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<button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Leroy%2C+A&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Leroy%2C+A&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Leroy%2C+A&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Leroy%2C+A&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Leroy%2C+A&start=150" class="pagination-link " aria-label="Page 4" aria-current="page">4 </a> </li> <li> <a 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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/2410.13353">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/2410.02864">arXiv:2410.02864</a> <span> [<a href="https://arxiv.org/pdf/2410.02864">pdf</a>, <a href="https://arxiv.org/format/2410.02864">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: the universal relation between PAH band and optical line ratios across nearby star-forming galaxies </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">Karin Sandstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Sutter%2C+J">Jessica Sutter</a>, <a href="/search/astro-ph?searchtype=author&query=Hassani%2C+H">Hamid Hassani</a>, <a href="/search/astro-ph?searchtype=author&query=Groves%2C+B">Brent Groves</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=Boquien%2C+M">M茅d茅ric Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Brazzini%2C+M">Matilde Brazzini</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">Daniel Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Egorov%2C+O">Oleg Egorov</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S">Simon Glover</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R">Ralf Klessen</a>, <a href="/search/astro-ph?searchtype=author&query=Pathak%2C+D">Debosmita Pathak</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</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">M茅lanie Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Grasha%2C+K">Kathryn Grasha</a>, <a href="/search/astro-ph?searchtype=author&query=Hughes%2C+A">Annie Hughes</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=Pety%2C+J">J茅r么me Pety</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T">Thomas Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Hannon%2C+S">Stephen Hannon</a>, <a href="/search/astro-ph?searchtype=author&query=Sarbadhicary%2C+S">Sumit Sarbadhicary</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="2410.02864v1-abstract-short" style="display: inline;"> The structure and chemistry of the dusty interstellar medium (ISM) are shaped by complex processes that depend on the local radiation field, gas composition, and dust grain properties. Of particular importance are Polycyclic Aromatic Hydrocarbons (PAHs), which emit strong vibrational bands in the mid-infrared, and play a key role in the ISM energy balance. We recently identified global correlation… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.02864v1-abstract-full').style.display = 'inline'; document.getElementById('2410.02864v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.02864v1-abstract-full" style="display: none;"> The structure and chemistry of the dusty interstellar medium (ISM) are shaped by complex processes that depend on the local radiation field, gas composition, and dust grain properties. Of particular importance are Polycyclic Aromatic Hydrocarbons (PAHs), which emit strong vibrational bands in the mid-infrared, and play a key role in the ISM energy balance. We recently identified global correlations between PAH band and optical line ratios across three nearby galaxies, suggesting a connection between PAH heating and gas ionization throughout the ISM. In this work, we perform a census of the PAH heating -- gas ionization connection using $\sim$700,000 independent pixels that probe scales of 40--150 pc in nineteen nearby star-forming galaxies from the PHANGS survey. We find a universal relation between $\log$PAH(11.3 \mic/7.7 \mic) and $\log$([SII]/H$伪$) with a slope of $\sim$0.2 and a scatter of $\sim$0.025 dex. The only exception is a group of anomalous pixels that show unusually high (11.3 \mic/7.7 \mic) PAH ratios in regions with old stellar populations and high starlight-to-dust emission ratios. Their mid-infrared spectra resemble those of elliptical galaxies. AGN hosts show modestly steeper slopes, with a $\sim$10\% increase in PAH(11.3 \mic/7.7 \mic) in the diffuse gas on kpc scales. This universal relation implies an emerging simplicity in the complex ISM, with a sequence that is driven by a single varying property: the spectral shape of the interstellar radiation field. This suggests that other properties, such as gas-phase abundances, gas ionization parameter, and grain charge distribution, are relatively uniform in all but specific cases. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.02864v1-abstract-full').style.display = 'none'; document.getElementById('2410.02864v1-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 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">resubmitted to ApJ after addressing referee report; Figure 12 summarizes the results</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.03999">arXiv:2409.03999</a> <span> [<a href="https://arxiv.org/pdf/2409.03999">pdf</a>, <a href="https://arxiv.org/format/2409.03999">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> The LBT Satellites of Nearby Galaxies Survey (LBT-SONG): The Diffuse Satellite Population of Local Volume Hosts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Davis%2C+A+B">A. Bianca Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Garling%2C+C+T">Christopher T. Garling</a>, <a href="/search/astro-ph?searchtype=author&query=Nierenberg%2C+A+M">Anna M. Nierenberg</a>, <a href="/search/astro-ph?searchtype=author&query=Peter%2C+A+H+G">Annika H. G. Peter</a>, <a href="/search/astro-ph?searchtype=author&query=Sardone%2C+A">Amy Sardone</a>, <a href="/search/astro-ph?searchtype=author&query=Kochanek%2C+C+S">Christopher S. Kochanek</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=Casey%2C+K+J">Kirsten J. Casey</a>, <a href="/search/astro-ph?searchtype=author&query=Pogge%2C+R+W">Richard W. Pogge</a>, <a href="/search/astro-ph?searchtype=author&query=Roberts%2C+D+M">Daniella M. Roberts</a>, <a href="/search/astro-ph?searchtype=author&query=Sand%2C+D+J">David J. Sand</a>, <a href="/search/astro-ph?searchtype=author&query=Greco%2C+J+P">Johnny P. Greco</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="2409.03999v1-abstract-short" style="display: inline;"> We present the results of the Large Binocular Telescope Satellites Of Nearby Galaxies Survey (LBT-SONG) ``Far Sample,'' including survey completeness estimates. We find 10 satellite candidates in the inner virial regions of 13 star-forming galaxies outside the Local Group. The hosts are at distances between $\sim 5-11$ Mpc and have stellar masses in the little explored range of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.03999v1-abstract-full').style.display = 'inline'; document.getElementById('2409.03999v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.03999v1-abstract-full" style="display: none;"> We present the results of the Large Binocular Telescope Satellites Of Nearby Galaxies Survey (LBT-SONG) ``Far Sample,'' including survey completeness estimates. We find 10 satellite candidates in the inner virial regions of 13 star-forming galaxies outside the Local Group. The hosts are at distances between $\sim 5-11$ Mpc and have stellar masses in the little explored range of $\sim 5 \times 10^8 - 5\times 10^{10}~\text{M}_{\odot}$. Among the 10 satellite candidates, 3 are new discoveries in this survey. In this paper, we characterize the properties of 8 low-mass satellite candidates, including the 3 new discoveries but excluding 2 well-studied massive satellites. Of the 8 low-mass dwarfs, optical colors from the LBT imaging and measurements in the ultraviolet with GALEX suggest that 2 show signs of active star formation, and 6 are likely quenched (although some may still have H\textsc{i} gas reservoirs). Notably, we report the discovery of an ultrafaint dwarf candidate, NGC 672 dwD, with $\text{M}_{\text{V}} = -6.6$ and an estimated stellar mass of $5.6 \times 10^4 ~\text{M}_{\odot}$ if its association with the host is confirmed. It is spatially coincident with a weak detection of H\textsc{i}, with $\text{M}_{\text{HI}}/\text{M}_{\text{*}} \sim 1$. If confirmed, it would be the least luminous known ultrafaint satellite to be so gas-rich. The prevalence of quenched satellites in our sample suggests there are environmental effects at work in lower mass hosts that are similar to those at play in Milky Way-size hosts, although the preponderance of H\textsc{i} detections is at odds with the paucity of H\textsc{i} detections in Milky Way satellites. By robustly measuring our survey completeness function, we are able to compare our observational results to predictions from theory, finding good agreement with the Cold Dark Matter galaxy evolution paradigm. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.03999v1-abstract-full').style.display = 'none'; document.getElementById('2409.03999v1-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 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">18 pages, 9 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/2408.14497">arXiv:2408.14497</a> <span> [<a href="https://arxiv.org/pdf/2408.14497">pdf</a>, <a href="https://arxiv.org/format/2408.14497">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Key Science Goals for the Next Generation Very Large Array (ngVLA): Update from the ngVLA Science Advisory Council (2024) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wilner%2C+D+J">David J. Wilner</a>, <a href="/search/astro-ph?searchtype=author&query=Matthews%2C+B+C">Brenda C. Matthews</a>, <a href="/search/astro-ph?searchtype=author&query=McGuire%2C+B">Brett McGuire</a>, <a href="/search/astro-ph?searchtype=author&query=Bergner%2C+J">Jennifer Bergner</a>, <a href="/search/astro-ph?searchtype=author&query=Walter%2C+F">Fabian Walter</a>, <a href="/search/astro-ph?searchtype=author&query=Somerville%2C+R">Rachel Somerville</a>, <a href="/search/astro-ph?searchtype=author&query=DeCesar%2C+M">Megan DeCesar</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Horst%2C+A">Alexander van der Horst</a>, <a href="/search/astro-ph?searchtype=author&query=Osten%2C+R">Rachel Osten</a>, <a href="/search/astro-ph?searchtype=author&query=Corsi%2C+A">Alessandra Corsi</a>, <a href="/search/astro-ph?searchtype=author&query=Baker%2C+A">Andrew Baker</a>, <a href="/search/astro-ph?searchtype=author&query=Bergin%2C+E">Edwin Bergin</a>, <a href="/search/astro-ph?searchtype=author&query=Bolatto%2C+A">Alberto Bolatto</a>, <a href="/search/astro-ph?searchtype=author&query=Blecha%2C+L">Laura Blecha</a>, <a href="/search/astro-ph?searchtype=author&query=Bower%2C+G">Geoff Bower</a>, <a href="/search/astro-ph?searchtype=author&query=Burke-Spolaor%2C+S">Sarah Burke-Spolaor</a>, <a href="/search/astro-ph?searchtype=author&query=Carrasco-Gonzalez%2C+C">Carlos Carrasco-Gonzalez</a>, <a href="/search/astro-ph?searchtype=author&query=de+Keller%2C+K">Katherine de Keller</a>, <a href="/search/astro-ph?searchtype=author&query=de+Pater%2C+I">Imke de