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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=Caminha%2C+G+B&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Caminha%2C+G+B&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Caminha%2C+G+B&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Caminha%2C+G+B&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </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/2411.07289">arXiv:2411.07289</a> <span> [<a href="https://arxiv.org/pdf/2411.07289">pdf</a>, <a href="https://arxiv.org/format/2411.07289">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"> Cosmography from accurate mass modeling of the lens group SDSS J0100+1818: five sources at three different redshifts </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=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=Granata%2C+G">G. Granata</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=Ca%C3%B1ameras%2C+R">R. Ca帽ameras</a>, <a href="/search/astro-ph?searchtype=author&query=Christensen%2C+L">L. Christensen</a>, <a href="/search/astro-ph?searchtype=author&query=Vernet%2C+J">J. Vernet</a>, <a href="/search/astro-ph?searchtype=author&query=Zanella%2C+A">A. Zanella</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.07289v1-abstract-short" style="display: inline;"> Systems where multiple sources at different redshifts are strongly lensed by the same deflector allow one to directly investigate the evolution of the angular diameter distances with redshift, and thus to learn about the geometry of the Universe. We present measurements of the values of the total matter density, $惟_m$, and of the dark energy equation of state parameter, $w$, through a strong lensi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.07289v1-abstract-full').style.display = 'inline'; document.getElementById('2411.07289v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.07289v1-abstract-full" style="display: none;"> Systems where multiple sources at different redshifts are strongly lensed by the same deflector allow one to directly investigate the evolution of the angular diameter distances with redshift, and thus to learn about the geometry of the Universe. We present measurements of the values of the total matter density, $惟_m$, and of the dark energy equation of state parameter, $w$, through a strong lensing analysis of SDSSJ0100+1818, a group-scale system at $z=0.581$ with five lensed sources, from $z=1.698$ to $4.95$. We use new MUSE data to securely measure the redshift of 65 sources, including the five multiply imaged background sources (lensed into a total of 18 multiple images) and 19 galaxies on the deflector plane (the brightest group galaxy, BGG, and 18 fainter members), all employed to build robust strong lensing models with the software GLEE. We measure $惟_m = 0.14^{+0.16}_{-0.09}$ in a flat $螞$ cold dark matter (CDM) model, and $惟_m = 0.19^{+0.17}_{-0.10}$ and $w=-1.27_{-0.48}^{+0.43}$ in a flat $w$CDM model. We quantify, through a multi-plane approach, the impact of different sources angularly close in projection on the inferred values of the cosmological parameters. We obtain consistent median values, with uncertainties for only $惟_m$ increasing by a factor of 1.5. We accurately measure a total mass of $(1.55 \pm 0.01) \times 10^{13}$ M$_\odot$ within 50 kpc and a stellar over total mass profile decreasing from $45.6^{+8.7}_{-8.3}\%$ at the BGG effective radius to $(6.6\pm 1.1)\%$ at $R\approx 77$ kpc. Our results confirm that SDSSJ0100+1818 is one of the most massive (lens) galaxies known at intermediate redshift and that group-scale systems that act as lenses for $\geq 3$ background sources at different redshifts enable to estimate the values of the cosmological parameters with an accuracy that is competitive with that obtained from lens galaxy clusters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.07289v1-abstract-full').style.display = 'none'; document.getElementById('2411.07289v1-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 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A. 14 pages, 10 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/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/2404.13205">arXiv:2404.13205</a> <span> [<a href="https://arxiv.org/pdf/2404.13205">pdf</a>, <a href="https://arxiv.org/format/2404.13205">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/10.1051/0004-6361/202449910">10.1051/0004-6361/202449910 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Strong-lensing and kinematic analysis of CASSOWARY 31: can strong lensing constrain the masses of multi-plane lenses? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wang%2C+H">H. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Canameras%2C+R">R. Canameras</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=Galan%2C+A">A. Galan</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=Christensen%2C+L">L. Christensen</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.13205v3-abstract-short" style="display: inline;"> We present a mass measurement for the secondary lens along the line of sight (LoS) in the multi-plane strong lens modeling of the group-scale lens CASSOWARY 31 (CSWA 31). The secondary lens at redshift $z = 1.49$ is a spiral galaxy well aligned along the LoS with the main lens at $z = 0.683$. Using the MUSE integral-field spectroscopy of this spiral galaxy, we measure its rotation velocities and d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.13205v3-abstract-full').style.display = 'inline'; document.getElementById('2404.13205v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.13205v3-abstract-full" style="display: none;"> We present a mass measurement for the secondary lens along the line of sight (LoS) in the multi-plane strong lens modeling of the group-scale lens CASSOWARY 31 (CSWA 31). The secondary lens at redshift $z = 1.49$ is a spiral galaxy well aligned along the LoS with the main lens at $z = 0.683$. Using the MUSE integral-field spectroscopy of this spiral galaxy, we measure its rotation velocities and determine the mass from the gas kinematics. We compare the mass estimation of the secondary lens from the lensing models to the mass measurement from kinematics, finding that the predictions from strong lensing tend to be higher. By introducing an additional lens plane at $z = 1.36$ for an overdensity known to be present, we find a mass of $\simeq 10^{10}$ M$_\odot$ enclosed within 3.3 kpc from the centroid of the spiral galaxy, approaching the estimate from kinematics. This shows that secondary-lens mass measurements from multiple-plane modeling are affected by systematic uncertainties from the degeneracies between lens planes and the complex LoS structure. Conducting a detailed analysis of the LoS structures is therefore essential to improve the mass measurement of the secondary lens. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.13205v3-abstract-full').style.display = 'none'; document.getElementById('2404.13205v3-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 9 figures, 1 table, accepted for publication in Astronomy & Astrophysics. We welcome the comments from readers</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 690, A1 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.02139">arXiv:2404.02139</a> <span> [<a href="https://arxiv.org/pdf/2404.02139">pdf</a>, <a href="https://arxiv.org/format/2404.02139">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/10.3847/2041-8213/ad4648">10.3847/2041-8213/ad4648 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Lensed Type Ia Supernova "Encore" at z=2: The First Instance of Two Multiply-Imaged Supernovae in the Same Host Galaxy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pierel%2C+J+D+R">J. D. R. Pierel</a>, <a href="/search/astro-ph?searchtype=author&query=Newman%2C+A+B">A. B. Newman</a>, <a href="/search/astro-ph?searchtype=author&query=Dhawan%2C+S">S. Dhawan</a>, <a href="/search/astro-ph?searchtype=author&query=Gu%2C+M">M. Gu</a>, <a href="/search/astro-ph?searchtype=author&query=Joshi%2C+B+A">B. A. Joshi</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+T">T. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Schuldt%2C+S">S. Schuldt</a>, <a href="/search/astro-ph?searchtype=author&query=Strolger%2C+L+G">L. G. Strolger</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=Caminha%2C+G+B">G. B. Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+S+H">S. H. Cohen</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=Dsilva%2C+J+C+J">J. C. J. Dsilva</a>, <a href="/search/astro-ph?searchtype=author&query=Ertl%2C+S">S. Ertl</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=Granata%2C+G">G. Granata</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">A. M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+J">J. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Robotham%2C+A">A. Robotham</a>, <a href="/search/astro-ph?searchtype=author&query=Summers%2C+J">J. Summers</a>, <a href="/search/astro-ph?searchtype=author&query=Treu%2C+T">T. Treu</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=Zitrin%2C+A">A. Zitrin</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+S">S. Agarwal</a> , et al. (38 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.02139v3-abstract-short" style="display: inline;"> A bright ($m_{\rm F150W,AB}$=24 mag), $z=1.95$ supernova (SN) candidate was discovered in JWST/NIRCam imaging acquired on 2023 November 17. The SN is quintuply-imaged as a result of strong gravitational lensing by a foreground galaxy cluster, detected in three locations, and remarkably is the second lensed SN found in the same host galaxy. The previous lensed SN was called "Requiem", and therefore… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.02139v3-abstract-full').style.display = 'inline'; document.getElementById('2404.02139v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.02139v3-abstract-full" style="display: none;"> A bright ($m_{\rm F150W,AB}$=24 mag), $z=1.95$ supernova (SN) candidate was discovered in JWST/NIRCam imaging acquired on 2023 November 17. The SN is quintuply-imaged as a result of strong gravitational lensing by a foreground galaxy cluster, detected in three locations, and remarkably is the second lensed SN found in the same host galaxy. The previous lensed SN was called "Requiem", and therefore the new SN is named "Encore". This makes the MACS J0138.0$-$2155 cluster the first known system to produce more than one multiply-imaged SN. Moreover, both SN Requiem and SN Encore are Type Ia SNe (SNe Ia), making this the most distant case of a galaxy hosting two SNe Ia. Using parametric host fitting, we determine the probability of detecting two SNe Ia in this host galaxy over a $\sim10$ year window to be $\approx3\%$. These observations have the potential to yield a Hubble Constant ($H_0$) measurement with $\sim10\%$ precision, only the third lensed SN capable of such a result, using the three visible images of the SN. Both SN Requiem and SN Encore have a fourth image that is expected to appear within a few years of $\sim2030$, providing an unprecedented baseline for time-delay cosmography. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.02139v3-abstract-full').style.display = 'none'; document.getElementById('2404.02139v3-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted, 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/2403.18954">arXiv:2403.18954</a> <span> [<a href="https://arxiv.org/pdf/2403.18954">pdf</a>, <a href="https://arxiv.org/format/2403.18954">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/10.3847/1538-4357/ad3c43">10.3847/1538-4357/ad3c43 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> JWST Photometric Time-Delay and Magnification Measurements for the Triply-Imaged Type Ia "Supernova H0pe" at z = 1.78 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pierel%2C+J+D+R">J. D. R. Pierel</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=Pascale%2C+M">M. Pascale</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=Chen%2C+W">W. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Dhawan%2C+S">S. Dhawan</a>, <a href="/search/astro-ph?searchtype=author&query=Gilman%2C+D">D. Gilman</a>, <a href="/search/astro-ph?searchtype=author&query=Grayling%2C+M">M. Grayling</a>, <a href="/search/astro-ph?searchtype=author&query=Huber%2C+S">S. Huber</a>, <a href="/search/astro-ph?searchtype=author&query=Kelly%2C+P">P. Kelly</a>, <a href="/search/astro-ph?searchtype=author&query=Thorp%2C+S">S. Thorp</a>, <a href="/search/astro-ph?searchtype=author&query=Arendse%2C+N">N. Arendse</a>, <a href="/search/astro-ph?searchtype=author&query=Birrer%2C+S">S. Birrer</a>, <a href="/search/astro-ph?searchtype=author&query=Bronikowski%2C+M">M. Bronikowski</a>, <a href="/search/astro-ph?searchtype=author&query=Canameras%2C+R">R. Canameras</a>, <a href="/search/astro-ph?searchtype=author&query=Coe%2C+D">D. Coe</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+S+H">S. H. Cohen</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=Driver%2C+S+P">S. P. Driver</a>, <a href="/search/astro-ph?searchtype=author&query=Dsilva%2C+J+C+J">J. C. J. Dsilva</a>, <a href="/search/astro-ph?searchtype=author&query=Engesser%2C+M">M. Engesser</a>, <a href="/search/astro-ph?searchtype=author&query=Foo%2C+N">N. Foo</a>, <a href="/search/astro-ph?searchtype=author&query=Gall%2C+C">C. Gall</a>, <a href="/search/astro-ph?searchtype=author&query=Garuda%2C+N">N. Garuda</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a> , et al. (38 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="2403.18954v2-abstract-short" style="display: inline;"> Supernova (SN) H0pe is a gravitationally lensed, triply-imaged, Type Ia SN (SN Ia) discovered in James Webb Space Telescope imaging of the PLCK G165.7+67.0 cluster of galaxies. Well-observed multiply-imaged SNe provide a rare opportunity to constrain the Hubble constant ($H_0$), by measuring the relative time delay between the images and modeling the foreground mass distribution. SN H0pe is locate… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.18954v2-abstract-full').style.display = 'inline'; document.getElementById('2403.18954v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.18954v2-abstract-full" style="display: none;"> Supernova (SN) H0pe is a gravitationally lensed, triply-imaged, Type Ia SN (SN Ia) discovered in James Webb Space Telescope imaging of the PLCK G165.7+67.0 cluster of galaxies. Well-observed multiply-imaged SNe provide a rare opportunity to constrain the Hubble constant ($H_0$), by measuring the relative time delay between the images and modeling the foreground mass distribution. SN H0pe is located at $z=1.783$, and is the first SN Ia with sufficient light curve sampling and long enough time delays for an $H_0$ inference. Here we present photometric time-delay measurements and SN properties of SN H0pe. Using JWST/NIRCam photometry we measure time delays of $螖t_{ab}=-116.6^{+10.8}_{-9.3}$ and $螖t_{cb}=-48.6^{+3.6}_{-4.0}$ observer-frame days relative to the last image to arrive (image 2b; all uncertainties are $1蟽$), which corresponds to a $\sim5.6\%$ uncertainty contribution for $H_0$ assuming $70 \rm{km s^{-1} Mpc^{-1}}$. We also constrain the absolute magnification of each image to $渭_{a}=4.3^{+1.6}_{-1.8}$, $渭_{b}=7.6^{+3.6}_{-2.6}$, $渭_{c}=6.4^{+1.6}_{-1.5}$ by comparing the observed peak near-IR magnitude of SN H0pe to the non-lensed population of SNe Ia. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.18954v2-abstract-full').style.display = 'none'; document.getElementById('2403.18954v2-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 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 in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.18636">arXiv:2402.18636</a> <span> [<a href="https://arxiv.org/pdf/2402.18636">pdf</a>, <a href="https://arxiv.org/format/2402.18636">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1051/0004-6361/202449876">10.1051/0004-6361/202449876 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> El Gordo needs El Anzuelo: Probing the structure of cluster members with multi-band extended arcs in JWST data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Galan%2C+A">A. Galan</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=Knollm%C3%BCller%2C+J">J. Knollm眉ller</a>, <a href="/search/astro-ph?searchtype=author&query=Roth%2C+J">J. Roth</a>, <a href="/search/astro-ph?searchtype=author&query=Suyu%2C+S+H">S. H. Suyu</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="2402.18636v2-abstract-short" style="display: inline;"> Gravitational lensing by galaxy clusters involves hundreds of galaxies over a large redshift range and increases the likelihood of rare phenomena (supernovae, dark substructures, etc.). We present the detailed analysis of \elanz, a prominent quintuply imaged dusty star-forming galaxy ($\zs=2.29$), mainly lensed by three members of the massive galaxy cluster ACT-CL\,J0102$-$4915, also known as \elg… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.18636v2-abstract-full').style.display = 'inline'; document.getElementById('2402.18636v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.18636v2-abstract-full" style="display: none;"> Gravitational lensing by galaxy clusters involves hundreds of galaxies over a large redshift range and increases the likelihood of rare phenomena (supernovae, dark substructures, etc.). We present the detailed analysis of \elanz, a prominent quintuply imaged dusty star-forming galaxy ($\zs=2.29$), mainly lensed by three members of the massive galaxy cluster ACT-CL\,J0102$-$4915, also known as \elgor ($z_{\rm d}=0.87$). We leverage JWST/NIRCam images, which contain lensing features that were unseen in previous HST images, using a Bayesian, multi-wavelength, differentiable and GPU-accelerated modeling framework that combines \herculens (lens modeling) and \nifty (field model and inference) software packages. For one of the deflectors, we complement lensing constraints with stellar kinematics measured from VLT/MUSE data. In our lens model, we explicitly include the mass distribution of the cluster, locally corrected by a constant shear field. We find that the two main deflectors (L1 and L2) have logarithmic mass density slopes steeper than isothermal, with $纬_{\rm L1} = 2.23\pm0.05$ and $纬_{\rm L2} = 2.21\pm0.04$. We argue that such steep density profiles can arise due to tidally truncated mass distributions, which we probe thanks to the cluster lensing boost and the strong asymmetry of the lensing configuration. Moreover, our three-dimensional source model captures most of the surface brightness of the lensed galaxy, revealing a clump with a maximum diameter of $400$ parsecs at the source redshift, visible at wavelengths $位_{\rm rest}\gtrsim0.6$ $渭$m. Finally, we caution on using point-like features within extended arcs to constrain galaxy-scale lens models before securing them with extended arc modeling. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.18636v2-abstract-full').style.display = 'none'; document.getElementById('2402.18636v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 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">27 pages, published in Astronomy & Astrophysics (September 2024)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 689, A304 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.18543">arXiv:2402.18543</a> <span> [<a href="https://arxiv.org/pdf/2402.18543">pdf</a>, <a href="https://arxiv.org/format/2402.18543">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"> Primordial Rotating Disk Composed of $\geq$15 Dense Star-Forming Clumps at Cosmic Dawn </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fujimoto%2C+S">S. Fujimoto</a>, <a href="/search/astro-ph?searchtype=author&query=Ouchi%2C+M">M. Ouchi</a>, <a href="/search/astro-ph?searchtype=author&query=Kohno%2C+K">K. Kohno</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">F. Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Gim%C3%A9nez-Arteaga%2C+C">C. Gim茅nez-Arteaga</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G+B">G. B. Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Furtak%2C+L+J">L. J. Furtak</a>, <a href="/search/astro-ph?searchtype=author&query=Kohandel%2C+M">M. Kohandel</a>, <a href="/search/astro-ph?searchtype=author&query=Oguri%2C+M">M. Oguri</a>, <a href="/search/astro-ph?searchtype=author&query=Pallottini%2C+A">A. Pallottini</a>, <a href="/search/astro-ph?searchtype=author&query=Richard%2C+J">J. Richard</a>, <a href="/search/astro-ph?searchtype=author&query=Zitrin%2C+A">A. Zitrin</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">F. E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Boylan-Kolchin%2C+M">M. Boylan-Kolchin</a>, <a href="/search/astro-ph?searchtype=author&query=Dessauges-Zavadsky%2C+M">M. Dessauges-Zavadsky</a>, <a href="/search/astro-ph?searchtype=author&query=Egami%2C+E">E. Egami</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">S. L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Ma%2C+Z">Z. Ma</a>, <a href="/search/astro-ph?searchtype=author&query=Smail%2C+I">I. Smail</a>, <a href="/search/astro-ph?searchtype=author&query=Watson%2C+D">D. Watson</a>, <a href="/search/astro-ph?searchtype=author&query=Hutchison%2C+T+A">T. A. Hutchison</a>, <a href="/search/astro-ph?searchtype=author&query=Rigby%2C+J+R">J. R. Rigby</a>, <a href="/search/astro-ph?searchtype=author&query=Welch%2C+B+D">B. D. Welch</a>, <a href="/search/astro-ph?searchtype=author&query=Ao%2C+Y">Y. Ao</a>, <a href="/search/astro-ph?searchtype=author&query=Bradley%2C+L+D">L. D. Bradley</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="2402.18543v2-abstract-short" style="display: inline;"> Early galaxy formation, initiated by the dark matter and gas assembly, evolves through frequent mergers and feedback processes into dynamically hot, chaotic structures. In contrast, dynamically cold, smooth rotating disks have been observed in massive evolved galaxies merely 1.4 billion years after the Big Bang, suggesting rapid morphological and dynamical evolution in the early Universe. Probing… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.18543v2-abstract-full').style.display = 'inline'; document.getElementById('2402.18543v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.18543v2-abstract-full" style="display: none;"> Early galaxy formation, initiated by the dark matter and gas assembly, evolves through frequent mergers and feedback processes into dynamically hot, chaotic structures. In contrast, dynamically cold, smooth rotating disks have been observed in massive evolved galaxies merely 1.4 billion years after the Big Bang, suggesting rapid morphological and dynamical evolution in the early Universe. Probing this evolution mechanism necessitates studies of young galaxies, yet efforts have been hindered by observational limitations in both sensitivity and spatial resolution. Here we report high-resolution observations of a strongly lensed and quintuply imaged, low-luminosity, young galaxy at $z=6.072$ (dubbed the Cosmic Grapes), 930 million years after the Big Bang. Magnified by gravitational lensing, the galaxy is resolved into at least 15 individual star-forming clumps with effective radii of $r_{\rm e}\simeq$ 10--60 parsec (pc), which dominate $\simeq$ 70\% of the galaxy's total flux. The cool gas emission unveils a smooth, underlying rotating disk characterized by a high rotational-to-random motion ratio and a gravitationally unstable state (Toomre $Q \simeq$ 0.2--0.3), with high surface gas densities comparable to local dusty starbursts with $\simeq10^{3-5}$ $M_{\odot}$/pc$^{2}$. These gas properties suggest that the numerous star-forming clumps are formed through disk instabilities with weak feedback effects. The clumpiness of the Cosmic Grapes significantly exceeds that of galaxies at later epochs and the predictions from current simulations for early galaxies. Our findings shed new light on internal galaxy substructures and their relation to the underlying dynamics and feedback mechanisms at play during their early formation phases, potentially explaining the high abundance of bright galaxies observed in the early Universe and the dark matter core-cusp problem. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.18543v2-abstract-full').style.display = 'none'; document.getElementById('2402.18543v2-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 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted. 44 pages, 14 figures, 5 tables. Comments are welcome! See also the companion papers on arXiv. Valentino+2024: arXiv:2402.17845 Gim茅nez-Arteaga+2024: arXiv:2402.17875</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.04767">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/2401.03024">arXiv:2401.03024</a> <span> [<a href="https://arxiv.org/pdf/2401.03024">pdf</a>, <a href="https://arxiv.org/format/2401.03024">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"> Probing coherence in metal absorption towards multiple images of strong gravitationally lensed quasars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dutta%2C+R">Rajeshwari Dutta</a>, <a href="/search/astro-ph?searchtype=author&query=Acebron%2C+A">Ana Acebron</a>, <a href="/search/astro-ph?searchtype=author&query=Fumagalli%2C+M">Michele Fumagalli</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+B">Gabriel B. Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Fossati%2C+M">Matteo Fossati</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="2401.03024v1-abstract-short" style="display: inline;"> We present a tomographic analysis of metal absorption lines arising from the circumgalactic medium (CGM) of galaxies at z~0.5-2, using Multi Unit Spectroscopic Explorer (MUSE) observations of two background quasars at z~2.2 and 2.8, which are two of the few currently known quasars with multiple images due to strong gravitational lensing by galaxy clusters at z~0.6 and 0.5, respectively. The angula… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.03024v1-abstract-full').style.display = 'inline'; document.getElementById('2401.03024v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.03024v1-abstract-full" style="display: none;"> We present a tomographic analysis of metal absorption lines arising from the circumgalactic medium (CGM) of galaxies at z~0.5-2, using Multi Unit Spectroscopic Explorer (MUSE) observations of two background quasars at z~2.2 and 2.8, which are two of the few currently known quasars with multiple images due to strong gravitational lensing by galaxy clusters at z~0.6 and 0.5, respectively. The angular separations between different pairs of quasar multiple images enable us to probe the absorption over transverse physical separations of ~0.4-150 kpc, which are based on strong lensing models exploiting MUSE observations. The fractional difference in rest-frame equivalent width (Delta Wr) of MgII, FeII, CIV absorption increases on average with physical separation, indicating that the metal-enriched gaseous structures become less coherent with distance, with a likely coherence length scale of ~10 kpc. However, Delta Wr for all the ions vary considerably over ~0.08-0.9, indicating a clumpy CGM over the full range of length scales probed. At the same time, paired MgII absorption is detected across ~100-150 kpc at similar line-of-sight velocities, which could be probing cool gas clouds within the same halo. No significant dependence of Delta Wr is found on the equivalent width and redshift of the absorbing gas and on the galaxy environment associated with the absorption. The high-ionization gas phase traced by CIV shows a higher degree of coherence than the low-ionization gas phase traced by MgII, with ~90 percent of CIV systems exhibiting Delta Wr <=0.5 at separations <=10 kpc compared to ~50 percent of MgII systems. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.03024v1-abstract-full').style.display = 'none'; document.getElementById('2401.03024v1-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 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">9 pages + appendix, 8 figures, accepted 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/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/2310.02310">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/2309.16832">arXiv:2309.16832</a> <span> [<a href="https://arxiv.org/pdf/2309.16832">pdf</a>, <a href="https://arxiv.org/format/2309.16832">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/stad2916">10.1093/mnras/stad2916 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> ALMA Lensing Cluster Survey: average dust, gas, and star formation properties of cluster and field galaxies from stacking analysis </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Guerrero%2C+A">Andrea Guerrero</a>, <a href="/search/astro-ph?searchtype=author&query=Nagar%2C+N">Neil Nagar</a>, <a href="/search/astro-ph?searchtype=author&query=Kohno%2C+K">Kotaro Kohno</a>, <a href="/search/astro-ph?searchtype=author&query=Fujimoto%2C+S">Seiji Fujimoto</a>, <a href="/search/astro-ph?searchtype=author&query=Kokorev%2C+V">Vasily Kokorev</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">Gabriel Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Jolly%2C+J">Jean-Baptiste Jolly</a>, <a href="/search/astro-ph?searchtype=author&query=Knudsen%2C+K">Kirsten Knudsen</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+F">Fengwu Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</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=Caputi%2C+K">Karina Caputi</a>, <a href="/search/astro-ph?searchtype=author&query=Neumann%2C+G">Gerald Neumann</a>, <a href="/search/astro-ph?searchtype=author&query=Orellana-Gonz%C3%A1lez%2C+G">Gustavo Orellana-Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Cerulo%2C+P">Pierluigi Cerulo</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez-L%C3%B3pez%2C+J">Jorge Gonz谩lez-L贸pez</a>, <a href="/search/astro-ph?searchtype=author&query=Laporte%2C+N">Nicolas Laporte</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Ao%2C+Y">Yiping Ao</a>, <a href="/search/astro-ph?searchtype=author&query=Espada%2C+D">Daniel Espada</a>, <a href="/search/astro-ph?searchtype=author&query=Arancibia%2C+A+M+M">Alejandra M. Mu帽oz Arancibia</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="2309.16832v1-abstract-short" style="display: inline;"> We develop new tools for continuum and spectral stacking of ALMA data, and apply these to the ALMA Lensing Cluster Survey (ALCS). We derive average dust masses, gas masses and star formation rates (SFR) from the stacked observed 260~GHz continuum of 3402 individually undetected star-forming galaxies, of which 1450 are cluster galaxies and 1952 field galaxies, over three redshift and stellar mass b… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.16832v1-abstract-full').style.display = 'inline'; document.getElementById('2309.16832v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.16832v1-abstract-full" style="display: none;"> We develop new tools for continuum and spectral stacking of ALMA data, and apply these to the ALMA Lensing Cluster Survey (ALCS). We derive average dust masses, gas masses and star formation rates (SFR) from the stacked observed 260~GHz continuum of 3402 individually undetected star-forming galaxies, of which 1450 are cluster galaxies and 1952 field galaxies, over three redshift and stellar mass bins (over $z = 0$-1.6 and log $M_{*} [M_{\odot}] = 8$-11.7), and derive the average molecular gas content by stacking the emission line spectra in a SFR-selected subsample. The average SFRs and specific SFRs of both cluster and field galaxies are lower than those expected for Main Sequence (MS) star-forming galaxies, and only galaxies with stellar mass of log $M_{*} [M_{\odot}] = 9.35$-10.6 show dust and gas fractions comparable to those in the MS. The ALMA-traced average `highly obscured' SFRs are typically lower than the SFRs observed from optical to near-IR spectral analysis. Cluster and field galaxies show similar trends in their contents of dust and gas, even when field galaxies were brighter in the stacked maps. From spectral stacking we find a potential CO ($J=4\to3$) line emission (SNR $\sim4$) when stacking cluster and field galaxies with the highest SFRs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.16832v1-abstract-full').style.display = 'none'; document.getElementById('2309.16832v1-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 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">13 pages, 8 figures, 1 table (+4 pages, 4 figures in Appendix). 