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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Williams%2C+T+G&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Williams%2C+T+G&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Williams%2C+T+G&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Williams%2C+T+G&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> </ul> </nav> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.04481">arXiv:2502.04481</a> <span> [<a href="https://arxiv.org/pdf/2502.04481">pdf</a>, <a href="https://arxiv.org/format/2502.04481">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"> Cloud-scale gas properties, depletion times, and star formation efficiency per free-fall time in PHANGS--ALMA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A+K">Adam K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+J">Jiayi Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Meidt%2C+S">Sharon Meidt</a>, <a href="/search/astro-ph?searchtype=author&query=Agertz%2C+O">Oscar Agertz</a>, <a href="/search/astro-ph?searchtype=author&query=Chiang%2C+I">I-Da Chiang</a>, <a href="/search/astro-ph?searchtype=author&query=Gensior%2C+J">Jindra Gensior</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S+C+O">Simon C. O. Glover</a>, <a href="/search/astro-ph?searchtype=author&query=Gnedin%2C+O+Y">Oleg Y. Gnedin</a>, <a href="/search/astro-ph?searchtype=author&query=Hughes%2C+A">Annie Hughes</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A+T">Ashley T. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">Frank Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Bolatto%2C+A+D">Alberto D. Bolatto</a>, <a href="/search/astro-ph?searchtype=author&query=Colombo%2C+D">Dario Colombo</a>, <a href="/search/astro-ph?searchtype=author&query=Brok%2C+J+d">Jakob den Brok</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">Melanie Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Chown%2C+R">Ryan Chown</a>, <a href="/search/astro-ph?searchtype=author&query=Eibensteiner%2C+C">Cosima Eibensteiner</a>, <a href="/search/astro-ph?searchtype=author&query=Gleis%2C+D+R">Damian R. Gleis</a>, <a href="/search/astro-ph?searchtype=author&query=Grasha%2C+K">Kathryn Grasha</a>, <a href="/search/astro-ph?searchtype=author&query=Henshaw%2C+J+D">Jonathan D. Henshaw</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R+S">Ralf S. Klessen</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=Oakes%2C+E+K">Elias K. Oakes</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+H">Hsi-An Pan</a> , et al. (9 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2502.04481v1-abstract-short" style="display: inline;"> We compare measurements of star formation efficiency to cloud-scale gas properties across PHANGS-ALMA. Dividing 67 galaxies into 1.5 kpc scale regions, we calculate the molecular gas depletion time, tau_dep= Sigma_mol/Sigma_SFR, and the star formation efficiency per free-fall time, eff=tau_ff/tau_dep, for each region. Then we test how tau_dep and eff vary as functions of the regional mass-weighted… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.04481v1-abstract-full').style.display = 'inline'; document.getElementById('2502.04481v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.04481v1-abstract-full" style="display: none;"> We compare measurements of star formation efficiency to cloud-scale gas properties across PHANGS-ALMA. Dividing 67 galaxies into 1.5 kpc scale regions, we calculate the molecular gas depletion time, tau_dep= Sigma_mol/Sigma_SFR, and the star formation efficiency per free-fall time, eff=tau_ff/tau_dep, for each region. Then we test how tau_dep and eff vary as functions of the regional mass-weighted mean molecular gas properties on cloud scales (60-150pc): gas surface density, <Sigma_mol^cloud>, velocity dispersion, <sigma_mol^cloud>, virial parameter, <alpha_vir^cloud>, and gravitational free-fall time, <tau_ff^cloud>. <tau_ff^cloud> and tau_dep correlate positively, consistent with the expectation that gas density plays a key role in setting the rate of star formation. Our fiducial measurements suggest tau_dep \propto <tau_ff^cloud>^0.5 and eff \approx 0.34%, though the exact numbers depend on the adopted fitting methods. We also observe anti-correlations between tau_dep and <Sigma_mol^cloud> and between tau_dep^mol and <sigma_mol^cloud> . All three correlations may reflect the same underlying link between density and star formation efficiency combined with systematic variations in the degree to which self-gravity binds molecular gas in galaxies. We highlight the tau_dep-<sigma_mol^cloud> relation because of the lower degree of correlation between the axes. Contrary to theoretical expectations, we observe an anti-correlation between tau_dep^mol and <alpha_vir^cloud> and no significant correlation between eff and <alpha_vir^cloud>. Our results depend sensitively on the adopted CO-to-H2 conversion factor, with corrections for excitation and emissivity effects in inner galaxies playing an important role. We emphasize that our simple methodology and clean selection allow easy comparison to numerical simulations and highlight this as a logical next direction. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.04481v1-abstract-full').style.display = 'none'; document.getElementById('2502.04481v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 February, 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">Accepted for publication in the Astrophysical Journal. 35 pages, 16 figures, 9 tables. Full data tables available here: https://www.canfar.net/storage/vault/list/phangs/RELEASES/Leroy_etal_2025</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.10539">arXiv:2501.10539</a> <span> [<a href="https://arxiv.org/pdf/2501.10539">pdf</a>, <a href="https://arxiv.org/format/2501.10539">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"> PAH Feature Ratios Around Stellar Clusters and Associations in 19 Nearby Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">Daniel A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Graham%2C+G+B">Gabrielle B. Graham</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A+T">Ashley T. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Baron%2C+D">Dalya Baron</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">Frank Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Boquien%2C+M">M茅d茅ric Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Chandar%2C+R">Rupali Chandar</a>, <a href="/search/astro-ph?searchtype=author&query=Chastenet%2C+J">J茅r茅my Chastenet</a>, <a href="/search/astro-ph?searchtype=author&query=Chown%2C+R">Ryan Chown</a>, <a href="/search/astro-ph?searchtype=author&query=Egorov%2C+O+V">Oleg V. Egorov</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S+C+O">Simon C. O. Glover</a>, <a href="/search/astro-ph?searchtype=author&query=Hands%2C+L">Lindsey Hands</a>, <a href="/search/astro-ph?searchtype=author&query=Henny%2C+K+F">Kiana F. Henny</a>, <a href="/search/astro-ph?searchtype=author&query=Indebetouw%2C+R">Remy Indebetouw</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R+S">Ralf S. Klessen</a>, <a href="/search/astro-ph?searchtype=author&query=Larson%2C+K+L">Kirsten L. Larson</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J+C">Janice C. Lee</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=Maschmann%2C+D">Daniel Maschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Pathak%2C+D">Debosmita Pathak</a>, <a href="/search/astro-ph?searchtype=author&query=Rodr%C3%ADguez%2C+M+J">M. Jimena Rodr铆guez</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">Karin Sandstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Sutter%2C+J">Jessica Sutter</a> , et al. (5 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2501.10539v1-abstract-short" style="display: inline;"> We present a comparison of observed polycyclic aromatic hydrocarbon (PAH) feature ratios in 19 nearby galaxies with a grid of theoretical expectations for near- and mid-infrared dust emission. The PAH feature ratios are drawn from Cycle 1 JWST observations and are measured for 7224 stellar clusters and 29176 stellar associations for which we have robust ages and mass estimates from HST five-band p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.10539v1-abstract-full').style.display = 'inline'; document.getElementById('2501.10539v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.10539v1-abstract-full" style="display: none;"> We present a comparison of observed polycyclic aromatic hydrocarbon (PAH) feature ratios in 19 nearby galaxies with a grid of theoretical expectations for near- and mid-infrared dust emission. The PAH feature ratios are drawn from Cycle 1 JWST observations and are measured for 7224 stellar clusters and 29176 stellar associations for which we have robust ages and mass estimates from HST five-band photometry. Though there are galaxy-to-galaxy variations, the observed PAH feature ratios largely agree with the theoretical models, particularly those that are skewed toward more ionized and larger PAH size distributions. For each galaxy we also extract PAH feature ratios for 200 pc-wide circular regions in the diffuse interstellar medium, which serve as a non-cluster/association control sample. Compared to what we find for stellar clusters and associations, the 3.3um/7.7um and 3.3um/11.3um ratios from the diffuse interstellar medium are $\sim 0.10-0.15$ dex smaller. When the observed PAH feature ratios are compared to the radiation field hardness as probed by the [OIII]/H$尾$ ratio, we find anti-correlations for nearly all galaxies in the sample. These results together suggest that the PAH feature ratios are driven by the shape intensity of the radiation field, and that the smallest PAHs -- observed via JWST F335M imaging -- are increasingly 'processed' or destroyed in regions with the most intense and hard radiation fields. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.10539v1-abstract-full').style.display = 'none'; document.getElementById('2501.10539v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">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 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/2501.06303">arXiv:2501.06303</a> <span> [<a href="https://arxiv.org/pdf/2501.06303">pdf</a>, <a href="https://arxiv.org/format/2501.06303">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/staf055">10.1093/mnras/staf055 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> WISDOM Project -- XXII. A 5% precision CO-dynamical supermassive black hole mass measurement in the galaxy NGC 383 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+H">Hengyue Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Bureau%2C+M">Martin Bureau</a>, <a href="/search/astro-ph?searchtype=author&query=Ruffa%2C+I">Ilaria Ruffa</a>, <a href="/search/astro-ph?searchtype=author&query=Cappellari%2C+M">Michele Cappellari</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+A">Timothy A. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Dominiak%2C+P">Pandora Dominiak</a>, <a href="/search/astro-ph?searchtype=author&query=Elford%2C+J+S">Jacob S. Elford</a>, <a href="/search/astro-ph?searchtype=author&query=Iguchi%2C+S">Satoru Iguchi</a>, <a href="/search/astro-ph?searchtype=author&query=Lelli%2C+F">Federico Lelli</a>, <a href="/search/astro-ph?searchtype=author&query=Sarzi%2C+M">Marc Sarzi</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. 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="2501.06303v1-abstract-short" style="display: inline;"> We present a measurement of the supermassive black hole (SMBH) mass of the nearby lenticular galaxy NGC 383, based on Atacama Large Millimeter/sub-millimeter Array (ALMA) observations of the $^{12}$CO(2-1) emission line with an angular resolution of $0.''050\times0.''024$ ($\approx16\times8$ pc$^2$). These observations spatially resolve the nuclear molecular gas disc down to $\approx41,300$ Schwar… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.06303v1-abstract-full').style.display = 'inline'; document.getElementById('2501.06303v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.06303v1-abstract-full" style="display: none;"> We present a measurement of the supermassive black hole (SMBH) mass of the nearby lenticular galaxy NGC 383, based on Atacama Large Millimeter/sub-millimeter Array (ALMA) observations of the $^{12}$CO(2-1) emission line with an angular resolution of $0.''050\times0.''024$ ($\approx16\times8$ pc$^2$). These observations spatially resolve the nuclear molecular gas disc down to $\approx41,300$ Schwarzschild radii and the SMBH sphere of influence by a factor of $\approx24$ radially, better than any other SMBH mass measurement using molecular gas to date. The high resolution enables us to probe material with a maximum circular velocity of $\approx1040$ km/s, even higher than those of the highest-resolution SMBH mass measurements using megamasers. We detect a clear Keplerian increase (from the outside in) of the line-of-sight rotation velocities, a slight offset between the gas disc kinematic (i.e. the position of the SMBH) and morphological (i.e. the centre of the molecular gas emission) centres, an asymmetry of the innermost rotation velocity peaks and evidence for a mild position angle warp and/or non-circular motions within the central $\approx0.''3$. By forward modelling the mass distribution and ALMA data cube, we infer a SMBH mass of $(3.58\pm0.19)\times10^9$ M$_\odot$ ($1蟽$ confidence interval), more precise ($5\%$) but consistent within $\approx1.4蟽$ with the previous measurement using lower-resolution molecular gas data. Our measurement emphasises the importance of high spatial resolution observations for precise SMBH mass determinations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.06303v1-abstract-full').style.display = 'none'; document.getElementById('2501.06303v1-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">17 pages, 12 figures. Accepted by MNRAS on January 10th</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.10506">arXiv:2412.10506</a> <span> [<a href="https://arxiv.org/pdf/2412.10506">pdf</a>, <a href="https://arxiv.org/format/2412.10506">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202453208">10.1051/0004-6361/202453208 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Dense gas scaling relations at kiloparsec scales across nearby galaxies with the ALMA ALMOND and IRAM 30m EMPIRE surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Neumann%2C+L">Lukas Neumann</a>, <a href="/search/astro-ph?searchtype=author&query=Jimenez-Donaire%2C+M+J">Maria J. Jimenez-Donaire</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=Bigiel%2C+F">Frank Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Usero%2C+A">Antonio Usero</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+J">Jiayi Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Querejeta%2C+M">Miguel Querejeta</a>, <a href="/search/astro-ph?searchtype=author&query=Stuber%2C+S+K">Sophia K. Stuber</a>, <a href="/search/astro-ph?searchtype=author&query=Beslic%2C+I">Ivana Beslic</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A">Ashley Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Brok%2C+J+d">Jakob den Brok</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Y">Yixian Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Eibensteiner%2C+C">Cosima Eibensteiner</a>, <a href="/search/astro-ph?searchtype=author&query=He%2C+H">Hao He</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R+S">Ralf S. Klessen</a>, <a href="/search/astro-ph?searchtype=author&query=Liang%2C+F">Fu-Heng Liang</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">Daizhong Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+H">Hsi-An Pan</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. 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="2412.10506v3-abstract-short" style="display: inline;"> Dense, cold gas is the key ingredient for star formation. Over the last two decades, HCN(1-0) emission has been utilised as the most accessible dense gas tracer to study external galaxies. We present new measurements tracing the relationship between dense gas tracers, bulk molecular gas tracers, and star formation in the ALMA ALMOND survey, the largest sample of resolved (1-2 kpc resolution) HCN m… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.10506v3-abstract-full').style.display = 'inline'; document.getElementById('2412.10506v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.10506v3-abstract-full" style="display: none;"> Dense, cold gas is the key ingredient for star formation. Over the last two decades, HCN(1-0) emission has been utilised as the most accessible dense gas tracer to study external galaxies. We present new measurements tracing the relationship between dense gas tracers, bulk molecular gas tracers, and star formation in the ALMA ALMOND survey, the largest sample of resolved (1-2 kpc resolution) HCN maps of galaxies in the local universe (d < 25 Mpc). We measure HCN/CO, a line ratio sensitive to the physical density distribution, and SFR/HCN, a proxy for the dense gas star formation efficiency, as a function of molecular gas surface density, stellar mass surface density, and dynamical equilibrium pressure across 31 galaxies, increasing the number of galaxies by a factor of > 3 over the previous largest such study (EMPIRE). HCN/CO increases (slope of ~ 0.5 and scatter of ~ 0.2 dex), while SFR/HCN decreases (slope of ~ -0.6 and scatter of ~ 0.4 dex) with increasing molecular gas surface density, stellar mass surface density and pressure. Galaxy centres with high stellar mass surface density show a factor of a few higher HCN/CO and lower SFR/HCN compared to the disc average, but both environments follow the same average trend. Our results emphasise that molecular gas properties vary systematically with the galactic environment and demonstrate that the scatter in the Gao-Solomon relation (SFR against HCN) is of physical origin. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.10506v3-abstract-full').style.display = 'none'; document.getElementById('2412.10506v3-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 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, 3 figures. Accepted for publication in Astronomy & Astrophysics Letters (update after language checks)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 693, L13 (2025) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.07862">arXiv:2412.07862</a> <span> [<a href="https://arxiv.org/pdf/2412.07862">pdf</a>, <a href="https://arxiv.org/format/2412.07862">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"> Tracing the earliest stages of star and cluster formation in 19 nearby galaxies with PHANGS-JWST and HST: compact 3.3 $渭$m PAH emitters and their relation to the optical census of star clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rodr%C3%ADguez%2C+M+J">M. Jimena Rodr铆guez</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J+C">Janice C. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Indebetouw%2C+R">Remy Indebetouw</a>, <a href="/search/astro-ph?searchtype=author&query=Whitmore%2C+B+C">B. C. Whitmore</a>, <a href="/search/astro-ph?searchtype=author&query=Maschmann%2C+D">Daniel Maschmann</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=Chandar%2C+R">Rupali Chandar</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A+T">A. T. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Gnedin%2C+O+Y">Oleg Y. Gnedin</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=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+J">Jiayi Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R+S">Ralf S. Klessen</a>, <a href="/search/astro-ph?searchtype=author&query=Groves%2C+B">Brent Groves</a>, <a href="/search/astro-ph?searchtype=author&query=Wofford%2C+A">Aida Wofford</a>, <a href="/search/astro-ph?searchtype=author&query=Boquien%2C+M">M茅d茅ric Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">Daniel A. Dale</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=Thilker%2C+D+A">David A. Thilker</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+H">Hwihyun Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Levy%2C+R+C">Rebecca C. Levy</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=Ubeda%2C+L">Leonardo Ubeda</a>, <a href="/search/astro-ph?searchtype=author&query=Larson%2C+K+L">Kirsten L. Larson</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+K+E">Kelsey E. Johnson</a> , et al. (3 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.07862v1-abstract-short" style="display: inline;"> The earliest stages of star and cluster formation are hidden within dense cocoons of gas and dust, limiting their detection at optical wavelengths. With the unprecedented infrared capabilities of JWST, we can now observe dust-enshrouded star formation with $\sim$10 pc resolution out to $\sim$20 Mpc. Early findings from PHANGS-JWST suggest that 3.3 $渭$m polycyclic aromatic hydrocarbon (PAH) emissio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.07862v1-abstract-full').style.display = 'inline'; document.getElementById('2412.07862v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.07862v1-abstract-full" style="display: none;"> The earliest stages of star and cluster formation are hidden within dense cocoons of gas and dust, limiting their detection at optical wavelengths. With the unprecedented infrared capabilities of JWST, we can now observe dust-enshrouded star formation with $\sim$10 pc resolution out to $\sim$20 Mpc. Early findings from PHANGS-JWST suggest that 3.3 $渭$m polycyclic aromatic hydrocarbon (PAH) emission can identify star clusters in their dust-embedded phases. Here, we extend this analysis to 19 galaxies from the PHANGS-JWST Cycle 1 Treasury Survey, providing the first characterization of compact sources exhibiting 3.3$渭$m PAH emission across a diverse sample of nearby star-forming galaxies. We establish selection criteria, a median color threshold of F300M-F335M=0.67 at F335M=20, and identify of 1816 sources. These sources are predominantly located in dust lanes, spiral arms, rings, and galaxy centers, with $\sim$87% showing concentration indices similar to optically detected star clusters. Comparison with the PHANGS-HST catalogs suggests that PAH emission fades within $\sim$3 Myr. The H$伪$ equivalent width of PAH emitters is 1-2.8 times higher than that of young PHANGS-HST clusters, providing evidence that PAH emitters are on average younger. Analysis of the bright portions of luminosity functions (which should not suffer from incompleteness) shows that young dusty clusters may increase the number of optically visible $\leq$ 3 Myr-old clusters in PHANGS-HST by a factor between $\sim$1.8x-8.5x. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.07862v1-abstract-full').style.display = 'none'; document.getElementById('2412.07862v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.03954">arXiv:2412.03954</a> <span> [<a href="https://arxiv.org/pdf/2412.03954">pdf</a>, <a href="https://arxiv.org/format/2412.03954">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stae2697">10.1093/mnras/stae2697 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CO-to-H$_2$ conversion factor and grain size distribution through the analysis of $伪_\mathrm{CO}$-$q_\mathrm{PAH}$ relation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chiang%2C+I">I-Da Chiang</a>, <a href="/search/astro-ph?searchtype=author&query=Hirashita%2C+H">Hiroyuki Hirashita</a>, <a href="/search/astro-ph?searchtype=author&query=Chastenet%2C+J">Jeremy Chastenet</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=Koch%2C+E+W">Eric W. Koch</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=Teng%2C+Y">Yu-Hsuan Teng</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. 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="2412.03954v1-abstract-short" style="display: inline;"> The CO-to-H$_2$ conversion factor ($伪_\mathrm{CO}$) is expected to vary with dust abundance and grain size distribution through the efficiency of shielding gas from CO-dissociation radiation. We present a comprehensive analysis of $伪_\mathrm{CO}$ and grain size distribution for nearby galaxies, using the PAH fraction ($q_\mathrm{PAH}$) as an observable proxy of grain size distribution. We adopt th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.03954v1-abstract-full').style.display = 'inline'; document.getElementById('2412.03954v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.03954v1-abstract-full" style="display: none;"> The CO-to-H$_2$ conversion factor ($伪_\mathrm{CO}$) is expected to vary with dust abundance and grain size distribution through the efficiency of shielding gas from CO-dissociation radiation. We present a comprehensive analysis of $伪_\mathrm{CO}$ and grain size distribution for nearby galaxies, using the PAH fraction ($q_\mathrm{PAH}$) as an observable proxy of grain size distribution. We adopt the resolved observations at 2-kpc resolution in 42 nearby galaxies, where $伪_\mathrm{CO}$ is derived from measured metallicity and surface densities of dust and HI assuming a fixed dust-to-metals ratio. We use an analytical model for the evolution of H$_2$ and CO, in which the evolution of grain size distribution is controlled by the dense gas fraction ($畏$). We find that the observed level of $q_\mathrm{PAH}$ is consistent with the diffuse-gas-dominated model ($畏=0.2$) where dust shattering is more efficient. Meanwhile, the slight decreasing trend of observed $q_\mathrm{PAH}$ with metallicity is more consistent with high-$畏$ predictions, likely due to the more efficient loss of PAHs by coagulation. We discuss how grain size distribution (indicated by $q_\mathrm{PAH}$) and metallicity impact $伪_\mathrm{CO}$; we however did not obtain conclusive evidence that the grain size distribution affects $伪_\mathrm{CO}$. Observations and model predictions show similar anti-correlation between $伪_\mathrm{CO}$ and 12+log(O/H). Meanwhile, there is a considerable difference in how resolved $伪_\mathrm{CO}$ behaves with $q_\mathrm{PAH}$. The observed $伪_\mathrm{CO}$ has a positive correlation with $q_\mathrm{PAH}$, while the model-predicted $伪_\mathrm{CO}$ does not have a definite correlation with $q_\mathrm{PAH}$. This difference is likely due to the limitation of one-zone treatment in the model. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.03954v1-abstract-full').style.display = 'none'; document.getElementById('2412.03954v1-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 7 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.21399">arXiv:2410.21399</a> <span> [<a href="https://arxiv.org/pdf/2410.21399">pdf</a>, <a href="https://arxiv.org/format/2410.21399">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"> CO isotopologue-derived molecular gas conditions and CO-to-H$_2$ conversion factors in M51 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Brok%2C+J+d">Jakob den Brok</a>, <a href="/search/astro-ph?searchtype=author&query=Jim%C3%A9nez-Donaire%2C+M+J">Mar铆a J. Jim茅nez-Donaire</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A">Adam Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">Frank Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Pety%2C+J">J茅r么me Pety</a>, <a href="/search/astro-ph?searchtype=author&query=Petitpas%2C+G">Glen Petitpas</a>, <a href="/search/astro-ph?searchtype=author&query=Usero%2C+A">Antonio Usero</a>, <a href="/search/astro-ph?searchtype=author&query=Teng%2C+Y">Yu-Hsuan Teng</a>, <a href="/search/astro-ph?searchtype=author&query=Humire%2C+P">Pedro Humire</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=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Sandstrom%2C+K">Karin Sandstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">Daizhong Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+Q">Qizhou Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Stuber%2C+S">Sophia Stuber</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">M茅lanie Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">Daniel A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Eibensteiner%2C+C">Cosima Eibensteiner</a>, <a href="/search/astro-ph?searchtype=author&query=Gali%C4%87%2C+I">Ina Gali膰</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S+C+O">Simon C. O. Glover</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+H">Hsi-An Pan</a>, <a href="/search/astro-ph?searchtype=author&query=Querejeta%2C+M">Miguel Querejeta</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+R+J">Rowan J. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. Williams</a> , et al. (2 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.21399v1-abstract-short" style="display: inline;"> Over the past decade, several millimeter interferometer programs have mapped the nearby star-forming galaxy M51 at a spatial resolution of ${\le}170$ pc. This study combines observations from three major programs: the PdBI Arcsecond Whirlpool Survey (PAWS), the SMA M51 large program (SMA-PAWS), and the Surveying the Whirlpool at Arcseconds with NOEMA (SWAN). The dataset includes the (1-0) and (2-1… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.21399v1-abstract-full').style.display = 'inline'; document.getElementById('2410.21399v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.21399v1-abstract-full" style="display: none;"> Over the past decade, several millimeter interferometer programs have mapped the nearby star-forming galaxy M51 at a spatial resolution of ${\le}170$ pc. This study combines observations from three major programs: the PdBI Arcsecond Whirlpool Survey (PAWS), the SMA M51 large program (SMA-PAWS), and the Surveying the Whirlpool at Arcseconds with NOEMA (SWAN). The dataset includes the (1-0) and (2-1) rotational transitions of $^{12}$CO, $^{13}$CO, and C$^{18}$O isotopologues. The observations cover the $r{<}\rm 3\,kpc$ region including center and part of the disk, thereby ensuring strong detections of the weaker $^{13}$CO and C$^{18}$O lines. All observations are convolved in this analysis to an angular resolution of 4$''$, corresponding to a physical scale of ${\sim}$170 pc. We investigate empirical line ratio relations and quantitatively evaluate molecular gas conditions such as temperature, density, and the CO-to-H$_2$ conversion factor ($伪_{\rm CO}$). We employ two approaches to study the molecular gas conditions: (i) assuming local thermal equilibrium (LTE) to analytically determine the CO column density and $伪_{\rm CO}$, and (ii) using non-LTE modeling with RADEX to fit physical conditions to observed CO isotopologue intensities. We find that the $伪_{\rm CO}$ values {in the center and along the inner spiral arm} are $\sim$0.5 dex (LTE) and ${\sim}$0.1 dex (non-LTE) below the Milky Way inner disk value. The average non-LTE $伪_{\rm CO}$ is $2.4{\pm}0.5$ M$_\odot$ pc$^{-2}$ (K km s$^{-1}$)$^{-1}$. While both methods show dispersion due to underlying assumptions, the scatter is larger for LTE-derived values. This study underscores the necessity for robust CO line modeling to accurately constrain the molecular ISM's physical and chemical conditions in nearby galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.21399v1-abstract-full').style.display = 'none'; document.getElementById('2410.21399v1-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 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">accepted for publication in AJ; 31 pages, 16 figures, 7 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.16370">arXiv:2410.16370</a> <span> [<a href="https://arxiv.org/pdf/2410.16370">pdf</a>, <a href="https://arxiv.org/format/2410.16370">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202451934">10.1051/0004-6361/202451934 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Machine learning the gap between real and simulated nebulae: A domain-adaptation approach to classify ionised nebulae in nearby galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Belfiore%2C+F">Francesco Belfiore</a>, <a href="/search/astro-ph?searchtype=author&query=Ginolfi%2C+M">Michele Ginolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Blanc%2C+G">Guillermo Blanc</a>, <a href="/search/astro-ph?searchtype=author&query=Boquien%2C+M">Mederic Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">Melanie Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Congiu%2C+E">Enrico Congiu</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S+C+O">Simon C. O. Glover</a>, <a href="/search/astro-ph?searchtype=author&query=Groves%2C+B">Brent Groves</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R+S">Ralf S. Klessen</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%A9ndez-Delgado%2C+E">Eduardo M茅ndez-Delgado</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. 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="2410.16370v2-abstract-short" style="display: inline;"> Classifying ionised nebulae in nearby galaxies is crucial to studying stellar feedback mechanisms and understanding the physical conditions of the interstellar medium. This classification task is generally performed by comparing observed line ratios with photoionisation simulations of different types of nebulae (HII regions, planetary nebulae, and supernova remnants). However, due to simplifying a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.16370v2-abstract-full').style.display = 'inline'; document.getElementById('2410.16370v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.16370v2-abstract-full" style="display: none;"> Classifying ionised nebulae in nearby galaxies is crucial to studying stellar feedback mechanisms and understanding the physical conditions of the interstellar medium. This classification task is generally performed by comparing observed line ratios with photoionisation simulations of different types of nebulae (HII regions, planetary nebulae, and supernova remnants). However, due to simplifying assumptions, such simulations are generally unable to fully reproduce the line ratios in observed nebulae. This discrepancy limits the performance of the classical machine-learning approach, where a model is trained on the simulated data and then used to classify real nebulae. For this study, we used a domain-adversarial neural network (DANN) to bridge the gap between photoionisation models (source domain) and observed ionised nebulae from the PHANGS-MUSE survey (target domain). The DANN is an example of a domain-adaptation algorithm, whose goal is to maximise the performance of a model trained on labelled data in the source domain on an unlabelled target domain by extracting domain-invariant features. Our results indicate a significant improvement in classification performance in the target domain when employing the DANN framework compared to a classical neural network (NN) classifier. Additionally, we investigated the impact of adding noise to the source dataset, finding that noise injection acts as a form of regularisation, further enhancing the performances of both the NN and DANN models on the observational data. The combined use of domain adaptation and noise injection improved the classification accuracy in the target domain by 23%. This study highlights the potential of domain adaptation methods in tackling the domain-shift challenge when using theoretical models to train machine-learning pipelines in astronomy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.16370v2-abstract-full').style.display = 'none'; document.getElementById('2410.16370v2-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 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 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">Accepted in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 694, A212 (2025) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.13353">arXiv:2410.13353</a> <span> [<a href="https://arxiv.org/pdf/2410.13353">pdf</a>, <a href="https://arxiv.org/format/2410.13353">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"> Dynamical resonances in PHANGS galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ruiz-Garc%C3%ADa%2C+M">Marina Ruiz-Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Querejeta%2C+M">Miguel Querejeta</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Burillo%2C+S">Santiago Garc铆a-Burillo</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Meidt%2C+S+E">Sharon E. Meidt</a>, <a href="/search/astro-ph?searchtype=author&query=Sormani%2C+M+C">Mattia C. Sormani</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</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=Bazzi%2C+Z">Zein Bazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Colombo%2C+D">Dario Colombo</a>, <a href="/search/astro-ph?searchtype=author&query=Gleis%2C+D+R">Damian R. Gleis</a>, <a href="/search/astro-ph?searchtype=author&query=Gnedin%2C+O+Y">Oleg Y. Gnedin</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R+S">Ralf S. Klessen</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=S%C3%A1nchez-Bl%C3%A1zquez%2C+P">Patricia S谩nchez-Bl谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Stuber%2C+S+K">Sophia K. Stuber</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="2410.13353v1-abstract-short" style="display: inline;"> Bars are remarkable stellar structures that can transport gas toward centers and drive the secular evolution of galaxies. In this context, it is important to locate dynamical resonances associated with bars. For this study, we used ${Spitzer}$ near-infrared images as a proxy for the stellar gravitational potential and the ALMA CO(J=2-1) gas distribution from the PHANGS survey to determine the posi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.13353v1-abstract-full').style.display = 'inline'; document.getElementById('2410.13353v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.13353v1-abstract-full" style="display: none;"> Bars are remarkable stellar structures that can transport gas toward centers and drive the secular evolution of galaxies. In this context, it is important to locate dynamical resonances associated with bars. For this study, we used ${Spitzer}$ near-infrared images as a proxy for the stellar gravitational potential and the ALMA CO(J=2-1) gas distribution from the PHANGS survey to determine the position of the main dynamical resonances associated with the bars in the PHANGS sample of 74 nearby star-forming galaxies. We used the gravitational torque method to estimate the location of the bar corotation radius ($R_{\rm CR}$), where stars and gas rotate at the same angular velocity as the bar. Of the 46 barred galaxies in PHANGS, we have successfully determined the corotation (CR) for 38 of them. The mean ratio of the $R_{\rm CR}$ to the bar radius ($R_{\rm bar}$) is $\mathcal{R} = R_{\rm CR}/R_{\rm bar} = 1.12$, with a standard deviation of $0.39$. This is consistent with the average value expected from theory and suggests that bars are predominantly fast. We also compared our results with other bar CR measurements from the literature, which employ different methods, and find good agreement ($蟻= 0.64$). Finally, using rotation curves, we have estimated other relevant resonances such as the inner Lindblad resonance (ILR) and the outer Lindblad resonance (OLR), which are often associated with rings. This work provides a useful catalog of resonances for a large sample of nearby galaxies and emphasizes the clear connection between bar dynamics and morphology. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.13353v1-abstract-full').style.display = 'none'; document.getElementById('2410.13353v1-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.11821">arXiv:2410.11821</a> <span> [<a href="https://arxiv.org/pdf/2410.11821">pdf</a>, <a href="https://arxiv.org/format/2410.11821">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> A First-look at Spatially-resolved Infrared Supernova Remnants in M33 with JWST </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sarbadhicary%2C+S+K">Sumit K. Sarbadhicary</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</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=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=Peltonen%2C+J">Joshua Peltonen</a>, <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=Glover%2C+S+C+O">Simon C. O. Glover</a>, <a href="/search/astro-ph?searchtype=author&query=Lazzarini%2C+M">Margaret Lazzarini</a>, <a href="/search/astro-ph?searchtype=author&query=Chown%2C+R">Ryan Chown</a>, <a href="/search/astro-ph?searchtype=author&query=Meyer%2C+J+D">Jennifer Donovan Meyer</a>, <a href="/search/astro-ph?searchtype=author&query=Sandstrom%2C+K">Karin Sandstrom</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=Tarantino%2C+E">Elizabeth Tarantino</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="2410.11821v1-abstract-short" style="display: inline;"> We present the first spatially-resolved infrared images of supernova remnants (SNRs) in M33 with the unprecedented sensitivity and resolution of JWST. We analyze 43 SNRs in four JWST fields: two covering central and southern M33 with separate NIRCam (F335M, F444W) and MIRI (F560W, F2100W) observations, one $\sim$5 kpc-long radial strip observed with MIRI F770W, and one covering the giant HII regio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.11821v1-abstract-full').style.display = 'inline'; document.getElementById('2410.11821v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.11821v1-abstract-full" style="display: none;"> We present the first spatially-resolved infrared images of supernova remnants (SNRs) in M33 with the unprecedented sensitivity and resolution of JWST. We analyze 43 SNRs in four JWST fields: two covering central and southern M33 with separate NIRCam (F335M, F444W) and MIRI (F560W, F2100W) observations, one $\sim$5 kpc-long radial strip observed with MIRI F770W, and one covering the giant HII region NGC 604 with multiple NIRCam and MIRI broad/narrowband filters. Of the 21 SNRs in the MIRI field, we found three clear detections (i.e., identical infrared and \ha morphologies), and six partial-detections, implying a detection fraction of 43\% in these bands. In contrast, only one SNR (out of 16) is detectable in the NIRCam field. One of the SNRs, L10-080, is a potential candidate for having freshly-formed ejecta dust, based on its size and centrally-concentrated 21 \mum emission. Two SNRs near NGC 604 have strong evidence of molecular (H$_2$) emission at 4.7 \mum, making them the farthest known SNRs with visible molecular shocks. Five SNRs have F770W observations, with the smaller younger objects showing tentative signs of emission, while the older, larger ones have voids. Multi-wavelength data indicate that the clearly-detected SNRs are also among the smallest, brightest at other wavelengths (\ha, radio and X-ray), have the broadest line widths (H$伪$ FWHM$\sim$250-350 km/s), and the densest environments. No strong correlation with star-formation histories are seen, with the clearly-detected SNRs having both high-mass ($\sim$35 \Msun) and low-mass ($\lesssim$10 \Msun) progenitors. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.11821v1-abstract-full').style.display = 'none'; document.getElementById('2410.11821v1-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">33 pages, 17 figures, 2 tables, submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.05397">arXiv:2410.05397</a> <span> [<a href="https://arxiv.org/pdf/2410.05397">pdf</a>, <a href="https://arxiv.org/format/2410.05397">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"> Polycyclic Aromatic Hydrocarbon and CO(2-1) Emission at 50-150 pc Scales in 66 Nearby Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chown%2C+R">Ryan Chown</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=Sandstrom%2C+K">Karin Sandstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Chastenet%2C+J">Jeremy Chastenet</a>, <a href="/search/astro-ph?searchtype=author&query=Sutter%2C+J">Jessica Sutter</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=Koziol%2C+H+B">Hannah B. Koziol</a>, <a href="/search/astro-ph?searchtype=author&query=Neumann%2C+L">Lukas Neumann</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+J">Jiayi Sun</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=Baron%2C+D">Dalya Baron</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=Barnes%2C+A+T">Ashley T. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Bazzi%2C+Z">Zein Bazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Belfiore%2C+F">Francesco Belfiore</a>, <a href="/search/astro-ph?searchtype=author&query=Bolatto%2C+A">Alberto Bolatto</a>, <a href="/search/astro-ph?searchtype=author&query=Boquien%2C+M">Mederic Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Y">Yixian Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">Melanie Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Colombo%2C+D">Dario Colombo</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">Daniel A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Egorov%2C+O+V">Oleg V. Egorov</a>, <a href="/search/astro-ph?searchtype=author&query=Eibensteiner%2C+C">Cosima Eibensteiner</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Hassani%2C+H">Hamid Hassani</a> , et al. (14 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.05397v1-abstract-short" style="display: inline;"> Combining Atacama Large Millimeter/sub-millimeter Array CO(2-1) mapping and JWST near- and mid-infrared imaging, we characterize the relationship between CO(2-1) and polycyclic aromatic hydrocarbon (PAH) emission at ~100 pc resolution in 66 nearby star-forming galaxies, expanding the sample size from previous ~100 pc resolution studies by more than an order of magnitude. Focusing on regions of gal… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.05397v1-abstract-full').style.display = 'inline'; document.getElementById('2410.05397v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.05397v1-abstract-full" style="display: none;"> Combining Atacama Large Millimeter/sub-millimeter Array CO(2-1) mapping and JWST near- and mid-infrared imaging, we characterize the relationship between CO(2-1) and polycyclic aromatic hydrocarbon (PAH) emission at ~100 pc resolution in 66 nearby star-forming galaxies, expanding the sample size from previous ~100 pc resolution studies by more than an order of magnitude. Focusing on regions of galaxies where most of the gas is likely to be molecular, we find strong correlations between CO(2-1) and 3.3 micron, 7.7 micron, and 11.3 micron PAH emission, estimated from JWST's F335M, F770W, and F1130W filters. We derive power law relations between CO(2-1) and PAH emission, which have indices in the range 0.8-1.2, implying relatively weak variations in the observed CO-to-PAH ratios across the regions that we study. We find that CO-to-PAH ratios and scaling relationships near HII regions are similar to those in diffuse sight lines. The main difference between the two types of regions is that sight lines near HII regions show higher intensities in all tracers. Galaxy centers, on the other hand, show higher overall intensities and enhanced CO-to-PAH ratios compared to galaxy disks. Individual galaxies show 0.19 dex scatter in the normalization of CO at fixed I_PAH and this normalization anti-correlates with specific star formation rate (SFR/M*) and correlates with stellar mass. We provide a prescription that accounts for these galaxy-to-galaxy variations and represents our best current empirical predictor to estimate CO(2-1) intensity from PAH emission, which allows one to take advantage of JWST's excellent sensitivity and resolution to trace cold gas. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.05397v1-abstract-full').style.display = 'none'; document.getElementById('2410.05397v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 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">21 pages, 4 figures, 3 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/2410.03835">arXiv:2410.03835</a> <span> [<a href="https://arxiv.org/pdf/2410.03835">pdf</a>, <a href="https://arxiv.org/format/2410.03835">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 Resolved Behavior of Dust Mass, Polycyclic Aromatic Hydrocarbon Fraction, and Radiation Field in ~ 800 Nearby Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chastenet%2C+J">J茅r茅my Chastenet</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=Leroy%2C+A+K">Adam K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Bot%2C+C">Caroline Bot</a>, <a href="/search/astro-ph?searchtype=author&query=Chiang%2C+I">I-Da Chiang</a>, <a href="/search/astro-ph?searchtype=author&query=Chown%2C+R">Ryan Chown</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=Koch%2C+E+W">Eric W. Koch</a>, <a href="/search/astro-ph?searchtype=author&query=Roussel%2C+H">H茅l猫ne Roussel</a>, <a href="/search/astro-ph?searchtype=author&query=Sutter%2C+J">Jessica Sutter</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. 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="2410.03835v1-abstract-short" style="display: inline;"> We present resolved $3.6-250~渭$m dust spectral energy distribution (SED) fitting for $\sim 800$ nearby galaxies. We measure the distribution of radiation field intensities heating the dust, the dust mass surface density ($危_{\rm d}$), and the fraction of dust in the form of polycyclic aromatic hydrocarbons (PAHs; $q_{\rm PAH}$). We find that the average interstellar radiation field (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.03835v1-abstract-full').style.display = 'inline'; document.getElementById('2410.03835v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.03835v1-abstract-full" style="display: none;"> We present resolved $3.6-250~渭$m dust spectral energy distribution (SED) fitting for $\sim 800$ nearby galaxies. We measure the distribution of radiation field intensities heating the dust, the dust mass surface density ($危_{\rm d}$), and the fraction of dust in the form of polycyclic aromatic hydrocarbons (PAHs; $q_{\rm PAH}$). We find that the average interstellar radiation field ($\overline{U}$) is correlated both with stellar mass surface density ($危_{\star}$) and star formation rate surface density ($危_{\rm SFR}$), while more intense radiation fields are only correlated with $危_{\rm SFR}$. We show that $q_{\rm PAH}$ is a steeply decreasing function of $危_{\rm SFR}$, likely reflecting PAH destruction in H II regions. Galaxy integrated $q_{\rm PAH}$ is strongly, negatively correlated with specific star formation rate (sSFR) and offset from the star-forming ``main sequence'' ($螖$MS), suggesting that both metallicity and star formation intensity play a role in setting the global $q_{\rm PAH}$. We also find a nearly constant M$_{\rm d}$/M$_\star$ ratio for galaxies on the main sequence, with a lower ratio for more quiescent galaxies, likely due to their lower gas fractions. From these results, we construct prescriptions to estimate the radiation field distribution in both integrated and resolved galaxies. We test these prescriptions by comparing our predicted $\overline{U}$ to results of SED fitting for stacked "main sequence" galaxies at $0<z<4$ from B茅thermin et al. (2015) and find sSFR is an accurate predictor of $\overline{U}$ even at these high redshifts. Finally, we describe the public delivery of matched-resolution WISE and Herschel maps along with the resolved dust SED fitting results through the InfraRed Science Archive (IRSA). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.03835v1-abstract-full').style.display = 'none'; document.getElementById('2410.03835v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted in ApJS; 38 pages, 15 figures + 2 Appendices. The data will be hosted at IPAC under DOI https://www.ipac.caltech.edu/doi/10.26131/IRSA581. The link to the delivery https://irsa.ipac.caltech.edu/data/Herschel/z0MGS_Dust/overview.html will be online soon!</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.00106">arXiv:2410.00106</a> <span> [<a href="https://arxiv.org/pdf/2410.00106">pdf</a>, <a href="https://arxiv.org/format/2410.00106">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202451007">10.1051/0004-6361/202451007 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Metallicity calibrations based on auroral lines from PHANGS-MUSE data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Brazzini%2C+M">Matilde Brazzini</a>, <a href="/search/astro-ph?searchtype=author&query=Belfiore%2C+F">Francesco Belfiore</a>, <a href="/search/astro-ph?searchtype=author&query=Ginolfi%2C+M">Michele Ginolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Groves%2C+B">Brent Groves</a>, <a href="/search/astro-ph?searchtype=author&query=Kreckel%2C+K">Kathryn Kreckel</a>, <a href="/search/astro-ph?searchtype=author&query=Vaught%2C+R+J+R">Ryan J. Rickards Vaught</a>, <a href="/search/astro-ph?searchtype=author&query=Baron%2C+D">Dalya Baron</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">Frank Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Blanc%2C+G+A">Guillermo A. Blanc</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">Daniel A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Grasha%2C+K">Kathryn Grasha</a>, <a href="/search/astro-ph?searchtype=author&query=Habjan%2C+E">Eric Habjan</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R+S">Ralf S. Klessen</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%A9ndez-Delgado%2C+J+E">J. Eduardo M茅ndez-Delgado</a>, <a href="/search/astro-ph?searchtype=author&query=Sandstrom%2C+K">Karin Sandstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. 