Pater</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Drout%2C+M">Maria Drout</a>, <a href="/search/astro-ph?searchtype=author&query=Hallinan%2C+G">Gregg Hallinan</a>, <a href="/search/astro-ph?searchtype=author&query=Hatsukade%2C+B">Bunyo Hatsukade</a>, <a href="/search/astro-ph?searchtype=author&query=Isella%2C+A">Andrea Isella</a>, <a href="/search/astro-ph?searchtype=author&query=Izumi%2C+T">Takuma Izumi</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="2408.14497v1-abstract-short" style="display: inline;"> In 2017, the next generation Very Large Array (ngVLA) Science Advisory Council, together with the international astronomy community, developed a set of five Key Science Goals (KSGs) to inform, prioritize and refine the technical capabilities of a future radio telescope array for high angular resolution operation from 1.2 - 116 GHz with 10 times the sensitivity of the Jansky VLA and ALMA. The resul… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.14497v1-abstract-full').style.display = 'inline'; document.getElementById('2408.14497v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.14497v1-abstract-full" style="display: none;"> In 2017, the next generation Very Large Array (ngVLA) Science Advisory Council, together with the international astronomy community, developed a set of five Key Science Goals (KSGs) to inform, prioritize and refine the technical capabilities of a future radio telescope array for high angular resolution operation from 1.2 - 116 GHz with 10 times the sensitivity of the Jansky VLA and ALMA. The resulting KSGs, which require observations at centimeter and millimeter wavelengths that cannot be achieved by any other facility, represent a small subset of the broad range of astrophysical problems that the ngVLA will be able address. This document presents an update to the original ngVLA KSGs, taking account of new results and progress in the 7+ years since their initial presentation, again drawing on the expertise of the ngVLA Science Advisory Council and the broader community in the ngVLA Science Working Groups. As the design of the ngVLA has also matured substantially in this period, this document also briefly addresses initial expectations for ngVLA data products and processing that will be needed to achieve the KSGs. The original ngVLA KSGs endure as outstanding problems of high priority. In brief, they are: (1) Unveiling the Formation of Solar System Analogues; (2) Probing the Initial Conditions for Planetary Systems and Life with Astrochemistry; (3) Charting the Assembly, Structure, and Evolution of Galaxies from the First Billion Years to the Present; (4) Science at the Extremes: Pulsars as Laboratories for Fundamental Physics; (5) Understanding the Formation and Evolution of Stellar and Supermassive Black Holes in the Era of Multi-Messenger Astronomy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.14497v1-abstract-full').style.display = 'none'; document.getElementById('2408.14497v1-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 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">29 pages, 9 figures, ngVLA memo 125. arXiv admin note: text overlap with arXiv:1711.09960</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.04135">arXiv:2408.04135</a> <span> [<a href="https://arxiv.org/pdf/2408.04135">pdf</a>, <a href="https://arxiv.org/format/2408.04135">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 Observations of Starbursts: Massive Star Clusters in the Central Starburst of M82 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Levy%2C+R+C">Rebecca C. Levy</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=Mayya%2C+D">Divakara Mayya</a>, <a href="/search/astro-ph?searchtype=author&query=Cuevas-Otahola%2C+B">Bolivia Cuevas-Otahola</a>, <a href="/search/astro-ph?searchtype=author&query=Tarantino%2C+E">Elizabeth Tarantino</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=Boogaard%2C+L+A">Leindert A. Boogaard</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ker%2C+T">Torsten B枚ker</a>, <a href="/search/astro-ph?searchtype=author&query=Cronin%2C+S+A">Serena A. Cronin</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=Donaghue%2C+K">Keaton Donaghue</a>, <a href="/search/astro-ph?searchtype=author&query=Emig%2C+K+L">Kimberly L. Emig</a>, <a href="/search/astro-ph?searchtype=author&query=Fisher%2C+D+B">Deanne B. Fisher</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=Herrera-Camus%2C+R">Rodrigo Herrera-Camus</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=Klessen%2C+R+S">Ralf S. Klessen</a>, <a href="/search/astro-ph?searchtype=author&query=Lenki%C4%87%2C+L">Laura Lenki膰</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=De+Looze%2C+I">Ilse De Looze</a>, <a href="/search/astro-ph?searchtype=author&query=Meier%2C+D+S">David S. Meier</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=Ott%2C+J">Juergen Ott</a>, <a href="/search/astro-ph?searchtype=author&query=Rela%C3%B1o%2C+M">M贸nica Rela帽o</a>, <a href="/search/astro-ph?searchtype=author&query=Veilleux%2C+S">Sylvain Veilleux</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="2408.04135v2-abstract-short" style="display: inline;"> We present a near infrared (NIR) candidate star cluster catalog for the central kiloparsec of M82 based on new JWST NIRCam images. We identify star cluster candidates using the F250M filter, finding 1357 star cluster candidates with stellar masses $>10^4$ M$_\odot$. Compared to previous optical catalogs, nearly all (87%) of the candidates we identify are new. The star cluster candidates have a med… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.04135v2-abstract-full').style.display = 'inline'; document.getElementById('2408.04135v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.04135v2-abstract-full" style="display: none;"> We present a near infrared (NIR) candidate star cluster catalog for the central kiloparsec of M82 based on new JWST NIRCam images. We identify star cluster candidates using the F250M filter, finding 1357 star cluster candidates with stellar masses $>10^4$ M$_\odot$. Compared to previous optical catalogs, nearly all (87%) of the candidates we identify are new. The star cluster candidates have a median intrinsic cluster radius of $\approx$1 pc and have stellar masses up to $10^6$ M$_\odot$. By comparing the color-color diagram to dust-free yggdrasil stellar population models, we estimate that the star cluster candidates have A$_{\rm V}\sim3-24$ mag, corresponding to A$_{\rm 2.5渭m}\sim0.3-2.1$ mag. There is still appreciable dust extinction towards these clusters into the NIR. We measure the stellar masses of the star cluster candidates, assuming ages of 0 and 8 Myr. The slope of the resulting cluster mass function is $尾=1.9\pm0.2$, in excellent agreement with studies of star clusters in other galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.04135v2-abstract-full').style.display = 'none'; document.getElementById('2408.04135v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 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">Resubmitted to ApJL</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/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/2405.03686">arXiv:2405.03686</a> <span> [<a href="https://arxiv.org/pdf/2405.03686">pdf</a>, <a href="https://arxiv.org/format/2405.03686">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 Observations of Starbursts: Cold Clouds and Plumes Launching in the M82 Outflow </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fisher%2C+D+B">Deanne B. Fisher</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=Chisholm%2C+J">John Chisholm</a>, <a href="/search/astro-ph?searchtype=author&query=Fielding%2C+D">Drummond Fielding</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=Tarantino%2C+E">Elizabeth Tarantino</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=Cronin%2C+S+A">Serena A. Cronin</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=Smith%2C+J+D">J. D. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Berg%2C+D+A">Danielle A. Berg</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+S">Sebastian Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Veilleux%2C+S">Sylvain Veilleux</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Werf%2C+P+P">Paul P. van der Werf</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ker%2C+T">Torsten B枚ker</a>, <a href="/search/astro-ph?searchtype=author&query=Boogaard%2C+L+A">Leindert A. Boogaard</a>, <a href="/search/astro-ph?searchtype=author&query=Lenki%C4%87%2C+L">Laura Lenki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=Villanueva%2C+V">Vicente Villanueva</a>, <a href="/search/astro-ph?searchtype=author&query=Mayya%2C+D">Divakara Mayya</a>, <a href="/search/astro-ph?searchtype=author&query=Lai%2C+T+S+-">Thomas S. -Y. Lai</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=Emig%2C+K+L">Kimberly L. Emig</a>, <a href="/search/astro-ph?searchtype=author&query=Walter%2C+F">Fabian Walter</a>, <a href="/search/astro-ph?searchtype=author&query=Rela%C3%B1o%2C+M">Monica Rela帽o</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="2405.03686v1-abstract-short" style="display: inline;"> In this paper we study the filamentary substructure of 3.3 $渭$m PAH emission from JWST/NIRCam observations in the base of the M82 star-burst driven wind. We identify plume-like substructure within the PAH emission with widths of $\sim$50 pc. Several of the plumes extend to the edge of the field-of-view, and thus are at least 200-300 pc in length. In this region of the outflow, the vast majority (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.03686v1-abstract-full').style.display = 'inline'; document.getElementById('2405.03686v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.03686v1-abstract-full" style="display: none;"> In this paper we study the filamentary substructure of 3.3 $渭$m PAH emission from JWST/NIRCam observations in the base of the M82 star-burst driven wind. We identify plume-like substructure within the PAH emission with widths of $\sim$50 pc. Several of the plumes extend to the edge of the field-of-view, and thus are at least 200-300 pc in length. In this region of the outflow, the vast majority ($\sim$70\%) of PAH emission is associated with the plumes. We show that those structures contain smaller scale "clouds" with widths that are $\sim$5-15 pc, and they are morphologically similar to the results of "cloud-crushing" simulations. We estimate the cloud-crushing time-scales of $\sim$0.5-3 Myr, depending on assumptions. We show this time scale is consistent with a picture in which these observed PAH clouds survived break-out from the disk rather than being destroyed by the hot wind. The PAH emission in both the midplane and the outflow is shown to tightly correlate with that of Pa$伪$ emission (from HST/NICMOS data), at the scale of both plumes and clouds, though the ratio of PAH-to-Pa$伪$ increases at further distances from the midplane. Finally, we show that the outflow PAH emission is suppressed in regions of the M82 wind that are bright in X-ray emission. Overall, our results are broadly consistent with a picture in which cold gas in galactic outflows is launched via hierarchically structured plumes, and those small scale clouds are more likely to survive the wind environment when collected into the larger plume structure. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.03686v1-abstract-full').style.display = 'none'; document.getElementById('2405.03686v1-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 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">Submitted 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/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/2404.04555">arXiv:2404.04555</a> <span> [<a href="https://arxiv.org/pdf/2404.04555">pdf</a>, <a href="https://arxiv.org/format/2404.04555">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 Molecular Gas Properties of the Antennae Merger: A Comparative Study with PHANGS-ALMA Galaxies and NGC 3256 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Brunetti%2C+N">Nathan Brunetti</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=He%2C+H">Hao He</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=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Bemis%2C+A">Ashley Bemis</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">Frank Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Groves%2C+B">Brent Groves</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> </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="2404.04555v1-abstract-short" style="display: inline;"> We present observations of the central 9 kpc of the Antennae merger (NGC 4038/9) at 55 pc resolution in the CO 2-1 line obtained with the Atacama Large Millimeter/submillimeter Array (ALMA). We use a pixel-based analysis to compare the gas properties in the Antennae to those in 70 nearby spiral galaxies from the PHANGS-ALMA survey, as well as the merger and nearest luminous infrared galaxy NGC 325… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.04555v1-abstract-full').style.display = 'inline'; document.getElementById('2404.04555v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.04555v1-abstract-full" style="display: none;"> We present observations of the central 9 kpc of the Antennae merger (NGC 4038/9) at 55 pc resolution in the CO 2-1 line obtained with the Atacama Large Millimeter/submillimeter Array (ALMA). We use a pixel-based analysis to compare the gas properties in the Antennae to those in 70 nearby spiral galaxies from the PHANGS-ALMA survey, as well as the merger and nearest luminous infrared galaxy NGC 3256. Compared to PHANGS galaxies at matched spatial resolution, the molecular gas in the Antennae exhibits some of the highest surface densities, velocity dispersions, peak brightness temperatures, and turbulent pressures. However, the virial parameters in the Antennae are consistent with many of the PHANGS galaxies. NGC 3256 has similar gas surface densities but higher nuclear velocity dispersions than the Antennae, as well as higher system-wide peak brightness temperatures and virial parameters. NGC 3256 is at a later stage in the merging process than the Antennae, which may result in more intense merger-driven gas flows that could drive up the turbulence in the gas. The high virial parameters in NGC 3256 may indicate that this increased turbulence is suppressing future star formation as NGC 3256 moves out of the starburst phase. In comparison, the relatively normal virial parameters in the Antennae may imply that it is about to undergo a new burst of star formation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.04555v1-abstract-full').style.display = 'none'; document.getElementById('2404.04555v1-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 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">16 pages, 8 figures, 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/2404.01774">arXiv:2404.01774</a> <span> [<a href="https://arxiv.org/pdf/2404.01774">pdf</a>, <a href="https://arxiv.org/format/2404.01774">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/10.1051/0004-6361/202348297">10.1051/0004-6361/202348297 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MHONGOOSE -- A MeerKAT Nearby Galaxy HI Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Healy%2C+J">J. Healy</a>, <a href="/search/astro-ph?searchtype=author&query=Maccagni%2C+F+M">F. M. Maccagni</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=Bosma%2C+A">A. Bosma</a>, <a href="/search/astro-ph?searchtype=author&query=English%2C+J">J. English</a>, <a href="/search/astro-ph?searchtype=author&query=Jarrett%2C+T">T. Jarrett</a>, <a href="/search/astro-ph?searchtype=author&query=Marasco%2C+A">A. Marasco</a>, <a href="/search/astro-ph?searchtype=author&query=Meurer%2C+G+R">G. R. Meurer</a>, <a href="/search/astro-ph?searchtype=author&query=Veronese%2C+S">S. Veronese</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">F. Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Chemin%2C+L">L. Chemin</a>, <a href="/search/astro-ph?searchtype=author&query=Fraternali%2C+F">F. Fraternali</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">B. W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Kamphuis%2C+P">P. Kamphuis</a>, <a href="/search/astro-ph?searchtype=author&query=Kl%C3%B6ckner%2C+H+R">H. R. Kl枚ckner</a>, <a href="/search/astro-ph?searchtype=author&query=Kleiner%2C+D">D. Kleiner</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=Mogotsi%2C+M">M. Mogotsi</a>, <a href="/search/astro-ph?searchtype=author&query=Oman%2C+K+A">K. A. Oman</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">E. Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Verdes-Montenegro%2C+L">L. Verdes-Montenegro</a>, <a href="/search/astro-ph?searchtype=author&query=Westmeier%2C+T">T. Westmeier</a>, <a href="/search/astro-ph?searchtype=author&query=Wong%2C+O+I">O. I. Wong</a>, <a href="/search/astro-ph?searchtype=author&query=Zabel%2C+N">N. Zabel</a> , et al. (35 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.01774v2-abstract-short" style="display: inline;"> The MHONGOOSE (MeerKAT HI Observations of Nearby Galactic Objects: Observing Southern Emitters) survey maps the distribution and kinematics of the neutral atomic hydrogen (HI) gas in and around 30 nearby star-forming spiral and dwarf galaxies to extremely low HI column densities. The HI column density sensitivity (3 sigma over 16 km/s) ranges from ~ 5 x 10^{17} cm^{-2} at 90'' resolution to ~4 x 1… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.01774v2-abstract-full').style.display = 'inline'; document.getElementById('2404.01774v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.01774v2-abstract-full" style="display: none;"> The MHONGOOSE (MeerKAT HI Observations of Nearby Galactic Objects: Observing Southern Emitters) survey maps the distribution and kinematics of the neutral atomic hydrogen (HI) gas in and around 30 nearby star-forming spiral and dwarf galaxies to extremely low HI column densities. The HI column density sensitivity (3 sigma over 16 km/s) ranges from ~ 5 x 10^{17} cm^{-2} at 90'' resolution to ~4 x 10^{19} cm^{-2} at the highest resolution of 7''. The HI mass sensitivity (3 sigma over 50 km/s) is ~5.5 X 10^5 M_sun at a distance of 10 Mpc (the median distance of the sample galaxies). The velocity resolution of the data is 1.4 km/s. One of the main science goals of the survey is the detection of cold, accreting gas in the outskirts of the sample galaxies. The sample was selected to cover a range in HI masses, from 10^7 M_sun to almost 10^{11} M_sun, to optimally sample possible accretion scenarios and environments. The distance to the sample galaxies ranges from 3 to 23 Mpc. In this paper, we present the sample selection, survey design, and observation and reduction procedures. We compare the integrated HI fluxes based on the MeerKAT data with those derived from single-dish measurement and find good agreement, indicating that our MeerKAT observations are recovering all flux. We present HI moment maps of the entire sample based on the first ten percent of the survey data, and find that a comparison of the zeroth- and second-moment values shows a clear separation between the physical properties of the HI in areas with star formation and areas without, related to the formation of a cold neutral medium. Finally, we give an overview of the HI-detected companion and satellite galaxies in the 30 fields, five of which have not previously been catalogued. We find a clear relation between the number of companion galaxies and the mass of the main target galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.01774v2-abstract-full').style.display = 'none'; document.getElementById('2404.01774v2-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted 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 688, A109 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.19843">arXiv:2403.19843</a> <span> [<a href="https://arxiv.org/pdf/2403.19843">pdf</a>, <a href="https://arxiv.org/format/2403.19843">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"> Molecular Gas and the Star Formation Process on Cloud Scales in Nearby Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A+K">Adam K. Leroy</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="2403.19843v1-abstract-short" style="display: inline;"> Observations that resolve nearby galaxies into individual regions across multiple phases of the gas-star formation-feedback ``matter cycle'' have provided a sharp new view of molecular clouds, star formation efficiencies, timescales for region evolution, and stellar feedback. We synthesize these results, cover aspects relevant to the interpretation of observables, and conclude that: (1) The obse… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.19843v1-abstract-full').style.display = 'inline'; document.getElementById('2403.19843v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.19843v1-abstract-full" style="display: none;"> Observations that resolve nearby galaxies into individual regions across multiple phases of the gas-star formation-feedback ``matter cycle'' have provided a sharp new view of molecular clouds, star formation efficiencies, timescales for region evolution, and stellar feedback. We synthesize these results, cover aspects relevant to the interpretation of observables, and conclude that: (1) The observed cloud-scale molecular gas surface density, line width, and internal pressure all reflect the large-scale galactic environment while also appearing mostly consistent with properties of a turbulent medium strongly affected by self-gravity. (2) Cloud-scale data allow for statistical inference of both evolutionary and physical timescales. These suggest that clouds collapse on timescale of order the free-fall or turbulent crossing time ($\sim 10{-}30$~Myr) followed by the formation of massive stars and subsequent rapid ($\lesssim$ 5 Myr) gas clearing. The star formation efficiency per free-fall time is well determined over thousands of regions to be $蔚_{\rm ff}\approx 0.5_{-0.3}^{+0.7}\%$. (3) The role of stellar feedback is now measured using multiple observational approaches. The net momentum yield is constrained by the requirement to support the vertical weight of the galaxy disk. Meanwhile, the short gas clearing timescales suggest a large role for pre-supernova feedback in cloud disruption. This leaves the supernovae free to exert a large influence on the larger scale galaxy, including driving turbulence, launching galactic-scale winds, and carving superbubbles. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.19843v1-abstract-full').style.display = 'none'; document.getElementById('2403.19843v1-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 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">70 pages, 15 figures, 9 tables. Authors' version of an article to appear in Annual Reviews of Astronomy and Astrophysics 2024, Vol 62</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/2401.16648">arXiv:2401.16648</a> <span> [<a href="https://arxiv.org/pdf/2401.16648">pdf</a>, <a href="https://arxiv.org/format/2401.16648">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 Observations of Starbursts: Polycyclic Aromatic Hydrocarbon Emission at the Base of the M 82 Galactic Wind </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bolatto%2C+A+D">Alberto D. Bolatto</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=Tarantino%2C+E">Elizabeth Tarantino</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=Fisher%2C+D+B">Deanne B. Fisher</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=Cronin%2C+S+A">Serena A. Cronin</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=Smith%2C+J+D">J. D. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Berg%2C+D+A">Dannielle A. Berg</a>, <a href="/search/astro-ph?searchtype=author&query=Boeker%2C+T">Torsten Boeker</a>, <a href="/search/astro-ph?searchtype=author&query=Boogaard%2C+L+A">Leindert A. Boogaard</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=Thompson%2C+T+A">Todd A. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Ott%2C+J">Juergen Ott</a>, <a href="/search/astro-ph?searchtype=author&query=Lenkic%2C+L">Laura Lenkic</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=Dale%2C+D+A">Daniel A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Veilleux%2C+S">Sylvain Veilleux</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Werf%2C+P+P">Paul P. van der Werf</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=Sandstrom%2C+K+M">Karin M. Sandstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Skillman%2C+E+D">Evan D. Skillman</a>, <a href="/search/astro-ph?searchtype=author&query=Chisholm%2C+J">John Chisholm</a>, <a href="/search/astro-ph?searchtype=author&query=Villanueva%2C+V">Vicente Villanueva</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="2401.16648v4-abstract-short" style="display: inline;"> We present new observations of the central 1 kpc of the M 82 starburst obtained with the James Webb Space Telescope (JWST) near-infrared camera (NIRCam) instrument at a resolution ~0.05"-0.1" (~1-2 pc). The data comprises images in three mostly continuum filters (F140M, F250M, and F360M), and filters that contain [FeII] (F164N), H2 v=1-0 (F212N), and the 3.3 um PAH feature (F335M). We find promine… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.16648v4-abstract-full').style.display = 'inline'; document.getElementById('2401.16648v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.16648v4-abstract-full" style="display: none;"> We present new observations of the central 1 kpc of the M 82 starburst obtained with the James Webb Space Telescope (JWST) near-infrared camera (NIRCam) instrument at a resolution ~0.05"-0.1" (~1-2 pc). The data comprises images in three mostly continuum filters (F140M, F250M, and F360M), and filters that contain [FeII] (F164N), H2 v=1-0 (F212N), and the 3.3 um PAH feature (F335M). We find prominent plumes of PAH emission extending outward from the central starburst region, together with a network of complex filamentary substructure and edge-brightened bubble-like features. The structure of the PAH emission closely resembles that of the ionized gas, as revealed in Paschen alpha and free-free radio emission. We discuss the origin of the structure, and suggest the PAHs are embedded in a combination of neutral, molecular, and photoionized gas. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.16648v4-abstract-full').style.display = 'none'; document.getElementById('2401.16648v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to The Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/2401.13181">arXiv:2401.13181</a> <span> [<a href="https://arxiv.org/pdf/2401.13181">pdf</a>, <a href="https://arxiv.org/format/2401.13181">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/10.5281/zenodo.10431797">10.5281/zenodo.10431797 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </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/10.5281/zenodo.10256731">10.5281/zenodo.10256731 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The EDGE-CALIFA Survey: An Extragalactic Database for Galaxy Evolution Studies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wong%2C+T">Tony Wong</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Y">Yixian Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Luo%2C+Y">Yufeng Luo</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=S%C3%A1nchez%2C+S+F">Sebasti谩n F. S谩nchez</a>, <a href="/search/astro-ph?searchtype=author&query=Barrera-Ballesteros%2C+J+K">Jorge K. Barrera-Ballesteros</a>, <a href="/search/astro-ph?searchtype=author&query=Blitz%2C+L">Leo Blitz</a>, <a href="/search/astro-ph?searchtype=author&query=Colombo%2C+D">Dario Colombo</a>, <a href="/search/astro-ph?searchtype=author&query=Dannerbauer%2C+H">Helmut Dannerbauer</a>, <a href="/search/astro-ph?searchtype=author&query=Green%2C+A">Alex Green</a>, <a href="/search/astro-ph?searchtype=author&query=Kalinova%2C+V">Veselina Kalinova</a>, <a href="/search/astro-ph?searchtype=author&query=Khan%2C+F">Ferzem Khan</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+A">Andrew Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lacerda%2C+E+A+D">Eduardo A. D. Lacerda</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=Levy%2C+R+C">Rebecca C. Levy</a>, <a href="/search/astro-ph?searchtype=author&query=Lin%2C+X">Xincheng Lin</a>, <a href="/search/astro-ph?searchtype=author&query=Luo%2C+Y">Yuanze Luo</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=Rubio%2C+M">M贸nica Rubio</a>, <a href="/search/astro-ph?searchtype=author&query=Teuben%2C+P">Peter Teuben</a>, <a href="/search/astro-ph?searchtype=author&query=Utomo%2C+D">Dyas Utomo</a>, <a href="/search/astro-ph?searchtype=author&query=Villanueva%2C+V">Vicente Villanueva</a>, <a href="/search/astro-ph?searchtype=author&query=Vogel%2C+S+N">Stuart N. Vogel</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+X">Xinyu Wang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.13181v1-abstract-short" style="display: inline;"> The EDGE-CALIFA survey provides spatially resolved optical integral field unit (IFU) and CO spectroscopy for 125 galaxies selected from the CALIFA Data Release 3 sample. The Extragalactic Database for Galaxy Evolution (EDGE) presents the spatially resolved products of the survey as pixel tables that reduce the oversampling in the original images and facilitate comparison of pixels from different i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.13181v1-abstract-full').style.display = 'inline'; document.getElementById('2401.13181v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.13181v1-abstract-full" style="display: none;"> The EDGE-CALIFA survey provides spatially resolved optical integral field unit (IFU) and CO spectroscopy for 125 galaxies selected from the CALIFA Data Release 3 sample. The Extragalactic Database for Galaxy Evolution (EDGE) presents the spatially resolved products of the survey as pixel tables that reduce the oversampling in the original images and facilitate comparison of pixels from different images. By joining these pixel tables to lower dimensional tables that provide radial profiles, integrated spectra, or global properties, it is possible to investigate the dependence of local conditions on large-scale properties. The database is freely accessible and has been utilized in several publications. We illustrate the use of this database and highlight the effects of CO upper limits on the inferred slopes of the local scaling relations between stellar mass, star formation rate (SFR), and H$_2$ surface densities. We find that the correlation between H$_2$ and SFR surface density is the tightest among the three relations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.13181v1-abstract-full').style.display = 'none'; document.getElementById('2401.13181v1-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 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">21 pages, accepted for publication in ApJS, see DOIs below for code and data access</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.09810">arXiv:2312.09810</a> <span> [<a href="https://arxiv.org/pdf/2312.09810">pdf</a>, <a href="https://arxiv.org/format/2312.09810">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/10.1051/0004-6361/202348205">10.1051/0004-6361/202348205 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Surveying the Whirlpool at Arcseconds with NOEMA (SWAN)- I. Mapping the HCN and N$_2$H$^+$ 3mm lines </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Stuber%2C+S+K">Sophia K. Stuber</a>, <a href="/search/astro-ph?searchtype=author&query=Pety%2C+J">Jerome Pety</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=Usero%2C+A">Antonio Usero</a>, <a href="/search/astro-ph?searchtype=author&query=Besli%C4%87%2C+I">Ivana Besli膰</a>, <a href="/search/astro-ph?searchtype=author&query=Querejeta%2C+M">Miguel Querejeta</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=Brok%2C+J+d">Jakob den Brok</a>, <a href="/search/astro-ph?searchtype=author&query=Neumann%2C+L">Lukas Neumann</a>, <a href="/search/astro-ph?searchtype=author&query=Eibensteiner%2C+C">Cosima Eibensteiner</a>, <a href="/search/astro-ph?searchtype=author&query=Teng%2C+Y">Yu-Hsuan Teng</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A">Ashley Barnes</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=Glover%2C+S+C+O">Simon C. O. Glover</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> </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="2312.09810v1-abstract-short" style="display: inline;"> We present the first results from "Surveying the Whirlpool at Arcseconds with NOEMA" (SWAN), an IRAM Northern Extended Millimetre Array (NOEMA)+30m large program that maps emission from several molecular lines at 90 and 110 GHz in the iconic nearby grand-design spiral galaxy M~51 at cloud-scale resolution ($\sim$3\arcsec=125\,pc). As part of this work, we have obtained the first sensitive cloud-sc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.09810v1-abstract-full').style.display = 'inline'; document.getElementById('2312.09810v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.09810v1-abstract-full" style="display: none;"> We present the first results from "Surveying the Whirlpool at Arcseconds with NOEMA" (SWAN), an IRAM Northern Extended Millimetre Array (NOEMA)+30m large program that maps emission from several molecular lines at 90 and 110 GHz in the iconic nearby grand-design spiral galaxy M~51 at cloud-scale resolution ($\sim$3\arcsec=125\,pc). As part of this work, we have obtained the first sensitive cloud-scale map of N$_2$H$^+$(1-0) of the inner $\sim5\,\times 7\,$kpc of a normal star-forming galaxy, which we compare to HCN(1-0) and CO(1-0) emission to test their ability in tracing dense, star-forming gas. The average N$_2$H$^+$-to-HCN line ratio of our total FoV is $0.20\pm0.09$, with strong regional variations of a factor of $\gtrsim 2$ throughout the disk, including the south-western spiral arm and the center. The central $\sim1\,$kpc exhibits elevated HCN emission compared to N$_2$H$^+$, probably caused by AGN-driven excitation effects. We find that HCN and N$_2$H$^+$ are strongly super-linearily correlated in intensity ($蟻_\mathrm{Sp}\sim 0.8$), with an average scatter of $\sim0.14\,$dex over a span of $\gtrsim 1.5\,$dex in intensity. When excluding the central region, the data is best described by a power-law of exponent $1.2$, indicating that there is more N$_2$H$^+$ per unit HCN in brighter regions. Our observations demonstrate that the HCN-to-CO line ratio is a sensitive tracer of gas density in agreement with findings of recent Galactic studies which utilize N$_2$H$^+$. The peculiar line ratios present near the AGN and the scatter of the power-law fit in the disk suggest that in addition to a first-order correlation with gas density, second-order physics (such as optical depth, gas temperature) or chemistry (abundance variations) are encoded in the N$_2$H$^+$/CO, HCN/CO and N$_2$H$^+$/HCN ratios. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.09810v1-abstract-full').style.display = 'none'; document.getElementById('2312.09810v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 December, 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">Accepted for publication in A&A. 6 pages, 3 figures (+ Appendix 4 pages, 2 figures)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.09188">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/2312.06880">arXiv:2312.06880</a> <span> [<a href="https://arxiv.org/pdf/2312.06880">pdf</a>, <a href="https://arxiv.org/format/2312.06880">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"> Detection of diffuse HI emission in the circumgalactic medium of NGC891 and NGC4565 -- II </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Das%2C+S">Sanskriti Das</a>, <a href="/search/astro-ph?searchtype=author&query=Rickel%2C+M">Mary Rickel</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A">Adam Leroy</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=Pisano%2C+D+J">D. J. Pisano</a>, <a href="/search/astro-ph?searchtype=author&query=Heald%2C+G">George Heald</a>, <a href="/search/astro-ph?searchtype=author&query=Mathur%2C+S">Smita Mathur</a>, <a href="/search/astro-ph?searchtype=author&query=Kingsbury%2C+J">Joshua Kingsbury</a>, <a href="/search/astro-ph?searchtype=author&query=Sardone%2C+A">Amy Sardone</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="2312.06880v1-abstract-short" style="display: inline;"> We probe the neutral circumgalactic medium (CGM) along the major axes of NGC891 and NGC4565 in 21-cm emission out to $\gtrsim 100$kpc using the Green Bank Telescope (GBT), extending our previous minor axes observations. We achieve an unprecedented $5蟽$ sensitivity of $6.1\times 10^{16}$ cm$^{-2}$ per 20 km s$^{-1}$ velocity channel. We detect HI with diverse spectral shapes, velocity widths, and c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.06880v1-abstract-full').style.display = 'inline'; document.getElementById('2312.06880v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.06880v1-abstract-full" style="display: none;"> We probe the neutral circumgalactic medium (CGM) along the major axes of NGC891 and NGC4565 in 21-cm emission out to $\gtrsim 100$kpc using the Green Bank Telescope (GBT), extending our previous minor axes observations. We achieve an unprecedented $5蟽$ sensitivity of $6.1\times 10^{16}$ cm$^{-2}$ per 20 km s$^{-1}$ velocity channel. We detect HI with diverse spectral shapes, velocity widths, and column densities. We compare our detections to the interferometric maps from the Westerbork Synthesis Radio Telescope (WSRT) obtained as part of the HALOGAS survey. At small impact parameters, $> 31-43\%$ of the emission detected by the GBT cannot be explained by emission seen in the WSRT maps, and it increases to $> 64-73\%$ at large impact parameters. This implies the presence of diffuse circumgalactic HI. The mass ratio between HI in the CGM and HI in the disk is an order of magnitude larger than previous estimates based on shallow GBT mapping. The diffuse HI along the major axes pointings is corotating with the HI disk. The velocity along the minor axes pointings is consistent with an inflow and/or fountain in NGC891 and an inflow/outflow in NGC4565. Including the circumgalactic HI, the depletion time and the accretion rate of NGC4565 are sufficient to sustain its star formation. In NGC891, most of the required accreting material is still missing. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.06880v1-abstract-full').style.display = 'none'; document.getElementById('2312.06880v1-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, 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">18 pages, 12 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/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/2312.03995">arXiv:2312.03995</a> <span> [<a href="https://arxiv.org/pdf/2312.03995">pdf</a>, <a href="https://arxiv.org/format/2312.03995">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 EDGE-CALIFA survey: Molecular Gas and Star Formation Activity Across the Green Valley </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Villanueva%2C+V">Vicente Villanueva</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=Vogel%2C+S+N">Stuart N. Vogel</a>, <a href="/search/astro-ph?searchtype=author&query=Wong%2C+T">Tony Wong</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=Sanchez%2C+S+F">Sebastian F. Sanchez</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=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Colombo%2C+D">Dario Colombo</a>, <a href="/search/astro-ph?searchtype=author&query=Kalinova%2C+V">Veselina Kalinova</a>, <a href="/search/astro-ph?searchtype=author&query=Cronin%2C+S">Serena Cronin</a>, <a href="/search/astro-ph?searchtype=author&query=Teuben%2C+P">Peter Teuben</a>, <a href="/search/astro-ph?searchtype=author&query=Rubio%2C+M">Monica Rubio</a>, <a href="/search/astro-ph?searchtype=author&query=Bazzi%2C+Z">Zein Bazzi</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="2312.03995v1-abstract-short" style="display: inline;"> We present a $^{12}$CO($J$=2-1) survey of 60 local galaxies using data from the Atacama Large Millimeter/submillimeter Compact Array as part of the Extragalactic Database for Galaxy Evolution: the ACA EDGE survey. These galaxies all have integral field spectroscopy from the CALIFA survey. Compared to other local galaxy surveys, ACA EDGE is designed to mitigate selection effects based on CO brightn… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.03995v1-abstract-full').style.display = 'inline'; document.getElementById('2312.03995v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.03995v1-abstract-full" style="display: none;"> We present a $^{12}$CO($J$=2-1) survey of 60 local galaxies using data from the Atacama Large Millimeter/submillimeter Compact Array as part of the Extragalactic Database for Galaxy Evolution: the ACA EDGE survey. These galaxies all have integral field spectroscopy from the CALIFA survey. Compared to other local galaxy surveys, ACA EDGE is designed to mitigate selection effects based on CO brightness and morphological type. Of the 60 galaxies in ACA EDGE, 36 are on the star-formation main sequence, 13 are on the red sequence, and 11 lie in the ``green valley" transition between these sequences. We test how star formation quenching processes affect the star formation rate (SFR) per unit molecular gas mass, SFE$_{\rm mol}=$SFR/$M_{\rm mol}$, and related quantities in galaxies with stellar masses $10\leq$log[$M_\star/$M$_\odot$]$\leq11.5$ covering the full range of morphological types. We observe a systematic decrease of the molecular-to-stellar mass fraction ($R^{\rm mol}_{\star}$) with decreasing level of star formation activity, with green valley galaxies having also lower SFE$_{\rm mol}$ than galaxies on the main sequence. On average, we find that the spatially resolved SFE$_{\rm mol}$ within the bulge region of green valley galaxies is lower than in the bulges of main sequence galaxies if we adopt a constant CO-to-H$_2$ conversion factor, $伪_{\rm CO}$. While efficiencies in main sequence galaxies remain almost constant with galactocentric radius, in green valley galaxies we note a systematic increase of SFE$_{\rm mol}$, $R^{\rm mol}_{\star}$, and specific star formation rate, sSFR, with increasing radius. Our results suggest that although gas depletion (or removal) seems to be the most important driver of the star-formation quenching in galaxies transiting through the green valley, a reduction in star formation efficiency is also required during this stage. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.03995v1-abstract-full').style.display = 'none'; document.getElementById('2312.03995v1-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 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </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/2311.13684">arXiv:2311.13684</a> <span> [<a href="https://arxiv.org/pdf/2311.13684">pdf</a>, <a href="https://arxiv.org/format/2311.13684">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"> GBT/Argus Observations of Molecular Gas in the Inner Regions of IC 342 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Li%2C+J">Jialu Li</a>, <a href="/search/astro-ph?searchtype=author&query=Harris%2C+A+I">Andrew I Harris</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Kepley%2C+A">Amanda Kepley</a>, <a href="/search/astro-ph?searchtype=author&query=Frayer%2C+D">David Frayer</a>, <a href="/search/astro-ph?searchtype=author&query=Bolatto%2C+A">Alberto Bolatto</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=Meyer%2C+J+D">Jennifer Donovan Meyer</a>, <a href="/search/astro-ph?searchtype=author&query=Church%2C+S">Sarah Church</a>, <a href="/search/astro-ph?searchtype=author&query=Gundersen%2C+J+O">Joshua Ott Gundersen</a>, <a href="/search/astro-ph?searchtype=author&query=Cleary%2C+K">Kieran Cleary</a>, <a href="/search/astro-ph?searchtype=author&query=members%2C+D+t">DEGAS team members</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="2311.13684v1-abstract-short" style="display: inline;"> We report observations of the ground state transitions of $^{12}$CO, $^{13}$CO C$^{18}$O, HCN, and HCO$^+$ at 88-115 GHz in the inner region of the nearby galaxy IC 342. These data were obtained with the 16-pixel spectroscopic focal plane array Argus on the 100-m Robert C. Byrd Green Bank Telescope (GBT) at 6-9$^{\prime\prime}$ resolution. In the nuclear bar region, the intensity distributions of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.13684v1-abstract-full').style.display = 'inline'; document.getElementById('2311.13684v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.13684v1-abstract-full" style="display: none;"> We report observations of the ground state transitions of $^{12}$CO, $^{13}$CO C$^{18}$O, HCN, and HCO$^+$ at 88-115 GHz in the inner region of the nearby galaxy IC 342. These data were obtained with the 16-pixel spectroscopic focal plane array Argus on the 100-m Robert C. Byrd Green Bank Telescope (GBT) at 6-9$^{\prime\prime}$ resolution. In the nuclear bar region, the intensity distributions of $^{12}$CO(1-0) and $^{13}$CO(1-0) emission trace moderate densities, and differ from the dense gas distributions sampled in C$^{18}$O(1-0), HCN(1-0), and HCO$^+$(1-0). We observe a constant HCN(1-0)-to-HCO$^+$(1-0) ratio of 1.2$\pm$0.1 across the whole $\sim$1 kpc bar. This indicates that HCN(1-0) and HCO$^+$(1-0) lines have intermediate optical depth, and that the corresponding $n_{\textrm{H}_2}$ of the gas producing the emission is of 10$^{4.5-6}$ cm$^{-3}$. We show that HCO$^+$(1-0) is thermalized and HCN(1-0) is close to thermalization. The very tight correlation between HCN(1-0) and HCO$^+$(1-0) intensities across the 1~kpc bar suggests that this ratio is more sensitive to the relative abundance of the two species than to the gas density. We confirm the angular offset ($\sim$10$^{\prime\prime}$) between the spatial distribution of molecular gas and the star formation sites. Finally, we find a breakdown of the $L_\textrm{IR}$-$L_\textrm{HCN}$ correlation at high spatial resolution due to the effect of incomplete sampling of star-forming regions by HCN emission in IC 342. The scatter of the $L_\textrm{IR}$-$L_\textrm{HCN}$ relation decreases as the spatial scale increases from 10$^{\prime\prime}$~to 30$^{\prime\prime}$ (170-510~pc), and is comparable to the scatter of the global relation at the scale of 340 pc. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.13684v1-abstract-full').style.display = 'none'; document.getElementById('2311.13684v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">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">Accepted for publication in ApJ. 18 pages, 10 figures, and 4 tables. Comments are more than 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/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/2310.06501">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/2309.15906">arXiv:2309.15906</a> <span> [<a href="https://arxiv.org/pdf/2309.15906">pdf</a>, <a href="https://arxiv.org/format/2309.15906">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"> [CII] Spectral Mapping of the Galactic Wind and Starbursting Disk of M82 with SOFIA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Levy%2C+R+C">Rebecca C. Levy</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=Tarantino%2C+E">Elizabeth Tarantino</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=Armus%2C+L">Lee Armus</a>, <a href="/search/astro-ph?searchtype=author&query=Emig%2C+K+L">Kimberly L. Emig</a>, <a href="/search/astro-ph?searchtype=author&query=Herrera-Camus%2C+R">Rodrigo Herrera-Camus</a>, <a href="/search/astro-ph?searchtype=author&query=Marrone%2C+D+P">Daniel P. Marrone</a>, <a href="/search/astro-ph?searchtype=author&query=Mills%2C+E">Elisabeth Mills</a>, <a href="/search/astro-ph?searchtype=author&query=Ricken%2C+O">Oliver Ricken</a>, <a href="/search/astro-ph?searchtype=author&query=Stutzki%2C+J">Juergen Stutzki</a>, <a href="/search/astro-ph?searchtype=author&query=Veilleux%2C+S">Sylvain Veilleux</a>, <a href="/search/astro-ph?searchtype=author&query=Walter%2C+F">Fabian Walter</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="2309.15906v1-abstract-short" style="display: inline;"> M82 is an archetypal starburst galaxy in the local Universe. The central burst of star formation, thought to be triggered by M82's interaction with other members in the M81 group, is driving a multiphase galaxy-scale wind away from the plane of the disk that has been studied across the electromagnetic spectrum. Here, we present new velocity-resolved observations of the [CII] 158$渭$m line in the ce… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.15906v1-abstract-full').style.display = 'inline'; document.getElementById('2309.15906v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.15906v1-abstract-full" style="display: none;"> M82 is an archetypal starburst galaxy in the local Universe. The central burst of star formation, thought to be triggered by M82's interaction with other members in the M81 group, is driving a multiphase galaxy-scale wind away from the plane of the disk that has been studied across the electromagnetic spectrum. Here, we present new velocity-resolved observations of the [CII] 158$渭$m line in the central disk and the southern outflow of M82 using the upGREAT instrument onboard SOFIA. We also report the first detections of velocity-resolved ($螖V = 10$ km s$^{-1}$) [CII] emission in the outflow of M82 at projected distances of $\approx1-2$ kpc south of the galaxy center. We compare the [CII] line profiles to observations of CO and HI and find that likely the majority ($>55$%) of the [CII] emission in the outflow is associated with the neutral atomic medium. We find that the fraction of [CII] actually outflowing from M82 is small compared to the bulk gas outside the midplane (which may be in a halo or tidal streamers), which has important implications for observations of [CII] outflows at higher redshift. Finally, by comparing the observed ratio of the [CII] and CO intensities to models of photodissociation regions, we estimate that the far-ultraviolet (FUV) radiation field in the disk is $\sim10^{3.5}~G_0$, in agreement with previous estimates. In the outflow, however, the FUV radiation field is 2-3 orders of magnitudes lower, which may explain the high fraction of [CII] arising from the neutral medium in the wind. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.15906v1-abstract-full').style.display = 'none'; document.getElementById('2309.15906v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 September, 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">22 pages, 9 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/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> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.10277">arXiv:2307.10277</a> <span> [<a href="https://arxiv.org/pdf/2307.10277">pdf</a>, <a href="https://arxiv.org/format/2307.10277">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/10.1051/0004-6361/202346919">10.1051/0004-6361/202346919 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Quantifying the energy balance between the turbulent ionised gas and young stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Egorov%2C+O+V">Oleg V. Egorov</a>, <a href="/search/astro-ph?searchtype=author&query=Kreckel%2C+K">Kathryn Kreckel</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=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=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=Sarbadhicary%2C+S+K">Sumit K. Sarbadhicary</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Watkins%2C+E+J">Elizabeth J. Watkins</a>, <a href="/search/astro-ph?searchtype=author&query=Whitmore%2C+B+C">Brad C. Whitmore</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=Congiu%2C+E">Enrico Congiu</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=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=M%C3%A9ndez-Delgado%2C+J+E">J. Eduardo M茅ndez-Delgado</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=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="2307.10277v2-abstract-short" style="display: inline;"> We investigate the ionised gas morphology, excitation properties, and kinematics in 19 nearby star-forming galaxies from the PHANGS-MUSE survey. We directly compare the kinetic energy of expanding superbubbles and the turbulent motions in the interstellar medium with the mechanical energy deposited by massive stars in the form of winds and supernovae, with the aim to answer whether the stellar fee… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.10277v2-abstract-full').style.display = 'inline'; document.getElementById('2307.10277v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.10277v2-abstract-full" style="display: none;"> We investigate the ionised gas morphology, excitation properties, and kinematics in 19 nearby star-forming galaxies from the PHANGS-MUSE survey. We directly compare the kinetic energy of expanding superbubbles and the turbulent motions in the interstellar medium with the mechanical energy deposited by massive stars in the form of winds and supernovae, with the aim to answer whether the stellar feedback is responsible for the observed turbulent motions and to quantify the fraction of mechanical energy retained in the superbubbles. Based on the distribution of the flux and velocity dispersion in the H$伪$ line, we select 1484 regions of locally elevated velocity dispersion ($蟽$(H$伪$)>45 km/s), including at least 171 expanding superbubbles. We analyse these regions and relate their properties to those of the young stellar associations and star clusters identified in PHANGS-HST data. We find a good correlation between the kinetic energy of the ionised gas and the total mechanical energy input from supernovae and stellar winds from the stellar associations, with a typical coupling efficiency of 10-20%. The contribution of mechanical energy by the supernovae alone is not sufficient to explain the measured kinetic energy of the ionised gas, which implies that pre-supernova feedback in the form of radiation/thermal pressure and winds is necessary. We find that the gas kinetic energy decreases with metallicity for our sample covering Z=0.5-1.0 Zsun, reflecting the lower impact of stellar feedback. For the sample of superbubbles, we find that about 40% of the young stellar associations are preferentially located in their rims. We also find a slightly higher (by ~15%) fraction of the youngest (<3 Myr) stellar associations in the rims of the superbubbles than in the centres, and the opposite for older associations, which implies possible propagation or triggering of star formation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.10277v2-abstract-full').style.display = 'none'; document.getElementById('2307.10277v2-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 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by A&A. The abstract is abridged. 