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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/?searchtype=author&query=Greenwell%2C+C+L">Claire L. Greenwell</a>, <a href="/search/?searchtype=author&query=Klindt%2C+L">Lizelke Klindt</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">George B. Lansbury</a>, <a href="/search/?searchtype=author&query=Rosario%2C+D+J">David J. Rosario</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">David M. Alexander</a>, <a href="/search/?searchtype=author&query=Aird%2C+J">James Aird</a>, <a href="/search/?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/?searchtype=author&query=Forster%2C+K">Karl Forster</a>, <a href="/search/?searchtype=author&query=Koss%2C+M+J">Michael J. Koss</a>, <a href="/search/?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/?searchtype=author&query=Tomsick%2C+J">John Tomsick</a>, <a href="/search/?searchtype=author&query=Brandt%2C+W+N">William N. Brandt</a>, <a href="/search/?searchtype=author&query=Connor%2C+T">Thomas Connor</a>, <a href="/search/?searchtype=author&query=Boorman%2C+P+G">Peter G. Boorman</a>, <a href="/search/?searchtype=author&query=Annuar%2C+A">Adlyka Annuar</a>, <a href="/search/?searchtype=author&query=Ballantyne%2C+D+R">David R. Ballantyne</a>, <a href="/search/?searchtype=author&query=Chen%2C+C">Chien-Ting Chen</a>, <a href="/search/?searchtype=author&query=Civano%2C+F">Francesca Civano</a>, <a href="/search/?searchtype=author&query=Comastri%2C+A">Andrea Comastri</a>, <a href="/search/?searchtype=author&query=Fawcett%2C+V+A">Victoria A. Fawcett</a>, <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</a>, <a href="/search/?searchtype=author&query=Gandhi%2C+P">Poshak Gandhi</a>, <a href="/search/?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/?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/2201.02208">arXiv:2201.02208</a> <span> [<a href="https://arxiv.org/pdf/2201.02208">pdf</a>, <a href="https://arxiv.org/format/2201.02208">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stac073">10.1093/mnras/stac073 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Quasar Feedback Survey: Multi-phase outflows, turbulence and evidence for feedback caused by low power radio jets inclined into the galaxy disk </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Girdhar%2C+A">A. Girdhar</a>, <a href="/search/?searchtype=author&query=Harrison%2C+C+M">C. M. Harrison</a>, <a href="/search/?searchtype=author&query=Mainieri%2C+V">V. Mainieri</a>, <a href="/search/?searchtype=author&query=Bittner%2C+A">A. Bittner</a>, <a href="/search/?searchtype=author&query=Costa%2C+T">T. Costa</a>, <a href="/search/?searchtype=author&query=Kharb%2C+P">P. Kharb</a>, <a href="/search/?searchtype=author&query=Mukherjee%2C+D">D. Mukherjee</a>, <a href="/search/?searchtype=author&query=Battaia%2C+F+A">F. Arrigoni Battaia</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Rivera%2C+G+C">G. Calistro Rivera</a>, <a href="/search/?searchtype=author&query=Circosta%2C+C">C. Circosta</a>, <a href="/search/?searchtype=author&query=De+Breuck%2C+C">C. De Breuck</a>, <a href="/search/?searchtype=author&query=Edge%2C+A+C">A. C. Edge</a>, <a href="/search/?searchtype=author&query=Farina%2C+E+P">E. P. Farina</a>, <a href="/search/?searchtype=author&query=Kakkad%2C+D">D. Kakkad</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">G. B. Lansbury</a>, <a href="/search/?searchtype=author&query=Molyneux%2C+S+J">S. J. Molyneux</a>, <a href="/search/?searchtype=author&query=Mullaney%2C+J+R">J. R. Mullaney</a>, <a href="/search/?searchtype=author&query=S.%2C+S">Silpa S.</a>, <a href="/search/?searchtype=author&query=Thomson%2C+A+P">A. P. Thomson</a>, <a href="/search/?searchtype=author&query=Ward%2C+S+R">S. R. Ward</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="2201.02208v2-abstract-short" style="display: inline;"> We present a study of a luminous, z=0.15, type-2 quasar (log [L([OIII])/(erg/s)]=42.8) from the Quasar Feedback Survey. It is classified as 'radio-quiet' (log [L(1.4 GHz)/(W/Hz)]=23.8); however, radio imaging reveals ~1 kpc low-power jets (log [Pjet/(erg/s)]=44) inclined into the plane of the galaxy disk. We combine MUSE and ALMA observations to map stellar kinematics and ionised and molecular gas… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.02208v2-abstract-full').style.display = 'inline'; document.getElementById('2201.02208v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.02208v2-abstract-full" style="display: none;"> We present a study of a luminous, z=0.15, type-2 quasar (log [L([OIII])/(erg/s)]=42.8) from the Quasar Feedback Survey. It is classified as 'radio-quiet' (log [L(1.4 GHz)/(W/Hz)]=23.8); however, radio imaging reveals ~1 kpc low-power jets (log [Pjet/(erg/s)]=44) inclined into the plane of the galaxy disk. We combine MUSE and ALMA observations to map stellar kinematics and ionised and molecular gas properties. The jets are seen to drive galaxy-wide bi-conical turbulent outflows, reaching W80 = 1000-1300 km/s, in the ionised phase (traced via optical emission-lines), which also have increased electron densities compared to the quiescent gas. The turbulent gas is driven perpendicular to the jet axis and is escaping along the galaxy minor axis, reaching 7.5 kpc on both sides. Traced via CO(3-2) emission, the turbulent material in molecular gas phase is one-third as spatially extended and has 3 times lower velocity-dispersion as compared to ionised gas. The jets are seen to be strongly interacting with the interstellar medium (ISM) through enhanced ionised emission and disturbed/depleted molecular gas at the jet termini. We see further evidence for jet-induced feedback through significantly higher stellar velocity-dispersion aligned, and co-spatial with, the jet axis (<5 deg). We discuss possible negative and positive feedback scenarios arising due to the interaction of the low-power jets with the ISM in the context of recent jet-ISM interaction simulations, which qualitatively agree with our observations. We discuss how jet-induced feedback could be an important feedback mechanism even in bolometrically luminous 'radio-quiet' quasars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.02208v2-abstract-full').style.display = 'none'; document.getElementById('2201.02208v2-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">v1</span> submitted 6 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS. Main manuscript has 21 pages with 8 figures. Supplementary material is available for download under "Ancillary files" or by downloading the source file listed under "Other formats"</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.02078">arXiv:2105.02078</a> <span> [<a href="https://arxiv.org/pdf/2105.02078">pdf</a>, <a href="https://arxiv.org/format/2105.02078">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/stab1306">10.1093/mnras/stab1306 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Highly Accreting Low-Mass Black Hole Hidden in the Dust: Suzaku and NuSTAR observations of the NLS1 Mrk 1239 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Jiang%2C+J">Jiachen Jiang</a>, <a href="/search/?searchtype=author&query=Balokovi%C4%87%2C+M">Mislav Balokovi膰</a>, <a href="/search/?searchtype=author&query=Brightman%2C+M">Murray Brightman</a>, <a href="/search/?searchtype=author&query=Liu%2C+H">Honghui Liu</a>, <a href="/search/?searchtype=author&query=Harrison%2C+F+A">Fiona A. Harrison</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">George B. Lansbury</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="2105.02078v1-abstract-short" style="display: inline;"> We present torus modelling for the X-ray spectra of a nearby narrow-line Seyfert 1 galaxy Mrk 1239 ($z=0.0199$), based on archival Suzaku, NuSTAR and Swift observations. Our model suggests very soft intrinsic power-law continuum emission of $螕\approx2.57$ in 2019 and $螕\approx2.98$ in 2007. By applying a correction factor to the unabsorbed X-ray luminosity, we find that Mrk 1239 is accreting near… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.02078v1-abstract-full').style.display = 'inline'; document.getElementById('2105.02078v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.02078v1-abstract-full" style="display: none;"> We present torus modelling for the X-ray spectra of a nearby narrow-line Seyfert 1 galaxy Mrk 1239 ($z=0.0199$), based on archival Suzaku, NuSTAR and Swift observations. Our model suggests very soft intrinsic power-law continuum emission of $螕\approx2.57$ in 2019 and $螕\approx2.98$ in 2007. By applying a correction factor to the unabsorbed X-ray luminosity, we find that Mrk 1239 is accreting near or around the Eddington limit. Our best-fit spectral model also suggests a torus with a column density of $\log(N_{\rm H, ave}/$cm$^{-2})=25.0\pm0.2$ and a high covering factor of $0.90$ in Mrk 1239, indicating that this source is most likely to be viewed almost face-on with $i\approx26^{\circ}$. Our line of sight might cross the edge of the torus with $N_{\rm H, los}=2-5\times10^{23}$cm$^{-2}$. The high Eddington ratio and the high line-of-sight column density makes Mrk 1239 one of the AGNs that are close to the limit where wind may form near the edge of the torus due to high radiation pressure. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.02078v1-abstract-full').style.display = 'none'; document.getElementById('2105.02078v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">11 pages, 8 figures (accepted by MNRAS)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2103.00014">arXiv:2103.00014</a> <span> [<a href="https://arxiv.org/pdf/2103.00014">pdf</a>, <a href="https://arxiv.org/format/2103.00014">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/10.1093/mnras/stab549">10.1093/mnras/stab549 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Quasar Feedback Survey: Discovering hidden Radio-AGN and their connection to the host galaxy ionised gas </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Jarvis%2C+M+E">M. E. Jarvis</a>, <a href="/search/?searchtype=author&query=Harrison%2C+C+M">C. M. Harrison</a>, <a href="/search/?searchtype=author&query=Mainieri%2C+V">V. Mainieri</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Battaia%2C+F+A">F. Arrigoni Battaia</a>, <a href="/search/?searchtype=author&query=Rivera%2C+G+C">G. Calistro Rivera</a>, <a href="/search/?searchtype=author&query=Circosta%2C+C">C. Circosta</a>, <a href="/search/?searchtype=author&query=Costa%2C+T">T. Costa</a>, <a href="/search/?searchtype=author&query=De+Breuck%2C+C">C. De Breuck</a>, <a href="/search/?searchtype=author&query=Edge%2C+A+C">A. C. Edge</a>, <a href="/search/?searchtype=author&query=Girdhar%2C+A">A. Girdhar</a>, <a href="/search/?searchtype=author&query=Kakkad%2C+D">D. Kakkad</a>, <a href="/search/?searchtype=author&query=Kharb%2C+P">P. Kharb</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">G. B. Lansbury</a>, <a href="/search/?searchtype=author&query=Molyneux%2C+S+J">S. J. Molyneux</a>, <a href="/search/?searchtype=author&query=Mukherjee%2C+D">D. Mukherjee</a>, <a href="/search/?searchtype=author&query=Mullaney%2C+J+R">J. R. Mullaney</a>, <a href="/search/?searchtype=author&query=Farina%2C+E+P">E. P. Farina</a>, <a href="/search/?searchtype=author&query=S.%2C+S">Silpa S.</a>, <a href="/search/?searchtype=author&query=Thomson%2C+A+P">A. P. Thomson</a>, <a href="/search/?searchtype=author&query=Ward%2C+S+R">S. R. Ward</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="2103.00014v1-abstract-short" style="display: inline;"> We present the first results from the Quasar Feedback Survey, a sample of 42 z<0.2, [O III] luminous AGN (L[O III]>10^42.1 ergs/s) with moderate radio luminosities (i.e. L(1.4GHz)>10^23.4 W/Hz; median L(1.4GHz)=5.9x10^23 W/Hz). Using high spatial resolution (~0.3-1 arcsec), 1.5-6 GHz radio images from the Very Large Array, we find that 67 percent of the sample have spatially extended radio feature… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.00014v1-abstract-full').style.display = 'inline'; document.getElementById('2103.00014v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.00014v1-abstract-full" style="display: none;"> We present the first results from the Quasar Feedback Survey, a sample of 42 z<0.2, [O III] luminous AGN (L[O III]>10^42.1 ergs/s) with moderate radio luminosities (i.e. L(1.4GHz)>10^23.4 W/Hz; median L(1.4GHz)=5.9x10^23 W/Hz). Using high spatial resolution (~0.3-1 arcsec), 1.5-6 GHz radio images from the Very Large Array, we find that 67 percent of the sample have spatially extended radio features, on ~1-60 kpc scales. The radio sizes and morphologies suggest that these may be lower radio luminosity versions of compact, radio-loud AGN. By combining the radio-to-infrared excess parameter, spectral index, radio morphology and brightness temperature, we find radio emission in at least 57 percent of the sample that is associated with AGN-related processes (e.g. jets, quasar-driven winds or coronal emission). This is despite only 9.5-21 percent being classified as radio-loud using traditional criteria. The origin of the radio emission in the remainder of the sample is unclear. We find that both the established anti-correlation between radio size and the width of the [O III] line, and the known trend for the most [O III] luminous AGN to be associated with spatially-extended radio emission, also hold for our sample of moderate radio luminosity quasars. These observations add to the growing evidence of a connection between the radio emission and ionised gas in quasar host galaxies. This work lays the foundation for deeper investigations into the drivers and impact of feedback in this unique sample. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.00014v1-abstract-full').style.display = 'none'; document.getElementById('2103.00014v1-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> 26 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS. Data products from this paper and the survey pilot papers are available through our website: https://blogs.ncl.ac.uk/quasarfeedbacksurvey/. The extensive supplementary material (containing additional figures and information on individual targets) is available for download under "Ancillary files" or by downloading the source file listed under "Other formats"</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.08870">arXiv:2011.08870</a> <span> [<a href="https://arxiv.org/pdf/2011.08870">pdf</a>, <a href="https://arxiv.org/ps/2011.08870">ps</a>, <a href="https://arxiv.org/format/2011.08870">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/staa3666">10.1093/mnras/staa3666 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A New Transient Ultraluminous X-ray Source in NGC 7090 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Walton%2C+D+J">D. J. Walton</a>, <a href="/search/?searchtype=author&query=Heida%2C+M">M. Heida</a>, <a href="/search/?searchtype=author&query=Bachetti%2C+M">M. Bachetti</a>, <a href="/search/?searchtype=author&query=Furst%2C+F">F. Furst</a>, <a href="/search/?searchtype=author&query=Brightman%2C+M">M. Brightman</a>, <a href="/search/?searchtype=author&query=Earnshaw%2C+H">H. Earnshaw</a>, <a href="/search/?searchtype=author&query=Evans%2C+P+A">P. A. Evans</a>, <a href="/search/?searchtype=author&query=Fabian%2C+A+C">A. C. Fabian</a>, <a href="/search/?searchtype=author&query=Grefenstette%2C+B+W">B. W. Grefenstette</a>, <a href="/search/?searchtype=author&query=Harrison%2C+F+A">F. A. Harrison</a>, <a href="/search/?searchtype=author&query=Israel%2C+G+L">G. L. Israel</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">G. B. Lansbury</a>, <a href="/search/?searchtype=author&query=Middleton%2C+M+J">M. J. Middleton</a>, <a href="/search/?searchtype=author&query=Pike%2C+S">S. Pike</a>, <a href="/search/?searchtype=author&query=Rana%2C+V">V. Rana</a>, <a href="/search/?searchtype=author&query=Roberts%2C+T+P">T. P. Roberts</a>, <a href="/search/?searchtype=author&query=Castillo%2C+G+A+R">G. A. Rodriguez Castillo</a>, <a href="/search/?searchtype=author&query=Salvaterra%2C+R">R. Salvaterra</a>, <a href="/search/?searchtype=author&query=Song%2C+X">X. Song</a>, <a href="/search/?searchtype=author&query=Stern%2C+D">D. Stern</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="2011.08870v2-abstract-short" style="display: inline;"> We report on the discovery of a new, transient ultraluminous X-ray source (ULX) in the galaxy NGC 7090. This new ULX, which we refer to as NGC 7090 ULX3, was discovered via monitoring with $Swift$ during 2019-20, and to date has exhibited a peak luminosity of $L_{\rm{X}} \sim 6 \times 10^{39}$ erg s$^{-1}$. Archival searches show that, prior to its recent transition into the ULX regime, ULX3 appea… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.08870v2-abstract-full').style.display = 'inline'; document.getElementById('2011.08870v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.08870v2-abstract-full" style="display: none;"> We report on the discovery of a new, transient ultraluminous X-ray source (ULX) in the galaxy NGC 7090. This new ULX, which we refer to as NGC 7090 ULX3, was discovered via monitoring with $Swift$ during 2019-20, and to date has exhibited a peak luminosity of $L_{\rm{X}} \sim 6 \times 10^{39}$ erg s$^{-1}$. Archival searches show that, prior to its recent transition into the ULX regime, ULX3 appeared to exhibit a fairly stable luminosity of $L_{\rm{X}} \sim 10^{38}$ erg s$^{-1}$. Such strong long-timescale variability may be reminiscent of the small population of known ULX pulsars, although deep follow-up observations with $XMM$-$Newton$ and $NuSTAR$ do not reveal any robust X-ray pulsation signals. Pulsations similar to those seen from known ULX pulsars cannot be completely excluded, however, as the limit on the pulsed fraction of any signal that remains undetected in these data is $\lesssim$20\%. The broadband spectrum from these observations is well modelled with a simple thin disc model, consistent with sub-Eddington accretion, which may instead imply a moderately large black hole accretor ($M_{\rm{BH}} \sim 40 ~ M_{\odot}$). Similarly, though, more complex models consistent with the super-Eddington spectra seen in other ULXs (and the known ULX pulsars) cannot be excluded given the limited signal-to-noise of the available broadband data. The nature of the accretor powering this new ULX therefore remains uncertain. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.08870v2-abstract-full').style.display = 'none'; document.getElementById('2011.08870v2-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 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 7 figures; accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.10351">arXiv:2007.10351</a> <span> [<a href="https://arxiv.org/pdf/2007.10351">pdf</a>, <a href="https://arxiv.org/format/2007.10351">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/staa2196">10.1093/mnras/staa2196 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> High molecular gas content and star formation rates in local galaxies that host quasars, outflows and jets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Jarvis%2C+M+E">M. E. Jarvis</a>, <a href="/search/?searchtype=author&query=Harrison%2C+C+M">C. M. Harrison</a>, <a href="/search/?searchtype=author&query=Mainieri%2C+V">V. Mainieri</a>, <a href="/search/?searchtype=author&query=Rivera%2C+G+C">G. Calistro Rivera</a>, <a href="/search/?searchtype=author&query=Jethwa%2C+P">P. Jethwa</a>, <a href="/search/?searchtype=author&query=Zhang%2C+Z+-">Z. -Y. Zhang</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Circosta%2C+C">C. Circosta</a>, <a href="/search/?searchtype=author&query=Costa%2C+T">T. Costa</a>, <a href="/search/?searchtype=author&query=De+Breuck%2C+C">C. De Breuck</a>, <a href="/search/?searchtype=author&query=Kakkad%2C+D">D. Kakkad</a>, <a href="/search/?searchtype=author&query=Kharb%2C+P">P. Kharb</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">G. B. Lansbury</a>, <a href="/search/?searchtype=author&query=Thomson%2C+A+P">A. P. Thomson</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2007.10351v1-abstract-short" style="display: inline;"> We use a sample of powerful z~0.1 type 2 quasars ('obscured'; log[L(AGN)/erg/s]>~45), which host kiloparsec-scale ionized outflows and jets, to identify possible signatures of AGN feedback on the total molecular gas reservoirs of their host galaxies. Specifically, we present Atacama Pathfinder EXperiment (APEX) observations of the CO(2-1) transition for nine sources and the CO(6-5) for a subset of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.10351v1-abstract-full').style.display = 'inline'; document.getElementById('2007.10351v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.10351v1-abstract-full" style="display: none;"> We use a sample of powerful z~0.1 type 2 quasars ('obscured'; log[L(AGN)/erg/s]>~45), which host kiloparsec-scale ionized outflows and jets, to identify possible signatures of AGN feedback on the total molecular gas reservoirs of their host galaxies. Specifically, we present Atacama Pathfinder EXperiment (APEX) observations of the CO(2-1) transition for nine sources and the CO(6-5) for a subset of three. We find that the majority of our sample reside in starburst galaxies (average specific star formation rates of 1.7/Gyr), with the seven CO-detected quasars also having large molecular gas reservoirs (average Mgas = 1.3x10^10Msun), even though we had no pre-selection on the star formation or molecular gas properties. Despite the presence of quasars and outflows, we find that the molecular gas fractions (Mgas/Mstar = 0.1-1.2) and depletion times (Mgas/SFR = 0.16-0.95Gyr) are consistent with those expected for the overall galaxy population with matched stellar masses and specific star formation rates. Furthermore, for at least two of the three targets with the required measurements, the CO(6-5)/CO(2-1) emission-line ratios are consistent with star formation dominating the CO excitation over this range of transitions. The targets in our study represent a gas-rich phase of galaxy evolution with simultaneously high levels of star formation and nuclear activity; furthermore, the jets and outflows do not have an immediate appreciable impact on the global molecular gas reservoirs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.10351v1-abstract-full').style.display = 'none'; document.getElementById('2007.10351v1-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 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS. Supplementary material is available for download under "Ancillary files"</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2006.13583">arXiv:2006.13583</a> <span> [<a href="https://arxiv.org/pdf/2006.13583">pdf</a>, <a href="https://arxiv.org/ps/2006.13583">ps</a>, <a href="https://arxiv.org/format/2006.13583">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/staa1820">10.1093/mnras/staa1820 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> $NuSTAR$ Observations of Four Nearby X-ray Faint AGN: Low Luminosity or Heavy Obscuration? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Annuar%2C+A">A. Annuar</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Gandhi%2C+P">P. Gandhi</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">G. B. Lansbury</a>, <a href="/search/?searchtype=author&query=Asmus%2C+D">D. Asmus</a>, <a href="/search/?searchtype=author&query=Balokovic%2C+M">M. Balokovic</a>, <a href="/search/?searchtype=author&query=Ballantyne%2C+D+R">D. R. Ballantyne</a>, <a href="/search/?searchtype=author&query=Bauer%2C+F+E">F. E. Bauer</a>, <a href="/search/?searchtype=author&query=Boorman%2C+P+G">P. G. Boorman</a>, <a href="/search/?searchtype=author&query=Brandt%2C+W+N">W. N. Brandt</a>, <a href="/search/?searchtype=author&query=Brightman%2C+M">M. Brightman</a>, <a href="/search/?searchtype=author&query=Chen%2C+C+-+J">C. -T. J. Chen</a>, <a href="/search/?searchtype=author&query=Del+Moro%2C+A">A. Del Moro</a>, <a href="/search/?searchtype=author&query=Farrah%2C+D">D. Farrah</a>, <a href="/search/?searchtype=author&query=Harrison%2C+F+A">F. A. Harrison</a>, <a href="/search/?searchtype=author&query=Koss%2C+M+J">M. J. Koss</a>, <a href="/search/?searchtype=author&query=Lanz%2C+L">L. Lanz</a>, <a href="/search/?searchtype=author&query=Marchesi%2C+S">S. Marchesi</a>, <a href="/search/?searchtype=author&query=Masini%2C+A">A. Masini</a>, <a href="/search/?searchtype=author&query=Nardini%2C+E">E. Nardini</a>, <a href="/search/?searchtype=author&query=Ricci%2C+C">C. Ricci</a>, <a href="/search/?