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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=Privon%2C+G&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Privon%2C+G&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Privon%2C+G&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Privon%2C+G&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> </ul> </nav> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.19397">arXiv:2501.19397</a> <span> [<a href="https://arxiv.org/pdf/2501.19397">pdf</a>, <a href="https://arxiv.org/format/2501.19397">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 Spectroscopically Calibrated Prescription for Extracting PAH Flux from JWST MIRI Imaging </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Donnelly%2C+G+P">Grant P. Donnelly</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=Armus%2C+L">Lee Armus</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%ADaz-Santos%2C+T">Tanio D铆az-Santos</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=Barcos-Mu%C3%B1oz%2C+L">Loreto Barcos-Mu帽oz</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchin%2C+M">Marina Bianchin</a>, <a href="/search/astro-ph?searchtype=author&query=Bohn%2C+T">Thomas Bohn</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=Buiten%2C+V+A">Victorine A. Buiten</a>, <a href="/search/astro-ph?searchtype=author&query=Charmandaris%2C+V">Vassilis Charmandaris</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+A+S">Aaron S. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Howell%2C+J">Justin Howell</a>, <a href="/search/astro-ph?searchtype=author&query=Inami%2C+H">Hanae Inami</a>, <a href="/search/astro-ph?searchtype=author&query=Kakkad%2C+D">Darshan Kakkad</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=Linden%2C+S+T">Sean T. Linden</a>, <a href="/search/astro-ph?searchtype=author&query=Lofaro%2C+C+M">Cristina M. Lofaro</a>, <a href="/search/astro-ph?searchtype=author&query=Malkan%2C+M+A">Matthew A. Malkan</a>, <a href="/search/astro-ph?searchtype=author&query=Medling%2C+A+M">Anne M. Medling</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+J+D+T">J. D. T. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Song%2C+Y">Yiqing Song</a>, <a href="/search/astro-ph?searchtype=author&query=Stierwalt%2C+S">Sabrina Stierwalt</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="2501.19397v1-abstract-short" style="display: inline;"> We introduce a prescription for estimating the flux of the 7.7 micron and 11.3 micron\ polycyclic aromatic hydrocarbon (PAH) features from broadband JWST/MIRI images. Probing PAH flux with MIRI imaging data has advantages in field of view, spatial resolution, and sensitivity compared with MIRI spectral maps, but comparisons with spectra are needed to calibrate these flux estimations over a wide va… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.19397v1-abstract-full').style.display = 'inline'; document.getElementById('2501.19397v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.19397v1-abstract-full" style="display: none;"> We introduce a prescription for estimating the flux of the 7.7 micron and 11.3 micron\ polycyclic aromatic hydrocarbon (PAH) features from broadband JWST/MIRI images. Probing PAH flux with MIRI imaging data has advantages in field of view, spatial resolution, and sensitivity compared with MIRI spectral maps, but comparisons with spectra are needed to calibrate these flux estimations over a wide variety of environments. For 267 MIRI/MRS spectra from independent regions in the four luminous infrared galaxies (LIRGs) in the Great Observatories All-sky LIRG Survey (GOALS) early release science program, we derive synthetic filter photometry and directly compare estimated PAH fluxes to those measured from detailed spectral fits. We find that for probing PAH 7.7 micron, the best combination of filters is F560W, F770W, and either F1500W or F2100W, and the best for PAH 11.3 micron is F560W, F1000W, F1130W, and F1500W. The prescription with these combinations yields predicted flux densities that typically agree with values from spectral decomposition within ~7% and ~5% for PAH 7.7 and 11.3 micron, respectively. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.19397v1-abstract-full').style.display = 'none'; document.getElementById('2501.19397v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.07985">arXiv:2412.07985</a> <span> [<a href="https://arxiv.org/pdf/2412.07985">pdf</a>, <a href="https://arxiv.org/format/2412.07985">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ad9bab">10.3847/1538-4357/ad9bab <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Arp 240 Galaxy Merger: A Detailed Look at the Molecular Kennicutt-Schmidt Star Formation Law on Sub-kpc Scales </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Saravia%2C+A">Alejandro Saravia</a>, <a href="/search/astro-ph?searchtype=author&query=Rodas-Quito%2C+E">Eduardo Rodas-Quito</a>, <a href="/search/astro-ph?searchtype=author&query=Barcos-Mu%C3%B1oz%2C+L">Loreto Barcos-Mu帽oz</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+A+S">Aaron S. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Kunneriath%2C+D">Devaky Kunneriath</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G">George Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Song%2C+Y">Yiqing Song</a>, <a href="/search/astro-ph?searchtype=author&query=Yoon%2C+I">Ilsang Yoon</a>, <a href="/search/astro-ph?searchtype=author&query=Emig%2C+K">Kimberly Emig</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Garc%C3%ADa%2C+M">Mar铆a S谩nchez-Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Linden%2C+S">Sean Linden</a>, <a href="/search/astro-ph?searchtype=author&query=Green%2C+K">Kara Green</a>, <a href="/search/astro-ph?searchtype=author&query=Johnstone%2C+M">Makoto Johnstone</a>, <a href="/search/astro-ph?searchtype=author&query=Nagarajan-Swenson%2C+J">Jaya Nagarajan-Swenson</a>, <a href="/search/astro-ph?searchtype=author&query=Meza%2C+G">Gabriela Meza</a>, <a href="/search/astro-ph?searchtype=author&query=Momjian%2C+E">Emmanuel Momjian</a>, <a href="/search/astro-ph?searchtype=author&query=Armus%2C+L">Lee Armus</a>, <a href="/search/astro-ph?searchtype=author&query=Charmandaris%2C+V">Vassilis Charmandaris</a>, <a href="/search/astro-ph?searchtype=author&query=Diaz-Santos%2C+T">Tanio Diaz-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Eibensteiner%2C+C">Cosima Eibensteiner</a>, <a href="/search/astro-ph?searchtype=author&query=Howell%2C+J">Justin Howell</a>, <a href="/search/astro-ph?searchtype=author&query=Inami%2C+H">Hanae Inami</a>, <a href="/search/astro-ph?searchtype=author&query=Kader%2C+J">Justin Kader</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Treister%2C+E">Ezequiel Treister</a> , et al. (3 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.07985v1-abstract-short" style="display: inline;"> The molecular Kennicutt-Schmidt (mK-S) Law has been key for understanding star formation (SF) in galaxies across all redshifts. However, recent sub-kpc observations of nearby galaxies reveal deviations from the nearly unity slope (N) obtained with disk-averaged measurements. We study SF and molecular gas (MG) distribution in the early-stage luminous infrared galaxy merger Arp240 (NGC5257-8). Using… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.07985v1-abstract-full').style.display = 'inline'; document.getElementById('2412.07985v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.07985v1-abstract-full" style="display: none;"> The molecular Kennicutt-Schmidt (mK-S) Law has been key for understanding star formation (SF) in galaxies across all redshifts. However, recent sub-kpc observations of nearby galaxies reveal deviations from the nearly unity slope (N) obtained with disk-averaged measurements. We study SF and molecular gas (MG) distribution in the early-stage luminous infrared galaxy merger Arp240 (NGC5257-8). Using VLA radio continuum (RC) and ALMA CO(2-1) observations with a uniform grid analysis, we estimate SF rates and MG surface densities ($危_{\mathrm{SFR}}$ and $危_{\mathrm{H_2}}$, respectively). In Arp 240, N is sub-linear at 0.52 $\pm$ 0.17. For NGC 5257 and NGC 5258, N is 0.52 $\pm$ 0.16 and 0.75 $\pm$ 0.15, respectively. We identify two SF regimes: high surface brightness (HSB) regions in RC with N $\sim$1, and low surface brightness (LSB) regions with shallow N (ranging 0.15 $\pm$ 0.09 to 0.48 $\pm$ 0.04). Median CO(2-1) linewidth and MG turbulent pressure (P$_{\mathrm{turb}}$) are 25 km s$^{-1}$ and 9 $\times$10$^{5}$ K cm$^{-3}$. No significant correlation was found between $危_{\mathrm{SFR}}$ and CO(2-1) linewidth. However, $危_{\mathrm{SFR}}$ correlates with P$_{\mathrm{turb}}$, particularly in HSB regions ($蟻>$0.60). In contrast, SF efficiency moderately anti-correlates with P$_{\mathrm{turb}}$ in LSB regions but shows no correlation in HSB regions. Additionally, we identify regions where peaks in SF and MG are decoupled, yielding a shallow N ($\leq$ 0.28 $\pm$ 0.18). Overall, the range of N reflects distinct physical properties and distribution of both the SF and MG, which can be masked by disk-averaged measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.07985v1-abstract-full').style.display = 'none'; document.getElementById('2412.07985v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.05371">arXiv:2410.05371</a> <span> [<a href="https://arxiv.org/pdf/2410.05371">pdf</a>, <a href="https://arxiv.org/format/2410.05371">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"> Evolution of the Dual AGN in Mrk 266: A Young AGN and a Rotation Dominated Disk in the SW Nucleus </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ruby%2C+M">Mason Ruby</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%BCller-S%C3%A1nchez%2C+F">Francisco M眉ller-S谩nchez</a>, <a href="/search/astro-ph?searchtype=author&query=Comerford%2C+J+M">Julia M. Comerford</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Cales%2C+S+L">Sabrina L. Cales</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Malkan%2C+M+A">Matthew A. Malkan</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Treister%2C+E">Ezequiel Treister</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="2410.05371v1-abstract-short" style="display: inline;"> Dual active galactic nuclei (AGN) offer a unique opportunity to probe the relationship between super massive black holes (SMBH) and their host galaxies as well as the role of major mergers in triggering AGN activity. The confirmed dual AGN Mrk 266 has been studied extensively with multi-wavelength imaging. Now, high spatial resolution IFU spectroscopy of Mrk 266 provides an opportunity to probe th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.05371v1-abstract-full').style.display = 'inline'; document.getElementById('2410.05371v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.05371v1-abstract-full" style="display: none;"> Dual active galactic nuclei (AGN) offer a unique opportunity to probe the relationship between super massive black holes (SMBH) and their host galaxies as well as the role of major mergers in triggering AGN activity. The confirmed dual AGN Mrk 266 has been studied extensively with multi-wavelength imaging. Now, high spatial resolution IFU spectroscopy of Mrk 266 provides an opportunity to probe the kinematics of both the merger event and AGN feedback. We present for the first time high spatial resolution kinematic maps for both nuclei of Mrk 266 obtained with the Keck OSIRIS IFU spectrograph, utilizing adaptive optics to achieve a resolution of 0.31" and 0.20" for the NE and SW nuclei, respectively. Using the M-sigma relation for mergers, we infer a SMBH mass of approximately 7e7 solar masses for the southwestern nucleus. Additionally, we report that the molecular gas kinematics of the southwestern nucleus are dominated by rotation rather than large-scale chaotic motions. The southwest nucleus also contains both a circumnuclear ring of star formation from which an inflow of molecular gas is likely fueling the AGN and a compact, AGN-dominated outflow of highly ionized gas with a timescale of approximately 2 Myr, significantly shorter than the timescale of the merger. The northeastern nucleus, on the other hand, exhibits complex kinematics related to the merger, including molecular gas that appears to have decoupled from the rotation of the stars. Our results suggest that while the AGN activity in Mrk 266 was likely triggered during the merger, AGN feeding is currently the result of processes internal to each host galaxy, thus resulting in a strong asymmetry between the two nuclei. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.05371v1-abstract-full').style.display = 'none'; document.getElementById('2410.05371v1-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">18 pages, 18 figures, 3 tables. 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/2409.16503">arXiv:2409.16503</a> <span> [<a href="https://arxiv.org/pdf/2409.16503">pdf</a>, <a href="https://arxiv.org/format/2409.16503">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"> GOALS-JWST: Constraining the Emergence Timescale for Massive Star Clusters in NGC 3256 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Linden%2C+S+T">Sean T. Linden</a>, <a href="/search/astro-ph?searchtype=author&query=Lai%2C+T">Thomas Lai</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+A+S">Aaron S. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Armus%2C+L">Lee Armus</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=Rich%2C+J+A">Jeffrey A. Rich</a>, <a href="/search/astro-ph?searchtype=author&query=U%2C+V">Vivian U</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Inami%2C+H">Hanae Inami</a>, <a href="/search/astro-ph?searchtype=author&query=Song%2C+Y">Yiqing Song</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchin%2C+M">Marina Bianchin</a>, <a href="/search/astro-ph?searchtype=author&query=Bohn%2C+T">Thomas Bohn</a>, <a href="/search/astro-ph?searchtype=author&query=Buiten%2C+V+A">Victorine A. Buiten</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez-Garcia%2C+M">Maria Sanchez-Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Kader%2C+J">Justin Kader</a>, <a href="/search/astro-ph?searchtype=author&query=Lenkic%2C+L">Laura Lenkic</a>, <a href="/search/astro-ph?searchtype=author&query=Medling%2C+A+M">Anne M. Medling</a>, <a href="/search/astro-ph?searchtype=author&query=Boeker%2C+T">Torsten Boeker</a>, <a href="/search/astro-ph?searchtype=author&query=Diaz-Santos%2C+T">Tanio Diaz-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Charmandaris%2C+V">Vassilis Charmandaris</a>, <a href="/search/astro-ph?searchtype=author&query=Barcos-Munoz%2C+L">Loreto Barcos-Munoz</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Werf%2C+P">Paul van der Werf</a>, <a href="/search/astro-ph?searchtype=author&query=Stierwalt%2C+S">Sabrina Stierwalt</a>, <a href="/search/astro-ph?searchtype=author&query=Aalto%2C+S">Susanne Aalto</a>, <a href="/search/astro-ph?searchtype=author&query=Appleton%2C+P">Philip Appleton</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="2409.16503v1-abstract-short" style="display: inline;"> We present the results of a James Webb Space Telescope (JWST) NIRCam and NIRSpec investigation into the young massive star cluster (YMC) population of NGC 3256, the most cluster-rich luminous infrared galaxy (LIRG) in the Great Observatories All Sky LIRG Survey. We detect 3061 compact YMC candidates with a $S/N \geq 3$ at F150W, F200W, and F335M. Based on yggdrasil stellar population models, we id… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.16503v1-abstract-full').style.display = 'inline'; document.getElementById('2409.16503v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.16503v1-abstract-full" style="display: none;"> We present the results of a James Webb Space Telescope (JWST) NIRCam and NIRSpec investigation into the young massive star cluster (YMC) population of NGC 3256, the most cluster-rich luminous infrared galaxy (LIRG) in the Great Observatories All Sky LIRG Survey. We detect 3061 compact YMC candidates with a $S/N \geq 3$ at F150W, F200W, and F335M. Based on yggdrasil stellar population models, we identify 116/3061 sources with F150W - F200W $> 0.47$ and F200W - F355M $> -1.37$ colors suggesting they are young (t $\leq 5$ Myr), dusty ($A_{V} = 5 - 15$), and massive ($M_{\odot} > 10^{5}$). This increases the sample of dust-enshrouded YMCs detected in this system by an order of magnitude relative to previous HST studies. With NIRSpec IFU pointings centered on the northern and southern nucleus, we extract the Pa$伪$ and 3.3$渭$m PAH equivalent widths for 8 bright and isolated YMCs. Variations in both the F200W - F335M color and 3.3$渭$m PAH emission with the Pa$伪$ line strength suggest a rapid dust clearing ($< 3 - 4$ Myr) for the emerging YMCs in the nuclei of NGC 3256. Finally, with both the age and dust emission accurately measured we use yggdrasil to derive the color excess (E(B - V)) for all 8 YMCs. We demonstrate that YMCs with strong 3.3$渭$m PAH emission (F200W - F335M $> 0$) correspond to sources with E(B - V) $> 3$, which are typically missed in UV-optical studies. This underscores the importance of deep near-infrared imaging for finding and characterizing these very young and dust-embedded sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.16503v1-abstract-full').style.display = 'none'; document.getElementById('2409.16503v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">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, 7 figures, 1 table; Accepted for publication in ApJL</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.12126">arXiv:2406.12126</a> <span> [<a href="https://arxiv.org/pdf/2406.12126">pdf</a>, <a href="https://arxiv.org/format/2406.12126">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/ad55c9">10.3847/1538-4365/ad55c9 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An Imaging and Spectroscopic Exploration of the Dusty Compact Obscured Nucleus Galaxy Zw~049.057 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gallagher%2C+J+S">J. S. Gallagher</a>, <a href="/search/astro-ph?searchtype=author&query=Kotulla%2C+R">R. Kotulla</a>, <a href="/search/astro-ph?searchtype=author&query=Laufman%2C+L">L. Laufman</a>, <a href="/search/astro-ph?searchtype=author&query=Geist%2C+E">E. Geist</a>, <a href="/search/astro-ph?searchtype=author&query=Aalto%2C+S">S. Aalto</a>, <a href="/search/astro-ph?searchtype=author&query=Falstad%2C+N">N. Falstad</a>, <a href="/search/astro-ph?searchtype=author&query=K%C3%B6nig%2C+S">S. K枚nig</a>, <a href="/search/astro-ph?searchtype=author&query=Krause%2C+J">J. Krause</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G">G. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Wethers%2C+C">C. Wethers</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+A+S">A. S. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Gorski%2C+M">M. Gorski</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.12126v1-abstract-short" style="display: inline;"> Zw~049.057 is a moderate mass, dusty, early-type galaxy that hosts a powerful compact obscured nucleus (CON, L$_{FIR,CON} \geq$10$^{11}$~L$_{\odot}$). The resolution of HST enabled measurements of the stellar light distribution and characterization of dust features. Zw~049.057 is inclined with a prominent three zone disk; the R$\approx$ 1kpc star forming inner dusty disk contains molecular gas, a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.12126v1-abstract-full').style.display = 'inline'; document.getElementById('2406.12126v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.12126v1-abstract-full" style="display: none;"> Zw~049.057 is a moderate mass, dusty, early-type galaxy that hosts a powerful compact obscured nucleus (CON, L$_{FIR,CON} \geq$10$^{11}$~L$_{\odot}$). The resolution of HST enabled measurements of the stellar light distribution and characterization of dust features. Zw~049.057 is inclined with a prominent three zone disk; the R$\approx$ 1kpc star forming inner dusty disk contains molecular gas, a main disk with less dust and an older stellar population, and a newly detected outer stellar region at R$>$6~kpc with circular isophotes. Previously unknown polar dust lanes are signatures of a past minor merger that could have warped the outer disk to near face-on. Dust transmission measurements provide lower limit gas mass estimates for dust features. An extended region with moderate optical depth and M$\geq$ 2$\times$10$^8$~M$_{\odot}$ obscures the central 2~kpc. Optical spectra show strong interstellar Na~D absorption with a constant velocity across the main disk, likely arising in this extraplanar medium. Opacity measurements of the two linear dust features, pillars, give a total mass of $\geq$10$^6$~M$_{\odot}$, flow rates of $\geq$2~M$_{\odot}$~yr$^{-1}$, and few Myr flow times. Dust pillars are associated with the CON and are visible signs of its role in driving large-scale feedback. Our assessments of feedback processes suggest gas recycling sustains the CON. However, radiation pressure driven mass loss and efficient star formation must be avoided for the AGN to retain sufficient gas over its lifespan to produce substantial mass growth of the central black hole. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.12126v1-abstract-full').style.display = 'none'; document.getElementById('2406.12126v1-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">Astrophysical Journal Supplement, in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.06684">arXiv:2406.06684</a> <span> [<a href="https://arxiv.org/pdf/2406.06684">pdf</a>, <a href="https://arxiv.org/format/2406.06684">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Search for neutrino emission from hard X-ray AGN with IceCube </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/astro-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/astro-ph?searchtype=author&query=Ausborm%2C+L">L. Ausborm</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Bash%2C+S">S. Bash</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Beise%2C+J">J. Beise</a>, <a href="/search/astro-ph?searchtype=author&query=Bellenghi%2C+C">C. Bellenghi</a> , et al. (401 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="2406.06684v2-abstract-short" style="display: inline;"> Active Galactic Nuclei (AGN) are promising candidate sources of high-energy astrophysical neutrinos since they provide environments rich in matter and photon targets where cosmic ray interactions may lead to the production of gamma rays and neutrinos. We searched for high-energy neutrino emission from AGN using the $\textit{Swift}$-BAT Spectroscopic Survey (BASS) catalog of hard X-ray sources and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.06684v2-abstract-full').style.display = 'inline'; document.getElementById('2406.06684v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.06684v2-abstract-full" style="display: none;"> Active Galactic Nuclei (AGN) are promising candidate sources of high-energy astrophysical neutrinos since they provide environments rich in matter and photon targets where cosmic ray interactions may lead to the production of gamma rays and neutrinos. We searched for high-energy neutrino emission from AGN using the $\textit{Swift}$-BAT Spectroscopic Survey (BASS) catalog of hard X-ray sources and 12 years of IceCube muon track data. First, upon performing a stacked search, no significant emission was found. Second, we searched for neutrinos from a list of 43 candidate sources and found an excess from the direction of two sources, Seyfert galaxies NGC 1068 and NGC 4151. We observed NGC 1068 at flux $蠁_{谓_渭+\bar谓_渭}$ = $4.02_{-1.52}^{+1.58} \times 10^{-11}$ TeV$^{-1}$ cm$^{-2}$ s$^{-1}$ normalized at 1 TeV, with power-law spectral index, $纬$ = 3.10$^{+0.26}_{-0.22}$, consistent with previous IceCube results. The observation of a neutrino excess from the direction of NGC 4151 is at a post-trial significance of 2.9$蟽$. If interpreted as an astrophysical signal, the excess observed from NGC 4151 corresponds to a flux $蠁_{谓_渭+\bar谓_渭}$ = $1.51_{-0.81}^{+0.99} \times 10^{-11}$ TeV$^{-1}$ cm$^{-2}$ s$^{-1}$ normalized at 1 TeV and $纬$ = 2.83$^{+0.35}_{-0.28}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.06684v2-abstract-full').style.display = 'none'; document.getElementById('2406.06684v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.13459">arXiv:2404.13459</a> <span> [<a href="https://arxiv.org/pdf/2404.13459">pdf</a>, <a href="https://arxiv.org/format/2404.13459">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ad41b5">10.3847/1538-4357/ad41b5 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Stellar Abundances at the Center of Early Type Galaxies with Fine Structure </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Barth%2C+N">Nicholas Barth</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Ezzeddine%2C+R">Rana Ezzeddine</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+A+S">Aaron S. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Treister%2C+E">Ezequiel Treister</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="2404.13459v1-abstract-short" style="display: inline;"> Our understanding of early-type galaxies (ETGs) has grown in the past decade with the advance of full-spectrum fitting techniques used to infer the properties of the stellar populations that make-up the galaxy. We present ages, central velocity dispersions, and abundance ratios relative to Fe of C, N, O, Mg, Si, Ca, Ti, Cr, Mn, Co, Ni, Cu, Sr, Ba, and Eu, derived using full-spectrum fitting techni… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.13459v1-abstract-full').style.display = 'inline'; document.getElementById('2404.13459v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.13459v1-abstract-full" style="display: none;"> Our understanding of early-type galaxies (ETGs) has grown in the past decade with the advance of full-spectrum fitting techniques used to infer the properties of the stellar populations that make-up the galaxy. We present ages, central velocity dispersions, and abundance ratios relative to Fe of C, N, O, Mg, Si, Ca, Ti, Cr, Mn, Co, Ni, Cu, Sr, Ba, and Eu, derived using full-spectrum fitting techniques for three ETGs NGC 2865, NGC 3818, and NGC 4915. Each of these three galaxies were selected because they have optical, disturbed structures (fine structure) that are linked to major merger events that occurred 1, 7, and 6 Gyr ago, respectively. Two of the ETGs, NGC 3818 and NGC 4915, show chemical signatures similar to ETGs without fine structure, which is consistent with a gas-poor merger of elliptical galaxies in which substantial star formation is not expected. For NGC 2865, we find a statistically higher abundance of Ca (an $伪$-element) and Cr and Mn (Fe-peak elements). We show that for NGC 2865, a simple gas-rich merger scenario fails to explain the larger abundance ratios compared to ETGs without fine structure. These three early-type galaxies with fine structure exhibit a range of abundances, suggesting ETGs with fine structure can form via multiple pathways and types of galaxy mergers. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.13459v1-abstract-full').style.display = 'none'; document.getElementById('2404.13459v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 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">26 pages, 8 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/2403.19524">arXiv:2403.19524</a> <span> [<a href="https://arxiv.org/pdf/2403.19524">pdf</a>, <a href="https://arxiv.org/format/2403.19524">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </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/10.1051/0004-6361/202450133">10.1051/0004-6361/202450133 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Joint ALMA/X-ray monitoring of the radio-quiet type 1 AGN IC 4329A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shablovinskaya%2C+E">E. Shablovinskaya</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">C. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+C">C-S. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Tortosa%2C+A">A. Tortosa</a>, <a href="/search/astro-ph?searchtype=author&query=del+Palacio%2C+S">S. del Palacio</a>, <a href="/search/astro-ph?searchtype=author&query=Kawamuro%2C+T">T. Kawamuro</a>, <a href="/search/astro-ph?searchtype=author&query=Aalto%2C+S">S. Aalto</a>, <a href="/search/astro-ph?searchtype=author&query=Arzoumanian%2C+Z">Z. Arzoumanian</a>, <a href="/search/astro-ph?searchtype=author&query=Balokovic%2C+M">M. Balokovic</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">F. E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Gendreau%2C+K+C">K. C. Gendreau</a>, <a href="/search/astro-ph?searchtype=author&query=Ho%2C+L+C">L. C. Ho</a>, <a href="/search/astro-ph?searchtype=author&query=Kakkad%2C+D">D. Kakkad</a>, <a href="/search/astro-ph?searchtype=author&query=Kara%2C+E">E. Kara</a>, <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M+J">M. J. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+T">T. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Loewenstein%2C+M">M. Loewenstein</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotzky%2C+R">R. Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Paltani%2C+S">S. Paltani</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">G. C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+K">K. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Tombesi%2C+F">F. Tombesi</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">B. Trakhtenbrot</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="2403.19524v1-abstract-short" style="display: inline;"> The origin of a compact millimeter (mm, 100-250 GHz) emission in radio-quiet active galactic nuclei (RQ AGN) remains debated. Recent studies propose a connection with self-absorbed synchrotron emission from the accretion disk X-ray corona. We present the first joint ALMA ($\sim$100 GHz) and X-ray (NICER/XMM-Newton/Swift; 2-10 keV) observations of the unobscured RQ AGN, IC 4329A ($z = 0.016$). The… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.19524v1-abstract-full').style.display = 'inline'; document.getElementById('2403.19524v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.19524v1-abstract-full" style="display: none;"> The origin of a compact millimeter (mm, 100-250 GHz) emission in radio-quiet active galactic nuclei (RQ AGN) remains debated. Recent studies propose a connection with self-absorbed synchrotron emission from the accretion disk X-ray corona. We present the first joint ALMA ($\sim$100 GHz) and X-ray (NICER/XMM-Newton/Swift; 2-10 keV) observations of the unobscured RQ AGN, IC 4329A ($z = 0.016$). The time-averaged mm-to-X-ray flux ratio aligns with recently established trends for larger samples (Kawamuro et al. 2022, Ricci et al. 2023), but with a tighter scatter ($\sim$0.1 dex) compared to previous studies. However, there is no significant correlation on timescales of less than 20 days. The compact mm emission exhibits a spectral index of $-0.23 \pm 0.18$, remains unresolved with a 13 pc upper limit, and shows no jet signatures. Notably, the mm flux density varies significantly (factor of 3) within 4 days, exceeding the contemporaneous X-ray variability (37% vs. 18%) and showing the largest mm variations ever detected in RQ AGN over daily timescales. The high amplitude variability rules out scenarios of heated dust and thermal free-free emission, pointing toward a synchrotron origin for the mm radiation in a source of $\sim$1 light day size. While the exact source is not yet certain, an X-ray corona scenario emerges as the most plausible compared to a scaled-down jet or outflow-driven shocks.} <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.19524v1-abstract-full').style.display = 'none'; document.getElementById('2403.19524v1-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">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, A232 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.14751">arXiv:2403.14751</a> <span> [<a href="https://arxiv.org/pdf/2403.14751">pdf</a>, <a href="https://arxiv.org/format/2403.14751">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"> GOALS-JWST: The Warm Molecular Outflows of the Merging Starburst Galaxy NGC 3256 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bohn%2C+T">Thomas Bohn</a>, <a href="/search/astro-ph?searchtype=author&query=Inami%2C+H">Hanae Inami</a>, <a href="/search/astro-ph?searchtype=author&query=Togi%2C+A">Aditya Togi</a>, <a href="/search/astro-ph?searchtype=author&query=Armus%2C+L">Lee Armus</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=Barcos-Munoz%2C+L">Loreto Barcos-Munoz</a>, <a href="/search/astro-ph?searchtype=author&query=Song%2C+Y">Yiqing Song</a>, <a href="/search/astro-ph?searchtype=author&query=Linden%2C+S+T">Sean T. Linden</a>, <a href="/search/astro-ph?searchtype=author&query=Surace%2C+J">Jason Surace</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchin%2C+M">Marina Bianchin</a>, <a href="/search/astro-ph?searchtype=author&query=U%2C+V">Vivian U</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+A+S">Aaron S. Evans</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=Malkan%2C+M+A">Matthew A. Malkan</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=Stierwalt%2C+S">Sabrina Stierwalt</a>, <a href="/search/astro-ph?searchtype=author&query=Buiten%2C+V+A">Victorine A. Buiten</a>, <a href="/search/astro-ph?searchtype=author&query=Charmandaris%2C+V">Vassilis Charmandaris</a>, <a href="/search/astro-ph?searchtype=author&query=Diaz-Santos%2C+T">Tanio Diaz-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Howell%2C+J+H">Justin H. Howell</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</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=Aalto%2C+S">Susanne Aalto</a>, <a href="/search/astro-ph?searchtype=author&query=Hayward%2C+C+C">Christopher C. Hayward</a> , et al. (4 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.14751v2-abstract-short" style="display: inline;"> We present James Webb Space Telescope (JWST) Integral Field Spectrograph observations of NGC 3256, a local infrared-luminous late-stage merging system with two nuclei roughly 1$\;\rm{kpc}$ apart, both of which have evidence of cold molecular outflows. Using JWST/NIRSpec and MIRI datasets, we investigate this morphologically complex system on spatial scales of $<$100$\;\rm{pc}$, where we focus on t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.14751v2-abstract-full').style.display = 'inline'; document.getElementById('2403.14751v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.14751v2-abstract-full" style="display: none;"> We present James Webb Space Telescope (JWST) Integral Field Spectrograph observations of NGC 3256, a local infrared-luminous late-stage merging system with two nuclei roughly 1$\;\rm{kpc}$ apart, both of which have evidence of cold molecular outflows. Using JWST/NIRSpec and MIRI datasets, we investigate this morphologically complex system on spatial scales of $<$100$\;\rm{pc}$, where we focus on the warm molecular H$_2$ gas surrounding the nuclei. We detect collimated outflowing warm H$_2$ gas originating from the southern nucleus, though we do not find significant outflowing H$_2$ gas surrounding the northern nucleus. We measure maximum intrinsic outflow velocities of $\sim$1,000$\;\rm{km}\;\rm{s}^{-1}$, which extend out to a distance of 0.7$\;\rm{kpc}$. Based on H$_2$ S(7)/S(1) ratios, we find a larger fraction of warmer gas near the S nucleus, which decreases with increasing distance from the nucleus, signifying the southern nucleus as a primary source of H$_2$ heating. The gas mass of the warm H$_2$ outflow component is estimated to be $M\rm{_{warm,out}}=(1.4\pm0.2)\times10^6\;\rm{M}_{\odot}$, as much as 6$\%$ of the cold H$_2$ mass estimated using ALMA CO data. The outflow time scale is about $7\times10^5\;\rm{yr}$, resulting in a mass outflow rate $\dot{M}\rm{_{warm,out}}=2.0\pm0.8\;\rm{M}_{\odot}\;\rm{yr}^{-1}$ and kinetic power $P\rm{_{warm,out}}\;\sim\;4\times10^{41}\;\rm{erg}\;\rm{s}^{-1}$. Lastly, regions within our 3.0"x3.0" NIRSpec data where the outflowing gas reside show high [Fe II]/Pa$尾$ and H$_2$/Br$纬$ line ratios, indicate enhanced mechanical heating caused by the outflows. The fluxes and ratios of Polycyclic Aromatic Hydrocarbons (PAH) in these regions are not significantly different compared to those elsewhere in the disk, suggesting the outflows may not significantly alter the PAH ionization state or grain size. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.14751v2-abstract-full').style.display = 'none'; document.getElementById('2403.14751v2-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 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">19 pages, 9 figures. Accepted by 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/2402.17590">arXiv:2402.17590</a> <span> [<a href="https://arxiv.org/pdf/2402.17590">pdf</a>, <a href="https://arxiv.org/format/2402.17590">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"> Double, double, toil, and trouble: The tails, bubbles, and knots of the local compact obscured nucleus galaxy NGC4418 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wethers%2C+C+F">C. F. Wethers</a>, <a href="/search/astro-ph?searchtype=author&query=Aalto%2C+S">S. Aalto</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">G. C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Stanley%2C+F">F. Stanley</a>, <a href="/search/astro-ph?searchtype=author&query=Gallagher%2C+J">J. Gallagher</a>, <a href="/search/astro-ph?searchtype=author&query=Gorski%2C+M">M. Gorski</a>, <a href="/search/astro-ph?searchtype=author&query=K%C3%B6nig%2C+S">S. K枚nig</a>, <a href="/search/astro-ph?searchtype=author&query=Onishi%2C+K">K. Onishi</a>, <a href="/search/astro-ph?searchtype=author&query=Sato%2C+M">M. Sato</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+C">C. Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Beswick%2C+R">R. Beswick</a>, <a href="/search/astro-ph?searchtype=author&query=Combes%2C+L+B+F">L. Barcos-Munoz F. Combes</a>, <a href="/search/astro-ph?searchtype=author&query=Diaz-Santos%2C+T">T. Diaz-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+A+S">A. S. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia-Bernete%2C+I">I. Garcia-Bernete</a>, <a href="/search/astro-ph?searchtype=author&query=Henkel%2C+C">C. Henkel</a>, <a href="/search/astro-ph?searchtype=author&query=Imanishi%2C+M">M. Imanishi</a>, <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADn%2C+S">S. Mart铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Muller%2C+S">S. Muller</a>, <a href="/search/astro-ph?searchtype=author&query=Nishimura%2C+Y">Y. Nishimura</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">C. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Rigopoulou%2C+D">D. Rigopoulou</a>, <a href="/search/astro-ph?searchtype=author&query=Viti%2C+S">S. Viti</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2402.17590v1-abstract-short" style="display: inline;"> Compact obscured nuclei (CONs) are an extremely obscured (N$_{H2}$ >10$^{25}$ cm$^{-2}$) class of galaxy nuclei thought to exist in 20-40 per cent of nearby (ultra-)luminous infrared galaxies. While they have been proposed to represent a key phase of the active galactic nucleus (AGN) feedback cycle, the nature of these CONs - what powers them, their dynamics, and their impact on the host galaxy -… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.17590v1-abstract-full').style.display = 'inline'; document.getElementById('2402.17590v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.17590v1-abstract-full" style="display: none;"> Compact obscured nuclei (CONs) are an extremely obscured (N$_{H2}$ >10$^{25}$ cm$^{-2}$) class of galaxy nuclei thought to exist in 20-40 per cent of nearby (ultra-)luminous infrared galaxies. While they have been proposed to represent a key phase of the active galactic nucleus (AGN) feedback cycle, the nature of these CONs - what powers them, their dynamics, and their impact on the host galaxy - remains unknown. This work analyses the large-scale optical properties of the local CON, NGC4418 (z=0.00727). We present new, targeted integral field unit observations of the galaxy with the Multi-Unit Spectroscopic Explorer (MUSE). For the first time, we map the ionised and neutral gas components of the galaxy, along with their dynamical structure, to reveal several previously unknown features of the galaxy. We confirm the presence of a previously postulated blueshifted outflow along the minor axis of NGC4418. We find this outflow to be decelerating and, for the first time, show it to extend bilaterally from the nucleus. We report the discovery of two further outflow structures: a redshifted southern outflow connected to a tail of ionised gas surrounding the galaxy and a blueshifted bubble to the north. In addition to these features, we find the [OIII] emission reveals the presence of knots across the galaxy, which are consistent with regions of the galaxy that have been photoionised by an AGN. Based on the properties of these features, we conclude that the CON in NGC4418 is most likely powered by AGN activity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.17590v1-abstract-full').style.display = 'none'; document.getElementById('2402.17590v1-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 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">17 pages, 15 figures, accepted to A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.15436">arXiv:2402.15436</a> <span> [<a href="https://arxiv.org/pdf/2402.15436">pdf</a>, <a href="https://arxiv.org/format/2402.15436">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/10.1051/0004-6361/202348331">10.1051/0004-6361/202348331 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CON-quest II. Spatially and spectrally resolved HCN/HCO+ line ratios in local luminous and ultraluminous infrared galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Nishimura%2C+Y">Y. Nishimura</a>, <a href="/search/astro-ph?searchtype=author&query=Aalto%2C+S">S. Aalto</a>, <a href="/search/astro-ph?searchtype=author&query=Gorski%2C+M+D">M. D. Gorski</a>, <a href="/search/astro-ph?searchtype=author&query=K%C3%B6nig%2C+S">S. K枚nig</a>, <a href="/search/astro-ph?searchtype=author&query=Onishi%2C+K">K. Onishi</a>, <a href="/search/astro-ph?searchtype=author&query=Wethers%2C+C">C. Wethers</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+C">C. Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Barcos-Mu%C3%B1oz%2C+L">L. Barcos-Mu帽oz</a>, <a href="/search/astro-ph?searchtype=author&query=Combes%2C+F">F. Combes</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%ADaz-Santos%2C+T">T. D铆az-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Gallagher%2C+J+S">J. S. Gallagher</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Burillo%2C+S">S. Garc铆a-Burillo</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez-Alfonso%2C+E">E. Gonz谩lez-Alfonso</a>, <a href="/search/astro-ph?searchtype=author&query=Greve%2C+T+R">T. R. Greve</a>, <a href="/search/astro-ph?searchtype=author&query=Harada%2C+N">N. Harada</a>, <a href="/search/astro-ph?searchtype=author&query=Henkel%2C+C">C. Henkel</a>, <a href="/search/astro-ph?searchtype=author&query=Imanishi%2C+M">M. Imanishi</a>, <a href="/search/astro-ph?searchtype=author&query=Kohno%2C+K">K. Kohno</a>, <a href="/search/astro-ph?searchtype=author&query=Linden%2C+S+T">S. T. Linden</a>, <a href="/search/astro-ph?searchtype=author&query=Mangum%2C+J+G">J. G. Mangum</a>, <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADn%2C+S">S. Mart铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Muller%2C+S">S. Muller</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">G. C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">C. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Stanley%2C+F">F. Stanley</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="2402.15436v4-abstract-short" style="display: inline;"> Nuclear regions of ultraluminous and luminous infrared galaxies (U/LIRGs) are powered by starbursts and/or active galactic nuclei (AGNs). These regions are often obscured by extremely high columns of gas and dust. Molecular lines in the submillimeter windows have the potential to determine the physical conditions of these compact obscured nuclei (CONs). We aim to reveal the distributions of HCN an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.15436v4-abstract-full').style.display = 'inline'; document.getElementById('2402.15436v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.15436v4-abstract-full" style="display: none;"> Nuclear regions of ultraluminous and luminous infrared galaxies (U/LIRGs) are powered by starbursts and/or active galactic nuclei (AGNs). These regions are often obscured by extremely high columns of gas and dust. Molecular lines in the submillimeter windows have the potential to determine the physical conditions of these compact obscured nuclei (CONs). We aim to reveal the distributions of HCN and HCO$^+$ emission in local U/LIRGs and investigate whether and how they are related to galaxy properties. Using ALMA, we have conducted sensitive observations of the HCN J=3--2 and HCO$^+$ J=3--2 lines toward 23 U/LIRGs in the local Universe (z < 0.07) with a spatial resolution of ~0.3" (~50--400 pc). We detected both HCN and HCO$^+$ in 21 galaxies, only HCN in one galaxy, and neither in one galaxy. The global HCN/HCO$^+$ line ratios, averaged over scales of ~0.5--4 kpc, range from 0.4 to 2.3, with an unweighted mean of 1.1. These line ratios appear to have no systematic trend with bolometric AGN luminosity or star formation rate. The line ratio varies with position and velocity within each galaxy, with an average interquartile range of 0.38 on a spaxel-by-spaxel basis. In eight out of ten galaxies known to have outflows and/or inflows, we found spatially and kinematically symmetric structures of high line ratios. These structures appear as a collimated bicone in two galaxies and as a thin spherical shell in six galaxies. Non-LTE analysis suggests that the high HCN/HCO$^+$ line ratio in outflows is predominantly influenced by the abundance ratio. Chemical model calculations indicate that the enhancement of HCN abundance in outflows is likely due to high-temperature chemistry triggered by shock heating. These results imply that the HCN/HCO$^+$ line ratio can aid in identifying the outflow geometry when the shock velocity of the outflows is sufficiently high to heat the gas. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.15436v4-abstract-full').style.display = 'none'; document.getElementById('2402.15436v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 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">52 pages, 35 figures, 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 686, A48 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.01945">arXiv:2312.01945</a> <span> [<a href="https://arxiv.org/pdf/2312.01945">pdf</a>, <a href="https://arxiv.org/format/2312.01945">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"> GOALS-JWST: Mid-Infrared Molecular Gas Excitation Probes the Local Conditions of Nuclear Star Clusters and the AGN in the LIRG VV 114 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Buiten%2C+V+A">Victorine A. Buiten</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=Viti%2C+S">Serena Viti</a>, <a href="/search/astro-ph?searchtype=author&query=Armus%2C+L">Lee Armus</a>, <a href="/search/astro-ph?searchtype=author&query=Barr%2C+A+G">Andrew G. Barr</a>, <a href="/search/astro-ph?searchtype=author&query=Barcos-Mu%C3%B1oz%2C+L">Loreto Barcos-Mu帽oz</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+A+S">Aaron S. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Inami%2C+H">Hanae Inami</a>, <a href="/search/astro-ph?searchtype=author&query=Linden%2C+S+T">Sean T. Linden</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Song%2C+Y">Yiqing Song</a>, <a href="/search/astro-ph?searchtype=author&query=Rich%2C+J+A">Jeffrey A. Rich</a>, <a href="/search/astro-ph?searchtype=author&query=Aalto%2C+S">Susanne Aalto</a>, <a href="/search/astro-ph?searchtype=author&query=Appleton%2C+P+N">Philip N. Appleton</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=Charmandaris%2C+V">Vassilis Charmandaris</a>, <a href="/search/astro-ph?searchtype=author&query=Diaz-Santos%2C+T">Tanio Diaz-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Hayward%2C+C+C">Christopher C. Hayward</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=Medling%2C+A+M">Anne M. Medling</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=U%2C+V">Vivian U</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="2312.01945v2-abstract-short" style="display: inline;"> The enormous increase in mid-IR sensitivity and spatial and spectral resolution provided by the JWST spectrographs enables, for the first time, detailed extragalactic studies of molecular vibrational bands. This opens an entirely new window for the study of the molecular interstellar medium in luminous infrared galaxies (LIRGs). We present a detailed analysis of rovibrational bands of gas-phase CO… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.01945v2-abstract-full').style.display = 'inline'; document.getElementById('2312.01945v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.01945v2-abstract-full" style="display: none;"> The enormous increase in mid-IR sensitivity and spatial and spectral resolution provided by the JWST spectrographs enables, for the first time, detailed extragalactic studies of molecular vibrational bands. This opens an entirely new window for the study of the molecular interstellar medium in luminous infrared galaxies (LIRGs). We present a detailed analysis of rovibrational bands of gas-phase CO, H$_2$O, C$_2$H$_2$ and HCN towards the heavily-obscured eastern nucleus of the LIRG VV 114, as observed by NIRSpec and MIRI MRS. Spectra extracted from apertures of 130 pc in radius show a clear dichotomy between the obscured AGN and two intense starburst regions. We detect the 2.3 $渭$m CO bandheads, characteristic of cool stellar atmospheres, in the star-forming regions, but not towards the AGN. Surprisingly, at 4.7 $\mathrm渭$m we find highly-excited CO ($T_\mathrm{ex} \approx 700-800$ K out to at least rotational level $J = 27$) towards the star-forming regions, but only cooler gas ($T_\mathrm{ex} \approx 200$ K) towards the AGN. We conclude that only mid-infrared pumping through the rovibrational lines can account for the equilibrium conditions found for CO and H$_2$O in the deeply-embedded starbursts. Here the CO bands probe regions with an intense local radiation field inside dusty young massive star clusters or near the most massive young stars. The lack of high-excitation molecular gas towards the AGN is attributed to geometric dilution of the intense radiation from the bright point source. An overview of the relevant excitation and radiative transfer physics is provided in an appendix. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.01945v2-abstract-full').style.display = 'none'; document.getElementById('2312.01945v2-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 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 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">28 pages, 17 figures. Accepted for publication in ApJ. This version includes small revisions following the referee report</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.00783">arXiv:2312.00783</a> <span> [<a href="https://arxiv.org/pdf/2312.00783">pdf</a>, <a href="https://arxiv.org/format/2312.00783">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </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/10.1051/0004-6361/202348760">10.1051/0004-6361/202348760 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> XMM-Newton --NuSTAR monitoring campaign of the Seyfert 1 galaxy IC 4329A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tortosa%2C+A">A. Tortosa</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">C. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Shablovinskaia%2C+E">E. Shablovinskaia</a>, <a href="/search/astro-ph?searchtype=author&query=Tombesi%2C+F">F. Tombesi</a>, <a href="/search/astro-ph?searchtype=author&query=Kawamuro%2C+T">T. Kawamuro</a>, <a href="/search/astro-ph?searchtype=author&query=Kara%2C+E">E. Kara</a>, <a href="/search/astro-ph?searchtype=author&query=Mantovani%2C+G">G. Mantovani</a>, <a href="/search/astro-ph?searchtype=author&query=Balokovic%2C+M">M. Balokovic</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+C">C-S. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Gendreau%2C+K">K. Gendreau</a>, <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M+J">M. J. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+T">T. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Loewenstein%2C+M">M. Loewenstein</a>, <a href="/search/astro-ph?searchtype=author&query=Paltani%2C+S">S. Paltani</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">G. C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">B. Trakhtenbrot</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="2312.00783v4-abstract-short" style="display: inline;"> We present the results of a joint {\it XMM-Newton} and {\it NuSTAR} campaign on the active galactic nucleus (AGN) IC 4329A, consisting of 9 $\times$ 20 ks {\it XMM-Newton} observations, and 5 $\times$ 20 ks {\it NuSTAR} observations within nine days, performed in August 2021. Within each observation, the AGN is not very variable, with the fractional variability never exceeding 5%. Flux variations… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.00783v4-abstract-full').style.display = 'inline'; document.getElementById('2312.00783v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.00783v4-abstract-full" style="display: none;"> We present the results of a joint {\it XMM-Newton} and {\it NuSTAR} campaign on the active galactic nucleus (AGN) IC 4329A, consisting of 9 $\times$ 20 ks {\it XMM-Newton} observations, and 5 $\times$ 20 ks {\it NuSTAR} observations within nine days, performed in August 2021. Within each observation, the AGN is not very variable, with the fractional variability never exceeding 5%. Flux variations are observed between the different observations, on timescales of days, with a 30% ratio between the minimum and the maximum 2-10 keV flux. These variations follow the softer-when-brighter behavior typically observed in AGN. In all observations, a soft excess is clearly present. Consistently with previous observations, the X-ray spectra of the source exhibit a cut-off energy between 140 and 250 keV, constant within the error in the different observations. We detected a prominent component of the $6.4$\,keV Fe~K$伪$ line consistent with being constant during the monitoring, consisting of an unresolved narrow core and a broader component likely originating in the inner accredion disc. We find that the reflection component is weak ($R_{\rm max}=0.009\pm0.002$) and most likely originating in distant neutral medium. We also found the presence of a warm absorber component together with an ultra-fast outflow. Looking at their energetic, these outflows have enough mechanical power to exercise a significant feedback impact on the AGN surrounding environment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.00783v4-abstract-full').style.display = 'none'; document.getElementById('2312.00783v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 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 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 687, A51 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.01494">arXiv:2311.01494</a> <span> [<a href="https://arxiv.org/pdf/2311.01494">pdf</a>, <a href="https://arxiv.org/ps/2311.01494">ps</a>, <a href="https://arxiv.org/format/2311.01494">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> BASS XLII: The relation between the covering factor of dusty gas and the Eddington ratio in nearby active galactic nuclei </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">C. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Ichikawa%2C+K">K. Ichikawa</a>, <a href="/search/astro-ph?searchtype=author&query=Stalevski%2C+M">M. Stalevski</a>, <a href="/search/astro-ph?searchtype=author&query=Kawamuro%2C+T">T. Kawamuro</a>, <a href="/search/astro-ph?searchtype=author&query=Yamada%2C+S">S. Yamada</a>, <a href="/search/astro-ph?searchtype=author&query=Ueda%2C+Y">Y. Ueda</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotzky%2C+R">R. Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">G. C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M+J">M. J. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">B. Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Fabian%2C+A+C">A. C. Fabian</a>, <a href="/search/astro-ph?searchtype=author&query=Ho%2C+L+C">L. C. Ho</a>, <a href="/search/astro-ph?searchtype=author&query=Asmus%2C+D">D. Asmus</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">F. E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+C+S">C. S. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Gupta%2C+K+K">K. K. Gupta</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">K. Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M">M. Powell</a>, <a href="/search/astro-ph?searchtype=author&query=Pfeifle%2C+R+W">R. W. Pfeifle</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas%2C+A">A. Rojas</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">F. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Temple%2C+M+J">M. J. Temple</a>, <a href="/search/astro-ph?searchtype=author&query=Toba%2C+Y">Y. Toba</a>, <a href="/search/astro-ph?searchtype=author&query=Tortosa%2C+A">A. Tortosa</a>, <a href="/search/astro-ph?searchtype=author&query=Treister%2C+E">E. Treister</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="2311.01494v2-abstract-short" style="display: inline;"> Accreting supermassive black holes (SMBHs) located at the center of galaxies are typically surrounded by large quantities of gas and dust. The structure and evolution of this circumnuclear material can be studied at different wavelengths, from the submillimeter to the X-rays. Recent X-ray studies have shown that the covering factor of the obscuring material tends to decrease with increasing Edding… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.01494v2-abstract-full').style.display = 'inline'; document.getElementById('2311.01494v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.01494v2-abstract-full" style="display: none;"> Accreting supermassive black holes (SMBHs) located at the center of galaxies are typically surrounded by large quantities of gas and dust. The structure and evolution of this circumnuclear material can be studied at different wavelengths, from the submillimeter to the X-rays. Recent X-ray studies have shown that the covering factor of the obscuring material tends to decrease with increasing Eddington ratio, likely due to radiative feedback on dusty gas. Here we study a sample of 549 nearby (z<0.1) hard X-ray (14-195 keV) selected non-blazar active galactic nuclei (AGN), and use the ratio between the AGN infrared and bolometric luminosity as a proxy of the covering factor. We find that, in agreement with what has been found by X-ray studies of the same sample, the covering factor decreases with increasing Eddington ratio. We also confirm previous findings which showed that obscured AGN typically have larger covering factors than unobscured sources. Finally, we find that the median covering factors of AGN located in different regions of the column density-Eddington ratio diagram are in good agreement with what would be expected from a radiation-regulated growth of SMBHs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.01494v2-abstract-full').style.display = 'none'; document.getElementById('2311.01494v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 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">ApJ in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.13228">arXiv:2309.13228</a> <span> [<a href="https://arxiv.org/pdf/2309.13228">pdf</a>, <a href="https://arxiv.org/format/2309.13228">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 physically motivated framework to compare pair fractions of isolated low and high mass galaxies across cosmic time </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chamberlain%2C+K">Katie Chamberlain</a>, <a href="/search/astro-ph?searchtype=author&query=Besla%2C+G">Gurtina Besla</a>, <a href="/search/astro-ph?searchtype=author&query=Patel%2C+E">Ekta Patel</a>, <a href="/search/astro-ph?searchtype=author&query=Rodriguez-Gomez%2C+V">Vicente Rodriguez-Gomez</a>, <a href="/search/astro-ph?searchtype=author&query=Torrey%2C+P">Paul Torrey</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+G">Garreth Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+K">Kelsey Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Kallivayalil%2C+N">Nitya Kallivayalil</a>, <a href="/search/astro-ph?searchtype=author&query=Patton%2C+D">David Patton</a>, <a href="/search/astro-ph?searchtype=author&query=Pearson%2C+S">Sarah Pearson</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G">George Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Stierwalt%2C+S">Sabrina Stierwalt</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="2309.13228v2-abstract-short" style="display: inline;"> Low mass galaxy pair fractions are understudied, and it is unclear whether low mass pair fractions evolve in the same way as more massive systems over cosmic time. In the era of JWST, Roman, and Rubin, selecting galaxy pairs in a self-consistent way will be critical to connect observed pair fractions to cosmological merger rates across all mass scales and redshifts. Utilizing the Illustris TNG100… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.13228v2-abstract-full').style.display = 'inline'; document.getElementById('2309.13228v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.13228v2-abstract-full" style="display: none;"> Low mass galaxy pair fractions are understudied, and it is unclear whether low mass pair fractions evolve in the same way as more massive systems over cosmic time. In the era of JWST, Roman, and Rubin, selecting galaxy pairs in a self-consistent way will be critical to connect observed pair fractions to cosmological merger rates across all mass scales and redshifts. Utilizing the Illustris TNG100 simulation, we create a sample of physically associated low mass ($\rm 10^8<M_*<5\times10^9\,M_\odot$) and high mass ($\rm 5\times10^9<M_*<10^{11}\,M_\odot$) pairs between $z=0$ and $4.2$. The low mass pair fraction increases from $z=0$ to $2.5$, while the high mass pair fraction peaks at $z=0$ and is constant or slightly decreasing at $z>1$. At $z=0$, the low mass major (1:4 mass ratio) pair fraction is 4$\times$ lower than high mass pairs, consistent with findings for cosmological merger rates. We show that separation limits that vary with the mass and redshift of the system, such as scaling by the virial radius of the host halo ($r_{\mathrm{sep}}< 1 R_{\rm vir}$), are critical for recovering pair fraction differences between low mass and high mass systems. Alternatively, static physical separation limits applied equivalently to all galaxy pairs do not recover the differences between low and high mass pair fractions, even up to separations of $300$ kpc. Finally, we place isolated mass-analogs of Local Group galaxy pairs, i.e., Milky Way (MW)--M31, MW--LMC, LMC--SMC, in a cosmological context, showing that isolated analogs of LMC--SMC-mass pairs and low-separation ($<50$ kpc) MW--LMC-mass pairs are $2-3\times$ more common at $z\gtrsim2-3$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.13228v2-abstract-full').style.display = 'none'; document.getElementById('2309.13228v2-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">v1</span> submitted 22 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">18 pages, 5 figures, accepted for publication in ApJ, updated Feb 2024 to reflect accepted version</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.02776">arXiv:2309.02776</a> <span> [<a href="https://arxiv.org/pdf/2309.02776">pdf</a>, <a href="https://arxiv.org/format/2309.02776">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"> BASS XXXIV: A Catalog of the Nuclear Mm-wave Continuum Emission Properties of AGNs Constrained on Scales $\lesssim$ 100--200 pc </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kawamuro%2C+T">Taiki Kawamuro</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotzky%2C+R+F">Richard F. Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Imanishi%2C+M">Masatoshi Imanishi</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">Federica Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M+J">Michael J. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">Benny Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Izumi%2C+T">Takuma Izumi</a>, <a href="/search/astro-ph?searchtype=author&query=Ichikawa%2C+K">Kohei Ichikawa</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas%2C+A+F">Alejandra F. Rojas</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+K+L">Krista Lynne Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Shimizu%2C+T">Taro Shimizu</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">Kyuseok Oh</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=Baba%2C+S">Shunsuke Baba</a>, <a href="/search/astro-ph?searchtype=author&query=Balokovic%2C+M">Mislav Balokovic</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+C">Chin-Shin Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Kakkad%2C+D">Darshan Kakkad</a>, <a href="/search/astro-ph?searchtype=author&query=Pfeifle%2C+R+W">Ryan W. Pfeifle</a>, <a href="/search/astro-ph?searchtype=author&query=Temple%2C+M+J">Matthew J. Temple</a>, <a href="/search/astro-ph?searchtype=author&query=Ueda%2C+Y">Yoshihiro Ueda</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M+C">Meredith C. Powell</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="2309.02776v1-abstract-short" style="display: inline;"> We present a catalog of the millimeter-wave (mm-wave) continuum properties of 98 nearby ($z <$ 0.05) active galactic nuclei (AGNs) selected from the 70-month Swift/BAT hard X-ray catalog that have precisely determined X-ray spectral properties and subarcsec-resolution ALMA Band-6 (211--275 GHz) observations as of 2021 April. Due to the hard-X-ray ($>$ 10 keV) selection, the sample is nearly unbias… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.02776v1-abstract-full').style.display = 'inline'; document.getElementById('2309.02776v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.02776v1-abstract-full" style="display: none;"> We present a catalog of the millimeter-wave (mm-wave) continuum properties of 98 nearby ($z <$ 0.05) active galactic nuclei (AGNs) selected from the 70-month Swift/BAT hard X-ray catalog that have precisely determined X-ray spectral properties and subarcsec-resolution ALMA Band-6 (211--275 GHz) observations as of 2021 April. Due to the hard-X-ray ($>$ 10 keV) selection, the sample is nearly unbiased for obscured systems at least up to Compton-thick-level obscuration, and provides the largest number of AGNs with high physical resolution mm-wave data ($\lesssim$ 100--200 pc). Our catalog reports emission peak coordinates, spectral indices, and peak fluxes and luminosities at 1.3 mm (230 GHz). Additionally, high-resolution mm-wave images are provided. Using the images and creating radial surface brightness profiles of mm-wave emission, we identify emission extending from the central source and isolated blob-like emission. Flags indicating the presence of these emission features are tabulated. Among 90 AGNs with significant detections of nuclear emission, 37 AGNs ($\approx$ 41%) appear to have both or one of extended or blob-like components. We, in particular, investigate AGNs that show well-resolved mm-wave components and find that these seem to have a variety of origins (i.e., a jet, radio lobes, a secondary AGN, stellar clusters, a narrow line region, galaxy disk, active star-formation regions, and AGN-driven outflows), and some components have currently unclear origins. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.02776v1-abstract-full').style.display = 'none'; document.getElementById('2309.02776v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 September, 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">49 pages, 7 figures, 3 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/2309.01616">arXiv:2309.01616</a> <span> [<a href="https://arxiv.org/pdf/2309.01616">pdf</a>, <a href="https://arxiv.org/format/2309.01616">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"> Large-Scale Features of the CON Galaxy NGC4418 with MUSE </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wethers%2C+C+F">C. F. Wethers</a>, <a href="/search/astro-ph?searchtype=author&query=Aalto%2C+S">S. Aalto</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">G. C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Stanley%2C+F">F. Stanley</a>, <a href="/search/astro-ph?searchtype=author&query=Gallagher%2C+J">J. Gallagher</a>, <a href="/search/astro-ph?searchtype=author&query=Gorski%2C+M">M. Gorski</a>, <a href="/search/astro-ph?searchtype=author&query=K%C3%B6nig%2C+S">S. K枚nig</a>, <a href="/search/astro-ph?searchtype=author&query=Onishi%2C+K">K. Onishi</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+C">C. Yang</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="2309.01616v1-abstract-short" style="display: inline;"> Compact obscured nuclei (CONs) are relatively common in the centers of local (U)LIRGs, yet their nature remains unknown. Both AGN activity and extreme nuclear starbursts have been suggested as plausible nuclear power sources. The prevalence of outflows in these systems suggest that CONs represent a key phase in the nuclear feedback cycle, in which material is ejected from the central regions of th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.01616v1-abstract-full').style.display = 'inline'; document.getElementById('2309.01616v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.01616v1-abstract-full" style="display: none;"> Compact obscured nuclei (CONs) are relatively common in the centers of local (U)LIRGs, yet their nature remains unknown. Both AGN activity and extreme nuclear starbursts have been suggested as plausible nuclear power sources. The prevalence of outflows in these systems suggest that CONs represent a key phase in the nuclear feedback cycle, in which material is ejected from the central regions of the galaxy. Here, we present results from MUSE for the confirmed local CON galaxy NGC4418. For the first time we spatially map the spectral features and kinematics of the galaxy in the optical, revealing several previously unknown structures. In particular, we discover a bilateral outflow along the minor axis, an outflowing bubble, several knot structures and a receding outflow partially obscured by the galactic disk. Based on the properties of these features, we conclude that the CON in NGC4418 is most likely powered by an AGN. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.01616v1-abstract-full').style.display = 'none'; document.getElementById('2309.01616v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 September, 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">4 pages, 3 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.00209">arXiv:2308.00209</a> <span> [<a href="https://arxiv.org/pdf/2308.00209">pdf</a>, <a href="https://arxiv.org/format/2308.00209">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"> GOALS-JWST: Gas Dynamics and Excitation in NGC7469 revealed by NIRSpec </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bianchin%2C+M">Marina Bianchin</a>, <a href="/search/astro-ph?searchtype=author&query=U%2C+V">Vivian U</a>, <a href="/search/astro-ph?searchtype=author&query=Song%2C+Y">Yiqing Song</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=Remigio%2C+R+P">Raymond P. Remigio</a>, <a href="/search/astro-ph?searchtype=author&query=Barcos-Munoz%2C+L">Loreto Barcos-Munoz</a>, <a href="/search/astro-ph?searchtype=author&query=Diaz-Santos%2C+T">Tanio Diaz-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Armus%2C+L">Lee Armus</a>, <a href="/search/astro-ph?searchtype=author&query=Inami%2C+H">Hanae Inami</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=Evans%2C+A+S">Aaron S. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Boker%2C+T">Torsten Boker</a>, <a href="/search/astro-ph?searchtype=author&query=Kader%2C+J+A">Justin A. Kader</a>, <a href="/search/astro-ph?searchtype=author&query=Linden%2C+S+T">Sean T. Linden</a>, <a href="/search/astro-ph?searchtype=author&query=Charmandaris%2C+V">Vassilis Charmandaris</a>, <a href="/search/astro-ph?searchtype=author&query=Malkan%2C+M+A">Matthew A. Malkan</a>, <a href="/search/astro-ph?searchtype=author&query=Rich%2C+J">Jeff Rich</a>, <a href="/search/astro-ph?searchtype=author&query=Bohn%2C+T">Thomas Bohn</a>, <a href="/search/astro-ph?searchtype=author&query=Medling%2C+A+M">Anne M. Medling</a>, <a href="/search/astro-ph?searchtype=author&query=Stierwalt%2C+S">Sabrina Stierwalt</a>, <a href="/search/astro-ph?searchtype=author&query=Mazzarella%2C+J+M">Joseph M. Mazzarella</a>, <a href="/search/astro-ph?searchtype=author&query=Law%2C+D+R">David R. Law</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Aalto%2C+S">Susanne Aalto</a>, <a href="/search/astro-ph?searchtype=author&query=Appleton%2C+P">Philip Appleton</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="2308.00209v2-abstract-short" style="display: inline;"> We present new JWST-NIRSpec IFS data for the luminous infrared galaxy NGC7469: a nearby (70.6Mpc) active galaxy with a Sy 1.5 nucleus that drives a highly ionized gas outflow and a prominent nuclear star-forming ring. Using the superb sensitivity and high spatial resolution of the JWST instrument NIRSpec-IFS, we investigate the role of the Seyfert nucleus in the excitation and dynamics of the circ… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.00209v2-abstract-full').style.display = 'inline'; document.getElementById('2308.00209v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.00209v2-abstract-full" style="display: none;"> We present new JWST-NIRSpec IFS data for the luminous infrared galaxy NGC7469: a nearby (70.6Mpc) active galaxy with a Sy 1.5 nucleus that drives a highly ionized gas outflow and a prominent nuclear star-forming ring. Using the superb sensitivity and high spatial resolution of the JWST instrument NIRSpec-IFS, we investigate the role of the Seyfert nucleus in the excitation and dynamics of the circumnuclear gas. Our analysis focuses on the [Fe ii], H2, and hydrogen recombination lines that trace the radiation/shocked-excited molecular and ionized ISM around the AGN. We investigate the gas excitation through H2/Br纬 and [Fe ii]/Pa\b{eta} emission line ratios and find that photoionization by the AGN dominates within the central 300 pc of the galaxy and together with a small region show ing signatures of shock-heated gas; these shock-heated regions are likely associated with a compact radio jet. In addition, the velocity field and velocity dispersion maps reveal complex gas kinematics. Rotation is the dominant feature, but we also identify non-circular motions consistent with gas inflows as traced by the velocity residuals and the spiral pattern in the Pa伪 velocity dispersion map. The inflow is consistent with the mass outflow rate and two orders of magnitude higher than the AGN accretion rate. The compact nuclear radio jet has enough power to drive the highly ionized outflow. This scenario suggests that the inflow and outflow are in a self-regulating feeding-feedback process, with a contribution from the radio jet helping to drive the outflow. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.00209v2-abstract-full').style.display = 'none'; document.getElementById('2308.00209v2-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 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 31 July, 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">15 pages, 4 figures, 3 tables, accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.15169">arXiv:2307.15169</a> <span> [<a href="https://arxiv.org/pdf/2307.15169">pdf</a>, <a href="https://arxiv.org/format/2307.15169">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"> GOALS-JWST: Small neutral grains and enhanced 3.3 micron PAH emission in the Seyfert galaxy NGC 7469 </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Armus%2C+L">Lee Armus</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchin%2C+M">Marina Bianchin</a>, <a href="/search/astro-ph?searchtype=author&query=Diaz-Santos%2C+T">Tanio Diaz-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Linden%2C+S+T">Sean T. Linden</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Inami%2C+H">Hanae Inami</a>, <a href="/search/astro-ph?searchtype=author&query=U%2C+V">Vivian U</a>, <a href="/search/astro-ph?searchtype=author&query=Bohn%2C+T">Thomas Bohn</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+A+S">Aaron S. Evans</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=Hensley%2C+B+S">Brandon S. Hensley</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+J+-+T">J. -D. T. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Malkan%2C+M+A">Matthew A. Malkan</a>, <a href="/search/astro-ph?searchtype=author&query=Song%2C+Y">Yiqing Song</a>, <a href="/search/astro-ph?searchtype=author&query=Stierwalt%2C+S">Sabrina Stierwalt</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=McKinney%2C+J">Jed McKinney</a>, <a href="/search/astro-ph?searchtype=author&query=Aalto%2C+S">Susanne Aalto</a>, <a href="/search/astro-ph?searchtype=author&query=Buiten%2C+V+A">Victorine A. Buiten</a>, <a href="/search/astro-ph?searchtype=author&query=Rich%2C+J">Jeff Rich</a>, <a href="/search/astro-ph?searchtype=author&query=Charmandaris%2C+V">Vassilis Charmandaris</a>, <a href="/search/astro-ph?searchtype=author&query=Appleton%2C+P">Philip Appleton</a>, <a href="/search/astro-ph?searchtype=author&query=Barcos-Munoz%2C+L">Loreto Barcos-Munoz</a>, <a href="/search/astro-ph?searchtype=author&query=Boker%2C+T">Torsten Boker</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="2307.15169v1-abstract-short" style="display: inline;"> We present James Webb Space Telescope (JWST) Near Infrared Spectrograph (NIRSpec) integral-field spectroscopy of the nearby luminous infrared galaxy, NGC 7469. We take advantage of the high spatial/spectral resolution and wavelength coverage of JWST /NIRSpec to study the 3.3 um neutral polycyclic aromatic hydrocarbon (PAH) grain emission on ~60 pc scales. We find a clear change in the average grai… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.15169v1-abstract-full').style.display = 'inline'; document.getElementById('2307.15169v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.15169v1-abstract-full" style="display: none;"> We present James Webb Space Telescope (JWST) Near Infrared Spectrograph (NIRSpec) integral-field spectroscopy of the nearby luminous infrared galaxy, NGC 7469. We take advantage of the high spatial/spectral resolution and wavelength coverage of JWST /NIRSpec to study the 3.3 um neutral polycyclic aromatic hydrocarbon (PAH) grain emission on ~60 pc scales. We find a clear change in the average grain properties between the star-forming ring and the central AGN. Regions in the vicinity of the AGN, with [NeIII]/[NeII]>0.25, tend to have larger grain sizes and lower aliphatic-to-aromatic (3.4/3.3) ratios indicating that smaller grains are preferentially removed by photo-destruction in the vicinity of the AGN. We find an overall suppression of the total PAH emission relative to the ionized gas in the central 1 kpc region of the AGN in NGC 7469 compared to what has been observed with Spitzer on 3 kpc scales. However, the fractional 3.3 um to total PAH power is enhanced in the starburst ring, possibly due to a variety of physical effects on sub-kpc scales, including recurrent fluorescence of small grains or multiple photon absorption by large grains. Finally, the IFU data show that while the 3.3 um PAH-derived star formation rate (SFR) in the ring is 8% higher than that inferred from the [NeII] and [NeIII] emission lines, the integrated SFR derived from the 3.3 um feature would be underestimated by a factor of two due to the deficit of PAHs around the AGN, as might occur if a composite system like NGC 7469 were to be observed at high-redshift. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.15169v1-abstract-full').style.display = 'none'; document.getElementById('2307.15169v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 July, 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">14 pages, 5 figures, 2 tables, Submitted to ApJL</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.07338">arXiv:2306.07338</a> <span> [<a href="https://arxiv.org/pdf/2306.07338">pdf</a>, <a href="https://arxiv.org/format/2306.07338">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"> Cosmic Sands II: Challenges in Predicting and Measuring High-z Dust Temperatures </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lower%2C+S">Sidney Lower</a>, <a href="/search/astro-ph?searchtype=author&query=Narayanan%2C+D">Desika Narayanan</a>, <a href="/search/astro-ph?searchtype=author&query=Hu%2C+C">Chia-Yu Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</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="2306.07338v2-abstract-short" style="display: inline;"> In the current era of high-z galaxy discovery with JWST and ALMA, our ability to study the stellar populations and ISM conditions in a diverse range of galaxies at Cosmic Dawn has rapidly improved. At the same time, the need to understand the current limitations in modeling galaxy formation processes and physical properties in order to interpret these observations is critical. Here, we study the c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.07338v2-abstract-full').style.display = 'inline'; document.getElementById('2306.07338v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.07338v2-abstract-full" style="display: none;"> In the current era of high-z galaxy discovery with JWST and ALMA, our ability to study the stellar populations and ISM conditions in a diverse range of galaxies at Cosmic Dawn has rapidly improved. At the same time, the need to understand the current limitations in modeling galaxy formation processes and physical properties in order to interpret these observations is critical. Here, we study the challenges in modeling galaxy dust temperatures, both in the context of forward modeling galaxy spectral properties from a hydrodynamical simulation and via backwards modeling galaxy physical properties from mock observations of far-infrared dust emission. Using the Simba model for galaxy formation combined with Powderday radiative transfer, we can accurately predict the evolution of dust at high redshift, though several aspects of the model are essentially free parameters (dust composition, sub-resolution dust in star-forming regions) that dull the predictive power of the model dust temperature distributions. We also highlight the uncertainties in the backwards modeling methods, where we find the commonly used models and assumptions to fit FIR SEDs and infer dust temperatures (e.g., single temperature, optically thin modified blackbody) largely fail to capture the complexity of high-z dusty galaxies. We caution that conclusions inferred from both simulations -- limited by resolution and post-processing techniques -- and observations -- limited by sparse data and simplistic model parameterizations -- are susceptible to unique and nuanced uncertainties that can limit the usefulness of current high-z dust measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.07338v2-abstract-full').style.display = 'none'; document.getElementById('2306.07338v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 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">20 pages main text, 12 figures. Accepted to ApJ, newest version</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.04679">arXiv:2306.04679</a> <span> [<a href="https://arxiv.org/pdf/2306.04679">pdf</a>, <a href="https://arxiv.org/ps/2306.04679">ps</a>, <a href="https://arxiv.org/format/2306.04679">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/acda27">10.3847/2041-8213/acda27 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Tight Correlation Between Millimeter and X-ray Emission in Accreting Massive Black Holes from <100 Milliarcsecond-resolution ALMA Observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+C">Chin-Shin Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Kawamuro%2C+T">Taiki Kawamuro</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G">George Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotzky%2C+R">Richard Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">Benny Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Laor%2C+A">Ari Laor</a>, <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M+J">Michael J. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+K+L">Krista L. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Gupta%2C+K+K">Kriti K. Gupta</a>, <a href="/search/astro-ph?searchtype=author&query=Dimopoulos%2C+G">Georgios Dimopoulos</a>, <a href="/search/astro-ph?searchtype=author&query=Aalto%2C+S">Susanne Aalto</a>, <a href="/search/astro-ph?searchtype=author&query=Ros%2C+E">Eduardo Ros</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="2306.04679v2-abstract-short" style="display: inline;"> Recent studies have proposed that the nuclear millimeter continuum emission observed in nearby active galactic nuclei (AGN) could be created by the same population of electrons that gives rise to the X-ray emission that is ubiquitously observed in accreting black holes. We present the results of a dedicated high spatial resolution ($\sim$60-100 milliarcsecond) ALMA campaign on a volume-limited (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.04679v2-abstract-full').style.display = 'inline'; document.getElementById('2306.04679v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.04679v2-abstract-full" style="display: none;"> Recent studies have proposed that the nuclear millimeter continuum emission observed in nearby active galactic nuclei (AGN) could be created by the same population of electrons that gives rise to the X-ray emission that is ubiquitously observed in accreting black holes. We present the results of a dedicated high spatial resolution ($\sim$60-100 milliarcsecond) ALMA campaign on a volume-limited ($<50$ Mpc) sample of 26 hard X-ray ($>10$ keV) selected radio-quiet AGN. We find an extremely high detection rate (25/26 or $94^{+3}_{-6}\%$), which shows that nuclear emission at mm-wavelengths is nearly ubiquitous in accreting SMBHs. Our high-resolution observations show a tight correlation between the nuclear (1-23 pc) 100GHz and the intrinsic X-ray emission (1$蟽$ scatter of $0.22$ dex). The ratio between the 100GHz continuum and the X-ray emission does not show any correlation with column density, black hole mass, Eddington ratio or star formation rate, which suggests that the 100GHz emission can be used as a proxy of SMBH accretion over a very broad range of these parameters. The strong correlation between 100GHz and X-ray emission in radio-quiet AGN could be used to estimate the column density based on the ratio between the observed 2-10keV ($F^{\rm obs}_{2-10\rm\,keV}$) and 100GHz ($F_{100\rm\,GHz}$) fluxes. Specifically, a ratio $\log (F^{\rm obs}_{2-10\rm\,keV}/F_{100\rm\,GHz})\leq 3.5$ strongly suggests that a source is heavily obscured [$\log (N_{\rm H}/\rm cm^{-2})\gtrsim 23.8$]. Our work shows the potential of ALMA continuum observations to detect heavily obscured AGN (up to an optical depth of one at 100GHz, i.e. $N_{\rm H}\simeq 10^{27}\rm\,cm^{-2}$), and to identify binary SMBHs with separations $<100$ pc, which cannot be probed by current X-ray facilities. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.04679v2-abstract-full').style.display = 'none'; document.getElementById('2306.04679v2-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 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 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">ApJL in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.01020">arXiv:2304.01020</a> <span> [<a href="https://arxiv.org/pdf/2304.01020">pdf</a>, <a href="https://arxiv.org/format/2304.01020">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </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/10.1103/PhysRevD.108.023015">10.1103/PhysRevD.108.023015 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Investigating starburst-driven neutrino emission from galaxies in the Great Observatories All-Sky LIRG Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Merckx%2C+Y">Yarno Merckx</a>, <a href="/search/astro-ph?searchtype=author&query=Correa%2C+P">Pablo Correa</a>, <a href="/search/astro-ph?searchtype=author&query=de+Vries%2C+K+D">Krijn D. de Vries</a>, <a href="/search/astro-ph?searchtype=author&query=Kotera%2C+K">Kumiko Kotera</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=van+Eijndhoven%2C+N">Nick van Eijndhoven</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.01020v2-abstract-short" style="display: inline;"> We present a phenomenological framework for starburst-driven neutrino production via proton-proton collisions and apply it to (ultra)luminous infrared galaxies (U/LIRGs) in the Great Observatories All-Sky LIRG Survey (GOALS). The framework relates the infrared luminosity of a GOALS galaxy, derived from consistently available Herschel Space Observatory data, to the expected starburst-driven neutrin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.01020v2-abstract-full').style.display = 'inline'; document.getElementById('2304.01020v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.01020v2-abstract-full" style="display: none;"> We present a phenomenological framework for starburst-driven neutrino production via proton-proton collisions and apply it to (ultra)luminous infrared galaxies (U/LIRGs) in the Great Observatories All-Sky LIRG Survey (GOALS). The framework relates the infrared luminosity of a GOALS galaxy, derived from consistently available Herschel Space Observatory data, to the expected starburst-driven neutrino flux. The model parameters that define this relation can be estimated from multiwavelength data. We apply the framework in a case study to the LIRG NGC 3690 (Arp 299, Mrk 171) and compare the obtained neutrino fluxes to the current sensitivity of the IceCube Neutrino Observatory. Using our framework, we also conclude that the neutrino emission in the LIRG NGC 1068, recently presented as the first steady IceCube neutrino point source, cannot be explained by a starburst-driven scenario and is therefore likely dominated by the active galactic nucleus in this galaxy. In addition to the single-source investigations, we also estimate the diffuse starburst-driven neutrino flux from GOALS galaxies and the total LIRG population over cosmic history. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.01020v2-abstract-full').style.display = 'none'; document.getElementById('2304.01020v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">26 pages, 11 figures, published version in Phys. Rev. D</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 108 (2023) 023015 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.03609">arXiv:2301.03609</a> <span> [<a href="https://arxiv.org/pdf/2301.03609">pdf</a>, <a href="https://arxiv.org/format/2301.03609">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="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/aca8f0">10.3847/2041-8213/aca8f0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> UGC 4211: A Confirmed Dual Active Galactic Nucleus in the Local Universe at 230 pc Nuclear Separation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M+J">Michael J. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Treister%2C+E">Ezequiel Treister</a>, <a href="/search/astro-ph?searchtype=author&query=Kakkad%2C+D">Darshan Kakkad</a>, <a href="/search/astro-ph?searchtype=author&query=Casey-Clyde%2C+J+A">J. Andrew Casey-Clyde</a>, <a href="/search/astro-ph?searchtype=author&query=Kawamuro%2C+T">Taiki Kawamuro</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+J">Jonathan Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Foord%2C+A">Adi Foord</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">Benny Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotzky%2C+R">Richard Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Barcos-Munoz%2C+L">Loreto Barcos-Munoz</a>, <a href="/search/astro-ph?searchtype=author&query=Blecha%2C+L">Laura Blecha</a>, <a href="/search/astro-ph?searchtype=author&query=Connor%2C+T">Thomas Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+T">Tingting Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Magno%2C+M">Macon Magno</a>, <a href="/search/astro-ph?searchtype=author&query=Mingarelli%2C+C+M+F">Chiara M. F. Mingarelli</a>, <a href="/search/astro-ph?searchtype=author&query=Muller-Sanchez%2C+F">Francisco Muller-Sanchez</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">Kyuseok Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Shimizu%2C+T+T">T. Taro Shimizu</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+K+L">Krista L. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Tello%2C+M+P">Miguel Parra Tello</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2301.03609v1-abstract-short" style="display: inline;"> We present multi-wavelength high-spatial resolution (~0.1'', 70 pc) observations of UGC 4211 at z=0.03474, a late-stage major galaxy merger at the closest nuclear separation yet found in near-IR imaging (0.32'', ~230 pc projected separation). Using Hubble Space Telescope/STIS, VLT/MUSE+AO, Keck/OSIRIS+AO spectroscopy, and ALMA observations, we show that the spatial distribution, optical and NIR em… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.03609v1-abstract-full').style.display = 'inline'; document.getElementById('2301.03609v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.03609v1-abstract-full" style="display: none;"> We present multi-wavelength high-spatial resolution (~0.1'', 70 pc) observations of UGC 4211 at z=0.03474, a late-stage major galaxy merger at the closest nuclear separation yet found in near-IR imaging (0.32'', ~230 pc projected separation). Using Hubble Space Telescope/STIS, VLT/MUSE+AO, Keck/OSIRIS+AO spectroscopy, and ALMA observations, we show that the spatial distribution, optical and NIR emission lines, and millimeter continuum emission are all consistent with both nuclei being powered by accreting supermassive black holes (SMBHs). Our data, combined with common black hole mass prescriptions, suggests that both SMBHs have similar masses, log MBH~8.1 (south) and log MBH~8.3 (north), respectively. The projected separation of 230 pc (~6X the black hole sphere of influence) represents the closest-separation dual AGN studied to date with multi-wavelength resolved spectroscopy and shows the potential of nuclear (<50 pc) continuum observations with ALMA to discover hidden growing SMBH pairs. While the exact occurrence rate of close-separation dual AGN is not yet known, it may be surprisingly high, given that UGC 4211 was found within a small, volume-limited sample of nearby hard X-ray detected AGN. Observations of dual SMBH binaries in the sub-kpc regime at the final stages of dynamical friction provide important constraints for future gravitational wave observatories. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.03609v1-abstract-full').style.display = 'none'; document.getElementById('2301.03609v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 7 figures, 2 tables, published in ApJL</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJL, 942, 1, L24, Published 9 January 2023 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.02338">arXiv:2301.02338</a> <span> [<a href="https://arxiv.org/pdf/2301.02338">pdf</a>, <a href="https://arxiv.org/format/2301.02338">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/acb2b8">10.3847/2041-8213/acb2b8 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> GOALS-JWST: Pulling Back the Curtain on the AGN and Star Formation in VV 114 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rich%2C+J">J. Rich</a>, <a href="/search/astro-ph?searchtype=author&query=Aalto%2C+S">S. Aalto</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+A+S">A. S. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Charmandaris%2C+V">V. Charmandaris</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">G. C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Lai%2C+T">T. Lai</a>, <a href="/search/astro-ph?searchtype=author&query=Inami%2C+H">H. Inami</a>, <a href="/search/astro-ph?searchtype=author&query=Linden%2C+S">S. Linden</a>, <a href="/search/astro-ph?searchtype=author&query=Armus%2C+L">L. Armus</a>, <a href="/search/astro-ph?searchtype=author&query=Diaz-Santos%2C+T">T. Diaz-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Appleton%2C+P">P. Appleton</a>, <a href="/search/astro-ph?searchtype=author&query=Barcos-Mu%C3%B1oz%2C+L">L. Barcos-Mu帽oz</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ker%2C+T">T. B枚ker</a>, <a href="/search/astro-ph?searchtype=author&query=Larson%2C+K+L">K. L. Larson</a>, <a href="/search/astro-ph?searchtype=author&query=Law%2C+D+R">D. R. Law</a>, <a href="/search/astro-ph?searchtype=author&query=Malkan%2C+M+A">M. A. Malkan</a>, <a href="/search/astro-ph?searchtype=author&query=Medling%2C+A+M">A. M. Medling</a>, <a href="/search/astro-ph?searchtype=author&query=Song%2C+Y">Y. Song</a>, <a href="/search/astro-ph?searchtype=author&query=U%2C+V">V. U</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Werf%2C+P">P. van der Werf</a>, <a href="/search/astro-ph?searchtype=author&query=Bohn%2C+T">T. Bohn</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+M+J+I">M. J. I. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Finnerty%2C+L">L. Finnerty</a>, <a href="/search/astro-ph?searchtype=author&query=Hayward%2C+C">C. Hayward</a>, <a href="/search/astro-ph?searchtype=author&query=Howell%2C+J">J. Howell</a> , et al. (11 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2301.02338v1-abstract-short" style="display: inline;"> We present results from the James Webb Space Telescope (JWST) Director's Discretionary Time Early Release Science (ERS) program 1328 targeting the nearby, Luminous Infrared Galaxy (LIRG), VV 114. We use the MIRI and NIRSpec instruments to obtain integral-field spectroscopy of the heavily obscured Eastern nucleus (V114E) and surrounding regions. The spatially resolved, high-resolution, spectra reve… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.02338v1-abstract-full').style.display = 'inline'; document.getElementById('2301.02338v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.02338v1-abstract-full" style="display: none;"> We present results from the James Webb Space Telescope (JWST) Director's Discretionary Time Early Release Science (ERS) program 1328 targeting the nearby, Luminous Infrared Galaxy (LIRG), VV 114. We use the MIRI and NIRSpec instruments to obtain integral-field spectroscopy of the heavily obscured Eastern nucleus (V114E) and surrounding regions. The spatially resolved, high-resolution, spectra reveal the physical conditions in the gas and dust over a projected area of 2-3 kpc that includes the two brightest IR sources, the NE and SW cores. Our observations show for the first time spectroscopic evidence that the SW core hosts an AGN as evidenced by its very low 6.2 渭m and 3.3 渭m PAH equivalent widths (0.12 and 0.017 渭m respectively) and mid and near-IR colors. Our observations of the NE core show signs of deeply embedded star formation including absorption features due to aliphatic hydrocarbons, large quantities of amorphous silicates, as well as HCN due to cool gas along the line of sight. We detect elevated [Fe II]/Pf伪 consistent with extended shocks coincident with enhanced emission from warm H$_{2}$, far from the IR-bright cores and clumps. We also identify broadening and multiple kinematic components in both H$_{2}$ and fine structure lines caused by outflows and previously identified tidal features. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.02338v1-abstract-full').style.display = 'none'; document.getElementById('2301.02338v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 4 figures, accepted for publication in ApJL</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.05763">arXiv:2210.05763</a> <span> [<a href="https://arxiv.org/pdf/2210.05763">pdf</a>, <a href="https://arxiv.org/format/2210.05763">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/acb335">10.3847/2041-8213/acb335 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> GOALS-JWST: Revealing the Buried Star Clusters in the Luminous Infrared Galaxy VV 114 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Linden%2C+S+T">Sean T. Linden</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+A+S">Aaron S. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Armus%2C+L">Lee Armus</a>, <a href="/search/astro-ph?searchtype=author&query=Rich%2C+J+A">Jeffrey A. Rich</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=Lai%2C+T">Thomas Lai</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=U%2C+V">Vivian U</a>, <a href="/search/astro-ph?searchtype=author&query=Inami%2C+H">Hanae Inami</a>, <a href="/search/astro-ph?searchtype=author&query=Bohn%2C+T">Thomas Bohn</a>, <a href="/search/astro-ph?searchtype=author&query=Song%2C+Y">Yiqing Song</a>, <a href="/search/astro-ph?searchtype=author&query=Barcos-Mu%C3%B1oz%2C+L">Loreto Barcos-Mu帽oz</a>, <a href="/search/astro-ph?searchtype=author&query=Charmandaris%2C+V">Vassilis Charmandaris</a>, <a href="/search/astro-ph?searchtype=author&query=Medling%2C+A+M">Anne M. Medling</a>, <a href="/search/astro-ph?searchtype=author&query=Stierwalt%2C+S">Sabrina Stierwalt</a>, <a href="/search/astro-ph?searchtype=author&query=Diaz-Santos%2C+T">Tanio Diaz-Santos</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=van+der+Werf%2C+P">Paul van der Werf</a>, <a href="/search/astro-ph?searchtype=author&query=Aalto%2C+S">Susanne Aalto</a>, <a href="/search/astro-ph?searchtype=author&query=Appleton%2C+P">Philip Appleton</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+M+J+I">Michael J. I. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Hayward%2C+C+C">Christopher C. Hayward</a>, <a href="/search/astro-ph?searchtype=author&query=Howell%2C+J+H">Justin H. Howell</a>, <a href="/search/astro-ph?searchtype=author&query=Iwasawa%2C+K">Kazushi Iwasawa</a>, <a href="/search/astro-ph?searchtype=author&query=Kemper%2C+F">Francisca Kemper</a> , et al. (8 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2210.05763v2-abstract-short" style="display: inline;"> We present the results of a {\it James Webb Space Telescope} NIRCam investigation into the young massive star cluster (YMC) population in the luminous infrared galaxy VV 114. We identify 374 compact YMC candidates with a $S/N \geq 3$, 5, and 5 at F150W, F200W, and F356W respectively. A direct comparison with our {\it HST} cluster catalog reveals that $\sim 20\%$ of these sources are undetected at… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.05763v2-abstract-full').style.display = 'inline'; document.getElementById('2210.05763v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.05763v2-abstract-full" style="display: none;"> We present the results of a {\it James Webb Space Telescope} NIRCam investigation into the young massive star cluster (YMC) population in the luminous infrared galaxy VV 114. We identify 374 compact YMC candidates with a $S/N \geq 3$, 5, and 5 at F150W, F200W, and F356W respectively. A direct comparison with our {\it HST} cluster catalog reveals that $\sim 20\%$ of these sources are undetected at optical wavelengths. Based on {\it yggdrasil} stellar population models, we identify 17 YMC candidates in our {\it JWST} imaging alone with F150W-F200W and F200W-F356W colors suggesting they are all very young, dusty ($A_{V} = 5 - 15$), and massive ($10^{5.8} < M_{\odot} < 10^{6.1}$). The discovery of these `hidden' sources, many of which are found in the `overlap' region between the two nuclei, quadruples the number of $t < 3$ Myr clusters, and nearly doubles the number of $t < 6$ Myr clusters detected in VV 114. Now extending the cluster age distribution ($dN/d蟿\propto 蟿^纬$) to the youngest ages, we find a slope of $纬= -1.30 \pm 0.39$ for $10^{6} < 蟿(\mathrm{yr}) < 10^{7}$, which is consistent with the previously determined value from $10^{7} < 蟿(\mathrm{yr}) < 10^{8.5}$, and confirms that VV 114 has a steep age distribution slope for all massive star clusters across the entire range of cluster ages observed. Finally, the consistency between our {\it JWST}- and {\it HST}-derived age distribution slopes indicates that the balance between cluster formation and destruction has not been significantly altered in VV 114 over the last 0.5 Gyr. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.05763v2-abstract-full').style.display = 'none'; document.getElementById('2210.05763v2-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 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 4 figures, 1 table, published in 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/2209.13125">arXiv:2209.13125</a> <span> [<a href="https://arxiv.org/pdf/2209.13125">pdf</a>, <a href="https://arxiv.org/format/2209.13125">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/acac66">10.3847/2041-8213/acac66 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> GOALS-JWST: Mid-Infrared Spectroscopy of the Nucleus of NGC 7469 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Armus%2C+L">L. Armus</a>, <a href="/search/astro-ph?searchtype=author&query=Lai%2C+T">T. Lai</a>, <a href="/search/astro-ph?searchtype=author&query=U%2C+V">V. U</a>, <a href="/search/astro-ph?searchtype=author&query=Larson%2C+K+L">K. L. Larson</a>, <a href="/search/astro-ph?searchtype=author&query=Diaz-Santos%2C+T">T. Diaz-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+A+S">A. S. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Malkan%2C+M+A">M. A. Malkan</a>, <a href="/search/astro-ph?searchtype=author&query=Rich%2C+J">J. Rich</a>, <a href="/search/astro-ph?searchtype=author&query=Medling%2C+A+M">A. M. Medling</a>, <a href="/search/astro-ph?searchtype=author&query=law%2C+D+R">D. R. law</a>, <a href="/search/astro-ph?searchtype=author&query=Inami%2C+H">H. Inami</a>, <a href="/search/astro-ph?searchtype=author&query=Muller-Sanchez%2C+F">F. Muller-Sanchez</a>, <a href="/search/astro-ph?searchtype=author&query=Charmandaris%2C+V">V. Charmandaris</a>, <a href="/search/astro-ph?searchtype=author&query=der+Werf%2C+P+c">P. can der Werf</a>, <a href="/search/astro-ph?searchtype=author&query=Stierwalt%2C+S">S. Stierwalt</a>, <a href="/search/astro-ph?searchtype=author&query=Linden%2C+S">S. Linden</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">G. C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Barcos-Munoz%2C+L">L. Barcos-Munoz</a>, <a href="/search/astro-ph?searchtype=author&query=Hayward%2C+C">C. Hayward</a>, <a href="/search/astro-ph?searchtype=author&query=Song%2C+Y">Y. Song</a>, <a href="/search/astro-ph?searchtype=author&query=Appleton%2C+P">P. Appleton</a>, <a href="/search/astro-ph?searchtype=author&query=Aalto%2C+S">S. Aalto</a>, <a href="/search/astro-ph?searchtype=author&query=Bohn%2C+T">T. Bohn</a>, <a href="/search/astro-ph?searchtype=author&query=Boker%2C+T">T. Boker</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+M+J+I">M. J. I. Brown</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="2209.13125v1-abstract-short" style="display: inline;"> We present mid-infrared spectroscopic observations of the nucleus of the nearby Seyfert galaxy NGC 7469 taken with the MIRI instrument on the James Webb Space Telescope (JWST) as part of Directors Discretionary Time Early Release Science (ERS) program 1328. The high resolution nuclear spectrum contains 19 emission lines covering a wide range of ionization. The high ionization lines show broad, blu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.13125v1-abstract-full').style.display = 'inline'; document.getElementById('2209.13125v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.13125v1-abstract-full" style="display: none;"> We present mid-infrared spectroscopic observations of the nucleus of the nearby Seyfert galaxy NGC 7469 taken with the MIRI instrument on the James Webb Space Telescope (JWST) as part of Directors Discretionary Time Early Release Science (ERS) program 1328. The high resolution nuclear spectrum contains 19 emission lines covering a wide range of ionization. The high ionization lines show broad, blueshifted emission reaching velocities up to 1700 km s$^{-1}$ and FWHM ranging from $\sim500 - 1100$ km s$^{-1}$. The width of the broad emission and the broad to narrow line flux ratios correlate with ionization potential. The results suggest a decelerating, stratified, AGN driven outflow emerging from the nucleus. The estimated mass outflow rate is one to two orders of magnitude larger than the current black hole accretion rate needed to power the AGN. Eight pure rotational H$_{2}$ emission lines are detected with intrinsic widths ranging from FWHM $\sim 125-330$ km s$^{-1}$. We estimate a total mass of warm H$_{2}$ gas of $\sim1.2\times10^{7}$M$_{\odot}$ in the central 100 pc. The PAH features are extremely weak in the nuclear spectrum, but a $6.2渭$m PAH feature with an equivalent width $\sim0.07渭$m and a flux of $2.7\times10^{-17}$ W m$^{-2}$ is detected. The spectrum is steeply rising in the mid-infrared, with a silicate strength $\sim0.02$, significantly smaller than seen in most PG QSOs, but comparable to other Seyfert 1's. These early MIRI mid-infrared IFU data highlight the power of JWST to probe the multi-phase interstellar media surrounding actively accreting supermassive black holes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.13125v1-abstract-full').style.display = 'none'; document.getElementById('2209.13125v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.06741">arXiv:2209.06741</a> <span> [<a href="https://arxiv.org/pdf/2209.06741">pdf</a>, <a href="https://arxiv.org/format/2209.06741">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/ac9ebf">10.3847/2041-8213/ac9ebf <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> GOALS-JWST: Tracing AGN Feedback on the Star-Forming ISM in NGC 7469 </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Armus%2C+L">Lee Armus</a>, <a href="/search/astro-ph?searchtype=author&query=U%2C+V">Vivian U</a>, <a href="/search/astro-ph?searchtype=author&query=Diaz-Santos%2C+T">Tanio Diaz-Santos</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=Evans%2C+A">Aaron Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Malkan%2C+M+A">Matthew A. Malkan</a>, <a href="/search/astro-ph?searchtype=author&query=Appleton%2C+P">Philip Appleton</a>, <a href="/search/astro-ph?searchtype=author&query=Rich%2C+J">Jeff Rich</a>, <a href="/search/astro-ph?searchtype=author&query=Muller-Sanchez%2C+F">Francisco Muller-Sanchez</a>, <a href="/search/astro-ph?searchtype=author&query=Inami%2C+H">Hanae Inami</a>, <a href="/search/astro-ph?searchtype=author&query=Bohn%2C+T">Thomas Bohn</a>, <a href="/search/astro-ph?searchtype=author&query=McKinney%2C+J">Jed McKinney</a>, <a href="/search/astro-ph?searchtype=author&query=Finnerty%2C+L">Luke Finnerty</a>, <a href="/search/astro-ph?searchtype=author&query=Law%2C+D+R">David R. Law</a>, <a href="/search/astro-ph?searchtype=author&query=Linden%2C+S">Sean Linden</a>, <a href="/search/astro-ph?searchtype=author&query=Medling%2C+A+M">Anne M. Medling</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Song%2C+Y">Yiqing Song</a>, <a href="/search/astro-ph?searchtype=author&query=Stierwalt%2C+S">Sabrina Stierwalt</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=Barcos-Mu%C3%B1oz%2C+L">Loreto Barcos-Mu帽oz</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+J+D+T">J. D. T. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Togi%2C+A">Aditya Togi</a>, <a href="/search/astro-ph?searchtype=author&query=Aalto%2C+S">Susanne Aalto</a> , et al. (12 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.06741v1-abstract-short" style="display: inline;"> We present James Webb Space Telescope (JWST) Mid-InfraRed Instrument (MIRI) integral-field spectroscopy of the nearby merging, luminous infrared galaxy, NGC 7469. This galaxy hosts a Seyfert type-1.5 nucleus, a highly ionized outflow, and a bright, circumnuclear star-forming ring, making it an ideal target to study AGN feedback in the local Universe. We take advantage of the high spatial/spectral… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.06741v1-abstract-full').style.display = 'inline'; document.getElementById('2209.06741v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.06741v1-abstract-full" style="display: none;"> We present James Webb Space Telescope (JWST) Mid-InfraRed Instrument (MIRI) integral-field spectroscopy of the nearby merging, luminous infrared galaxy, NGC 7469. This galaxy hosts a Seyfert type-1.5 nucleus, a highly ionized outflow, and a bright, circumnuclear star-forming ring, making it an ideal target to study AGN feedback in the local Universe. We take advantage of the high spatial/spectral resolution of JWST/MIRI to isolate the star-forming regions surrounding the central active nucleus and study the properties of the dust and warm molecular gas on ~100 pc scales. The starburst ring exhibits prominent Polycyclic Aromatic Hydrocarbon (PAH) emission, with grain sizes and ionization states varying by only ~30%, and a total star formation rate of $\rm 10 - 30 \ M_\odot$/yr derived from fine structure and recombination emission lines. Using pure rotational lines of H2, we detect 1.2$\times$10$^{7} \rm \ M_\odot$ of warm molecular gas at a temperature higher than 200 K in the ring. All PAH bands get significantly weaker towards the central source, where larger and possibly more ionized grains dominate the emission. However, the bulk of the dust and molecular gas in the ring appears unaffected by the ionizing radiation or the outflowing wind from the AGN. These observations highlight the power of JWST to probe the inner regions of dusty, rapidly evolving galaxies for signatures of feedback and inform models that seek to explain the co-evolution of supermassive black holes and their hosts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.06741v1-abstract-full').style.display = 'none'; document.getElementById('2209.06741v1-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 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 4 figures, 2 tables, Submitted to ApJL</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.04466">arXiv:2209.04466</a> <span> [<a href="https://arxiv.org/pdf/2209.04466">pdf</a>, <a href="https://arxiv.org/format/2209.04466">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/acab61">10.3847/2041-8213/acab61 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> GOALS-JWST: NIRCam and MIRI Imaging of the Circumnuclear Starburst Ring in NGC 7469 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bohn%2C+T">Thomas Bohn</a>, <a href="/search/astro-ph?searchtype=author&query=Inami%2C+H">Hanae Inami</a>, <a href="/search/astro-ph?searchtype=author&query=Diaz-Santos%2C+T">Tanio Diaz-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Armus%2C+L">Lee Armus</a>, <a href="/search/astro-ph?searchtype=author&query=Linden%2C+S+T">Sean T. Linden</a>, <a href="/search/astro-ph?searchtype=author&query=U%2C+V">Vivian U</a>, <a href="/search/astro-ph?searchtype=author&query=Surace%2C+J">Jason Surace</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=Evans%2C+A+S">Aaron S. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Hoshioka%2C+S">Shunshi Hoshioka</a>, <a href="/search/astro-ph?searchtype=author&query=Lai%2C+T">Thomas Lai</a>, <a href="/search/astro-ph?searchtype=author&query=Song%2C+Y">Yiqing Song</a>, <a href="/search/astro-ph?searchtype=author&query=Mazzarella%2C+J+M">Joseph M. Mazzarella</a>, <a href="/search/astro-ph?searchtype=author&query=Barcos-Munoz%2C+L">Loreto Barcos-Munoz</a>, <a href="/search/astro-ph?searchtype=author&query=Charmandaris%2C+V">Vassilis Charmandaris</a>, <a href="/search/astro-ph?searchtype=author&query=Howell%2C+J+H">Justin H. Howell</a>, <a href="/search/astro-ph?searchtype=author&query=Medling%2C+A+M">Anne M. Medling</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Rich%2C+J+A">Jeffrey A. Rich</a>, <a href="/search/astro-ph?searchtype=author&query=Stierwalt%2C+S">Sabrina Stierwalt</a>, <a href="/search/astro-ph?searchtype=author&query=Aalto%2C+S">Susanne Aalto</a>, <a href="/search/astro-ph?searchtype=author&query=Boker%2C+T">Torsten Boker</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+M+J+I">Michael J. I. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Iwasawa%2C+K">Kazushi Iwasawa</a>, <a href="/search/astro-ph?searchtype=author&query=Malkan%2C+M+A">Matthew A. Malkan</a> , et al. (8 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.04466v2-abstract-short" style="display: inline;"> We present James Webb Space Telescope (JWST) imaging of NGC 7469 with the Near-Infrared Camera (NIRCam) and the Mid-InfraRed Instrument (MIRI). NGC 7469 is a nearby, $z=0.01627$, luminous infrared galaxy (LIRG) that hosts both a Seyfert Type-1.5 nucleus and a circumnuclear starburst ring with a radius of $\sim$0.5 kpc. The new near-infrared (NIR) JWST imaging reveals 66 star-forming regions, 37 of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.04466v2-abstract-full').style.display = 'inline'; document.getElementById('2209.04466v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.04466v2-abstract-full" style="display: none;"> We present James Webb Space Telescope (JWST) imaging of NGC 7469 with the Near-Infrared Camera (NIRCam) and the Mid-InfraRed Instrument (MIRI). NGC 7469 is a nearby, $z=0.01627$, luminous infrared galaxy (LIRG) that hosts both a Seyfert Type-1.5 nucleus and a circumnuclear starburst ring with a radius of $\sim$0.5 kpc. The new near-infrared (NIR) JWST imaging reveals 66 star-forming regions, 37 of which were not detected by HST observations. Twenty-eight of the 37 sources have very red NIR colors that indicate obscurations up to A$_{\rm{v}}\sim7$ and a contribution of at least 25$\%$ from hot dust emission to the 4.4$渭$m band. Their NIR colors are also consistent with young ($<$5 Myr) stellar populations and more than half of them are coincident with the MIR emission peaks. These younger, dusty star-forming regions account for $\sim$6$\%$ and $\sim$17$\%$ of the total 1.5$渭$m and 4.4$渭$m luminosity of the starburst ring, respectively. Thanks to JWST, we find a significant number of young dusty sources that were previously unseen due to dust extinction. The newly identified 28 young sources are a significant increase compared to the number of HST-detected young sources (4-5). This makes the total percentage of the young population rise from $\sim$15$\%$ to 48$\%$. These results illustrate the effectiveness of JWST in identifying and characterizing previously hidden star formation in the densest star-forming environments around AGN. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.04466v2-abstract-full').style.display = 'none'; document.getElementById('2209.04466v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">4 figures, 1 table, Accepted by 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/2209.04002">arXiv:2209.04002</a> <span> [<a href="https://arxiv.org/pdf/2209.04002">pdf</a>, <a href="https://arxiv.org/format/2209.04002">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac923b">10.3847/1538-4357/ac923b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Characterizing Compact 15-33 GHz Radio Continuum Sources in Local U/LIRGs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Song%2C+Y">Y. Song</a>, <a href="/search/astro-ph?searchtype=author&query=Linden%2C+S+T">S. T. Linden</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+A+S">A. S. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Barcos-Munoz%2C+L">L. Barcos-Munoz</a>, <a href="/search/astro-ph?searchtype=author&query=Murphy%2C+E+J">E. J. Murphy</a>, <a href="/search/astro-ph?searchtype=author&query=Momjian%2C+E">E. Momjian</a>, <a href="/search/astro-ph?searchtype=author&query=Diaz-Santos%2C+T">T. Diaz-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Larson%2C+K+L">K. L. Larson</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">G. C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Huang%2C+X">X. Huang</a>, <a href="/search/astro-ph?searchtype=author&query=Armus%2C+L">L. Armus</a>, <a href="/search/astro-ph?searchtype=author&query=Mazzarella%2C+J+M">J. M. Mazzarella</a>, <a href="/search/astro-ph?searchtype=author&query=U%2C+V">V. U</a>, <a href="/search/astro-ph?searchtype=author&query=Inami%2C+H">H. Inami</a>, <a href="/search/astro-ph?searchtype=author&query=Charmandaris%2C+V">V. Charmandaris</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">C. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Emig%2C+K+L">K. L. Emig</a>, <a href="/search/astro-ph?searchtype=author&query=McKinney%2C+J">J. McKinney</a>, <a href="/search/astro-ph?searchtype=author&query=Yoon%2C+I">I. Yoon</a>, <a href="/search/astro-ph?searchtype=author&query=Kunneriath%2C+D">D. Kunneriath</a>, <a href="/search/astro-ph?searchtype=author&query=Lai%2C+T+S+-">T. S. -Y. Lai</a>, <a href="/search/astro-ph?searchtype=author&query=Rodas-Quito%2C+E+E">E. E. Rodas-Quito</a>, <a href="/search/astro-ph?searchtype=author&query=Saravia%2C+A">A. Saravia</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+T">T. Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Meynardie%2C+W">W. Meynardie</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.04002v1-abstract-short" style="display: inline;"> We present the analysis of $\sim 100$pc-scale compact radio continuum sources detected in 63 local (Ultra) Luminous Infrared Galaxies (U/LIRGs; $L_{\rm IR} \ge 10^{11} L_\odot$), using FWHM $\lesssim 0''.1 - 0''.2$ resolution 15 and 33 GHz observations with the Karl G. Jansky Very Large Array. We identify a total of 133 compact radio sources with effective radii of 8 - 170pc, which are classified… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.04002v1-abstract-full').style.display = 'inline'; document.getElementById('2209.04002v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.04002v1-abstract-full" style="display: none;"> We present the analysis of $\sim 100$pc-scale compact radio continuum sources detected in 63 local (Ultra) Luminous Infrared Galaxies (U/LIRGs; $L_{\rm IR} \ge 10^{11} L_\odot$), using FWHM $\lesssim 0''.1 - 0''.2$ resolution 15 and 33 GHz observations with the Karl G. Jansky Very Large Array. We identify a total of 133 compact radio sources with effective radii of 8 - 170pc, which are classified into four main categories -- "AGN" (AGN), "AGN/SBnuc" (AGN-starburst composite nucleus), "SBnuc" (starburst nucleus) and "SF" (star-forming clumps) -- based on ancillary datasets and the literature. We find that "AGN" and "AGN/SBnuc" more frequently occur in late-stage mergers and have up to 3 dex higher 33 GHz luminosities and surface densities compared with "SBnuc" and "SF", which may be attributed to extreme nuclear starburst and/or AGN activity in the former. Star formation rates (SFRs) and surface densities ($危_{\rm SFR}$) are measured for "SF" and "SBnuc" using both the total 33 GHz continuum emission (SFR $\sim 0.14 - 13$ M$_\odot$ yr$^{-1}$, $危_{\rm SFR} \sim 13 - 1600$ M$_\odot$ yr$^{-1}$ kpc$^{-2}$) and the thermal free-free emission from HII regions (median SFR$_{\rm th} \sim 0.4$ M$_\odot$ yr$^{-1}$, $危_{\rm SFR_{th}} \sim 44$ M$_\odot$ yr$^{-1}$ kpc$^{-2}$). These values are 1 - 2 dex higher than those measured for similar-sized clumps in nearby normal (non-U/LIRGs). The latter also have much flatter median 15 - 33 GHz spectral index ($\sim -0.08$) compared with "SBnuc" and "SF" ($\sim -0.46$), which may reflect higher non-thermal contribution from supernovae and/or ISM densities in local U/LIRGs that directly result from and/or lead to their extreme star-forming activities on 100\,pc scales. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.04002v1-abstract-full').style.display = 'none'; document.getElementById('2209.04002v1-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 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in 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/2209.01210">arXiv:2209.01210</a> <span> [<a href="https://arxiv.org/pdf/2209.01210">pdf</a>, <a href="https://arxiv.org/format/2209.01210">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/ac961c">10.3847/2041-8213/ac961c <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> GOALS-JWST: Resolving the Circumnuclear Gas Dynamics in NGC 7469 in the Mid-Infrared </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=U%2C+V">Vivian U</a>, <a href="/search/astro-ph?searchtype=author&query=Lai%2C+T">Thomas Lai</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchin%2C+M">Marina Bianchin</a>, <a href="/search/astro-ph?searchtype=author&query=Remigio%2C+R+P">Raymond P. Remigio</a>, <a href="/search/astro-ph?searchtype=author&query=Armus%2C+L">Lee Armus</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=Diaz-Santos%2C+T">Tanio Diaz-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+A">Aaron Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Stierwalt%2C+S">Sabrina Stierwalt</a>, <a href="/search/astro-ph?searchtype=author&query=Law%2C+D+R">David R. Law</a>, <a href="/search/astro-ph?searchtype=author&query=Malkan%2C+M+A">Matthew A. Malkan</a>, <a href="/search/astro-ph?searchtype=author&query=Linden%2C+S">Sean Linden</a>, <a href="/search/astro-ph?searchtype=author&query=Song%2C+Y">Yiqing Song</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=Gao%2C+T">Tianmu Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Medling%2C+A+M">Anne M. Medling</a>, <a href="/search/astro-ph?searchtype=author&query=Barcos-Mu%C3%B1oz%2C+L">Loreto Barcos-Mu帽oz</a>, <a href="/search/astro-ph?searchtype=author&query=Hayward%2C+C+C">Christopher C. Hayward</a>, <a href="/search/astro-ph?searchtype=author&query=Inami%2C+H">Hanae Inami</a>, <a href="/search/astro-ph?searchtype=author&query=Rich%2C+J">Jeff Rich</a>, <a href="/search/astro-ph?searchtype=author&query=Aalto%2C+S">Susanne Aalto</a>, <a href="/search/astro-ph?searchtype=author&query=Appleton%2C+P">Philip Appleton</a>, <a href="/search/astro-ph?searchtype=author&query=Bohn%2C+T">Thomas Bohn</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ker%2C+T">Torsten B枚ker</a> , et al. (13 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.01210v2-abstract-short" style="display: inline;"> The nearby, luminous infrared galaxy (LIRG) NGC 7469 hosts a Seyfert nucleus with a circumnuclear star-forming ring and is thus the ideal local laboratory for investigating the starburst--AGN connection in detail. We present integral-field observations of the central 1.3 kpc region in NGC 7469 obtained with the JWST Mid-InfraRed Instrument. Molecular and ionized gas distributions and kinematics at… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.01210v2-abstract-full').style.display = 'inline'; document.getElementById('2209.01210v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.01210v2-abstract-full" style="display: none;"> The nearby, luminous infrared galaxy (LIRG) NGC 7469 hosts a Seyfert nucleus with a circumnuclear star-forming ring and is thus the ideal local laboratory for investigating the starburst--AGN connection in detail. We present integral-field observations of the central 1.3 kpc region in NGC 7469 obtained with the JWST Mid-InfraRed Instrument. Molecular and ionized gas distributions and kinematics at a resolution of {\sim}100 pc over the 4.9 - 7.6渭m region are examined to study gas dynamics influenced by the central AGN. The low-ionization [Fe II] 位5.34渭m and [Ar II] 位6.99渭m lines are bright on the nucleus and in the starburst ring, as opposed to H2 S(5) 位6.91渭m which is strongly peaked at the center and surrounding ISM. The high-ionization [Mg V] line is resolved and shows a broad, blueshifted component associated with the outflow. It has a nearly face-on geometry that is strongly peaked on the nucleus, where it reaches a maximum velocity of -650 km/s, and extends about 400 pc to the East. Regions of enhanced velocity dispersion in H2 and [Fe II] {\sim}180 pc from the AGN that also show high L(H2)/L(PAH) and L([Fe II])/L(Pf伪) ratios to the W and N of the nucleus pinpoint regions where the ionized outflow is depositing energy, via shocks, into the dense interstellar medium between the nucleus and the starburst ring. These resolved mid-infrared observations of the nuclear gas dynamics demonstrate the power of JWST and its high-sensitivity integral-field spectroscopic capability to resolve feedback processes around supermassive black holes in the dusty cores of nearby LIRGs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.01210v2-abstract-full').style.display = 'none'; document.getElementById('2209.01210v2-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 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 6 figures, 1 table; accepted for publication in ApJL</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.00014">arXiv:2209.00014</a> <span> [<a href="https://arxiv.org/pdf/2209.00014">pdf</a>, <a href="https://arxiv.org/ps/2209.00014">ps</a>, <a href="https://arxiv.org/format/2209.00014">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="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac8e67">10.3847/1538-4357/ac8e67 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BASS XXXVII: The role of radiative feedback in the growth and obscuration properties of nearby supermassive black holes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">C. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Ananna%2C+T+T">T. T. Ananna</a>, <a href="/search/astro-ph?searchtype=author&query=Temple%2C+M+J">M. J. Temple</a>, <a href="/search/astro-ph?searchtype=author&query=Urry%2C+C+M">C. M. Urry</a>, <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M+J">M. J. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">B. Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Ueda%2C+Y">Y. Ueda</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">F. E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Treister%2C+E">E. Treister</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">G. C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">K. Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Paltani%2C+S">S. Paltani</a>, <a href="/search/astro-ph?searchtype=author&query=Stalevski%2C+M">M. Stalevski</a>, <a href="/search/astro-ph?searchtype=author&query=Ho%2C+L+C">L. C. Ho</a>, <a href="/search/astro-ph?searchtype=author&query=Fabian%2C+A+C">A. C. Fabian</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotzky%2C+R">R. Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+C+S">C. S. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">F. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Kakkad%2C+D">D. Kakkad</a>, <a href="/search/astro-ph?searchtype=author&query=Sartori%2C+L">L. Sartori</a>, <a href="/search/astro-ph?searchtype=author&query=Baer%2C+R">R. Baer</a>, <a href="/search/astro-ph?searchtype=author&query=Caglar%2C+T">T. Caglar</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M">M. Powell</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">F. Harrison</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.00014v1-abstract-short" style="display: inline;"> We study the relation between obscuration and supermassive black hole (SMBH) growth using a large sample of hard X-ray selected Active Galactic Nuclei (AGN). We find a strong decrease in the fraction of obscured sources above the Eddington limit for dusty gas ($\log 位_{\rm Edd}\gtrsim -2$) confirming earlier results, and consistent with the radiation-regulated unification model. This also explains… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.00014v1-abstract-full').style.display = 'inline'; document.getElementById('2209.00014v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.00014v1-abstract-full" style="display: none;"> We study the relation between obscuration and supermassive black hole (SMBH) growth using a large sample of hard X-ray selected Active Galactic Nuclei (AGN). We find a strong decrease in the fraction of obscured sources above the Eddington limit for dusty gas ($\log 位_{\rm Edd}\gtrsim -2$) confirming earlier results, and consistent with the radiation-regulated unification model. This also explains the difference in the Eddington ratio distribution functions (ERDFs) of type 1 and type 2 AGN obtained by a recent study. The break in the ERDF of nearby AGN is at $\log 位_{\rm Edd}^{*}=-1.34\pm0.07$. This corresponds to the $位_{\rm Edd}$ where AGN transition from having most of their sky covered by obscuring material to being mostly devoid of absorbing material. A similar trend is observed for the luminosity function, which implies that most of the SMBH growth in the local Universe happens when the AGN is covered by a large reservoir of gas and dust. These results could be explained with a radiation-regulated growth model, in which AGN move in the $N_{\rm H}-位_{\rm Edd}$ plane during their life cycle. The growth episode starts with the AGN mostly unobscured and accreting at low $位_{\rm Edd}$. As the SMBH is further fueled, $位_{\rm Edd}$, $N_{\rm H}$ and covering factor increase, leading AGN to be preferentially observed as obscured. Once $位_{\rm Edd}$ reaches the Eddington limit for dusty gas, the covering factor and $N_{\rm H}$ rapidly decrease, leading the AGN to be typically observed as unobscured. As the remaining fuel is depleted, the SMBH goes back into a quiescent phase. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.00014v1-abstract-full').style.display = 'none'; document.getElementById('2209.00014v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in 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/2208.14507">arXiv:2208.14507</a> <span> [<a href="https://arxiv.org/pdf/2208.14507">pdf</a>, <a href="https://arxiv.org/format/2208.14507">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/ac9971">10.3847/2041-8213/ac9971 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> GOALS-JWST: Hidden Star Formation and Extended PAH Emission in the Luminous Infrared Galaxy VV 114 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Evans%2C+A+S">Aaron S. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Frayer%2C+D">David Frayer</a>, <a href="/search/astro-ph?searchtype=author&query=Charmandaris%2C+V">Vassilis Charmandaris</a>, <a href="/search/astro-ph?searchtype=author&query=Armus%2C+L">Lee Armus</a>, <a href="/search/astro-ph?searchtype=author&query=Inami%2C+H">Hanae Inami</a>, <a href="/search/astro-ph?searchtype=author&query=Surace%2C+J">Jason Surace</a>, <a href="/search/astro-ph?searchtype=author&query=Linden%2C+S">Sean Linden</a>, <a href="/search/astro-ph?searchtype=author&query=Soifer%2C+B">Baruch Soifer</a>, <a href="/search/astro-ph?searchtype=author&query=Diaz-Santos%2C+T">Tanio Diaz-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Larson%2C+K">Kirsten Larson</a>, <a href="/search/astro-ph?searchtype=author&query=Rich%2C+J">Jeffrey Rich</a>, <a href="/search/astro-ph?searchtype=author&query=Song%2C+Y">Yiqing Song</a>, <a href="/search/astro-ph?searchtype=author&query=Barcos-Munoz%2C+L">Loreto Barcos-Munoz</a>, <a href="/search/astro-ph?searchtype=author&query=Mazzarella%2C+J">Joseph Mazzarella</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G">George Privon</a>, <a href="/search/astro-ph?searchtype=author&query=U%2C+V">Vivian U</a>, <a href="/search/astro-ph?searchtype=author&query=Medling%2C+A">Anne Medling</a>, <a href="/search/astro-ph?searchtype=author&query=Boeker%2C+T">Torsten Boeker</a>, <a href="/search/astro-ph?searchtype=author&query=Aalto%2C+S">Susanne Aalto</a>, <a href="/search/astro-ph?searchtype=author&query=Iwasawa%2C+K">Kazushi Iwasawa</a>, <a href="/search/astro-ph?searchtype=author&query=Howell%2C+J">Justin Howell</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Werf%2C+P">Paul van der Werf</a>, <a href="/search/astro-ph?searchtype=author&query=Appleton%2C+P+N">Philip N. Appleton</a>, <a href="/search/astro-ph?searchtype=author&query=Bohn%2C+T">Thomas Bohn</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+M">Michael Brown</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="2208.14507v1-abstract-short" style="display: inline;"> James Webb Space Telescope (JWST) Mid-InfraRed Instrument (MIRI) images of the luminous infrared (IR) galaxy VV 114 are presented. This redshift ~ 0.020 merger has a western component (VV 114W) rich in optical star clusters and an eastern component (VV 114E) hosting a luminous mid-IR nucleus hidden at UV and optical wavelengths by dust lanes. With MIRI, the VV 114E nucleus resolves primarily into… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.14507v1-abstract-full').style.display = 'inline'; document.getElementById('2208.14507v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.14507v1-abstract-full" style="display: none;"> James Webb Space Telescope (JWST) Mid-InfraRed Instrument (MIRI) images of the luminous infrared (IR) galaxy VV 114 are presented. This redshift ~ 0.020 merger has a western component (VV 114W) rich in optical star clusters and an eastern component (VV 114E) hosting a luminous mid-IR nucleus hidden at UV and optical wavelengths by dust lanes. With MIRI, the VV 114E nucleus resolves primarily into bright NE and SW cores separated by 630 pc. This nucleus comprises 45% of the 15um light of VV 114, with the NE and SW cores having IR luminosities, L_ IR (8-1000um) ~ 8+/-0.8x10^10 L_sun and ~ 5+/-0.5x10^10 L_sun, respectively, and IR densities, Sigma_IR >~ 2+/-0.2x10^13 L_sun / kpc^2 and >~ 7+/-0.7x10^12 L_sun / kpc^2, respectively -- in the range of Sigma_IR for the Orion star-forming core and the nuclei of Arp 220. The NE core, previously speculated to have an Active Galactic Nucleus (AGN), has starburst-like mid-IR colors. In contrast, the VV 114E SW has AGN-like colors. Approximately 40 star-forming knots with L_IR ~ 0.02-5x10^10 L_sun are identified, 25% of which have no optical counterpart. Finally, diffuse emission accounts for 40-60% of the mid-IR emission. Mostly notably, filamentary Poly-cyclic Aromatic Hydrocarbon (PAH) emission stochastically excited by UV and optical photons accounts for half of the 7.7um light of VV 114. This study illustrates the ability of JWST to detect obscured compact activity and distributed PAH emission in the most extreme starburst galaxies in the local Universe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.14507v1-abstract-full').style.display = 'none'; document.getElementById('2208.14507v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 4 figures, 1 table, Submitted to ApJL</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.10647">arXiv:2208.10647</a> <span> [<a href="https://arxiv.org/pdf/2208.10647">pdf</a>, <a href="https://arxiv.org/format/2208.10647">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/ac9389">10.3847/2041-8213/ac9389 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> GOALS-JWST: Unveiling Dusty Compact Sources in the Merging Galaxy IIZw096 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Inami%2C+H">Hanae Inami</a>, <a href="/search/astro-ph?searchtype=author&query=Surace%2C+J">Jason Surace</a>, <a href="/search/astro-ph?searchtype=author&query=Armus%2C+L">Lee Armus</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+A+S">Aaron S. Evans</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=Barcos-Munoz%2C+L">Loreto Barcos-Munoz</a>, <a href="/search/astro-ph?searchtype=author&query=Stierwalt%2C+S">Sabrina Stierwalt</a>, <a href="/search/astro-ph?searchtype=author&query=Mazzarella%2C+J+M">Joseph M. Mazzarella</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Song%2C+Y">Yiqing Song</a>, <a href="/search/astro-ph?searchtype=author&query=Linden%2C+S">Sean Linden</a>, <a href="/search/astro-ph?searchtype=author&query=Hayward%2C+C+C">Christopher C. Hayward</a>, <a href="/search/astro-ph?searchtype=author&query=Boker%2C+T">Torsten Boker</a>, <a href="/search/astro-ph?searchtype=author&query=U%2C+V">Vivian U</a>, <a href="/search/astro-ph?searchtype=author&query=Bohn%2C+T">Thomas Bohn</a>, <a href="/search/astro-ph?searchtype=author&query=Charmandaris%2C+V">Vassilis Charmandaris</a>, <a href="/search/astro-ph?searchtype=author&query=Diaz-Santos%2C+T">Tanio Diaz-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Howell%2C+J+H">Justin H. Howell</a>, <a href="/search/astro-ph?searchtype=author&query=Lai%2C+T">Thomas Lai</a>, <a href="/search/astro-ph?searchtype=author&query=Medling%2C+A+M">Anne M. Medling</a>, <a href="/search/astro-ph?searchtype=author&query=Rich%2C+J+A">Jeffrey A. Rich</a>, <a href="/search/astro-ph?searchtype=author&query=Aalto%2C+S">Susanne Aalto</a>, <a href="/search/astro-ph?searchtype=author&query=Appleton%2C+P">Philip Appleton</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+M+J+I">Michael J. I. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Hoshioka%2C+S">Shunshi Hoshioka</a> , et al. (8 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2208.10647v2-abstract-short" style="display: inline;"> We have used the Mid-InfraRed Instrument (MIRI) on the James Webb Space Telescope (JWST) to obtain the first spatially resolved, mid-infrared (mid-IR) images of IIZw096, a merging luminous infrared galaxy (LIRG) at $z = 0.036$. Previous observations with the Spitzer Space Telescope suggested that the vast majority of the total IR luminosity (LIR) of the system originated from a small region outsid… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.10647v2-abstract-full').style.display = 'inline'; document.getElementById('2208.10647v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.10647v2-abstract-full" style="display: none;"> We have used the Mid-InfraRed Instrument (MIRI) on the James Webb Space Telescope (JWST) to obtain the first spatially resolved, mid-infrared (mid-IR) images of IIZw096, a merging luminous infrared galaxy (LIRG) at $z = 0.036$. Previous observations with the Spitzer Space Telescope suggested that the vast majority of the total IR luminosity (LIR) of the system originated from a small region outside of the two merging nuclei. New observations with JWST/MIRI now allow an accurate measurement of the location and luminosity density of the source that is responsible for the bulk of the IR emission. We estimate that 40-70% of the IR bolometric luminosity, or $3-5 \times 10^{11}\,{\rm{L_{\odot}}}$, arises from a source no larger than 175pc in radius, suggesting a luminosity density of at least $3-5 \times 10^{12} \, {\rm{L_{\odot} \, kpc^{-2}}}$. In addition, we detect 11 other star forming sources, five of which were previously unknown. The MIRI F1500W/F560W colors of most of these sources, including the source responsible for the bulk of the far-IR emission, are much redder than the nuclei of local LIRGs. These observations reveal the power of JWST to disentangle the complex regions at the hearts of merging, dusty galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.10647v2-abstract-full').style.display = 'none'; document.getElementById('2208.10647v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">3 figures, 1 table, Accepted for publication in ApJL</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.03880">arXiv:2208.03880</a> <span> [<a href="https://arxiv.org/pdf/2208.03880">pdf</a>, <a href="https://arxiv.org/format/2208.03880">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="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac8794">10.3847/1538-4357/ac8794 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BASS XXXII: Studying the Nuclear Mm-wave Continuum Emission of AGNs with ALMA at Scales $\lesssim$ 100-200 pc </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kawamuro%2C+T">Taiki Kawamuro</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Imanishi%2C+M">Masatoshi Imanishi</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotzky%2C+R+F">Richard F. Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Izumi%2C+T">Takuma Izumi</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">Federica Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M+J">Michael J. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">Benny Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Ichikawa%2C+K">Kohei Ichikawa</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas%2C+A+F">Alejandra F. Rojas</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+K+L">Krista Lynne Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Shimizu%2C+T">Taro Shimizu</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">Kyuseok Oh</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=Baba%2C+S">Shunsuke Baba</a>, <a href="/search/astro-ph?searchtype=author&query=Balokovi%C4%87%2C+M">Mislav Balokovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+C">Chin-Shin Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Kakkad%2C+D">Darshan Kakkad</a>, <a href="/search/astro-ph?searchtype=author&query=Pfeifle%2C+R+W">Ryan W. Pfeifle</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Temple%2C+M+J">Matthew J. Temple</a>, <a href="/search/astro-ph?searchtype=author&query=Ueda%2C+Y">Yoshihiro Ueda</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M+C">Meredith C. Powell</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="2208.03880v2-abstract-short" style="display: inline;"> To understand the origin of nuclear ($\lesssim$ 100 pc) millimeter-wave (mm-wave) continuum emission in active galactic nuclei (AGNs), we systematically analyzed sub-arcsec resolution Band-6 (211-275 GHz) ALMA data of 98 nearby AGNs ($z <$ 0.05) from the 70-month Swift/BAT catalog. The sample, almost unbiased for obscured systems, provides the largest number of AGNs to date with high mm-wave spati… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.03880v2-abstract-full').style.display = 'inline'; document.getElementById('2208.03880v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.03880v2-abstract-full" style="display: none;"> To understand the origin of nuclear ($\lesssim$ 100 pc) millimeter-wave (mm-wave) continuum emission in active galactic nuclei (AGNs), we systematically analyzed sub-arcsec resolution Band-6 (211-275 GHz) ALMA data of 98 nearby AGNs ($z <$ 0.05) from the 70-month Swift/BAT catalog. The sample, almost unbiased for obscured systems, provides the largest number of AGNs to date with high mm-wave spatial resolution sampling ($\sim$ 1-200 pc), and spans broad ranges of 14-150 keV luminosity {$40 < \log[L_{\rm 14-150}/({\rm erg\,s^{-1}})] < 45$}, black hole mass [$5 < \log(M_{\rm BH}/M_\odot) < 10$], and Eddington ratio ($-4 < \log 位_{\rm Edd} < 2$). We find a significant correlation between 1.3 mm (230 GHz) and 14-150 keV luminosities. Its scatter is $\approx$ 0.36 dex, and the mm-wave emission may serve as a good proxy of the AGN luminosity, free of dust extinction up to $N_{\rm H} \sim 10^{26}$ cm$^{-2}$. While the mm-wave emission could be self-absorbed synchrotron radiation around the X-ray corona according to past works, we also discuss different possible origins of the mm-wave emission; AGN-related dust emission, outflow-driven shocks, and a small-scale ($<$ 200 pc) jet. The dust emission is unlikely to be dominant, as the mm-wave slope is generally flatter than expected. Also, due to no increase in the mm-wave luminosity with the Eddington ratio, a radiation-driven outflow model is possibly not the common mechanism. Furthermore, we find independence of the mm-wave luminosity on indicators of the inclination angle from the polar axis of the nuclear structure, which is inconsistent with a jet model whose luminosity depends only on the angle. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.03880v2-abstract-full').style.display = 'none'; document.getElementById('2208.03880v2-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 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">44 pages, 35 figures, 3 tables, accepted for publication in ApJ; modified format, added supplementary figure (Fig. 32)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.12435">arXiv:2207.12435</a> <span> [<a href="https://arxiv.org/pdf/2207.12435">pdf</a>, <a href="https://arxiv.org/format/2207.12435">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="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/ac650b">10.3847/1538-4365/ac650b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BASS XXVI: DR2 Host Galaxy Stellar Velocity Dispersions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M+J">Michael J. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">Benny Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">Kyuseok Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Caglar%2C+T">Turgay Caglar</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=Mushotzky%2C+R">Richard Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">Federica Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Mejia-Restrepo%2C+J+E">Julian E. Mejia-Restrepo</a>, <a href="/search/astro-ph?searchtype=author&query=Lamperti%2C+I">Isabella Lamperti</a>, <a href="/search/astro-ph?searchtype=author&query=Treister%2C+E">Ezequiel Treister</a>, <a href="/search/astro-ph?searchtype=author&query=Bar%2C+R+E">Rudolf E. Bar</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M+C">Meredith C. Powell</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Riffel%2C+R">Rogerio Riffel</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas%2C+A+F">Alejandra F. Rojas</a>, <a href="/search/astro-ph?searchtype=author&query=Schawinski%2C+K">Kevin Schawinski</a>, <a href="/search/astro-ph?searchtype=author&query=Urry%2C+C+M">C. Megan Urry</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2207.12435v1-abstract-short" style="display: inline;"> We present new central stellar velocity dispersions for 484 Sy 1.9 and Sy 2 from the second data release of the Swift/BAT AGN Spectroscopic Survey (BASS DR2). This constitutes the largest study of velocity dispersion measurements in X-ray selected, obscured AGN with 956 independent measurements of the Ca H+K and Mg b region (3880-5550A) and the Ca triplet region (8350-8730A) from 642 spectra mainl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.12435v1-abstract-full').style.display = 'inline'; document.getElementById('2207.12435v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.12435v1-abstract-full" style="display: none;"> We present new central stellar velocity dispersions for 484 Sy 1.9 and Sy 2 from the second data release of the Swift/BAT AGN Spectroscopic Survey (BASS DR2). This constitutes the largest study of velocity dispersion measurements in X-ray selected, obscured AGN with 956 independent measurements of the Ca H+K and Mg b region (3880-5550A) and the Ca triplet region (8350-8730A) from 642 spectra mainly from VLT/Xshooter or Palomar/DoubleSpec. Our sample spans velocity dispersions of 40-360 km/s, corresponding to 4-5 orders of magnitude in black holes mass (MBH=10^5.5-9.6 Msun), bolometric luminosity (LBol~10^{42-46 ergs/s), and Eddington ratio (L/Ledd~10^{-5}-2). For 281 AGN, our data provide the first published central velocity dispersions, including 6 AGN with low mass black holes (MBH=10^5.5-6.5 Msun), discovered thanks to our high spectral resolution observations (sigma~25 km/s). The survey represents a significant advance with a nearly complete census of hard-X-ray selected obscured AGN with measurements for 99% of nearby AGN (z<0.1) outside the Galactic plane. The BASS AGN have higher velocity dispersions than the more numerous optically selected narrow line AGN (i.e., ~150 vs. ~100 km/s), but are not biased towards the highest velocity dispersions of massive ellipticals (i.e., >250 km/s). Despite sufficient spectral resolution to resolve the velocity dispersions associated with the bulges of small black holes (~10^4-5 Msun), we do not find a significant population of super-Eddington AGN. Using estimates of the black hole sphere of influence, direct stellar and gas black hole mass measurements could be obtained with existing facilities for more than ~100 BASS AGN. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.12435v1-abstract-full').style.display = 'none'; document.getElementById('2207.12435v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">32 pages, 16 figures, 8 tables, published in ApJS as part of BASS DR2 special issue</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJS, 261, 6 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.12432">arXiv:2207.12432</a> <span> [<a href="https://arxiv.org/pdf/2207.12432">pdf</a>, <a href="https://arxiv.org/format/2207.12432">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="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/ac6c05">10.3847/1538-4365/ac6c05 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BASS XXII: The BASS DR2 AGN Catalog and Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M+J">Michael J. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">Benny Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">Kyuseok Oh</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=Mejia-Restrepo%2C+J+E">Julian E. Mejia-Restrepo</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Treister%2C+E">Ezequiel Treister</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M+C">Meredith C. Powell</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotzky%2C+R">Richard Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Ananna%2C+T+T">Tonima T. Ananna</a>, <a href="/search/astro-ph?searchtype=author&query=Balokovic%2C+M">Mislav Balokovic</a>, <a href="/search/astro-ph?searchtype=author&query=Bar%2C+R+E">Rudolf E. Bar</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+G">George Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Bessiere%2C+P">Patricia Bessiere</a>, <a href="/search/astro-ph?searchtype=author&query=Burtscher%2C+L">Leonard Burtscher</a>, <a href="/search/astro-ph?searchtype=author&query=Caglar%2C+T">Turgay Caglar</a>, <a href="/search/astro-ph?searchtype=author&query=Congiu%2C+E">Enrico Congiu</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+P">Phil Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Heida%2C+M">Marianne Heida</a>, <a href="/search/astro-ph?searchtype=author&query=Ichikawa%2C+K">Kohei Ichikawa</a>, <a href="/search/astro-ph?searchtype=author&query=Kamraj%2C+N">Nikita Kamraj</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="2207.12432v1-abstract-short" style="display: inline;"> We present the AGN catalog and optical spectroscopy for the second data release of the Swift BAT AGN Spectroscopic Survey (BASS DR2). With this DR2 release we provide 1425 optical spectra, of which 1181 are released for the first time, for the 858 hard X-ray selected AGN in the Swift BAT 70-month sample. The majority of the spectra (813/1425, 57%) are newly obtained from VLT/Xshooter or Palomar/Do… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.12432v1-abstract-full').style.display = 'inline'; document.getElementById('2207.12432v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.12432v1-abstract-full" style="display: none;"> We present the AGN catalog and optical spectroscopy for the second data release of the Swift BAT AGN Spectroscopic Survey (BASS DR2). With this DR2 release we provide 1425 optical spectra, of which 1181 are released for the first time, for the 858 hard X-ray selected AGN in the Swift BAT 70-month sample. The majority of the spectra (813/1425, 57%) are newly obtained from VLT/Xshooter or Palomar/Doublespec. Many of the spectra have both higher resolution (R>2500, N~450) and/or very wide wavelength coverage (3200-10000 A, N~600) that are important for a variety of AGN and host galaxy studies. We include newly revised AGN counterparts for the full sample and review important issues for population studies, with 44 AGN redshifts determined for the first time and 780 black hole mass and accretion rate estimates. This release is spectroscopically complete for all AGN (100%, 858/858) with 99.8% having redshift measurements (857/858) and 96% completion in black hole mass estimates of unbeamed AGN (outside the Galactic plane). This AGN sample represents a unique census of the brightest hard X-ray selected AGN in the sky, spanning many orders of magnitude in Eddington ratio (Ledd=10^-5-100), black hole mass (MBH=10^5-10^10 Msun), and AGN bolometric luminosity (Lbol=10^40-10^47 ergs/s). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.12432v1-abstract-full').style.display = 'none'; document.getElementById('2207.12432v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">34 pages, 11 figures, 15 tables, published in ApJS as part of BASS DR2 special issue</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJS, 261, 2 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.12428">arXiv:2207.12428</a> <span> [<a href="https://arxiv.org/pdf/2207.12428">pdf</a>, <a href="https://arxiv.org/format/2207.12428">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="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/ac6c8f">10.3847/1538-4365/ac6c8f <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BAT AGN Spectroscopic Survey XXI: The Data Release 2 Overview </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M+J">Michael J. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">Benny Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Treister%2C+E">Ezequiel Treister</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotzky%2C+R">Richard Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Urry%2C+C+M">C. Megan Urry</a>, <a href="/search/astro-ph?searchtype=author&query=Ananna%2C+T+T">Tonima T. Ananna</a>, <a href="/search/astro-ph?searchtype=author&query=Balokovic%2C+M">Mislav Balokovic</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=Cenko%2C+S+B">S. Bradley Cenko</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Ichikawa%2C+K">Kohei Ichikawa</a>, <a href="/search/astro-ph?searchtype=author&query=Lamperti%2C+I">Isabella Lamperti</a>, <a href="/search/astro-ph?searchtype=author&query=Lein%2C+A">Amy Lein</a>, <a href="/search/astro-ph?searchtype=author&query=Mejia-Restrepo%2C+J+E">Julian E. Mejia-Restrepo</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">Kyuseok Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Pacucci%2C+F">Fabio Pacucci</a>, <a href="/search/astro-ph?searchtype=author&query=Pfeifle%2C+R+W">Ryan W. Pfeifle</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M+C">Meredith C. Powell</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">Federica Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Salvato%2C+M">Mara Salvato</a>, <a href="/search/astro-ph?searchtype=author&query=Schawinski%2C+K">Kevin Schawinski</a>, <a href="/search/astro-ph?searchtype=author&query=Shimizu%2C+T">Taro Shimizu</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="2207.12428v1-abstract-short" style="display: inline;"> The BAT AGN Spectroscopic Survey (BASS) is designed to provide a highly complete census of the key physical parameters of supermassive black holes (SMBHs) that power local active galactic nuclei (AGN) (z<0.3), including their bolometric luminosity, black hole mass, accretion rates, and line-of-sight gas obscuration, and the distinctive properties of their host galaxies (e.g., star formation rates,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.12428v1-abstract-full').style.display = 'inline'; document.getElementById('2207.12428v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.12428v1-abstract-full" style="display: none;"> The BAT AGN Spectroscopic Survey (BASS) is designed to provide a highly complete census of the key physical parameters of supermassive black holes (SMBHs) that power local active galactic nuclei (AGN) (z<0.3), including their bolometric luminosity, black hole mass, accretion rates, and line-of-sight gas obscuration, and the distinctive properties of their host galaxies (e.g., star formation rates, masses, and gas fractions). We present an overview of the BASS data release 2 (DR2), an unprecedented spectroscopic survey in spectral range, resolution, and sensitivity, including 1449 optical (3200-10000 A) and 233 NIR (1-2.5 um) spectra for the brightest 858 ultra-hard X-ray (14-195 keV) selected AGN across the entire sky and essentially all levels of obscuration. This release provides a highly complete set of key measurements (emission line measurements and central velocity dispersions), with 99.9% measured redshifts and 98% black hole masses estimated (for unbeamed AGN outside the Galactic plane). The BASS DR2 AGN sample represents a unique census of nearby powerful AGN, spanning over 5 orders of magnitude in AGN bolometric luminosity, black hole mass, Eddington ratio, and obscuration. The public BASS DR2 sample and measurements can thus be used to answer fundamental questions about SMBH growth and its links to host galaxy evolution and feedback in the local universe, as well as open questions concerning SMBH physics. Here we provide a brief overview of the survey strategy, the key BASS DR2 measurements, data sets and catalogs, and scientific highlights from a series of DR2-based works. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.12428v1-abstract-full').style.display = 'none'; document.getElementById('2207.12428v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 6 figures, 5 tables, published in ApJS as part of BASS DR2 special issue</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJS, 261, 1 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.05321">arXiv:2204.05321</a> <span> [<a href="https://arxiv.org/pdf/2204.05321">pdf</a>, <a href="https://arxiv.org/format/2204.05321">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/ac6602">10.3847/1538-4365/ac6602 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BASS XXV: DR2 Broad-line Based Black Hole Mass Estimates and Biases from Obscuration </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mej%C4%B1a-Restrepo%2C+J+E">Julian E. Mej谋a-Restrepo</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">Benny Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M+J">Michael J. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">Kyuseok Oh</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=Stern%2C+D">Daniel Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M+C">Meredith C. Powell</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">Federica Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Caglar%2C+T">Turgay Caglar</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Treister%2C+E">Ezequiel Treister</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F+A">Fiona A. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Urry%2C+C+M">C. M. Urry</a>, <a href="/search/astro-ph?searchtype=author&query=Ananna%2C+T+T">Tonima Tasnim Ananna</a>, <a href="/search/astro-ph?searchtype=author&query=Asmus%2C+D">Daniel Asmus</a>, <a href="/search/astro-ph?searchtype=author&query=Assef%2C+R+J">Roberto J. Assef</a>, <a href="/search/astro-ph?searchtype=author&query=Bar%2C+R+E">Rudolf E. Bar</a>, <a href="/search/astro-ph?searchtype=author&query=Bessiere%2C+P+S">Patricia S. Bessiere</a>, <a href="/search/astro-ph?searchtype=author&query=Burtscher%2C+L">Leonard Burtscher</a>, <a href="/search/astro-ph?searchtype=author&query=Ichikawa%2C+K">Kohei Ichikawa</a>, <a href="/search/astro-ph?searchtype=author&query=Kakkad%2C+D">Darshan Kakkad</a>, <a href="/search/astro-ph?searchtype=author&query=Kamraj%2C+N">Nikita Kamraj</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotzky%2C+R">Richard Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a> , et al. (4 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2204.05321v2-abstract-short" style="display: inline;"> We present measurements of broad emission lines and virial estimates of supermassive black hole masses ($M_{BH}$) for a large sample of ultra-hard X-ray selected active galactic nuclei (AGNs) as part of the second data release of the BAT AGN Spectroscopic Survey (BASS/DR2). Our catalog includes $M_{BH}$ estimates for a total 689 AGNs, determined from the H$伪$, H$尾$, $MgII\lambda2798$, and/or… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.05321v2-abstract-full').style.display = 'inline'; document.getElementById('2204.05321v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.05321v2-abstract-full" style="display: none;"> We present measurements of broad emission lines and virial estimates of supermassive black hole masses ($M_{BH}$) for a large sample of ultra-hard X-ray selected active galactic nuclei (AGNs) as part of the second data release of the BAT AGN Spectroscopic Survey (BASS/DR2). Our catalog includes $M_{BH}$ estimates for a total 689 AGNs, determined from the H$伪$, H$尾$, $MgII\lambda2798$, and/or $CIV\lambda1549$ broad emission lines. The core sample includes a total of 512 AGNs drawn from the 70-month Swift/BAT all-sky catalog. We also provide measurements for 177 additional AGNs that are drawn from deeper Swift/BAT survey data. We study the links between $M_{BH}$ estimates and line-of-sight obscuration measured from X-ray spectral analysis. We find that broad H$伪$ emission lines in obscured AGNs ($\log (N_{\rm H}/{\rm cm}^{-2})> 22.0$) are on average a factor of $8.0_{-2.4}^{+4.1}$ weaker, relative to ultra-hard X-ray emission, and about $35_{-12}^{~+7}$\% narrower than in unobscured sources (i.e., $\log (N_{\rm H}/{\rm cm}^{-2}) < 21.5$). This indicates that the innermost part of the broad-line region is preferentially absorbed. Consequently, current single-epoch $M_{BH}$ prescriptions result in severely underestimated ($>$1 dex) masses for Type 1.9 sources (AGNs with broad H$伪$ but no broad H$尾$) and/or sources with $\log (N_{\rm H}/{\rm cm}^{-2}) > 22.0$. We provide simple multiplicative corrections for the observed luminosity and width of the broad H$伪$ component ($L[{\rm b}{\rm H}伪]$ and FWHM[bH$伪$]) in such sources to account for this effect, and to (partially) remedy $M_{BH}$ estimates for Type 1.9 objects. As key ingredient of BASS/DR2, our work provides the community with the data needed to further study powerful AGNs in the low-redshift Universe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.05321v2-abstract-full').style.display = 'none'; document.getElementById('2204.05321v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">published 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/2202.09739">arXiv:2202.09739</a> <span> [<a href="https://arxiv.org/pdf/2202.09739">pdf</a>, <a href="https://arxiv.org/format/2202.09739">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/ac7ff0">10.3847/2041-8213/ac7ff0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Radio Constraints on $r$-process Nucleosynthesis by Collapsars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lee%2C+K+H">K. H. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Bartos%2C+I">I. Bartos</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+A">A. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Corsi%2C+A">A. Corsi</a>, <a href="/search/astro-ph?searchtype=author&query=Marka%2C+Z">Z. Marka</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">G. C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Marka%2C+S">S. Marka</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2202.09739v1-abstract-short" style="display: inline;"> The heaviest elements in the Universe are synthesized through rapid neutron capture ($r$-process) in extremely neutron rich outflows. Neutron star mergers were established as an important $r$-process source through the multi-messenger observation of GW170817. Collapsars were also proposed as a potentially major source of heavy elements; however, this is difficult to probe through optical observati… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.09739v1-abstract-full').style.display = 'inline'; document.getElementById('2202.09739v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.09739v1-abstract-full" style="display: none;"> The heaviest elements in the Universe are synthesized through rapid neutron capture ($r$-process) in extremely neutron rich outflows. Neutron star mergers were established as an important $r$-process source through the multi-messenger observation of GW170817. Collapsars were also proposed as a potentially major source of heavy elements; however, this is difficult to probe through optical observations due to contamination by other emission mechanisms. Here we present observational constraints on $r$-process nucleosynthesis by collapsars based on radio follow-up observations of nearby long gamma-ray bursts. We make the hypothesis that late-time radio emission arises from the collapsar wind ejecta responsible for forging $r$-process elements, and consider the constraints that can be set on this scenario using radio observations of a sample of Swift/BAT GRBs located within 2 Gpc. No radio counterpart was identified in excess of the radio afterglow of the GRBs in our sample, limiting the collapsar $r$-process contribution to $\lesssim0.2$ M$_\odot$ under the models we considered, with constant circum-merger densities giving more stringent constraints. While our results are in tension with collapsars being the majority $r$-process production sites, the ejecta mass and velocity profile of collapsar winds is not yet well modeled. As such, our results are currently subject to large uncertainties, but further theoretical work could greatly improve them. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.09739v1-abstract-full').style.display = 'none'; document.getElementById('2202.09739v1-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 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, 1 figure</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.04149">arXiv:2201.04149</a> <span> [<a href="https://arxiv.org/pdf/2201.04149">pdf</a>, <a href="https://arxiv.org/format/2201.04149">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="High Energy Astrophysical Phenomena">astro-ph.HE</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/stac103">10.1093/mnras/stac103 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BASS XXXI: Outflow scaling relations in low redshift X-ray AGN host galaxies with MUSE </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kakkad%2C+D">D. Kakkad</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas%2C+A+F">A. F. Rojas</a>, <a href="/search/astro-ph?searchtype=author&query=Mallmann%2C+N+D">Nicolas D. Mallmann</a>, <a href="/search/astro-ph?searchtype=author&query=Veilleux%2C+S">S. Veilleux</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">F. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotsky%2C+R">R. Mushotsky</a>, <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M">M. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">C. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Treister%2C+E">E. Treister</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Nguyen%2C+N">N. Nguyen</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%A4r%2C+R">R. B盲r</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">F. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">K. Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M">M. Powell</a>, <a href="/search/astro-ph?searchtype=author&query=Riffel%2C+R">R. Riffel</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">B. Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Urry%2C+C+M">C. M. Urry</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2201.04149v1-abstract-short" style="display: inline;"> Ionised gas kinematics provide crucial evidence of the impact that active galactic nuclei (AGN) have in regulating star formation in their host galaxies. Although the presence of outflows in AGN host galaxies has been firmly established, the calculation of outflow properties such as mass outflow rates and kinetic energy remains challenging. We present the [OIII]5007 ionised gas outflow properties… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.04149v1-abstract-full').style.display = 'inline'; document.getElementById('2201.04149v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.04149v1-abstract-full" style="display: none;"> Ionised gas kinematics provide crucial evidence of the impact that active galactic nuclei (AGN) have in regulating star formation in their host galaxies. Although the presence of outflows in AGN host galaxies has been firmly established, the calculation of outflow properties such as mass outflow rates and kinetic energy remains challenging. We present the [OIII]5007 ionised gas outflow properties of 22 z$<$0.1 X-ray AGN, derived from the BAT AGN Spectroscopic Survey using MUSE/VLT. With an average spatial resolution of 1" (0.1-1.2 kpc), the observations resolve the ionised gas clouds down to sub-kiloparsec scales. Resolved maps show that the [OIII] velocity dispersion is, on average, higher in regions ionised by the AGN, compared to star formation. We calculate the instantaneous outflow rates in individual MUSE spaxels by constructing resolved mass outflow rate maps, incorporating variable outflow density and velocity. We compare the instantaneous values with time-averaged outflow rates by placing mock fibres and slits on the MUSE field-of-view, a method often used in the literature. The instantaneous outflow rates (0.2-275 $M_{\odot}$ yr$^{-1}$) tend to be 2 orders of magnitude higher than the time-averaged outflow rates (0.001-40 $M_{\odot}$ yr$^{-1}$). The outflow rates correlate with the AGN bolometric luminosity ($L_{\rm bol}\sim$ 10$^{42.71}$-10$^{45.62}$ erg/s) but we find no correlations with black hole mass (10$^{6.1}$-10$^{8.9}$ M$_{\odot}$), Eddington ratio (0.002-1.1) and radio luminosity (10$^{21}$-10$^{26}$ W/Hz). We find the median coupling between the kinetic energy and $L_{\rm bol}$ to be 1%, consistent with the theoretical predictions for an AGN-driven outflow. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.04149v1-abstract-full').style.display = 'none'; document.getElementById('2201.04149v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Main paper: 20 pages, 15 figures, 3 tables. 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/2201.03564">arXiv:2201.03564</a> <span> [<a href="https://arxiv.org/pdf/2201.03564">pdf</a>, <a href="https://arxiv.org/format/2201.03564">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac43b8">10.3847/1538-4357/ac43b8 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The BPT Diagram in Cosmological Galaxy Formation Simulations: Understanding the Physics Driving Offsets at High-Redshift </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Garg%2C+P">Prerak Garg</a>, <a href="/search/astro-ph?searchtype=author&query=Narayanan%2C+D">Desika Narayanan</a>, <a href="/search/astro-ph?searchtype=author&query=Byler%2C+N">Nell Byler</a>, <a href="/search/astro-ph?searchtype=author&query=Sanders%2C+R+L">Ryan L. Sanders</a>, <a href="/search/astro-ph?searchtype=author&query=Shapley%2C+A+E">Alice E. Shapley</a>, <a href="/search/astro-ph?searchtype=author&query=Strom%2C+A+L">Allison L. Strom</a>, <a href="/search/astro-ph?searchtype=author&query=Dav%C3%A9%2C+R">Romeel Dav茅</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">Michaela Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Lovell%2C+C+C">Christopher C. Lovell</a>, <a href="/search/astro-ph?searchtype=author&query=Otter%2C+J">Justin Otter</a>, <a href="/search/astro-ph?searchtype=author&query=Popping%2C+G">Gerg枚 Popping</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2201.03564v1-abstract-short" style="display: inline;"> The Baldwin, Philips, & Terlevich diagram of [O III]/H$尾$ vs. [N II]/H$伪$ (hereafter N2-BPT) has long been used as a tool for classifying galaxies based on the dominant source of ionizing radiation. Recent observations have demonstrated that galaxies at $z\sim2$ reside offset from local galaxies in the N2-BPT space. In this paper, we conduct a series of controlled numerical experiments to understa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.03564v1-abstract-full').style.display = 'inline'; document.getElementById('2201.03564v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.03564v1-abstract-full" style="display: none;"> The Baldwin, Philips, & Terlevich diagram of [O III]/H$尾$ vs. [N II]/H$伪$ (hereafter N2-BPT) has long been used as a tool for classifying galaxies based on the dominant source of ionizing radiation. Recent observations have demonstrated that galaxies at $z\sim2$ reside offset from local galaxies in the N2-BPT space. In this paper, we conduct a series of controlled numerical experiments to understand the potential physical processes driving this offset. We model nebular line emission in a large sample of galaxies, taken from the SIMBA cosmological hydrodynamic galaxy formation simulation, using the CLOUDY photoionization code to compute the nebular line luminosities from H II regions. We find that the observed shift toward higher [O III]/H$尾$ and [N II]/H$伪$ values at high redshift arises from sample selection: when we consider only the most massive galaxies $M_* \sim 10^{10-11} M_\odot$, the offset naturally appears, due to their high metallicities. We predict that deeper observations that probe lower-mass galaxies will reveal galaxies that lie on a locus comparable to $z\sim 0$ observations. Even when accounting for sample selection effects, we find that there is a subtle mismatch between simulations and observations. To resolve this discrepancy, we investigate the impact of varying ionization parameters, H II region densities, gas-phase abundance patterns, and increasing radiation field hardness on N2-BPT diagrams. We find that either decreasing the ionization parameter or increasing the N/O ratio of galaxies at fixed O/H can move galaxies along a self-similar arc in N2-BPT space that is occupied by high-redshift galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.03564v1-abstract-full').style.display = 'none'; document.getElementById('2201.03564v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 15 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/2111.05349">arXiv:2111.05349</a> <span> [<a href="https://arxiv.org/pdf/2111.05349">pdf</a>, <a href="https://arxiv.org/format/2111.05349">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/ac399f">10.3847/2041-8213/ac399f <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> High Molecular-Gas to Dust Mass Ratios Predicted in Most Quiescent Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Whitaker%2C+K+E">Katherine E. Whitaker</a>, <a href="/search/astro-ph?searchtype=author&query=Narayanan%2C+D">Desika Narayanan</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+C+C">Christina C. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Q">Qi Li</a>, <a href="/search/astro-ph?searchtype=author&query=Spilker%2C+J+S">Justin S. Spilker</a>, <a href="/search/astro-ph?searchtype=author&query=Dav%C3%A9%2C+R">Romeel Dav茅</a>, <a href="/search/astro-ph?searchtype=author&query=Akhshik%2C+M">Mohammad Akhshik</a>, <a href="/search/astro-ph?searchtype=author&query=Akins%2C+H+B">Hollis B. Akins</a>, <a href="/search/astro-ph?searchtype=author&query=Bezanson%2C+R">Rachel Bezanson</a>, <a href="/search/astro-ph?searchtype=author&query=Katz%2C+N">Neal Katz</a>, <a href="/search/astro-ph?searchtype=author&query=Leja%2C+J">Joel Leja</a>, <a href="/search/astro-ph?searchtype=author&query=Magdis%2C+G+E">Georgios E. Magdis</a>, <a href="/search/astro-ph?searchtype=author&query=Mowla%2C+L">Lamiya Mowla</a>, <a href="/search/astro-ph?searchtype=author&query=Nelson%2C+E+J">Erica J. Nelson</a>, <a href="/search/astro-ph?searchtype=author&query=Pope%2C+A">Alexandra Pope</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Toft%2C+S">Sune Toft</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">Francesco Valentino</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2111.05349v2-abstract-short" style="display: inline;"> Observations of cold molecular gas reservoirs are critical for understanding the shutdown of star formation in massive galaxies. While dust continuum is an efficient and affordable tracer, this method relies upon the assumption of a "normal" molecular-gas to dust mass ratio, $未_{\mathrm{GDR}}$, typically of order one hundred. Recent null detections of quiescent galaxies in deep dust continuum obse… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.05349v2-abstract-full').style.display = 'inline'; document.getElementById('2111.05349v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.05349v2-abstract-full" style="display: none;"> Observations of cold molecular gas reservoirs are critical for understanding the shutdown of star formation in massive galaxies. While dust continuum is an efficient and affordable tracer, this method relies upon the assumption of a "normal" molecular-gas to dust mass ratio, $未_{\mathrm{GDR}}$, typically of order one hundred. Recent null detections of quiescent galaxies in deep dust continuum observations support a picture where the cold gas and dust has been rapidly depleted or expelled. In this work, we present another viable explanation: a significant fraction of galaxies with low star formation per unit stellar mass are predicted to have extreme $未_{\mathrm{GDR}}$ ratios. We show that simulated massive quiescent galaxies at $0 < z < 3$ in the \textsc{simba} cosmological simulations have $未_{\mathrm{GDR}}$ values that extend $>$4 orders of magnitude. The dust in most simulated quiescent galaxies is destroyed significantly more rapidly than the molecular gas depletes, and cannot be replenished. The transition from star-forming to quiescent halts dust formation via star formation processes, with dust subsequently destroyed by supernova shocks and thermal sputtering of dust grains embedded in hot plasma. After this point, the dust growth rate in the models is not sufficient to overcome the loss of $>$3 orders of magnitude in dust mass to return to normal values of $未_{\mathrm{GDR}}$ despite having high metallicity. Our results indicate that it is not straight forward to use a single observational indicator to robustly pre-select exotic versus normal ratios. These simulations make strong predictions that can be tested with millimeter facilities. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.05349v2-abstract-full').style.display = 'none'; document.getElementById('2111.05349v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 5 figures, version accepted for publication in the Astrophysical Journal Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.01025">arXiv:2111.01025</a> <span> [<a href="https://arxiv.org/pdf/2111.01025">pdf</a>, <a href="https://arxiv.org/format/2111.01025">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac2ebb">10.3847/1538-4357/ac2ebb <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Tracing the Ionization Structure of the Shocked Filaments of NGC 6240 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Medling%2C+A+M">Anne M. Medling</a>, <a href="/search/astro-ph?searchtype=author&query=Kewley%2C+L+J">Lisa J. Kewley</a>, <a href="/search/astro-ph?searchtype=author&query=Calzetti%2C+D">Daniela Calzetti</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Larson%2C+K">Kirsten Larson</a>, <a href="/search/astro-ph?searchtype=author&query=Rich%2C+J+A">Jeffrey A. Rich</a>, <a href="/search/astro-ph?searchtype=author&query=Armus%2C+L">Lee Armus</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+M+G">Mark G. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Bicknell%2C+G+V">Geoffrey V. Bicknell</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%ADaz-Santos%2C+T">Tanio D铆az-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Heckman%2C+T+M">Timothy M. Heckman</a>, <a href="/search/astro-ph?searchtype=author&query=Leitherer%2C+C">Claus Leitherer</a>, <a href="/search/astro-ph?searchtype=author&query=Max%2C+C+E">Claire E. Max</a>, <a href="/search/astro-ph?searchtype=author&query=Rupke%2C+D+S+N">David S. N. Rupke</a>, <a href="/search/astro-ph?searchtype=author&query=Treister%2C+E">Ezequiel Treister</a>, <a href="/search/astro-ph?searchtype=author&query=Messias%2C+H">Hugo Messias</a>, <a href="/search/astro-ph?searchtype=author&query=Wagner%2C+A+Y">Alexander Y. Wagner</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2111.01025v1-abstract-short" style="display: inline;"> We study the ionization and excitation structure of the interstellar medium in the late-stage gas-rich galaxy merger NGC 6240 using a suite of emission line maps at $\sim$25 pc resolution from the Hubble Space Telescope, Keck NIRC2 with Adaptive Optics, and ALMA. NGC 6240 hosts a superwind driven by intense star formation and/or one or both of two active nuclei; the outflows produce bubbles and fi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.01025v1-abstract-full').style.display = 'inline'; document.getElementById('2111.01025v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.01025v1-abstract-full" style="display: none;"> We study the ionization and excitation structure of the interstellar medium in the late-stage gas-rich galaxy merger NGC 6240 using a suite of emission line maps at $\sim$25 pc resolution from the Hubble Space Telescope, Keck NIRC2 with Adaptive Optics, and ALMA. NGC 6240 hosts a superwind driven by intense star formation and/or one or both of two active nuclei; the outflows produce bubbles and filaments seen in shock tracers from warm molecular gas (H$_2$ 2.12$渭$m) to optical ionized gas ([O III], [N II], [S II], [O I]) and hot plasma (Fe XXV). In the most distinct bubble, we see a clear shock front traced by high [O III]/H$尾$ and [O III]/[O I]. Cool molecular gas (CO(2-1)) is only present near the base of the bubble, towards the nuclei launching the outflow. We interpret the lack of molecular gas outside the bubble to mean that the shock front is not responsible for dissociating molecular gas, and conclude that the molecular clouds are partly shielded and either entrained briefly in the outflow, or left undisturbed while the hot wind flows around them. Elsewhere in the galaxy, shock-excited H$_2$ extends at least $\sim$4 kpc from the nuclei, tracing molecular gas even warmer than that between the nuclei, where the two galaxies' interstellar media are colliding. A ridgeline of high [O III]/H$尾$ emission along the eastern arm aligns with the south nucleus' stellar disk minor axis; optical integral field spectroscopy from WiFeS suggests this highly ionized gas is centered at systemic velocity and likely photoionized by direct line-of-sight to the south AGN. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.01025v1-abstract-full').style.display = 'none'; document.getElementById('2111.01025v1-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 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">27 pages, 18 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/2110.03638">arXiv:2110.03638</a> <span> [<a href="https://arxiv.org/pdf/2110.03638">pdf</a>, <a href="https://arxiv.org/format/2110.03638">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac2892">10.3847/1538-4357/ac2892 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Massive Star Cluster Formation and Destruction in Luminous Infrared Galaxies in GOALS II: An ACS/WFC3 Survey of Nearby LIRGs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Linden%2C+S">Sean Linden</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+A">Aaron Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Larson%2C+K">Kirsten Larson</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G">George Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Armus%2C+L">Lee Armus</a>, <a href="/search/astro-ph?searchtype=author&query=Rich%2C+J">Jeff Rich</a>, <a href="/search/astro-ph?searchtype=author&query=Diaz-Santos%2C+T">Tanio Diaz-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Murphy%2C+E">Eric Murphy</a>, <a href="/search/astro-ph?searchtype=author&query=Song%2C+Y">Yiqing Song</a>, <a href="/search/astro-ph?searchtype=author&query=Barcos-Munoz%2C+L">Loreto Barcos-Munoz</a>, <a href="/search/astro-ph?searchtype=author&query=Howell%2C+J">Justin Howell</a>, <a href="/search/astro-ph?searchtype=author&query=Charmandaris%2C+V">Vassilis Charmandaris</a>, <a href="/search/astro-ph?searchtype=author&query=Inami%2C+H">Hanae Inami</a>, <a href="/search/astro-ph?searchtype=author&query=U%2C+V">Vivian U</a>, <a href="/search/astro-ph?searchtype=author&query=Surace%2C+J">Jason Surace</a>, <a href="/search/astro-ph?searchtype=author&query=Mazzarella%2C+J">Joseph Mazzarella</a>, <a href="/search/astro-ph?searchtype=author&query=Calzetti%2C+D">Daniela Calzetti</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2110.03638v1-abstract-short" style="display: inline;"> We present the results of a Hubble Space Telescope WFC3 near-UV and ACS/WFC optical study into the star cluster populations of 10 luminous and ultra-luminous infrared galaxies (U/LIRGs) in the Great Observatories All-Sky LIRG Survey (GOALS). Through integrated broadband photometry we have derived ages, masses, and extinctions for a total of 1027 star clusters in galaxies with $d_{L} <$ 110 Mpc in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.03638v1-abstract-full').style.display = 'inline'; document.getElementById('2110.03638v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.03638v1-abstract-full" style="display: none;"> We present the results of a Hubble Space Telescope WFC3 near-UV and ACS/WFC optical study into the star cluster populations of 10 luminous and ultra-luminous infrared galaxies (U/LIRGs) in the Great Observatories All-Sky LIRG Survey (GOALS). Through integrated broadband photometry we have derived ages, masses, and extinctions for a total of 1027 star clusters in galaxies with $d_{L} <$ 110 Mpc in order to avoid issues related to cluster blending. The measured cluster age distribution slope of $dN/d蟿\propto 蟿^{-0.5 +/- 0.2}$ is steeper than what has been observed in lower-luminosity star-forming galaxies. Further, differences in the slope of the observed cluster age distribution between inner- ($dN/d蟿\propto 蟿^{-1.07 +/- 0.12}$) and outer-disk ($dN/d蟿\propto 蟿^{-0.37 +/- 0.09}$) star clusters provides evidence of mass-dependent cluster destruction in the central regions of LIRGs driven primarily by the combined effect of strong tidal shocks and encounters with massive GMCs. Excluding the nuclear ring surrounding the Seyfert 1 nucleus in NGC 7469, the derived cluster mass function (CMF: $dN/dM \propto M^伪$) has marginal evidence for a truncation in the power-law (PL) at $M_{t} \sim 2$x$10^{6} M_{\odot}$ for our three most cluster-rich galaxies, which are all classified as early-stage mergers. Finally, we find evidence of a flattening of the CMF slope of $dN/dM \propto M^{-1.42 \pm 0.1}$ for clusters in late-stage mergers relative to early-stage ($伪= -1.65 \pm 0.02$), which we attribute to an increase in the formation of massive clusters over the course of the interaction. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.03638v1-abstract-full').style.display = 'none'; document.getElementById('2110.03638v1-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">70 pages, 21 figures, 5 tables, accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.03231">arXiv:2108.03231</a> <span> [<a href="https://arxiv.org/pdf/2108.03231">pdf</a>, <a href="https://arxiv.org/format/2108.03231">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac5d5f">10.3847/1538-4357/ac5d5f <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> After The Fall: Resolving the Molecular Gas in Post-Starburst Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Smercina%2C+A">Adam Smercina</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+J+T">John-David T. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=French%2C+K+D">K. Decker French</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">Daniel A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Medling%2C+A+M">Anne M. Medling</a>, <a href="/search/astro-ph?searchtype=author&query=Nyland%2C+K">Kristina Nyland</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Rowlands%2C+K">Kate Rowlands</a>, <a href="/search/astro-ph?searchtype=author&query=Walter%2C+F">Fabian Walter</a>, <a href="/search/astro-ph?searchtype=author&query=Zabludoff%2C+A+I">Ann I. Zabludoff</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="2108.03231v2-abstract-short" style="display: inline;"> Post-starburst (PSB), or 'E+A', galaxies represent a rapid transitional phase between major, gas-rich mergers and gas-poor, quiescent early-type galaxies. Surprisingly, many PSBs have been shown to host a significant interstellar medium (ISM), despite theoretical predictions that the majority of star-forming gas should be expelled in AGN- or starburst-driven outflows. To-date, the resolved propert… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.03231v2-abstract-full').style.display = 'inline'; document.getElementById('2108.03231v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.03231v2-abstract-full" style="display: none;"> Post-starburst (PSB), or 'E+A', galaxies represent a rapid transitional phase between major, gas-rich mergers and gas-poor, quiescent early-type galaxies. Surprisingly, many PSBs have been shown to host a significant interstellar medium (ISM), despite theoretical predictions that the majority of star-forming gas should be expelled in AGN- or starburst-driven outflows. To-date, the resolved properties of this surviving ISM have remained unknown. We present high resolution ALMA continuum and CO(2$-$1) observations in six gas- and dust-rich PSBs, revealing for the first time the spatial and kinematic structure of their ISM on sub-kpc scales. We find extremely compact molecular reservoirs, with dust and gas surface densities rivaling those found in (ultra-)luminous infrared galaxies. We observe spatial and kinematic disturbances in all sources, with some also displaying disk-like kinematics. Estimates of the internal turbulent pressure in the gas exceed those of normal star-forming disks by at least 2 orders of magnitude, and rival the turbulent gas found in local interacting galaxies, such as the Antennae. Though the source of this high turbulent pressure remains uncertain, we suggest that the high incidence of tidal disruption events (TDEs) in PSBs could play a role. The star formation in these PSBs' turbulent central molecular reservoirs is suppressed, forming stars only 10% as efficiently as starburst galaxies with similar gas surface densities. "The fall" of star formation in these galaxies was not precipitated by complete gas expulsion or redistribution. Rather, this high-resolution view of PSBs' ISM indicates that star formation in their remaining compact gas reservoirs is suppressed by significant turbulent heating. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.03231v2-abstract-full').style.display = 'none'; document.getElementById('2108.03231v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 9 figures, 3 tables; Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.10864">arXiv:2107.10864</a> <span> [<a href="https://arxiv.org/pdf/2107.10864">pdf</a>, <a href="https://arxiv.org/ps/2107.10864">ps</a>, <a href="https://arxiv.org/format/2107.10864">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="High Energy Astrophysical Phenomena">astro-ph.HE</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/stab2052">10.1093/mnras/stab2052 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A hard X-ray view of Luminous and Ultra-luminous Infrared Galaxies in GOALS: I - AGN obscuration along the merger sequence </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">C. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">G. C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Pfeifle%2C+R+W">R. W. Pfeifle</a>, <a href="/search/astro-ph?searchtype=author&query=Armus%2C+L">L. Armus</a>, <a href="/search/astro-ph?searchtype=author&query=Iwasawa%2C+K">K. Iwasawa</a>, <a href="/search/astro-ph?searchtype=author&query=Torres-Alba%2C+N">N. Torres-Alba</a>, <a href="/search/astro-ph?searchtype=author&query=Satyapal%2C+S">S. Satyapal</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">F. E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Treister%2C+E">E. Treister</a>, <a href="/search/astro-ph?searchtype=author&query=Ho%2C+L+C">L. C. Ho</a>, <a href="/search/astro-ph?searchtype=author&query=Aalto%2C+S">S. Aalto</a>, <a href="/search/astro-ph?searchtype=author&query=Arevalo%2C+P">P. Arevalo</a>, <a href="/search/astro-ph?searchtype=author&query=Barcos-Munoz%2C+L">L. Barcos-Munoz</a>, <a href="/search/astro-ph?searchtype=author&query=Charmandaris%2C+V">V. Charmandaris</a>, <a href="/search/astro-ph?searchtype=author&query=Diaz-Santos%2C+T">T. Diaz-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+A+S">A. S. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+T">T. Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Inami%2C+H">H. Inami</a>, <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M+J">M. J. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Lansbury%2C+G">G. Lansbury</a>, <a href="/search/astro-ph?searchtype=author&query=Linden%2C+S+T">S. T. Linden</a>, <a href="/search/astro-ph?searchtype=author&query=Medling%2C+A">A. Medling</a>, <a href="/search/astro-ph?searchtype=author&query=Sanders%2C+D+B">D. B. Sanders</a>, <a href="/search/astro-ph?searchtype=author&query=Song%2C+Y">Y. Song</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">D. Stern</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="2107.10864v2-abstract-short" style="display: inline;"> The merger of two or more galaxies can enhance the inflow of material from galactic scales into the close environments of Active Galactic Nuclei (AGN), obscuring and feeding the supermassive black hole (SMBH). Both recent simulations and observations of AGN in mergers have confirmed that mergers are related to strong nuclear obscuration. However, it is still unclear how AGN obscuration evolves in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.10864v2-abstract-full').style.display = 'inline'; document.getElementById('2107.10864v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.10864v2-abstract-full" style="display: none;"> The merger of two or more galaxies can enhance the inflow of material from galactic scales into the close environments of Active Galactic Nuclei (AGN), obscuring and feeding the supermassive black hole (SMBH). Both recent simulations and observations of AGN in mergers have confirmed that mergers are related to strong nuclear obscuration. However, it is still unclear how AGN obscuration evolves in the last phases of the merger process. We study a sample of 60 Luminous and Ultra-luminous IR galaxies (U/LIRGs) from the GOALS sample observed by NuSTAR. We find that the fraction of AGN that are Compton-thick (CT; $N_{\rm H}\geq 10^{24}\rm\,cm^{-2}$) peaks at $74_{-19}^{+14}\%$ at a late merger stage, prior to coalescence, when the nuclei have projected separations of $d_{\rm sep}\sim 0.4-6$ kpc. A similar peak is also observed in the median $N_{\rm H}$ [$(1.6\pm0.5)\times10^{24}\rm\,cm^{-2}$]. The vast majority ($85^{+7}_{-9}\%$) of the AGN in the final merger stages ($d_{\rm sep}\lesssim 10$ kpc) are heavily obscured ($N_{\rm H}\geq 10^{23}\rm\,cm^{-2}$), and the median $N_{\rm H}$ of the accreting SMBHs in our sample is systematically higher than that of local hard X-ray selected AGN, regardless of the merger stage. This implies that these objects have very obscured nuclear environments, with the $N_{\rm H}\geq 10^{23}\rm\,cm^{-2}$ gas almost completely covering the AGN in late mergers. CT AGN tend to have systematically higher absorption-corrected X-ray luminosities than less obscured sources. This could either be due to an evolutionary effect, with more obscured sources accreting more rapidly because they have more gas available in their surroundings, or to a selection bias. The latter scenario would imply that we are still missing a large fraction of heavily obscured, lower luminosity ($L_{2-10}\lesssim 10^{43}\rm\,erg\,s^{-1}$) AGN in U/LIRGs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.10864v2-abstract-full').style.display = 'none'; document.getElementById('2107.10864v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2021. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.10855">arXiv:2107.10855</a> <span> [<a href="https://arxiv.org/pdf/2107.10855">pdf</a>, <a href="https://arxiv.org/format/2107.10855">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/ac17f5">10.3847/1538-4365/ac17f5 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Comprehensive Broadband X-ray and Multiwavelength Study of Active Galactic Nuclei in Local 57 Ultra/luminous Infrared Galaxies Observed with NuSTAR and/or Swift/BAT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yamada%2C+S">Satoshi Yamada</a>, <a href="/search/astro-ph?searchtype=author&query=Ueda%2C+Y">Yoshihiro Ueda</a>, <a href="/search/astro-ph?searchtype=author&query=Tanimoto%2C+A">Atsushi Tanimoto</a>, <a href="/search/astro-ph?searchtype=author&query=Imanishi%2C+M">Masatoshi Imanishi</a>, <a href="/search/astro-ph?searchtype=author&query=Toba%2C+Y">Yoshiki Toba</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2107.10855v1-abstract-short" style="display: inline;"> We perform a systematic X-ray spectroscopic analysis of 57 local ultra/luminous infrared galaxy systems (containing 84 individual galaxies) observed with Nuclear Spectroscopic Telescope Array and/or Swift/BAT. Combining soft X-ray data obtained with Chandra, XMM-Newton, Suzaku and/or Swift/XRT, we identify 40 hard ($>$10 keV) X-ray detected active galactic nuclei (AGNs) and constrain their torus p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.10855v1-abstract-full').style.display = 'inline'; document.getElementById('2107.10855v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.10855v1-abstract-full" style="display: none;"> We perform a systematic X-ray spectroscopic analysis of 57 local ultra/luminous infrared galaxy systems (containing 84 individual galaxies) observed with Nuclear Spectroscopic Telescope Array and/or Swift/BAT. Combining soft X-ray data obtained with Chandra, XMM-Newton, Suzaku and/or Swift/XRT, we identify 40 hard ($>$10 keV) X-ray detected active galactic nuclei (AGNs) and constrain their torus parameters with the X-ray clumpy torus model XCLUMPY (Tanimoto et al. 2019). Among the AGNs at $z < 0.03$, for which sample biases are minimized, the fraction of Compton-thick ($N_{\rm H} \geq 10^{24}$ cm$^{-2}$) AGNs reaches 64$^{+14}_{-15}$% (6/9 sources) in late mergers, while 24$^{+12}_{-10}$% (3/14 sources) in early mergers, consistent with the tendency reported by Ricci et al. (2017). We find that the bolometric AGN luminosities derived from the infrared data increase, but the X-ray to bolometric luminosity ratios decrease, with merger stage. The X-ray weak AGNs in late mergers ubiquitously show massive outflows at sub-pc to kpc scales. Among them, the most luminous AGNs ($L_{\rm bol,AGN} \sim 10^{46}$ erg s$^{-1}$) have relatively small column densities of $\lesssim$10$^{23}$ cm$^{-2}$ and almost super-Eddington ratios ($位_{\rm Edd} \sim$ 1.0). Their torus covering factors ($C_{\rm T}^{\rm (22)} \sim 0.6$) are larger than those of Swift/BAT selected AGNs with similarly high Eddington ratios. These results suggest a scenario that, in the final stage of mergers, multiphase strong outflows are produced due to chaotic quasi-spherical inflows and the AGN becomes extremely X-ray weak and deeply buried due to obscuration by inflowing and/or outflowing material. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.10855v1-abstract-full').style.display = 'none'; document.getElementById('2107.10855v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">85 pages, 88 figures, accepted 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/2107.08366">arXiv:2107.08366</a> <span> [<a href="https://arxiv.org/pdf/2107.08366">pdf</a>, <a href="https://arxiv.org/format/2107.08366">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </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/10.1088/1748-0221/16/09/C09013">10.1088/1748-0221/16/09/C09013 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for high-energy neutrino emission from hard X-ray AGN with IceCube </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Goswami%2C+S">Sreetama Goswami</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Santander%2C+M">Marcos Santander</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2107.08366v1-abstract-short" style="display: inline;"> The IceCube Neutrino Observatory has detected high-energy astrophysical neutrinos in the TeV-PeV range. These neutrinos have an isotropic distribution on the sky, and therefore, likely originate from extragalactic sources. Active Galactic Nuclei form a class of astronomical objects which are promising neutrino source candidates given their high electromagnetic luminosity and potential ability to a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.08366v1-abstract-full').style.display = 'inline'; document.getElementById('2107.08366v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.08366v1-abstract-full" style="display: none;"> The IceCube Neutrino Observatory has detected high-energy astrophysical neutrinos in the TeV-PeV range. These neutrinos have an isotropic distribution on the sky, and therefore, likely originate from extragalactic sources. Active Galactic Nuclei form a class of astronomical objects which are promising neutrino source candidates given their high electromagnetic luminosity and potential ability to accelerate cosmic rays up to energies greater than 10$^{16}$ eV. Interactions of these cosmic rays within the AGN environment are expected to produce both neutrinos and pionic gamma rays. Some hadronic models of AGN emission suggest that such gamma rays can in turn interact with the dense photon fields of AGN and cascade down to hard X-rays and MeV gamma rays. We present an update on the IceCube stacking analysis searching for high-energy neutrinos from hard X-ray sources sampled from the $\textit{Swift}$-BAT AGN Spectroscopic Survey. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.08366v1-abstract-full').style.display = 'none'; document.getElementById('2107.08366v1-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Presented at the 37th International Cosmic Ray Conference (ICRC 2021). See arXiv:2107.06966 for all IceCube contributions, 11 pages, 5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> PoS-ICRC2021-1142 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.00412">arXiv:2107.00412</a> <span> [<a href="https://arxiv.org/pdf/2107.00412">pdf</a>, <a href="https://arxiv.org/format/2107.00412">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac05c2">10.3847/1538-4357/ac05c2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Comparison between Nuclear Ring Star Formation in LIRGs and Normal Galaxies with the Very Large Array </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Song%2C+Y">Y. Song</a>, <a href="/search/astro-ph?searchtype=author&query=Linden%2C+S+T">S. T. Linden</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+A+S">A. S. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Barcos-Mu%C3%B1oz%2C+L">L. Barcos-Mu帽oz</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">G. C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Yoon%2C+I">I. Yoon</a>, <a href="/search/astro-ph?searchtype=author&query=Murphy%2C+E+J">E. J. Murphy</a>, <a href="/search/astro-ph?searchtype=author&query=Larson%2C+K+L">K. L. Larson</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%ADaz-Santos%2C+T">T. D铆az-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Armus%2C+L">L. Armus</a>, <a href="/search/astro-ph?searchtype=author&query=Mazzarella%2C+J+M">Joseph M. Mazzarella</a>, <a href="/search/astro-ph?searchtype=author&query=Howell%2C+J">J. Howell</a>, <a href="/search/astro-ph?searchtype=author&query=Inami%2C+H">H. Inami</a>, <a href="/search/astro-ph?searchtype=author&query=Torres-Alb%C3%A0%2C+N">N. Torres-Alb脿</a>, <a href="/search/astro-ph?searchtype=author&query=U%2C+V">V. U</a>, <a href="/search/astro-ph?searchtype=author&query=Charmandaris%2C+V">V. Charmandaris</a>, <a href="/search/astro-ph?searchtype=author&query=Momjian%2C+E">E. Momjian</a>, <a href="/search/astro-ph?searchtype=author&query=McKinney%2C+J">J. McKinney</a>, <a href="/search/astro-ph?searchtype=author&query=Kunneriath%2C+D">D. Kunneriath</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2107.00412v1-abstract-short" style="display: inline;"> Nuclear rings are excellent laboratories for studying intense star formation. We present results from a study of nuclear star-forming rings in five nearby normal galaxies from the Star Formation in Radio Survey (SFRS) and four local LIRGs from the Great Observatories All-sky LIRG Survey (GOALS) at sub-kpc resolutions using VLA high-frequency radio continuum observations. We find that nuclear ring… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.00412v1-abstract-full').style.display = 'inline'; document.getElementById('2107.00412v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.00412v1-abstract-full" style="display: none;"> Nuclear rings are excellent laboratories for studying intense star formation. We present results from a study of nuclear star-forming rings in five nearby normal galaxies from the Star Formation in Radio Survey (SFRS) and four local LIRGs from the Great Observatories All-sky LIRG Survey (GOALS) at sub-kpc resolutions using VLA high-frequency radio continuum observations. We find that nuclear ring star formation (NRSF) contributes 49 - 60\% of the total star formation of the LIRGs, compared to 7 - 40\% for the normal galaxies. We characterize a total of 58 individual star-forming regions in these rings, and find that with measured sizes of 10 - 200 pc, NRSF regions in the LIRGs have SFR and $危_\mathrm{SFR}$ up to 1.7 M$_\odot$yr$^{-1}$ and 402 M$_\odot$yr$^{-1}$kpc$^{-2}$, respectively, which are about 10 times higher than NRSF regions in the normal galaxies with similar sizes, and comparable to lensed high-$z$ star-forming regions. At $\sim 100 - 300$ pc scales, we estimate low contributions ($< 50\%$) of thermal free-free emission to total radio continuum emission at 33 GHz in the NRSF regions in the LIRGs, but large variations possibly exist at smaller physical scales. Finally, using archival sub-kpc resolution CO (J=1-0) data of nuclear rings in the normal galaxies and NGC 7469 (LIRG), we find a large scatter in gas depletion times at similar molecular gas surface densities, which tentatively points to a multi-modal star formation relation on sub-kpc scales. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.00412v1-abstract-full').style.display = 'none'; document.getElementById('2107.00412v1-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">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/2106.11588">arXiv:2106.11588</a> <span> [<a href="https://arxiv.org/pdf/2106.11588">pdf</a>, <a href="https://arxiv.org/format/2106.11588">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/stac2008">10.1093/mnras/stac2008 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An Orientation Bias in Observations of Submillimetre Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lovell%2C+C+C">C. C. Lovell</a>, <a href="/search/astro-ph?searchtype=author&query=Geach%2C+J+E">J. E. Geach</a>, <a href="/search/astro-ph?searchtype=author&query=Dav%C3%A9%2C+R">R. Dav茅</a>, <a href="/search/astro-ph?searchtype=author&query=Narayanan%2C+D">D. Narayanan</a>, <a href="/search/astro-ph?searchtype=author&query=Coppin%2C+K+E+K">K. E. K. Coppin</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Q">Q. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Franco%2C+M">M. Franco</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">G. C. Privon</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2106.11588v2-abstract-short" style="display: inline;"> Recent high-resolution interferometric images of submillimetre galaxies (SMGs) reveal fascinatingly complex morphologies. This raises a number of questions: how does the relative orientation of a galaxy affect its observed submillimetre emission, and does this result in an `orientation bias' in the selection and analysis of such galaxies in flux-limited cosmological surveys? We investigated these… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.11588v2-abstract-full').style.display = 'inline'; document.getElementById('2106.11588v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.11588v2-abstract-full" style="display: none;"> Recent high-resolution interferometric images of submillimetre galaxies (SMGs) reveal fascinatingly complex morphologies. This raises a number of questions: how does the relative orientation of a galaxy affect its observed submillimetre emission, and does this result in an `orientation bias' in the selection and analysis of such galaxies in flux-limited cosmological surveys? We investigated these questions using the \textsc{Simba} cosmological simulation paired with the dust radiative transfer code \textsc{Powderday}. We selected eight simulated SMGs ($S_{850}\gtrsim2$ mJy) at $z = 2$, and measured the variance of their `observed' emission over 50 random orientations. Each galaxy exhibits significant scatter in its emission close to the peak of the thermal dust emission, with variation in flux density of up to a factor of 2.7. This results in an appreciable dispersion in the inferred dust temperatures and infrared luminosities ($16^{\mathrm{th}}-84^{\mathrm{th}}$ percentile ranges of 5\,K and 0.1\,dex, respectively) and therefore a fundamental uncertainty in derived parameters such as dust mass and star formation rate ($\sim$30% for the latter using simple calibrations). Using a Monte Carlo simulation we also assessed the impact of orientation on flux-limited surveys, finding a bias in the selection of SMGs towards those with face--on orientations, as well as those at lower redshifts. We predict that the orientation bias will affect flux-limited single-dish surveys, most significantly at THz frequencies, and this bias should be taken into account when placing the results of targeted follow--up studies in a statistical context. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.11588v2-abstract-full').style.display = 'none'; document.getElementById('2106.11588v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 11 figures, accepted to MNRAS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Monthly Notices of the Royal Astronomical Society, Volume 515, Issue 3, pp.3644-3655, 2022 </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Privon%2C+G&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Privon%2C+G&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Privon%2C+G&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Privon%2C+G&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> </ul> </nav> <div class="is-hidden-tablet">  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