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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=Lopez%2C+L+A&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Lopez%2C+L+A&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Lopez%2C+L+A&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> </ul> </nav> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.06934">arXiv:2502.06934</a> <span> [<a href="https://arxiv.org/pdf/2502.06934">pdf</a>, <a href="https://arxiv.org/format/2502.06934">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> <p class="title is-5 mathjax"> Observational Constraints on Cool Gas Clouds in M82's Starburst-Driven Outflow </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+S">Sebastian Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+T+A">Todd A. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A+K">Adam K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Bolatto%2C+A+D">Alberto D. Bolatto</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2502.06934v1-abstract-short" style="display: inline;"> Star formation feedback can drive large-scale, multi-phase galactic outflows. The dynamical and thermodynamical interaction between the hot and cooler phases is a prime focus of both observational and theoretical work. Here, we analyze H$伪$-emitting structures in the extraplanar wind of the nearby starburst M82. We use high-resolution, narrow-band, observations from the Hubble Legacy Archive (Mutc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.06934v1-abstract-full').style.display = 'inline'; document.getElementById('2502.06934v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.06934v1-abstract-full" style="display: none;"> Star formation feedback can drive large-scale, multi-phase galactic outflows. The dynamical and thermodynamical interaction between the hot and cooler phases is a prime focus of both observational and theoretical work. Here, we analyze H$伪$-emitting structures in the extraplanar wind of the nearby starburst M82. We use high-resolution, narrow-band, observations from the Hubble Legacy Archive (Mutchler et al. 2007). Our analysis constrains the morphology, number density, and column density of the structures. We highlight conspicuous arc-like structures that differ significantly from the linear cometary clouds that emerge from galactic wind simulations and discuss their possible origins, such as bow shocks or instabilities driven by cosmic rays. The most prominent structures range in size from $\sim24 -110$ pc. Using the H$伪$ brightness and assumptions about the depth of the emitting structures, we estimate number densities of $\sim1-23$ cm$^{-3}$, which are lower than previous constraints from spectroscopic nebular line studies. The derived column densities, $\sim10^{20}-10^{21}$ cm$^{-2}$, along the path of the outflow are above theoretical thresholds for cool cloud survival in a hot supersonic background, but small enough that the structures could be accelerated by the hot wind momentum. Using diffuse X-ray emission maps from $\textit{Chandra}$, we also find that even on small ($\sim100$ pc) scales, the H$伪$ "leads" the X-rays, a behavior long noted in the literature on kiloparsec scales, and one we observe in the brightness profiles of the structures we analyze. This behavior, along with previous observational studies of ionization in the wind, may signal that shock ionization is responsible for the H$伪$ emission we observe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.06934v1-abstract-full').style.display = 'none'; document.getElementById('2502.06934v1-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 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 9 Figures; submitted to ApJ (10 February 2025)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.14893">arXiv:2501.14893</a> <span> [<a href="https://arxiv.org/pdf/2501.14893">pdf</a>, <a href="https://arxiv.org/format/2501.14893">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> JWST Observations of Starbursts: Relations between PAH features and CO clouds in the starburst galaxy M 82 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Villanueva%2C+V">V. Villanueva</a>, <a href="/search/astro-ph?searchtype=author&query=Bolatto%2C+A+D">A. D. Bolatto</a>, <a href="/search/astro-ph?searchtype=author&query=Herrera-Camus%2C+R">R. Herrera-Camus</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A">A. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Fisher%2C+D+B">D. B. Fisher</a>, <a href="/search/astro-ph?searchtype=author&query=Levy%2C+R+C">R. C. Levy</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=Boogaard%2C+L">L. Boogaard</a>, <a href="/search/astro-ph?searchtype=author&query=Cronin%2C+S+A">S. A. Cronin</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">D. A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Emig%2C+K">K. Emig</a>, <a href="/search/astro-ph?searchtype=author&query=De+Looze%2C+I">I. De Looze</a>, <a href="/search/astro-ph?searchtype=author&query=Donnelly%2C+G+P">G. P. Donnelly</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=Lenkic%2C+L">L. Lenkic</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">L. A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+S">S. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Meier%2C+D+S">D. S. Meier</a>, <a href="/search/astro-ph?searchtype=author&query=Ott%2C+J">J. Ott</a>, <a href="/search/astro-ph?searchtype=author&query=Relano%2C+M">M. Relano</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+J+D">J. D. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Tarantino%2C+E">E. Tarantino</a>, <a href="/search/astro-ph?searchtype=author&query=Veilleux%2C+S">S. Veilleux</a>, <a href="/search/astro-ph?searchtype=author&query=Walter%2C+F">F. Walter</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Werf%2C+P">P. van der Werf</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2501.14893v4-abstract-short" style="display: inline;"> We present a study of new 7.7-11.3 $渭$m data obtained with the James Webb Space Telescope Mid-InfraRed Instrument in the starburst galaxy M 82. In particular, we focus on the dependency of the integrated CO(1-0) line intensity on the MIRI-F770W and MIRI-F1130W filter intensities to investigate the correlation between CO content and the 7.7 and 11.3 $渭$m features from polycyclic aromatic hydrocarbo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.14893v4-abstract-full').style.display = 'inline'; document.getElementById('2501.14893v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.14893v4-abstract-full" style="display: none;"> We present a study of new 7.7-11.3 $渭$m data obtained with the James Webb Space Telescope Mid-InfraRed Instrument in the starburst galaxy M 82. In particular, we focus on the dependency of the integrated CO(1-0) line intensity on the MIRI-F770W and MIRI-F1130W filter intensities to investigate the correlation between CO content and the 7.7 and 11.3 $渭$m features from polycyclic aromatic hydrocarbons (PAH) in M 82's outflows. To perform our analysis, we identify CO clouds using archival $^{12}$CO($J$=1-0) NOEMA moment 0 map within 2 kpc from the center of M 82, with sizes ranging between $\sim$21 and 270 pc; then, we compute the CO-to-PAH relations for the 306 validated CO clouds. On average, the power-law slopes for the two relations in M 82 are lower than what is seen in local main-sequence spirals. In addition, there is a moderate correlation between $I_{\rm CO(1-0)}$-$I_{\rm 7.7渭m} /I_{\rm 11.3渭m}$ for most of the CO cloud groups analyzed in this work. Our results suggest that the extreme conditions in M 82 translate into CO not tracing the full budget of molecular gas in smaller clouds, perhaps as a consequence of photoionization and/or emission suppression of CO molecules due to hard radiation fields from the central starburst. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.14893v4-abstract-full').style.display = 'none'; document.getElementById('2501.14893v4-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 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.08974">arXiv:2405.08974</a> <span> [<a href="https://arxiv.org/pdf/2405.08974">pdf</a>, <a href="https://arxiv.org/format/2405.08974">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202450730">10.1051/0004-6361/202450730 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of $\sim$2200 new supernova remnants in 19 nearby star-forming galaxies with MUSE spectroscopy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Li%2C+J">Jing Li</a>, <a href="/search/astro-ph?searchtype=author&query=Kreckel%2C+K">K. Kreckel</a>, <a href="/search/astro-ph?searchtype=author&query=Sarbadhicary%2C+S">S. Sarbadhicary</a>, <a href="/search/astro-ph?searchtype=author&query=Egorov%2C+O+V">Oleg V. Egorov</a>, <a href="/search/astro-ph?searchtype=author&query=Groves%2C+B">B. Groves</a>, <a href="/search/astro-ph?searchtype=author&query=Long%2C+K+S">K. S. Long</a>, <a href="/search/astro-ph?searchtype=author&query=Congiu%2C+E">Enrico Congiu</a>, <a href="/search/astro-ph?searchtype=author&query=Belfiore%2C+F">Francesco Belfiore</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S+C+O">Simon C. O. Glover</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A+.+T">Ashley . T Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">Frank Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Blanc%2C+G+A">Guillermo A. Blanc</a>, <a href="/search/astro-ph?searchtype=author&query=Grasha%2C+K">Kathryn Grasha</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R+S">Ralf S. Klessen</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A">Adam Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%A9ndez-Delgado%2C+J+E">J. Eduardo M茅ndez-Delgado</a>, <a href="/search/astro-ph?searchtype=author&query=Neumann%2C+J">Justus Neumann</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=collaborators%2C+P">PHANGS collaborators</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.08974v1-abstract-short" style="display: inline;"> We present the largest extragalactic survey of supernova remnant (SNR) candidates in nearby star-forming galaxies using exquisite spectroscopic maps from MUSE. Supernova remnants exhibit distinctive emission-line ratios and kinematic signatures, which are apparent in optical spectroscopy. Using optical integral field spectra from the PHANGS-MUSE project, we identify SNRs in 19 nearby galaxies at ~… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.08974v1-abstract-full').style.display = 'inline'; document.getElementById('2405.08974v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.08974v1-abstract-full" style="display: none;"> We present the largest extragalactic survey of supernova remnant (SNR) candidates in nearby star-forming galaxies using exquisite spectroscopic maps from MUSE. Supernova remnants exhibit distinctive emission-line ratios and kinematic signatures, which are apparent in optical spectroscopy. Using optical integral field spectra from the PHANGS-MUSE project, we identify SNRs in 19 nearby galaxies at ~ 100~pc scales. We use five different optical diagnostics: (1) line ratio maps of [SII]/H$伪$; (2) line ratio maps of [OI]/H$伪$; (3) velocity dispersion map of the gas; (4) and (5) two line ratio diagnostic diagrams from BPT diagrams to identify and distinguish SNRs from other nebulae. Given that our SNRs are seen in projection against HII regions and diffuse ionized gas, in our line ratio maps we use a novel technique to search for objects with [SII]/H$伪$ or [OI]/H$伪$ in excess of what is expected at fixed H$伪$ surface brightness within photoionized gas. In total, we identify 2,233 objects using at least one of our diagnostics, and define a subsample of 1,166 high-confidence SNRs that have been detected with at least two diagnostics. The line ratios of these SNRs agree well with the MAPPINGS shock models, and we validate our technique using the well-studied nearby galaxy M83, where all SNRs we found are also identified in literature catalogs and we recover 51% of the known SNRs. The remaining 1,067 objects in our sample are detected with only one diagnostic and we classify them as SNR candidates. We find that ~ 35% of all our objects overlap with the boundaries of HII regions from literature catalogs, highlighting the importance of using indicators beyond line intensity morphology to select SNRs. [OI]/H$伪$ line ratio is responsible for selecting the most objects (1,368; 61%), (abridged). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.08974v1-abstract-full').style.display = 'none'; document.getElementById('2405.08974v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">35 pages, 24 figures,6 tables, submitted to A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 690, A161 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.03686">arXiv:2405.03686</a> <span> [<a href="https://arxiv.org/pdf/2405.03686">pdf</a>, <a href="https://arxiv.org/format/2405.03686">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> JWST Observations of Starbursts: Cold Clouds and Plumes Launching in the M82 Outflow </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fisher%2C+D+B">Deanne B. Fisher</a>, <a href="/search/astro-ph?searchtype=author&query=Bolatto%2C+A+D">Alberto D. Bolatto</a>, <a href="/search/astro-ph?searchtype=author&query=Chisholm%2C+J">John Chisholm</a>, <a href="/search/astro-ph?searchtype=author&query=Fielding%2C+D">Drummond Fielding</a>, <a href="/search/astro-ph?searchtype=author&query=Levy%2C+R+C">Rebecca C. Levy</a>, <a href="/search/astro-ph?searchtype=author&query=Tarantino%2C+E">Elizabeth Tarantino</a>, <a href="/search/astro-ph?searchtype=author&query=Boyer%2C+M+L">Martha L. Boyer</a>, <a href="/search/astro-ph?searchtype=author&query=Cronin%2C+S+A">Serena A. Cronin</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+J+D">J. D. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Berg%2C+D+A">Danielle A. Berg</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+S">Sebastian Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Veilleux%2C+S">Sylvain Veilleux</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Werf%2C+P+P">Paul P. van der Werf</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ker%2C+T">Torsten B枚ker</a>, <a href="/search/astro-ph?searchtype=author&query=Boogaard%2C+L+A">Leindert A. Boogaard</a>, <a href="/search/astro-ph?searchtype=author&query=Lenki%C4%87%2C+L">Laura Lenki膰</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S+C+O">Simon C. O. Glover</a>, <a href="/search/astro-ph?searchtype=author&query=Villanueva%2C+V">Vicente Villanueva</a>, <a href="/search/astro-ph?searchtype=author&query=Mayya%2C+D">Divakara Mayya</a>, <a href="/search/astro-ph?searchtype=author&query=Lai%2C+T+S+-">Thomas S. -Y. Lai</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">Daniel A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Emig%2C+K+L">Kimberly L. Emig</a>, <a href="/search/astro-ph?searchtype=author&query=Walter%2C+F">Fabian Walter</a>, <a href="/search/astro-ph?searchtype=author&query=Rela%C3%B1o%2C+M">Monica Rela帽o</a> , et al. (6 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.03686v1-abstract-short" style="display: inline;"> In this paper we study the filamentary substructure of 3.3 $渭$m PAH emission from JWST/NIRCam observations in the base of the M82 star-burst driven wind. We identify plume-like substructure within the PAH emission with widths of $\sim$50 pc. Several of the plumes extend to the edge of the field-of-view, and thus are at least 200-300 pc in length. In this region of the outflow, the vast majority (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.03686v1-abstract-full').style.display = 'inline'; document.getElementById('2405.03686v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.03686v1-abstract-full" style="display: none;"> In this paper we study the filamentary substructure of 3.3 $渭$m PAH emission from JWST/NIRCam observations in the base of the M82 star-burst driven wind. We identify plume-like substructure within the PAH emission with widths of $\sim$50 pc. Several of the plumes extend to the edge of the field-of-view, and thus are at least 200-300 pc in length. In this region of the outflow, the vast majority ($\sim$70\%) of PAH emission is associated with the plumes. We show that those structures contain smaller scale "clouds" with widths that are $\sim$5-15 pc, and they are morphologically similar to the results of "cloud-crushing" simulations. We estimate the cloud-crushing time-scales of $\sim$0.5-3 Myr, depending on assumptions. We show this time scale is consistent with a picture in which these observed PAH clouds survived break-out from the disk rather than being destroyed by the hot wind. The PAH emission in both the midplane and the outflow is shown to tightly correlate with that of Pa$伪$ emission (from HST/NICMOS data), at the scale of both plumes and clouds, though the ratio of PAH-to-Pa$伪$ increases at further distances from the midplane. Finally, we show that the outflow PAH emission is suppressed in regions of the M82 wind that are bright in X-ray emission. Overall, our results are broadly consistent with a picture in which cold gas in galactic outflows is launched via hierarchically structured plumes, and those small scale clouds are more likely to survive the wind environment when collected into the larger plume structure. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.03686v1-abstract-full').style.display = 'none'; document.getElementById('2405.03686v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.19001">arXiv:2404.19001</a> <span> [<a href="https://arxiv.org/pdf/2404.19001">pdf</a>, <a href="https://arxiv.org/format/2404.19001">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"> Constraining the Diffusion Coefficient and Cosmic-Ray Acceleration Efficiency using Gamma-ray Emission from the Star-Forming Region RCW 38 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pandey%2C+P">Paarmita Pandey</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Rosen%2C+A+L">Anna L. Rosen</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+T+A">Todd A. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Linden%2C+T">Tim Linden</a>, <a href="/search/astro-ph?searchtype=author&query=Blackstone%2C+I">Ian Blackstone</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="2404.19001v2-abstract-short" style="display: inline;"> Stellar winds from massive stars may be significant sources of cosmic rays (CRs). To investigate this connection, we report a detailed study of gamma-ray emission near the young Milky Way star cluster ($\approx$ 0.5 Myr old) in the star-forming region RCW 38 and compare this emission to its stellar wind properties and diffuse X-ray emission. Using 15 years of Fermi-LAT data in the 0.2 $-$ 300 GeV… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.19001v2-abstract-full').style.display = 'inline'; document.getElementById('2404.19001v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.19001v2-abstract-full" style="display: none;"> Stellar winds from massive stars may be significant sources of cosmic rays (CRs). To investigate this connection, we report a detailed study of gamma-ray emission near the young Milky Way star cluster ($\approx$ 0.5 Myr old) in the star-forming region RCW 38 and compare this emission to its stellar wind properties and diffuse X-ray emission. Using 15 years of Fermi-LAT data in the 0.2 $-$ 300 GeV band, we find a significant ($ 蟽> 22$) detection coincident with the star cluster, producing a total $纬$-ray luminosity (extrapolated over 0.1 $-$ 500 GeV) of $L_纬 = (2.66\pm 0.92) \times 10^{34}$ erg s$^{-1}$ adopting a power-law spectral model ($螕= 2.34\pm0.04$). Using an empirical relationship and Starburst99, we estimate the total wind power to be $8 \times 10^{36}$ erg s$^{-1}$, corresponding to a CR acceleration efficiency of $畏_{\rm CR} \simeq 0.4$ for an assumed diffusion coefficient consistent with $D = 10^{28}$ cm$^{2}$ s$^{-1}$. Alternatively, a lower acceleration efficiency of 0.1 can produce this $L_纬$ if the diffusion coefficient is smaller, $D\simeq 2.5\times10^{27}\,{\rm cm^2\,\,s^{-1}}$. Additionally, we analyze Chandra X-ray data from the region and compare the hot-gas pressure to the CR pressure. We find the former is four orders of magnitude greater, suggesting that the CR pressure is not dynamically important relative to stellar winds. As RCW 38 is too young for supernovae to have occurred, the high CR acceleration efficiency in RCW 38 demonstrates that stellar winds may be an important source of Galactic CRs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.19001v2-abstract-full').style.display = 'none'; document.getElementById('2404.19001v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.10762">arXiv:2404.10762</a> <span> [<a href="https://arxiv.org/pdf/2404.10762">pdf</a>, <a href="https://arxiv.org/format/2404.10762">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> H-alpha emission and HII regions at the locations of recent supernovae in nearby galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chen%2C+N+M">Ness Mayker Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A+K">Adam K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Sarbadhicary%2C+S+K">Sumit K. Sarbadhicary</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+T+A">Todd A. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A+T">Ashley T. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Groves%2C+B">Brent Groves</a>, <a href="/search/astro-ph?searchtype=author&query=Chandar%2C+R">Rupali Chandar</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">M茅lanie Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Chown%2C+R">Ryan Chown</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">Daniel A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Egorov%2C+O+V">Oleg V. Egorov</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S+C+O">Simon C. O. Glover</a>, <a href="/search/astro-ph?searchtype=author&query=Grasha%2C+K">Kathryn Grasha</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R+S">Ralf S. Klessen</a>, <a href="/search/astro-ph?searchtype=author&query=Kreckel%2C+K">Kathryn Kreckel</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+J">Jing Li</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%A9ndez-Delgado%2C+J+E">J. Eduardo M茅ndez-Delgado</a>, <a href="/search/astro-ph?searchtype=author&query=Murphy%2C+E+J">Eric J. Murphy</a>, <a href="/search/astro-ph?searchtype=author&query=Pathak%2C+D">Debosmita Pathak</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Thilker%2C+D+A">David A. Thilker</a>, <a href="/search/astro-ph?searchtype=author&query=%C3%9Abeda%2C+L">Leonardo 脷beda</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. Williams</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.10762v1-abstract-short" style="display: inline;"> We present a statistical analysis of the local, approximately 50-100 pc scale, H-alpha emission at the locations of recent (less than 125 years) supernovae (SNe) in nearby star-forming galaxies. Our sample consists of 32 SNe in 10 galaxies that are targets of the PHANGS-MUSE survey. We find that 41% (13/32) of these SNe occur coincident with a previously identified HII region. For comparison, HII… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.10762v1-abstract-full').style.display = 'inline'; document.getElementById('2404.10762v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.10762v1-abstract-full" style="display: none;"> We present a statistical analysis of the local, approximately 50-100 pc scale, H-alpha emission at the locations of recent (less than 125 years) supernovae (SNe) in nearby star-forming galaxies. Our sample consists of 32 SNe in 10 galaxies that are targets of the PHANGS-MUSE survey. We find that 41% (13/32) of these SNe occur coincident with a previously identified HII region. For comparison, HII regions cover 32% of the area within 1 kpc of any recent SN. Contrasting this local covering fraction with the fraction of SNe coincident with HII regions, we find a statistical excess of 7.6% +/- 8.7% of all SNe to be associated with HII regions. This increases to an excess of 19.2% +/- 10.4% when considering only core-collapse SNe. These estimates appear to be in good agreement with qualitative results from new, higher resolution HST H-alpha imaging, which also suggest many CCSNe detonate near but not in HII regions. Our results appear consistent with the expectation that only a modest fraction of stars explode during the first 5 Myr of the life of a stellar population, when H-alpha emission is expected to be bright. Of the HII region associated SNe, 8% (11/13) also have associated detected CO(2-1) emission, indicating the presence of molecular gas. The HII region associated SNe have typical Av extinctions approximately equal to 1 mag, consistent with a significant amount of pre-clearing of gas from the region before the SNe explode. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.10762v1-abstract-full').style.display = 'none'; document.getElementById('2404.10762v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ; 33 pages, 13 figures, 3 tables in two-column AASTEX63 format</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.14056">arXiv:2402.14056</a> <span> [<a href="https://arxiv.org/pdf/2402.14056">pdf</a>, <a href="https://arxiv.org/format/2402.14056">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"> Detection of Diffuse Hot Gas Around the Young, Potential Superstar Cluster H72.97-69.39 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Webb%2C+T+L">Trinity L. Webb</a>, <a href="/search/astro-ph?searchtype=author&query=Rodriguez%2C+J+A">Jennifer A. Rodriguez</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Rosen%2C+A+L">Anna L. Rosen</a>, <a href="/search/astro-ph?searchtype=author&query=Lancaster%2C+L">Lachlan Lancaster</a>, <a href="/search/astro-ph?searchtype=author&query=Nayak%2C+O">Omnarayani Nayak</a>, <a href="/search/astro-ph?searchtype=author&query=McLeod%2C+A+F">Anna F. McLeod</a>, <a href="/search/astro-ph?searchtype=author&query=Pandey%2C+P">Paarmita Pandey</a>, <a href="/search/astro-ph?searchtype=author&query=Olivier%2C+G+M">Grace M. Olivier</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="2402.14056v2-abstract-short" style="display: inline;"> We present the first Chandra X-ray observations of H72.97-69.39, a highly-embedded, potential super-star cluster (SSC) in its infancy located in the star-forming complex N79 of the Large Magellanic Cloud. We detect particularly hard, diffuse X-ray emission that is coincident with the young stellar objects (YSOs) identified with JWST, and the hot gas fills cavities in the dense gas mapped by ALMA.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.14056v2-abstract-full').style.display = 'inline'; document.getElementById('2402.14056v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.14056v2-abstract-full" style="display: none;"> We present the first Chandra X-ray observations of H72.97-69.39, a highly-embedded, potential super-star cluster (SSC) in its infancy located in the star-forming complex N79 of the Large Magellanic Cloud. We detect particularly hard, diffuse X-ray emission that is coincident with the young stellar objects (YSOs) identified with JWST, and the hot gas fills cavities in the dense gas mapped by ALMA. The X-ray spectra are best fit with either a thermal plasma or power-law model, and assuming the former, we show that the X-ray luminosity of L_X = (1.0 +- 0.3)e34 erg/s is a factor of ~20 below the expectation for a fully-confined wind bubble. Our results suggest that stellar wind feedback produces diffuse hot gas in the earliest stages of massive star cluster formation and that wind energy can be lost quickly via either turbulent mixing followed by radiative cooling or by physical leakage. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.14056v2-abstract-full').style.display = 'none'; document.getElementById('2402.14056v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 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">13 pages, 7 figures, 3 tables, accepted to ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 977 45 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.16648">arXiv:2401.16648</a> <span> [<a href="https://arxiv.org/pdf/2401.16648">pdf</a>, <a href="https://arxiv.org/format/2401.16648">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> JWST Observations of Starbursts: Polycyclic Aromatic Hydrocarbon Emission at the Base of the M 82 Galactic Wind </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bolatto%2C+A+D">Alberto D. Bolatto</a>, <a href="/search/astro-ph?searchtype=author&query=Levy%2C+R+C">Rebecca C. Levy</a>, <a href="/search/astro-ph?searchtype=author&query=Tarantino%2C+E">Elizabeth Tarantino</a>, <a href="/search/astro-ph?searchtype=author&query=Boyer%2C+M+L">Martha L. Boyer</a>, <a href="/search/astro-ph?searchtype=author&query=Fisher%2C+D+B">Deanne B. Fisher</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A+K">Adam K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Cronin%2C+S+A">Serena A. Cronin</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R+S">Ralf S. Klessen</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+J+D">J. D. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Berg%2C+D+A">Dannielle A. Berg</a>, <a href="/search/astro-ph?searchtype=author&query=Boeker%2C+T">Torsten Boeker</a>, <a href="/search/astro-ph?searchtype=author&query=Boogaard%2C+L+A">Leindert A. Boogaard</a>, <a href="/search/astro-ph?searchtype=author&query=Ostriker%2C+E+C">Eve C. Ostriker</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+T+A">Todd A. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Ott%2C+J">Juergen Ott</a>, <a href="/search/astro-ph?searchtype=author&query=Lenkic%2C+L">Laura Lenkic</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">Daniel A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Veilleux%2C+S">Sylvain Veilleux</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Werf%2C+P+P">Paul P. van der Werf</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S+C+O">Simon C. O. Glover</a>, <a href="/search/astro-ph?searchtype=author&query=Sandstrom%2C+K+M">Karin M. Sandstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Skillman%2C+E+D">Evan D. Skillman</a>, <a href="/search/astro-ph?searchtype=author&query=Chisholm%2C+J">John Chisholm</a>, <a href="/search/astro-ph?searchtype=author&query=Villanueva%2C+V">Vicente Villanueva</a> , et al. (15 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.16648v4-abstract-short" style="display: inline;"> We present new observations of the central 1 kpc of the M 82 starburst obtained with the James Webb Space Telescope (JWST) near-infrared camera (NIRCam) instrument at a resolution ~0.05"-0.1" (~1-2 pc). The data comprises images in three mostly continuum filters (F140M, F250M, and F360M), and filters that contain [FeII] (F164N), H2 v=1-0 (F212N), and the 3.3 um PAH feature (F335M). We find promine… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.16648v4-abstract-full').style.display = 'inline'; document.getElementById('2401.16648v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.16648v4-abstract-full" style="display: none;"> We present new observations of the central 1 kpc of the M 82 starburst obtained with the James Webb Space Telescope (JWST) near-infrared camera (NIRCam) instrument at a resolution ~0.05"-0.1" (~1-2 pc). The data comprises images in three mostly continuum filters (F140M, F250M, and F360M), and filters that contain [FeII] (F164N), H2 v=1-0 (F212N), and the 3.3 um PAH feature (F335M). We find prominent plumes of PAH emission extending outward from the central starburst region, together with a network of complex filamentary substructure and edge-brightened bubble-like features. The structure of the PAH emission closely resembles that of the ionized gas, as revealed in Paschen alpha and free-free radio emission. We discuss the origin of the structure, and suggest the PAHs are embedded in a combination of neutral, molecular, and photoionized gas. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.16648v4-abstract-full').style.display = 'none'; document.getElementById('2401.16648v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to The Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.08444">arXiv:2312.08444</a> <span> [<a href="https://arxiv.org/pdf/2312.08444">pdf</a>, <a href="https://arxiv.org/format/2312.08444">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/10.3847/1538-4357/ad4606">10.3847/1538-4357/ad4606 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Hot Gas Outflow Properties of the Starburst Galaxy NGC 4945 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Barrera%2C+N+P">Natalia Porraz Barrera</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+S">Sebastian Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Foord%2C+A">Adi Foord</a>, <a href="/search/astro-ph?searchtype=author&query=Nguyen%2C+D+D">Dustin D. Nguyen</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+T+A">Todd A. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Mathur%2C+S">Smita Mathur</a>, <a href="/search/astro-ph?searchtype=author&query=Bolatto%2C+A+D">Alberto D. Bolatto</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="2312.08444v2-abstract-short" style="display: inline;"> We analyze 330 ks of {\it Chandra} X-ray imaging and spectra of the nearby, edge-on starburst and Seyfert Type 2 galaxy NGC 4945 to measure the hot gas properties along the galactic outflows. We extract and model spectra from 15 regions extending from $-$0.55 kpc to $+$0.85 kpc above and below the galactic disk to determine the best-fit parameters and metal abundances. We find that the hot gas tem… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.08444v2-abstract-full').style.display = 'inline'; document.getElementById('2312.08444v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.08444v2-abstract-full" style="display: none;"> We analyze 330 ks of {\it Chandra} X-ray imaging and spectra of the nearby, edge-on starburst and Seyfert Type 2 galaxy NGC 4945 to measure the hot gas properties along the galactic outflows. We extract and model spectra from 15 regions extending from $-$0.55 kpc to $+$0.85 kpc above and below the galactic disk to determine the best-fit parameters and metal abundances. We find that the hot gas temperatures and number densities peak in the central regions and decrease along the outflows. These profiles are inconsistent with a spherical, adiabatically-expanding wind model, suggesting the need to include mass loading and/or a non-spherical outflow geometry. We estimate the mass outflow rate of the hot wind to be $1.6\:M_{\odot}~\rm{yr}^{-1}$. Emission from charge exchange is detected in the northern outflow, and we estimate it contributes 12\% to the emitted, broad-band ($0.5-7$ keV) X-ray flux. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.08444v2-abstract-full').style.display = 'none'; document.getElementById('2312.08444v2-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 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">11 pages, 7 figures; submitted (13 December 2023), accepted ApJ (11 April 2023)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.06031">arXiv:2312.06031</a> <span> [<a href="https://arxiv.org/pdf/2312.06031">pdf</a>, <a href="https://arxiv.org/format/2312.06031">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The PHANGS-AstroSat Atlas of Nearby Star Forming Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hassani%2C+H">Hamid Hassani</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Koch%2C+E+W">Eric W. Koch</a>, <a href="/search/astro-ph?searchtype=author&query=Postma%2C+J">Joseph Postma</a>, <a href="/search/astro-ph?searchtype=author&query=Nofech%2C+J">Joseph Nofech</a>, <a href="/search/astro-ph?searchtype=author&query=Corbould%2C+H">Harrisen Corbould</a>, <a href="/search/astro-ph?searchtype=author&query=Thilker%2C+D">David Thilker</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A+K">Adam K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Belfiore%2C+F">Francesco Belfiore</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">Frank Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Boquien%2C+M">Mederic Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">Melanie Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">Daniel A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Egorov%2C+O+V">Oleg V. Egorov</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S+C+O">Simon C. O. Glover</a>, <a href="/search/astro-ph?searchtype=author&query=Grasha%2C+K">Kathryn Grasha</a>, <a href="/search/astro-ph?searchtype=author&query=Groves%2C+B">Brent Groves</a>, <a href="/search/astro-ph?searchtype=author&query=Henny%2C+K">Kiana Henny</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+J">Jaeyeon Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R+S">Ralf S. Klessen</a>, <a href="/search/astro-ph?searchtype=author&query=Kreckel%2C+K">Kathryn Kreckel</a>, <a href="/search/astro-ph?searchtype=author&query=Kruijssen%2C+J+M+D">J. M. Diederik Kruijssen</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J+C">Janice C. Lee</a> , et al. (7 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.06031v1-abstract-short" style="display: inline;"> We present the Physics at High Angular resolution in Nearby GalaxieS (PHANGS)-AstroSat atlas, which contains ultraviolet imaging of 31 nearby star-forming galaxies captured by the Ultraviolet Imaging Telescope (UVIT) on the AstroSat satellite. The atlas provides a homogeneous data set of far- and near-ultraviolet maps of galaxies within a distance of 22 Mpc and a median angular resolution of 1.4 a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.06031v1-abstract-full').style.display = 'inline'; document.getElementById('2312.06031v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.06031v1-abstract-full" style="display: none;"> We present the Physics at High Angular resolution in Nearby GalaxieS (PHANGS)-AstroSat atlas, which contains ultraviolet imaging of 31 nearby star-forming galaxies captured by the Ultraviolet Imaging Telescope (UVIT) on the AstroSat satellite. The atlas provides a homogeneous data set of far- and near-ultraviolet maps of galaxies within a distance of 22 Mpc and a median angular resolution of 1.4 arcseconds (corresponding to a physical scale between 25 and 160 pc). After subtracting a uniform ultraviolet background and accounting for Milky Way extinction, we compare our estimated flux densities to GALEX observations, finding good agreement. We find candidate extended UV disks around the galaxies NGC 6744 and IC 5332. We present the first statistical measurements of the clumping of the UV emission and compare it to the clumping of molecular gas traced with ALMA. We find that bars and spiral arms exhibit the highest degree of clumping, and the molecular gas is even more clumped than the FUV emission in galaxies. We investigate the variation of the ratio of observed FUV to H$伪$ in different galactic environments and kpc-sized apertures. We report that $\sim 65 \%$ varation of the $\log_{10}$(FUV/H$伪$) can be described through a combination of dust attenuation with star formation history parameters. The PHANGS-AstroSat atlas enhances the multi-wavelength coverage of our sample, offering a detailed perspective on star formation. When integrated with PHANGS data sets from ALMA, VLT-MUSE, HST and JWST, it develops our comprehensive understanding of attenuation curves and dust attenuation in star-forming galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.06031v1-abstract-full').style.display = 'none'; document.getElementById('2312.06031v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">35 pages, 16 figures. The survey webpage is available at https://sites.google.com/view/phangs/home/data/astrosat and the data archive can be accessed at https://www.canfar.net/storage/vault/list/phangs/RELEASES/PHANGS-AstroSat/v1p0</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.18067">arXiv:2311.18067</a> <span> [<a href="https://arxiv.org/pdf/2311.18067">pdf</a>, <a href="https://arxiv.org/format/2311.18067">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> A Two-Component Probability Distribution Function Describes the mid-IR Emission from the Disks of Star-Forming Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pathak%2C+D">Debosmita Pathak</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A+K">Adam K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+T+A">Todd A. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Belfiore%2C+F">Francesco Belfiore</a>, <a href="/search/astro-ph?searchtype=author&query=Boquien%2C+M">Mederic Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">Daniel A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S+C+O">Simon C. O. Glover</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R+S">Ralf S. Klessen</a>, <a href="/search/astro-ph?searchtype=author&query=Koch%2C+E+W">Eric W. Koch</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Sandstrom%2C+K+M">Karin M. Sandstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+R">Rowan Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+J">Jiayi Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Sutter%2C+J">Jessica Sutter</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">Frank Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Y">Yixian Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Chastenet%2C+J">Jeremy Chastenet</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">Melanie Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Chown%2C+R">Ryan Chown</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Faesi%2C+C+M">Christopher M. Faesi</a>, <a href="/search/astro-ph?searchtype=author&query=Larson%2C+K+L">Kirsten L. Larson</a> , et al. (6 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.18067v1-abstract-short" style="display: inline;"> High-resolution JWST-MIRI images of nearby spiral galaxies reveal emission with complex substructures that trace dust heated both by massive young stars and the diffuse interstellar radiation field. We present high angular (0."85) and physical resolution (20-80 pc) measurements of the probability distribution function (PDF) of mid-infrared (mid-IR) emission (7.7-21 $渭$m) from 19 nearby star-formin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.18067v1-abstract-full').style.display = 'inline'; document.getElementById('2311.18067v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.18067v1-abstract-full" style="display: none;"> High-resolution JWST-MIRI images of nearby spiral galaxies reveal emission with complex substructures that trace dust heated both by massive young stars and the diffuse interstellar radiation field. We present high angular (0."85) and physical resolution (20-80 pc) measurements of the probability distribution function (PDF) of mid-infrared (mid-IR) emission (7.7-21 $渭$m) from 19 nearby star-forming galaxies from the PHANGS-JWST Cycle-1 Treasury. The PDFs of mid-IR emission from the disks of all 19 galaxies consistently show two distinct components: an approximately log-normal distribution at lower intensities and a high-intensity power-law component. These two components only emerge once individual star-forming regions are resolved. Comparing with locations of HII regions identified from VLT/MUSE H$伪$-mapping, we infer that the power-law component arises from star-forming regions and thus primarily traces dust heated by young stars. In the continuum-dominated 21 $渭$m band, the power-law is more prominent and contains roughly half of the total flux. At 7.7-11.3 $渭$m, the power-law is suppressed by the destruction of small grains (including PAHs) close to HII regions while the log-normal component tracing the dust column in diffuse regions appears more prominent. The width and shape of the log-normal diffuse emission PDFs in galactic disks remain consistent across our sample, implying a log-normal gas column density $N$(H)$\approx10^{21}$cm$^{-2}$ shaped by supersonic turbulence with typical (isothermal) turbulent Mach numbers $\approx5-15$. Finally, we describe how the PDFs of galactic disks are assembled from dusty HII regions and diffuse gas, and discuss how the measured PDF parameters correlate with global properties such as star-formation rate and gas surface density. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.18067v1-abstract-full').style.display = 'none'; document.getElementById('2311.18067v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">30 pages without appendix, 17 figures, (with appendix images of full sample: 56 pages, 39 figures), accepted in AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.07661">arXiv:2311.07661</a> <span> [<a href="https://arxiv.org/pdf/2311.07661">pdf</a>, <a href="https://arxiv.org/format/2311.07661">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> The evolution of galaxies and clusters at high spatial resolution with AXIS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Russell%2C+H+R">H. R. Russell</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">L. A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+S+W">S. W. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Chartas%2C+G">G. Chartas</a>, <a href="/search/astro-ph?searchtype=author&query=Choudhury%2C+P+P">P. P. Choudhury</a>, <a href="/search/astro-ph?searchtype=author&query=Dupke%2C+R+A">R. A. Dupke</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=Flores%2C+A+M">A. M. Flores</a>, <a href="/search/astro-ph?searchtype=author&query=Garofali%2C+K">K. Garofali</a>, <a href="/search/astro-ph?searchtype=author&query=Hodges-Kluck%2C+E">E. Hodges-Kluck</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=Lanz%2C+L">L. Lanz</a>, <a href="/search/astro-ph?searchtype=author&query=Lehmer%2C+B+D">B. D. Lehmer</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+J+-">J. -T. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Maksym%2C+W+P">W. P. Maksym</a>, <a href="/search/astro-ph?searchtype=author&query=Mantz%2C+A+B">A. B. Mantz</a>, <a href="/search/astro-ph?searchtype=author&query=McDonald%2C+M">M. McDonald</a>, <a href="/search/astro-ph?searchtype=author&query=Miller%2C+E+D">E. D. Miller</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotzky%2C+R+F">R. F. Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Qiu%2C+Y">Y. Qiu</a>, <a href="/search/astro-ph?searchtype=author&query=Reynolds%2C+C+S">C. S. Reynolds</a>, <a href="/search/astro-ph?searchtype=author&query=Tombesi%2C+F">F. Tombesi</a>, <a href="/search/astro-ph?searchtype=author&query=Tozzi%2C+P">P. Tozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Trindade-Falcao%2C+A">A. Trindade-Falcao</a>, <a href="/search/astro-ph?searchtype=author&query=Walker%2C+S+A">S. A. Walker</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="2311.07661v1-abstract-short" style="display: inline;"> Stellar and black hole feedback heat and disperse surrounding cold gas clouds, launching gas flows off circumnuclear and galactic disks and producing a dynamic interstellar medium. On large scales bordering the cosmic web, feedback drives enriched gas out of galaxies and groups, seeding the intergalactic medium with heavy elements. In this way, feedback shapes galaxy evolution by shutting down sta… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.07661v1-abstract-full').style.display = 'inline'; document.getElementById('2311.07661v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.07661v1-abstract-full" style="display: none;"> Stellar and black hole feedback heat and disperse surrounding cold gas clouds, launching gas flows off circumnuclear and galactic disks and producing a dynamic interstellar medium. On large scales bordering the cosmic web, feedback drives enriched gas out of galaxies and groups, seeding the intergalactic medium with heavy elements. In this way, feedback shapes galaxy evolution by shutting down star formation and ultimately curtailing the growth of structure after the peak at redshift 2-3. To understand the complex interplay between gravity and feedback, we must resolve both the key physics within galaxies and map the impact of these processes over large scales, out into the cosmic web. The Advanced X-ray Imaging Satellite (AXIS) is a proposed X-ray probe mission for the 2030s with arcsecond spatial resolution, large effective area, and low background. AXIS will untangle the interactions of winds, radiation, jets, and supernovae with the surrounding ISM across the wide range of mass scales and large volumes driving galaxy evolution and trace the establishment of feedback back to the main event at cosmic noon. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.07661v1-abstract-full').style.display = 'none'; document.getElementById('2311.07661v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 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">29 pages, 18 figures; this white paper is part of a series commissioned for the AXIS Probe mission concept</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.02057">arXiv:2311.02057</a> <span> [<a href="https://arxiv.org/pdf/2311.02057">pdf</a>, <a href="https://arxiv.org/format/2311.02057">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="Fluid Dynamics">physics.flu-dyn</span> </div> </div> <p class="title is-5 mathjax"> Neural ODEs as a discovery tool to characterize the structure of the hot galactic wind of M82 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Nguyen%2C+D+D">Dustin D. Nguyen</a>, <a href="/search/astro-ph?searchtype=author&query=Ting%2C+Y">Yuan-Sen Ting</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+T+A">Todd A. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+S">Sebastian Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.02057v2-abstract-short" style="display: inline;"> Dynamic astrophysical phenomena are predominantly described by differential equations, yet our understanding of these systems is constrained by our incomplete grasp of non-linear physics and scarcity of comprehensive datasets. As such, advancing techniques in solving non-linear inverse problems becomes pivotal to addressing numerous outstanding questions in the field. In particular, modeling hot g… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.02057v2-abstract-full').style.display = 'inline'; document.getElementById('2311.02057v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.02057v2-abstract-full" style="display: none;"> Dynamic astrophysical phenomena are predominantly described by differential equations, yet our understanding of these systems is constrained by our incomplete grasp of non-linear physics and scarcity of comprehensive datasets. As such, advancing techniques in solving non-linear inverse problems becomes pivotal to addressing numerous outstanding questions in the field. In particular, modeling hot galactic winds is difficult because of unknown structure for various physical terms, and the lack of \textit{any} kinematic observational data. Additionally, the flow equations contain singularities that lead to numerical instability, making parameter sweeps non-trivial. We leverage differentiable programming, which enables neural networks to be embedded as individual terms within the governing coupled ordinary differential equations (ODEs), and show that this method can adeptly learn hidden physics. We robustly discern the structure of a mass-loading function which captures the physical effects of cloud destruction and entrainment into the hot superwind. Within a supervised learning framework, we formulate our loss function anchored on the astrophysical entropy ($K \propto P/蟻^{5/3}$). Our results demonstrate the efficacy of this approach, even in the absence of kinematic data $v$. We then apply these models to real Chandra X-Ray observations of starburst galaxy M82, providing the first systematic description of mass-loading within the superwind. This work further highlights neural ODEs as a useful discovery tool with mechanistic interpretability in non-linear inverse problems. We make our code public at this GitHub repository (https://github.com/dustindnguyen/2023_NeurIPS_NeuralODEs_M82). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.02057v2-abstract-full').style.display = 'none'; document.getElementById('2311.02057v2-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 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 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">9 Pages, 2 Figures, Accepted at the NeurIPS 2023 workshop on Machine Learning and the Physical Sciences</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.00780">arXiv:2311.00780</a> <span> [<a href="https://arxiv.org/pdf/2311.00780">pdf</a>, <a href="https://arxiv.org/format/2311.00780">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1117/12.2677468">10.1117/12.2677468 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Overview of the Advanced X-ray Imaging Satellite (AXIS) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Reynolds%2C+C+S">Christopher S. Reynolds</a>, <a href="/search/astro-ph?searchtype=author&query=Kara%2C+E+A">Erin A. Kara</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=Ptak%2C+A">Andrew Ptak</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=Williams%2C+B+J">Brian J. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+S+W">Steven W. Allen</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=Bautz%2C+M">Marshall Bautz</a>, <a href="/search/astro-ph?searchtype=author&query=Bodaghee%2C+A">Arash Bodaghee</a>, <a href="/search/astro-ph?searchtype=author&query=Burdge%2C+K+B">Kevin B. Burdge</a>, <a href="/search/astro-ph?searchtype=author&query=Cappelluti%2C+N">Nico Cappelluti</a>, <a href="/search/astro-ph?searchtype=author&query=Cenko%2C+B">Brad Cenko</a>, <a href="/search/astro-ph?searchtype=author&query=Chartas%2C+G">George Chartas</a>, <a href="/search/astro-ph?searchtype=author&query=Chan%2C+K">Kai-Wing Chan</a>, <a href="/search/astro-ph?searchtype=author&query=Corrales%2C+L">L铆a Corrales</a>, <a href="/search/astro-ph?searchtype=author&query=Daylan%2C+T">Tansu Daylan</a>, <a href="/search/astro-ph?searchtype=author&query=Falcone%2C+A+D">Abraham D. Falcone</a>, <a href="/search/astro-ph?searchtype=author&query=Foord%2C+A">Adi Foord</a>, <a href="/search/astro-ph?searchtype=author&query=Grant%2C+C+E">Catherine E. Grant</a>, <a href="/search/astro-ph?searchtype=author&query=Habouzit%2C+M">M茅lanie Habouzit</a>, <a href="/search/astro-ph?searchtype=author&query=Haggard%2C+D">Daryl Haggard</a>, <a href="/search/astro-ph?searchtype=author&query=Herrmann%2C+S">Sven Herrmann</a>, <a href="/search/astro-ph?searchtype=author&query=Hodges-Kluck%2C+E">Edmund Hodges-Kluck</a>, <a href="/search/astro-ph?searchtype=author&query=Kargaltsev%2C+O">Oleg Kargaltsev</a> , et al. (18 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.00780v1-abstract-short" style="display: inline;"> The Advanced X-ray Imaging Satellite (AXIS) is a Probe-class concept that will build on the legacy of the Chandra X-ray Observatory by providing low-background, arcsecond-resolution imaging in the 0.3-10 keV band across a 450 arcminute$^2$ field of view, with an order of magnitude improvement in sensitivity. AXIS utilizes breakthroughs in the construction of lightweight segmented X-ray optics usin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.00780v1-abstract-full').style.display = 'inline'; document.getElementById('2311.00780v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.00780v1-abstract-full" style="display: none;"> The Advanced X-ray Imaging Satellite (AXIS) is a Probe-class concept that will build on the legacy of the Chandra X-ray Observatory by providing low-background, arcsecond-resolution imaging in the 0.3-10 keV band across a 450 arcminute$^2$ field of view, with an order of magnitude improvement in sensitivity. AXIS utilizes breakthroughs in the construction of lightweight segmented X-ray optics using single-crystal silicon, and developments in the fabrication of large-format, small-pixel, high readout rate CCD detectors with good spectral resolution, allowing a robust and cost-effective design. Further, AXIS will be responsive to target-of-opportunity alerts and, with onboard transient detection, will be a powerful facility for studying the time-varying X-ray universe, following on from the legacy of the Neil Gehrels (Swift) X-ray observatory that revolutionized studies of the transient X-ray Universe. In this paper, we present an overview of AXIS, highlighting the prime science objectives driving the AXIS concept and how the observatory design will achieve these objectives. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.00780v1-abstract-full').style.display = 'none'; document.getElementById('2311.00780v1-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, 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">Published in Proceedings of SPIE Optics & Photonics 2023, San Diego</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.17694">arXiv:2310.17694</a> <span> [<a href="https://arxiv.org/pdf/2310.17694">pdf</a>, <a href="https://arxiv.org/format/2310.17694">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Where do stars explode in the ISM? -- The distribution of dense gas around massive stars and supernova remnants in M33 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sarbadhicary%2C+S+K">Sumit K. Sarbadhicary</a>, <a href="/search/astro-ph?searchtype=author&query=Wagner%2C+J">Jordan Wagner</a>, <a href="/search/astro-ph?searchtype=author&query=Koch%2C+E+W">Eric W. Koch</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+N+M">Ness Mayker Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A+K">Adam K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Lah%C3%A9n%2C+N">Natalia Lah茅n</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Neugent%2C+K+F">Kathryn F. Neugent</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+C">Chang-Goo Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Chomiuk%2C+L">Laura Chomiuk</a>, <a href="/search/astro-ph?searchtype=author&query=Dalcanton%2C+J+J">Julianne J. Dalcanton</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Pingel%2C+N+M">Nickolas M. Pingel</a>, <a href="/search/astro-ph?searchtype=author&query=Indebetouw%2C+R">Remy Indebetouw</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Tarantino%2C+E">Elizabeth Tarantino</a>, <a href="/search/astro-ph?searchtype=author&query=Meyer%2C+J+D">Jennifer Donovan Meyer</a>, <a href="/search/astro-ph?searchtype=author&query=Skillman%2C+E+D">Evan D. Skillman</a>, <a href="/search/astro-ph?searchtype=author&query=Smercina%2C+A">Adam Smercina</a>, <a href="/search/astro-ph?searchtype=author&query=Kepley%2C+A+A">Amanda A. Kepley</a>, <a href="/search/astro-ph?searchtype=author&query=Murphy%2C+E+J">Eric J. Murphy</a>, <a href="/search/astro-ph?searchtype=author&query=Strader%2C+J">Jay Strader</a>, <a href="/search/astro-ph?searchtype=author&query=Wong%2C+T">Tony Wong</a>, <a href="/search/astro-ph?searchtype=author&query=Stanimirovi%C4%87%2C+S">Sne啪ana Stanimirovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Villanueva%2C+V">Vicente Villanueva</a> , et al. (5 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.17694v1-abstract-short" style="display: inline;"> Star formation in galaxies is regulated by turbulence, outflows, gas heating and cloud dispersal -- processes which depend sensitively on the properties of the interstellar medium (ISM) into which supernovae (SNe) explode. Unfortunately, direct measurements of ISM environments around SNe remain scarce, as SNe are rare and often distant. Here we demonstrate a new approach: mapping the ISM around th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.17694v1-abstract-full').style.display = 'inline'; document.getElementById('2310.17694v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.17694v1-abstract-full" style="display: none;"> Star formation in galaxies is regulated by turbulence, outflows, gas heating and cloud dispersal -- processes which depend sensitively on the properties of the interstellar medium (ISM) into which supernovae (SNe) explode. Unfortunately, direct measurements of ISM environments around SNe remain scarce, as SNe are rare and often distant. Here we demonstrate a new approach: mapping the ISM around the massive stars that are soon to explode. This provides a much larger census of explosion sites than possible with only SNe, and allows comparison with sensitive, high-resolution maps of the atomic and molecular gas from the Jansky VLA and ALMA. In the well-resolved Local Group spiral M33, we specifically observe the environments of red supergiants (RSGs, progenitors of Type II SNe), Wolf-Rayet stars (WRs, tracing stars $>$30 M$_{\odot}$, and possibly future stripped-envelope SNe), and supernova remnants (SNRs, locations where SNe have exploded). We find that massive stars evolve not only in dense, molecular-dominated gas (with younger stars in denser gas), but also a substantial fraction ($\sim$45\% of WRs; higher for RSGs) evolve in lower-density, atomic-gas-dominated, inter-cloud media. We show that these measurements are consistent with expectations from different stellar-age tracer maps, and can be useful for validating SN feedback models in numerical simulations of galaxies. Along with the discovery of a 20-pc diameter molecular gas cavity around a WR, these findings re-emphasize the importance of pre-SN/correlated-SN feedback evacuating the dense gas around massive stars before explosion, and the need for high-resolution (down to pc-scale) surveys of the multi-phase ISM in nearby galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.17694v1-abstract-full').style.display = 'none'; document.getElementById('2310.17694v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">34 pages, 14 figures. Submitted to ApJ. Comments welcome! The density distributions will be made publicly available after journal acceptance of manuscript. Please feel free to contact us in the meantime if you would like to use them</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.15527">arXiv:2308.15527</a> <span> [<a href="https://arxiv.org/pdf/2308.15527">pdf</a>, <a href="https://arxiv.org/format/2308.15527">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"> Estimating Ejecta Mass Ratios in Kepler's SNR: Global X-Ray Spectral Analysis Including Suzaku Systematics and Emitting Volume Uncertainties </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Holland-Ashford%2C+T">Tyler Holland-Ashford</a>, <a href="/search/astro-ph?searchtype=author&query=Slane%2C+P">Patrick Slane</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Auchettl%2C+K">Katie Auchettl</a>, <a href="/search/astro-ph?searchtype=author&query=Kashyap%2C+V">Vinay Kashyap</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2308.15527v1-abstract-short" style="display: inline;"> The exact origins of many Type Ia supernovae$\unicode{x2013}$progenitor scenarios and explosive mechanisms$\unicode{x2013}$remain uncertain. In this work, we analyze the global Suzaku X-Ray spectrum of Kepler's supernova remnant in order to constrain mass ratios of various ejecta species synthesized during explosion. Critically, we account for the Suzaku telescope effective area calibration uncert… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.15527v1-abstract-full').style.display = 'inline'; document.getElementById('2308.15527v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.15527v1-abstract-full" style="display: none;"> The exact origins of many Type Ia supernovae$\unicode{x2013}$progenitor scenarios and explosive mechanisms$\unicode{x2013}$remain uncertain. In this work, we analyze the global Suzaku X-Ray spectrum of Kepler's supernova remnant in order to constrain mass ratios of various ejecta species synthesized during explosion. Critically, we account for the Suzaku telescope effective area calibration uncertainties of 5$\unicode{x2013}$20% by generating 100 mock effective area curves and using Markov Chain Monte Carlo based spectral fitting to produce 100 sets of best-fit parameter values. Additionally, we characterize the uncertainties from assumptions made about the emitting volumes of each model plasma component: finding that these uncertainties can be the dominant source of error. We then compare our calculated mass ratios to previous observational studies of Kepler's SNR and to the predictions of SN Ia simulations. Our mass ratio estimates require a $\sim$90% attenuated $^{12}$C$+^{16}$O reaction rate and are potentially consistent with both near- and sub-M$_{\rm Ch}$ progenitors, but are inconsistent with the dynamically stable double detonation origin scenario and only marginally consistent with the dynamically unstable dynamically-driven double-degenerate double detonation (D$^6$) scenario. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.15527v1-abstract-full').style.display = 'none'; document.getElementById('2308.15527v1-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 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 12 figures, 4 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.13101">arXiv:2308.13101</a> <span> [<a href="https://arxiv.org/pdf/2308.13101">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1017/pasa.2024.66">10.1017/pasa.2024.66 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Probing the Soft X-ray Properties and Multi-Wavelength Variability of SN2023ixf and its Progenitor </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Panjkov%2C+S">Sonja Panjkov</a>, <a href="/search/astro-ph?searchtype=author&query=Auchettl%2C+K">Katie Auchettl</a>, <a href="/search/astro-ph?searchtype=author&query=Shappee%2C+B+J">Benjamin J. Shappee</a>, <a href="/search/astro-ph?searchtype=author&query=Do%2C+A">Aaron Do</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Beacom%2C+J+F">John F. Beacom</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2308.13101v4-abstract-short" style="display: inline;"> We present a detailed analysis of nearly two decades of optical/UV and X-ray data to study the multi-wavelength pre-explosion properties and post-explosion X-ray properties of nearby SN2023ixf located in M101. We find no evidence of precursor activity in the optical to UV down to a luminosity of $\lesssim 7\times10^{4}\, \rm L_{\odot}$, while X-ray observations covering nearly 18 years prior to ex… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.13101v4-abstract-full').style.display = 'inline'; document.getElementById('2308.13101v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.13101v4-abstract-full" style="display: none;"> We present a detailed analysis of nearly two decades of optical/UV and X-ray data to study the multi-wavelength pre-explosion properties and post-explosion X-ray properties of nearby SN2023ixf located in M101. We find no evidence of precursor activity in the optical to UV down to a luminosity of $\lesssim 7\times10^{4}\, \rm L_{\odot}$, while X-ray observations covering nearly 18 years prior to explosion show no evidence of luminous precursor X-ray emission down to an absorbed 0.3 - 10.0 keV X-ray luminosity of $\sim6\times10^{36}$ erg s$^{-1}$. Extensive Swift observations taken post-explosion did not detect soft X-ray emission from SN2023ixf within the first $\sim$3.3 days after first light, which suggests a mass-loss rate for the progenitor of $\lesssim5\times10^{-4}\,\rm M_{\odot}$ yr$^{-1}$ or a radius of $\lesssim4\times10^{15}$ cm for the circumstellar material. Our analysis also suggests that if the progenitor underwent a mass-loss episode, this had to occur $>$ 0.5 - 1.5 years prior to explosion, consistent with previous estimates. Swift detected soft X-rays from SN2023ixf $\sim4.25$ days after first light, and it rose to a peak luminosity of $\sim10^{39}$ erg s$^{-1}$ after 10 days and has maintained this luminosity for nearly 50 days post first light. This peak luminosity is lower than expected, given the evidence that SN2023ixf is interacting with dense material. However, this might be a natural consequence of an asymmetric circumstellar medium. X-ray spectra derived from merging all Swift observations over the first 50 days are best described by a two-component bremsstrahlung model consisting of a heavily absorbed and hotter component similar to that found using NuSTAR, and a less-absorbed, cooler component. We suggest that this soft component arises from cooling of the forward shock similar to that found in Type IIn SN2010jl. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.13101v4-abstract-full').style.display = 'none'; document.getElementById('2308.13101v4-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 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 13 figures, published in PASA</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Publ. Astron. Soc. Aust. 41 (2024) e059 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.05718">arXiv:2301.05718</a> <span> [<a href="https://arxiv.org/pdf/2301.05718">pdf</a>, <a href="https://arxiv.org/format/2301.05718">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"> Serendipitous Nebular-phase JWST Imaging of SN Ia 2021aefx: Testing the Confinement of 56-Co Decay Energy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chen%2C+N+M">Ness Mayker Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Tucker%2C+M+A">Michael A. Tucker</a>, <a href="/search/astro-ph?searchtype=author&query=Hoyer%2C+N">Nils Hoyer</a>, <a href="/search/astro-ph?searchtype=author&query=Jha%2C+S+W">Saurabh W. Jha</a>, <a href="/search/astro-ph?searchtype=author&query=Kwok%2C+L">Lindsey Kwok</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A+K">Adam K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Ashall%2C+C">Chris Ashall</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+G">Gagandeep Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">Frank Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Boquien%2C+M">M茅d茅ric Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Burns%2C+C">Chris Burns</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D">Daniel Dale</a>, <a href="/search/astro-ph?searchtype=author&query=DerKacy%2C+J+M">James M. DerKacy</a>, <a href="/search/astro-ph?searchtype=author&query=Egorov%2C+O+V">Oleg V. Egorov</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Grasha%2C+K">Kathryn Grasha</a>, <a href="/search/astro-ph?searchtype=author&query=Hassani%2C+H">Hamid Hassani</a>, <a href="/search/astro-ph?searchtype=author&query=Hoeflich%2C+P">Peter Hoeflich</a>, <a href="/search/astro-ph?searchtype=author&query=Hsiao%2C+E">Eric Hsiao</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R+S">Ralf S. Klessen</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Lu%2C+J">Jing Lu</a>, <a href="/search/astro-ph?searchtype=author&query=Morrell%2C+N">Nidia Morrell</a>, <a href="/search/astro-ph?searchtype=author&query=Orellana%2C+M">Mariana Orellana</a> , et al. (7 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2301.05718v2-abstract-short" style="display: inline;"> We present new 0.3-21 micron photometry of SN 2021aefx in the spiral galaxy NGC 1566 at +357 days after B-band maximum, including the first detection of any SN Ia at >15 micron. These observations follow earlier JWST observations of SN 2021aefx at +255 days after the time of maximum brightness, allowing us to probe the temporal evolution of the emission properties. We measure the fraction of flux… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.05718v2-abstract-full').style.display = 'inline'; document.getElementById('2301.05718v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.05718v2-abstract-full" style="display: none;"> We present new 0.3-21 micron photometry of SN 2021aefx in the spiral galaxy NGC 1566 at +357 days after B-band maximum, including the first detection of any SN Ia at >15 micron. These observations follow earlier JWST observations of SN 2021aefx at +255 days after the time of maximum brightness, allowing us to probe the temporal evolution of the emission properties. We measure the fraction of flux emerging at different wavelengths and its temporal evolution. Additionally, the integrated 0.3-14 micron decay rate of $螖m_{0.3-14} = 1.35 \pm 0.05$ mag/100 days is higher than the decline rate from the radioactive decay of $^{56}$Co of $\sim 1.2$mag/100 days. The most plausible explanation for this discrepancy is that flux is shifting to >14 micron, and future JWST observations of SNe Ia will be able to directly test this hypothesis. However, models predicting non-radiative energy loss cannot be excluded with the present data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.05718v2-abstract-full').style.display = 'none'; document.getElementById('2301.05718v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 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">Accepted for publication in ApJL; 11 pages, 4 figures, 2 tables in two-column AASTEX63 format</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.00854">arXiv:2301.00854</a> <span> [<a href="https://arxiv.org/pdf/2301.00854">pdf</a>, <a href="https://arxiv.org/format/2301.00854">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/acb0cf">10.3847/2041-8213/acb0cf <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> PHANGS-JWST First Results: Mapping the 3.3 micron Polycyclic Aromatic Hydrocarbon Vibrational Band in Nearby Galaxies with NIRCam Medium Bands </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sandstrom%2C+K">Karin Sandstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Chastenet%2C+J">J茅r茅my Chastenet</a>, <a href="/search/astro-ph?searchtype=author&query=Sutter%2C+J">Jessica Sutter</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A+K">Adam K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Egorov%2C+O+V">Oleg V. Egorov</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Bolatto%2C+A+D">Alberto D. Bolatto</a>, <a href="/search/astro-ph?searchtype=author&query=Boquien%2C+M">M茅d茅ric Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Y">Yixian Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">Daniel A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J+C">Janice C. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A+T">Ashley. T. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Belfiore%2C+F">Francesco Belfiore</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">F. Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">M茅lanie Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Grasha%2C+K">Kathryn Grasha</a>, <a href="/search/astro-ph?searchtype=author&query=Groves%2C+B">Brent Groves</a>, <a href="/search/astro-ph?searchtype=author&query=Hassani%2C+H">Hamid Hassani</a>, <a href="/search/astro-ph?searchtype=author&query=Hughes%2C+A">Annie Hughes</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R+S">Ralf S. Klessen</a>, <a href="/search/astro-ph?searchtype=author&query=Kruijssen%2C+J+M+D">J. M. Diederik Kruijssen</a>, <a href="/search/astro-ph?searchtype=author&query=Larson%2C+K+L">Kirsten L. Larson</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">Daizhong Liu</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="2301.00854v1-abstract-short" style="display: inline;"> We present maps of the 3.3 micron polycyclic aromatic hydrocarbon (PAH) emission feature in NGC 628, NGC 1365, and NGC 7496 as observed with the Near-Infrared Camera (NIRCam) imager on JWST from the PHANGS-JWST Cycle 1 Treasury project. We create maps that isolate the 3.3 micron PAH feature in the F335M filter (F335M$_{\rm PAH}$) using combinations of the F300M and F360M filters for removal of sta… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.00854v1-abstract-full').style.display = 'inline'; document.getElementById('2301.00854v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.00854v1-abstract-full" style="display: none;"> We present maps of the 3.3 micron polycyclic aromatic hydrocarbon (PAH) emission feature in NGC 628, NGC 1365, and NGC 7496 as observed with the Near-Infrared Camera (NIRCam) imager on JWST from the PHANGS-JWST Cycle 1 Treasury project. We create maps that isolate the 3.3 micron PAH feature in the F335M filter (F335M$_{\rm PAH}$) using combinations of the F300M and F360M filters for removal of starlight continuum. This continuum removal is complicated by contamination of the F360M by PAH emission and variations in the stellar spectral energy distribution slopes between 3.0 and 3.6 micron. We modify the empirical prescription from Lai et al. (2020) to remove the starlight continuum in our highly resolved galaxies, which have a range of starlight- and PAH-dominated lines-of-sight. Analyzing radially binned profiles of the F335M$_{\rm PAH}$ emission, we find that between 5-65% of the F335M intensity comes from the 3.3 micron feature within the inner 0.5 $r_{25}$ of our targets. This percentage systematically varies from galaxy to galaxy, and shows radial trends within the galaxies related to each galaxy's distribution of stellar mass, interstellar medium, and star formation. The 3.3 micron emission is well correlated with the 11.3 micron PAH feature traced with the MIRI F1130W filter, as is expected, since both features arise from C-H vibrational modes. The average F335M$_{\rm PAH}$/F1130W ratio agrees with the predictions of recent models by Draine et al. (2021) for PAHs with size and charge distributions shifted towards larger grains with normal or higher ionization. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.00854v1-abstract-full').style.display = 'none'; document.getElementById('2301.00854v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 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">submitted to AAS journals and revised according to referee comments, part of a PHANGS-JWST Focus Issue to appear 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/2212.11177">arXiv:2212.11177</a> <span> [<a href="https://arxiv.org/pdf/2212.11177">pdf</a>, <a href="https://arxiv.org/format/2212.11177">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/aca972">10.3847/2041-8213/aca972 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> PHANGS-JWST First Results: Tracing the Diffuse ISM with JWST Imaging of Polycyclic Aromatic Hydrocarbon Emission in Nearby Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sandstrom%2C+K+M">Karin M. Sandstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Koch%2C+E+W">Eric W. Koch</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A+K">Adam K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+R+J">Rowan J. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Egorov%2C+O+V">Oleg V. Egorov</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Larson%2C+K+L">Kirsten L. Larson</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J+C">Janice C. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Thilker%2C+D+A">David A. Thilker</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A+T">Ashley. T. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Belfiore%2C+F">Francesco Belfiore</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">F. Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Blanc%2C+G+A">Guillermo A. Blanc</a>, <a href="/search/astro-ph?searchtype=author&query=Bolatto%2C+A+D">Alberto D. Bolatto</a>, <a href="/search/astro-ph?searchtype=author&query=Boquien%2C+M">M茅d茅ric Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Y">Yixian Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Chastenet%2C+J">J茅r茅my Chastenet</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">M茅lanie Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Chiang%2C+I">I-Da Chiang</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=Faesi%2C+C+M">Christopher M. Faesi</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S+C+O">Simon C. O. Glover</a> , et al. (21 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2212.11177v1-abstract-short" style="display: inline;"> JWST observations of polycyclic aromatic hydrocarbon (PAH) emission provide some of the deepest and highest resolution views of the cold interstellar medium (ISM) in nearby galaxies. If PAHs are well mixed with the atomic and molecular gas and illuminated by the average diffuse interstellar radiation field, PAH emission may provide an approximately linear, high resolution, high sensitivity tracer… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.11177v1-abstract-full').style.display = 'inline'; document.getElementById('2212.11177v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.11177v1-abstract-full" style="display: none;"> JWST observations of polycyclic aromatic hydrocarbon (PAH) emission provide some of the deepest and highest resolution views of the cold interstellar medium (ISM) in nearby galaxies. If PAHs are well mixed with the atomic and molecular gas and illuminated by the average diffuse interstellar radiation field, PAH emission may provide an approximately linear, high resolution, high sensitivity tracer of diffuse gas surface density. We present a pilot study that explores using PAH emission in this way based on MIRI observations of IC 5332, NGC 628, NGC 1365, and NGC 7496 from the PHANGS-JWST Treasury. Using scaling relationships calibrated in Leroy et al. (2022), scaled F1130W provides 10--40 pc resolution and 3$蟽$ sensitivity of $危_{\rm gas} \sim 2$ M$_\odot$ pc$^{-2}$. We characterize the surface densities of structures seen at $< 7$ M$_\odot$ pc$^{-2}$ in our targets, where we expect the gas to be HI-dominated. We highlight the existence of filaments, inter-arm emission, and holes in the diffuse ISM at these low surface densities. Below $\sim 10$ M$_\odot$ pc$^{-2}$ for NGC 628, NGC 1365, and NGC 7496 the gas distribution shows a ``Swiss cheese''-like topology due to holes and bubbles pervading the relatively smooth distribution of diffuse ISM. Comparing to recent galaxy simulations, we observe similar topology for the low surface density gas, though with notable variations between simulations with different setups and resolution. Such a comparison of high resolution, low surface density gas with simulations is not possible with existing atomic and molecular gas maps, highlighting the unique power of JWST maps of PAH emission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.11177v1-abstract-full').style.display = 'none'; document.getElementById('2212.11177v1-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 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 6 figures, accepted as part of a PHANGS-JWST Focus Issue to appear 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/2212.10574">arXiv:2212.10574</a> <span> [<a href="https://arxiv.org/pdf/2212.10574">pdf</a>, <a href="https://arxiv.org/format/2212.10574">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/acaf85">10.3847/2041-8213/acaf85 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> PHANGS-JWST First Results: Mid-infrared emission traces both gas column density and heating at 100 pc scales </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A+K">Adam K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Sandstrom%2C+K">Karin Sandstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Belfiore%2C+F">Francesco Belfiore</a>, <a href="/search/astro-ph?searchtype=author&query=Bolatto%2C+A+D">Alberto D. Bolatto</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Y">Yixian Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Koch%2C+E+W">Eric W. Koch</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A+T">Ashley. T. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Be%C5%A1li%C4%87%2C+I">Ivana Be拧li膰</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">F. Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Blanc%2C+G+A">Guillermo A. Blanc</a>, <a href="/search/astro-ph?searchtype=author&query=Chastenet%2C+J">J茅r茅my Chastenet</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+N+M">Ness Mayker Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">M茅lanie Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Chown%2C+R">Ryan Chown</a>, <a href="/search/astro-ph?searchtype=author&query=Congiu%2C+E">Enrico Congiu</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">Daniel A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Egorov%2C+O+V">Oleg V. Egorov</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Eibensteiner%2C+C">Cosima Eibensteiner</a>, <a href="/search/astro-ph?searchtype=author&query=Faesi%2C+C+M">Christopher M. Faesi</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S+C+O">Simon C. O. Glover</a>, <a href="/search/astro-ph?searchtype=author&query=Grasha%2C+K">Kathryn Grasha</a>, <a href="/search/astro-ph?searchtype=author&query=Groves%2C+B">Brent Groves</a> , et al. (26 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2212.10574v2-abstract-short" style="display: inline;"> We compare mid-infrared (mid-IR), extinction-corrected H$伪$, and CO (2-1) emission at 70--160 pc resolution in the first four PHANGS-JWST targets. We report correlation strengths, intensity ratios, and power law fits relating emission in JWST's F770W, F1000W, F1130W, and F2100W bands to CO and H$伪$. At these scales, CO and H$伪$ each correlate strongly with mid-IR emission, and these correlations a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.10574v2-abstract-full').style.display = 'inline'; document.getElementById('2212.10574v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.10574v2-abstract-full" style="display: none;"> We compare mid-infrared (mid-IR), extinction-corrected H$伪$, and CO (2-1) emission at 70--160 pc resolution in the first four PHANGS-JWST targets. We report correlation strengths, intensity ratios, and power law fits relating emission in JWST's F770W, F1000W, F1130W, and F2100W bands to CO and H$伪$. At these scales, CO and H$伪$ each correlate strongly with mid-IR emission, and these correlations are each stronger than the one relating CO to H$伪$ emission. This reflects that mid-IR emission simultaneously acts as a dust column density tracer, leading to the good match with the molecular gas-tracing CO, and as a heating tracer, leading to the good match with the H$伪$. By combining mid-IR, CO, and H$伪$ at scales where the overall correlation between cold gas and star formation begins to break down, we are able to separate these two effects. We model the mid-IR above $I_谓= 0.5$~MJy sr$^{-1}$ at F770W, a cut designed to select regions where the molecular gas dominates the interstellar medium (ISM) mass. This bright emission can be described to first order by a model that combines a CO-tracing component and an H$伪$-tracing component. The best-fitting models imply that $\sim 50\%$ of the mid-IR flux arises from molecular gas heated by the diffuse interstellar radiation field, with the remaining $\sim 50\%$ associated with bright, dusty star forming regions. We discuss differences between the F770W, F1000W, F1130W bands and the continuum dominated F2100W band and suggest next steps for using the mid-IR as an ISM tracer. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.10574v2-abstract-full').style.display = 'none'; document.getElementById('2212.10574v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">49 pages, 17 figures, Section 8 provides a detailed summary, accepted for publication in ApJ Letters, part of a PHANGS-JWST Focus Issue to appear 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/2212.09766">arXiv:2212.09766</a> <span> [<a href="https://arxiv.org/pdf/2212.09766">pdf</a>, <a href="https://arxiv.org/format/2212.09766">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/acab00">10.3847/1538-4357/acab00 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Comparing the Locations of Supernovae to CO (2-1) Emission in their Host Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chen%2C+N+M">Ness Mayker Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A+K">Adam K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Benincasa%2C+S">Samantha Benincasa</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">M茅lanie Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S+C+O">Simon C. O. Glover</a>, <a href="/search/astro-ph?searchtype=author&query=Hughes%2C+A">Annie Hughes</a>, <a href="/search/astro-ph?searchtype=author&query=Kreckel%2C+K">Kathryn Kreckel</a>, <a href="/search/astro-ph?searchtype=author&query=Sarbadhicary%2C+S">Sumit Sarbadhicary</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+J">Jiayi Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+T+A">Todd A. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Utomo%2C+D">Dyas Utomo</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">Frank Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Blanc%2C+G+A">Guillermo A. Blanc</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">Daniel A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Grasha%2C+K">Kathryn Grasha</a>, <a href="/search/astro-ph?searchtype=author&query=Kruijssen%2C+J+M+D">J. M. Diederik Kruijssen</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+H">Hsi-An Pan</a>, <a href="/search/astro-ph?searchtype=author&query=Querejeta%2C+M">Miguel Querejeta</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Watkins%2C+E+J">Elizabeth J. Watkins</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. Williams</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2212.09766v1-abstract-short" style="display: inline;"> We measure the molecular gas environment near recent ($< 100$ yr old) supernovae (SNe) using $\sim1''$ or $\leq 150$pc resolution CO (2-1) maps from the PHANGS-ALMA survey of nearby star-forming galaxies. This is arguably the first such study to approach the scales of individual massive molecular clouds ($M_{\rm mol} \gtrsim 10^{5.3}$ M$_{\odot}$). Using the Open Supernova Catalog (OSC), we identi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.09766v1-abstract-full').style.display = 'inline'; document.getElementById('2212.09766v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.09766v1-abstract-full" style="display: none;"> We measure the molecular gas environment near recent ($< 100$ yr old) supernovae (SNe) using $\sim1''$ or $\leq 150$pc resolution CO (2-1) maps from the PHANGS-ALMA survey of nearby star-forming galaxies. This is arguably the first such study to approach the scales of individual massive molecular clouds ($M_{\rm mol} \gtrsim 10^{5.3}$ M$_{\odot}$). Using the Open Supernova Catalog (OSC), we identify 63 SNe within the PHANGS-ALMA footprint. We detect CO (2-1) emission near $\sim60\%$ of the sample at 150pc resolution, compared to $\sim35\%$ of map pixels with CO (2-1) emission, and up to $\sim95\%$ of the SNe at 1kpc resolution compared to $\sim80\%$ of map pixels with CO (2-1) emission. We expect the $\sim60\%$ of SNe within the same 150pc beam as a GMC will likely interact with these clouds in the future, consistent with the observation of widespread SN-molecular gas interaction in the Milky Way, while the other $\sim40\%$ of SNe without strong CO (2-1) detections will deposit their energy in the diffuse interstellar medium (ISM), perhaps helping drive large-scale turbulence or galactic outflows. Broken down by type, we detect CO (2-1) emission at the sites of $\sim85\%$ of our 9 stripped-envelope SNe (SESNe), $\sim40\%$ of our 34 Type II SNe, and $\sim35\%$ of our 13 Type Ia SNe, indicating that SESNe are most closely associated with the brightest CO (2-1) emitting regions in our sample. Our results confirm that SN explosions are not restricted to only the densest gas, and instead exert feedback across a wide range of molecular gas densities. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.09766v1-abstract-full').style.display = 'none'; document.getElementById('2212.09766v1-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 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to ApJ; 38 pages, 12 figures, 7 tables in two-column AASTEX63 format</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.09652">arXiv:2212.09652</a> <span> [<a href="https://arxiv.org/pdf/2212.09652">pdf</a>, <a href="https://arxiv.org/format/2212.09652">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/aca973">10.3847/2041-8213/aca973 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> PHANGS-JWST First Results: Stellar Feedback-Driven Excitation and Dissociation of Molecular Gas in the Starburst Ring of NGC 1365? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">Daizhong Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Y">Yixian Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A">Adam Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Usero%2C+A">Antonio Usero</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Kruijssen%2C+J+M+D">J. M. Diederik Kruijssen</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">M茅lanie Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S+C+O">Simon C. O. Glover</a>, <a href="/search/astro-ph?searchtype=author&query=Sormani%2C+M+C">Mattia C. Sormani</a>, <a href="/search/astro-ph?searchtype=author&query=Bolatto%2C+A+D">Alberto D. Bolatto</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+J">Jiayi Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Stuber%2C+S+K">Sophia K. Stuber</a>, <a href="/search/astro-ph?searchtype=author&query=Teng%2C+Y">Yu-Hsuan Teng</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">Frank Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Be%C5%A1li%C4%87%2C+I">Ivana Be拧li膰</a>, <a href="/search/astro-ph?searchtype=author&query=Grasha%2C+K">Kathryn Grasha</a>, <a href="/search/astro-ph?searchtype=author&query=Henshaw%2C+J+D">Jonathan D. Henshaw</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A+T">Ashley. T. Barnes</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=Saito%2C+T">Toshiki Saito</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=Watkins%2C+E+J">Elizabeth J. Watkins</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+H">Hsi-An Pan</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="2212.09652v1-abstract-short" style="display: inline;"> We compare embedded young massive star clusters (YMCs) to (sub-)millimeter line observations tracing the excitation and dissociation of molecular gas in the starburst ring of NGC 1365. This galaxy hosts one of the strongest nuclear starbursts and richest populations of YMCs within 20 Mpc. Here we combine near-/mid-IR PHANGS-JWST imaging with new ALMA multi-J CO (1-0, 2-1 and 4-3) and [CI](1-0) map… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.09652v1-abstract-full').style.display = 'inline'; document.getElementById('2212.09652v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.09652v1-abstract-full" style="display: none;"> We compare embedded young massive star clusters (YMCs) to (sub-)millimeter line observations tracing the excitation and dissociation of molecular gas in the starburst ring of NGC 1365. This galaxy hosts one of the strongest nuclear starbursts and richest populations of YMCs within 20 Mpc. Here we combine near-/mid-IR PHANGS-JWST imaging with new ALMA multi-J CO (1-0, 2-1 and 4-3) and [CI](1-0) mapping, which we use to trace CO excitation via R42 = I_CO(4-3)/I_CO(2-1) and R21 = I_CO(2-1)/I_CO(1-0) and dissociation via RCICO = I_[CI](1-0)/I_CO(2-1) at 330 pc resolution. We find that the gas flowing into the starburst ring from northeast to southwest appears strongly affected by stellar feedback, showing decreased excitation (lower R42) and increased signatures of dissociation (higher RCICO) in the downstream regions. There, radiative transfer modeling suggests that the molecular gas density decreases and temperature and [CI/CO] abundance ratio increase. We compare R42 and RCICO with local conditions across the regions and find that both correlate with near-IR 2 um emission tracing the YMCs and with both PAH (11.3 um) and dust continuum (21 um) emission. In general, RCICO exhibits ~ 0.1 dex tighter correlations than R42, suggesting CI to be a more sensitive tracer of changing physical conditions in the NGC 1365 starburst than CO (4-3). Our results are consistent with a scenario where gas flows into the two arm regions along the bar, becomes condensed/shocked, forms YMCs, and then these YMCs heat and dissociate the gas. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.09652v1-abstract-full').style.display = 'none'; document.getElementById('2212.09652v1-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 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 7 figures and 2 tables in total (12 pages and 6 figures in main text). Accepted as part of a PHANGS-JWST Focus Issue to appear 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/2212.02667">arXiv:2212.02667</a> <span> [<a href="https://arxiv.org/pdf/2212.02667">pdf</a>, <a href="https://arxiv.org/format/2212.02667">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/acaaae">10.3847/2041-8213/acaaae <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The PHANGS-JWST Treasury Survey: Star Formation, Feedback, and Dust Physics at High Angular resolution in Nearby GalaxieS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J+C">Janice C. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Sandstrom%2C+K+M">Karin M. Sandstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A+K">Adam K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Thilker%2C+D+A">David A. Thilker</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Larson%2C+K+L">Kirsten L. Larson</a>, <a href="/search/astro-ph?searchtype=author&query=Egorov%2C+O+V">Oleg V. Egorov</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Schmidt%2C+J">Judy Schmidt</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+G+S">Gagandeep S. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A+T">Ashley T. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Belfiore%2C+F">Francesco Belfiore</a>, <a href="/search/astro-ph?searchtype=author&query=Beslic%2C+I">Ivana Beslic</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">Frank Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Blanc%2C+G+A">Guillermo A. Blanc</a>, <a href="/search/astro-ph?searchtype=author&query=Bolatto%2C+A+D">Alberto D. Bolatto</a>, <a href="/search/astro-ph?searchtype=author&query=Boquien%2C+M">Mederic Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Brok%2C+J+d">Jakob den Brok</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Y">Yixian Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Chandar%2C+R">Rupali Chandar</a>, <a href="/search/astro-ph?searchtype=author&query=Chastenet%2C+J">Jeremy Chastenet</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">Melanie Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Chiang%2C+I">I-Da Chiang</a> , et al. (52 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2212.02667v1-abstract-short" style="display: inline;"> The PHANGS collaboration has been building a reference dataset for the multi-scale, multi-phase study of star formation and the interstellar medium in nearby galaxies. With the successful launch and commissioning of JWST, we can now obtain high-resolution infrared imaging to probe the youngest stellar populations and dust emission on the scales of star clusters and molecular clouds ($\sim$5-50 pc)… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.02667v1-abstract-full').style.display = 'inline'; document.getElementById('2212.02667v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.02667v1-abstract-full" style="display: none;"> The PHANGS collaboration has been building a reference dataset for the multi-scale, multi-phase study of star formation and the interstellar medium in nearby galaxies. With the successful launch and commissioning of JWST, we can now obtain high-resolution infrared imaging to probe the youngest stellar populations and dust emission on the scales of star clusters and molecular clouds ($\sim$5-50 pc). In Cycle 1, PHANGS is conducting an 8-band imaging survey from 2-21$渭$m of 19 nearby spiral galaxies. CO(2-1) mapping, optical integral field spectroscopy, and UV-optical imaging for all 19 galaxies have been obtained through large programs with ALMA, VLT/MUSE, and Hubble. PHANGS-JWST enables a full inventory of star formation, accurate measurement of the mass and age of star clusters, identification of the youngest embedded stellar populations, and characterization of the physical state of small dust grains. When combined with Hubble catalogs of $\sim$10,000 star clusters, MUSE spectroscopic mapping of $\sim$20,000 HII regions, and $\sim$12,000 ALMA-identified molecular clouds, it becomes possible to measure the timescales and efficiencies of the earliest phases of star formation and feedback, build an empirical model of the dependence of small dust grain properties on local ISM conditions, and test our understanding of how dust-reprocessed starlight traces star formation activity, all across a diversity of galactic environments. Here we describe the PHANGS-JWST Treasury survey, present the remarkable imaging obtained in the first few months of science operations, and provide context for the initial results presented in the first series of PHANGS-JWST publications. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.02667v1-abstract-full').style.display = 'none'; document.getElementById('2212.02667v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Re-submitted after addressing minor comments from referee. To be published as part of PHANGS-JWST ApJL Focus Issue</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.02514">arXiv:2212.02514</a> <span> [<a href="https://arxiv.org/pdf/2212.02514">pdf</a>, <a href="https://arxiv.org/format/2212.02514">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"> A Multiwavelength Study of the Massive Colliding Wind Binary WR 20a: A Possible Progenitor for Fast-Spinning LIGO Binary Black Hole Mergers </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Olivier%2C+G+M">Grace M. Olivier</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Auchettl%2C+K">Katie Auchettl</a>, <a href="/search/astro-ph?searchtype=author&query=Rosen%2C+A+L">Anna L. Rosen</a>, <a href="/search/astro-ph?searchtype=author&query=Batta%2C+A">Aldo Batta</a>, <a href="/search/astro-ph?searchtype=author&query=Neugent%2C+K+F">Kathryn F. Neugent</a>, <a href="/search/astro-ph?searchtype=author&query=Ramirez-Ruiz%2C+E">Enrico Ramirez-Ruiz</a>, <a href="/search/astro-ph?searchtype=author&query=Jayasinghe%2C+T">Tharindu Jayasinghe</a>, <a href="/search/astro-ph?searchtype=author&query=Vallely%2C+P+J">Patrick J. Vallely</a>, <a href="/search/astro-ph?searchtype=author&query=Rowan%2C+D+M">Dominick M. Rowan</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2212.02514v1-abstract-short" style="display: inline;"> WR 20a is the most massive close-in binary known in our Galaxy. It is composed of two $\approx$80 M$_\odot$ Wolf-Rayet stars with a short period of $\approx$3.7 days in the open cluster Westerlund 2. As such, WR 20a presents us with a unique laboratory for studying the currently uncertain physics of binary evolution and compact object formation as well as for studying the wind collision region in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.02514v1-abstract-full').style.display = 'inline'; document.getElementById('2212.02514v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.02514v1-abstract-full" style="display: none;"> WR 20a is the most massive close-in binary known in our Galaxy. It is composed of two $\approx$80 M$_\odot$ Wolf-Rayet stars with a short period of $\approx$3.7 days in the open cluster Westerlund 2. As such, WR 20a presents us with a unique laboratory for studying the currently uncertain physics of binary evolution and compact object formation as well as for studying the wind collision region in an massive eclipsing binary system. We use deep Chandra observations of WR 20a to study the time variability of the wind collision region between the two Wolf-Rayet stars and are able to produce an X-ray light curve covering $\approx$2/3 of its orbital period. We find that the X-ray light curve is asymmetric because the flux of one peak is 2.5$蟽$ larger than the flux of the other peak. This asymmetry could be caused by asymmetric mass-loss from the two stars or by the lopsidedness of the wind collision region due to the unusually fast rotation of the system. The X-ray light curve is also shifted in phase space when compared to the optical light curves measured by TESS and ASAS-SN. Additionally, we explore the ultimate fate of this system by modeling the resultant binary black hole merger expected at the end of the two stars' lives. We conclude that this system will evolve to be a representative of the sub-population of LIGO progenitors of fast-spinning binary black hole merger events. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.02514v1-abstract-full').style.display = 'none'; document.getElementById('2212.02514v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 5 figures, 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/2212.00812">arXiv:2212.00812</a> <span> [<a href="https://arxiv.org/pdf/2212.00812">pdf</a>, <a href="https://arxiv.org/format/2212.00812">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/aca7b9">10.3847/2041-8213/aca7b9 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> PHANGS-JWST First Results: Multi-wavelength view of feedback-driven bubbles (The Phantom Voids) across NGC 628 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A+T">Ashley T. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Watkins%2C+E+J">Elizabeth J. Watkins</a>, <a href="/search/astro-ph?searchtype=author&query=Meidt%2C+S+E">Sharon E. Meidt</a>, <a href="/search/astro-ph?searchtype=author&query=Kreckel%2C+K">Kathryn Kreckel</a>, <a href="/search/astro-ph?searchtype=author&query=Sormani%2C+M+C">Mattia C. Sormani</a>, <a href="/search/astro-ph?searchtype=author&query=Tress%2C+R+G">Robin G. Tress</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S+C+O">Simon C. O. Glover</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">Frank Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Chandar%2C+R">Rupali Chandar</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J+C">Janice C. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A+K">Adam K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Sandstrom%2C+K+M">Karin M. Sandstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E+W">Erik W. Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Belfiore%2C+F">Francesco Belfiore</a>, <a href="/search/astro-ph?searchtype=author&query=Blanc%2C+G">Guillermo Blanc</a>, <a href="/search/astro-ph?searchtype=author&query=Boquien%2C+M">Mederic Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Brok%2C+J+S+d">Jakob S. den Brok</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Y">Yixian Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">M茅lanie Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">Daniel A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Egorov%2C+O">Oleg Egorov</a>, <a href="/search/astro-ph?searchtype=author&query=Eibensteiner%2C+C">Cosima Eibensteiner</a>, <a href="/search/astro-ph?searchtype=author&query=Grasha%2C+K">Kathryn Grasha</a> , et al. (29 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2212.00812v1-abstract-short" style="display: inline;"> We present a high-resolution view of bubbles within The Phantom Galaxy (NGC 628); a nearby (~10Mpc), star-forming (~2Msun/yr), face-on (i~9deg) grand-design spiral galaxy. With new data obtained as part of the PHANGS-JWST treasury program, we perform a detailed case-study of two regions of interest, one of which contains the largest and most prominent bubble in the galaxy (The Phantom Void; over 1… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.00812v1-abstract-full').style.display = 'inline'; document.getElementById('2212.00812v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.00812v1-abstract-full" style="display: none;"> We present a high-resolution view of bubbles within The Phantom Galaxy (NGC 628); a nearby (~10Mpc), star-forming (~2Msun/yr), face-on (i~9deg) grand-design spiral galaxy. With new data obtained as part of the PHANGS-JWST treasury program, we perform a detailed case-study of two regions of interest, one of which contains the largest and most prominent bubble in the galaxy (The Phantom Void; over 1kpc in diameter), and the other being a smaller region that may be the precursor to such a large bubble (The Precursor Phantom Void). When comparing to matched resolution Halpha observations from the Hubble Space Telescope (HST), we see that the ionized gas is brightest in the shells of both bubbles, and is coincident with the youngest (~1Myr) and most massive (~100,000Msun) stellar associations. We also find an older generation (~20Myr) of stellar associations is present within the bubble of The Phantom Void. From our kinematic analysis of the HI, H2 (CO) and HII gas across The Phantom Void, we infer a high expansion speed of around 15 to 50km/s. The large size and high expansion speed of The Phantom Void suggest that the driving mechanism is sustained stellar feedback due to multiple mechanisms, where early feedback first cleared a bubble (as we observe now in The Precursor Phantom Void), and since then SNe have been exploding within the cavity, and have accelerated the shell. Finally, comparison to simulations shows a striking resemblance to our JWST observations, and suggests that such large-scale stellar feedback-driven bubbles should be common within other galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.00812v1-abstract-full').style.display = 'none'; document.getElementById('2212.00812v1-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 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages total, 8 figures, and 1 table. Accepted as part of a PHANGS-JWST Focus Issue to appear 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/2212.00811">arXiv:2212.00811</a> <span> [<a href="https://arxiv.org/pdf/2212.00811">pdf</a>, <a href="https://arxiv.org/format/2212.00811">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/aca6e4">10.3847/2041-8213/aca6e4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> PHANGS-JWST First Results: A statistical view on bubble evolution in NGC628 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Watkins%2C+E+J">Elizabeth J. Watkins</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A">Ashley Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Henny%2C+K+F">Kiana F. Henny</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+H">Hwihyun Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kreckel%2C+K">Kathryn Kreckel</a>, <a href="/search/astro-ph?searchtype=author&query=Meidt%2C+S+E">Sharon E. Meidt</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R+S">Ralf S. Klessen</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S+C+O">Simon C. O. Glover</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Keller%2C+B+W">B. W. Keller</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A+K">Adam K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E+W">Erik W. Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Boquien%2C+M">Mederic Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+G+S">Gagandeep S. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Belfiore%2C+F">Francesco Belfiore</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">Frank Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Blanc%2C+G">Guillermo Blanc</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Y">Yixian Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Chandar%2C+R">Rupali Chandar</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+N+M">Ness Mayker Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">M茅lanie Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Congiu%2C+E">Enrico Congiu</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">Daniel A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Deger%2C+S">Sinan Deger</a>, <a href="/search/astro-ph?searchtype=author&query=Egorov%2C+O">Oleg Egorov</a> , et al. (27 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2212.00811v1-abstract-short" style="display: inline;"> The first JWST observations of nearby galaxies have unveiled a rich population of bubbles that trace the stellar feedback mechanisms responsible for their creation. Studying these bubbles therefore allows us to chart the interaction between stellar feedback and the interstellar medium, and the larger galactic flows needed to regulate star formation processes globally. We present the first catalog… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.00811v1-abstract-full').style.display = 'inline'; document.getElementById('2212.00811v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.00811v1-abstract-full" style="display: none;"> The first JWST observations of nearby galaxies have unveiled a rich population of bubbles that trace the stellar feedback mechanisms responsible for their creation. Studying these bubbles therefore allows us to chart the interaction between stellar feedback and the interstellar medium, and the larger galactic flows needed to regulate star formation processes globally. We present the first catalog of bubbles in NGC628, visually identified using MIRI F770W PHANGS-JWST observations, and use them to statistically evaluate bubble characteristics. We classify 1694 structures as bubbles with radii between 6-552 pc. Of these, 31% contain at least one smaller bubble at their edge, indicating that previous generations of star formation have a local impact on where new stars form. On large scales, most bubbles lie near a spiral arm, and their radii increase downstream compared to upstream. Furthermore, bubbles are elongated in a similar direction to the spiral arm ridge-line. These azimuthal trends demonstrate that star formation is intimately connected to the spiral arm passage. Finally, the bubble size distribution follows a power-law of index $p=-2.2\pm0.1$, which is slightly shallower than the theoretical value by 1-3.5$蟽$ that did not include bubble mergers. The fraction of bubbles identified within the shells of larger bubbles suggests that bubble merging is a common process. Our analysis therefore allows us to quantify the number of star-forming regions that are influenced by an earlier generation, and the role feedback processes have in setting the global star formation rate. With the full PHANGS-JWST sample, we can do this for more galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.00811v1-abstract-full').style.display = 'none'; document.getElementById('2212.00811v1-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 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages total, 13 Figures and 1 Table. Accepted for publication in ApJL as part of a PHANGS-JWST First Results Focus issue</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.07193">arXiv:2210.07193</a> <span> [<a href="https://arxiv.org/pdf/2210.07193">pdf</a>, <a href="https://arxiv.org/format/2210.07193">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/mnrasl/slac141">10.1093/mnrasl/slac141 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Dynamics of hot galactic winds launched from spherically-stratified starburst cores </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Nguyen%2C+D+D">Dustin D. Nguyen</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+T+A">Todd A. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Schneider%2C+E+E">Evan E. Schneider</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+S">Sebastian Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</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="2210.07193v2-abstract-short" style="display: inline;"> The analytic galactic wind model derived by Chevalier and Clegg in 1985 (CC85) assumes $\textit{uniform}$ energy and mass-injection within the starburst galaxy nucleus. However, the structure of nuclear star clusters, bulges, and star-forming knots are non-uniform. We generalize to cases with spherically-symmetric energy/mass injection that scale as $r^{-螖}$ within the starburst volume $R$, provid… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.07193v2-abstract-full').style.display = 'inline'; document.getElementById('2210.07193v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.07193v2-abstract-full" style="display: none;"> The analytic galactic wind model derived by Chevalier and Clegg in 1985 (CC85) assumes $\textit{uniform}$ energy and mass-injection within the starburst galaxy nucleus. However, the structure of nuclear star clusters, bulges, and star-forming knots are non-uniform. We generalize to cases with spherically-symmetric energy/mass injection that scale as $r^{-螖}$ within the starburst volume $R$, providing solutions for $螖= 0$, 1/2, 1, 3/2, and 2. In marked contrast with the CC85 model ($螖=0$), which predicts zero velocity at the center, for a singular isothermal sphere profile ($螖=2$), we find that the flow maintains a $\textit{constant}$ Mach number of $\mathcal{M}=\sqrt{3/5} \simeq 0.77$ throughout the volume. The fast interior flow can be written as $v_{r < R} = (\dot{E}_T/3\dot{M}_T)^{1/2} \simeq 0.41 \, v_\infty$, where $v_\infty$ is the asymptotic velocity, and $\dot{E}_T$ and $\dot{M}_T$ are the total energy and mass injection rates. For $v_\infty \simeq 2000 \, \mathrm{km \, s^{-1}}$, $v_{r<R} \simeq 820 \, \mathrm{km\, s^{-1}}$ throughout the wind-driving region. The temperature and density profiles of the non-uniform models may be important for interpreting spatially-resolved maps of starburst nuclei. We compute velocity resolved spectra to contrast the $螖=0$ (CC85) and $螖=2$ models. Next generation X-ray space telescopes such as XRISM may assess these kinematic predictions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.07193v2-abstract-full').style.display = 'none'; document.getElementById('2210.07193v2-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 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 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">submitted (13 October 2022), accepted MNRAS Letters (08 November 2022)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.10554">arXiv:2209.10554</a> <span> [<a href="https://arxiv.org/pdf/2209.10554">pdf</a>, <a href="https://arxiv.org/format/2209.10554">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> <p class="title is-5 mathjax"> On Odd Radio Circles as Supernova Remnants </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sarbadhicary%2C+S+K">Sumit K. Sarbadhicary</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+T+A">Todd A. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Mathur%2C+S">Smita Mathur</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="2209.10554v1-abstract-short" style="display: inline;"> The origin of arcmin-sized Odd Radio Circles (ORCs) found in modern all-sky radio surveys remain uncertain, with explanations ranging from starburst/AGN-driven shocks to supernova remnants (SNRs) in the low-density ambient medium. Using well-calibrated radio light curve models, we assess the possibility that ORCs are radio SNRs evolving in low ambient densities. Our models imply that ORCs 1-5 and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.10554v1-abstract-full').style.display = 'inline'; document.getElementById('2209.10554v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.10554v1-abstract-full" style="display: none;"> The origin of arcmin-sized Odd Radio Circles (ORCs) found in modern all-sky radio surveys remain uncertain, with explanations ranging from starburst/AGN-driven shocks to supernova remnants (SNRs) in the low-density ambient medium. Using well-calibrated radio light curve models, we assess the possibility that ORCs are radio SNRs evolving in low ambient densities. Our models imply that ORCs 1-5 and J0624-6948 (near the LMC) as SNRs must be within 200 kpc and 100 kpc from the Sun respectively, given their observed flux densities and angular sizes. To be evolving in the circumgalactic medium of the Milky Way, our models require ORCs 1-5 to be ejecta-dominated SNRs within 50 kpc, evolving in ambient densities of $(0.2-1.2) \times 10^{-3}$ cm$^{-3}$. However, this is statistically unlikely because ORCs 1-5 would have ages $<640$ yrs, much smaller than their expected lifetimes of $\gtrsim$10$^5$ yrs at these densities, and because the low SN rate and steep profile of the stellar halo imply a negligible number of ORC-like SNRs within 50 kpc. The circumgalactic medium SNR scenario for J0624-6948 is more likely (though still low probability) compared to ORCs 1-5, as our models allow J0624-6948 to be $\lesssim$3000 yrs. On the other hand, the interpretation of J0624-6948 as a Sedov-Taylor SNR at 50 kpc (LMC) distance is possible for a wide range of ambient densities ($6 \times 10^{-4} - 0.5$ cm$^{-3}$) and ages $\sim$$(0.2-2.6) \times 10^4$ yr, while also being consistent with the local HI environment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.10554v1-abstract-full').style.display = 'none'; document.getElementById('2209.10554v1-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 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">9 pages, 4 figures. Submitted to MNRAAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.09260">arXiv:2209.09260</a> <span> [<a href="https://arxiv.org/pdf/2209.09260">pdf</a>, <a href="https://arxiv.org/format/2209.09260">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/10.3847/1538-4357/aca65e">10.3847/1538-4357/aca65e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> X-ray Properties of NGC 253's Starburst-Driven Outflow </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+S">Sebastian Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Nguyen%2C+D+D">Dustin D. Nguyen</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+T+A">Todd A. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Mathur%2C+S">Smita Mathur</a>, <a href="/search/astro-ph?searchtype=author&query=Bolatto%2C+A+D">Alberto D. Bolatto</a>, <a href="/search/astro-ph?searchtype=author&query=Vulic%2C+N">Neven Vulic</a>, <a href="/search/astro-ph?searchtype=author&query=Sardone%2C+A">Amy Sardone</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.09260v2-abstract-short" style="display: inline;"> We analyze image and spectral data from $\approx$365~ks of observations from the {\it Chandra} X-ray Observatory of the nearby, edge-on starburst galaxy NGC 253 to constrain properties of the hot phase of the outflow. We focus our analysis on the $-$1.1 to $+$0.63 kpc region of the outflow and define several regions for spectral extraction where we determine best-fit temperatures and metal abundan… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.09260v2-abstract-full').style.display = 'inline'; document.getElementById('2209.09260v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.09260v2-abstract-full" style="display: none;"> We analyze image and spectral data from $\approx$365~ks of observations from the {\it Chandra} X-ray Observatory of the nearby, edge-on starburst galaxy NGC 253 to constrain properties of the hot phase of the outflow. We focus our analysis on the $-$1.1 to $+$0.63 kpc region of the outflow and define several regions for spectral extraction where we determine best-fit temperatures and metal abundances. We find that the temperatures and electron densities peak in the central $\sim$250 pc region of the outflow and decrease with distance. These temperature and density profiles are in disagreement with an adiabatic spherically expanding starburst wind model and suggest the presence of additional physics such as mass loading and non-spherical outflow geometry. Our derived temperatures and densities yield few-Myr cooling times in the nuclear region, which may imply that the hot gas can undergo bulk radiative cooling as it escapes along the minor axis. Our metal abundances of O, Ne, Mg, Si, S, and Fe all peak in the central region and decrease with distance along the outflow, with the exception of Ne which maintains a flat distribution. The metal abundances indicate significant dilution outside of the starburst region. We also find estimates on the mass outflow rates which are $2.8\:M_{\odot}/\rm{yr}$ in the northern outflow and $3.2\:M_{\odot}/\rm{yr}$ in the southern outflow. Additionally, we detect emission from charge exchange and find it has a significant contribution ($20-42$\%) to the total broad-band ($0.5-7$ keV) X-ray emission in the central and southern regions of the outflow. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.09260v2-abstract-full').style.display = 'none'; document.getElementById('2209.09260v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 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">15 pages, 9 figures; submitted (19 September 2022), accepted ApJ (22 November 2022)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.05679">arXiv:2205.05679</a> <span> [<a href="https://arxiv.org/pdf/2205.05679">pdf</a>, <a href="https://arxiv.org/format/2205.05679">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243766">10.1051/0004-6361/202243766 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Linking stellar populations to HII regions across nearby galaxies: I. Constraining pre-supernova feedback from young clusters in NGC1672 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A+T">A. T. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Chandar%2C+R">R. Chandar</a>, <a href="/search/astro-ph?searchtype=author&query=Kreckel%2C+K">K. Kreckel</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S+C+O">S. C. O. Glover</a>, <a href="/search/astro-ph?searchtype=author&query=Scheuermann%2C+F">F. Scheuermann</a>, <a href="/search/astro-ph?searchtype=author&query=Belfiore%2C+F">F. Belfiore</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">F. Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Blanc%2C+G+A">G. A. Blanc</a>, <a href="/search/astro-ph?searchtype=author&query=Boquien%2C+M">M. Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Brok%2C+J+d">J. den Brok</a>, <a href="/search/astro-ph?searchtype=author&query=Congiu%2C+E">E. Congiu</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">M. Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">D. A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Deger%2C+S">S. Deger</a>, <a href="/search/astro-ph?searchtype=author&query=Kruijssen%2C+J+M+D">J. M. D. Kruijssen</a>, <a href="/search/astro-ph?searchtype=author&query=Egorov%2C+O+V">O. V. Egorov</a>, <a href="/search/astro-ph?searchtype=author&query=Eibensteiner%2C+C">C. Eibensteiner</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">E. Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Grasha%2C+K">K. Grasha</a>, <a href="/search/astro-ph?searchtype=author&query=Groves%2C+B">B. Groves</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R+S">R. S. Klessen</a>, <a href="/search/astro-ph?searchtype=author&query=Hannon%2C+S">S. Hannon</a>, <a href="/search/astro-ph?searchtype=author&query=Hassani%2C+H">H. Hassani</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J+C">J. C. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A+K">A. K. Leroy</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="2205.05679v2-abstract-short" style="display: inline;"> One of the fundamental factors regulating the evolution of galaxies is stellar feedback. However, we still do not have strong observational constraints on the relative importance of the different feedback mechanisms (e.g. radiation, ionised gas pressure, stellar winds) in driving HII region evolution and molecular cloud disruption. In this letter, we constrain the relative importance of the variou… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.05679v2-abstract-full').style.display = 'inline'; document.getElementById('2205.05679v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.05679v2-abstract-full" style="display: none;"> One of the fundamental factors regulating the evolution of galaxies is stellar feedback. However, we still do not have strong observational constraints on the relative importance of the different feedback mechanisms (e.g. radiation, ionised gas pressure, stellar winds) in driving HII region evolution and molecular cloud disruption. In this letter, we constrain the relative importance of the various feedback mechanisms from young massive star populations by resolving HII regions across the disk of the nearby star-forming galaxy NGC 1672. We combine measurements of ionised gas nebular lines obtained by PHANGS-MUSE, with high-resolution imaging from the HST in both the narrow-band H伪 and broad-band filters. We identify a sample of 40 isolated, compact HII regions in the HST H伪 image, for which we measure the sizes that were previously unresolved in seeing-limited ground-based observations. Additionally, we identify the ionisation source(s) for each HII region from catalogues produced as part of the PHANGS-HST survey. We find that the HII regions investigated are mildly dominated by thermal or wind pressure, yet their elevation above the radiation pressure is within the expected uncertainty range. We see that radiation pressure provides a substantially higher contribution to the total pressure than previously found in the literature over similar size scales. In general, we find higher pressures within more compact HII regions, which is driven by the inherent size scaling relations of each pressure term, albeit with significant scatter introduced by the variation in the stellar population properties (e.g. luminosity, mass, age, metallicity). For nearby galaxies, here we provide a promising approach that could yield the statistics required to map out how the importance of different stellar feedback mechanisms evolve over the lifetime of an HII region. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.05679v2-abstract-full').style.display = 'none'; document.getElementById('2205.05679v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5(+4) pages, 6 figures, 1 table (available online), accepted for publication in A&A Letters</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 662, L6 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.02209">arXiv:2201.02209</a> <span> [<a href="https://arxiv.org/pdf/2201.02209">pdf</a>, <a href="https://arxiv.org/format/2201.02209">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/10.1051/0004-6361/202142624">10.1051/0004-6361/202142624 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A 2-3 mm high-resolution molecular line survey towards the centre of the nearby spiral galaxy NGC 6946 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Eibensteiner%2C+C">Cosima Eibensteiner</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A+T">Ashley T. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">Frank Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">Daizhong Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Meier%2C+D+S">David S. Meier</a>, <a href="/search/astro-ph?searchtype=author&query=Usero%2C+A">Antonio Usero</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A+K">Adam K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Puschnig%2C+J">Johannes Puschnig</a>, <a href="/search/astro-ph?searchtype=author&query=Lazar%2C+I">Ilin Lazar</a>, <a href="/search/astro-ph?searchtype=author&query=Pety%2C+J">J茅r么me Pety</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Be%C5%A1li%C4%87%2C+I">Ivana Be拧li膰</a>, <a href="/search/astro-ph?searchtype=author&query=Querejeta%2C+M">Miguel Querejeta</a>, <a href="/search/astro-ph?searchtype=author&query=Murphy%2C+E+J">Eric J. Murphy</a>, <a href="/search/astro-ph?searchtype=author&query=Brok%2C+J+d">Jakob den Brok</a>, <a href="/search/astro-ph?searchtype=author&query=Schruba%2C+A">Andreas Schruba</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">M茅lanie Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S+C+O">Simon C. O. Glover</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+Y">Yu Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Grasha%2C+K">Kathryn Grasha</a>, <a href="/search/astro-ph?searchtype=author&query=Hassani%2C+H">Hamid Hassani</a>, <a href="/search/astro-ph?searchtype=author&query=Henshaw%2C+J+D">Jonathan D. Henshaw</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="2201.02209v2-abstract-short" style="display: inline;"> The complex physical, kinematic, and chemical properties of galaxy centres make them interesting environments to examine with molecular line emission. We present new $2-4$" (${\sim}75{-}150$ pc at $7.7$ Mpc) observations at 2 and 3 mm covering the central $50$" (${\sim}1.9$ kpc) of the nearby double-barred spiral galaxy NGC 6946 obtained with the IRAM Plateau de Bure Interferometer. We detect spec… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.02209v2-abstract-full').style.display = 'inline'; document.getElementById('2201.02209v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.02209v2-abstract-full" style="display: none;"> The complex physical, kinematic, and chemical properties of galaxy centres make them interesting environments to examine with molecular line emission. We present new $2-4$" (${\sim}75{-}150$ pc at $7.7$ Mpc) observations at 2 and 3 mm covering the central $50$" (${\sim}1.9$ kpc) of the nearby double-barred spiral galaxy NGC 6946 obtained with the IRAM Plateau de Bure Interferometer. We detect spectral lines from ten molecules: CO, HCN, HCO$^+$, HNC, CS, HC$_3$N, N$_2$H$^+$, C$_2$H, CH$_3$OH, and H$_2$CO. We complemented these with published 1mm CO observations and 33 GHz continuum observations to explore the star formation rate surface density ${危_{\mathrm{SFR}}}$ on 150 pc scales. In this paper, we analyse regions associated with the inner bar of NGC 6946 $-$ the nuclear region (NUC), the northern (NBE), and southern inner bar end (SBE) and we focus on short-spacing corrected bulk (CO) and dense gas tracers (HCN, HCO$^+$, and HNC). We find that HCO$^+$ correlates best with ${危_{\mathrm{SFR}}}$, but the dense gas fraction ($f_{\mathrm{dense}}$) and star formation efficiency of the dense gas (${\mathrm{SFE_{dense}}}$) fits show different behaviours than expected from large-scale disc observations.The SBE has a higher ${危_{\mathrm{SFR}}}$, $f_{\mathrm{dense}}$, and shocked gas fraction than the NBE. We examine line ratio diagnostics and find a higher CO(2-1)/CO(1-0) ratio towards NBE than for the NUC. Moreover, comparison with existing extragalactic datasets suggests that using the HCN/HNC ratio to probe kinetic temperatures is not suitable on kiloparsec and sub-kiloparsec scales in extragalactic regions. Lastly, our study shows that the HCO$^+$/HCN ratio might not be a unique indicator to diagnose AGN activity in galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.02209v2-abstract-full').style.display = 'none'; document.getElementById('2201.02209v2-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">v1</span> submitted 6 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">38 pages, 23 figures, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 659, A173 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.10437">arXiv:2109.10437</a> <span> [<a href="https://arxiv.org/pdf/2109.10437">pdf</a>, <a href="https://arxiv.org/format/2109.10437">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/ac2c08">10.3847/1538-4357/ac2c08 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> ALMA Imaging of a Galactic Molecular Outflow in NGC4945 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bolatto%2C+A+D">Alberto D. Bolatto</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A+K">Adam K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Levy%2C+R+C">Rebecca C. Levy</a>, <a href="/search/astro-ph?searchtype=author&query=Meier%2C+D+S">David S. Meier</a>, <a href="/search/astro-ph?searchtype=author&query=Mills%2C+E+A+C">Elisabeth A. C. Mills</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+T+A">Todd A. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Emig%2C+K+L">Kimberly L. Emig</a>, <a href="/search/astro-ph?searchtype=author&query=Veilleux%2C+S">Sylvain Veilleux</a>, <a href="/search/astro-ph?searchtype=author&query=Ott%2C+J">Juergen Ott</a>, <a href="/search/astro-ph?searchtype=author&query=Gorski%2C+M">Mark Gorski</a>, <a href="/search/astro-ph?searchtype=author&query=Walter%2C+F">Fabian Walter</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Lenkic%2C+L">Laura Lenkic</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="2109.10437v2-abstract-short" style="display: inline;"> We present the ALMA detection of molecular outflowing gas in the central regions of NGC4945, one of the nearest starbursts and also one of the nearest hosts of an active galactic nucleus (AGN). We detect four outflow plumes in CO (3-2) at ~0.3" resolution that appear to correspond to molecular gas located near the edges of the known ionized outflow cone and its (unobserved) counterpart behind the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.10437v2-abstract-full').style.display = 'inline'; document.getElementById('2109.10437v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.10437v2-abstract-full" style="display: none;"> We present the ALMA detection of molecular outflowing gas in the central regions of NGC4945, one of the nearest starbursts and also one of the nearest hosts of an active galactic nucleus (AGN). We detect four outflow plumes in CO (3-2) at ~0.3" resolution that appear to correspond to molecular gas located near the edges of the known ionized outflow cone and its (unobserved) counterpart behind the disk. The fastest and brightest of these plumes has emission reaching observed line-of-sight projected velocities of over 450 km/s beyond systemic, equivalent to an estimated physical outflow velocity v>600 km/s for the fastest emission. Most of these plumes have corresponding emission in HCN or HCO+ (4-3). We discuss a kinematic model for the outflow emission where the molecular gas has the geometry of the ionized gas cone and shares the rotation velocity of the galaxy when ejected. We use this model to explain the velocities we observe, constrain the physical speed of the ejected material, and account for the fraction of outflowing gas that is not detected due to confusion with the galaxy disk. We estimate a total molecular mass outflow rate dMmol/dt~20 Msun/yr flowing through a surface within 100 pc of the disk midplane, likely driven by a combination of the central starburst and AGN. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.10437v2-abstract-full').style.display = 'none'; document.getElementById('2109.10437v2-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 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 12 figures, accepted by The Astrophysical Journal on September 28, 2021</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.07453">arXiv:2109.07453</a> <span> [<a href="https://arxiv.org/pdf/2109.07453">pdf</a>, <a href="https://arxiv.org/format/2109.07453">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/ac28a2">10.3847/1538-4357/ac28a2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Local Environments of Low-Redshift Supernovae </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cronin%2C+S+A">Serena A. Cronin</a>, <a href="/search/astro-ph?searchtype=author&query=Utomo%2C+D">Dyas Utomo</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A+K">Adam K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Behrens%2C+E+A">Erica A. Behrens</a>, <a href="/search/astro-ph?searchtype=author&query=Chastenet%2C+J">Jeremy Chastenet</a>, <a href="/search/astro-ph?searchtype=author&query=Holland-Ashford%2C+T">Tyler Holland-Ashford</a>, <a href="/search/astro-ph?searchtype=author&query=Koch%2C+E+W">Eric W. Koch</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Sandstrom%2C+K+M">Karin M. Sandstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. Williams</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2109.07453v1-abstract-short" style="display: inline;"> We characterize the local (2-kpc sized) environments of Type Ia, II, and Ib/c supernovae (SNe) that have recently occurred in nearby ($d\lesssim50$ Mpc) galaxies. Using ultraviolet (UV, from GALEX) and infrared (IR, from WISE) maps of 359 galaxies and a sample of 472 SNe, we measure the star formation rate surface density ($危_{\rm SFR}$) and stellar mass surface density ($危_\star$) in a 2-kpc beam… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.07453v1-abstract-full').style.display = 'inline'; document.getElementById('2109.07453v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.07453v1-abstract-full" style="display: none;"> We characterize the local (2-kpc sized) environments of Type Ia, II, and Ib/c supernovae (SNe) that have recently occurred in nearby ($d\lesssim50$ Mpc) galaxies. Using ultraviolet (UV, from GALEX) and infrared (IR, from WISE) maps of 359 galaxies and a sample of 472 SNe, we measure the star formation rate surface density ($危_{\rm SFR}$) and stellar mass surface density ($危_\star$) in a 2-kpc beam centered on each SN site. We show that core-collapse SNe are preferentially located along the resolved galactic star-forming main sequence, whereas Type Ia SNe are extended to lower values of $危_{\rm SFR}$ at fixed $危_\star$, indicative of locations inside quiescent galaxies or quiescent regions of galaxies. We also test how well the radial distribution of each SN type matches the radial distributions of UV and IR light in each host galaxy. We find that, to first order, the distributions of all types of SNe mirror that of both near-IR light (3.4 and 4.5 microns, tracing the stellar mass distribution) and mid-IR light (12 and 22 microns, tracing emission from hot, small grains), and also resemble our best-estimate $危_{\rm SFR}$. All types of SNe appear more radially concentrated than the UV emission of their host galaxies. In more detail, the distributions of Type II SNe show small statistical differences from that of near-IR light. We attribute this overall structural uniformity to the fact that within any individual galaxy, $危_{\rm SFR}$ and $危_\star$ track one another well, with variations in $危_{\rm SFR}/危_\star$ most visible when comparing between galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.07453v1-abstract-full').style.display = 'none'; document.getElementById('2109.07453v1-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 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2021. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.12397">arXiv:2107.12397</a> <span> [<a href="https://arxiv.org/pdf/2107.12397">pdf</a>, <a href="https://arxiv.org/format/2107.12397">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Blowing Bubbles around Intermediate-Mass Stars: Feedback from Main-Sequence Winds is not Enough </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rosen%2C+A+L">Anna L. Rosen</a>, <a href="/search/astro-ph?searchtype=author&query=Offner%2C+S+S+R">Stella S. R. Offner</a>, <a href="/search/astro-ph?searchtype=author&query=Foley%2C+M+M">Michael M. Foley</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</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="2107.12397v1-abstract-short" style="display: inline;"> Numerous spherical ``shells" have been observed in young star-forming environments that host low- and intermediate-mass stars. These observations suggest that these shells may be produced by isotropic stellar wind feedback from young main-sequence stars. However, the driving mechanism for these shells remains uncertain because the momentum injected by winds is too low to explain their sizes and dy… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.12397v1-abstract-full').style.display = 'inline'; document.getElementById('2107.12397v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.12397v1-abstract-full" style="display: none;"> Numerous spherical ``shells" have been observed in young star-forming environments that host low- and intermediate-mass stars. These observations suggest that these shells may be produced by isotropic stellar wind feedback from young main-sequence stars. However, the driving mechanism for these shells remains uncertain because the momentum injected by winds is too low to explain their sizes and dynamics due to their low mass-loss rates. However, these studies neglect how the wind kinetic energy is transferred to the ISM and instead assume it is instantly lost via radiation, suggesting that these shells are momentum-driven. Intermediate-mass stars have fast ($v_w \gtrsim 1000$ km/s) stellar winds and therefore the energy injected by winds should produce energy-driven adiabatic wind bubbles that are larger than momentum-driven wind bubbles. Here, we explore if energy-driven wind feedback can produce the observed shells by performing a series of 3D magneto-hydrodynamic simulations of wind feedback from intermediate-mass and high-mass stars that are placed in a magnetized, turbulent molecular cloud. We find that, for the high-mass stars modeled, energy-driven wind feedback produces $\sim$pc scale wind bubbles in molecular clouds that agree with the observed shell sizes but winds from intermediate-mass stars can not produce similar shells because of their lower mass-loss rates and velocities. Therefore, such shells must be driven by other feedback processes inherent to low- and intermediate-mass star formation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.12397v1-abstract-full').style.display = 'none'; document.getElementById('2107.12397v1-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 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">17 pages, 5 figures. Submitted to the Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2104.07739">arXiv:2104.07739</a> <span> [<a href="https://arxiv.org/pdf/2104.07739">pdf</a>, <a href="https://arxiv.org/format/2104.07739">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/ac17f3">10.3847/1538-4365/ac17f3 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> PHANGS-ALMA: Arcsecond CO(2-1) Imaging of Nearby Star-Forming Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A+K">Adam K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Hughes%2C+A">Annie Hughes</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Pety%2C+J">J茅r么me Pety</a>, <a href="/search/astro-ph?searchtype=author&query=Schruba%2C+A">Andreas Schruba</a>, <a href="/search/astro-ph?searchtype=author&query=Usero%2C+A">Antonio Usero</a>, <a href="/search/astro-ph?searchtype=author&query=Blanc%2C+G+A">Guillermo A. Blanc</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">M茅lanie Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Faesi%2C+C+M">Christopher M. Faesi</a>, <a href="/search/astro-ph?searchtype=author&query=Herrera%2C+C+N">Cinthya N. Herrera</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">Daizhong Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Meidt%2C+S+E">Sharon E. Meidt</a>, <a href="/search/astro-ph?searchtype=author&query=Querejeta%2C+M">Miguel Querejeta</a>, <a href="/search/astro-ph?searchtype=author&query=Saito%2C+T">Toshiki Saito</a>, <a href="/search/astro-ph?searchtype=author&query=Sandstrom%2C+K+M">Karin M. Sandstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+J">Jiayi Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+G+S">Gagandeep S. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A+T">Ashley T. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Behrens%2C+E+A">Erica A. Behrens</a>, <a href="/search/astro-ph?searchtype=author&query=Belfiore%2C+F">Francesco Belfiore</a>, <a href="/search/astro-ph?searchtype=author&query=Benincasa%2C+S+M">Samantha M. Benincasa</a>, <a href="/search/astro-ph?searchtype=author&query=Be%C5%A1li%C4%87%2C+I">Ivana Be拧li膰</a> , et al. (47 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="2104.07739v2-abstract-short" style="display: inline;"> We present PHANGS-ALMA, the first survey to map CO J=2-1 line emission at ~1" ~ 100pc spatial resolution from a representative sample of 90 nearby (d<~20 Mpc) galaxies that lie on or near the z=0 "main sequence" of star-forming galaxies. CO line emission traces the bulk distribution of molecular gas, which is the cold, star-forming phase of the interstellar medium. At the resolution achieved by PH… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.07739v2-abstract-full').style.display = 'inline'; document.getElementById('2104.07739v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.07739v2-abstract-full" style="display: none;"> We present PHANGS-ALMA, the first survey to map CO J=2-1 line emission at ~1" ~ 100pc spatial resolution from a representative sample of 90 nearby (d<~20 Mpc) galaxies that lie on or near the z=0 "main sequence" of star-forming galaxies. CO line emission traces the bulk distribution of molecular gas, which is the cold, star-forming phase of the interstellar medium. At the resolution achieved by PHANGS-ALMA, each beam reaches the size of a typical individual giant molecular cloud (GMC), so that these data can be used to measure the demographics, life-cycle, and physical state of molecular clouds across the population of galaxies where the majority of stars form at z=0. This paper describes the scientific motivation and background for the survey, sample selection, global properties of the targets, ALMA observations, and characteristics of the delivered ALMA data and derived data products. As the ALMA sample serves as the parent sample for parallel surveys with VLT/MUSE, HST, AstroSat, VLA, and other facilities, we include a detailed discussion of the sample selection. We detail the estimation of galaxy mass, size, star formation rate, CO luminosity, and other properties, compare estimates using different systems and provide best-estimate integrated measurements for each target. We also report the design and execution of the ALMA observations, which combine a Cycle~5 Large Program, a series of smaller programs, and archival observations. Finally, we present the first 1" resolution atlas of CO emission from nearby galaxies and describe the properties and contents of the first PHANGS-ALMA public data release. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.07739v2-abstract-full').style.display = 'none'; document.getElementById('2104.07739v2-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 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">76 pages, 33 figures. Accepted for publication in the Astrophysical Journal Supplement series. Full resolution version and the image atlas to appear as a figure set in the published version can be found https://sites.google.com/view/phangs/publications . Data release coming soon to the ALMA archive and CADC temporarily available at http://phangs.org/data</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2102.01507">arXiv:2102.01507</a> <span> [<a href="https://arxiv.org/pdf/2102.01507">pdf</a>, <a href="https://arxiv.org/format/2102.01507">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/10.1051/0004-6361/202039170">10.1051/0004-6361/202039170 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Three-dimensional morphological asymmetries in the ejecta of Cassiopeia A using a component separation method in X-rays </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Picquenot%2C+A">Adrien Picquenot</a>, <a href="/search/astro-ph?searchtype=author&query=Acero%2C+F">Fabio Acero</a>, <a href="/search/astro-ph?searchtype=author&query=Holland-Ashford%2C+T">Tyler Holland-Ashford</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Bobin%2C+J">J茅r么me Bobin</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2102.01507v2-abstract-short" style="display: inline;"> Recent simulations have shown that asymmetries in the ejecta distribution of supernova remnants (SNR) can still reflect asymmetries from the initial supernova explosion. Thus, their study provides a great means to test and constrain model predictions in relation to the distributions of heavy elements or the neutron star kicks, both of which are key to better understanding the explosion mechanisms… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.01507v2-abstract-full').style.display = 'inline'; document.getElementById('2102.01507v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2102.01507v2-abstract-full" style="display: none;"> Recent simulations have shown that asymmetries in the ejecta distribution of supernova remnants (SNR) can still reflect asymmetries from the initial supernova explosion. Thus, their study provides a great means to test and constrain model predictions in relation to the distributions of heavy elements or the neutron star kicks, both of which are key to better understanding the explosion mechanisms in core-collapse supernovae. The use of a novel blind source separation method applied to the megasecond X-ray observations of the well-known Cassiopeia A SNR has revealed maps of the distribution of the ejecta endowed with an unprecedented level of detail and clearly separated from continuum emission. Our method also provides a three-dimensional view of the ejecta by disentangling the red- and blue-shifted spectral components and associated images of the Si, S, Ar, Ca and Fe, providing insights into the morphology of the ejecta distribution in Cassiopeia A. These mappings allow us to thoroughly investigate the asymmetries in the heavy elements distribution and probe simulation predictions about the neutron star kicks and the relative asymmetries between the different elements. We find in our study that most of the ejecta X-ray flux stems from the red-shifted component, suggesting an asymmetry in the explosion. In addition, the red-shifted ejecta can physically be described as a broad, relatively symmetric plume, whereas the blue-shifted ejecta is more similar to a dense knot. The neutron star also moves directly opposite to the red-shifted parts of the ejecta similar to what is seen with 44Ti. Regarding the morphological asymmetries, it appears that heavier elements have more asymmetrical distributions, which confirms predictions made by simulations. This study is a showcase of the capacities of new analysis methods to revisit archival observations to fully exploit their scientific content. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.01507v2-abstract-full').style.display = 'none'; document.getElementById('2102.01507v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">revised version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A Volume 646, February 2021, Article number A82 (for the published version) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.02855">arXiv:2101.02855</a> <span> [<a href="https://arxiv.org/pdf/2101.02855">pdf</a>, <a href="https://arxiv.org/format/2101.02855">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/ac1fe5">10.3847/1538-4365/ac1fe5 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The PHANGS-HST Survey: Physics at High Angular resolution in Nearby GalaxieS with the Hubble Space Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J+C">Janice C. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Whitmore%2C+B+C">Bradley C. Whitmore</a>, <a href="/search/astro-ph?searchtype=author&query=Thilker%2C+D+A">David A. Thilker</a>, <a href="/search/astro-ph?searchtype=author&query=Deger%2C+S">Sinan Deger</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=Ubeda%2C+L">Leonardo Ubeda</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+G+S">Gagandeep S. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Boquien%2C+M">Mederic Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Chandar%2C+R">Rupali Chandar</a>, <a href="/search/astro-ph?searchtype=author&query=Dale%2C+D+A">Daniel A. Dale</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A+K">Adam K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Schmidt%2C+J">Judy Schmidt</a>, <a href="/search/astro-ph?searchtype=author&query=Turner%2C+J">Jordan Turner</a>, <a href="/search/astro-ph?searchtype=author&query=Van+Dyk%2C+S">Schuyler Van Dyk</a>, <a href="/search/astro-ph?searchtype=author&query=White%2C+R+L">Richard L. White</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A+T">Ashley T. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Belfiore%2C+F">Francesco Belfiore</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">Frank Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Blanc%2C+G+A">Guillermo A. Blanc</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Y">Yixian Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">Melanie Chevance</a>, <a href="/search/astro-ph?searchtype=author&query=Congiu%2C+E">Enrico Congiu</a> , et al. (29 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2101.02855v2-abstract-short" style="display: inline;"> The PHANGS program is building the first dataset to enable the multi-phase, multi-scale study of star formation across the nearby spiral galaxy population. This effort is enabled by large survey programs with ALMA, VLT/MUSE, and HST, with which we have obtained CO(2-1) imaging, optical spectroscopic mapping, and high resolution UV-optical imaging, respectively. Here, we present PHANGS-HST, which h… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.02855v2-abstract-full').style.display = 'inline'; document.getElementById('2101.02855v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.02855v2-abstract-full" style="display: none;"> The PHANGS program is building the first dataset to enable the multi-phase, multi-scale study of star formation across the nearby spiral galaxy population. This effort is enabled by large survey programs with ALMA, VLT/MUSE, and HST, with which we have obtained CO(2-1) imaging, optical spectroscopic mapping, and high resolution UV-optical imaging, respectively. Here, we present PHANGS-HST, which has obtained five band NUV-U-B-V-I imaging of the disks of 38 spiral galaxies at distances of 4-23 Mpc, and parallel V and I band imaging of their halos, to provide a census of tens of thousands of compact star clusters, and multi-scale stellar associations. The combination of HST, ALMA, and VLT/MUSE observations will yield an unprecedented joint catalog of the observed and physical properties of ~100,000 star clusters, associations, HII regions, and molecular clouds. With these basic units of star formation, PHANGS will systematically chart the evolutionary cycling between gas and stars, across a diversity of galactic environments found in nearby galaxies. We discuss the design of the PHANGS-HST survey, and provide an overview of the HST data processing pipeline and first results, highlighting new methods for selecting star cluster candidates, morphological classification of candidates with convolutional neural networks, and identification of stellar associations over a range of physical scales with a watershed algorithm. We describe the cross-observatory imaging, catalogs, and software products to be released. These high-level science products will seed a broad range of investigations, in particular, the study of embedded stellar populations and dust with JWST, for which a PHANGS Cycle 1 Treasury program to obtain eight band 2-21 $渭$m imaging has been approved. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.02855v2-abstract-full').style.display = 'none'; document.getElementById('2101.02855v2-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 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">ApJS in press. Accepted draft includes moderate revision and updates to the originally posted submitted version. 27 pages, 11 figures, 1 table. Data products released at https://archive.stsci.edu/hlsp/phangs-hst/</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.02212">arXiv:2101.02212</a> <span> [<a href="https://arxiv.org/pdf/2101.02212">pdf</a>, <a href="https://arxiv.org/format/2101.02212">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</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/stab907">10.1093/mnras/stab907 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Unicorn in Monoceros: the $3M_\odot$ dark companion to the bright, nearby red giant V723 Mon is a non-interacting, mass-gap black hole candidate </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jayasinghe%2C+T">T. Jayasinghe</a>, <a href="/search/astro-ph?searchtype=author&query=Stanek%2C+K+Z">K. Z. Stanek</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+T+A">Todd A. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Kochanek%2C+C+S">C. S. Kochanek</a>, <a href="/search/astro-ph?searchtype=author&query=Rowan%2C+D+M">D. M. Rowan</a>, <a href="/search/astro-ph?searchtype=author&query=Vallely%2C+P+J">P. J. Vallely</a>, <a href="/search/astro-ph?searchtype=author&query=Strassmeier%2C+K+G">K. G. Strassmeier</a>, <a href="/search/astro-ph?searchtype=author&query=Weber%2C+M">M. Weber</a>, <a href="/search/astro-ph?searchtype=author&query=Hinkle%2C+J+T">J. T. Hinkle</a>, <a href="/search/astro-ph?searchtype=author&query=Hambsch%2C+F+-">F. -J. Hambsch</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+D">D. Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+J+L">J. L. Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Pessi%2C+T">T. Pessi</a>, <a href="/search/astro-ph?searchtype=author&query=Huber%2C+D">D. Huber</a>, <a href="/search/astro-ph?searchtype=author&query=Auchettl%2C+K">K. Auchettl</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">L. A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Ilyin%2C+I">I. Ilyin</a>, <a href="/search/astro-ph?searchtype=author&query=Badenes%2C+C">C. Badenes</a>, <a href="/search/astro-ph?searchtype=author&query=Howard%2C+A+W">A. W. Howard</a>, <a href="/search/astro-ph?searchtype=author&query=Isaacson%2C+H">H. Isaacson</a>, <a href="/search/astro-ph?searchtype=author&query=Murphy%2C+S+J">S. J. Murphy</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2101.02212v2-abstract-short" style="display: inline;"> We report the discovery of the closest known black hole candidate as a binary companion to V723 Mon. V723 Mon is a nearby ($d\sim460\,\rm pc$), bright ($V\simeq8.3$~mag), evolved ($T_{\rm eff, giant}\simeq4440$~K, and $L_{\rm giant}\simeq173~L_\odot$) red giant in a high mass function, $f(M)=1.72\pm 0.01~M_\odot$, nearly circular binary ($P=59.9$ d, $e\simeq 0$). V723 Mon is a known variable star,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.02212v2-abstract-full').style.display = 'inline'; document.getElementById('2101.02212v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.02212v2-abstract-full" style="display: none;"> We report the discovery of the closest known black hole candidate as a binary companion to V723 Mon. V723 Mon is a nearby ($d\sim460\,\rm pc$), bright ($V\simeq8.3$~mag), evolved ($T_{\rm eff, giant}\simeq4440$~K, and $L_{\rm giant}\simeq173~L_\odot$) red giant in a high mass function, $f(M)=1.72\pm 0.01~M_\odot$, nearly circular binary ($P=59.9$ d, $e\simeq 0$). V723 Mon is a known variable star, previously classified as an eclipsing binary, but its All-Sky Automated Survey (ASAS), Kilodegree Extremely Little Telescope (KELT), and Transiting Exoplanet Survey Satellite (TESS) light curves are those of a nearly edge-on ellipsoidal variable. Detailed models of the light curves constrained by the period, radial velocities and stellar temperature give an inclination of $87.0^\circ{}^{+1.7^{\circ}}_{-1.4^{\circ}} $, a mass ratio of $q\simeq0.33\pm0.02$, a companion mass of $M_{\rm comp}=3.04\pm0.06~M_\odot$, a stellar radius of $R_{\rm giant}=24.9\pm0.7~R_\odot$, and a giant mass of $M_{\rm giant}=1.00\pm0.07~ M_\odot$. We identify a likely non-stellar, diffuse veiling component with contributions in the $B$ and $V$-band of ${\sim}63\%$ and ${\sim}24\%$, respectively. The SED and the absence of continuum eclipses imply that the companion mass must be dominated by a compact object. We do observe eclipses of the Balmer lines when the dark companion passes behind the giant, but their velocity spreads are low compared to observed accretion disks. The X-ray luminosity of the system is $L_{\rm X}\simeq7.6\times10^{29}~\rm ergs~s^{-1}$, corresponding to $L/L_{\rm edd}{\sim}10^{-9}$. The simplest explanation for the massive companion is a single compact object, most likely a black hole in the "mass gap". <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.02212v2-abstract-full').style.display = 'none'; document.getElementById('2101.02212v2-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 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 16 figures. Accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2009.10079">arXiv:2009.10079</a> <span> [<a href="https://arxiv.org/pdf/2009.10079">pdf</a>, <a href="https://arxiv.org/format/2009.10079">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/abd24a">10.3847/1538-4357/abd24a <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Evolution of Stellar Feedback in HII Regions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Olivier%2C+G+M">Grace M. Olivier</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Rosen%2C+A+L">Anna L. Rosen</a>, <a href="/search/astro-ph?searchtype=author&query=Nayak%2C+O">Omnarayani Nayak</a>, <a href="/search/astro-ph?searchtype=author&query=Reiter%2C+M">Megan Reiter</a>, <a href="/search/astro-ph?searchtype=author&query=Krumholz%2C+M+R">Mark R. Krumholz</a>, <a href="/search/astro-ph?searchtype=author&query=Bolatto%2C+A+D">Alberto D. Bolatto</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2009.10079v2-abstract-short" style="display: inline;"> Stellar feedback is needed to produce realistic giant molecular clouds (GMCs) and galaxies in simulations, but due to limited numerical resolution, feedback must be implemented using subgrid models. Observational work is an important means to test and anchor these models, but limited studies have assessed the relative dynamical role of multiple feedback modes, particularly at the earliest stages o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.10079v2-abstract-full').style.display = 'inline'; document.getElementById('2009.10079v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.10079v2-abstract-full" style="display: none;"> Stellar feedback is needed to produce realistic giant molecular clouds (GMCs) and galaxies in simulations, but due to limited numerical resolution, feedback must be implemented using subgrid models. Observational work is an important means to test and anchor these models, but limited studies have assessed the relative dynamical role of multiple feedback modes, particularly at the earliest stages of expansion when HII regions are still deeply embedded. In this paper, we use multiwavelength (radio, infrared, and X-ray) data to measure the pressures associated with direct radiation ($P_{\rm dir}$), dust-processed radiation ($P_{\rm IR}$), photoionization heating ($P_{\rm HII}$), and shock-heating from stellar winds ($P_{\rm X}$) in a sample of 106 young, resolved HII regions with radii $\lesssim$0.5 pc to determine how stellar feedback drives their expansion. We find that the $P_{\rm IR}$ dominates in 84% of the regions and that the median $P_{\rm dir}$ and $P_{\rm HII}$ are smaller than the median $P_{\rm IR}$ by factors of $\approx 6$ and $\approx 9$, respectively. Based on the radial dependences of the pressure terms, we show that HII regions transition from $P_{\rm IR}$-dominated to $P_{\rm HII}$-dominated at radii of $\sim$3 pc. We find a median trapping factor of $f_{\rm trap} \sim$ 8 without any radial dependence for the sample, suggesting this value can be adopted in sub-grid feedback models. Moreover, we show that the total pressure is greater than the gravitational pressure in the majority of our sample, indicating that the feedback is sufficient to expel gas from the regions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.10079v2-abstract-full').style.display = 'none'; document.getElementById('2009.10079v2-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 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 8 figures, ApJ, in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2009.03321">arXiv:2009.03321</a> <span> [<a href="https://arxiv.org/pdf/2009.03321">pdf</a>, <a href="https://arxiv.org/format/2009.03321">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/10.3847/1538-4357/abe38d">10.3847/1538-4357/abe38d <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> ASASSN-14ko is a Periodic Nuclear Transient in ESO 253-G003 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Payne%2C+A+V">Anna V. Payne</a>, <a href="/search/astro-ph?searchtype=author&query=Shappee%2C+B+J">Benjamin J. Shappee</a>, <a href="/search/astro-ph?searchtype=author&query=Hinkle%2C+J+T">Jason T. Hinkle</a>, <a href="/search/astro-ph?searchtype=author&query=Vallely%2C+P+J">Patrick J. Vallely</a>, <a href="/search/astro-ph?searchtype=author&query=Kochanek%2C+C+S">Christopher S. Kochanek</a>, <a href="/search/astro-ph?searchtype=author&query=Holoien%2C+T+W+-">Thomas W. -S. Holoien</a>, <a href="/search/astro-ph?searchtype=author&query=Auchettl%2C+K">Katie Auchettl</a>, <a href="/search/astro-ph?searchtype=author&query=Stanek%2C+K+Z">K. Z. Stanek</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+T+A">Todd A. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Neustadt%2C+J+M+M">Jack M. M. Neustadt</a>, <a href="/search/astro-ph?searchtype=author&query=Tucker%2C+M+A">Michael A. Tucker</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+J+D">James D. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Brimacombe%2C+J">Joseph Brimacombe</a>, <a href="/search/astro-ph?searchtype=author&query=Cacella%2C+P">Paulo Cacella</a>, <a href="/search/astro-ph?searchtype=author&query=Cornect%2C+R">Robert Cornect</a>, <a href="/search/astro-ph?searchtype=author&query=Denneau%2C+L">Larry Denneau</a>, <a href="/search/astro-ph?searchtype=author&query=Fausnaugh%2C+M+M">Michael M. Fausnaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Flewelling%2C+H">Heather Flewelling</a>, <a href="/search/astro-ph?searchtype=author&query=Grupe%2C+D">Dirk Grupe</a>, <a href="/search/astro-ph?searchtype=author&query=Heinze%2C+A+N">A. N. Heinze</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Monard%2C+B">Berto Monard</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+J+L">Jose L. Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Schneider%2C+A+C">Adam C. Schneider</a>, <a href="/search/astro-ph?searchtype=author&query=Sheppard%2C+S+S">Scott S. Sheppard</a> , et al. (2 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2009.03321v1-abstract-short" style="display: inline;"> We present the discovery that ASASSN-14ko is a periodically flaring AGN at the center of the galaxy ESO 253-G003. At the time of its discovery by the All-Sky Automated Survey for Supernovae (ASAS-SN), it was classified as a supernova close to the nucleus. The subsequent six years of V- and g-band ASAS-SN observations reveal that ASASSN-14ko has nuclear flares occurring at regular intervals. The se… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.03321v1-abstract-full').style.display = 'inline'; document.getElementById('2009.03321v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.03321v1-abstract-full" style="display: none;"> We present the discovery that ASASSN-14ko is a periodically flaring AGN at the center of the galaxy ESO 253-G003. At the time of its discovery by the All-Sky Automated Survey for Supernovae (ASAS-SN), it was classified as a supernova close to the nucleus. The subsequent six years of V- and g-band ASAS-SN observations reveal that ASASSN-14ko has nuclear flares occurring at regular intervals. The seventeen observed outbursts show evidence of a decreasing period over time, with a mean period of $P_0 = 114.2 \pm 0.4$ days and a period derivative of $\dot{P} = -0.0017\pm0.0003$. The most recent outburst in May 2020, which took place as predicted, exhibited spectroscopic changes during the rise and a had a UV bright, blackbody spectral energy distribution similar to tidal disruption events (TDEs). The X-ray flux decreased by a factor of 4 at the beginning of the outburst and then returned to its quiescent flux after ~8 days. TESS observed an outburst during Sectors 4-6, revealing a rise time of $5.60 \pm 0.05$ days in the optical and a decline that is best fit with an exponential model. We discuss several possible scenarios to explain ASASSN-14ko's periodic outbursts, but currently favor a repeated partial TDE. The next outbursts should peak in the optical on UT 2020-09-7.4$ \pm $1.1 and UT 2020-12-26.5$ \pm $1.4. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.03321v1-abstract-full').style.display = 'none'; document.getElementById('2009.03321v1-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 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">26 pages, 15 figures, 7 tables. Will be submitted to ApJ. The latest flare is currently ongoing, as we predicted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.11593">arXiv:2007.11593</a> <span> [<a href="https://arxiv.org/pdf/2007.11593">pdf</a>, <a href="https://arxiv.org/format/2007.11593">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/10.3847/1538-4357/abb808">10.3847/1538-4357/abb808 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spatially-Resolved Study of Recombining Plasma in W49B Using XMM-Newton </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Holland-Ashford%2C+T">Tyler Holland-Ashford</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Auchettl%2C+K">Katie Auchettl</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="2007.11593v1-abstract-short" style="display: inline;"> W49B is the youngest SNR to date that exhibits recombining plasma. The two prevailing theories of this overionization are rapid cooling via adiabatic expansion or through thermal conduction with an adjacent cooler medium. To constrain the origin of the recombining plasma in W49B, we perform a spatially-resolved spectroscopic study of deep XMM-Newton data across 46 regions. We adopt a 3-component m… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.11593v1-abstract-full').style.display = 'inline'; document.getElementById('2007.11593v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.11593v1-abstract-full" style="display: none;"> W49B is the youngest SNR to date that exhibits recombining plasma. The two prevailing theories of this overionization are rapid cooling via adiabatic expansion or through thermal conduction with an adjacent cooler medium. To constrain the origin of the recombining plasma in W49B, we perform a spatially-resolved spectroscopic study of deep XMM-Newton data across 46 regions. We adopt a 3-component model (with one ISM and two ejecta components), and we find that recombining plasma is present throughout the entire SNR, with increasing overionization from east to west. The latter result is consistent with previous studies, and we attribute the overionization in the west to adiabatic expansion. However, our findings contrast these prior works as we find evidence of overionization in the east as well. As the SNR is interacting with molecular material there, we investigate the plausibility of thermal conduction as the origin of the rapid cooling. We show that based on the estimated timescales, it is possible that small-scale thermal conduction through evaporation of clumpy, dense clouds with a scale of 0.1-1.0 pc can explain the observed overionization in the east. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.11593v1-abstract-full').style.display = 'none'; document.getElementById('2007.11593v1-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, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 8 figures, 2 tables, submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2006.08681">arXiv:2006.08681</a> <span> [<a href="https://arxiv.org/pdf/2006.08681">pdf</a>, <a href="https://arxiv.org/format/2006.08681">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"> Evidence of a Type Ia Progenitor for Supernova Remnant 3C 397 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADnez-Rodr%C3%ADguez%2C+H">H茅ctor Mart铆nez-Rodr铆guez</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Auchettl%2C+K">Katie Auchettl</a>, <a href="/search/astro-ph?searchtype=author&query=Badenes%2C+C">Carles Badenes</a>, <a href="/search/astro-ph?searchtype=author&query=Holland-Ashford%2C+T">Tyler Holland-Ashford</a>, <a href="/search/astro-ph?searchtype=author&query=Patnaude%2C+D+J">Daniel J. Patnaude</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+S">Shiu-Hang Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Foster%2C+A+R">Adam R. Foster</a>, <a href="/search/astro-ph?searchtype=author&query=Slane%2C+P+O">Patrick O. Slane</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="2006.08681v1-abstract-short" style="display: inline;"> The explosive origin of the young supernova remnant (SNR) 3C 397 (G41.1-0.3) is debated. Its elongated morphology and proximity to a molecular cloud are suggestive of a core-collapse (CC) SN origin, yet recent X-ray studies of heavy metals show chemical yields and line centroid energies consistent with a Type Ia SN. In this paper, we analyze the full X-ray spectrum from 0.7-10 keV of 3C 397 observ… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.08681v1-abstract-full').style.display = 'inline'; document.getElementById('2006.08681v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.08681v1-abstract-full" style="display: none;"> The explosive origin of the young supernova remnant (SNR) 3C 397 (G41.1-0.3) is debated. Its elongated morphology and proximity to a molecular cloud are suggestive of a core-collapse (CC) SN origin, yet recent X-ray studies of heavy metals show chemical yields and line centroid energies consistent with a Type Ia SN. In this paper, we analyze the full X-ray spectrum from 0.7-10 keV of 3C 397 observed with Suzaku and compare the line centroid energies, fluxes, and elemental abundances of intermediate-mass and heavy metals (Mg to Ni) to Type Ia and CC hydrodynamical model predictions. Based on the results, we conclude that 3C 397 likely arises from an energetic Type Ia explosion in a high-density ambient medium, and we show that the progenitor was a near Chandrasekhar mass white dwarf. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.08681v1-abstract-full').style.display = 'none'; document.getElementById('2006.08681v1-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 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 4 figures, submitted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2006.08623">arXiv:2006.08623</a> <span> [<a href="https://arxiv.org/pdf/2006.08623">pdf</a>, <a href="https://arxiv.org/format/2006.08623">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/10.3847/1538-4357/abc010">10.3847/1538-4357/abc010 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Temperature and Metallicity Gradients in the Hot Gas Outflows of M82 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Mathur%2C+S">Smita Mathur</a>, <a href="/search/astro-ph?searchtype=author&query=Nguyen%2C+D+D">Dustin D. Nguyen</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+T+A">Todd A. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Olivier%2C+G+M">Grace M. Olivier</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="2006.08623v2-abstract-short" style="display: inline;"> We utilize deep Chandra X-ray Observatory imaging and spectra of M82, the prototype of a starbursting galaxy with a multiphase wind, to map the hot plasma properties along the minor axis of the galaxy. We extract spectra from 11 regions up to 2.5 kpc from the starbursting midplane and model the data as a multi-temperature, optically thin thermal plasma with contributions from a non-thermal (power-… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.08623v2-abstract-full').style.display = 'inline'; document.getElementById('2006.08623v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.08623v2-abstract-full" style="display: none;"> We utilize deep Chandra X-ray Observatory imaging and spectra of M82, the prototype of a starbursting galaxy with a multiphase wind, to map the hot plasma properties along the minor axis of the galaxy. We extract spectra from 11 regions up to 2.5 kpc from the starbursting midplane and model the data as a multi-temperature, optically thin thermal plasma with contributions from a non-thermal (power-law) component and from charge exchange (CX). We examine the gradients in best-fit parameters, including the intrinsic column density, plasma temperature, metal abundances, and number density of the hot gas as a function of distance from the M82 nucleus. We find that the temperatures and number densities of the warm-hot and hot plasma peak at the starbursting ridge and decreases along the minor axis. The temperature and density profiles are inconsistent with spherical adiabatic expansion of a super-heated wind and suggest mass loading and mixing of the hot phase with colder material. Non-thermal emission is detected in all of the regions considered, and CX comprises 8-25% of the total absorption-corrected, broad-band (0.5-7 keV) X-ray flux. We show that the abundances of O, Ne, Mg, and Fe are roughly constant across the regions considered, while Si and S peak within 500 pc of the central starburst. These findings support a direct connection between the M82 superwind and the warm-hot, metal-rich circumgalactic medium (CGM). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.08623v2-abstract-full').style.display = 'none'; document.getElementById('2006.08623v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 8 figures, ApJ in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2005.09664">arXiv:2005.09664</a> <span> [<a href="https://arxiv.org/pdf/2005.09664">pdf</a>, <a href="https://arxiv.org/ps/2005.09664">ps</a>, <a href="https://arxiv.org/format/2005.09664">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/10.3847/1538-4357/ab94a6">10.3847/1538-4357/ab94a6 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Element Stratification in the Middle-Aged Type Ia Supernova Remnant G344.7-0.1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fukushima%2C+K">Kotaro Fukushima</a>, <a href="/search/astro-ph?searchtype=author&query=Yamaguchi%2C+H">Hiroya Yamaguchi</a>, <a href="/search/astro-ph?searchtype=author&query=Slane%2C+P+O">Patrick O. Slane</a>, <a href="/search/astro-ph?searchtype=author&query=Park%2C+S">Sangwook Park</a>, <a href="/search/astro-ph?searchtype=author&query=Katsuda%2C+S">Satoru Katsuda</a>, <a href="/search/astro-ph?searchtype=author&query=Sano%2C+H">Hidetoshi Sano</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Plucinsky%2C+P+P">Paul P. Plucinsky</a>, <a href="/search/astro-ph?searchtype=author&query=Kobayashi%2C+S+B">Shogo B. Kobayashi</a>, <a href="/search/astro-ph?searchtype=author&query=Matsushita%2C+K">Kyoko Matsushita</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="2005.09664v3-abstract-short" style="display: inline;"> Despite their importance, a detailed understanding of Type Ia supernovae (SNe Ia) remains elusive. X-ray measurements of the element distributions in supernova remnants (SNRs) offer important clues for understanding the explosion and nucleosynthesis mechanisms for SNe Ia. However, it is challenging to observe the entire ejecta mass in X-rays for young SNRs, because the central ejecta may not have… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.09664v3-abstract-full').style.display = 'inline'; document.getElementById('2005.09664v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2005.09664v3-abstract-full" style="display: none;"> Despite their importance, a detailed understanding of Type Ia supernovae (SNe Ia) remains elusive. X-ray measurements of the element distributions in supernova remnants (SNRs) offer important clues for understanding the explosion and nucleosynthesis mechanisms for SNe Ia. However, it is challenging to observe the entire ejecta mass in X-rays for young SNRs, because the central ejecta may not have been heated by the reverse shock yet. Here we present over 200 kilosecond Chandra observations of the Type Ia SNR G344.7-0.1, whose age is old enough for the reverse shock to have reached the SNR center, providing an opportunity to investigate the distribution of the entire ejecta mass. We reveal a clear stratification of heavy elements with a centrally peaked distribution of the Fe ejecta surrounded by intermediate-mass elements (IMEs: Si, S, Ar Ca) with an arc-like structure. The centroid energy of the Fe K emission is marginally lower in the central Fe-rich region than in the outer IME-rich regions, suggesting that the Fe ejecta were shock-heated more recently. These results are consistent with the prediction for standard SN Ia models, where the heavier elements are synthesized in the interior of an exploding white dwarf. We find, however, that the peak location of the Fe K emission is slightly offset to the west with respect to the geometric center of the SNR. This apparent asymmetry is likely due to the inhomogeneous density distribution of the ambient medium, consistent with our radio observations of the ambient molecular and neutral gas. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.09664v3-abstract-full').style.display = 'none'; document.getElementById('2005.09664v3-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 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 May, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 10 figures, Accepted for publication in Astrophysical Journal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 897, 62 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2002.12775">arXiv:2002.12775</a> <span> [<a href="https://arxiv.org/pdf/2002.12775">pdf</a>, <a href="https://arxiv.org/format/2002.12775">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ab54ca">10.3847/1538-4357/ab54ca <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> NuSTAR observations of G11.2-0.3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Madsen%2C+K+K">K. K. Madsen</a>, <a href="/search/astro-ph?searchtype=author&query=Fryer%2C+C+L">C. L. Fryer</a>, <a href="/search/astro-ph?searchtype=author&query=Grefenstette%2C+B+W">B. W. Grefenstette</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">L. A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Reynolds%2C+S">S. Reynolds</a>, <a href="/search/astro-ph?searchtype=author&query=Zoglauer%2C+A">A. Zoglauer</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="2002.12775v2-abstract-short" style="display: inline;"> We present in this paper the hard X-ray view of the pulsar wind nebula in G11.2-0.3 and its central pulsar PSR J1811-1925 as seen by NuSTAR. We complement the data with Chandra for a more complete picture and confirm the existence of a hard, power-law component in the shell with photon index Gamma = 2.1 +/- 0.1, which we attribute to synchrotron emission. Our imaging observations of the shell show… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.12775v2-abstract-full').style.display = 'inline'; document.getElementById('2002.12775v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2002.12775v2-abstract-full" style="display: none;"> We present in this paper the hard X-ray view of the pulsar wind nebula in G11.2-0.3 and its central pulsar PSR J1811-1925 as seen by NuSTAR. We complement the data with Chandra for a more complete picture and confirm the existence of a hard, power-law component in the shell with photon index Gamma = 2.1 +/- 0.1, which we attribute to synchrotron emission. Our imaging observations of the shell show a slightly smaller radius at higher energies, consistent with Chandra results, and we find shrinkage as a function of increased energy along the jet direction, indicating that the electron outflow in the PWN may be simpler than that seen in other young PWNe. Combining NuSTAR with Integral, we find that the pulsar spectrum can be fit by a power-law with Gamma=1.32 +/- 0.07 up to 300 keV without evidence of curvature. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.12775v2-abstract-full').style.display = 'none'; document.getElementById('2002.12775v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ, 2020, 889, 23 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1912.05549">arXiv:1912.05549</a> <span> [<a href="https://arxiv.org/pdf/1912.05549">pdf</a>, <a href="https://arxiv.org/format/1912.05549">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </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/ab793a">10.3847/1538-4357/ab793a <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Catalog of M-dwarf Flares with ASAS-SN </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADnez%2C+R+R">Romy Rodr铆guez Mart铆nez</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Shappee%2C+B+J">Benjamin J. Shappee</a>, <a href="/search/astro-ph?searchtype=author&query=Schmidt%2C+S+J">Sarah J. Schmidt</a>, <a href="/search/astro-ph?searchtype=author&query=Jayasinghe%2C+T">Tharindu Jayasinghe</a>, <a href="/search/astro-ph?searchtype=author&query=Kochanek%2C+C+S">Christopher S. Kochanek</a>, <a href="/search/astro-ph?searchtype=author&query=Auchettl%2C+K">Katie Auchettl</a>, <a href="/search/astro-ph?searchtype=author&query=Holoien%2C+T+W+-">Thomas W. -S. Holoien</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="1912.05549v1-abstract-short" style="display: inline;"> We analyzed the light curves of 1376 early-to-late, nearby M dwarfs to search for white-light flares using photometry from the All-Sky Automated Survey for Supernovae (ASAS-SN). We identified 480 M dwarfs with at least one potential flare employing a simple statistical algorithm that searches for sudden increases in $V$-band flux. After more detailed evaluation, we identified 62 individual flares… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.05549v1-abstract-full').style.display = 'inline'; document.getElementById('1912.05549v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1912.05549v1-abstract-full" style="display: none;"> We analyzed the light curves of 1376 early-to-late, nearby M dwarfs to search for white-light flares using photometry from the All-Sky Automated Survey for Supernovae (ASAS-SN). We identified 480 M dwarfs with at least one potential flare employing a simple statistical algorithm that searches for sudden increases in $V$-band flux. After more detailed evaluation, we identified 62 individual flares on 62 stars. The event amplitudes range from $0.12 <螖V < 2.04$ mag. Using classical-flare models, we place lower limits on the flare energies and obtain $V$-band energies spanning $2.0\times10^{30} \lesssim E_{V} \lesssim 6.9\times10^{35}$ erg. The fraction of flaring stars increases with spectral type, and most flaring stars show moderate to strong H$伪$ emission. Additionally, we find that 14 of the 62 flaring stars are rotational variables, and they have shorter rotation periods and stronger H$伪$ emission than non-flaring rotational variable M dwarfs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.05549v1-abstract-full').style.display = 'none'; document.getElementById('1912.05549v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 December, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 5 figures, 7 tables, submitted to the AAS Journals</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1905.00311">arXiv:1905.00311</a> <span> [<a href="https://arxiv.org/pdf/1905.00311">pdf</a>, <a href="https://arxiv.org/format/1905.00311">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"> Astro2020 Science White Paper: Making the Connection between Feedback andSpatially Resolved Emission Line Diagnostics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pellegrini%2C+E+W">E. W. Pellegrini</a>, <a href="/search/astro-ph?searchtype=author&query=Drory%2C+N">N. Drory</a>, <a href="/search/astro-ph?searchtype=author&query=B.%2C+G+A">Guillermo A. B.</a>, <a href="/search/astro-ph?searchtype=author&query=Kollmeier%2C+J+A">J. A. Kollmeier</a>, <a href="/search/astro-ph?searchtype=author&query=Tuttle%2C+S+E">S. E. Tuttle</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">L. A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Simon%2C+J">Josh Simon</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+A+M">A. M. Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Avila-Reese%2C+V">V. Avila-Reese</a>, <a href="/search/astro-ph?searchtype=author&query=Kreckel%2C+K">K. Kreckel</a>, <a href="/search/astro-ph?searchtype=author&query=Yan%2C+R">R. Yan</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="1905.00311v1-abstract-short" style="display: inline;"> Crucial progress in our understanding of star formation and feedback will depend on the ability to obtain spatially resolved spectroscopic observations of \ion{H}{ii} regions, from which reliable instantaneous measurements of their physical conditions can be obtained. Acquiring these datasets across full galactic systems will prove crucial for obtaining population samples that enable us to underst… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.00311v1-abstract-full').style.display = 'inline'; document.getElementById('1905.00311v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1905.00311v1-abstract-full" style="display: none;"> Crucial progress in our understanding of star formation and feedback will depend on the ability to obtain spatially resolved spectroscopic observations of \ion{H}{ii} regions, from which reliable instantaneous measurements of their physical conditions can be obtained. Acquiring these datasets across full galactic systems will prove crucial for obtaining population samples that enable us to understand the time evolution of similar regions, and the variability of conditions among coeval regions. Separating the spatial and temporal dependencies in such way for different physical processes involved in star formation and the injection of feedback is crucial to overcome the inherit degeneracies associated with observing instantaneous snapshots of a dynamic ISM at any given time. Emission line diagnostics are at the core of measuring the physical condition in \ion{H}{ii} regions (e.g. dynamics, SFR, chemical abundances, dust extinction, ionization and excitation, etc.). These measurements require high spatial resolution, contiguous coverage across full galactic systems, and sensitivities significantly deeper than past efforts. The spatial scale required to resolve the \ion{H}{ii} regions of a few pc is only attainable in the Local Group where very large sky coverage is necessary. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.00311v1-abstract-full').style.display = 'none'; document.getElementById('1905.00311v1-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 May, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 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/1904.06357">arXiv:1904.06357</a> <span> [<a href="https://arxiv.org/pdf/1904.06357">pdf</a>, <a href="https://arxiv.org/format/1904.06357">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/10.3847/1538-4357/ab64e4">10.3847/1538-4357/ab64e4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Asymmetries of Heavy Elements in the Young Supernova Remnant Cassiopeia A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Holland-Ashford%2C+T">Tyler Holland-Ashford</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Auchettl%2C+K">Katie Auchettl</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="1904.06357v2-abstract-short" style="display: inline;"> Supernova remnants (SNRs) offer the means to study supernovae (SNe) long after the original explosion and can provide a unique insight into the mechanism that governs these energetic events. In this work, we examine the morphologies of X-ray emission from different elements found in the youngest known core-collapse (CC) SNR in the Milky Way, Cassiopeia A. The heaviest elements exhibit the highest… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.06357v2-abstract-full').style.display = 'inline'; document.getElementById('1904.06357v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.06357v2-abstract-full" style="display: none;"> Supernova remnants (SNRs) offer the means to study supernovae (SNe) long after the original explosion and can provide a unique insight into the mechanism that governs these energetic events. In this work, we examine the morphologies of X-ray emission from different elements found in the youngest known core-collapse (CC) SNR in the Milky Way, Cassiopeia A. The heaviest elements exhibit the highest levels of asymmetry, which we relate to the burning process that created the elements and their proximity to the center of explosion. Our findings support recent model predictions that the material closest to the source of explosion will reflect the asymmetries inherent to the SN mechanism. Additionally, we find that the heaviest elements are moving more directly opposed to the neutron star (NS) than the lighter elements. This result is consistent with NS kicks arising from ejecta asymmetries. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.06357v2-abstract-full').style.display = 'none'; document.getElementById('1904.06357v2-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 May, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2019. </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, 2 tables Updated to include an analysis of Emission Measure Maps (vs the, still-included, continuum-subtracted flux maps), used as another proxy for mass maps. The results have not changed; the emission measure maps also show increasing asymmetry with ejecta mass. (Now matches the version published in ApJ. Vol 889 Issue 2 (2020) 144)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ. Vol 889 Issue 2 (2020) 144 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1904.05857">arXiv:1904.05857</a> <span> [<a href="https://arxiv.org/pdf/1904.05857">pdf</a>, <a href="https://arxiv.org/format/1904.05857">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"> Astro2020 Science White Paper: Future X-ray Studies of Supernova Remnants </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Williams%2C+B+J">Brian J. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Auchettl%2C+K">Katie Auchettl</a>, <a href="/search/astro-ph?searchtype=author&query=Badenes%2C+C">Carles Badenes</a>, <a href="/search/astro-ph?searchtype=author&query=Castro%2C+D">Daniel Castro</a>, <a href="/search/astro-ph?searchtype=author&query=Kargaltsev%2C+O">Oleg Kargaltsev</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+L+A">Laura A. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Mori%2C+K">Koji Mori</a>, <a href="/search/astro-ph?searchtype=author&query=Patnaude%2C+D+J">Daniel J. Patnaude</a>, <a href="/search/astro-ph?searchtype=author&query=Plucinsky%2C+P">Paul Plucinsky</a>, <a href="/search/astro-ph?searchtype=author&query=Raymond%2C+J+C">John C. Raymond</a>, <a href="/search/astro-ph?searchtype=author&query=Safi-Harb%2C+S">Samar Safi-Harb</a>, <a href="/search/astro-ph?searchtype=author&query=Slane%2C+P">Patrick Slane</a>, <a href="/search/astro-ph?searchtype=author&query=Tanaka%2C+T">Takaaki Tanaka</a>, <a href="/search/astro-ph?searchtype=author&query=Temim%2C+T">Tea Temim</a>, <a href="/search/astro-ph?searchtype=author&query=Vink%2C+J">Jacco Vink</a>, <a href="/search/astro-ph?searchtype=author&query=Yamaguchi%2C+H">Hiroya Yamaguchi</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="1904.05857v1-abstract-short" style="display: inline;"> This is a white paper submitted in response to the call from the Astro2020 Decadal Survey Committee. We outline the scientific progress that will be made in the next few decades in the study of supernova remnants in the X-ray band, using observatories like Athena, Lynx, and AXIS. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.05857v1-abstract-full" style="display: none;"> This is a white paper submitted in response to the call from the Astro2020 Decadal Survey Committee. We outline the scientific progress that will be made in the next few decades in the study of supernova remnants in the X-ray band, using observatories like Athena, Lynx, and AXIS. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.05857v1-abstract-full').style.display = 'none'; document.getElementById('1904.05857v1-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 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2019. </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 as an Astro2020 Science White Paper</span> </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous 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