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/?searchtype=author&query=Zappacosta%2C+L">L. Zappacosta</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2006.13583v1-abstract-short" style="display: inline;"> We present $NuSTAR$ observations of four active galactic nuclei (AGN) located within 15 Mpc. These AGN, namely ESO 121-G6, NGC 660, NGC 3486 and NGC 5195, have observed X-ray luminosities of $L_{\rm 2-10\ keV, obs} \lesssim$ 10$^{39}$ erg s$^{-1}$, classifying them as low luminosity AGN (LLAGN). We perform broadband X-ray spectral analysis for the AGN by combining our $NuSTAR$ data with $Chandra$… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.13583v1-abstract-full').style.display = 'inline'; document.getElementById('2006.13583v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.13583v1-abstract-full" style="display: none;"> We present $NuSTAR$ observations of four active galactic nuclei (AGN) located within 15 Mpc. These AGN, namely ESO 121-G6, NGC 660, NGC 3486 and NGC 5195, have observed X-ray luminosities of $L_{\rm 2-10\ keV, obs} \lesssim$ 10$^{39}$ erg s$^{-1}$, classifying them as low luminosity AGN (LLAGN). We perform broadband X-ray spectral analysis for the AGN by combining our $NuSTAR$ data with $Chandra$ or $XMM-Newton$ observations to directly measure their column densities ($N_{\rm H}$) and infer their intrinsic power. We complement our X-ray data with archival and new high angular resolution mid-infrared (mid-IR) data for all objects, except NGC 5195. Based on our X-ray spectral analysis, we found that both ESO 121-G6 and NGC 660 are heavily obscured ($N_{\rm H}$ > 10$^{23}$ cm$^{-2}$; $L_{\rm 2-10\ keV,\ int} \sim$ 10$^{41}$ erg s$^{-1}$), and NGC 660 may be Compton-thick. We also note that the X-ray flux and spectral slope for ESO 121-G6 have significantly changed over the last decade, indicating significant changes in the obscuration and potentially accretion rate. On the other hand, NGC 3486 and NGC 5195 appear to be unobscured and just mildly obscured, respectively, with $L_{\rm 2-10\ keV,\ int} <$ 10$^{39}$ erg s$^{-1}$; i.e., genuine LLAGN. Both of the heavily obscured AGN have $L_{\rm bol} >$ 10$^{41}$ erg s$^{-1}$ and $位_{\rm Edd} \gtrsim$ 10$^{-3}$, and are detected in high angular resolution mid-IR imaging, indicating the presence of obscuring dust on nuclear scale. NGC 3486 however, is undetected in high-resolution mid-IR imaging, and the current data do not provide stringent constraints on the presence or absence of obscuring nuclear dust in the AGN. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.13583v1-abstract-full').style.display = 'none'; document.getElementById('2006.13583v1-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 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 11 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/1910.11857">arXiv:1910.11857</a> <span> [<a href="https://arxiv.org/pdf/1910.11857">pdf</a>, <a href="https://arxiv.org/ps/1910.11857">ps</a>, <a href="https://arxiv.org/format/1910.11857">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/stz3036">10.1093/mnras/stz3036 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Hunt for Pulsating Ultraluminous X-ray Sources </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Song%2C+X">X. Song</a>, <a href="/search/?searchtype=author&query=Walton%2C+D+J">D. J. Walton</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">G. B. Lansbury</a>, <a href="/search/?searchtype=author&query=Evans%2C+P+A">P. A. Evans</a>, <a href="/search/?searchtype=author&query=Fabian%2C+A+C">A. C. Fabian</a>, <a href="/search/?searchtype=author&query=Earnshaw%2C+H">H. Earnshaw</a>, <a href="/search/?searchtype=author&query=Roberts%2C+T+P">T. P. Roberts</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="1910.11857v1-abstract-short" style="display: inline;"> Motivated by the recent discoveries that six Ultraluminous X-ray Sources (ULXs) are powered by highly super-Eddington X-ray pulsars, we searched for additional pulsating ULX (PULX) candidates by identifying sources that exhibit long-term flux variability of at least an order of magnitude (a common feature seen in the 6 known PULXs, which may potentially be related to transitions to the propeller r… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.11857v1-abstract-full').style.display = 'inline'; document.getElementById('1910.11857v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1910.11857v1-abstract-full" style="display: none;"> Motivated by the recent discoveries that six Ultraluminous X-ray Sources (ULXs) are powered by highly super-Eddington X-ray pulsars, we searched for additional pulsating ULX (PULX) candidates by identifying sources that exhibit long-term flux variability of at least an order of magnitude (a common feature seen in the 6 known PULXs, which may potentially be related to transitions to the propeller regime). Expanding on previous studies, we used the available fluxes from XMM-Newton, Swift and Chandra, along with carefully computed upper limits in cases of a non-detection, to construct long-term lightcurves for a sample of 296 ULXs selected from the XMM-Newton archive. Among these 296, we find 25 sources showing flux variability larger than a factor of 10, of which 17 show some evidence for (or are at least consistent with) exhibiting bi-modal flux distributions, as would be expected for sources undergoing propeller transitions. These sources are excellent candidates for continued monitoring programs to further test for this behaviour. There are 3 sources in our final sample with fluxes similar to NGC 5907 ULX1, currently the faintest known PULX, which would also be good targets for deeper observations with current facilities to search for pulsations. For the rest of the PULX candidates identified here, the next generation of X-ray telescopes (such as Athena) may be required to determine their nature owing to their lower peak fluxes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.11857v1-abstract-full').style.display = 'none'; document.getElementById('1910.11857v1-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 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 11 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/1910.00602">arXiv:1910.00602</a> <span> [<a href="https://arxiv.org/pdf/1910.00602">pdf</a>, <a href="https://arxiv.org/format/1910.00602">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/staa1220">10.1093/mnras/staa1220 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> X-ray Observations of Luminous Dusty Quasars at z > 2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">G. B. Lansbury</a>, <a href="/search/?searchtype=author&query=Banerji%2C+M">M. Banerji</a>, <a href="/search/?searchtype=author&query=Fabian%2C+A+C">A. C. Fabian</a>, <a href="/search/?searchtype=author&query=Temple%2C+M+J">M. J. Temple</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="1910.00602v2-abstract-short" style="display: inline;"> We present new X-ray observations of luminous heavily dust-reddened quasars (HRQs) selected from infrared sky surveys. HRQs appear to be a dominant population at high redshifts and the highest luminosities, and may be associated with a transitional "blowout" phase of black hole and galaxy co-evolution models. Despite this, their high-energy properties have been poorly known. We use the overall sam… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.00602v2-abstract-full').style.display = 'inline'; document.getElementById('1910.00602v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1910.00602v2-abstract-full" style="display: none;"> We present new X-ray observations of luminous heavily dust-reddened quasars (HRQs) selected from infrared sky surveys. HRQs appear to be a dominant population at high redshifts and the highest luminosities, and may be associated with a transitional "blowout" phase of black hole and galaxy co-evolution models. Despite this, their high-energy properties have been poorly known. We use the overall sample of $10$ objects with XMM-Newton coverage to study the high-energy properties of HRQs at $\left< L_{\rm bol} \right> = 10^{47.5}$ erg/s and $\left< z \right>= 2.5$. For the seven sources with strong X-ray detections, we perform spectral analyses. These find a median X-ray luminosity of $\left< L_{\rm 2-10\,keV} \right> = 10^{45.1}$ erg/s, comparable to the most powerful X-ray quasars known. The gas column densities are $N_{\rm H}=(1$-$8)\times 10^{22}$ cm$^{-2}$, in agreement with the amount of dust extinction observed. The dust to gas ratios are sub-Galactic, but are higher than found in local AGN. The intrinsic X-ray luminosities of HRQs are weak compared to the mid-infrared ($L_{\rm 6渭m}$) and bolometric luminosities ($L_{\rm bol}$), in agreement with findings for other luminous quasar samples. For instance, the X-ray to bolometric corrections range from $魏_{\rm bol}\approx 50$-$3000$. The moderate absorption levels and accretion rates close to the Eddington limit ($\left< 位_{\rm Edd} \right>=1.06$) are in agreement with a quasar blowout phase. Indeed, we find that the HRQs lie in the forbidden region of the $N_{\rm H}$-$位_{\rm Edd}$ plane, and therefore that radiation pressure feedback on the dusty interstellar medium may be driving a phase of blowout that has been ongoing for a few $10^{5}$ years. The wider properties, including [OIII] narrow-line region kinematics, broadly agree with this interpretation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.00602v2-abstract-full').style.display = 'none'; document.getElementById('1910.00602v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">In press. 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/1905.11439">arXiv:1905.11439</a> <span> [<a href="https://arxiv.org/pdf/1905.11439">pdf</a>, <a href="https://arxiv.org/format/1905.11439">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"> Resolving the cosmic X-ray background with a next-generation high-energy X-ray observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Hickox%2C+R+C">R. C. Hickox</a>, <a href="/search/?searchtype=author&query=Civano%2C+F">F. Civano</a>, <a href="/search/?searchtype=author&query=Ballantyne%2C+D+R">D. R. Ballantyne</a>, <a href="/search/?searchtype=author&query=Balokovic%2C+M">M. Balokovic</a>, <a href="/search/?searchtype=author&query=Boorman%2C+P+G">P. G. Boorman</a>, <a href="/search/?searchtype=author&query=Brandt%2C+W+N">W. N. Brandt</a>, <a href="/search/?searchtype=author&query=Canning%2C+R+E+A">R. E. A. Canning</a>, <a href="/search/?searchtype=author&query=Fornasini%2C+F">F. Fornasini</a>, <a href="/search/?searchtype=author&query=Gandhi%2C+P">P. Gandhi</a>, <a href="/search/?searchtype=author&query=Jones%2C+M+L">M. L. Jones</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">G. B. Lansbury</a>, <a href="/search/?searchtype=author&query=Lanz%2C+L">L. Lanz</a>, <a href="/search/?searchtype=author&query=Lanzuisi%2C+G">G. Lanzuisi</a>, <a href="/search/?searchtype=author&query=Madsen%2C+K+K">K. K. Madsen</a>, <a href="/search/?searchtype=author&query=Marchesi%2C+S">S. Marchesi</a>, <a href="/search/?searchtype=author&query=Masini%2C+A">A. Masini</a>, <a href="/search/?searchtype=author&query=Ananna%2C+T">T. Ananna</a>, <a href="/search/?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/?searchtype=author&query=Ricci%2C+C">C. Ricci</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1905.11439v1-abstract-short" style="display: inline;"> The cosmic X-ray background (CXB), which peaks at an energy of ~30 keV, is produced primarily by emission from accreting supermassive black holes (SMBHs). The CXB therefore serves as a constraint on the integrated SMBH growth in the Universe and the accretion physics and obscuration in active galactic nuclei (AGNs). This paper gives an overview of recent progress in understanding the high-energy (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.11439v1-abstract-full').style.display = 'inline'; document.getElementById('1905.11439v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1905.11439v1-abstract-full" style="display: none;"> The cosmic X-ray background (CXB), which peaks at an energy of ~30 keV, is produced primarily by emission from accreting supermassive black holes (SMBHs). The CXB therefore serves as a constraint on the integrated SMBH growth in the Universe and the accretion physics and obscuration in active galactic nuclei (AGNs). This paper gives an overview of recent progress in understanding the high-energy (>~10 keV) X-ray emission from AGNs and the synthesis of the CXB, with an emphasis on results from NASA's NuSTAR hard X-ray mission. We then discuss remaining challenges and open questions regarding the nature of AGN obscuration and AGN physics. Finally, we highlight the exciting opportunities for a next-generation, high-resolution hard X-ray mission to achieve the long-standing goal of resolving and characterizing the vast majority of the accreting SMBHs that produce the CXB. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.11439v1-abstract-full').style.display = 'none'; document.getElementById('1905.11439v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 May, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Science White paper submitted to Astro2020 Decadal Survey; 5 pages, 3 figures, plus references and cover page</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1902.07727">arXiv:1902.07727</a> <span> [<a href="https://arxiv.org/pdf/1902.07727">pdf</a>, <a href="https://arxiv.org/format/1902.07727">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stz556">10.1093/mnras/stz556 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Prevalence of radio jets associated with galactic outflows and feedback from quasars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Jarvis%2C+M+E">M. E. Jarvis</a>, <a href="/search/?searchtype=author&query=Harrison%2C+C+M">C. M. Harrison</a>, <a href="/search/?searchtype=author&query=Thomson%2C+A+P">A. P. Thomson</a>, <a href="/search/?searchtype=author&query=Circosta%2C+C">C. Circosta</a>, <a href="/search/?searchtype=author&query=Mainieri%2C+V">V. Mainieri</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Edge%2C+A+C">A. C. Edge</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">G. B. Lansbury</a>, <a href="/search/?searchtype=author&query=Molyneux%2C+S+J">S. J. Molyneux</a>, <a href="/search/?searchtype=author&query=Mullaney%2C+J+R">J. R. Mullaney</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="1902.07727v1-abstract-short" style="display: inline;"> We present 1-7 GHz high-resolution radio imaging (VLA and e-MERLIN) and spatially-resolved ionized gas kinematics for ten z<0.2 type~2 `obscured' quasars (log [L(AGN)/(erg/s)]>~45) with moderate radio luminosities (log [L(1.4GHz)/(W/Hz)]=23.3-24.4). These targets were selected to have known ionized outflows based on broad [OIII] emission-line components (FWHM~800-1800 km/s). Although `radio-quiet'… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.07727v1-abstract-full').style.display = 'inline'; document.getElementById('1902.07727v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1902.07727v1-abstract-full" style="display: none;"> We present 1-7 GHz high-resolution radio imaging (VLA and e-MERLIN) and spatially-resolved ionized gas kinematics for ten z<0.2 type~2 `obscured' quasars (log [L(AGN)/(erg/s)]>~45) with moderate radio luminosities (log [L(1.4GHz)/(W/Hz)]=23.3-24.4). These targets were selected to have known ionized outflows based on broad [OIII] emission-line components (FWHM~800-1800 km/s). Although `radio-quiet' and not `radio AGN' by many traditional criteria, we show that for nine of the targets, star formation likely accounts for <~10 per cent of the radio emission. We find that ~80-90 per cent of these nine targets exhibit extended radio structures on 1-25 kpc scales. The quasars' radio morphologies, spectral indices and position on the radio size-luminosity relationship reveals that these sources are consistent with being low power compact radio galaxies. Therefore, we favour radio jets as dominating the radio emission in the majority of these quasars. The radio jets we observe are associated with morphologically and kinematically distinct features in the ionized gas, such as increased turbulence and outflowing bubbles, revealing jet-gas interaction on galactic scales. Importantly, such conclusions could not have been drawn from current low-resolution radio surveys such as FIRST. Our observations support a scenario where compact radio jets, with modest radio luminosities, are a crucial feedback mechanism for massive galaxies during a quasar phase. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.07727v1-abstract-full').style.display = 'none'; document.getElementById('1902.07727v1-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, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS. Main manuscript is 22 pages with 12 figures. Supplementary material is available for download under "Ancillary files" or by downloading the source file listed under "Other formats"</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1901.03731">arXiv:1901.03731</a> <span> [<a href="https://arxiv.org/pdf/1901.03731">pdf</a>, <a href="https://arxiv.org/format/1901.03731">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/10.1038/s41550-018-0661-3">10.1038/s41550-018-0661-3 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A new class of flares from accreting supermassive black holes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Trakhtenbrot%2C+B">Benny Trakhtenbrot</a>, <a href="/search/?searchtype=author&query=Arcavi%2C+I">Iair Arcavi</a>, <a href="/search/?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/?searchtype=author&query=Tacchella%2C+S">Sandro Tacchella</a>, <a href="/search/?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/?searchtype=author&query=Netzer%2C+H">Hagai Netzer</a>, <a href="/search/?searchtype=author&query=Jonker%2C+P+G">Peter G. Jonker</a>, <a href="/search/?searchtype=author&query=Horesh%2C+A">Assaf Horesh</a>, <a href="/search/?searchtype=author&query=Mej%C3%ADa-Restrepo%2C+J+E">Juli谩n Esteban Mej铆a-Restrepo</a>, <a href="/search/?searchtype=author&query=Hosseinzadeh%2C+G">Griffin Hosseinzadeh</a>, <a href="/search/?searchtype=author&query=Hallefors%2C+V">Valentina Hallefors</a>, <a href="/search/?searchtype=author&query=Howell%2C+D+A">D. Andrew Howell</a>, <a href="/search/?searchtype=author&query=McCully%2C+C">Curtis McCully</a>, <a href="/search/?searchtype=author&query=Balokovi%C4%87%2C+M">Mislav Balokovi膰</a>, <a href="/search/?searchtype=author&query=Heida%2C+M">Marianne Heida</a>, <a href="/search/?searchtype=author&query=Kamraj%2C+N">Nikita Kamraj</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">George Benjamin Lansbury</a>, <a href="/search/?searchtype=author&query=Wyrzykowski%2C+%C5%81">艁ukasz Wyrzykowski</a>, <a href="/search/?searchtype=author&query=Gromadzki%2C+M">Mariusz Gromadzki</a>, <a href="/search/?searchtype=author&query=Hamanowicz%2C+A">Aleksandra Hamanowicz</a>, <a href="/search/?searchtype=author&query=Cenko%2C+S+B">S. Bradley Cenko</a>, <a href="/search/?searchtype=author&query=Sand%2C+D+J">David J. Sand</a>, <a href="/search/?searchtype=author&query=Hsiao%2C+E+Y">Eric Y. Hsiao</a>, <a href="/search/?searchtype=author&query=Phillips%2C+M+M">Mark M. Phillips</a>, <a href="/search/?searchtype=author&query=Diamond%2C+T+R">Tiara R. Diamond</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="1901.03731v1-abstract-short" style="display: inline;"> Accreting supermassive black holes (SMBHs) can exhibit variable emission across the electromagnetic spectrum and over a broad range of timescales. The variability of active galactic nuclei (AGNs) in the ultraviolet and optical is usually at the few tens of per cent level over timescales of hours to weeks. Recently, rare, more dramatic changes to the emission from accreting SMBHs have been observed… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.03731v1-abstract-full').style.display = 'inline'; document.getElementById('1901.03731v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1901.03731v1-abstract-full" style="display: none;"> Accreting supermassive black holes (SMBHs) can exhibit variable emission across the electromagnetic spectrum and over a broad range of timescales. The variability of active galactic nuclei (AGNs) in the ultraviolet and optical is usually at the few tens of per cent level over timescales of hours to weeks. Recently, rare, more dramatic changes to the emission from accreting SMBHs have been observed, including tidal disruption events, 'changing look' AGNs and other extreme variability objects. The physics behind the 're-ignition', enhancement and 'shut-down' of accretion onto SMBHs is not entirely understood. Here we present a rapid increase in ultraviolet-optical emission in the centre of a nearby galaxy, marking the onset of sudden increased accretion onto a SMBH. The optical spectrum of this flare, dubbed AT 2017bgt, exhibits a mix of emission features. Some are typical of luminous, unobscured AGNs, but others are likely driven by Bowen fluorescence - robustly linked here with high-velocity gas in the vicinity of the accreting SMBH. The spectral features and increased ultraviolet flux show little evolution over a period of at least 14 months. This disfavours the tidal disruption of a star as their origin, and instead suggests a longer-term event of intensified accretion. Together with two other recently reported events with similar properties, we define a new class of SMBH-related flares. This has important implications for the classification of different types of enhanced accretion onto SMBHs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.03731v1-abstract-full').style.display = 'none'; document.getElementById('1901.03731v1-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, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published in Nature Astronomy</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1811.05492">arXiv:1811.05492</a> <span> [<a href="https://arxiv.org/pdf/1811.05492">pdf</a>, <a href="https://arxiv.org/ps/1811.05492">ps</a>, <a href="https://arxiv.org/format/1811.05492">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/aaf007">10.3847/1538-4357/aaf007 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Chandra Observations of NuSTAR Serendipitous Sources near the Galactic Plane </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Tomsick%2C+J+A">John A. Tomsick</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">George B. Lansbury</a>, <a href="/search/?searchtype=author&query=Rahoui%2C+F">Farid Rahoui</a>, <a href="/search/?searchtype=author&query=Aird%2C+J">James Aird</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">David M. Alexander</a>, <a href="/search/?searchtype=author&query=Clavel%2C+M">Maica Clavel</a>, <a href="/search/?searchtype=author&query=Cuturilo%2C+A">AnaSofija Cuturilo</a>, <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</a>, <a href="/search/?searchtype=author&query=Hong%2C+J">JaeSub Hong</a>, <a href="/search/?searchtype=author&query=Klindt%2C+L">Lizelke Klindt</a>, <a href="/search/?searchtype=author&query=Stern%2C+D">Daniel