters are characterised by steep UV slopes, $\rm尾_{UV}\lesssim-2.5$, in some cases associated with a dearth of line emission, indicating possible leaking of the ionising radiation, as also supported by a Lyman-$\rm 伪$ emission peaking at $\rm \sim100~km~s^{-1}$ from the systemic redshift. While the entire system is characterised by low-metallicity, $\sim0.1~Z_\odot$, the NIRSpec-IFU map also reveals the presence of a low-luminosity, metal-poor region with $\rm Z\lesssim2\%~Z_\odot$, barely detected in NIRCam imaging; this region is displaced by $\rm >200~pc$ from one of the UV brightest structures of the system, and it would have been too faint to detect if not for the large magnification of the system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.20331v1-abstract-full').style.display = 'none'; document.getElementById('2407.20331v1-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 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">19 pages (11 figures, 2 tables) + appendix (3 pages, 4 figures, 1 table). Submitted to A&A; comments are welcome</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.20327">arXiv:2407.20327</a> <span> [<a href="https://arxiv.org/pdf/2407.20327">pdf</a>, <a href="https://arxiv.org/format/2407.20327">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202451696">10.1051/0004-6361/202451696 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Extreme Ionizing Properties of Metal-Poor, Muv ~ -12 Star Complex in the first Gyr </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Loiacono%2C+F">F. Loiacono</a>, <a href="/search/astro-ph?searchtype=author&query=Messa%2C+M">M. Messa</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">P. Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Zanella%2C+A">A. Zanella</a>, <a href="/search/astro-ph?searchtype=author&query=Annibali%2C+F">F. Annibali</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+B">B. Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">M. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Adamo%2C+A">A. Adamo</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">F. Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Ricotti%2C+M">M. Ricotti</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">M. Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Bradac%2C+M">M. Bradac</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C+J">C. J. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Yan%2C+H">H. Yan</a>, <a href="/search/astro-ph?searchtype=author&query=Bolamperti%2C+A">A. Bolamperti</a>, <a href="/search/astro-ph?searchtype=author&query=Mestric%2C+U">U. Mestric</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">R. Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Gronke%2C+M">M. Gronke</a>, <a href="/search/astro-ph?searchtype=author&query=Willott%2C+C">C. Willott</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Acebron%2C+A">A. Acebron</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="2407.20327v1-abstract-short" style="display: inline;"> We report the serendipitous discovery of a faint (M_UV > -12.2), low-metallicity (Z ~ 0.02 Zsun), ionizing source (dubbed T2c) with a spectroscopic redshift of z=6.146. T2c is part of a larger structure amplified by the Hubble Frontier Field galaxy cluster MACSJ0416, and was observed with JWST/NIRSpec IFU. Stacking the short-wavelength NIRCam data reveals no stellar continuum detection down to a m… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.20327v1-abstract-full').style.display = 'inline'; document.getElementById('2407.20327v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.20327v1-abstract-full" style="display: none;"> We report the serendipitous discovery of a faint (M_UV > -12.2), low-metallicity (Z ~ 0.02 Zsun), ionizing source (dubbed T2c) with a spectroscopic redshift of z=6.146. T2c is part of a larger structure amplified by the Hubble Frontier Field galaxy cluster MACSJ0416, and was observed with JWST/NIRSpec IFU. Stacking the short-wavelength NIRCam data reveals no stellar continuum detection down to a magnitude limit of m_UV ~ 31.0 (3 sigma). However, prominent Hb, [OIII]4959,5007, and Ha emissions are detected, with equivalent widths exceeding 200A, 800A, and 1300A (3 sigma), respectively. The corresponding intrinsic (magnification-corrected x23 +/- 3) ultraviolet and optical rest-frame magnitudes exceed 34.4 and 33.9 (corresponding to M_uv and M_opt fainter than -12.2 and -12.8, at lambda_rest ~ 2000A and ~5000A, respectively), suggesting a stellar mass lower than a few 10^4 Msun under an instantaneous burst scenario. The inferred ionizing photon production efficiency (xi_ion) is high, xi_ion >~ 26.08(25.86) 3(5)sigma, assuming no dust attenuation and no Lyman continuum leakage, indicating the presence of massive stars despite the low mass of the object. The very poor sampling of the initial mass function at such low mass star-forming complex suggests that the formation of very massive stars might be favored in very low metallicity environments. T2c is surrounded by Balmer and weak oxygen emission on a spatial scale of a few hundred parsecs after correcting for lensing effects. This system resembles an HII region potentially powered by currently undetected, extremely efficient, low-metallicity star complexes or clusters. We propose that massive O-type stars populate this low-mass and metallicity high-redshift satellites, likely caught in an early and short formation phase, contributing to the ionization of the surrounding medium. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.20327v1-abstract-full').style.display = 'none'; document.getElementById('2407.20327v1-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 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">9 pages, 5 figures, 1 table. Submitted to A&A. Comments are welcome</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 691, A251 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.07940">arXiv:2407.07940</a> <span> [<a href="https://arxiv.org/pdf/2407.07940">pdf</a>, <a href="https://arxiv.org/format/2407.07940">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202451425">10.1051/0004-6361/202451425 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Euclid preparation. LI. Forecasting the recovery of galaxy physical properties and their relations with template-fitting and machine-learning methods </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Enia%2C+A">A. Enia</a>, <a href="/search/astro-ph?searchtype=author&query=Bolzonella%2C+M">M. Bolzonella</a>, <a href="/search/astro-ph?searchtype=author&query=Pozzetti%2C+L">L. Pozzetti</a>, <a href="/search/astro-ph?searchtype=author&query=Humphrey%2C+A">A. Humphrey</a>, <a href="/search/astro-ph?searchtype=author&query=Cunha%2C+P+A+C">P. A. C. Cunha</a>, <a href="/search/astro-ph?searchtype=author&query=Hartley%2C+W+G">W. G. Hartley</a>, <a href="/search/astro-ph?searchtype=author&query=Dubath%2C+F">F. Dubath</a>, <a href="/search/astro-ph?searchtype=author&query=Paltani%2C+S">S. Paltani</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+X+L">X. Lopez Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Quai%2C+S">S. Quai</a>, <a href="/search/astro-ph?searchtype=author&query=Bardelli%2C+S">S. Bardelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bisigello%2C+L">L. Bisigello</a>, <a href="/search/astro-ph?searchtype=author&query=Cavuoti%2C+S">S. Cavuoti</a>, <a href="/search/astro-ph?searchtype=author&query=De+Lucia%2C+G">G. De Lucia</a>, <a href="/search/astro-ph?searchtype=author&query=Ginolfi%2C+M">M. Ginolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Grazian%2C+A">A. Grazian</a>, <a href="/search/astro-ph?searchtype=author&query=Siudek%2C+M">M. Siudek</a>, <a href="/search/astro-ph?searchtype=author&query=Tortora%2C+C">C. Tortora</a>, <a href="/search/astro-ph?searchtype=author&query=Zamorani%2C+G">G. Zamorani</a>, <a href="/search/astro-ph?searchtype=author&query=Aghanim%2C+N">N. Aghanim</a>, <a href="/search/astro-ph?searchtype=author&query=Altieri%2C+B">B. Altieri</a>, <a href="/search/astro-ph?searchtype=author&query=Amara%2C+A">A. Amara</a>, <a href="/search/astro-ph?searchtype=author&query=Andreon%2C+S">S. Andreon</a>, <a href="/search/astro-ph?searchtype=author&query=Auricchio%2C+N">N. Auricchio</a> , et al. (238 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="2407.07940v3-abstract-short" style="display: inline;"> Euclid will collect an enormous amount of data during the mission's lifetime, observing billions of galaxies in the extragalactic sky. Along with traditional template-fitting methods, numerous machine learning algorithms have been presented for computing their photometric redshifts and physical parameters (PPs), requiring significantly less computing effort while producing equivalent performance m… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.07940v3-abstract-full').style.display = 'inline'; document.getElementById('2407.07940v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.07940v3-abstract-full" style="display: none;"> Euclid will collect an enormous amount of data during the mission's lifetime, observing billions of galaxies in the extragalactic sky. Along with traditional template-fitting methods, numerous machine learning algorithms have been presented for computing their photometric redshifts and physical parameters (PPs), requiring significantly less computing effort while producing equivalent performance measures. However, their performance is limited by the quality and amount of input information, to the point where the recovery of some well-established physical relationships between parameters might not be guaranteed. To forecast the reliability of Euclid photo-$z$s and PPs calculations, we produced two mock catalogs simulating Euclid photometry. We simulated the Euclid Wide Survey (EWS) and Euclid Deep Fields (EDF). We tested the performance of a template-fitting algorithm (Phosphoros) and four ML methods in recovering photo-$z$s, PPs (stellar masses and star formation rates), and the SFMS. To mimic the Euclid processing as closely as possible, the models were trained with Phosphoros-recovered labels. For the EWS, we found that the best results are achieved with a mixed labels approach, training the models with wide survey features and labels from the Phosphoros results on deeper photometry, that is, with the best possible set of labels for a given photometry. This imposes a prior, helping the models to better discern cases in degenerate regions of feature space, that is, when galaxies have similar magnitudes and colors but different redshifts and PPs, with performance metrics even better than those found with Phosphoros. We found no more than 3% performance degradation using a COSMOS-like reference sample or removing u band data, which will not be available until after data release DR1. The best results are obtained for the EDF, with appropriate recovery of photo-$z$, PPs, and the SFMS. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.07940v3-abstract-full').style.display = 'none'; document.getElementById('2407.07940v3-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 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 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">26 pages, 13 figures. Accepted for publication on A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 691, A175 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.13504">arXiv:2405.13504</a> <span> [<a href="https://arxiv.org/pdf/2405.13504">pdf</a>, <a href="https://arxiv.org/format/2405.13504">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"> Euclid: Early Release Observations -- A preview of the Euclid era through a galaxy cluster magnifying lens </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Atek%2C+H">H. Atek</a>, <a href="/search/astro-ph?searchtype=author&query=Gavazzi%2C+R">R. Gavazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Weaver%2C+J+R">J. R. Weaver</a>, <a href="/search/astro-ph?searchtype=author&query=Diego%2C+J+M">J. M. Diego</a>, <a href="/search/astro-ph?searchtype=author&query=Schrabback%2C+T">T. Schrabback</a>, <a href="/search/astro-ph?searchtype=author&query=Hatch%2C+N+A">N. A. Hatch</a>, <a href="/search/astro-ph?searchtype=author&query=Aghanim%2C+N">N. Aghanim</a>, <a href="/search/astro-ph?searchtype=author&query=Dole%2C+H">H. Dole</a>, <a href="/search/astro-ph?searchtype=author&query=Hartley%2C+W+G">W. G. Hartley</a>, <a href="/search/astro-ph?searchtype=author&query=Taamoli%2C+S">S. Taamoli</a>, <a href="/search/astro-ph?searchtype=author&query=Congedo%2C+G">G. Congedo</a>, <a href="/search/astro-ph?searchtype=author&query=Jimenez-Teja%2C+Y">Y. Jimenez-Teja</a>, <a href="/search/astro-ph?searchtype=author&query=Cuillandre%2C+J+-">J. -C. Cuillandre</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=Belladitta%2C+S">S. Belladitta</a>, <a href="/search/astro-ph?searchtype=author&query=Bowler%2C+R+A+A">R. A. A. Bowler</a>, <a href="/search/astro-ph?searchtype=author&query=Franco%2C+M">M. Franco</a>, <a href="/search/astro-ph?searchtype=author&query=Jauzac%2C+M">M. Jauzac</a>, <a href="/search/astro-ph?searchtype=author&query=Mahler%2C+G">G. Mahler</a>, <a href="/search/astro-ph?searchtype=author&query=Richard%2C+J">J. Richard</a>, <a href="/search/astro-ph?searchtype=author&query=Rocci%2C+P+-">P. -F. Rocci</a>, <a href="/search/astro-ph?searchtype=author&query=Serjeant%2C+S">S. Serjeant</a>, <a href="/search/astro-ph?searchtype=author&query=Toft%2C+S">S. Toft</a>, <a href="/search/astro-ph?searchtype=author&query=Abriola%2C+D">D. Abriola</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">P. Bergamini</a> , et al. (178 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="2405.13504v1-abstract-short" style="display: inline;"> We present the first analysis of the Euclid Early Release Observations (ERO) program that targets fields around two lensing clusters, Abell 2390 and Abell 2764. We use VIS and NISP imaging to produce photometric catalogs for a total of $\sim 500\,000$ objects. The imaging data reach a $5\,蟽$ typical depth in the range 25.1-25.4 AB in the NISP bands, and 27.1-27.3 AB in the VIS band. Using the Lyma… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13504v1-abstract-full').style.display = 'inline'; document.getElementById('2405.13504v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.13504v1-abstract-full" style="display: none;"> We present the first analysis of the Euclid Early Release Observations (ERO) program that targets fields around two lensing clusters, Abell 2390 and Abell 2764. We use VIS and NISP imaging to produce photometric catalogs for a total of $\sim 500\,000$ objects. The imaging data reach a $5\,蟽$ typical depth in the range 25.1-25.4 AB in the NISP bands, and 27.1-27.3 AB in the VIS band. Using the Lyman-break method in combination with photometric redshifts, we identify $30$ Lyman-break galaxy (LBG) candidates at $z>6$ and 139 extremely red sources (ERSs), most likely at lower redshift. The deeper VIS imaging compared to NISP means we can routinely identify high-redshift Lyman breaks of the order of $3$ magnitudes, which reduces contamination by brown dwarf stars and low-redshift galaxies. Spectroscopic follow-up campaigns of such bright sources will help constrain both the bright end of the ultraviolet galaxy luminosity function and the quasar luminosity function at $z>6$, and constrain the physical nature of these objects. Additionally, we have performed a combined strong lensing and weak lensing analysis of A2390, and demonstrate how Euclid will contribute to better constraining the virial mass of galaxy clusters. From these data, we also identify optical and near-infrared counterparts of known $z>0.6$ clusters, which exhibit strong lensing features, establishing the ability of Euclid to characterize high-redshift clusters. Finally, we provide a glimpse of Euclid's ability to map the intracluster light out to larger radii than current facilities, enabling a better understanding of the cluster assembly history and mapping of the dark matter distribution. This initial dataset illustrates the diverse spectrum of legacy science that will be enabled by the Euclid survey. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13504v1-abstract-full').style.display = 'none'; document.getElementById('2405.13504v1-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 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">Paper submitted as part of the A&A special issue `Euclid on Sky', which contains Euclid key reference papers and first results from the Euclid Early Release Observations. 17 pages, 12 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.13491">arXiv:2405.13491</a> <span> [<a href="https://arxiv.org/pdf/2405.13491">pdf</a>, <a href="https://arxiv.org/format/2405.13491">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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="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"> Euclid. I. Overview of the Euclid mission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Mellier%2C+Y">Y. Mellier</a>, <a href="/search/astro-ph?searchtype=author&query=Abdurro%27uf"> Abdurro'uf</a>, <a href="/search/astro-ph?searchtype=author&query=Barroso%2C+J+A+A">J. A. Acevedo Barroso</a>, <a href="/search/astro-ph?searchtype=author&query=Ach%C3%BAcarro%2C+A">A. Ach煤carro</a>, <a href="/search/astro-ph?searchtype=author&query=Adamek%2C+J">J. Adamek</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+R">R. Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Addison%2C+G+E">G. E. Addison</a>, <a href="/search/astro-ph?searchtype=author&query=Aghanim%2C+N">N. Aghanim</a>, <a href="/search/astro-ph?searchtype=author&query=Aguena%2C+M">M. Aguena</a>, <a href="/search/astro-ph?searchtype=author&query=Ajani%2C+V">V. Ajani</a>, <a href="/search/astro-ph?searchtype=author&query=Akrami%2C+Y">Y. Akrami</a>, <a href="/search/astro-ph?searchtype=author&query=Al-Bahlawan%2C+A">A. Al-Bahlawan</a>, <a href="/search/astro-ph?searchtype=author&query=Alavi%2C+A">A. Alavi</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I+S">I. S. Albuquerque</a>, <a href="/search/astro-ph?searchtype=author&query=Alestas%2C+G">G. Alestas</a>, <a href="/search/astro-ph?searchtype=author&query=Alguero%2C+G">G. Alguero</a>, <a href="/search/astro-ph?searchtype=author&query=Allaoui%2C+A">A. Allaoui</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+S+W">S. W. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Allevato%2C+V">V. Allevato</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso-Tetilla%2C+A+V">A. V. Alonso-Tetilla</a>, <a href="/search/astro-ph?searchtype=author&query=Altieri%2C+B">B. Altieri</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Candal%2C+A">A. Alvarez-Candal</a>, <a href="/search/astro-ph?searchtype=author&query=Alvi%2C+S">S. Alvi</a>, <a href="/search/astro-ph?searchtype=author&query=Amara%2C+A">A. Amara</a> , et al. (1115 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="2405.13491v2-abstract-short" style="display: inline;"> The current standard model of cosmology successfully describes a variety of measurements, but the nature of its main ingredients, dark matter and dark energy, remains unknown. Euclid is a medium-class mission in the Cosmic Vision 2015-2025 programme of the European Space Agency (ESA) that will provide high-resolution optical imaging, as well as near-infrared imaging and spectroscopy, over about 14… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13491v2-abstract-full').style.display = 'inline'; document.getElementById('2405.13491v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.13491v2-abstract-full" style="display: none;"> The current standard model of cosmology successfully describes a variety of measurements, but the nature of its main ingredients, dark matter and dark energy, remains unknown. Euclid is a medium-class mission in the Cosmic Vision 2015-2025 programme of the European Space Agency (ESA) that will provide high-resolution optical imaging, as well as near-infrared imaging and spectroscopy, over about 14,000 deg^2 of extragalactic sky. In addition to accurate weak lensing and clustering measurements that probe structure formation over half of the age of the Universe, its primary probes for cosmology, these exquisite data will enable a wide range of science. This paper provides a high-level overview of the mission, summarising the survey characteristics, the various data-processing steps, and data products. We also highlight the main science objectives and expected performance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13491v2-abstract-full').style.display = 'none'; document.getElementById('2405.13491v2-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 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in the A&A special issue`Euclid on Sky'</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.12287">arXiv:2405.12287</a> <span> [<a href="https://arxiv.org/pdf/2405.12287">pdf</a>, <a href="https://arxiv.org/format/2405.12287">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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/10.1051/0004-6361/202449528">10.1051/0004-6361/202449528 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Improved model of the Supernova Refsdal cluster MACS J1149.5+2223 thanks to VLT/MUSE </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Schuldt%2C+S">S. Schuldt</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Caminha%2C+G+B">G. B. Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">A. Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Morishita%2C+T">T. Morishita</a>, <a href="/search/astro-ph?searchtype=author&query=Stiavelli%2C+M">M. Stiavelli</a>, <a href="/search/astro-ph?searchtype=author&query=Suyu%2C+S+H">S. H. Suyu</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">P. Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Brescia%2C+M">M. Brescia</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">F. Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">M. Meneghetti</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.12287v2-abstract-short" style="display: inline;"> We present new VLT/MUSE observations of the Hubble Frontier Field (HFF) galaxy cluster MACS J1149.5+2223, lensing the well-known supernova "Refsdal" into multiple images, which enabled the first cosmological applications with a strongly lensed supernova. Thanks to these data, targeting a northern region of the cluster and thus complementing our previous MUSE program on the cluster core, we release… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.12287v2-abstract-full').style.display = 'inline'; document.getElementById('2405.12287v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.12287v2-abstract-full" style="display: none;"> We present new VLT/MUSE observations of the Hubble Frontier Field (HFF) galaxy cluster MACS J1149.5+2223, lensing the well-known supernova "Refsdal" into multiple images, which enabled the first cosmological applications with a strongly lensed supernova. Thanks to these data, targeting a northern region of the cluster and thus complementing our previous MUSE program on the cluster core, we release a new catalog containing 162 secure spectroscopic redshifts. We confirm 22 cluster members, which were previously only photometrically selected, and detect ten additional ones, resulting in a total of 308 secure members, of which 63% are spectroscopically confirmed. We further identify 17 new spectroscopic multiple images belonging to 6 different background sources. By exploiting MUSE data, in combination with the deep HFF images, we develop an improved total mass model of MACS J1149.5+2223. This model includes 308 total mass components for the member galaxies and requires four additional mass profiles, one of which is associated with a cluster galaxy overdensity identified in the North, representing the DM mass distribution on larger scales. The values of the resulting 34 free parameters are optimized based on the observed positions of 106 multiple images from 34 different families, that cover the redshift range between 1.240 and 5.983. Our final model has a multiple image position rms value of 0.39", which is well in agreement with that of other cluster lens models. With this refined mass model, we pave the way towards even better strong-lensing analyses that will exploit the deep and high resolution observations with HST and JWST on a pixel level in the region of the supernova Refsdal host. This will increase the number of observables by around two orders of magnitudes, thus offering us the opportunity of carrying out more precise and accurate cosmographic measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.12287v2-abstract-full').style.display = 'none'; document.getElementById('2405.12287v2-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 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 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">14 pages, 7 figures, 4+1 tables, published with A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.10491">arXiv:2403.10491</a> <span> [<a href="https://arxiv.org/pdf/2403.10491">pdf</a>, <a href="https://arxiv.org/format/2403.10491">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1038/s41550-024-02397-3">10.1038/s41550-024-02397-3 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A luminous and young galaxy at z=12.33 revealed by a JWST/MIRI detection of H伪 and [OIII] </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zavala%2C+J+A">Jorge A. Zavala</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">Marco Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Akins%2C+H+B">Hollis B. Akins</a>, <a href="/search/astro-ph?searchtype=author&query=Bakx%2C+T+J+L+C">Tom J. L. C. Bakx</a>, <a href="/search/astro-ph?searchtype=author&query=Burgarella%2C+D">Denis Burgarella</a>, <a href="/search/astro-ph?searchtype=author&query=Casey%2C+C+M">Caitlin M. Casey</a>, <a href="/search/astro-ph?searchtype=author&query=Ortiz%2C+%C3%93+A+C">脫scar A. Ch谩vez Ortiz</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Mitsuhashi%2C+I">Ikki Mitsuhashi</a>, <a href="/search/astro-ph?searchtype=author&query=Nakajima%2C+K">Kimihiko Nakajima</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Gonz%C3%A1lez%2C+P+G">Pablo G. P茅rez-Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Haro%2C+P+A">Pablo Arrabal Haro</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">Pietro Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Buat%2C+V">Veronique Buat</a>, <a href="/search/astro-ph?searchtype=author&query=Backhaus%2C+B">Bren Backhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Calabr%C3%B2%2C+A">Antonello Calabr貌</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N+J">Nikko J. Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Arenas%2C+D">David Fern谩ndez-Arenas</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">Adriano Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Franco%2C+M">Maximilien Franco</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">Claudio Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Giavalisco%2C+M">Mauro Giavalisco</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">Norman A. Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N">Nimish Hathi</a> , et al. (15 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.10491v2-abstract-short" style="display: inline;"> The James Webb Space Telescope (JWST) has discovered a surprising population of bright galaxies in the very early universe (<500 Myrs after the Big Bang) that is hard to explain with conventional galaxy formation models and whose physical properties remain to be fully understood. Insight into their internal physics is best captured through nebular lines but, at these early epochs, the brightest of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.10491v2-abstract-full').style.display = 'inline'; document.getElementById('2403.10491v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.10491v2-abstract-full" style="display: none;"> The James Webb Space Telescope (JWST) has discovered a surprising population of bright galaxies in the very early universe (<500 Myrs after the Big Bang) that is hard to explain with conventional galaxy formation models and whose physical properties remain to be fully understood. Insight into their internal physics is best captured through nebular lines but, at these early epochs, the brightest of these spectral features are redshifted into the mid-infrared and remain elusive. Using the JWST Mid-Infrared Instrument, MIRI, here we present the first detection of H伪 and doubly-ionized oxygen ([OIII]5007AA) at z>10. These detections place the bright galaxy GHZ2/GLASS-z12 at z=12.33+/-0.04, making it the most distant astronomical object with direct spectroscopic detection of these lines. These observations provide key insights into the conditions of this primeval, luminous galaxy, which shows hard ionizing conditions rarely seen in the local Universe likely driven by compact and young (~30Myr) burst of star formation. Its oxygen-to-hydrogen abundance is close to a tenth of the solar value, indicating a rapid metal enrichment. This study confirms the unique conditions of this remarkably bright and distant galaxy and the huge potential of mid-IR observations to characterize these objects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.10491v2-abstract-full').style.display = 'none'; document.getElementById('2403.10491v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published in Nature Astronomy on 30 October 2024 (this represents the authors' submitted version)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.10238">arXiv:2403.10238</a> <span> [<a href="https://arxiv.org/pdf/2403.10238">pdf</a>, <a href="https://arxiv.org/format/2403.10238">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"> JWST NIRSpec Spectroscopy of the Remarkable Bright Galaxy GHZ2/GLASS-z12 at Redshift 12.34 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">Marco Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+L">Lorenzo Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">Adriano Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Roberts-Borsani%2C+G">Guido Roberts-Borsani</a>, <a href="/search/astro-ph?searchtype=author&query=Treu%2C+T">Tommaso Treu</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">Eros Vanzella</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=Haro%2C+P+A">Pablo Arrabal Haro</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=Llerena%2C+M">Mario Llerena</a>, <a href="/search/astro-ph?searchtype=author&query=Mascia%2C+S">Sara Mascia</a>, <a href="/search/astro-ph?searchtype=author&query=Merlin%2C+E">Emiliano Merlin</a>, <a href="/search/astro-ph?searchtype=author&query=Paris%2C+D">Diego Paris</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">Laura Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Santini%2C+P">Paola Santini</a>, <a href="/search/astro-ph?searchtype=author&query=Bakx%2C+T+J+L+C">Tom J. L. C. Bakx</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">Pietro Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Cupani%2C+G">Guido Cupani</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Filippenko%2C+A+V">Alexei V. Filippenko</a>, <a href="/search/astro-ph?searchtype=author&query=Glazebrook%2C+K">Karl Glazebrook</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">Claudio Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Kelly%2C+P+L">Patrick L. Kelly</a>, <a href="/search/astro-ph?searchtype=author&query=Malkan%2C+M+A">Matthew A. Malkan</a>, <a href="/search/astro-ph?searchtype=author&query=Mason%2C+C+A">Charlotte A. Mason</a> , et al. (6 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.10238v2-abstract-short" style="display: inline;"> We spectroscopically confirm the $M_{\rm UV} = -20.5$ mag galaxy GHZ2/GLASS-z12 to be at redshift $z=12.34$. The source was selected via NIRCam photometry in GLASS-JWST ERS data, providing the first evidence of a surprising abundance of bright galaxies at $z \gtrsim 10$. The NIRSpec PRISM spectrum shows detections of N IV, C IV, He II, O III, C III, O II, and Ne III lines, and the first detection… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.10238v2-abstract-full').style.display = 'inline'; document.getElementById('2403.10238v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.10238v2-abstract-full" style="display: none;"> We spectroscopically confirm the $M_{\rm UV} = -20.5$ mag galaxy GHZ2/GLASS-z12 to be at redshift $z=12.34$. The source was selected via NIRCam photometry in GLASS-JWST ERS data, providing the first evidence of a surprising abundance of bright galaxies at $z \gtrsim 10$. The NIRSpec PRISM spectrum shows detections of N IV, C IV, He II, O III, C III, O II, and Ne III lines, and the first detection at high-redshift of the O III Bowen fluorescence line at 3133 脜 rest-frame. The prominent C IV line with rest-frame equivalent width (EW) $\approx 46$ 脜 puts GHZ2 in the category of extreme C IV emitters. GHZ2 displays UV lines with EWs that are only found in active galactic nuclei (AGNs) or composite objects at low/intermediate redshifts. The UV line-intensity ratios are compatible both with AGNs and star formation in a low-metallicity environment, with the low limit on the [Ne IV]/[N IV] ratio favoring a stellar origin of the ionizing photons. We discuss a possible scenario in which the high ionizing output is due to low metallicity stars forming in a dense environment. We estimate a metallicity $\lesssim 0.1 Z/{\rm Z}_{\odot}$, a high ionization parameter logU $> -2$, a N/O abundance 4--5 times the solar value, and a subsolar C/O ratio similar to the recently discovered class of nitrogen-enhanced objects. Considering its abundance patterns and the high stellar mass density ($10^4$~M$_{\odot}$~pc$^{-2}$), GHZ2 is an ideal formation site for the progenitors of today's globular clusters. The remarkable brightness of GHZ2 makes it a ``Rosetta stone'' for understanding the physics of galaxy formation within just 360 Myr after the Big Bang. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.10238v2-abstract-full').style.display = 'none'; document.getElementById('2403.10238v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in The Astrophysical Journal. 20 pages, 7 figures, 2 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.07103">arXiv:2403.07103</a> <span> [<a href="https://arxiv.org/pdf/2403.07103">pdf</a>, <a href="https://arxiv.org/format/2403.07103">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"> Between the Extremes: A JWST Spectroscopic Benchmark for High Redshift Galaxies Using ~500 Confirmed Sources at $z\geqslant5$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Roberts-Borsani%2C+G">Guido Roberts-Borsani</a>, <a href="/search/astro-ph?searchtype=author&query=Treu%2C+T">Tommaso Treu</a>, <a href="/search/astro-ph?searchtype=author&query=Shapley%2C+A">Alice Shapley</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">Adriano Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">Laura Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">Marco Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Morishita%2C+T">Takahiro Morishita</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">Pietro Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">Piero Rosati</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.07103v1-abstract-short" style="display: inline;"> The exceptional spectra of the most luminous $z>10$ sources observed so far have challenged our understanding of early galaxy evolution, requiring a new observational benchmark for meaningful interpretation. As such, we construct spectroscopic templates representative of high-redshift, star-forming populations, using 482 confirmed sources at $z=5.0-12.9$ with JWST/NIRSpec prism observations, and r… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.07103v1-abstract-full').style.display = 'inline'; document.getElementById('2403.07103v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.07103v1-abstract-full" style="display: none;"> The exceptional spectra of the most luminous $z>10$ sources observed so far have challenged our understanding of early galaxy evolution, requiring a new observational benchmark for meaningful interpretation. As such, we construct spectroscopic templates representative of high-redshift, star-forming populations, using 482 confirmed sources at $z=5.0-12.9$ with JWST/NIRSpec prism observations, and report on their average properties. We find $z=5-11$ galaxies are dominated by blue UV continuum slopes ($尾=-2.3$ to $-2.7$) and inverse Balmer jumps, characteristic of dust-poor and young systems, with a shift towards bluer slopes and younger ages with redshift. The evolution is mirrored by ubiquitous CIII] detections across all redshifts (EW$_{0}=5-14$ 脜), which increase in strength towards early times. Rest-frame optical lines reveal elevated ratios ($O32=7-31$, $R23=5-8$, and $Ne3O2=1-2$) and subsolar metallicities (log O/H$=7.3-7.9$), typical of ionization conditions and metallicities rarely observed in $z\sim0$ populations. Within our sample, we identify 57 Ly$伪$-emitters which we stack and compare to a matched sample of non-emitters. The former are characterized by more extreme ionizing conditions with enhanced CIII], CIV, and HeII+[OIII] line emission, younger stellar populations from inverse Balmer jumps, and a more pristine ISM seen through bluer UV slopes and elevated rest-frame optical line ratios. The novel comparison illustrates important intrinsic differences between the two populations, with implications for Ly$伪$ visibility. The spectral templates derived here represent a new observational benchmark with which to interpret high-redshift sources, lifting our constraints on their global properties to unprecedented heights and extending out to the earliest of cosmic times. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.07103v1-abstract-full').style.display = 'none'; document.getElementById('2403.07103v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to ApJ. 33 pages (24 pages for main body), 13 figures, 6 tables. All composite spectra available online or upon request. 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/2402.14084">arXiv:2402.14084</a> <span> [<a href="https://arxiv.org/pdf/2402.14084">pdf</a>, <a href="https://arxiv.org/format/2402.14084">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"> Diverse Oxygen Abundance in Early Galaxies Unveiled by Auroral Line Analysis with JWST </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Morishita%2C+T">Takahiro Morishita</a>, <a href="/search/astro-ph?searchtype=author&query=Stiavelli%2C+M">Massimo Stiavelli</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">Claudio Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">Piero Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Schuldt%2C+S">Stefan Schuldt</a>, <a href="/search/astro-ph?searchtype=author&query=Trenti%2C+M">Michele Trenti</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">Pietro Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Boyett%2C+K+N">Kristan N. Boyett</a>, <a href="/search/astro-ph?searchtype=author&query=Chary%2C+R">Ranga-Ram Chary</a>, <a href="/search/astro-ph?searchtype=author&query=Leethochawalit%2C+N">Nicha Leethochawalit</a>, <a href="/search/astro-ph?searchtype=author&query=Roberts-Borsani%2C+G">Guido Roberts-Borsani</a>, <a href="/search/astro-ph?searchtype=author&query=Treu%2C+T">Tommaso Treu</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">Eros Vanzella</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="2402.14084v3-abstract-short" style="display: inline;"> We present deep JWST NIRSpec observations in the sightline of MACS J1149.5+2223, a massive cluster of galaxies at $z=0.54$. We report the spectroscopic redshift of 28 sources at $3<z<9.1$, including 9 sources with the detection of the [OIII]4363 auroral line. Combining these with 16 [OIII]4363-detected sources from publicly available JWST data, our sample consists of 25 galaxies with robust gas-ph… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.14084v3-abstract-full').style.display = 'inline'; document.getElementById('2402.14084v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.14084v3-abstract-full" style="display: none;"> We present deep JWST NIRSpec observations in the sightline of MACS J1149.5+2223, a massive cluster of galaxies at $z=0.54$. We report the spectroscopic redshift of 28 sources at $3<z<9.1$, including 9 sources with the detection of the [OIII]4363 auroral line. Combining these with 16 [OIII]4363-detected sources from publicly available JWST data, our sample consists of 25 galaxies with robust gas-phase metallicity measurements via the direct method. We observe a positive correlation between stellar mass and metallicity, with a $\sim0.5$\,dex offset down below the local relation. Interestingly, we find a larger than expected scatter of $\sim0.3$\,dex around the relation, which cannot be explained by redshift evolution among our sample or other third parameter. The scatter increases at higher redshift, and we attribute this to the enrichment process having higher stochasticity due to shallower potential wells, more intense feedback processes, and a higher galaxy merger rate. Despite reaching to a considerably low-mass regime ($\log M_*/M_\odot \sim7.3$), our samples have metallicity of $\log$(O/H)$+12>7$, i.e. comparable to the most metal poor galaxies in the local Universe. The search of primordial galaxies may be accomplished by extending toward a lower mass and/or by investigating inhomogeneities at smaller spatial scales. Lastly, we investigate potential systematics caused by the limitation of JWST's MSA observations. Caution is warranted when the target exceeds the slit size, as this situation could allow an overestimation of "global" metallicity, especially under the presence of strong negative metallicity gradient. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.14084v3-abstract-full').style.display = 'none'; document.getElementById('2402.14084v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication on May 29, 2024 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/2402.08364">arXiv:2402.08364</a> <span> [<a href="https://arxiv.org/pdf/2402.08364">pdf</a>, <a href="https://arxiv.org/format/2402.08364">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> An improved Magellan weak lensing analysis of the galaxy cluster Abell 2744 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abriola%2C+D">Davide Abriola</a>, <a href="/search/astro-ph?searchtype=author&query=Della+Pergola%2C+D">Daniele Della Pergola</a>, <a href="/search/astro-ph?searchtype=author&query=Lombardi%2C+M">Marco Lombardi</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">Pietro Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">Mario Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">Claudio Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">Piero Rosati</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="2402.08364v1-abstract-short" style="display: inline;"> We present a new weak lensing analysis of the Hubble Frontier Fields galaxy cluster Abell 2744 ($z$ = 0.308) using new Magellan/MegaCam multi-band $gri$ imaging data. We carry out our study by applying brand-new PSF and shape measurement softwares that allow for the use of multi-band data simultaneously, which we first test on Subaru/Suprime-Cam $BR_cz'$ imaging data of the same cluster. The proje… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.08364v1-abstract-full').style.display = 'inline'; document.getElementById('2402.08364v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.08364v1-abstract-full" style="display: none;"> We present a new weak lensing analysis of the Hubble Frontier Fields galaxy cluster Abell 2744 ($z$ = 0.308) using new Magellan/MegaCam multi-band $gri$ imaging data. We carry out our study by applying brand-new PSF and shape measurement softwares that allow for the use of multi-band data simultaneously, which we first test on Subaru/Suprime-Cam $BR_cz'$ imaging data of the same cluster. The projected total mass of this system within $2.35 \, \mathrm{Mpc}$ from the south-west BCG is $(2.56 \pm 0.26) \times 10^{15} \, \mathrm{M}_\odot$, which makes Abell 2744 one of the most massive clusters known. This value is consistent, within the errors, with previous weak lensing and dynamical studies. Our analysis reveals the presence of three high-density substructures, thus supporting the picture of a complex merging scenario. This result is also confirmed by a comparison with a recent strong lensing study based on high-resolution JWST imaging. Moreover, our reconstructed total mass profile nicely agrees with an extrapolation of the strong lensing best-fit model up to several Mpc from the BCG centre. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.08364v1-abstract-full').style.display = 'none'; document.getElementById('2402.08364v1-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> 13 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.16473">arXiv:2401.16473</a> <span> [<a href="https://arxiv.org/pdf/2401.16473">pdf</a>, <a href="https://arxiv.org/format/2401.16473">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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/10.1051/0004-6361/202349060">10.1051/0004-6361/202349060 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The powerful lens galaxy cluster PLCK G287.0+32.9 ($胃_E \sim 43''$) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=D%27Addona%2C+M">Maurizio D'Addona</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">Amata Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">Piero Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">Claudio Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Caminha%2C+G">Gabriel Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Acebron%2C+A">Ana Acebron</a>, <a href="/search/astro-ph?searchtype=author&query=Angora%2C+G">Giuseppe Angora</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">Pietro Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Bozza%2C+V">Valerio Bozza</a>, <a href="/search/astro-ph?searchtype=author&query=Granata%2C+G">Giovanni Granata</a>, <a href="/search/astro-ph?searchtype=author&query=Annunziatella%2C+M">Marianna Annunziatella</a>, <a href="/search/astro-ph?searchtype=author&query=Gargiulo%2C+A">Adriana Gargiulo</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">Raphael Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Tozzi%2C+P">Paolo Tozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Girardi%2C+M">Marisa Girardi</a>, <a href="/search/astro-ph?searchtype=author&query=Lombardi%2C+M">Marco Lombardi</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">Massimo Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Schipani%2C+P">Pietro Schipani</a>, <a href="/search/astro-ph?searchtype=author&query=Tortorelli%2C+L">Luca Tortorelli</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">Eros Vanzella</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="2401.16473v2-abstract-short" style="display: inline;"> We present a new high-precision strong lensing model of PLCK G287.0$+$32.9, a massive lens galaxy cluster at $z=0.383$, with the aim to get an accurate estimation of its effective Einstein radius and total mass distribution. We also present a spectroscopic catalog containing accurate redshift measurements for 490 objects, including multiply-lensed sources and cluster member galaxies. We exploit hi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.16473v2-abstract-full').style.display = 'inline'; document.getElementById('2401.16473v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.16473v2-abstract-full" style="display: none;"> We present a new high-precision strong lensing model of PLCK G287.0$+$32.9, a massive lens galaxy cluster at $z=0.383$, with the aim to get an accurate estimation of its effective Einstein radius and total mass distribution. We also present a spectroscopic catalog containing accurate redshift measurements for 490 objects, including multiply-lensed sources and cluster member galaxies. We exploit high-quality spectroscopic data from three pointings of the VLT Multi Unit Spectroscopic Explorer, covering a central $3~\rm{arcmin}^2$ region of the cluster. We complete the spectroscopic catalog by including redshift measurements from VLT-VIMOS and KECK-DEIMOS. We identify 129 spectroscopic cluster member galaxies, with redshift values $0.360 \leq z \leq 0.405$ and $m_{\rm{F160W}} \leq 21$, and 24 photometric ones identified with a Convolutional Neural Network from ancillary HST imaging. We also identify 114 multiple images from 28 background sources, of which 84 images from 16 sources are new and the remaining ones were identified in previous work. The best-fitting lens model shows a root mean square separation value between the predicted and observed positions of the multiple images of $0.75''$, corresponding to an improvement in reconstructing the observed positions of the multiple images of a factor of $2.5$ with respect to previous models. Using the predictive power of our new lens model we find 3 new multiple images and we confirm the configuration of three systems of multiple images that were not used for the optimization of the model. The derived total mass distribution confirms this cluster to be a very prominent gravitational lens with an effective Einstein $胃_{E} = 43.4'' \pm 0.1''$, that is in agreement with previous estimates and corresponds to a total mass enclosed in the critical curve of $M_E = {3.33}_{-0.07}^{+0.02} \times{ 10^{14} M_\odot}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.16473v2-abstract-full').style.display = 'none'; document.getElementById('2401.16473v2-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 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 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">submitted to "Astronomy & Astrophysics" and accepted the on January 29th 2024</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A Volume 686, June 2024, A4 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.04767">arXiv:2401.04767</a> <span> [<a href="https://arxiv.org/pdf/2401.04767">pdf</a>, <a href="https://arxiv.org/format/2401.04767">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Augmenting the power of time-delay cosmography in lens galaxy clusters by probing their member galaxies. II. Cosmic chronometers </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">P. Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Schuldt%2C+S">S. Schuldt</a>, <a href="/search/astro-ph?searchtype=author&query=Acebron%2C+A">A. Acebron</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Mestric%2C+U">U. Mestric</a>, <a href="/search/astro-ph?searchtype=author&query=Granata%2C+G">G. Granata</a>, <a href="/search/astro-ph?searchtype=author&query=Caminha%2C+G+B">G. B. Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">M. Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">A. Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Suyu%2C+S+H">S. H. Suyu</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</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="2401.04767v1-abstract-short" style="display: inline;"> We present a novel approach to measuring the expansion rate and the geometry of the Universe, which combine time-delay cosmography in lens galaxy clusters with pure samples of 'cosmic chronometers' (CCs) by probing the member galaxies. The former makes use of the measured time delays between the multiple images of time-varying sources strongly lensed by galaxy clusters, while the latter exploits t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.04767v1-abstract-full').style.display = 'inline'; document.getElementById('2401.04767v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.04767v1-abstract-full" style="display: none;"> We present a novel approach to measuring the expansion rate and the geometry of the Universe, which combine time-delay cosmography in lens galaxy clusters with pure samples of 'cosmic chronometers' (CCs) by probing the member galaxies. The former makes use of the measured time delays between the multiple images of time-varying sources strongly lensed by galaxy clusters, while the latter exploits the most massive and passive cluster member galaxies to measure the differential time evolution of the Universe. We applied two different statistical techniques, adopting realistic errors on the measured quantities, to assess the accuracy and the gain in precision on the values of the cosmological parameters. We demonstrate that the proposed combined method allows for a robust and accurate measurement of the value of the Hubble constant. In addition, this provides valuable information on the other cosmological parameters thanks to the complementarity between the two different probes in breaking parameter degeneracies. Finally, we showcase the immediate observational feasibility of the proposed joint method by taking advantage of the existing high-quality spectro-photometric data for several lens galaxy clusters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.04767v1-abstract-full').style.display = 'none'; document.getElementById('2401.04767v1-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 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">6 pages, 2 figures. Accepted for publication in A&A Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.03440">arXiv:2311.03440</a> <span> [<a href="https://arxiv.org/pdf/2311.03440">pdf</a>, <a href="https://arxiv.org/format/2311.03440">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Augmenting the power of time-delay cosmography in lens galaxy clusters by probing their member galaxies I. Type Ia supernovae </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Acebron%2C+A">A. Acebron</a>, <a href="/search/astro-ph?searchtype=author&query=Schuldt%2C+S">S. Schuldt</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">P. Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Granata%2C+G">G. Granata</a>, <a href="/search/astro-ph?searchtype=author&query=Mestric%2C+U">U. Mestric</a>, <a href="/search/astro-ph?searchtype=author&query=Caminha%2C+G+B">G. B. Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">M. Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">A. Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Suyu%2C+S+H">S. H. Suyu</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.03440v2-abstract-short" style="display: inline;"> We present a simple and promising new method to measure the expansion rate and the geometry of the universe that combines observations related to the time delays between the multiple images of time-varying sources, strongly lensed by galaxy clusters, and Type Ia supernovae, exploding in galaxies belonging to the same lens clusters. By means of two different statistical techniques that adopt realis… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.03440v2-abstract-full').style.display = 'inline'; document.getElementById('2311.03440v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.03440v2-abstract-full" style="display: none;"> We present a simple and promising new method to measure the expansion rate and the geometry of the universe that combines observations related to the time delays between the multiple images of time-varying sources, strongly lensed by galaxy clusters, and Type Ia supernovae, exploding in galaxies belonging to the same lens clusters. By means of two different statistical techniques that adopt realistic errors on the relevant quantities, we quantify the accuracy of the inferred cosmological parameter values. We show that the estimate of the Hubble constant is robust and competitive, and depends only mildly on the chosen cosmological model. Remarkably, the two probes separately produce confidence regions on the cosmological parameter planes that are oriented in complementary ways, thus providing in combination valuable information on the values of the other cosmological parameters. We conclude by illustrating the immediate observational feasibility of the proposed joint method in a well-studied lens galaxy cluster, with a relatively small investment of telescope time for monitoring from a 2 to 3m class ground-based telescope. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.03440v2-abstract-full').style.display = 'none'; document.getElementById('2311.03440v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 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">6 pages, 2 figures, 1 table. Published in A&A Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.04498">arXiv:2310.04498</a> <span> [<a href="https://arxiv.org/pdf/2310.04498">pdf</a>, <a href="https://arxiv.org/format/2310.04498">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"> UV-continuum $尾$ slopes of individual $z \sim 2-6$ clumps and their evolution </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bolamperti%2C+A">A. Bolamperti</a>, <a href="/search/astro-ph?searchtype=author&query=Zanella%2C+A">A. Zanella</a>, <a href="/search/astro-ph?searchtype=author&query=Me%C5%A1tri%C4%87%2C+U">U. Me拧tri膰</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">P. Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">F. Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">M. Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">A. Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Devereaux%2C+T">T. Devereaux</a>, <a href="/search/astro-ph?searchtype=author&query=Iani%2C+E">E. Iani</a>, <a href="/search/astro-ph?searchtype=author&query=Vernet%2C+J">J. Vernet</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.04498v1-abstract-short" style="display: inline;"> We study the ultraviolet (UV) continuum $尾$ slope of a sample of 166 clumps, individual star-forming regions observed in high redshift galaxies. They are hosted by 67 galaxies with redshift between 2 and 6.2, strongly lensed by the Hubble Frontier Fields cluster of galaxies MACS J0416.1-2403. The $尾$ slope is sensitive to a variety of physical properties, such as the metallicity, the age of the st… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.04498v1-abstract-full').style.display = 'inline'; document.getElementById('2310.04498v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.04498v1-abstract-full" style="display: none;"> We study the ultraviolet (UV) continuum $尾$ slope of a sample of 166 clumps, individual star-forming regions observed in high redshift galaxies. They are hosted by 67 galaxies with redshift between 2 and 6.2, strongly lensed by the Hubble Frontier Fields cluster of galaxies MACS J0416.1-2403. The $尾$ slope is sensitive to a variety of physical properties, such as the metallicity, the age of the stellar population, the dust attenuation throughout the galaxy, the stellar initial mass function (IMF), and the star-formation history (SFH). The aim of this study is to compare the $尾$ values of individual clumps with those measured on the entire galaxy, to investigate possible physical differences between these regions and their hosts. We found a median value of $尾\sim -2.4$, lower than that of integrated galaxies. This result confirms that clumps are sites of intense star formation, populated by young, massive stars, whose spectrum strongly emits in the UV. This is also consistent with the assumption that the dust extinction at the location of the clumps is lower than the average extinction of the galaxy, or that clumps have a different IMF or SFH. We made use of the correlations, discovered for high-redshift galaxies, of the $尾$ value with those of redshift and UV magnitude, $M_{UV}$, finding that clumps follow the same relations, extended to much fainter magnitudes ($M_{UV}<-13$). We also find evidence of eight clumps with extremely blue ($尾\lesssim -2.7$) slopes, which could be the signpost of low-metallicity stars and constrain the emissivity of ionizing photons at high redshift. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.04498v1-abstract-full').style.display = 'none'; document.getElementById('2310.04498v1-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 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">16 pages, 9 figures. 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/2310.02310">arXiv:2310.02310</a> <span> [<a href="https://arxiv.org/pdf/2310.02310">pdf</a>, <a href="https://arxiv.org/format/2310.02310">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/10.1051/0004-6361/202347521">10.1051/0004-6361/202347521 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Exploring the low-mass regime of galaxy-scale strong lensing: Insights into the mass structure of cluster galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Granata%2C+G">Giovanni Granata</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">Pietro Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">Claudio Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">Massimo Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">Amata Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Me%C5%A1tri%C4%87%2C+U">Uros Me拧tri膰</a>, <a href="/search/astro-ph?searchtype=author&query=Ragagnin%2C+A">Antonio Ragagnin</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">Piero Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Caminha%2C+G+B">Gabriel Bartosch Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Tortorelli%2C+L">Luca Tortorelli</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">Eros Vanzella</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.02310v2-abstract-short" style="display: inline;"> We aim at a direct measurement of the compactness of three galaxy-scale lenses in massive clusters, testing the accuracy of the scaling laws that describe the members in strong lensing (SL) models of galaxy clusters. We selected the multiply imaged sources MACS J0416.1$-$2403 ID14 ($z=3.221$), MACS J0416.1$-$2403 ID16 ($z=2.095$), and MACS J1206.2$-$0847 ID14 ($z=3.753$). Eight images were observe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.02310v2-abstract-full').style.display = 'inline'; document.getElementById('2310.02310v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.02310v2-abstract-full" style="display: none;"> We aim at a direct measurement of the compactness of three galaxy-scale lenses in massive clusters, testing the accuracy of the scaling laws that describe the members in strong lensing (SL) models of galaxy clusters. We selected the multiply imaged sources MACS J0416.1$-$2403 ID14 ($z=3.221$), MACS J0416.1$-$2403 ID16 ($z=2.095$), and MACS J1206.2$-$0847 ID14 ($z=3.753$). Eight images were observed for the first SL system, and six for the latter two. We focused on the main deflector of each galaxy-scale SL system (identified as members 8971, 8785, and 3910, respectively), and modelled its total mass distribution with a truncated isothermal sphere. We accounted for the lensing effects of the remaining cluster components, and included the uncertainty on the cluster-scale mass distribution through a bootstrapping procedure. We measured a truncation radius value of $6.1^{+2.3}_{-1.1} \, \mathrm{kpc}$, $4.0^{+0.6}_{-0.4} \, \mathrm{kpc}$, and $5.2^{+1.3}_{-1.1} \, \mathrm{kpc}$ for members 8971, 8785, and 3910, respectively. Alternative non-truncated models with a higher number of free parameters do not lead to an improved description of the SL system. We measured the stellar-to-total mass fraction within the effective radius $R_e$ for the three members, finding $0.51\pm0.21$, $1.0\pm0.4$, and $0.39\pm0.16$, respectively. We find that a parameterisation of the properties of cluster galaxies in SL models based on power-law scaling relations with respect to the total luminosity cannot accurately describe their compactness over their full total mass range. Our results agree with modelling of the cluster members based on the Fundamental Plane relation. Finally, we report good agreement between our values of the stellar-to-total mass fraction within $R_e$ and those of early-type galaxies from the SLACS Survey. Our work significantly extends the regime of the current samples of lens galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.02310v2-abstract-full').style.display = 'none'; document.getElementById('2310.02310v2-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, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 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">Astronomy & Astrophysics, 679, A124 (2023), 15 pages, 12 figures, 8 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 679, A124 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.05799">arXiv:2309.05799</a> <span> [<a href="https://arxiv.org/pdf/2309.05799">pdf</a>, <a href="https://arxiv.org/format/2309.05799">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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/10.1051/0004-6361/202346975">10.1051/0004-6361/202346975 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A persistent excess of galaxy-galaxy strong lensing observed in galaxy clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">Massimo Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Cui%2C+W">Weiguang Cui</a>, <a href="/search/astro-ph?searchtype=author&query=Rasia%2C+E">Elena Rasia</a>, <a href="/search/astro-ph?searchtype=author&query=Yepes%2C+G">Gustavo Yepes</a>, <a href="/search/astro-ph?searchtype=author&query=Acebron%2C+A">Ana Acebron</a>, <a href="/search/astro-ph?searchtype=author&query=Angora%2C+G">Giuseppe Angora</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">Pietro Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Borgani%2C+S">Stefano Borgani</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">Francesco Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Despali%2C+G">Giulia Despali</a>, <a href="/search/astro-ph?searchtype=author&query=Giocoli%2C+C">Carlo Giocoli</a>, <a href="/search/astro-ph?searchtype=author&query=Granata%2C+G">Giovanni Granata</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">Claudio Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Knebe%2C+A">Alexander Knebe</a>, <a href="/search/astro-ph?searchtype=author&query=Macci%C3%B2%2C+A">Andrea Macci貌</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">Amata Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Moscardini%2C+L">Lauro Moscardini</a>, <a href="/search/astro-ph?searchtype=author&query=Natarajan%2C+P">Priyamvada Natarajan</a>, <a href="/search/astro-ph?searchtype=author&query=Ragagnin%2C+A">Antonio Ragagnin</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">Piero Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">Eros Vanzella</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="2309.05799v2-abstract-short" style="display: inline;"> Previous studies have revealed that the estimated probability of galaxy-galaxy strong lensing in observed galaxy clusters exceeds the expectations from the $螞$ Cold Dark Matter cosmological model by one order of magnitude. We aim to understand the origin of this excess by analyzing a larger set of simulated galaxy clusters and investigating how the theoretical expectations vary under different ado… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.05799v2-abstract-full').style.display = 'inline'; document.getElementById('2309.05799v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.05799v2-abstract-full" style="display: none;"> Previous studies have revealed that the estimated probability of galaxy-galaxy strong lensing in observed galaxy clusters exceeds the expectations from the $螞$ Cold Dark Matter cosmological model by one order of magnitude. We aim to understand the origin of this excess by analyzing a larger set of simulated galaxy clusters and investigating how the theoretical expectations vary under different adopted prescriptions and numerical implementations of star formation and feedback in simulations. We perform a ray-tracing analysis of 324 galaxy clusters from the Three Hundred project, comparing the Gadget-X and Gizmo-Simba runs. These simulations, which start from the same initial conditions, are performed with different implementations of hydrodynamics and galaxy formation models tailored to match different observational properties of the Intra-Cluster-Medium and cluster galaxies. We find that galaxies in the Gizmo-Simba simulations develop denser stellar cores than their Gadget-X counterparts. Consequently, their probability for galaxy-galaxy strong lensing is higher by a factor of $\sim 3$. This increment is still insufficient to fill the gap with observations, as a discrepancy by a factor $\sim 4$ still persists. In addition, we find that several simulated galaxies have Einstein radii that are too large compared to observations. We conclude that a persistent excess of galaxy-galaxy strong lensing exists in observed galaxy clusters. The origin of this discrepancy with theoretical predictions is still unexplained in the framework of the cosmological hydrodynamical simulations. This might signal a hitherto unknown issue with either the simulation methods or our assumptions regarding the standard cosmological model. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.05799v2-abstract-full').style.display = 'none'; document.getElementById('2309.05799v2-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> 13 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, 2 figures, accepted for publication on A&A Letters. See companion paper Srivastava et al. (2023)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 678, L2 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.05018">arXiv:2308.05018</a> <span> [<a href="https://arxiv.org/pdf/2308.05018">pdf</a>, <a href="https://arxiv.org/format/2308.05018">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"> Enhanced Sub-kpc Scale Star-formation: Results From A JWST Size Analysis of 341 Galaxies At 5<z<14 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Morishita%2C+T">Takahiro Morishita</a>, <a href="/search/astro-ph?searchtype=author&query=Stiavelli%2C+M">Massimo Stiavelli</a>, <a href="/search/astro-ph?searchtype=author&query=Chary%2C+R">Ranga-Ram Chary</a>, <a href="/search/astro-ph?searchtype=author&query=Trenti%2C+M">Michele Trenti</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">Pietro Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Chiaberge%2C+M">Marco Chiaberge</a>, <a href="/search/astro-ph?searchtype=author&query=Leethochawalit%2C+N">Nicha Leethochawalit</a>, <a href="/search/astro-ph?searchtype=author&query=Roberts-Borsani%2C+G">Guido Roberts-Borsani</a>, <a href="/search/astro-ph?searchtype=author&query=Shen%2C+X">Xuejian Shen</a>, <a href="/search/astro-ph?searchtype=author&query=Treu%2C+T">Tommaso Treu</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="2308.05018v2-abstract-short" style="display: inline;"> We present a comprehensive search and analysis of high-redshift galaxies in a suite of nine public JWST extragalactic fields taken in Cycle 1, covering a total effective search area of $\sim358{\rm arcmin^2}$. Through conservative ($8蟽$) photometric selection, we identify 341 galaxies at $5<z<14$, with 109 having spectroscopic redshift measurements from the literature, including recent JWST NIRSpe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.05018v2-abstract-full').style.display = 'inline'; document.getElementById('2308.05018v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.05018v2-abstract-full" style="display: none;"> We present a comprehensive search and analysis of high-redshift galaxies in a suite of nine public JWST extragalactic fields taken in Cycle 1, covering a total effective search area of $\sim358{\rm arcmin^2}$. Through conservative ($8蟽$) photometric selection, we identify 341 galaxies at $5<z<14$, with 109 having spectroscopic redshift measurements from the literature, including recent JWST NIRSpec observations. Our regression analysis reveals that the rest-frame UV size-stellar mass relation follows $R_{\rm eff}\propto M_*^{0.19\pm0.03}$, similar to that of star-forming galaxies at $z\sim3$, but scaled down in size by $\sim0.7$dex. We find a much slower rate for the average size evolution over the redshift range, $R_{\rm eff}\propto(1+z)^{-0.4\pm0.2}$, than that derived in the literature. A fraction ($\sim13\,\%$) of our sample are marginally resolved even in the NIRCam imaging ($<100$pc), located at $>1.5\,蟽$ below the derived size-mass slope. These compact sources exhibit a high star formation surface density $危_{\rm SFR}>10\,M_\odot\,{\rm yr^{-1}\,kpc^{-2}}$, a range in which only $<0.01\,\%$ of the local star-forming galaxy sample is found. For those with available NIRSpec data, no evidence of ongoing supermassive black hole accretion is observed. A potential explanation for the observed high [OIII]-to-Hbeta ratios could be high shock velocities, likely originating within intense star-forming regions characterized by high $危_{\rm SFR}$. Lastly, we find that the rest-frame UV and optical sizes of our sample are comparable. Our results are consistent with these early galaxies building up their structures inside-out and yet to exhibit the strong color gradient seen at lower redshift. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.05018v2-abstract-full').style.display = 'none'; document.getElementById('2308.05018v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 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">Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.08736">arXiv:2307.08736</a> <span> [<a href="https://arxiv.org/pdf/2307.08736">pdf</a>, <a href="https://arxiv.org/format/2307.08736">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202347244">10.1051/0004-6361/202347244 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Euclid Preparation XXXIII. Characterization of convolutional neural networks for the identification of galaxy-galaxy strong lensing events </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Leuzzi%2C+L">L. Leuzzi</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">M. Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Angora%2C+G">G. Angora</a>, <a href="/search/astro-ph?searchtype=author&query=Metcalf%2C+R+B">R. B. Metcalf</a>, <a href="/search/astro-ph?searchtype=author&query=Moscardini%2C+L">L. Moscardini</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">P. Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">F. Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Cl%C3%A9ment%2C+B">B. Cl茅ment</a>, <a href="/search/astro-ph?searchtype=author&query=Gavazzi%2C+R">R. Gavazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Gentile%2C+F">F. Gentile</a>, <a href="/search/astro-ph?searchtype=author&query=Lochner%2C+M">M. Lochner</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Vernardos%2C+G">G. Vernardos</a>, <a href="/search/astro-ph?searchtype=author&query=Aghanim%2C+N">N. Aghanim</a>, <a href="/search/astro-ph?searchtype=author&query=Amara%2C+A">A. Amara</a>, <a href="/search/astro-ph?searchtype=author&query=Amendola%2C+L">L. Amendola</a>, <a href="/search/astro-ph?searchtype=author&query=Andreon%2C+S">S. Andreon</a>, <a href="/search/astro-ph?searchtype=author&query=Auricchio%2C+N">N. Auricchio</a>, <a href="/search/astro-ph?searchtype=author&query=Bardelli%2C+S">S. Bardelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bodendorf%2C+C">C. Bodendorf</a>, <a href="/search/astro-ph?searchtype=author&query=Bonino%2C+D">D. Bonino</a>, <a href="/search/astro-ph?searchtype=author&query=Branchini%2C+E">E. Branchini</a>, <a href="/search/astro-ph?searchtype=author&query=Brescia%2C+M">M. Brescia</a> , et al. (194 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="2307.08736v2-abstract-short" style="display: inline;"> Forthcoming imaging surveys will potentially increase the number of known galaxy-scale strong lenses by several orders of magnitude. For this to happen, images of tens of millions of galaxies will have to be inspected to identify potential candidates. In this context, deep learning techniques are particularly suitable for the finding patterns in large data sets, and convolutional neural networks (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.08736v2-abstract-full').style.display = 'inline'; document.getElementById('2307.08736v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.08736v2-abstract-full" style="display: none;"> Forthcoming imaging surveys will potentially increase the number of known galaxy-scale strong lenses by several orders of magnitude. For this to happen, images of tens of millions of galaxies will have to be inspected to identify potential candidates. In this context, deep learning techniques are particularly suitable for the finding patterns in large data sets, and convolutional neural networks (CNNs) in particular can efficiently process large volumes of images. We assess and compare the performance of three network architectures in the classification of strong lensing systems on the basis of their morphological characteristics. We train and test our models on different subsamples of a data set of forty thousand mock images, having characteristics similar to those expected in the wide survey planned with the ESA mission \Euclid, gradually including larger fractions of faint lenses. We also evaluate the importance of adding information about the colour difference between the lens and source galaxies by repeating the same training on single-band and multi-band images. Our models find samples of clear lenses with $\gtrsim 90\%$ precision and completeness, without significant differences in the performance of the three architectures. Nevertheless, when including lenses with fainter arcs in the training set, the three models' performance deteriorates with accuracy values of $\sim 0.87$ to $\sim 0.75$ depending on the model. Our analysis confirms the potential of the application of CNNs to the identification of galaxy-scale strong lenses. We suggest that specific training with separate classes of lenses might be needed for detecting the faint lenses since the addition of the colour information does not yield a significant improvement in the current analysis, with the accuracy ranging from $\sim 0.89$ to $\sim 0.78$ for the different models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.08736v2-abstract-full').style.display = 'none'; document.getElementById('2307.08736v2-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 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 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">23 pages,12 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astronomy & Astrophysics,2024, 681, A68 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.14413">arXiv:2305.14413</a> <span> [<a href="https://arxiv.org/pdf/2305.14413">pdf</a>, <a href="https://arxiv.org/format/2305.14413">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202346981">10.1051/0004-6361/202346981 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An extremely metal poor star complex in the reionization era: Approaching Population III stars with JWST </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Loiacono%2C+F">F. Loiacono</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">P. Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Mestric%2C+U">U. Mestric</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">M. Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">F. Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Mignoli%2C+M">M. Mignoli</a>, <a href="/search/astro-ph?searchtype=author&query=Bradac%2C+M">M. Bradac</a>, <a href="/search/astro-ph?searchtype=author&query=Adamo%2C+A">A. Adamo</a>, <a href="/search/astro-ph?searchtype=author&query=Rihtarsic%2C+G">G. Rihtarsic</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">M. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Gronke%2C+M">M. Gronke</a>, <a href="/search/astro-ph?searchtype=author&query=Zanella%2C+A">A. Zanella</a>, <a href="/search/astro-ph?searchtype=author&query=Annibali%2C+F">F. Annibali</a>, <a href="/search/astro-ph?searchtype=author&query=Willott%2C+C">C. Willott</a>, <a href="/search/astro-ph?searchtype=author&query=Messa%2C+M">M. Messa</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Acebron%2C+A">A. Acebron</a>, <a href="/search/astro-ph?searchtype=author&query=Bolamperti%2C+A">A. Bolamperti</a>, <a href="/search/astro-ph?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">R. Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Caputi%2C+K+I">K. I. Caputi</a> , et al. (9 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="2305.14413v1-abstract-short" style="display: inline;"> We present JWST/NIRSpec integral field spectroscopy (IFS) of a lensed Population III candidate stellar complex (dubbed Lensed And Pristine 1, LAP1), with a lensing-corrected stellar mass ~<10^4 Msun, absolute luminosity M_UV > -11.2 (m_UV > 35.6), confirmed at redshift 6.639 +/- 0.004. The system is strongly amplified (渭>~ 100) by straddling a critical line of the Hubble Frontier Field galaxy clus… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.14413v1-abstract-full').style.display = 'inline'; document.getElementById('2305.14413v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.14413v1-abstract-full" style="display: none;"> We present JWST/NIRSpec integral field spectroscopy (IFS) of a lensed Population III candidate stellar complex (dubbed Lensed And Pristine 1, LAP1), with a lensing-corrected stellar mass ~<10^4 Msun, absolute luminosity M_UV > -11.2 (m_UV > 35.6), confirmed at redshift 6.639 +/- 0.004. The system is strongly amplified (渭>~ 100) by straddling a critical line of the Hubble Frontier Field galaxy cluster MACS J0416. Despite the stellar continuum is currently not detected in the Hubble and JWST/NIRCam and NIRISS imaging, arclet-like shapes of Lyman and Balmer lines, Lya, Hg, Hb and Ha are detected with NIRSpec IFS with signal-to-noise ratios SNR=5-13 and large equivalent widths (>300-2000A), along with a remarkably weak [OIII]4959-5007 at SNR ~ 4. LAP1 shows a large ionizing photon production efficiency, log(尉_{ion}[erg~Hz^{-1}])>26. From the metallicity indexes R23 = ([OIII]4959-5007 + [OII]3727) / Hb ~< 0.74 and R3 = ([OIII]5007 / Hb) = 0.55 +/- 0.14, we derive an oxygen abundance 12+log(O/H) ~< 6.3. Intriguingly, the Ha emission is also measured in mirrored sub-components where no [OIII] is detected, providing even more stringent upper limits on the metallicity if in-situ star formation is ongoing in this region (12+log(O/H) < 6, or Z < 0.002 Zsun). The formal stellar mass limit of the sub-components would correspond to ~10^{3} Msun or M_UV fainter than -10. Alternatively, such a metal-free pure line emitting region could be the first case of a fluorescing HI gas region, induced by transverse escaping ionizing radiation from a nearby star-complex. The presence of large equivalent-width hydrogen lines and the deficiency of metal lines in such a small region, make LAP1 the most metal poor star-forming region currently known in the reionization era and a promising site that may host isolated, pristine stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.14413v1-abstract-full').style.display = 'none'; document.getElementById('2305.14413v1-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">15 pages, 10 figures, 1 table. Submitted to A&A. Comments welcome</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 678, A173 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.10210">arXiv:2303.10210</a> <span> [<a href="https://arxiv.org/pdf/2303.10210">pdf</a>, <a href="https://arxiv.org/format/2303.10210">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/10.3847/1538-4357/acd643">10.3847/1538-4357/acd643 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The GLASS-JWST Early Release Science Program. III. Strong lensing model of Abell 2744 and its infalling regions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">Pietro Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Acebron%2C+A">Ana Acebron</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">Claudio Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">Piero Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Caminha%2C+G+B">Gabriel Bartosch Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">Amata Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">Eros Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Mason%2C+C">Charlotte Mason</a>, <a href="/search/astro-ph?searchtype=author&query=Treu%2C+T">Tommaso Treu</a>, <a href="/search/astro-ph?searchtype=author&query=Angora%2C+G">Giuseppe Angora</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G+B">Gabriel B. Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">Massimo Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">Mario Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Boyett%2C+K">Kristan Boyett</a>, <a href="/search/astro-ph?searchtype=author&query=Bradac%2C+M">Marusa Bradac</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">Marco Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">Adriano Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Morishita%2C+T">Takahiro Morishita</a>, <a href="/search/astro-ph?searchtype=author&query=Paris%2C+D">Diego Paris</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto-Lyon%2C+G">Gonzalo Prieto-Lyon</a>, <a href="/search/astro-ph?searchtype=author&query=Roberts-Borsani%2C+G">Guido Roberts-Borsani</a>, <a href="/search/astro-ph?searchtype=author&query=Roy%2C+N">Namrata Roy</a>, <a href="/search/astro-ph?searchtype=author&query=Santini%2C+P">Paola Santini</a>, <a href="/search/astro-ph?searchtype=author&query=Vulcani%2C+B">Benedetta Vulcani</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+X">Xin Wang</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.10210v2-abstract-short" style="display: inline;"> We present a new high-precision, JWST-based, strong lensing model for the galaxy cluster Abell 2744 at $z=0.3072$. By combining the deep, high-resolution JWST imaging from the GLASS-JWST and UNCOVER programs and a Director's Discretionary Time program, with newly obtained VLT/MUSE data, we identify 32 multiple images from 11 background sources lensed by two external sub-clusters at distances of ~1… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.10210v2-abstract-full').style.display = 'inline'; document.getElementById('2303.10210v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.10210v2-abstract-full" style="display: none;"> We present a new high-precision, JWST-based, strong lensing model for the galaxy cluster Abell 2744 at $z=0.3072$. By combining the deep, high-resolution JWST imaging from the GLASS-JWST and UNCOVER programs and a Director's Discretionary Time program, with newly obtained VLT/MUSE data, we identify 32 multiple images from 11 background sources lensed by two external sub-clusters at distances of ~160" from the main cluster. The new MUSE observations enable the first spectroscopic confirmation of a multiple image system in the external clumps. Moreover, the re-analysis of the spectro-photometric archival and JWST data yields 27 additional multiple images in the main cluster. The new lens model is constrained by 149 multiple images ($\sim66\%$ more than in our previous Bergamini et al. 2023 model) covering an extended redshift range between 1.03 and 9.76. The subhalo mass component of the cluster includes 177 member galaxies down to $m_{\rm F160W}=21$, 163 of which are spectroscopically confirmed. Internal velocity dispersions are measured for 85 members. The new lens model is characterized by a remarkably low scatter between predicted and observed positions of the multiple images (0.43"). This precision is unprecedented given the large multiple image sample, the complexity of the cluster mass distribution, and the large modeled area. The improved accuracy and resolution of the cluster total mass distribution provides a robust magnification map over a $\sim\!45$ arcmin$^2$ area, which is critical for inferring the intrinsic physical properties of the highly magnified, high-$z$ sources. The lens model and the new MUSE redshift catalog are released with this publication. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.10210v2-abstract-full').style.display = 'none'; document.getElementById('2303.10210v2-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 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 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">Submitted to ApJ., 23 pages, 10 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/2303.01115">arXiv:2303.01115</a> <span> [<a href="https://arxiv.org/pdf/2303.01115">pdf</a>, <a href="https://arxiv.org/format/2303.01115">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/accbc4">10.3847/2041-8213/accbc4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Early results from GLASS-JWST. XX: Unveiling a population of "red-excess'' galaxies in Abell2744 and in the coeval field </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vulcani%2C+B">Benedetta Vulcani</a>, <a href="/search/astro-ph?searchtype=author&query=Treu%2C+T">Tommaso Treu</a>, <a href="/search/astro-ph?searchtype=author&query=Calabro%2C+A">Antonello Calabro</a>, <a href="/search/astro-ph?searchtype=author&query=Fritz%2C+J">Jacopo Fritz</a>, <a href="/search/astro-ph?searchtype=author&query=Poggianti%2C+B">Bianca Poggianti</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">Pietro Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Bonchi%2C+A">Andrea Bonchi</a>, <a href="/search/astro-ph?searchtype=author&query=Boyett%2C+K">Kit Boyett</a>, <a href="/search/astro-ph?searchtype=author&query=Caminha%2C+G">Gabriel Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">Marco Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Dressler%2C+A">Alan Dressler</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">Adriano Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Glazebrook%2C+K">Karl Glazebrook</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">Claudio Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Malkan%2C+M">Matthew Malkan</a>, <a href="/search/astro-ph?searchtype=author&query=Mascia%2C+S">Sara Mascia</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">Amata Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Merlin%2C+E">Emiliano Merlin</a>, <a href="/search/astro-ph?searchtype=author&query=Metha%2C+B">Benjamin Metha</a>, <a href="/search/astro-ph?searchtype=author&query=Morishita%2C+T">Takahiro Morishita</a>, <a href="/search/astro-ph?searchtype=author&query=Nanayakkara%2C+T">Themiya Nanayakkara</a>, <a href="/search/astro-ph?searchtype=author&query=Paris%2C+D">Diego Paris</a>, <a href="/search/astro-ph?searchtype=author&query=Roberts-Borsani%2C+G">Guido Roberts-Borsani</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">Piero Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Roy%2C+N">Namrata Roy</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="2303.01115v2-abstract-short" style="display: inline;"> We combine JWST/NIRCam imaging and MUSE data to characterize the properties of galaxies in different environmental conditions in the cluster Abell2744 ($z=0.3064$) and in its immediate surroundings. We investigate how galaxy colors, morphology and star forming fractions depend on wavelength and on different parameterizations of environment. Our most striking result is the discovery of a ``red-exce… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.01115v2-abstract-full').style.display = 'inline'; document.getElementById('2303.01115v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.01115v2-abstract-full" style="display: none;"> We combine JWST/NIRCam imaging and MUSE data to characterize the properties of galaxies in different environmental conditions in the cluster Abell2744 ($z=0.3064$) and in its immediate surroundings. We investigate how galaxy colors, morphology and star forming fractions depend on wavelength and on different parameterizations of environment. Our most striking result is the discovery of a ``red-excess'' population in F200W$-$F444W colors both in the cluster regions and the field. These galaxies have normal F115W$-$F150W colors, but are up to 0.8 mag redder than red sequence galaxies in F200W$-$F444W. They also have rather blue rest frame B$-$V colors. {Galaxies in the field and at the cluster virial radius are overall characterized by redder colors, but galaxies with the largest color deviations are found in the field and in the cluster core. Several results} suggest that mechanisms taking place in these regions might be more effective in producing these colors. Looking at their morphology, many cluster galaxies show signatures consistent with ram pressure stripping, while field galaxies have features resembling interactions and mergers. Our hypothesis is that these galaxies are characterized by dust enshrouded star formation: a JWST/NIRSpec spectrum for one of the galaxies is dominated by a strong PAH at 3.3$渭m$, suggestive of dust obscured star formation. Larger spectroscopic samples are needed to understand if the color excess is due exclusively to dust-obscured star formation, and the role of environment in triggering it. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.01115v2-abstract-full').style.display = 'none'; document.getElementById('2303.01115v2-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 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 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</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.00769">arXiv:2303.00769</a> <span> [<a href="https://arxiv.org/pdf/2303.00769">pdf</a>, <a href="https://arxiv.org/format/2303.00769">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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="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/10.1051/0004-6361/202346283">10.1051/0004-6361/202346283 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Searching for galaxy-scale strong-lenses in galaxy clusters with deep networks -- I: methodology and network performance </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Angora%2C+G">G. Angora</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">M. Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Brescia%2C+M">M. Brescia</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">A. Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">P. Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Acebron%2C+A">A. Acebron</a>, <a href="/search/astro-ph?searchtype=author&query=Caminha%2C+G">G. Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">M. Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Tortorelli%2C+L">L. Tortorelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bazzanini%2C+L">L. Bazzanini</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.00769v2-abstract-short" style="display: inline;"> Galaxy-scale strong lenses in galaxy clusters provide a unique tool to investigate their inner mass distribution and the sub-halo density profiles in the low-mass regime, which can be compared with the predictions from cosmological simulations. We search for galaxy-galaxy strong-lensing systems in HST multi-band imaging of galaxy cluster cores from the CLASH and HFF programs by exploring the class… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.00769v2-abstract-full').style.display = 'inline'; document.getElementById('2303.00769v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.00769v2-abstract-full" style="display: none;"> Galaxy-scale strong lenses in galaxy clusters provide a unique tool to investigate their inner mass distribution and the sub-halo density profiles in the low-mass regime, which can be compared with the predictions from cosmological simulations. We search for galaxy-galaxy strong-lensing systems in HST multi-band imaging of galaxy cluster cores from the CLASH and HFF programs by exploring the classification capabilities of deep learning techniques. Convolutional neural networks are trained utilising highly-realistic simulations of galaxy-scale strong lenses injected into the HST cluster fields around cluster members. To this aim, we take advantage of extensive spectroscopic information on member galaxies in 16 clusters and the accurate knowledge of the deflection fields in half of these from high-precision strong lensing models. Using observationally-based distributions, we sample magnitudes, redshifts and sizes of the background galaxy population. By placing these sources within the secondary caustics associated with cluster galaxies, we build a sample of ~3000 galaxy-galaxy strong lenses which preserve the full complexity of real multi-colour data and produce a wide diversity of strong lensing configurations. We study two deep learning networks processing a large sample of image cutouts in three HST/ACS bands, and we quantify their classification performance using several standard metrics. We find that both networks achieve a very good trade-off between purity and completeness (85%-95%), as well as good stability with fluctuations within 2%-4%. We characterise the limited number of false negatives and false positives in terms of the physical properties of the background sources and cluster members. We also demonstrate the neural networks' high degree of generalisation by applying our method to HST observations of 12 clusters with previously known galaxy-scale lensing systems. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.00769v2-abstract-full').style.display = 'none'; document.getElementById('2303.00769v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 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">17 pages, 13 figures, to be published on A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 676, A40 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.07896">arXiv:2302.07896</a> <span> [<a href="https://arxiv.org/pdf/2302.07896">pdf</a>, <a href="https://arxiv.org/format/2302.07896">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202346151">10.1051/0004-6361/202346151 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Kormendy relation of early-type galaxies as a function of wavelength in Abell S1063, MACS J0416.1-2403, and MACS J1149.5+2223 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tortorelli%2C+L">L. Tortorelli</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">A. Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Granata%2C+G">G. Granata</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">M. Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Acebron%2C+A">A. Acebron</a>, <a href="/search/astro-ph?searchtype=author&query=Angora%2C+G">G. Angora</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">P. Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Caminha%2C+G+B">G. B. Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Me%C5%A1tri%C4%87%2C+U">U. Me拧tri膰</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</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="2302.07896v2-abstract-short" style="display: inline;"> The wavelength dependence of the Kormendy relation (KR) is well characterised at low redshift but poorly studied at intermediate redshifts. The KR provides information on the evolution of the population of early-type galaxies (ETGs). Therefore, by studying it, we may shed light on the assembly processes of these objects and their size evolution. As studies at different redshifts are generally cond… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.07896v2-abstract-full').style.display = 'inline'; document.getElementById('2302.07896v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.07896v2-abstract-full" style="display: none;"> The wavelength dependence of the Kormendy relation (KR) is well characterised at low redshift but poorly studied at intermediate redshifts. The KR provides information on the evolution of the population of early-type galaxies (ETGs). Therefore, by studying it, we may shed light on the assembly processes of these objects and their size evolution. As studies at different redshifts are generally conducted in different rest-frame wavebands, it is important to investigate whether the KR is dependent on wavelength. Knowledge of such a dependence is fundamental to correctly interpreting the conclusions we might draw from these studies. We analyse the KRs of the three Hubble Frontier Fields clusters, Abell S1063 (z = 0.348), MACSJ0416.1-2403 (z = 0.396), and MACS J1149.5+2223 (z = 0.542), as a function of wavelength. This is the first time the KR of ETGs has been explored consistently over such a large range of wavelengths at intermediate redshifts. We exploit very deep HST photometry, ranging from the observed B-band to the H-band, and MUSE integral field spectroscopy. We improve the structural parameter estimation we performed in a previous work by means of a newly developed Python package called morphofit. With its use on cluster ETGs, we find that the KR slopes increase smoothly with wavelength from the optical to the near-infrared (NIR) bands in all three clusters, with the intercepts becoming fainter at lower redshifts due to the passive ageing of the ETG stellar populations. The slope trend is consistent with previous findings at lower redshifts. The slope increase with wavelength implies that smaller ETGs are more centrally concentrated than larger ETGs in the NIR with respect to the optical regime. As different bands probe different stellar populations in galaxies, the slope increase also implies that smaller ETGs have stronger internal gradients with respect to larger ETGs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.07896v2-abstract-full').style.display = 'none'; document.getElementById('2302.07896v2-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 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 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">Accepted for publication in A&A as letter to the editor, 6 pages, 1 figure, 1 table</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 671, L9 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.07126">arXiv:2301.07126</a> <span> [<a href="https://arxiv.org/pdf/2301.07126">pdf</a>, <a href="https://arxiv.org/format/2301.07126">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/acd938">10.3847/2041-8213/acd938 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Early Results from GLASS-JWST. XXI: Rapid assembly of a galaxy at z=6.23 revealed by its C/O abundance </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jones%2C+T">Tucker Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Sanders%2C+R">Ryan Sanders</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Y">Yuguang Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+X">Xin Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Morishita%2C+T">Takahiro Morishita</a>, <a href="/search/astro-ph?searchtype=author&query=Roberts-Borsani%2C+G">Guido Roberts-Borsani</a>, <a href="/search/astro-ph?searchtype=author&query=Treu%2C+T">Tommaso Treu</a>, <a href="/search/astro-ph?searchtype=author&query=Dressler%2C+A">Alan Dressler</a>, <a href="/search/astro-ph?searchtype=author&query=Merlin%2C+E">Emiliano Merlin</a>, <a href="/search/astro-ph?searchtype=author&query=Paris%2C+D">Diego Paris</a>, <a href="/search/astro-ph?searchtype=author&query=Santini%2C+P">Paola Santini</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">Pietro Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Huntzinger%2C+E">Erin Huntzinger</a>, <a href="/search/astro-ph?searchtype=author&query=Nanayakkara%2C+T">Themiya Nanayakkara</a>, <a href="/search/astro-ph?searchtype=author&query=Boyett%2C+K">Kristan Boyett</a>, <a href="/search/astro-ph?searchtype=author&query=Bradac%2C+M">Marusa Bradac</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">Gabriel Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Calabro%2C+A">Antonello Calabro</a>, <a href="/search/astro-ph?searchtype=author&query=Glazebrook%2C+K">Karl Glazebrook</a>, <a href="/search/astro-ph?searchtype=author&query=Grasha%2C+K">Kathryn Grasha</a>, <a href="/search/astro-ph?searchtype=author&query=Mascia%2C+S">Sara Mascia</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">Laura Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Trenti%2C+M">Michele Trenti</a>, <a href="/search/astro-ph?searchtype=author&query=Vulcani%2C+B">Benedetta Vulcani</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="2301.07126v2-abstract-short" style="display: inline;"> The abundance of carbon relative to oxygen (C/O) is a promising probe of star formation history in the early universe, as the ratio changes with time due to production of these elements by different nucleosynthesis pathways. We present a measurement of $\log{\mathrm{(C/O)}} = -1.01\pm0.12$ (stat) $\pm0.15$ (sys) in a $z=6.23$ galaxy observed as part of the GLASS-JWST Early Release Science Program.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.07126v2-abstract-full').style.display = 'inline'; document.getElementById('2301.07126v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.07126v2-abstract-full" style="display: none;"> The abundance of carbon relative to oxygen (C/O) is a promising probe of star formation history in the early universe, as the ratio changes with time due to production of these elements by different nucleosynthesis pathways. We present a measurement of $\log{\mathrm{(C/O)}} = -1.01\pm0.12$ (stat) $\pm0.15$ (sys) in a $z=6.23$ galaxy observed as part of the GLASS-JWST Early Release Science Program. Notably, we achieve good precision thanks to the detection of the rest-frame ultraviolet O III], C III], and C IV emission lines delivered by JWST/NIRSpec. The C/O abundance is $\sim$0.8 dex lower than the solar value and is consistent with the expected yield from core-collapse supernovae, indicating that longer-lived intermediate mass stars have not fully contributed to carbon enrichment. This in turn implies rapid buildup of a young stellar population with age $\lesssim100$ Myr in a galaxy seen $\sim$900 million years after the Big Bang. Our chemical abundance analysis is consistent with spectral energy distribution modeling of JWST/NIRCam photometric data, which indicates a current stellar mass $\log\,\mathrm{M}_* / \mathrm{M_{sun}} = 8.4^{+0.4}_{-0.2}$ and specific star formation rate sSFR $\simeq 20$ Gyr$^{-1}$. These results showcase the value of chemical abundances and C/O in particular to study the earliest stages of galaxy assembly. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.07126v2-abstract-full').style.display = 'none'; document.getElementById('2301.07126v2-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 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 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, 4 figures, 2 tables. 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/2301.04672">arXiv:2301.04672</a> <span> [<a href="https://arxiv.org/pdf/2301.04672">pdf</a>, <a href="https://arxiv.org/format/2301.04672">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202345895">10.1051/0004-6361/202345895 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Clues on the presence and segregation of very massive stars in the Sunburst Lyman-continuum cluster at z=2.37 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mestric%2C+U">U. Mestric</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Upadhyaya%2C+A">A. Upadhyaya</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+F">F. Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Marques-Chaves%2C+R">R. Marques-Chaves</a>, <a href="/search/astro-ph?searchtype=author&query=Schaerer%2C+D">D. Schaerer</a>, <a href="/search/astro-ph?searchtype=author&query=Guibert%2C+J">J. Guibert</a>, <a href="/search/astro-ph?searchtype=author&query=Zanella%2C+A">A. Zanella</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">F. Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Caminha%2C+G+B">G. B. Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Bolamperti%2C+A">A. Bolamperti</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">M. Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">P. Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">A. Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">M. Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Pascale%2C+R">R. Pascale</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="2301.04672v2-abstract-short" style="display: inline;"> We report the identification of very massive stars (VMS; mass $> 100$\,\msun) that may be segregated in the center of the young massive star cluster at $z$=2.37 hosted in the lensed galaxy called {\tt Sunburst} galaxy. This result is based on two pieces of evidence: (1) VLT/MUSE spectra of several multiple images of the same star cluster show key spectral signatures of VMS, such as the \heii\ broa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.04672v2-abstract-full').style.display = 'inline'; document.getElementById('2301.04672v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.04672v2-abstract-full" style="display: none;"> We report the identification of very massive stars (VMS; mass $> 100$\,\msun) that may be segregated in the center of the young massive star cluster at $z$=2.37 hosted in the lensed galaxy called {\tt Sunburst} galaxy. This result is based on two pieces of evidence: (1) VLT/MUSE spectra of several multiple images of the same star cluster show key spectral signatures of VMS, such as the \heii\ broad emission, \nivblue\ emission, and an \niv\ P-Cygni profile. In particular, \heii\ is broad ($\sim1610\pm300$ \kms), with an equivalent width of 3脜,\ and asymmetric profile. These features require an extremely young ($\sim2.5$ Myr) stellar population component in which the masses of the stars exceed 100~\msun. When a Salpeter initial mass function and BPASS models for normal massive stars are assumed, the observed spectral features require $\sim$400 VMS. (2) The same star cluster is detected at a signal-to-noise ratio of~$\sim100$ in the Lyman continuum domain ($位< 900$脜). The Lyman continuum emission emerges from a region with a radius that is at least twice smaller than what is observed at 1700脜~(independently of magnification) and is located in the center of the cluster. After delensing, the effective radii in absolute scales are R$_{\tt eff}[{\tt LyC}]\sim4.7 \pm 1.5$ pc and R$_{\tt eff}[1700]= 7.8 \pm 1.4$ pc. The Lyman continuum radiation is mainly produced by hot and massive stars, which implies that their spatial distribution (including that of VMS) is preferentially more confined in the central parts of the cluster. Approximately 400 VMS hosted by a cluster of $\sim 10^7$ \msun\ produce $\sim$15\% of the escaping Lyman continuum photons, and the remaining photons are produced by other massive early-type stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.04672v2-abstract-full').style.display = 'none'; document.getElementById('2301.04672v2-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 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 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">10 pages, 8 figures, Accepted to publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 673, A50 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.02816">arXiv:2301.02816</a> <span> [<a href="https://arxiv.org/pdf/2301.02816">pdf</a>, <a href="https://arxiv.org/format/2301.02816">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202345866">10.1051/0004-6361/202345866 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Closing in on the sources of cosmic reionization: first results from the GLASS-JWST program </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mascia%2C+S">S. Mascia</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Calabro%27%2C+A">A. Calabro'</a>, <a href="/search/astro-ph?searchtype=author&query=Treu%2C+T">T. Treu</a>, <a href="/search/astro-ph?searchtype=author&query=Santini%2C+P">P. Santini</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+L">L. Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+L">L. Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Roberts-Borsani%2C+G">G. Roberts-Borsani</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">P. Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Vulcani%2C+B">B. Vulcani</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Boyett%2C+K">K. Boyett</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">A. Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Glazebrook%2C+K">K. Glazebrook</a>, <a href="/search/astro-ph?searchtype=author&query=Henry%2C+A">A. Henry</a>, <a href="/search/astro-ph?searchtype=author&query=Mason%2C+C">C. Mason</a>, <a href="/search/astro-ph?searchtype=author&query=Merlin%2C+E">E. Merlin</a>, <a href="/search/astro-ph?searchtype=author&query=Morishita%2C+T">T. Morishita</a>, <a href="/search/astro-ph?searchtype=author&query=Nanayakkara%2C+T">T. Nanayakkara</a>, <a href="/search/astro-ph?searchtype=author&query=Paris%2C+D">D. Paris</a>, <a href="/search/astro-ph?searchtype=author&query=Roy%2C+N">N. Roy</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+H">H. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+X">X. Wang</a> , et al. (7 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2301.02816v2-abstract-short" style="display: inline;"> The escape fraction of Lyman-continuum (LyC) photons ($f_{esc}$) is a key parameter for determining the sources of cosmic reionization at $z\geq 6$. At these redshifts, owing to the opacity of the intergalactic medium, the LyC emission cannot be measured directly. However, LyC leakers during the epoch of reionization could be identified using indirect indicators that have been extensively tested a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.02816v2-abstract-full').style.display = 'inline'; document.getElementById('2301.02816v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.02816v2-abstract-full" style="display: none;"> The escape fraction of Lyman-continuum (LyC) photons ($f_{esc}$) is a key parameter for determining the sources of cosmic reionization at $z\geq 6$. At these redshifts, owing to the opacity of the intergalactic medium, the LyC emission cannot be measured directly. However, LyC leakers during the epoch of reionization could be identified using indirect indicators that have been extensively tested at low and intermediate redshifts. These include a high [OIII]/[OII] flux ratio, high star-formation surface density, and compact sizes. In this work, we present observations of 29 $4.5 \leq z \leq 8$ gravitationally lensed galaxies in the Abell 2744 cluster field. From a combined analysis of JWST-NIRSpec and NIRCam data, we accurately derived their physical and spectroscopic properties: our galaxies have low masses $(\log(M_\star)\sim 8.5)$, blue UV spectral slopes ($尾\sim -2.1$), compact sizes ($r_e \sim 0.3-0.5$ kpc), and high [OIII]/[OII] flux ratios. We confirm that these properties are similar to those characterizing low-redshift LyC leakers. Indirectly inferring the fraction of escaping ionizing photons, we find that more than 80% of our galaxies have predicted $f_{esc}$ values larger than 0.05, indicating that they would be considered leakers. The average predicted $f_{esc}$ value of our sample is 0.12, suggesting that similar galaxies at $z\geq 6$ have provided a substantial contribution to cosmic reionization. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.02816v2-abstract-full').style.display = 'none'; document.getElementById('2301.02816v2-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 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 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 the 4. Extragalactic astronomy section of A&A, 12 pages, 8 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 672, A155 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.11298">arXiv:2212.11298</a> <span> [<a href="https://arxiv.org/pdf/2212.11298">pdf</a>, <a href="https://arxiv.org/format/2212.11298">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/10.1093/mnras/stad1692">10.1093/mnras/stad1692 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Near-infrared characterization of ultra-diffuse galaxies in Abell 2744 by JWST/NIRISS imaging </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ikeda%2C+R">Ryota Ikeda</a>, <a href="/search/astro-ph?searchtype=author&query=Morishita%2C+T">Takahiro Morishita</a>, <a href="/search/astro-ph?searchtype=author&query=Tsukui%2C+T">Takafumi Tsukui</a>, <a href="/search/astro-ph?searchtype=author&query=Vulcani%2C+B">Benedetta Vulcani</a>, <a href="/search/astro-ph?searchtype=author&query=Trenti%2C+M">Michele Trenti</a>, <a href="/search/astro-ph?searchtype=author&query=Metha%2C+B">Benjamin Metha</a>, <a href="/search/astro-ph?searchtype=author&query=Acebron%2C+A">Ana Acebron</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">Pietro Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">Claudio Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Iono%2C+D">Daisuke Iono</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">Amata Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">Piero Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">Eros Vanzella</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="2212.11298v3-abstract-short" style="display: inline;"> We present a search and characterization of ultra-diffuse galaxies (UDGs) in the Frontier Fields cluster Abell~2744 at $z=0.308$. We use JWST/NIRISS F200W observations, acquired as part of the GLASS-JWST Early Release Science Program, aiming to characterize morphologies of cluster UDGs and their diffuse stellar components. A total number of 22 UDGs are identified by our selection criteria using mo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.11298v3-abstract-full').style.display = 'inline'; document.getElementById('2212.11298v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.11298v3-abstract-full" style="display: none;"> We present a search and characterization of ultra-diffuse galaxies (UDGs) in the Frontier Fields cluster Abell~2744 at $z=0.308$. We use JWST/NIRISS F200W observations, acquired as part of the GLASS-JWST Early Release Science Program, aiming to characterize morphologies of cluster UDGs and their diffuse stellar components. A total number of 22 UDGs are identified by our selection criteria using morphological parameters, down to stellar mass of $\sim10^{7}M_{\odot}$. The selected UDGs are systematically larger in effective radius in F200W than in HST/ACS F814W images, which implies that some of them would not have been identified as UDGs when selected at rest-frame optical wavelengths. In fact, we find that about one third of the UDGs were not previously identified based on the F814W data. We observe a flat distribution of the UDGs in the stellar mass-size plane, similar to what is found for cluster quiescent galaxies at comparable mass. Our pilot study using the new JWST F200W filter showcases the efficiency of searching UDGs at cosmological distances, with 1/30 of the exposure time of the previous deep observing campaign with HST. Further studies with JWST focusing on spatially-resolved properties of individual sources will provide insight into their origin. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.11298v3-abstract-full').style.display = 'none'; document.getElementById('2212.11298v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 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">Accepted for publication in MNRAS, 10 pages, 7 figures, 2 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.06666">arXiv:2212.06666</a> <span> [<a href="https://arxiv.org/pdf/2212.06666">pdf</a>, <a href="https://arxiv.org/format/2212.06666">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/accea5">10.3847/2041-8213/accea5 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Early Results from GLASS-JWST. XIX: A High Density of Bright Galaxies at $z\approx10$ in the Abell 2744 Region </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">Marco Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">Adriano Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Treu%2C+T">Tommaso Treu</a>, <a href="/search/astro-ph?searchtype=author&query=Merlin%2C+E">Emiliano Merlin</a>, <a href="/search/astro-ph?searchtype=author&query=Santini%2C+P">Paola Santini</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">Pietro Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">Claudio Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">Piero Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Acebron%2C+A">Ana Acebron</a>, <a href="/search/astro-ph?searchtype=author&query=Leethochawalit%2C+N">Nicha Leethochawalit</a>, <a href="/search/astro-ph?searchtype=author&query=Paris%2C+D">Diego Paris</a>, <a href="/search/astro-ph?searchtype=author&query=Bonchi%2C+A">Andrea Bonchi</a>, <a href="/search/astro-ph?searchtype=author&query=Belfiori%2C+D">Davide Belfiori</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=Correnti%2C+M">Matteo Correnti</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">Mario Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Polenta%2C+G">Gianluca Polenta</a>, <a href="/search/astro-ph?searchtype=author&query=Trenti%2C+M">Michele Trenti</a>, <a href="/search/astro-ph?searchtype=author&query=Boyett%2C+K">Kristan Boyett</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">G. Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Broadhurst%2C+T">Tom Broadhurst</a>, <a href="/search/astro-ph?searchtype=author&query=Caminha%2C+G+B">Gabriel B. Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W">Wenlei Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Filippenko%2C+A+V">Alexei V. Filippenko</a>, <a href="/search/astro-ph?searchtype=author&query=Fortuni%2C+F">Flaminia Fortuni</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="2212.06666v3-abstract-short" style="display: inline;"> We report the detection of a high density of redshift $z\approx 10$ galaxies behind the foreground cluster Abell 2744, selected from imaging data obtained recently with NIRCam onboard {\it JWST} by three programs -- GLASS-JWST, UNCOVER, and DDT\#2756. To ensure robust estimates of the lensing magnification $渭$, we use an improved version of our model that exploits the first epoch of NIRCam images… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.06666v3-abstract-full').style.display = 'inline'; document.getElementById('2212.06666v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.06666v3-abstract-full" style="display: none;"> We report the detection of a high density of redshift $z\approx 10$ galaxies behind the foreground cluster Abell 2744, selected from imaging data obtained recently with NIRCam onboard {\it JWST} by three programs -- GLASS-JWST, UNCOVER, and DDT\#2756. To ensure robust estimates of the lensing magnification $渭$, we use an improved version of our model that exploits the first epoch of NIRCam images and newly obtained MUSE spectra, and avoids regions with $渭>5$ where the uncertainty may be higher. We detect seven bright $z\approx 10$ galaxies with demagnified rest-frame $-22 \lesssim M_{\rm UV}\lesssim -19$ mag, over an area of $\sim37$ sq. arcmin. Taking into account photometric incompleteness and the effects of lensing on luminosity and cosmological volume, we find that the density of $z\approx 10$ galaxies in the field is about $10\times$ ($3\times$) larger than the average at $M_{UV}\approx -21~ (-20)$ mag reported so far. The density is even higher when considering only the GLASS-JWST data, which are the deepest and the least affected by magnification and incompleteness. The GLASS-JWST field contains 5 out of 7 galaxies, distributed along an apparent filamentary structure of 2 Mpc in projected length, and includes a close pair of candidates with $M_{\rm UV}< -20$ mag having a projected separation of only 16 kpc. These findings suggest the presence of a $z\approx 10$ overdensity in the field. In addition to providing excellent targets for efficient spectroscopic follow-up observations, our study confirms the high density of bright galaxies observed in early {\it JWST} observations, but calls for multiple surveys along independent lines of sight to achieve an unbiased estimate of their average density and a first estimate of their clustering. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.06666v3-abstract-full').style.display = 'none'; document.getElementById('2212.06666v3-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, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 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">Accepted for publication in ApJL, 13 pages, 4 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/2211.12548">arXiv:2211.12548</a> <span> [<a href="https://arxiv.org/pdf/2211.12548">pdf</a>, <a href="https://arxiv.org/format/2211.12548">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202245532">10.1051/0004-6361/202245532 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The production of ionizing photons in UV-faint z~3-7 galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Prieto-Lyon%2C+G">Gonzalo Prieto-Lyon</a>, <a href="/search/astro-ph?searchtype=author&query=Strait%2C+V">Victoria Strait</a>, <a href="/search/astro-ph?searchtype=author&query=Mason%2C+C+A">Charlotte A. Mason</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">Gabriel Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Caminha%2C+G+B">Gabriel B. Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">Amata Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Acebron%2C+A">Ana Acebron</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">Pietro Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">Claudio Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">Piero Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">Eros Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">Marco Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Merlin%2C+E">Emiliano Merlin</a>, <a href="/search/astro-ph?searchtype=author&query=Paris%2C+D">Diego Paris</a>, <a href="/search/astro-ph?searchtype=author&query=Boyett%2C+K">Kristan Boyett</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=Morishita%2C+T">Takahiro Morishita</a>, <a href="/search/astro-ph?searchtype=author&query=Mascia%2C+S">Sara Mascia</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">Laura Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Roberts-Borsani%2C+G">Guido Roberts-Borsani</a>, <a href="/search/astro-ph?searchtype=author&query=Roy%2C+N">Namrata Roy</a>, <a href="/search/astro-ph?searchtype=author&query=Treu%2C+T">Tommaso Treu</a>, <a href="/search/astro-ph?searchtype=author&query=Vulcani%2C+B">Benedetta Vulcani</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="2211.12548v2-abstract-short" style="display: inline;"> The demographics of the production and escape of ionizing photons from UV-faint early galaxies is a key unknown in discovering the primary drivers of reionization. With the advent of JWST it is finally possible to observe the rest-frame optical nebular emission from individual sub-L$^*$ z>3 galaxies to measure the production of ionizing photons, $尉_\mathrm{ion}$. Here we study a sample of 370 z~3-… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.12548v2-abstract-full').style.display = 'inline'; document.getElementById('2211.12548v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.12548v2-abstract-full" style="display: none;"> The demographics of the production and escape of ionizing photons from UV-faint early galaxies is a key unknown in discovering the primary drivers of reionization. With the advent of JWST it is finally possible to observe the rest-frame optical nebular emission from individual sub-L$^*$ z>3 galaxies to measure the production of ionizing photons, $尉_\mathrm{ion}$. Here we study a sample of 370 z~3-7 galaxies spanning -23 <M$_\mathrm{UV}$ < -15.5 (median M$_\mathrm{UV}\approx$ -18) with deep multi-band HST and JWST/NIRCam photometry covering the rest-UV to optical from the GLASS and UNCOVER JWST surveys. Our sample includes 102 galaxies with Lyman-alpha emission detected in MUSE spectroscopy. We use H-alpha fluxes inferred from NIRCam photometry to estimate the production rate of ionizing photons which do not escape these galaxies $尉_\mathrm{ion}(1-f_\mathrm{esc})$. We find median $\log_{10}尉_\mathrm{ion}(1-f_\mathrm{esc})=25.33\pm 0.47$, with a broad intrinsic scatter 0.42 dex, implying a broad range of galaxy properties and ages in our UV-faint sample. Galaxies detected with Lyman-alpha have ~0.1 dex higher $尉_\mathrm{ion}(1-f_\mathrm{esc})$, which is explained by their higher H-alpha EW distribution, implying younger ages, higher sSFR and thus more O/B stars. We find significant trends of increasing $尉_\mathrm{ion}(1-f_\mathrm{esc})$ with increasing H-alpha EW, decreasing UV luminosity, and decreasing UV slope, implying the production of ionizing photons is enhanced in young, low metallicity galaxies. We find no significant evidence for sources with very high ionizing escape fraction ($f_\mathrm{esc}$>0.5) in our sample, based on their photometric properties, even amongst the Lyman-alpha selected galaxies. This work demonstrates that considering the full distribution of $尉_\mathrm{ion}$ across galaxy properties is important for assessing the primary drivers of reionization. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.12548v2-abstract-full').style.display = 'none'; document.getElementById('2211.12548v2-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 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 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">10 pages, 7 figures, submitted to A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 672, A186 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.09097">arXiv:2211.09097</a> <span> [<a href="https://arxiv.org/pdf/2211.09097">pdf</a>, <a href="https://arxiv.org/format/2211.09097">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/acb99e">10.3847/2041-8213/acb99e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Early results from GLASS-JWST. XIV: A spectroscopically confirmed protocluster 650 million years after the Big Bang </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Morishita%2C+T">Takahiro Morishita</a>, <a href="/search/astro-ph?searchtype=author&query=Roberts-Borsani%2C+G">Guido Roberts-Borsani</a>, <a href="/search/astro-ph?searchtype=author&query=Treu%2C+T">Tommaso Treu</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">Gabriel Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Mason%2C+C+A">Charlotte A. Mason</a>, <a href="/search/astro-ph?searchtype=author&query=Trenti%2C+M">Michele Trenti</a>, <a href="/search/astro-ph?searchtype=author&query=Vulcani%2C+B">Benedetta Vulcani</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+X">Xin Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Acebron%2C+A">Ana Acebron</a>, <a href="/search/astro-ph?searchtype=author&query=Bah%C3%A9%2C+Y">Yannick Bah茅</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">Pietro Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Boyett%2C+K">Kristan Boyett</a>, <a href="/search/astro-ph?searchtype=author&query=Bradac%2C+M">Marusa Bradac</a>, <a href="/search/astro-ph?searchtype=author&query=Calabr%C3%B2%2C+A">Antonello Calabr貌</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">Marco Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W">Wenlei Chen</a>, <a href="/search/astro-ph?searchtype=author&query=De+Lucia%2C+G">Gabriella De Lucia</a>, <a href="/search/astro-ph?searchtype=author&query=Filippenko%2C+A+V">Alexei V. Filippenko</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">Adriano Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Glazebrook%2C+K">Karl Glazebrook</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">Claudio Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Henry%2C+A">Alaina Henry</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+T">Tucker Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Kelly%2C+P+L">Patrick L. Kelly</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a> , et al. (17 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="2211.09097v3-abstract-short" style="display: inline;"> We present the spectroscopic confirmation of a protocluster at $z=7.88$ behind the galaxy cluster Abell2744 (hereafter A2744-z7p9OD). Using JWST NIRSpec, we find seven galaxies within a projected radius of 60kpc. Although the galaxies reside in an overdensity around $>20\times$ greater than a random volume, they do not show strong Lyman-alpha emission. We place 2-$蟽$ upper limits on the rest-frame… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.09097v3-abstract-full').style.display = 'inline'; document.getElementById('2211.09097v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.09097v3-abstract-full" style="display: none;"> We present the spectroscopic confirmation of a protocluster at $z=7.88$ behind the galaxy cluster Abell2744 (hereafter A2744-z7p9OD). Using JWST NIRSpec, we find seven galaxies within a projected radius of 60kpc. Although the galaxies reside in an overdensity around $>20\times$ greater than a random volume, they do not show strong Lyman-alpha emission. We place 2-$蟽$ upper limits on the rest-frame equivalent width $<16$-$28$AA. Based on the tight upper limits to the Lyman-alpha emission, we constrain the volume-averaged neutral fraction of hydrogen in the intergalactic medium to be $x_{\rm HI} > 0.45$ (68% CI). Using an empirical $M_{\rm UV}$-$M_{\rm halo}$ relation for individual galaxies, we estimate that the total halo mass of the system is $\gtrsim 4\times10^{11}\,M_\odot$. Likewise, the line of sight velocity dispersion is estimated to be $1100 \pm 200$km/s. Using an empirical relation, we estimate the present-day halo mass of A2744-z7p9OD to be $\sim2\times10^{15}\,M_\odot$, comparable to the Coma cluster. A2744-z7p9OD is the highest redshift spectroscopically confirmed protocluster to date, demonstrating the power of JWST to investigate the connection between dark-matter halo assembly and galaxy formation at very early times with medium-deep observations at $<20$hrs total exposure time. Follow-up spectroscopy of the remaining photometric candidates of the overdensity will further refine the features of this system and help characterize the role of such overdensities in cosmic reionization. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.09097v3-abstract-full').style.display = 'none'; document.getElementById('2211.09097v3-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">v1</span> submitted 16 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">The title has been updated to reflect the published numbering; a minor change has been made to Figure 1 with regard to the MSA shutters on the rgb stamp image. NASA press release article can be found at: https://www.nasa.gov/feature/goddard/2023/webb-reveals-early-universe-prequel-to-huge-galaxy-cluster</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.15639">arXiv:2210.15639</a> <span> [<a href="https://arxiv.org/pdf/2210.15639">pdf</a>, <a href="https://arxiv.org/format/2210.15639">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/s41586-023-05994-w">10.1038/s41586-023-05994-w <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The nature of an ultra-faint galaxy in the cosmic Dark Ages seen with JWST </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Roberts-Borsani%2C+G">Guido Roberts-Borsani</a>, <a href="/search/astro-ph?searchtype=author&query=Treu%2C+T">Tommaso Treu</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W">Wenlei Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Morishita%2C+T">Takahiro Morishita</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">Eros Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Zitrin%2C+A">Adi Zitrin</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">Pietro Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">Marco Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">Adriano Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Glazebrook%2C+K">Karl Glazebrook</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">Claudio Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Kelly%2C+P+L">Patrick L. Kelly</a>, <a href="/search/astro-ph?searchtype=author&query=Merlin%2C+E">Emiliano Merlin</a>, <a href="/search/astro-ph?searchtype=author&query=Nanayakkara%2C+T">Themiya Nanayakkara</a>, <a href="/search/astro-ph?searchtype=author&query=Paris%2C+D">Diego Paris</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">Piero Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+L">Lilan Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Acebron%2C+A">Ana Acebron</a>, <a href="/search/astro-ph?searchtype=author&query=Bonchi%2C+A">Andrea Bonchi</a>, <a href="/search/astro-ph?searchtype=author&query=Boyett%2C+K">Kit Boyett</a>, <a href="/search/astro-ph?searchtype=author&query=Brada%C4%8D%2C+M">Maru拧a Brada膷</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">Gabriel Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Broadhurst%2C+T">Tom Broadhurst</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=Diego%2C+J+M">Jose M. Diego</a> , et al. (22 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="2210.15639v2-abstract-short" style="display: inline;"> In the first billion years after the Big Bang, sources of ultraviolet (UV) photons are believed to have ionized intergalactic hydrogen, rendering the Universe transparent to UV radiation. Galaxies brighter than the characteristic luminosity $L^{*}$ do not provide enough ionizing photons to drive this cosmic reionization. Fainter galaxies are thought to dominate the photon budget; however they are… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.15639v2-abstract-full').style.display = 'inline'; document.getElementById('2210.15639v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.15639v2-abstract-full" style="display: none;"> In the first billion years after the Big Bang, sources of ultraviolet (UV) photons are believed to have ionized intergalactic hydrogen, rendering the Universe transparent to UV radiation. Galaxies brighter than the characteristic luminosity $L^{*}$ do not provide enough ionizing photons to drive this cosmic reionization. Fainter galaxies are thought to dominate the photon budget; however they are surrounded by neutral gas that prevents the escape of the Lyman-$伪$ photons, which has been the dominant way to identify them so far. JD1 was previously identified as a triply-imaged galaxy with a magnification factor of 13 provided by the foreground cluster Abell 2744, and a photometric redshift of $z\sim10$. Here we report the spectroscopic confirmation of this very low luminosity ($\sim0.05 L^{*}$) galaxy at $z=9.79$, observed 480 Myr after the Big Bang, by means of the identification of the Lyman break and redward continuum, as well as multiple $\gtrsim4蟽$ emission lines, with the Near-InfraRed Spectrograph (NIRSpec) and Near-InfraRed Camera (NIRCam) instruments. The combination of the James Webb Space Telescope (JWST) and gravitational lensing shows that this ultra-faint galaxy ($M_{\rm UV}=-17.35$) -- with a luminosity typical of the sources responsible for cosmic reionization -- has a compact ($\sim$150 pc) and complex morphology, low stellar mass (10$^{7.19}$ M$_\odot$), and subsolar ($\sim$0.6 $Z_{\odot}$) gas-phase metallicity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.15639v2-abstract-full').style.display = 'none'; document.getElementById('2210.15639v2-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, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">Matched to the published Nature version of the article. 19 pages, 4 main figures, 1 supplementary figure, 1 supplementary tables. This version includes an updated version of the NIRSpec spectrum and NIRCam photometry</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.02718">arXiv:2209.02718</a> <span> [<a href="https://arxiv.org/pdf/2209.02718">pdf</a>, <a href="https://arxiv.org/format/2209.02718">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/10.1051/0004-6361/202244897">10.1051/0004-6361/202244897 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A MUSE view of the massive merging galaxy cluster ACT-CL J0102-4915 (El Gordo) at z = 0.87: robust strong lensing model and data release </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Caminha%2C+G+B">G. B. Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+A">A. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Acebron%2C+A">A. Acebron</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">P. Bergamini</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=Mercurio%2C+A">A. Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Tozzi%2C+P">P. Tozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Demarco%2C+R">R. Demarco</a>, <a href="/search/astro-ph?searchtype=author&query=Frye%2C+B">B. Frye</a>, <a href="/search/astro-ph?searchtype=author&query=Rosani%2C+G">G. Rosani</a>, <a href="/search/astro-ph?searchtype=author&query=Sharon%2C+K">K. Sharon</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="2209.02718v2-abstract-short" style="display: inline;"> We present a detailed strong lensing analysis of the massive and distant ($z=0.870$) galaxy cluster ACT-CL J0102$-$4915 (ACT0102, also known as El Gordo), taking advantage of new spectroscopic data from the Multi Unit Spectroscopic Explorer (MUSE) on the Very Large Telescope, and archival imaging from the Hubble Space Telescope. Thanks to the MUSE data, we measure secure redshifts for 374 single o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.02718v2-abstract-full').style.display = 'inline'; document.getElementById('2209.02718v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.02718v2-abstract-full" style="display: none;"> We present a detailed strong lensing analysis of the massive and distant ($z=0.870$) galaxy cluster ACT-CL J0102$-$4915 (ACT0102, also known as El Gordo), taking advantage of new spectroscopic data from the Multi Unit Spectroscopic Explorer (MUSE) on the Very Large Telescope, and archival imaging from the Hubble Space Telescope. Thanks to the MUSE data, we measure secure redshifts for 374 single objects, including 23 multiply lensed galaxies, and 167 cluster members of ACT0102. The observed positions of 56 multiple images, along with their new spectroscopic redshift measurements, are used as constraints for our strong lensing model. Remarkably, some multiple images are detected out to a large projected distance of $\approx 1$ Mpc from the brightest cluster galaxy, allowing us to estimate a projected total mass value of $1.84_{-0.04}^{+0.03} \times 10^{15}\, \rm M_{\odot}$ within that radius. We find that we need two extended cluster mass components, the mass contributions from the cluster members and the additional lensing effect of a foreground ($z=0.633$) group of galaxies, to predict the positions of all multiple images with a root mean square offset of $0.75"$. The main cluster-scale mass component is centered very closely to the brightest cluster galaxy and the other extended mass component is located in the north-west region of the cluster. These two mass components have very similar values of mass projected within 300 kpc from their centers, namely $2.29_{-0.10}^{+0.09}\times10^{14}\,\rm M_{\odot}$ and $2.10_{-0.09}^{+0.08}\times10^{14}\,\rm M_{\odot}$, in agreement with the major merging scenario of ACT0102. We make publicly available the lens model, including the magnification maps and posterior distributions of the model parameter values, as well as the full spectroscopic catalogue containing all redshift measurements obtained with MUSE. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.02718v2-abstract-full').style.display = 'none'; document.getElementById('2209.02718v2-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">v1</span> submitted 6 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">12 pages, 9 figures, 4 tables + appendix. Minor changes, A&A in press. MUSE redshift catalogue and lens model are publicly available</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 678, A3 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.14020">arXiv:2208.14020</a> <span> [<a href="https://arxiv.org/pdf/2208.14020">pdf</a>, <a href="https://arxiv.org/format/2208.14020">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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/10.1051/0004-6361/202244834">10.1051/0004-6361/202244834 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A state-of-the-art strong lensing model of MACS J0416.1-2403 with the largest sample of spectroscopic multiple images </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">P. Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Mestric%2C+U">U. Mestric</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">A. Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Acebron%2C+A">A. Acebron</a>, <a href="/search/astro-ph?searchtype=author&query=Caminha%2C+G+B">G. B. Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Granata%2C+G">G. Granata</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">M. Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Angora%2C+G">G. Angora</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">M. Nonino</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="2208.14020v2-abstract-short" style="display: inline;"> The combination of multi-band imaging from HST with MUSE integral field spectroscopy, obtained at the VLT, has recently driven remarkable progress in strong lensing (SL) modeling of galaxy clusters. From a few tens of multiple images with photometric redshifts per cluster, a new generation of high-precision SL models have recently been developed, by exploiting in some cases over a hundred of spect… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.14020v2-abstract-full').style.display = 'inline'; document.getElementById('2208.14020v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.14020v2-abstract-full" style="display: none;"> The combination of multi-band imaging from HST with MUSE integral field spectroscopy, obtained at the VLT, has recently driven remarkable progress in strong lensing (SL) modeling of galaxy clusters. From a few tens of multiple images with photometric redshifts per cluster, a new generation of high-precision SL models have recently been developed, by exploiting in some cases over a hundred of spectroscopically confirmed multiple images and cluster member galaxies. A further step forward is expected with JWST observations of SL clusters (from hundreds to possibly a thousand of multiple images). In this context, we present a new, state-of-the-art SL model of the galaxy cluster MACS J0416.1-2403, utilizing 237 spectroscopically confirmed multiple images, which is the largest sample of secure multiply lensed sources utilized to date. This model incorporates stellar kinematics information of 64 cluster galaxies and the hot-gas mass distribution of the cluster determined from Chandra X-ray observations. The observed positions of the many multiple images are reproduced with a remarkable accuracy of 0.43 arcsec. To further assess the reliability of this lens model and to highlight the improvement over previously published models, we show the extended surface brightness reconstruction of several lensed galaxies through a newly developed forward modeling software. The comparison with other SL models of the same cluster demonstrates that this new model is better suited to accurately reproduce the positions, shapes and fluxes of the observed multiple images. Besides a robust characterization of the total mass distribution of the cluster, our model can provide accurate and precise magnification maps that are key to studying the intrinsic physical properties of faint, high-redshift lensed sources. The model is made publicly available through our newly developed Strong Lensing Online Tool (or SLOT). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.14020v2-abstract-full').style.display = 'none'; document.getElementById('2208.14020v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">Accepted for publication in Astronomy & Astrophysics (16 pages, 13 figures)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 674, A79 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.13788">arXiv:2208.13788</a> <span> [<a href="https://arxiv.org/pdf/2208.13788">pdf</a>, <a href="https://arxiv.org/format/2208.13788">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/10.1051/0004-6361/202244836">10.1051/0004-6361/202244836 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> New strong lensing modelling of SDSS J2222+2745 enhanced with VLT/MUSE spectroscopy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Acebron%2C+A">A. Acebron</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">P. Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Caminha%2C+G+B">G. B. Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Tozzi%2C+P">P. Tozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">A. Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">G. Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">M. Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">M. Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</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="2208.13788v2-abstract-short" style="display: inline;"> SDSS J2222+2745, at z = 0.489, is one of the few currently known lens clusters with multiple images of a background (z = 2.801) quasar with measured time delays. We combine imaging from the Hubble Space Telescope (HST) with recent Multi Unit Spectroscopic Explorer (MUSE) spectroscopic data to securely identify 34 cluster members and 12 multiple images from 3 background sources. We measure the stel… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.13788v2-abstract-full').style.display = 'inline'; document.getElementById('2208.13788v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.13788v2-abstract-full" style="display: none;"> SDSS J2222+2745, at z = 0.489, is one of the few currently known lens clusters with multiple images of a background (z = 2.801) quasar with measured time delays. We combine imaging from the Hubble Space Telescope (HST) with recent Multi Unit Spectroscopic Explorer (MUSE) spectroscopic data to securely identify 34 cluster members and 12 multiple images from 3 background sources. We measure the stellar velocity dispersions of 13 cluster galaxies, enabling an independent estimate of the contribution of the sub-halo mass component to the lens total mass. The projected total mass distribution of the lens cluster is best modelled with a single large-scale mass component, a galaxy-scale component, anchored by the MUSE kinematic information, and an external shear. The best-fit strong lensing model yields a root mean square separation between the model-predicted and observed positions of the multiple images of 0".29. When analysing the impact of systematic uncertainties, stemming from modelling assumptions and used observables, we find that the projected total mass profile, relative weight of the sub-halo mass component, and critical lines are consistent, within the statistical uncertainties. The predicted magnification and time delay values are, instead, more sensitive to the local details of the lens total mass distribution, and vary significantly among lens models that are similarly good at reproducing the observed multiple image positions. Due to its complex morphology, the low number of point-like multiple images, and current model degeneracies, it becomes clear that additional information (from the observed surface brightness distribution of lensed sources and the measured time delays) needs to be included in the modelling of SDSS J2222+2745 for accurate and precise cosmological measurements. The full MUSE secure spectroscopic catalogue presented in this work is made publicly available. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.13788v2-abstract-full').style.display = 'none'; document.getElementById('2208.13788v2-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 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">17 pages, 9 Figures, 5 Tables. Accepted for publication in Astronomy & Astrophysics. The full MUSE spectroscopic catalogue presented in this work is made publicly available at www.fe.infn.it/astro/lensing</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 668, A142 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.00520">arXiv:2208.00520</a> <span> [<a href="https://arxiv.org/pdf/2208.00520">pdf</a>, <a href="https://arxiv.org/format/2208.00520">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/ac8c2d">10.3847/2041-8213/ac8c2d <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Early results from GLASS-JWST. VII: evidence for lensed, gravitationally bound proto-globular clusters at z=4 in the Hubble Frontier Field A2744 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">P. Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Treu%2C+T">T. Treu</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">A. Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Scarlata%2C+C">C. Scarlata</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Acebron%2C+A">A. Acebron</a>, <a href="/search/astro-ph?searchtype=author&query=Caminha%2C+G+B">G. B. Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">M. Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Nanayakkara%2C+T">T. Nanayakkara</a>, <a href="/search/astro-ph?searchtype=author&query=Roberts-Borsani%2C+G">G. Roberts-Borsani</a>, <a href="/search/astro-ph?searchtype=author&query=Bradac%2C+M">M. Bradac</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+X">X. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">G. Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Strait%2C+V">V. Strait</a>, <a href="/search/astro-ph?searchtype=author&query=Vulcani%2C+B">B. Vulcani</a>, <a href="/search/astro-ph?searchtype=author&query=Mestric%2C+U">U. Mestric</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">M. Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">F. Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Henry%2C+A">A. Henry</a>, <a href="/search/astro-ph?searchtype=author&query=Zanella%2C+A">A. Zanella</a>, <a href="/search/astro-ph?searchtype=author&query=Trenti%2C+M">M. Trenti</a>, <a href="/search/astro-ph?searchtype=author&query=Boyett%2C+K">K. Boyett</a> , et al. (7 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2208.00520v1-abstract-short" style="display: inline;"> We investigate the blue and optical rest-frame sizes (lambda~2300A-4000A) of three compact star-forming regions in a galaxy at z=4 strongly lensed (x30, x45, x100) by the Hubble Frontier Field galaxy cluster A2744 using GLASS-ERS JWST/NIRISS imaging at 1.15um, 1.50mu and 2.0mu with PSF < 0.1". In particular, the Balmer break is probed in detail for all multiply-imaged sources of the system. With a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.00520v1-abstract-full').style.display = 'inline'; document.getElementById('2208.00520v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.00520v1-abstract-full" style="display: none;"> We investigate the blue and optical rest-frame sizes (lambda~2300A-4000A) of three compact star-forming regions in a galaxy at z=4 strongly lensed (x30, x45, x100) by the Hubble Frontier Field galaxy cluster A2744 using GLASS-ERS JWST/NIRISS imaging at 1.15um, 1.50mu and 2.0mu with PSF < 0.1". In particular, the Balmer break is probed in detail for all multiply-imaged sources of the system. With ages of a few tens of Myr, stellar masses in the range (0.7-4.0) x 10^6 Msun and optical/ultraviolet effective radii spanning the interval 3 < R_eff < 20 pc, such objects are currently the highest redshift (spectroscopically-confirmed) gravitationally-bound young massive star clusters (YMCs), with stellar mass surface densities resembling those of local globular clusters. Optical (4000A, JWST-based) and ultraviolet (1600A, HST-based) sizes are fully compatible. The contribution to the ultraviolet underlying continuum emission (1600A) is ~30%, which decreases by a factor of two in the optical for two of the YMCs (~4000A rest-frame), reflecting the young ages (<30 Myr) inferred from the SED fitting and supported by the presence of high-ionization lines secured with VLT/MUSE. Such bursty forming regions enhance the sSFR of the galaxy, which is ~10 Gyr^-1. This galaxy would be among the extreme analogs observed in the local Universe having high star formation rate surface density and high occurrence of massive stellar clusters in formation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.00520v1-abstract-full').style.display = 'none'; document.getElementById('2208.00520v1-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 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">10 pages, 4 figures, 1 table. 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/2207.13625">arXiv:2207.13625</a> <span> [<a href="https://arxiv.org/pdf/2207.13625">pdf</a>, <a href="https://arxiv.org/format/2207.13625">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/acaaac">10.3847/2041-8213/acaaac <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Early results from GLASS-JWST. IX: First spectroscopic confirmation of low-mass quiescent galaxies at $z>2$ with NIRISS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Marchesini%2C+D">Danilo Marchesini</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">Gabriel Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Morishita%2C+T">Takahiro Morishita</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">Pietro Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+X">Xin Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Bradac%2C+M">Marusa Bradac</a>, <a href="/search/astro-ph?searchtype=author&query=Roberts-Borsani%2C+G">Guido Roberts-Borsani</a>, <a href="/search/astro-ph?searchtype=author&query=Strait%2C+V">Victoria Strait</a>, <a href="/search/astro-ph?searchtype=author&query=Treu%2C+T">Tommaso Treu</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">Adriano Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+T">Tucker Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Santini%2C+P">Paola Santini</a>, <a href="/search/astro-ph?searchtype=author&query=Vulcani%2C+B">Benedetta Vulcani</a>, <a href="/search/astro-ph?searchtype=author&query=Acebron%2C+A">Ana Acebron</a>, <a href="/search/astro-ph?searchtype=author&query=Calabr%C3%B2%2C+A">Antonello Calabr貌</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">Marco Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Glazebrook%2C+K">Karl Glazebrook</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">Claudio Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">Amata Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Nanayakkara%2C+T">Themiya Nanayakkara</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">Piero Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Tubthong%2C+C">Chanita Tubthong</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">Eros Vanzella</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="2207.13625v1-abstract-short" style="display: inline;"> How passive galaxies form, and the physical mechanisms which prevent star formation over long timescales, are some of the most outstanding questions in understanding galaxy evolution. The properties of quiescent galaxies over cosmic time provide crucial information to identify the quenching mechanisms. Passive galaxies have been confirmed and studied out to $z\sim4$, but all of these studies have… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.13625v1-abstract-full').style.display = 'inline'; document.getElementById('2207.13625v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.13625v1-abstract-full" style="display: none;"> How passive galaxies form, and the physical mechanisms which prevent star formation over long timescales, are some of the most outstanding questions in understanding galaxy evolution. The properties of quiescent galaxies over cosmic time provide crucial information to identify the quenching mechanisms. Passive galaxies have been confirmed and studied out to $z\sim4$, but all of these studies have been limited to massive systems (mostly with $\log{(M_{\rm star}/M_{\odot})}>10.8$). Using James Webb Space Telescope (JWST) NIRISS grism slitless spectroscopic data from the GLASS JWST ERS program, we present spectroscopic confirmation of two quiescent galaxies at $z_{\rm spec}=2.650^{+0.004}_{-0.006}$ and $z_{\rm spec}=2.433^{+0.032}_{-0.016}$ (3$蟽$ errors) with stellar masses of $\log{(M_{\rm star}/M_{\odot})}=10.53^{+0.18}_{-0.06}$ and $\log{(M_{\rm star}/M_{\odot})}=9.93^{+0.06}_{-0.07}$ (corrected for magnification factors of $渭=2.0$ and $渭=2.1$, respectively). The latter represents the first spectroscopic confirmation of the existence of low-mass quiescent galaxies at cosmic noon, showcasing the power of JWST to identify and characterize this enigmatic population. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.13625v1-abstract-full').style.display = 'none'; document.getElementById('2207.13625v1-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 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to ApJL. 8 pages, 3 figures, 1 table</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.13459">arXiv:2207.13459</a> <span> [<a href="https://arxiv.org/pdf/2207.13459">pdf</a>, <a href="https://arxiv.org/format/2207.13459">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/ac9f17">10.3847/2041-8213/ac9f17 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Early results from GLASS-JWST. VI: Extreme rest-optical equivalent widths detected in NIRISS Wide Field Slitless Spectroscopy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Boyett%2C+K">K. Boyett</a>, <a href="/search/astro-ph?searchtype=author&query=Mascia%2C+S">S. Mascia</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Leethochawalit%2C+N">N. Leethochawalit</a>, <a href="/search/astro-ph?searchtype=author&query=Trenti%2C+M">M. Trenti</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">G. Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Roberts-Borsani%2C+G">G. Roberts-Borsani</a>, <a href="/search/astro-ph?searchtype=author&query=Strait%2C+V">V. Strait</a>, <a href="/search/astro-ph?searchtype=author&query=Treu%2C+T">T. Treu</a>, <a href="/search/astro-ph?searchtype=author&query=Bradac%2C+M">M. Bradac</a>, <a href="/search/astro-ph?searchtype=author&query=Glazebrook%2C+K">K. Glazebrook</a>, <a href="/search/astro-ph?searchtype=author&query=Acebron%2C+A">A. Acebron</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">P. Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Calabro%60%2C+A">A. Calabro`</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=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Henry%2C+A">A. Henry</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+T">T. Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Marchesini%2C+D">D. Marchesini</a>, <a href="/search/astro-ph?searchtype=author&query=Mason%2C+C">C. Mason</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">A. Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Morishita%2C+T">T. Morishita</a>, <a href="/search/astro-ph?searchtype=author&query=Nanayakkara%2C+T">T. Nanayakkara</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</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="2207.13459v1-abstract-short" style="display: inline;"> Wide Field Slitless Spectroscopy (WFSS) provides a powerful tool for detecting strong line emission in star forming galaxies (SFGs) without the need for target pre-selection. As part of the GLASS-JWST-ERS program, we leverage the near-infrared wavelength capabilities of NIRISS ($1-2.2渭$m) to observe rest-optical emission lines out to $\rm{z}\sim 3.4$, to a depth and with a spatial resolution highe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.13459v1-abstract-full').style.display = 'inline'; document.getElementById('2207.13459v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.13459v1-abstract-full" style="display: none;"> Wide Field Slitless Spectroscopy (WFSS) provides a powerful tool for detecting strong line emission in star forming galaxies (SFGs) without the need for target pre-selection. As part of the GLASS-JWST-ERS program, we leverage the near-infrared wavelength capabilities of NIRISS ($1-2.2渭$m) to observe rest-optical emission lines out to $\rm{z}\sim 3.4$, to a depth and with a spatial resolution higher than ever before (H$伪$ to z<2.4; [OIII]+H$尾$ to z<3.4). In this letter we constrain the rest-frame [OIII]$\lambda5007$ equivalent width (EW) distribution for a sample of 76 $1<\rm{z}<3.4$ SFGs in the Abell 2744 Hubble Frontier Field and determine an abundance fraction of extreme emission line galaxies with EW$>750$A in our sample to be $12\%$. We determine a strong correlation between the measured H$尾$ and [OIII]$\lambda5007$ EWs, supporting that the high [OIII]$\lambda5007$ EW objects require massive stars in young stellar populations to generate the high energy photons needed to doubly ionise oxygen. We extracted spectra for objects up to 2 mag fainter in the near-infrared than previous WFSS studies with the Hubble Space Telescope. Thus, this work clearly highlights the potential of JWST/NIRISS to provide high quality WFSS datasets in crowded cluster environments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.13459v1-abstract-full').style.display = 'none'; document.getElementById('2207.13459v1-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 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">9 pages, 3 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/2207.11387">arXiv:2207.11387</a> <span> [<a href="https://arxiv.org/pdf/2207.11387">pdf</a>, <a href="https://arxiv.org/format/2207.11387">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/ac8e6e">10.3847/2041-8213/ac8e6e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Early Results from GLASS-JWST. I: Confirmation of Lensed $z\geqslant7$ Lyman-Break Galaxies Behind the Abell 2744 Cluster With NIRISS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Roberts-Borsani%2C+G">Guido Roberts-Borsani</a>, <a href="/search/astro-ph?searchtype=author&query=Morishita%2C+T">Takahiro Morishita</a>, <a href="/search/astro-ph?searchtype=author&query=Treu%2C+T">Tommaso Treu</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">Gabriel Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Strait%2C+V">Victoria Strait</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+X">Xin Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Bradac%2C+M">Marusa Bradac</a>, <a href="/search/astro-ph?searchtype=author&query=Acebron%2C+A">Ana Acebron</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">Pietro Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Boyett%2C+K">Kristan Boyett</a>, <a href="/search/astro-ph?searchtype=author&query=Calabr%C3%B3%2C+A">Antonello Calabr贸</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">Marco Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">Adriano Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Glazebrook%2C+K">Karl Glazebrook</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">Claudio Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Henry%2C+A">Alaina Henry</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+T">Tucker Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Malkan%2C+M">Matthew Malkan</a>, <a href="/search/astro-ph?searchtype=author&query=Marchesini%2C+D">Danilo Marchesini</a>, <a href="/search/astro-ph?searchtype=author&query=Mascia%2C+S">Sara Mascia</a>, <a href="/search/astro-ph?searchtype=author&query=Mason%2C+C">Charlotte Mason</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">Amata Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Merlin%2C+E">Emiliano Merlin</a>, <a href="/search/astro-ph?searchtype=author&query=Nanayakkara%2C+T">Themiya Nanayakkara</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">Laura Pentericci</a> , et al. (7 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2207.11387v2-abstract-short" style="display: inline;"> We present the first search for $z\geqslant7$, continuum-confirmed sources with NIRISS/WFS spectroscopy over the Abell 2744 Frontier Fields cluster, as part of the GLASS-JWST ERS survey. With $\sim15$ hrs of pre-imaging and multi-angle grism exposures in the F115W, F150W, and F200W filters, we describe the general data handling (i.e., reduction, cleaning, modeling, and extraction processes) and an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.11387v2-abstract-full').style.display = 'inline'; document.getElementById('2207.11387v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.11387v2-abstract-full" style="display: none;"> We present the first search for $z\geqslant7$, continuum-confirmed sources with NIRISS/WFS spectroscopy over the Abell 2744 Frontier Fields cluster, as part of the GLASS-JWST ERS survey. With $\sim15$ hrs of pre-imaging and multi-angle grism exposures in the F115W, F150W, and F200W filters, we describe the general data handling (i.e., reduction, cleaning, modeling, and extraction processes) and analysis for the GLASS-JWST survey. We showcase the power of JWST to peer deep into reionization, when most intergalactic hydrogen is neutral, by confirming two galaxies at $z=8.04\pm0.15$ and $z=7.90\pm0.13$ by means of their Lyman breaks. Fainter continuum spectra are observed in both the F150W and F200W bands, indicative of blue ($-1.69$ and $-1.33$) UV slopes and moderately-bright absolute magnitudes ($-20.37$ and $-19.68$ mag). We do not detect strong Ly$伪$ in either galaxy, but do observe tentative ($\sim2.7-3.8蟽$) HeII$位$1640 A, OIII]$位位$1661,1666 A, and NIII]$位位$1747,1749 A line emission in one, suggestive of low metallicity, star-forming systems with possible non-thermal contributions. These novel observations provide a first look at the extraordinary potential of JWST/NIRISS for confirming representative samples of bright $z\geqslant7$ sources in the absence of strong emission lines, and gain unprecedented insight into their contributions towards cosmic reionization. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.11387v2-abstract-full').style.display = 'none'; document.getElementById('2207.11387v2-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 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">Accepted for publication in ApJL on 1st September 2022, after minor modifications based on the referee report. 10 pages, 3 figures, 1 table</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.09416">arXiv:2207.09416</a> <span> [<a href="https://arxiv.org/pdf/2207.09416">pdf</a>, <a href="https://arxiv.org/format/2207.09416">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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/10.1051/0004-6361/202244575">10.1051/0004-6361/202244575 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> New high-precision strong lensing modeling of Abell 2744. Preparing for JWST observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">P. Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Acebron%2C+A">A. Acebron</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Caminha%2C+G+B">G. B. Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">A. Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Angora%2C+G">G. Angora</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">G. Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">M. Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">M. Nonino</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="2207.09416v1-abstract-short" style="display: inline;"> We present a new strong lensing (SL) model of the Hubble Frontier Fields galaxy cluster Abell 2744, at z=0.3072, by exploiting archival Hubble Space Telescope (HST) multi-band imaging and Multi Unit Spectroscopic Explorer (MUSE) follow-up spectroscopy. The lens model considers 90 spectroscopically confirmed multiple images (from 30 background sources), which represents the largest secure sample fo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.09416v1-abstract-full').style.display = 'inline'; document.getElementById('2207.09416v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.09416v1-abstract-full" style="display: none;"> We present a new strong lensing (SL) model of the Hubble Frontier Fields galaxy cluster Abell 2744, at z=0.3072, by exploiting archival Hubble Space Telescope (HST) multi-band imaging and Multi Unit Spectroscopic Explorer (MUSE) follow-up spectroscopy. The lens model considers 90 spectroscopically confirmed multiple images (from 30 background sources), which represents the largest secure sample for this cluster field prior to the recently acquired James Webb Space Telescope observations. The inclusion of the sub-structures within several extended sources as model constraints allows us to accurately characterize the inner total mass distribution of the cluster and the position of the cluster critical lines. We include the lensing contribution of 225 cluster members, 202 of which are spectroscopically confirmed. We also measure the internal velocity dispersion of 85 cluster galaxies to independently estimate the role of the subhalo mass component in the lens model. We investigate the effect of the cluster environment on the total mass reconstruction of the cluster core with two different mass parameterizations. We consider the mass contribution from three external clumps, either based on previous weak-lensing studies, or extended HST imaging of luminous members around the cluster core. In the latter case, the observed positions of the multiple images are better reproduced, with a remarkable accuracy of 0.37", a factor of $\sim2$ smaller than previous lens models. We develop and make publicly available a Strong Lensing Online Tool (SLOT) to exploit the predictive power and the full statistical information of this and future models, through a simple graphical interface. We plan to apply our high-precision SL model to the first analysis of the GLASS-JWST-ERS program, specifically to measure the intrinsic physical properties of high-$z$ galaxies from robust magnification maps. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.09416v1-abstract-full').style.display = 'none'; document.getElementById('2207.09416v1-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 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">14 pages, 9 figures, 4 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 670, A60 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.07567">arXiv:2207.07567</a> <span> [<a href="https://arxiv.org/pdf/2207.07567">pdf</a>, <a href="https://arxiv.org/format/2207.07567">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202244517">10.1051/0004-6361/202244517 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First JWST observations of a gravitational lens: Mass model from new multiple images with near-infrared observations of SMACS J0723.3-7327 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Caminha%2C+G+B">G. B. Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Suyu%2C+S+H">S. H. Suyu</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">A. Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">G. Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">P. Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Acebron%2C+A">A. Acebron</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="2207.07567v3-abstract-short" style="display: inline;"> We present our lens mass model of SMACS J0723, the first strong gravitational lens observed by the James Webb Space Telescope (JWST). We use data from the Hubble Space Telescope and Multi Unit Spectroscopic Explorer (MUSE) to build our 'pre-JWST' lens model, and refine it with newly available JWST near-infrared imaging in our JWST model. To reproduce the positions of all multiple lensed images wit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.07567v3-abstract-full').style.display = 'inline'; document.getElementById('2207.07567v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.07567v3-abstract-full" style="display: none;"> We present our lens mass model of SMACS J0723, the first strong gravitational lens observed by the James Webb Space Telescope (JWST). We use data from the Hubble Space Telescope and Multi Unit Spectroscopic Explorer (MUSE) to build our 'pre-JWST' lens model, and refine it with newly available JWST near-infrared imaging in our JWST model. To reproduce the positions of all multiple lensed images with good accuracy, the adopted mass parameterization consists of one cluster-scale component, accounting mainly for the dark matter distribution, the galaxy cluster members and an external shear component. The pre-JWST model has, as constraints, 19 multiple images from six background sources, of which four have secure spectroscopic redshift measurements from this work. The JWST model has more than twice the number of constraints, 30 additional multiple images from another eleven lensed sources. Both models can reproduce very well the multiple image positions with a $未_{rms}$ of $0.39''$ and $0.51''$, for the pre-JWST and JWST models, respectively. The total mass estimates within a radius of 128~kpc (~ the Einstein radius) are $7.9_{-0.2}^{+0.3}\times 10^{13}\rm M_{\odot}$ and $8.7_{-0.2}^{+0.2}\times 10^{13}\rm M_{\odot}$, for the pre-JWST and JWST models, respectively. We predict with our mass models the redshifts of the newly detected JWST sources, which are crucial information for systems without spectroscopic measurements for further studies and follow-up observations. Interestingly, one family detected with JWST is found to be at a very high redshift, $z>7.5$ (68% confidence level) and with one image having lensing magnification of $|渭|=9.5_{-0.8}^{+0.9}$, making it an interesting case for future studies. The lens models, including magnification maps and redshifts estimated from the model are made publicly available, along with the full spectroscopic redshift catalogue from MUSE. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.07567v3-abstract-full').style.display = 'none'; document.getElementById('2207.07567v3-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> 13 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">5 pages, 2 figures, 1 table, plus appendix. Published in A&A Letters. Lens model and redshift catalogue available at: http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/666/L9</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 666, L9 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.07978">arXiv:2206.07978</a> <span> [<a href="https://arxiv.org/pdf/2206.07978">pdf</a>, <a href="https://arxiv.org/format/2206.07978">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/10.3847/1538-4357/ac8158">10.3847/1538-4357/ac8158 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The GLASS James Webb Space Telescope Early Release Science Program. I. Survey Design and Release Plans </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Treu%2C+T">T. Treu</a>, <a href="/search/astro-ph?searchtype=author&query=Roberts-Borsani%2C+G">G. Roberts-Borsani</a>, <a href="/search/astro-ph?searchtype=author&query=Bradac%2C+M">M. Bradac</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">G. Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">A. Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Henry%2C+A">A. Henry</a>, <a href="/search/astro-ph?searchtype=author&query=Mason%2C+C">C. Mason</a>, <a href="/search/astro-ph?searchtype=author&query=Morishita%2C+T">T. Morishita</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+X">X. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Acebron%2C+A">A. Acebron</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M">M. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">P. Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Belfiori%2C+D">D. Belfiori</a>, <a href="/search/astro-ph?searchtype=author&query=Bonchi%2C+A">A. Bonchi</a>, <a href="/search/astro-ph?searchtype=author&query=Boyett%2C+K">K. Boyett</a>, <a href="/search/astro-ph?searchtype=author&query=Boutsia%2C+K">K. Boutsia</a>, <a href="/search/astro-ph?searchtype=author&query=Calabro%2C+A">A. Calabro</a>, <a href="/search/astro-ph?searchtype=author&query=Caminha%2C+G+B">G. B. Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Dressler%2C+A">A. Dressler</a>, <a href="/search/astro-ph?searchtype=author&query=Glazebrook%2C+K">K. Glazebrook</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Jacobs%2C+C">C. Jacobs</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+T">T. Jones</a> , et al. (21 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="2206.07978v2-abstract-short" style="display: inline;"> The GLASS James Webb Space Telescope Early Release Science (hereafter GLASS-JWST-ERS) Program will obtain and make publicly available the deepest extragalactic data of the ERS campaign. It is primarily designed to address two key science questions, namely, "what sources ionized the universe and when?" and "how do baryons cycle through galaxies?", while also enabling a broad variety of first look s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.07978v2-abstract-full').style.display = 'inline'; document.getElementById('2206.07978v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.07978v2-abstract-full" style="display: none;"> The GLASS James Webb Space Telescope Early Release Science (hereafter GLASS-JWST-ERS) Program will obtain and make publicly available the deepest extragalactic data of the ERS campaign. It is primarily designed to address two key science questions, namely, "what sources ionized the universe and when?" and "how do baryons cycle through galaxies?", while also enabling a broad variety of first look scientific investigations. In primary mode, it will obtain NIRISS and NIRSpec spectroscopy of galaxies lensed by the foreground Hubble Frontier Field cluster, Abell 2744. In parallel, it will use NIRCam to observe two fields that are offset from the cluster center, where lensing magnification is negligible, and which can thus be effectively considered blank fields. In order to prepare the community for access to this unprecedented data, we describe the scientific rationale, the survey design (including target selection and observational setups), and present pre-commissioning estimates of the expected sensitivity. In addition, we describe the planned public releases of high-level data products, for use by the wider astronomical community. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.07978v2-abstract-full').style.display = 'none'; document.getElementById('2206.07978v2-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 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">23 pages, 10 figures; ApJ 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/2204.09067">arXiv:2204.09067</a> <span> [<a href="https://arxiv.org/pdf/2204.09067">pdf</a>, <a href="https://arxiv.org/format/2204.09067">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243651">10.1051/0004-6361/202243651 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxies in the central regions of simulated galaxy clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ragagnin%2C+A">Antonio Ragagnin</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">Massimo Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Bassini%2C+L">Luigi Bassini</a>, <a href="/search/astro-ph?searchtype=author&query=Ragone-Figueroa%2C+C">Cinthia Ragone-Figueroa</a>, <a href="/search/astro-ph?searchtype=author&query=Granato%2C+G+L">Gian Luigi Granato</a>, <a href="/search/astro-ph?searchtype=author&query=Despali%2C+G">Giulia Despali</a>, <a href="/search/astro-ph?searchtype=author&query=Giocoli%2C+C">Carlo Giocoli</a>, <a href="/search/astro-ph?searchtype=author&query=Granata%2C+G">Giovanni Granata</a>, <a href="/search/astro-ph?searchtype=author&query=Moscardini%2C+L">Lauro Moscardini</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">Pietro Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Rasia%2C+E">Elena Rasia</a>, <a href="/search/astro-ph?searchtype=author&query=Valentini%2C+M">Milena Valentini</a>, <a href="/search/astro-ph?searchtype=author&query=Borgani%2C+S">Stefano Borgani</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">Francesco Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Dolag%2C+K">Klaus Dolag</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">Claudio Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">Amata Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Murante%2C+G">Giuseppe Murante</a>, <a href="/search/astro-ph?searchtype=author&query=Natarajan%2C+P">Priyamvada Natarajan</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">Piero Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Taffoni%2C+G">Giuliano Taffoni</a>, <a href="/search/astro-ph?searchtype=author&query=Tornatore%2C+L">Luca Tornatore</a>, <a href="/search/astro-ph?searchtype=author&query=Tortorelli%2C+L">Luca Tortorelli</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="2204.09067v1-abstract-short" style="display: inline;"> In this paper, we assess the impact of numerical resolution and of the implementation of energy input from AGN feedback models on the inner structure of cluster sub-haloes in hydrodynamic simulations. We compare several zoom-in re-simulations of a sub-sample of the cluster-sized haloes studied in Meneghetti et al. (2020), obtained by varying mass resolution, softening length and AGN energy feedbac… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.09067v1-abstract-full').style.display = 'inline'; document.getElementById('2204.09067v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.09067v1-abstract-full" style="display: none;"> In this paper, we assess the impact of numerical resolution and of the implementation of energy input from AGN feedback models on the inner structure of cluster sub-haloes in hydrodynamic simulations. We compare several zoom-in re-simulations of a sub-sample of the cluster-sized haloes studied in Meneghetti et al. (2020), obtained by varying mass resolution, softening length and AGN energy feedback scheme. We study the impact of these different setups on the subhalo abundances, their radial distribution, their density and mass profiles and the relation between the maximum circular velocity, which is a proxy for subhalo compactness. Regardless of the adopted numerical resolution and feedback model, subhaloes with masses Msub < 1e11Msun/h, the most relevant mass-range for galaxy-galaxy strong lensing, have maximum circular velocities ~30% smaller than those measured from strong lensing observations of Bergamini et al. (2019). We also find that simulations with less effective AGN energy feedback produce massive subhaloes (Msub> 1e11 Msun/h ) with higher maximum circular velocity and that their Vmax - Msub relation approaches the observed one. However the stellar-mass number count of these objects exceeds the one found in observations and we find that the compactness of these simulated subhaloes is the result of an extremely over-efficient star formation in their cores, also leading to larger-than-observed subhalo stellar mass. We conclude that simulations are unable to simultaneously reproduce the observed stellar masses and compactness (or maximum circular velocities) of cluster galaxies. Thus, the discrepancy between theory and observations that emerged from the analysis of Meneghetti et al. (2020) persists. It remains an open question as to whether such a discrepancy reflects limitations of the current implementation of galaxy formation models or the LCDM paradigm. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.09067v1-abstract-full').style.display = 'none'; document.getElementById('2204.09067v1-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 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">11 pages, 10 figures, abstract is redacted to fit arXiv character count limit</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 665, A16 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.09065">arXiv:2204.09065</a> <span> [<a href="https://arxiv.org/pdf/2204.09065">pdf</a>, <a href="https://arxiv.org/format/2204.09065">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243779">10.1051/0004-6361/202243779 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The probability of galaxy-galaxy strong lensing events in hydrodynamical simulations of galaxy clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">Massimo Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Ragagnin%2C+A">Antonio Ragagnin</a>, <a href="/search/astro-ph?searchtype=author&query=Borgani%2C+S">Stefano Borgani</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">Francesco Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Despali%2C+G">Giulia Despali</a>, <a href="/search/astro-ph?searchtype=author&query=Giocoli%2C+C">Carlo Giocoli</a>, <a href="/search/astro-ph?searchtype=author&query=Granato%2C+G+L">Gian Luigi Granato</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">Claudio Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Moscardini%2C+L">Lauro Moscardini</a>, <a href="/search/astro-ph?searchtype=author&query=Rasia%2C+E">Elena Rasia</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">Piero Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Angora%2C+G">Giuseppe Angora</a>, <a href="/search/astro-ph?searchtype=author&query=Bassini%2C+L">Luigi Bassini</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">Pietro Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Caminha%2C+G+B">Gabriel B. Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Granata%2C+G">Giovanni Granata</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">Amata Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Metcalf%2C+R+B">Robert Benton Metcalf</a>, <a href="/search/astro-ph?searchtype=author&query=Natarajan%2C+P">Priyamvada Natarajan</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">Mario Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Pignataro%2C+G+V">Giada Venusta Pignataro</a>, <a href="/search/astro-ph?searchtype=author&query=Ragone-Figueroa%2C+C">Cinthia Ragone-Figueroa</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">Eros Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Acebron%2C+A">Ana Acebron</a>, <a href="/search/astro-ph?searchtype=author&query=Dolag%2C+K">Klaus Dolag</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="2204.09065v1-abstract-short" style="display: inline;"> Meneghetti et al. (2020) recently reported an excess of galaxy-galaxy strong lensing (GGSL) in galaxy clusters compared to expectations from the LCDM cosmological model. Theoretical estimates of the GGSL probability are based on the analysis of numerical hydrodynamical simulations in the LCDM cosmology. We quantify the impact of the numerical resolution and AGN feedback scheme adopted in cosmologi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.09065v1-abstract-full').style.display = 'inline'; document.getElementById('2204.09065v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.09065v1-abstract-full" style="display: none;"> Meneghetti et al. (2020) recently reported an excess of galaxy-galaxy strong lensing (GGSL) in galaxy clusters compared to expectations from the LCDM cosmological model. Theoretical estimates of the GGSL probability are based on the analysis of numerical hydrodynamical simulations in the LCDM cosmology. We quantify the impact of the numerical resolution and AGN feedback scheme adopted in cosmological simulations on the predicted GGSL probability and determine if varying these simulation properties can alleviate the gap with observations. We repeat the analysis of Meneghetti et al. (2020) on cluster-size halos simulated with different mass and force resolutions and implementing several independent AGN feedback schemes. We find that improving the mass resolution by a factor of ten and twenty-five, while using the same galaxy formation model that includes AGN feedback, does not affect the GGSL probability. We find similar results regarding the choice of gravitational softening. On the contrary, adopting an AGN feedback scheme that is less efficient at suppressing gas cooling and star formation leads to an increase in the GGSL probability by a factor between three and six. However, we notice that such simulations form overly massive subhalos whose contribution to the lensing cross-section would be significant while their Einstein radii are too large to be consistent with the observations. The primary contributors to the observed GGSL cross-sections are subhalos with smaller masses, that are compact enough to become critical for lensing. The population with these required characteristics appears to be absent in simulations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.09065v1-abstract-full').style.display = 'none'; document.getElementById('2204.09065v1-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 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">13 pages, 11 figures. Submitted for publication on Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 668, A188 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.09377">arXiv:2202.09377</a> <span> [<a href="https://arxiv.org/pdf/2202.09377">pdf</a>, <a href="https://arxiv.org/format/2202.09377">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/10.1093/mnras/stac2309">10.1093/mnras/stac2309 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Exploring the physical properties of lensed star-forming clumps at $2\lesssim z \lesssim6$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Me%C5%A1tri%C4%87%2C+U">U. Me拧tri膰</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Zanella%2C+A">A. Zanella</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">F. Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">P. Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">A. Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">M. Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Caminha%2C+G+B">G. B. Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">M. Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Merlin%2C+E">E. Merlin</a>, <a href="/search/astro-ph?searchtype=author&query=Cupani%2C+G">G. Cupani</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</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="2202.09377v2-abstract-short" style="display: inline;"> We study the physical properties (size, stellar mass, luminosity, star formation rate) and scaling relations for a sample of 166 star-forming clumps with redshift $z \sim 2-6.2$. They are magnified by the Hubble Frontier Field galaxy cluster MACS~J0416 and have robust lensing magnification ($2\lesssim 渭\lesssim 82$) computed by using our high-precision lens model, based on 182 multiple images. Our… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.09377v2-abstract-full').style.display = 'inline'; document.getElementById('2202.09377v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.09377v2-abstract-full" style="display: none;"> We study the physical properties (size, stellar mass, luminosity, star formation rate) and scaling relations for a sample of 166 star-forming clumps with redshift $z \sim 2-6.2$. They are magnified by the Hubble Frontier Field galaxy cluster MACS~J0416 and have robust lensing magnification ($2\lesssim 渭\lesssim 82$) computed by using our high-precision lens model, based on 182 multiple images. Our sample extends by $\sim 3$ times the number of spectroscopically-confirmed lensed clumps at $z \gtrsim 2$. We identify clumps in ultraviolet continuum images and find that, whenever the effective spatial resolution (enhanced by gravitational lensing) increases, they fragment into smaller entities, likely reflecting the hierarchically-organized nature of star formation. Kpc-scale clumps, most commonly observed in field, are not found in our sample. The physical properties of our sample extend the parameter space typically probed by $z \gtrsim 1$ field observations and simulations, by populating the low mass (M$_\star \lesssim 10^7$ M$_\odot$), low star formation rate (SFR $\lesssim 0.5$ M$_\odot$ yr$^{-1}$), and small size (R$_\mathrm{eff} \lesssim 100$ pc) regime. The new domain probed by our study approaches the regime of compact stellar complexes and star clusters. In the mass-size plane, our sample spans the region between galaxies and globular clusters, with a few clumps in the region populated by young star clusters and globular-clusters. For the bulk of our sample, we measure star-formation rates which are higher than those observed locally in compact stellar systems, indicating different conditions for star formation at high redshift than in the local Universe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.09377v2-abstract-full').style.display = 'none'; document.getElementById('2202.09377v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">25 pages, 20 figures, 3 table. Accepted to publication in MNRAS</span> </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Bergamini%2C+P&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Bergamini%2C+P&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Bergamini%2C+P&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> </ul> </nav> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div 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