31 pages (including 8 pages in appendix), 20 figures, 2 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 678, A153 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.11811">arXiv:2306.11811</a> <span> [<a href="https://arxiv.org/pdf/2306.11811">pdf</a>, <a href="https://arxiv.org/format/2306.11811">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/10.1051/0004-6361/202347175">10.1051/0004-6361/202347175 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Calibrating mid-infrared emission as a tracer of obscured star formation on HII-region scales in the era of JWST </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=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=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=Congiu%2C+E">Enrico Congiu</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=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=Hassani%2C+H">Hamid Hassani</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=Neumann%2C+L">Lukas Neumann</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=Rosolowsky%2C+E">Erik Rosolowsky</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=Sandstrom%2C+K">Karin Sandstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</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="2306.11811v2-abstract-short" style="display: inline;"> Measurements of the star formation activity on cloud scales are fundamental to uncovering the physics of the molecular cloud, star formation, and stellar feedback cycle in galaxies. Infrared (IR) emission from small dust grains and polycyclic aromatic hydrocarbons (PAHs) are widely used to trace the obscured component of star formation. However, the relation between these emission features and dus… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.11811v2-abstract-full').style.display = 'inline'; document.getElementById('2306.11811v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.11811v2-abstract-full" style="display: none;"> Measurements of the star formation activity on cloud scales are fundamental to uncovering the physics of the molecular cloud, star formation, and stellar feedback cycle in galaxies. Infrared (IR) emission from small dust grains and polycyclic aromatic hydrocarbons (PAHs) are widely used to trace the obscured component of star formation. However, the relation between these emission features and dust attenuation is complicated by the combined effects of dust heating from old stellar populations and an uncertain dust geometry with respect to heating sources. We use images obtained with NIRCam and MIRI as part of the PHANGS--JWST survey to calibrate dust emission at 21$\rm 渭m$, and the emission in the PAH-tracing bands at 3.3, 7.7, 10, and 11.3$\rm 渭m$ as tracers of obscured star formation. We analyse $\sim$ 20000 optically selected HII regions across 19 nearby star-forming galaxies, and benchmark their IR emission against dust attenuation measured from the Balmer decrement. We model the extinction-corrected H$伪$ flux as the sum of the observed H$伪$ emission and a term proportional to the IR emission, with $a_{IR}$ as the proportionality coefficient. A constant $a_{IR}$ leads to extinction-corrected H$伪$ estimates which agree with those obtained with the Balmer decrement with a scatter of $\sim$ 0.1 dex for all bands considered. Among these bands, 21$\rm 渭m$ emission is demonstrated to be the best tracer of dust attenuation. The PAH-tracing bands underestimate the correction for bright HII regions, since in these environments the ratio of PAH-tracing bands to 21$\rm 渭m$ decreases, signalling destruction of the PAH molecules. For fainter HII regions all bands suffer from an increasing contamination from the diffuse infrared background. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.11811v2-abstract-full').style.display = 'none'; document.getElementById('2306.11811v2-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 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">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 678, A129 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.07640">arXiv:2306.07640</a> <span> [<a href="https://arxiv.org/pdf/2306.07640">pdf</a>, <a href="https://arxiv.org/format/2306.07640">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 EDGE-CALIFA Survey: Spatially Resolved 13CO(1-0) Observations and Variations in 12CO(1-0)/13CO(1-0) in Nearby Galaxies on kpc Scales </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Y">Yixian Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Wong%2C+T">Tony Wong</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=Leroy%2C+A">Adam Leroy</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=Utomo%2C+D">Dyas Utomo</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez%2C+S">Sebastian Sanchez</a>, <a href="/search/astro-ph?searchtype=author&query=Barrera-Ballesteros%2C+J">Jorge Barrera-Ballesteros</a>, <a href="/search/astro-ph?searchtype=author&query=Levy%2C+R">Rebecca Levy</a>, <a href="/search/astro-ph?searchtype=author&query=Colombo%2C+D">Dario Colombo</a>, <a href="/search/astro-ph?searchtype=author&query=Blitz%2C+L">Leo Blitz</a>, <a href="/search/astro-ph?searchtype=author&query=Vogel%2C+S">Stuart Vogel</a>, <a href="/search/astro-ph?searchtype=author&query=Puschnig%2C+J">Johannes Puschnig</a>, <a href="/search/astro-ph?searchtype=author&query=Villanueva%2C+V">Vicente Villanueva</a>, <a href="/search/astro-ph?searchtype=author&query=Rubio%2C+M">Monica Rubio</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.07640v1-abstract-short" style="display: inline;"> We present 13CO(1-0) observations for the EDGE-CALIFA survey, which is a mapping survey of 126 nearby galaxies at a typical spatial resolution of 1.5 kpc. Using detected 12CO(1-0) emission as a prior, we detect 13CO(1-0) in 41 galaxies via integrated line flux over the entire galaxy, and in 30 galaxies via integrated line intensity in resolved synthesized beams. Incorporating our CO observations a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.07640v1-abstract-full').style.display = 'inline'; document.getElementById('2306.07640v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.07640v1-abstract-full" style="display: none;"> We present 13CO(1-0) observations for the EDGE-CALIFA survey, which is a mapping survey of 126 nearby galaxies at a typical spatial resolution of 1.5 kpc. Using detected 12CO(1-0) emission as a prior, we detect 13CO(1-0) in 41 galaxies via integrated line flux over the entire galaxy, and in 30 galaxies via integrated line intensity in resolved synthesized beams. Incorporating our CO observations and optical IFU spectroscopy, we perform a systematic comparison between the line ratio R12/13 and the properties of the stars and ionized gas. Higher R12/13 values are found in interacting galaxies than in non-interacting galaxies. The global R12/13 slightly increases with infrared color F60/F100, but appears insensitive to other host galaxy properties such as morphology, stellar mass, or galaxy size. We also present annulus-averaged R12/13 profiles for our sample up to a galactocentric radius of 0.4r25 (~6 kpc), taking into account the 13CO(1-0) non-detections by spectral stacking. The radial profiles of R12/13 are quite flat across our sample. Within galactocentric distances of 0.2r25, azimuthally-averaged R12/13 increases with star formation rate. However, the Spearman rank correlation tests show the azimuthally-averaged R12/13 does not strongly correlate with any other gas or stellar properties in general, especially beyond 0.2r25 from the galaxy centers. Our findings suggest that in the complex environments in galaxy disks, R12/13 is not a sensitive tracer for ISM properties. Dynamical disturbances, like galaxy interactions or the presence of a bar, also have an overall impact on R12/13, which further complicate the interpretations of R12/13 variations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.07640v1-abstract-full').style.display = 'none'; document.getElementById('2306.07640v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">35pages, 11 figure, 6 tables, accepted for publication in ApJS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.17172">arXiv:2305.17172</a> <span> [<a href="https://arxiv.org/pdf/2305.17172">pdf</a>, <a href="https://arxiv.org/format/2305.17172">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/10.1051/0004-6361/202346318">10.1051/0004-6361/202346318 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gas Morphology of Nearby Star-Forming Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Stuber%2C+S+K">S. K. Stuber</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">E. Schinnerer</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=Querejeta%2C+M">M. Querejeta</a>, <a href="/search/astro-ph?searchtype=author&query=Meidt%2C+S">S. Meidt</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">E. Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A">A. Barnes</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+J">J. Neumann</a>, <a href="/search/astro-ph?searchtype=author&query=Sormani%2C+M+C">M. C. Sormani</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=Dale%2C+D">D. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Faesi%2C+C">C. Faesi</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=Grasha%2C+K">K. Grasha</a>, <a href="/search/astro-ph?searchtype=author&query=Kruijssen%2C+J+M+D">J. M. D. Kruijssen</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">D. Liu</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=Pinna%2C+F">F. Pinna</a>, <a href="/search/astro-ph?searchtype=author&query=Saito%2C+T">T. Saito</a>, <a href="/search/astro-ph?searchtype=author&query=Usero%2C+A">A. Usero</a>, <a href="/search/astro-ph?searchtype=author&query=Watkins%2C+E+J">E. 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="2305.17172v1-abstract-short" style="display: inline;"> The morphology of a galaxy stems from secular and environmental processes during its evolutionary history. Thus galaxy morphologies have been a long used tool to gain insights on galaxy evolution. We visually classify morphologies on cloud-scales based on the molecular gas distribution of a large sample of 79 nearby main-sequence galaxies, using 1'' resolution CO(2-1) ALMA observations taken as pa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.17172v1-abstract-full').style.display = 'inline'; document.getElementById('2305.17172v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.17172v1-abstract-full" style="display: none;"> The morphology of a galaxy stems from secular and environmental processes during its evolutionary history. Thus galaxy morphologies have been a long used tool to gain insights on galaxy evolution. We visually classify morphologies on cloud-scales based on the molecular gas distribution of a large sample of 79 nearby main-sequence galaxies, using 1'' resolution CO(2-1) ALMA observations taken as part of the PHANGS survey. To do so, we devise a morphology classification scheme for different types of bars, spiral arms (grand-design, flocculent, multi-arm and smooth), rings (central and non-central rings) similar to the well-established optical ones, and further introduce bar lane classes. In general, our cold gas based morphologies agree well with the ones based on stellar light. Both our bars as well as grand-design spiral arms are preferentially found at the higher mass end of our sample. Our gas-based classification indicates a potential for misidentification of unbarred galaxies in the optical when massive star formation is present. Central or nuclear rings are present in a third of the sample with a strong preferences for barred galaxies (59%). As stellar bars are present in 45$\pm$5% of our sample galaxies, we explore the utility of molecular gas as tracer of bar lane properties. We find that more curved bar lanes have a shorter radial extent in molecular gas and reside in galaxies with lower molecular to stellar mass ratios than those with straighter geometries. Galaxies display a wide range of CO morphology, and this work provides a catalogue of morphological features in a representative sample of nearby galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.17172v1-abstract-full').style.display = 'none'; document.getElementById('2305.17172v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 14 figures (+ Appendix 9 pages, 4 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 676, A113 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.14437">arXiv:2305.14437</a> <span> [<a href="https://arxiv.org/pdf/2305.14437">pdf</a>, <a href="https://arxiv.org/format/2305.14437">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/stad1554">10.1093/mnras/stad1554 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Fuelling the nuclear ring of NGC 1097 </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Sun%2C+J">Jiayi Sun</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=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</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=Glover%2C+S+C+O">Simon C. O. Glover</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=Meidt%2C+S+E">Sharon E. 