Stern</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="1811.05492v1-abstract-short" style="display: inline;"> The NuSTAR serendipitous survey has already uncovered a large number of Active Galactic Nuclei (AGN), providing new information about the composition of the Cosmic X-ray Background. For the AGN off the Galactic plane, it has been possible to use the existing X-ray archival data to improve source localizations, identify optical counterparts, and classify the AGN with optical spectroscopy. However,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.05492v1-abstract-full').style.display = 'inline'; document.getElementById('1811.05492v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1811.05492v1-abstract-full" style="display: none;"> The NuSTAR serendipitous survey has already uncovered a large number of Active Galactic Nuclei (AGN), providing new information about the composition of the Cosmic X-ray Background. For the AGN off the Galactic plane, it has been possible to use the existing X-ray archival data to improve source localizations, identify optical counterparts, and classify the AGN with optical spectroscopy. However, near the Galactic Plane, better X-ray positions are necessary to achieve optical or near-IR identifications due to the higher levels of source crowding. Thus, we have used observations with the Chandra X-ray Observatory to obtain the best possible X-ray positions. With eight observations, we have obtained coverage for 19 NuSTAR serendips within 12 deg of the plane. One or two Chandra sources are detected within the error circle of 15 of the serendips, and we report on these sources and search for optical counterparts. For one source (NuSTAR J202421+3350.9), we obtained a new optical spectrum and detected the presence of hydrogen emission lines. The source is Galactic, and we argue that it is likely a Cataclysmic Variable. For the other sources, the Chandra positions will enable future classifications in order to place limits on faint Galactic populations, including high-mass X-ray binaries and magnetars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.05492v1-abstract-full').style.display = 'none'; document.getElementById('1811.05492v1-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, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2018. </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, 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/1803.00009">arXiv:1803.00009</a> <span> [<a href="https://arxiv.org/pdf/1803.00009">pdf</a>, <a href="https://arxiv.org/format/1803.00009">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/aab357">10.3847/2041-8213/aab357 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Storm in a Teacup: X-ray view of an obscured quasar and superbubble </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">G. B. Lansbury</a>, <a href="/search/?searchtype=author&query=Jarvis%2C+M+E">M. E. Jarvis</a>, <a href="/search/?searchtype=author&query=Harrison%2C+C+M">C. M. Harrison</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Del+Moro%2C+A">A. Del Moro</a>, <a href="/search/?searchtype=author&query=Edge%2C+A+C">A. C. Edge</a>, <a href="/search/?searchtype=author&query=Mullaney%2C+J+R">J. R. Mullaney</a>, <a href="/search/?searchtype=author&query=Thomson%2C+A">A. Thomson</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="1803.00009v2-abstract-short" style="display: inline;"> We present the X-ray properties of the 'Teacup AGN' (SDSS J1430+1339), a $z=0.085$ type 2 quasar which is interacting dramatically with its host galaxy. Spectral modelling of the central quasar reveals a powerful, highly obscured AGN with a column density of $N_{\rm H}=(4.2$-$6.5)\times 10^{23}$ cm$^{-2}$ and an intrinsic luminosity of $L_{\rm 2\mbox{-}10\,keV}=(0.8$-$1.4)\times 10^{44}$ erg s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.00009v2-abstract-full').style.display = 'inline'; document.getElementById('1803.00009v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1803.00009v2-abstract-full" style="display: none;"> We present the X-ray properties of the 'Teacup AGN' (SDSS J1430+1339), a $z=0.085$ type 2 quasar which is interacting dramatically with its host galaxy. Spectral modelling of the central quasar reveals a powerful, highly obscured AGN with a column density of $N_{\rm H}=(4.2$-$6.5)\times 10^{23}$ cm$^{-2}$ and an intrinsic luminosity of $L_{\rm 2\mbox{-}10\,keV}=(0.8$-$1.4)\times 10^{44}$ erg s$^{-1}$. The current high bolometric luminosity inferred ($L_{\rm bol}\approx 10^{45}$-$10^{46}$ erg s$^{-1}$) has ramifications for previous interpretations of the Teacup as a fading/dying quasar. High resolution Chandra imaging data reveal a $\approx 10$ kpc loop of X-ray emission, co-spatial with the 'eastern bubble' previously identified in luminous radio and ionised gas (e.g., [OIII] line) emission. The X-ray emission from this structure is in good agreement with a shocked thermal gas, with $T=(4$-$8)\times 10^{6}$ K, and there is evidence for an additional hot component with $T\gtrsim 3\times 10^{7}$ K. Although the Teacup is a radiatively dominated AGN, the estimated ratio between the bubble power and the X-ray luminosity is in remarkable agreement with observations of ellipticals, groups, and clusters of galaxies undergoing AGN feedback. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.00009v2-abstract-full').style.display = 'none'; document.getElementById('1803.00009v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 March, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 February, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 4 figures, 1 table; Accepted for publication in ApJL</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1802.04272">arXiv:1802.04272</a> <span> [<a href="https://arxiv.org/pdf/1802.04272">pdf</a>, <a href="https://arxiv.org/format/1802.04272">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/aab040">10.3847/1538-4357/aab040 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> High redshift extremely red quasars in X-rays </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Goulding%2C+A+D">Andy D. Goulding</a>, <a href="/search/?searchtype=author&query=Zakamska%2C+N+L">Nadia L. Zakamska</a>, <a href="/search/?searchtype=author&query=Alexandroff%2C+R+M">Rachael M. Alexandroff</a>, <a href="/search/?searchtype=author&query=Assef%2C+R+J">Roberto J. Assef</a>, <a href="/search/?searchtype=author&query=Banerji%2C+M">Manda Banerji</a>, <a href="/search/?searchtype=author&query=Hamann%2C+F">Fred Hamann</a>, <a href="/search/?searchtype=author&query=Wylezalek%2C+D">Dominika Wylezalek</a>, <a href="/search/?searchtype=author&query=Brandt%2C+W+N">William N. Brandt</a>, <a href="/search/?searchtype=author&query=Greene%2C+J+E">Jenny E. Greene</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">George B. Lansbury</a>, <a href="/search/?searchtype=author&query=Paris%2C+I">Isabelle Paris</a>, <a href="/search/?searchtype=author&query=Richards%2C+G">Gordon Richards</a>, <a href="/search/?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/?searchtype=author&query=Strauss%2C+M+A">Michael A. Strauss</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="1802.04272v1-abstract-short" style="display: inline;"> Quasars may have played a key role in limiting the stellar mass of massive galaxies. Identifying those quasars in the process of removing star formation fuel from their hosts is an exciting ongoing challenge in extragalactic astronomy. In this paper we present X-ray observations of eleven extremely red quasars (ERQs) with $L_{\rm bol}\sim 10^{47}$ erg s$^{-1}$ at $z=1.5-3.2$ with evidence for high… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.04272v1-abstract-full').style.display = 'inline'; document.getElementById('1802.04272v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1802.04272v1-abstract-full" style="display: none;"> Quasars may have played a key role in limiting the stellar mass of massive galaxies. Identifying those quasars in the process of removing star formation fuel from their hosts is an exciting ongoing challenge in extragalactic astronomy. In this paper we present X-ray observations of eleven extremely red quasars (ERQs) with $L_{\rm bol}\sim 10^{47}$ erg s$^{-1}$ at $z=1.5-3.2$ with evidence for high-velocity ($v > 1000$ km s$^{-1}$) [OIII]$位$5007脜 outflows. X-rays allow us to directly probe circumnuclear obscuration and to measure the instantaneous accretion luminosity. We detect ten out of eleven extremely red quasars available in targeted and archival data. Using a combination of X-ray spectral fitting and hardness ratios, we find that all of the ERQs show signs of absorption in the X-rays with inferred column densities of $N_{\rm H}\approx 10^{23}$ cm$^{-2}$, including four Compton-thick candidates ($N_{\rm H} > 10^{24}$ cm$^{-2}$). We stack the X-ray emission of the seven weakly detected sources, measuring an average column density of $N_{\rm H}\sim 8\times 10^{23}$ cm$^{-2}$. The absorption-corrected (intrinsic) $2-10$ keV X-ray luminosity of the stack is $2.7\times 10^{45}$ erg s$^{-1}$, consistent with X-ray luminosities of type 1 quasars of the same infrared luminosity. Thus, we find that ERQs are a highly obscured, borderline Compton-thick population, and based on optical and infrared data we suggest that these objects are partially hidden by their own equatorial outflows. However, unlike some quasars with known outflows, ERQs do not appear to be intrinsically underluminous in X-rays for their bolometric luminosity. Our observations indicate that low X-rays are not necessary to enable some types of radiatively driven winds. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.04272v1-abstract-full').style.display = 'none'; document.getElementById('1802.04272v1-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 February, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 6 figures, 2 tables. Re-submitted to ApJ following referee's comments</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1801.04280">arXiv:1801.04280</a> <span> [<a href="https://arxiv.org/pdf/1801.04280">pdf</a>, <a href="https://arxiv.org/ps/1801.04280">ps</a>, <a href="https://arxiv.org/format/1801.04280">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/aaa550">10.3847/1538-4357/aaa550 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The NuSTAR Extragalactic Surveys: X-ray spectroscopic analysis of the bright hard-band selected sample </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Zappacosta%2C+L">L. Zappacosta</a>, <a href="/search/?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/?searchtype=author&query=Civano%2C+F">F. Civano</a>, <a href="/search/?searchtype=author&query=Puccetti%2C+S">S. Puccetti</a>, <a href="/search/?searchtype=author&query=Fiore%2C+F">F. Fiore</a>, <a href="/search/?searchtype=author&query=Aird%2C+J">J. Aird</a>, <a href="/search/?searchtype=author&query=Del+Moro%2C+A">A. Del Moro</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">G. B. Lansbury</a>, <a href="/search/?searchtype=author&query=Lanzuisi%2C+G">G. Lanzuisi</a>, <a href="/search/?searchtype=author&query=Goulding%2C+A">A. Goulding</a>, <a href="/search/?searchtype=author&query=Mullaney%2C+J+R">J. R. Mullaney</a>, <a href="/search/?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/?searchtype=author&query=Ajello%2C+M">M. Ajello</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Ballantyne%2C+D+R">D. R. Ballantyne</a>, <a href="/search/?searchtype=author&query=Bauer%2C+F+E">F. E. Bauer</a>, <a href="/search/?searchtype=author&query=Brandt%2C+W+N">W. N. Brandt</a>, <a href="/search/?searchtype=author&query=Chen%2C+C+-+J">C. -T. J. Chen</a>, <a href="/search/?searchtype=author&query=Farrah%2C+D">D. Farrah</a>, <a href="/search/?searchtype=author&query=Harrison%2C+F+A">F. A. Harrison</a>, <a href="/search/?searchtype=author&query=Gandhi%2C+P">P. Gandhi</a>, <a href="/search/?searchtype=author&query=Lanz%2C+L">L. Lanz</a>, <a href="/search/?searchtype=author&query=Masini%2C+A">A. Masini</a>, <a href="/search/?searchtype=author&query=Marchesi%2C+S">S. Marchesi</a>, <a href="/search/?searchtype=author&query=Ricci%2C+C">C. Ricci</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="1801.04280v1-abstract-short" style="display: inline;"> We discuss the spectral analysis of a sample of 63 Active Galactic Nuclei (AGN) detected above a limiting flux of $S(8-24$ keV$)=7\times10^{-14}$ erg/s/cm$^2$ in the multi-tiered NuSTAR Extragalactic Survey program. The sources span a redshift range z=0-2.1 (median $\langle$z$\rangle=$0.58). The spectral analysis is performed over the broad 0.5-24 keV energy range, combining NuSTAR with Chandra an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.04280v1-abstract-full').style.display = 'inline'; document.getElementById('1801.04280v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1801.04280v1-abstract-full" style="display: none;"> We discuss the spectral analysis of a sample of 63 Active Galactic Nuclei (AGN) detected above a limiting flux of $S(8-24$ keV$)=7\times10^{-14}$ erg/s/cm$^2$ in the multi-tiered NuSTAR Extragalactic Survey program. The sources span a redshift range z=0-2.1 (median $\langle$z$\rangle=$0.58). The spectral analysis is performed over the broad 0.5-24 keV energy range, combining NuSTAR with Chandra and/or XMM-Newton data and employing empirical and physically motivated models. This constitutes the largest sample of AGN selected at $ >10$ keV to be homogeneously spectrally analyzed at these flux levels. We study the distribution of spectral parameters such as photon index, column density ($N_{\rm H}$), reflection parameter ($R$) and 10-40 keV luminosity ($L_{X}$). Heavily obscured ($\log [N_{\rm H}/cm^{-2}]\ge23$) and Compton Thick (CT; $\log [N_{\rm H}/cm^{-2}]\ge24$) AGN constitute $\sim$25% (15-17 sources) and $\sim$2-3% ( 1-2 sources) of the sample, respectively. The observed $N_{\rm H}$ distribution fairly agrees with predictions of Cosmic X-ray Background population synthesis models (CXBPSM). We estimate the intrinsic fraction of AGN as a function of $N_{H}$, accounting for the bias against obscured AGN in a flux-selected sample. The fraction of CT AGN relative to $\log [N_{\rm H}/cm^{-2}]=20-24$ AGN is poorly constrainted, formally in the range 2-56% (90% upper limit of 66%). We derived a fraction ($f_{abs}$) of obscured AGN ($\log [N_{\rm H}/cm^{-2}]=22-24$) as a function of $L_{X}$ in agreement with CXBPSM and previous z < 1 X-ray determinations. Furthermore $f_{abs}$ at z=0.1-0.5 and $\log (L_{X}/erg$ $s^{-1})\approx43.6-44.3$ agrees with observational measurements/trends obtained over larger redshift intervals. We report a significant anti-correlation of $R$ with $L_{X}$ (confirmed by our companion paper on stacked spectra) with considerable scatter around the median $R$ values. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.04280v1-abstract-full').style.display = 'none'; document.getElementById('1801.04280v1-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 January, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2018. </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">Comments: 38 pages, 17 figures, 8 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/1801.01881">arXiv:1801.01881</a> <span> [<a href="https://arxiv.org/pdf/1801.01881">pdf</a>, <a href="https://arxiv.org/format/1801.01881">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/aaa83d">10.3847/1538-4365/aaa83d <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The NuSTAR Extragalactic Surveys: source catalog and the Compton-thick fraction in the UDS field </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Masini%2C+A">A. Masini</a>, <a href="/search/?searchtype=author&query=Civano%2C+F">F. Civano</a>, <a href="/search/?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/?searchtype=author&query=Fornasini%2C+F">F. Fornasini</a>, <a href="/search/?searchtype=author&query=Ballantyne%2C+D+R">D. R. Ballantyne</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">G. B. Lansbury</a>, <a href="/search/?searchtype=author&query=Treister%2C+E">E. Treister</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Boorman%2C+P+G">P. G. Boorman</a>, <a href="/search/?searchtype=author&query=Brandt%2C+W+N">W. N. Brandt</a>, <a href="/search/?searchtype=author&query=Farrah%2C+D">D. Farrah</a>, <a href="/search/?searchtype=author&query=Gandhi%2C+P">P. Gandhi</a>, <a href="/search/?searchtype=author&query=Harrison%2C+F+A">F. A. Harrison</a>, <a href="/search/?searchtype=author&query=Hickox%2C+R+C">R. C. Hickox</a>, <a href="/search/?searchtype=author&query=Kocevski%2C+D+D">D. D. Kocevski</a>, <a href="/search/?searchtype=author&query=Lanz%2C+L">L. Lanz</a>, <a href="/search/?searchtype=author&query=Marchesi%2C+S">S. Marchesi</a>, <a href="/search/?searchtype=author&query=Puccetti%2C+S">S. Puccetti</a>, <a href="/search/?searchtype=author&query=Ricci%2C+C">C. Ricci</a>, <a href="/search/?searchtype=author&query=Saez%2C+C">C. Saez</a>, <a href="/search/?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/?searchtype=author&query=Zappacosta%2C+L">L. Zappacosta</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="1801.01881v1-abstract-short" style="display: inline;"> We present the results and the source catalog of the NuSTAR survey in the UKIDSS Ultra Deep Survey (UDS) field, bridging the gap in depth and area between NuSTAR's ECDFS and COSMOS surveys. The survey covers a $\sim 0.6$ deg$^2$ area of the field for a total observing time of $\sim$ 1.75 Ms, to a half-area depth of $\sim$ 155 ks corrected for vignetting at $3-24$ keV, and reaching sensitivity limi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.01881v1-abstract-full').style.display = 'inline'; document.getElementById('1801.01881v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1801.01881v1-abstract-full" style="display: none;"> We present the results and the source catalog of the NuSTAR survey in the UKIDSS Ultra Deep Survey (UDS) field, bridging the gap in depth and area between NuSTAR's ECDFS and COSMOS surveys. The survey covers a $\sim 0.6$ deg$^2$ area of the field for a total observing time of $\sim$ 1.75 Ms, to a half-area depth of $\sim$ 155 ks corrected for vignetting at $3-24$ keV, and reaching sensitivity limits at half-area in the full ($3-24$ keV), soft ($3-8$ keV) and hard ($8-24$ keV) bands of $2.2 \times 10^{-14}$ erg cm$^{-2}$ s$^{-1}$, $1.0 \times 10^{-14}$ erg cm$^{-2}$ s$^{-1}$, and $2.7 \times 10^{-14}$ erg cm$^{-2}$ s$^{-1}$, respectively. A total of 67 sources are detected in at least one of the three bands, 56 of which have a robust optical redshift with a median of $\langle z\rangle \sim 1.1$. Through a broadband ($0.5-24$ keV) spectral analysis of the whole sample combined with the NuSTAR hardness ratios, we compute the observed Compton-thick (CT; $N_{\rm H} > 10^{24}$ cm$^{-2}$) fraction. Taking into account the uncertainties on each $N_{\rm H}$ measurement, the final number of CT sources is $6.8\pm1.2$. This corresponds to an observed CT fraction of $(11.5\pm2.0)\%$, providing a robust lower limit to the intrinsic fraction of CT AGN and placing constraints on cosmic X-ray background synthesis models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.01881v1-abstract-full').style.display = 'none'; document.getElementById('1801.01881v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 January, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2018. </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, accepted for publication in The Astrophysical Journal Supplement Series</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1710.01041">arXiv:1710.01041</a> <span> [<a href="https://arxiv.org/pdf/1710.01041">pdf</a>, <a href="https://arxiv.org/format/1710.01041">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/aa9115">10.3847/1538-4357/aa9115 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The NuSTAR Extragalactic Survey: Average broad-band X-ray spectral properties of the NuSTAR detected AGN </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Del+Moro%2C+A">A. Del Moro</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Aird%2C+J+A">J. A. Aird</a>, <a href="/search/?searchtype=author&query=Bauer%2C+F+E">F. E. Bauer</a>, <a href="/search/?searchtype=author&query=Civano%2C+F">F. Civano</a>, <a href="/search/?searchtype=author&query=Mullaney%2C+J+R">J. R. Mullaney</a>, <a href="/search/?searchtype=author&query=Ballantyne%2C+D+R">D. R. Ballantyne</a>, <a href="/search/?searchtype=author&query=Brandt%2C+W+N">W. N. Brandt</a>, <a href="/search/?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/?searchtype=author&query=Gandhi%2C+P">P. Gandhi</a>, <a href="/search/?searchtype=author&query=Harrison%2C+F+A">F. A. Harrison</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">G. B. Lansbury</a>, <a href="/search/?searchtype=author&query=Lanz%2C+L">L. Lanz</a>, <a href="/search/?searchtype=author&query=Luo%2C+B">B. Luo</a>, <a href="/search/?searchtype=author&query=Marchesi%2C+S">S. Marchesi</a>, <a href="/search/?searchtype=author&query=Puccetti%2C+S">S. Puccetti</a>, <a href="/search/?searchtype=author&query=Ricci%2C+C">C. Ricci</a>, <a href="/search/?searchtype=author&query=Saez%2C+C">C. Saez</a>, <a href="/search/?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/?searchtype=author&query=Treister%2C+E">E. Treister</a>, <a href="/search/?searchtype=author&query=Zappacosta%2C+L">L. Zappacosta</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="1710.01041v1-abstract-short" style="display: inline;"> We present a study of the average X-ray spectral properties of the sources detected by the NuSTAR extragalactic survey, comprising observations of the E-CDFS, EGS and COSMOS fields. The sample includes 182 NuSTAR sources (64 detected at 8-24 keV), with 3-24 keV fluxes ranging between $f_{\rm 3-24 keV}\approx10^{-14}$ and $6\times10^{-13}$ erg/cm$^2$/s (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.01041v1-abstract-full').style.display = 'inline'; document.getElementById('1710.01041v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1710.01041v1-abstract-full" style="display: none;"> We present a study of the average X-ray spectral properties of the sources detected by the NuSTAR extragalactic survey, comprising observations of the E-CDFS, EGS and COSMOS fields. The sample includes 182 NuSTAR sources (64 detected at 8-24 keV), with 3-24 keV fluxes ranging between $f_{\rm 3-24 keV}\approx10^{-14}$ and $6\times10^{-13}$ erg/cm$^2$/s ($f_{\rm 8-24 keV}\approx3\times10^{-14}-3\times10^{-13}$ erg/cm$^2$/s) and redshifts of $z=0.04-3.21$. We produce composite spectra from the Chandra+NuSTAR data ($E\approx2-40$ keV, rest frame) for all the sources with redshift identifications (95%) and investigate the intrinsic, average spectra of the sources, divided into broad-line (BL) and narrow-line (NL) AGN, and also in different bins of X-ray column density and luminosity. The average power-law photon index for the whole sample is $螕=1.65_{-0.03}^{+0.03}$, flatter than $螕\approx1.8$ typically found for AGN. While the spectral slope of BL and X-ray unabsorbed AGN is consistent with typical values ($螕=1.79_{-0.01}^{+0.01}$), a significant flattening is seen in NL AGN and heavily-absorbed sources ($螕=1.60_{-0.05}^{+0.08}$ and $螕=1.38_{-0.12}^{+0.12}$, respectively), likely due to the effect of absorption and to the contribution from Compton reflection to the high-energy flux (E>10 keV). We find that the typical reflection fraction in our spectra is $R\approx0.5$ (for $螕=1.8$), with a tentative indication of an increase of the reflection strength with column density. While there is no significant evidence for a dependence of the photon index with X-ray luminosity in our sample, we find that $R$ decreases with luminosity, with relatively high levels of reflection ($R\approx1.2$) for $L_{\rm 10-40 keV}<10^{44}$ erg/s and $R\approx0.3$ for $L_{\rm 10-40 keV}>10^{44}$ erg/s AGN, assuming $螕=1.8$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.01041v1-abstract-full').style.display = 'none'; document.getElementById('1710.01041v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 October, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2017. </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, 14 figures, 4 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/1707.06651">arXiv:1707.06651</a> <span> [<a href="https://arxiv.org/pdf/1707.06651">pdf</a>, <a href="https://arxiv.org/format/1707.06651">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/aa8176">10.3847/1538-4357/aa8176 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The NuSTAR Serendipitous Survey: Hunting for The Most Extreme Obscured AGN at >10 keV </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">G. B. Lansbury</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Aird%2C+J">J. Aird</a>, <a href="/search/?searchtype=author&query=Gandhi%2C+P">P. Gandhi</a>, <a href="/search/?