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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Harrison%2C+F&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Harrison%2C+F&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Harrison%2C+F&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Harrison%2C+F&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Harrison%2C+F&start=150" class="pagination-link " aria-label="Page 4" aria-current="page">4 </a> </li> <li> <a href="/search/?searchtype=author&query=Harrison%2C+F&start=200" class="pagination-link " aria-label="Page 5" aria-current="page">5 </a> </li> <li><span class="pagination-ellipsis">…</span></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/2411.07459">arXiv:2411.07459</a> <span> [<a href="https://arxiv.org/pdf/2411.07459">pdf</a>, <a href="https://arxiv.org/format/2411.07459">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"> The long-term variability of a population of ULXs monitored by Chandra </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Earnshaw%2C+H+P">Hannah P. Earnshaw</a>, <a href="/search/astro-ph?searchtype=author&query=Patti%2C+G">Gauri Patti</a>, <a href="/search/astro-ph?searchtype=author&query=Brightman%2C+M">Murray Brightman</a>, <a href="/search/astro-ph?searchtype=author&query=Sathyaprakash%2C+R">Rajath Sathyaprakash</a>, <a href="/search/astro-ph?searchtype=author&query=Walton%2C+D+J">Dominic J. Walton</a>, <a href="/search/astro-ph?searchtype=author&query=Fuerst%2C+F">Felix Fuerst</a>, <a href="/search/astro-ph?searchtype=author&query=Roberts%2C+T+P">Timothy P. Roberts</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F+A">Fiona A. Harrison</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.07459v1-abstract-short" style="display: inline;"> We present preliminary results of a Chandra Large Program to monitor the ultraluminous X-ray source (ULX) populations of three nearby, ULX-rich galaxies over the course of a year, finding the ULX population to show a variety of long-term variability behaviours. Of a sample of 36 ULXs, some show persistent or moderately variable flux, often with a significant relationship between hardness and lumin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.07459v1-abstract-full').style.display = 'inline'; document.getElementById('2411.07459v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.07459v1-abstract-full" style="display: none;"> We present preliminary results of a Chandra Large Program to monitor the ultraluminous X-ray source (ULX) populations of three nearby, ULX-rich galaxies over the course of a year, finding the ULX population to show a variety of long-term variability behaviours. Of a sample of 36 ULXs, some show persistent or moderately variable flux, often with a significant relationship between hardness and luminosity, consistent with a supercritically accreting source with varying accretion rates. Six show very high-amplitude variability with no strong relationship between luminosity and hardness, though not all of them show evidence of any long-term periodicity, nor of the bimodal distribution indicative of the propeller effect. We find evidence of additional eclipses for two previously-identified eclipsing ULXs. Additionally, many sources that were previously identified as ULXs in previous studies were not detected at ULX luminosities during our monitoring campaign, indicating a large number of transient ULXs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.07459v1-abstract-full').style.display = 'none'; document.getElementById('2411.07459v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">7 pages, 4 figures, to be published in Proceedings of the XMM-Newton Workshop 2024 "The X-ray Mysteries of Neutron Stars and White Dwarfs", Astronomische Nachrichten, 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/2410.07342">arXiv:2410.07342</a> <span> [<a href="https://arxiv.org/pdf/2410.07342">pdf</a>, <a href="https://arxiv.org/format/2410.07342">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"> An Intermediate Mass Black Hole Hidden Behind Thick Obscuration </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Boorman%2C+P+G">Peter G. Boorman</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Assef%2C+R+J">Roberto J. Assef</a>, <a href="/search/astro-ph?searchtype=author&query=Borkar%2C+A">Abhijeet Borkar</a>, <a href="/search/astro-ph?searchtype=author&query=Brightman%2C+M">Murray Brightman</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+J">Johannes Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+C">Chien-Ting Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Earnshaw%2C+H+P">Hannah P. Earnshaw</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F+A">Fiona A. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Matzeu%2C+G+A">Gabriele A. Matzeu</a>, <a href="/search/astro-ph?searchtype=author&query=Pfeifle%2C+R+W">Ryan W. Pfeifle</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Svoboda%2C+J">Ji艡铆 Svoboda</a>, <a href="/search/astro-ph?searchtype=author&query=Torres-Alb%C3%A0%2C+N">N煤ria Torres-Alb脿</a>, <a href="/search/astro-ph?searchtype=author&query=Zaw%2C+I">Ingyin Zaw</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.07342v1-abstract-short" style="display: inline;"> Recent models suggest approximately half of all accreting supermassive black holes (SMBHs; $M_{\rm BH}$ $\gtrsim$ 10$^{5}$ M$_{\odot}$) are expected to undergo intense growth phases behind Compton-thick ($N_{\rm H}$ $>$ 1.5 $\times$ 10$^{24}$ cm$^{-2}$) veils of obscuring gas. However, despite being a viable source for the seeding of SMBHs, there are currently no examples known of a Compton-thick… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.07342v1-abstract-full').style.display = 'inline'; document.getElementById('2410.07342v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.07342v1-abstract-full" style="display: none;"> Recent models suggest approximately half of all accreting supermassive black holes (SMBHs; $M_{\rm BH}$ $\gtrsim$ 10$^{5}$ M$_{\odot}$) are expected to undergo intense growth phases behind Compton-thick ($N_{\rm H}$ $>$ 1.5 $\times$ 10$^{24}$ cm$^{-2}$) veils of obscuring gas. However, despite being a viable source for the seeding of SMBHs, there are currently no examples known of a Compton-thick accreting intermediate mass black hole (IMBH; $M_{\rm BH}$ $\sim$ 10$^{2}$ $-$ 10$^{5}$ M$_{\odot}$). We present a detailed X-ray spectral analysis of IC 750 $-$ the only AGN to-date with a precise megamaser-based intermediate mass $<$ 10$^{5}$ M$_{\odot}$. We find the equivalent width of neutral 6.4 keV Fe K$伪$ to be 1.9$^{+2.2}_{-1.0}$ keV via phenomenological modelling of the co-added 177 ks Chandra spectrum. Such large equivalent widths are seldom produced by processes other than fluorescence from dense obscuration. We fit three physically-motivated X-ray spectral models to infer a range of possible intrinsic 2$-$10 keV luminosity posteriors that encompass the systematic uncertainties associated with a choice of model. Despite a wide range of predicted intrinsic 2$-$10 keV luminosities between $\sim$ 10$^{41}$ and 10$^{43}$ erg s$^{-1}$, all three models agree that IC 750 has a Compton-thick line-of-sight column density to $>$ 99\% confidence. Compton-thick obscuration is well-documented to impinge substantial bias on the pursuit of SMBH AGN. Our results thus provide the first indication that Compton-thick obscuration should also be properly considered to uncover and understand the IMBH population in an unbiased manner. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.07342v1-abstract-full').style.display = 'none'; document.getElementById('2410.07342v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ. 15 pages, 6 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/2410.07339">arXiv:2410.07339</a> <span> [<a href="https://arxiv.org/pdf/2410.07339">pdf</a>, <a href="https://arxiv.org/format/2410.07339">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <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 NuSTAR Local AGN $N_{\rm H}$ Distribution Survey (NuLANDS) I: Towards a Truly Representative Column Density Distribution in the Local Universe </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Boorman%2C+P+G">Peter G. Boorman</a>, <a href="/search/astro-ph?searchtype=author&query=Gandhi%2C+P">Poshak Gandhi</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+J">Johannes Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Balokovi%C4%87%2C+M">Mislav Balokovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Asmus%2C+D">Daniel Asmus</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F+A">Fiona A. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Svoboda%2C+J">Ji艡铆 Svoboda</a>, <a href="/search/astro-ph?searchtype=author&query=Greenwell%2C+C">Claire Greenwell</a>, <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M">Michael Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+D+M">David M. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Annuar%2C+A">Adlyka Annuar</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F">Franz Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Brandt%2C+W+N">William N. Brandt</a>, <a href="/search/astro-ph?searchtype=author&query=Brightman%2C+M">Murray Brightman</a>, <a href="/search/astro-ph?searchtype=author&query=Panessa%2C+F">Francesca Panessa</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+C+J">Chien-Ting J. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Farrah%2C+D">Duncan Farrah</a>, <a href="/search/astro-ph?searchtype=author&query=Forster%2C+K">Karl Forster</a>, <a href="/search/astro-ph?searchtype=author&query=Grefenstette%2C+B">Brian Grefenstette</a>, <a href="/search/astro-ph?searchtype=author&query=H%C3%B6nig%2C+S+F">Sebastian F. H枚nig</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+A+B">Adam B. Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Kammoun%2C+E">Elias Kammoun</a>, <a href="/search/astro-ph?searchtype=author&query=Lansbury%2C+G">George Lansbury</a> , et al. (11 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.07339v1-abstract-short" style="display: inline;"> Hard X-ray-selected samples of Active Galactic Nuclei (AGN) provide one of the cleanest views of supermassive black hole accretion, but are biased against objects obscured by Compton-thick gas column densities of $N_{\rm H}$ $>$ 10$^{24}$ cm$^{-2}$. To tackle this issue, we present the NuSTAR Local AGN $N_{\rm H}$ Distribution Survey (NuLANDS)$-$a legacy sample of 122 nearby ($z$ $<$ 0.044) AGN pr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.07339v1-abstract-full').style.display = 'inline'; document.getElementById('2410.07339v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.07339v1-abstract-full" style="display: none;"> Hard X-ray-selected samples of Active Galactic Nuclei (AGN) provide one of the cleanest views of supermassive black hole accretion, but are biased against objects obscured by Compton-thick gas column densities of $N_{\rm H}$ $>$ 10$^{24}$ cm$^{-2}$. To tackle this issue, we present the NuSTAR Local AGN $N_{\rm H}$ Distribution Survey (NuLANDS)$-$a legacy sample of 122 nearby ($z$ $<$ 0.044) AGN primarily selected to have warm infrared colors from IRAS between 25$-$60 $渭$m. We show that optically classified type 1 and 2 AGN in NuLANDS are indistinguishable in terms of optical [OIII] line flux and mid-to-far infrared AGN continuum bolometric indicators, as expected from an isotropically selected AGN sample, while type 2 AGN are deficient in terms of their observed hard X-ray flux. By testing many X-ray spectroscopic models, we show the measured line-of-sight column density varies on average by $\sim$ 1.4 orders of magnitude depending on the obscurer geometry. To circumvent such issues we propagate the uncertainties per source into the parent column density distribution, finding a directly measured Compton-thick fraction of 35 $\pm$ 9%. By construction, our sample will miss sources affected by severe narrow-line reddening, and thus segregates sources dominated by small-scale nuclear obscuration from large-scale host-galaxy obscuration. This bias implies an even higher intrinsic obscured AGN fraction may be possible, although tests for additional biases arising from our infrared selection find no strong effects on the measured column-density distribution. NuLANDS thus holds potential as an optimized sample for future follow-up with current and next-generation instruments aiming to study the local AGN population in an isotropic manner. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.07339v1-abstract-full').style.display = 'none'; document.getElementById('2410.07339v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ. 50 pages (78 including appendix and bibliography), 21 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/2410.05371">arXiv:2410.05371</a> <span> [<a href="https://arxiv.org/pdf/2410.05371">pdf</a>, <a href="https://arxiv.org/format/2410.05371">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Evolution of the Dual AGN in Mrk 266: A Young AGN and a Rotation Dominated Disk in the SW Nucleus </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ruby%2C+M">Mason Ruby</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%BCller-S%C3%A1nchez%2C+F">Francisco M眉ller-S谩nchez</a>, <a href="/search/astro-ph?searchtype=author&query=Comerford%2C+J+M">Julia M. Comerford</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Cales%2C+S+L">Sabrina L. Cales</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Malkan%2C+M+A">Matthew A. Malkan</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Treister%2C+E">Ezequiel Treister</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.05371v1-abstract-short" style="display: inline;"> Dual active galactic nuclei (AGN) offer a unique opportunity to probe the relationship between super massive black holes (SMBH) and their host galaxies as well as the role of major mergers in triggering AGN activity. The confirmed dual AGN Mrk 266 has been studied extensively with multi-wavelength imaging. Now, high spatial resolution IFU spectroscopy of Mrk 266 provides an opportunity to probe th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.05371v1-abstract-full').style.display = 'inline'; document.getElementById('2410.05371v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.05371v1-abstract-full" style="display: none;"> Dual active galactic nuclei (AGN) offer a unique opportunity to probe the relationship between super massive black holes (SMBH) and their host galaxies as well as the role of major mergers in triggering AGN activity. The confirmed dual AGN Mrk 266 has been studied extensively with multi-wavelength imaging. Now, high spatial resolution IFU spectroscopy of Mrk 266 provides an opportunity to probe the kinematics of both the merger event and AGN feedback. We present for the first time high spatial resolution kinematic maps for both nuclei of Mrk 266 obtained with the Keck OSIRIS IFU spectrograph, utilizing adaptive optics to achieve a resolution of 0.31" and 0.20" for the NE and SW nuclei, respectively. Using the M-sigma relation for mergers, we infer a SMBH mass of approximately 7e7 solar masses for the southwestern nucleus. Additionally, we report that the molecular gas kinematics of the southwestern nucleus are dominated by rotation rather than large-scale chaotic motions. The southwest nucleus also contains both a circumnuclear ring of star formation from which an inflow of molecular gas is likely fueling the AGN and a compact, AGN-dominated outflow of highly ionized gas with a timescale of approximately 2 Myr, significantly shorter than the timescale of the merger. The northeastern nucleus, on the other hand, exhibits complex kinematics related to the merger, including molecular gas that appears to have decoupled from the rotation of the stars. Our results suggest that while the AGN activity in Mrk 266 was likely triggered during the merger, AGN feeding is currently the result of processes internal to each host galaxy, thus resulting in a strong asymmetry between the two nuclei. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.05371v1-abstract-full').style.display = 'none'; document.getElementById('2410.05371v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 18 figures, 3 tables. Accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.01134">arXiv:2410.01134</a> <span> [<a href="https://arxiv.org/pdf/2410.01134">pdf</a>, <a href="https://arxiv.org/format/2410.01134">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"> Characterizing the Broadband Reflection Spectrum of MAXI J1803-298 During its 2021 Outburst with NuSTAR and NICER </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Adegoke%2C+O">Oluwashina Adegoke</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia%2C+J">Javier Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Connors%2C+R">Riley Connors</a>, <a href="/search/astro-ph?searchtype=author&query=Ding%2C+Y">Yuanze Ding</a>, <a href="/search/astro-ph?searchtype=author&query=Mastroserio%2C+G">Guglielmo Mastroserio</a>, <a href="/search/astro-ph?searchtype=author&query=Steiner%2C+J">James Steiner</a>, <a href="/search/astro-ph?searchtype=author&query=Ingram%2C+A">Adam Ingram</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Tomsick%2C+J">John Tomsick</a>, <a href="/search/astro-ph?searchtype=author&query=Kara%2C+E">Erin Kara</a>, <a href="/search/astro-ph?searchtype=author&query=Mehdipour%2C+M">Missagh Mehdipour</a>, <a href="/search/astro-ph?searchtype=author&query=Fukumura%2C+K">Keigo Fukumura</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Ubach%2C+S">Santiago Ubach</a>, <a href="/search/astro-ph?searchtype=author&query=Lucchini%2C+M">Matteo Lucchini</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.01134v1-abstract-short" style="display: inline;"> MAXI J1803-298 is a transient black hole candidate discovered in May of 2021 during an outburst that lasted several months. Multiple X-ray observations reveal recurring "dipping" intervals in several of its light curves, particularly during the hard/intermediate states, with a typical recurrence period of $\sim7\,\mathrm{hours}$. We report analysis of four NuSTAR observations of the source, supple… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.01134v1-abstract-full').style.display = 'inline'; document.getElementById('2410.01134v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.01134v1-abstract-full" style="display: none;"> MAXI J1803-298 is a transient black hole candidate discovered in May of 2021 during an outburst that lasted several months. Multiple X-ray observations reveal recurring "dipping" intervals in several of its light curves, particularly during the hard/intermediate states, with a typical recurrence period of $\sim7\,\mathrm{hours}$. We report analysis of four NuSTAR observations of the source, supplemented with NICER data where available, over the duration of the outburst evolution covering the hard, intermediate and the soft states. Reflection spectroscopy reveals the black hole to be rapidly spinning ($a_*=0.990\pm{0.001}$) with a near edge-on viewing angle ($i=70\pm{1}掳$). Additionally, we show that the light-curve dips are caused by photo-electric absorption from a moderately ionized absorber whose origin is not fully understood, although it is likely linked to material from the companion star impacting the outer edges of the accretion disk. We further detect absorption lines in some of the spectra, potentially associated with Fe XXV and Fe XXVI, indicative of disk winds with moderate to extreme velocities. During the intermediate state and just before transitioning into the soft state, the source showed a sudden flux increase which we found to be dominated by soft disk photons and consistent with the filling of the inner accretion disk, at the onset of state transition. In the soft state, we show that models of disk self-irradiation provide a better fit and a preferred explanation to the broadband reflection spectrum, consistent with previous studies of other accreting sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.01134v1-abstract-full').style.display = 'none'; document.getElementById('2410.01134v1-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 9 figures, accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.17334">arXiv:2409.17334</a> <span> [<a href="https://arxiv.org/pdf/2409.17334">pdf</a>, <a href="https://arxiv.org/format/2409.17334">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> BASS XLI: the correlation between Mid-infrared emission lines and Active Galactic Nuclei emission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bierschenk%2C+M">M. Bierschenk</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">C. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Temple%2C+M+J">M. J. Temple</a>, <a href="/search/astro-ph?searchtype=author&query=Satyapal%2C+S">S. Satyapal</a>, <a href="/search/astro-ph?searchtype=author&query=Cann%2C+J">J. Cann</a>, <a href="/search/astro-ph?searchtype=author&query=Xie%2C+Y">Y. Xie</a>, <a href="/search/astro-ph?searchtype=author&query=Diaz%2C+Y">Y. Diaz</a>, <a href="/search/astro-ph?searchtype=author&query=Ichikawa%2C+K">K. Ichikawa</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=Bauer%2C+F+E">F. E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas%2C+A">A. Rojas</a>, <a href="/search/astro-ph?searchtype=author&query=Kakkad%2C+D">D. Kakkad</a>, <a href="/search/astro-ph?searchtype=author&query=Tortosa%2C+A">A. Tortosa</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">F. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotzky%2C+R">R. Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Kawamuro%2C+T">T. Kawamuro</a>, <a href="/search/astro-ph?searchtype=author&query=Gupta%2C+K+K">K. K. Gupta</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">B. Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+C+S">C. S. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Riffel%2C+R">R. Riffel</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">K. Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">F. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M">M. Powell</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Urry%2C+C+M">C. M. Urry</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.17334v1-abstract-short" style="display: inline;"> We analyze the Spitzer spectra of 140 active galactic nuclei (AGN) detected in the hard X-rays (14-195 keV) by the Burst Alert Telescope (BAT) on board Swift. This sample allows us to probe several orders of magnitude in black hole masses ($10^6-10^9 M_{\odot}$), Eddington ratios ($10^{-3}-1$), X-ray luminosities ($10^{42}-10^{45}\rm\,erg\,s^{-1}$), and X-ray column densities (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.17334v1-abstract-full').style.display = 'inline'; document.getElementById('2409.17334v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.17334v1-abstract-full" style="display: none;"> We analyze the Spitzer spectra of 140 active galactic nuclei (AGN) detected in the hard X-rays (14-195 keV) by the Burst Alert Telescope (BAT) on board Swift. This sample allows us to probe several orders of magnitude in black hole masses ($10^6-10^9 M_{\odot}$), Eddington ratios ($10^{-3}-1$), X-ray luminosities ($10^{42}-10^{45}\rm\,erg\,s^{-1}$), and X-ray column densities ($10^{20}-10^{24}\rm\,cm^{-2}$). The AGN emission is expected to be the dominant source of ionizing photons with energies $\gtrsim50$ eV, and therefore high-ionization mid-infrared (MIR) emission lines such as [Ne V] 14.32, 24.32 $渭$m and [O IV] 25.89 $渭$m are predicted to be good proxies of AGN activity, and robust against obscuration effects. We find high detection rates ($\gtrsim85-90$ per cent) for the mid-infrared coronal emission lines in our AGN sample. The luminosities of these lines are correlated with the 14-150 keV luminosity (with a typical scatter of $蟽\sim 0.4-0.5$ dex), strongly indicating that the mid-infrared coronal line emission is driven by AGN activity. Interestingly, we find that the coronal lines are more tightly correlated to the bolometric luminosity ($蟽\sim 0.2-0.3$ dex), calculated from careful analysis of the spectral energy distribution, than to the X-ray luminosity. We find that the relationship between the coronal line strengths and $L_{14-150\rm\,keV}$ is independent of black hole mass, Eddington ratio and X-ray column density. This confirms that the mid-infrared coronal lines can be used as unbiased tracers of the AGN power for X-ray luminosities in the $10^{42}-10^{45}\rm\,erg\,s^{-1}$ range. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.17334v1-abstract-full').style.display = 'none'; document.getElementById('2409.17334v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">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/2409.12241">arXiv:2409.12241</a> <span> [<a href="https://arxiv.org/pdf/2409.12241">pdf</a>, <a href="https://arxiv.org/ps/2409.12241">ps</a>, <a href="https://arxiv.org/format/2409.12241">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"> A New Broadband Spectral State in the Ultraluminous X-ray Source Holmberg IX X-1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Walton%2C+D+J">D. J. Walton</a>, <a href="/search/astro-ph?searchtype=author&query=Bachetti%2C+M">M. Bachetti</a>, <a href="/search/astro-ph?searchtype=author&query=Kosec%2C+P">P. Kosec</a>, <a href="/search/astro-ph?searchtype=author&query=Furst%2C+F">F. Furst</a>, <a href="/search/astro-ph?searchtype=author&query=Pinto%2C+C">C. Pinto</a>, <a href="/search/astro-ph?searchtype=author&query=Roberts%2C+T+P">T. P. Roberts</a>, <a href="/search/astro-ph?searchtype=author&query=Soria%2C+R">R. Soria</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Alston%2C+W+N">W. N. Alston</a>, <a href="/search/astro-ph?searchtype=author&query=Brightman%2C+M">M. Brightman</a>, <a href="/search/astro-ph?searchtype=author&query=Earnshaw%2C+H+P">H. P. Earnshaw</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=Harrison%2C+F+A">F. A. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Middleton%2C+M+J">M. J. Middleton</a>, <a href="/search/astro-ph?searchtype=author&query=Sathyaprakash%2C+R">R. Sathyaprakash</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.12241v1-abstract-short" style="display: inline;"> We present a series of five new broadband X-ray observations of the ultraluminous X-ray source Holmberg IX X-1, performed by $XMM$-$Newton$ and $NuSTAR$ in coordination. The first three of these show high soft X-ray fluxes but a near total collapse of the high-energy ($\gtrsim$15 keV) emission, previously seen to be surprisingly stable across all prior broadband observations of the source. The lat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.12241v1-abstract-full').style.display = 'inline'; document.getElementById('2409.12241v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.12241v1-abstract-full" style="display: none;"> We present a series of five new broadband X-ray observations of the ultraluminous X-ray source Holmberg IX X-1, performed by $XMM$-$Newton$ and $NuSTAR$ in coordination. The first three of these show high soft X-ray fluxes but a near total collapse of the high-energy ($\gtrsim$15 keV) emission, previously seen to be surprisingly stable across all prior broadband observations of the source. The latter two show a recovery in hard X-rays, remarkably once again respecting the same stable high-energy flux exhibited by all of the archival observations. We also present a joint analysis of all broadband observations of Holmberg IX X-1 to date (encompassing 11 epochs in total) in order to investigate whether it shows the same luminosity-temperature behaviour as NGC 1313 X-1 (which also shows a stable high-energy flux), whereby the hotter disc component in the spectrum exhibits two distinct, positively-correlated tracks in the luminosity-temperature plane. Holmberg IX X-1 may show similar behaviour, but the results depend on whether the highest energy emission is assumed to be an up-scattering corona or an accretion column. The strongest evidence for this behaviour is found in the former case, while in the latter the new 'soft' epochs appear distinct from the other high-flux epochs. We discuss possible explanations for these new 'soft' spectra in the context of the expected structure of super-Eddington accretion flows around black holes and neutron stars, and highlight a potentially interesting analogy with the recent destruction and re-creation of the corona seen in the AGN 1ES 1927+654. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.12241v1-abstract-full').style.display = 'none'; document.getElementById('2409.12241v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 5 figures, submitted for publication in MNRAS (comments welcome)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.12239">arXiv:2409.12239</a> <span> [<a href="https://arxiv.org/pdf/2409.12239">pdf</a>, <a href="https://arxiv.org/format/2409.12239">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"> BASS. XLIII: Optical, UV, and X-ray emission properties of unobscured Swift/BAT active galactic nuclei </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gupta%2C+K+K">Kriti K. Gupta</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Temple%2C+M+J">Matthew J. Temple</a>, <a href="/search/astro-ph?searchtype=author&query=Tortosa%2C+A">Alessia Tortosa</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=Assef%2C+R+J">Roberto J. Assef</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=Mushotzy%2C+R">Richard Mushotzy</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">Federica Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Ueda%2C+Y">Yoshihiro Ueda</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas%2C+A+F">Alejandra F. Rojas</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">Benny Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+C">Chin-Shin Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">Kyuseok Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+R">Ruancun Li</a>, <a href="/search/astro-ph?searchtype=author&query=Kawamuro%2C+T">Taiki Kawamuro</a>, <a href="/search/astro-ph?searchtype=author&query=Diaz%2C+Y">Yaherlyn Diaz</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M+C">Meredith C. Powell</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Urry%2C+C+M">C. Megan Urry</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Cenko%2C+B">Brad Cenko</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.12239v1-abstract-short" style="display: inline;"> We present one of the largest multiwavelength studies of simultaneous optical-to-X-ray spectral energy distributions (SEDs) of unobscured active galactic nuclei (AGN) in the local Universe. Using a representative sample of hard-X-ray-selected AGN from the 70-month Swift/BAT catalog, with optical/UV photometric data from Swift/UVOT and X-ray spectral data from Swift/XRT, we constructed broadband SE… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.12239v1-abstract-full').style.display = 'inline'; document.getElementById('2409.12239v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.12239v1-abstract-full" style="display: none;"> We present one of the largest multiwavelength studies of simultaneous optical-to-X-ray spectral energy distributions (SEDs) of unobscured active galactic nuclei (AGN) in the local Universe. Using a representative sample of hard-X-ray-selected AGN from the 70-month Swift/BAT catalog, with optical/UV photometric data from Swift/UVOT and X-ray spectral data from Swift/XRT, we constructed broadband SEDs of 236 nearby AGN (0.001<z<0.3). We employed GALFIT to estimate host galaxy contamination in the optical/UV and determine the intrinsic AGN fluxes. We used an absorbed power law with a reflection component to model the X-ray spectra and a dust-reddened multi-temperature blackbody to fit the optical/UV SED. We calculated total bolometric luminosities ($L_{bol}$), optical-to-X-ray spectral indices ($伪_{ox}$), and multiple bolometric corrections (BCs) in the optical, UV, and X-rays. We used black hole masses obtained by reverberation mapping and the virial method to estimate Eddington ratios ($位_{Edd}$) for all our AGN. We confirm the tight correlation between UV and X-ray luminosity for our sample. We observe a significant decrease in $伪_{ox}$ with $L_{bol}$ and $位_{Edd}$, suggesting that brighter sources emit more UV photons per X-rays. We report a second-order regression relation between the 2-10 keV BC and $伪_{ox}$, which is useful to compute $L_{bol}$ in the absence of multiband SEDs. We also investigate the dependence of optical/UV BCs on the physical properties of AGN and obtain a significant increase in the UV BCs with $L_{bol}$ and $位_{Edd}$, unlike those in the optical, which are constant across five orders of $L_{bol}$ and $位_{Edd}$. We obtain significant dispersions (~0.1-1 dex) in all BCs, and hence recommend using appropriate relations with observed quantities while including the reported scatter, instead of their median values. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.12239v1-abstract-full').style.display = 'none'; document.getElementById('2409.12239v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">42 pages, 36 figures, 17 tables. Accepted for publication in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.00253">arXiv:2409.00253</a> <span> [<a href="https://arxiv.org/pdf/2409.00253">pdf</a>, <a href="https://arxiv.org/format/2409.00253">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Next Generation Accretion Disk Reflection Model: High-Density Plasma Effects </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ding%2C+Y">Yuanze Ding</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa%2C+J+A">Javier A. Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Kallman%2C+T+R">Timothy R. Kallman</a>, <a href="/search/astro-ph?searchtype=author&query=Mendoza%2C+C">Claudio Mendoza</a>, <a href="/search/astro-ph?searchtype=author&query=Bautista%2C+M">Manuel Bautista</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F+A">Fiona A. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Tomsick%2C+J+A">John A. Tomsick</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+J">Jameson Dong</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.00253v1-abstract-short" style="display: inline;"> Luminous accretion disks around black holes are expected to have densities of $\sim 10^{15-22}\,$cm$^{-3}$, which are high enough such that plasma physics effects become important. Many of these effects have been traditionally neglected in the calculation of atomic parameters, and therefore from photoionization models, and ultimately also from X-ray reflection models. In this paper, we describe up… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.00253v1-abstract-full').style.display = 'inline'; document.getElementById('2409.00253v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.00253v1-abstract-full" style="display: none;"> Luminous accretion disks around black holes are expected to have densities of $\sim 10^{15-22}\,$cm$^{-3}$, which are high enough such that plasma physics effects become important. Many of these effects have been traditionally neglected in the calculation of atomic parameters, and therefore from photoionization models, and ultimately also from X-ray reflection models. In this paper, we describe updates to the atomic rates used by the XSTAR code, which is in turn part of the XILLVER disk reflection model. We discuss the effect of adding necessary high density corrections into the XILLVER code. Specifically, we find that the change of recombination rates play an important role, dominating the differences between model versions. With synthetic spectra, we show that even in a highly ionized state, high density slabs can produce strong iron ($\sim$6.5-9$\,$keV) and oxygen ($\sim0.6-0.8\,$keV) resonance features. The significant iron emission could address the problem of the supersolar iron abundances found in some sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.00253v1-abstract-full').style.display = 'none'; document.getElementById('2409.00253v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 13 figures. Accepted by ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.02645">arXiv:2408.02645</a> <span> [<a href="https://arxiv.org/pdf/2408.02645">pdf</a>, <a href="https://arxiv.org/format/2408.02645">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> PKS~J0805$-$0111: A Second Owens Valley Radio Observatory Blazar Showing Highly Significant Sinusoidal Radio Variability -- The Tip of the Iceberg </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=de+la+Parra%2C+P+V">P. V. de la Parra</a>, <a href="/search/astro-ph?searchtype=author&query=Kiehlmann%2C+S">S. Kiehlmann</a>, <a href="/search/astro-ph?searchtype=author&query=Mroz%2C+P">P. Mroz</a>, <a href="/search/astro-ph?searchtype=author&query=Readhead%2C+A+C+S">A. C. S. Readhead</a>, <a href="/search/astro-ph?searchtype=author&query=Synani%2C+A">A. Synani</a>, <a href="/search/astro-ph?searchtype=author&query=Begelman%2C+M+C">M. C. Begelman</a>, <a href="/search/astro-ph?searchtype=author&query=Blandford%2C+R+D">R. D. Blandford</a>, <a href="/search/astro-ph?searchtype=author&query=Ding%2C+Y">Y. Ding</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">F. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Liodakis%2C+I">I. Liodakis</a>, <a href="/search/astro-ph?searchtype=author&query=Max-Moerbeck%2C+W">W. Max-Moerbeck</a>, <a href="/search/astro-ph?searchtype=author&query=Pavlidou%2C+V">V. Pavlidou</a>, <a href="/search/astro-ph?searchtype=author&query=Reeves%2C+R">R. Reeves</a>, <a href="/search/astro-ph?searchtype=author&query=Vallisneri%2C+M">M. Vallisneri</a>, <a href="/search/astro-ph?searchtype=author&query=Aller%2C+M+F">M. F. Aller</a>, <a href="/search/astro-ph?searchtype=author&query=Graham%2C+M+J">M. J. Graham</a>, <a href="/search/astro-ph?searchtype=author&query=Hovatta%2C+T">T. Hovatta</a>, <a href="/search/astro-ph?searchtype=author&query=Lawrence%2C+C+R">C. R. Lawrence</a>, <a href="/search/astro-ph?searchtype=author&query=Lazio%2C+T+J+W">T. J. W. Lazio</a>, <a href="/search/astro-ph?searchtype=author&query=Mahabal%2C+A+A">A. A. Mahabal</a>, <a href="/search/astro-ph?searchtype=author&query=Molina%2C+B">B. Molina</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Neill%2C+S">S. O'Neill</a>, <a href="/search/astro-ph?searchtype=author&query=Pearson%2C+T+J">T. J. Pearson</a>, <a href="/search/astro-ph?searchtype=author&query=Ravi%2C+V">V. Ravi</a>, <a href="/search/astro-ph?searchtype=author&query=Tassis%2C+K">K. Tassis</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.02645v1-abstract-short" style="display: inline;"> Owens Valley Radio Observatory (OVRO) observations of supermassive black hole binary (SMBHB) candidate PKS~2131$-$021 revealed, for the first time, six likely characteristics of the phenomenology exhibited by SMBHB in blazars, of which the most unexpected and critical is sinusoidal flux density variations. We have now identified a second blazar, PKS~J0805$-$0111, showing significant sinusoidal var… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.02645v1-abstract-full').style.display = 'inline'; document.getElementById('2408.02645v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.02645v1-abstract-full" style="display: none;"> Owens Valley Radio Observatory (OVRO) observations of supermassive black hole binary (SMBHB) candidate PKS~2131$-$021 revealed, for the first time, six likely characteristics of the phenomenology exhibited by SMBHB in blazars, of which the most unexpected and critical is sinusoidal flux density variations. We have now identified a second blazar, PKS~J0805$-$0111, showing significant sinusoidal variations, with an observed period that translates to $1.422 \pm 0.005$ yr in the rest frame of the $z = 1.388$ object. We generate $10^6$ simulated light curves to reproduce the radio variability characteristics of PKS~J0805$-$0111, and show that the global probability, considering the \textit{look-elsewhere effect}, indicates that the observed periodicity can be attributed to the red noise tail of the power spectral density, with a $p_0$ value of $7.8 \times 10^{-5}$ (i.e. 3.78$蟽$). PKS J0805$-$0111 displays all six characteristics observed in PKS 2131$-$021. Taking into account the well-defined OVRO sample size, the false positive probability $\sim 0.22$, but the rare behavior makes this a strong SMBHB candidate. The discovery of a second SMBHB candidate exhibiting these rare characteristics reveals that PKS~2131$-$021 is not a unique, isolated case. With these two strong cases we are clearly seeing only the tip of the iceberg. We estimate that the number of SMBHB candidates amongst blazars $\sim$ 1 in 100. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.02645v1-abstract-full').style.display = 'none'; document.getElementById('2408.02645v1-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 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.09647">arXiv:2407.09647</a> <span> [<a href="https://arxiv.org/pdf/2407.09647">pdf</a>, <a href="https://arxiv.org/format/2407.09647">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"> PKS 2131-021 -- Discovery of Strong Coherent Sinusoidal Variations from Radio to Optical Frequencies: Compelling Evidence for a Blazar Supermassive Black Hole Binary </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kiehlmann%2C+S">Sebastian Kiehlmann</a>, <a href="/search/astro-ph?searchtype=author&query=De+La+Parra%2C+P+V">Philipe Vergara De La Parra</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+A">Andrew Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=Synani%2C+A">A. Synani</a>, <a href="/search/astro-ph?searchtype=author&query=Liodakis%2C+I">Ioannis Liodakis</a>, <a href="/search/astro-ph?searchtype=author&query=Readhead%2C+A">Anthony Readhead</a>, <a href="/search/astro-ph?searchtype=author&query=Graham%2C+M">Matthew Graham</a>, <a href="/search/astro-ph?searchtype=author&query=Begelman%2C+M">Mitchell Begelman</a>, <a href="/search/astro-ph?searchtype=author&query=Blandford%2C+R">Roger Blandford</a>, <a href="/search/astro-ph?searchtype=author&query=Chatziioannou%2C+K">Katerina Chatziioannou</a>, <a href="/search/astro-ph?searchtype=author&query=Ding%2C+Y">Yuanze Ding</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Homan%2C+D">D. Homan</a>, <a href="/search/astro-ph?searchtype=author&query=Hovatta%2C+T">Talvikki Hovatta</a>, <a href="/search/astro-ph?searchtype=author&query=Kulkarni%2C+S">Shrinivas Kulkarni</a>, <a href="/search/astro-ph?searchtype=author&query=Lister%2C+M">Matthew Lister</a>, <a href="/search/astro-ph?searchtype=author&query=Maiolino%2C+R">Roberto Maiolino</a>, <a href="/search/astro-ph?searchtype=author&query=Max-Moerbeck%2C+W">Walter Max-Moerbeck</a>, <a href="/search/astro-ph?searchtype=author&query=Molina%2C+B">B. Molina</a>, <a href="/search/astro-ph?searchtype=author&query=Mroz%2C+P">Przemyslaw Mroz</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Dea%2C+C">Christopher O'Dea</a>, <a href="/search/astro-ph?searchtype=author&query=Pavlidou%2C+V">Vasiliki Pavlidou</a>, <a href="/search/astro-ph?searchtype=author&query=Pearson%2C+T+J">Timothy J. Pearson</a>, <a href="/search/astro-ph?searchtype=author&query=Aller%2C+M">Margo Aller</a>, <a href="/search/astro-ph?searchtype=author&query=Lawrence%2C+C">C. Lawrence</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="2407.09647v1-abstract-short" style="display: inline;"> Haystack and Owens Valley Radio Observatory (OVRO) observations recently revealed strong sinusoidal total flux density variations that maintained coherence between 1975 and 2021 in the blazar PKS 2131-021 ($z=1.283)$. This was interpreted as possible evidence of a supermassive black hole binary (SMBHB). Extended observations through 2023 show coherence over 47.9~years, with an observed period… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.09647v1-abstract-full').style.display = 'inline'; document.getElementById('2407.09647v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.09647v1-abstract-full" style="display: none;"> Haystack and Owens Valley Radio Observatory (OVRO) observations recently revealed strong sinusoidal total flux density variations that maintained coherence between 1975 and 2021 in the blazar PKS 2131-021 ($z=1.283)$. This was interpreted as possible evidence of a supermassive black hole binary (SMBHB). Extended observations through 2023 show coherence over 47.9~years, with an observed period $P_\textrm{15 GHz}=(1739.3 \pm 1.2) \, {\rm days}$. We reject, with $p$-value = $5.3 \times 10^{-7}$, the hypothesis that the variations are due to random fluctuations in the red noise tail of the power spectral density. There is clearly a constant-period physical phenomenon in PKS 2131-021 producing coherent intermittent sinusoidal flux density variations. We find the coherent sinusoidal intensity variations extend from below 2.7 GHz to optical frequencies, from which we derive an observed period $P_\textrm{optical}=(1764 \pm 36)$ days. Across this broad frequency range there is a monotonic phase shift in the sinusoidal variations with frequency. The same coherent periodicity is possibly also observed at $纬$-ray energies. The importance of well-vetted SMBHB candidates to searches for gravitational waves is pointed out. We estimate the fraction of blazars that are SMBHB candidates to be $>1$ in 100. Thus monitoring programs covering tens of thousands of blazars could discover hundreds of SMBHB candidates. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.09647v1-abstract-full').style.display = 'none'; document.getElementById('2407.09647v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 17 figures, 5 tables, submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.17637">arXiv:2404.17637</a> <span> [<a href="https://arxiv.org/pdf/2404.17637">pdf</a>, <a href="https://arxiv.org/format/2404.17637">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"> The NuSTAR Serendipitous Survey: the 80-month catalog and source properties of the high-energy emitting AGN and quasar population </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Greenwell%2C+C+L">Claire L. Greenwell</a>, <a href="/search/astro-ph?searchtype=author&query=Klindt%2C+L">Lizelke Klindt</a>, <a href="/search/astro-ph?searchtype=author&query=Lansbury%2C+G+B">George B. Lansbury</a>, <a href="/search/astro-ph?searchtype=author&query=Rosario%2C+D+J">David J. Rosario</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+D+M">David M. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Aird%2C+J">James Aird</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Forster%2C+K">Karl Forster</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=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Tomsick%2C+J">John Tomsick</a>, <a href="/search/astro-ph?searchtype=author&query=Brandt%2C+W+N">William N. Brandt</a>, <a href="/search/astro-ph?searchtype=author&query=Connor%2C+T">Thomas Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Boorman%2C+P+G">Peter G. Boorman</a>, <a href="/search/astro-ph?searchtype=author&query=Annuar%2C+A">Adlyka Annuar</a>, <a href="/search/astro-ph?searchtype=author&query=Ballantyne%2C+D+R">David R. Ballantyne</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+C">Chien-Ting Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Civano%2C+F">Francesca Civano</a>, <a href="/search/astro-ph?searchtype=author&query=Comastri%2C+A">Andrea Comastri</a>, <a href="/search/astro-ph?searchtype=author&query=Fawcett%2C+V+A">Victoria A. Fawcett</a>, <a href="/search/astro-ph?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</a>, <a href="/search/astro-ph?searchtype=author&query=Gandhi%2C+P">Poshak Gandhi</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Heida%2C+M">Marianne Heida</a> , 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="2404.17637v1-abstract-short" style="display: inline;"> We present a catalog of hard X-ray serendipitous sources detected in the first 80 months of observations by the Nuclear Spectroscopic Telescope Array (NuSTAR). The NuSTAR serendipitous survey 80-month (NSS80) catalog has an unprecedented $\sim$ 62 Ms of effective exposure time over 894 unique fields (a factor of three increase over the 40-month catalog), with an areal coverage of $\sim $36 deg… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.17637v1-abstract-full').style.display = 'inline'; document.getElementById('2404.17637v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.17637v1-abstract-full" style="display: none;"> We present a catalog of hard X-ray serendipitous sources detected in the first 80 months of observations by the Nuclear Spectroscopic Telescope Array (NuSTAR). The NuSTAR serendipitous survey 80-month (NSS80) catalog has an unprecedented $\sim$ 62 Ms of effective exposure time over 894 unique fields (a factor of three increase over the 40-month catalog), with an areal coverage of $\sim $36 deg$^2$, larger than all NuSTAR extragalactic surveys. NSS80 provides 1274 hard X-ray sources in the $3-24$ keV band (822 new detections compared to the previous 40-month catalog). Approximately 76% of the NuSTAR sources have lower-energy ($<10$ keV) X-ray counterparts from Chandra, XMM-Newton, and Swift-XRT. We have undertaken an extensive campaign of ground-based spectroscopic follow-up to obtain new source redshifts and classifications for 427 sources. Combining these with existing archival spectroscopy provides redshifts for 550 NSS80 sources, of which 547 are classified. The sample is primarily composed of active galactic nuclei (AGN), detected over a large range in redshift ($z$ = 0.012-3.43), but also includes 58 spectroscopically confirmed Galactic sources. In addition, five AGN/galaxy pairs, one dual AGN system, one BL Lac candidate, and a hotspot of 4C 74.26 (radio quasar) have been identified. The median rest-frame $10-40$ keV luminosity and redshift of the NSS80 are $\langle{L_\mathrm{10-40 keV}}\rangle$ = 1.2 $\times$ 10$^{44}$ erg s$^{-1}$ and $\langle z \rangle = 0.56$. We investigate the optical properties and construct composite optical spectra to search for subtle signatures not present in the individual spectra, finding an excess of redder BL AGN compared to optical quasar surveys predominantly due to the presence of the host-galaxy and, at least in part, due to dust obscuration. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.17637v1-abstract-full').style.display = 'none'; document.getElementById('2404.17637v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">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:S. 57 pages, 32 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.13973">arXiv:2403.13973</a> <span> [<a href="https://arxiv.org/pdf/2403.13973">pdf</a>, <a href="https://arxiv.org/format/2403.13973">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"> Return to the forgotten ULX: a broadband NICER+NuSTAR study of NGC 4190 ULX-1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Earnshaw%2C+H+P">Hannah P Earnshaw</a>, <a href="/search/astro-ph?searchtype=author&query=Bachetti%2C+M">Matteo Bachetti</a>, <a href="/search/astro-ph?searchtype=author&query=Brightman%2C+M">Murray Brightman</a>, <a href="/search/astro-ph?searchtype=author&query=F%C3%BCrst%2C+F">Felix F眉rst</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F+A">Fiona A. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Middleton%2C+M">Matthew Middleton</a>, <a href="/search/astro-ph?searchtype=author&query=Ludlam%2C+R">Renee Ludlam</a>, <a href="/search/astro-ph?searchtype=author&query=Pike%2C+S+N">Sean N. Pike</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Walton%2C+D+J">Dominic J. Walton</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.13973v2-abstract-short" style="display: inline;"> We observed the nearby and relatively understudied ultraluminous X-ray source (ULX) NGC 4190 ULX-1 jointly with NICER and NuSTAR to investigate its broadband spectrum, timing properties, and spectral variation over time. We found NGC 4190 ULX-1 to have a hard spectrum characterized by two thermal components (with temperatures ~0.25keV and ~1.6keV) and a high-energy excess typical of the ULX popula… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.13973v2-abstract-full').style.display = 'inline'; document.getElementById('2403.13973v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.13973v2-abstract-full" style="display: none;"> We observed the nearby and relatively understudied ultraluminous X-ray source (ULX) NGC 4190 ULX-1 jointly with NICER and NuSTAR to investigate its broadband spectrum, timing properties, and spectral variation over time. We found NGC 4190 ULX-1 to have a hard spectrum characterized by two thermal components (with temperatures ~0.25keV and ~1.6keV) and a high-energy excess typical of the ULX population, although the spectrum turns over at an unusually low energy. While no pulsations were detected, (with pulsed fraction 3-sigma upper limits of 16% for NICER and 35% for NuSTAR), the source shows significant stochastic variability and the covariance spectrum indicates the presence of a high-energy cut-off power-law component, potentially indicative of an accretion column. Additionally, when fitting archival XMM-Newton data with a similar model, we find that the luminosity-temperature evolution of the hot thermal component follows the behavior of a super-Eddington slim disk though the expected spectral broadening for such a disk is not seen, suggesting that the inner accretion disk may be truncated by a magnetic field. Therefore, despite the lack of detected pulsations, there is tantalizing evidence for NGC 4190 ULX-1 being a candidate neutron star accretor, although further broadband observations will be required to confirm this behavior. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.13973v2-abstract-full').style.display = 'none'; document.getElementById('2403.13973v2-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 9 figures, 2 tables, accepted for publication in The Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.04949">arXiv:2311.04949</a> <span> [<a href="https://arxiv.org/pdf/2311.04949">pdf</a>, <a href="https://arxiv.org/format/2311.04949">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> The High Energy X-ray Probe (HEX-P): The Circum-nuclear Environment of Growing Supermassive Black Holes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Boorman%2C+P+G">P. G. Boorman</a>, <a href="/search/astro-ph?searchtype=author&query=Torres-Alb%C3%A0%2C+N">N. Torres-Alb脿</a>, <a href="/search/astro-ph?searchtype=author&query=Annuar%2C+A">A. Annuar</a>, <a href="/search/astro-ph?searchtype=author&query=Marchesi%2C+S">S. Marchesi</a>, <a href="/search/astro-ph?searchtype=author&query=Pfeifle%2C+R">R. Pfeifle</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Civano%2C+F">F. Civano</a>, <a href="/search/astro-ph?searchtype=author&query=Balokovi%C4%87%2C+M">M. Balokovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+J">J. Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">C. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Brandt%2C+W+N">W. N. Brandt</a>, <a href="/search/astro-ph?searchtype=author&query=Brightman%2C+M">M. Brightman</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+C+T">C. T. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Creech%2C+S">S. Creech</a>, <a href="/search/astro-ph?searchtype=author&query=Gandhi%2C+P">P. Gandhi</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa%2C+J+A">J. A. Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">F. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Hickox%2C+R">R. Hickox</a>, <a href="/search/astro-ph?searchtype=author&query=Kammoun%2C+E">E. Kammoun</a>, <a href="/search/astro-ph?searchtype=author&query=LaMassa%2C+S">S. LaMassa</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzuisi%2C+G">G. Lanzuisi</a>, <a href="/search/astro-ph?searchtype=author&query=Marcotulli%2C+L">L. Marcotulli</a>, <a href="/search/astro-ph?searchtype=author&query=Madsen%2C+K">K. Madsen</a>, <a href="/search/astro-ph?searchtype=author&query=Matt%2C+G">G. Matt</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="2311.04949v1-abstract-short" style="display: inline;"> Ever since the discovery of the first Active Galactic Nuclei (AGN), substantial observational and theoretical effort has been invested into understanding how massive black holes have evolved across cosmic time. Circum-nuclear obscuration is now established as a crucial component, with almost every AGN observed known to display signatures of some level of obscuration in their X-ray spectra. But des… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.04949v1-abstract-full').style.display = 'inline'; document.getElementById('2311.04949v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.04949v1-abstract-full" style="display: none;"> Ever since the discovery of the first Active Galactic Nuclei (AGN), substantial observational and theoretical effort has been invested into understanding how massive black holes have evolved across cosmic time. Circum-nuclear obscuration is now established as a crucial component, with almost every AGN observed known to display signatures of some level of obscuration in their X-ray spectra. But despite more than six decades of effort, substantial open questions remain: How does the accretion power impact the structure of the circum-nuclear obscurer? What are the dynamical properties of the obscurer? Can dense circum-nuclear obscuration exist around intrinsically weak AGN? How many intermediate mass black holes occupy the centers of dwarf galaxies? In this paper, we showcase a number of next-generation prospects attainable with the High Energy X-ray Probe (https://hexp.org) to contribute towards solving these questions in the 2030s. The uniquely broad (0.2--80 keV) and strictly simultaneous X-ray passband of HEX-P makes it ideally suited for studying the temporal co-evolution between the central engine and circum-nuclear obscurer. Improved sensitivities and reduced background will enable the development of spectroscopic models complemented by current and future multi-wavelength observations. We show that the angular resolution of HEX-P both below and above 10 keV will enable the discovery and confirmation of accreting massive black holes at both low accretion power and low black hole masses even when concealed by thick obscuration. In combination with other next-generation observations of the dusty hearts of nearby galaxies, HEX-P will hence be pivotal in paving the way towards a complete picture of black hole growth and galaxy co-evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.04949v1-abstract-full').style.display = 'none'; document.getElementById('2311.04949v1-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, 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">To be submitted for peer review to a HEX-P Collection in Frontiers of Astronomy and Space Science. Constructive comments welcome!</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.01494">arXiv:2311.01494</a> <span> [<a href="https://arxiv.org/pdf/2311.01494">pdf</a>, <a href="https://arxiv.org/ps/2311.01494">ps</a>, <a href="https://arxiv.org/format/2311.01494">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> BASS XLII: The relation between the covering factor of dusty gas and the Eddington ratio in nearby active galactic nuclei </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">C. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Ichikawa%2C+K">K. Ichikawa</a>, <a href="/search/astro-ph?searchtype=author&query=Stalevski%2C+M">M. Stalevski</a>, <a href="/search/astro-ph?searchtype=author&query=Kawamuro%2C+T">T. Kawamuro</a>, <a href="/search/astro-ph?searchtype=author&query=Yamada%2C+S">S. Yamada</a>, <a href="/search/astro-ph?searchtype=author&query=Ueda%2C+Y">Y. Ueda</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotzky%2C+R">R. Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">G. C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M+J">M. J. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">B. Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Fabian%2C+A+C">A. C. Fabian</a>, <a href="/search/astro-ph?searchtype=author&query=Ho%2C+L+C">L. C. Ho</a>, <a href="/search/astro-ph?searchtype=author&query=Asmus%2C+D">D. Asmus</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">F. E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+C+S">C. S. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Gupta%2C+K+K">K. K. Gupta</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">K. Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M">M. Powell</a>, <a href="/search/astro-ph?searchtype=author&query=Pfeifle%2C+R+W">R. W. Pfeifle</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas%2C+A">A. Rojas</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">F. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Temple%2C+M+J">M. J. Temple</a>, <a href="/search/astro-ph?searchtype=author&query=Toba%2C+Y">Y. Toba</a>, <a href="/search/astro-ph?searchtype=author&query=Tortosa%2C+A">A. Tortosa</a>, <a href="/search/astro-ph?searchtype=author&query=Treister%2C+E">E. Treister</a> , et al. (3 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.01494v2-abstract-short" style="display: inline;"> Accreting supermassive black holes (SMBHs) located at the center of galaxies are typically surrounded by large quantities of gas and dust. The structure and evolution of this circumnuclear material can be studied at different wavelengths, from the submillimeter to the X-rays. Recent X-ray studies have shown that the covering factor of the obscuring material tends to decrease with increasing Edding… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.01494v2-abstract-full').style.display = 'inline'; document.getElementById('2311.01494v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.01494v2-abstract-full" style="display: none;"> Accreting supermassive black holes (SMBHs) located at the center of galaxies are typically surrounded by large quantities of gas and dust. The structure and evolution of this circumnuclear material can be studied at different wavelengths, from the submillimeter to the X-rays. Recent X-ray studies have shown that the covering factor of the obscuring material tends to decrease with increasing Eddington ratio, likely due to radiative feedback on dusty gas. Here we study a sample of 549 nearby (z<0.1) hard X-ray (14-195 keV) selected non-blazar active galactic nuclei (AGN), and use the ratio between the AGN infrared and bolometric luminosity as a proxy of the covering factor. We find that, in agreement with what has been found by X-ray studies of the same sample, the covering factor decreases with increasing Eddington ratio. We also confirm previous findings which showed that obscured AGN typically have larger covering factors than unobscured sources. Finally, we find that the median covering factors of AGN located in different regions of the column density-Eddington ratio diagram are in good agreement with what would be expected from a radiation-regulated growth of SMBHs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.01494v2-abstract-full').style.display = 'none'; document.getElementById('2311.01494v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">ApJ in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.03280">arXiv:2309.03280</a> <span> [<a href="https://arxiv.org/pdf/2309.03280">pdf</a>, <a href="https://arxiv.org/format/2309.03280">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/10.1093/mnras/stad2775">10.1093/mnras/stad2775 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BASS-XL: X-ray variability properties of unobscured Active Galactic Nuclei </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tortosa%2C+A">Alessia Tortosa</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Ar%C3%A9valo%2C+P">Patricia Ar茅valo</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=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">Benny Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotzky%2C+R">Richard Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Temple%2C+M+J">Matthew J. Temple</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">Federica Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Lilayu%2C+A+R">Alejandra Rojas Lilayu</a>, <a href="/search/astro-ph?searchtype=author&query=Kawamuro%2C+T">Taiki Kawamuro</a>, <a href="/search/astro-ph?searchtype=author&query=Caglar%2C+T">Turgay Caglar</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+T">Tingting Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">Kyuseok Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M+C">Meredith Clark Powell</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Urry%2C+C+M">Claudia Megan Urry</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.03280v2-abstract-short" style="display: inline;"> We investigate the X-ray variability properties of Seyfert1 Galaxies belonging to the BAT AGN Spectroscopic Survey (BASS). The sample includes 151 unobscured (N$_{\rm H}<10^{22}$ cm$^{-2}$) AGNs observed with XMM-Newton for a total exposure time of ~27 Ms, representing the deepest variability study done so far with high signal-to-noise XMM-Newton observations, almost doubling the number of observa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.03280v2-abstract-full').style.display = 'inline'; document.getElementById('2309.03280v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.03280v2-abstract-full" style="display: none;"> We investigate the X-ray variability properties of Seyfert1 Galaxies belonging to the BAT AGN Spectroscopic Survey (BASS). The sample includes 151 unobscured (N$_{\rm H}<10^{22}$ cm$^{-2}$) AGNs observed with XMM-Newton for a total exposure time of ~27 Ms, representing the deepest variability study done so far with high signal-to-noise XMM-Newton observations, almost doubling the number of observations analysed in previous works. We constrain the relation between the normalised excess variance and the 2-10 keV AGN luminosities, black hole masses and Eddington ratios. We find a highly significant correlation between $蟽^{2}_{NXS}$ and $M_{\rm BH}$, with a scatter of ~0.85 dex. For sources with high $L_{2-10}$ this correlation has a lower normalization, confirming that more luminous (higher mass) AGNs show less variability. We explored the $蟽^{2}_{NXS}$ vs $M_{\rm BH}$ relation for the sub-sample of sources with $M_{\rm BH}$ estimated via the "reverberation mapping" technique, finding a tighter anti-correlation, with a scatter of ~ 0.65 dex. We examine how the $蟽^{2}_{NXS}$ changes with energy by studying the relation between the variability in the hard (3-10 keV) and the soft (0.2-1 keV)/medium (1-3 keV) energy bands, finding that the spectral components dominating the hard energy band are more variable than the spectral components dominating in softer energy bands, on timescales shorter than 10 ks. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.03280v2-abstract-full').style.display = 'none'; document.getElementById('2309.03280v2-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">v1</span> submitted 6 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Monthly Notices of the Royal Astronomical Society, Volume 526, Issue 2, pp.1687-1698</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.02776">arXiv:2309.02776</a> <span> [<a href="https://arxiv.org/pdf/2309.02776">pdf</a>, <a href="https://arxiv.org/format/2309.02776">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> BASS XXXIV: A Catalog of the Nuclear Mm-wave Continuum Emission Properties of AGNs Constrained on Scales $\lesssim$ 100--200 pc </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kawamuro%2C+T">Taiki Kawamuro</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotzky%2C+R+F">Richard F. Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Imanishi%2C+M">Masatoshi Imanishi</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">Federica Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M+J">Michael J. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">Benny Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Izumi%2C+T">Takuma Izumi</a>, <a href="/search/astro-ph?searchtype=author&query=Ichikawa%2C+K">Kohei Ichikawa</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas%2C+A+F">Alejandra F. Rojas</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+K+L">Krista Lynne Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Shimizu%2C+T">Taro Shimizu</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">Kyuseok Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Brok%2C+J+S+d">Jakob S. den Brok</a>, <a href="/search/astro-ph?searchtype=author&query=Baba%2C+S">Shunsuke Baba</a>, <a href="/search/astro-ph?searchtype=author&query=Balokovic%2C+M">Mislav Balokovic</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+C">Chin-Shin Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Kakkad%2C+D">Darshan Kakkad</a>, <a href="/search/astro-ph?searchtype=author&query=Pfeifle%2C+R+W">Ryan W. Pfeifle</a>, <a href="/search/astro-ph?searchtype=author&query=Temple%2C+M+J">Matthew J. Temple</a>, <a href="/search/astro-ph?searchtype=author&query=Ueda%2C+Y">Yoshihiro Ueda</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M+C">Meredith C. Powell</a> , et al. (3 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.02776v1-abstract-short" style="display: inline;"> We present a catalog of the millimeter-wave (mm-wave) continuum properties of 98 nearby ($z <$ 0.05) active galactic nuclei (AGNs) selected from the 70-month Swift/BAT hard X-ray catalog that have precisely determined X-ray spectral properties and subarcsec-resolution ALMA Band-6 (211--275 GHz) observations as of 2021 April. Due to the hard-X-ray ($>$ 10 keV) selection, the sample is nearly unbias… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.02776v1-abstract-full').style.display = 'inline'; document.getElementById('2309.02776v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.02776v1-abstract-full" style="display: none;"> We present a catalog of the millimeter-wave (mm-wave) continuum properties of 98 nearby ($z <$ 0.05) active galactic nuclei (AGNs) selected from the 70-month Swift/BAT hard X-ray catalog that have precisely determined X-ray spectral properties and subarcsec-resolution ALMA Band-6 (211--275 GHz) observations as of 2021 April. Due to the hard-X-ray ($>$ 10 keV) selection, the sample is nearly unbiased for obscured systems at least up to Compton-thick-level obscuration, and provides the largest number of AGNs with high physical resolution mm-wave data ($\lesssim$ 100--200 pc). Our catalog reports emission peak coordinates, spectral indices, and peak fluxes and luminosities at 1.3 mm (230 GHz). Additionally, high-resolution mm-wave images are provided. Using the images and creating radial surface brightness profiles of mm-wave emission, we identify emission extending from the central source and isolated blob-like emission. Flags indicating the presence of these emission features are tabulated. Among 90 AGNs with significant detections of nuclear emission, 37 AGNs ($\approx$ 41%) appear to have both or one of extended or blob-like components. We, in particular, investigate AGNs that show well-resolved mm-wave components and find that these seem to have a variety of origins (i.e., a jet, radio lobes, a secondary AGN, stellar clusters, a narrow line region, galaxy disk, active star-formation regions, and AGN-driven outflows), and some components have currently unclear origins. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.02776v1-abstract-full').style.display = 'none'; document.getElementById('2309.02776v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">49 pages, 7 figures, 3 tables, accepted for publication in ApJS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.09834">arXiv:2308.09834</a> <span> [<a href="https://arxiv.org/pdf/2308.09834">pdf</a>, <a href="https://arxiv.org/format/2308.09834">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"> The On-axis Jetted Tidal Disruption Event AT2022cmc: X-ray Observations and Broadband Spectral Modeling </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yao%2C+Y">Yuhan Yao</a>, <a href="/search/astro-ph?searchtype=author&query=Lu%2C+W">Wenbin Lu</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Kulkarni%2C+S+R">S. R. Kulkarni</a>, <a href="/search/astro-ph?searchtype=author&query=Gezari%2C+S">Suvi Gezari</a>, <a href="/search/astro-ph?searchtype=author&query=Guolo%2C+M">Muryel Guolo</a>, <a href="/search/astro-ph?searchtype=author&query=Cenko%2C+S+B">S. Bradley Cenko</a>, <a href="/search/astro-ph?searchtype=author&query=Ho%2C+A+Y+Q">Anna Y. Q. Ho</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="2308.09834v2-abstract-short" style="display: inline;"> AT2022cmc was recently reported as the first on-axis jetted tidal disruption event (TDE) discovered in the last decade, and the fourth on-axis jetted TDE candidate known so far. In this work, we present NuSTAR hard X-ray (3--30 keV) observations of AT2022cmc, as well as soft X-ray (0.3--6 keV) observations obtained by NICER, Swift, and XMM-Newton. Our analysis reveals that the broadband X-ray spec… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.09834v2-abstract-full').style.display = 'inline'; document.getElementById('2308.09834v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.09834v2-abstract-full" style="display: none;"> AT2022cmc was recently reported as the first on-axis jetted tidal disruption event (TDE) discovered in the last decade, and the fourth on-axis jetted TDE candidate known so far. In this work, we present NuSTAR hard X-ray (3--30 keV) observations of AT2022cmc, as well as soft X-ray (0.3--6 keV) observations obtained by NICER, Swift, and XMM-Newton. Our analysis reveals that the broadband X-ray spectra can be well described by a broken power-law with $f_谓\propto 谓^{-0.5}$ ($f_谓\propto 谓^{-1}$) below (above) the rest-frame break energy of $E_{\rm bk}\sim 10$ keV at observer-frame $t_{\rm obs}=7.8$ and 17.6 days since discovery. At $t_{\rm obs} = 36.2$ days, the X-ray spectrum is consistent with either a single power-law or a broken power-law. By modeling the spectral energy distribution evolution from radio to hard X-ray across the three NuSTAR observing epochs, we find that the sub-millimeter/radio emission originates from external shocks at large distances $\gtrsim\! 10^{17}$ cm from the black hole, the UV/optical light comes from a thermal envelope with radius $\sim\!10^{15}$ cm, and the X-ray emission is consistent with synchrotron radiation powered by energy dissipation at intermediate radii within the (likely magnetically dominated) jet. We constrain the bulk Lorentz factor of the jet to be of the order 10--100. Our interpretation differs from the model proposed by Pasham et al. (2023) where both the radio and X-rays come from the same emitting zone in a matter-dominated jet. Our model for the jet X-ray emission has broad implications on the nature of relativistic jets in other sources such as gamma-ray bursts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.09834v2-abstract-full').style.display = 'none'; document.getElementById('2308.09834v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 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">17 pages, 11 figures, ApJ accepted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.01800">arXiv:2308.01800</a> <span> [<a href="https://arxiv.org/pdf/2308.01800">pdf</a>, <a href="https://arxiv.org/format/2308.01800">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> BASS XXXV. The $M_\rm{BH}$-$蟽_\rm{\star}$ Relation of 105-Month Swift-BAT Type 1 AGNs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Caglar%2C+T">Turgay Caglar</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=Burtscher%2C+L">Leonard Burtscher</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">Benny Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Erdim%2C+M+K">M. Kiyami Erdim</a>, <a href="/search/astro-ph?searchtype=author&query=Mej%C3%ADa-Restrepo%2C+J+E">Julian E. Mej铆a-Restrepo</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">Federica Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M+C">Meredith C. Powell</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotzky%2C+R">Richard Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Ananna%2C+T+T">Tonima T. Ananna</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%A4r%2C+R+E">Rudolf E. B盲r</a>, <a href="/search/astro-ph?searchtype=author&query=Brandl%2C+B">Bernhard Brandl</a>, <a href="/search/astro-ph?searchtype=author&query=Brinchmann%2C+J">Jarle Brinchmann</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Ichikawa%2C+K">Kohei Ichikawa</a>, <a href="/search/astro-ph?searchtype=author&query=Kakkad%2C+D">Darshan Kakkad</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">Kyuseok Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Riffel%2C+R">Rog茅rio Riffel</a>, <a href="/search/astro-ph?searchtype=author&query=Sartori%2C+L+F">Lia F. Sartori</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+K+L">Krista L. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Urry%2C+C+M">C. Megan Urry</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2308.01800v1-abstract-short" style="display: inline;"> We present two independent measurements of stellar velocity dispersions ( $蟽_\rm{\star}$ ) from the Ca\,H+K \& Mg\,\textsc{i} region (3880--5550~脜) and the Calcium Triplet region (CaT, 8350--8750~脜) for 173 hard X-ray-selected Type 1 AGNs ($z \leq$ 0.08) from the 105-month Swift-BAT catalog. We construct one of the largest samples of local Type 1 AGNs that have both single-epoch (SE) 'virial' blac… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.01800v1-abstract-full').style.display = 'inline'; document.getElementById('2308.01800v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.01800v1-abstract-full" style="display: none;"> We present two independent measurements of stellar velocity dispersions ( $蟽_\rm{\star}$ ) from the Ca\,H+K \& Mg\,\textsc{i} region (3880--5550~脜) and the Calcium Triplet region (CaT, 8350--8750~脜) for 173 hard X-ray-selected Type 1 AGNs ($z \leq$ 0.08) from the 105-month Swift-BAT catalog. We construct one of the largest samples of local Type 1 AGNs that have both single-epoch (SE) 'virial' black hole mass ($M_\rm{BH}$) estimates and $蟽_\rm{\star}$ measurements obtained from high spectral resolution data, allowing us to test the usage of such methods for SMBH studies. We find that the two independent $蟽_\rm{\star}$ measurements are highly consistent with each other, with an average offset of only $0.002\pm0.001$ dex. Comparing $M_\rm{BH}$ estimates based on broad emission lines and stellar velocity dispersion measurements, we find that the former is systematically lower by $\approx$0.12 dex. Consequently, Eddington ratios estimated through broad-line $M_\rm{BH}$ determinations are similarly biased (but in the opposite way). We argue that the discrepancy is driven by extinction in the broad-line region (BLR). We also find an anti-correlation between the offset from the $M_\rm{BH}$ - $蟽_\rm{\star}$ relation and the Eddington ratio. Our sample of Type 1 AGNs shows a shallower $M_\rm{BH}$ - $蟽_\rm{\star}$ relation (with a power law exponent of $\approx$3.5) compared with that of inactive galaxies (with a power-law exponent of $\approx$4.5), confirming earlier results obtained from smaller samples. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.01800v1-abstract-full').style.display = 'none'; document.getElementById('2308.01800v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by the ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.13959">arXiv:2307.13959</a> <span> [<a href="https://arxiv.org/pdf/2307.13959">pdf</a>, <a href="https://arxiv.org/format/2307.13959">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Swift Deep Galactic Plane Survey Classification of Swift J170800$-$402551.8 as a Candidate Intermediate Polar Cataclysmic Variable </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=O%27Connor%2C+B">B. O'Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Gogus%2C+E">E. Gogus</a>, <a href="/search/astro-ph?searchtype=author&query=Hare%2C+J">J. Hare</a>, <a href="/search/astro-ph?searchtype=author&query=Mukai%2C+K">K. Mukai</a>, <a href="/search/astro-ph?searchtype=author&query=Huppenkothen%2C+D">D. Huppenkothen</a>, <a href="/search/astro-ph?searchtype=author&query=Brink%2C+J">J. Brink</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+D+A+H">D. A. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Levan%2C+A">A. Levan</a>, <a href="/search/astro-ph?searchtype=author&query=Baring%2C+M+G">M. G. Baring</a>, <a href="/search/astro-ph?searchtype=author&query=Stewart%2C+R">R. Stewart</a>, <a href="/search/astro-ph?searchtype=author&query=Kouveliotou%2C+C">C. Kouveliotou</a>, <a href="/search/astro-ph?searchtype=author&query=Woudt%2C+P">P. Woudt</a>, <a href="/search/astro-ph?searchtype=author&query=Bellm%2C+E">E. Bellm</a>, <a href="/search/astro-ph?searchtype=author&query=Cenko%2C+S+B">S. B. Cenko</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+P+A">P. A. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Granot%2C+J">J. Granot</a>, <a href="/search/astro-ph?searchtype=author&query=Hailey%2C+C">C. Hailey</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">F. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Hartmann%2C+D">D. Hartmann</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Horst%2C+A+J">A. J. van der Horst</a>, <a href="/search/astro-ph?searchtype=author&query=Kaper%2C+L">L. Kaper</a>, <a href="/search/astro-ph?searchtype=author&query=Kennea%2C+J+A">J. A. Kennea</a>, <a href="/search/astro-ph?searchtype=author&query=Potter%2C+S+B">S. B. Potter</a>, <a href="/search/astro-ph?searchtype=author&query=Slane%2C+P+O">P. O. Slane</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">D. Stern</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="2307.13959v3-abstract-short" style="display: inline;"> Here, we present the results of our multi-wavelength campaign aimed at classifying \textit{Swift} J170800$-$402551.8 as part of the \textit{Swift} Deep Galactic Plane Survey (DGPS). We utilized Target of Opportunity (ToO) observations with \textit{Swift}, \textit{NICER}, \textit{XMM-Newton}, \textit{NuSTAR}, and the Southern African Large Telescope (SALT), as well as multi-wavelength archival obse… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.13959v3-abstract-full').style.display = 'inline'; document.getElementById('2307.13959v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.13959v3-abstract-full" style="display: none;"> Here, we present the results of our multi-wavelength campaign aimed at classifying \textit{Swift} J170800$-$402551.8 as part of the \textit{Swift} Deep Galactic Plane Survey (DGPS). We utilized Target of Opportunity (ToO) observations with \textit{Swift}, \textit{NICER}, \textit{XMM-Newton}, \textit{NuSTAR}, and the Southern African Large Telescope (SALT), as well as multi-wavelength archival observations from \textit{Gaia}, VPHAS, and VVV. The source displays a periodicity of 784 s in our \textit{XMM-Newton} observation. The X-ray spectrum (\textit{XMM-Newton} and \textit{NuSTAR}) can be described by thermal bremsstrahlung radiation with a temperature of $kT$\,$\approx$\,$30$ keV. The phase-folded X-ray lightcurve displays a double-peaked, energy-dependent pulse-profile. We used \textit{Chandra} to precisely localize the source, allowing us to identify and study the multi-wavelength counterpart. Spectroscopy with SALT identified a Balmer H$伪$ line, and potential HeI lines, from the optical counterpart. The faintness of the counterpart ($r$\,$\approx$\,$21$ AB mag) favors a low-mass donor star. Based on these criteria, we classify \textit{Swift} J170800$-$402551.8 as a candidate intermediate polar cataclysmic variable, where the spin period of the white dwarf is 784 s. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.13959v3-abstract-full').style.display = 'none'; document.getElementById('2307.13959v3-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 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted 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/2306.14354">arXiv:2306.14354</a> <span> [<a href="https://arxiv.org/pdf/2306.14354">pdf</a>, <a href="https://arxiv.org/format/2306.14354">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"> The Swift Deep Galactic Plane Survey (DGPS) Phase-I Catalog </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=O%27Connor%2C+B">B. O'Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Kouveliotou%2C+C">C. Kouveliotou</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+P+A">P. A. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Gorgone%2C+N">N. Gorgone</a>, <a href="/search/astro-ph?searchtype=author&query=van+Kooten%2C+A+J">A. J. van Kooten</a>, <a href="/search/astro-ph?searchtype=author&query=Gagnon%2C+S">S. Gagnon</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+H">H. Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Baring%2C+M+G">M. G. Baring</a>, <a href="/search/astro-ph?searchtype=author&query=Bellm%2C+E">E. Bellm</a>, <a href="/search/astro-ph?searchtype=author&query=Beniamini%2C+P">P. Beniamini</a>, <a href="/search/astro-ph?searchtype=author&query=Brink%2C+J">J. Brink</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+D+A+H">D. A. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Cenko%2C+S+B">S. B. Cenko</a>, <a href="/search/astro-ph?searchtype=author&query=Egbo%2C+O+D">O. D. Egbo</a>, <a href="/search/astro-ph?searchtype=author&query=Gogus%2C+E">E. Gogus</a>, <a href="/search/astro-ph?searchtype=author&query=Granot%2C+J">J. Granot</a>, <a href="/search/astro-ph?searchtype=author&query=Hailey%2C+C">C. Hailey</a>, <a href="/search/astro-ph?searchtype=author&query=Hare%2C+J">J. Hare</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">F. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Hartmann%2C+D">D. Hartmann</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Horst%2C+A+J">A. J. van der Horst</a>, <a href="/search/astro-ph?searchtype=author&query=Huppenkothen%2C+D">D. Huppenkothen</a>, <a href="/search/astro-ph?searchtype=author&query=Kaper%2C+L">L. Kaper</a>, <a href="/search/astro-ph?searchtype=author&query=Kargaltsev%2C+O">O. Kargaltsev</a>, <a href="/search/astro-ph?searchtype=author&query=Kennea%2C+J+A">J. A. Kennea</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="2306.14354v3-abstract-short" style="display: inline;"> The \textit{Swift} Deep Galactic Plane Survey is a \textit{Swift} Key Project consisting of 380 tiled pointings covering 40 deg$^{2}$ of the Galactic Plane between longitude $10$\,$<$\,$|l|$\,$<$\,$30$ deg and latitude $|b|$\,$<$\,$0.5$ deg. Each pointing has a $5$ ks exposure, yielding a total of 1.9 Ms spread across the entire survey footprint. Phase-I observations were carried out between March… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.14354v3-abstract-full').style.display = 'inline'; document.getElementById('2306.14354v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.14354v3-abstract-full" style="display: none;"> The \textit{Swift} Deep Galactic Plane Survey is a \textit{Swift} Key Project consisting of 380 tiled pointings covering 40 deg$^{2}$ of the Galactic Plane between longitude $10$\,$<$\,$|l|$\,$<$\,$30$ deg and latitude $|b|$\,$<$\,$0.5$ deg. Each pointing has a $5$ ks exposure, yielding a total of 1.9 Ms spread across the entire survey footprint. Phase-I observations were carried out between March 2017 and May 2021. The Survey is complete to depth $L_X$\,$>$\,$10^{34}$ erg s$^{-1}$ to the edge of the Galaxy. The main Survey goal is to produce a rich sample of new X-ray sources and transients, while also covering a broad discovery space. Here, we introduce the Survey strategy and present a catalog of sources detected during Phase-I observations. In total, we identify 928 X-ray sources, of which 348 are unique to our X-ray catalog. We report on the characteristics of sources in our catalog and highlight sources newly classified and published by the DGPS team. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.14354v3-abstract-full').style.display = 'none'; document.getElementById('2306.14354v3-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, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted in ApJS. This is the final version</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.05576">arXiv:2306.05576</a> <span> [<a href="https://arxiv.org/pdf/2306.05576">pdf</a>, <a href="https://arxiv.org/format/2306.05576">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"> Identification of 1RXS J165424.6-433758 as a polar cataclysmic variable </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=O%27Connor%2C+B">B. O'Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Brink%2C+J">J. Brink</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+D+A+H">D. A. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Mukai%2C+K">K. Mukai</a>, <a href="/search/astro-ph?searchtype=author&query=Kouveliotou%2C+C">C. Kouveliotou</a>, <a href="/search/astro-ph?searchtype=author&query=Gogus%2C+E">E. Gogus</a>, <a href="/search/astro-ph?searchtype=author&query=Potter%2C+S+B">S. B. Potter</a>, <a href="/search/astro-ph?searchtype=author&query=Woudt%2C+P">P. Woudt</a>, <a href="/search/astro-ph?searchtype=author&query=Lien%2C+A">A. Lien</a>, <a href="/search/astro-ph?searchtype=author&query=Levan%2C+A">A. Levan</a>, <a href="/search/astro-ph?searchtype=author&query=Kargaltsev%2C+O">O. Kargaltsev</a>, <a href="/search/astro-ph?searchtype=author&query=Baring%2C+M+G">M. G. Baring</a>, <a href="/search/astro-ph?searchtype=author&query=Bellm%2C+E">E. Bellm</a>, <a href="/search/astro-ph?searchtype=author&query=Cenko%2C+S+B">S. B. Cenko</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+P+A">P. A. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Granot%2C+J">J. Granot</a>, <a href="/search/astro-ph?searchtype=author&query=Hailey%2C+C">C. Hailey</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">F. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Hartmann%2C+D">D. Hartmann</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Horst%2C+A+J">A. J. van der Horst</a>, <a href="/search/astro-ph?searchtype=author&query=Huppenkothen%2C+D">D. Huppenkothen</a>, <a href="/search/astro-ph?searchtype=author&query=Kaper%2C+L">L. Kaper</a>, <a href="/search/astro-ph?searchtype=author&query=Kennea%2C+J+A">J. A. Kennea</a>, <a href="/search/astro-ph?searchtype=author&query=Slane%2C+P+O">P. O. Slane</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">D. Stern</a> , et al. (3 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.05576v2-abstract-short" style="display: inline;"> We present the results of our X-ray, ultraviolet, and optical follow-up campaigns of 1RXS J165424.6-433758, an X-ray source detected with the \textit{Swift} Deep Galactic Plane Survey (DGPS). The source X-ray spectrum (\textit{Swift} and \textit{NuSTAR}) is described by thermal bremsstrahlung radiation with a temperature of $kT=10.1\pm1.2$ keV, yielding an X-ray ($0.3-10$ keV) luminosity… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.05576v2-abstract-full').style.display = 'inline'; document.getElementById('2306.05576v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.05576v2-abstract-full" style="display: none;"> We present the results of our X-ray, ultraviolet, and optical follow-up campaigns of 1RXS J165424.6-433758, an X-ray source detected with the \textit{Swift} Deep Galactic Plane Survey (DGPS). The source X-ray spectrum (\textit{Swift} and \textit{NuSTAR}) is described by thermal bremsstrahlung radiation with a temperature of $kT=10.1\pm1.2$ keV, yielding an X-ray ($0.3-10$ keV) luminosity $L_X=(6.5\pm0.8)\times10^{31}$ erg s$^{-1}$ at a \textit{Gaia} distance of 460 pc. Spectroscopy with the Southern African Large Telescope (SALT) revealed a flat continuum dominated by emission features, demonstrating an inverse Balmer decrement, the $\lambda4640$ Bowen blend, almost a dozen HeI lines, and HeII $\lambda4541$, $\lambda4686$ and $位5411$. Our high-speed photometry demonstrates a preponderance of flickering and flaring episodes, and revealed the orbital period of the system, $P_\textrm{orb}=2.87$ hr, which fell well within the cataclysmic variable (CV) period gap between $2-3$ hr. These features classify 1RXS J165424.6-433758 as a nearby polar magnetic CV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.05576v2-abstract-full').style.display = 'none'; document.getElementById('2306.05576v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.04827">arXiv:2306.04827</a> <span> [<a href="https://arxiv.org/pdf/2306.04827">pdf</a>, <a href="https://arxiv.org/format/2306.04827">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/acdf4e">10.3847/2041-8213/acdf4e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Early hard X-rays from the nearby core-collapse supernova SN2023ixf </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Grefenstette%2C+B+W">Brian W. Grefenstette</a>, <a href="/search/astro-ph?searchtype=author&query=Brightman%2C+M">Murray Brightman</a>, <a href="/search/astro-ph?searchtype=author&query=Earnshaw%2C+H+P">Hannah P. Earnshaw</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F+A">Fiona A. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Margutti%2C+R">Raffaella Margutti</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.04827v1-abstract-short" style="display: inline;"> We present NuSTAR observations of the nearby SN 2023ixf in M101 (d=6.9 Mpc) which provide the earliest hard X-ray detection of a non-relativistic stellar explosion to date at $未t\approx$4-d and $未t\approx$11-d. The spectra are well described by a hot thermal bremsstrahlung continuum with $T>25 \rm{keV}$ shining through a thick neutral medium with a neutral hydrogen column that decreases with time… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.04827v1-abstract-full').style.display = 'inline'; document.getElementById('2306.04827v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.04827v1-abstract-full" style="display: none;"> We present NuSTAR observations of the nearby SN 2023ixf in M101 (d=6.9 Mpc) which provide the earliest hard X-ray detection of a non-relativistic stellar explosion to date at $未t\approx$4-d and $未t\approx$11-d. The spectra are well described by a hot thermal bremsstrahlung continuum with $T>25 \rm{keV}$ shining through a thick neutral medium with a neutral hydrogen column that decreases with time (initial $N_{\rm{Hint}}=2.6\times 10^{23} \rm{cm^{-2}}$). A prominent neutral Fe K$伪$ emission line is clearly detected, similar to other strongly interacting SNe such as SN2020jl. The rapidly decreasing intrinsic absorption with time suggests the presence of a dense but confined circumstellar medium (CSM). The absorbed broadband X-ray luminosity (0.3--79 keV) is $L_{X} \approx 2.5 \times 10^{40}$ erg s$^{-1}$ during both epochs, with the increase in overall X-ray flux related to the decrease in the absorbing column. Interpreting these observations in the context of thermal bremsstrahlung radiation originating from the interaction of the SN shock with a dense medium we infer large particle densities in excess of $n_{\rm{CSM}}\approx 4\times 10^{8} \rm{cm^{-3}}$ at $r<10^{15} \rm{cm}$, corresponding to an enhanced progenitor mass-loss rate of $\dot M \approx 3\times 10^{-4}$ M$_{\odot}$ yr$^{-1}$ for an assumed wind velocity of $v_w=50$ km s$^{-1}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.04827v1-abstract-full').style.display = 'none'; document.getElementById('2306.04827v1-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 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 2 figures. Submitted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.07962">arXiv:2304.07962</a> <span> [<a href="https://arxiv.org/pdf/2304.07962">pdf</a>, <a href="https://arxiv.org/format/2304.07962">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="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/acd0ae">10.3847/1538-3881/acd0ae <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measuring the Cosmic X-ray Background in 3-20keV with Straylight from NuSTAR </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rossland%2C+S">Steven Rossland</a>, <a href="/search/astro-ph?searchtype=author&query=Wik%2C+D">Daniel Wik</a>, <a href="/search/astro-ph?searchtype=author&query=Grefenstette%2C+B">Brian Grefenstette</a>, <a href="/search/astro-ph?searchtype=author&query=Cappelluti%2C+N">Nico Cappelluti</a>, <a href="/search/astro-ph?searchtype=author&query=Civano%2C+F">Francesca Civano</a>, <a href="/search/astro-ph?searchtype=author&query=Gastaldello%2C+F">Fabio Gastaldello</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">Roberto Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Hornschemeier%2C+A">Ann Hornschemeier</a>, <a href="/search/astro-ph?searchtype=author&query=Hickox%2C+R">Ryan Hickox</a>, <a href="/search/astro-ph?searchtype=author&query=Krivonos%2C+R">Roman Krivonos</a>, <a href="/search/astro-ph?searchtype=author&query=Madsen%2C+K">Kristin Madsen</a>, <a href="/search/astro-ph?searchtype=author&query=Molendi%2C+S">Silvano Molendi</a>, <a href="/search/astro-ph?searchtype=author&query=Ptak%2C+A">Andrew Ptak</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Zoglauer%2C+A">Andreas 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="2304.07962v2-abstract-short" style="display: inline;"> By characterizing the contribution of stray light to large datasets from the NuSTAR X-ray observatory collected over 2012--2017, we report a measurement of the cosmic X-ray background in the 3--20 keV energy range. These data represent $\sim20\%$ sky coverage while avoiding Galactic Ridge X-ray emission and are less weighted by deep, survey fields than previous measurements with NuSTAR. Images in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.07962v2-abstract-full').style.display = 'inline'; document.getElementById('2304.07962v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.07962v2-abstract-full" style="display: none;"> By characterizing the contribution of stray light to large datasets from the NuSTAR X-ray observatory collected over 2012--2017, we report a measurement of the cosmic X-ray background in the 3--20 keV energy range. These data represent $\sim20\%$ sky coverage while avoiding Galactic Ridge X-ray emission and are less weighted by deep, survey fields than previous measurements with NuSTAR. Images in narrow energy bands are stacked in detector space and spatially fit with a model representing the stray light and uniform pattern expected from the cosmic X-ray background and the instrumental background, respectively. We establish baseline flux values from Earth-occulted data and validate the fitting method on stray light observations of the Crab, which further serve to calibrate the resulting spectra. We present independent spectra of the cosmic X-ray background with the FPMA and FPMB detector arrays, which are in excellent agreement with the canonical characterization by HEAO 1 and are $10\%$ lower than most subsequent measurements; $F_{\rm{3-20~keV}}^{FPMA} = 2.63 \times 10^{-11}~\rm{erg~s^{-1}~cm^{-2}~deg^{-2}}$ and $F_{\rm{3-20~keV}}^{FPMB} = 2.58 \times 10^{-11}~\rm{erg~s^{-1}~cm^{-2}~deg^{-2}}$. We discuss these results in light of previous measurements of the cosmic X-ray background and consider the impact of systematic uncertainties on our spectra. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.07962v2-abstract-full').style.display = 'none'; document.getElementById('2304.07962v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 15 figures, 4 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.03609">arXiv:2301.03609</a> <span> [<a href="https://arxiv.org/pdf/2301.03609">pdf</a>, <a href="https://arxiv.org/format/2301.03609">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/aca8f0">10.3847/2041-8213/aca8f0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> UGC 4211: A Confirmed Dual Active Galactic Nucleus in the Local Universe at 230 pc Nuclear Separation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M+J">Michael J. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Treister%2C+E">Ezequiel Treister</a>, <a href="/search/astro-ph?searchtype=author&query=Kakkad%2C+D">Darshan Kakkad</a>, <a href="/search/astro-ph?searchtype=author&query=Casey-Clyde%2C+J+A">J. Andrew Casey-Clyde</a>, <a href="/search/astro-ph?searchtype=author&query=Kawamuro%2C+T">Taiki Kawamuro</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+J">Jonathan Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Foord%2C+A">Adi Foord</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">Benny Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotzky%2C+R">Richard Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Barcos-Munoz%2C+L">Loreto Barcos-Munoz</a>, <a href="/search/astro-ph?searchtype=author&query=Blecha%2C+L">Laura Blecha</a>, <a href="/search/astro-ph?searchtype=author&query=Connor%2C+T">Thomas Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+T">Tingting Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Magno%2C+M">Macon Magno</a>, <a href="/search/astro-ph?searchtype=author&query=Mingarelli%2C+C+M+F">Chiara M. F. Mingarelli</a>, <a href="/search/astro-ph?searchtype=author&query=Muller-Sanchez%2C+F">Francisco Muller-Sanchez</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">Kyuseok Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Shimizu%2C+T+T">T. Taro Shimizu</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+K+L">Krista L. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Tello%2C+M+P">Miguel Parra Tello</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2301.03609v1-abstract-short" style="display: inline;"> We present multi-wavelength high-spatial resolution (~0.1'', 70 pc) observations of UGC 4211 at z=0.03474, a late-stage major galaxy merger at the closest nuclear separation yet found in near-IR imaging (0.32'', ~230 pc projected separation). Using Hubble Space Telescope/STIS, VLT/MUSE+AO, Keck/OSIRIS+AO spectroscopy, and ALMA observations, we show that the spatial distribution, optical and NIR em… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.03609v1-abstract-full').style.display = 'inline'; document.getElementById('2301.03609v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.03609v1-abstract-full" style="display: none;"> We present multi-wavelength high-spatial resolution (~0.1'', 70 pc) observations of UGC 4211 at z=0.03474, a late-stage major galaxy merger at the closest nuclear separation yet found in near-IR imaging (0.32'', ~230 pc projected separation). Using Hubble Space Telescope/STIS, VLT/MUSE+AO, Keck/OSIRIS+AO spectroscopy, and ALMA observations, we show that the spatial distribution, optical and NIR emission lines, and millimeter continuum emission are all consistent with both nuclei being powered by accreting supermassive black holes (SMBHs). Our data, combined with common black hole mass prescriptions, suggests that both SMBHs have similar masses, log MBH~8.1 (south) and log MBH~8.3 (north), respectively. The projected separation of 230 pc (~6X the black hole sphere of influence) represents the closest-separation dual AGN studied to date with multi-wavelength resolved spectroscopy and shows the potential of nuclear (<50 pc) continuum observations with ALMA to discover hidden growing SMBH pairs. While the exact occurrence rate of close-separation dual AGN is not yet known, it may be surprisingly high, given that UGC 4211 was found within a small, volume-limited sample of nearby hard X-ray detected AGN. Observations of dual SMBH binaries in the sub-kpc regime at the final stages of dynamical friction provide important constraints for future gravitational wave observatories. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.03609v1-abstract-full').style.display = 'none'; document.getElementById('2301.03609v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 7 figures, 2 tables, published in ApJL</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJL, 942, 1, L24, Published 9 January 2023 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.04478">arXiv:2211.04478</a> <span> [<a href="https://arxiv.org/pdf/2211.04478">pdf</a>, <a href="https://arxiv.org/format/2211.04478">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/10.1093/mnras/stac3279">10.1093/mnras/stac3279 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BASS XXXIX: Swift-BAT AGN with changing-look optical spectra </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Temple%2C+M+J">Matthew J. Temple</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M+J">Michael J. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">Benny Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotzky%2C+R">Richard Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas%2C+A+F">Alejandra F. Rojas</a>, <a href="/search/astro-ph?searchtype=author&query=Caglar%2C+T">Turgay Caglar</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">Kyuseok Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Gonzalez%2C+E+P">Estefania Padilla Gonzalez</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M+C">Meredith C. Powell</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">Federica Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Riffel%2C+R">Rog茅rio Riffel</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Urry%2C+C+M">C. Megan Urry</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2211.04478v2-abstract-short" style="display: inline;"> Changing-look (CL) AGN are unique probes of accretion onto supermassive black holes (SMBHs), especially when simultaneous observations in complementary wavebands allow investigations into the properties of their accretion flows. We present the results of a search for CL behaviour in 412 Swift-BAT detected AGN with multiple epochs of optical spectroscopy from the BAT AGN Spectroscopic Survey (BASS)… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.04478v2-abstract-full').style.display = 'inline'; document.getElementById('2211.04478v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.04478v2-abstract-full" style="display: none;"> Changing-look (CL) AGN are unique probes of accretion onto supermassive black holes (SMBHs), especially when simultaneous observations in complementary wavebands allow investigations into the properties of their accretion flows. We present the results of a search for CL behaviour in 412 Swift-BAT detected AGN with multiple epochs of optical spectroscopy from the BAT AGN Spectroscopic Survey (BASS). 125 of these AGN also have 14-195 keV ultra-hard X-ray light-curves from Swift-BAT which are contemporaneous with the epochs of optical spectroscopy. Eight CL events are presented for the first time, where the appearance or disappearance of broad Balmer line emission leads to a change in the observed Seyfert type classification. Combining with known events from the literature, 21 AGN from BASS are now known to display CL behaviour. Nine CL events have 14-195 keV data available, and five of these CL events can be associated with significant changes in their 14-195 keV flux from BAT. The ultra-hard X-ray flux is less affected by obscuration and so these changes in the 14-195 keV band suggest that the majority of our CL events are not due to changes in line-of-sight obscuration. We derive a CL rate of 0.7-6.2 per cent on 10-25 year time-scales, and show that many transitions happen within at most a few years. Our results motivate further multi-wavelength observations with higher cadence to better understand the variability physics of accretion onto SMBHs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.04478v2-abstract-full').style.display = 'none'; document.getElementById('2211.04478v2-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 7 figures, plus appendix. v2: updated references. Published in MNRAS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> MNRAS 518, 2938 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.08401">arXiv:2210.08401</a> <span> [<a href="https://arxiv.org/pdf/2210.08401">pdf</a>, <a href="https://arxiv.org/format/2210.08401">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/ac9979">10.3847/2041-8213/ac9979 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Probing the Structure and Evolution of BASS AGN through Eddington Ratios </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ananna%2C+T+T">Tonima Tasnim Ananna</a>, <a href="/search/astro-ph?searchtype=author&query=Urry%2C+C+M">C. Megan Urry</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Natarajan%2C+P">Priyamvada Natarajan</a>, <a href="/search/astro-ph?searchtype=author&query=Hickox%2C+R+C">Ryan C. Hickox</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">Benny Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Treister%2C+E">Ezequiel Treister</a>, <a href="/search/astro-ph?searchtype=author&query=Weigel%2C+A+K">Anna K. Weigel</a>, <a href="/search/astro-ph?searchtype=author&query=Ueda%2C+Y">Yoshihiro Ueda</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=Bauer%2C+F+E">F. E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Temple%2C+M+J">Matthew J. Temple</a>, <a href="/search/astro-ph?searchtype=author&query=Balokovic%2C+M">Mislav Balokovic</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotzky%2C+R">Richard Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Auge%2C+C">Connor Auge</a>, <a href="/search/astro-ph?searchtype=author&query=Sanders%2C+D+B">David B. Sanders</a>, <a href="/search/astro-ph?searchtype=author&query=Kakkad%2C+D">Darshan Kakkad</a>, <a href="/search/astro-ph?searchtype=author&query=Sartori%2C+L+F">Lia F. Sartori</a>, <a href="/search/astro-ph?searchtype=author&query=Marchesi%2C+S">Stefano Marchesi</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">Kyuseok Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Caglar%2C+T">Turgay Caglar</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M+C">Meredith C. Powell</a>, <a href="/search/astro-ph?searchtype=author&query=Podjed%2C+S+A">Stephanie A. Podjed</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2210.08401v1-abstract-short" style="display: inline;"> We constrain the intrinsic Eddington ratio (\lamEdd ) distribution function for local AGN in bins of low and high obscuration (log NH <= 22 and 22 < log NH < 25), using the Swift-BAT 70-month/BASS DR2 survey. We interpret the fraction of obscured AGN in terms of circum-nuclear geometry and temporal evolution. Specifically, at low Eddington ratios (log lamEdd < -2), obscured AGN outnumber unobscure… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.08401v1-abstract-full').style.display = 'inline'; document.getElementById('2210.08401v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.08401v1-abstract-full" style="display: none;"> We constrain the intrinsic Eddington ratio (\lamEdd ) distribution function for local AGN in bins of low and high obscuration (log NH <= 22 and 22 < log NH < 25), using the Swift-BAT 70-month/BASS DR2 survey. We interpret the fraction of obscured AGN in terms of circum-nuclear geometry and temporal evolution. Specifically, at low Eddington ratios (log lamEdd < -2), obscured AGN outnumber unobscured ones by a factor of ~4, reflecting the covering factor of the circum-nuclear material (0.8, or a torus opening angle of ~ 34 degrees). At high Eddington ratios (\log lamEdd > -1), the trend is reversed, with < 30% of AGN having log NH > 22, which we suggest is mainly due to the small fraction of time spent in a highly obscured state. Considering the Eddington ratio distribution function of narrow-line and broad-line AGN from our prior work, we see a qualitatively similar picture. To disentangle temporal and geometric effects at high lamEdd, we explore plausible clearing scenarios such that the time-weighted covering factors agree with the observed population ratio. We find that the low fraction of obscured AGN at high lamEdd is primarily due to the fact that the covering factor drops very rapidly, with more than half the time is spent with < 10% covering factor. We also find that nearly all obscured AGN at high-lamEdd exhibit some broad-lines. We suggest that this is because the height of the depleted torus falls below the height of the broad-line region, making the latter visible from all lines of sight. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.08401v1-abstract-full').style.display = 'none'; document.getElementById('2210.08401v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 October, 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">Accepted by ApJL</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.09929">arXiv:2209.09929</a> <span> [<a href="https://arxiv.org/pdf/2209.09929">pdf</a>, <a href="https://arxiv.org/format/2209.09929">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/ac937f">10.3847/1538-4357/ac937f <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BASS XXXIII: Swift-BAT blazars and their jets through cosmic time </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Marcotulli%2C+L">L. Marcotulli</a>, <a href="/search/astro-ph?searchtype=author&query=Ajello%2C+M">M. Ajello</a>, <a href="/search/astro-ph?searchtype=author&query=Urry%2C+C+M">C. M. Urry</a>, <a href="/search/astro-ph?searchtype=author&query=Paliya%2C+V+S">V. S. Paliya</a>, <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M">M. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">K. Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Madejski%2C+G">G. Madejski</a>, <a href="/search/astro-ph?searchtype=author&query=Ueda%2C+Y">Y. Ueda</a>, <a href="/search/astro-ph?searchtype=author&query=Balokovi%C4%87%2C+M">M. Balokovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">B. Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">F. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">C. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">F. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M+C">M. C. Powell</a>, <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+B">BASS Collaboration</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="2209.09929v1-abstract-short" style="display: inline;"> We derive the most up-to-date Swift-Burst Alert Telescope (BAT) blazar luminosity function in the 14-195 keV range, making use of a clean sample of 118 blazars detected in the BAT 105-month survey catalog, with newly obtained redshifts from the BAT AGN Spectroscopic Survey (BASS). We determine the best-fit X-ray luminosity function for the whole blazar population, as well as for Flat Spectrum Radi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.09929v1-abstract-full').style.display = 'inline'; document.getElementById('2209.09929v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.09929v1-abstract-full" style="display: none;"> We derive the most up-to-date Swift-Burst Alert Telescope (BAT) blazar luminosity function in the 14-195 keV range, making use of a clean sample of 118 blazars detected in the BAT 105-month survey catalog, with newly obtained redshifts from the BAT AGN Spectroscopic Survey (BASS). We determine the best-fit X-ray luminosity function for the whole blazar population, as well as for Flat Spectrum Radio Quasars (FSRQs) alone. The main results are: (1) at any redshift, BAT detects the most luminous blazars, above any possible break in their luminosity distribution, which means we cannot differentiate between density and luminosity evolution; (2) the whole blazar population, dominated by FSRQs, evolves positively up to redshift z~4.3, confirming earlier results and implying lower number densities of blazars at higher redshifts than previously estimated. The contribution of this source class to the Cosmic X-ray Background at 14-195 keV can range from 5-18%, while possibly accounting for 100% of the MeV background. We also derived the average 14 keV-10 GeV SED for BAT blazars, which allows us to predict the number counts of sources in the MeV range, as well as the expected number of high-energy (>100 TeV) neutrinos. A mission like COSI, will detect 40 MeV blazars and 2 coincident neutrinos. Finally, taking into account beaming selection effects, the distribution and properties of the parent population of these extragalactic jets are derived. We find that the distribution of viewing angles is quite narrow, with most sources aligned within < 5掳 of the line of sight. Moreover, the average Lorentz factor, <$螕$>= 8-12, is lower than previously suggested for these powerful sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.09929v1-abstract-full').style.display = 'none'; document.getElementById('2209.09929v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in the Astrophysical Journal; 33 pages; 8 Tables; 16 Figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.02728">arXiv:2209.02728</a> <span> [<a href="https://arxiv.org/pdf/2209.02728">pdf</a>, <a href="https://arxiv.org/format/2209.02728">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac8f8e">10.3847/1538-4357/ac8f8e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BASS. XXXVI. Constraining the Local Supermassive Black Hole - Halo Connection with BASS DR2 AGN </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M+C">M. C. Powell</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=Caglar%2C+T">T. Caglar</a>, <a href="/search/astro-ph?searchtype=author&query=Cappelluti%2C+N">N. Cappelluti</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">F. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Irving%2C+B+E">B. E. Irving</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=Mantz%2C+A+B">A. B. Mantz</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">K. Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">C. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Shaper%2C+R+J">R. J. Shaper</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">B. Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Urry%2C+C+M">C. M. Urry</a>, <a href="/search/astro-ph?searchtype=author&query=Wong%2C+J">J. Wong</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="2209.02728v2-abstract-short" style="display: inline;"> We investigate the connection between supermassive black holes (SMBHs) and their host dark matter halos in the local universe using the clustering statistics and luminosity function of AGN from the Swift/BAT AGN Spectroscopic survey (BASS DR2). By forward-modeling AGN activity into snapshot halo catalogs from N-body simulations, we test a scenario in which SMBH mass correlates with dark matter (su… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.02728v2-abstract-full').style.display = 'inline'; document.getElementById('2209.02728v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.02728v2-abstract-full" style="display: none;"> We investigate the connection between supermassive black holes (SMBHs) and their host dark matter halos in the local universe using the clustering statistics and luminosity function of AGN from the Swift/BAT AGN Spectroscopic survey (BASS DR2). By forward-modeling AGN activity into snapshot halo catalogs from N-body simulations, we test a scenario in which SMBH mass correlates with dark matter (sub)halo mass for fixed stellar mass. We compare this to a model absent of this correlation, where stellar mass alone determines the SMBH mass. We find that while both simple models are able to largely reproduce the abundance and overall clustering of AGN, the model in which black hole mass is tightly correlated with halo mass is preferred by the data by $1.8蟽$. When including an independent measurement on the black hole mass-halo mass correlation, this model is preferred by $4.6蟽$. We show that the clustering trends with black hole mass can further break the degeneracies between the two scenarios, and that our preferred model reproduces the measured clustering differences on 1-halo scales between large and small black hole masses. These results indicate that the halo binding energy is fundamentally connected to the growth of supermassive black holes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.02728v2-abstract-full').style.display = 'none'; document.getElementById('2209.02728v2-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 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 938, 77 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.00014">arXiv:2209.00014</a> <span> [<a href="https://arxiv.org/pdf/2209.00014">pdf</a>, <a href="https://arxiv.org/ps/2209.00014">ps</a>, <a href="https://arxiv.org/format/2209.00014">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac8e67">10.3847/1538-4357/ac8e67 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BASS XXXVII: The role of radiative feedback in the growth and obscuration properties of nearby supermassive black holes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">C. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Ananna%2C+T+T">T. T. Ananna</a>, <a href="/search/astro-ph?searchtype=author&query=Temple%2C+M+J">M. J. Temple</a>, <a href="/search/astro-ph?searchtype=author&query=Urry%2C+C+M">C. M. Urry</a>, <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M+J">M. J. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">B. Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Ueda%2C+Y">Y. Ueda</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">F. E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Treister%2C+E">E. Treister</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">G. C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">K. Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Paltani%2C+S">S. Paltani</a>, <a href="/search/astro-ph?searchtype=author&query=Stalevski%2C+M">M. Stalevski</a>, <a href="/search/astro-ph?searchtype=author&query=Ho%2C+L+C">L. C. Ho</a>, <a href="/search/astro-ph?searchtype=author&query=Fabian%2C+A+C">A. C. Fabian</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotzky%2C+R">R. Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+C+S">C. S. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">F. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Kakkad%2C+D">D. Kakkad</a>, <a href="/search/astro-ph?searchtype=author&query=Sartori%2C+L">L. Sartori</a>, <a href="/search/astro-ph?searchtype=author&query=Baer%2C+R">R. Baer</a>, <a href="/search/astro-ph?searchtype=author&query=Caglar%2C+T">T. Caglar</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M">M. Powell</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">F. Harrison</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.00014v1-abstract-short" style="display: inline;"> We study the relation between obscuration and supermassive black hole (SMBH) growth using a large sample of hard X-ray selected Active Galactic Nuclei (AGN). We find a strong decrease in the fraction of obscured sources above the Eddington limit for dusty gas ($\log 位_{\rm Edd}\gtrsim -2$) confirming earlier results, and consistent with the radiation-regulated unification model. This also explains… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.00014v1-abstract-full').style.display = 'inline'; document.getElementById('2209.00014v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.00014v1-abstract-full" style="display: none;"> We study the relation between obscuration and supermassive black hole (SMBH) growth using a large sample of hard X-ray selected Active Galactic Nuclei (AGN). We find a strong decrease in the fraction of obscured sources above the Eddington limit for dusty gas ($\log 位_{\rm Edd}\gtrsim -2$) confirming earlier results, and consistent with the radiation-regulated unification model. This also explains the difference in the Eddington ratio distribution functions (ERDFs) of type 1 and type 2 AGN obtained by a recent study. The break in the ERDF of nearby AGN is at $\log 位_{\rm Edd}^{*}=-1.34\pm0.07$. This corresponds to the $位_{\rm Edd}$ where AGN transition from having most of their sky covered by obscuring material to being mostly devoid of absorbing material. A similar trend is observed for the luminosity function, which implies that most of the SMBH growth in the local Universe happens when the AGN is covered by a large reservoir of gas and dust. These results could be explained with a radiation-regulated growth model, in which AGN move in the $N_{\rm H}-位_{\rm Edd}$ plane during their life cycle. The growth episode starts with the AGN mostly unobscured and accreting at low $位_{\rm Edd}$. As the SMBH is further fueled, $位_{\rm Edd}$, $N_{\rm H}$ and covering factor increase, leading AGN to be preferentially observed as obscured. Once $位_{\rm Edd}$ reaches the Eddington limit for dusty gas, the covering factor and $N_{\rm H}$ rapidly decrease, leading the AGN to be typically observed as unobscured. As the remaining fuel is depleted, the SMBH goes back into a quiescent phase. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.00014v1-abstract-full').style.display = 'none'; document.getElementById('2209.00014v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.09010">arXiv:2208.09010</a> <span> [<a href="https://arxiv.org/pdf/2208.09010">pdf</a>, <a href="https://arxiv.org/format/2208.09010">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/acd5d5">10.3847/1538-4357/acd5d5 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> AT2019wxt: An ultra-stripped supernova candidate discovered in electromagnetic follow-up of a gravitational wave trigger </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shivkumar%2C+H">Hinna Shivkumar</a>, <a href="/search/astro-ph?searchtype=author&query=Jaodand%2C+A+D">Amruta D. Jaodand</a>, <a href="/search/astro-ph?searchtype=author&query=Balasubramanian%2C+A">Arvind Balasubramanian</a>, <a href="/search/astro-ph?searchtype=author&query=Fremling%2C+C">Christoffer Fremling</a>, <a href="/search/astro-ph?searchtype=author&query=Corsi%2C+A">Alessandra Corsi</a>, <a href="/search/astro-ph?searchtype=author&query=Tzanidakis%2C+A">Anastasios Tzanidakis</a>, <a href="/search/astro-ph?searchtype=author&query=Nissanke%2C+S">Samaya Nissanke</a>, <a href="/search/astro-ph?searchtype=author&query=Kasliwal%2C+M">Mansi Kasliwal</a>, <a href="/search/astro-ph?searchtype=author&query=Brightman%2C+M">Murray Brightman</a>, <a href="/search/astro-ph?searchtype=author&query=Raaijmakers%2C+G">Geert Raaijmakers</a>, <a href="/search/astro-ph?searchtype=author&query=Madsen%2C+K+K">Kristin Kruse Madsen</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Carbone%2C+D">Dario Carbone</a>, <a href="/search/astro-ph?searchtype=author&query=J.%2C+N+A">Nayana A. J.</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%A9sert%2C+J">Jean-Michel D茅sert</a>, <a href="/search/astro-ph?searchtype=author&query=Andreoni%2C+I">Igor Andreoni</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="2208.09010v1-abstract-short" style="display: inline;"> We present optical, radio and X-ray observations of a rapidly-evolving transient AT2019wxt (PS19hgw), discovered during the search for an electromagnetic (EM) counterpart to the gravitational-wave (GW) trigger S191213g (LIGO Scientific Collaboration & Virgo Collaboration 2019a). Although S191213g was not confirmed as a significant GW event in the off-line analysis of LIGO-Virgo data, AT2019wxt rem… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.09010v1-abstract-full').style.display = 'inline'; document.getElementById('2208.09010v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.09010v1-abstract-full" style="display: none;"> We present optical, radio and X-ray observations of a rapidly-evolving transient AT2019wxt (PS19hgw), discovered during the search for an electromagnetic (EM) counterpart to the gravitational-wave (GW) trigger S191213g (LIGO Scientific Collaboration & Virgo Collaboration 2019a). Although S191213g was not confirmed as a significant GW event in the off-line analysis of LIGO-Virgo data, AT2019wxt remained an interesting transient due its peculiar nature. The optical/NIR light curve of AT2019wxt displayed a double-peaked structure evolving rapidly in a manner analogous to currently know ultra-stripped supernovae (USSNe) candidates. This double-peaked structure suggests presence of an extended envelope around the progenitor, best modelled with two-components: i) early-time shock-cooling emission and ii) late-time radioactive $^{56}$Ni decay. We constrain the ejecta mass of AT2019wxt at $M_{ej} \approx{0.20 M_{\odot}}$ which indicates a significantly stripped progenitor that was possibly in a binary system. We also followed-up AT2019wxt with long-term Chandra and Jansky Very Large Array observations spanning $\sim$260 days. We detected no definitive counterparts at the location of AT2019wxt in these long-term X-ray and radio observational campaigns. We establish the X-ray upper limit at $9.93\times10^{-17}$ erg cm$^{-2}$ s$^{-1}$ and detect an excess radio emission from the region of AT2019wxt. However, there is little evidence for SN1993J- or GW170817-like variability of the radio flux over the course of our observations. A substantial host galaxy contribution to the measured radio flux is likely. The discovery and early-time peak capture of AT2019wxt in optical/NIR observation during EMGW follow-up observations highlights the need of dedicated early, multi-band photometric observations to identify USSNe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.09010v1-abstract-full').style.display = 'none'; document.getElementById('2208.09010v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 14 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/2208.03880">arXiv:2208.03880</a> <span> [<a href="https://arxiv.org/pdf/2208.03880">pdf</a>, <a href="https://arxiv.org/format/2208.03880">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac8794">10.3847/1538-4357/ac8794 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BASS XXXII: Studying the Nuclear Mm-wave Continuum Emission of AGNs with ALMA at Scales $\lesssim$ 100-200 pc </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kawamuro%2C+T">Taiki Kawamuro</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Imanishi%2C+M">Masatoshi Imanishi</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotzky%2C+R+F">Richard F. Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Izumi%2C+T">Takuma Izumi</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">Federica Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M+J">Michael J. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">Benny Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Ichikawa%2C+K">Kohei Ichikawa</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas%2C+A+F">Alejandra F. Rojas</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+K+L">Krista Lynne Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Shimizu%2C+T">Taro Shimizu</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">Kyuseok Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Brok%2C+J+S+d">Jakob S. den Brok</a>, <a href="/search/astro-ph?searchtype=author&query=Baba%2C+S">Shunsuke Baba</a>, <a href="/search/astro-ph?searchtype=author&query=Balokovi%C4%87%2C+M">Mislav Balokovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+C">Chin-Shin Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Kakkad%2C+D">Darshan Kakkad</a>, <a href="/search/astro-ph?searchtype=author&query=Pfeifle%2C+R+W">Ryan W. Pfeifle</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Temple%2C+M+J">Matthew J. Temple</a>, <a href="/search/astro-ph?searchtype=author&query=Ueda%2C+Y">Yoshihiro Ueda</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M+C">Meredith C. Powell</a> , et al. (3 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2208.03880v2-abstract-short" style="display: inline;"> To understand the origin of nuclear ($\lesssim$ 100 pc) millimeter-wave (mm-wave) continuum emission in active galactic nuclei (AGNs), we systematically analyzed sub-arcsec resolution Band-6 (211-275 GHz) ALMA data of 98 nearby AGNs ($z <$ 0.05) from the 70-month Swift/BAT catalog. The sample, almost unbiased for obscured systems, provides the largest number of AGNs to date with high mm-wave spati… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.03880v2-abstract-full').style.display = 'inline'; document.getElementById('2208.03880v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.03880v2-abstract-full" style="display: none;"> To understand the origin of nuclear ($\lesssim$ 100 pc) millimeter-wave (mm-wave) continuum emission in active galactic nuclei (AGNs), we systematically analyzed sub-arcsec resolution Band-6 (211-275 GHz) ALMA data of 98 nearby AGNs ($z <$ 0.05) from the 70-month Swift/BAT catalog. The sample, almost unbiased for obscured systems, provides the largest number of AGNs to date with high mm-wave spatial resolution sampling ($\sim$ 1-200 pc), and spans broad ranges of 14-150 keV luminosity {$40 < \log[L_{\rm 14-150}/({\rm erg\,s^{-1}})] < 45$}, black hole mass [$5 < \log(M_{\rm BH}/M_\odot) < 10$], and Eddington ratio ($-4 < \log 位_{\rm Edd} < 2$). We find a significant correlation between 1.3 mm (230 GHz) and 14-150 keV luminosities. Its scatter is $\approx$ 0.36 dex, and the mm-wave emission may serve as a good proxy of the AGN luminosity, free of dust extinction up to $N_{\rm H} \sim 10^{26}$ cm$^{-2}$. While the mm-wave emission could be self-absorbed synchrotron radiation around the X-ray corona according to past works, we also discuss different possible origins of the mm-wave emission; AGN-related dust emission, outflow-driven shocks, and a small-scale ($<$ 200 pc) jet. The dust emission is unlikely to be dominant, as the mm-wave slope is generally flatter than expected. Also, due to no increase in the mm-wave luminosity with the Eddington ratio, a radiation-driven outflow model is possibly not the common mechanism. Furthermore, we find independence of the mm-wave luminosity on indicators of the inclination angle from the polar axis of the nuclear structure, which is inconsistent with a jet model whose luminosity depends only on the angle. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.03880v2-abstract-full').style.display = 'none'; document.getElementById('2208.03880v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">44 pages, 35 figures, 3 tables, accepted for publication in ApJ; modified format, added supplementary figure (Fig. 32)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.12435">arXiv:2207.12435</a> <span> [<a href="https://arxiv.org/pdf/2207.12435">pdf</a>, <a href="https://arxiv.org/format/2207.12435">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/ac650b">10.3847/1538-4365/ac650b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BASS XXVI: DR2 Host Galaxy Stellar Velocity Dispersions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M+J">Michael J. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">Benny Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">Kyuseok Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Caglar%2C+T">Turgay Caglar</a>, <a href="/search/astro-ph?searchtype=author&query=Brok%2C+J+S+d">Jakob S. den Brok</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotzky%2C+R">Richard Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">Federica Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Mejia-Restrepo%2C+J+E">Julian E. Mejia-Restrepo</a>, <a href="/search/astro-ph?searchtype=author&query=Lamperti%2C+I">Isabella Lamperti</a>, <a href="/search/astro-ph?searchtype=author&query=Treister%2C+E">Ezequiel Treister</a>, <a href="/search/astro-ph?searchtype=author&query=Bar%2C+R+E">Rudolf E. Bar</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M+C">Meredith C. Powell</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Riffel%2C+R">Rogerio Riffel</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas%2C+A+F">Alejandra F. Rojas</a>, <a href="/search/astro-ph?searchtype=author&query=Schawinski%2C+K">Kevin Schawinski</a>, <a href="/search/astro-ph?searchtype=author&query=Urry%2C+C+M">C. Megan Urry</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2207.12435v1-abstract-short" style="display: inline;"> We present new central stellar velocity dispersions for 484 Sy 1.9 and Sy 2 from the second data release of the Swift/BAT AGN Spectroscopic Survey (BASS DR2). This constitutes the largest study of velocity dispersion measurements in X-ray selected, obscured AGN with 956 independent measurements of the Ca H+K and Mg b region (3880-5550A) and the Ca triplet region (8350-8730A) from 642 spectra mainl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.12435v1-abstract-full').style.display = 'inline'; document.getElementById('2207.12435v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.12435v1-abstract-full" style="display: none;"> We present new central stellar velocity dispersions for 484 Sy 1.9 and Sy 2 from the second data release of the Swift/BAT AGN Spectroscopic Survey (BASS DR2). This constitutes the largest study of velocity dispersion measurements in X-ray selected, obscured AGN with 956 independent measurements of the Ca H+K and Mg b region (3880-5550A) and the Ca triplet region (8350-8730A) from 642 spectra mainly from VLT/Xshooter or Palomar/DoubleSpec. Our sample spans velocity dispersions of 40-360 km/s, corresponding to 4-5 orders of magnitude in black holes mass (MBH=10^5.5-9.6 Msun), bolometric luminosity (LBol~10^{42-46 ergs/s), and Eddington ratio (L/Ledd~10^{-5}-2). For 281 AGN, our data provide the first published central velocity dispersions, including 6 AGN with low mass black holes (MBH=10^5.5-6.5 Msun), discovered thanks to our high spectral resolution observations (sigma~25 km/s). The survey represents a significant advance with a nearly complete census of hard-X-ray selected obscured AGN with measurements for 99% of nearby AGN (z<0.1) outside the Galactic plane. The BASS AGN have higher velocity dispersions than the more numerous optically selected narrow line AGN (i.e., ~150 vs. ~100 km/s), but are not biased towards the highest velocity dispersions of massive ellipticals (i.e., >250 km/s). Despite sufficient spectral resolution to resolve the velocity dispersions associated with the bulges of small black holes (~10^4-5 Msun), we do not find a significant population of super-Eddington AGN. Using estimates of the black hole sphere of influence, direct stellar and gas black hole mass measurements could be obtained with existing facilities for more than ~100 BASS AGN. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.12435v1-abstract-full').style.display = 'none'; document.getElementById('2207.12435v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">32 pages, 16 figures, 8 tables, published in ApJS as part of BASS DR2 special issue</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJS, 261, 6 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.12432">arXiv:2207.12432</a> <span> [<a href="https://arxiv.org/pdf/2207.12432">pdf</a>, <a href="https://arxiv.org/format/2207.12432">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/ac6c05">10.3847/1538-4365/ac6c05 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BASS XXII: The BASS DR2 AGN Catalog and Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M+J">Michael J. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">Benny Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">Kyuseok Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Brok%2C+J+S+d">Jakob S. den Brok</a>, <a href="/search/astro-ph?searchtype=author&query=Mejia-Restrepo%2C+J+E">Julian E. Mejia-Restrepo</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Treister%2C+E">Ezequiel Treister</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M+C">Meredith C. Powell</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotzky%2C+R">Richard Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Ananna%2C+T+T">Tonima T. Ananna</a>, <a href="/search/astro-ph?searchtype=author&query=Balokovic%2C+M">Mislav Balokovic</a>, <a href="/search/astro-ph?searchtype=author&query=Bar%2C+R+E">Rudolf E. Bar</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+G">George Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Bessiere%2C+P">Patricia Bessiere</a>, <a href="/search/astro-ph?searchtype=author&query=Burtscher%2C+L">Leonard Burtscher</a>, <a href="/search/astro-ph?searchtype=author&query=Caglar%2C+T">Turgay Caglar</a>, <a href="/search/astro-ph?searchtype=author&query=Congiu%2C+E">Enrico Congiu</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+P">Phil Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Heida%2C+M">Marianne Heida</a>, <a href="/search/astro-ph?searchtype=author&query=Ichikawa%2C+K">Kohei Ichikawa</a>, <a href="/search/astro-ph?searchtype=author&query=Kamraj%2C+N">Nikita Kamraj</a> , et al. (10 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2207.12432v1-abstract-short" style="display: inline;"> We present the AGN catalog and optical spectroscopy for the second data release of the Swift BAT AGN Spectroscopic Survey (BASS DR2). With this DR2 release we provide 1425 optical spectra, of which 1181 are released for the first time, for the 858 hard X-ray selected AGN in the Swift BAT 70-month sample. The majority of the spectra (813/1425, 57%) are newly obtained from VLT/Xshooter or Palomar/Do… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.12432v1-abstract-full').style.display = 'inline'; document.getElementById('2207.12432v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.12432v1-abstract-full" style="display: none;"> We present the AGN catalog and optical spectroscopy for the second data release of the Swift BAT AGN Spectroscopic Survey (BASS DR2). With this DR2 release we provide 1425 optical spectra, of which 1181 are released for the first time, for the 858 hard X-ray selected AGN in the Swift BAT 70-month sample. The majority of the spectra (813/1425, 57%) are newly obtained from VLT/Xshooter or Palomar/Doublespec. Many of the spectra have both higher resolution (R>2500, N~450) and/or very wide wavelength coverage (3200-10000 A, N~600) that are important for a variety of AGN and host galaxy studies. We include newly revised AGN counterparts for the full sample and review important issues for population studies, with 44 AGN redshifts determined for the first time and 780 black hole mass and accretion rate estimates. This release is spectroscopically complete for all AGN (100%, 858/858) with 99.8% having redshift measurements (857/858) and 96% completion in black hole mass estimates of unbeamed AGN (outside the Galactic plane). This AGN sample represents a unique census of the brightest hard X-ray selected AGN in the sky, spanning many orders of magnitude in Eddington ratio (Ledd=10^-5-100), black hole mass (MBH=10^5-10^10 Msun), and AGN bolometric luminosity (Lbol=10^40-10^47 ergs/s). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.12432v1-abstract-full').style.display = 'none'; document.getElementById('2207.12432v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">34 pages, 11 figures, 15 tables, published in ApJS as part of BASS DR2 special issue</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJS, 261, 2 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.12428">arXiv:2207.12428</a> <span> [<a href="https://arxiv.org/pdf/2207.12428">pdf</a>, <a href="https://arxiv.org/format/2207.12428">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/ac6c8f">10.3847/1538-4365/ac6c8f <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BAT AGN Spectroscopic Survey XXI: The Data Release 2 Overview </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M+J">Michael J. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">Benny Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Treister%2C+E">Ezequiel Treister</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotzky%2C+R">Richard Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Urry%2C+C+M">C. Megan Urry</a>, <a href="/search/astro-ph?searchtype=author&query=Ananna%2C+T+T">Tonima T. Ananna</a>, <a href="/search/astro-ph?searchtype=author&query=Balokovic%2C+M">Mislav Balokovic</a>, <a href="/search/astro-ph?searchtype=author&query=Brok%2C+J+S+d">Jakob S. den Brok</a>, <a href="/search/astro-ph?searchtype=author&query=Cenko%2C+S+B">S. Bradley Cenko</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Ichikawa%2C+K">Kohei Ichikawa</a>, <a href="/search/astro-ph?searchtype=author&query=Lamperti%2C+I">Isabella Lamperti</a>, <a href="/search/astro-ph?searchtype=author&query=Lein%2C+A">Amy Lein</a>, <a href="/search/astro-ph?searchtype=author&query=Mejia-Restrepo%2C+J+E">Julian E. Mejia-Restrepo</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">Kyuseok Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Pacucci%2C+F">Fabio Pacucci</a>, <a href="/search/astro-ph?searchtype=author&query=Pfeifle%2C+R+W">Ryan W. Pfeifle</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M+C">Meredith C. Powell</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">Federica Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Salvato%2C+M">Mara Salvato</a>, <a href="/search/astro-ph?searchtype=author&query=Schawinski%2C+K">Kevin Schawinski</a>, <a href="/search/astro-ph?searchtype=author&query=Shimizu%2C+T">Taro Shimizu</a> , et al. (2 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2207.12428v1-abstract-short" style="display: inline;"> The BAT AGN Spectroscopic Survey (BASS) is designed to provide a highly complete census of the key physical parameters of supermassive black holes (SMBHs) that power local active galactic nuclei (AGN) (z<0.3), including their bolometric luminosity, black hole mass, accretion rates, and line-of-sight gas obscuration, and the distinctive properties of their host galaxies (e.g., star formation rates,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.12428v1-abstract-full').style.display = 'inline'; document.getElementById('2207.12428v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.12428v1-abstract-full" style="display: none;"> The BAT AGN Spectroscopic Survey (BASS) is designed to provide a highly complete census of the key physical parameters of supermassive black holes (SMBHs) that power local active galactic nuclei (AGN) (z<0.3), including their bolometric luminosity, black hole mass, accretion rates, and line-of-sight gas obscuration, and the distinctive properties of their host galaxies (e.g., star formation rates, masses, and gas fractions). We present an overview of the BASS data release 2 (DR2), an unprecedented spectroscopic survey in spectral range, resolution, and sensitivity, including 1449 optical (3200-10000 A) and 233 NIR (1-2.5 um) spectra for the brightest 858 ultra-hard X-ray (14-195 keV) selected AGN across the entire sky and essentially all levels of obscuration. This release provides a highly complete set of key measurements (emission line measurements and central velocity dispersions), with 99.9% measured redshifts and 98% black hole masses estimated (for unbeamed AGN outside the Galactic plane). The BASS DR2 AGN sample represents a unique census of nearby powerful AGN, spanning over 5 orders of magnitude in AGN bolometric luminosity, black hole mass, Eddington ratio, and obscuration. The public BASS DR2 sample and measurements can thus be used to answer fundamental questions about SMBH growth and its links to host galaxy evolution and feedback in the local universe, as well as open questions concerning SMBH physics. Here we provide a brief overview of the survey strategy, the key BASS DR2 measurements, data sets and catalogs, and scientific highlights from a series of DR2-based works. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.12428v1-abstract-full').style.display = 'none'; document.getElementById('2207.12428v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 6 figures, 5 tables, published in ApJS as part of BASS DR2 special issue</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJS, 261, 1 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.12426">arXiv:2207.12426</a> <span> [<a href="https://arxiv.org/pdf/2207.12426">pdf</a>, <a href="https://arxiv.org/format/2207.12426">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/ac5b66">10.3847/1538-4365/ac5b66 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BASS XXVIII: Near-infrared Data Release 2, High-Ionization and Broad Lines in Active Galactic Nuclei </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Brok%2C+J+d">Jakob den Brok</a>, <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M+J">Michael J. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">Benny Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Cantalupo%2C+S">Sebastiano Cantalupo</a>, <a href="/search/astro-ph?searchtype=author&query=Lamperti%2C+I">Isabella Lamperti</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">Federica Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">Kyuseok Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Riffel%2C+R">Rogerio Riffel</a>, <a href="/search/astro-ph?searchtype=author&query=Rodriguez-Ardila%2C+A">Alberto Rodriguez-Ardila</a>, <a href="/search/astro-ph?searchtype=author&query=Baer%2C+R">Rudolf Baer</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Ichikawa%2C+K">Kohei Ichikawa</a>, <a href="/search/astro-ph?searchtype=author&query=Mejia-Restrepo%2C+J+E">Julian E. Mejia-Restrepo</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotzky%2C+R">Richard Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M+C">Meredith C. Powell</a>, <a href="/search/astro-ph?searchtype=author&query=Boissay-Malaquin%2C+R">Rozenn Boissay-Malaquin</a>, <a href="/search/astro-ph?searchtype=author&query=Stalevski%2C+M">Marko Stalevski</a>, <a href="/search/astro-ph?searchtype=author&query=Treister%2C+E">Ezequiel Treister</a>, <a href="/search/astro-ph?searchtype=author&query=Urry%2C+C+M">C. Megan Urry</a>, <a href="/search/astro-ph?searchtype=author&query=Veilleux%2C+S">Sylvain Veilleux</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2207.12426v1-abstract-short" style="display: inline;"> We present the BAT AGN Spectroscopic Survey (BASS) Near-infrared Data Release 2 (DR2), a study of 168 nearby ($\bar z$ = 0.04, $z$ < 0.6) active galactic nuclei (AGN) from the all-sky Swift Burst Array Telescope X-ray survey observed with Very Large Telescope (VLT)/X-shooter in the near-infrared (NIR; 0.8 - 2.4 $渭$m). We find that 49/109 (45%) Seyfert 2 and 35/58 (60%) Seyfert 1 galaxies observed… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.12426v1-abstract-full').style.display = 'inline'; document.getElementById('2207.12426v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.12426v1-abstract-full" style="display: none;"> We present the BAT AGN Spectroscopic Survey (BASS) Near-infrared Data Release 2 (DR2), a study of 168 nearby ($\bar z$ = 0.04, $z$ < 0.6) active galactic nuclei (AGN) from the all-sky Swift Burst Array Telescope X-ray survey observed with Very Large Telescope (VLT)/X-shooter in the near-infrared (NIR; 0.8 - 2.4 $渭$m). We find that 49/109 (45%) Seyfert 2 and 35/58 (60%) Seyfert 1 galaxies observed with VLT/X-shooter show at least one NIR high-ionization coronal line (CL, ionization potential $蠂$ > 100 eV). Comparing the emission of the [Si vi] $位$1.9640 CL with the X-ray emission for the DR2 AGN, we find a significantly tighter correlation, with a lower scatter (0.37 dex) than for the optical [O iii] $位$5007 line (0.71 dex). We do not find any correlation between CL emission and the X-ray photon index $螕$. We find a clear trend of line blueshifts with increasing ionization potential in several CLs, such as [Si vi] $位$1.9640, [Si x] $位$1.4300, [S viii] $位$0.9915, and [S ix] $位$1.2520, indicating the radial structure of the CL region. Finally, we find a strong underestimation bias in black hole mass measurements of Sy 1.9 using broad H$伪$ due to the presence of significant dust obscuration. In contrast, the broad Pa$伪$ and Pa$尾$ emission lines are in agreement with the $M$-$蟽$ relation. Based on the combined DR1 and DR2 X-shooter sample, the NIR BASS sample now comprises 266 AGN with rest-frame NIR spectroscopic observations, the largest set assembled to date. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.12426v1-abstract-full').style.display = 'none'; document.getElementById('2207.12426v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">36 pages, 24 figures, 10 tables, published in ApJS as part of BASS DR2 special issue</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJS, 261, 7 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.06567">arXiv:2207.06567</a> <span> [<a href="https://arxiv.org/pdf/2207.06567">pdf</a>, <a href="https://arxiv.org/format/2207.06567">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/ac7ff2">10.3847/1538-4357/ac7ff2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The long-stable hard state of XTE J1752-223 and the disk truncation dilemma </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Connors%2C+R+M+T">Riley M. T. Connors</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia%2C+J+A">Javier A. Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Tomsick%2C+J">John Tomsick</a>, <a href="/search/astro-ph?searchtype=author&query=Mastroserio%2C+G">Guglielmo Mastroserio</a>, <a href="/search/astro-ph?searchtype=author&query=Grinberg%2C+V">Victoria Grinberg</a>, <a href="/search/astro-ph?searchtype=author&query=Steiner%2C+J+F">James F. Steiner</a>, <a href="/search/astro-ph?searchtype=author&query=Jiang%2C+J">Jiachen Jiang</a>, <a href="/search/astro-ph?searchtype=author&query=Fabian%2C+A+C">Andrew C. Fabian</a>, <a href="/search/astro-ph?searchtype=author&query=Parker%2C+M+L">Michael L. Parker</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Hare%2C+J">Jeremy Hare</a>, <a href="/search/astro-ph?searchtype=author&query=Mallick%2C+L">Labani Mallick</a>, <a href="/search/astro-ph?searchtype=author&query=Lazar%2C+H">Hadar Lazar</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2207.06567v2-abstract-short" style="display: inline;"> The degree to which the thin accretion disks of black hole X-ray binaries are truncated during hard spectral states remains a contentious open question in black hole astrophysics. During its singular observed outburst in $2009\mbox{--}2010$, the black hole X-ray binary XTE J1752-223 spent $\sim1$~month in a long-stable hard spectral state at a luminosity of $\sim0.02\mbox{--}0.1~L_{\rm Edd}$. It w… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.06567v2-abstract-full').style.display = 'inline'; document.getElementById('2207.06567v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.06567v2-abstract-full" style="display: none;"> The degree to which the thin accretion disks of black hole X-ray binaries are truncated during hard spectral states remains a contentious open question in black hole astrophysics. During its singular observed outburst in $2009\mbox{--}2010$, the black hole X-ray binary XTE J1752-223 spent $\sim1$~month in a long-stable hard spectral state at a luminosity of $\sim0.02\mbox{--}0.1~L_{\rm Edd}$. It was observed with 56 RXTE pointings during this period, with simultaneous Swift-XRT daily coverage during the first 10 days of the RXTE observations. Whilst reflection modeling has been extensively explored in the analysis of these data, there is a disagreement surrounding the geometry of the accretion disk and corona implied by the reflection features. We re-examine the combined, high signal-to-noise, simultaneous Swift and RXTE observations, and perform extensive reflection modeling with the latest relxill suite of reflection models, including newer high disk density models. We show that reflection modeling requires that the disk be within $\sim5~R_{\rm ISCO}$ during the hard spectral state, whilst weaker constraints from the thermal disk emission imply higher truncation ($R_{\rm in}=6\mbox{--}80~R_{\rm ISCO}$). We also explore more complex coronal continuum models, allowing for two Comptonization components instead of one, and show that the reflection features still require only a mildly truncated disk. Finally we present a full comparison of our results to previous constraints found from analyses of the same dataset. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.06567v2-abstract-full').style.display = 'none'; document.getElementById('2207.06567v2-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 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 9 figures, accepted by ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.12713">arXiv:2206.12713</a> <span> [<a href="https://arxiv.org/pdf/2206.12713">pdf</a>, <a href="https://arxiv.org/format/2206.12713">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/ac898a">10.3847/1538-4357/ac898a <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Tidal Disruption Event AT2021ehb: Evidence of Relativistic Disk Reflection, and Rapid Evolution of the Disk-Corona System </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yao%2C+Y">Yuhan Yao</a>, <a href="/search/astro-ph?searchtype=author&query=Lu%2C+W">Wenbin Lu</a>, <a href="/search/astro-ph?searchtype=author&query=Guolo%2C+M">Muryel Guolo</a>, <a href="/search/astro-ph?searchtype=author&query=Pasham%2C+D+R">Dheeraj R. Pasham</a>, <a href="/search/astro-ph?searchtype=author&query=Gezari%2C+S">Suvi Gezari</a>, <a href="/search/astro-ph?searchtype=author&query=Gilfanov%2C+M">Marat Gilfanov</a>, <a href="/search/astro-ph?searchtype=author&query=Gendreau%2C+K+C">Keith C. Gendreau</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Cenko%2C+S+B">S. Bradley Cenko</a>, <a href="/search/astro-ph?searchtype=author&query=Kulkarni%2C+S+R">S. R. Kulkarni</a>, <a href="/search/astro-ph?searchtype=author&query=Miller%2C+J+M">Jon M. Miller</a>, <a href="/search/astro-ph?searchtype=author&query=Walton%2C+D+J">Dominic J. Walton</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa%2C+J+A">Javier A. Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=van+Velzen%2C+S">Sjoert van Velzen</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+K+D">Kate D. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Miller-Jones%2C+J+C+A">James C. A. Miller-Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Nicholl%2C+M">Matt Nicholl</a>, <a href="/search/astro-ph?searchtype=author&query=Hammerstein%2C+E">Erica Hammerstein</a>, <a href="/search/astro-ph?searchtype=author&query=Medvedev%2C+P">Pavel Medvedev</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Ravi%2C+V">Vikram Ravi</a>, <a href="/search/astro-ph?searchtype=author&query=Sunyaev%2C+R">R. Sunyaev</a>, <a href="/search/astro-ph?searchtype=author&query=Bloom%2C+J+S">Joshua S. Bloom</a>, <a href="/search/astro-ph?searchtype=author&query=Graham%2C+M+J">Matthew J. Graham</a>, <a href="/search/astro-ph?searchtype=author&query=Kool%2C+E+C">Erik C. Kool</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="2206.12713v2-abstract-short" style="display: inline;"> We present X-ray, UV, optical, and radio observations of the nearby ($\approx78$ Mpc) tidal disruption event (TDE) AT2021ehb/ZTF21aanxhjv during its first 430 days of evolution. AT2021ehb occurs in the nucleus of a galaxy hosting a $\approx 10^{7}\,M_\odot$ black hole ($M_{\rm BH}$ inferred from host galaxy scaling relations). High-cadence Swift and NICER monitoring reveals a delayed X-ray brighte… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.12713v2-abstract-full').style.display = 'inline'; document.getElementById('2206.12713v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.12713v2-abstract-full" style="display: none;"> We present X-ray, UV, optical, and radio observations of the nearby ($\approx78$ Mpc) tidal disruption event (TDE) AT2021ehb/ZTF21aanxhjv during its first 430 days of evolution. AT2021ehb occurs in the nucleus of a galaxy hosting a $\approx 10^{7}\,M_\odot$ black hole ($M_{\rm BH}$ inferred from host galaxy scaling relations). High-cadence Swift and NICER monitoring reveals a delayed X-ray brightening. The spectrum first undergoes a gradual ${\rm soft }\rightarrow{\rm hard}$ transition and then suddenly turns soft again within 3 days at $未t\approx 272$ days during which the X-ray flux drops by a factor of ten. In the joint NICER+NuSTAR observation ($未t =264$ days, harder state), we observe a prominent non-thermal component up to 30 keV and an extremely broad emission line in the iron K band. The bolometric luminosity of AT2021ehb reaches a maximum of $6.0^{+10.4}_{-3.8}\% L_{\rm Edd}$ when the X-ray spectrum is the hardest. During the dramatic X-ray evolution, no radio emission is detected, the UV/optical luminosity stays relatively constant, and the optical spectra are featureless. We propose the following interpretations: (i) the ${\rm soft }\rightarrow{\rm hard}$ transition may be caused by the gradual formation of a magnetically dominated corona; (ii) hard X-ray photons escape from the system along solid angles with low scattering optical depth ($\sim\,$a few) whereas the UV/optical emission is likely generated by reprocessing materials with much larger column density -- the system is highly aspherical; (iii) the abrupt X-ray flux drop may be triggered by the thermal-viscous instability in the inner accretion flow leading to a much thinner disk. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.12713v2-abstract-full').style.display = 'none'; document.getElementById('2206.12713v2-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 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">35 pages, 21 figures, accepted by ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.08397">arXiv:2206.08397</a> <span> [<a href="https://arxiv.org/pdf/2206.08397">pdf</a>, <a href="https://arxiv.org/format/2206.08397">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/ac79b0">10.3847/1538-4357/ac79b0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The variability behavior of NGC 925 ULX-3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Earnshaw%2C+H+P">Hannah P. Earnshaw</a>, <a href="/search/astro-ph?searchtype=author&query=Brightman%2C+M">Murray Brightman</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F+A">Fiona A. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Heida%2C+M">Marianne Heida</a>, <a href="/search/astro-ph?searchtype=author&query=Jaodand%2C+A">Amruta Jaodand</a>, <a href="/search/astro-ph?searchtype=author&query=Middleton%2C+M+J">Matthew J. Middleton</a>, <a href="/search/astro-ph?searchtype=author&query=Roberts%2C+T+P">Timothy P. Roberts</a>, <a href="/search/astro-ph?searchtype=author&query=Walton%2C+D+J">Dominic J. Walton</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2206.08397v1-abstract-short" style="display: inline;"> We report the results of a 2019-2021 monitoring campaign with Swift and associated target-of-opportunity observations with XMM-Newton and NuSTAR, examining the spectral and timing behavior of the highly variable ultraluminous X-ray source (ULX) NGC 925 ULX-3. We find that the source exhibits a 127-128 day periodicity, with fluxes typically ranging from 1e-13 to 8e-13 ergs/s/cm2. We do not find str… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.08397v1-abstract-full').style.display = 'inline'; document.getElementById('2206.08397v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.08397v1-abstract-full" style="display: none;"> We report the results of a 2019-2021 monitoring campaign with Swift and associated target-of-opportunity observations with XMM-Newton and NuSTAR, examining the spectral and timing behavior of the highly variable ultraluminous X-ray source (ULX) NGC 925 ULX-3. We find that the source exhibits a 127-128 day periodicity, with fluxes typically ranging from 1e-13 to 8e-13 ergs/s/cm2. We do not find strong evidence for a change in period over the time that NGC 925 ULX-3 has been observed, although the source may have been in a much lower flux state when first observed with Chandra in 2005. We do not detect pulsations, and we place an upper limit on the pulsed fraction of ~40% in the XMM-Newton band, consistent with some previous pulsation detections at low energies in other ULXs. The source exhibits a typical ULX spectrum that turns over in the NuSTAR band and can be fitted using two thermal components. These components have a high temperature ratio that may indicate the lack of extreme inner disk truncation by a magnetar-level magnetic field. We examine the implications for a number of different models for superorbital periods in ULXs, finding that a neutron star with a magnetic field of ~10^12 G may be plausible for this source. The future detection of pulsations from this source would allow for the further testing and constraining of such models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.08397v1-abstract-full').style.display = 'none'; document.getElementById('2206.08397v1-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 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 6 figures, 2 tables. Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.08227">arXiv:2205.08227</a> <span> [<a href="https://arxiv.org/pdf/2205.08227">pdf</a>, <a href="https://arxiv.org/format/2205.08227">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/10.1093/mnras/stac1401">10.1093/mnras/stac1401 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A NuSTAR and Swift View of the Hard State of MAXI J1813-095 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jiang%2C+J">Jiachen Jiang</a>, <a href="/search/astro-ph?searchtype=author&query=Buisson%2C+D+J+K">Douglas J. K. Buisson</a>, <a href="/search/astro-ph?searchtype=author&query=Dauser%2C+T">Thomas Dauser</a>, <a href="/search/astro-ph?searchtype=author&query=Fabian%2C+A+C">Andrew C. Fabian</a>, <a href="/search/astro-ph?searchtype=author&query=F%C3%BCrst%2C+F">Felix F眉rst</a>, <a href="/search/astro-ph?searchtype=author&query=Gallo%2C+L+C">Luigi C. Gallo</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F+A">Fiona A. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Parker%2C+M+L">Michael L. Parker</a>, <a href="/search/astro-ph?searchtype=author&query=Steiner%2C+J+F">James F. Steiner</a>, <a href="/search/astro-ph?searchtype=author&query=Tomsick%2C+J+A">John A. Tomsick</a>, <a href="/search/astro-ph?searchtype=author&query=Ubach%2C+S">Santiago Ubach</a>, <a href="/search/astro-ph?searchtype=author&query=Walton%2C+D+J">Dominic J. Walton</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="2205.08227v1-abstract-short" style="display: inline;"> We present an analysis of the NuSTAR and Swift spectra of the black hole candidate MAXI J1813-095 in a failed-transition outburst in 2018. The NuSTAR observations show evidence of reflected emission from the inner region of the accretion disc. By modelling the reflection component in the spectra, we find a disc inner radius of $R_{\rm in}<7$ $r_{\rm g}$. This result suggests that either a slightly… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.08227v1-abstract-full').style.display = 'inline'; document.getElementById('2205.08227v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.08227v1-abstract-full" style="display: none;"> We present an analysis of the NuSTAR and Swift spectra of the black hole candidate MAXI J1813-095 in a failed-transition outburst in 2018. The NuSTAR observations show evidence of reflected emission from the inner region of the accretion disc. By modelling the reflection component in the spectra, we find a disc inner radius of $R_{\rm in}<7$ $r_{\rm g}$. This result suggests that either a slightly truncated disc or a non-truncated disc forms at a few percent of the Eddington limit in MAXI J1813-095. Our best-fit reflection models indicate that the geometry of the innermost accretion remains consistent during the period of NuSTAR observations. The spectral variability of MAXI J1813-095 from multi-epoch observations is dominated by the variable photon index of the Comptonisation emission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.08227v1-abstract-full').style.display = 'none'; document.getElementById('2205.08227v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 May, 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">9 pages, 12 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.05321">arXiv:2204.05321</a> <span> [<a href="https://arxiv.org/pdf/2204.05321">pdf</a>, <a href="https://arxiv.org/format/2204.05321">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/ac6602">10.3847/1538-4365/ac6602 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BASS XXV: DR2 Broad-line Based Black Hole Mass Estimates and Biases from Obscuration </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mej%C4%B1a-Restrepo%2C+J+E">Julian E. Mej谋a-Restrepo</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">Benny Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M+J">Michael J. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">Kyuseok Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Brok%2C+J+d">Jakob den Brok</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M+C">Meredith C. Powell</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">Federica Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Caglar%2C+T">Turgay Caglar</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Treister%2C+E">Ezequiel Treister</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F+A">Fiona A. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Urry%2C+C+M">C. M. Urry</a>, <a href="/search/astro-ph?searchtype=author&query=Ananna%2C+T+T">Tonima Tasnim Ananna</a>, <a href="/search/astro-ph?searchtype=author&query=Asmus%2C+D">Daniel Asmus</a>, <a href="/search/astro-ph?searchtype=author&query=Assef%2C+R+J">Roberto J. Assef</a>, <a href="/search/astro-ph?searchtype=author&query=Bar%2C+R+E">Rudolf E. Bar</a>, <a href="/search/astro-ph?searchtype=author&query=Bessiere%2C+P+S">Patricia S. Bessiere</a>, <a href="/search/astro-ph?searchtype=author&query=Burtscher%2C+L">Leonard Burtscher</a>, <a href="/search/astro-ph?searchtype=author&query=Ichikawa%2C+K">Kohei Ichikawa</a>, <a href="/search/astro-ph?searchtype=author&query=Kakkad%2C+D">Darshan Kakkad</a>, <a href="/search/astro-ph?searchtype=author&query=Kamraj%2C+N">Nikita Kamraj</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotzky%2C+R">Richard Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a> , et al. (4 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2204.05321v2-abstract-short" style="display: inline;"> We present measurements of broad emission lines and virial estimates of supermassive black hole masses ($M_{BH}$) for a large sample of ultra-hard X-ray selected active galactic nuclei (AGNs) as part of the second data release of the BAT AGN Spectroscopic Survey (BASS/DR2). Our catalog includes $M_{BH}$ estimates for a total 689 AGNs, determined from the H$伪$, H$尾$, $MgII\lambda2798$, and/or… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.05321v2-abstract-full').style.display = 'inline'; document.getElementById('2204.05321v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.05321v2-abstract-full" style="display: none;"> We present measurements of broad emission lines and virial estimates of supermassive black hole masses ($M_{BH}$) for a large sample of ultra-hard X-ray selected active galactic nuclei (AGNs) as part of the second data release of the BAT AGN Spectroscopic Survey (BASS/DR2). Our catalog includes $M_{BH}$ estimates for a total 689 AGNs, determined from the H$伪$, H$尾$, $MgII\lambda2798$, and/or $CIV\lambda1549$ broad emission lines. The core sample includes a total of 512 AGNs drawn from the 70-month Swift/BAT all-sky catalog. We also provide measurements for 177 additional AGNs that are drawn from deeper Swift/BAT survey data. We study the links between $M_{BH}$ estimates and line-of-sight obscuration measured from X-ray spectral analysis. We find that broad H$伪$ emission lines in obscured AGNs ($\log (N_{\rm H}/{\rm cm}^{-2})> 22.0$) are on average a factor of $8.0_{-2.4}^{+4.1}$ weaker, relative to ultra-hard X-ray emission, and about $35_{-12}^{~+7}$\% narrower than in unobscured sources (i.e., $\log (N_{\rm H}/{\rm cm}^{-2}) < 21.5$). This indicates that the innermost part of the broad-line region is preferentially absorbed. Consequently, current single-epoch $M_{BH}$ prescriptions result in severely underestimated ($>$1 dex) masses for Type 1.9 sources (AGNs with broad H$伪$ but no broad H$尾$) and/or sources with $\log (N_{\rm H}/{\rm cm}^{-2}) > 22.0$. We provide simple multiplicative corrections for the observed luminosity and width of the broad H$伪$ component ($L[{\rm b}{\rm H}伪]$ and FWHM[bH$伪$]) in such sources to account for this effect, and to (partially) remedy $M_{BH}$ estimates for Type 1.9 objects. As key ingredient of BASS/DR2, our work provides the community with the data needed to further study powerful AGNs in the low-redshift Universe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.05321v2-abstract-full').style.display = 'none'; document.getElementById('2204.05321v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">published in ApJS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.00017">arXiv:2203.00017</a> <span> [<a href="https://arxiv.org/pdf/2203.00017">pdf</a>, <a href="https://arxiv.org/ps/2203.00017">ps</a>, <a href="https://arxiv.org/format/2203.00017">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/ac5b68">10.3847/1538-4365/ac5b68 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BASS XXIV: The BASS DR2 Spectroscopic Line Measurements and AGN Demographics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">Kyuseok Oh</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=Ueda%2C+Y">Yoshihiro Ueda</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">Benny Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M+C">Meredith C. Powell</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=Lamperti%2C+I">Isabella Lamperti</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotzky%2C+R">Richard Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">Federica Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%A4r%2C+R+E">Rudolf E. B盲r</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas%2C+A+F">Alejandra F. Rojas</a>, <a href="/search/astro-ph?searchtype=author&query=Ichikawa%2C+K">Kohei Ichikawa</a>, <a href="/search/astro-ph?searchtype=author&query=Riffel%2C+R">Rogerio Riffel</a>, <a href="/search/astro-ph?searchtype=author&query=Treister%2C+E">Ezequiel Treister</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Urry%2C+C+M">C. Megan Urry</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Schawinski%2C+K">Kevin Schawinski</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="2203.00017v1-abstract-short" style="display: inline;"> We present the second catalog and data release of optical spectral line measurements and AGN demographics of the BAT AGN Spectroscopic Survey, which focuses on the of Swift-BAT hard X-ray detected AGNs. We use spectra from dedicated campaigns and publicly available archives to investigate spectral properties of most of the AGNs listed in the 70-month Swift-BAT all-sky catalog; specifically, 743 of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.00017v1-abstract-full').style.display = 'inline'; document.getElementById('2203.00017v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.00017v1-abstract-full" style="display: none;"> We present the second catalog and data release of optical spectral line measurements and AGN demographics of the BAT AGN Spectroscopic Survey, which focuses on the of Swift-BAT hard X-ray detected AGNs. We use spectra from dedicated campaigns and publicly available archives to investigate spectral properties of most of the AGNs listed in the 70-month Swift-BAT all-sky catalog; specifically, 743 of the 746 unbeamed and unlensed AGNs (99.6%). We find a good correspondence between the optical emission line widths and the hydrogen column density distributions using the X-ray spectra, with a clear dichotomy of AGN types for NH = 10^22 cm-2. Based on optical emission-line diagnostics, we show that 48%-75% of BAT AGNs are classified as Seyfert, depending on the choice of emission lines used in the diagnostics. The fraction of objects with upper limits on line emission varies from 6% to 20%. Roughly 4% of the BAT AGNs have lines too weak to be placed on the most commonly used diagnostic diagram, [O III]位5007/H\b{eta} versus [N II]位6584/H伪, despite the high signal-to-noise ratio (S/N) of their spectra. This value increases to 35% in the [O III]位5007/[O II]位3727 diagram, owing to difficulties in line detection. Compared to optically-selected narrow-line AGNs in the Sloan Digital Sky Survey, the BAT narrow-line AGNs have a higher rate of reddening/extinction, with H伪/H\b{eta} > 5 (~ 36%), indicating that hard X-ray selection more effectively detects obscured AGNs from the underlying AGN population. Finally, we present a subpopulation of AGNs that feature complex broad-lines (34%, 250/743) or double-peaked narrow emission lines (2%, 17/743). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.00017v1-abstract-full').style.display = 'none'; document.getElementById('2203.00017v1-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">30 pages, 17 figures, 11 tables, accepted for publication in ApJS; part of BASS DR2 special 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/2202.04685">arXiv:2202.04685</a> <span> [<a href="https://arxiv.org/pdf/2202.04685">pdf</a>, <a href="https://arxiv.org/format/2202.04685">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> <p class="title is-5 mathjax"> Reconstruction of the NuSTAR point spread function using single-laser metrology </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Earnshaw%2C+H+P">Hannah P. Earnshaw</a>, <a href="/search/astro-ph?searchtype=author&query=Madsen%2C+K+K">Kristin K. Madsen</a>, <a href="/search/astro-ph?searchtype=author&query=Forster%2C+K">Karl Forster</a>, <a href="/search/astro-ph?searchtype=author&query=Grefenstette%2C+B+W">Brian W. Grefenstette</a>, <a href="/search/astro-ph?searchtype=author&query=Brightman%2C+M">Murray Brightman</a>, <a href="/search/astro-ph?searchtype=author&query=Zoglauer%2C+A">Andreas Zoglauer</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2202.04685v1-abstract-short" style="display: inline;"> This paper describes a method by which the metrology system of the Nuclear Spectroscopic Telescope Array (NuSTAR) X-ray space observatory, which uses two lasers to characterize the relative motion of the optics and focal plane benches, can be approximated should one laser fail. The two benches are separated by a ten-meter-long rigid mast that undergoes small amounts of thermal flexing which need t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.04685v1-abstract-full').style.display = 'inline'; document.getElementById('2202.04685v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.04685v1-abstract-full" style="display: none;"> This paper describes a method by which the metrology system of the Nuclear Spectroscopic Telescope Array (NuSTAR) X-ray space observatory, which uses two lasers to characterize the relative motion of the optics and focal plane benches, can be approximated should one laser fail. The two benches are separated by a ten-meter-long rigid mast that undergoes small amounts of thermal flexing which need to be compensated for in order to produce a non-blurred image. We analyze the trends of mast motion by archival observation parameters in order to discover whether the mast motion in future observations can be predicted. We find that, by using the solar aspect angle (SAA), observation date, and orbital phase, we can simulate the motion of one laser by translating the track produced by the other and applying modifications to the resulting mast aspect solution, allowing the reconstruction of a minimally distorted point spread function in most cases. We will implement the generation of simulated mast files alongside the usual NuSTAR data reduction pipeline for contingency purposes. This work has implications for reducing the risk of implementing laser metrology systems on future missions that use deployable masts to achieve the long focal lengths required in high-energy astronomy by mitigating the impact of a metrology laser failure in the extended phase of a mission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.04685v1-abstract-full').style.display = 'none'; document.getElementById('2202.04685v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">36 pages, 20 figures, 1 table. Accepted for publication in JATIS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.02883">arXiv:2202.02883</a> <span> [<a href="https://arxiv.org/pdf/2202.02883">pdf</a>, <a href="https://arxiv.org/format/2202.02883">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/ac5258">10.3847/1538-4357/ac5258 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MAXI and NuSTAR observations of the faint X-ray transient MAXI J1848-015 in the GLIMPSE-C01 Cluster </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pike%2C+S+N">Sean N. Pike</a>, <a href="/search/astro-ph?searchtype=author&query=Negoro%2C+H">Hitoshi Negoro</a>, <a href="/search/astro-ph?searchtype=author&query=Tomsick%2C+J+A">John A. Tomsick</a>, <a href="/search/astro-ph?searchtype=author&query=Bachetti%2C+M">Matteo Bachetti</a>, <a href="/search/astro-ph?searchtype=author&query=Brumback%2C+M">McKinley Brumback</a>, <a href="/search/astro-ph?searchtype=author&query=Connors%2C+R+M+T">Riley M. T. Connors</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa%2C+J+A">Javier A. Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Grefenstette%2C+B">Brian Grefenstette</a>, <a href="/search/astro-ph?searchtype=author&query=Hare%2C+J">Jeremy Hare</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F+A">Fiona A. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Jaodand%2C+A">Amruta Jaodand</a>, <a href="/search/astro-ph?searchtype=author&query=Ludlam%2C+R+M">R. M. Ludlam</a>, <a href="/search/astro-ph?searchtype=author&query=Mastroserio%2C+G">Guglielmo Mastroserio</a>, <a href="/search/astro-ph?searchtype=author&query=Mihara%2C+T">Tatehiro Mihara</a>, <a href="/search/astro-ph?searchtype=author&query=Shidatsu%2C+M">Megumi Shidatsu</a>, <a href="/search/astro-ph?searchtype=author&query=Sugizaki%2C+M">Mutsumi Sugizaki</a>, <a href="/search/astro-ph?searchtype=author&query=Takagi%2C+R">Ryohei Takagi</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2202.02883v2-abstract-short" style="display: inline;"> We present the results of MAXI monitoring and two NuSTAR observations of the recently discovered faint X-ray transient MAXI J1848-015. Analysis of the MAXI light-curve shows that the source underwent a rapid flux increase beginning on 2020 December 20, followed by a rapid decrease in flux after only $\sim5$ days. NuSTAR observations reveal that the source transitioned from a bright soft state with… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.02883v2-abstract-full').style.display = 'inline'; document.getElementById('2202.02883v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.02883v2-abstract-full" style="display: none;"> We present the results of MAXI monitoring and two NuSTAR observations of the recently discovered faint X-ray transient MAXI J1848-015. Analysis of the MAXI light-curve shows that the source underwent a rapid flux increase beginning on 2020 December 20, followed by a rapid decrease in flux after only $\sim5$ days. NuSTAR observations reveal that the source transitioned from a bright soft state with unabsorbed, bolometric ($0.1$-$100$ keV) flux $F=6.9 \pm 0.1 \times 10^{-10}\,\mathrm{erg\,cm^{-2}\,s^{-1}}$, to a low hard state with flux $F=2.85 \pm 0.04 \times 10^{-10}\,\mathrm{erg\,cm^{-2}\,s^{-1}}$. Given a distance of $3.3$ kpc, inferred via association of the source with the GLIMPSE-C01 cluster, these fluxes correspond to an Eddington fraction of order $10^{-3}$ for an accreting neutron star of mass $M=1.4M_\odot$, or even lower for a more massive accretor. However, the source spectra exhibit strong relativistic reflection features, indicating the presence of an accretion disk which extends close to the accretor, for which we measure a high spin, $a=0.967\pm0.013$. In addition to a change in flux and spectral shape, we find evidence for other changes between the soft and hard states, including moderate disk truncation with the inner disk radius increasing from $R_\mathrm{in}\approx3\,R_\mathrm{g}$ to $R_\mathrm{in}\approx8\,R_\mathrm{g}$, narrow Fe emission whose centroid decreases from $6.8\pm0.1$ keV to $6.3 \pm 0.1$ keV, and an increase in low-frequency ($10^{-3}$-$10^{-1}$ Hz) variability. Due to the high spin we conclude that the source is likely to be a black hole rather than a neutron star, and we discuss physical interpretations of the low apparent luminosity as well as the narrow Fe emission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.02883v2-abstract-full').style.display = 'none'; document.getElementById('2202.02883v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 9 figures, 3 tables. Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.00895">arXiv:2202.00895</a> <span> [<a href="https://arxiv.org/pdf/2202.00895">pdf</a>, <a href="https://arxiv.org/format/2202.00895">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/ac45f6">10.3847/1538-4357/ac45f6 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> X-ray Coronal Properties of Swift/BAT-Selected Seyfert 1 Active Galactic Nuclei </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kamraj%2C+N">Nikita Kamraj</a>, <a href="/search/astro-ph?searchtype=author&query=Brightman%2C+M">Murray Brightman</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F+A">Fiona A. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa%2C+J+A">Javier A. Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Balokovi%C4%87%2C+M">Mislav Balokovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M+J">Michael J. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Mej%C3%ADa-Restrepo%2C+J+E">Julian E. Mej铆a-Restrepo</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">Kyuseok Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M+C">Meredith C. Powell</a>, <a href="/search/astro-ph?searchtype=author&query=Urry%2C+C+M">C. Megan Urry</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2202.00895v1-abstract-short" style="display: inline;"> The corona is an integral component of Active Galactic Nuclei (AGN) which produces the bulk of the X-ray emission above 1--2 keV. However, many of its physical properties and the mechanisms powering this emission remain a mystery. In particular, the temperature of the coronal plasma has been difficult to constrain for large samples of AGN, as constraints require high quality broadband X-ray spectr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.00895v1-abstract-full').style.display = 'inline'; document.getElementById('2202.00895v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.00895v1-abstract-full" style="display: none;"> The corona is an integral component of Active Galactic Nuclei (AGN) which produces the bulk of the X-ray emission above 1--2 keV. However, many of its physical properties and the mechanisms powering this emission remain a mystery. In particular, the temperature of the coronal plasma has been difficult to constrain for large samples of AGN, as constraints require high quality broadband X-ray spectral coverage extending above 10 keV in order to measure the high energy cutoff, which provides constraints on the combination of coronal optical depth and temperature. We present constraints on the coronal temperature for a large sample of Seyfert 1 AGN selected from the Swift/BAT survey using high quality hard X-ray data from the NuSTAR observatory combined with simultaneous soft X-ray data from Swift/XRT or XMM-Newton. When applying a physically-motivated, non-relativistic disk reflection model to the X-ray spectra, we find a mean coronal temperature kT $=$ 84$\pm$9 keV. We find no significant correlation between the coronal cutoff energy and accretion parameters such as the Eddington ratio and black hole mass. We also do not find a statistically significant correlation between the X-ray photon index, $螕$, and Eddington ratio. This calls into question the use of such relations to infer properties of supermassive black hole systems. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.00895v1-abstract-full').style.display = 'none'; document.getElementById('2202.00895v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 10 figures. Accepted November 2021 for publication in ApJ; passed to production January 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/2201.05603">arXiv:2201.05603</a> <span> [<a href="https://arxiv.org/pdf/2201.05603">pdf</a>, <a href="https://arxiv.org/format/2201.05603">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/10.3847/1538-4365/ac5b64">10.3847/1538-4365/ac5b64 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BASS XXX: Distribution Functions of DR2 Eddington-ratios, Black Hole Masses, and X-ray Luminosities </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ananna%2C+T+T">Tonima Tasnim Ananna</a>, <a href="/search/astro-ph?searchtype=author&query=Weigel%2C+A+K">Anna K. Weigel</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">Benny Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M+J">Michael J. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Urry%2C+C+M">C. Megan Urry</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Hickox%2C+R+C">Ryan C. Hickox</a>, <a href="/search/astro-ph?searchtype=author&query=Treister%2C+E">Ezequiel Treister</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=Ueda%2C+Y">Yoshihiro Ueda</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotzky%2C+R">Richard Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">Federica Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">Kyuseok Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Mejia-Restrepo%2C+J+E">Julian E. Mejia-Restrepo</a>, <a href="/search/astro-ph?searchtype=author&query=Brok%2C+J+D">Jakob Den Brok</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M+C">Meredith C. Powell</a>, <a href="/search/astro-ph?searchtype=author&query=Caglar%2C+T">Turgay Caglar</a>, <a href="/search/astro-ph?searchtype=author&query=Ichikawa%2C+K">Kohei Ichikawa</a>, <a href="/search/astro-ph?searchtype=author&query=Wong%2C+O+I">O. Ivy Wong</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F+A">Fiona A. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Schawinski%2C+K">Kevin Schawinski</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2201.05603v3-abstract-short" style="display: inline;"> We determine the low-redshift X-ray luminosity function (XLF), active black hole mass function (BHMF), and Eddington-ratio distribution function (ERDF) for both unobscured (Type 1) and obscured (Type 2) active galactic nuclei (AGN) using the unprecedented spectroscopic completeness of the BAT AGN Spectroscopic Survey (BASS) data release 2. In addition to a straightforward 1/Vmax approach, we also… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.05603v3-abstract-full').style.display = 'inline'; document.getElementById('2201.05603v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.05603v3-abstract-full" style="display: none;"> We determine the low-redshift X-ray luminosity function (XLF), active black hole mass function (BHMF), and Eddington-ratio distribution function (ERDF) for both unobscured (Type 1) and obscured (Type 2) active galactic nuclei (AGN) using the unprecedented spectroscopic completeness of the BAT AGN Spectroscopic Survey (BASS) data release 2. In addition to a straightforward 1/Vmax approach, we also compute the intrinsic distributions, accounting for sample truncation by employing a forward modeling approach to recover the observed BHMF and ERDF. As previous BHMFs and ERDFs have been robustly determined only for samples of bright, broad-line (Type 1) AGNs and/or quasars, ours is the first directly observationally constrained BHMF and ERDF of Type 2 AGN. We find that after accounting for all observational biases, the intrinsic ERDF of Type 2 AGN is significantly skewed towards lower Eddington ratios than the intrinsic ERDF of Type 1 AGN. This result supports the radiation-regulated unification scenario, in which radiation pressure dictates the geometry of the dusty obscuring structure around an AGN. Calculating the ERDFs in two separate mass bins, we verify that the derived shape is consistent, validating the assumption that the ERDF (shape) is mass independent. We report the local AGN duty cycle as a function of mass and Eddington ratio, by comparing the BASS active BHMF with the local mass function for all SMBH. We also present the log N-log S of Swift-BAT 70-month sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.05603v3-abstract-full').style.display = 'none'; document.getElementById('2201.05603v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 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">Accepted by APJS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.04149">arXiv:2201.04149</a> <span> [<a href="https://arxiv.org/pdf/2201.04149">pdf</a>, <a href="https://arxiv.org/format/2201.04149">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stac103">10.1093/mnras/stac103 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BASS XXXI: Outflow scaling relations in low redshift X-ray AGN host galaxies with MUSE </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kakkad%2C+D">D. Kakkad</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas%2C+A+F">A. F. Rojas</a>, <a href="/search/astro-ph?searchtype=author&query=Mallmann%2C+N+D">Nicolas D. Mallmann</a>, <a href="/search/astro-ph?searchtype=author&query=Veilleux%2C+S">S. Veilleux</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">F. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotsky%2C+R">R. Mushotsky</a>, <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M">M. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">C. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Treister%2C+E">E. Treister</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Nguyen%2C+N">N. Nguyen</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%A4r%2C+R">R. B盲r</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">F. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">K. Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M">M. Powell</a>, <a href="/search/astro-ph?searchtype=author&query=Riffel%2C+R">R. Riffel</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">B. Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Urry%2C+C+M">C. M. Urry</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2201.04149v1-abstract-short" style="display: inline;"> Ionised gas kinematics provide crucial evidence of the impact that active galactic nuclei (AGN) have in regulating star formation in their host galaxies. Although the presence of outflows in AGN host galaxies has been firmly established, the calculation of outflow properties such as mass outflow rates and kinetic energy remains challenging. We present the [OIII]5007 ionised gas outflow properties… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.04149v1-abstract-full').style.display = 'inline'; document.getElementById('2201.04149v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.04149v1-abstract-full" style="display: none;"> Ionised gas kinematics provide crucial evidence of the impact that active galactic nuclei (AGN) have in regulating star formation in their host galaxies. Although the presence of outflows in AGN host galaxies has been firmly established, the calculation of outflow properties such as mass outflow rates and kinetic energy remains challenging. We present the [OIII]5007 ionised gas outflow properties of 22 z$<$0.1 X-ray AGN, derived from the BAT AGN Spectroscopic Survey using MUSE/VLT. With an average spatial resolution of 1" (0.1-1.2 kpc), the observations resolve the ionised gas clouds down to sub-kiloparsec scales. Resolved maps show that the [OIII] velocity dispersion is, on average, higher in regions ionised by the AGN, compared to star formation. We calculate the instantaneous outflow rates in individual MUSE spaxels by constructing resolved mass outflow rate maps, incorporating variable outflow density and velocity. We compare the instantaneous values with time-averaged outflow rates by placing mock fibres and slits on the MUSE field-of-view, a method often used in the literature. The instantaneous outflow rates (0.2-275 $M_{\odot}$ yr$^{-1}$) tend to be 2 orders of magnitude higher than the time-averaged outflow rates (0.001-40 $M_{\odot}$ yr$^{-1}$). The outflow rates correlate with the AGN bolometric luminosity ($L_{\rm bol}\sim$ 10$^{42.71}$-10$^{45.62}$ erg/s) but we find no correlations with black hole mass (10$^{6.1}$-10$^{8.9}$ M$_{\odot}$), Eddington ratio (0.002-1.1) and radio luminosity (10$^{21}$-10$^{26}$ W/Hz). We find the median coupling between the kinetic energy and $L_{\rm bol}$ to be 1%, consistent with the theoretical predictions for an AGN-driven outflow. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.04149v1-abstract-full').style.display = 'none'; document.getElementById('2201.04149v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Main paper: 20 pages, 15 figures, 3 tables. Accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.01691">arXiv:2112.01691</a> <span> [<a href="https://arxiv.org/pdf/2112.01691">pdf</a>, <a href="https://arxiv.org/format/2112.01691">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Characterization of Low Light Performance of a CMOS sensor for Ultraviolet Astronomical Applications </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Greffe%2C+T">Timothee Greffe</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+R">Roger Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Sherman%2C+M">Myles Sherman</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Earnshaw%2C+H">Hannah Earnshaw</a>, <a href="/search/astro-ph?searchtype=author&query=Grefenstette%2C+B">Brian Grefenstette</a>, <a href="/search/astro-ph?searchtype=author&query=Hennessy%2C+J">John Hennessy</a>, <a href="/search/astro-ph?searchtype=author&query=Nikzad%2C+S">Shouleh Nikzad</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="2112.01691v3-abstract-short" style="display: inline;"> CMOS detectors offer many advantages over CCDs for optical and UV astronomical applications, especially in space where high radiation tolerance is required. However, astronomical instruments are most often designed for low light-level observations demanding low dark current and read noise, good linearity and high dynamic range, characteristics that have not been widely demonstrated for CMOS imager… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.01691v3-abstract-full').style.display = 'inline'; document.getElementById('2112.01691v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.01691v3-abstract-full" style="display: none;"> CMOS detectors offer many advantages over CCDs for optical and UV astronomical applications, especially in space where high radiation tolerance is required. However, astronomical instruments are most often designed for low light-level observations demanding low dark current and read noise, good linearity and high dynamic range, characteristics that have not been widely demonstrated for CMOS imagers. We report the performance, over temperatures from 140 - 240 K, of a radiation hardened SRI 4Kx2K back-side illuminated CMOS image sensor with surface treatments that make it highly sensitive in blue and UV bands. After suppressing emission from glow sites resulting from defects in the engineering grade device examined in this work, a 0.077 me-/s dark current floor is reached at 160 K, rising to 1 me$^-$/s at 184 K, rivaling that of the best CCDs. We examine the trade-off between readout speed and read noise, finding that 1.43 e$^-$ median read noise is achieved using line-wise digital correlated double sampling at 700 kpix/s/ch corresponding to a 1.5 s readout time. The 15 ke$^-$ well capacity in high gain mode extends to 120 ke$^-$ in dual gain mode. Continued collection of photo-generated charge during readout enables a further dynamic range extension beyond $10^6$ e$^-$ effective well capacity with only 1% loss of exposure efficiency by combining short and long exposures. A quadratic fit to correct for non-linearity reduces gain correction residuals from 1.5% to 0.2% in low gain mode and to 0.4% in high gain mode. Cross-talk to adjacent pixels is only 0.4% vertically, 0.6% horizontally and 0.1% diagonally. These characteristics plus the relatively large 10 $渭$m pixel size, quasi 4-side buttability, electronic shutter and sub-array readout make this sensor an excellent choice for wide field astronomical imaging in space, even at FUV wavelengths where sky background is very low. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.01691v3-abstract-full').style.display = 'none'; document.getElementById('2112.01691v3-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 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">41 pages, 27 figures, 3 tables; improved statistical approach, added 3 figures, corrected typos, added references, revised abstract and introduction</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.00339">arXiv:2112.00339</a> <span> [<a href="https://arxiv.org/pdf/2112.00339">pdf</a>, <a href="https://arxiv.org/format/2112.00339">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/ac8d67">10.3847/1538-4357/ac8d67 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Orbital decay in M82 X-2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bachetti%2C+M">Matteo Bachetti</a>, <a href="/search/astro-ph?searchtype=author&query=Heida%2C+M">Marianne Heida</a>, <a href="/search/astro-ph?searchtype=author&query=Maccarone%2C+T">Thomas Maccarone</a>, <a href="/search/astro-ph?searchtype=author&query=Huppenkothen%2C+D">Daniela Huppenkothen</a>, <a href="/search/astro-ph?searchtype=author&query=Israel%2C+G+L">Gian Luca Israel</a>, <a href="/search/astro-ph?searchtype=author&query=Barret%2C+D">Didier Barret</a>, <a href="/search/astro-ph?searchtype=author&query=Brightman%2C+M">Murray Brightman</a>, <a href="/search/astro-ph?searchtype=author&query=Brumback%2C+M">McKinley Brumback</a>, <a href="/search/astro-ph?searchtype=author&query=Earnshaw%2C+H+P">Hannah P. Earnshaw</a>, <a href="/search/astro-ph?searchtype=author&query=Forster%2C+K">Karl Forster</a>, <a href="/search/astro-ph?searchtype=author&query=F%C3%BCrst%2C+F">Felix F眉rst</a>, <a href="/search/astro-ph?searchtype=author&query=Grefenstette%2C+B+W">Brian W. Grefenstette</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F+A">Fiona A. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Jaodand%2C+A+D">Amruta D. Jaodand</a>, <a href="/search/astro-ph?searchtype=author&query=Madsen%2C+K+K">Kristin K. Madsen</a>, <a href="/search/astro-ph?searchtype=author&query=Middleton%2C+M">Matthew Middleton</a>, <a href="/search/astro-ph?searchtype=author&query=Pike%2C+S+N">Sean N. Pike</a>, <a href="/search/astro-ph?searchtype=author&query=Pilia%2C+M">Maura Pilia</a>, <a href="/search/astro-ph?searchtype=author&query=Poutanen%2C+J">Juri Poutanen</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Tomsick%2C+J+A">John A. Tomsick</a>, <a href="/search/astro-ph?searchtype=author&query=Walton%2C+D+J">Dominic J. Walton</a>, <a href="/search/astro-ph?searchtype=author&query=Webb%2C+N">Natalie Webb</a>, <a href="/search/astro-ph?searchtype=author&query=Wilms%2C+J">J枚rn Wilms</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="2112.00339v2-abstract-short" style="display: inline;"> M82 X-2 is the first pulsating ultraluminous X-ray source (PULX) discovered. The luminosity of these extreme pulsars, if isotropic, implies an extreme mass transfer rate. An alternative is to assume a much lower mass transfer rate, but with an apparent luminosity boosted by geometrical beaming. Only an independent measurement of the mass transfer rate can help discriminate between these two scenar… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.00339v2-abstract-full').style.display = 'inline'; document.getElementById('2112.00339v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.00339v2-abstract-full" style="display: none;"> M82 X-2 is the first pulsating ultraluminous X-ray source (PULX) discovered. The luminosity of these extreme pulsars, if isotropic, implies an extreme mass transfer rate. An alternative is to assume a much lower mass transfer rate, but with an apparent luminosity boosted by geometrical beaming. Only an independent measurement of the mass transfer rate can help discriminate between these two scenarios. In this Paper, we follow the orbit of the neutron star for seven years, measure the decay of the orbit ($\dot{P}_{orb}/{P}_{orb}\approx-8\cdot10^{-6}\mathrm{yr}^{-1}$), and argue that this orbital decay is driven by extreme mass transfer of more than 150 times the mass transfer limit set by the Eddington luminosity. If this is true, the mass available to the accretor is more than enough to justify its luminosity, with no need for beaming. This also strongly favors models where the accretor is a highly-magnetized neutron star. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.00339v2-abstract-full').style.display = 'none'; document.getElementById('2112.00339v2-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">18 pages, 6 figures, accepted for publication in ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 937, 125 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.15608">arXiv:2111.15608</a> <span> [<a href="https://arxiv.org/pdf/2111.15608">pdf</a>, <a href="https://arxiv.org/format/2111.15608">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Science with the Ultraviolet Explorer (UVEX) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kulkarni%2C+S+R">S. R. Kulkarni</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F+A">Fiona A. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Grefenstette%2C+B+W">Brian W. Grefenstette</a>, <a href="/search/astro-ph?searchtype=author&query=Earnshaw%2C+H+P">Hannah P. Earnshaw</a>, <a href="/search/astro-ph?searchtype=author&query=Andreoni%2C+I">Igor Andreoni</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=Bloom%2C+J+S">Joshua S. Bloom</a>, <a href="/search/astro-ph?searchtype=author&query=Cenko%2C+S+B">S. Bradley Cenko</a>, <a href="/search/astro-ph?searchtype=author&query=Chornock%2C+R">Ryan Chornock</a>, <a href="/search/astro-ph?searchtype=author&query=Christiansen%2C+J+L">Jessie L. Christiansen</a>, <a href="/search/astro-ph?searchtype=author&query=Coughlin%2C+M+W">Michael W. Coughlin</a>, <a href="/search/astro-ph?searchtype=author&query=Criswell%2C+A+W">Alexander Wuollet Criswell</a>, <a href="/search/astro-ph?searchtype=author&query=Darvish%2C+B">Behnam Darvish</a>, <a href="/search/astro-ph?searchtype=author&query=Das%2C+K+K">Kaustav K. Das</a>, <a href="/search/astro-ph?searchtype=author&query=De%2C+K">Kishalay De</a>, <a href="/search/astro-ph?searchtype=author&query=Dessart%2C+L">Luc Dessart</a>, <a href="/search/astro-ph?searchtype=author&query=Dixon%2C+D">Don Dixon</a>, <a href="/search/astro-ph?searchtype=author&query=Dorsman%2C+B">Bas Dorsman</a>, <a href="/search/astro-ph?searchtype=author&query=El-Badry%2C+K">Kareem El-Badry</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+C">Christopher Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Ford%2C+K+E+S">K. E. Saavik Ford</a>, <a href="/search/astro-ph?searchtype=author&query=Fremling%2C+C">Christoffer Fremling</a>, <a href="/search/astro-ph?searchtype=author&query=Gansicke%2C+B+T">Boris T. Gansicke</a>, <a href="/search/astro-ph?searchtype=author&query=Gezari%2C+S">Suvi Gezari</a>, <a href="/search/astro-ph?searchtype=author&query=Goetberg%2C+Y">Y. Goetberg</a> , et al. (31 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="2111.15608v3-abstract-short" style="display: inline;"> UVEX is a proposed medium class Explorer mission designed to provide crucial missing capabilities that will address objectives central to a broad range of modern astrophysics. The UVEX design has two co-aligned wide-field imagers operating in the FUV and NUV and a powerful broadband medium resolution spectrometer. In its two-year baseline mission, UVEX will perform a multi-cadence synoptic all-sky… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.15608v3-abstract-full').style.display = 'inline'; document.getElementById('2111.15608v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.15608v3-abstract-full" style="display: none;"> UVEX is a proposed medium class Explorer mission designed to provide crucial missing capabilities that will address objectives central to a broad range of modern astrophysics. The UVEX design has two co-aligned wide-field imagers operating in the FUV and NUV and a powerful broadband medium resolution spectrometer. In its two-year baseline mission, UVEX will perform a multi-cadence synoptic all-sky survey 50/100 times deeper than GALEX in the NUV/FUV, cadenced surveys of the Large and Small Magellanic Clouds, rapid target of opportunity followup, as well as spectroscopic followup of samples of stars and galaxies. The science program is built around three pillars. First, UVEX will explore the low-mass, low-metallicity galaxy frontier through imaging and spectroscopic surveys that will probe key aspects of the evolution of galaxies by understanding how star formation and stellar evolution at low metallicities affect the growth and evolution of low-metallicity, low-mass galaxies in the local universe. Such galaxies contain half the mass in the local universe, and are analogs for the first galaxies, but observed at distances that make them accessible to detailed study. Second, UVEX will explore the dynamic universe through time-domain surveys and prompt spectroscopic followup capability will probe the environments, energetics, and emission processes in the early aftermaths of gravitational wave-discovered compact object mergers, discover hot, fast UV transients, and diagnose the early stages of stellar explosions. Finally, UVEX will become a key community resource by leaving a large all-sky legacy data set, enabling a wide range of scientific studies and filling a gap in the new generation of wide-field, sensitive optical and infrared surveys provided by the Rubin, Euclid, and Roman observatories. This paper discusses the scientific potential of UVEX, and the broad scientific program. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.15608v3-abstract-full').style.display = 'none'; document.getElementById('2111.15608v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">69 pages, 43 figures</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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