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="2410.00106v1-abstract-short" style="display: inline;"> We present a chemical analysis of selected HII regions from the PHANGS-MUSE nebular catalogue. Our intent is to empirically re-calibrate strong-line diagnostics of gas-phase metallicity, applicable across a wide range of metallicities within nearby star-forming galaxies. To ensure reliable measurements of auroral line fluxes, we carried out a new spectral fitting procedure whereby only restricted… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.00106v1-abstract-full').style.display = 'inline'; document.getElementById('2410.00106v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.00106v1-abstract-full" style="display: none;"> We present a chemical analysis of selected HII regions from the PHANGS-MUSE nebular catalogue. Our intent is to empirically re-calibrate strong-line diagnostics of gas-phase metallicity, applicable across a wide range of metallicities within nearby star-forming galaxies. To ensure reliable measurements of auroral line fluxes, we carried out a new spectral fitting procedure whereby only restricted wavelength regions around the emission lines of interest are taken into account: this assures a better fit for the stellar continuum. No prior cuts to nebulae luminosity were applied to limit biases in auroral line detections. Ionic abundances of O+, O++, N+, S+, and S++ were estimated by applying the direct method. We integrated the selected PHANGS-MUSE sample with other existing auroral line catalogues, appropriately re-analysed to obtain a homogeneous dataset. This was used to derive strong-line diagnostic calibrations that span from 12+log(O/H) = 7.5 to 8.8. We investigate their dependence on the ionisation parameter and conclude that it is likely the primary cause of the significant scatter observed in these diagnostics. We apply our newly calibrated strong-line diagnostics to the total sample of HII regions from the PHANGS-MUSE nebular catalogue, and we exploit these indirect metallicity estimates to study the radial metallicity gradient within each of the 19 galaxies of the sample. We compare our results with the literature and find good agreement, validating our procedure and findings. With this paper, we release the full catalogue of auroral and nebular line fluxes for the selected HII regions from the PHANGS-MUSE nebular catalogue. This is the first catalogue of direct chemical abundance measurements carried out with PHANGS-MUSE data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.00106v1-abstract-full').style.display = 'none'; document.getElementById('2410.00106v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <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, 14 figures, 6 tables; accepted for publication in Astronomy & Astrophysics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.03835">arXiv:2409.03835</a> <span> [<a href="https://arxiv.org/pdf/2409.03835">pdf</a>, <a href="https://arxiv.org/format/2409.03835">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"> McFine: python-based Monte-Carlo multi-component hyperfine structure fitting </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Watkins%2C+E+J">Elizabeth J. Watkins</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="2409.03835v2-abstract-short" style="display: inline;"> Modelling complex line emission in the interstellar medium (ISM) is a degenerate, high-dimensional problem. Here, we present McFine, a tool for automated multi-component fitting of emission lines with complex hyperfine structure, in a fully automated way. We use Markov chain Monte Carlo (MCMC) to efficiently explore the complex parameter space, allowing for characterising model denegeracies. This… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.03835v2-abstract-full').style.display = 'inline'; document.getElementById('2409.03835v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.03835v2-abstract-full" style="display: none;"> Modelling complex line emission in the interstellar medium (ISM) is a degenerate, high-dimensional problem. Here, we present McFine, a tool for automated multi-component fitting of emission lines with complex hyperfine structure, in a fully automated way. We use Markov chain Monte Carlo (MCMC) to efficiently explore the complex parameter space, allowing for characterising model denegeracies. This tool allows for both local thermodynamic equilibrium (LTE) and radiative-transfer (RT) models. McFine can fit individual spectra and data cubes, and for cubes encourage spatial coherence between neighbouring pixels. It is also built to fit the minimum number of distinct components, to avoid overfitting. We have carried out tests on synthetic spectra, where in around 90~per~cent of cases it fits the correct number of components, otherwise slightly fewer components. Typically, $T_{\rm ex}$ is overestimated and $蟿$ underestimated, but accurate within the estimated uncertainties. The velocity and line widths are recovered with extremely high accuracy, however. We verify McFine by applying to a large Atacama Large Millimeter/submillimeter Array (ALMA) N$_2$H$^+$ mosaic of an high-mass star forming region, G316.75-00.00. We find a similar quality of fit to our synthetic tests, aside from in the active regions forming O-stars, where the assumptions of Gaussian line profiles or LTE may break down. To show the general applicability of this code, we fit CO(J = 2-1) observations of NGC 3627, a nearby star-forming galaxy, again obtaining excellent fit quality. McFine provides a fully automated way to analyse rich datasets from interferometric observations, is open source, and pip-installable. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.03835v2-abstract-full').style.display = 'none'; document.getElementById('2409.03835v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 2 Appendices, 22 Figures (7 in Appendices), 1 Table. Accepted to 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/2408.12975">arXiv:2408.12975</a> <span> [<a href="https://arxiv.org/pdf/2408.12975">pdf</a>, <a href="https://arxiv.org/format/2408.12975">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> </div> </div> <p class="title is-5 mathjax"> The UK Submillimetre and Millimetre Astronomy Roadmap 2024 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pattle%2C+K">K. Pattle</a>, <a href="/search/astro-ph?searchtype=author&query=Barry%2C+P+S">P. S. Barry</a>, <a href="/search/astro-ph?searchtype=author&query=Blain%2C+A+W">A. W. Blain</a>, <a href="/search/astro-ph?searchtype=author&query=Booth%2C+M">M. Booth</a>, <a href="/search/astro-ph?searchtype=author&query=Booth%2C+R+A">R. A. Booth</a>, <a href="/search/astro-ph?searchtype=author&query=Clements%2C+D+L">D. L. Clements</a>, <a href="/search/astro-ph?searchtype=author&query=Currie%2C+M+J">M. J. Currie</a>, <a href="/search/astro-ph?searchtype=author&query=Doyle%2C+S">S. Doyle</a>, <a href="/search/astro-ph?searchtype=author&query=Eden%2C+D">D. Eden</a>, <a href="/search/astro-ph?searchtype=author&query=Fuller%2C+G+A">G. A. Fuller</a>, <a href="/search/astro-ph?searchtype=author&query=Griffin%2C+M">M. Griffin</a>, <a href="/search/astro-ph?searchtype=author&query=Huggard%2C+P+G">P. G. Huggard</a>, <a href="/search/astro-ph?searchtype=author&query=Ilee%2C+J+D">J. D. Ilee</a>, <a href="/search/astro-ph?searchtype=author&query=Karoly%2C+J">J. Karoly</a>, <a href="/search/astro-ph?searchtype=author&query=Khan%2C+Z+A">Z. A. Khan</a>, <a href="/search/astro-ph?searchtype=author&query=Klimovich%2C+N">N. Klimovich</a>, <a href="/search/astro-ph?searchtype=author&query=Kontar%2C+E">E. Kontar</a>, <a href="/search/astro-ph?searchtype=author&query=Klaassen%2C+P">P. Klaassen</a>, <a href="/search/astro-ph?searchtype=author&query=Rigby%2C+A+J">A. J. Rigby</a>, <a href="/search/astro-ph?searchtype=author&query=Scicluna%2C+P">P. Scicluna</a>, <a href="/search/astro-ph?searchtype=author&query=Serjeant%2C+S">S. Serjeant</a>, <a href="/search/astro-ph?searchtype=author&query=Tan%2C+B+-">B. -K. Tan</a>, <a href="/search/astro-ph?searchtype=author&query=Ward-Thompson%2C+D">D. Ward-Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">T. G. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+A">T. A. Davis</a> , et al. (9 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.12975v3-abstract-short" style="display: inline;"> In this Roadmap, we present a vision for the future of submillimetre and millimetre astronomy in the United Kingdom over the next decade and beyond. This Roadmap has been developed in response to the recommendation of the Astronomy Advisory Panel (AAP) of the STFC in the AAP Astronomy Roadmap 2022. In order to develop our stragetic priorities and recommendations, we surveyed the UK submillimetre a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.12975v3-abstract-full').style.display = 'inline'; document.getElementById('2408.12975v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.12975v3-abstract-full" style="display: none;"> In this Roadmap, we present a vision for the future of submillimetre and millimetre astronomy in the United Kingdom over the next decade and beyond. This Roadmap has been developed in response to the recommendation of the Astronomy Advisory Panel (AAP) of the STFC in the AAP Astronomy Roadmap 2022. In order to develop our stragetic priorities and recommendations, we surveyed the UK submillimetre and millimetre community to determine their key priorities for both the near-term and long-term future of the field. We further performed detailed reviews of UK leadership in submillimetre/millimetre science and instrumentation. Our key strategic priorities are as follows: 1. The UK must be a key partner in the forthcoming AtLAST telescope, for which it is essential that the UK remains a key partner in the JCMT in the intermediate term. 2. The UK must maintain, and if possible enhance, access to ALMA and aim to lead parts of instrument development for ALMA2040. Our strategic priorities complement one another: AtLAST (a 50m single-dish telescope) and an upgraded ALMA (a large configurable interferometric array) would be in synergy, not competition, with one another. Both have identified and are working towards the same overarching science goals, and both are required in order to fully address these goals. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.12975v3-abstract-full').style.display = 'none'; document.getElementById('2408.12975v3-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">91 pages plus cover, 38 figures. Submitted to the Science and Technology Facilities Council, August 2024. One figure corrected (v2); new appendix with STFC Q&A; corrected SMA access statement; updated references, acronyms & author list (v3)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.08026">arXiv:2408.08026</a> <span> [<a href="https://arxiv.org/pdf/2408.08026">pdf</a>, <a href="https://arxiv.org/format/2408.08026">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202451033">10.1051/0004-6361/202451033 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> JWST MIRI and NIRCam observations of NGC 891 and its circumgalactic medium </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chastenet%2C+J">J茅r茅my Chastenet</a>, <a href="/search/astro-ph?searchtype=author&query=De+Looze%2C+I">Ilse De Looze</a>, <a href="/search/astro-ph?searchtype=author&query=Rela%C3%B1o%2C+M">Monica Rela帽o</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">Daniel A. Dale</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=Bianchi%2C+S">Simone Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Xilouris%2C+E+M">Emmanuel M. Xilouris</a>, <a href="/search/astro-ph?searchtype=author&query=Baes%2C+M">Maarten Baes</a>, <a href="/search/astro-ph?searchtype=author&query=Bolatto%2C+A+D">Alberto D. Bolatto</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=Casasola%2C+V">Viviana Casasola</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=Fraternali%2C+F">Filippo Fraternali</a>, <a href="/search/astro-ph?searchtype=author&query=Fritz%2C+J">Jacopo Fritz</a>, <a href="/search/astro-ph?searchtype=author&query=Galliano%2C+F">Fr茅d茅ric Galliano</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S+C+O">Simon C. O. Glover</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=Hirashita%2C+H">Hiroyuki Hirashita</a>, <a href="/search/astro-ph?searchtype=author&query=Kennicutt%2C+R">Robert Kennicutt</a>, <a href="/search/astro-ph?searchtype=author&query=Nagamine%2C+K">Kentaro Nagamine</a>, <a href="/search/astro-ph?searchtype=author&query=Kirchschlager%2C+F">Florian Kirchschlager</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R+S">Ralf S. Klessen</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=Levy%2C+R+C">Rebecca C. Levy</a>, <a href="/search/astro-ph?searchtype=author&query=McCallum%2C+L">Lewis McCallum</a> , et al. (15 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.08026v1-abstract-short" style="display: inline;"> We present new JWST observations of the nearby, prototypical edge-on, spiral galaxy NGC 891. The northern half of the disk was observed with NIRCam in its F150W and F277W filters. Absorption is clearly visible in the mid-plane of the F150W image, along with vertical dusty plumes that closely resemble the ones seen in the optical. A $\sim 10 \times 3~{\rm kpc}^2$ area of the lower circumgalactic me… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.08026v1-abstract-full').style.display = 'inline'; document.getElementById('2408.08026v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.08026v1-abstract-full" style="display: none;"> We present new JWST observations of the nearby, prototypical edge-on, spiral galaxy NGC 891. The northern half of the disk was observed with NIRCam in its F150W and F277W filters. Absorption is clearly visible in the mid-plane of the F150W image, along with vertical dusty plumes that closely resemble the ones seen in the optical. A $\sim 10 \times 3~{\rm kpc}^2$ area of the lower circumgalactic medium (CGM) was mapped with MIRI F770W at 12 pc scales. Thanks to the sensitivity and resolution of JWST, we detect dust emission out to $\sim 4$ kpc from the disk, in the form of filaments, arcs, and super-bubbles. Some of these filaments can be traced back to regions with recent star formation activity, suggesting that feedback-driven galactic winds play an important role in regulating baryonic cycling. The presence of dust at these altitudes raises questions about the transport mechanisms at play and suggests that small dust grains are able to survive for several tens of million years after having been ejected by galactic winds in the disk-halo interface. We lay out several scenarios that could explain this emission: dust grains may be shielded in the outer layers of cool dense clouds expelled from the galaxy disk, and/or the emission comes from the mixing layers around these cool clumps where material from the hot gas is able to cool down and mix with these cool cloudlets. This first set of data and upcoming spectroscopy will be very helpful to understand the survival of dust grains in energetic environments, and their contribution to recycling baryonic material in the mid-plane of galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.08026v1-abstract-full').style.display = 'none'; document.getElementById('2408.08026v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy & Astrophysics; 16 pages, 8 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 690, A348 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.13829">arXiv:2407.13829</a> <span> [<a href="https://arxiv.org/pdf/2407.13829">pdf</a>, <a href="https://arxiv.org/format/2407.13829">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 Local Group L-Band Survey: The First Measurements of Localized Cold Neutral Medium Properties in the Low-Metallicity Dwarf Galaxy NGC 6822 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pingel%2C+N+M">Nickolas M. Pingel</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+H">Hongxing Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Stanimirovi%C4%87%2C+S">Sne啪ana Stanimirovi膰</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=Leroy%2C+A+K">Adam K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+C">Chang-Goo Kim</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=Walter%2C+F">Fabian Walter</a>, <a href="/search/astro-ph?searchtype=author&query=Busch%2C+M+P">Michael P. Busch</a>, <a href="/search/astro-ph?searchtype=author&query=Chown%2C+R">Ryan Chown</a>, <a href="/search/astro-ph?searchtype=author&query=Meyer%2C+J+D">Jennifer Donovan Meyer</a>, <a href="/search/astro-ph?searchtype=author&query=Eibensteiner%2C+C">Cosima Eibensteiner</a>, <a href="/search/astro-ph?searchtype=author&query=Hunter%2C+D+A">Deidre A. Hunter</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=Tarantino%2C+E">Elizabeth Tarantino</a>, <a href="/search/astro-ph?searchtype=author&query=Villanueva%2C+V">Vicente Villanueva</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. 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="2407.13829v1-abstract-short" style="display: inline;"> Measuring the properties of the cold neutral medium (CNM) in low-metallicity galaxies provides insight into heating and cooling mechanisms in early Universe-like environments. We report detections of two localized atomic neutral hydrogen (HI) absorption features in NGC 6822, a low-metallicity (0.2 Z$_{\odot}$) dwarf galaxy in the Local Group. These are the first unambiguous CNM detections in a low… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.13829v1-abstract-full').style.display = 'inline'; document.getElementById('2407.13829v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.13829v1-abstract-full" style="display: none;"> Measuring the properties of the cold neutral medium (CNM) in low-metallicity galaxies provides insight into heating and cooling mechanisms in early Universe-like environments. We report detections of two localized atomic neutral hydrogen (HI) absorption features in NGC 6822, a low-metallicity (0.2 Z$_{\odot}$) dwarf galaxy in the Local Group. These are the first unambiguous CNM detections in a low-metallicity dwarf galaxy outside the Magellanic Clouds. The Local Group L-Band Survey (LGLBS) enabled these detections due to its high spatial (15 pc for HI emission) and spectral (0.4 \kms) resolution. We introduce LGLBS and describe a custom pipeline to search for HI absorption at high angular resolution and extract associated HI emission. A detailed Gaussian decomposition and radiative transfer analysis of the NGC 6822 detections reveals five CNM components, with key properties: a mean spin temperature of 32$\pm$6 K, a mean CNM column density of 3.1$\times$10$^{20}$ cm$^{-2}$, and CNM mass fractions of 0.33 and 0.12 for the two sightlines. Stacking non-detections does not reveal low-level signals below our median optical depth sensitivity of 0.05. One detection intercepts a star-forming region, with the HI absorption profile encompassing the CO (2$-$1) emission, indicating coincident molecular gas and a depression in high-resolution HI emission. We also analyze a nearby sightline with deep, narrow HI self-absorption dips, where the background warm neutral medium is attenuated by intervening CNM. The association of CNM, CO, and H$伪$ emissions suggests a close link between the colder, denser HI phase and star formation in NGC 6822. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.13829v1-abstract-full').style.display = 'none'; document.getElementById('2407.13829v1-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, 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">20 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/2407.04531">arXiv:2407.04531</a> <span> [<a href="https://arxiv.org/pdf/2407.04531">pdf</a>, <a href="https://arxiv.org/format/2407.04531">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202450265">10.1051/0004-6361/202450265 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Neutral atomic and molecular gas dynamics in the nearby spiral galaxies NGC 1512, NGC 4535, and NGC 7496 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Laudage%2C+S">Sebastian Laudage</a>, <a href="/search/astro-ph?searchtype=author&query=Eibensteiner%2C+C">Cosima Eibensteiner</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">Frank Bigiel</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=Meidt%2C+S">Sharon Meidt</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Querejeta%2C+M">Miguele Querejeta</a>, <a href="/search/astro-ph?searchtype=author&query=Stuber%2C+S">Sophia Stuber</a>, <a href="/search/astro-ph?searchtype=author&query=Colombo%2C+D">Dario Colombo</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Pisano%2C+D+J">D. J. Pisano</a>, <a href="/search/astro-ph?searchtype=author&query=Utomo%2C+D">Dyas Utomo</a>, <a href="/search/astro-ph?searchtype=author&query=Levy%2C+R+C">Rebecca C. Levy</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R">Ralf Klessen</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Y">Yixian Cao</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=Kurapati%2C+S">Sushma Kurapati</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez-Blazquez%2C+P">Patricia Sanchez-Blazquez</a>, <a href="/search/astro-ph?searchtype=author&query=Neumann%2C+J">Justus Neumann</a>, <a href="/search/astro-ph?searchtype=author&query=Neumann%2C+L">Lukas Neumann</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+H">Hsi-An Pan</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. 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="2407.04531v1-abstract-short" style="display: inline;"> Neutral atomic gas (HI) effectively traces galactic dynamics across mid to large galactocentric radii. However, its limitations in observing small-scale changes within the central few kiloparsecs, coupled with the often observed HI deficit in galactic centers, necessitates using molecular gas emission as a preferred tracer in these regions. Understanding the dynamics of both neutral atomic and mol… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.04531v1-abstract-full').style.display = 'inline'; document.getElementById('2407.04531v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.04531v1-abstract-full" style="display: none;"> Neutral atomic gas (HI) effectively traces galactic dynamics across mid to large galactocentric radii. However, its limitations in observing small-scale changes within the central few kiloparsecs, coupled with the often observed HI deficit in galactic centers, necessitates using molecular gas emission as a preferred tracer in these regions. Understanding the dynamics of both neutral atomic and molecular gas is crucial for a more complete understanding of how galaxies evolve, funnel gas from the outer disk into their central parts, and eventually form stars. In this work we aim to quantify the dynamics of both, the neutral atomic and molecular gas, in the nearby spiral galaxies NGC 1512, NGC 4535, and NGC 7496 using new MeerKAT-HI observations together with ALMA CO (2-1) observations from the PHANGS collaboration. We use the analysis tool 3D-Barolo to fit tilted ring models to the HI and CO observations. A combined approach of using the HI to constrain the true disk orientation parameters before applying these to the CO datasets is tested. This paper sets expectations for the results of the upcoming high-resolution HI coverage of many galaxies in the PHANGS-ALMA sample using MeerKAT or VLA, to establish a robust methodology for characterizing galaxy orientations and deriving dynamics from combining new HI with existing CO data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.04531v1-abstract-full').style.display = 'none'; document.getElementById('2407.04531v1-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">accepted for publication in A&A; 13 pages, 9 Figures (+2 appendix pages)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 690, A169 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.01716">arXiv:2407.01716</a> <span> [<a href="https://arxiv.org/pdf/2407.01716">pdf</a>, <a href="https://arxiv.org/format/2407.01716">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202449944">10.1051/0004-6361/202449944 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> PHANGS-MeerKAT and MHONGOOSE HI observations of nearby spiral galaxies: physical drivers of the molecular gas fraction, $R_{\mathrm{mol}}$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Eibensteiner%2C+C">Cosima Eibensteiner</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+J">Jiayi Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">Frank Bigiel</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=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Kurapati%2C+S">Sushma Kurapati</a>, <a href="/search/astro-ph?searchtype=author&query=Pisano%2C+D+J">D. J. Pisano</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A+T">Ashley T. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Thorp%2C+M">Mallory Thorp</a>, <a href="/search/astro-ph?searchtype=author&query=Colombo%2C+D">Dario Colombo</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=Chiang%2C+I">I-Da Chiang</a>, <a href="/search/astro-ph?searchtype=author&query=Ostriker%2C+E+C">Eve C. Ostriker</a>, <a href="/search/astro-ph?searchtype=author&query=Murphy%2C+E+J">Eric J. Murphy</a>, <a href="/search/astro-ph?searchtype=author&query=Zabel%2C+N">Nikki Zabel</a>, <a href="/search/astro-ph?searchtype=author&query=Laudage%2C+S">Sebstian Laudage</a>, <a href="/search/astro-ph?searchtype=author&query=Maccagni%2C+F+M">Filippo M. Maccagni</a>, <a href="/search/astro-ph?searchtype=author&query=Healy%2C+J">Julia Healy</a>, <a href="/search/astro-ph?searchtype=author&query=Sekhar%2C+S">Srikrishna Sekhar</a>, <a href="/search/astro-ph?searchtype=author&query=Utomo%2C+D">Dyas Utomo</a>, <a href="/search/astro-ph?searchtype=author&query=Brok%2C+J+d">Jakob den Brok</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Y">Yixian Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">M茅lanie Chevance</a> , et al. (14 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.01716v1-abstract-short" style="display: inline;"> The molecular-to-atomic gas ratio is crucial to the evolution of the interstellar medium in galaxies. We investigate the balance between the atomic ($危_{\rm HI}$) and molecular gas ($危_{\rm H2}$) surface densities in eight nearby star-forming galaxies using new high-quality observations from MeerKAT and ALMA (for HI and CO, respectively). We define the molecular gas ratio as… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.01716v1-abstract-full').style.display = 'inline'; document.getElementById('2407.01716v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.01716v1-abstract-full" style="display: none;"> The molecular-to-atomic gas ratio is crucial to the evolution of the interstellar medium in galaxies. We investigate the balance between the atomic ($危_{\rm HI}$) and molecular gas ($危_{\rm H2}$) surface densities in eight nearby star-forming galaxies using new high-quality observations from MeerKAT and ALMA (for HI and CO, respectively). We define the molecular gas ratio as $R_{\rm mol} = 危_{\rm H2} / 危_{\rm HI}$ and measure how it depends on local conditions in the galaxy disks using multi-wavelength observations. We find that, depending on the galaxy, HI is detected at $>3蟽$ out to 20-120 kpc in galactocentric radius ($r_{\rm gal}$). The typical radius at which $危_{\rm HI}$ reaches 1~$\rm M_\odot~pc^{-2}$ is $r_{\rm HI}\approx22$~kpc, which corresponds to 1-3 times the optical radius ($r_{25}$). $R_{\rm mol}$ correlates best with the dynamical equilibrium pressure, P$_{\rm DE}$, among potential drivers studied, with a median correlation coefficient of $<蟻>=0.89$. Correlations between $R_{\rm mol}$ and star formation rate, total gas and stellar surface density, metallicity, and $危_{\rm SFR}$/P$_{\rm DE}$ are present but somewhat weaker. Our results also show a direct correlation between P$_{\rm DE}$ and $危_{\rm SFR}$, supporting self-regulation models. Quantitatively, we measure similar scalings as previous works and attribute the modest differences that we find to the effect of varying resolution and sensitivity. At $r_{\rm gal} {\gtrsim}0.4~r_{25}$, atomic gas dominates over molecular gas, and at the balance of these two gas phases, we find that the baryon mass is dominated by stars, with $危_{*} > 5~危_{\rm gas}$. Our study constitutes an important step in the statistical investigation of how local galaxy properties impact the conversion from atomic to molecular gas in nearby galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.01716v1-abstract-full').style.display = 'none'; document.getElementById('2407.01716v1-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 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">accepted for publication in A&A; 20 pages, 12 Figures (+4 appendix pages)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 691, A163 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.12025">arXiv:2406.12025</a> <span> [<a href="https://arxiv.org/pdf/2406.12025">pdf</a>, <a href="https://arxiv.org/format/2406.12025">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202449496">10.1051/0004-6361/202449496 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A 260 pc resolution ALMA map of HCN(1-0) in the galaxy NGC 4321 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Neumann%2C+L">Lukas Neumann</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">Frank Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A+T">Ashley T. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Gallagher%2C+M+J">Molly J. Gallagher</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A">Adam Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Usero%2C+A">Antonio Usero</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Be%C5%A1li%C4%87%2C+I">Ivana Be拧li膰</a>, <a href="/search/astro-ph?searchtype=author&query=Boquien%2C+M">M茅d茅ric Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Y">Yixian Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">M茅lanie Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Colombo%2C+D">Dario Colombo</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">Daniel A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Eibensteiner%2C+C">Cosima Eibensteiner</a>, <a href="/search/astro-ph?searchtype=author&query=Grasha%2C+K">Kathryn Grasha</a>, <a href="/search/astro-ph?searchtype=author&query=Henshaw%2C+J+D">Jonathan D. Henshaw</a>, <a href="/search/astro-ph?searchtype=author&query=Jim%C3%A9nez-Donaire%2C+M+J">Mar铆a J. Jim茅nez-Donaire</a>, <a href="/search/astro-ph?searchtype=author&query=Meidt%2C+S">Sharon Meidt</a>, <a href="/search/astro-ph?searchtype=author&query=Menon%2C+S+H">Shyam H. Menon</a>, <a href="/search/astro-ph?searchtype=author&query=Murphy%2C+E+J">Eric J. Murphy</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+H">Hsi-An Pan</a>, <a href="/search/astro-ph?searchtype=author&query=Querejeta%2C+M">Miguel Querejeta</a>, <a href="/search/astro-ph?searchtype=author&query=Saito%2C+T">Toshiki Saito</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Stuber%2C+S+K">Sophia K. Stuber</a> , et al. (2 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.12025v1-abstract-short" style="display: inline;"> The star formation rate (SFR) is tightly connected to the amount of dense gas in molecular clouds. However, it is not fully understood how the relationship between dense molecular gas and star formation varies within galaxies and in different morphological environments. In this work, we study dense gas and star formation in the nearby spiral galaxy NGC 4321 to test how the amount of dense gas and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.12025v1-abstract-full').style.display = 'inline'; document.getElementById('2406.12025v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.12025v1-abstract-full" style="display: none;"> The star formation rate (SFR) is tightly connected to the amount of dense gas in molecular clouds. However, it is not fully understood how the relationship between dense molecular gas and star formation varies within galaxies and in different morphological environments. In this work, we study dense gas and star formation in the nearby spiral galaxy NGC 4321 to test how the amount of dense gas and its ability to form stars varies with environmental properties at 260 pc scales. We present new ALMA observations of HCN(1-0) line emission. Combined with existing CO(2-1) observations from ALMA, and H-alpha from MUSE, as well as F2100W from JWST to trace the SFR, we measure the HCN/CO line ratio, a proxy for the dense gas fraction and SFR/HCN, a proxy for the star formation efficiency of the dense gas. Towards the centre of the galaxy, HCN/CO systematically increases while SFR/HCN decreases, but these ratios stay roughly constant throughout the disc. Spiral arms, interarm regions, and bar ends show similar HCN/CO and SFR/HCN. On the bar, there is a significantly lower SFR/HCN at a similar HCN/CO. We conclude that the centres of galaxies show the strongest environmental influence on dense gas and star formation, suggesting either that clouds couple strongly to the surrounding pressure or that HCN is tracing more of the bulk molecular gas that is less efficiently converted into stars. On the contrary, across the disc of NGC 4321, where the ISM pressure is typically low, SFR/HCN does not show large variations (< 0.3 dex) in agreement with Galactic observations of molecular clouds. Despite the large variations across environments and physical conditions, HCN/CO is a good predictor of the mean molecular gas surface density at 260 pc scales. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.12025v1-abstract-full').style.display = 'none'; document.getElementById('2406.12025v1-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">18 pages, 9 figures, accepted for pub in A&A, Jun 13, 2024</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 691, A121 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.01291">arXiv:2406.01291</a> <span> [<a href="https://arxiv.org/pdf/2406.01291">pdf</a>, <a href="https://arxiv.org/format/2406.01291">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"> WISDOM project XX -- Strong shear tearing molecular clouds apart in NGC 524 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lu%2C+A">Anan Lu</a>, <a href="/search/astro-ph?searchtype=author&query=Haggard%2C+D">Daryl Haggard</a>, <a href="/search/astro-ph?searchtype=author&query=Bureau%2C+M">Martin Bureau</a>, <a href="/search/astro-ph?searchtype=author&query=Gensior%2C+J">Jindra Gensior</a>, <a href="/search/astro-ph?searchtype=author&query=Jeffreson%2C+S">Sarah Jeffreson</a>, <a href="/search/astro-ph?searchtype=author&query=Robert%2C+C">Carmelle Robert</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=Liang%2C+F">Fu-Heng Liang</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+W">Woorak Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+A">Timothy A. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Babic%2C+S">Sara Babic</a>, <a href="/search/astro-ph?searchtype=author&query=Boyce%2C+H">Hope Boyce</a>, <a href="/search/astro-ph?searchtype=author&query=Cheung%2C+B">Benjamin Cheung</a>, <a href="/search/astro-ph?searchtype=author&query=Drissen%2C+L">Laurent Drissen</a>, <a href="/search/astro-ph?searchtype=author&query=Elford%2C+J+S">Jacob S. Elford</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+L">Lijie Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+T">Thomas Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Rhea%2C+C">Carter Rhea</a>, <a href="/search/astro-ph?searchtype=author&query=Rousseau-Nepton%2C+L">Laurie Rousseau-Nepton</a>, <a href="/search/astro-ph?searchtype=author&query=Ruffa%2C+I">Ilaria Ruffa</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="2406.01291v1-abstract-short" style="display: inline;"> Early-type galaxies (ETGs) are known to harbour dense spheroids of stars but scarce star formation (SF). Approximately a quarter of these galaxies have rich molecular gas reservoirs yet do not form stars efficiently. We study here the ETG NGC~524, with strong shear suspected to result in a smooth molecular gas disc and low star-formation efficiency (SFE). We present new spatially-resolved observat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.01291v1-abstract-full').style.display = 'inline'; document.getElementById('2406.01291v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.01291v1-abstract-full" style="display: none;"> Early-type galaxies (ETGs) are known to harbour dense spheroids of stars but scarce star formation (SF). Approximately a quarter of these galaxies have rich molecular gas reservoirs yet do not form stars efficiently. We study here the ETG NGC~524, with strong shear suspected to result in a smooth molecular gas disc and low star-formation efficiency (SFE). We present new spatially-resolved observations of the \textsuperscript{12}CO(2-1)-emitting cold molecular gas from the Atacama Large Millimeter/sub-millimeter Array (ALMA) and of the warm ionised-gas emission lines from SITELLE at the Canada-France-Hawaii Telescope. Although constrained by the resolution of the ALMA observations ($\approx37$~pc), we identify only $52$ GMCs with radii ranging from $30$ to $140$~pc, a low mean molecular gas mass surface density $\langle危_{\rm gas}\rangle\approx125$~M$_\odot$~pc$^{-2}$ and a high mean virial parameter $\langle伪_{\rm obs,vir}\rangle\approx5.3$. We measure spatially-resolved molecular gas depletion times ($蟿_{\rm dep}\equiv1/{\rm SFE}$) with a spatial resolution of $\approx100$~pc within a galactocentric distance of $1.5$~kpc. The global depletion time is $\approx2.0$~Gyr but $蟿_{\rm dep}$ increases toward the galaxy centre, with a maximum $蟿_{\rm dep,max}\approx5.2$~Gyr. However, no pure \ion{H}{II} region is identified in NGC~524 using ionised-gas emission-line ratio diagnostics, so the $蟿_{\rm dep}$ inferred are in fact lower limits. Measuring the GMC properties and dynamical states, we conclude that shear is the dominant mechanism shaping the molecular gas properties and regulating SF in NGC~524. This is supported by analogous analyses of the GMCs in a simulated ETG similar to NGC~524. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.01291v1-abstract-full').style.display = 'none'; document.getElementById('2406.01291v1-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">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">17 pages, 10 figures. To be published in MNRAS, accepted on May 27</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.19709">arXiv:2405.19709</a> <span> [<a href="https://arxiv.org/pdf/2405.19709">pdf</a>, <a href="https://arxiv.org/format/2405.19709">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"> WISDOM Project -- XXI. Giant molecular clouds in the central region of the barred spiral galaxy NGC 613: a steep size -- linewidth relation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Choi%2C+W">Woorak Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Bureau%2C+M">Martin Bureau</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+L">Lijie Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Cappellari%2C+M">Michele Cappellari</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+A">Timothy A. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Gensior%2C+J">Jindra Gensior</a>, <a href="/search/astro-ph?searchtype=author&query=Liang%2C+F">Fu-Heng Liang</a>, <a href="/search/astro-ph?searchtype=author&query=Lu%2C+A">Anan Lu</a>, <a href="/search/astro-ph?searchtype=author&query=Moon%2C+S">Sanghyuk Moon</a>, <a href="/search/astro-ph?searchtype=author&query=Ruffa%2C+I">Ilaria Ruffa</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=Chung%2C+A">Aeree Chung</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="2405.19709v2-abstract-short" style="display: inline;"> NGC~613 is a nearby barred spiral galaxy with a nuclear ring. Exploiting high spatial resolution ($\approx20$ pc) Atacama Large Millimeter/sub-millimeter Array $^{12}$CO(1-0) observations, we study the giant molecular clouds (GMCs) in the nuclear ring and its vicinity, identifying $158$ spatially- and spectrally-resolved GMCs. The GMC sizes ($R_{\mathrm{c}}$) are comparable to those of the clouds… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.19709v2-abstract-full').style.display = 'inline'; document.getElementById('2405.19709v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.19709v2-abstract-full" style="display: none;"> NGC~613 is a nearby barred spiral galaxy with a nuclear ring. Exploiting high spatial resolution ($\approx20$ pc) Atacama Large Millimeter/sub-millimeter Array $^{12}$CO(1-0) observations, we study the giant molecular clouds (GMCs) in the nuclear ring and its vicinity, identifying $158$ spatially- and spectrally-resolved GMCs. The GMC sizes ($R_{\mathrm{c}}$) are comparable to those of the clouds in the Milky Way (MW) disc, but their gas masses, observed linewidths ($蟽_{\mathrm{obs,los}}$) and gas mass surface densities are larger. The GMC size -- linewidth relation ($蟽_{\mathrm{obs,los}}\propto R_{\mathrm{c}}^{0.77}$) is steeper than that of the clouds of the MW disc and centre, and the GMCs are on average only marginally gravitationally bound (with a mean virial parameter $\langle伪_{\mathrm{obs,vir}}\rangle\approx1.7$). We discuss the possible origins of the steep size -- linewidth relation and enhanced observed linewidths of the clouds and suggest that a combination of mechanisms such as stellar feedback, gas accretion and cloud-cloud collisions, as well as the gas inflows driven by the large-scale bar, may play a role. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.19709v2-abstract-full').style.display = 'none'; document.getElementById('2405.19709v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 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">15 pages, 8 figures, accepted for publication in MNRAS. arXiv admin note: text overlap with arXiv:2304.10471</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.15102">arXiv:2405.15102</a> <span> [<a href="https://arxiv.org/pdf/2405.15102">pdf</a>, <a href="https://arxiv.org/format/2405.15102">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 Fraction of Dust Mass in the Form of PAHs on 10-50 pc Scales in Nearby Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sutter%2C+J">Jessica Sutter</a>, <a href="/search/astro-ph?searchtype=author&query=Sandstrom%2C+K">Karin Sandstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Chastenet%2C+J">J茅r茅my Chastenet</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=Koch%2C+E+W">Eric W. Koch</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=Chown%2C+R">Ryan Chown</a>, <a href="/search/astro-ph?searchtype=author&query=Belfiore%2C+F">Francesco Belfiore</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">Frank Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Boquien%2C+M">M茅d茅ric Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Y">Yixian Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">M茅lanie Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">Daniel A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Egorov%2C+O+V">Oleg V. Egorov</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S+C+O">Simon C. O. Glover</a>, <a href="/search/astro-ph?searchtype=author&query=Groves%2C+B">Brent Groves</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R+S">Ralf S. Klessen</a>, <a href="/search/astro-ph?searchtype=author&query=Kreckel%2C+K">Kathryn Kreckel</a>, <a href="/search/astro-ph?searchtype=author&query=Larson%2C+K+L">Kirsten L. Larson</a>, <a href="/search/astro-ph?searchtype=author&query=Oakes%2C+E+K">Elias K. Oakes</a>, <a href="/search/astro-ph?searchtype=author&query=Pathak%2C+D">Debosmita Pathak</a>, <a href="/search/astro-ph?searchtype=author&query=Ramambason%2C+L">Lise Ramambason</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Watkins%2C+E+J">Elizabeth J. Watkins</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="2405.15102v1-abstract-short" style="display: inline;"> Polycyclic aromatic hydrocarbons (PAHs) are a ubiquitous component of the interstellar medium (ISM) in z~0 massive, star-forming galaxies and play key roles in ISM energy balance, chemistry, and shielding. Wide field of view, high resolution mid-infrared (MIR) images from JWST provides the ability to map the fraction of dust in the form of PAHs and the properties of these key dust grains at 10-50… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.15102v1-abstract-full').style.display = 'inline'; document.getElementById('2405.15102v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.15102v1-abstract-full" style="display: none;"> Polycyclic aromatic hydrocarbons (PAHs) are a ubiquitous component of the interstellar medium (ISM) in z~0 massive, star-forming galaxies and play key roles in ISM energy balance, chemistry, and shielding. Wide field of view, high resolution mid-infrared (MIR) images from JWST provides the ability to map the fraction of dust in the form of PAHs and the properties of these key dust grains at 10-50 pc resolution in galaxies outside the Local Group. We use MIR JWST photometric observations of a sample of 19 nearby galaxies from the "Physics at High Angular Resolution in Nearby GalaxieS" (PHANGS) survey to investigate the variations of the PAH fraction. By comparison to lower resolution far-IR mapping, we show that a combination of the MIRI filters (R$_{\rm{PAH}}$ = [F770W+F1130W]/F2100W) traces the fraction of dust by mass in the form of PAHs (i.e., the PAH fraction, or q$_{\rm{PAH}}$). Mapping R$_{\rm{PAH}}$ across the 19 PHANGS galaxies, we find that the PAH fraction steeply decreases in HII regions, revealing the destruction of these small grains in regions of ionized gas. Outside HII regions, we find R$_{\rm{PAH}}$ is constant across the PHANGS sample with an average value of 3.43$\pm$0.98, which, for an illuminating radiation field of intensity 2-5 times that of the radiation field in the solar neighborhood, corresponds to q$_{\rm{PAH}}$ values of 3-6%. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.15102v1-abstract-full').style.display = 'none'; document.getElementById('2405.15102v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 May, 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 at ApJ, 39 pages, 25 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/2405.08974">arXiv:2405.08974</a> <span> [<a href="https://arxiv.org/pdf/2405.08974">pdf</a>, <a href="https://arxiv.org/format/2405.08974">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202450730">10.1051/0004-6361/202450730 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of $\sim$2200 new supernova remnants in 19 nearby star-forming galaxies with MUSE spectroscopy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Li%2C+J">Jing Li</a>, <a href="/search/astro-ph?searchtype=author&query=Kreckel%2C+K">K. Kreckel</a>, <a href="/search/astro-ph?searchtype=author&query=Sarbadhicary%2C+S">S. Sarbadhicary</a>, <a href="/search/astro-ph?searchtype=author&query=Egorov%2C+O+V">Oleg V. Egorov</a>, <a href="/search/astro-ph?searchtype=author&query=Groves%2C+B">B. Groves</a>, <a href="/search/astro-ph?searchtype=author&query=Long%2C+K+S">K. S. Long</a>, <a href="/search/astro-ph?searchtype=author&query=Congiu%2C+E">Enrico Congiu</a>, <a href="/search/astro-ph?searchtype=author&query=Belfiore%2C+F">Francesco Belfiore</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S+C+O">Simon C. O. Glover</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A+.+T">Ashley . T Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">Frank Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Blanc%2C+G+A">Guillermo A. Blanc</a>, <a href="/search/astro-ph?searchtype=author&query=Grasha%2C+K">Kathryn Grasha</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R+S">Ralf S. Klessen</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A">Adam Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%A9ndez-Delgado%2C+J+E">J. Eduardo M茅ndez-Delgado</a>, <a href="/search/astro-ph?searchtype=author&query=Neumann%2C+J">Justus Neumann</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</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=collaborators%2C+P">PHANGS collaborators</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="2405.08974v1-abstract-short" style="display: inline;"> We present the largest extragalactic survey of supernova remnant (SNR) candidates in nearby star-forming galaxies using exquisite spectroscopic maps from MUSE. Supernova remnants exhibit distinctive emission-line ratios and kinematic signatures, which are apparent in optical spectroscopy. Using optical integral field spectra from the PHANGS-MUSE project, we identify SNRs in 19 nearby galaxies at ~… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.08974v1-abstract-full').style.display = 'inline'; document.getElementById('2405.08974v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.08974v1-abstract-full" style="display: none;"> We present the largest extragalactic survey of supernova remnant (SNR) candidates in nearby star-forming galaxies using exquisite spectroscopic maps from MUSE. Supernova remnants exhibit distinctive emission-line ratios and kinematic signatures, which are apparent in optical spectroscopy. Using optical integral field spectra from the PHANGS-MUSE project, we identify SNRs in 19 nearby galaxies at ~ 100~pc scales. We use five different optical diagnostics: (1) line ratio maps of [SII]/H$伪$; (2) line ratio maps of [OI]/H$伪$; (3) velocity dispersion map of the gas; (4) and (5) two line ratio diagnostic diagrams from BPT diagrams to identify and distinguish SNRs from other nebulae. Given that our SNRs are seen in projection against HII regions and diffuse ionized gas, in our line ratio maps we use a novel technique to search for objects with [SII]/H$伪$ or [OI]/H$伪$ in excess of what is expected at fixed H$伪$ surface brightness within photoionized gas. In total, we identify 2,233 objects using at least one of our diagnostics, and define a subsample of 1,166 high-confidence SNRs that have been detected with at least two diagnostics. The line ratios of these SNRs agree well with the MAPPINGS shock models, and we validate our technique using the well-studied nearby galaxy M83, where all SNRs we found are also identified in literature catalogs and we recover 51% of the known SNRs. The remaining 1,067 objects in our sample are detected with only one diagnostic and we classify them as SNR candidates. We find that ~ 35% of all our objects overlap with the boundaries of HII regions from literature catalogs, highlighting the importance of using indicators beyond line intensity morphology to select SNRs. [OI]/H$伪$ line ratio is responsible for selecting the most objects (1,368; 61%), (abridged). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.08974v1-abstract-full').style.display = 'none'; document.getElementById('2405.08974v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 May, 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">35 pages, 24 figures,6 tables, submitted to A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 690, A161 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.05364">arXiv:2405.05364</a> <span> [<a href="https://arxiv.org/pdf/2405.05364">pdf</a>, <a href="https://arxiv.org/format/2405.05364">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"> Do spiral arms enhance star formation efficiency? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Querejeta%2C+M">Miguel Querejeta</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=Meidt%2C+S+E">Sharon E. Meidt</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Belfiore%2C+F">Francesco Belfiore</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R+S">Ralf S. Klessen</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+J">Jiayi Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Sormani%2C+M">Mattia Sormani</a>, <a href="/search/astro-ph?searchtype=author&query=Be%C5%A1lic%2C+I">Ivana Be拧lic</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Y">Yixian Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">M茅lanie Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Colombo%2C+D">Dario Colombo</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">Daniel A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Burillo%2C+S">Santiago Garc铆a-Burillo</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S+C+O">Simon C. O. Glover</a>, <a href="/search/astro-ph?searchtype=author&query=Grasha%2C+K">Kathryn Grasha</a>, <a href="/search/astro-ph?searchtype=author&query=Groves%2C+B">Brent Groves</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=Neumann%2C+L">Lukas Neumann</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+H">Hsi-An Pan</a>, <a href="/search/astro-ph?searchtype=author&query=Pessa%2C+I">Ismael Pessa</a>, <a href="/search/astro-ph?searchtype=author&query=Pety%2C+J">J茅r么me Pety</a>, <a href="/search/astro-ph?searchtype=author&query=Pinna%2C+F">Francesca Pinna</a>, <a href="/search/astro-ph?searchtype=author&query=Ramambason%2C+L">Lise Ramambason</a> , et al. (10 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.05364v1-abstract-short" style="display: inline;"> Spiral arms are some of the most spectacular features in disc galaxies, and also present in our own Milky Way. It has been argued that star formation should proceed more efficiently in spiral arms as a result of gas compression. Yet, observational studies have so far yielded contradictory results. Here we examine arm/interarm surface density contrasts at ~100 pc resolution in 28 spiral galaxies fr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.05364v1-abstract-full').style.display = 'inline'; document.getElementById('2405.05364v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.05364v1-abstract-full" style="display: none;"> Spiral arms are some of the most spectacular features in disc galaxies, and also present in our own Milky Way. It has been argued that star formation should proceed more efficiently in spiral arms as a result of gas compression. Yet, observational studies have so far yielded contradictory results. Here we examine arm/interarm surface density contrasts at ~100 pc resolution in 28 spiral galaxies from the PHANGS survey. We find that the arm/interarm contrast in stellar mass surface density (Sigma_*) is very modest, typically a few tens of percent. This is much smaller than the contrasts measured for molecular gas (Sigma_mol) or star formation rate (Sigma_SFR) surface density, which typically reach a factor of ~2-3. Yet, Sigma_mol and Sigma_SFR contrasts show a significant correlation with the enhancement in Sigma_*, suggesting that the small stellar contrast largely dictates the stronger accumulation of gas and star formation. All these contrasts increase for grand-design spirals compared to multi-armed and flocculent systems (and for galaxies with high stellar mass). The median star formation efficiency (SFE) of the molecular gas is 16% higher in spiral arms than in interarm regions, with a large scatter, and the contrast increases significantly (median SFE contrast 2.34) for regions of particularly enhanced stellar contrast (Sigma_* contrast >1.97). The molecular-to-atomic gas ratio (Sigma_mol/Sigma_atom) is higher in spiral arms, pointing to a transformation of atomic to molecular gas. In conclusion, the boost in the star formation efficiency of molecular gas in spiral arms is generally modest or absent, except for locations with exceptionally large stellar contrasts. (abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.05364v1-abstract-full').style.display = 'none'; document.getElementById('2405.05364v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 May, 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">26 pages, 16 figures. Accepted for publication in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.16345">arXiv:2404.16345</a> <span> [<a href="https://arxiv.org/pdf/2404.16345">pdf</a>, <a href="https://arxiv.org/format/2404.16345">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/stae1106">10.1093/mnras/stae1106 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> WISDOM Project -- XIX. Figures of merit for supermassive black hole mass measurements using molecular gas and/or megamaser kinematics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+H">Hengyue Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Bureau%2C+M">Martin Bureau</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+M+D">Mark D. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Cappellari%2C+M">Michele Cappellari</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+A">Timothy A. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Dominiak%2C+P">Pandora Dominiak</a>, <a href="/search/astro-ph?searchtype=author&query=Elford%2C+J+S">Jacob S. Elford</a>, <a href="/search/astro-ph?searchtype=author&query=Liang%2C+F">Fu-Heng Liang</a>, <a href="/search/astro-ph?searchtype=author&query=Ruffa%2C+I">Ilaria Ruffa</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. 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="2404.16345v2-abstract-short" style="display: inline;"> The mass ($M_\mathrm{BH}$) of a supermassive black hole (SMBH) can be measured using spatially-resolved kinematics of the region where the SMBH dominates gravitationally. The most reliable measurements are those that resolve the smallest physical scales around the SMBHs. We consider here three metrics to compare the physical scales probed by kinematic tracers dominated by rotation: the radius of t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.16345v2-abstract-full').style.display = 'inline'; document.getElementById('2404.16345v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.16345v2-abstract-full" style="display: none;"> The mass ($M_\mathrm{BH}$) of a supermassive black hole (SMBH) can be measured using spatially-resolved kinematics of the region where the SMBH dominates gravitationally. The most reliable measurements are those that resolve the smallest physical scales around the SMBHs. We consider here three metrics to compare the physical scales probed by kinematic tracers dominated by rotation: the radius of the innermost detected kinematic tracer $R_\mathrm{min}$ normalised by respectively the SMBH's Schwarzschild radius ($R_\mathrm{Schw}\equiv 2GM_\mathrm{BH}/c^2$, where $G$ is the gravitational constant and $c$ the speed of light), sphere-of-influence (SOI) radius ($R_\mathrm{SOI}\equiv GM_\mathrm{BH}/蟽_\mathrm{e}^2$, where $蟽_\mathrm{e}$ is the stellar velocity dispersion within the galaxy's effective radius) and equality radius [the radius $R_\mathrm{eq}$ at which the SMBH mass equals the enclosed stellar mass, $M_\mathrm{BH}=M_*(R_\mathrm{eq})$, where $M_*(R)$ is the stellar mass enclosed within the radius $R$]. All metrics lead to analogous simple relations between $R_\mathrm{min}$ and the highest circular velocity probed $V_\mathrm{c}$. Adopting these metrics to compare the SMBH mass measurements using molecular gas kinematics to those using megamaser kinematics, we demonstrate that the best molecular gas measurements resolve material that is physically closer to the SMBHs in terms of $R_\mathrm{Schw}$ but is slightly farther in terms of $R_\mathrm{SOI}$ and $R_\mathrm{eq}$. However, molecular gas observations of nearby galaxies using the most extended configurations of the Atacama Large Millimeter/sub-millimeter Array can resolve the SOI comparably well and thus enable SMBH mass measurements as precise as the best megamaser measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.16345v2-abstract-full').style.display = 'none'; document.getElementById('2404.16345v2-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 9 figures. Accepted by 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/2404.11260">arXiv:2404.11260</a> <span> [<a href="https://arxiv.org/pdf/2404.11260">pdf</a>, <a href="https://arxiv.org/format/2404.11260">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"> WISDOM Project -- XXIV. Cross-checking supermassive black hole mass estimates from ALMA CO gas kinematics and SINFONI stellar kinematics in the galaxy NGC 4751 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dominiak%2C+P">Pandora Dominiak</a>, <a href="/search/astro-ph?searchtype=author&query=Cappellari%2C+M">Michele Cappellari</a>, <a href="/search/astro-ph?searchtype=author&query=Bureau%2C+M">Martin Bureau</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+A">Timothy A. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Sarzi%2C+M">Marc Sarzi</a>, <a href="/search/astro-ph?searchtype=author&query=Ruffa%2C+I">Ilaria Ruffa</a>, <a href="/search/astro-ph?searchtype=author&query=Iguchi%2C+S">Satoru Iguchi</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=Zhang%2C+H">Hengyue Zhang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.11260v1-abstract-short" style="display: inline;"> Supermassive black hole (SMBH) masses can be measured by observing the impacts of the SMBHs on dynamical tracers around them. We present high angular resolution ($0.19$ arcsec or $\approx24$ pc) Atacama Large Millimeter/submillimeter Array observations of the $^{12}$CO(3-2) line emission of the early-type galaxy NGC 4751, which reveal a highly-inclined regularly-rotating molecular gas disc with cl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.11260v1-abstract-full').style.display = 'inline'; document.getElementById('2404.11260v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.11260v1-abstract-full" style="display: none;"> Supermassive black hole (SMBH) masses can be measured by observing the impacts of the SMBHs on dynamical tracers around them. We present high angular resolution ($0.19$ arcsec or $\approx24$ pc) Atacama Large Millimeter/submillimeter Array observations of the $^{12}$CO(3-2) line emission of the early-type galaxy NGC 4751, which reveal a highly-inclined regularly-rotating molecular gas disc with clear central Keplerian motions. Using a Hubble Space Telescope image to constrain the stellar mass distribution, we forward model the molecular gas kinematics and data cube in a Bayesian framework using the Kinematic Molecular Simulation code. Assuming a constant mass-to-light ratio ($M/L$), we infer a SMBH mass $M_\text{BH}=3.43^{+0.45}_{-0.44}\times10^9$ $\text{M}_\odot$ and a F160W filter stellar $M/L$ $M/L_\text{F160W}=(2.68\pm0.11)$ $\text{M}_\odot/\text{L}_{\odot,\text{F160W}}$ (all quoted uncertainties are at $3蟽$ confidence). Assuming a linearly spatially-varying $M/L$, we infer $M_\text{BH}=2.79_{-0.57}^{+0.75}\times10^9$ $\text{M}_\odot$ and $\left(M/L_\text{F160W}\right)/\left(\text{M}_\odot/\text{L}_{\odot,\text{F160W}}\right)=3.07^{+0.27}_{-0.35}-0.09^{+0.08}_{-0.06}\,\left(R/\text{arcsec}\right)$, where $R$ is the galactocentric radius. We also present alternative SMBH mass estimates using the Jeans Anisotropic Modelling (JAM) method and SINFONI stellar kinematics. Assuming a cylindrically-aligned velocity ellipsoid (JAM$_\text{cyl}$) we infer $M_\text{BH}=(2.52\pm 0.36)\times10^9$ $\text{M}_\odot$, while assuming a spherically-aligned velocity ellipsoid (JAM$_\text{sph}$) we infer $M_\text{BH}=(3.24\pm0.87)\times10^9$ $\text{M}_\odot$. Our derived masses are all consistent with one another, but they are larger than (and inconsistent with) one previous stellar dynamical measurement using Schwarzschil's method and the same SINFONI kinematics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.11260v1-abstract-full').style.display = 'none'; document.getElementById('2404.11260v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 13 figures, submitted to MNRAS. arXiv admin note: text overlap with arXiv:2401.16376</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.10762">arXiv:2404.10762</a> <span> [<a href="https://arxiv.org/pdf/2404.10762">pdf</a>, <a href="https://arxiv.org/format/2404.10762">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"> H-alpha emission and HII regions at the locations of recent supernovae in nearby galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chen%2C+N+M">Ness Mayker Chen</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=Sarbadhicary%2C+S+K">Sumit K. Sarbadhicary</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+T+A">Todd A. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A+T">Ashley T. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Groves%2C+B">Brent Groves</a>, <a href="/search/astro-ph?searchtype=author&query=Chandar%2C+R">Rupali Chandar</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">M茅lanie Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Chown%2C+R">Ryan Chown</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">Daniel A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Egorov%2C+O+V">Oleg V. Egorov</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S+C+O">Simon C. O. Glover</a>, <a href="/search/astro-ph?searchtype=author&query=Grasha%2C+K">Kathryn Grasha</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R+S">Ralf S. Klessen</a>, <a href="/search/astro-ph?searchtype=author&query=Kreckel%2C+K">Kathryn Kreckel</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+J">Jing Li</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%A9ndez-Delgado%2C+J+E">J. Eduardo M茅ndez-Delgado</a>, <a href="/search/astro-ph?searchtype=author&query=Murphy%2C+E+J">Eric J. Murphy</a>, <a href="/search/astro-ph?searchtype=author&query=Pathak%2C+D">Debosmita Pathak</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Thilker%2C+D+A">David A. Thilker</a>, <a href="/search/astro-ph?searchtype=author&query=%C3%9Abeda%2C+L">Leonardo 脷beda</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. 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="2404.10762v1-abstract-short" style="display: inline;"> We present a statistical analysis of the local, approximately 50-100 pc scale, H-alpha emission at the locations of recent (less than 125 years) supernovae (SNe) in nearby star-forming galaxies. Our sample consists of 32 SNe in 10 galaxies that are targets of the PHANGS-MUSE survey. We find that 41% (13/32) of these SNe occur coincident with a previously identified HII region. For comparison, HII… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.10762v1-abstract-full').style.display = 'inline'; document.getElementById('2404.10762v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.10762v1-abstract-full" style="display: none;"> We present a statistical analysis of the local, approximately 50-100 pc scale, H-alpha emission at the locations of recent (less than 125 years) supernovae (SNe) in nearby star-forming galaxies. Our sample consists of 32 SNe in 10 galaxies that are targets of the PHANGS-MUSE survey. We find that 41% (13/32) of these SNe occur coincident with a previously identified HII region. For comparison, HII regions cover 32% of the area within 1 kpc of any recent SN. Contrasting this local covering fraction with the fraction of SNe coincident with HII regions, we find a statistical excess of 7.6% +/- 8.7% of all SNe to be associated with HII regions. This increases to an excess of 19.2% +/- 10.4% when considering only core-collapse SNe. These estimates appear to be in good agreement with qualitative results from new, higher resolution HST H-alpha imaging, which also suggest many CCSNe detonate near but not in HII regions. Our results appear consistent with the expectation that only a modest fraction of stars explode during the first 5 Myr of the life of a stellar population, when H-alpha emission is expected to be bright. Of the HII region associated SNe, 8% (11/13) also have associated detected CO(2-1) emission, indicating the presence of molecular gas. The HII region associated SNe have typical Av extinctions approximately equal to 1 mag, consistent with a significant amount of pre-clearing of gas from the region before the SNe explode. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.10762v1-abstract-full').style.display = 'none'; document.getElementById('2404.10762v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ; 33 pages, 13 figures, 3 tables in two-column AASTEX63 format</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.09791">arXiv:2404.09791</a> <span> [<a href="https://arxiv.org/pdf/2404.09791">pdf</a>, <a href="https://arxiv.org/format/2404.09791">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202348772">10.1051/0004-6361/202348772 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Simulating nearby disc galaxies on the main star formation sequence I. Bar formation and the building of the central gas reservoir </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Verwilghen%2C+P">Pierrick Verwilghen</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Renaud%2C+F">Florent Renaud</a>, <a href="/search/astro-ph?searchtype=author&query=Valentini%2C+M">Milena Valentini</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+J">Jiayi Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Jeffreson%2C+S">Sarah Jeffreson</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R+S">Ralf S. Klessen</a>, <a href="/search/astro-ph?searchtype=author&query=Sormani%2C+M+C">Mattia C. Sormani</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A+T">Ashley. T. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Dolag%2C+K">Klaus Dolag</a>, <a href="/search/astro-ph?searchtype=author&query=Grasha%2C+K">Kathryn Grasha</a>, <a href="/search/astro-ph?searchtype=author&query=Liang%2C+F">Fu-Heng Liang</a>, <a href="/search/astro-ph?searchtype=author&query=Meidt%2C+S">Sharon Meidt</a>, <a href="/search/astro-ph?searchtype=author&query=Neumann%2C+J">Justus Neumann</a>, <a href="/search/astro-ph?searchtype=author&query=Querejeta%2C+M">Miguel Querejeta</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. 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="2404.09791v1-abstract-short" style="display: inline;"> Past studies have long emphasised the key role played by galactic stellar bars in the context of disc secular evolution, via the redistribution of gas and stars, the triggering of star formation, and the formation of prominent structures such as rings and central mass concentrations. However, the exact physical processes acting on those structures, as well as the timescales associated with the bui… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.09791v1-abstract-full').style.display = 'inline'; document.getElementById('2404.09791v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.09791v1-abstract-full" style="display: none;"> Past studies have long emphasised the key role played by galactic stellar bars in the context of disc secular evolution, via the redistribution of gas and stars, the triggering of star formation, and the formation of prominent structures such as rings and central mass concentrations. However, the exact physical processes acting on those structures, as well as the timescales associated with the building and consumption of central gas reservoirs are still not well understood. We are building a suite of hydro-dynamical RAMSES simulations of isolated, low-redshift galaxies that mimic the properties of the PHANGS sample. The initial conditions of the models reproduce the observed stellar mass, disc scale length, or gas fraction, and this paper presents a first subset of these models. Most of our simulated galaxies develop a prominent bar structure, which itself triggers central gas fuelling and the building of an over-density with a typical scale of 100-1000 pc. We confirm that if the host galaxy features an ellipsoidal component, the formation of the bar and gas fuelling are delayed. We show that most of our simulations follow a common time evolution, when accounting for mass scaling and the bar formation time. In our simulations, the stellar mass of $10^{10}$~M$_{\odot}$ seems to mark a change in the phases describing the time evolution of the bar and its impact on the interstellar medium. In massive discs (M$_{\star} \geq 10^{10}$~M$_{\odot}$), we observe the formation of a central gas reservoir with star formation mostly occurring within a restricted starburst region, leading to a gas depletion phase. Lower-mass systems (M$_{\star} < 10^{10}$~M$_{\odot}$) do not exhibit such a depletion phase, and show a more homogeneous spread of star-forming regions along the bar structure, and do not appear to host inner bar-driven discs or rings. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.09791v1-abstract-full').style.display = 'none'; document.getElementById('2404.09791v1-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 17 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 687, A53 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.01427">arXiv:2404.01427</a> <span> [<a href="https://arxiv.org/pdf/2404.01427">pdf</a>, <a href="https://arxiv.org/ps/2404.01427">ps</a>, <a href="https://arxiv.org/format/2404.01427">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/pasj/psae116">10.1093/pasj/psae116 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Quantitative analysis of the molecular gas morphology in nearby disk galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yamamoto%2C+T">Takashi Yamamoto</a>, <a href="/search/astro-ph?searchtype=author&query=Iono%2C+D">Daisuke Iono</a>, <a href="/search/astro-ph?searchtype=author&query=Saito%2C+T">Toshiki Saito</a>, <a href="/search/astro-ph?searchtype=author&query=Kuno%2C+N">Nario Kuno</a>, <a href="/search/astro-ph?searchtype=author&query=Stuber%2C+S+K">Sophia K. Stuber</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">Daizhong Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. 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="2404.01427v2-abstract-short" style="display: inline;"> We present a quantitative and statistical analysis of the molecular gas morphology in 73 nearby galaxies using high spatial resolution CO ($J$ = 2-1) data obtained from the Atacama Large Millimeter/submillimeter Array (ALMA) by the PHANGS large program. We applied three model-independent parameters: Concentration ($C$), Asymmetry ($A$), and Clumpiness ($S$) which are commonly used to parameterize… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.01427v2-abstract-full').style.display = 'inline'; document.getElementById('2404.01427v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.01427v2-abstract-full" style="display: none;"> We present a quantitative and statistical analysis of the molecular gas morphology in 73 nearby galaxies using high spatial resolution CO ($J$ = 2-1) data obtained from the Atacama Large Millimeter/submillimeter Array (ALMA) by the PHANGS large program. We applied three model-independent parameters: Concentration ($C$), Asymmetry ($A$), and Clumpiness ($S$) which are commonly used to parameterize the optical and infrared morphology of galaxies. We find a clear apparent correlation between $A$ and $S$, with a Spearman's rank correlation coefficient of $0.52$ with a $p$-value of $2\times10^{-6}$. This suggests a higher abundance of molecular clumps (i.e. giant molecular cloud associations) in galaxies that display stronger distortion or biased large-scale molecular gas distribution. In addition, the analysis of the $C$ parameter suggests high central molecular concentration in most barred spiral galaxies investigated in this study. Furthermore, we found a positive correlation between the length of the bar structure ($R_\mathrm{bar}/R_{25}$) and the $C$ parameter, with a Spearman's rank correlation coefficient of $0.63$ with a $p$-value of $3.8 \times 10^{-5}$, suggesting that larger bar structure can facilitate overall molecular gas transport and yield higher central concentration than galaxies with shorter bars. Finally, we offer a possible classification scheme of nearby disk galaxies which is based on the CAS parameters of molecular gas. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.01427v2-abstract-full').style.display = 'none'; document.getElementById('2404.01427v2-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 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 24 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/2403.13908">arXiv:2403.13908</a> <span> [<a href="https://arxiv.org/pdf/2403.13908">pdf</a>, <a href="https://arxiv.org/format/2403.13908">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/ad1889">10.3847/1538-3881/ad1889 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> PHANGS-HST: Globular Cluster Systems in 17 Nearby Spiral Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Floyd%2C+M">Matthew Floyd</a>, <a href="/search/astro-ph?searchtype=author&query=Chandar%2C+R">Rupali Chandar</a>, <a href="/search/astro-ph?searchtype=author&query=Whitmore%2C+B+C">Bradley C. Whitmore</a>, <a href="/search/astro-ph?searchtype=author&query=Thilker%2C+D+A">David A. Thilker</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J+C">Janice C. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Pauline%2C+R+E">Rachel E. Pauline</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+Z+L">Zion L. Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Berschback%2C+W+J">William J. Berschback</a>, <a href="/search/astro-ph?searchtype=author&query=Henny%2C+K+F">Kiana F. Henny</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">Daniel A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R+S">Ralf S. Klessen</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Grasha%2C+K">Kathryn Grasha</a>, <a href="/search/astro-ph?searchtype=author&query=Boquien%2C+M">Mederic Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Larson%2C+K+L">Kirsten L. Larson</a>, <a href="/search/astro-ph?searchtype=author&query=Deger%2C+S">Sinan Deger</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A+T">Ashley T. Barnes</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=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=Ubeda%2C+L">Leonardo Ubeda</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="2403.13908v1-abstract-short" style="display: inline;"> We present new catalogs of likely globular clusters (GCs) in 17 nearby spiral galaxies studied as part of the PHANGS-HST Treasury Survey. The galaxies were imaged in five broad-band filters from the near-ultraviolet through the $I$ band. PHANGS-HST has produced catalogs of stellar clusters of all ages by selecting extended sources (from multiple concentration index measurements) followed by morpho… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.13908v1-abstract-full').style.display = 'inline'; document.getElementById('2403.13908v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.13908v1-abstract-full" style="display: none;"> We present new catalogs of likely globular clusters (GCs) in 17 nearby spiral galaxies studied as part of the PHANGS-HST Treasury Survey. The galaxies were imaged in five broad-band filters from the near-ultraviolet through the $I$ band. PHANGS-HST has produced catalogs of stellar clusters of all ages by selecting extended sources (from multiple concentration index measurements) followed by morphological classification (centrally concentrated and symmetric or asymmetric, multiple peaks, contaminant) by visually examining the V-band image and separately by a machine-learning algorithm which classified larger samples to reach fainter limits. From both cluster catalogs, we select an initial list of candidate GCs to have $B-V \geq 0.5$ and $V-I \geq 0.73$~mag, then remove likely contaminants (including reddened young clusters, background galaxies misclassified by the neural network, and chance superpositions/blends of stars) after a careful visual inspection. We find that $\approx86$ % of the color-selected candidates classified as spherically symmetric, and $\approx68$ of those classified as centrally concentrated but asymmetric are likely to be GCs. The luminosity functions of the GC candidates in 2 of our 17 galaxies, NGC 628 and NGC 3627, are atypical, and continue to rise at least 1~mag fainter than the expected turnover near $M_V \sim -7.4$. These faint candidate GCs have more extended spatial distributions than their bright counterparts, and may reside in the disk rather than the bulge/halo, similar to faint GCs previously discovered in M101. These faint clusters may be somewhat younger since the age-metallicity degeneracy makes it difficult to determine precise cluster ages from integrated colors once they reach $\approx1$~Gyr. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.13908v1-abstract-full').style.display = 'none'; document.getElementById('2403.13908v1-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, 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">21 pages, 12 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astronomical Journal, Volume 167, Issue 3, id.95, 16 pp. March 2024 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.13751">arXiv:2403.13751</a> <span> [<a href="https://arxiv.org/pdf/2403.13751">pdf</a>, <a href="https://arxiv.org/format/2403.13751">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 properties and kinematics of HCN emission across the closest starburst galaxy NGC 253 observed with ALMA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Beslic%2C+I">Ivana Beslic</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A+T">Ashley T. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">Frank Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Jimenez-Donaire%2C+M+J">Maria Jesus Jimenez-Donaire</a>, <a href="/search/astro-ph?searchtype=author&query=Usero%2C+A">Antonio Usero</a>, <a href="/search/astro-ph?searchtype=author&query=Henshaw%2C+J+D">Jonathan D. Henshaw</a>, <a href="/search/astro-ph?searchtype=author&query=Faesi%2C+C">Christopher Faesi</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=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Brok%2C+J+S+d">Jakob S. den Brok</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">Melanie Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Eibensteiner%2C+C">Cosima Eibensteiner</a>, <a href="/search/astro-ph?searchtype=author&query=Grasha%2C+K">Kathryn Grasha</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R+S">Ralf S. Klessen</a>, <a href="/search/astro-ph?searchtype=author&query=Kruijssen%2C+J+M+D">J. M. Diedrerik Kruijssen</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">Daizhong Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Meidt%2C+S">Sharon Meidt</a>, <a href="/search/astro-ph?searchtype=author&query=Neumann%2C+J">Justus Neumann</a>, <a href="/search/astro-ph?searchtype=author&query=Neumann%2C+L">Lukas Neumann</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+H">Hsi-An Pan</a>, <a href="/search/astro-ph?searchtype=author&query=Puschnig%2C+J">Johannes Puschnig</a>, <a href="/search/astro-ph?searchtype=author&query=Querejeta%2C+M">Miguel Querejeta</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. 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="2403.13751v1-abstract-short" style="display: inline;"> Studying molecular gas in nearby galaxies using hydrogen cyanide (HCN) as a tracer for higher densities than CO emission still poses a significant challenge. Even though several galaxies have HCN maps on a few kpc scales, higher-resolution maps are still required. Our goal is to examine the contrast in intensity between two tracers that probe different density regimes - HCN(1-0)/CO(2-1) ratio - an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.13751v1-abstract-full').style.display = 'inline'; document.getElementById('2403.13751v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.13751v1-abstract-full" style="display: none;"> Studying molecular gas in nearby galaxies using hydrogen cyanide (HCN) as a tracer for higher densities than CO emission still poses a significant challenge. Even though several galaxies have HCN maps on a few kpc scales, higher-resolution maps are still required. Our goal is to examine the contrast in intensity between two tracers that probe different density regimes - HCN(1-0)/CO(2-1) ratio - and their kinematics across NGC 253. By utilizing the advanced capabilities of the Atacama Large Millimeter/submillimeter Array (ALMA), we can map these features at high resolution across a large field of view and uncover the nature of such dense gas in extragalactic systems. We present new ALMA Atacama Compact Array and Total Power (ACA+TP) observations of the HCN emission across NGC 253, covering the inner 8.6' of the galaxy disk at 300 pc scales. We analyze the integrated intensity and mean velocity of HCN and CO along each line of sight and use SCOUSE software to perform spectral decomposition, which considers each velocity component separately. Molecular gas traced by HCN piles up in a ring-like structure at a radius of 2 kpc. The HCN emission is enhanced by 2 orders of magnitude in the central 2 kpc regions, beyond which its intensity decreases with increasing galactocentric distance. The number of components in the HCN spectra shows a robust environmental dependence, with multiple velocity features across the center and bar. We have identified an increase in the HCN/CO ratio in these regions, corresponding to a velocity component likely associated with a molecular outflow. We have also discovered that the ratio between the total infrared luminosity and dense gas mass, which indicates the star formation efficiency of dense gas, is anti-correlated with the molecular gas surface density up to approximately 200 Msul/pc^2. In contrast, beyond this point, the ratio starts to increase. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.13751v1-abstract-full').style.display = 'none'; document.getElementById('2403.13751v1-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication to Astronomy and Astrophysics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.04901">arXiv:2403.04901</a> <span> [<a href="https://arxiv.org/pdf/2403.04901">pdf</a>, <a href="https://arxiv.org/format/2403.04901">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"> PHANGS-HST catalogs for $\sim$100,000 star clusters and compact associations in 38 galaxies: I. Observed properties </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Maschmann%2C+D">Daniel Maschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J+C">Janice C. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Thilker%2C+D+A">David A. Thilker</a>, <a href="/search/astro-ph?searchtype=author&query=Whitmore%2C+B+C">Bradley C. Whitmore</a>, <a href="/search/astro-ph?searchtype=author&query=Deger%2C+S">Sinan Deger</a>, <a href="/search/astro-ph?searchtype=author&query=Boquien%2C+M">Mederic Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Chandar%2C+R">Rupali Chandar</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">Daniel A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Wofford%2C+A">Aida Wofford</a>, <a href="/search/astro-ph?searchtype=author&query=Hannon%2C+S">Stephen Hannon</a>, <a href="/search/astro-ph?searchtype=author&query=Larson%2C+K+L">Kirsten L. Larson</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=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E+W">Erik W. Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Ubeda%2C+L">Leonardo Ubeda</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A">Ashley Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Grasha%2C+K">Kathryn Grasha</a>, <a href="/search/astro-ph?searchtype=author&query=Groves%2C+B">Brent Groves</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+H">Hwihyun Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R+S">Ralf S. Klessen</a>, <a href="/search/astro-ph?searchtype=author&query=Kreckel%2C+K">Kathryn Kreckel</a>, <a href="/search/astro-ph?searchtype=author&query=Levy%2C+R+C">Rebecca C. Levy</a>, <a href="/search/astro-ph?searchtype=author&query=Pinna%2C+F">Francesca Pinna</a>, <a href="/search/astro-ph?searchtype=author&query=Rodriguez%2C+J">Jimena Rodriguez</a> , et al. (2 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.04901v1-abstract-short" style="display: inline;"> We present the largest catalog to-date of star clusters and compact associations in nearby galaxies. We have performed a V-band-selected census of clusters across the 38 spiral galaxies of the PHANGS-HST Treasury Survey, and measured integrated, aperture-corrected NUV-U-B-V-I photometry. This work has resulted in uniform catalogs that contain $\sim$20,000 clusters and compact associations which ha… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.04901v1-abstract-full').style.display = 'inline'; document.getElementById('2403.04901v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.04901v1-abstract-full" style="display: none;"> We present the largest catalog to-date of star clusters and compact associations in nearby galaxies. We have performed a V-band-selected census of clusters across the 38 spiral galaxies of the PHANGS-HST Treasury Survey, and measured integrated, aperture-corrected NUV-U-B-V-I photometry. This work has resulted in uniform catalogs that contain $\sim$20,000 clusters and compact associations which have passed human inspection and morphological classification, and a larger sample of $\sim$100,000 classified by neural network models. Here, we report on the observed properties of these samples, and demonstrate that tremendous insight can be gained from just the observed properties of clusters, even in the absence of their transformation into physical quantities. In particular, we show the utility of the UBVI color-color diagram, and the three principal features revealed by the PHANGS-HST cluster sample: the young cluster locus, the middle-age plume, and the old globular cluster clump. We present an atlas of maps of the 2D spatial distribution of clusters and compact associations in the context of the molecular clouds from PHANGS-ALMA. We explore new ways of understanding this large dataset in a multi-scale context by bringing together once-separate techniques for the characterization of clusters (color-color diagrams and spatial distributions) and their parent galaxies (galaxy morphology and location relative to the galaxy main sequence). A companion paper presents the physical properties: ages, masses, and dust reddenings derived using improved spectral energy distribution (SED) fitting techniques. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.04901v1-abstract-full').style.display = 'none'; document.getElementById('2403.04901v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 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">48 pages, 26 figures, article in review 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/2402.04330">arXiv:2402.04330</a> <span> [<a href="https://arxiv.org/pdf/2402.04330">pdf</a>, <a href="https://arxiv.org/format/2402.04330">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"> PHANGS-ML: dissecting multiphase gas and dust in nearby galaxies using machine learning </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Baron%2C+D">Dalya Baron</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=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Egorov%2C+O+V">Oleg V. Egorov</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R+S">Ralf S. Klessen</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=Boquien%2C+M">M茅d茅ric Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Belfiore%2C+F">Francesco Belfiore</a>, <a href="/search/astro-ph?searchtype=author&query=Groves%2C+B">Brent Groves</a>, <a href="/search/astro-ph?searchtype=author&query=Chastenet%2C+J">J茅r茅my Chastenet</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">Daniel A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Blanc%2C+G+A">Guillermo A. Blanc</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%A9ndez-Delgado%2C+J+E">Jos茅 E. M茅ndez-Delgado</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=Grasha%2C+K">Kathryn Grasha</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">M茅lanie Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Thilker%2C+D+A">David A. Thilker</a>, <a href="/search/astro-ph?searchtype=author&query=Colombo%2C+D">Dario Colombo</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=Pathak%2C+D">Debosmita Pathak</a>, <a href="/search/astro-ph?searchtype=author&query=Sutter%2C+J">Jessica Sutter</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+T">Toby Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+J+F">John F. Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Peek%2C+J+E+G">J. E. G. Peek</a> , et al. (3 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2402.04330v1-abstract-short" style="display: inline;"> The PHANGS survey uses ALMA, HST, VLT, and JWST to obtain an unprecedented high-resolution view of nearby galaxies, covering millions of spatially independent regions. The high dimensionality of such a diverse multi-wavelength dataset makes it challenging to identify new trends, particularly when they connect observables from different wavelengths. Here we use unsupervised machine learning algorit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.04330v1-abstract-full').style.display = 'inline'; document.getElementById('2402.04330v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.04330v1-abstract-full" style="display: none;"> The PHANGS survey uses ALMA, HST, VLT, and JWST to obtain an unprecedented high-resolution view of nearby galaxies, covering millions of spatially independent regions. The high dimensionality of such a diverse multi-wavelength dataset makes it challenging to identify new trends, particularly when they connect observables from different wavelengths. Here we use unsupervised machine learning algorithms to mine this information-rich dataset to identify novel patterns. We focus on three of the PHANGS-JWST galaxies, for which we extract properties pertaining to their stellar populations; warm ionized and cold molecular gas; and Polycyclic Aromatic Hydrocarbons (PAHs), as measured over 150 pc-scale regions. We show that we can divide the regions into groups with distinct multiphase gas and PAH properties. In the process, we identify previously-unknown galaxy-wide correlations between PAH band and optical line ratios and use our identified groups to interpret them. The correlations we measure can be naturally explained in a scenario where the PAHs and the ionized gas are exposed to different parts of the same radiation field that varies spatially across the galaxies. This scenario has several implications for nearby galaxies: (i) The uniform PAH ionized fraction on 150 pc scales suggests significant self-regulation in the ISM, (ii) the PAH 11.3/7.7 \mic~ band ratio may be used to constrain the shape of the non-ionizing far-ultraviolet to optical part of the radiation field, and (iii) the varying radiation field affects line ratios that are commonly used as PAH size diagnostics. Neglecting this effect leads to incorrect or biased PAH sizes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.04330v1-abstract-full').style.display = 'none'; document.getElementById('2402.04330v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">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">Main results in figures 6 and 12. Submitted to ApJ, and comments are welcome!</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.15142">arXiv:2401.15142</a> <span> [<a href="https://arxiv.org/pdf/2401.15142">pdf</a>, <a href="https://arxiv.org/format/2401.15142">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"> PHANGS-JWST: Data Processing Pipeline and First Full Public Data Release </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J+C">Janice C. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Larson%2C+K+L">Kirsten L. Larson</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=Sandstrom%2C+K">Karin Sandstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Thilker%2C+D+A">David A. Thilker</a>, <a href="/search/astro-ph?searchtype=author&query=Belfiore%2C+F">Francesco Belfiore</a>, <a href="/search/astro-ph?searchtype=author&query=Egorov%2C+O+V">Oleg V. Egorov</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Sutter%2C+J">Jessica Sutter</a>, <a href="/search/astro-ph?searchtype=author&query=DePasquale%2C+J">Joseph DePasquale</a>, <a href="/search/astro-ph?searchtype=author&query=Pagan%2C+A">Alyssa Pagan</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+T+A">Travis A. Berger</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=Barnes%2C+A+T">Ashley T. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">Frank Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Boquien%2C+M">M茅d茅ric Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Y">Yixian Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Chastenet%2C+J">J茅r茅my Chastenet</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">M茅lanie Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Chown%2C+R">Ryan Chown</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">Daniel A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Deger%2C+S">Sinan Deger</a>, <a href="/search/astro-ph?searchtype=author&query=Eibensteiner%2C+C">Cosima Eibensteiner</a> , et al. (33 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.15142v3-abstract-short" style="display: inline;"> The exquisite angular resolution and sensitivity of JWST is opening a new window for our understanding of the Universe. In nearby galaxies, JWST observations are revolutionizing our understanding of the first phases of star formation and the dusty interstellar medium. Nineteen local galaxies spanning a range of properties and morphologies across the star-forming main sequence have been observed as… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.15142v3-abstract-full').style.display = 'inline'; document.getElementById('2401.15142v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.15142v3-abstract-full" style="display: none;"> The exquisite angular resolution and sensitivity of JWST is opening a new window for our understanding of the Universe. In nearby galaxies, JWST observations are revolutionizing our understanding of the first phases of star formation and the dusty interstellar medium. Nineteen local galaxies spanning a range of properties and morphologies across the star-forming main sequence have been observed as part of the PHANGS-JWST Cycle 1 Treasury program at spatial scales of $\sim$5-50pc. Here, we describe pjpipe, an image processing pipeline developed for the PHANGS-JWST program that wraps around and extends the official JWST pipeline. We release this pipeline to the community as it contains a number of tools generally useful for JWST NIRCam and MIRI observations. Particularly for extended sources, pjpipe products provide significant improvements over mosaics from the MAST archive in terms of removing instrumental noise in NIRCam data, background flux matching, and calibration of relative and absolute astrometry. We show that slightly smoothing F2100W MIRI data to 0.9" (degrading the resolution by about 30 percent) reduces the noise by a factor of $\approx$3. We also present the first public release (DR1.1.0) of the pjpipe processed eight-band 2-21 $渭$m imaging for all nineteen galaxies in the PHANGS-JWST Cycle 1 Treasury program. An additional 55 galaxies will soon follow from a new PHANGS-JWST Cycle 2 Treasury program. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.15142v3-abstract-full').style.display = 'none'; document.getElementById('2401.15142v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 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">49 pages (27 in Appendices), 54 Figures (39 in Appendices), 3 Tables. Accepted for publication in ApJS. Updated to match accepted version. Data available at https://archive.stsci.edu/hlsp/phangs/phangs-jwst</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.14453">arXiv:2401.14453</a> <span> [<a href="https://arxiv.org/pdf/2401.14453">pdf</a>, <a href="https://arxiv.org/format/2401.14453">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Hidden Gems on a Ring: Infant Massive Clusters and Their Formation Timeline Unveiled by ALMA, HST, and JWST in NGC 3351 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sun%2C+J">Jiayi Sun</a>, <a href="/search/astro-ph?searchtype=author&query=He%2C+H">Hao He</a>, <a href="/search/astro-ph?searchtype=author&query=Batschkun%2C+K">Kyle Batschkun</a>, <a href="/search/astro-ph?searchtype=author&query=Levy%2C+R+C">Rebecca C. Levy</a>, <a href="/search/astro-ph?searchtype=author&query=Emig%2C+K">Kimberly Emig</a>, <a href="/search/astro-ph?searchtype=author&query=Rodriguez%2C+M+J">M. Jimena Rodriguez</a>, <a href="/search/astro-ph?searchtype=author&query=Hassani%2C+H">Hamid Hassani</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=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Ostriker%2C+E+C">Eve C. Ostriker</a>, <a href="/search/astro-ph?searchtype=author&query=Wilson%2C+C+D">Christine D. Wilson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolatto%2C+A+D">Alberto D. Bolatto</a>, <a href="/search/astro-ph?searchtype=author&query=Mills%2C+E+A+C">Elisabeth A. C. Mills</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J+C">Janice C. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">Daniel A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Larson%2C+K+L">Kirsten L. Larson</a>, <a href="/search/astro-ph?searchtype=author&query=Thilker%2C+D+A">David A. Thilker</a>, <a href="/search/astro-ph?searchtype=author&query=Ubeda%2C+L">Leonardo Ubeda</a>, <a href="/search/astro-ph?searchtype=author&query=Whitmore%2C+B+C">Bradley C. Whitmore</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=Barnes%2C+A+T">Ashley. T. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">Frank Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">Melanie Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S+C+O">Simon C. O. Glover</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="2401.14453v2-abstract-short" style="display: inline;"> We study young massive clusters (YMCs) in their embedded "infant" phase with $\sim0.\!^{\prime\prime}1$ ALMA, HST, and JWST observations targeting the central starburst ring in NGC 3351, a nearby Milky Way analog galaxy. Our new ALMA data reveal 18 bright and compact (sub-)millimeter continuum sources, of which 8 have counterparts in JWST images and only 6 have counterparts in HST images. Based on… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.14453v2-abstract-full').style.display = 'inline'; document.getElementById('2401.14453v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.14453v2-abstract-full" style="display: none;"> We study young massive clusters (YMCs) in their embedded "infant" phase with $\sim0.\!^{\prime\prime}1$ ALMA, HST, and JWST observations targeting the central starburst ring in NGC 3351, a nearby Milky Way analog galaxy. Our new ALMA data reveal 18 bright and compact (sub-)millimeter continuum sources, of which 8 have counterparts in JWST images and only 6 have counterparts in HST images. Based on the ALMA continuum and molecular line data, as well as ancillary measurements for the HST and JWST counterparts, we identify 14 sources as infant star clusters with high stellar and/or gas masses (${\sim}10^5\;\mathrm{M_\odot}$), small radii (${\lesssim}\,5\;\mathrm{pc}$), large escape velocities ($6{-}10\;\mathrm{km/s}$), and short free-fall times ($0.5{-}1\;\mathrm{Myr}$). Their multiwavelength properties motivate us to divide them into four categories, likely corresponding to four evolutionary stages from starless clumps to exposed HII region-cluster complexes. Leveraging age estimates for HST-identified clusters in the same region, we infer an evolutionary timeline going from $\sim$1-2 Myr before cluster formation as starless clumps, to $\sim$4-6 Myr after as exposed HII region-cluster complexes. Finally, we show that the YMCs make up a substantial fraction of recent star formation across the ring, exhibit an non-uniform azimuthal distribution without a very coherent evolutionary trend along the ring, and are capable of driving large-scale gas outflows. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.14453v2-abstract-full').style.display = 'none'; document.getElementById('2401.14453v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 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">27 pages, 12 figures; ApJ 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/2312.06031">arXiv:2312.06031</a> <span> [<a href="https://arxiv.org/pdf/2312.06031">pdf</a>, <a href="https://arxiv.org/format/2312.06031">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 PHANGS-AstroSat Atlas of Nearby Star Forming Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hassani%2C+H">Hamid Hassani</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</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=Postma%2C+J">Joseph Postma</a>, <a href="/search/astro-ph?searchtype=author&query=Nofech%2C+J">Joseph Nofech</a>, <a href="/search/astro-ph?searchtype=author&query=Corbould%2C+H">Harrisen Corbould</a>, <a href="/search/astro-ph?searchtype=author&query=Thilker%2C+D">David Thilker</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=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Belfiore%2C+F">Francesco Belfiore</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">Frank Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Boquien%2C+M">Mederic Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">Melanie Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">Daniel A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Egorov%2C+O+V">Oleg V. Egorov</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S+C+O">Simon C. O. Glover</a>, <a href="/search/astro-ph?searchtype=author&query=Grasha%2C+K">Kathryn Grasha</a>, <a href="/search/astro-ph?searchtype=author&query=Groves%2C+B">Brent Groves</a>, <a href="/search/astro-ph?searchtype=author&query=Henny%2C+K">Kiana Henny</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+J">Jaeyeon Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R+S">Ralf S. Klessen</a>, <a href="/search/astro-ph?searchtype=author&query=Kreckel%2C+K">Kathryn Kreckel</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=Lee%2C+J+C">Janice C. Lee</a> , et al. (7 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.06031v1-abstract-short" style="display: inline;"> We present the Physics at High Angular resolution in Nearby GalaxieS (PHANGS)-AstroSat atlas, which contains ultraviolet imaging of 31 nearby star-forming galaxies captured by the Ultraviolet Imaging Telescope (UVIT) on the AstroSat satellite. The atlas provides a homogeneous data set of far- and near-ultraviolet maps of galaxies within a distance of 22 Mpc and a median angular resolution of 1.4 a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.06031v1-abstract-full').style.display = 'inline'; document.getElementById('2312.06031v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.06031v1-abstract-full" style="display: none;"> We present the Physics at High Angular resolution in Nearby GalaxieS (PHANGS)-AstroSat atlas, which contains ultraviolet imaging of 31 nearby star-forming galaxies captured by the Ultraviolet Imaging Telescope (UVIT) on the AstroSat satellite. The atlas provides a homogeneous data set of far- and near-ultraviolet maps of galaxies within a distance of 22 Mpc and a median angular resolution of 1.4 arcseconds (corresponding to a physical scale between 25 and 160 pc). After subtracting a uniform ultraviolet background and accounting for Milky Way extinction, we compare our estimated flux densities to GALEX observations, finding good agreement. We find candidate extended UV disks around the galaxies NGC 6744 and IC 5332. We present the first statistical measurements of the clumping of the UV emission and compare it to the clumping of molecular gas traced with ALMA. We find that bars and spiral arms exhibit the highest degree of clumping, and the molecular gas is even more clumped than the FUV emission in galaxies. We investigate the variation of the ratio of observed FUV to H$伪$ in different galactic environments and kpc-sized apertures. We report that $\sim 65 \%$ varation of the $\log_{10}$(FUV/H$伪$) can be described through a combination of dust attenuation with star formation history parameters. The PHANGS-AstroSat atlas enhances the multi-wavelength coverage of our sample, offering a detailed perspective on star formation. When integrated with PHANGS data sets from ALMA, VLT-MUSE, HST and JWST, it develops our comprehensive understanding of attenuation curves and dust attenuation in star-forming galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.06031v1-abstract-full').style.display = 'none'; document.getElementById('2312.06031v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 December, 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">35 pages, 16 figures. The survey webpage is available at https://sites.google.com/view/phangs/home/data/astrosat and the data archive can be accessed at https://www.canfar.net/storage/vault/list/phangs/RELEASES/PHANGS-AstroSat/v1p0</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.18067">arXiv:2311.18067</a> <span> [<a href="https://arxiv.org/pdf/2311.18067">pdf</a>, <a href="https://arxiv.org/format/2311.18067">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> A Two-Component Probability Distribution Function Describes the mid-IR Emission from the Disks of Star-Forming Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pathak%2C+D">Debosmita Pathak</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=Thompson%2C+T+A">Todd A. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Belfiore%2C+F">Francesco Belfiore</a>, <a href="/search/astro-ph?searchtype=author&query=Boquien%2C+M">Mederic Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">Daniel A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S+C+O">Simon C. O. Glover</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R+S">Ralf S. Klessen</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=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=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+R">Rowan Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+J">Jiayi Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Sutter%2C+J">Jessica Sutter</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=Bigiel%2C+F">Frank Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Y">Yixian Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Chastenet%2C+J">Jeremy Chastenet</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">Melanie Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Chown%2C+R">Ryan Chown</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Faesi%2C+C+M">Christopher M. Faesi</a>, <a href="/search/astro-ph?searchtype=author&query=Larson%2C+K+L">Kirsten L. Larson</a> , et al. (6 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.18067v1-abstract-short" style="display: inline;"> High-resolution JWST-MIRI images of nearby spiral galaxies reveal emission with complex substructures that trace dust heated both by massive young stars and the diffuse interstellar radiation field. We present high angular (0."85) and physical resolution (20-80 pc) measurements of the probability distribution function (PDF) of mid-infrared (mid-IR) emission (7.7-21 $渭$m) from 19 nearby star-formin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.18067v1-abstract-full').style.display = 'inline'; document.getElementById('2311.18067v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.18067v1-abstract-full" style="display: none;"> High-resolution JWST-MIRI images of nearby spiral galaxies reveal emission with complex substructures that trace dust heated both by massive young stars and the diffuse interstellar radiation field. We present high angular (0."85) and physical resolution (20-80 pc) measurements of the probability distribution function (PDF) of mid-infrared (mid-IR) emission (7.7-21 $渭$m) from 19 nearby star-forming galaxies from the PHANGS-JWST Cycle-1 Treasury. The PDFs of mid-IR emission from the disks of all 19 galaxies consistently show two distinct components: an approximately log-normal distribution at lower intensities and a high-intensity power-law component. These two components only emerge once individual star-forming regions are resolved. Comparing with locations of HII regions identified from VLT/MUSE H$伪$-mapping, we infer that the power-law component arises from star-forming regions and thus primarily traces dust heated by young stars. In the continuum-dominated 21 $渭$m band, the power-law is more prominent and contains roughly half of the total flux. At 7.7-11.3 $渭$m, the power-law is suppressed by the destruction of small grains (including PAHs) close to HII regions while the log-normal component tracing the dust column in diffuse regions appears more prominent. The width and shape of the log-normal diffuse emission PDFs in galactic disks remain consistent across our sample, implying a log-normal gas column density $N$(H)$\approx10^{21}$cm$^{-2}$ shaped by supersonic turbulence with typical (isothermal) turbulent Mach numbers $\approx5-15$. Finally, we describe how the PDFs of galactic disks are assembled from dusty HII regions and diffuse gas, and discuss how the measured PDF parameters correlate with global properties such as star-formation rate and gas surface density. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.18067v1-abstract-full').style.display = 'none'; document.getElementById('2311.18067v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">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">30 pages without appendix, 17 figures, (with appendix images of full sample: 56 pages, 39 figures), accepted 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/2311.17848">arXiv:2311.17848</a> <span> [<a href="https://arxiv.org/pdf/2311.17848">pdf</a>, <a href="https://arxiv.org/format/2311.17848">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"> WISDOM Project -- XVI. The link between circumnuclear molecular gas reservoirs and active galactic nucleus fuelling </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Elford%2C+J+S">Jacob S. Elford</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+A">Timothy A. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Ruffa%2C+I">Ilaria Ruffa</a>, <a href="/search/astro-ph?searchtype=author&query=Bureau%2C+M">Martin Bureau</a>, <a href="/search/astro-ph?searchtype=author&query=Cappellari%2C+M">Michele Cappellari</a>, <a href="/search/astro-ph?searchtype=author&query=Gensior%2C+J">Jindra Gensior</a>, <a href="/search/astro-ph?searchtype=author&query=Iguchi%2C+S">Satoru Iguchi</a>, <a href="/search/astro-ph?searchtype=author&query=Liang%2C+F">Fu-Heng Liang</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+L">Lijie Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Lu%2C+A">Anan Lu</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. 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="2311.17848v2-abstract-short" style="display: inline;"> We use high-resolution data from the millimetre-Wave Interferometric Survey of Dark Object Masses (WISDOM) project to investigate the connection between circumnuclear gas reservoirs and nuclear activity in a sample of nearby galaxies. Our sample spans a wide range of nuclear activity types including radio galaxies, Seyfert galaxies, low-luminosity active galactic nuclei (AGN) and inactive galaxies… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.17848v2-abstract-full').style.display = 'inline'; document.getElementById('2311.17848v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.17848v2-abstract-full" style="display: none;"> We use high-resolution data from the millimetre-Wave Interferometric Survey of Dark Object Masses (WISDOM) project to investigate the connection between circumnuclear gas reservoirs and nuclear activity in a sample of nearby galaxies. Our sample spans a wide range of nuclear activity types including radio galaxies, Seyfert galaxies, low-luminosity active galactic nuclei (AGN) and inactive galaxies. We use measurements of nuclear millimetre continuum emission along with other archival tracers of AGN accretion/activity to investigate previous claims that at, circumnuclear scales (<100 pc), these should correlate with the mass of the cold molecular gas. We find that the molecular gas mass does not correlate with any tracer of nuclear activity. This suggests the level of nuclear activity cannot solely be regulated by the amount of cold gas around the supermassive black hole (SMBH). This indicates that AGN fuelling, that drives gas from the large scale galaxy to the nuclear regions, is not a ubiquitous process and may vary between AGN type, with timescale variations likely to be very important. By studying the structure of the central molecular gas reservoirs, we find our galaxies have a range of nuclear molecular gas concentrations. This could indicate that some of our galaxies may have had their circumnuclear regions impacted by AGN feedback, even though they currently have low nuclear activity. On the other hand, the nuclear molecular gas concentrations in our galaxies could instead be set by secular processes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.17848v2-abstract-full').style.display = 'none'; document.getElementById('2311.17848v2-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 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 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">15 pages plus 3 in the appendix, 8 figures plus 1 in the appendix, 3 tables plus 4 in the appendix</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.15447">arXiv:2311.15447</a> <span> [<a href="https://arxiv.org/pdf/2311.15447">pdf</a>, <a href="https://arxiv.org/format/2311.15447">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"> WISDOM project -- XVIII. Molecular gas distributions and kinematics of three megamaser galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Liang%2C+F">Fu-Heng Liang</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+M+D">Mark D. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Bureau%2C+M">Martin Bureau</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+F">Feng Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+A">Timothy A. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Cappellari%2C+M">Michele Cappellari</a>, <a href="/search/astro-ph?searchtype=author&query=Elford%2C+J+S">Jacob S. Elford</a>, <a href="/search/astro-ph?searchtype=author&query=Greene%2C+J+E">Jenny E. Greene</a>, <a href="/search/astro-ph?searchtype=author&query=Iguchi%2C+S">Satoru Iguchi</a>, <a href="/search/astro-ph?searchtype=author&query=Lelli%2C+F">Federico Lelli</a>, <a href="/search/astro-ph?searchtype=author&query=Lu%2C+A">Anan Lu</a>, <a href="/search/astro-ph?searchtype=author&query=Ruffa%2C+I">Ilaria Ruffa</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=Zhang%2C+H">Hengyue Zhang</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="2311.15447v2-abstract-short" style="display: inline;"> The co-evolution of galaxies and supermassive black holes (SMBHs) underpins our understanding of galaxy evolution, but different methods to measure SMBH masses have only infrequently been cross-checked. We attempt to identify targets to cross-check two of the most accurate methods, megamaser and cold molecular gas dynamics. Three promising galaxies are selected from all those with existing megamas… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.15447v2-abstract-full').style.display = 'inline'; document.getElementById('2311.15447v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.15447v2-abstract-full" style="display: none;"> The co-evolution of galaxies and supermassive black holes (SMBHs) underpins our understanding of galaxy evolution, but different methods to measure SMBH masses have only infrequently been cross-checked. We attempt to identify targets to cross-check two of the most accurate methods, megamaser and cold molecular gas dynamics. Three promising galaxies are selected from all those with existing megamaser SMBH mass measurements. We present Atacama Large Millimeter/sub-millimeter Array (ALMA) 12CO(2-1) and 230-GHz continuum observations with angular resolutions of about 0.5". Every galaxy has an extended rotating molecular gas disc and 230-GHz continuum source(s), but all also have irregularities and/or non-axisymmetric features: NGC1194 is highly inclined and has disturbed and lopsided central 12CO(2-1) emission; NGC3393 has a nuclear disc with fairly regular but patchy 12CO(2-1) emission with little gas near the kinematic major axis, faint emission in the very centre and two brighter structures reminiscent of a nuclear ring and/or spiral; NGC5765B has a strong bar and very bright 12CO(2-1) emission concentrated along two bisymmetric offset dust lanes and two bisymmetric nuclear spiral arms. 12CO(2-1) and 12CO(3-2) observations with the James Clerk Maxwell Telescope are compared with the ALMA observations. Because of the disturbed gas kinematics and the impractically long integration times required for higher angular resolution observations, none of the three galaxies is suitable for a future SMBH mass measurement. Nonetheless, increasing the number of molecular gas observations of megamaser galaxies is valuable, and the ubiquitous disturbances suggest a link between large-scale gas properties and the existence of megamasers. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.15447v2-abstract-full').style.display = 'none'; document.getElementById('2311.15447v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 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">17 pages, 5 figures, accepted by MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.00407">arXiv:2311.00407</a> <span> [<a href="https://arxiv.org/pdf/2311.00407">pdf</a>, <a href="https://arxiv.org/format/2311.00407">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"> Resolved Measurements of the CO-to-H$_2$ Conversion Factor in 37 Nearby Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chiang%2C+I">I-Da Chiang</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=Chastenet%2C+J">Jeremy Chastenet</a>, <a href="/search/astro-ph?searchtype=author&query=Bolatto%2C+A+D">Alberto D. Bolatto</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=Leroy%2C+A+K">Adam K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+J">Jiayi Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Teng%2C+Y">Yu-Hsuan Teng</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. 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="2311.00407v2-abstract-short" style="display: inline;"> We measure the CO-to-H$_2$ conversion factor ($伪_\mathrm{CO}$) in 37 galaxies at 2~kpc resolution, using dust surface density inferred from far-infrared emission as a tracer of the gas surface density and assuming a constant dust-to-metals ratio. In total, we have $\sim790$ and $\sim610$ independent measurements of $伪_\mathrm{CO}$ for CO (2-1) and (1-0), respectively. The mean values for… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.00407v2-abstract-full').style.display = 'inline'; document.getElementById('2311.00407v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.00407v2-abstract-full" style="display: none;"> We measure the CO-to-H$_2$ conversion factor ($伪_\mathrm{CO}$) in 37 galaxies at 2~kpc resolution, using dust surface density inferred from far-infrared emission as a tracer of the gas surface density and assuming a constant dust-to-metals ratio. In total, we have $\sim790$ and $\sim610$ independent measurements of $伪_\mathrm{CO}$ for CO (2-1) and (1-0), respectively. The mean values for $伪_\mathrm{CO~(2-1)}$ and $伪_\mathrm{CO~(1-0)}$ are $9.3^{+4.6}_{-5.4}$ and $4.2^{+1.9}_{-2.0}~M_\odot~pc^{-2}~(K~km~s^{-1})^{-1}$, respectively. The CO-intensity-weighted mean for $伪_\mathrm{CO~(2-1)}$ is 5.69, and 3.33 for $伪_\mathrm{CO~(1-0)}$. We examine how $伪_\mathrm{CO}$ scales with several physical quantities, e.g.\ star-formation rate (SFR), stellar mass, and dust-mass-weighted average interstellar radiation field strength ($\overline{U}$). Among them, $\overline{U}$, $危_{\rm SFR}$, and integrated CO intensity ($W_\mathrm{CO}$) have the strongest anti-correlation with spatially resolved $伪_\mathrm{CO}$. We provide linear regression results to \aco for all quantities tested. At galaxy integrated scales, we observe significant correlations between $伪_\mathrm{CO}$ and $W_\mathrm{CO}$, metallicity, $\overline{U}$, and $危_{\rm SFR}$. We also find that the normalized $伪_\mathrm{CO}$ decreases with stellar mass surface density ($危_\star$) in the high surface density regions ($危_\star\geq100~{\rm M_\odot~pc^{-2}}$), following the power-law relations $伪_\mathrm{CO~(2-1)}\propto危_\star^{-0.5}$ and $伪_\mathrm{CO~(1-0)}\propto危_\star^{-0.2}$. The power-law index is insensitive to the assumed dust-to-metals ratio. (abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.00407v2-abstract-full').style.display = 'none'; document.getElementById('2311.00407v2-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 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 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">27 pages, 13 figures, 4 tables, submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.18407">arXiv:2310.18407</a> <span> [<a href="https://arxiv.org/pdf/2310.18407">pdf</a>, <a href="https://arxiv.org/format/2310.18407">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"> Resolved low-J $^{12}$CO excitation at 190 parsec resolution across NGC 2903 and NGC 3627 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Brok%2C+J+S+d">J. S. den Brok</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A+K">A. K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Usero%2C+A">A. Usero</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">E. Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">E. Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Koch%2C+E+W">E. W. Koch</a>, <a href="/search/astro-ph?searchtype=author&query=Querejeta%2C+M">M. Querejeta</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">D. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">F. Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A+T">A. T. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">M. Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Colombo%2C+D">D. Colombo</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">D. A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S+C+O">S. C. O. Glover</a>, <a href="/search/astro-ph?searchtype=author&query=Jimenez-Donaire%2C+M+J">M. J. Jimenez-Donaire</a>, <a href="/search/astro-ph?searchtype=author&query=Teng%2C+Y+-">Y. -H. Teng</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">T. G. 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="2310.18407v1-abstract-short" style="display: inline;"> The low-$J$ rotational transitions of $^{12}$CO are commonly used to trace the distribution of molecular gas in galaxies. Their ratios are sensitive to excitation and physical conditions in the molecular gas. Spatially resolved studies of CO ratios are still sparse and affected by flux calibration uncertainties, especially since most do not have high angular resolution or do not have short-spacing… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.18407v1-abstract-full').style.display = 'inline'; document.getElementById('2310.18407v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.18407v1-abstract-full" style="display: none;"> The low-$J$ rotational transitions of $^{12}$CO are commonly used to trace the distribution of molecular gas in galaxies. Their ratios are sensitive to excitation and physical conditions in the molecular gas. Spatially resolved studies of CO ratios are still sparse and affected by flux calibration uncertainties, especially since most do not have high angular resolution or do not have short-spacing information and hence miss any diffuse emission. We compare the low-$J$ CO ratios across the disk of two massive, star-forming spiral galaxies NGC2903 and NGC3627 to investigate whether and how local environments drive excitation variations at GMC scales. We use Atacama Large Millimeter Array (ALMA) observations of the three lowest-$J$ CO transitions at a common angular resolution of 4$''$ (190pc). We measure median line ratios of $R_{21}=0.67^{+0.13}_{-0.11}$, $R_{32}=0.33^{+0.09}_{-0.08}$, and $R_{31}=0.24^{+0.10}_{-0.09}$ across the full disk of NGC3627. We see clear CO line ratio variation across the galaxy consistent with changes in temperature and density of the molecular gas. In particular, toward the center, $R_{21}$, $R_{32}$, and $R_{31}$ increase by 35\%, 50\%, and 66\%, respectively compared to their average disk values. The overall line ratio trends suggest that CO(3-2) is more sensitive to changes in the excitation conditions than the two lower-$J$ transitions. Furthermore, we find a similar radial $R_{32}$ trend in NGC2903, albite a larger disk-wide average of $\langle R_{32}\rangle=0.47^{+0.14}_{-0.08}$. We conclude that the CO low-$J$ line ratios vary across environments in such a way that they can trace changes in the molecular gas conditions, with the main driver being changes in temperature. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.18407v1-abstract-full').style.display = 'none'; document.getElementById('2310.18407v1-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 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 for publication in MNRAS, 17 pages, 16 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/2310.17694">arXiv:2310.17694</a> <span> [<a href="https://arxiv.org/pdf/2310.17694">pdf</a>, <a href="https://arxiv.org/format/2310.17694">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"> Where do stars explode in the ISM? -- The distribution of dense gas around massive stars and supernova remnants in M33 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sarbadhicary%2C+S+K">Sumit K. Sarbadhicary</a>, <a href="/search/astro-ph?searchtype=author&query=Wagner%2C+J">Jordan Wagner</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=Chen%2C+N+M">Ness Mayker Chen</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=Lah%C3%A9n%2C+N">Natalia Lah茅n</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Neugent%2C+K+F">Kathryn F. Neugent</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+C">Chang-Goo Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Chomiuk%2C+L">Laura Chomiuk</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=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Pingel%2C+N+M">Nickolas M. Pingel</a>, <a href="/search/astro-ph?searchtype=author&query=Indebetouw%2C+R">Remy Indebetouw</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=Tarantino%2C+E">Elizabeth Tarantino</a>, <a href="/search/astro-ph?searchtype=author&query=Meyer%2C+J+D">Jennifer Donovan Meyer</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=Kepley%2C+A+A">Amanda A. Kepley</a>, <a href="/search/astro-ph?searchtype=author&query=Murphy%2C+E+J">Eric J. Murphy</a>, <a href="/search/astro-ph?searchtype=author&query=Strader%2C+J">Jay Strader</a>, <a href="/search/astro-ph?searchtype=author&query=Wong%2C+T">Tony Wong</a>, <a href="/search/astro-ph?searchtype=author&query=Stanimirovi%C4%87%2C+S">Sne啪ana Stanimirovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Villanueva%2C+V">Vicente Villanueva</a> , et al. (5 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.17694v1-abstract-short" style="display: inline;"> Star formation in galaxies is regulated by turbulence, outflows, gas heating and cloud dispersal -- processes which depend sensitively on the properties of the interstellar medium (ISM) into which supernovae (SNe) explode. Unfortunately, direct measurements of ISM environments around SNe remain scarce, as SNe are rare and often distant. Here we demonstrate a new approach: mapping the ISM around th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.17694v1-abstract-full').style.display = 'inline'; document.getElementById('2310.17694v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.17694v1-abstract-full" style="display: none;"> Star formation in galaxies is regulated by turbulence, outflows, gas heating and cloud dispersal -- processes which depend sensitively on the properties of the interstellar medium (ISM) into which supernovae (SNe) explode. Unfortunately, direct measurements of ISM environments around SNe remain scarce, as SNe are rare and often distant. Here we demonstrate a new approach: mapping the ISM around the massive stars that are soon to explode. This provides a much larger census of explosion sites than possible with only SNe, and allows comparison with sensitive, high-resolution maps of the atomic and molecular gas from the Jansky VLA and ALMA. In the well-resolved Local Group spiral M33, we specifically observe the environments of red supergiants (RSGs, progenitors of Type II SNe), Wolf-Rayet stars (WRs, tracing stars $>$30 M$_{\odot}$, and possibly future stripped-envelope SNe), and supernova remnants (SNRs, locations where SNe have exploded). We find that massive stars evolve not only in dense, molecular-dominated gas (with younger stars in denser gas), but also a substantial fraction ($\sim$45\% of WRs; higher for RSGs) evolve in lower-density, atomic-gas-dominated, inter-cloud media. We show that these measurements are consistent with expectations from different stellar-age tracer maps, and can be useful for validating SN feedback models in numerical simulations of galaxies. Along with the discovery of a 20-pc diameter molecular gas cavity around a WR, these findings re-emphasize the importance of pre-SN/correlated-SN feedback evacuating the dense gas around massive stars before explosion, and the need for high-resolution (down to pc-scale) surveys of the multi-phase ISM in nearby galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.17694v1-abstract-full').style.display = 'none'; document.getElementById('2310.17694v1-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 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">34 pages, 14 figures. Submitted to ApJ. Comments welcome! The density distributions will be made publicly available after journal acceptance of manuscript. Please feel free to contact us in the meantime if you would like to use them</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.16037">arXiv:2310.16037</a> <span> [<a href="https://arxiv.org/pdf/2310.16037">pdf</a>, <a href="https://arxiv.org/format/2310.16037">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"> Star Formation Efficiency in Nearby Galaxies Revealed with a New CO-to-H2 Conversion Factor Prescription </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Teng%2C+Y">Yu-Hsuan