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/?searchtype=author&query=Koss%2C+M">M. Koss</a>, <a href="/search/?searchtype=author&query=Lamperti%2C+I">I. Lamperti</a>, <a href="/search/?searchtype=author&query=Ajello%2C+M">M. Ajello</a>, <a href="/search/?searchtype=author&query=Annuar%2C+A">A. Annuar</a>, <a href="/search/?searchtype=author&query=Assef%2C+R+J">R. J. Assef</a>, <a href="/search/?searchtype=author&query=Ballantyne%2C+D+R">D. R. Ballantyne</a>, <a href="/search/?searchtype=author&query=Balokovic%2C+M">M. Balokovic</a>, <a href="/search/?searchtype=author&query=Bauer%2C+F+E">F. E. Bauer</a>, <a href="/search/?searchtype=author&query=Brandt%2C+N">N. Brandt</a>, <a href="/search/?searchtype=author&query=Brightman%2C+M">M. Brightman</a>, <a href="/search/?searchtype=author&query=Chen%2C+C+-+J">C. -T. J. Chen</a>, <a href="/search/?searchtype=author&query=Civano%2C+F">F. Civano</a>, <a href="/search/?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/?searchtype=author&query=Moro%2C+A+D">A. D. Moro</a>, <a href="/search/?searchtype=author&query=Fuentes%2C+C">C. Fuentes</a>, <a href="/search/?searchtype=author&query=Harrison%2C+F+A">F. A. Harrison</a>, <a href="/search/?searchtype=author&query=Marchesi%2C+S">S. Marchesi</a>, <a href="/search/?searchtype=author&query=Masini%2C+A">A. Masini</a>, <a href="/search/?searchtype=author&query=Mullaney%2C+J+R">J. R. Mullaney</a>, <a href="/search/?searchtype=author&query=Ricci%2C+C">C. Ricci</a> , et al. (5 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1707.06651v2-abstract-short" style="display: inline;"> We identify sources with extremely hard X-ray spectra (i.e., with photon indices of Gamma<0.6 in the 13 sq. deg. NuSTAR serendipitous survey, to search for the most highly obscured AGNs detected at >10 keV. Eight extreme NuSTAR sources are identified, and we use the NuSTAR data in combination with lower energy X-ray observations (from Chandra, Swift XRT, and XMM-Newton) to characterize the broad-b… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.06651v2-abstract-full').style.display = 'inline'; document.getElementById('1707.06651v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1707.06651v2-abstract-full" style="display: none;"> We identify sources with extremely hard X-ray spectra (i.e., with photon indices of Gamma<0.6 in the 13 sq. deg. NuSTAR serendipitous survey, to search for the most highly obscured AGNs detected at >10 keV. Eight extreme NuSTAR sources are identified, and we use the NuSTAR data in combination with lower energy X-ray observations (from Chandra, Swift XRT, and XMM-Newton) to characterize the broad-band (0.5-24 keV) X-ray spectra. We find that all of the extreme sources are highly obscured AGNs, including three robust Compton-thick (CT; N_H > 1.5e24 cm^-2) AGNs at low redshift (z<0.1), and a likely-CT AGN at higher redshift (z=0.16). Most of the extreme sources would not have been identified as highly obscured based on the low energy (<10 keV) X-ray coverage alone. The multiwavelength properties (e.g., optical spectra and X-ray/MIR luminosity ratios) provide further support for the eight sources being significantly obscured. Correcting for absorption, the intrinsic rest-frame 10-40 keV luminosities of the extreme sources cover a broad range, from ~ 5 x 10^42 to 10^45 erg s^-1. The estimated number counts of CT AGNs in the NuSTAR serendipitous survey are in broad agreement with model expectations based on previous X-ray surveys, except for the lowest redshifts (z<0.07) where we measure a high CT fraction of f_CT^obs = 30 (+16 -12) %. For the small sample of CT AGNs, we find a high fraction of galaxy major mergers (50 +/- 33%) compared to control samples of "normal" AGNs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.06651v2-abstract-full').style.display = 'none'; document.getElementById('1707.06651v2-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 August, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 July, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2017. </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, 15 figures, 5 tables; Accepted for publication in ApJ; Author list updated</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1705.08476">arXiv:1705.08476</a> <span> [<a href="https://arxiv.org/pdf/1705.08476">pdf</a>, <a href="https://arxiv.org/ps/1705.08476">ps</a>, <a href="https://arxiv.org/format/1705.08476">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/10.3847/1538-4365/aa7517">10.3847/1538-4365/aa7517 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galactic Sources Detected in the NuSTAR Serendipitous Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Tomsick%2C+J+A">John A. Tomsick</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">George B. Lansbury</a>, <a href="/search/?searchtype=author&query=Rahoui%2C+F">Farid Rahoui</a>, <a href="/search/?searchtype=author&query=Clavel%2C+M">Maica Clavel</a>, <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</a>, <a href="/search/?searchtype=author&query=Hong%2C+J">JaeSub Hong</a>, <a href="/search/?searchtype=author&query=Aird%2C+J">James Aird</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">David M. Alexander</a>, <a href="/search/?searchtype=author&query=Bodaghee%2C+A">Arash Bodaghee</a>, <a href="/search/?searchtype=author&query=Chiu%2C+J">Jeng-Lun Chiu</a>, <a href="/search/?searchtype=author&query=Grindlay%2C+J+E">Jonathan E. Grindlay</a>, <a href="/search/?searchtype=author&query=Hailey%2C+C+J">Charles J. Hailey</a>, <a href="/search/?searchtype=author&query=Harrison%2C+F+A">Fiona A. Harrison</a>, <a href="/search/?searchtype=author&query=Krivonos%2C+R+A">Roman A. Krivonos</a>, <a href="/search/?searchtype=author&query=Mori%2C+K">Kaya Mori</a>, <a href="/search/?searchtype=author&query=Stern%2C+D">Daniel Stern</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="1705.08476v1-abstract-short" style="display: inline;"> The Nuclear Spectroscopic Telescope Array (NuSTAR) provides an improvement in sensitivity at energies above 10 keV by two orders of magnitude over non-focusing satellites, making it possible to probe deeper into the Galaxy and Universe. Lansbury and collaborators recently completed a catalog of 497 sources serendipitously detected in the 3-24 keV band using 13 deg2 of NuSTAR coverage. Here, we rep… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1705.08476v1-abstract-full').style.display = 'inline'; document.getElementById('1705.08476v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1705.08476v1-abstract-full" style="display: none;"> The Nuclear Spectroscopic Telescope Array (NuSTAR) provides an improvement in sensitivity at energies above 10 keV by two orders of magnitude over non-focusing satellites, making it possible to probe deeper into the Galaxy and Universe. Lansbury and collaborators recently completed a catalog of 497 sources serendipitously detected in the 3-24 keV band using 13 deg2 of NuSTAR coverage. Here, we report on an optical and X-ray study of 16 Galactic sources in the catalog. We identify eight of them as stars (but some or all could have binary companions), and use information from Gaia to report distances and X-ray luminosities for three of them. There are four CVs or CV candidates, and we argue that NuSTAR J233426-2343.9 is a relatively strong CV candidate based partly on an X-ray spectrum from XMM-Newton. NuSTAR J092418-3142.2, which is the brightest serendipitous source in the Lansbury catalog, and NuSTAR J073959-3147.8 are LMXB candidates, but it is also possible that these two sources are CVs. One of the sources is a known HMXB, and NuSTAR J105008-5958.8 is a new HMXB candidate, which has strong Balmer emission lines in its optical spectrum and a hard X-ray spectrum. We discuss the implications of finding these HMXBs for the surface density (logN-logS) and luminosity function of Galactic HMXBs. We conclude that, with the large fraction of unclassified sources in the Galactic plane detected by NuSTAR in the 8-24 keV band, there could be a significant population of low luminosity HMXBs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1705.08476v1-abstract-full').style.display = 'none'; document.getElementById('1705.08476v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 May, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2017. </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, 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/1701.00497">arXiv:1701.00497</a> <span> [<a href="https://arxiv.org/pdf/1701.00497">pdf</a>, <a href="https://arxiv.org/ps/1701.00497">ps</a>, <a href="https://arxiv.org/format/1701.00497">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/10.3847/1538-4357/836/2/165">10.3847/1538-4357/836/2/165 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A New Compton-thick AGN in our Cosmic Backyard: Unveiling the Buried Nucleus in NGC 1448 with NuSTAR </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Annuar%2C+A">A. Annuar</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Gandhi%2C+P">P. Gandhi</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">G. B. Lansbury</a>, <a href="/search/?searchtype=author&query=Asmus%2C+D">D. Asmus</a>, <a href="/search/?searchtype=author&query=Ballantyne%2C+D+R">D. R. Ballantyne</a>, <a href="/search/?searchtype=author&query=Bauer%2C+F+E">F. E. Bauer</a>, <a href="/search/?searchtype=author&query=Boggs%2C+S+E">S. E. Boggs</a>, <a href="/search/?searchtype=author&query=Boorman%2C+P+G">P. G. Boorman</a>, <a href="/search/?searchtype=author&query=Brandt%2C+W+N">W. N. Brandt</a>, <a href="/search/?searchtype=author&query=Brightman%2C+M">M. Brightman</a>, <a href="/search/?searchtype=author&query=Christensen%2C+F+E">F. E. Christensen</a>, <a href="/search/?searchtype=author&query=Craig%2C+W+W">W. W. Craig</a>, <a href="/search/?searchtype=author&query=Farrah%2C+D">D. Farrah</a>, <a href="/search/?searchtype=author&query=Goulding%2C+A+D">A. D. Goulding</a>, <a href="/search/?searchtype=author&query=Hailey%2C+C+J">C. J. Hailey</a>, <a href="/search/?searchtype=author&query=Harrison%2C+F+A">F. A. Harrison</a>, <a href="/search/?searchtype=author&query=Koss%2C+M+J">M. J. Koss</a>, <a href="/search/?searchtype=author&query=LaMassa%2C+S+M">S. M. LaMassa</a>, <a href="/search/?searchtype=author&query=Murray%2C+S+S">S. S. Murray</a>, <a href="/search/?searchtype=author&query=Ricci%2C+C">C. Ricci</a>, <a href="/search/?searchtype=author&query=Rosario%2C+D+J">D. J. Rosario</a>, <a href="/search/?searchtype=author&query=Stanley%2C+F">F. Stanley</a>, <a href="/search/?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/?searchtype=author&query=Zhang%2C+W">W. Zhang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1701.00497v1-abstract-short" style="display: inline;"> NGC 1448 is one of the nearest luminous galaxies ($L_{8-1000渭m} >$ 10$^{9} L_{\odot}$) to ours ($z$ $=$ 0.00390), and yet the active galactic nucleus (AGN) it hosts was only recently discovered, in 2009. In this paper, we present an analysis of the nuclear source across three wavebands: mid-infrared (MIR) continuum, optical, and X-rays. We observed the source with the Nuclear Spectroscopic Telesco… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1701.00497v1-abstract-full').style.display = 'inline'; document.getElementById('1701.00497v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1701.00497v1-abstract-full" style="display: none;"> NGC 1448 is one of the nearest luminous galaxies ($L_{8-1000渭m} >$ 10$^{9} L_{\odot}$) to ours ($z$ $=$ 0.00390), and yet the active galactic nucleus (AGN) it hosts was only recently discovered, in 2009. In this paper, we present an analysis of the nuclear source across three wavebands: mid-infrared (MIR) continuum, optical, and X-rays. We observed the source with the Nuclear Spectroscopic Telescope Array (NuSTAR), and combined this data with archival Chandra data to perform broadband X-ray spectral fitting ($\approx$0.5-40 keV) of the AGN for the first time. Our X-ray spectral analysis reveals that the AGN is buried under a Compton-thick (CT) column of obscuring gas along our line-of-sight, with a column density of $N_{\rm H}$(los) $\gtrsim$ 2.5 $\times$ 10$^{24}$ cm$^{-2}$. The best-fitting torus models measured an intrinsic 2-10 keV luminosity of $L_{2-10\rm{,int}}$ $=$ (3.5-7.6) $\times$ 10$^{40}$ erg s$^{-1}$, making NGC 1448 one of the lowest luminosity CTAGNs known. In addition to the NuSTAR observation, we also performed optical spectroscopy for the nucleus in this edge-on galaxy using the European Southern Observatory New Technology Telescope. We re-classify the optical nuclear spectrum as a Seyfert on the basis of the Baldwin-Philips-Terlevich diagnostic diagrams, thus identifying the AGN at optical wavelengths for the first time. We also present high spatial resolution MIR observations of NGC 1448 with Gemini/T-ReCS, in which a compact nucleus is clearly detected. The absorption-corrected 2-10 keV luminosity measured from our X-ray spectral analysis agrees with that predicted from the optical [OIII]$位$5007脜 emission line and the MIR 12$渭$m continuum, further supporting the CT nature of the AGN. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1701.00497v1-abstract-full').style.display = 'none'; document.getElementById('1701.00497v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 January, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2017. </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 on Dec. 27th, 2016; 14 pages; 9 figures and 2 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/1612.06389">arXiv:1612.06389</a> <span> [<a href="https://arxiv.org/pdf/1612.06389">pdf</a>, <a href="https://arxiv.org/format/1612.06389">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/10.3847/1538-4357/836/1/99">10.3847/1538-4357/836/1/99 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The NuSTAR Serendipitous Survey: The 40 month Catalog and the Properties of the Distant High Energy X-ray Source Population </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">G. B. Lansbury</a>, <a href="/search/?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/?searchtype=author&query=Aird%2C+J">J. Aird</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Fuentes%2C+C">C. Fuentes</a>, <a href="/search/?searchtype=author&query=Harrison%2C+F+A">F. A. Harrison</a>, <a href="/search/?searchtype=author&query=Treister%2C+E">E. Treister</a>, <a href="/search/?searchtype=author&query=Bauer%2C+F+E">F. E. Bauer</a>, <a href="/search/?searchtype=author&query=Tomsick%2C+J+A">J. A. Tomsick</a>, <a href="/search/?searchtype=author&query=Balokovic%2C+M">M. Balokovic</a>, <a href="/search/?searchtype=author&query=Del+Moro%2C+A">A. Del Moro</a>, <a href="/search/?searchtype=author&query=Gandhi%2C+P">P. Gandhi</a>, <a href="/search/?searchtype=author&query=Ajello%2C+M">M. Ajello</a>, <a href="/search/?searchtype=author&query=Annuar%2C+A">A. Annuar</a>, <a href="/search/?searchtype=author&query=Ballantyne%2C+D+R">D. R. Ballantyne</a>, <a href="/search/?searchtype=author&query=Boggs%2C+S+E">S. E. Boggs</a>, <a href="/search/?searchtype=author&query=Brandt%2C+N">N. Brandt</a>, <a href="/search/?searchtype=author&query=Brightman%2C+M">M. Brightman</a>, <a href="/search/?searchtype=author&query=Chen%2C+C+J">C. J. Chen</a>, <a href="/search/?searchtype=author&query=Christensen%2C+F+E">F. E. Christensen</a>, <a href="/search/?searchtype=author&query=Civano%2C+F">F. Civano</a>, <a href="/search/?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/?searchtype=author&query=Craig%2C+W+W">W. W. Craig</a>, <a href="/search/?searchtype=author&query=Forster%2C+K">K. Forster</a>, <a href="/search/?searchtype=author&query=Grefenstette%2C+B+W">B. W. Grefenstette</a> , et al. (13 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1612.06389v1-abstract-short" style="display: inline;"> We present the first full catalog and science results for the NuSTAR serendipitous survey. The catalog incorporates data taken during the first 40 months of NuSTAR operation, which provide ~20Ms of effective exposure time over 331 fields, with an areal coverage of 13 sq deg, and 497 sources detected in total over the 3-24 keV energy range. There are 276 sources with spectroscopic redshifts and cla… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1612.06389v1-abstract-full').style.display = 'inline'; document.getElementById('1612.06389v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1612.06389v1-abstract-full" style="display: none;"> We present the first full catalog and science results for the NuSTAR serendipitous survey. The catalog incorporates data taken during the first 40 months of NuSTAR operation, which provide ~20Ms of effective exposure time over 331 fields, with an areal coverage of 13 sq deg, and 497 sources detected in total over the 3-24 keV energy range. There are 276 sources with spectroscopic redshifts and classifications, largely resulting from our extensive campaign of ground-based spectroscopic followup. We characterize the overall sample in terms of the X-ray, optical, and infrared source properties. The sample is primarily comprised of active galactic nuclei (AGNs), detected over a large range in redshift from z = 0.002 - 3.4 (median of <z> = 0.56), but also includes 16 spectroscopically confirmed Galactic sources. There is a large range in X-ray flux, from log( f_3-24keV / erg s^-1 cm^-2 ) ~ -14 to -11, and in rest-frame 10-40 keV luminosity, from log( L_10-40keV / erg s^-1 ) ~ 39 to 46, with a median of 44.1. Approximately 79% of the NuSTAR sources have lower energy (<10 keV) X-ray counterparts from XMM-Newton, Chandra, and Swift/XRT. The mid-infrared (MIR) analysis, using WISE all-sky survey data, shows that MIR AGN color selections miss a large fraction of the NuSTAR-selected AGN population, from ~15% at the highest luminosities (Lx > 10^44 erg s^-1) to ~80% at the lowest luminosities (Lx < 10^43 erg s^-1). Our optical spectroscopic analysis finds that the observed fraction of optically obscured AGNs (i.e., the Type 2 fraction) is F_Type2 = 53(+14-15)%, for a well-defined subset of the 8-24 keV selected sample. This is higher, albeit at a low significance level, than the Type 2 fraction measured for redshift- and luminosity-matched AGNs selected by <10 keV X-ray missions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1612.06389v1-abstract-full').style.display = 'none'; document.getElementById('1612.06389v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 December, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2016. </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, 23 figures, 8 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/1609.04808">arXiv:1609.04808</a> <span> [<a href="https://arxiv.org/pdf/1609.04808">pdf</a>, <a href="https://arxiv.org/ps/1609.04808">ps</a>, <a href="https://arxiv.org/format/1609.04808">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> <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/10.3847/1538-4357/835/1/105">10.3847/1538-4357/835/1/105 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> NuSTAR observations of WISE J1036+0449, a Galaxy at z$\sim1$ obscured by hot dust </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Ricci%2C+C">C. Ricci</a>, <a href="/search/?searchtype=author&query=Assef%2C+R+J">R. J. Assef</a>, <a href="/search/?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/?searchtype=author&query=Nikutta%2C+R">R. Nikutta</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Asmus%2C+D">D. Asmus</a>, <a href="/search/?searchtype=author&query=Ballantyne%2C+D+R">D. R. Ballantyne</a>, <a href="/search/?searchtype=author&query=Bauer%2C+F+E">F. E. Bauer</a>, <a href="/search/?searchtype=author&query=Blain%2C+A+W">A. W. Blain</a>, <a href="/search/?searchtype=author&query=Boggs%2C+S">S. Boggs</a>, <a href="/search/?searchtype=author&query=Boorman%2C+P+G">P. G. Boorman</a>, <a href="/search/?searchtype=author&query=Brandt%2C+W+N">W. N. Brandt</a>, <a href="/search/?searchtype=author&query=Brightman%2C+M">M. Brightman</a>, <a href="/search/?searchtype=author&query=Chang%2C+C+S">C. S. Chang</a>, <a href="/search/?searchtype=author&query=Chen%2C+C+-+J">C. -T. J. Chen</a>, <a href="/search/?searchtype=author&query=Christensen%2C+F+E">F. E. Christensen</a>, <a href="/search/?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/?searchtype=author&query=Craig%2C+W+W">W. W. Craig</a>, <a href="/search/?searchtype=author&query=D%C3%ADaz-Santos%2C+T">T. D铆az-Santos</a>, <a href="/search/?searchtype=author&query=Eisenhardt%2C+P+R">P. R. Eisenhardt</a>, <a href="/search/?searchtype=author&query=Farrah%2C+D">D. Farrah</a>, <a href="/search/?searchtype=author&query=Gandhi%2C+P">P. Gandhi</a>, <a href="/search/?searchtype=author&query=Hailey%2C+C+J">C. J. Hailey</a>, <a href="/search/?searchtype=author&query=Harrison%2C+F+A">F. A. Harrison</a>, <a href="/search/?searchtype=author&query=Jun%2C+H+D">H. D. Jun</a> , et al. (12 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1609.04808v2-abstract-short" style="display: inline;"> Hot, Dust-Obscured Galaxies (Hot DOGs), selected from the WISE all sky infrared survey, host some of the most powerful Active Galactic Nuclei (AGN) known, and might represent an important stage in the evolution of galaxies. Most known Hot DOGs are at $z> 1.5$, due in part to a strong bias against identifying them at lower redshift related to the selection criteria. We present a new selection metho… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.04808v2-abstract-full').style.display = 'inline'; document.getElementById('1609.04808v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1609.04808v2-abstract-full" style="display: none;"> Hot, Dust-Obscured Galaxies (Hot DOGs), selected from the WISE all sky infrared survey, host some of the most powerful Active Galactic Nuclei (AGN) known, and might represent an important stage in the evolution of galaxies. Most known Hot DOGs are at $z> 1.5$, due in part to a strong bias against identifying them at lower redshift related to the selection criteria. We present a new selection method that identifies 153 Hot DOG candidates at $z\sim 1$, where they are significantly brighter and easier to study. We validate this approach by measuring a redshift $z=1.009$, and an SED similar to higher redshift Hot DOGs for one of these objects, WISE J1036+0449 ($L_{\rm\,Bol}\simeq 8\times 10^{46}\rm\,erg\,s^{-1}$), using data from Keck/LRIS and NIRSPEC, SDSS, and CSO. We find evidence of a broadened component in MgII, which, if due to the gravitational potential of the supermassive black hole, would imply a black hole mass of $M_{\rm\,BH}\simeq 2 \times 10^8 M_{\odot}$, and an Eddington ratio of $位_{\rm\,Edd}\simeq 2.7$. WISE J1036+0449 is the first Hot DOG detected by NuSTAR, and the observations show that the source is heavily obscured, with a column density of $N_{\rm\,H}\simeq(2-15)\times10^{23}\rm\,cm^{-2}$. The source has an intrinsic 2-10 keV luminosity of $\sim 6\times 10^{44}\rm\,erg\,s^{-1}$, a value significantly lower than that expected from the mid-infrared/X-ray correlation. We also find that the other Hot DOGs observed by X-ray facilities show a similar deficiency of X-ray flux. We discuss the origin of the X-ray weakness and the absorption properties of Hot DOGs. Hot DOGs at $z\lesssim1$ could be excellent laboratories to probe the characteristics of the accretion flow and of the X-ray emitting plasma at extreme values of the Eddington ratio. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.04808v2-abstract-full').style.display = 'none'; document.getElementById('1609.04808v2-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 November, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 September, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2016. </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, 16 pages</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1606.05649">arXiv:1606.05649</a> <span> [<a href="https://arxiv.org/pdf/1606.05649">pdf</a>, <a href="https://arxiv.org/ps/1606.05649">ps</a>, <a href="https://arxiv.org/format/1606.05649">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/10.3847/0004-637X/831/1/76">10.3847/0004-637X/831/1/76 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Geometry of the Infrared and X-ray Obscurer in a Dusty Hyperluminous Quasar </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Farrah%2C+D">Duncan Farrah</a>, <a href="/search/?searchtype=author&query=Balokovic%2C+M">Mislav Balokovic</a>, <a href="/search/?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/?searchtype=author&query=Harris%2C+K">Kathryn Harris</a>, <a href="/search/?searchtype=author&query=Kunimoto%2C+M">Michelle Kunimoto</a>, <a href="/search/?searchtype=author&query=Walton%2C+D+J">Dominic J. Walton</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">David M. Alexander</a>, <a href="/search/?searchtype=author&query=Arevalo%2C+P">Patricia Arevalo</a>, <a href="/search/?searchtype=author&query=Ballantyne%2C+D+R">David R. Ballantyne</a>, <a href="/search/?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/?searchtype=author&query=Boggs%2C+S">Steven Boggs</a>, <a href="/search/?searchtype=author&query=Brandt%2C+W+N">William N. Brandt</a>, <a href="/search/?searchtype=author&query=Brightman%2C+M">Murray Brightman</a>, <a href="/search/?searchtype=author&query=Christensen%2C+F">Finn Christensen</a>, <a href="/search/?searchtype=author&query=Clements%2C+D+L">David L. Clements</a>, <a href="/search/?searchtype=author&query=Craig%2C+W">William Craig</a>, <a href="/search/?searchtype=author&query=Fabian%2C+A">Andrew Fabian</a>, <a href="/search/?searchtype=author&query=Hailey%2C+C">Charles Hailey</a>, <a href="/search/?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/?searchtype=author&query=Koss%2C+M">Michael Koss</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">George B. Lansbury</a>, <a href="/search/?searchtype=author&query=Luo%2C+B">Bin Luo</a>, <a href="/search/?searchtype=author&query=Paine%2C+J">Jennie Paine</a>, <a href="/search/?searchtype=author&query=Petty%2C+S">Sara Petty</a>, <a href="/search/?searchtype=author&query=Pitchford%2C+K">Kate Pitchford</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="1606.05649v1-abstract-short" style="display: inline;"> We study the geometry of the AGN obscurer in IRAS 09104+4109, an IR-luminous, radio-intermediate FR-I source at $z=0.442$, using infrared data from Spitzer and Herschel, X-ray data from Nustar, Swift, Suzaku, and Chandra, and an optical spectrum from Palomar. The infrared data imply a total rest-frame 1-1000$渭$m luminosity of $5.5\times10^{46}$erg s$^{-1}$ and require both an AGN torus and starbur… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1606.05649v1-abstract-full').style.display = 'inline'; document.getElementById('1606.05649v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1606.05649v1-abstract-full" style="display: none;"> We study the geometry of the AGN obscurer in IRAS 09104+4109, an IR-luminous, radio-intermediate FR-I source at $z=0.442$, using infrared data from Spitzer and Herschel, X-ray data from Nustar, Swift, Suzaku, and Chandra, and an optical spectrum from Palomar. The infrared data imply a total rest-frame 1-1000$渭$m luminosity of $5.5\times10^{46}$erg s$^{-1}$ and require both an AGN torus and starburst model. The AGN torus has an anisotropy-corrected IR luminosity of $4.9\times10^{46}$erg s$^{-1}$, and a viewing angle and half opening angle both of approximately $36$ degrees from pole-on. The starburst has a star formation rate of $(110\pm34)$M$_{\odot}$ yr$^{-1}$ and an age of $<50$Myr. These results are consistent with two epochs of luminous activity in 09104: one approximately $150$Myr ago, and one ongoing. The X-ray data suggest a photon index of $螕\simeq 1.8$ and a line-of-sight column of $N_{\rm H} \simeq 5\times10^{23}$cm$^{-2}$. This argues against a reflection-dominated hard X-ray spectrum, which would have implied a much higher $N_{\rm H}$ and luminosity. The X-ray and infrared data are consistent with a bolometric AGN luminosity of $L_{\rm bol}\sim(0.5-2.5)\times10^{47}$erg s$^{-1}$. The X-ray and infrared data are further consistent with coaligned AGN obscurers in which the line of sight "skims" the torus. This is also consistent with the optical spectra, which show both coronal iron lines and broad lines in polarized but not direct light. Combining constraints from the X-ray, optical, and infrared data suggests that the AGN obscurer is within a vertical height of $20$pc, and a radius of $125$pc, of the nucleus. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1606.05649v1-abstract-full').style.display = 'none'; document.getElementById('1606.05649v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 June, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1605.08041">arXiv:1605.08041</a> <span> [<a href="https://arxiv.org/pdf/1605.08041">pdf</a>, <a href="https://arxiv.org/ps/1605.08041">ps</a>, <a href="https://arxiv.org/format/1605.08041">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/stx357">10.1093/mnras/stx357 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The weak neutral Fe fluorescence line and long-term X-ray evolution of the Compton-thick AGN in NGC 7674 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Gandhi%2C+P">P. Gandhi</a>, <a href="/search/?searchtype=author&query=Annuar%2C+A">A. Annuar</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">G. B. Lansbury</a>, <a href="/search/?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Bauer%2C+F+E">F. E. Bauer</a>, <a href="/search/?searchtype=author&query=Bianchi%2C+S">S. Bianchi</a>, <a href="/search/?searchtype=author&query=Boggs%2C+S+E">S. E. Boggs</a>, <a href="/search/?searchtype=author&query=Boorman%2C+P+G">P. G. Boorman</a>, <a href="/search/?searchtype=author&query=Brandt%2C+W+N">W. N. Brandt</a>, <a href="/search/?searchtype=author&query=Brightman%2C+M">M. Brightman</a>, <a href="/search/?searchtype=author&query=Christensen%2C+F+E">F. E. Christensen</a>, <a href="/search/?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/?searchtype=author&query=Craig%2C+W+W">W. W. Craig</a>, <a href="/search/?searchtype=author&query=Del+Moro%2C+A">A. Del Moro</a>, <a href="/search/?searchtype=author&query=Elvis%2C+M">M. Elvis</a>, <a href="/search/?searchtype=author&query=Guainazzi%2C+M">M. Guainazzi</a>, <a href="/search/?searchtype=author&query=Hailey%2C+C+J">C. J. Hailey</a>, <a href="/search/?searchtype=author&query=Harrison%2C+F+A">F. A. Harrison</a>, <a href="/search/?searchtype=author&query=Koss%2C+M">M. Koss</a>, <a href="/search/?searchtype=author&query=Lamperti%2C+I">I. Lamperti</a>, <a href="/search/?searchtype=author&query=Malaguti%2C+G">G. Malaguti</a>, <a href="/search/?searchtype=author&query=Masini%2C+A">A. Masini</a>, <a href="/search/?searchtype=author&query=Matt%2C+G">G. Matt</a>, <a href="/search/?searchtype=author&query=Puccetti%2C+S">S. Puccetti</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="1605.08041v2-abstract-short" style="display: inline;"> We present $NuSTAR$ X-ray observations of the active galactic nucleus (AGN) in NGC 7674. The source shows a flat X-ray spectrum, suggesting that it is obscured by Compton-thick gas columns. Based upon long-term flux dimming, previous work suggested the alternate possibility that the source is a recently switched-off AGN with the observed X-rays being the lagged echo from the torus. Our high-qualit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.08041v2-abstract-full').style.display = 'inline'; document.getElementById('1605.08041v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1605.08041v2-abstract-full" style="display: none;"> We present $NuSTAR$ X-ray observations of the active galactic nucleus (AGN) in NGC 7674. The source shows a flat X-ray spectrum, suggesting that it is obscured by Compton-thick gas columns. Based upon long-term flux dimming, previous work suggested the alternate possibility that the source is a recently switched-off AGN with the observed X-rays being the lagged echo from the torus. Our high-quality data show the source to be reflection-dominated in hard X-rays, but with a relatively weak neutral Fe K$伪$ emission line (equivalent width [EW] of $\approx$ 0.4 keV) and a strong Fe XXVI ionised line (EW $\approx$ 0.2 keV). We construct an updated long-term X-ray light curve of NGC 7674 and find that the observed 2-10 keV flux has remained constant for the past $\approx$ 20 years, following a high flux state probed by $Ginga$. Light travel time arguments constrain the minimum radius of the reflector to be $\sim$ 3.2 pc under the switched-off AGN scenario, $\approx$ 30 times larger than the expected dust sublimation radius, rendering this possibility unlikely. A patchy Compton-thick AGN (CTAGN) solution is plausible, requiring a minimum line-of-sight column density ($N_{\rm H}$) of 3 $\times$ 10$^{24}$ cm$^{-2}$ at present, and yields an intrinsic 2-10 keV luminosity of (3-5) $\times$ 10$^{43}$ erg s$^{-1}$. Realistic uncertainties span the range of $\approx$ (1-13) $\times$ 10$^{43}$ erg s$^{-1}$. The source has one of the weakest fluorescence lines amongst {\em bona fide} CTAGN, and is potentially a local analogue of bolometrically luminous systems showing complex neutral and ionised Fe emission. It exemplifies the difficulty of identification and proper characterisation of distant CTAGN based on the strength of the neutral Fe K$伪$ line. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.08041v2-abstract-full').style.display = 'none'; document.getElementById('1605.08041v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 June, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 May, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2016. </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">MNRAS accepted version</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1603.08040">arXiv:1603.08040</a> <span> [<a href="https://arxiv.org/pdf/1603.08040">pdf</a>, <a href="https://arxiv.org/format/1603.08040">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/0067-0049/224/2/36">10.3847/0067-0049/224/2/36 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The AllWISE Motion Survey, Part 2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kirkpatrick%2C+J+D">J. Davy Kirkpatrick</a>, <a href="/search/?searchtype=author&query=Kellogg%2C+K">Kendra Kellogg</a>, <a href="/search/?searchtype=author&query=Schneider%2C+A+C">Adam C. Schneider</a>, <a href="/search/?searchtype=author&query=Fajardo-Acosta%2C+S">Sergio Fajardo-Acosta</a>, <a href="/search/?searchtype=author&query=Cushing%2C+M+C">Michael C. Cushing</a>, <a href="/search/?searchtype=author&query=Greco%2C+J">Jennifer Greco</a>, <a href="/search/?searchtype=author&query=Mace%2C+G+N">Gregory N. Mace</a>, <a href="/search/?searchtype=author&query=Gelino%2C+C+R">Christopher R. Gelino</a>, <a href="/search/?searchtype=author&query=Wright%2C+E+L">Edward L. Wright</a>, <a href="/search/?searchtype=author&query=Eisenhardt%2C+P+R+M">Peter R. M. Eisenhardt</a>, <a href="/search/?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/?searchtype=author&query=Faherty%2C+J+K">Jacqueline K. Faherty</a>, <a href="/search/?searchtype=author&query=Sheppard%2C+S+S">Scott S. Sheppard</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">George B. Lansbury</a>, <a href="/search/?searchtype=author&query=Logsdon%2C+S+E">Sarah E. Logsdon</a>, <a href="/search/?searchtype=author&query=Martin%2C+E+C">Emily C. Martin</a>, <a href="/search/?searchtype=author&query=McLean%2C+I+S">Ian S. McLean</a>, <a href="/search/?searchtype=author&query=Schurr%2C+S+D">Steven D. Schurr</a>, <a href="/search/?searchtype=author&query=Cutri%2C+R+M">Roc M. Cutri</a>, <a href="/search/?searchtype=author&query=Conrow%2C+T">Tim Conrow</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="1603.08040v2-abstract-short" style="display: inline;"> We use the AllWISE Data Release to continue our search for WISE-detected motions. In this paper, we publish another 27,846 motion objects, bringing the total number to 48,000 when objects found during our original AllWISE motion survey are included. We use this list, along with the lists of confirmed WISE-based motion objects from the recent papers by Luhman and by Schneider et al. and candidate m… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1603.08040v2-abstract-full').style.display = 'inline'; document.getElementById('1603.08040v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1603.08040v2-abstract-full" style="display: none;"> We use the AllWISE Data Release to continue our search for WISE-detected motions. In this paper, we publish another 27,846 motion objects, bringing the total number to 48,000 when objects found during our original AllWISE motion survey are included. We use this list, along with the lists of confirmed WISE-based motion objects from the recent papers by Luhman and by Schneider et al. and candidate motion objects from the recent paper by Gagne et al. to search for widely separated, common-proper-motion systems. We identify 1,039 such candidate systems. All 48,000 objects are further analyzed using color-color and color-mag plots to provide possible characterizations prior to spectroscopic follow-up. We present spectra of 172 of these, supplemented with new spectra of 23 comparison objects from the literature, and provide classifications and physical interpretations of interesting sources. Highlights include: (1) the identification of three G/K dwarfs that can be used as standard candles to study clumpiness and grain size in nearby molecular clouds because these objects are currently moving behind the clouds, (2) the confirmation/discovery of several M, L, and T dwarfs and one white dwarf whose spectrophotometric distance estimates place them 5-20 pc from the Sun, (3) the suggestion that the Na 'D' line be used as a diagnostic tool for interpreting and classifying metal-poor late-M and L dwarfs, (4) the recognition of a triple system including a carbon dwarf and late-M subdwarf, for which model fits of the late-M subdwarf (giving [Fe/H] ~ -1.0) provide a measured metallicity for the carbon star, and (5) a possible 24-pc-distant K5 dwarf + peculiar red L5 system with an apparent physical separation of 0.1 pc. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1603.08040v2-abstract-full').style.display = 'none'; document.getElementById('1603.08040v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 April, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 March, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2016. </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">62 pages with 80 figures, accepted for publication in The Astrophysical Journal Supplement Series, 23 Mar 2016; second version fixes a few small typos and corrects the footnotes for Table 4</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1602.03532">arXiv:1602.03532</a> <span> [<a href="https://arxiv.org/pdf/1602.03532">pdf</a>, <a href="https://arxiv.org/ps/1602.03532">ps</a>, <a href="https://arxiv.org/format/1602.03532">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/10.3847/0004-637X/820/1/70">10.3847/0004-637X/820/1/70 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Peering through the Dust: NuSTAR Observations of Two FIRST-2MASS Red Quasars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=LaMassa%2C+S+M">Stephanie M. LaMassa</a>, <a href="/search/?searchtype=author&query=Ricarte%2C+A">Angelo Ricarte</a>, <a href="/search/?searchtype=author&query=Glikman%2C+E">Eilat Glikman</a>, <a href="/search/?searchtype=author&query=Urry%2C+C+M">C. Megan Urry</a>, <a href="/search/?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/?searchtype=author&query=Yaqoob%2C+T">Tahir Yaqoob</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">George B. Lansbury</a>, <a href="/search/?searchtype=author&query=Civano%2C+F">Francesca Civano</a>, <a href="/search/?searchtype=author&query=Boggs%2C+S+E">Steve E. Boggs</a>, <a href="/search/?searchtype=author&query=Brandt%2C+W+N">W. N. Brandt</a>, <a href="/search/?searchtype=author&query=Chen%2C+C+J">Chien-Ting J. Chen</a>, <a href="/search/?searchtype=author&query=Christensen%2C+F+E">Finn E. Christensen</a>, <a href="/search/?searchtype=author&query=Craig%2C+W+W">William W. Craig</a>, <a href="/search/?searchtype=author&query=Hailey%2C+C+J">Chuck J. Hailey</a>, <a href="/search/?searchtype=author&query=Harrison%2C+F">Fiona Harrison</a>, <a href="/search/?searchtype=author&query=Hickox%2C+R+C">Ryan C. Hickox</a>, <a href="/search/?searchtype=author&query=Koss%2C+M">Michael Koss</a>, <a href="/search/?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/?searchtype=author&query=Treister%2C+E">Ezequiel Treister</a>, <a href="/search/?searchtype=author&query=Zhang%2C+W">Will Zhang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1602.03532v1-abstract-short" style="display: inline;"> Some reddened quasars appear to be transitional objects in the merger-induced black hole growth/galaxy evolution paradigm, where a heavily obscured nucleus starts to be unveiled by powerful quasar winds evacuating the surrounding cocoon of dust and gas. Hard X-ray observations are able to peer through this gas and dust, revealing the properties of circumnuclear obscuration. Here, we present NuSTAR… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1602.03532v1-abstract-full').style.display = 'inline'; document.getElementById('1602.03532v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1602.03532v1-abstract-full" style="display: none;"> Some reddened quasars appear to be transitional objects in the merger-induced black hole growth/galaxy evolution paradigm, where a heavily obscured nucleus starts to be unveiled by powerful quasar winds evacuating the surrounding cocoon of dust and gas. Hard X-ray observations are able to peer through this gas and dust, revealing the properties of circumnuclear obscuration. Here, we present NuSTAR and XMM-Newton/Chandra observations of FIRST-2MASS selected red quasars F2M 0830+3759 and F2M 1227+3214. We find that though F2M 0830+3759 is moderately obscured ($N_{\rm H,Z} = 2.1\pm0.2 \times10^{22}$ cm$^{-2}$) and F2M 1227+3214 is mildly absorbed ($N_{\rm H,Z} = 3.4^{+0.8}_{-0.7}\times10^{21}$ cm$^{-2}$) along the line-of-sight, heavier global obscuration may be present in both sources, with $N_{\rm H,S} = 3.7^{+4.1}_{-2.6} \times 10^{23}$ cm$^{-2}$ and $< 5.5\times10^{23}$ cm$^{-2}$, for F2M 0830+3759 and F2M 1227+3214, respectively. F2M 0830+3759 also has an excess of soft X-ray emission below 1 keV which is well accommodated by a model where 7% of the intrinsic AGN X-ray emission is scattered into the line-of-sight. While F2M 1227+3214 has a dust-to-gas ratio ($E(B-V)$/$N_{\rm H}$) consistent with the Galactic value, the $E(B-V)$/$N_{\rm H}$ value for F2M 0830+3759 is lower than the Galactic standard, consistent with the paradigm that the dust resides on galactic scales while the X-ray reprocessing gas originates within the dust-sublimation zone of the broad-line-region. The X-ray and 6.1$渭$m luminosities of these red quasars are consistent with the empirical relations derived for high-luminosity, unobscured quasars, extending the parameter space of obscured AGN previously observed by NuSTAR to higher luminosities. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1602.03532v1-abstract-full').style.display = 'none'; document.getElementById('1602.03532v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 February, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted for publication to ApJ; 34 pages, 8 figures, 5 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/1512.04825">arXiv:1512.04825</a> <span> [<a href="https://arxiv.org/pdf/1512.04825">pdf</a>, <a href="https://arxiv.org/format/1512.04825">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/stv2945">10.1093/mnras/stv2945 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A variable ULX and possible IMBH candidate in M51a </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Earnshaw%2C+H+M">Hannah M. Earnshaw</a>, <a href="/search/?searchtype=author&query=Roberts%2C+T+P">Timothy P. Roberts</a>, <a href="/search/?searchtype=author&query=Heil%2C+L+M">Lucy M. Heil</a>, <a href="/search/?searchtype=author&query=Mezcua%2C+M">Mar Mezcua</a>, <a href="/search/?searchtype=author&query=Walton%2C+D+J">Dominic J. Walton</a>, <a href="/search/?searchtype=author&query=Done%2C+C">Chris Done</a>, <a href="/search/?searchtype=author&query=Harrison%2C+F+A">Fiona A. Harrison</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">George B. Lansbury</a>, <a href="/search/?searchtype=author&query=Middleton%2C+M+J">Matthew J. Middleton</a>, <a href="/search/?searchtype=author&query=Sutton%2C+A+D">Andrew D. Sutton</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="1512.04825v2-abstract-short" style="display: inline;"> ULX-7, in the northern spiral arm of M51, demonstrates unusual behaviour for an ultraluminous X-ray source, with a hard X-ray spectrum but very high short-term variability. This suggests that it is not in a typical ultraluminous state. We analyse the source using archival data from XMM-Newton, Chandra and NuSTAR, and by examining optical and radio data from HST and VLA. Our X-ray spectral analysis… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1512.04825v2-abstract-full').style.display = 'inline'; document.getElementById('1512.04825v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1512.04825v2-abstract-full" style="display: none;"> ULX-7, in the northern spiral arm of M51, demonstrates unusual behaviour for an ultraluminous X-ray source, with a hard X-ray spectrum but very high short-term variability. This suggests that it is not in a typical ultraluminous state. We analyse the source using archival data from XMM-Newton, Chandra and NuSTAR, and by examining optical and radio data from HST and VLA. Our X-ray spectral analysis shows that the source has a hard power-law spectral shape with a photon index Gamma~1.5, which persists despite the source's X-ray luminosity varying by over an order of magnitude. The power spectrum of the source features a break at 6.5^{+0.5}_{-1.1}x10^-3 Hz, from a low-frequency spectral index of alpha_1=-0.1^{+0.5}_{-0.2} to a high-frequency spectral index of alpha_2=0.65^{+0.05}_{-0.14}, making it analogous to the low-frequency break found in the power spectra of low/hard state black holes (BHs). We can take a lower frequency limit for a corresponding high-frequency break to calculate a BH mass upper limit of 1.6x10^3 solar masses. Using the X-ray/radio fundamental plane we calculate another upper limit to the BH mass of 3.5x10^4 solar masses for a BH in the low/hard state. The hard spectrum, high rms variability and mass limits are consistent with ULX-7 being an intermediate-mass BH; however we cannot exclude other interpretations of this source's interesting behaviour, most notably a neutron star with an extreme accretion rate. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1512.04825v2-abstract-full').style.display = 'none'; document.getElementById('1512.04825v2-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 January, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 December, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2015. </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, 12 figures, 6 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/1511.04186">arXiv:1511.04186</a> <span> [<a href="https://arxiv.org/pdf/1511.04186">pdf</a>, <a href="https://arxiv.org/ps/1511.04186">ps</a>, <a href="https://arxiv.org/format/1511.04186">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/808/2/184">10.1088/0004-637X/808/2/184 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The NuSTAR Extragalactic Surveys: Initial Results and Catalog from the Extended Chandra Deep Field South </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Mullaney%2C+J+R">J. R. Mullaney</a>, <a href="/search/?searchtype=author&query=Del-Moro%2C+A">A. Del-Moro</a>, <a href="/search/?searchtype=author&query=Aird%2C+J">J. Aird</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Civano%2C+F+M">F. M. Civano</a>, <a href="/search/?searchtype=author&query=Hickox%2C+R+C">R. C. Hickox</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">G. B. Lansbury</a>, <a href="/search/?searchtype=author&query=Ajello%2C+M">M. Ajello</a>, <a href="/search/?searchtype=author&query=Assef%2C+R">R. Assef</a>, <a href="/search/?searchtype=author&query=Ballantyne%2C+D+R">D. R. Ballantyne</a>, <a href="/search/?searchtype=author&query=Balokovic%2C+M">M. Balokovic</a>, <a href="/search/?searchtype=author&query=Bauer%2C+F+E">F. E. Bauer</a>, <a href="/search/?searchtype=author&query=Brandt%2C+W+N">W. N. Brandt</a>, <a href="/search/?searchtype=author&query=Boggs%2C+S+E">S. E. Boggs</a>, <a href="/search/?searchtype=author&query=Brightman%2C+M">M. Brightman</a>, <a href="/search/?searchtype=author&query=Christensen%2C+F+E">F. E. Christensen</a>, <a href="/search/?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/?searchtype=author&query=Craig%2C+W+W">W. W. Craig</a>, <a href="/search/?searchtype=author&query=Elvis%2C+M">M. Elvis</a>, <a href="/search/?searchtype=author&query=Forster%2C+K">K. Forster</a>, <a href="/search/?searchtype=author&query=Gandhi%2C+P">P. Gandhi</a>, <a href="/search/?searchtype=author&query=Grefenstette%2C+B+W">B. W. Grefenstette</a>, <a href="/search/?searchtype=author&query=Hailey%2C+C+J">C. J. Hailey</a>, <a href="/search/?searchtype=author&query=Harrison%2C+F+A">F. A. Harrison</a>, <a href="/search/?searchtype=author&query=Koss%2C+M">M. Koss</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="1511.04186v1-abstract-short" style="display: inline;"> We present initial results and the source catalog from the NuSTAR survey of the Extended Chandra Deep Field South (hereafter, ECDFS) - currently the deepest contiguous component of the NuSTAR extragalactic survey program. The survey covers the full ~30 arcmin x 30 arcmin area of this field to a maximum depth of ~360 ks (~220 ks when corrected for vignetting at 3-24 keV), reaching sensitivity limit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.04186v1-abstract-full').style.display = 'inline'; document.getElementById('1511.04186v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1511.04186v1-abstract-full" style="display: none;"> We present initial results and the source catalog from the NuSTAR survey of the Extended Chandra Deep Field South (hereafter, ECDFS) - currently the deepest contiguous component of the NuSTAR extragalactic survey program. The survey covers the full ~30 arcmin x 30 arcmin area of this field to a maximum depth of ~360 ks (~220 ks when corrected for vignetting at 3-24 keV), reaching sensitivity limits of ~1.3 x 10^-14 erg/cm2/s (3-8 keV), ~3.4 x 10^-14 erg/cm2/s (8-24 keV) and ~3.0 x 10^-14 erg/cm2/s (3-24 keV). Fifty four (54) sources are detected over the full field, although five of these are found to lie below our significance threshold once contaminating flux from neighboring (i.e., blended) sources is taken into account. Of the remaining 49 that are significant, 19 are detected in the 8-24 keV band. The 8-24 keV to 3-8 keV band ratios of the twelve sources that are detected in both bands span the range 0.39-1.7, corresponding to a photon index range of Gamma ~ 0.5-2.3, with a median photon index of 1.70 +/- 0.52. The redshifts of the 49 sources in our main sample span the range z = 0.21-2.7, and their rest-frame 10-40 keV luminosities (derived from the observed 8-24 keV fluxes) span the range L(10-40 keV) ~ (0.7-300) x 10^43 erg/s, sampling below the "knee" of the X-ray luminosity function out to z ~ 0.8-1. Finally, we identify one NuSTAR source that has neither a Chandra nor an XMM-Newton counterpart, but that shows evidence of nuclear activity at infrared wavelengths, and thus may represent a genuine, new X-ray source detected by NuSTAR in the ECDFS. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.04186v1-abstract-full').style.display = 'none'; document.getElementById('1511.04186v1-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, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2015. </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, published in the Astrophysical Journal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ , 808, 184 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1511.04185">arXiv:1511.04185</a> <span> [<a href="https://arxiv.org/pdf/1511.04185">pdf</a>, <a href="https://arxiv.org/ps/1511.04185">ps</a>, <a href="https://arxiv.org/format/1511.04185">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/808/2/185">10.1088/0004-637X/808/2/185 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The NuSTAR Extragalactic Surveys: Overview and Catalog from the COSMOS Field </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Civano%2C+F">F. Civano</a>, <a href="/search/?searchtype=author&query=Hickox%2C+R+C">R. C. Hickox</a>, <a href="/search/?searchtype=author&query=Puccetti%2C+S">S. Puccetti</a>, <a href="/search/?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/?searchtype=author&query=Mullaney%2C+J+R">J. R. Mullaney</a>, <a href="/search/?searchtype=author&query=Zappacosta%2C+L">L. Zappacosta</a>, <a href="/search/?searchtype=author&query=LaMassa%2C+S+M">S. M. LaMassa</a>, <a href="/search/?searchtype=author&query=Aird%2C+J">J. Aird</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Ballantyne%2C+D+R">D. R. Ballantyne</a>, <a href="/search/?searchtype=author&query=Bauer%2C+F+E">F. E. Bauer</a>, <a href="/search/?searchtype=author&query=Brandt%2C+W+N">W. N. Brandt</a>, <a href="/search/?searchtype=author&query=Boggs%2C+S+E">S. E. Boggs</a>, <a href="/search/?searchtype=author&query=Christensen%2C+F+E">F. E. Christensen</a>, <a href="/search/?searchtype=author&query=Craig%2C+W+W">W. W. Craig</a>, <a href="/search/?searchtype=author&query=Del-Moro%2C+A">A. Del-Moro</a>, <a href="/search/?searchtype=author&query=Elvis%2C+M">M. Elvis</a>, <a href="/search/?searchtype=author&query=Forster%2C+K">K. Forster</a>, <a href="/search/?searchtype=author&query=Gandhi%2C+P">P. Gandhi</a>, <a href="/search/?searchtype=author&query=Grefenstette%2C+B+W">B. W. Grefenstette</a>, <a href="/search/?searchtype=author&query=Hailey%2C+C+J">C. J. Hailey</a>, <a href="/search/?searchtype=author&query=Harrison%2C+F+A">F. A. Harrison</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">G. B. Lansbury</a>, <a href="/search/?searchtype=author&query=Luo%2C+B">B. Luo</a>, <a href="/search/?searchtype=author&query=Madsen%2C+K">K. Madsen</a> , et al. (6 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1511.04185v1-abstract-short" style="display: inline;"> To provide the census of the sources contributing to the X-ray background peak above 10 keV, NuSTAR is performing extragalactic surveys using a three-tier "wedding cake" approach. We present the NuSTAR survey of the COSMOS field, the medium sensitivity and medium area tier, covering 1.7 deg2 and overlapping with both Chandra and XMM-Newton data. This survey consists of 121 observations for a total… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.04185v1-abstract-full').style.display = 'inline'; document.getElementById('1511.04185v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1511.04185v1-abstract-full" style="display: none;"> To provide the census of the sources contributing to the X-ray background peak above 10 keV, NuSTAR is performing extragalactic surveys using a three-tier "wedding cake" approach. We present the NuSTAR survey of the COSMOS field, the medium sensitivity and medium area tier, covering 1.7 deg2 and overlapping with both Chandra and XMM-Newton data. This survey consists of 121 observations for a total exposure of ~3 Ms. To fully exploit these data, we developed a new detection strategy, carefully tested through extensive simulations. The survey sensitivity at 20% completeness is 5.9, 2.9 and 6.4 x 10^-14 erg/cm2/s in the 3-24 keV, 3-8 keV and 8-24 keV bands, respectively. By combining detections in 3 bands, we have a sample of 91 NuSTAR sources with 10^42 -10^45.5 erg/s luminosities and redshift z=0.04-2.5. Thirty two sources are detected in the 8-24 keV band with fluxes ~100 times fainter than sources detected by Swift-BAT. Of the 91 detections, all but four are associated with a Chandra and/or XMM-Newton point-like counterpart. One source is associated with an extended lower energy X-ray source. We present the X-ray (hardness ratio and luminosity) and optical-to-X-ray properties. The observed fraction of candidate Compton-thick AGN measured from the hardness ratio is between 13-20%. We discuss the spectral properties of NuSTAR J100259+0220.6 (ID 330) at z=0.044, with the highest hardness ratio in the entire sample. The measured column density exceeds 10^24 /cm2, implying the source is Compton-thick. This source was not previously recognized as such without the >10 keV data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.04185v1-abstract-full').style.display = 'none'; document.getElementById('1511.04185v1-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, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2015. </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, published in the Astrophysical Journal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ, 808, 185 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1511.04184">arXiv:1511.04184</a> <span> [<a href="https://arxiv.org/pdf/1511.04184">pdf</a>, <a href="https://arxiv.org/ps/1511.04184">ps</a>, <a href="https://arxiv.org/format/1511.04184">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/815/1/66">10.1088/0004-637X/815/1/66 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The NuSTAR Extragalactic Surveys: First Direct Measurements of the >10 keV X-Ray Luminosity Function for Active Galactic Nuclei at z>0.1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Aird%2C+J">J. Aird</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Ballantyne%2C+D+R">D. R. Ballantyne</a>, <a href="/search/?searchtype=author&query=Civano%2C+F">F. Civano</a>, <a href="/search/?searchtype=author&query=Del-Moro%2C+A">A. Del-Moro</a>, <a href="/search/?searchtype=author&query=Hickox%2C+R+C">R. C. Hickox</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">G. B. Lansbury</a>, <a href="/search/?searchtype=author&query=Mullaney%2C+J+R">J. R. Mullaney</a>, <a href="/search/?searchtype=author&query=Bauer%2C+F+E">F. E. Bauer</a>, <a href="/search/?searchtype=author&query=Brandt%2C+W+N">W. N. Brandt</a>, <a href="/search/?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/?searchtype=author&query=Fabian%2C+A+C">A. C. Fabian</a>, <a href="/search/?searchtype=author&query=Gandhi%2C+P">P. Gandhi</a>, <a href="/search/?searchtype=author&query=Harrison%2C+F+A">F. A. Harrison</a>, <a href="/search/?searchtype=author&query=Luo%2C+B">B. Luo</a>, <a href="/search/?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/?searchtype=author&query=Treister%2C+E">E. Treister</a>, <a href="/search/?searchtype=author&query=Zappacosta%2C+L">L. Zappacosta</a>, <a href="/search/?searchtype=author&query=Ajello%2C+M">M. Ajello</a>, <a href="/search/?searchtype=author&query=Assef%2C+R">R. Assef</a>, <a href="/search/?searchtype=author&query=Boggs%2C+S+E">S. E. Boggs</a>, <a href="/search/?searchtype=author&query=Brightman%2C+M">M. Brightman</a>, <a href="/search/?searchtype=author&query=Christensen%2C+F+E">F. E. Christensen</a>, <a href="/search/?searchtype=author&query=Craig%2C+W+W">W. W. Craig</a>, <a href="/search/?searchtype=author&query=Elvis%2C+M">M. Elvis</a> , et al. (12 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1511.04184v1-abstract-short" style="display: inline;"> We present the first direct measurements of the rest-frame 10-40 keV X-ray luminosity function (XLF) of Active Galactic Nuclei (AGNs) based on a sample of 94 sources at 0.1 < z <3, selected at 8-24 keV energies from sources in the NuSTAR extragalactic survey program. Our results are consistent with the strong evolution of the AGN population seen in prior, lower-energy studies of the XLF. However,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.04184v1-abstract-full').style.display = 'inline'; document.getElementById('1511.04184v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1511.04184v1-abstract-full" style="display: none;"> We present the first direct measurements of the rest-frame 10-40 keV X-ray luminosity function (XLF) of Active Galactic Nuclei (AGNs) based on a sample of 94 sources at 0.1 < z <3, selected at 8-24 keV energies from sources in the NuSTAR extragalactic survey program. Our results are consistent with the strong evolution of the AGN population seen in prior, lower-energy studies of the XLF. However, different models of the intrinsic distribution of absorption, which are used to correct for selection biases, give significantly different predictions for the total number of sources in our sample, leading to small, systematic differences in our binned estimates of the XLF. Adopting a model with a lower intrinsic fraction of Compton-thick sources and a larger population of sources with column densities N_H ~ 10^{23-24} /cm2 or a model with stronger Compton reflection component (with a relative normalization of R ~ 2 at all luminosities) can bring extrapolations of the XLF from 2-10 keV into agreement with our NuSTAR sample. Ultimately, X-ray spectral analysis of the NuSTAR sources is required to break this degeneracy between the distribution of absorbing column densities and the strength of the Compton reflection component and thus refine our measurements of the XLF. Furthermore, the models that successfully describe the high-redshift population seen by NuSTAR tend to over-predict previous, high-energy measurements of the local XLF, indicating that there is evolution of the AGN population that is not fully captured by the current models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.04184v1-abstract-full').style.display = 'none'; document.getElementById('1511.04184v1-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, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2015. </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, 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/1509.03322">arXiv:1509.03322</a> <span> [<a href="https://arxiv.org/pdf/1509.03322">pdf</a>, <a href="https://arxiv.org/ps/1509.03322">ps</a>, <a href="https://arxiv.org/format/1509.03322">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/815/1/36">10.1088/0004-637X/815/1/36 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> NuSTAR Observations of the Compton-thick Active Galactic Nucleus and Ultraluminous X-ray Source Candidate in NGC 5643 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Annuar%2C+A">A. Annuar</a>, <a href="/search/?searchtype=author&query=Gandhi%2C+P">P. Gandhi</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">G. B. Lansbury</a>, <a href="/search/?searchtype=author&query=Ar%C3%A9valo%2C+P">P. Ar茅valo</a>, <a href="/search/?searchtype=author&query=Ballantyne%2C+D+R">D. R. Ballantyne</a>, <a href="/search/?searchtype=author&query=Balokovi%C4%87%2C+M">M. Balokovi膰</a>, <a href="/search/?searchtype=author&query=Bauer%2C+F+E">F. E. Bauer</a>, <a href="/search/?searchtype=author&query=Boggs%2C+S+E">S. E. Boggs</a>, <a href="/search/?searchtype=author&query=Brandt%2C+W+N">W. N. Brandt</a>, <a href="/search/?searchtype=author&query=Brightman%2C+M">M. Brightman</a>, <a href="/search/?searchtype=author&query=Christensen%2C+F+E">F. E. Christensen</a>, <a href="/search/?searchtype=author&query=Craig%2C+W+W">W. W. Craig</a>, <a href="/search/?searchtype=author&query=Del+Moro%2C+A">A. Del Moro</a>, <a href="/search/?searchtype=author&query=Hailey%2C+C+J">C. J. Hailey</a>, <a href="/search/?searchtype=author&query=Harrison%2C+F+A">F. A. Harrison</a>, <a href="/search/?searchtype=author&query=Hickox%2C+R+C">R. C. Hickox</a>, <a href="/search/?searchtype=author&query=Matt%2C+G">G. Matt</a>, <a href="/search/?searchtype=author&query=Puccetti%2C+S">S. Puccetti</a>, <a href="/search/?searchtype=author&query=Ricci%2C+C">C. Ricci</a>, <a href="/search/?searchtype=author&query=Rigby%2C+J+R">J. R. Rigby</a>, <a href="/search/?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/?searchtype=author&query=Walton%2C+D+J">D. J. Walton</a>, <a href="/search/?searchtype=author&query=Zappacosta%2C+L">L. Zappacosta</a>, <a href="/search/?searchtype=author&query=Zhang%2C+W">W. Zhang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1509.03322v1-abstract-short" style="display: inline;"> We present two NuSTAR observations of the local Seyfert 2 active galactic nucleus (AGN) and an ultraluminous X-ray source (ULX) candidate in NGC 5643. Together with archival data from Chandra, XMM-Newton and Swift-BAT, we perform a high-quality broadband spectral analysis of the AGN over two decades in energy ($\sim$0.5-100 keV). Previous X-ray observations suggested that the AGN is obscured by a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.03322v1-abstract-full').style.display = 'inline'; document.getElementById('1509.03322v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1509.03322v1-abstract-full" style="display: none;"> We present two NuSTAR observations of the local Seyfert 2 active galactic nucleus (AGN) and an ultraluminous X-ray source (ULX) candidate in NGC 5643. Together with archival data from Chandra, XMM-Newton and Swift-BAT, we perform a high-quality broadband spectral analysis of the AGN over two decades in energy ($\sim$0.5-100 keV). Previous X-ray observations suggested that the AGN is obscured by a Compton-thick (CT) column of obscuring gas along our line-of-sight. However, the lack of high-quality $\gtrsim$ 10 keV observations, together with the presence of a nearby X-ray luminous source, NGC 5643 X-1, had left significant uncertainties in the characterization of the nuclear spectrum. NuSTAR now enables the AGN and NGC 5643 X-1 to be separately resolved above 10 keV for the first time and allows a direct measurement of the absorbing column density toward the nucleus. The new data show that the nucleus is indeed obscured by a CT column of $N_{\rm{H}}$ $\gtrsim$ 5 $\times$ 10$^{24}$ cm$^{-2}$. The range of 2-10 keV absorption-corrected luminosity inferred from the best fitting models is $L_{2-10,\rm{int}} =$ (0.8-1.7) $\times$ 10$^{42}$ erg s$^{-1}$, consistent with that predicted from multiwavelength intrinsic luminosity indicators. We also study the NuSTAR data for NGC 5643 X-1, and show that it exhibits evidence for a spectral cut-off at energy, $E$ $\sim$ 10 keV, similar to that seen in other ULXs observed by NuSTAR. Along with the evidence for significant X-ray luminosity variations in the 3-8 keV band from 2003-2014, our results further strengthen the ULX classification of NGC 5643 X-1. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.03322v1-abstract-full').style.display = 'none'; document.getElementById('1509.03322v1-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, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Resubmitted to ApJ on Sept. 10, 2015 after incorporating the referee's comments; 14 pages, 6 figures and 3 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/1507.04534">arXiv:1507.04534</a> <span> [<a href="https://arxiv.org/pdf/1507.04534">pdf</a>, <a href="https://arxiv.org/ps/1507.04534">ps</a>, <a href="https://arxiv.org/format/1507.04534">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/809/2/140">10.1088/0004-637X/809/2/140 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> NuSTAR discovery of an unusually steady long-term spin-up of the Be binary 2RXP J130159.6-635806 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Krivonos%2C+R+A">Roman A. Krivonos</a>, <a href="/search/?searchtype=author&query=Tsygankov%2C+S+S">Sergey S. Tsygankov</a>, <a href="/search/?searchtype=author&query=Lutovinov%2C+A+A">Alexander A. Lutovinov</a>, <a href="/search/?searchtype=author&query=Tomsick%2C+J+A">John A. Tomsick</a>, <a href="/search/?searchtype=author&query=Chakrabarty%2C+D">Deepto Chakrabarty</a>, <a href="/search/?searchtype=author&query=Bachetti%2C+M">Matteo Bachetti</a>, <a href="/search/?searchtype=author&query=Boggs%2C+S+E">Steven E. Boggs</a>, <a href="/search/?searchtype=author&query=Chernyakova%2C+M">Masha Chernyakova</a>, <a href="/search/?searchtype=author&query=Christensen%2C+F+E">Finn E. Christensen</a>, <a href="/search/?searchtype=author&query=Craig%2C+W+W">William W. Craig</a>, <a href="/search/?searchtype=author&query=Fuerst%2C+F">Felix Fuerst</a>, <a href="/search/?searchtype=author&query=Hailey%2C+C+J">Charles J. Hailey</a>, <a href="/search/?searchtype=author&query=Harrison%2C+F+A">Fiona A. Harrison</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">George B. Lansbury</a>, <a href="/search/?searchtype=author&query=Rahoui%2C+F">Farid Rahoui</a>, <a href="/search/?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/?searchtype=author&query=Zhang%2C+W+W">William W. Zhang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1507.04534v1-abstract-short" style="display: inline;"> We present spectral and timing analysis of NuSTAR observations of the accreting X-ray pulsar 2RXP J130159.6-635806. The source was serendipitously observed during a campaign focused on the gamma-ray binary PSR B1259-63 and was later targeted for a dedicated observation. The spectrum has a typical shape for accreting X-ray pulsars, consisting of a simple power law with an exponential cutoff startin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1507.04534v1-abstract-full').style.display = 'inline'; document.getElementById('1507.04534v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1507.04534v1-abstract-full" style="display: none;"> We present spectral and timing analysis of NuSTAR observations of the accreting X-ray pulsar 2RXP J130159.6-635806. The source was serendipitously observed during a campaign focused on the gamma-ray binary PSR B1259-63 and was later targeted for a dedicated observation. The spectrum has a typical shape for accreting X-ray pulsars, consisting of a simple power law with an exponential cutoff starting at ~7 keV with a folding energy of E_fold=~18 keV. There is also an indication of the presence of a 6.4 keV iron line in the spectrum at the ~3 sigma significance level. NuSTAR measurements of the pulsation period reveal that the pulsar has undergone a strong and steady spin-up for the last 20 years. The pulsed fraction is estimated to be ~80%, and is constant with energy up to 40 keV. The power density spectrum shows a break towards higher frequencies relative to the current spin period. This, together with steady persistent luminosity, points to a long-term mass accretion rate high enough to bring the pulsar out of spin equilibrium. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1507.04534v1-abstract-full').style.display = 'none'; document.getElementById('1507.04534v1-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 July, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 7 figures, 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/1506.05120">arXiv:1506.05120</a> <span> [<a href="https://arxiv.org/pdf/1506.05120">pdf</a>, <a href="https://arxiv.org/format/1506.05120">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/10.1088/0004-637X/809/2/115">10.1088/0004-637X/809/2/115 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> NuSTAR Reveals Extreme Absorption in z < 0.5 Type 2 Quasars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">G. B. Lansbury</a>, <a href="/search/?searchtype=author&query=Gandhi%2C+P">P. Gandhi</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Assef%2C+R+J">R. J. Assef</a>, <a href="/search/?searchtype=author&query=Aird%2C+J">J. Aird</a>, <a href="/search/?searchtype=author&query=Annuar%2C+A">A. Annuar</a>, <a href="/search/?searchtype=author&query=Ballantyne%2C+D+R">D. R. Ballantyne</a>, <a href="/search/?searchtype=author&query=Balokovic%2C+M">M. Balokovic</a>, <a href="/search/?searchtype=author&query=Bauer%2C+F+E">F. E. Bauer</a>, <a href="/search/?searchtype=author&query=Boggs%2C+S+E">S. E. Boggs</a>, <a href="/search/?searchtype=author&query=Brandt%2C+W+N">W. N. Brandt</a>, <a href="/search/?searchtype=author&query=Brightman%2C+M">M. Brightman</a>, <a href="/search/?searchtype=author&query=Christensen%2C+F+E">F. E. Christensen</a>, <a href="/search/?searchtype=author&query=Civano%2C+F">F. Civano</a>, <a href="/search/?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/?searchtype=author&query=Craig%2C+W+W">W. W. Craig</a>, <a href="/search/?searchtype=author&query=Del+Moro%2C+A">A. Del Moro</a>, <a href="/search/?searchtype=author&query=Grefenstette%2C+B+W">B. W. Grefenstette</a>, <a href="/search/?searchtype=author&query=Hailey%2C+C+J">C. J. Hailey</a>, <a href="/search/?searchtype=author&query=Harrison%2C+F+A">F. A. Harrison</a>, <a href="/search/?searchtype=author&query=Hickox%2C+R+C">R. C. Hickox</a>, <a href="/search/?searchtype=author&query=Koss%2C+M">M. Koss</a>, <a href="/search/?searchtype=author&query=LaMassa%2C+S+M">S. M. LaMassa</a>, <a href="/search/?searchtype=author&query=Luo%2C+B">B. Luo</a>, <a href="/search/?searchtype=author&query=Puccetti%2C+S">S. Puccetti</a> , et al. (5 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1506.05120v1-abstract-short" style="display: inline;"> The intrinsic column density (NH) distribution of quasars is poorly known. At the high obscuration end of the quasar population and for redshifts z<1, the X-ray spectra can only be reliably characterized using broad-band measurements which extend to energies above 10 keV. Using the hard X-ray observatory NuSTAR, along with archival Chandra and XMM-Newton data, we study the broad-band X-ray spectra… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1506.05120v1-abstract-full').style.display = 'inline'; document.getElementById('1506.05120v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1506.05120v1-abstract-full" style="display: none;"> The intrinsic column density (NH) distribution of quasars is poorly known. At the high obscuration end of the quasar population and for redshifts z<1, the X-ray spectra can only be reliably characterized using broad-band measurements which extend to energies above 10 keV. Using the hard X-ray observatory NuSTAR, along with archival Chandra and XMM-Newton data, we study the broad-band X-ray spectra of nine optically selected (from the SDSS), candidate Compton-thick (NH > 1.5e24 cm^-2) type 2 quasars (CTQSO2s); five new NuSTAR observations are reported herein, and four have been previously published. The candidate CTQSO2s lie at z<0.5, have observed [OIII] luminosities in the range 8.4 < log (L_[OIII]/L_solar) < 9.6, and show evidence for extreme, Compton-thick absorption when indirect absorption diagnostics are considered. Amongst the nine candidate CTQSO2s, five are detected by NuSTAR in the high energy (8-24 keV) band: two are weakly detected at the ~ 3 sigma confidence level and three are strongly detected with sufficient counts for spectral modeling (>~ 90 net source counts at 8-24 keV). For these NuSTAR-detected sources direct (i.e., X-ray spectral) constraints on the intrinsic AGN properties are feasible, and we measure column densities ~2.5-1600 times higher and intrinsic (unabsorbed) X-ray luminosities ~10-70 times higher than pre-NuSTAR constraints from Chandra and XMM-Newton. Assuming the NuSTAR-detected type 2 quasars are representative of other Compton-thick candidates, we make a correction to the NH distribution for optically selected type 2 quasars as measured by Chandra and XMM-Newton for 39 objects. With this approach, we predict a Compton-thick fraction of f_CT = 36^{+14}_{-12} %, although higher fractions (up to 76%) are possible if indirect absorption diagnostics are assumed to be reliable. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1506.05120v1-abstract-full').style.display = 'none'; document.getElementById('1506.05120v1-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, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2015. </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, 13 figures, 5 tables. Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1408.5414">arXiv:1408.5414</a> <span> [<a href="https://arxiv.org/pdf/1408.5414">pdf</a>, <a href="https://arxiv.org/ps/1408.5414">ps</a>, <a href="https://arxiv.org/format/1408.5414">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/10.1088/0004-637X/794/2/111">10.1088/0004-637X/794/2/111 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The NuSTAR View of Nearby Compton-thick AGN: The Cases of NGC 424, NGC 1320 and IC 2560 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Balokovi%C4%87%2C+M">M. Balokovi膰</a>, <a href="/search/?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/?searchtype=author&query=Harrison%2C+F+A">F. A. Harrison</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Ballantyne%2C+D+R">D. R. Ballantyne</a>, <a href="/search/?searchtype=author&query=Bauer%2C+F+E">F. E. Bauer</a>, <a href="/search/?searchtype=author&query=Boggs%2C+S+E">S. E. Boggs</a>, <a href="/search/?searchtype=author&query=Brandt%2C+W+N">W. N. Brandt</a>, <a href="/search/?searchtype=author&query=Brightman%2C+M">M. Brightman</a>, <a href="/search/?searchtype=author&query=Christensen%2C+F+E">F. E. Christensen</a>, <a href="/search/?searchtype=author&query=Craig%2C+W+W">W. W. Craig</a>, <a href="/search/?searchtype=author&query=Del+Moro%2C+A">A. Del Moro</a>, <a href="/search/?searchtype=author&query=Gandhi%2C+P">P. Gandhi</a>, <a href="/search/?searchtype=author&query=Hailey%2C+C+J">C. J. Hailey</a>, <a href="/search/?searchtype=author&query=Koss%2C+M">M. Koss</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">G. B. Lansbury</a>, <a href="/search/?searchtype=author&query=Luo%2C+B">B. Luo</a>, <a href="/search/?searchtype=author&query=Madejski%2C+G+M">G. M. Madejski</a>, <a href="/search/?searchtype=author&query=Marinucci%2C+A">A. Marinucci</a>, <a href="/search/?searchtype=author&query=Matt%2C+G">G. Matt</a>, <a href="/search/?searchtype=author&query=Markwardt%2C+C+B">C. B. Markwardt</a>, <a href="/search/?searchtype=author&query=Puccetti%2C+S">S. Puccetti</a>, <a href="/search/?searchtype=author&query=Reynolds%2C+C+S">C. S. Reynolds</a>, <a href="/search/?searchtype=author&query=Risaliti%2C+G">G. Risaliti</a>, <a href="/search/?searchtype=author&query=Rivers%2C+E">E. Rivers</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="1408.5414v1-abstract-short" style="display: inline;"> We present X-ray spectral analyses for three Seyfert 2 active galactic nuclei, NGC 424, NGC 1320, and IC 2560, observed by NuSTAR in the 3-79 keV band. The high quality hard X-ray spectra allow detailed modeling of the Compton reflection component for the first time in these sources. Using quasi-simultaneous NuSTAR and Swift/XRT data, as well as archival XMM-Newton data, we find that all three nuc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.5414v1-abstract-full').style.display = 'inline'; document.getElementById('1408.5414v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1408.5414v1-abstract-full" style="display: none;"> We present X-ray spectral analyses for three Seyfert 2 active galactic nuclei, NGC 424, NGC 1320, and IC 2560, observed by NuSTAR in the 3-79 keV band. The high quality hard X-ray spectra allow detailed modeling of the Compton reflection component for the first time in these sources. Using quasi-simultaneous NuSTAR and Swift/XRT data, as well as archival XMM-Newton data, we find that all three nuclei are obscured by Compton-thick material with column densities in excess of ~5 x $10^{24}$ cm$^{-2}$, and that their X-ray spectra above 3 keV are dominated by reflection of the intrinsic continuum on Compton-thick material. Due to the very high obscuration, absorbed intrinsic continuum components are not formally required by the data in any of the sources. We constrain the intrinsic photon indices and the column density of the reflecting medium through the shape of the reflection spectra. Using archival multi-wavelength data we recover the intrinsic X-ray luminosities consistent with the broadband spectral energy distributions. Our results are consistent with the reflecting medium being an edge-on clumpy torus with a relatively large global covering factor and overall reflection efficiency of the order of 1%. Given the unambiguous confirmation of the Compton-thick nature of the sources, we investigate whether similar sources are likely to be missed by commonly used selection criteria for Compton-thick AGN, and explore the possibility of finding their high-redshift counterparts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.5414v1-abstract-full').style.display = 'none'; document.getElementById('1408.5414v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 August, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2014. </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, 794, 111 (2014) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1407.3974">arXiv:1407.3974</a> <span> [<a href="https://arxiv.org/pdf/1407.3974">pdf</a>, <a href="https://arxiv.org/ps/1407.3974">ps</a>, <a href="https://arxiv.org/format/1407.3974">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/793/1/26">10.1088/0004-637X/793/1/26 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The variable hard X-ray emission of NGC4945 as observed by NuSTAR </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Puccetti%2C+S">Simonetta Puccetti</a>, <a href="/search/?searchtype=author&query=Comastri%2C+A">Andrea Comastri</a>, <a href="/search/?searchtype=author&query=Fiore%2C+F">Fabrizio Fiore</a>, <a href="/search/?searchtype=author&query=Ar%C3%A9valo%2C+P">Patricia Ar茅valo</a>, <a href="/search/?searchtype=author&query=Risaliti%2C+G">Guido Risaliti</a>, <a href="/search/?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/?searchtype=author&query=Brandt%2C+W+N">William N. Brandt</a>, <a href="/search/?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/?searchtype=author&query=Harrison%2C+F+A">Fiona A. Harrison</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">David M. Alexander</a>, <a href="/search/?searchtype=author&query=Boggs%2C+S+E">Steve E. Boggs</a>, <a href="/search/?searchtype=author&query=Christensen%2C+F+E">Finn E. Christensen</a>, <a href="/search/?searchtype=author&query=Craig%2C+W+W">William W. Craig</a>, <a href="/search/?searchtype=author&query=Gandhi%2C+P">Poshak Gandhi</a>, <a href="/search/?searchtype=author&query=Hailey%2C+C+J">Charles J. Hailey</a>, <a href="/search/?searchtype=author&query=Koss%2C+M+R">Michael R. Koss</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">George B. Lansbury</a>, <a href="/search/?searchtype=author&query=Luo%2C+B">Bin Luo</a>, <a href="/search/?searchtype=author&query=Madejski%2C+G+M">Greg M. Madejski</a>, <a href="/search/?searchtype=author&query=Matt%2C+G">Giorgio Matt</a>, <a href="/search/?searchtype=author&query=Walton%2C+D+J">Dominic J. Walton</a>, <a href="/search/?searchtype=author&query=Zhang%2C+W">Will Zhang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1407.3974v1-abstract-short" style="display: inline;"> We present a broadband (~0.5-79 keV) spectral and temporal analysis of multiple NuSTAR observations combined with archival Suzaku and Chandra data of NGC4945, the brightest extragalactic source at 100 keV. We observe hard X-ray (> 10 keV) flux and spectral variability, with flux variations of a factor 2 on timescales of 20 ksec. A variable primary continuum dominates the high energy spectrum (>10… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1407.3974v1-abstract-full').style.display = 'inline'; document.getElementById('1407.3974v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1407.3974v1-abstract-full" style="display: none;"> We present a broadband (~0.5-79 keV) spectral and temporal analysis of multiple NuSTAR observations combined with archival Suzaku and Chandra data of NGC4945, the brightest extragalactic source at 100 keV. We observe hard X-ray (> 10 keV) flux and spectral variability, with flux variations of a factor 2 on timescales of 20 ksec. A variable primary continuum dominates the high energy spectrum (>10 keV) in all the states, while the reflected/scattered flux which dominates at E< 10 keV stays approximately constant. From modelling the complex reflection/transmission spectrum we derive a Compton depth along the line of sight of tau_Thomson ~ 2.9, and a global covering factor for the circumnuclear gas of ~ 0.15. This agrees with the constraints derived from the high energy variability, which implies that most of the high energy flux is transmitted, rather that Compton-scattered. This demonstrates the effectiveness of spectral analysis in constraining the geometric properties of the circumnuclear gas, and validates similar methods used for analyzing the spectra of other bright, Compton-thick AGN. The lower limits on the e-folding energy are between 200-300 keV, consistent with previous BeppoSAX, Suzaku and Swift BAT observations. The accretion rate, estimated from the X-ray luminosity and assuming a bolometric correction typical of type 2 AGN, is in the range ~0.1-0.3 lambda_Edd depending on the flux state. The substantial observed X-ray luminosity variability of NGC4945 implies that large errors can arise from using single-epoch X-ray data to derive L/L_Edd values for obscured AGNs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1407.3974v1-abstract-full').style.display = 'none'; document.getElementById('1407.3974v1-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 July, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2014. </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/1407.1844">arXiv:1407.1844</a> <span> [<a href="https://arxiv.org/pdf/1407.1844">pdf</a>, <a href="https://arxiv.org/ps/1407.1844">ps</a>, <a href="https://arxiv.org/format/1407.1844">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> <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/10.1088/0004-637X/792/2/117">10.1088/0004-637X/792/2/117 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> NuSTAR unveils a Compton-thick Type 2 quasar in Mrk 34 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Gandhi%2C+P">P. Gandhi</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">G. B. Lansbury</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/?searchtype=author&query=Ar%C3%A9valo%2C+P">P. Ar茅valo</a>, <a href="/search/?searchtype=author&query=Ballantyne%2C+D+R">D. R. Ballantyne</a>, <a href="/search/?searchtype=author&query=Balokovi%C4%87%2C+M">M. Balokovi膰</a>, <a href="/search/?searchtype=author&query=Bauer%2C+F+E">F. E. Bauer</a>, <a href="/search/?searchtype=author&query=Boggs%2C+S+E">S. E. Boggs</a>, <a href="/search/?searchtype=author&query=Brandt%2C+W+N">W. N. Brandt</a>, <a href="/search/?searchtype=author&query=Brightman%2C+M">M. Brightman</a>, <a href="/search/?searchtype=author&query=Christensen%2C+F+E">F. E. Christensen</a>, <a href="/search/?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/?searchtype=author&query=Craig%2C+W+W">W. W. Craig</a>, <a href="/search/?searchtype=author&query=Del+Moro%2C+A">A. Del Moro</a>, <a href="/search/?searchtype=author&query=Elvis%2C+M">M. Elvis</a>, <a href="/search/?searchtype=author&query=Fabian%2C+A+C">A. C. Fabian</a>, <a href="/search/?searchtype=author&query=Hailey%2C+C+J">C. J. Hailey</a>, <a href="/search/?searchtype=author&query=Harrison%2C+F+A">F. A. Harrison</a>, <a href="/search/?searchtype=author&query=Hickox%2C+R+C">R. C. Hickox</a>, <a href="/search/?searchtype=author&query=Koss%2C+M">M. Koss</a>, <a href="/search/?searchtype=author&query=LaMassa%2C+S+M">S. M. LaMassa</a>, <a href="/search/?searchtype=author&query=Luo%2C+B">B. Luo</a>, <a href="/search/?searchtype=author&query=Madejski%2C+G+M">G. M. Madejski</a>, <a href="/search/?searchtype=author&query=Ptak%2C+A+F">A. F. Ptak</a> , et al. (5 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1407.1844v1-abstract-short" style="display: inline;"> We present Nustar 3-40 keV observations of the optically selected Type 2 quasar (QSO2) SDSS J1034+6001 or Mrk 34. The high-quality hard X-ray spectrum and archival XMM-Newton data can be fitted self-consistently with a reflection-dominated continuum and strong Fe Kalpha fluorescence line with equivalent-width >1 keV. Prior X-ray spectral fitting below 10 keV showed the source to be consistent with… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1407.1844v1-abstract-full').style.display = 'inline'; document.getElementById('1407.1844v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1407.1844v1-abstract-full" style="display: none;"> We present Nustar 3-40 keV observations of the optically selected Type 2 quasar (QSO2) SDSS J1034+6001 or Mrk 34. The high-quality hard X-ray spectrum and archival XMM-Newton data can be fitted self-consistently with a reflection-dominated continuum and strong Fe Kalpha fluorescence line with equivalent-width >1 keV. Prior X-ray spectral fitting below 10 keV showed the source to be consistent with being obscured by Compton-thin column densities of gas along the line-of-sight, despite evidence for much higher columns from multiwavelength data. NuSTAR now enables a direct measurement of this column, and shows that Nh lies in the Compton-thick (CT) regime. The new data also show a high intrinsic 2-10 keV luminosity of L_{2-10}~10^{44} erg/s, in contrast to previous low-energy X-ray measurements for which L_{2-10}<~10^{43} erg/s (i.e. X-ray selection below 10 keV does not pick up this source as an intrinsically luminous obscured quasar). Both the obscuring column and the intrinsic power are about an order of magnitude (or more) larger than inferred from pre-NuSTAR X-ray spectral fitting. Mrk34 is thus a 'gold standard' CT QSO2 and is the nearest non-merging system in this class, in contrast to the other local CT quasar NGC6240 which is currently undergoing a major merger coupled with strong star-formation. For typical X-ray bolometric correction factors, the accretion luminosity of Mrk34 is high enough to potentially power the total infrared luminosity. X-ray spectral fitting also shows that thermal emission related to star-formation is unlikely to drive the observed bright soft component below ~3 keV, favoring photionization instead. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1407.1844v1-abstract-full').style.display = 'none'; document.getElementById('1407.1844v1-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 July, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2014. </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/1403.3078">arXiv:1403.3078</a> <span> [<a href="https://arxiv.org/pdf/1403.3078">pdf</a>, <a href="https://arxiv.org/ps/1403.3078">ps</a>, <a href="https://arxiv.org/format/1403.3078">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/794/2/102">10.1088/0004-637X/794/2/102 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> NuSTAR and XMM-Newton Observations of Luminous, Heavily Obscured, WISE-Selected Quasars at z ~ 2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">G. B. Lansbury</a>, <a href="/search/?searchtype=author&query=Assef%2C+R+J">R. J. Assef</a>, <a href="/search/?searchtype=author&query=Brandt%2C+W+N">W. N. Brandt</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Ballantyne%2C+D+R">D. R. Ballantyne</a>, <a href="/search/?searchtype=author&query=Balokovic%2C+M">M. Balokovic</a>, <a href="/search/?searchtype=author&query=Benford%2C+D">D. Benford</a>, <a href="/search/?searchtype=author&query=Blain%2C+A">A. Blain</a>, <a href="/search/?searchtype=author&query=Boggs%2C+S+E">S. E. Boggs</a>, <a href="/search/?searchtype=author&query=Bridge%2C+C">C. Bridge</a>, <a href="/search/?searchtype=author&query=Brightman%2C+M">M. Brightman</a>, <a href="/search/?searchtype=author&query=Christensen%2C+F+E">F. E. Christensen</a>, <a href="/search/?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/?searchtype=author&query=Craig%2C+W+W">W. W. Craig</a>, <a href="/search/?searchtype=author&query=Del+Moro%2C+A">A. Del Moro</a>, <a href="/search/?searchtype=author&query=Eisenhardt%2C+P+R+M">P. R. M. Eisenhardt</a>, <a href="/search/?searchtype=author&query=Gandhi%2C+P">P. Gandhi</a>, <a href="/search/?searchtype=author&query=Griffith%2C+R">R. Griffith</a>, <a href="/search/?searchtype=author&query=Hailey%2C+C+J">C. J. Hailey</a>, <a href="/search/?searchtype=author&query=Harrison%2C+F+A">F. A. Harrison</a>, <a href="/search/?searchtype=author&query=Hickox%2C+R+C">R. C. Hickox</a>, <a href="/search/?searchtype=author&query=Jarrett%2C+T+H">T. H. Jarrett</a>, <a href="/search/?searchtype=author&query=Koss%2C+M">M. Koss</a>, <a href="/search/?searchtype=author&query=Lake%2C+S">S. Lake</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="1403.3078v1-abstract-short" style="display: inline;"> We report on a NuSTAR and XMM-Newton program that has observed a sample of three extremely luminous, heavily obscured WISE-selected AGN at z~2 in a broad X-ray band (0.1 - 79 keV). The parent sample, selected to be faint or undetected in the WISE 3.4um (W1) and 4.6um (W2) bands but bright at 12um (W3) and 22um (W4), are extremely rare, with only ~1000 so-called W1W2-dropouts across the extragalact… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1403.3078v1-abstract-full').style.display = 'inline'; document.getElementById('1403.3078v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1403.3078v1-abstract-full" style="display: none;"> We report on a NuSTAR and XMM-Newton program that has observed a sample of three extremely luminous, heavily obscured WISE-selected AGN at z~2 in a broad X-ray band (0.1 - 79 keV). The parent sample, selected to be faint or undetected in the WISE 3.4um (W1) and 4.6um (W2) bands but bright at 12um (W3) and 22um (W4), are extremely rare, with only ~1000 so-called W1W2-dropouts across the extragalactic sky. Optical spectroscopy reveals typical redshifts of z~2 for this population, implying rest-frame mid-IR luminosities of L(6um)~6e46 erg/s and bolometric luminosities that can exceed L(bol)~1e14 L(sun). The corresponding intrinsic, unobscured hard X-ray luminosities are L(2-10)~4e45 erg/s for typical quasar templates. These are amongst the most luminous AGN known, though the optical spectra rarely show evidence of a broad-line region and the selection criteria imply heavy obscuration even at rest-frame 1.5um. We designed our X-ray observations to obtain robust detections for gas column densities N(H)<1e24 /cm2. In fact, the sources prove to be fainter than these predictions. Two of the sources were observed by both NuSTAR and XMM-Newton, with neither being detected by NuSTAR and one being faintly detected by XMM-Newton. A third source was observed only with XMM-Newton, yielding a faint detection. The X-ray data require gas column densities N(H)>1e24 /cm2, implying the sources are extremely obscured, consistent with Compton-thick, luminous quasars. The discovery of a significant population of heavily obscured, extremely luminous AGN does not conform to the standard paradigm of a receding torus, in which more luminous quasars are less likely to be obscured. If a larger sample conforms with this finding, then this suggests an additional source of obscuration for these extreme sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1403.3078v1-abstract-full').style.display = 'none'; document.getElementById('1403.3078v1-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 March, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2014. </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; 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/1403.2491">arXiv:1403.2491</a> <span> [<a href="https://arxiv.org/pdf/1403.2491">pdf</a>, <a href="https://arxiv.org/format/1403.2491">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/786/1/16">10.1088/0004-637X/786/1/16 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> NuSTAR J033202-2746.8: direct constraints on the Compton reflection in a heavily obscured quasar at z~2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Del+Moro%2C+A">A. Del Moro</a>, <a href="/search/?searchtype=author&query=Mullaney%2C+J+R">J. R. Mullaney</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/?searchtype=author&query=Bauer%2C+F+E">F. E. Bauer</a>, <a href="/search/?searchtype=author&query=Treister%2C+E">E. Treister</a>, <a href="/search/?