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/2307.06804">arXiv:2307.06804</a> <span> [<a href="https://arxiv.org/pdf/2307.06804">pdf</a>, <a href="https://arxiv.org/format/2307.06804">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/10.3847/1538-4357/acf832">10.3847/1538-4357/acf832 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CLASH-VLT: The inner slope of the MACS J1206.2-0847 dark matter density profile </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Biviano%2C+A">A. Biviano</a>, <a href="/search/astro-ph?searchtype=author&query=Pizzuti%2C+L">L. Pizzuti</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">A. Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Sartoris%2C+B">B. Sartoris</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Ettori%2C+S">S. Ettori</a>, <a href="/search/astro-ph?searchtype=author&query=Girardi%2C+M">M. Girardi</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> </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="2307.06804v2-abstract-short" style="display: inline;"> The inner slope (gammadm) of the dark matter (DM) density profile of cosmological halos carries information about the properties of DM and/or baryonic processes affecting the halo gravitational potential. Cold DM cosmological simulations predict steep inner slopes, gammadm~1. We test this prediction on the MACS J1206.2-0847 cluster at redshift z=0.44, whose DM density profile was claimed to be cor… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.06804v2-abstract-full').style.display = 'inline'; document.getElementById('2307.06804v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.06804v2-abstract-full" style="display: none;"> The inner slope (gammadm) of the dark matter (DM) density profile of cosmological halos carries information about the properties of DM and/or baryonic processes affecting the halo gravitational potential. Cold DM cosmological simulations predict steep inner slopes, gammadm~1. We test this prediction on the MACS J1206.2-0847 cluster at redshift z=0.44, whose DM density profile was claimed to be cored at the center. We determine the cluster DM density profile from 2 kpc from the cluster center to the virial radius (~2 Mpc), using the velocity distribution of ~500 cluster galaxies and the internal velocity dispersion profile of the Brightest Cluster Galaxy (BCG), obtained from VIMOS@VLT and MUSE@VLT data. We solve the Jeans equation of dynamical equilibrium using an upgraded version of the MAMPOSSt method. The total mass profile is modeled as a sum of a generalized-NFW profile that describes the DM component, allowing for a free inner slope of the density profile, a Jaffe profile that describes the BCG stellar mass component, and a non-parametric baryonic profile that describes the sum of the remaining galaxy stellar mass and of the hot intra-cluster gas mass. Our total mass profile is in remarkable agreement with independent determinations based on X-ray observations and strong lensing. We find gammadm=0.7 (-0.1 +0.2) (68\% confidence levels), consistent with predictions from recent LambdaCDM cosmological numerical simulations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.06804v2-abstract-full').style.display = 'none'; document.getElementById('2307.06804v2-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 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 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">ApJ, 958, 148. Minor modifications to the text, two figures and the table, with respect to the previous 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/2305.15126">arXiv:2305.15126</a> <span> [<a href="https://arxiv.org/pdf/2305.15126">pdf</a>, <a href="https://arxiv.org/format/2305.15126">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"> Unbiased surveys of dust-enshrouded galaxies using ALMA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kohno%2C+K">K. Kohno</a>, <a href="/search/astro-ph?searchtype=author&query=Fujimoto%2C+S">S. Fujimoto</a>, <a href="/search/astro-ph?searchtype=author&query=Tsujita%2C+A">A. Tsujita</a>, <a href="/search/astro-ph?searchtype=author&query=Kokorev%2C+V">V. Kokorev</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">G. Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Magdis%2C+G+E">G. E. Magdis</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">F. Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Laporte%2C+N">N. Laporte</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+F">Fengwu Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Egami%2C+E">E. Egami</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">F. E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Guerrero%2C+A">A. Guerrero</a>, <a href="/search/astro-ph?searchtype=author&query=Nagar%2C+N">N. Nagar</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=Caminha%2C+G+B">G. B. Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Jolly%2C+J+-">J. -B. Jolly</a>, <a href="/search/astro-ph?searchtype=author&query=Knudsen%2C+K+K">K. K. Knudsen</a>, <a href="/search/astro-ph?searchtype=author&query=Uematsu%2C+R">R. Uematsu</a>, <a href="/search/astro-ph?searchtype=author&query=Ueda%2C+Y">Y. Ueda</a>, <a href="/search/astro-ph?searchtype=author&query=Oguri%2C+M">M. Oguri</a>, <a href="/search/astro-ph?searchtype=author&query=Zitrin%2C+A">A. Zitrin</a>, <a href="/search/astro-ph?searchtype=author&query=Ouchi%2C+M">M. Ouchi</a>, <a href="/search/astro-ph?searchtype=author&query=Ono%2C+Y">Y. Ono</a>, <a href="/search/astro-ph?searchtype=author&query=Gonzalez-Lopez%2C+J">J. Gonzalez-Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Richard%2C+J">J. Richard</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="2305.15126v1-abstract-short" style="display: inline;"> The ALMA lensing cluster survey (ALCS) is a 96-hr large program dedicated to uncovering and characterizing intrinsically faint continuum sources and line emitters with the assistance of gravitational lensing. All 33 cluster fields were selected from HST/Spitzer treasury programs including CLASH, Hubble Frontier Fields, and RELICS, which also have Herschel and Chandra coverages. The total sky area… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.15126v1-abstract-full').style.display = 'inline'; document.getElementById('2305.15126v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.15126v1-abstract-full" style="display: none;"> The ALMA lensing cluster survey (ALCS) is a 96-hr large program dedicated to uncovering and characterizing intrinsically faint continuum sources and line emitters with the assistance of gravitational lensing. All 33 cluster fields were selected from HST/Spitzer treasury programs including CLASH, Hubble Frontier Fields, and RELICS, which also have Herschel and Chandra coverages. The total sky area surveyed reaches $\sim$133 arcmin$^2$ down to a depth of $\sim$60 $渭$Jy beam$^{-1}$ (1$蟽$) at 1.2 mm, yielding 141 secure blind detections of continuum sources and additional 39 sources aided by priors. We present scientific motivation, survey design, the status of spectroscopy follow-up observations, and number counts down to $\sim$7 $渭$Jy. Synergies with JWST are also discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.15126v1-abstract-full').style.display = 'none'; document.getElementById('2305.15126v1-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 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">6 pages, 4 figures, Proceedings of the 7th Chile-Cologne-Bonn-Symposium: Physics and Chemistry of Star Formation, V. Ossenkopf-Okada, R. Schaaf, I. Breloy (eds.)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.14413">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/2303.01658">arXiv:2303.01658</a> <span> [<a href="https://arxiv.org/pdf/2303.01658">pdf</a>, <a href="https://arxiv.org/format/2303.01658">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"> ALMA Lensing Cluster Survey: Deep 1.2 mm Number Counts and Infrared Luminosity Functions at $z\simeq1-8$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fujimoto%2C+S">Seiji Fujimoto</a>, <a href="/search/astro-ph?searchtype=author&query=Kohno%2C+K">Kotaro Kohno</a>, <a href="/search/astro-ph?searchtype=author&query=Ouchi%2C+M">Masami Ouchi</a>, <a href="/search/astro-ph?searchtype=author&query=Oguri%2C+M">Masamune Oguri</a>, <a href="/search/astro-ph?searchtype=author&query=Kokorev%2C+V">Vasily Kokorev</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">Gabriel Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+F">Fengwu Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Gonzalez-Lopez%2C+J">Jorge Gonzalez-Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</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=Hatsukade%2C+B">Bunyo Hatsukade</a>, <a href="/search/astro-ph?searchtype=author&query=Richard%2C+J">Johan Richard</a>, <a href="/search/astro-ph?searchtype=author&query=Smail%2C+I">Ian Smail</a>, <a href="/search/astro-ph?searchtype=author&query=Tsujita%2C+A">Akiyoshi Tsujita</a>, <a href="/search/astro-ph?searchtype=author&query=Ueda%2C+Y">Yoshihiro Ueda</a>, <a href="/search/astro-ph?searchtype=author&query=Uematsu%2C+R">Ryosuke Uematsu</a>, <a href="/search/astro-ph?searchtype=author&query=Zitrin%2C+A">Adi Zitrin</a>, <a href="/search/astro-ph?searchtype=author&query=Coe%2C+D">Dan Coe</a>, <a href="/search/astro-ph?searchtype=author&query=Kneib%2C+J">Jean-Paul Kneib</a>, <a href="/search/astro-ph?searchtype=author&query=Postman%2C+M">Marc Postman</a>, <a href="/search/astro-ph?searchtype=author&query=Umetsu%2C+K">Keiichi Umetsu</a>, <a href="/search/astro-ph?searchtype=author&query=Lagos%2C+C+d+P">Claudia del P. Lagos</a>, <a href="/search/astro-ph?searchtype=author&query=Popping%2C+G">Gergo Popping</a>, <a href="/search/astro-ph?searchtype=author&query=Ao%2C+Y">Yiping Ao</a>, <a href="/search/astro-ph?searchtype=author&query=Bradley%2C+L">Larry Bradley</a> , et al. (18 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="2303.01658v4-abstract-short" style="display: inline;"> We present a statistical study of 180 dust continuum sources identified in 33 massive cluster fields by the ALMA Lensing Cluster Survey (ALCS) over a total of 133 arcmin$^{2}$ area, homogeneously observed at 1.2 mm. ALCS enables us to detect extremely faint mm sources by lensing magnification, including near-infrared (NIR) dark objects showing no counterparts in existing {\it Hubble Space Telescop… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.01658v4-abstract-full').style.display = 'inline'; document.getElementById('2303.01658v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.01658v4-abstract-full" style="display: none;"> We present a statistical study of 180 dust continuum sources identified in 33 massive cluster fields by the ALMA Lensing Cluster Survey (ALCS) over a total of 133 arcmin$^{2}$ area, homogeneously observed at 1.2 mm. ALCS enables us to detect extremely faint mm sources by lensing magnification, including near-infrared (NIR) dark objects showing no counterparts in existing {\it Hubble Space Telescope} and {\it Spitzer} images. The dust continuum sources belong to a blind sample ($N=141$) with S/N $\gtrsim$ 5.0 (a purity of $>$ 0.99) or a secondary sample ($N=39$) with S/N= $4.0-5.0$ screened by priors. With the blind sample, we securely derive 1.2-mm number counts down to $\sim7$ $渭$Jy, and find that the total integrated 1.2mm flux is 20.7$^{+8.5}_{-6.5}$ Jy deg$^{-2}$, resolving $\simeq$ 80 % of the cosmic infrared background light. The resolved fraction varies by a factor of $0.6-1.1$ due to the completeness correction depending on the spatial size of the mm emission. We also derive infrared (IR) luminosity functions (LFs) at $z=0.6-7.5$ with the $1/V_{\rm max}$ method, finding the redshift evolution of IR LFs characterized by positive luminosity and negative density evolution. The total (=UV+IR) cosmic star-formation rate density (SFRD) at $z>4$ is estimated to be $161^{+25}_{-21}$ % of the established measurements, which were almost exclusively based on optical$-$NIR surveys. Although our general understanding of the cosmic SFRD is unlikely to change beyond a factor of 2, these results add to the weight of evidence for an additional ($\approx 60$ %) SFRD component contributed by the faint-mm population, including NIR dark objects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.01658v4-abstract-full').style.display = 'none'; document.getElementById('2303.01658v4-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 June, 2024; <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">ApJS in press, 34 pages, 8 Tables, and 18 Figures (+38 pages, 5 Tables, and 6 Figures in Appendix)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.00025">arXiv:2303.00025</a> <span> [<a href="https://arxiv.org/pdf/2303.00025">pdf</a>, <a href="https://arxiv.org/format/2303.00025">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/10.1093/mnras/stad1321">10.1093/mnras/stad1321 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A variable active galactic nucleus at $z=2.06$ triply-imaged by the galaxy cluster MACS J0035.4-2015 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Furtak%2C+L+J">Lukas J. Furtak</a>, <a href="/search/astro-ph?searchtype=author&query=Mainali%2C+R">Ramesh Mainali</a>, <a href="/search/astro-ph?searchtype=author&query=Zitrin%2C+A">Adi Zitrin</a>, <a href="/search/astro-ph?searchtype=author&query=Plat%2C+A">Ad猫le Plat</a>, <a href="/search/astro-ph?searchtype=author&query=Fujimoto%2C+S">Seiji Fujimoto</a>, <a href="/search/astro-ph?searchtype=author&query=Donahue%2C+M">Megan Donahue</a>, <a href="/search/astro-ph?searchtype=author&query=Nelson%2C+E+J">Erica J. Nelson</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Uematsu%2C+R">Ryosuke Uematsu</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=Andrade-Santos%2C+F">Felipe Andrade-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Bradley%2C+L+D">Larry D. Bradley</a>, <a