Teng</a>, <a href="/search/astro-ph?searchtype=author&query=Chiang%2C+I">I-Da Chiang</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=Sun%2C+J">Jiayi Sun</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=Bolatto%2C+A+D">Alberto D. Bolatto</a>, <a href="/search/astro-ph?searchtype=author&query=Usero%2C+A">Antonio Usero</a>, <a href="/search/astro-ph?searchtype=author&query=Ostriker%2C+E+C">Eve C. Ostriker</a>, <a href="/search/astro-ph?searchtype=author&query=Querejeta%2C+M">Miguel Querejeta</a>, <a href="/search/astro-ph?searchtype=author&query=Chastenet%2C+J">Jeremy Chastenet</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">Frank Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Boquien%2C+M">Mederic Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Brok%2C+J+d">Jakob den Brok</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Y">Yixian Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">Melanie Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Chown%2C+R">Ryan Chown</a>, <a href="/search/astro-ph?searchtype=author&query=Colombo%2C+D">Dario Colombo</a>, <a href="/search/astro-ph?searchtype=author&query=Eibensteiner%2C+C">Cosima Eibensteiner</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S+C+O">Simon C. O. Glover</a>, <a href="/search/astro-ph?searchtype=author&query=Grasha%2C+K">Kathryn Grasha</a>, <a href="/search/astro-ph?searchtype=author&query=Henshaw%2C+J+D">Jonathan D. Henshaw</a>, <a href="/search/astro-ph?searchtype=author&query=Jimenez-Donaire%2C+M+J">Maria J. Jimenez-Donaire</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">Daizhong Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Murphy%2C+E+J">Eric J. Murphy</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+H">Hsi-An Pan</a> , et al. (2 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.16037v2-abstract-short" style="display: inline;"> Determining how galactic environment, especially the high gas densities and complex dynamics in bar-fed galaxy centers, alters the star formation efficiency (SFE) of molecular gas is critical to understanding galaxy evolution. However, these same physical or dynamical effects also alter the emissivity properties of CO, leading to variations in the CO-to-H$_2$ conversion factor ($伪_\rm{CO}$) that i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.16037v2-abstract-full').style.display = 'inline'; document.getElementById('2310.16037v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.16037v2-abstract-full" style="display: none;"> Determining how galactic environment, especially the high gas densities and complex dynamics in bar-fed galaxy centers, alters the star formation efficiency (SFE) of molecular gas is critical to understanding galaxy evolution. However, these same physical or dynamical effects also alter the emissivity properties of CO, leading to variations in the CO-to-H$_2$ conversion factor ($伪_\rm{CO}$) that impact the assessment of the gas column densities and thus of the SFE. To address such issues, we investigate the dependence of $伪_\rm{CO}$ on local CO velocity dispersion at 150-pc scales using a new set of dust-based $伪_\rm{CO}$ measurements, and propose a new $伪_\rm{CO}$ prescription that accounts for CO emissivity variations across galaxies. Based on this prescription, we estimate the SFE in a sample of 65 galaxies from the PHANGS-ALMA survey. We find increasing SFE towards high surface density regions like galaxy centers, while using a constant or metallicity-based $伪_\rm{CO}$ results in a more homogeneous SFE throughout the centers and disks. Our prescription further reveals a mean molecular gas depletion time of 700 Myr in the centers of barred galaxies, which is overall 3-4 times shorter than in non-barred galaxy centers or the disks. Across the galaxy disks, the depletion time is consistently around 2-3 Gyr regardless of the choice of $伪_\rm{CO}$ prescription. All together, our results suggest that the high level of star formation activity in barred centers is not simply due to an increased amount of molecular gas but also an enhanced SFE compared to non-barred centers or disk regions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.16037v2-abstract-full').style.display = 'none'; document.getElementById('2310.16037v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 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">12 pages of main text, 4 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/2310.06890">arXiv:2310.06890</a> <span> [<a href="https://arxiv.org/pdf/2310.06890">pdf</a>, <a href="https://arxiv.org/format/2310.06890">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 WISDOM of power spectra: how the galactic gravitational potential impacts a galaxy's central gas reservoir in simulations and observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gensior%2C+J">Jindra Gensior</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+A">Timothy A. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Bureau%2C+M">Martin Bureau</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=Cappellari%2C+M">Michele Cappellari</a>, <a href="/search/astro-ph?searchtype=author&query=Ruffa%2C+I">Ilaria Ruffa</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. 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="2310.06890v1-abstract-short" style="display: inline;"> Observations indicate that the central gas discs are smoother in early-type galaxies than their late-type counterparts, while recent simulations predict that the dynamical suppression of star formation in spheroid-dominated galaxies is preceded by the suppression of fragmentation of their interstellar media. The mass surface density power spectrum is a powerful tool to constrain the degree of stru… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.06890v1-abstract-full').style.display = 'inline'; document.getElementById('2310.06890v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.06890v1-abstract-full" style="display: none;"> Observations indicate that the central gas discs are smoother in early-type galaxies than their late-type counterparts, while recent simulations predict that the dynamical suppression of star formation in spheroid-dominated galaxies is preceded by the suppression of fragmentation of their interstellar media. The mass surface density power spectrum is a powerful tool to constrain the degree of structure within a gas reservoir. Specifically here, we focus on the power spectrum slope and aim to constrain whether the shear induced by a dominant spheroidal potential can induce sufficient turbulence to suppress fragmentation, resulting in the smooth central gas discs observed. We compute surface density power spectra for the nuclear gas reservoirs of fourteen simulated isolated galaxies and twelve galaxies observed as part of the mm-Wave Interferometric Survey of Dark Object Masses (WISDOM) project. Both simulated and observed galaxies range from disc-dominated galaxies to spheroids, with central stellar mass surface densities, a measure of bulge dominance, varying by more than an order of magnitude. For the simulations, the power spectra steepen with increasing central stellar mass surface density, thereby clearly linking the suppression of fragmentation to the shear-driven turbulence induced by the spheroid. The WISDOM observations show a different (but potentially consistent) picture: while there is no correlation between the power spectrum slopes and the central stellar mass surface densities, the slopes scatter around a value of 2.6. This is similar to the behaviour of the slopes of the simulated galaxies with high central stellar mass surface densities, and could indicate that high shear eventually drives incompressible turbulence. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.06890v1-abstract-full').style.display = 'none'; document.getElementById('2310.06890v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 October, 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">14 pages, 7 figures + appendices (7 pages, 9 figures); accepted by MNRAS (October 09th, 2023)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.06501">arXiv:2310.06501</a> <span> [<a href="https://arxiv.org/pdf/2310.06501">pdf</a>, <a href="https://arxiv.org/format/2310.06501">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202143023">10.1051/0004-6361/202143023 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A sensitive, high-resolution, wide-field IRAM NOEMA CO(1-0) survey of the very nearby spiral galaxy IC 342 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Querejeta%2C+M">M. Querejeta</a>, <a href="/search/astro-ph?searchtype=author&query=Pety%2C+J">J. Pety</a>, <a href="/search/astro-ph?searchtype=author&query=Schruba%2C+A">A. Schruba</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A+K">A. K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Herrera%2C+C+N">C. N. Herrera</a>, <a href="/search/astro-ph?searchtype=author&query=Chiang%2C+I">I-D. Chiang</a>, <a href="/search/astro-ph?searchtype=author&query=Meidt%2C+S+E">S. E. Meidt</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">E. Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">E. Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Schuster%2C+K">K. Schuster</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+J">J. Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Herrmann%2C+K+A">K. A. Herrmann</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A+T">A. T. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Beslic%2C+I">I. Beslic</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">F. Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Y">Y. Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">M. Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Eibensteiner%2C+C">C. Eibensteiner</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">E. Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Faesi%2C+C+M">C. M. Faesi</a>, <a href="/search/astro-ph?searchtype=author&query=Hughes%2C+A">A. Hughes</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+J">J. Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R+S">R. S. Klessen</a>, <a href="/search/astro-ph?searchtype=author&query=Kreckel%2C+K">K. Kreckel</a>, <a href="/search/astro-ph?searchtype=author&query=Kruijssen%2C+J+M+D">J. M. D. Kruijssen</a> , et al. (9 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.06501v1-abstract-short" style="display: inline;"> We present a new wide-field 10.75 x 10.75 arcmin^2 (~11x11 kpc^2), high-resolution (theta = 3.6" ~ 60 pc) NOEMA CO(1-0) survey of the very nearby (d=3.45 Mpc) spiral galaxy IC 342. The survey spans out to about 1.5 effective radii and covers most of the region where molecular gas dominates the cold interstellar medium. We resolved the CO emission into >600 individual giant molecular clouds and ass… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.06501v1-abstract-full').style.display = 'inline'; document.getElementById('2310.06501v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.06501v1-abstract-full" style="display: none;"> We present a new wide-field 10.75 x 10.75 arcmin^2 (~11x11 kpc^2), high-resolution (theta = 3.6" ~ 60 pc) NOEMA CO(1-0) survey of the very nearby (d=3.45 Mpc) spiral galaxy IC 342. The survey spans out to about 1.5 effective radii and covers most of the region where molecular gas dominates the cold interstellar medium. We resolved the CO emission into >600 individual giant molecular clouds and associations. We assessed their properties and found that overall the clouds show approximate virial balance, with typical virial parameters of alpha_vir=1-2. The typical surface density and line width of molecular gas increase from the inter-arm region to the arm and bar region, and they reach their highest values in the inner kiloparsec of the galaxy (median Sigma_mol~80, 140, 160, and 1100 M_sun/pc^2, sigma_CO~6.6, 7.6, 9.7, and 18.4 km/s for inter-arm, arm, bar, and center clouds, respectively). Clouds in the central part of the galaxy show an enhanced line width relative to their surface densities and evidence of additional sources of dynamical broadening. All of these results agree well with studies of clouds in more distant galaxies at a similar physical resolution. Leveraging our measurements to estimate the density and gravitational free-fall time at 90 pc resolution, averaged on 1.5 kpc hexagonal apertures, we estimate a typical star formation efficiency per free-fall time of 0.45% with a 16-84% variation of 0.33-0.71% among such 1.5 kpc regions. We speculate that bar-driven gas inflow could explain the large gas concentration in the central kiloparsec and the buildup of the massive nuclear star cluster. This wide-area CO map of the closest face-on massive spiral galaxy demonstrates the current mapping power of NOEMA and has many potential applications. The data and products are publicly available. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.06501v1-abstract-full').style.display = 'none'; document.getElementById('2310.06501v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 6 figures, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 680, A4 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.17440">arXiv:2309.17440</a> <span> [<a href="https://arxiv.org/pdf/2309.17440">pdf</a>, <a href="https://arxiv.org/format/2309.17440">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"> Investigating the Drivers of Electron Temperature Variations in HII Regions with Keck-KCWI and VLT-MUSE </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vaught%2C+R+J+R">Ryan J. Rickards Vaught</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=Belfiore%2C+F">Francesco Belfiore</a>, <a href="/search/astro-ph?searchtype=author&query=Kreckel%2C+K">Kathryn Kreckel</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%A9ndez-Delgado%2C+J+E">J. Eduardo M茅ndez-Delgado</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Groves%2C+B">Brent Groves</a>, <a href="/search/astro-ph?searchtype=author&query=Blanc%2C+G+A">Guillermo A. Blanc</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">Daniel A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Egorov%2C+O+V">Oleg V. Egorov</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S+C+O">Simon C. O. Glover</a>, <a href="/search/astro-ph?searchtype=author&query=Grasha%2C+K">Kathryn Grasha</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R+S">Ralf S. Klessen</a>, <a href="/search/astro-ph?searchtype=author&query=Neumann%2C+J">Justus Neumann</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. 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="2309.17440v2-abstract-short" style="display: inline;"> HII region electron temperatures are a critical ingredient in metallicity determinations and recent observations reveal systematic variations in the temperatures measured using different ions. We present electron temperatures ($T_e$) measured using the optical auroral lines ([NII]$\lambda5756$, [OII]$位\lambda7320,7330$, [SII]$位\lambda4069,4076$, [OIII]$\lambda4363$, and [SIII]$\lambda6312$) for a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.17440v2-abstract-full').style.display = 'inline'; document.getElementById('2309.17440v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.17440v2-abstract-full" style="display: none;"> HII region electron temperatures are a critical ingredient in metallicity determinations and recent observations reveal systematic variations in the temperatures measured using different ions. We present electron temperatures ($T_e$) measured using the optical auroral lines ([NII]$\lambda5756$, [OII]$位\lambda7320,7330$, [SII]$位\lambda4069,4076$, [OIII]$\lambda4363$, and [SIII]$\lambda6312$) for a sample of HII regions in seven nearby galaxies. We use observations from the Physics at High Angular resolution in Nearby Galaxies survey (PHANGS) obtained with integral field spectrographs on Keck (Keck Cosmic Web Imager; KCWI) and the Very Large Telescope (Multi-Unit Spectroscopic Explorer; MUSE). We compare the different $T_e$ measurements with HII region and interstellar medium environmental properties such as electron density, ionization parameter, molecular gas velocity dispersion, and stellar association/cluster mass and age obtained from PHANGS. We find that the temperatures from [OII] and [SII] are likely over-estimated due to the presence of electron density inhomogeneities in HII regions. We observe that differences between [NII] and [SIII] temperatures are weakly correlated with stellar association mass and molecular gas velocity dispersion. We measure high [OIII] temperatures in a subset of regions with high molecular gas velocity dispersion and low ionization parameter, which may be explained by the presence of low-velocity shocks. In agreement with previous studies, the $T_{\rm{e}}$--$T_{\rm{e}}$ between [NII] and [SIII] temperatures have the lowest observed scatter and generally follow predictions from photoionization modeling, which suggests that these tracers reflect HII region temperatures across the various ionization zones better than [OII], [SII], and [OIII]. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.17440v2-abstract-full').style.display = 'none'; document.getElementById('2309.17440v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 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">Accepted to ApJ, 66 pages, 36 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.05146">arXiv:2308.05146</a> <span> [<a href="https://arxiv.org/pdf/2308.05146">pdf</a>, <a href="https://arxiv.org/format/2308.05146">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"> WISDOM Project -- XVII. Beam-by-beam Properties of the Molecular Gas in Early-type Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Bureau%2C+M">Martin Bureau</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+A">Timothy A. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Cappellari%2C+M">Michele Cappellari</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+W">Woorak Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Elford%2C+J+S">Jacob S. Elford</a>, <a href="/search/astro-ph?searchtype=author&query=Iguchi%2C+S">Satoru Iguchi</a>, <a href="/search/astro-ph?searchtype=author&query=Gensior%2C+J">Jindra Gensior</a>, <a href="/search/astro-ph?searchtype=author&query=Liang%2C+F">Fu-Heng Liang</a>, <a href="/search/astro-ph?searchtype=author&query=Lu%2C+A">Anan Lu</a>, <a href="/search/astro-ph?searchtype=author&query=Ruffa%2C+I">Ilaria Ruffa</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+H">Hengyue Zhang</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="2308.05146v1-abstract-short" style="display: inline;"> We present a study of the molecular gas of seven early-type galaxies with high angular resolution data obtained as part of the mm-Wave Interferometric Survey of Dark Object Masses (WISDOM) project with the Atacama Large Millimeter/submillimeter Array. Using a fixed spatial scale approach, we study the mass surface density ($危$) and velocity dispersion ($蟽$) of the molecular gas on spatial scales r… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.05146v1-abstract-full').style.display = 'inline'; document.getElementById('2308.05146v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.05146v1-abstract-full" style="display: none;"> We present a study of the molecular gas of seven early-type galaxies with high angular resolution data obtained as part of the mm-Wave Interferometric Survey of Dark Object Masses (WISDOM) project with the Atacama Large Millimeter/submillimeter Array. Using a fixed spatial scale approach, we study the mass surface density ($危$) and velocity dispersion ($蟽$) of the molecular gas on spatial scales ranging from $60$ to $120$pc. Given the spatial resolution of our data ($20$ - $70$pc), we characterise these properties across many thousands of individual sight lines ($\approx50,000$ at our highest physical resolution). The molecular gas along these sight lines has a large range ($\approx2$dex) of mass surface densities and velocity dispersions $\approx40\%$ higher than those of star-forming spiral galaxies. It has virial parameters $伪_\mathrm{vir}$ that depend weakly on the physical scale observed, likely due to beam smearing of the bulk galactic rotation, and is generally super-virial. Comparing the internal turbulent pressure ($P_\mathrm{turb}$) to the pressure required for dynamic equilibrium ($P_\mathrm{DE}$), the ratio $P_\mathrm{turb}$/$P_\mathrm{DE}$ is significantly less than unity in all galaxies, indicating that the gas is not in dynamic equilibrium and is strongly compressed, in apparent contradiction to the virial parameters. This may be due to our neglect of shear and tidal forces, and/or the combination of three-dimensional and vertical diagnostics. Both $伪_\mathrm{vir}$ and $P_\mathrm{turb}$ anti-correlate with the global star-formation rate of our galaxies. We therefore conclude that the molecular gas in early-type galaxies is likely unbound, and that large-scale dynamics likely plays a critical role in its regulation. This contrasts to the giant molecular clouds in the discs of late-type galaxies, that are much closer to dynamical equilibrium. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.05146v1-abstract-full').style.display = 'none'; document.getElementById('2308.05146v1-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 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">32 pages (16 of Appendices), 39 Figures (27 in Appendices). Accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.01342">arXiv:2308.01342</a> <span> [<a href="https://arxiv.org/pdf/2308.01342">pdf</a>, <a href="https://arxiv.org/format/2308.01342">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202347050">10.1051/0004-6361/202347050 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A constant N$_2$H$^+$(1-0)-to-HCN(1-0) ratio on kiloparsec scales </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jim%C3%A9nez-Donaire%2C+M+J">M. J. Jim茅nez-Donaire</a>, <a href="/search/astro-ph?searchtype=author&query=Usero%2C+A">A. Usero</a>, <a href="/search/astro-ph?searchtype=author&query=Be%C5%A1li%C4%87%2C+I">I. Be拧li膰</a>, <a href="/search/astro-ph?searchtype=author&query=Tafalla%2C+M">M. Tafalla</a>, <a href="/search/astro-ph?searchtype=author&query=Chac%C3%B3n-Tanarro%2C+A">A. Chac贸n-Tanarro</a>, <a href="/search/astro-ph?searchtype=author&query=Salom%C3%A9%2C+Q">Q. Salom茅</a>, <a href="/search/astro-ph?searchtype=author&query=Eibensteiner%2C+C">C. Eibensteiner</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Rodr%C3%ADguez%2C+A">A. Garc铆a-Rodr铆guez</a>, <a href="/search/astro-ph?searchtype=author&query=Hacar%2C+A">A. Hacar</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A+T">A. T. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">F. Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">M. Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Colombo%2C+D">D. Colombo</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">D. A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+A">T. A. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S+C+O">S. C. O. Glover</a>, <a href="/search/astro-ph?searchtype=author&query=Kauffmann%2C+J">J. Kauffmann</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R+S">R. S. Klessen</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A+K">A. K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Neumann%2C+L">L. Neumann</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+H">H. Pan</a>, <a href="/search/astro-ph?searchtype=author&query=Pety%2C+J">J. Pety</a>, <a href="/search/astro-ph?searchtype=author&query=Querejeta%2C+M">M. Querejeta</a>, <a href="/search/astro-ph?searchtype=author&query=Saito%2C+T">T. Saito</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">E. Schinnerer</a> , et al. (2 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2308.01342v1-abstract-short" style="display: inline;"> Nitrogen hydrides such as NH$_3$ and N$_2$H$^+$ are widely used by Galactic observers to trace the cold dense regions of the interstellar medium. In external galaxies, because of limited sensitivity, HCN has become the most common tracer of dense gas over large parts of galaxies. We provide the first systematic measurements of N$_2$H$^+$(1-0) across different environments of an external spiral gal… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.01342v1-abstract-full').style.display = 'inline'; document.getElementById('2308.01342v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.01342v1-abstract-full" style="display: none;"> Nitrogen hydrides such as NH$_3$ and N$_2$H$^+$ are widely used by Galactic observers to trace the cold dense regions of the interstellar medium. In external galaxies, because of limited sensitivity, HCN has become the most common tracer of dense gas over large parts of galaxies. We provide the first systematic measurements of N$_2$H$^+$(1-0) across different environments of an external spiral galaxy, NGC6946. We find a strong correlation ($r>0.98,p<0.01$) between the HCN(1-0) and N$_2$H$^+$(1-0) intensities across the inner $\sim8\mathrm{kpc}$ of the galaxy, at kiloparsec scales. This correlation is equally strong between the ratios N$_2$H$^+$(1-0)/CO(1-0) and HCN(1-0)/CO(1-0), tracers of dense gas fractions ($f_\mathrm{dense}$). We measure an average intensity ratio of N$_2$H$^+$(1-0)/HCN(1-0)$=0.15\pm0.02$ over our set of five IRAM-30m pointings. These trends are further supported by existing measurements for Galactic and extragalactic sources. This narrow distribution in the average ratio suggests that the observed systematic trends found in kiloparsec-scale extragalactic studies of $f_\mathrm{dense}$ and the efficiency of dense gas (SFE$_\mathrm{dense}$) would not change if we employed N$_2$H$^+$(1-0) as a more direct tracer of dense gas. At kiloparsec scales our results indicate that the HCN(1-0) emission can be used to predict the expected N$_2$H$^+$(1-0) over those regions. Our results suggest that, even if HCN(1-0) and N$_2$H$^+$(1-0) trace different density regimes within molecular clouds, subcloud differences average out at kiloparsec scales, yielding the two tracers proportional to each other. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.01342v1-abstract-full').style.display = 'none'; document.getElementById('2308.01342v1-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 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 676, L11 (2023) </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Williams%2C+T+G&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Williams%2C+T+G&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Williams%2C+T+G&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Williams%2C+T+G&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> </ul> </nav> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> 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