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/?searchtype=author&query=Civano%2C+F">F. Civano</a>, <a href="/search/?searchtype=author&query=Ranalli%2C+P">P. Ranalli</a>, <a href="/search/?searchtype=author&query=Vignali%2C+C">C. Vignali</a>, <a href="/search/?searchtype=author&query=Aird%2C+J+A">J. A. Aird</a>, <a href="/search/?searchtype=author&query=Ballantyne%2C+D+R">D. R. Ballantyne</a>, <a href="/search/?searchtype=author&query=Balokovi%C4%87%2C+M">M. Balokovi膰</a>, <a href="/search/?searchtype=author&query=Boggs%2C+S+E">S. E. Boggs</a>, <a href="/search/?searchtype=author&query=Brandt%2C+W+N">W. N. Brandt</a>, <a href="/search/?searchtype=author&query=Christensen%2C+F+E">F. E. Christensen</a>, <a href="/search/?searchtype=author&query=Craig%2C+W+W">W. W. Craig</a>, <a href="/search/?searchtype=author&query=Gandhi%2C+P">P. Gandhi</a>, <a href="/search/?searchtype=author&query=Gilli%2C+R">R. Gilli</a>, <a href="/search/?searchtype=author&query=Hailey%2C+C+J">C. J. Hailey</a>, <a href="/search/?searchtype=author&query=Harrison%2C+F+A">F. A. Harrison</a>, <a href="/search/?searchtype=author&query=Hickox%2C+R+C">R. C. Hickox</a>, <a href="/search/?searchtype=author&query=LaMassa%2C+S+M">S. M. LaMassa</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">G. B. Lansbury</a>, <a href="/search/?searchtype=author&query=Luo%2C+B">B. Luo</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="1403.2491v1-abstract-short" style="display: inline;"> We report NuSTAR observations of NuSTAR J033202-2746.8, a heavily obscured, radio-loud quasar detected in the Extended Chandra Deep Field-South, the deepest layer of the NuSTAR extragalactic survey (~400 ks, at its deepest). NuSTAR J033202-2746.8 is reliably detected by NuSTAR only at E>8 keV and has a very flat spectral slope in the NuSTAR energy band (Gamma=0.55^{+0.62}_{-0.64}; 3-30 keV). Combi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1403.2491v1-abstract-full').style.display = 'inline'; document.getElementById('1403.2491v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1403.2491v1-abstract-full" style="display: none;"> We report NuSTAR observations of NuSTAR J033202-2746.8, a heavily obscured, radio-loud quasar detected in the Extended Chandra Deep Field-South, the deepest layer of the NuSTAR extragalactic survey (~400 ks, at its deepest). NuSTAR J033202-2746.8 is reliably detected by NuSTAR only at E>8 keV and has a very flat spectral slope in the NuSTAR energy band (Gamma=0.55^{+0.62}_{-0.64}; 3-30 keV). Combining the NuSTAR data with extremely deep observations by Chandra and XMM-Newton (4 Ms and 3 Ms, respectively), we constrain the broad-band X-ray spectrum of NuSTAR J033202-2746.8, indicating that this source is a heavily obscured quasar (N_H=5.6^{+0.9}_{-0.8}x10^23 cm^-2) with luminosity L_{10-40 keV}~6.4x10^44 erg s^-1. Although existing optical and near-infrared (near-IR) data, as well as follow-up spectroscopy with the Keck and VLT telescopes, failed to provide a secure redshift identification for NuSTAR J033202-2746.8, we reliably constrain the redshift z=2.00+/-0.04 from the X-ray spectral features (primarily from the iron K edge). The NuSTAR spectrum shows a significant reflection component (R=0.55^{+0.44}_{-0.37}), which was not constrained by previous analyses of Chandra and XMM-Newton data alone. The measured reflection fraction is higher than the R~0 typically observed in bright radio-loud quasars such as NuSTAR J033202-2746.8, which has L_{1.4 GHz}~10^27 W Hz^-1. Constraining the spectral shape of AGN, including bright quasars, is very important for understanding the AGN population, and can have a strong impact on the modeling of the X-ray background. Our results show the importance of NuSTAR in investigating the broad-band spectral properties of quasars out to high redshift. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1403.2491v1-abstract-full').style.display = 'none'; document.getElementById('1403.2491v1-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 March, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 5 figures; 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/1402.2666">arXiv:1402.2666</a> <span> [<a href="https://arxiv.org/pdf/1402.2666">pdf</a>, <a href="https://arxiv.org/format/1402.2666">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/10.1088/0004-637X/785/1/17">10.1088/0004-637X/785/1/17 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> NuSTAR Observations of Heavily Obscured Quasars at z ~ 0.5 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">G. B. Lansbury</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Del+Moro%2C+A">A. Del Moro</a>, <a href="/search/?searchtype=author&query=Gandhi%2C+P">P. Gandhi</a>, <a href="/search/?searchtype=author&query=Assef%2C+R+J">R. J. Assef</a>, <a href="/search/?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/?searchtype=author&query=Aird%2C+J">J. Aird</a>, <a href="/search/?searchtype=author&query=Ballantyne%2C+D+R">D. R. Ballantyne</a>, <a href="/search/?searchtype=author&query=Balokovic%2C+M">M. Balokovic</a>, <a href="/search/?searchtype=author&query=Bauer%2C+F+E">F. E. Bauer</a>, <a href="/search/?searchtype=author&query=Boggs%2C+S+E">S. E. Boggs</a>, <a href="/search/?searchtype=author&query=Brandt%2C+W+N">W. N. Brandt</a>, <a href="/search/?searchtype=author&query=Christensen%2C+F+E">F. E. Christensen</a>, <a href="/search/?searchtype=author&query=Craig%2C+W+W">W. W. Craig</a>, <a href="/search/?searchtype=author&query=Elvis%2C+M">M. Elvis</a>, <a href="/search/?searchtype=author&query=Grefenstette%2C+B+W">B. W. Grefenstette</a>, <a href="/search/?searchtype=author&query=Hailey%2C+C+J">C. J. Hailey</a>, <a href="/search/?searchtype=author&query=Harrison%2C+F+A">F. A. Harrison</a>, <a href="/search/?searchtype=author&query=Hickox%2C+R+C">R. C. Hickox</a>, <a href="/search/?searchtype=author&query=Koss%2C+M">M. Koss</a>, <a href="/search/?searchtype=author&query=LaMassa%2C+S+M">S. M. LaMassa</a>, <a href="/search/?searchtype=author&query=Luo%2C+B">B. Luo</a>, <a href="/search/?searchtype=author&query=Mullaney%2C+J+R">J. R. Mullaney</a>, <a href="/search/?searchtype=author&query=Teng%2C+S+H">S. H. Teng</a>, <a href="/search/?searchtype=author&query=Urry%2C+C+M">C. M. Urry</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="1402.2666v1-abstract-short" style="display: inline;"> We present NuSTAR hard X-ray (3-79 keV) observations of three Type 2 quasars at z ~ 0.4-0.5, optically selected from the Sloan Digital Sky Survey (SDSS). Although the quasars show evidence for being heavily obscured Compton-thick systems on the basis of the 2-10 keV to [OIII] luminosity ratio and multiwavelength diagnostics, their X-ray absorbing column densities (N_H) are poorly known. In this an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1402.2666v1-abstract-full').style.display = 'inline'; document.getElementById('1402.2666v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1402.2666v1-abstract-full" style="display: none;"> We present NuSTAR hard X-ray (3-79 keV) observations of three Type 2 quasars at z ~ 0.4-0.5, optically selected from the Sloan Digital Sky Survey (SDSS). Although the quasars show evidence for being heavily obscured Compton-thick systems on the basis of the 2-10 keV to [OIII] luminosity ratio and multiwavelength diagnostics, their X-ray absorbing column densities (N_H) are poorly known. In this analysis: (1) we study X-ray emission at >10 keV, where X-rays from the central black hole are relatively unabsorbed, in order to better constrain N_H; (2) we further characterize the physical properties of the sources through broad-band near-UV to mid-IR spectral energy distribution (SED) analyses. One of the quasars is detected with NuSTAR at >8 keV with a no-source probability of <0.1%, and its X-ray band ratio suggests near Compton-thick absorption with N_H \gtrsim 5 x 10^23 cm^-2. The other two quasars are undetected, and have low X-ray to mid-IR luminosity ratios in both the low energy (2-10 keV) and high energy (10-40 keV) X-ray regimes that are consistent with extreme, Compton-thick absorption (N_H \gtrsim 10^24 cm^-2). We find that for quasars at z ~ 0.5, NuSTAR provides a significant improvement compared to lower energy (<10 keV) Chandra and XMM-Newton observations alone, as higher column densities can now be directly constrained. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1402.2666v1-abstract-full').style.display = 'none'; document.getElementById('1402.2666v1-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 February, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 6 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/1402.0661">arXiv:1402.0661</a> <span> [<a href="https://arxiv.org/pdf/1402.0661">pdf</a>, <a href="https://arxiv.org/format/1402.0661">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/783/2/122">10.1088/0004-637X/783/2/122 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The AllWISE Motion Survey and The Quest for Cold Subdwarfs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kirkpatrick%2C+J+D">J. Davy Kirkpatrick</a>, <a href="/search/?searchtype=author&query=Schneider%2C+A">Adam Schneider</a>, <a href="/search/?searchtype=author&query=Fajardo-Acosta%2C+S">Sergio Fajardo-Acosta</a>, <a href="/search/?searchtype=author&query=Gelino%2C+C+R">Christopher R. Gelino</a>, <a href="/search/?searchtype=author&query=Mace%2C+G+N">Gregory N. Mace</a>, <a href="/search/?searchtype=author&query=Wright%2C+E+L">Edward L. Wright</a>, <a href="/search/?searchtype=author&query=Logsdon%2C+S+E">Sarah E. Logsdon</a>, <a href="/search/?searchtype=author&query=McLean%2C+I+S">Ian S. McLean</a>, <a href="/search/?searchtype=author&query=Cushing%2C+M+C">Michael C. Cushing</a>, <a href="/search/?searchtype=author&query=Skrutskie%2C+M+F">Michael F. Skrutskie</a>, <a href="/search/?searchtype=author&query=Eisenhardt%2C+P+R">Peter R. Eisenhardt</a>, <a href="/search/?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/?searchtype=author&query=Balokovic%2C+M">Mislav Balokovic</a>, <a href="/search/?searchtype=author&query=Burgasser%2C+A+J">Adam J. Burgasser</a>, <a href="/search/?searchtype=author&query=Faherty%2C+J+K">Jacqueline K. Faherty</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">George B. Lansbury</a>, <a href="/search/?searchtype=author&query=Rich%2C+J+A">J. A. Rich</a>, <a href="/search/?searchtype=author&query=Skrzypek%2C+N">Nathalie Skrzypek</a>, <a href="/search/?searchtype=author&query=Fowler%2C+J+W">John W. Fowler</a>, <a href="/search/?searchtype=author&query=Cutri%2C+R+M">Roc M. Cutri</a>, <a href="/search/?searchtype=author&query=Masci%2C+F+J">Frank J. Masci</a>, <a href="/search/?searchtype=author&query=Conrow%2C+T">Tim Conrow</a>, <a href="/search/?searchtype=author&query=Grillmair%2C+C+J">Carl J. Grillmair</a>, <a href="/search/?searchtype=author&query=McCallon%2C+H+L">Howard L. McCallon</a>, <a href="/search/?searchtype=author&query=Beichman%2C+C+A">Charles A. Beichman</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="1402.0661v1-abstract-short" style="display: inline;"> The AllWISE processing pipeline has measured motions for all objects detected on WISE images taken between 2010 January and 2011 February. In this paper, we discuss new capabilities made to the software pipeline in order to make motion measurements possible, and we characterize the resulting data products for use by future researchers. Using a stringent set of selection criteria, we find 22,445 ob… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1402.0661v1-abstract-full').style.display = 'inline'; document.getElementById('1402.0661v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1402.0661v1-abstract-full" style="display: none;"> The AllWISE processing pipeline has measured motions for all objects detected on WISE images taken between 2010 January and 2011 February. In this paper, we discuss new capabilities made to the software pipeline in order to make motion measurements possible, and we characterize the resulting data products for use by future researchers. Using a stringent set of selection criteria, we find 22,445 objects that have significant AllWISE motions, of which 3,525 have motions that can be independently confirmed from earlier 2MASS images yet lack any published motions in SIMBAD. Another 58 sources lack 2MASS counterparts and are presented as motion candidates only. Limited spectroscopic follow-up of this list has already revealed eight new L subdwarfs. These may provide the first hints of a "subdwarf gap" at mid-L types that would indicate the break between the stellar and substellar populations at low metallicities (i.e., old ages). Another object in the motion list -- WISEA J154045.67-510139.3 -- is a bright (J ~ 9 mag) object of type M6; both the spectrophotometric distance and a crude preliminary parallax place it ~6 pc from the Sun. We also compare our list of motion objects to the recently published list of 762 WISE motion objects from Luhman (2014). While these first large motion studies with WISE data have been very successful in revealing previously overlooked nearby dwarfs, both studies missed objects that the other found, demonstrating that many other nearby objects likely await discovery in the AllWISE data products. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1402.0661v1-abstract-full').style.display = 'none'; document.getElementById('1402.0661v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 February, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2014. </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. Table 3 is a machine-readable ASCII file</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1401.3775">arXiv:1401.3775</a> <span> [<a href="https://arxiv.org/pdf/1401.3775">pdf</a>, <a href="https://arxiv.org/format/1401.3775">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div 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/stu049">10.1093/mnras/stu049 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Barred S0 Galaxies in the Coma Cluster </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">George B. Lansbury</a>, <a href="/search/?searchtype=author&query=Lucey%2C+J+R">John R. Lucey</a>, <a href="/search/?searchtype=author&query=Smith%2C+R+J">Russell J. Smith</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="1401.3775v1-abstract-short" style="display: inline;"> This study uses r-band images from the Eighth Data Release of the Sloan Digital Sky Survey (SDSS DR8) to study bars in lenticular (S0) galaxies in one of the nearest rich cluster environments, the Coma cluster. We develop techniques for bar detection, and assess their success when applied to SDSS image data. To detect and characterise bars we perform 2D bulge+disk+bar light decompositions of galax… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1401.3775v1-abstract-full').style.display = 'inline'; document.getElementById('1401.3775v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1401.3775v1-abstract-full" style="display: none;"> This study uses r-band images from the Eighth Data Release of the Sloan Digital Sky Survey (SDSS DR8) to study bars in lenticular (S0) galaxies in one of the nearest rich cluster environments, the Coma cluster. We develop techniques for bar detection, and assess their success when applied to SDSS image data. To detect and characterise bars we perform 2D bulge+disk+bar light decompositions of galaxy images with GALFIT. Using a sample of artificial galaxy images we determine the faintest magnitude at which bars can be successfully measured at the depth and resolution of SDSS. We perform detailed decompositions of 83 S0 galaxies in Coma, 64 from a central sample, and 19 from a cluster outskirts sample. For the central sample, the S0 bar fraction is 72^{+5}_{-6}%. This value is significantly higher than that obtained using an ellipse fitting method for bar detection, 48^{+6}_{-6}%. At a fixed luminosity, barred S0s are redder in (g-r) colour than unbarred S0s by 0.02 mag. The frequency and strength of bars increase towards fainter luminosities. Neither central metallicity nor stellar age distributions differ significantly between barred and unbarred S0s. There is an increase in the bar fraction towards the cluster core, but this is at a low significance level. Bars have at most a weak correlation with cluster-centric radius. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1401.3775v1-abstract-full').style.display = 'none'; document.getElementById('1401.3775v1-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 January, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2014. </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, 14 figures, 4 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/1307.1733">arXiv:1307.1733</a> <span> [<a href="https://arxiv.org/pdf/1307.1733">pdf</a>, <a href="https://arxiv.org/ps/1307.1733">ps</a>, <a href="https://arxiv.org/format/1307.1733">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/10.1088/0004-637X/773/2/125">10.1088/0004-637X/773/2/125 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The NuSTAR Extragalactic Survey: A First Sensitive Look at the High-Energy Cosmic X-ray Background Population </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/?searchtype=author&query=Del+Moro%2C+A">A. Del Moro</a>, <a href="/search/?searchtype=author&query=Lansbury%2C+G+B">G. B. Lansbury</a>, <a href="/search/?searchtype=author&query=Assef%2C+R+J">R. J. Assef</a>, <a href="/search/?searchtype=author&query=Aird%2C+J">J. Aird</a>, <a href="/search/?searchtype=author&query=Ajello%2C+M">M. Ajello</a>, <a href="/search/?searchtype=author&query=Ballantyne%2C+D+R">D. R. Ballantyne</a>, <a href="/search/?searchtype=author&query=Bauer%2C+F+E">F. E. Bauer</a>, <a href="/search/?searchtype=author&query=Boggs%2C+S+E">S. E. Boggs</a>, <a href="/search/?searchtype=author&query=Brandt%2C+W+N">W. N. Brandt</a>, <a href="/search/?searchtype=author&query=Christensen%2C+F+E">F. E. Christensen</a>, <a href="/search/?searchtype=author&query=Civano%2C+F">F. Civano</a>, <a href="/search/?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/?searchtype=author&query=Craig%2C+W+W">W. W. Craig</a>, <a href="/search/?searchtype=author&query=Elvis%2C+M">M. Elvis</a>, <a href="/search/?searchtype=author&query=Grefenstette%2C+B+W">B. W. Grefenstette</a>, <a href="/search/?searchtype=author&query=Hailey%2C+C+J">C. J. Hailey</a>, <a href="/search/?searchtype=author&query=Harrison%2C+F+A">F. A. Harrison</a>, <a href="/search/?searchtype=author&query=Hickox%2C+R+C">R. C. Hickox</a>, <a href="/search/?searchtype=author&query=Luo%2C+B">B. Luo</a>, <a href="/search/?searchtype=author&query=Madsen%2C+K+K">K. K. Madsen</a>, <a href="/search/?searchtype=author&query=Mullaney%2C+J+R">J. R. Mullaney</a>, <a href="/search/?searchtype=author&query=Perri%2C+M">M. Perri</a>, <a href="/search/?searchtype=author&query=Puccetti%2C+S">S. Puccetti</a> , et al. (9 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1307.1733v1-abstract-short" style="display: inline;"> We report on the first ten identifications of sources serendipitously detected by the NuSTAR to provide the first sensitive census of the cosmic X-ray background (CXB) source population at >10 keV. We find that these NuSTAR-detected sources are ~100x fainter than those previously detected at >10 keV and have a broad range in redshift and luminosity (z=0.020-2.923 and L_10-40 keV~4x10^{41}-5x10^{45… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1307.1733v1-abstract-full').style.display = 'inline'; document.getElementById('1307.1733v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1307.1733v1-abstract-full" style="display: none;"> We report on the first ten identifications of sources serendipitously detected by the NuSTAR to provide the first sensitive census of the cosmic X-ray background (CXB) source population at >10 keV. We find that these NuSTAR-detected sources are ~100x fainter than those previously detected at >10 keV and have a broad range in redshift and luminosity (z=0.020-2.923 and L_10-40 keV~4x10^{41}-5x10^{45} erg/s); the median redshift and luminosity are z~0.7 and L_10-40 keV~3x10^{44} erg/s, respectively. We characterize these sources on the basis of broad-band ~0.5-32 keV spectroscopy, optical spectroscopy, and broad-band ultraviolet-to-mid-infrared SED analyzes. We find that the dominant source population is quasars with L_10-40 keV>10^{44} erg/s, of which ~50% are obscured with N_H>10^{22} cm^{-2}. However, none of the ten NuSTAR sources are Compton thick (N_H>10^{24} cm^{-2}) and we place a 90% confidence upper limit on the fraction of Compton-thick quasars (L_10-40 keV>10^{44} erg/s) selected at >10 keV of ~33% over the redshift range z=0.5-1.1. We jointly fitted the rest-frame ~10-40 keV data for all of the non-beamed sources with L_10-40 keV>10^{43} erg/s to constrain the average strength of reflection; we find R<1.4 for 螕=1.8, broadly consistent with that found for local AGNs observed at >10 keV. We also constrain the host galaxy masses and find a median stellar mass of ~10^{11} M_sun, a factor ~5 times higher than the median stellar mass of nearby high-energy selected AGNs, which may be at least partially driven by the order of magnitude higher X-ray luminosities of the NuSTAR sources. Within the low source-statistic limitations of our study, our results suggest that the overall properties of the NuSTAR sources are broadly similar to those of nearby high-energy selected AGNs but scaled up in luminosity and mass. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1307.1733v1-abstract-full').style.display = 'none'; document.getElementById('1307.1733v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 July, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2013. </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; 22 pages, 12 figures, 5 tables</span> </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a 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