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=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=Eibensteiner%2C+C">Cosima Eibensteiner</a>, <a href="/search/astro-ph?searchtype=author&query=Fragkoudi%2C+F">Francesca Fragkoudi</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=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. Diederik Kruijssen</a>, <a href="/search/astro-ph?searchtype=author&query=Neumayer%2C+N">Nadine Neumayer</a>, <a href="/search/astro-ph?searchtype=author&query=Pinna%2C+F">Francesca Pinna</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=Smith%2C+R+J">Rowan J. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Teng%2C+Y">Yu-Hsuan Teng</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="2305.14437v1-abstract-short" style="display: inline;"> Galactic bars can drive cold gas inflows towards the centres of galaxies. The gas transport happens primarily through the so-called bar ``dust lanes'', which connect the galactic disc at kpc scales to the nuclear rings at hundreds of pc scales much like two gigantic galactic rivers. Once in the ring, the gas can fuel star formation activity, galactic outflows, and central supermassive black holes.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.14437v1-abstract-full').style.display = 'inline'; document.getElementById('2305.14437v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.14437v1-abstract-full" style="display: none;"> Galactic bars can drive cold gas inflows towards the centres of galaxies. The gas transport happens primarily through the so-called bar ``dust lanes'', which connect the galactic disc at kpc scales to the nuclear rings at hundreds of pc scales much like two gigantic galactic rivers. Once in the ring, the gas can fuel star formation activity, galactic outflows, and central supermassive black holes. Measuring the mass inflow rates is therefore important to understanding the mass/energy budget and evolution of galactic nuclei. In this work, we use CO datacubes from the PHANGS-ALMA survey and a simple geometrical method to measure the bar-driven mass inflow rate onto the nuclear ring of the barred galaxy NGC~1097. The method assumes that the gas velocity in the bar lanes is parallel to the lanes in the frame co-rotating with the bar, and allows one to derive the inflow rates from sufficiently sensitive and resolved position-position-velocity diagrams if the bar pattern speed and galaxy orientations are known. We find an inflow rate of $\dot{M}=(3.0 \pm 2.1)\, \rm M_\odot\, yr^{-1}$ averaged over a time span of 40 Myr, which varies by a factor of a few over timescales of $\sim$10 Myr. Most of the inflow appears to be consumed by star formation in the ring which is currently occurring at a rate of ${\rm SFR}\simeq~1.8$-$2 \rm M_\odot\, yr^{-1}$, suggesting that the inflow is causally controlling the star formation rate in the ring as a function of time. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.14437v1-abstract-full').style.display = 'none'; document.getElementById('2305.14437v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.10240">arXiv:2305.10240</a> <span> [<a href="https://arxiv.org/pdf/2305.10240">pdf</a>, <a href="https://arxiv.org/format/2305.10240">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/10.1051/0004-6361/202346129">10.1051/0004-6361/202346129 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spectral Stacking of Radio-Interferometric Data </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=Brok%2C+J+S+d">Jakob S. den Brok</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">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=Barnes%2C+A+T">Ashley T. Barnes</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=Eibensteiner%2C+C">Cosima Eibensteiner</a>, <a href="/search/astro-ph?searchtype=author&query=Held%2C+M">Malena Held</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=Pety%2C+J">J茅r么me Pety</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=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="2305.10240v1-abstract-short" style="display: inline;"> Mapping molecular line emission beyond the bright low-J CO transitions is still challenging in extragalactic studies, even with the latest generation of (sub-)mm interferometers, such as ALMA and NOEMA. We summarise and test a spectral stacking method that has been used in the literature to recover low-intensity molecular line emission, such as HCN(1-0), HCO+(1-0), and even fainter lines in extern… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.10240v1-abstract-full').style.display = 'inline'; document.getElementById('2305.10240v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.10240v1-abstract-full" style="display: none;"> Mapping molecular line emission beyond the bright low-J CO transitions is still challenging in extragalactic studies, even with the latest generation of (sub-)mm interferometers, such as ALMA and NOEMA. We summarise and test a spectral stacking method that has been used in the literature to recover low-intensity molecular line emission, such as HCN(1-0), HCO+(1-0), and even fainter lines in external galaxies. The goal is to study the capabilities and limitations of the stacking technique when applied to imaged interferometric observations. The core idea of spectral stacking is to align spectra of the low S/N spectral lines to a known velocity field calculated from a higher S/N line expected to share the kinematics of the fainter line, e.g., CO(1-0) or 21-cm emission. Then these aligned spectra can be coherently averaged to produce potentially high S/N spectral stacks. Here, we use imaged simulated interferometric and total power observations at different signal-to-noise levels, based on real CO observations. For the combined interferometric and total power data, we find that the spectral stacking technique is capable of recovering the integrated intensities even at low S/N levels across most of the region where the high S/N prior is detected. However, when stacking interferometer-only data for low S/N emission, the stacks can miss up to 50% of the emission from the fainter line. A key result of this analysis is that the spectral stacking method is able to recover the true mean line intensities in low S/N cubes and to accurately measure the statistical significance of the recovered lines. To facilitate the application of this technique we provide a public Python package, called PyStacker. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.10240v1-abstract-full').style.display = 'none'; document.getElementById('2305.10240v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 10 figures, accepted for pub in A&A, Apr 28, 2023</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 675, A104 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.03650">arXiv:2305.03650</a> <span> [<a href="https://arxiv.org/pdf/2305.03650">pdf</a>, <a href="https://arxiv.org/format/2305.03650">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/10.1051/0004-6361/202244520">10.1051/0004-6361/202244520 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The impact of HII regions on Giant Molecular Cloud properties in nearby galaxies sampled by PHANGS ALMA and MUSE </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zakardjian%2C+A">Antoine Zakardjian</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=Herrera%2C+C+N">Cinthya N. Herrera</a>, <a href="/search/astro-ph?searchtype=author&query=Hughes%2C+A">Annie Hughes</a>, <a href="/search/astro-ph?searchtype=author&query=Oakes%2C+E">Elias Oakes</a>, <a href="/search/astro-ph?searchtype=author&query=Kreckel%2C+K">Kathryn Kreckel</a>, <a href="/search/astro-ph?searchtype=author&query=Faesi%2C+C">Chris Faesi</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=Meidt%2C+S">Sharon Meidt</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A">Ashley Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Belfiore%2C+F">Francesco Belfiore</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=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=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=Brok%2C+J+d">Jakob den Brok</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=Garc%C3%ADa-Rodr%C3%ADguez%2C+A">Axel Garc铆a-Rodr铆guez</a>, <a href="/search/astro-ph?searchtype=author&query=Grasha%2C+K">Kathryn Grasha</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> , 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="2305.03650v1-abstract-short" style="display: inline;"> We identify giant molecular clouds (GMCs) associated with HII regions for a sample of 19 nearby galaxies using catalogs of GMCs and H regions released by the PHANGS-ALMA and PHANGS-MUSE surveys, using the overlap of the CO and H伪 emission as the key criterion for physical association. We compare the distributions of GMC and HII region properties for paired and non-paired objects. We investigate co… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.03650v1-abstract-full').style.display = 'inline'; document.getElementById('2305.03650v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.03650v1-abstract-full" style="display: none;"> We identify giant molecular clouds (GMCs) associated with HII regions for a sample of 19 nearby galaxies using catalogs of GMCs and H regions released by the PHANGS-ALMA and PHANGS-MUSE surveys, using the overlap of the CO and H伪 emission as the key criterion for physical association. We compare the distributions of GMC and HII region properties for paired and non-paired objects. We investigate correlations between GMC and HII region properties among galaxies and across different galactic environments to determine whether GMCs that are associated with HII regions have significantly distinct physical properties to the parent GMC population. We identify trends between the H伪 luminosity of an HII region and the CO peak brightness and the molecular mass of GMCs that we tentatively attribute to a direct physical connection between the matched objects, and which arise independently of underlying environmental variations of GMC and HII region properties within galaxies. The study of the full sample nevertheless hides a large variability galaxy by galaxy. Our results suggests that at the ~100 pc scales accessed by the PHANGS-ALMA and PHANGS-MUSE data, pre-supernova feedback mechanisms in HII regions have a subtle but measurable impact on the properties of the surrounding molecular gas, as inferred from CO observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.03650v1-abstract-full').style.display = 'none'; document.getElementById('2305.03650v1-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 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 678, A171 (2023) </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" 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