href="/search/astro-ph?searchtype=author&query=Caputi%2C+K+I">Karina I. Caputi</a>, <a href="/search/astro-ph?searchtype=author&query=Charlot%2C+S">St茅phane Charlot</a>, <a href="/search/astro-ph?searchtype=author&query=Chevallard%2C+J">Jacopo Chevallard</a>, <a href="/search/astro-ph?searchtype=author&query=Coe%2C+D">Dan Coe</a>, <a href="/search/astro-ph?searchtype=author&query=Curtis-Lake%2C+E">Emma Curtis-Lake</a>, <a href="/search/astro-ph?searchtype=author&query=Espada%2C+D">Daniel Espada</a>, <a href="/search/astro-ph?searchtype=author&query=Frye%2C+B+L">Brenda L. Frye</a>, <a href="/search/astro-ph?searchtype=author&query=Knudsen%2C+K+K">Kirsten K. Knudsen</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Kohno%2C+K">Kotaro Kohno</a>, <a href="/search/astro-ph?searchtype=author&query=Kokorev%2C+V">Vasily Kokorev</a>, <a href="/search/astro-ph?searchtype=author&query=Laporte%2C+N">Nicolas Laporte</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+M+M">Minju M. Lee</a> , et al. (10 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.00025v4-abstract-short" style="display: inline;"> We report the discovery of a triply imaged active galactic nucleus (AGN), lensed by the galaxy cluster MACS J0035.4-2015 ($z_{\mathrm{d}}=0.352$). The object is detected in Hubble Space Telescope imaging taken for the RELICS program. It appears to have a quasi-stellar nucleus consistent with a point-source, with a de-magnified radius of $r_e\lesssim100$ pc. The object is spectroscopically confirme… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.00025v4-abstract-full').style.display = 'inline'; document.getElementById('2303.00025v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.00025v4-abstract-full" style="display: none;"> We report the discovery of a triply imaged active galactic nucleus (AGN), lensed by the galaxy cluster MACS J0035.4-2015 ($z_{\mathrm{d}}=0.352$). The object is detected in Hubble Space Telescope imaging taken for the RELICS program. It appears to have a quasi-stellar nucleus consistent with a point-source, with a de-magnified radius of $r_e\lesssim100$ pc. The object is spectroscopically confirmed to be an AGN at $z_{\mathrm{spec}}=2.063\pm0.005$ showing broad rest-frame UV emission lines, and is detected in both X-ray observations with Chandra and in ALCS ALMA band 6 (1.2 mm) imaging. It has a relatively faint rest-frame UV luminosity for a quasar-like object, $M_{\mathrm{UV},1450}=-19.7\pm0.2$. The object adds to just a few quasars or other X-ray sources known to be multiply lensed by a galaxy cluster. Some diffuse emission from the host galaxy is faintly seen around the nucleus and there is a faint object nearby sharing the same multiple-imaging symmetry and geometric redshift, possibly an interacting galaxy or a star-forming knot in the host. We present an accompanying lens model, calculate the magnifications and time delays, and infer physical properties for the source. We find the rest-frame UV continuum and emission lines to be dominated by the AGN, and the optical emission to be dominated by the host galaxy of modest stellar mass $M_{\star}\simeq10^{9.2} \mathrm{M}_{\odot}$. We also observe some variation in the AGN emission with time, which may suggest that the AGN used to be more active. This object adds a low-redshift counterpart to several relatively faint AGN recently uncovered at high redshifts with HST and JWST. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.00025v4-abstract-full').style.display = 'none'; document.getElementById('2303.00025v4-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 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 February, 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">Published in MNRAS. Corrected miss-assignment of affiliations in the author list</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.07896">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/2301.04672">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/2301.03629">arXiv:2301.03629</a> <span> [<a href="https://arxiv.org/pdf/2301.03629">pdf</a>, <a href="https://arxiv.org/format/2301.03629">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/10.1051/0004-6361/202345868">10.1051/0004-6361/202345868 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> On the correlation between dark matter, intracluster light and globular cluster distribution in SMACS0723 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Diego%2C+J+M">J. M. Diego</a>, <a href="/search/astro-ph?searchtype=author&query=Pascale%2C+M">M. Pascale</a>, <a href="/search/astro-ph?searchtype=author&query=Frye%2C+B">B. Frye</a>, <a href="/search/astro-ph?searchtype=author&query=Zitrin%2C+A">A. Zitrin</a>, <a href="/search/astro-ph?searchtype=author&query=Broadhurst%2C+T">T. Broadhurst</a>, <a href="/search/astro-ph?searchtype=author&query=Mahler%2C+G">G. Mahler</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=Jauzac%2C+M">M. Jauzac</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+M+G">Myung Gyoon Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Bae%2C+J+H">Jang Ho Bae</a>, <a href="/search/astro-ph?searchtype=author&query=Jang%2C+I+S">In Sung Jang</a>, <a href="/search/astro-ph?searchtype=author&query=Montes%2C+M">Mireia Montes</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="2301.03629v1-abstract-short" style="display: inline;"> We present a free-form model of SMACS0723, the first cluster observed with JWST. This model makes no strong assumptions about the distribution of mass (mostly dark matter) in the cluster and we use it to study the possible correlation between dark matter with the intracluster light and distribution of globular clusters. To explore the uncertainty in mass modelling, we derive three lens models base… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.03629v1-abstract-full').style.display = 'inline'; document.getElementById('2301.03629v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.03629v1-abstract-full" style="display: none;"> We present a free-form model of SMACS0723, the first cluster observed with JWST. This model makes no strong assumptions about the distribution of mass (mostly dark matter) in the cluster and we use it to study the possible correlation between dark matter with the intracluster light and distribution of globular clusters. To explore the uncertainty in mass modelling, we derive three lens models based on spectroscopically confirmed systems and new candidate systems with redshifts predicted by the lens model derived from the spectroscopic systems. We find that beyond the radius of influence of the BCG, the total mass does not trace the ICL, implying the need for a dark component (dark matter). Two loop-like structures observed in the intracluster light do not have an obvious correspondence with the total mass (mostly dark matter) distribution. The radial profiles of the ICL and the distribution of globular clusters are similar to each other, but steeper than the profile of the lens model. More specifically, we find that the total mass is shallower by 1 dex in log scale than both ICL and globular cluster profiles. This is in excellent agreement with N-body simulations of cold dark matter. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.03629v1-abstract-full').style.display = 'none'; document.getElementById('2301.03629v1-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, 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">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 679, A159 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.06666">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/2212.00841">arXiv:2212.00841</a> <span> [<a href="https://arxiv.org/pdf/2212.00841">pdf</a>, <a href="https://arxiv.org/format/2212.00841">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/10.1051/0004-6361/202245070">10.1051/0004-6361/202245070 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> VST-GAME: Galaxy Assembly as a function of Mass and Environment with VST. Photometric assessment and density field of MACSJ0416 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Estrada%2C+N">Nicolas Estrada</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">Amata Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Vulcani%2C+B">Benedetta Vulcani</a>, <a href="/search/astro-ph?searchtype=author&query=Rodighiero%2C+G">Giulia Rodighiero</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">Mario Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Annunziatella%2C+M">Marianna Annunziatella</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+B">Gabriel Bartosch Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Angora%2C+G">Giuseppe Angora</a>, <a href="/search/astro-ph?searchtype=author&query=Biviano%2C+A">Andrea Biviano</a>, <a href="/search/astro-ph?searchtype=author&query=Brescia%2C+M">Massimo Brescia</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=Demarco%2C+R">Ricardo Demarco</a>, <a href="/search/astro-ph?searchtype=author&query=Girardi%2C+M">Marisa Girardi</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">Raphael Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Lemaux%2C+B+C">Brian C. Lemaux</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="2212.00841v2-abstract-short" style="display: inline;"> Observational studies have widely demonstrated that galaxy physical properties are strongly affected by the surrounding environment. On one side, gas inflows provide galaxies with new fuel for star formation. On the other side, the high temperatures and densities of the medium are expected to induce quenching in the star formation. Observations of large structures, in particular filaments at the c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.00841v2-abstract-full').style.display = 'inline'; document.getElementById('2212.00841v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.00841v2-abstract-full" style="display: none;"> Observational studies have widely demonstrated that galaxy physical properties are strongly affected by the surrounding environment. On one side, gas inflows provide galaxies with new fuel for star formation. On the other side, the high temperatures and densities of the medium are expected to induce quenching in the star formation. Observations of large structures, in particular filaments at the cluster outskirts (r>2r$_{200}$), are currently limited to the low redshift Universe. We present a multi-band dataset for the cluster MACS J0416.1-2403 (z=0.397), observed in the context of the Galaxy Assembly as a function of Mass and Environment with VST (VST-GAME) survey. The project aims at gathering deep ($r$<24.4) and wide (20x20Mpc$^2$) observations at optical wavelengths for six massive galaxy clusters at 0.2<z<0.6, complemented with near infrared data. This work describes the photometric analysis of the cluster, defines a density field and studies galaxy properties in the cluster outskirts. We extract sources paying particular attention to recover the faintest ones. We combine all the extractions in a multi-band catalog and compute photometric redshifts. We then define cluster memberships up to 5r$_{200}$ from the cluster core and measure the density field, comparing galaxy properties in different environments. We found that the $g-r$ colors show bimodal behaviours in all the environments, but the peak of the distribution of red galaxies shifts toward redder colors with increasing density and the fraction of galaxies in the blue cloud increases with decreasing density. We also found 3 overdense regions in the cluster outskirts at r$\sim$5r$_{200}$. The color of galaxies suggests the presence of evolved galaxy populations, an insight for pre-processing phenomena over these substructures. We release the multi-band catalog, down to the completeness limit $r$<24.4 mag. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.00841v2-abstract-full').style.display = 'none'; document.getElementById('2212.00841v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 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">19 pages, 15 figures and 5 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 671, A146 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.14131">arXiv:2211.14131</a> <span> [<a href="https://arxiv.org/pdf/2211.14131">pdf</a>, <a href="https://arxiv.org/format/2211.14131">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/10.1051/0004-6361/202244995">10.1051/0004-6361/202244995 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The uncertain interstellar medium of high-redshift quiescent galaxies: Impact of methodology </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">Rapha毛l Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+C">Chiara D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">Daizhong Liu</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=Daddi%2C+E">Emanuele Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Bl%C3%A1nquez%2C+D">David Bl谩nquez</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="2211.14131v1-abstract-short" style="display: inline;"> How much gas and dust is contained in high-redshift quiescent galaxies (QGs) is currently an open question with relatively few and contradictory answers, as well as important implications for our understanding of the nature of star formation quenching processes at cosmic noon. Here we revisit far-infrared (FIR) observations of the REQUIEM-ALMA sample of six z = 1.6 - 3.2 QGs strongly lensed by int… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.14131v1-abstract-full').style.display = 'inline'; document.getElementById('2211.14131v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.14131v1-abstract-full" style="display: none;"> How much gas and dust is contained in high-redshift quiescent galaxies (QGs) is currently an open question with relatively few and contradictory answers, as well as important implications for our understanding of the nature of star formation quenching processes at cosmic noon. Here we revisit far-infrared (FIR) observations of the REQUIEM-ALMA sample of six z = 1.6 - 3.2 QGs strongly lensed by intermediate-redshift galaxy clusters. We measured their continuum emission using priors obtained from high resolution near-infrared (NIR) imaging, as opposed to focusing on point-source extraction, converted it into dust masses using a FIR dust emission model derived from statistical samples of QGs, and compared the results to those of the reference work. We find that, while at least the most massive sample galaxy is indeed dust-poor, the picture is much more nuanced than previously reported. In particular, these more conservative constraints remain consistent with high dust fractions in early QGs. We find that these measurements are very sensitive to the adopted extraction method and conversion factors: the use of an extended light model to fit the FIR emission increases the flux of detections by up to 50% and the upper limit by up to a factor 6. Adding the FIR-to-dust conversion, this amounts to an order of magnitude difference in dust fraction, casting doubts on the power of these data to discriminate between star formation quenching scenarios. Unless these are identified by other means, mapping the dust and gas in high-redshift QGs will continue to require somewhat costly observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.14131v1-abstract-full').style.display = 'none'; document.getElementById('2211.14131v1-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 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">7 pages, 5 figures, 2 tables; accepted for publication in Astronomy & Astrophysics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/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/2207.09416">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/2204.09065">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/2203.13759">arXiv:2203.13759</a> <span> [<a href="https://arxiv.org/pdf/2203.13759">pdf</a>, <a href="https://arxiv.org/format/2203.13759">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/10.1051/0004-6361/202243600">10.1051/0004-6361/202243600 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraining the multi-scale dark-matter distribution in CASSOWARY 31 with strong gravitational lensing and stellar dynamics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wang%2C+H">H. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Ca%C3%B1ameras%2C+R">R. Ca帽ameras</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=Suyu%2C+S+H">S. H. Suyu</a>, <a href="/search/astro-ph?searchtype=author&query=Y%C4%B1ld%C4%B1r%C4%B1m%2C+A">A. Y谋ld谋r谋m</a>, <a href="/search/astro-ph?searchtype=author&query=Chiriv%C3%AC%2C+G">G. Chiriv矛</a>, <a href="/search/astro-ph?searchtype=author&query=Christensen%2C+L">L. Christensen</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Schuldt%2C+S">S. Schuldt</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="2203.13759v3-abstract-short" style="display: inline;"> We study the inner structure of the group-scale lens CASSOWARY 31 (CSWA 31) by adopting both strong lensing and dynamical modeling. CSWA 31 is a peculiar lens system. The brightest group galaxy (BGG) is an ultra-massive elliptical galaxy at z = 0.683 with a weighted mean velocity dispersion of $蟽= 432 \pm 31$ km s$^{-1}$. It is surrounded by group members and several lensed arcs probing up to ~150… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.13759v3-abstract-full').style.display = 'inline'; document.getElementById('2203.13759v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.13759v3-abstract-full" style="display: none;"> We study the inner structure of the group-scale lens CASSOWARY 31 (CSWA 31) by adopting both strong lensing and dynamical modeling. CSWA 31 is a peculiar lens system. The brightest group galaxy (BGG) is an ultra-massive elliptical galaxy at z = 0.683 with a weighted mean velocity dispersion of $蟽= 432 \pm 31$ km s$^{-1}$. It is surrounded by group members and several lensed arcs probing up to ~150 kpc in projection. Our results significantly improve previous analyses of CSWA 31 thanks to the new HST imaging and MUSE integral-field spectroscopy. From the secure identification of five sets of multiple images and measurements of the spatially-resolved stellar kinematics of the BGG, we conduct a detailed analysis of the multi-scale mass distribution using various modeling approaches, both in the single and multiple lens-plane scenarios. Our best-fit mass models reproduce the positions of multiple images and provide robust reconstructions for two background galaxies at z = 1.4869 and z = 2.763. The relative contributions from the BGG and group-scale halo are remarkably consistent in our three reference models, demonstrating the self-consistency between strong lensing analyses based on image position and extended image modeling. We find that the ultra-massive BGG dominates the projected total mass profiles within 20 kpc, while the group-scale halo dominates at larger radii. The total projected mass enclosed within $R_{eff}$ = 27.2 kpc is $1.10_{-0.04}^{+0.02} \times 10^{13}$ M$_\odot$. We find that CSWA 31 is a peculiar fossil group, strongly dark-matter dominated towards the central region, and with a projected total mass profile similar to higher-mass cluster-scale halos. The total mass-density slope within the effective radius is shallower than isothermal, consistent with previous analyses of early-type galaxies in overdense environments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.13759v3-abstract-full').style.display = 'none'; document.getElementById('2203.13759v3-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 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">22 pages, 12 figures, 5 tables, submitted to Astronomy & Astrophysics. We welcome the comments from readers</span> </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> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.03935">arXiv:2112.03935</a> <span> [<a href="https://arxiv.org/pdf/2112.03935">pdf</a>, <a href="https://arxiv.org/format/2112.03935">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac5d39">10.3847/1538-4357/ac5d39 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The galaxy starburst/main-sequence bimodality over five decades in stellar mass at z ~ 3-6.5 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rinaldi%2C+P">Pierluigi Rinaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Caputi%2C+K+I">Karina I. Caputi</a>, <a href="/search/astro-ph?searchtype=author&query=van+Mierlo%2C+S+E">Sophie E. van Mierlo</a>, <a href="/search/astro-ph?searchtype=author&query=Ashby%2C+M+L+N">Matthew L. N. Ashby</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=Iani%2C+E">Edoardo Iani</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="2112.03935v3-abstract-short" style="display: inline;"> We study the relation between stellar mass (M*) and star formation rate (SFR) for star-forming galaxies over approximately five decades in stellar mass (5.5 <~ log10(M*/Msun) <~ 10.5) at z ~ 3-6.5. This unprecedented coverage has been possible thanks to the joint analysis of blank non-lensed fields (COSMOS/SMUVS) and cluster lensing fields (Hubble Frontier Fields) which allow us to reach very low… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.03935v3-abstract-full').style.display = 'inline'; document.getElementById('2112.03935v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.03935v3-abstract-full" style="display: none;"> We study the relation between stellar mass (M*) and star formation rate (SFR) for star-forming galaxies over approximately five decades in stellar mass (5.5 <~ log10(M*/Msun) <~ 10.5) at z ~ 3-6.5. This unprecedented coverage has been possible thanks to the joint analysis of blank non-lensed fields (COSMOS/SMUVS) and cluster lensing fields (Hubble Frontier Fields) which allow us to reach very low stellar masses. Previous works have revealed the existence of a clear bimodality in the SFR-M* plane with a star-formation Main Sequence and a starburst cloud at z ~ 4-5. Here we show that this bimodality extends to all star-forming galaxies and is valid in the whole redshift range z ~ 3-6.5. We find that starbursts constitute at least 20% of all star-forming galaxies with M* >~ 10^9 Msun at these redshifts and reach a peak of 40% at z=4-5. More importantly, 60% to 90% of the total SFR budget at these redshifts is contained in starburst galaxies, indicating that the starburst mode of star-formation is dominant at high redshifts. Almost all the low stellar-mass starbursts with log10(M*/Msun) <~ 8.5 have ages comparable to the typical timescales of a starburst event, suggesting that these galaxies are being caught in the process of formation. Interestingly, galaxy formation models fail to predict the starburst/main-sequence bimodality and starbursts overall, suggesting that the starburst phenomenon may be driven by physical processes occurring at smaller scales than those probed by these models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.03935v3-abstract-full').style.display = 'none'; document.getElementById('2112.03935v3-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, including 15 figures (17 files in total) and 4 tables. The manuscript has been accepted for publication in the 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/2111.05871">arXiv:2111.05871</a> <span> [<a href="https://arxiv.org/pdf/2111.05871">pdf</a>, <a href="https://arxiv.org/format/2111.05871">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/ac3d35">10.3847/1538-4357/ac3d35 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> VLT/MUSE observations of SDSS J1029+2623: towards a high-precision strong lensing model </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=Bergamini%2C+P">Pietro Bergamini</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=Caminha%2C+G+B">Gabriel Bartosch Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Tozzi%2C+P">Paolo Tozzi</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=Morelli%2C+A">Andrea Morelli</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">Mario Nonino</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="2111.05871v1-abstract-short" style="display: inline;"> We present a strong lensing analysis of the galaxy cluster SDSS J1029+2623 at $z=0.588$, one of the few currently known lens clusters with multiple images of a background ($z=2.1992$) quasar with a measured time delay. We use archival Hubble Space Telescope multi-band imaging and new Multi Unit Spectroscopic Explorer follow-up spectroscopy to build an accurate lens mass model, a crucial step towar… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.05871v1-abstract-full').style.display = 'inline'; document.getElementById('2111.05871v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.05871v1-abstract-full" style="display: none;"> We present a strong lensing analysis of the galaxy cluster SDSS J1029+2623 at $z=0.588$, one of the few currently known lens clusters with multiple images of a background ($z=2.1992$) quasar with a measured time delay. We use archival Hubble Space Telescope multi-band imaging and new Multi Unit Spectroscopic Explorer follow-up spectroscopy to build an accurate lens mass model, a crucial step towards future cosmological applications. The spectroscopic data enable the secure identification of 57 cluster members and of two nearby perturbers along the line-of-sight. We estimate the inner kinematics of a sub-set of 20 cluster galaxies to calibrate the scaling relations parametrizing the sub-halo mass component. We also reliably determine the redshift of 4 multiply imaged sources, provide a tentative measurement for one system, and report the discovery of a new four-image system. The final catalog comprises 26 multiple images from 7 background sources, spanning a wide redshift range, from 1.02 to 5.06. We present two parametric lens models, with slightly different cluster mass parametrizations. The observed positions of the multiple images are accurately reproduced within approximately $0''.2$, the three image positions of the quasar within only $\sim0''.1$. We estimate a cluster projected total mass of $M(<300~ {\rm kpc}) \sim 2.1 \times 10^{14}~ M_{\odot}$, with a statistical uncertainty of a few percent. Both models, that include a small galaxy close to one of the quasar images, predict magnitude differences and time delays between the quasar images that are consistent with the observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.05871v1-abstract-full').style.display = 'none'; document.getElementById('2111.05871v1-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 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 10 figures, 6 Tables. Submitted to ApJ. The full MUSE spectroscopic catalog of SDSS J1029+2623 presented here is made publicly available at https://www.fe.infn.it/astro/lensing</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.06232">arXiv:2110.06232</a> <span> [<a href="https://arxiv.org/pdf/2110.06232">pdf</a>, <a href="https://arxiv.org/format/2110.06232">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/10.1051/0004-6361/202141994">10.1051/0004-6361/202141994 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy cluster strong lensing cosmography: cosmological constraints from a sample of regular galaxy clusters </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=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. 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="2110.06232v1-abstract-short" style="display: inline;"> Cluster strong lensing cosmography is a promising probe of the background geometry of the Universe and several studies have emerged, thanks to the increased quality of observations using space and ground-based telescopes. For the first time, we use a sample of five cluster strong lenses to measure the values of cosmological parameters and combine them with those from classical probes. In order to… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.06232v1-abstract-full').style.display = 'inline'; document.getElementById('2110.06232v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.06232v1-abstract-full" style="display: none;"> Cluster strong lensing cosmography is a promising probe of the background geometry of the Universe and several studies have emerged, thanks to the increased quality of observations using space and ground-based telescopes. For the first time, we use a sample of five cluster strong lenses to measure the values of cosmological parameters and combine them with those from classical probes. In order to assess the degeneracies and the effectiveness of strong-lensing cosmography in constraining the background geometry of the Universe, we adopt four cosmological scenarios. We find good constraining power on the total matter density of the Universe ($惟_{\rm m}$) and the equation of state of the dark energy parameter $w$. For a flat $w$CDM cosmology, we find $惟_{\rm m} = 0.30_{-0.11}^{+0.09}$ and $w=-1.12_{-0.32}^{+0.17}$ from strong lensing only. Interestingly, we show that the constraints from the Cosmic Microwave Background (CMB) are improved by factors of 2.5 and 4.0 on $惟_{\rm m}$ and $w$, respectively, when combined with our posterior distributions in this cosmological model. In a scenario where the equation of state of dark energy evolves with redshift, the strong lensing constraints are compatible with a cosmological constant (i.e. $w=-1$). In a curved cosmology, our strong lensing analyses can accommodate a large range of values for the curvature of the Universe of $惟_{\rm k}=0.28_{-0.21}^{+0.16}$. In all cosmological scenarios, we show that our strong lensing constraints are complementary and in good agreement with measurements from the CMB, baryon acoustic oscillations and Type Ia supernovae. Our results show that cluster strong lensing cosmography is a potentially powerful probe to be included in the cosmological analyses of future surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.06232v1-abstract-full').style.display = 'none'; document.getElementById('2110.06232v1-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 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2021. </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, 3 tables, 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 657, A83 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.03305">arXiv:2109.03305</a> <span> [<a href="https://arxiv.org/pdf/2109.03305">pdf</a>, <a href="https://arxiv.org/format/2109.03305">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/10.1051/0004-6361/202142168">10.1051/0004-6361/202142168 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CLASH-VLT: Abell~S1063. Cluster assembly history and spectroscopic catalogue </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Biviano%2C+A">A. Biviano</a>, <a href="/search/astro-ph?searchtype=author&query=Annunziatella%2C+M">M. Annunziatella</a>, <a href="/search/astro-ph?searchtype=author&query=Girardi%2C+M">M. Girardi</a>, <a href="/search/astro-ph?searchtype=author&query=Sartoris%2C+B">B. Sartoris</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">M. Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Brescia%2C+M">M. Brescia</a>, <a href="/search/astro-ph?searchtype=author&query=Riccio%2C+G">G. Riccio</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Balestra%2C+I">I. Balestra</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=De+Lucia%2C+G">G. De Lucia</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">R. Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Seitz%2C+S">S. Seitz</a>, <a href="/search/astro-ph?searchtype=author&query=Tozzi%2C+P">P. Tozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Scodeggio%2C+M">M. Scodeggio</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=Bergamini%2C+P">P. Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Borgani%2C+S">S. Borgani</a>, <a href="/search/astro-ph?searchtype=author&query=Demarco%2C+R">R. Demarco</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">M. Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Strazzullo%2C+V">V. Strazzullo</a>, <a href="/search/astro-ph?searchtype=author&query=Tortorelli%2C+L">L. Tortorelli</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="2109.03305v2-abstract-short" style="display: inline;"> Using the CLASH-VLT survey, we assembled an unprecedented sample of 1234 spectroscopically confirmed members in Abell~S1063, finding a dynamically complex structure at z_cl=0.3457 with a velocity dispersion 蟽_v=1380 -32 +26 km s^-1. We investigate cluster environmental and dynamical effects by analysing the projected phase-space diagram and the orbits as a function of galaxy spectral properties. W… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.03305v2-abstract-full').style.display = 'inline'; document.getElementById('2109.03305v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.03305v2-abstract-full" style="display: none;"> Using the CLASH-VLT survey, we assembled an unprecedented sample of 1234 spectroscopically confirmed members in Abell~S1063, finding a dynamically complex structure at z_cl=0.3457 with a velocity dispersion 蟽_v=1380 -32 +26 km s^-1. We investigate cluster environmental and dynamical effects by analysing the projected phase-space diagram and the orbits as a function of galaxy spectral properties. We classify cluster galaxies according to the presence and strength of the [OII] emission line, the strength of the H$未$ absorption line, and colours. We investigate the relationship between the spectral classes of galaxies and their position in the projected phase-space diagram. We analyse separately red and blue galaxy orbits. By correlating the observed positions and velocities with the projected phase-space constructed from simulations, we constrain the accretion redshift of galaxies with different spectral types. Passive galaxies are mainly located in the virialised region, while emission-line galaxies are outside r_200, and are accreted later into the cluster. Emission-lines and post-starbursts show an asymmetric distribution in projected phase-space within r_200, with the first being prominent at Delta_v/sigma <~-1.5$, and the second at Delta_v/ sigma >~ 1.5, suggesting that backsplash galaxies lie at large positive velocities. We find that low-mass passive galaxies are accreted in the cluster before the high-mass ones. This suggests that we observe as passives only the low-mass galaxies accreted early in the cluster as blue galaxies, that had the time to quench their star formation. We also find that red galaxies move on more radial orbits than blue galaxies. This can be explained if infalling galaxies can remain blue moving on tangential orbits. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.03305v2-abstract-full').style.display = 'none'; document.getElementById('2109.03305v2-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 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 28 figures, 3 tables, Accepted for publication in 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 656, A147 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.09079">arXiv:2107.09079</a> <span> [<a href="https://arxiv.org/pdf/2107.09079">pdf</a>, <a href="https://arxiv.org/format/2107.09079">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/10.1051/0004-6361/202141817">10.1051/0004-6361/202141817 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Improved strong lensing modelling of galaxy clusters using the Fundamental Plane: Detailed mapping of the baryonic and dark matter mass distribution of Abell S1063 </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=Mercurio%2C+A">Amata Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">Claudio Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Tortorelli%2C+L">Luca Tortorelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">Pietro Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">Massimo Meneghetti</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=Nonino%2C+M">Mario 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="2107.09079v2-abstract-short" style="display: inline;"> From Hubble Frontier Fields photometry, and data from the Multi Unit Spectroscopic Explorer on the Very Large Telescope, we build the Fundamental Plane (FP) relation for the early-type galaxies of the cluster Abell S1063. We use this relation to develop an improved strong lensing model of the total mass distribution of the cluster, determining the velocity dispersions of all 222 cluster members in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.09079v2-abstract-full').style.display = 'inline'; document.getElementById('2107.09079v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.09079v2-abstract-full" style="display: none;"> From Hubble Frontier Fields photometry, and data from the Multi Unit Spectroscopic Explorer on the Very Large Telescope, we build the Fundamental Plane (FP) relation for the early-type galaxies of the cluster Abell S1063. We use this relation to develop an improved strong lensing model of the total mass distribution of the cluster, determining the velocity dispersions of all 222 cluster members included in the model from their measured structural parameters. Fixing the hot gas component from X-ray data, the mass density distributions of the diffuse dark matter haloes are optimised by comparing the observed and model-predicted positions of 55 multiple images of 20 background sources, distributed over the redshift range $0.73-6.11$. We determine the uncertainties on the model parameters with Monte Carlo Markov chains. Compared to previous works, our model allows for the inclusion of a scatter on the relation between the total mass and the velocity dispersion of cluster members, which also shows a shallower slope. We notice a lower statistical uncertainty on the value of some parameters, such as the core radius, of the diffuse mass component of the cluster. Thanks to a new estimate of the stellar mass of all members, we measure the cumulative projected mass profiles out to a radius of 350 kpc, for all baryonic and dark matter components of the cluster. At the outermost radius, we find a baryon fraction of $0.147 \pm 0.002$. We compare the sub-haloes as described by our model with recent hydrodynamical cosmological simulations. We find good agreement in terms of the stellar over total mass fraction. On the other hand, we report some discrepancies in terms of the maximum circular velocity, which is an indication of their compactness, and the sub-halo mass function in the central cluster regions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.09079v2-abstract-full').style.display = 'none'; document.getElementById('2107.09079v2-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2021. </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, 13 figures, 5 tables, Astronomy and Astrophysics, in press</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 659, A24 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.10286">arXiv:2106.10286</a> <span> [<a href="https://arxiv.org/pdf/2106.10286">pdf</a>, <a href="https://arxiv.org/format/2106.10286">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/10.1051/0004-6361/202141586">10.1051/0004-6361/202141586 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A strong lensing model of the galaxy cluster PSZ1 G311.65-18.48 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pignataro%2C+G+V">G. V. Pignataro</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">P. Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">M. Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</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=Rosati%2C+P">P. Rosati</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=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=Nonino%2C+M">M. Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Tozzi%2C+P">P. Tozzi</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="2106.10286v1-abstract-short" style="display: inline;"> We present a strong lensing analysis of the galaxy cluster PSZ1 G311.65-18.48 (z=0.443) using multi-band observations with Hubble Space Telescope, complemented with VLT/MUSE spectroscopic data. The MUSE observations provide redshift estimates for the lensed sources and help reducing the mis-identification of the multiple images. Spectroscopic data are also used to measure the inner velocity disper… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.10286v1-abstract-full').style.display = 'inline'; document.getElementById('2106.10286v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.10286v1-abstract-full" style="display: none;"> We present a strong lensing analysis of the galaxy cluster PSZ1 G311.65-18.48 (z=0.443) using multi-band observations with Hubble Space Telescope, complemented with VLT/MUSE spectroscopic data. The MUSE observations provide redshift estimates for the lensed sources and help reducing the mis-identification of the multiple images. Spectroscopic data are also used to measure the inner velocity dispersions of 15 cluster galaxies and calibrate the scaling relations to model the subhalo cluster component. The model is based on 62 multiple images grouped in 17 families belonging to 4 different sources. The majority of them are multiple images of compact stellar knots belonging to a single star-forming galaxy at z=2.3702. This source is strongly lensed by the cluster to form the Sunburst Arc system. To accurately reproduce all the multiple images, we build a parametric mass model, which includes both cluster-scale and galaxy-scale components. The resulting model has a r.m.s. separation between the model-predicted and the observed positions of the multiple images of only 0.14''. We conclude that PSZ1 G311.65-18.48 has a relatively round projected shape and a large Einstein radius (29'' for z_s = 2.3702), which could indicate that the cluster is elongated along the line of sight. The Sunburst Arc source is located at the intersection of a complex network of caustics, which explains why parts of the arc are imaged with unprecedented multiplicity (up to 12 times). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.10286v1-abstract-full').style.display = 'none'; document.getElementById('2106.10286v1-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 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 655, A81 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.10280">arXiv:2106.10280</a> <span> [<a href="https://arxiv.org/pdf/2106.10280">pdf</a>, <a href="https://arxiv.org/format/2106.10280">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/10.1051/0004-6361/202141590">10.1051/0004-6361/202141590 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> High star cluster formation efficiency in the strongly lensed Sunburst Lyman-continuum galaxy at z=2.37 </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=Meneghetti%2C+M">M. Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Zanella%2C+A">A. Zanella</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=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Cupani%2C+G">G. Cupani</a>, <a href="/search/astro-ph?searchtype=author&query=Mestric%2C+U">U. Mestric</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">G. Brammer</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=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Cristiani%2C+S">S. Cristiani</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=Pignataro%2C+G+V">G. V. Pignataro</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="2106.10280v2-abstract-short" style="display: inline;"> We investigate the strongly lensed (渭x10-100) Lyman continuum (LyC) galaxy, dubbed Sunburst, at z=2.37, taking advantage of a new accurate model of the lens. A characterization of the intrinsic (delensed) properties of the galaxy yields a size of ~3 sq.kpc, a luminosity Muv=-20.3,and a stellar mass M~10^9 Msun;16% of the ultraviolet light is located in a 3 Myr old gravitationally-bound young massi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.10280v2-abstract-full').style.display = 'inline'; document.getElementById('2106.10280v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.10280v2-abstract-full" style="display: none;"> We investigate the strongly lensed (渭x10-100) Lyman continuum (LyC) galaxy, dubbed Sunburst, at z=2.37, taking advantage of a new accurate model of the lens. A characterization of the intrinsic (delensed) properties of the galaxy yields a size of ~3 sq.kpc, a luminosity Muv=-20.3,and a stellar mass M~10^9 Msun;16% of the ultraviolet light is located in a 3 Myr old gravitationally-bound young massive star cluster (YMC) with an effective radius of Re~8 pc and a dynamical mass of ~10^7 Msun (similar to the stellar mass), from which LyC radiation is detected (位< 912A). The inferred outflowing gas velocity (>300 km/s) exceeds the escape velocity of the star cluster. The resulting escape fraction of the ionizing radiation emerging from the Sunburst galaxy is >6-12%, whilst it is >46-93% if inferred from the YMC. 12 additional likely star clusters with 3<Re<20 pc are identified in the galaxy from which we derive a cluster formation efficiency 螕>~30%, which is consistent with the high 螕derived in local galaxies experiencing extreme gas physical conditions. The presence of the YMC influences the morphology (nucleation), photometry (photometric jumps) and spectroscopic output (nebular emission) of the entire galaxy. The de-lensed LyC and UV (1600A) magnitudes of the YMC are ~30.6 and ~26.9, whilst the galaxy has m1600~24.8. A relatively large rest-frame equivalent width of EWrest(Hb+[OIII]4959-5007)~450A emerges from the galaxy with the YMC contributing to ~30%. If O-type stars are mainly forged in star clusters, then such engines were the key ionizing agents during reionization and the increasing occurrence of high EW lines (Hb+[OIII]) observed at z>6.5 might be an indirect signature of a high 螕at reionization.Future facilities (like VLT/MAVIS or ELT), will probe bound clusters on moderately magnified (渭<5-10) galaxies across cosmic epochs up to reionization[ABRIDGED] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.10280v2-abstract-full').style.display = 'none'; document.getElementById('2106.10280v2-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 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </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 (12 main body), 10 Figures and 1 Table. Accepted for publication in Astronomy & Astrophysics. Figure 6 shows the stellar cluster formation