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<button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Dolphin%2C+A&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Dolphin%2C+A&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Dolphin%2C+A&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Dolphin%2C+A&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Dolphin%2C+A&start=150" class="pagination-link " aria-label="Page 4" aria-current="page">4 </a> </li> <li> <a 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VIII. The Spatially Resolved Star Formation History of WLM </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">Roger E. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=McQuinn%2C+K+B+W">Kristen B. W. McQuinn</a>, <a href="/search/astro-ph?searchtype=author&query=Savino%2C+A">Alessandro Savino</a>, <a href="/search/astro-ph?searchtype=author&query=Newman%2C+M+J+B">Max J. B. Newman</a>, <a href="/search/astro-ph?searchtype=author&query=Weisz%2C+D+R">Daniel R. Weisz</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">Andrew E. Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Boyer%2C+M+L">Martha L. Boyer</a>, <a href="/search/astro-ph?searchtype=author&query=Correnti%2C+M">Matteo Correnti</a>, <a href="/search/astro-ph?searchtype=author&query=Geha%2C+M+C">Marla C. Geha</a>, <a href="/search/astro-ph?searchtype=author&query=Gennaro%2C+M">Mario Gennaro</a>, <a href="/search/astro-ph?searchtype=author&query=Gilbert%2C+K+M">Karoline M. Gilbert</a>, <a href="/search/astro-ph?searchtype=author&query=Kallivayalil%2C+N">Nitya Kallivayalil</a>, <a href="/search/astro-ph?searchtype=author&query=Warfield%2C+J+T">Jack T. Warfield</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+F">Benjamin F. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+A+M">Alyson M. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+A+A">Andrew A. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Skillman%2C+E+D">Evan D. Skillman</a>, <a href="/search/astro-ph?searchtype=author&query=Garling%2C+C+T">Christopher T. Garling</a>, <a href="/search/astro-ph?searchtype=author&query=Kalirai%2C+J+S">Jason S. Kalirai</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">Jay Anderson</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2502.13887v1-abstract-short" style="display: inline;"> We measure radial stellar age gradients in the relatively isolated gas-rich dwarf irregular WLM, combining JWST NIRCam and NIRISS imaging with six archival Hubble fields over semi-major axis equivalent distances of 0$\lesssim$R$_{SMA}$$\lesssim$4 kpc ($\lesssim$3R$_{hl}$). Fitting lifetime star formation histories (SFHs) to resolved color-magnitude diagrams (CMDs), radial age gradients are quantif… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.13887v1-abstract-full').style.display = 'inline'; document.getElementById('2502.13887v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.13887v1-abstract-full" style="display: none;"> We measure radial stellar age gradients in the relatively isolated gas-rich dwarf irregular WLM, combining JWST NIRCam and NIRISS imaging with six archival Hubble fields over semi-major axis equivalent distances of 0$\lesssim$R$_{SMA}$$\lesssim$4 kpc ($\lesssim$3R$_{hl}$). Fitting lifetime star formation histories (SFHs) to resolved color-magnitude diagrams (CMDs), radial age gradients are quantified using $蟿_{90}$ and $蟿_{50}$, the lookback times to form 90\% and 50\% of the cumulative stellar mass. We find that globally, the outskirts of WLM are older on average, with ($未$$蟿_{90}$, $未$$蟿_{50}$)/$未$R$_{SMA}=$(0.82$^{+0.10}_{-0.10}$, 1.60$^{+0.23}_{-0.22}$) Gyr/kpc (stat.), in good agreement with simulations. However, we also detect an azimuthal dependence of radial stellar age gradients, finding that stars on the leading edge of WLM (relative to its proper motion) are both younger and have a flatter age gradient compared to the trailing edge. This difference persists over 0.6$\lesssim$R$_{SMA}$$\lesssim$3.2 kpc ($\sim$0.5$-$2.5R$_{hl}$) and lookback times up to $\sim$8 Gyr, and is robust to assumed stellar evolutionary model. Our results are consistent with star formation triggered by ram pressure stripping from a circumgalactic and/or intergalactic medium, suggested by recent HI observations. If confirmed, processes typifying dense environments, such as ram pressure stripping, may be more relevant to the evolution of isolated galaxies than previously thought. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.13887v1-abstract-full').style.display = 'none'; document.getElementById('2502.13887v1-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 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">ApJ in press. 23 pages, 8 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/2501.13152">arXiv:2501.13152</a> <span> [<a href="https://arxiv.org/pdf/2501.13152">pdf</a>, <a href="https://arxiv.org/format/2501.13152">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/0.3847/1538-4357/ada24f">0.3847/1538-4357/ada24f <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Hubble Space Telescope Survey of M31 Satellite Galaxies IV. Survey Overview and Lifetime Star Formation Histories </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Savino%2C+A">A. Savino</a>, <a href="/search/astro-ph?searchtype=author&query=Weisz%2C+D+R">D. R. Weisz</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">A. E. Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Durbin%2C+M+J">M. J. Durbin</a>, <a href="/search/astro-ph?searchtype=author&query=Kallivayalil%2C+N">N. Kallivayalil</a>, <a href="/search/astro-ph?searchtype=author&query=Wetzel%2C+A">A. Wetzel</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Besla%2C+G">G. Besla</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=Brown%2C+T+M">T. M. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Bullock%2C+J+S">J. S. Bullock</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+A+A">A. A. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Collins%2C+M+L+M">M. L. M. Collins</a>, <a href="/search/astro-ph?searchtype=author&query=Cooper%2C+M+C">M. C. Cooper</a>, <a href="/search/astro-ph?searchtype=author&query=Deason%2C+A+J">A. J. Deason</a>, <a href="/search/astro-ph?searchtype=author&query=Dotter%2C+A+L">A. L. Dotter</a>, <a href="/search/astro-ph?searchtype=author&query=Fardal%2C+M">M. Fardal</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+A+M+N">A. M. N. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Fritz%2C+T+K">T. K. Fritz</a>, <a href="/search/astro-ph?searchtype=author&query=Geha%2C+M+C">M. C. Geha</a>, <a href="/search/astro-ph?searchtype=author&query=Gilbert%2C+K+M">K. M. Gilbert</a>, <a href="/search/astro-ph?searchtype=author&query=Guhathakurta%2C+P">P. Guhathakurta</a>, <a href="/search/astro-ph?searchtype=author&query=Ibata%2C+R">R. Ibata</a>, <a href="/search/astro-ph?searchtype=author&query=Irwin%2C+M+J">M. J. Irwin</a>, <a href="/search/astro-ph?searchtype=author&query=Jeon%2C+M">M. Jeon</a> , et al. (13 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2501.13152v1-abstract-short" style="display: inline;"> From $>1000$ orbits of HST imaging, we present deep homogeneous resolved star color-magnitude diagrams that reach the oldest main sequence turnoff and uniformly measured star formation histories (SFHs) of 36 dwarf galaxies ($-6 \ge M_V \ge -17$) associated with the M31 halo, and for 10 additional fields in M31, M33, and the Giant Stellar Stream. From our SFHs we find: i) the median stellar age and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.13152v1-abstract-full').style.display = 'inline'; document.getElementById('2501.13152v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.13152v1-abstract-full" style="display: none;"> From $>1000$ orbits of HST imaging, we present deep homogeneous resolved star color-magnitude diagrams that reach the oldest main sequence turnoff and uniformly measured star formation histories (SFHs) of 36 dwarf galaxies ($-6 \ge M_V \ge -17$) associated with the M31 halo, and for 10 additional fields in M31, M33, and the Giant Stellar Stream. From our SFHs we find: i) the median stellar age and quenching epoch of M31 satellites correlate with galaxy luminosity and galactocentric distance. Satellite luminosity and present-day distance from M31 predict the satellite quenching epoch to within $1.8$ Gyr at all epochs. This tight relationship highlights the fundamental connection between satellite halo mass, environmental history, and star formation duration. ii) There is no difference between the median SFH of galaxies on and off the great plane of Andromeda satellites. iii) $\sim50$\% of our M31 satellites show prominent ancient star formation ($>12$ Gyr ago) followed by delayed quenching ($8-10$ Gyr ago), which is not commonly observed among the MW satellites. iv) A comparison with TNG50 and FIRE-2 simulated satellite dwarfs around M31-like hosts show that some of these trends (dependence of SFH on satellite luminosity) are reproduced in the simulations while others (dependence of SFH on galactocentric distance, presence of the delayed-quenching population) are weaker or absent. We provide all photometric catalogs and SFHs as High-Level Science Products on MAST. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.13152v1-abstract-full').style.display = 'none'; document.getElementById('2501.13152v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication on ApJ. 47 pages, 24 figures, 12 tables. Corresponding HLSP data can be retrieved at: https://archive.stsci.edu/hlsp/m31-satellites</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.06290">arXiv:2501.06290</a> <span> [<a href="https://arxiv.org/pdf/2501.06290">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ad8eb7">10.3847/1538-4357/ad8eb7 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Catalog of Stellar and Dust Properties for 500,000 Stars in the Southwest Bar of the Small Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Merica-Jones%2C+P+Y">Petia Yanchulova Merica-Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Gordon%2C+K">Karl Gordon</a>, <a href="/search/astro-ph?searchtype=author&query=Sandstrom%2C+K">Karin Sandstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Murray%2C+C+E">Claire E. Murray</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+L+C">L. Clifton Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Dalcanton%2C+J+J">Julianne J. Dalcanton</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Duval%2C+J">Julia Roman-Duval</a>, <a href="/search/astro-ph?searchtype=author&query=Chastenet%2C+J">Jeremy Chastenet</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+F">Benjamin F. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Weisz%2C+D+R">Daniel R. Weisz</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">Andrew E. Dolphin</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="2501.06290v1-abstract-short" style="display: inline;"> We present a catalog of individual stellar and dust extinction properties along close to 500,000 sight lines in the southwest bar of the Small Magellanic Cloud (SMC). The catalog is based on multiband Hubble Space Telescope photometric data spanning near-ultraviolet to near-infrared wavelengths from the Small Magellanic Cloud Investigation of Dust and Gas Evolution survey (SMIDGE) covering a 100 x… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.06290v1-abstract-full').style.display = 'inline'; document.getElementById('2501.06290v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.06290v1-abstract-full" style="display: none;"> We present a catalog of individual stellar and dust extinction properties along close to 500,000 sight lines in the southwest bar of the Small Magellanic Cloud (SMC). The catalog is based on multiband Hubble Space Telescope photometric data spanning near-ultraviolet to near-infrared wavelengths from the Small Magellanic Cloud Investigation of Dust and Gas Evolution survey (SMIDGE) covering a 100 x 200 pc area. We use the probabilistic technique of the Bayesian Extinction And Stellar Tool (BEAST) to model the spectral energy distributions of individual stars in SMIDGE and include the effects of observational uncertainties in the data. We compare BEAST-derived dust extinction properties with tracers of the interstellar medium, such as the emission from the 12CO (2-1) transition (I(CO)), the dust mass surface density (危dust) from far-IR emission, the H I column density (N(HI)) from the 21cm transition, and the mass fraction of polycyclic aromatic hydrocarbons (PAHs; qPAH, derived from IR emission). We find that the dust extinction (A(V )) in the SMIDGE field is strongly correlated with 危dust and I(CO), and less so with N(HI) and qPAH, and suggest potential explanations. Our extinction measurements are also sensitive to the presence of the 2175 脜 bump in the extinction curve toward UV bright stars. While most do not show evidence for the bump, we identify ~200 lines of sight that are 2175 脜 bump candidates. Furthermore, we find distinct structures in the dust extinction-distance distributions that provide insights into the 3D geometry of the SMC. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.06290v1-abstract-full').style.display = 'none'; document.getElementById('2501.06290v1-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 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 13 figures, 4 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 978 144 (2025) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.20454">arXiv:2410.20454</a> <span> [<a href="https://arxiv.org/pdf/2410.20454">pdf</a>, <a href="https://arxiv.org/format/2410.20454">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/ad76af">10.3847/1538-4365/ad76af <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Local Ultraviolet to Infrared Treasury I. Survey Overview of the Broadband Imaging </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gilbert%2C+K+M">Karoline M. Gilbert</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+Y">Yumi Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Boyer%2C+M+L">Martha L. Boyer</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+F">Benjamin F. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Weisz%2C+D+R">Daniel R. Weisz</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Dalcanton%2C+J+J">Julianne J. Dalcanton</a>, <a href="/search/astro-ph?searchtype=author&query=McQuinn%2C+K+B+W">Kristen B. W. McQuinn</a>, <a href="/search/astro-ph?searchtype=author&query=Skillman%2C+E+D">Evan D. Skillman</a>, <a href="/search/astro-ph?searchtype=author&query=Costa%2C+G">Guglielmo Costa</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">Andrew E. Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Fouesneau%2C+M">Morgan Fouesneau</a>, <a href="/search/astro-ph?searchtype=author&query=Girardi%2C+L">L茅o Girardi</a>, <a href="/search/astro-ph?searchtype=author&query=Goldman%2C+S+R">Steven R. Goldman</a>, <a href="/search/astro-ph?searchtype=author&query=Gordon%2C+K+D">Karl D. Gordon</a>, <a href="/search/astro-ph?searchtype=author&query=Guhathakurta%2C+P">Puragra Guhathakurta</a>, <a href="/search/astro-ph?searchtype=author&query=Gull%2C+M">Maude Gull</a>, <a href="/search/astro-ph?searchtype=author&query=Hagen%2C+L">Lea Hagen</a>, <a href="/search/astro-ph?searchtype=author&query=Huynh%2C+K">Ky Huynh</a>, <a href="/search/astro-ph?searchtype=author&query=Lindberg%2C+C+W">Christina W. Lindberg</a>, <a href="/search/astro-ph?searchtype=author&query=Marigo%2C+P">Paola Marigo</a>, <a href="/search/astro-ph?searchtype=author&query=Murray%2C+C+E">Claire E. Murray</a>, <a href="/search/astro-ph?searchtype=author&query=Pastorelli%2C+G">Giada Pastorelli</a>, <a href="/search/astro-ph?searchtype=author&query=Merica-Jones%2C+P+Y">Petia Yanchulova Merica-Jones</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="2410.20454v2-abstract-short" style="display: inline;"> The Local Ultraviolet to Infrared Treasury (LUVIT) is a Hubble Space Telescope program that combines newly acquired data in the near ultraviolet (NUV), optical, and near infrared (NIR) with archival optical and NIR imaging to produce multiband panchromatic resolved stellar catalogs for 23 pointings in 22 low-mass, star-forming galaxies ranging in distance from the outskirts of the Local Group to ~… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.20454v2-abstract-full').style.display = 'inline'; document.getElementById('2410.20454v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.20454v2-abstract-full" style="display: none;"> The Local Ultraviolet to Infrared Treasury (LUVIT) is a Hubble Space Telescope program that combines newly acquired data in the near ultraviolet (NUV), optical, and near infrared (NIR) with archival optical and NIR imaging to produce multiband panchromatic resolved stellar catalogs for 23 pointings in 22 low-mass, star-forming galaxies ranging in distance from the outskirts of the Local Group to ~3.8 Mpc. We describe the survey design, detail the LUVIT broadband filter observations and the archival datasets included in the LUVIT reductions, and summarize the simultaneous multiband data reduction steps. The spatial distributions and color-magnitude diagrams (CMDs) from the resulting stellar catalogs are presented for each target, from the NUV to the NIR. We demonstrate in which regions of the CMDs stars with NUV and optical, optical and NIR, and NUV through NIR detections reside. For each target, we use the results from artificial star tests to measure representative completeness, bias, and total photometric uncertainty as a function of magnitude in each broadband filter. We also assess which LUVIT targets have significant spatial variation in the fraction of stars recovered at a given magnitude. The panchromatic LUVIT stellar catalogs will provide a rich legacy dataset for a host of resolved stellar population studies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.20454v2-abstract-full').style.display = 'none'; document.getElementById('2410.20454v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 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">48 pages, 14 figures, 8 tables, published in ApJS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal Supplement Series, 2025, Volume 276, Issue 1, id.8, 33 pp </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.11697">arXiv:2410.11697</a> <span> [<a href="https://arxiv.org/pdf/2410.11697">pdf</a>, <a href="https://arxiv.org/format/2410.11697">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"> Scylla III. The Outside-In Radial Age Gradient in the Small Magellanic Cloud and the Star Formation Histories of the Main Body, Wing and Outer Regions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">Roger E. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=McQuinn%2C+K+B+W">Kristen B. W. McQuinn</a>, <a href="/search/astro-ph?searchtype=author&query=Murray%2C+C+E">Claire E. Murray</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+F">Benjamin F. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+Y">Yumi Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Lindberg%2C+C+W">Christina W. Lindberg</a>, <a href="/search/astro-ph?searchtype=author&query=Burhenne%2C+C">Clare Burhenne</a>, <a href="/search/astro-ph?searchtype=author&query=Gordon%2C+K+D">Karl D. Gordon</a>, <a href="/search/astro-ph?searchtype=author&query=Merica-Jones%2C+P+Y">Petia Yanchulova Merica-Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Bot%2C+C">Caroline Bot</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">Andrew E. Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Gilbert%2C+K+M">Karoline M. Gilbert</a>, <a href="/search/astro-ph?searchtype=author&query=Goldman%2C+S">Steven Goldman</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschauer%2C+A+S">Alec S. Hirschauer</a>, <a href="/search/astro-ph?searchtype=author&query=Sandstrom%2C+K+M">Karin M. Sandstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Telford%2C+O+G">O. Grace Telford</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="2410.11697v1-abstract-short" style="display: inline;"> The proximity of the Large and Small Magellanic Clouds (LMC and SMC) provides the opportunity to study the impact of dwarf-dwarf interactions on their mass assembly with a unique level of detail. To this end, we analyze two-filter broadband imaging of 83 Hubble Space Telescope (HST) pointings covering 0.203 deg$^2$ towards the SMC, extending out to $\sim$3.5 kpc in projection from its optical cent… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.11697v1-abstract-full').style.display = 'inline'; document.getElementById('2410.11697v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.11697v1-abstract-full" style="display: none;"> The proximity of the Large and Small Magellanic Clouds (LMC and SMC) provides the opportunity to study the impact of dwarf-dwarf interactions on their mass assembly with a unique level of detail. To this end, we analyze two-filter broadband imaging of 83 Hubble Space Telescope (HST) pointings covering 0.203 deg$^2$ towards the SMC, extending out to $\sim$3.5 kpc in projection from its optical center. Lifetime star formation histories (SFHs) fit to each pointing independently reveal an outside-in age gradient such that fields in the SMC outskirts are older on average. We measure radial gradients of the lookback time to form 90%, 75% and 50% of the cumulative stellar mass for the first time, finding $未$($蟿_{90}$, $蟿_{75}$, $蟿_{50}$)/$未$R = (0.61$^{+0.08}_{-0.07}$, 0.65$^{+0.09}_{-0.08}$, 0.82$^{+0.12}_{-0.16}$) Gyr/kpc assuming PARSEC evolutionary models and a commonly used elliptical geometry of the SMC, although our results are robust to these assumptions. The wing of the SMC deviates from this trend, forming 25\% of its cumulative mass over the most recent 3 Gyr due to a best-fit star formation rate that remains approximately constant. Our results are consistent with chemodynamical evidence of a tidally stripped SMC component in the foreground, and imply contributions to the observed SFH from multiple previous LMC-SMC interactions. We also compare our SMC SFH with results from a companion study of the LMC, finding that while the two galaxies present different internal, spatially resolved SFH trends, both the LMC and SMC have similar near-constant lifetime SFHs when viewed globally. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.11697v1-abstract-full').style.display = 'none'; document.getElementById('2410.11697v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 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">ApJ in press. 40 pages, 18 figures, 5 tables including Appendices</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.11696">arXiv:2410.11696</a> <span> [<a href="https://arxiv.org/pdf/2410.11696">pdf</a>, <a href="https://arxiv.org/format/2410.11696">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"> Scylla II. The Spatially Resolved Star Formation History of the Large Magellanic Cloud Reveals an Inverted Radial Age Gradient </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">Roger E. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=McQuinn%2C+K+B+W">Kristen B. W. McQuinn</a>, <a href="/search/astro-ph?searchtype=author&query=Murray%2C+C+E">Claire E. Murray</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+F">Benjamin F. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+Y">Yumi Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Lindberg%2C+C+W">Christina W. Lindberg</a>, <a href="/search/astro-ph?searchtype=author&query=Burhenne%2C+C">Clare Burhenne</a>, <a href="/search/astro-ph?searchtype=author&query=Gordon%2C+K+D">Karl D. Gordon</a>, <a href="/search/astro-ph?searchtype=author&query=Merica-Jones%2C+P+Y">Petia Yanchulova Merica-Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Gilbert%2C+K+M">Karoline M. Gilbert</a>, <a href="/search/astro-ph?searchtype=author&query=Boyer%2C+M+L">Martha L. Boyer</a>, <a href="/search/astro-ph?searchtype=author&query=Goldman%2C+S">Steven Goldman</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">Andrew E. Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Telford%2C+O+G">O. Grace Telford</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="2410.11696v1-abstract-short" style="display: inline;"> The proximity of the Magellanic Clouds provides the opportunity to study interacting dwarf galaxies near a massive host, and spatial trends in their stellar population properties in particular, with a unique level of detail. The Scylla pure parallel program has obtained deep (80% complete to >1 mag below the ancient main sequence turnoff), homogeneous two-filter Hubble Space Telescope (HST) imagin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.11696v1-abstract-full').style.display = 'inline'; document.getElementById('2410.11696v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.11696v1-abstract-full" style="display: none;"> The proximity of the Magellanic Clouds provides the opportunity to study interacting dwarf galaxies near a massive host, and spatial trends in their stellar population properties in particular, with a unique level of detail. The Scylla pure parallel program has obtained deep (80% complete to >1 mag below the ancient main sequence turnoff), homogeneous two-filter Hubble Space Telescope (HST) imaging sampling the inner star-forming disk of the Large Magellanic Cloud (LMC), the perfect complement to shallower, contiguous ground-based surveys. We harness this imaging together with extant archival data and fit lifetime star formation histories (SFHs) to resolved color-magnitude diagrams (CMDs) of 111 individual fields, using three different stellar evolutionary libraries. We validate per-field recovered distances and extinctions as well as the combined global LMC age-metallicity relation and SFH against independent estimates. We find that the present-day radial age gradient reverses from an inside-out gradient in the inner disk to an outside-in gradient beyond $\sim$2 disk scalelengths, supported by ground-based measurements. The gradients become relatively flatter at earlier lookback times, while the location of the inversion remains constant over an order of magnitude in lookback time, from $\sim$1$-$10 Gyr. This suggests at least one mechanism that predates the recent intense LMC-SMC interaction. We compare observed radial age trends to other late-type galaxies at fixed stellar mass and discuss similarities and differences in the context of potential drivers, implying strong radial migration in the LMC. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.11696v1-abstract-full').style.display = 'none'; document.getElementById('2410.11696v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 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">ApJ in press. 45 pages, 17 figures, 9 tables including Appendices</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.11695">arXiv:2410.11695</a> <span> [<a href="https://arxiv.org/pdf/2410.11695">pdf</a>, <a href="https://arxiv.org/format/2410.11695">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"> Scylla I: A pure-parallel, multi-wavelength imaging survey of the ULLYSES fields in the LMC and SMC </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Murray%2C+C+E">Claire E. Murray</a>, <a href="/search/astro-ph?searchtype=author&query=Lindberg%2C+C+W">Christina W. Lindberg</a>, <a href="/search/astro-ph?searchtype=author&query=Merica-Jones%2C+P+Y">Petia Yanchulova Merica-Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+F">Benjamin F. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">Roger E. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Gordon%2C+K+D">Karl D. Gordon</a>, <a href="/search/astro-ph?searchtype=author&query=McQuinn%2C+K+B+W">Kristen B. W. McQuinn</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+Y">Yumi Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Burhenne%2C+C">Clare Burhenne</a>, <a href="/search/astro-ph?searchtype=author&query=Sandstrom%2C+K+M">Karin M. Sandstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Bot%2C+C">Caroline Bot</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+L+C">L. Clifton Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Goldman%2C+S+R">Steven R. Goldman</a>, <a href="/search/astro-ph?searchtype=author&query=Clark%2C+C+J+R">Christopher J. R. Clark</a>, <a href="/search/astro-ph?searchtype=author&query=Roman-Duval%2C+J+C">Julia C. Roman-Duval</a>, <a href="/search/astro-ph?searchtype=author&query=Gilbert%2C+K+M">Karoline M. Gilbert</a>, <a href="/search/astro-ph?searchtype=author&query=Peek%2C+J+E+G">J. E. G. Peek</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschauer%2C+A+S">Alec S. Hirschauer</a>, <a href="/search/astro-ph?searchtype=author&query=Boyer%2C+M+L">Martha L. Boyer</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">Andrew E. Dolphin</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="2410.11695v1-abstract-short" style="display: inline;"> Scylla is a deep Hubble Space Telescope survey of the stellar populations, interstellar medium and star formation in the LMC and SMC. As a pure-parallel complement to the Ultraviolet Legacy Library of Young Stars as Essential Standards (ULLYSES) survey, Scylla obtained 342 orbits of ultraviolet (UV) through near-infrared (IR) imaging of the LMC and SMC with Wide Field Camera 3. In this paper, we d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.11695v1-abstract-full').style.display = 'inline'; document.getElementById('2410.11695v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.11695v1-abstract-full" style="display: none;"> Scylla is a deep Hubble Space Telescope survey of the stellar populations, interstellar medium and star formation in the LMC and SMC. As a pure-parallel complement to the Ultraviolet Legacy Library of Young Stars as Essential Standards (ULLYSES) survey, Scylla obtained 342 orbits of ultraviolet (UV) through near-infrared (IR) imaging of the LMC and SMC with Wide Field Camera 3. In this paper, we describe the science objectives, observing strategy, data reduction procedure, and initial results from our photometric analysis of 96 observed fields. Although our observations were constrained by ULYSSES primary exposures, we imaged all fields in at least two filters (F475W and F814W), and 64% of fields in at least three and as many as seven WFC3 filters spanning the UV to IR. Overall, we reach average 50% completeness of $m_{\rm F225W}=26.0$, $m_{\rm F275W}=26.2$, $m_{\rm F336W}=26.9$, $m_{\rm F475W}=27.8$, $m_{\rm F814W}=25.5$, $m_{\rm F110W}=24.7$, and $m_{\rm F160W}=24.0$ Vega magnitudes in our photometric catalogs, which is faintward of the ancient main sequence turnoff in all filters. The primary science goals of Scylla include characterizing the structure and properties of dust in the MCs, as well as their spatially-resolved star formation and chemical enrichment histories. Our images and photometric catalogs, which represent the widest-area coverage of MCs with HST photometry to date, are available as a high-level science product at the Barbara A. Mikulski Archive for Space Telescopes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.11695v1-abstract-full').style.display = 'none'; document.getElementById('2410.11695v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 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">25 pages, 16 figures, 8 tables. Accepted for publication in ApJS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.09256">arXiv:2410.09256</a> <span> [<a href="https://arxiv.org/pdf/2410.09256">pdf</a>, <a href="https://arxiv.org/format/2410.09256">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="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Measuring Star Formation Histories from Asymptotic Giant Branch Stars: A Demonstration in M31 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lee%2C+A+J">Abigail J. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Weisz%2C+D+R">Daniel R. Weisz</a>, <a href="/search/astro-ph?searchtype=author&query=Ren%2C+Y">Yi Ren</a>, <a href="/search/astro-ph?searchtype=author&query=Savino%2C+A">Alessandro Savino</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">Andrew E. Dolphin</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="2410.09256v2-abstract-short" style="display: inline;"> We demonstrate how near infrared (NIR) imaging of resolved luminous asymptotic giant branch (AGB) stars can be used to measure well-constrained star formation histories (SFHs) across cosmic time. Using UKIRT J and K-band imaging of M31, we first show excellent agreement over the past $\sim8$ Gyr between the PHAT SFH of M31's outer disk derived from a deep optical color-magnitude diagram (CMD;… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.09256v2-abstract-full').style.display = 'inline'; document.getElementById('2410.09256v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.09256v2-abstract-full" style="display: none;"> We demonstrate how near infrared (NIR) imaging of resolved luminous asymptotic giant branch (AGB) stars can be used to measure well-constrained star formation histories (SFHs) across cosmic time. Using UKIRT J and K-band imaging of M31, we first show excellent agreement over the past $\sim8$ Gyr between the PHAT SFH of M31's outer disk derived from a deep optical color-magnitude diagram (CMD; $\sim3.3\times10^{7}$ stars with $M_{F814W} \lesssim +2$), and our spatially-matched SFH based only on modeling AGB stars on a NIR CMD ($\sim2.3\times10^{4}$ stars with $M_{J} \lesssim -5$). We find that only hundreds of AGB stars are needed for reliable SFH recovery, owing to their excellent age sensitivity in the NIR. We then measure the spatially resolved SFH of M31's inner stellar halo ($D_{M31, projected} \sim20-30$ kpc) using $\sim10^4$ AGB stars. We find: (i) a dominant burst of star formation across M31's inner stellar halo from $4-5$ Gyr ago and lower level, spatially distributed star formation $\sim1-2$ Gyr ago; (ii) a younger 'quenching time' in the vicinity of NGC 205 ($\sim1$ Gyr ago) than near M32 ($\sim1.6$ Gyr ago); (iii) $M_{\star}\sim4\pm0.5\times10^9 M_{\odot}$ formed over the past $\sim8$ Gyr. We discuss some caveats and the enormous potential of resolved AGB stars in the NIR for measuring SFHs back to ancient epochs ($\sim13$ Gyr ago) in galaxies to large distances ($D\gtrsim20$ Mpc) with JWST, Roman, and Euclid. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.09256v2-abstract-full').style.display = 'none'; document.getElementById('2410.09256v2-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 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">25 pages, 19 figures, submitted to AAS Journals, typos in abstract were fixed in v2</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.19050">arXiv:2409.19050</a> <span> [<a href="https://arxiv.org/pdf/2409.19050">pdf</a>, <a href="https://arxiv.org/format/2409.19050">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The Ancient Star Formation History of the Extremely Low-Mass Galaxy Leo P: An Emerging Trend of a Post-Reionization Pause in Star Formation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=McQuinn%2C+K+B+W">Kristen B. W. McQuinn</a>, <a href="/search/astro-ph?searchtype=author&query=Newman%2C+M+J+B">Max J. B. Newman</a>, <a href="/search/astro-ph?searchtype=author&query=Skillman%2C+E+D">Evan D. Skillman</a>, <a href="/search/astro-ph?searchtype=author&query=Telford%2C+O+G">O. Grace Telford</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+A">Alyson Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+E+A+K">Elizabeth A. K. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Berg%2C+D+A">Danielle A. Berg</a>, <a href="/search/astro-ph?searchtype=author&query=Boyer%2C+M+L">Martha L. Boyer</a>, <a href="/search/astro-ph?searchtype=author&query=Cannon%2C+J+M">John M. Cannon</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">Andrew E. Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Pahl%2C+A">Anthony Pahl</a>, <a href="/search/astro-ph?searchtype=author&query=Rhode%2C+K+L">Katherine L. Rhode</a>, <a href="/search/astro-ph?searchtype=author&query=Salzer%2C+J+J">John J. Salzer</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">Roger E. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Goldman%2C+S+R">Steve R. Goldman</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.19050v1-abstract-short" style="display: inline;"> Isolated, low-mass galaxies provide the opportunity to assess the impact of reionization on their star formation histories (SFHs) without the ambiguity of environmental processes associated with massive host galaxies. There are very few isolated, low-mass galaxies that are close enough to determine their SFHs from resolved star photometry reaching below the oldest main sequence turnoff. JWST has i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.19050v1-abstract-full').style.display = 'inline'; document.getElementById('2409.19050v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.19050v1-abstract-full" style="display: none;"> Isolated, low-mass galaxies provide the opportunity to assess the impact of reionization on their star formation histories (SFHs) without the ambiguity of environmental processes associated with massive host galaxies. There are very few isolated, low-mass galaxies that are close enough to determine their SFHs from resolved star photometry reaching below the oldest main sequence turnoff. JWST has increased the volume for which this is possible, and here we report on JWST observations of the low-mass, isolated galaxy Leo P. From NIRCam imaging in F090W, F150W, and F277W, we derive a SFH which shows early star formation followed by a pause subsequent to the epoch of reionization which is then later followed by a re-ignition of star formation. This is very similar to the SFHs from previous studies of other dwarf galaxies in the ``transition zone'' between quenched very low-mass galaxies and the more massive galaxies which show no evidence of the impact of reionization on their SFHs; this pattern is rarely produced in simulations of SFHs. The lifetime SFH reveals that Leo P's stellar mass at the epoch of reionization was in the range that is normally associated with being totally quenched. The extended pause in star formation from z~5-1 has important implications for the contribution of low-mass galaxies to the UV photon budget at intermediate redshifts. We also demonstrate that, due to higher sensitivity and angular resolution, observing in two NIRCam short wavelength filters is superior to observing in a combination of a short and a long wavelength filter. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.19050v1-abstract-full').style.display = 'none'; document.getElementById('2409.19050v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 9 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/2407.04698">arXiv:2407.04698</a> <span> [<a href="https://arxiv.org/pdf/2407.04698">pdf</a>, <a href="https://arxiv.org/format/2407.04698">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"> Stellar Metallicities and Gradients in the Faint M31 Satellites Andromeda XVI and Andromeda XXVIII </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fu%2C+S+W">Sal Wanying Fu</a>, <a href="/search/astro-ph?searchtype=author&query=Weisz%2C+D+R">Daniel R. Weisz</a>, <a href="/search/astro-ph?searchtype=author&query=Starkenburg%2C+E">Else Starkenburg</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+N">Nicolas Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Collins%2C+M+L+M">Michelle L. M. Collins</a>, <a href="/search/astro-ph?searchtype=author&query=Savino%2C+A">Alessandro Savino</a>, <a href="/search/astro-ph?searchtype=author&query=Boylan-Kolchin%2C+M">Michael Boylan-Kolchin</a>, <a href="/search/astro-ph?searchtype=author&query=C%C3%B4t%C3%A9%2C+P">Patrick C么t茅</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">Andrew E. Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Longeard%2C+N">Nicolas Longeard</a>, <a href="/search/astro-ph?searchtype=author&query=Mateo%2C+M+L">Mario L. Mateo</a>, <a href="/search/astro-ph?searchtype=author&query=Mercado%2C+F+J">Francisco J. Mercado</a>, <a href="/search/astro-ph?searchtype=author&query=Sandford%2C+N+R">Nathan R. Sandford</a>, <a href="/search/astro-ph?searchtype=author&query=Skillman%2C+E+D">Evan D. Skillman</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="2407.04698v1-abstract-short" style="display: inline;"> We present $\sim300$ stellar metallicity measurements in two faint M31 dwarf galaxies, Andromeda XVI ($M_V = -7.5$) and Andromeda XXVIII ($M_V = -8.8$) derived using metallicity-sensitive Calcium H & K narrow-band Hubble Space Telescope imaging. These are the first individual stellar metallicities in And~XVI (95 stars). Our And~XXVIII sample (191 stars) is a factor of $\sim15$ increase over litera… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.04698v1-abstract-full').style.display = 'inline'; document.getElementById('2407.04698v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.04698v1-abstract-full" style="display: none;"> We present $\sim300$ stellar metallicity measurements in two faint M31 dwarf galaxies, Andromeda XVI ($M_V = -7.5$) and Andromeda XXVIII ($M_V = -8.8$) derived using metallicity-sensitive Calcium H & K narrow-band Hubble Space Telescope imaging. These are the first individual stellar metallicities in And~XVI (95 stars). Our And~XXVIII sample (191 stars) is a factor of $\sim15$ increase over literature metallicities. For And~XVI, we measure $\langle \mbox{[Fe/H]}\rangle = -2.17^{+0.05}_{-0.05}$, $蟽_{\mbox{[Fe/H]}}=0.33^{+0.07}_{-0.07}$, and $\nabla_{\mbox{[Fe/H]}} = -0.23\pm0.15$ dex $R_e^{-1}$. We find that And XVI is more metal-rich than MW UFDs of similar luminosity, which may be a result of its unusually extended star formation history. For And XXVIII, we measure $\langle \mbox{[Fe/H]}\rangle = -1.95^{+0.04}_{-0.04}$, $蟽_{\mbox{[Fe/H]}}=0.34^{+0.07}_{-0.07}$, and $\nabla_{\mbox{[Fe/H]}} = -0.46 \pm 0.10$~dex~$R_e^{-1}$, placing it on the dwarf galaxy mass-metallicity relation. Neither galaxy has a metallicity distribution function with an abrupt metal-rich truncation, suggesting that star formation fell off gradually. The stellar metallicity gradient measurements are among the first for faint ($L \lesssim 10^6~L_{\odot}$) galaxies outside the Milky Way halo. Both galaxies' gradients are consistent with predictions from the FIRE simulations, where an age-gradient strength relationship is the observational consequence of stellar feedback that produces dark matter cores. We include a catalog for community spectroscopic follow-up, including 19 extremely metal poor ($\mbox{[Fe/H]} < -3.0$) star candidates, which make up 7% of And~XVI's MDF and 6% of And~XXVIII's. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.04698v1-abstract-full').style.display = 'none'; document.getElementById('2407.04698v1-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 5 figures, 4 tables, ApJ submitted; comments welcome!</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.12129">arXiv:2406.12129</a> <span> [<a href="https://arxiv.org/pdf/2406.12129">pdf</a>, <a href="https://arxiv.org/format/2406.12129">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="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> The Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER). VI. The High-Mass Stellar Initial Mass Function of M33 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wainer%2C+T+M">Tobin M. Wainer</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+F">Benjamin F. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+L+C">L. Clifton Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Weisz%2C+D+R">Daniel R. Weisz</a>, <a href="/search/astro-ph?searchtype=author&query=Dalcanton%2C+J+J">Julianne J. Dalcanton</a>, <a href="/search/astro-ph?searchtype=author&query=Seth%2C+A+C">Anil C. Seth</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A">Andrew Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Durbin%2C+M+J">Meredith J. Durbin</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Z">Zhuo Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Guhathakurta%2C+P">Puragra Guhathakurta</a>, <a href="/search/astro-ph?searchtype=author&query=Koch%2C+E+W">Eric W. Koch</a>, <a href="/search/astro-ph?searchtype=author&query=Lindberg%2C+C+W">Christina W. Lindberg</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Sandstrom%2C+K+M">Karin M. Sandstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Skillman%2C+E+D">Evan D. Skillman</a>, <a href="/search/astro-ph?searchtype=author&query=Smercina%2C+A">Adam Smercina</a>, <a href="/search/astro-ph?searchtype=author&query=TorresVillanueva%2C+E+E">Estephani E. TorresVillanueva</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="2406.12129v1-abstract-short" style="display: inline;"> We measure the high-mass stellar initial mass function (IMF) from resolved stars in M33 young stellar clusters. Leveraging \textit{Hubble Space Telescope's} high resolving power, we fully model the IMF probabilistically. We first model the optical CMD of each cluster to constrain its power-law slope $螕$, marginalized over other cluster parameters in the fit (e.g., cluster age, mass, and radius). W… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.12129v1-abstract-full').style.display = 'inline'; document.getElementById('2406.12129v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.12129v1-abstract-full" style="display: none;"> We measure the high-mass stellar initial mass function (IMF) from resolved stars in M33 young stellar clusters. Leveraging \textit{Hubble Space Telescope's} high resolving power, we fully model the IMF probabilistically. We first model the optical CMD of each cluster to constrain its power-law slope $螕$, marginalized over other cluster parameters in the fit (e.g., cluster age, mass, and radius). We then probabilistically model the distribution of MF slopes for a highly strict cluster sample of 9 clusters more massive than log(Mass/M$_{\odot}$)=3.6; above this mass, all clusters have well-populated main sequences of massive stars and should have accurate recovery of their MF slopes, based on extensive tests with artificial clusters. We find the ensemble IMF is best described by a mean high-mass slope of $\overline螕 = 1.49\pm0.18$, with an intrinsic scatter of $蟽^{2}_螕 = 0.02^{+0.16}_{0.00}$, consistent with a universal IMF. We find no dependence of the IMF on environmental impacts such as the local star formation rate or galactocentric radius within M33, which serves as a proxy for metallicity. This $\overline螕$ measurement is consistent with similar measurements in M31, despite M33 having a much higher star formation rate intensity. While this measurement is formally consistent with the canonical Kroupa ($螕= 1.30$) IMF, as well as the Salpeter ($螕= 1.35)$) value, it is the second Local Group cluster sample to show evidence for a somewhat steeper high-mass IMF slope. We explore the impacts a steeper IMF slope has on a number of astronomical sub-fields. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.12129v1-abstract-full').style.display = 'none'; document.getElementById('2406.12129v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ. 9 Figures, 1 Table</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.03532">arXiv:2406.03532</a> <span> [<a href="https://arxiv.org/pdf/2406.03532">pdf</a>, <a href="https://arxiv.org/format/2406.03532">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> An Empirical Calibration of the Tip of the Red Giant Branch Distance Method in the Near Infrared. II. JWST NIRCam Wide Filters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Newman%2C+M+J+B">Max J. B. Newman</a>, <a href="/search/astro-ph?searchtype=author&query=McQuinn%2C+K+B+W">Kristen B. W. McQuinn</a>, <a href="/search/astro-ph?searchtype=author&query=Skillman%2C+E+D">Evan D. Skillman</a>, <a href="/search/astro-ph?searchtype=author&query=Boyer%2C+M+L">Martha L. Boyer</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">Roger E. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">Andrew E. Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Telford%2C+O+G">O. Grace Telford</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="2406.03532v2-abstract-short" style="display: inline;"> The tip of the red giant (TRGB) is a standardizable candle and is identifiable as the discontinuity at the bright extreme of the red giant branch (RGB) stars in color-magnitude diagram (CMD) space. The TRGB-based distance method has been calibrated and used to measured distances to galaxies out to $D\leq20$ Mpc with the $I$-band equivalent Hubble Space Telescope ($HST$) $F814W$ filter, and as an i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.03532v2-abstract-full').style.display = 'inline'; document.getElementById('2406.03532v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.03532v2-abstract-full" style="display: none;"> The tip of the red giant (TRGB) is a standardizable candle and is identifiable as the discontinuity at the bright extreme of the red giant branch (RGB) stars in color-magnitude diagram (CMD) space. The TRGB-based distance method has been calibrated and used to measured distances to galaxies out to $D\leq20$ Mpc with the $I$-band equivalent Hubble Space Telescope ($HST$) $F814W$ filter, and as an important rung in the distance ladder to measure the Hubble constant, $H_0$. In the infrared (IR), the TRGB apparent magnitude ranges from $1-2$ magnitudes brighter than in the optical, and now with the IR James Webb Space Telescope ($JWST$) observatory the feasible distance range of the TRGB method can be extended to $\sim50$ Mpc. However, in the IR the TRGB luminosity depends to varying degrees on stellar metallicity and age. In this study we standardize the TRGB luminosity using stellar colors as a proxy for metallicity/age to derive color-based corrections for the $JWST$ Near-Infrared Camera (NIRCam) short wavelength (SW) filters $F090W$, $F115W$, $F150W$ and the long wavelength (LW) filters $F277W$, $F356W,$ and $F444W$. We provide recommended filter combinations for distance measurements depending on the requisite precision. For science requiring high precision ($\leq1\%$ in distance) and robustness we recommend measuring the TRGB in $F090W$ vs $F090W-F150W$ or $F115W$ vs. $F115W-F277W$ with the caveat that even with $JWST$ long integration times will be necessary at further distances. If lower precision ($>1.5\%$ in distance) can be tolerated, or if shorter integration times are desirable, we recommend measuring the TRGB in either $F115W$ or $F150W$ paired with $F356W$. We do not recommend $F444W$ for precision TRGB measurements due to its lower angular resolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.03532v2-abstract-full').style.display = 'none'; document.getElementById('2406.03532v2-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 11 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.17547">arXiv:2405.17547</a> <span> [<a href="https://arxiv.org/pdf/2405.17547">pdf</a>, <a href="https://arxiv.org/format/2405.17547">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> The JWST Resolved Stellar Populations Early Release Science Program VII. Stress Testing the NIRCam Exposure Time Calculator </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Savino%2C+A">A. Savino</a>, <a href="/search/astro-ph?searchtype=author&query=Gennaro%2C+M">M. Gennaro</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">A. E. Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Weisz%2C+D+R">D. R. Weisz</a>, <a href="/search/astro-ph?searchtype=author&query=Correnti%2C+M">M. Correnti</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R">R. Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Boyer%2C+M+L">M. L. Boyer</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">R. E. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+A+A">A. A. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Durbin%2C+M+J">M. J. Durbin</a>, <a href="/search/astro-ph?searchtype=author&query=Garling%2C+C+T">C. T. Garling</a>, <a href="/search/astro-ph?searchtype=author&query=Geha%2C+M+C">M. C. Geha</a>, <a href="/search/astro-ph?searchtype=author&query=Gilbert%2C+K+M">K. M. Gilbert</a>, <a href="/search/astro-ph?searchtype=author&query=Kalirai%2C+J">J. Kalirai</a>, <a href="/search/astro-ph?searchtype=author&query=Kallivayalil%2C+N">N. Kallivayalil</a>, <a href="/search/astro-ph?searchtype=author&query=McQuinn%2C+K+B+W">K. B. W. McQuinn</a>, <a href="/search/astro-ph?searchtype=author&query=Newman%2C+M+J+B">M. J. B. Newman</a>, <a href="/search/astro-ph?searchtype=author&query=Richstein%2C+H">H. Richstein</a>, <a href="/search/astro-ph?searchtype=author&query=Skillman%2C+E+D">E. D. Skillman</a>, <a href="/search/astro-ph?searchtype=author&query=Warfield%2C+J+T">J. T. Warfield</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+F">B. F. Williams</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.17547v1-abstract-short" style="display: inline;"> We empirically assess estimates from v3.0 of the JWST NIRCam Exposure Time Calculator (ETC) using observations of resolved stars in Local Group targets taken as part of the Resolved Stellar Populations Early Release Science (ERS) Program. For bright stars, we find that: (i) purely Poissonian estimates of the signal-to-noise ratio (SNR) are in good agreement between the ETC and observations, but no… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.17547v1-abstract-full').style.display = 'inline'; document.getElementById('2405.17547v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.17547v1-abstract-full" style="display: none;"> We empirically assess estimates from v3.0 of the JWST NIRCam Exposure Time Calculator (ETC) using observations of resolved stars in Local Group targets taken as part of the Resolved Stellar Populations Early Release Science (ERS) Program. For bright stars, we find that: (i) purely Poissonian estimates of the signal-to-noise ratio (SNR) are in good agreement between the ETC and observations, but non-ideal effects (e.g., flat field uncertainties) are the current limiting factor in the photometric precision that can be achieved; (ii) source position offsets, relative to the detector pixels, have a large impact on the ETC saturation predictions and introducing sub-pixel dithers in the observation design can improve the saturation limits by up to ~1 mag. For faint stars, for which the sky dominates the error budget, we find that the choice in ETC extraction strategy (e.g., aperture size relative to point spread function size) can affect the exposure time estimates by up to a factor of 5. We provide guidelines for configuring the ETC aperture photometry to produce SNR predictions in line with the ERS data. Finally, we quantify the effects of crowding on the SNRs over a large dynamic range in stellar density and provide guidelines for approximating the effects of crowding on SNRs predicted by the ETC. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.17547v1-abstract-full').style.display = 'none'; document.getElementById('2405.17547v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ. 18 pages, 9 Figures, 2 Tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.03086">arXiv:2403.03086</a> <span> [<a href="https://arxiv.org/pdf/2403.03086">pdf</a>, <a href="https://arxiv.org/format/2403.03086">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="Solar and Stellar Astrophysics">astro-ph.SR</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/ad306d">10.3847/1538-4357/ad306d <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An Empirical Calibration of the Tip of the Red Giant Branch Distance Method in the Near Infrared. I. HST WFC3/IR F110W and F160W Filters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Newman%2C+M+J+B">Max J. B. Newman</a>, <a href="/search/astro-ph?searchtype=author&query=McQuinn%2C+K+B+W">Kristen B. W. McQuinn</a>, <a href="/search/astro-ph?searchtype=author&query=Skillman%2C+E+D">Evan D. Skillman</a>, <a href="/search/astro-ph?searchtype=author&query=Boyer%2C+M+L">Martha L. Boyer</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">Roger E. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">Andrew E. Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Telford%2C+O+G">O. Grace Telford</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.03086v2-abstract-short" style="display: inline;"> The Tip of the Red Giant Branch (TRGB)-based distance method in the I band is one of the most efficient and precise techniques for measuring distances to nearby galaxies (D <= 15 Mpc). The TRGB in the near infrared (NIR) is 1 to 2 magnitudes brighter relative to the I band, and has the potential to expand the range over which distance measurements to nearby galaxies are feasible. Using Hubble Spac… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.03086v2-abstract-full').style.display = 'inline'; document.getElementById('2403.03086v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.03086v2-abstract-full" style="display: none;"> The Tip of the Red Giant Branch (TRGB)-based distance method in the I band is one of the most efficient and precise techniques for measuring distances to nearby galaxies (D <= 15 Mpc). The TRGB in the near infrared (NIR) is 1 to 2 magnitudes brighter relative to the I band, and has the potential to expand the range over which distance measurements to nearby galaxies are feasible. Using Hubble Space Telescope (HST) imaging of 12 fields in 8 nearby galaxies, we determine color-based corrections and zero points of the TRGB in the Wide Field Camera 3 IR (WFC3/IR) F110W and F160W filters. First, we measure TRGB distances in the I band equivalent Advanced Camera System (ACS) F814W filter from resolved stellar populations with the HST. The TRGB in the ACS F814W filter is used for our distance anchor and to place the WFC3/IR magnitudes on an absolute scale. We then determine the color dependence (a proxy for metallicity/age) and zero point of the NIR TRGB from photometry of WFC3/IR fields which overlap with the ACS fields. The new calibration is accurate to ~1% in distance, relative to the F814W TRGB. Validating the accuracy of the calibrations, we find that the distance modulus for each field using the NIR TRGB calibration agrees with the distance modulus of the same fields as determined from the F814W TRGB. This is a JWST preparatory program and the work done here will directly inform our approach to calibrating the TRGB in JWST NIRCam and NIRISS photometric filters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.03086v2-abstract-full').style.display = 'none'; document.getElementById('2403.03086v2-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 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">23 pages, 8 figures, accepted by the Astrophysical Journal (ApJ)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ, Volume 966, Number 2, Year 2024 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.03504">arXiv:2402.03504</a> <span> [<a href="https://arxiv.org/pdf/2402.03504">pdf</a>, <a href="https://arxiv.org/format/2402.03504">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The JWST Resolved Stellar Populations Early Release Science Program V. DOLPHOT Stellar Photometry for NIRCam and NIRISS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Weisz%2C+D+R">Daniel R. Weisz</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">Andrew E. Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Savino%2C+A">Alessandro Savino</a>, <a href="/search/astro-ph?searchtype=author&query=McQuinn%2C+K+B+W">Kristen B. W. McQuinn</a>, <a href="/search/astro-ph?searchtype=author&query=Newman%2C+M+J+B">Max J. B. Newman</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+F">Benjamin F. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Kallivayalil%2C+N">Nitya Kallivayalil</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">Jay Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Boyer%2C+M+L">Martha L. Boyer</a>, <a href="/search/astro-ph?searchtype=author&query=Correnti%2C+M">Matteo Correnti</a>, <a href="/search/astro-ph?searchtype=author&query=Geha%2C+M+C">Marla C. Geha</a>, <a href="/search/astro-ph?searchtype=author&query=Sandstrom%2C+K+M">Karin M. Sandstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+A+A">Andrew A. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Warfield%2C+J+T">Jack T. Warfield</a>, <a href="/search/astro-ph?searchtype=author&query=Skillman%2C+E+D">Evan D. Skillman</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">Roger E. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R">Rachael Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Bressan%2C+A">Alessandro Bressan</a>, <a href="/search/astro-ph?searchtype=author&query=Bolatto%2C+A">Alberto Bolatto</a>, <a href="/search/astro-ph?searchtype=author&query=Boylan-Kolchin%2C+M">Michael Boylan-Kolchin</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+A+M">Alyson M. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Bullock%2C+J+S">James S. Bullock</a>, <a href="/search/astro-ph?searchtype=author&query=Conroy%2C+C">Charlie Conroy</a>, <a href="/search/astro-ph?searchtype=author&query=Cooper%2C+M+C">Michael C. Cooper</a>, <a href="/search/astro-ph?searchtype=author&query=Dalcanton%2C+J+J">Julianne J. Dalcanton</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="2402.03504v1-abstract-short" style="display: inline;"> We present NIRCam and NIRISS modules for DOLPHOT, a widely-used crowded field stellar photometry package. We describe details of the modules including pixel masking, astrometric alignment, star finding, photometry, catalog creation, and artificial star tests (ASTs). We tested these modules using NIRCam and NIRISS images of M92 (a Milky Way globular cluster), Draco II (an ultra-faint dwarf galaxy),… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.03504v1-abstract-full').style.display = 'inline'; document.getElementById('2402.03504v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.03504v1-abstract-full" style="display: none;"> We present NIRCam and NIRISS modules for DOLPHOT, a widely-used crowded field stellar photometry package. We describe details of the modules including pixel masking, astrometric alignment, star finding, photometry, catalog creation, and artificial star tests (ASTs). We tested these modules using NIRCam and NIRISS images of M92 (a Milky Way globular cluster), Draco II (an ultra-faint dwarf galaxy), and WLM (a star-forming dwarf galaxy). DOLPHOT's photometry is highly precise and the color-magnitude diagrams are deeper and have better definition than anticipated during original program design in 2017. The primary systematic uncertainties in DOLPHOT's photometry arise from mismatches in the model and observed point spread functions (PSFs) and aperture corrections, each contributing $\lesssim0.01$ mag to the photometric error budget. Version 1.2 of WebbPSF models, which include charge diffusion and interpixel capacitance effects, significantly reduced PSF-related uncertainties. We also observed minor ($\lesssim0.05$ mag) chip-to-chip variations in NIRCam's zero points, which will be addressed by the JWST flux calibration program. Globular cluster observations are crucial for photometric calibration. Temporal variations in the photometry are generally $\lesssim0.01$ mag, although rare large misalignment events can introduce errors up to 0.08 mag. We provide recommended DOLPHOT parameters, guidelines for photometric reduction, and advice for improved observing strategies. Our ERS DOLPHOT data products are available on MAST, complemented by comprehensive online documentation and tutorials for using DOLPHOT with JWST imaging data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.03504v1-abstract-full').style.display = 'none'; document.getElementById('2402.03504v1-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">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">30 pages, 17 figures. Accepted to ApJS. Data products to be hosted on MAST. For DOLPHOT/JWST tutorials, see https://dolphot-jwst.readthedocs.io/en/latest/ . For more program and DOLPHOT info, see https://ers-stars.github.io</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.14889">arXiv:2401.14889</a> <span> [<a href="https://arxiv.org/pdf/2401.14889">pdf</a>, <a href="https://arxiv.org/format/2401.14889">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="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> The JWST Resolved Stellar Populations Early Release Science Program VI. Identifying Evolved Stars in Nearby Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Boyer%2C+M+L">Martha L. Boyer</a>, <a href="/search/astro-ph?searchtype=author&query=Pastorelli%2C+G">Giada Pastorelli</a>, <a href="/search/astro-ph?searchtype=author&query=Girardi%2C+L">L茅o Girardi</a>, <a href="/search/astro-ph?searchtype=author&query=Marigo%2C+P">Paola Marigo</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">Andrew E. Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=McQuinn%2C+K+B+W">Kristen B. W. McQuinn</a>, <a href="/search/astro-ph?searchtype=author&query=Newman%2C+M+J+B">Max J. B. Newman</a>, <a href="/search/astro-ph?searchtype=author&query=Savino%2C+A">Alessandro Savino</a>, <a href="/search/astro-ph?searchtype=author&query=Weisz%2C+D+R">Daniel R. Weisz</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+F">Benjamin F. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">Jay Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">Roger E. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Correnti%2C+M">Matteo Correnti</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+A+A">Andrew A. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Geha%2C+M+C">Marla C. Geha</a>, <a href="/search/astro-ph?searchtype=author&query=Gennaro%2C+M">Mario Gennaro</a>, <a href="/search/astro-ph?searchtype=author&query=Kallivayalil%2C+N">Nitya Kallivayalil</a>, <a href="/search/astro-ph?searchtype=author&query=Kirby%2C+E+N">Evan N. Kirby</a>, <a href="/search/astro-ph?searchtype=author&query=Sandstrom%2C+K+M">Karin M. Sandstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Skillman%2C+E+D">Evan D. Skillman</a>, <a href="/search/astro-ph?searchtype=author&query=Garling%2C+C+T">Christopher T. Garling</a>, <a href="/search/astro-ph?searchtype=author&query=Richstein%2C+H">Hannah Richstein</a>, <a href="/search/astro-ph?searchtype=author&query=Warfield%2C+J+T">Jack T. Warfield</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="2401.14889v1-abstract-short" style="display: inline;"> We present an investigation of evolved stars in the nearby star-forming galaxy WLM, using NIRCam imaging from the JWST resolved stellar populations early-release science (ERS) program. We find that various combinations of the F090W, F150W, F250M, and F430M filters can effectively isolate red supergiants (RSGs) and thermally-pulsing asymptotic giant branch (TP-AGB) stars from one another, while als… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.14889v1-abstract-full').style.display = 'inline'; document.getElementById('2401.14889v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.14889v1-abstract-full" style="display: none;"> We present an investigation of evolved stars in the nearby star-forming galaxy WLM, using NIRCam imaging from the JWST resolved stellar populations early-release science (ERS) program. We find that various combinations of the F090W, F150W, F250M, and F430M filters can effectively isolate red supergiants (RSGs) and thermally-pulsing asymptotic giant branch (TP-AGB) stars from one another, while also providing a reasonable separation of the primary TP-AGB subtypes: carbon-rich C-type stars and oxygen-rich M-type stars. The classification scheme we present here agrees very well with the well-established Hubble Space Telescope (HST) medium-band filter technique. The ratio of C to M-type stars (C/M) is 0.8$\pm$0.1 for both the new JWST and the HST classifications, which is within one sigma of empirical predictions from optical narrow-band CN and TiO filters. The evolved star colors show good agreement with the predictions from the PARSEC$+$COLIBRI stellar evolutionary models, and the models indicate a strong metallicity dependence that makes stellar identification even more effective at higher metallicity. However, the models also indicate that evolved star identification with NIRCam may be more difficult at lower metallicies. We test every combination of NIRCam filters using the models and present additional filters that are also useful for evolved star studies. We also find that $\approx$90\% of the dusty evolved stars are carbon-rich, suggesting that carbonaceous dust dominates the present-day dust production in WLM, similar to the findings in the Magellanic Clouds. These results demonstrate the usefulness of NIRCam in identifying and classifying dust-producing stars without the need for mid-infrared data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.14889v1-abstract-full').style.display = 'none'; document.getElementById('2401.14889v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">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">15 page, 12 figures, submitted to AAS Journals</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.04776">arXiv:2401.04776</a> <span> [<a href="https://arxiv.org/pdf/2401.04776">pdf</a>, <a href="https://arxiv.org/format/2401.04776">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"> Tip of the Red Giant Branch Distances with JWST: An Absolute Calibration in NGC 4258 and First Applications to Type Ia Supernova Hosts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Anand%2C+G+S">Gagandeep S. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Riess%2C+A+G">Adam G. Riess</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+W">Wenlong Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R">Rachael Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Casertano%2C+S">Stefano Casertano</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+S">Siyang Li</a>, <a href="/search/astro-ph?searchtype=author&query=Makarov%2C+D+I">Dmitry I. Makarov</a>, <a href="/search/astro-ph?searchtype=author&query=Makarova%2C+L+N">Lidia N. Makarova</a>, <a href="/search/astro-ph?searchtype=author&query=Tully%2C+R+B">R. Brent Tully</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+R+I">Richard I. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Breuval%2C+L">Louise Breuval</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A">Andrew Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Karachentsev%2C+I+D">Igor D. Karachentsev</a>, <a href="/search/astro-ph?searchtype=author&query=Macri%2C+L+M">Lucas M. Macri</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Daniel Scolnic</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="2401.04776v2-abstract-short" style="display: inline;"> The tip of the red giant branch (TRGB) allows for the measurement of precise and accurate distances to nearby galaxies, based on the brightest ascent of low-mass red giant branch stars before they undergo the helium flash. With the advent of JWST, there is great promise to utilize the technique to measure galaxy distances out to at least 50 Mpc, significantly further than HST's reach of 20 Mpc. Ho… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.04776v2-abstract-full').style.display = 'inline'; document.getElementById('2401.04776v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.04776v2-abstract-full" style="display: none;"> The tip of the red giant branch (TRGB) allows for the measurement of precise and accurate distances to nearby galaxies, based on the brightest ascent of low-mass red giant branch stars before they undergo the helium flash. With the advent of JWST, there is great promise to utilize the technique to measure galaxy distances out to at least 50 Mpc, significantly further than HST's reach of 20 Mpc. However, with any standard candle, it is first necessary to provide an absolute reference. Here we use Cycle 1 data to provide an absolute calibration in the F090W filter. F090W is most similar to the F814W filter commonly used for TRGB measurements with HST, which had been adopted by the community due to minimal dependence from the underlying metallicities and ages of stars. The imaging we use was taken in the outskirts of NGC 4258, which has a direct geometrical distance measurement from the Keplerian motion of its water megamaser. Utilizing several measurement techniques, we find $M_{TRGB}^{F090W}$ = -4.362 $\pm$ 0.033 (stat) $\pm$ 0.045 (sys) mag (Vega) for the metal-poor TRGB. We also perform measurements of the TRGB in two Type Ia supernova hosts, NGC 1559, and NGC 5584. We find good agreement between our TRGB distances and previous distance determinations to these galaxies from Cepheids ($螖$ = 0.01 $\pm$ 0.06 mag), with these differences being too small to explain the Hubble tension ($\sim$0.17 mag). As a final bonus, we showcase the serendipitous discovery of a faint dwarf galaxy near NGC 5584. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.04776v2-abstract-full').style.display = 'none'; document.getElementById('2401.04776v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 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">20 pages, 12 figures, accepted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.04773">arXiv:2401.04773</a> <span> [<a href="https://arxiv.org/pdf/2401.04773">pdf</a>, <a href="https://arxiv.org/format/2401.04773">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> JWST Observations Reject Unrecognized Crowding of Cepheid Photometry as an Explanation for the Hubble Tension at 8 sigma Confidence </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Riess%2C+A+G">Adam G. Riess</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+G+S">Gagandeep S. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+W">Wenlong Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Macri%2C+L+M">Lucas M. Macri</a>, <a href="/search/astro-ph?searchtype=author&query=Casertano%2C+S">Stefano Casertano</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A">Andrew Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Breuval%2C+L">Louise Breuval</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Dan Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Perrin%2C+M">Marshall Perrin</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+R+I">Richard I. Anderson</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="2401.04773v1-abstract-short" style="display: inline;"> We present high-definition observations with the James Webb Space Telescope of >1000 Cepheids in a geometric anchor of the distance ladder, NGC4258, and in 5 hosts of 8 SNe~Ia, a far greater sample than previous studies with JWST. These galaxies individually contain the largest samples of Cepheids, an average of >150 each, producing the strongest statistical comparison to those previously measured… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.04773v1-abstract-full').style.display = 'inline'; document.getElementById('2401.04773v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.04773v1-abstract-full" style="display: none;"> We present high-definition observations with the James Webb Space Telescope of >1000 Cepheids in a geometric anchor of the distance ladder, NGC4258, and in 5 hosts of 8 SNe~Ia, a far greater sample than previous studies with JWST. These galaxies individually contain the largest samples of Cepheids, an average of >150 each, producing the strongest statistical comparison to those previously measured with the Hubble Space Telescope in the NIR. They also span the distance range of those used to determine the Hubble constant with HST, allowing us to search for a distance-dependent bias in HST measurements. The superior resolution of JWST negates crowding noise, the largest source of variance in the NIR Cepheid Period-Luminosity relations (Leavitt laws) measured with HST. Together with the use of two-epochs to constrain Cepheid phases and three filters to remove reddening, we reduce the dispersion in the Cepheid PL relations by a factor of 2.5. We find no significant difference in the mean distance measurements determined from HST and JWST, with a formal difference of -0.01+/-0.03 mag. This result is independent of zeropoints and analysis variants including metallicity dependence, local crowding, choice of filters, and relation slope. We can reject the hypothesis of unrecognized crowding of Cepheid photometry from HST that grows with distance as the cause of the ``Hubble Tension'' at 8.2 sigma, i.e., greater confidence than that of the Hubble Tension itself. We conclude that errors in photometric measurements of Cepheids across the distance ladder do not significantly contribute to the Tension. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.04773v1-abstract-full').style.display = 'none'; document.getElementById('2401.04773v1-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">ApJ Letters, accepted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.09188">arXiv:2312.09188</a> <span> [<a href="https://arxiv.org/pdf/2312.09188">pdf</a>, <a href="https://arxiv.org/format/2312.09188">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> JWST Reveals Star Formation Across a Spiral Arm in M33 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Peltonen%2C+J">Joshua Peltonen</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Koch%2C+E+W">Eric W. Koch</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A">Andrew Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Chastenet%2C+J">Jeremy Chastenet</a>, <a href="/search/astro-ph?searchtype=author&query=Dalcanton%2C+J+J">Julianne J. Dalcanton</a>, <a href="/search/astro-ph?searchtype=author&query=Ginsburg%2C+A">Adam Ginsburg</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+L+C">L. Clifton Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A+K">Adam K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Richardson%2C+T">Theo Richardson</a>, <a href="/search/astro-ph?searchtype=author&query=Sandstrom%2C+K+M">Karin M. Sandstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Sarbadhicary%2C+S+K">Sumit K. Sarbadhicary</a>, <a href="/search/astro-ph?searchtype=author&query=Smercina%2C+A">Adam Smercina</a>, <a href="/search/astro-ph?searchtype=author&query=Wainer%2C+T">Tobin Wainer</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+F">Benjamin F. Williams</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.09188v2-abstract-short" style="display: inline;"> Young stellar objects (YSOs) are the gold standard for tracing star formation in galaxies but have been unobservable beyond the Milky Way and Magellanic Clouds. But that all changed when the James Webb Space Telescope was launched, which we use to identify YSOs in the Local Group galaxy M33, marking the first time that individual YSOs have been identified at these large distances. We present MIRI… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.09188v2-abstract-full').style.display = 'inline'; document.getElementById('2312.09188v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.09188v2-abstract-full" style="display: none;"> Young stellar objects (YSOs) are the gold standard for tracing star formation in galaxies but have been unobservable beyond the Milky Way and Magellanic Clouds. But that all changed when the James Webb Space Telescope was launched, which we use to identify YSOs in the Local Group galaxy M33, marking the first time that individual YSOs have been identified at these large distances. We present MIRI imaging mosaics at 5.6 and 21 microns that cover a significant portion of one of M33's spiral arms that has existing panchromatic imaging from the Hubble Space Telescope and deep ALMA CO measurements. Using these MIRI and Hubble Space Telescope images, we identify point sources using the new DOLPHOT MIRI module. We identify 793 candidate YSOs from cuts based on colour, proximity to giant molecular clouds (GMCs), and visual inspection. Similar to Milky Way GMCs, we find that higher mass GMCs contain more YSOs and YSO emission, which further shows YSOs identify star formation better than most tracers that cannot capture this relationship at cloud scales. We find evidence of enhanced star formation efficiency in the southern spiral arm by comparing the YSOs to the molecular gas mass. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.09188v2-abstract-full').style.display = 'none'; document.getElementById('2312.09188v2-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 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 10 figures, 1 tables, accepted for publication at 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/2312.05981">arXiv:2312.05981</a> <span> [<a href="https://arxiv.org/pdf/2312.05981">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Stellar Metallicities and Gradients in the Isolated, Quenched Low-Mass Galaxy Tucana </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fu%2C+S+W">Sal Wanying Fu</a>, <a href="/search/astro-ph?searchtype=author&query=Weisz%2C+D+R">Daniel R. Weisz</a>, <a href="/search/astro-ph?searchtype=author&query=Starkenburg%2C+E">Else Starkenburg</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+N">Nicolas Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Mercado%2C+F+J">Francisco J. Mercado</a>, <a href="/search/astro-ph?searchtype=author&query=Savino%2C+A">Alessandro Savino</a>, <a href="/search/astro-ph?searchtype=author&query=Boylan-Kolchin%2C+M">Michael Boylan-Kolchin</a>, <a href="/search/astro-ph?searchtype=author&query=C%C3%B4t%C3%A9%2C+P">Patrick C么t茅</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">Andrew E. Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Longeard%2C+N">Nicolas Longeard</a>, <a href="/search/astro-ph?searchtype=author&query=Mateo%2C+M+L">Mario L. Mateo</a>, <a href="/search/astro-ph?searchtype=author&query=Samuel%2C+J">Jenna Samuel</a>, <a href="/search/astro-ph?searchtype=author&query=Sandford%2C+N+R">Nathan R. Sandford</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="2312.05981v2-abstract-short" style="display: inline;"> We measure the metallicities of 374 red giant branch (RGB) stars in the isolated, quenched dwarf galaxy Tucana using Hubble Space Telescope (HST) narrow-band (F395N) Calcium H & K (CaHK) imaging. Our sample is a factor of $\sim7$ larger than what is published. Our main findings are: (i) A global metallicity distribution function (MDF) with $\langle \mbox{[Fe/H]} \rangle = -1.55 \pm 0.04$ and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.05981v2-abstract-full').style.display = 'inline'; document.getElementById('2312.05981v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.05981v2-abstract-full" style="display: none;"> We measure the metallicities of 374 red giant branch (RGB) stars in the isolated, quenched dwarf galaxy Tucana using Hubble Space Telescope (HST) narrow-band (F395N) Calcium H & K (CaHK) imaging. Our sample is a factor of $\sim7$ larger than what is published. Our main findings are: (i) A global metallicity distribution function (MDF) with $\langle \mbox{[Fe/H]} \rangle = -1.55 \pm 0.04$ and $蟽_{\mbox{[Fe/H]}}=0.54\pm0.03$; (ii) A metallicity gradient of $-0.54 \pm 0.07$ dex $R_e^{-1}$ ($-2.1 \pm 0.3$ dex kpc$^{-1}$) over the extent of our imaging ($\sim 2.5 R_e$), which is steeper than literature measurements. Our finding is consistent with predicted gradients from the publicly-available FIRE-2 simulations, in which bursty star formation creates stellar population gradients and dark matter cores; (iii) Tucana's bifurcated RGB has distinct metallicities: a blue RGB with $\langle \mbox{[Fe/H]} \rangle = -1.78 \pm 0.06$ and $蟽_{\mbox{[Fe/H]}}=0.44^{+0.07}_{-0.06}$, and a red RGB with $\langle \mbox{[Fe/H]} \rangle = -1.08 \pm 0.07$ and $蟽_{\mbox{[Fe/H]}}=0.42 \pm 0.06$; (iv) At fixed stellar mass, Tucana is more MR than MW satellites by $\sim 0.4$ dex, but its blue RGB is chemically comparable to the satellites. Tucana's MDF appears consistent with star-forming isolated dwarfs, though MDFs of the latter are not as well-populated; (v) $\sim2$% of Tucana's stars have $\mbox{[Fe/H]} < -3$ and 20% $\mbox{[Fe/H]} > -1$. We provide a catalog for community spectroscopic follow-up. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.05981v2-abstract-full').style.display = 'none'; document.getElementById('2312.05981v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Replaced with ApJ published version; 23 pages, 18 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.03060">arXiv:2312.03060</a> <span> [<a href="https://arxiv.org/pdf/2312.03060">pdf</a>, <a href="https://arxiv.org/format/2312.03060">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The JWST Resolved Stellar Populations Early Release Science Program IV: The Star Formation History of the Local Group Galaxy WLM </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=McQuinn%2C+K+B+W">Kristen. B. W. McQuinn</a>, <a href="/search/astro-ph?searchtype=author&query=Newman%2C+M+J+B">Max J. B. Newman</a>, <a href="/search/astro-ph?searchtype=author&query=Savino%2C+A">Alessandro Savino</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">Andrew E. Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Weisz%2C+D+R">Daniel R. Weisz</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+F">Benjamin F. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Boyer%2C+M+L">Martha L. Boyer</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">Roger E. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Correnti%2C+M">Matteo Correnti</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+A+A">Andrew A. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Geha%2C+M+C">Marla C. Geha</a>, <a href="/search/astro-ph?searchtype=author&query=Gennaro%2C+M">Mario Gennaro</a>, <a href="/search/astro-ph?searchtype=author&query=Kallivayalil%2C+N">Nitya Kallivayalil</a>, <a href="/search/astro-ph?searchtype=author&query=Sandstrom%2C+K+M">Karin M. Sandstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Skillman%2C+E+D">Evan D. Skillman</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">Jay Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolatto%2C+A">Alberto Bolatto</a>, <a href="/search/astro-ph?searchtype=author&query=Boylan-Kolchin%2C+M">Michael Boylan-Kolchin</a>, <a href="/search/astro-ph?searchtype=author&query=Garling%2C+C+T">Christopher T. Garling</a>, <a href="/search/astro-ph?searchtype=author&query=Gilbert%2C+K+M">Karoline M. Gilbert</a>, <a href="/search/astro-ph?searchtype=author&query=Girardi%2C+L">Leo Girardi</a>, <a href="/search/astro-ph?searchtype=author&query=Kalirai%2C+J+S">Jason S. Kalirai</a>, <a href="/search/astro-ph?searchtype=author&query=Mazzi%2C+A">Alessandro Mazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Pastorelli%2C+G">Giada Pastorelli</a>, <a href="/search/astro-ph?searchtype=author&query=Richstein%2C+H">Hannah Richstein</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="2312.03060v1-abstract-short" style="display: inline;"> We present the first star formation history (SFH) and age-metallicity relation (AMR) derived from resolved stellar populations imaged with the JWST NIRCam instrument. The target is the Local Group star-forming galaxy WLM at 970 kpc. The depth of the color-magnitude diagram (CMD) reaches below the oldest main sequence turn-off with a SNR=10 at M_F090W=+4.6 mag; this is the deepest CMD for any galax… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.03060v1-abstract-full').style.display = 'inline'; document.getElementById('2312.03060v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.03060v1-abstract-full" style="display: none;"> We present the first star formation history (SFH) and age-metallicity relation (AMR) derived from resolved stellar populations imaged with the JWST NIRCam instrument. The target is the Local Group star-forming galaxy WLM at 970 kpc. The depth of the color-magnitude diagram (CMD) reaches below the oldest main sequence turn-off with a SNR=10 at M_F090W=+4.6 mag; this is the deepest CMD for any galaxy that is not a satellite of the Milky Way. We use Hubble Space Telescope (HST) optical imaging that overlaps with the NIRCam observations to directly evaluate the SFHs derived based on data from the two great observatories. The JWST and HST-based SFHs are in excellent agreement. We use the metallicity distribution function measured from stellar spectra to confirm the trends in the AMRs based on the JWST data. Together, these results confirm the efficacy of recovering a SFH and AMR with the NIRCam F090W-F150W filter combination and provide validation of the sensitivity and accuracy of stellar evolution libraries in the near-infrared relative to the optical for SFH recovery work. From the JWST data, WLM shows an early onset to star formation, followed by an extended pause post-reionization before star formation re-ignites, which is qualitatively similar to what has been observed in the isolated galaxies Leo~A and Aquarius. Quantitatively, 15% of the stellar mass formed in the first Gyr, while only 10% formed over the next ~5 Gyr; the stellar mass then rapidly doubled in ~2.5 Gyr, followed by constant star formation over the last ~5 Gyr. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.03060v1-abstract-full').style.display = 'none'; document.getElementById('2312.03060v1-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 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">27 pages, 10 figures, 1 table</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.16397">arXiv:2311.16397</a> <span> [<a href="https://arxiv.org/pdf/2311.16397">pdf</a>, <a href="https://arxiv.org/format/2311.16397">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="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> The Hubble Space Telescope Survey of M31 Satellite Galaxies. III. Calibrating the Horizontal Branch as an Age Indicator for Nearby Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jennings%2C+C">Connor Jennings</a>, <a href="/search/astro-ph?searchtype=author&query=Savino%2C+A">Alessandro Savino</a>, <a href="/search/astro-ph?searchtype=author&query=Weisz%2C+D">Daniel Weisz</a>, <a href="/search/astro-ph?searchtype=author&query=Kallivayalil%2C+N">Nitya Kallivayalil</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+A">Andrew Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Collins%2C+M">Michelle Collins</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A">Andrew Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+A">Annette Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Gilbert%2C+K">Karoline Gilbert</a>, <a href="/search/astro-ph?searchtype=author&query=Guhathakurta%2C+P">Puragra Guhathakurta</a>, <a href="/search/astro-ph?searchtype=author&query=Kirby%2C+E">Evan Kirby</a>, <a href="/search/astro-ph?searchtype=author&query=Lewis%2C+G">Geraint Lewis</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+N">Nicolas Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Rich%2C+M">Michael Rich</a>, <a href="/search/astro-ph?searchtype=author&query=Skillman%2C+E">Evan Skillman</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Marel%2C+R">Roeland van der Marel</a>, <a href="/search/astro-ph?searchtype=author&query=Warfield%2C+J">Jack Warfield</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="2311.16397v1-abstract-short" style="display: inline;"> We present a new method for measuring the mean age of old/intermediate stellar populations in resolved, metal-poor ($\rm \langle[Fe/H]\rangle \lesssim -1.5$) galaxies using only the morphology of the horizontal branch (HB) and an estimate of the average metallicity. We calculate the ratio of blue-to-red HB stars and the mass-weighted mean ages of 27 M31 satellite galaxies that have star formation… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.16397v1-abstract-full').style.display = 'inline'; document.getElementById('2311.16397v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.16397v1-abstract-full" style="display: none;"> We present a new method for measuring the mean age of old/intermediate stellar populations in resolved, metal-poor ($\rm \langle[Fe/H]\rangle \lesssim -1.5$) galaxies using only the morphology of the horizontal branch (HB) and an estimate of the average metallicity. We calculate the ratio of blue-to-red HB stars and the mass-weighted mean ages of 27 M31 satellite galaxies that have star formation histories (SFHs) measured from Hubble Space Telescope-based color-magnitude diagrams (CMDs) that include the oldest Main Sequence Turn-off (MSTO) ages. We find a strong correlation between mean age, metallicity, and HB morphology, for stellar populations older than $\sim6$~Gyr. The correlation allows us to predict a galaxy's mean age from its HB morphology to a precision of $\lesssim 1$~Gyr. We validate our method by recovering the correct ages of Local Group galaxies that have robust MSTO-based ages and are not in our calibration sample. We also use our technique to measure the mean ages of isolated field galaxies KKR25 ($11.21^{+0.70}_{-0.65}$~Gyr) and VV124 ($11.03^{+0.73}_{-0.68}$~Gyr), which indicate that their main star formation episodes may have lasted several Gyr and support the picture that they achieved their early-type characteristics (e.g., low gas content, low star formation activity) in isolation and not through environment. Because the HB is $\sim80\times$ brighter than the oldest MSTO, our method can provide precise characteristic ages of predominantly old galaxies at distances $\sim 9$ times farther. We provide our calibrations in commonly used HST/ACS filters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.16397v1-abstract-full').style.display = 'none'; document.getElementById('2311.16397v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 13 figures, 5 tables, submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.01498">arXiv:2310.01498</a> <span> [<a href="https://arxiv.org/pdf/2310.01498">pdf</a>, <a href="https://arxiv.org/format/2310.01498">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Considering the Single and Binary Origins of the Type IIP SN 2017eaw </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bostroem%2C+K+A">K. Azalee Bostroem</a>, <a href="/search/astro-ph?searchtype=author&query=Zapartas%2C+E">Emmanouil Zapartas</a>, <a href="/search/astro-ph?searchtype=author&query=Koplitz%2C+B">Brad Koplitz</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+F">Benjamin F. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Tran%2C+D">Debby Tran</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A">Andrew Dolphin</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="2310.01498v1-abstract-short" style="display: inline;"> Current population synthesis modeling suggests that 30-50% of Type II supernovae originate from binary progenitors, however, the identification of a binary progenitor is challenging. One indicator of a binary progenitor is that the surrounding stellar population is too old to contain a massive single star.Measurements of the progenitor mass of SN 2017eaw are starkly divided between observations ma… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.01498v1-abstract-full').style.display = 'inline'; document.getElementById('2310.01498v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.01498v1-abstract-full" style="display: none;"> Current population synthesis modeling suggests that 30-50% of Type II supernovae originate from binary progenitors, however, the identification of a binary progenitor is challenging. One indicator of a binary progenitor is that the surrounding stellar population is too old to contain a massive single star.Measurements of the progenitor mass of SN 2017eaw are starkly divided between observations made temporally close to core-collapse which show a progenitor mass of 13-15 solar masses (final helium core mass of 4.4 to 6.0 solar masses - which is a more informative property than initial mass) and those from the stellar population surrounding the SN which find M<10.8 solar masses (helium core mass <3.4 solar masses). In this paper, we reanalyze the surrounding stellar population with improved astrometry and photometry, finding a median age of 16.8 (+3.2, -1.0) Myr for all stars younger than 50 Myr (helium core mass of 4.7 solar masses) and 85.9 (+3.2, -6.5) Myr for stars younger than 150 Myr. 16.8 Myr is now consistent with the helium core mass range derived from the temporally near explosion observations for single stars. Applying the combined constraints to population synthesis models, we determine that the probability of the progenitor of SN 2017eaw being an initially single-star is 65% compared to 35% for prior binary interaction. 85.9 Myr is inconsistent with any formation scenarios. We demonstrate that combining progenitor age constraints with helium core mass estimates from red supergiant SED modeling, late-time spectra, and indirectly from light curve modeling can help to differentiate single and binary progenitor scenarios and provide a framework for the application of this technique to future observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.01498v1-abstract-full').style.display = 'none'; document.getElementById('2310.01498v1-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, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.01268">arXiv:2309.01268</a> <span> [<a href="https://arxiv.org/pdf/2309.01268">pdf</a>, <a href="https://arxiv.org/format/2309.01268">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"> Timescale of Stellar Feedback-Driven Turbulence in the ISM: A Deep Dive into UGC 4305 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hunter%2C+L+C">Laura Congreve Hunter</a>, <a href="/search/astro-ph?searchtype=author&query=van+Zee%2C+L">Liese van Zee</a>, <a href="/search/astro-ph?searchtype=author&query=McQuinn%2C+K+B+W">Kristen B. W. McQuinn</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">Roger E. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Markham%2C+M">Madison Markham</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">Andrew E Dolphin</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="2309.01268v1-abstract-short" style="display: inline;"> Understanding the interplay of stellar feedback and turbulence in the interstellar medium (ISM) is essential to modeling the evolution of galaxies. To determine the timescales over which stellar feedback drives turbulence in the ISM, we performed a spatially resolved, multi-wavelength study of the nearby star-forming dwarf galaxy UGC 4305 (aka Holmberg II). As indicators of turbulence on local sca… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.01268v1-abstract-full').style.display = 'inline'; document.getElementById('2309.01268v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.01268v1-abstract-full" style="display: none;"> Understanding the interplay of stellar feedback and turbulence in the interstellar medium (ISM) is essential to modeling the evolution of galaxies. To determine the timescales over which stellar feedback drives turbulence in the ISM, we performed a spatially resolved, multi-wavelength study of the nearby star-forming dwarf galaxy UGC 4305 (aka Holmberg II). As indicators of turbulence on local scales (400 pc), we utilized ionized gas velocity dispersion derived from IFU H$伪$ observations and atomic gas velocity dispersion and energy surface densities derived from HI synthesis observations with the Very Large Array. These indicators of turbulence were tested against star formation histories over the past 560 Myr derived from Color-Magnitude Diagrams (CMD) using Spearman's rank correlation coefficient. The strongest correlation identified at the 400 pc scale is between measures of HI turbulence and star formation 70-140 Myr ago. We repeated our analysis of UGC 4305's current turbulence and past star formation activity on multiple physical scales ($\sim$560, and 800 pc) to determine if there are indications of changes in the correlation timescale with changes to the physical scale. No notable correlations were found at larger physical scales emphasizing the importance of analyzing star formation driven turbulence as a local phenomenon. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.01268v1-abstract-full').style.display = 'none'; document.getElementById('2309.01268v1-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 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">17 pages, 9 figure, accepted to AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.11618">arXiv:2308.11618</a> <span> [<a href="https://arxiv.org/pdf/2308.11618">pdf</a>, <a href="https://arxiv.org/format/2308.11618">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER). V. The Structure of M33 in Resolved Stellar Populations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Smercina%2C+A">Adam Smercina</a>, <a href="/search/astro-ph?searchtype=author&query=Dalcanton%2C+J+J">Julianne J. Dalcanton</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+F">Benjamin F. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Durbin%2C+M+J">Meredith J. Durbin</a>, <a href="/search/astro-ph?searchtype=author&query=Lazzarini%2C+M">Margaret Lazzarini</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+Y">Yumi Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A">Andrew Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Gilbert%2C+K">Karoline Gilbert</a>, <a href="/search/astro-ph?searchtype=author&query=Guhathakurta%2C+P">Puragra Guhathakurta</a>, <a href="/search/astro-ph?searchtype=author&query=Koch%2C+E+W">Eric W. Koch</a>, <a href="/search/astro-ph?searchtype=author&query=Rix%2C+H">Hans-Walter Rix</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Seth%2C+A">Anil Seth</a>, <a href="/search/astro-ph?searchtype=author&query=Skillman%2C+E+D">Evan D. Skillman</a>, <a href="/search/astro-ph?searchtype=author&query=Weisz%2C+D+R">Daniel R. Weisz</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2308.11618v1-abstract-short" style="display: inline;"> We present a detailed analysis of the the structure of the Local Group flocculent spiral galaxy M33, as measured using the Panchromatic Hubble Andromeda Treasury Triangulum Extended Region (PHATTER) survey. Leveraging the multiwavelength coverage of PHATTER, we find that the oldest populations are dominated by a smooth exponential disk with two distinct spiral arms and a classical central bar $-$… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.11618v1-abstract-full').style.display = 'inline'; document.getElementById('2308.11618v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.11618v1-abstract-full" style="display: none;"> We present a detailed analysis of the the structure of the Local Group flocculent spiral galaxy M33, as measured using the Panchromatic Hubble Andromeda Treasury Triangulum Extended Region (PHATTER) survey. Leveraging the multiwavelength coverage of PHATTER, we find that the oldest populations are dominated by a smooth exponential disk with two distinct spiral arms and a classical central bar $-$ completely distinct from what is seen in broadband optical imaging, and the first-ever confirmation of a bar in M33. We estimate a bar extent of $\sim$1 kpc. The two spiral arms are asymmetric in orientation and strength, and likely represent the innermost impact of the recent tidal interaction responsible for M33's warp at larger scales. The flocculent multi-armed morphology for which M33 is known is only visible in the young upper main sequence population, which closely tracks the morphology of the ISM. We investigate the stability of M33's disk, finding $Q{\sim}1$ over the majority of the disk. We fit multiple components to the old stellar density distribution and find that, when considering recent stellar kinematics, M33's bulk structure favors the inclusion of an accreted halo component, modeled as a broken power-law. The best-fit halo model has an outer power-law index of $-$3 and accurately describes observational evidence of M33's stellar halo from both resolved stellar spectroscopy in the disk and its stellar populations at large radius. Integrating this profile yields a total halo stellar mass of ${\sim}5{\times}10^8\ M_{\odot}$, giving a total stellar halo mass fraction of 16%, most of which resides in the innermost 2.5 kpc. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.11618v1-abstract-full').style.display = 'none'; document.getElementById('2308.11618v1-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 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">31 pages, 17 figures, 5 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/2307.15806">arXiv:2307.15806</a> <span> [<a href="https://arxiv.org/pdf/2307.15806">pdf</a>, <a href="https://arxiv.org/format/2307.15806">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Crowded No More: The Accuracy of the Hubble Constant Tested with High Resolution Observations of Cepheids by JWST </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Riess%2C+A+G">Adam G. Riess</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+G+S">Gagandeep S. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+W">Wenlong Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Casertano%2C+S">Stefano Casertano</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A">Andrew Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Macri%2C+L+M">Lucas M. Macri</a>, <a href="/search/astro-ph?searchtype=author&query=Breuval%2C+L">Louise Breuval</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Dan Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Perrin%2C+M">Marshall Perrin</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+R+I">Richard I. Anderson</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="2307.15806v1-abstract-short" style="display: inline;"> High-resolution JWST observations can test confusion-limited HST observations for a photometric bias that could affect extragalactic Cepheids and the determination of the Hubble constant. We present JWST NIRCAM observations in two epochs and three filters of >330 Cepheids in NGC4258 (which has a 1.5% maser-based geometric distance) and in NGC5584 (host of SNIa 2007af), near the median distance of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.15806v1-abstract-full').style.display = 'inline'; document.getElementById('2307.15806v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.15806v1-abstract-full" style="display: none;"> High-resolution JWST observations can test confusion-limited HST observations for a photometric bias that could affect extragalactic Cepheids and the determination of the Hubble constant. We present JWST NIRCAM observations in two epochs and three filters of >330 Cepheids in NGC4258 (which has a 1.5% maser-based geometric distance) and in NGC5584 (host of SNIa 2007af), near the median distance of the SH0ES HST SNIa host sample and with the best leverage among them to detect such a bias. JWST provides far superior source separation from line-of-sight companions than HST in the NIR to largely negate confusion or crowding noise at these wavelengths, where extinction is minimal. The result is a remarkable >2.5x reduction in the dispersion of the Cepheid P-L relations, from 0.45 to 0.17 mag, improving individual Cepheid precision from 20% to 7%. Two-epoch photometry confirmed identifications, tested JWST photometric stability, and constrained Cepheid phases. The P-L relation intercepts are in very good agreement, with differences (JWST-HST) of 0.00+/-0.03 and 0.02+/-0.03 mag for NGC4258 and NGC5584, respectively. The difference in the determination of H_0 between HST and JWST from these intercepts is 0.02+/-0.04 mag, insensitive to JWST zeropoints or count-rate non-linearity thanks to error cancellation between rungs. We explore a broad range of analysis variants (including passband combinations, phase corrections, measured detector offsets, and crowding levels) indicating robust baseline results. These observations provide the strongest evidence yet that systematic errors in HST Cepheid photometry do not play a significant role in the present Hubble Tension. Upcoming JWST observations of >12 SNIa hosts should further refine the local measurement of the Hubble constant. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.15806v1-abstract-full').style.display = 'none'; document.getElementById('2307.15806v1-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 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">submitted to ApJ, comments welcome</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.09681">arXiv:2307.09681</a> <span> [<a href="https://arxiv.org/pdf/2307.09681">pdf</a>, <a href="https://arxiv.org/format/2307.09681">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The Panchromatic Hubble Andromeda Treasury XXI. The Legacy Resolved Stellar Photometry Catalog </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+F">Benjamin F. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Durbin%2C+M">Meredith Durbin</a>, <a href="/search/astro-ph?searchtype=author&query=Lang%2C+D">Dustin Lang</a>, <a href="/search/astro-ph?searchtype=author&query=Dalcanton%2C+J+J">Julianne J. Dalcanton</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">Andrew E. Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Smercina%2C+A">Adam Smercina</a>, <a href="/search/astro-ph?searchtype=author&query=Merica-Jones%2C+P+Y">Petia Yanchulova Merica-Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Weisz%2C+D+R">Daniel R. Weisz</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Gilbert%2C+K+M">Karoline M. Gilbert</a>, <a href="/search/astro-ph?searchtype=author&query=Girardi%2C+L">Leo Girardi</a>, <a href="/search/astro-ph?searchtype=author&query=Gordon%2C+K">Karl Gordon</a>, <a href="/search/astro-ph?searchtype=author&query=Guhathakurta%2C+P">Puragra Guhathakurta</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+L+C">L. Clifton Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Lauer%2C+T+R">Tod R. Lauer</a>, <a href="/search/astro-ph?searchtype=author&query=Seth%2C+A">Anil Seth</a>, <a href="/search/astro-ph?searchtype=author&query=Skillman%2C+E">Evan Skillman</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="2307.09681v1-abstract-short" style="display: inline;"> We present the final legacy version of stellar photometry for the Panchromatic Hubble Andromeda Treasury (PHAT) survey. We have reprocessed all of the Hubble Space Telescope (HST) Wide Field Camera 3 (WFC3) and Advanced Camera for Surveys (ACS) near ultraviolet (F275W, F336W), optical (F475W, F814W), and near infrared (F110W, F160W) imaging from the PHAT survey using an improved method that optimi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.09681v1-abstract-full').style.display = 'inline'; document.getElementById('2307.09681v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.09681v1-abstract-full" style="display: none;"> We present the final legacy version of stellar photometry for the Panchromatic Hubble Andromeda Treasury (PHAT) survey. We have reprocessed all of the Hubble Space Telescope (HST) Wide Field Camera 3 (WFC3) and Advanced Camera for Surveys (ACS) near ultraviolet (F275W, F336W), optical (F475W, F814W), and near infrared (F110W, F160W) imaging from the PHAT survey using an improved method that optimized the survey depth and chip gap coverage by including all overlapping exposures in all bands in the photometry. An additional improvement was gained through the use of charge transfer efficiency (CTE) corrected input images, which provide more complete star finding as well as more reliable photometry for the NUV bands, which had no CTE correction in the previous version of the PHAT photometry. While this method requires significantly more computing resources and time than earlier versions where the photometry was performed on individual pointings, it results in smaller systematic instrumental completeness variations as demonstrated by cleaner maps in stellar density, and it results in optimal constraints on stellar fluxes in all bands from the survey data. Our resulting catalog has 138 million stars, 18% more than the previous catalog, with lower density regions gaining as much as 40% more stars. The new catalog produces nearly seamless population maps which show relatively well-mixed distributions for populations associated with ages older than 1-2 Gyr, and highly structured distributions for the younger populations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.09681v1-abstract-full').style.display = 'none'; document.getElementById('2307.09681v1-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 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">28 pages, 4 tables, 18 figures, accepted for publication in The Astrophysical Journal Supplement Series</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.08738">arXiv:2307.08738</a> <span> [<a href="https://arxiv.org/pdf/2307.08738">pdf</a>, <a href="https://arxiv.org/format/2307.08738">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"> Discovery and Characterization of Two Ultra Faint-Dwarfs Outside the Halo of the Milky Way: Leo M and Leo K </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=McQuinn%2C+K+B+W">Kristen B. W. McQuinn</a>, <a href="/search/astro-ph?searchtype=author&query=Mao%2C+Y">Yao-Yuan Mao</a>, <a href="/search/astro-ph?searchtype=author&query=Tollerud%2C+E+J">Erik J. Tollerud</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">Roger E. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Shih%2C+D">David Shih</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+M+R">Matthew R. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">Andrew E. Dolphin</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="2307.08738v2-abstract-short" style="display: inline;"> We report the discovery of two ultra-faint dwarf galaxies, Leo M and Leo K, that lie outside the halo of the Milky Way. Using Hubble Space Telescope imaging of the resolved stars, we create color-magnitude diagrams reaching the old main sequence turn-off of each system and (i) fit for structural parameters of the galaxies; (ii) measure their distances using the luminosity of the Horizontal Branch… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.08738v2-abstract-full').style.display = 'inline'; document.getElementById('2307.08738v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.08738v2-abstract-full" style="display: none;"> We report the discovery of two ultra-faint dwarf galaxies, Leo M and Leo K, that lie outside the halo of the Milky Way. Using Hubble Space Telescope imaging of the resolved stars, we create color-magnitude diagrams reaching the old main sequence turn-off of each system and (i) fit for structural parameters of the galaxies; (ii) measure their distances using the luminosity of the Horizontal Branch stars; (iii) estimate integrated magnitudes and stellar masses; and (iv) reconstruct the star formation histories. Based on their location in the Local Group, neither galaxy is currently a satellite of the Milky Way, although Leo K is located ~26 kpc from the low-mass galaxy Leo T and these two systems may have had a past interaction. Leo M and Leo K have stellar masses of 1.8 (+0.3/-0.2) x 10^4 Msun and 1.2+/-0.2 x 10^4 Msun, and were quenched 10.6 (+2.2/-1.1) Gyr and 12.8 (+0.1/-4.2) Gyr ago, respectively. Given that the galaxies are not satellites of the MW, it is unlikely that they were quenched by environmental processing. Instead, given their low stellar masses, their early quenching timescales are consistent with the scenario that a combination of reionization and stellar feedback shut-down star formation at early cosmic times. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.08738v2-abstract-full').style.display = 'none'; document.getElementById('2307.08738v2-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 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 9 figures, 1 table</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.04853">arXiv:2307.04853</a> <span> [<a href="https://arxiv.org/pdf/2307.04853">pdf</a>, <a href="https://arxiv.org/format/2307.04853">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"> Spatially-Resolved Recent Star Formation History in NGC 6946 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tran%2C+D">Debby Tran</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B">Benjamin Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Levesque%2C+E">Emily Levesque</a>, <a href="/search/astro-ph?searchtype=author&query=Lazzarini%2C+M">Margaret Lazzarini</a>, <a href="/search/astro-ph?searchtype=author&query=Dalcanton%2C+J">Julianne Dalcanton</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A">Andrew Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Koplitz%2C+B">Brad Koplitz</a>, <a href="/search/astro-ph?searchtype=author&query=Smercina%2C+A">Adam Smercina</a>, <a href="/search/astro-ph?searchtype=author&query=Telford%2C+O+G">O. Grace Telford</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="2307.04853v1-abstract-short" style="display: inline;"> The nearby face-on star forming spiral galaxy NGC 6946 is known as the Fireworks Galaxy due to its hosting an unusually large number of supernova. We analyze its resolved near-ultraviolet (NUV) stellar photometry measured from images taken with the Hubble Space Telescope's (HST) Wide Field Camera 3 (WFC3) with F275W and F336W filters. We model the color-magnitude diagrams (CMD) of the UV photometr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.04853v1-abstract-full').style.display = 'inline'; document.getElementById('2307.04853v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.04853v1-abstract-full" style="display: none;"> The nearby face-on star forming spiral galaxy NGC 6946 is known as the Fireworks Galaxy due to its hosting an unusually large number of supernova. We analyze its resolved near-ultraviolet (NUV) stellar photometry measured from images taken with the Hubble Space Telescope's (HST) Wide Field Camera 3 (WFC3) with F275W and F336W filters. We model the color-magnitude diagrams (CMD) of the UV photometry to derive the spatially-resolved star formation history (SFH) of NGC 6946 over the last 25 Myr. From this analysis, we produce maps of the spatial distribution of young stellar populations and measure the total recent star formation rate (SFR) of nearly the entire young stellar disk. We find the global SFR(age$\leq$25 Myr)=$13.17 \substack{+0.91 \\-0.79} M_\odot/\rm yr$. Over this period, the SFR is initially very high ($23.39\substack{+2.43\\-2.11} M_\odot/\rm yr$ between 16-25 Myr ago), then monotonically decreases to a recent SFR of $5.31\substack{+0.19\\-0.17} M_\odot/\rm yr$ in the last 10 Myr. This decrease in global star formation rate over the last 25 Myr is consistent with measurements made with other SFR indicators. We discuss in detail two of the most active regions of the galaxy, which we find are responsible for 3% and 5% of the total star formation over the past 6.3 Myr. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.04853v1-abstract-full').style.display = 'none'; document.getElementById('2307.04853v1-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 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">19 pages, 11 figures, accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.06260">arXiv:2306.06260</a> <span> [<a href="https://arxiv.org/pdf/2306.06260">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ad0030">10.3847/1538-4357/ad0030 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Metallicity Distribution Functions of 13 Ultra-Faint Dwarf Galaxy Candidates from Hubble Space Telescope Narrowband Imaging </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fu%2C+S+W">Sal Wanying Fu</a>, <a href="/search/astro-ph?searchtype=author&query=Weisz%2C+D+R">Daniel R. Weisz</a>, <a href="/search/astro-ph?searchtype=author&query=Starkenburg%2C+E">Else Starkenburg</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+N">Nicolas Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Savino%2C+A">Alessandro Savino</a>, <a href="/search/astro-ph?searchtype=author&query=Boylan-Kolchin%2C+M">Michael Boylan-Kolchin</a>, <a href="/search/astro-ph?searchtype=author&query=Cote%2C+P">Patrick Cote</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">Andrew E. Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Ji%2C+A+P">Alexander P. Ji</a>, <a href="/search/astro-ph?searchtype=author&query=Longeard%2C+N">Nicolas Longeard</a>, <a href="/search/astro-ph?searchtype=author&query=Mateo%2C+M+L">Mario L. Mateo</a>, <a href="/search/astro-ph?searchtype=author&query=Patel%2C+E">Ekta Patel</a>, <a href="/search/astro-ph?searchtype=author&query=Sandford%2C+N+R">Nathan R. Sandford</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="2306.06260v2-abstract-short" style="display: inline;"> We present uniformly measured stellar metallicities for 463 stars in 13 Milky Way (MW) ultra-faint dwarf galaxies (UFDs; $M_V = -7.1$ to $-0.8$) using narrowband CaHK (F395N) imaging taken with the Hubble Space Telescope (HST). This represents the largest homogeneous set of stellar metallicities in UFDs, increasing the number of metallicities in these 13 galaxies by a factor of 5 and doubling the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.06260v2-abstract-full').style.display = 'inline'; document.getElementById('2306.06260v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.06260v2-abstract-full" style="display: none;"> We present uniformly measured stellar metallicities for 463 stars in 13 Milky Way (MW) ultra-faint dwarf galaxies (UFDs; $M_V = -7.1$ to $-0.8$) using narrowband CaHK (F395N) imaging taken with the Hubble Space Telescope (HST). This represents the largest homogeneous set of stellar metallicities in UFDs, increasing the number of metallicities in these 13 galaxies by a factor of 5 and doubling the number of metallicities in all known MW UFDs. We provide the first well-populated MDFs for all galaxies in this sample, with [Fe/H] ranging from -3.0 dex to -2.0 dex, and $蟽_{\mbox{[Fe/H]}}$ ranging from 0.3 dex to 0.7 dex. We find a nearly constant [Fe/H] ~ -2.6 over 3 decades in luminosity (~$10^2 - 10^5 L_{\odot}$), suggesting that the mass-metallicity relationship does not hold for such faint systems. We find a larger fraction (24%) of EMP ([Fe/H]<-3.0) stars across our sample compared to the literature (14%), but note that uncertainties in our most metal-poor measurements make this an upper limit. We find 19% of stars in our UFD sample to be metal-rich ([Fe/H]>-2.0), consistent with the sum of literature spectroscopic studies. MW UFDs are known to be predominantly >13 Gyr old, meaning that all stars in our sample are truly ancient, unlike metal-poor stars in the MW, which have a range of possible ages. Our UFD metallicities are not well-matched to known streams in the MW, providing further evidence that known MW substructures are not related to UFDs. We include a catalog of our stars to encourage community follow-up studies, including priority targets for ELT-era observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.06260v2-abstract-full').style.display = 'none'; document.getElementById('2306.06260v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">37 pages, 20 figures, ApJ accepted and published</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 958 167 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.13360">arXiv:2305.13360</a> <span> [<a href="https://arxiv.org/pdf/2305.13360">pdf</a>, <a href="https://arxiv.org/format/2305.13360">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The Hubble Space Telescope Survey of M31 Satellite Galaxies II. The Star Formation Histories of Ultra-Faint Dwarf Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Savino%2C+A">A. Savino</a>, <a href="/search/astro-ph?searchtype=author&query=Weisz%2C+D+R">D. R. Weisz</a>, <a href="/search/astro-ph?searchtype=author&query=Skillman%2C+E+D">E. D. Skillman</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A">A. Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+A+A">A. A. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Kallivayalil%2C+N">N. Kallivayalil</a>, <a href="/search/astro-ph?searchtype=author&query=Wetzel%2C+A">A. Wetzel</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Besla%2C+G">G. Besla</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=Brown%2C+T+M">T. M. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Bullock%2C+J+S">J. S. Bullock</a>, <a href="/search/astro-ph?searchtype=author&query=Collins%2C+M+L+M">M. L. M. Collins</a>, <a href="/search/astro-ph?searchtype=author&query=Cooper%2C+M+C">M. C. Cooper</a>, <a href="/search/astro-ph?searchtype=author&query=Deason%2C+A+J">A. J. Deason</a>, <a href="/search/astro-ph?searchtype=author&query=Dotter%2C+A+L">A. L. Dotter</a>, <a href="/search/astro-ph?searchtype=author&query=Fardal%2C+M">M. Fardal</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+A+M+N">A. M. N. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Fritz%2C+T+K">T. K. Fritz</a>, <a href="/search/astro-ph?searchtype=author&query=Geha%2C+M+C">M. C. Geha</a>, <a href="/search/astro-ph?searchtype=author&query=Gilbert%2C+K+M">K. M. Gilbert</a>, <a href="/search/astro-ph?searchtype=author&query=Guhathakurta%2C+P">P. Guhathakurta</a>, <a href="/search/astro-ph?searchtype=author&query=Ibata%2C+R">R. Ibata</a>, <a href="/search/astro-ph?searchtype=author&query=Irwin%2C+M+J">M. J. Irwin</a>, <a href="/search/astro-ph?searchtype=author&query=Jeon%2C+M">M. Jeon</a> , et al. (12 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2305.13360v2-abstract-short" style="display: inline;"> We present the lifetime star formation histories (SFHs) for six ultra-faint dwarf (UFD; $M_V>-7.0$, $ 4.9<\log_{10}({M_*(z=0)}/{M_{\odot}})<5.5$) satellite galaxies of M31 based on deep color-magnitude diagrams constructed from \textit{Hubble Space Telescope} imaging. These are the first SFHs obtained from the oldest main sequence turn-off of UFDs outside the halo of the Milky Way (MW). We find th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.13360v2-abstract-full').style.display = 'inline'; document.getElementById('2305.13360v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.13360v2-abstract-full" style="display: none;"> We present the lifetime star formation histories (SFHs) for six ultra-faint dwarf (UFD; $M_V>-7.0$, $ 4.9<\log_{10}({M_*(z=0)}/{M_{\odot}})<5.5$) satellite galaxies of M31 based on deep color-magnitude diagrams constructed from \textit{Hubble Space Telescope} imaging. These are the first SFHs obtained from the oldest main sequence turn-off of UFDs outside the halo of the Milky Way (MW). We find that five UFDs formed at least 50\% of their stellar mass by $z=5$ (12.6~Gyr ago), similar to known UFDs around the MW, but that 10-40\% of their stellar mass formed at later times. We uncover one remarkable UFD, \A{XIII}, which formed only 10\% of its stellar mass by $z=5$, and 75\% in a rapid burst at $z\sim2-3$, a result that is robust to choices of underlying stellar model and is consistent with its predominantly red horizontal branch. This "young" UFD is the first of its kind and indicates that not all UFDs are necessarily quenched by reionization, which is consistent with predictions from several cosmological simulations of faint dwarf galaxies. SFHs of the combined MW and M31 samples suggest reionization did not homogeneously quench UFDs. We find that the least massive MW UFDs ($M_*(z=5) \lesssim 5\times10^4 M_{\odot}$) are likely quenched by reionization, whereas more massive M31 UFDs ($M_*(z=5) \gtrsim 10^5 M_{\odot}$) may only have their star formation suppressed by reionization and quench at a later time. We discuss these findings in the context of the evolution and quenching of UFDs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.13360v2-abstract-full').style.display = 'none'; document.getElementById('2305.13360v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 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">18 pages, 14 figures, 5 appendices, 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/2304.08613">arXiv:2304.08613</a> <span> [<a href="https://arxiv.org/pdf/2304.08613">pdf</a>, <a href="https://arxiv.org/format/2304.08613">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/10.3847/1538-3881/accc83">10.3847/1538-3881/accc83 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Panchromatic Hubble Andromeda Treasury XX: The Disk of M31 is Thick </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dalcanton%2C+J+J">Julianne J. Dalcanton</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+Y">Yumi Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">Andrew E. Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Fouesneau%2C+M">Morgan Fouesneau</a>, <a href="/search/astro-ph?searchtype=author&query=Girardi%2C+L">L茅o Girardi</a>, <a href="/search/astro-ph?searchtype=author&query=Hogg%2C+D+W">David W. Hogg</a>, <a href="/search/astro-ph?searchtype=author&query=Seth%2C+A+C">Anil C. Seth</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+F">Benjamin F. Williams</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.08613v1-abstract-short" style="display: inline;"> We present a new approach to measuring the thickness of a partially face-on stellar disk, using dust geometry. In a moderately-inclined disk galaxy, the fraction of reddened stars is expected to be 50% everywhere, assuming that dust lies in a thin midplane. In a thickened disk, however, a wide range of radii project onto the line of sight. Assuming stellar density declines with radius, this geomet… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.08613v1-abstract-full').style.display = 'inline'; document.getElementById('2304.08613v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.08613v1-abstract-full" style="display: none;"> We present a new approach to measuring the thickness of a partially face-on stellar disk, using dust geometry. In a moderately-inclined disk galaxy, the fraction of reddened stars is expected to be 50% everywhere, assuming that dust lies in a thin midplane. In a thickened disk, however, a wide range of radii project onto the line of sight. Assuming stellar density declines with radius, this geometrical projection leads to differences in the numbers of stars on the near and far sides of the thin dust layer. The fraction of reddened stars will thus differ from the 50% prediction, with a deviation that becomes larger for puffier disks. We map the fraction of reddened red giant branch (RGB) stars across M31, which shows prominent dust lanes on only one side of the major axis. The fraction of reddened stars varies systematically from 20% to 80%, which requires that these stars have an exponential scale height h_z that is 0.14+/-0.015 times the exponential scale length (h_r~5.5kpc). M31's RGB stars must therefore have h_z=770+/-80pc, which is far thicker than the Milky Way's thin disk, but comparable to its thick disk. The lack of a significant thin disk in M31 is unexpected, but consistent with its interaction history and high disk velocity dispersion. We suggest that asymmetric reddening be used as a generic criteria for identifying ``thick disk'' dominated systems, and discuss prospects for future 3-dimensional tomographic mapping of the gas and stars in M31. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.08613v1-abstract-full').style.display = 'none'; document.getElementById('2304.08613v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages. Accepted to the Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.11348">arXiv:2303.11348</a> <span> [<a href="https://arxiv.org/pdf/2303.11348">pdf</a>, <a href="https://arxiv.org/format/2303.11348">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/acc328">10.3847/1538-4357/acc328 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> On the Reionization-Era Globular Cluster in Low-Mass Galaxy Eridanus II </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Weisz%2C+D+R">Daniel R. Weisz</a>, <a href="/search/astro-ph?searchtype=author&query=Savino%2C+A">Alessandro Savino</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">Andrew E. Dolphin</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.11348v1-abstract-short" style="display: inline;"> Using color-magnitude diagrams from deep archival Hubble Space Telescope imaging, we self-consistently measure the star formation history of Eridanus II (Eri II), the lowest-mass galaxy ($M_{\star}(z=0) \sim 10^5 M_{\odot}$) known to host a globular cluster (GC), and the age, mass, and metallicity of its GC. The GC ($\sim13.2\pm0.4$ Gyr, $\langle$[Fe/H]$\rangle = -2.75\pm0.2$ dex) and field (mean… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.11348v1-abstract-full').style.display = 'inline'; document.getElementById('2303.11348v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.11348v1-abstract-full" style="display: none;"> Using color-magnitude diagrams from deep archival Hubble Space Telescope imaging, we self-consistently measure the star formation history of Eridanus II (Eri II), the lowest-mass galaxy ($M_{\star}(z=0) \sim 10^5 M_{\odot}$) known to host a globular cluster (GC), and the age, mass, and metallicity of its GC. The GC ($\sim13.2\pm0.4$ Gyr, $\langle$[Fe/H]$\rangle = -2.75\pm0.2$ dex) and field (mean age $\sim13.5\pm0.3$ Gyr, $\langle$[Fe/H]$\rangle = -2.6\pm0.15$ dex) have similar ages and metallicities. Both are reionization-era relics that formed before the peak of cosmic star and GC formation ($z\sim2-4$). The ancient star formation properties of Eri II are not extreme and appear similar to $z=0$ dwarf galaxies. We find that the GC was $\lesssim4$ times more massive at birth than today and was $\sim$10% of the galaxy's stellar mass at birth. At formation, we estimate that the progenitor of Eri II and its GC had $M_{\rm UV} \sim -7$ to $-12$, making it one of the most common type of galaxy in the early Universe, though it is fainter than direct detection limits, absent gravitational lensing. Archaeological studies of GCs in nearby low-mass galaxies may be the only way to constrain GC formation in such low-mass systems. We discuss the strengths and limitations in comparing archaeological and high redshift studies of cluster formation, including challenges stemming from the Hubble Tension, which introduces uncertainties into the mapping between age and redshift. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.11348v1-abstract-full').style.display = 'none'; document.getElementById('2303.11348v1-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 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">11 pages, 3 Figures, 1 Table. 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/2303.07318">arXiv:2303.07318</a> <span> [<a href="https://arxiv.org/pdf/2303.07318">pdf</a>, <a href="https://arxiv.org/format/2303.07318">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</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/acc249">10.3847/1538-4357/acc249 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Masses of Supernova Remnant Progenitors in M33 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Koplitz%2C+B">Brad Koplitz</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+J">Jared Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+F">Benjamin F. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Diaz-Rodriguez%2C+M">Mariangelly Diaz-Rodriguez</a>, <a href="/search/astro-ph?searchtype=author&query=Murphy%2C+J+W">Jeremiah W. Murphy</a>, <a href="/search/astro-ph?searchtype=author&query=Lazzarini%2C+M">Margaret Lazzarini</a>, <a href="/search/astro-ph?searchtype=author&query=Guzman%2C+J">Joseph Guzman</a>, <a href="/search/astro-ph?searchtype=author&query=Dalcanton%2C+J+J">Julianne J. Dalcanton</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A">Andrew Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Durbin%2C+M">Meredith Durbin</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.07318v2-abstract-short" style="display: inline;"> Using resolved optical stellar photometry from the Panchromatic Hubble Andromeda Treasury Triangulum Extended Region (PHATTER) survey, we measured the star formation history (SFH) near the position of 85 supernova remnants (SNRs) in M33. We constrained the progenitor masses for 60 of these SNRs, finding the remaining 25 remnants had no local SF in the last 56 Myr consistent with core-collapse SNe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.07318v2-abstract-full').style.display = 'inline'; document.getElementById('2303.07318v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.07318v2-abstract-full" style="display: none;"> Using resolved optical stellar photometry from the Panchromatic Hubble Andromeda Treasury Triangulum Extended Region (PHATTER) survey, we measured the star formation history (SFH) near the position of 85 supernova remnants (SNRs) in M33. We constrained the progenitor masses for 60 of these SNRs, finding the remaining 25 remnants had no local SF in the last 56 Myr consistent with core-collapse SNe (CCSNe), making them potential Type Ia candidates. We then infer a progenitor mass distribution from the age distribution, assuming single star evolution. We find that the progenitor mass distribution is consistent with being drawn from a power-law with an index of $-2.9^{+1.2}_{-1.0}$. Additionally, we infer a minimum progenitor mass of $7.1^{+0.1}_{-0.2}\ M_{\odot}$ from this sample, consistent with several previous studies, providing further evidence that stars with ages older than the lifetimes of single 8 $M_{\odot}$ stars are producing supernovae. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.07318v2-abstract-full').style.display = 'none'; document.getElementById('2303.07318v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 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">20 pages, 7 figures, 2 tables, Accepted at 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/2303.03392">arXiv:2303.03392</a> <span> [<a href="https://arxiv.org/pdf/2303.03392">pdf</a>, <a href="https://arxiv.org/format/2303.03392">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</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/10.3847/1538-4357/acb775">10.3847/1538-4357/acb775 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Multiwavelength Classification and Study of Red Supergiant Candidates in NGC 6946 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+J+R">Jared R. Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Koplitz%2C+B">Brad Koplitz</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+F">Benjamin F. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Dalcanton%2C+J+J">Julianne J. Dalcanton</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A">Andrew Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Girardi%2C+L">Leo Girardi</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.03392v1-abstract-short" style="display: inline;"> We have combined resolved stellar photometry from Hubble Space Telescope (\emph{HST}), \emph{Spitzer}, and \emph{Gaia} to identify red supergiant (RSG) candidates in NGC~6946, based on their colors, proper motions, visual morphologies, and spectral energy distributions. We start with a large sample of 17,865 RSG candidates based solely on \emph{HST} near-infrared photometry. We then chose a small… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.03392v1-abstract-full').style.display = 'inline'; document.getElementById('2303.03392v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.03392v1-abstract-full" style="display: none;"> We have combined resolved stellar photometry from Hubble Space Telescope (\emph{HST}), \emph{Spitzer}, and \emph{Gaia} to identify red supergiant (RSG) candidates in NGC~6946, based on their colors, proper motions, visual morphologies, and spectral energy distributions. We start with a large sample of 17,865 RSG candidates based solely on \emph{HST} near-infrared photometry. We then chose a small sample of 385 of these candidates with Spitzer matches for more detailed study. Using evolutionary models and isochrones, we isolate a space where RSGs would be found in our photometry catalogs. We then visually inspect each candidate and compare to Gaia catalogs to identify and remove foreground stars. As a result, we classify 95 potential RSGs, with 40 of these being in our highest-quality sample. We fit the photometry of the populations of stars in the regions surrounding the RSGs to infer their ages. Placing our best candidate RSG stars into three age bins between 1 and 30 Myr, we find 27.5\% of the candidates falling between 1-10 Myr, 37.5\% between 10-20 Myr, and 35\% 20-30 Myr. A comparison of our results to the models of massive star evolution shows some agreement between model luminosities and the luminosities of our candidates for each age. Three of our candidates appear significantly more consistent with binary models than single-star evolution models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.03392v1-abstract-full').style.display = 'none'; document.getElementById('2303.03392v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 March, 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">32 pages, 18 figures, 4 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.07218">arXiv:2301.07218</a> <span> [<a href="https://arxiv.org/pdf/2301.07218">pdf</a>, <a href="https://arxiv.org/format/2301.07218">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The JWST Resolved Stellar Populations Early Release Science Program III: Photometric Star-Galaxy Separations for NIRCam </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Warfield%2C+J+T">Jack T. Warfield</a>, <a href="/search/astro-ph?searchtype=author&query=Richstein%2C+H">Hannah Richstein</a>, <a href="/search/astro-ph?searchtype=author&query=Kallivayalil%2C+N">Nitya Kallivayalil</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">Roger E. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Savino%2C+A">Alessandro Savino</a>, <a href="/search/astro-ph?searchtype=author&query=Boyer%2C+M+L">Martha L. Boyer</a>, <a href="/search/astro-ph?searchtype=author&query=Garling%2C+C+T">Christopher T. Garling</a>, <a href="/search/astro-ph?searchtype=author&query=Gennaro%2C+M">Mario Gennaro</a>, <a href="/search/astro-ph?searchtype=author&query=McQuinn%2C+K+B+W">Kristen B. W. McQuinn</a>, <a href="/search/astro-ph?searchtype=author&query=Newman%2C+M+J+B">Max J. B. Newman</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">Jay Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+A+A">Andrew A. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Correnti%2C+M">Matteo Correnti</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">Andrew E. Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Geha%2C+M+C">Marla C. Geha</a>, <a href="/search/astro-ph?searchtype=author&query=Sandstrom%2C+K+M">Karin M. Sandstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Weisz%2C+D+R">Daniel R. Weisz</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+F">Benjamin F. Williams</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2301.07218v1-abstract-short" style="display: inline;"> We present criteria for separately classifying stars and unresolved background galaxies in photometric catalogs generated with the point spread function (PSF) fitting photometry software DOLPHOT from images taken of Draco II, WLM, and M92 with the Near Infrared Camera (NIRCam) on JWST. Photometric quality metrics from DOLPHOT in one or two filters can recover a pure sample of stars. Conversely, co… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.07218v1-abstract-full').style.display = 'inline'; document.getElementById('2301.07218v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.07218v1-abstract-full" style="display: none;"> We present criteria for separately classifying stars and unresolved background galaxies in photometric catalogs generated with the point spread function (PSF) fitting photometry software DOLPHOT from images taken of Draco II, WLM, and M92 with the Near Infrared Camera (NIRCam) on JWST. Photometric quality metrics from DOLPHOT in one or two filters can recover a pure sample of stars. Conversely, colors formed between short-wavelength (SW) and long-wavelength (LW) filters can be used to effectively identify pure samples of galaxies. Our results highlight that the existing DOLPHOT output parameters can be used to reliably classify stars in our NIRCam data without the need to resort to external tools or more complex heuristics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.07218v1-abstract-full').style.display = 'none'; document.getElementById('2301.07218v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 January, 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">5 pages, 1 figure</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.04659">arXiv:2301.04659</a> <span> [<a href="https://arxiv.org/pdf/2301.04659">pdf</a>, <a href="https://arxiv.org/format/2301.04659">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="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> The JWST Resolved Stellar Populations Early Release Science Program II. Survey Overview </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Weisz%2C+D+R">Daniel R. Weisz</a>, <a href="/search/astro-ph?searchtype=author&query=McQuinn%2C+K+B+W">Kristen B. W. McQuinn</a>, <a href="/search/astro-ph?searchtype=author&query=Savino%2C+A">Alessandro Savino</a>, <a href="/search/astro-ph?searchtype=author&query=Kallivayalil%2C+N">Nitya Kallivayalil</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">Jay Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Boyer%2C+M+L">Martha L. Boyer</a>, <a href="/search/astro-ph?searchtype=author&query=Correnti%2C+M">Matteo Correnti</a>, <a href="/search/astro-ph?searchtype=author&query=Geha%2C+M+C">Marla C. Geha</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">Andrew E. Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Sandstrom%2C+K+M">Karin M. Sandstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+A+A">Andrew A. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+F">Benjamin F. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Skillman%2C+E+D">Evan D. Skillman</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">Roger E. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Newman%2C+M+J+B">Max J. B. Newman</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R">Rachael Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Bressan%2C+A">Alessandro Bressan</a>, <a href="/search/astro-ph?searchtype=author&query=Bolatto%2C+A">Alberto Bolatto</a>, <a href="/search/astro-ph?searchtype=author&query=Boylan-Kolchin%2C+M">Michael Boylan-Kolchin</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+A+M">Alyson M. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Bullock%2C+J+S">James S. Bullock</a>, <a href="/search/astro-ph?searchtype=author&query=Conroy%2C+C">Charlie Conroy</a>, <a href="/search/astro-ph?searchtype=author&query=Cooper%2C+M+C">M. C. Cooper</a>, <a href="/search/astro-ph?searchtype=author&query=Dalcanton%2C+J+J">Julianne J. Dalcanton</a>, <a href="/search/astro-ph?searchtype=author&query=Dotter%2C+A+L">Aaron L. Dotter</a> , et al. (17 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2301.04659v1-abstract-short" style="display: inline;"> We present the JWST Resolved Stellar Populations Early Release Science (ERS) science program. We obtained 27.5 hours of NIRCam and NIRISS imaging of three targets in the Local Group (Milky Way globular cluster M92, ultra-faint dwarf galaxy Draco II, star-forming dwarf galaxy WLM), which span factors of $\sim10^5$ in luminosity, $\sim10^4$ in distance, and $\sim10^5$ in surface brightness. We descr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.04659v1-abstract-full').style.display = 'inline'; document.getElementById('2301.04659v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.04659v1-abstract-full" style="display: none;"> We present the JWST Resolved Stellar Populations Early Release Science (ERS) science program. We obtained 27.5 hours of NIRCam and NIRISS imaging of three targets in the Local Group (Milky Way globular cluster M92, ultra-faint dwarf galaxy Draco II, star-forming dwarf galaxy WLM), which span factors of $\sim10^5$ in luminosity, $\sim10^4$ in distance, and $\sim10^5$ in surface brightness. We describe the survey strategy, scientific and technical goals, implementation details, present select NIRCam color-magnitude diagrams (CMDs), and validate the NIRCam exposure time calculator (ETC). Our CMDs are among the deepest in existence for each class of target. They touch the theoretical hydrogen burning limit in M92 ($<0.08$ $M_{\odot}$; SNR $\sim5$ at $m_{F090W}\sim28.2$; $M_{F090W}\sim+13.6$), include the lowest-mass stars observed outside the Milky Way in Draco II (0.09 $M_{\odot}$; SNR $=10$ at $m_{F090W}\sim29$; $M_{F090W}\sim+12.1$), and reach $\sim1.5$ magnitudes below the oldest main sequence turnoff in WLM (SNR $=10$ at $m_{F090W}\sim29.5$; $M_{F090W}\sim+4.6$). The PARSEC stellar models provide a good qualitative match to the NIRCam CMDs, though are $\sim0.05$ mag too blue compared to M92 F090W$-$F150W data. The NIRCam ETC (v2.0) matches the SNRs based on photon noise from DOLPHOT stellar photometry in uncrowded fields, but the ETC may not be accurate in more crowded fields, similar to what is known for HST. We release beta versions of DOLPHOT NIRCam and NIRISS modules to the community. Results from this ERS program will establish JWST as the premier instrument for resolved stellar populations studies for decades to come. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.04659v1-abstract-full').style.display = 'none'; document.getElementById('2301.04659v1-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 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">23 pages, 7 Figures, 3 Tables. Submitted to AAS Journals. Comments welcome</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.04157">arXiv:2301.04157</a> <span> [<a href="https://arxiv.org/pdf/2301.04157">pdf</a>, <a href="https://arxiv.org/format/2301.04157">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/acaec9">10.3847/1538-4357/acaec9 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Pegasus W: An Ultra-Faint Dwarf Galaxy Outside the Halo of M31 Not Quenched by Reionization </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=McQuinn%2C+K+B+W">Kristen. B. W. McQuinn</a>, <a href="/search/astro-ph?searchtype=author&query=Mao%2C+Y">Yao-Yuan Mao</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+M+R">Matthew R. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Shih%2C+D">David Shih</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">Roger E. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">Andrew E. Dolphin</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="2301.04157v3-abstract-short" style="display: inline;"> We report the discovery of an ultrafaint dwarf (UFD) galaxy, Pegasus W, located on the far side of the Milky Way-M31 system and outside the virial radius of M31. The distance to the galaxy is 915 (+60/-91) kpc, measured using the luminosity of horizontal branch (HB) stars identified in Hubble Space Telescope optical imaging. The galaxy has a half-light radius (r_h) of 100 (+11/-13) pc, M_V = -7.20… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.04157v3-abstract-full').style.display = 'inline'; document.getElementById('2301.04157v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.04157v3-abstract-full" style="display: none;"> We report the discovery of an ultrafaint dwarf (UFD) galaxy, Pegasus W, located on the far side of the Milky Way-M31 system and outside the virial radius of M31. The distance to the galaxy is 915 (+60/-91) kpc, measured using the luminosity of horizontal branch (HB) stars identified in Hubble Space Telescope optical imaging. The galaxy has a half-light radius (r_h) of 100 (+11/-13) pc, M_V = -7.20 (+0.17/-0.16) mag, and a present-day stellar mass of 6.5 (+1.1/-1.4) x 10^4 Msun. We identify sources in the color-magnitude diagram (CMD) that may be younger than ~500 Myr suggesting late-time star formation in the UFD galaxy, although further study is needed to confirm these are bona fide young stars in the galaxy. Based on fitting the CMD with stellar evolution libraries, Pegasus W shows an extended star formation history (SFH). Using the tau_90 metric (defined as the timescale by which the galaxy formed 90% of its stellar mass), the galaxy was quenched only 7.4 (+2.2/-2.6) Gyr ago, which is similar to the quenching timescale of a number of UFD satellites of M31 but significantly more recent than the UFD satellites of the Milky Way. Such late-time quenching is inconsistent with the more rapid timescale expected by reionization and suggests that, while not currently a satellite of M31, Pegasus W was nonetheless slowly quenched by environmental processes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.04157v3-abstract-full').style.display = 'none'; document.getElementById('2301.04157v3-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 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 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">15 pages, 10 figures, 2 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.12912">arXiv:2209.12912</a> <span> [<a href="https://arxiv.org/pdf/2209.12912">pdf</a>, <a href="https://arxiv.org/format/2209.12912">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/stac2794">10.1093/mnras/stac2794 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A detailed star formation history for the extremely diffuse Andromeda XIX dwarf galaxy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collins%2C+M+L+M">Michelle L. M. Collins</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+F">Benjamin F. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Tollerud%2C+E+J">Erik J. Tollerud</a>, <a href="/search/astro-ph?searchtype=author&query=Balbinot%2C+E">Eduardo Balbinot</a>, <a href="/search/astro-ph?searchtype=author&query=Gilbert%2C+K+M">Karoline M. Gilbert</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A">Andrew Dolphin</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="2209.12912v1-abstract-short" style="display: inline;"> We present deep imaging of the ultra-diffuse Andromeda XIX dwarf galaxy from the Advance Camera for Surveys on the Hubble Space Telescope which resolves its stellar populations to below the oldest main sequence turn-off. We derive a full star formation history for the galaxy using MATCH, and find no evidence of star formation in the past 8 Gyr. We calculate a quenching time of $蟿_{90}=9.7\pm0.2$~G… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.12912v1-abstract-full').style.display = 'inline'; document.getElementById('2209.12912v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.12912v1-abstract-full" style="display: none;"> We present deep imaging of the ultra-diffuse Andromeda XIX dwarf galaxy from the Advance Camera for Surveys on the Hubble Space Telescope which resolves its stellar populations to below the oldest main sequence turn-off. We derive a full star formation history for the galaxy using MATCH, and find no evidence of star formation in the past 8 Gyr. We calculate a quenching time of $蟿_{90}=9.7\pm0.2$~Gyr, suggesting Andromeda~XIX ceased forming stars very early on. This early quenching, combined with its extremely large half-light radius, low density dark matter halo and lower than expected metallicity make it a unique galaxy within the Local Group and raises questions about how it formed. The early quenching time allows us to rule out feedback from bursty star formation as a means to explain its diffuse stellar population and low density dark matter halo. We find that the extended stellar population, low density halo and star formation could be explained by either tidal interactions (such as tidal shocking) or by late dry mergers, with the latter also explaining its low metallicity. Proper motions and detailed abundances would allow us to distinguish between these two scenarios. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.12912v1-abstract-full').style.display = 'none'; document.getElementById('2209.12912v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 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">8 pages, 4 figures, accepted for publication in MNRAS, Published by Oxford University Press on behalf of the Royal Astronomical Society</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.03348">arXiv:2209.03348</a> <span> [<a href="https://arxiv.org/pdf/2209.03348">pdf</a>, <a href="https://arxiv.org/format/2209.03348">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> The JWST Resolved Stellar Populations Early Release Science Program I.: NIRCam Flux Calibration </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Boyer%2C+M+L">Martha L. Boyer</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">Jay Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Gennaro%2C+M">Mario Gennaro</a>, <a href="/search/astro-ph?searchtype=author&query=Geha%2C+M">Marla Geha</a>, <a href="/search/astro-ph?searchtype=author&query=McQuinn%2C+K+B+W">Kristen B. Wingfield McQuinn</a>, <a href="/search/astro-ph?searchtype=author&query=Tollerud%2C+E">Erik Tollerud</a>, <a href="/search/astro-ph?searchtype=author&query=Correnti%2C+M">Matteo Correnti</a>, <a href="/search/astro-ph?searchtype=author&query=Newman%2C+M+J+B">Max J. Brenner Newman</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">Roger E. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Kallivayalil%2C+N">Nitya Kallivayalil</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R">Rachel Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+A+A">Andrew A. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A">Andrew Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Kalirai%2C+J+S">Jason S. Kalirai</a>, <a href="/search/astro-ph?searchtype=author&query=Sandstrom%2C+K+M">Karin M. Sandstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Savino%2C+A">Alessandro Savino</a>, <a href="/search/astro-ph?searchtype=author&query=Skillman%2C+E+D">Evan D. Skillman</a>, <a href="/search/astro-ph?searchtype=author&query=Weisz%2C+D+R">Daniel R. Weisz</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+F">Benjamin F. Williams</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.03348v1-abstract-short" style="display: inline;"> We use globular cluster data from the Resolved Stellar Populations Early Release Science (ERS) program to validate the flux calibration for the Near Infrared Camera (NIRCam) on the James Webb Space Telescope (JWST). We find a significant flux offset between the eight short wavelength detectors, ranging from 1-23% (about 0.01-0.2 mag) that affects all NIRCam imaging observations. We deliver improve… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.03348v1-abstract-full').style.display = 'inline'; document.getElementById('2209.03348v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.03348v1-abstract-full" style="display: none;"> We use globular cluster data from the Resolved Stellar Populations Early Release Science (ERS) program to validate the flux calibration for the Near Infrared Camera (NIRCam) on the James Webb Space Telescope (JWST). We find a significant flux offset between the eight short wavelength detectors, ranging from 1-23% (about 0.01-0.2 mag) that affects all NIRCam imaging observations. We deliver improved zeropoints for the ERS filters and show that alternate zeropoints derived by the community also improve the calibration significantly. We also find that the detector offsets appear to be time variable by up to at least 0.1 mag. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.03348v1-abstract-full').style.display = 'none'; document.getElementById('2209.03348v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 September, 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">Accepted for publication in RNAAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.11393">arXiv:2206.11393</a> <span> [<a href="https://arxiv.org/pdf/2206.11393">pdf</a>, <a href="https://arxiv.org/format/2206.11393">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/ac7568">10.3847/1538-4357/ac7568 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER) II. The Spatially Resolved Recent Star Formation History of M33 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lazzarini%2C+M">Margaret Lazzarini</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+F">Benjamin F. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Durbin%2C+M+J">Meredith J. Durbin</a>, <a href="/search/astro-ph?searchtype=author&query=Dalcanton%2C+J+J">Julianne J. Dalcanton</a>, <a href="/search/astro-ph?searchtype=author&query=Smercina%2C+A">Adam Smercina</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+Y">Yumi Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A">Andrew Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Gilbert%2C+K">Karoline Gilbert</a>, <a href="/search/astro-ph?searchtype=author&query=Guhathakurta%2C+P">Puragra Guhathakurta</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Skillman%2C+E">Evan Skillman</a>, <a href="/search/astro-ph?searchtype=author&query=Telford%2C+O+G">O. Grace Telford</a>, <a href="/search/astro-ph?searchtype=author&query=Weisz%2C+D">Daniel Weisz</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="2206.11393v1-abstract-short" style="display: inline;"> We measure the spatially resolved recent star formation history (SFH) of M33 using optical images taken with the Hubble Space Telescope as part of the Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER) survey. The area covered by the observations used in this analysis covers a de-projected area of $\sim$38 kpc$^{2}$ and extends to $\sim$3.5 and $\sim$2 kpc from the center… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.11393v1-abstract-full').style.display = 'inline'; document.getElementById('2206.11393v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.11393v1-abstract-full" style="display: none;"> We measure the spatially resolved recent star formation history (SFH) of M33 using optical images taken with the Hubble Space Telescope as part of the Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER) survey. The area covered by the observations used in this analysis covers a de-projected area of $\sim$38 kpc$^{2}$ and extends to $\sim$3.5 and $\sim$2 kpc from the center of M33 along the major and semi-major axes, respectively. We divide the PHATTER optical survey into 2005 regions that measure 24 arcsec, $\sim$100 pc, on a side and fit color magnitude diagrams for each region individually to measure the spatially resolved SFH of M33 within the PHATTER footprint. There are significant fluctuations in the SFH on small spatial scales and also galaxy-wide scales that we measure back to about 630 Myr ago. We observe a more flocculent spiral structure in stellar populations younger than about 80 Myr, while the structure of the older stellar populations is dominated by two spiral arms. We also observe a bar in the center of M33, which dominates at ages older than about 80 Myr. Finally, we find that the mean star formation rate (SFR) over the last 100 Myr within the PHATTER footprint is 0.32$\pm$0.02 M$_{\odot}$ yr$^{-1}$. We measure a current SFR (over the last 10 Myr) of 0.20$\pm$0.03 M$_{\odot}$ yr$^{-1}$. This SFR is slightly higher than previous measurements from broadband estimates, when scaled to account for the fraction of the D25 area covered by the PHATTER survey footprint. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.11393v1-abstract-full').style.display = 'none'; document.getElementById('2206.11393v1-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 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">accepted for publication in ApJ, 37 pages, 18 figures, 6 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.02801">arXiv:2206.02801</a> <span> [<a href="https://arxiv.org/pdf/2206.02801">pdf</a>, <a href="https://arxiv.org/format/2206.02801">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/ac91cb">10.3847/1538-4357/ac91cb <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Hubble Space Telescope Survey of M31 Satellite Galaxies I. RR Lyrae-based Distances and Refined 3D Geometric Structure </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Savino%2C+A">Alessandro Savino</a>, <a href="/search/astro-ph?searchtype=author&query=Weisz%2C+D+R">Daniel R. Weisz</a>, <a href="/search/astro-ph?searchtype=author&query=Skillman%2C+E+D">Evan D. Skillman</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A">Andrew Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Kallivayalil%2C+N">Nitya Kallivayalil</a>, <a href="/search/astro-ph?searchtype=author&query=Wetzel%2C+A">Andrew Wetzel</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">Jay Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Besla%2C+G">Gurtina Besla</a>, <a href="/search/astro-ph?searchtype=author&query=Boylan-Kolchin%2C+M">Michael Boylan-Kolchin</a>, <a href="/search/astro-ph?searchtype=author&query=Bullock%2C+J+S">James S. Bullock</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+A+A">Andrew A. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Collins%2C+M+L+M">Michelle L. M. Collins</a>, <a href="/search/astro-ph?searchtype=author&query=Cooper%2C+M+C">M. C. Cooper</a>, <a href="/search/astro-ph?searchtype=author&query=Deason%2C+A+J">Alis J. Deason</a>, <a href="/search/astro-ph?searchtype=author&query=Dotter%2C+A+L">Aaron L. Dotter</a>, <a href="/search/astro-ph?searchtype=author&query=Fardal%2C+M">Mark Fardal</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+A+M+N">Annette M. N. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Fritz%2C+T+K">Tobias K. Fritz</a>, <a href="/search/astro-ph?searchtype=author&query=Geha%2C+M+C">Marla C. Geha</a>, <a href="/search/astro-ph?searchtype=author&query=Gilbert%2C+K+M">Karoline M. Gilbert</a>, <a href="/search/astro-ph?searchtype=author&query=Guhathakurta%2C+P">Puragra Guhathakurta</a>, <a href="/search/astro-ph?searchtype=author&query=Ibata%2C+R">Rodrigo Ibata</a>, <a href="/search/astro-ph?searchtype=author&query=Irwin%2C+M+J">Michael J. Irwin</a>, <a href="/search/astro-ph?searchtype=author&query=Jeon%2C+M">Myoungwon Jeon</a>, <a href="/search/astro-ph?searchtype=author&query=Kirby%2C+E">Evan Kirby</a> , et al. (11 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2206.02801v2-abstract-short" style="display: inline;"> We measure homogeneous distances to M31 and 38 associated stellar systems ($-$16.8$\le M_V \le$ $-$6.0), using time-series observations of RR Lyrae stars taken as part of the Hubble Space Telescope Treasury Survey of M31 Satellites. From $>700$ orbits of new/archival ACS imaging, we identify $>4700$ RR Lyrae stars and determine their periods and mean magnitudes to a typical precision of 0.01 days… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.02801v2-abstract-full').style.display = 'inline'; document.getElementById('2206.02801v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.02801v2-abstract-full" style="display: none;"> We measure homogeneous distances to M31 and 38 associated stellar systems ($-$16.8$\le M_V \le$ $-$6.0), using time-series observations of RR Lyrae stars taken as part of the Hubble Space Telescope Treasury Survey of M31 Satellites. From $>700$ orbits of new/archival ACS imaging, we identify $>4700$ RR Lyrae stars and determine their periods and mean magnitudes to a typical precision of 0.01 days and 0.04 mag. Based on Period-Wesenheit-Metallicity relationships consistent with the Gaia eDR3 distance scale, we uniformly measure heliocentric and M31-centric distances to a typical precision of $\sim20$ kpc (3%) and $\sim10$ kpc (8%), respectively. We revise the 3D structure of the M31 galactic ecosystem and: (i) confirm a highly anisotropic spatial distribution such that $\sim80$% of M31's satellites reside on the near side of M31; this feature is not easily explained by observational effects; (ii) affirm the thin (rms $7-23$ kpc) planar "arc" of satellites that comprises roughly half (15) of the galaxies within 300 kpc from M31; (iii) reassess physical proximity of notable associations such as the NGC 147/185 pair and M33/AND XXII; and (iv) illustrate challenges in tip-of-the-red-giant branch distances for galaxies with $M_V > -9.5$, which can be biased by up to 35%. We emphasize the importance of RR Lyrae for accurate distances to faint galaxies that should be discovered by upcoming facilities (e.g., Rubin Observatory). We provide updated luminosities and sizes for our sample. Our distances will serve as the basis for future investigation of the star formation and orbital histories of the entire known M31 satellite system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.02801v2-abstract-full').style.display = 'none'; document.getElementById('2206.02801v2-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 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 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">32 pages, 15 figures, accepted for publication on 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/2201.07339">arXiv:2201.07339</a> <span> [<a href="https://arxiv.org/pdf/2201.07339">pdf</a>, <a href="https://arxiv.org/format/2201.07339">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/10.3847/1538-3881/ac4d2c">10.3847/1538-3881/ac4d2c <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Determining the Timescale over Which Stellar Feedback Drives Turbulence in the ISM: A Study of four Nearby Dwarf Irregular Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hunter%2C+L+C">Laura Congreve Hunter</a>, <a href="/search/astro-ph?searchtype=author&query=van+Zee%2C+L">Liese van Zee</a>, <a href="/search/astro-ph?searchtype=author&query=McQuinn%2C+K+B+W">Kristen B. W. McQuinn</a>, <a href="/search/astro-ph?searchtype=author&query=Garner%2C+R">Ray Garner</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">Andrew E. Dolphin</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="2201.07339v1-abstract-short" style="display: inline;"> Stellar feedback is fundamental to the modeling of galaxy evolution as it drives turbulence and outflows in galaxies. Understanding the timescales involved are critical for constraining the impact of stellar feedback on the interstellar medium (ISM). We analyzed the resolved star formation histories along with the spatial distribution and kinematics of the atomic and ionized gas of four nearby sta… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.07339v1-abstract-full').style.display = 'inline'; document.getElementById('2201.07339v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.07339v1-abstract-full" style="display: none;"> Stellar feedback is fundamental to the modeling of galaxy evolution as it drives turbulence and outflows in galaxies. Understanding the timescales involved are critical for constraining the impact of stellar feedback on the interstellar medium (ISM). We analyzed the resolved star formation histories along with the spatial distribution and kinematics of the atomic and ionized gas of four nearby star-forming dwarf galaxies (NGC 4068, NGC 4163, NGC 6789, UGC 9128) to determine the timescales over which stellar feedback drives turbulence. The four galaxies are within 5 Mpc and have a range of properties including current star formation rates of 0.0005 to 0.01 M$_{\odot}$ yr$^{-1}$, log(M$_*$/M$_{\odot}$) between 7.2 and 8.2, and log(M$_{HI}$/M$_\odot$) between 7.2 and 8.3. Their Color-Magnitude Diagram (CMD) derived star formation histories over the past 500 Myrs were compared to their atomic and ionized gas velocity dispersion and HI energy surface densities as indicators of turbulence. The Spearman's rank correlation coefficient was used to identify any correlations between their current turbulence and their past star formation activity on local scales ($\sim$400 pc). The strongest correlation found was between the HI turbulence measures and the star formation rate 100-200 Myrs ago. This suggests a coupling between the star formation activity and atomic gas on this timescale. No strong correlation between the ionized gas velocity dispersion and the star formation activity between 5-500 Myrs ago was found. The sample and analysis are the foundation of a larger program aimed at understanding the timescales over which stellar feedback drives turbulence. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.07339v1-abstract-full').style.display = 'none'; document.getElementById('2201.07339v1-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 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">21 pages, 19 figures. Accepted for publication in AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.04161">arXiv:2201.04161</a> <span> [<a href="https://arxiv.org/pdf/2201.04161">pdf</a>, <a href="https://arxiv.org/format/2201.04161">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/ac51cf">10.3847/1538-4357/ac51cf <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER). III. The Mass Function of Young Star Clusters in M33 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wainer%2C+T+M">Tobin M. Wainer</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+L+C">L. Clifton Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Seth%2C+A+C">Anil C. Seth</a>, <a href="/search/astro-ph?searchtype=author&query=TorresVillanueva%2C+E+E">Estephani E. TorresVillanueva</a>, <a href="/search/astro-ph?searchtype=author&query=Dalcanton%2C+J+J">Julianne J. Dalcanton</a>, <a href="/search/astro-ph?searchtype=author&query=Durbin%2C+M+J">Meredith J. Durbin</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A">Andrew Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Weisz%2C+D+R">Daniel R. Weisz</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+F">Benjamin F. Williams</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2201.04161v2-abstract-short" style="display: inline;"> We measure the star cluster mass function for the Local Group galaxy M33. We use the catalog of stellar clusters selected from the Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER) survey. We analyze 711 clusters in M33 with $\rm 7.0 < log(Age/yr) < 8.5$, and log($M/M_{\odot}$) $>$ 3.0 as determined from color-magnitude diagram fits to individual stars. The M33 cluster m… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.04161v2-abstract-full').style.display = 'inline'; document.getElementById('2201.04161v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.04161v2-abstract-full" style="display: none;"> We measure the star cluster mass function for the Local Group galaxy M33. We use the catalog of stellar clusters selected from the Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER) survey. We analyze 711 clusters in M33 with $\rm 7.0 < log(Age/yr) < 8.5$, and log($M/M_{\odot}$) $>$ 3.0 as determined from color-magnitude diagram fits to individual stars. The M33 cluster mass function is best described by a Schechter function with power law slope $伪= -2.06^{+0.14}_{-0.13}$, and truncation mass log($M_c/M_{\odot}$) $= 4.24^{+0.16}_{-0.13}$. The data show strong evidence for a high-mass truncation, thus strongly favoring a Schechter function fit over a pure power law. M33's truncation mass is consistent with the previously identified linear trend between $M_c$, and star formation rate surface density, \SigSFR. We also explore the effect that individual cluster mass uncertainties have on derived mass function parameters, and find evidence to suggest that large cluster mass uncertainties have the potential to bias the truncation mass of fitted mass functions on the one sigma level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.04161v2-abstract-full').style.display = 'none'; document.getElementById('2201.04161v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">18 pages, 15 figures, 1 table, Accepted to ApJ (February 2, 2022)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.00045">arXiv:2111.00045</a> <span> [<a href="https://arxiv.org/pdf/2111.00045">pdf</a>, <a href="https://arxiv.org/format/2111.00045">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/ac3665">10.3847/1538-4357/ac3665 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Metallicity Distribution Function of the Eridanus~II Ultra-Faint Dwarf Galaxy from Hubble Space Telescope Narrow-band Imaging </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fu%2C+S+W">Sal Wanying Fu</a>, <a href="/search/astro-ph?searchtype=author&query=Weisz%2C+D+R">Daniel R. Weisz</a>, <a href="/search/astro-ph?searchtype=author&query=Starkenburg%2C+E">Else Starkenburg</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+N">Nicolas Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Ji%2C+A+P">Alexander P. Ji</a>, <a href="/search/astro-ph?searchtype=author&query=Patel%2C+E">Ekta Patel</a>, <a href="/search/astro-ph?searchtype=author&query=Boylan-Kolchin%2C+M">Michael Boylan-Kolchin</a>, <a href="/search/astro-ph?searchtype=author&query=Cote%2C+P">Patrick Cote</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">Andrew E. Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Longeard%2C+N">Nicolas Longeard</a>, <a href="/search/astro-ph?searchtype=author&query=Mateo%2C+M+L">Mario L. Mateo</a>, <a href="/search/astro-ph?searchtype=author&query=Sandford%2C+N+R">Nathan R. Sandford</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="2111.00045v1-abstract-short" style="display: inline;"> We use deep narrowband Ca H&K ($F395N$) imaging taken with the Hubble Space Telescope (HST) to construct the metallicity distribution function (MDF) of Local Group (LG) ultra-faint dwarf (UFD) galaxy Eridanus II (Eri II). When combined with archival $F475W$ and $F814W$ data, we measure metallicities for 60 resolved red giant branch stars as faint as $m_{F475W}\sim24$ mag, a factor of $\sim4$x more… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.00045v1-abstract-full').style.display = 'inline'; document.getElementById('2111.00045v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.00045v1-abstract-full" style="display: none;"> We use deep narrowband Ca H&K ($F395N$) imaging taken with the Hubble Space Telescope (HST) to construct the metallicity distribution function (MDF) of Local Group (LG) ultra-faint dwarf (UFD) galaxy Eridanus II (Eri II). When combined with archival $F475W$ and $F814W$ data, we measure metallicities for 60 resolved red giant branch stars as faint as $m_{F475W}\sim24$ mag, a factor of $\sim4$x more stars than current spectroscopic MDF determinations. We find that Eri II has a mean metallicity of [Fe/H]$=$-2.50$^{+0.07}_{-0.07}$ and a dispersion of $蟽_{\mbox{[Fe/H]}}=0.42^{+0.06}_{-0.06}$, which are consistent with spectroscopic MDFs, though more precisely constrained owing to a larger sample. We identify a handful of extremely metal-poor star candidates (EMP; [Fe/H] $< -3$) that are marginally bright enough for spectroscopic follow up. Eri II's MDF appears well-described by a leaky box chemical evolution model. We also compute an updated orbital history for Eri II using Gaia eDR3 proper motions, and find that it is likely on first infall into the Milky Way. Our findings suggest that Eri II underwent an evolutionary history similar to that of an isolated galaxy. Compared to MDFs for select cosmological simulations of similar mass galaxies, we find that Eri II has a lower fraction of stars with [Fe/H] $< -3$, though such comparisons should currently be treated with caution due to a paucity of simulations, selection effects, and known limitations of Ca H&K for EMPs. This study demonstrates the power of deep HST CaHK imaging for measuring the MDFs of UFDs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.00045v1-abstract-full').style.display = 'none'; document.getElementById('2111.00045v1-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 October, 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">Resubmitted to ApJ with revisions following a positive referee report of the initial draft; 29 pages, 19 figures, and 3 tables, including appendix. Comments welcome!</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.05100">arXiv:2105.05100</a> <span> [<a href="https://arxiv.org/pdf/2105.05100">pdf</a>, <a href="https://arxiv.org/format/2105.05100">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/ac03ae">10.3847/1538-4357/ac03ae <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy Properties at the Faint End of the HI Mass Function </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=McQuinn%2C+K+B+W">Kristen B. W. McQuinn</a>, <a href="/search/astro-ph?searchtype=author&query=Telidevara%2C+A+K">Anjana K. Telidevara</a>, <a href="/search/astro-ph?searchtype=author&query=Fuson%2C+J">Jackson Fuson</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+E+A+K">Elizabeth A. K. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Cannon%2C+J+M">John M. Cannon</a>, <a href="/search/astro-ph?searchtype=author&query=Skillman%2C+E+D">Evan D. Skillman</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">Andrew E. Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Haynes%2C+M+P">Martha P. Haynes</a>, <a href="/search/astro-ph?searchtype=author&query=Rhode%2C+K+L">Katherine L. Rhode</a>, <a href="/search/astro-ph?searchtype=author&query=Salzer%2C+J+J">John. J. Salzer</a>, <a href="/search/astro-ph?searchtype=author&query=Giovanelli%2C+R">Riccardo Giovanelli</a>, <a href="/search/astro-ph?searchtype=author&query=Gordon%2C+A+J+R">Alex J. R. Gordon</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="2105.05100v4-abstract-short" style="display: inline;"> The Survey of HI in Extremely Low-mass Dwarfs (SHIELD) includes a volumetrically complete sample of 82 gas-rich dwarfs with M_HI~<10^7.2 Msun selected from the ALFALFA survey. We are obtaining extensive follow-up observations of the SHIELD galaxies to study their gas, stellar, and chemical content, and to better understand galaxy evolution at the faint end of the HI mass function. Here, we investi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.05100v4-abstract-full').style.display = 'inline'; document.getElementById('2105.05100v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.05100v4-abstract-full" style="display: none;"> The Survey of HI in Extremely Low-mass Dwarfs (SHIELD) includes a volumetrically complete sample of 82 gas-rich dwarfs with M_HI~<10^7.2 Msun selected from the ALFALFA survey. We are obtaining extensive follow-up observations of the SHIELD galaxies to study their gas, stellar, and chemical content, and to better understand galaxy evolution at the faint end of the HI mass function. Here, we investigate the properties of 30 SHIELD galaxies using Hubble Space Telescope imaging of their resolved stars and Westerbork Synthesis Radio Telescope observations of their neutral hydrogen. We measure tip of the red giant branch (TRGB) distances, star formation activity, and gas properties. The TRGB distances are up to 4x greater than estimates from flow models, highlighting the importance of velocity-independent distance indicators in the nearby universe. The SHIELD galaxies are in under-dense regions, with 23% located in voids; one galaxy appears paired with a more massive dwarf. We quantify galaxy properties at low masses including stellar and HI masses, SFRs, sSFRs, SFEs, birthrate parameters, and gas fractions. The lowest mass systems lie below the mass thresholds where stellar mass assembly is predicted to be impacted by reionization. Even so, we find the star formation properties follow the same trends as higher mass gas-rich systems, albeit with a different normalization. The HI disks are small (<r><0.7 kpc) making it difficult to measure the HI rotation using standard techniques; we develop a new methodology and report the velocity extent, and its associated spatial extent, with robust uncertainties. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.05100v4-abstract-full').style.display = 'none'; document.getElementById('2105.05100v4-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 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">43 pages, 32 figures, 6 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2104.11118">arXiv:2104.11118</a> <span> [<a href="https://arxiv.org/pdf/2104.11118">pdf</a>, <a href="https://arxiv.org/format/2104.11118">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</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/abfb7b">10.3847/1538-4357/abfb7b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Masses of Supernova Remnant Progenitors in NGC 6946 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Koplitz%2C+B">Brad Koplitz</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+J">Jared Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+F">Benjamin F. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Long%2C+K+S">Knox S. Long</a>, <a href="/search/astro-ph?searchtype=author&query=Blair%2C+W+P">William P. Blair</a>, <a href="/search/astro-ph?searchtype=author&query=Murphy%2C+J+W">Jeremiah W. Murphy</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A">Andrew Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Hillis%2C+T">Tristan Hillis</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="2104.11118v1-abstract-short" style="display: inline;"> We constrained the progenitor masses for 169 supernova remnants, 8 historically observed supernovae, and the black hole formation candidate in NGC 6946, finding that they are consistent with originating from a standard initial mass function. Additionally, there were 16 remnants that showed no sign of nearby star formation consistent with a core-collapse supernova, making them good Type Ia candidat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.11118v1-abstract-full').style.display = 'inline'; document.getElementById('2104.11118v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.11118v1-abstract-full" style="display: none;"> We constrained the progenitor masses for 169 supernova remnants, 8 historically observed supernovae, and the black hole formation candidate in NGC 6946, finding that they are consistent with originating from a standard initial mass function. Additionally, there were 16 remnants that showed no sign of nearby star formation consistent with a core-collapse supernova, making them good Type Ia candidates. Using $Hubble$ $Space$ $Telescope$ broadband imaging, we measured stellar photometry of ACS/WFC fields in F435W, F555W, F606W, and F814W filters as well as WFC3/UVIS fields in F438W, F606W, and F814W. We then fitted this photometry with stellar evolutionary models to determine the ages of the young populations present at the positions of the SNRs and SNe. We then infer a progenitor mass probability distribution from the fitted age distribution. For 37 SNRs we tested how different filter combinations affected the inferred masses. We find that filters sensitive to H$伪$, [N II], and [S II] gas emission can bias mass estimates for remnants that rely on our technique. Using a KS-test analysis on our most reliable measurements, we find the progenitor mass distribution is well-matched by a power-law index of $-2.6^{+0.5}_{-0.6}$, which is consistent with a standard initial mass function. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.11118v1-abstract-full').style.display = 'none'; document.getElementById('2104.11118v1-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 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">28 pages, 13 figures, 4 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2104.03319">arXiv:2104.03319</a> <span> [<a href="https://arxiv.org/pdf/2104.03319">pdf</a>, <a href="https://arxiv.org/format/2104.03319">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/ac0335">10.3847/2041-8213/ac0335 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Tip of the Red Giant Branch Distance of $22.1 \pm 1.2$ Mpc to the Dark Matter Deficient Galaxy NGC1052-DF2 from 40 Orbits of Hubble Space Telescope Imaging </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shen%2C+Z">Zili Shen</a>, <a href="/search/astro-ph?searchtype=author&query=Danieli%2C+S">Shany Danieli</a>, <a href="/search/astro-ph?searchtype=author&query=van+Dokkum%2C+P">Pieter van Dokkum</a>, <a href="/search/astro-ph?searchtype=author&query=Abraham%2C+R">Roberto Abraham</a>, <a href="/search/astro-ph?searchtype=author&query=Brodie%2C+J+P">Jean P. Brodie</a>, <a href="/search/astro-ph?searchtype=author&query=Conroy%2C+C">Charlie Conroy</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">Andrew E. Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Romanowsky%2C+A+J">Aaron J. Romanowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Kruijssen%2C+J+M+D">J. M. Diederik Kruijssen</a>, <a href="/search/astro-ph?searchtype=author&query=Chowdhury%2C+D+D">Dhruba Dutta Chowdhury</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="2104.03319v2-abstract-short" style="display: inline;"> The large and diffuse galaxies NGC1052-DF2 and NGC1052-DF4 have been found to have very low dark matter content and a population of luminous globular clusters. Accurate distance measurements are key to interpreting these observations. Recently, the distance to NGC1052-DF4 was found to be $20.0\pm 1.6$ Mpc by identifying the tip of the red giant branch (TRGB) in 12 orbits of Hubble Space Telescope… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.03319v2-abstract-full').style.display = 'inline'; document.getElementById('2104.03319v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.03319v2-abstract-full" style="display: none;"> The large and diffuse galaxies NGC1052-DF2 and NGC1052-DF4 have been found to have very low dark matter content and a population of luminous globular clusters. Accurate distance measurements are key to interpreting these observations. Recently, the distance to NGC1052-DF4 was found to be $20.0\pm 1.6$ Mpc by identifying the tip of the red giant branch (TRGB) in 12 orbits of Hubble Space Telescope (HST) Advanced Camera for Surveys (ACS) imaging. Here we present 40 orbits of HST ACS data for NGC1052-DF2 and use these data to measure its TRGB. The TRGB is readily apparent in the color-magnitude diagram. Using a forward model that incorporates photometric uncertainties, we find a TRGB magnitude of $m_{\rm F814W, TRGB} = 27.67 \pm 0.10$ mag. The inferred distance is $D_{\rm TRGB} = 22.1 \pm 1.2$ Mpc, consistent with the previous surface brightness fluctuation distances to the bright elliptical galaxy NGC1052. The new HST distance rules out the idea that some of NGC1052-DF2's unusual properties can be explained if it were at $\sim 13$ Mpc; instead, it implies that the galaxy's globular clusters are even more luminous than had been derived using the previous distance of 20 Mpc. The distance from NGC1052-DF2 to NGC1052-DF4 is well-determined at $2.1\pm 0.5$ Mpc, significantly larger than the virial diameter of NGC1052. We discuss the implications for formation scenarios of the galaxies and for the external field effect, which has been invoked to explain the intrinsic dynamics of these objects in the context of modified Newtonian dynamics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.03319v2-abstract-full').style.display = 'none'; document.getElementById('2104.03319v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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 ApJ 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/2104.02649">arXiv:2104.02649</a> <span> [<a href="https://arxiv.org/pdf/2104.02649">pdf</a>, <a href="https://arxiv.org/format/2104.02649">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/10.3847/1538-3881/ac0440">10.3847/1538-3881/ac0440 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Extragalactic Distance Database: The Color-Magnitude Diagrams and Tip of the Red Giant Branch Distances Catalog </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Anand%2C+G+S">Gagandeep S. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Rizzi%2C+L">Luca Rizzi</a>, <a href="/search/astro-ph?searchtype=author&query=Tully%2C+R+B">R. Brent Tully</a>, <a href="/search/astro-ph?searchtype=author&query=Shaya%2C+E+J">Edward J. Shaya</a>, <a href="/search/astro-ph?searchtype=author&query=Karachentsev%2C+I+D">Igor D. Karachentsev</a>, <a href="/search/astro-ph?searchtype=author&query=Makarov%2C+D+I">Dmitry I. Makarov</a>, <a href="/search/astro-ph?searchtype=author&query=Makarova%2C+L">Lidia Makarova</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+P">Po-Feng Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">Andrew E. Dolphin</a>, <a href="/search/astro-ph?searchtype=author&query=Kourkchi%2C+E">Ehsan Kourkchi</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="2104.02649v2-abstract-short" style="display: inline;"> The Extragalactic Distance Database (EDD) was created as a repository for high quality, redshift-independent distances. A key component of EDD is the Color Magnitude Diagrams/Tip of the Red Giant Branch (CMDs/TRGB) catalog, which provides information on the stellar content of nearby galaxies observed with the Hubble Space Telescope (HST). Here we provide a decadal update to this catalog, which has… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.02649v2-abstract-full').style.display = 'inline'; document.getElementById('2104.02649v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.02649v2-abstract-full" style="display: none;"> The Extragalactic Distance Database (EDD) was created as a repository for high quality, redshift-independent distances. A key component of EDD is the Color Magnitude Diagrams/Tip of the Red Giant Branch (CMDs/TRGB) catalog, which provides information on the stellar content of nearby galaxies observed with the Hubble Space Telescope (HST). Here we provide a decadal update to this catalog, which has now doubled in size to over 500 galaxies. We highlight the additions to our data reduction and analysis techniques, and provide examples of the science that has been made possible with this large data set. We find the TRGB to be a reliable measure for distance, and we aim to extend its distance coverage with HST to every galaxy within 10 Mpc. In the near-future, the combination of the James Webb Space Telescope and the Nancy Grace Roman Space Telescope will dramatically increase the number of targets within our grasp. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.02649v2-abstract-full').style.display = 'none'; document.getElementById('2104.02649v2-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">8 figures, 20 pages. Accepted to AJ. Materials available at edd.ifa.hawaii.edu</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.11012">arXiv:2101.11012</a> <span> [<a href="https://arxiv.org/pdf/2101.11012">pdf</a>, <a href="https://arxiv.org/format/2101.11012">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</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/stab1800">10.1093/mnras/stab1800 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Progenitor Mass Distribution for 22 Historic Core-Collapse Supernovae </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=D%C3%ADaz-Rodr%C3%ADguez%2C+M">Mariangelly D铆az-Rodr铆guez</a>, <a href="/search/astro-ph?searchtype=author&query=Murphy%2C+J+W">Jeremiah W. Murphy</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+F">Benjamin F. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Dalcanton%2C+J+J">Julianne J. Dalcanton</a>, <a href="/search/astro-ph?searchtype=author&query=Dolphin%2C+A+E">Andrew E. Dolphin</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="2101.11012v2-abstract-short" style="display: inline;"> We infer the progenitor mass distribution for 22 historic core-collapse supernovae (CCSNe) using a Bayesian hierarchical model. For this inference, we use the local star formation histories to estimate the age for each supernova (SN). These star formation histories often show multiple bursts of star formation; our model assumes that one burst is associated with the SN progenitor and the others are… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.11012v2-abstract-full').style.display = 'inline'; document.getElementById('2101.11012v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.11012v2-abstract-full" style="display: none;"> We infer the progenitor mass distribution for 22 historic core-collapse supernovae (CCSNe) using a Bayesian hierarchical model. For this inference, we use the local star formation histories to estimate the age for each supernova (SN). These star formation histories often show multiple bursts of star formation; our model assumes that one burst is associated with the SN progenitor and the others are random bursts of star formation. The primary inference is the progenitor age distribution. Due to the limited number of historic SNe and highly uncertain star formation at young ages, we restrict our inference to the slope of the age distribution and the maximum age for CCSNe. Using single-star evolutionary models, we transform the progenitor age distribution into a progenitor mass distribution. Under these assumptions, the minimum mass for CCSNe is ${M_\textrm{min}}~=~8.60^{+0.37}_{-0.41} \ M_\odot$ and the slope of the progenitor mass distribution is $伪= -2.61^{+1.05}_{-1.18}$. The power-law slope for the progenitor mass distribution is consistent with the standard Salpeter initial mass function ($伪= -2.35$). These values are consistent with previous estimates using precursor imaging and the age-dating technique, further confirming that using stellar populations around SN and supernova remnants is a reliable way to infer the progenitor masses. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.11012v2-abstract-full').style.display = 'none'; document.getElementById('2101.11012v2-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 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2021. </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 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