efficiency of the Sunburst galaxy; Figure C.1 shows the MUSE narrow field mode image of the counter-arc</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 659, A2 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2102.05788">arXiv:2102.05788</a> <span> [<a href="https://arxiv.org/pdf/2102.05788">pdf</a>, <a href="https://arxiv.org/format/2102.05788">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/10.1051/0004-6361/202040249">10.1051/0004-6361/202040249 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Systematic search for lensed X-ray sources in the CLASH fields </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Liu%2C+A">Ang Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Tozzi%2C+P">Paolo Tozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">Piero Rosati</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 Bartosch Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">Roberto Gilli</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=Nonino%2C+M">Mario Nonino</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="2102.05788v2-abstract-short" style="display: inline;"> We search for unresolved X-ray emission from lensed sources in the FOV of 11 CLASH clusters with Chandra data. We consider the solid angle in the lens plane corresponding to a magnification $渭>1.5$, that amounts to a total of ~100 arcmin$^2$. Our main goal is to assess the efficiency of massive clusters as cosmic telescopes to explore the faint end of X-ray extragalactic source population. We sear… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.05788v2-abstract-full').style.display = 'inline'; document.getElementById('2102.05788v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2102.05788v2-abstract-full" style="display: none;"> We search for unresolved X-ray emission from lensed sources in the FOV of 11 CLASH clusters with Chandra data. We consider the solid angle in the lens plane corresponding to a magnification $渭>1.5$, that amounts to a total of ~100 arcmin$^2$. Our main goal is to assess the efficiency of massive clusters as cosmic telescopes to explore the faint end of X-ray extragalactic source population. We search for X-ray emission from strongly lensed sources identified in the optical, and perform an untargeted detection of lensed X-ray sources. We detect X-ray emission only in 9 out of 849 lensed/background optical sources. The stacked emission of the sources without detection does not reveal any signal in any band. Based on the untargeted detection, we find 66 additional X-ray sources that are consistent with being lensed sources. After accounting for completeness and sky coverage, we measure for the first time the soft- and hard-band number counts of lensed X-ray sources. The results are consistent with current modelization of the AGN population distribution. The distribution of de-lensed fluxes of the sources identified in moderately deep CLASH fields reaches a flux limit of ~$10^{-16}$ and ~$10^{-15}$ erg/s/cm$^{2}$ in the soft and hard bands, respectively. We conclude that, in order to match the depth of the CDFS exploiting massive clusters as cosmic telescopes, the required number of cluster fields is about two orders of magnitude larger than that offered by the 20 years Chandra archive. A significant step forward will be made when future X-ray facilities, with ~1' angular resolution and large effective area, will allow the serendipitous discovery of rare, strongly lensed high-$z$ X-ray sources, enabling the study of faint AGN activity in early Universe and the measurement of gravitational time delays in the X-ray variability of multiply imaged AGN. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.05788v2-abstract-full').style.display = 'none'; document.getElementById('2102.05788v2-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 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2021. </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</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 648, A47 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.01937">arXiv:2101.01937</a> <span> [<a href="https://arxiv.org/pdf/2101.01937">pdf</a>, <a href="https://arxiv.org/format/2101.01937">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/abd7ec">10.3847/1538-4357/abd7ec <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> ALMA Lensing Cluster Survey: Bright [CII] 158 $渭$m Lines from a Multiply Imaged Sub-$L^{\star}$ Galaxy at $z=6.0719$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fujimoto%2C+S">Seiji Fujimoto</a>, <a href="/search/astro-ph?searchtype=author&query=Oguri%2C+M">Masamune Oguri</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">Gabriel Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Yoshimura%2C+Y">Yuki Yoshimura</a>, <a href="/search/astro-ph?searchtype=author&query=Laporte%2C+N">Nicolas Laporte</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez-L%C3%B3pez%2C+J">Jorge Gonz谩lez-L贸pez</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=Kohno%2C+K">Kotaro Kohno</a>, <a href="/search/astro-ph?searchtype=author&query=Zitrin%2C+A">Adi Zitrin</a>, <a href="/search/astro-ph?searchtype=author&query=Richard%2C+J">Johan Richard</a>, <a href="/search/astro-ph?searchtype=author&query=Ouchi%2C+M">Masami Ouchi</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Smail%2C+I">Ian Smail</a>, <a href="/search/astro-ph?searchtype=author&query=Hatsukade%2C+B">Bunyo Hatsukade</a>, <a href="/search/astro-ph?searchtype=author&query=Ono%2C+Y">Yoshiaki Ono</a>, <a href="/search/astro-ph?searchtype=author&query=Kokorev%2C+V">Vasily Kokorev</a>, <a href="/search/astro-ph?searchtype=author&query=Umehata%2C+H">Hideki Umehata</a>, <a href="/search/astro-ph?searchtype=author&query=Schaerer%2C+D">Daniel Schaerer</a>, <a href="/search/astro-ph?searchtype=author&query=Knudsen%2C+K">Kirsten Knudsen</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+F">Fengwu Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Magdis%2C+G">Georgios Magdis</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">Francesco Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Ao%2C+Y">Yiping Ao</a>, <a href="/search/astro-ph?searchtype=author&query=Toft%2C+S">Sune Toft</a>, <a href="/search/astro-ph?searchtype=author&query=Dessauges-Zavadsky%2C+M">Miroslava Dessauges-Zavadsky</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="2101.01937v1-abstract-short" style="display: inline;"> We present bright [CII] 158 $渭$m line detections from a strongly magnified and multiply-imaged ($渭\sim20-160$) sub-$L^{*}$ ($M_{\rm UV}$ = $-19.75^{+0.55}_{-0.44}$) Lyman-break galaxy (LBG) at $z=6.0719\pm0.0004$ from the ALMA Lensing Cluster Survey (ALCS). Emission lines are identified at 268.7 GHz at $\geq$ 8$蟽$ exactly at positions of two multiple images of the LBG behind the massive galaxy clu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.01937v1-abstract-full').style.display = 'inline'; document.getElementById('2101.01937v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.01937v1-abstract-full" style="display: none;"> We present bright [CII] 158 $渭$m line detections from a strongly magnified and multiply-imaged ($渭\sim20-160$) sub-$L^{*}$ ($M_{\rm UV}$ = $-19.75^{+0.55}_{-0.44}$) Lyman-break galaxy (LBG) at $z=6.0719\pm0.0004$ from the ALMA Lensing Cluster Survey (ALCS). Emission lines are identified at 268.7 GHz at $\geq$ 8$蟽$ exactly at positions of two multiple images of the LBG behind the massive galaxy cluster RXCJ0600$-$2007. Our lens models, updated with the latest spectroscopy from VLT/MUSE, indicate that a sub region of the LBG crosses the caustic and is lensed into a long ($\sim6''$) arc with a local magnification of $渭\sim 160$, for which the [CII] line is also significantly detected. The source-plane reconstruction resolves the interstellar medium (ISM) structure, showing that the [CII] line is co-spatial with the rest-frame UV continuum at the scale of $\sim$300 pc. The [CII] line properties suggest that the LBG is a rotation-dominated system whose velocity gradient explains a slight difference of redshifts between the whole LBG and its sub region. The star formation rate (SFR)-$L_{\rm [CII]}$ relations from the sub to the whole regions of the LBG are consistent with those of local galaxies. We evaluate the lower limit of the faint-end of the [CII] luminosity function at $z=6$, and find that it is consistent with predictions from semi analytical models and from the local SFR-$L_{\rm [CII]}$ relation with a SFR function at $z=6$. These results imply that the local SFR-$L_{\rm [CII]}$ relation is universal for a wide range of scales including the spatially resolved ISM, the whole region of galaxy, and the cosmic scale, even in the epoch of reionization. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.01937v1-abstract-full').style.display = 'none'; document.getElementById('2101.01937v1-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 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">27 pages, 10 figures, 6 tables, 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/2101.01740">arXiv:2101.01740</a> <span> [<a href="https://arxiv.org/pdf/2101.01740">pdf</a>, <a href="https://arxiv.org/format/2101.01740">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/10.1093/mnras/stab191">10.1093/mnras/stab191 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> ALMA Lensing Cluster Survey: a strongly lensed multiply imaged dusty system at $z\geq$6 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Laporte%2C+N">N. Laporte</a>, <a href="/search/astro-ph?searchtype=author&query=Zitrin%2C+A">A. Zitrin</a>, <a href="/search/astro-ph?searchtype=author&query=Ellis%2C+R+S">R. S. Ellis</a>, <a href="/search/astro-ph?searchtype=author&query=Fujimoto%2C+S">S. Fujimoto</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">G. Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Richard%2C+J">J. Richard</a>, <a href="/search/astro-ph?searchtype=author&query=Oguri%2C+M">M. Oguri</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=Kohno%2C+K">K. Kohno</a>, <a href="/search/astro-ph?searchtype=author&query=Yoshimura%2C+Y">Y. Yoshimura</a>, <a href="/search/astro-ph?searchtype=author&query=Ao%2C+Y">Y. Ao</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">F. E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Caputi%2C+K">K. Caputi</a>, <a href="/search/astro-ph?searchtype=author&query=Egami%2C+E">E. Egami</a>, <a href="/search/astro-ph?searchtype=author&query=Espada%2C+D">D. Espada</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez-L%C3%B3pez%2C+J">J. Gonz谩lez-L贸pez</a>, <a href="/search/astro-ph?searchtype=author&query=Hatsukade%2C+B">B. Hatsukade</a>, <a href="/search/astro-ph?searchtype=author&query=Knudsen%2C+K+K">K. K. Knudsen</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+M+M">M. M. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Magdis%2C+G">G. Magdis</a>, <a href="/search/astro-ph?searchtype=author&query=Ouchi%2C+M">M. Ouchi</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">F. Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+T">T. Wang</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="2101.01740v1-abstract-short" style="display: inline;"> We report the discovery of an intrinsically faint, quintuply-imaged, dusty galaxy MACS0600-z6 at a redshift $z=$6.07 viewed through the cluster MACSJ0600.1-2008 ($z$=0.46). A $\simeq4蟽$ dust detection is seen at 1.2mm as part of the ALMA Lensing Cluster Survey (ALCS), an on-going ALMA Large program, and the redshift is secured via [C II] 158 $渭$m emission described in a companion paper. In additio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.01740v1-abstract-full').style.display = 'inline'; document.getElementById('2101.01740v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.01740v1-abstract-full" style="display: none;"> We report the discovery of an intrinsically faint, quintuply-imaged, dusty galaxy MACS0600-z6 at a redshift $z=$6.07 viewed through the cluster MACSJ0600.1-2008 ($z$=0.46). A $\simeq4蟽$ dust detection is seen at 1.2mm as part of the ALMA Lensing Cluster Survey (ALCS), an on-going ALMA Large program, and the redshift is secured via [C II] 158 $渭$m emission described in a companion paper. In addition, spectroscopic follow-up with GMOS/Gemini-North shows a break in the galaxy's spectrum, consistent with the Lyman break at that redshift. We use a detailed mass model of the cluster and infer a magnification $渭\gtrsim$30 for the most magnified image of this galaxy, which provides an unprecedented opportunity to probe the physical properties of a sub-luminous galaxy at the end of cosmic reionisation. Based on the spectral energy distribution, we infer lensing-corrected stellar and dust masses of $\rm{2.9^{+11.5}_{-2.3}\times10^9}$ and $\rm{4.8^{+4.5}_{-3.4}\times10^6}$ $\rm{M_{\odot}}$ respectively, a star formation rate of $\rm{9.7^{+22.0}_{-6.6} M_{\odot} yr^{-1}}$, an intrinsic size of $\rm{0.54^{+0.26}_{-0.14}}$ kpc, and a luminosity-weighted age of 200$\pm$100 Myr. Strikingly, the dust production rate in this relatively young galaxy appears to be larger than that observed for equivalent, lower redshift sources. We discuss if this implies that early supernovae are more efficient dust producers and the consequences for using dust mass as a probe of earlier star formation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.01740v1-abstract-full').style.display = 'none'; document.getElementById('2101.01740v1-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 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2021. </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 MNRAS, revised version after including referee's 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/2010.07302">arXiv:2010.07302</a> <span> [<a href="https://arxiv.org/pdf/2010.07302">pdf</a>, <a href="https://arxiv.org/format/2010.07302">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/staa3185">10.1093/mnras/staa3185 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraints on the [CII] luminosity of a proto-globular cluster at z~6 obtained with ALMA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">F. Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Carniani%2C+S">S. Carniani</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">R. Gilli</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=Paladino%2C+R">R. Paladino</a>, <a href="/search/astro-ph?searchtype=author&query=Decarli%2C+R">R. Decarli</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Lupi%2C+A">A. Lupi</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Amato%2C+Q">Q. D'Amato</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=-"> -</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="2010.07302v1-abstract-short" style="display: inline;"> We report on ALMA observations of D1, a system at z~6.15 with stellar mass M_* ~ 10^7 M_sun containing globular cluster (GC) precursors, strongly magnified by the galaxy cluster MACS J0416.1-2403. Since the discovery of GC progenitors at high redshift, ours is the first attempt to probe directly the physical properties of their neutral gas through infrared observations. A careful analysis of our d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.07302v1-abstract-full').style.display = 'inline'; document.getElementById('2010.07302v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.07302v1-abstract-full" style="display: none;"> We report on ALMA observations of D1, a system at z~6.15 with stellar mass M_* ~ 10^7 M_sun containing globular cluster (GC) precursors, strongly magnified by the galaxy cluster MACS J0416.1-2403. Since the discovery of GC progenitors at high redshift, ours is the first attempt to probe directly the physical properties of their neutral gas through infrared observations. A careful analysis of our dataset, performed with a suitable procedure designed to identify faint narrow lines and which can test various possible values for the unknown linewidth value, allowed us to identify a 4-sigma tentative detection of [CII] emission with intrinsic luminosity L_CII=(2.9 +/- 1.4) 10^6 L_sun, one of the lowest values ever detected at high redshift. This study offers a first insight on previously uncharted regions of the L_CII-SFR relation. Despite large uncertainties affecting our measure of the star formation rate, if taken at face value our estimate lies more than 1 dex below the values observed in local and high redshift systems. Our weak detection indicates a deficiency of [CII] emission, possibly ascribed to various explanations, such as a low-density gas and/or a strong radiation field caused by intense stellar feedback, and a low metal content. From the non-detection in the continuum we derive constraints on the dust mass, with 3-sigma upper limit values as low as a few 10^4 M_sun, consistent with the values measured in local metal-poor galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.07302v1-abstract-full').style.display = 'none'; document.getElementById('2010.07302v1-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, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2020. </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">MNRAS, accepted. 15 pages, 5 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/2010.00027">arXiv:2010.00027</a> <span> [<a href="https://arxiv.org/pdf/2010.00027">pdf</a>, <a href="https://arxiv.org/format/2010.00027">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <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/10.1051/0004-6361/202039564">10.1051/0004-6361/202039564 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A new high-precision strong lensing model of the galaxy cluster MACS J0416.1-2403 </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=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=Caminha%2C+G+B">Gabriel Bartosch Caminha</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=Meneghetti%2C+M">Massimo Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Angora%2C+G">Giuseppe Angora</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">Francesco Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">Mario Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Tozzi%2C+P">Paolo Tozzi</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="2010.00027v2-abstract-short" style="display: inline;"> We present a new high-precision parametric strong lensing model of the galaxy cluster MACS J0416.1-2403, at z=0.396, which takes advantage of the MUSE Deep Lensed Field (MDLF), with 17.1h integration in the northeast region of the cluster, and Hubble Frontier Fields data. We spectroscopically identify 182 multiple images from 48 background sources at 0.9<z<6.2, and 171 cluster member galaxies. Sev… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.00027v2-abstract-full').style.display = 'inline'; document.getElementById('2010.00027v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.00027v2-abstract-full" style="display: none;"> We present a new high-precision parametric strong lensing model of the galaxy cluster MACS J0416.1-2403, at z=0.396, which takes advantage of the MUSE Deep Lensed Field (MDLF), with 17.1h integration in the northeast region of the cluster, and Hubble Frontier Fields data. We spectroscopically identify 182 multiple images from 48 background sources at 0.9<z<6.2, and 171 cluster member galaxies. Several multiple images are associated to individual clumps in multiply lensed resolved sources. By defining a new metric, which is sensitive to the gradients of the deflection field, we show that we can accurately reproduce the positions of these star-forming knots despite their vicinity to the model critical lines. The high signal-to-noise ratio of the MDLF spectra enables the measurement of the internal velocity dispersion of 64 cluster galaxies, down to m(F160W)=22. This allowed us to independently estimate the contribution of the subhalo mass component of the lens model from the measured Faber-Jackson scaling relation. Our best reference model, which represents a significant step forward compared to our previous analyses, was selected from a comparative study of different mass parametrizations. The root-mean-square displacement between the observed and model-predicted image positions is only 0.40", which is 33% smaller than in all previous models. The mass model appears to be particularly well constrained in the MDLF region. We characterize the robustness of the magnification map at varying distances from the model critical lines and the total projected mass profile of the cluster. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.00027v2-abstract-full').style.display = 'none'; document.getElementById('2010.00027v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2020. </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, 15 figures. Accepted for publication in Astronomy & Astrophysics (A&A). Lens models are 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 645, A140 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2009.08458">arXiv:2009.08458</a> <span> [<a href="https://arxiv.org/pdf/2009.08458">pdf</a>, <a href="https://arxiv.org/format/2009.08458">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/10.1051/0004-6361/202039466">10.1051/0004-6361/202039466 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MUSE Deep Lensed Field on the Hubble Frontier Field MACS~J0416 </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=Caminha%2C+G+B">G. B. Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">A. Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</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=Sani%2C+E">E. Sani</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=Caputi%2C+K">K. Caputi</a>, <a href="/search/astro-ph?searchtype=author&query=Cristiani%2C+S">S. Cristiani</a>, <a href="/search/astro-ph?searchtype=author&query=Cupani%2C+G">G. Cupani</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">A. Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">R. Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Grazian%2C+A">A. Grazian</a>, <a href="/search/astro-ph?searchtype=author&query=Gronke%2C+M">M. Gronke</a>, <a href="/search/astro-ph?searchtype=author&query=Mignoli%2C+M">M. Mignoli</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">M. Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Tozzi%2C+P">P. Tozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Treu%2C+T">T. Treu</a>, <a href="/search/astro-ph?searchtype=author&query=Balestra%2C+I">I. Balestra</a>, <a href="/search/astro-ph?searchtype=author&query=Dijkstra%2C+M">M. Dijkstra</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="2009.08458v2-abstract-short" style="display: inline;"> Context: A census of faint and tiny star forming complexes at high redshift is key to improving our understanding of reionizing sources, galaxy growth and the formation of globular clusters. Aims: We present the MUSE Deep Lensed Field (MDLF) program. Methods: We describe Deep MUSE observations of 17.1 hours integration on a single pointing over the Hubble Frontier Field galaxy cluster MACS~J0416.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.08458v2-abstract-full').style.display = 'inline'; document.getElementById('2009.08458v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.08458v2-abstract-full" style="display: none;"> Context: A census of faint and tiny star forming complexes at high redshift is key to improving our understanding of reionizing sources, galaxy growth and the formation of globular clusters. Aims: We present the MUSE Deep Lensed Field (MDLF) program. Methods: We describe Deep MUSE observations of 17.1 hours integration on a single pointing over the Hubble Frontier Field galaxy cluster MACS~J0416. Results: We confirm spectroscopic redshifts for all 136 multiple images of 48 source galaxies at 0.9<z<6.2. Within those galaxies, we securely identify 182 multiple images of 66 galaxy components that we use to constrain our lens model. We identify 116 clumps belonging to background high-z galaxies; the majority of them are multiple images and span magnitude, size and redshift intervals of [-18,-10], [~400-3] parsec and 1<z<6.6, respectively, with the most magnified ones probing possible single gravitationally bound star clusters. The depth of the MDLF combined with lensing magnification lead us to reach a detection limit for unresolved emission lines of a few 10$^{-20}$ erg/s/cm2, after correction for lensing magnification. Ultraviolet high-ionization metal lines (and HeII1640) are detected with S/N>10 for individual objects down to de-lensed magnitude 28-30 suggesting that they are common in such faint sources. Conclusions:Deep MUSE observations, in combination with existing HST imaging, allowed us to:(1) confirm redshifts for extremely faint high-z sources;(2) peer into their internal clumps (down to 100-200 pc scale);(3) in some cases break down such clumps into bound star clusters (<20 pc scale);(4) double the number of constraints for the lens model,reaching an unprecedented set of 182 bona-fide multiple images and confirming up to 213 galaxy cluster members. These results demonstrate the power that JWST and future ELTs will have when combined to study gravitational telescopes.[abridged] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.08458v2-abstract-full').style.display = 'none'; document.getElementById('2009.08458v2-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 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2020. </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">43 pages total (17 pages main body); 5 appendices. Accepted for publication in A&A on October 26</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 646, A57 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2009.04838">arXiv:2009.04838</a> <span> [<a href="https://arxiv.org/pdf/2009.04838">pdf</a>, <a href="https://arxiv.org/format/2009.04838">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/abd4d0">10.3847/1538-4357/abd4d0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> ALMA Lensing Cluster Survey: an ALMA galaxy signposting a MUSE galaxy group at z=4.3 behind 'El Gordo' </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Caputi%2C+K+I">K. I. Caputi</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=Fujimoto%2C+S">S. Fujimoto</a>, <a href="/search/astro-ph?searchtype=author&query=Kohno%2C+K">K. Kohno</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+F">F. Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Egami%2C+E">E. Egami</a>, <a href="/search/astro-ph?searchtype=author&query=Deshmukh%2C+S">S. Deshmukh</a>, <a href="/search/astro-ph?searchtype=author&query=Tang%2C+F">F. Tang</a>, <a href="/search/astro-ph?searchtype=author&query=Ao%2C+Y">Y. Ao</a>, <a href="/search/astro-ph?searchtype=author&query=Bradley%2C+L">L. Bradley</a>, <a href="/search/astro-ph?searchtype=author&query=Coe%2C+D">D. Coe</a>, <a href="/search/astro-ph?searchtype=author&query=Espada%2C+D">D. Espada</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Hatsukade%2C+B">B. Hatsukade</a>, <a href="/search/astro-ph?searchtype=author&query=Knudsen%2C+K+K">K. K. Knudsen</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+M+M">M. M. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Magdis%2C+G+E">G. E. Magdis</a>, <a href="/search/astro-ph?searchtype=author&query=Morokuma-Matsui%2C+K">K. Morokuma-Matsui</a>, <a href="/search/astro-ph?searchtype=author&query=Oesch%2C+P">P. Oesch</a>, <a href="/search/astro-ph?searchtype=author&query=Ouchi%2C+M">M. Ouchi</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Umehata%2C+H">H. Umehata</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">F. Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+W+-">W. -H. 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="2009.04838v2-abstract-short" style="display: inline;"> We report the discovery of a Multi Unit Spectroscopic Explorer (MUSE) galaxy group at z=4.32 lensed by the massive galaxy cluster ACT-CL J0102-4915 (aka El Gordo) at z=0.87, associated with a 1.2 mm source which is at a 2.07+/-0.88 kpc projected distance from one of the group galaxies. Three images of the whole system appear in the image plane. The 1.2 mm source has been detected within the Atacam… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.04838v2-abstract-full').style.display = 'inline'; document.getElementById('2009.04838v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.04838v2-abstract-full" style="display: none;"> We report the discovery of a Multi Unit Spectroscopic Explorer (MUSE) galaxy group at z=4.32 lensed by the massive galaxy cluster ACT-CL J0102-4915 (aka El Gordo) at z=0.87, associated with a 1.2 mm source which is at a 2.07+/-0.88 kpc projected distance from one of the group galaxies. Three images of the whole system appear in the image plane. The 1.2 mm source has been detected within the Atacama Large Millimetre/submillimetre Array (ALMA) Lensing Cluster Survey (ALCS). As this ALMA source is undetected at wavelengths lambda < 2 microns, its redshift cannot be independently determined, however, the three lensing components indicate that it belongs to the same galaxy group at z=4.32. The four members of the MUSE galaxy group have low to intermediate stellar masses (~ 10^7-10^{10} Msun) and star formation rates (SFRs) of 0.4-24 Msun/yr, resulting in high specific SFRs (sSFRs) for two of them, which suggest that these galaxies are growing fast (with stellar-mass doubling times of only ~ 2x10^7 years). This high incidence of starburst galaxies is likely a consequence of interactions within the galaxy group, which is compact and has high velocity dispersion. Based on the magnification-corrected sub-/millimetre continuum flux density and estimated stellar mass, we infer that the ALMA source is classified as an ordinary ultra-luminous infrared galaxy (with associated dust-obscured SFR~200-300 Msun/yr) and lies on the star-formation main sequence. This reported case of an ALMA/MUSE group association suggests that some presumably isolated ALMA sources are in fact signposts of richer star-forming environments at high redshifts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.04838v2-abstract-full').style.display = 'none'; document.getElementById('2009.04838v2-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 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2020. </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 including 7 figures and 1 table. Accepted for publication at the ApJ. Minor changes with respect to version 1. Figure 6 has been expanded to broaden comparison with the literature</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=Caminha%2C+G+B&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Caminha%2C+G+B&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Caminha%2C+G+B&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Caminha%2C+G+B&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </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 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