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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/2402.13508">arXiv:2402.13508</a> <span> [<a href="https://arxiv.org/pdf/2402.13508">pdf</a>, <a href="https://arxiv.org/format/2402.13508">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/ad2b61">10.3847/1538-4357/ad2b61 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> PEARLS: NuSTAR and XMM-Newton Extragalactic Survey of the JWST North Ecliptic Pole Time-Domain Field II </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Zhao%2C+X">Xiurui Zhao</a>, <a href="/search/?searchtype=author&query=Civano%2C+F">Francesca Civano</a>, <a href="/search/?searchtype=author&query=Willmer%2C+C+N+A">Christopher N. A. Willmer</a>, <a href="/search/?searchtype=author&query=Bonoli%2C+S">Silvia Bonoli</a>, <a href="/search/?searchtype=author&query=Chen%2C+C">Chien-Ting Chen</a>, <a href="/search/?searchtype=author&query=Creech%2C+S">Samantha Creech</a>, <a href="/search/?searchtype=author&query=Dupke%2C+R">Renato Dupke</a>, <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</a>, <a href="/search/?searchtype=author&query=Jansen%2C+R+A">Rolf A. Jansen</a>, <a href="/search/?searchtype=author&query=Kikuta%2C+S">Satoshi Kikuta</a>, <a href="/search/?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/?searchtype=author&query=Laha%2C+S">Sibasish Laha</a>, <a href="/search/?searchtype=author&query=Marchesi%2C+S">Stefano Marchesi</a>, <a href="/search/?searchtype=author&query=O%27Brien%2C+R">Rosalia O'Brien</a>, <a href="/search/?searchtype=author&query=Silver%2C+R">Ross Silver</a>, <a href="/search/?searchtype=author&query=Willner%2C+S+P">S. P. Willner</a>, <a href="/search/?searchtype=author&query=Windhorst%2C+R+A">Rogier A. Windhorst</a>, <a href="/search/?searchtype=author&query=Yan%2C+H">Haojing Yan</a>, <a href="/search/?searchtype=author&query=Alcaniz%2C+J">Jailson Alcaniz</a>, <a href="/search/?searchtype=author&query=Benitez%2C+N">Narciso Benitez</a>, <a href="/search/?searchtype=author&query=Carneiro%2C+S">Saulo Carneiro</a>, <a href="/search/?searchtype=author&query=Cenarro%2C+J">Javier Cenarro</a>, <a href="/search/?searchtype=author&query=Crist%C3%B3bal-Hornillos%2C+D">David Crist贸bal-Hornillos</a>, <a href="/search/?searchtype=author&query=Ederoclite%2C+A">Alessandro Ederoclite</a>, <a href="/search/?searchtype=author&query=Hern%C3%A1n-Caballero%2C+A">Antonio Hern谩n-Caballero</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="2402.13508v2-abstract-short" style="display: inline;"> We present the second NuSTAR and XMM-Newton extragalactic survey of the JWST North Ecliptic Pole (NEP) Time-Domain Field (TDF). The first NuSTAR NEP-TDF survey (Zhao et al. 2021) had 681 ks total exposure time executed in NuSTAR cycle 5, in 2019 and 2020. This second survey, acquired from 2020 to 2022 in cycle 6, adds 880 ks of NuSTAR exposure time. The overall NuSTAR NEP-TDF survey is the most se… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.13508v2-abstract-full').style.display = 'inline'; document.getElementById('2402.13508v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.13508v2-abstract-full" style="display: none;"> We present the second NuSTAR and XMM-Newton extragalactic survey of the JWST North Ecliptic Pole (NEP) Time-Domain Field (TDF). The first NuSTAR NEP-TDF survey (Zhao et al. 2021) had 681 ks total exposure time executed in NuSTAR cycle 5, in 2019 and 2020. This second survey, acquired from 2020 to 2022 in cycle 6, adds 880 ks of NuSTAR exposure time. The overall NuSTAR NEP-TDF survey is the most sensitive NuSTAR extragalactic survey to date, and a total of 60 sources were detected above the 95% reliability threshold. We constrain the hard X-ray number counts, logN-log S, down to 1.7 x 10$^{-14}$ erg cm$^{-2}$ s$^{-1}$ at 8-24 keV and detect an excess of hard X-ray sources at the faint end. About 47% of the NuSTAR-detected sources are heavily obscured (NH > 10$^{23}$ cm$^{-2}$), and 18+20% of the NuSTAR-detected sources are Compton-thick (N>10$^{24}$ cm$^{-2}$). These fractions are consistent with those measured in other NuSTAR surveys. Four sources presented >2$蟽$ variability in the 3-year survey. In addition to NuSTAR, a total of 62 ks of XMM-Newton observations were taken during NuSTAR cycle 6. The XMM-Newton observations provide soft X-ray (0.5-10keV) coverage in the same field and enable more robust identification of the visible and infrared counterparts of the NuSTAR-detected sources. A total of 286 soft X-ray sources were detected, out of which 214 XMM-Newton sources have secure counterparts from multiwavelength catalogs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.13508v2-abstract-full').style.display = 'none'; document.getElementById('2402.13508v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">37 pages, 27 figures, Accepted by ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 965, 188 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.02645">arXiv:2308.02645</a> <span> [<a href="https://arxiv.org/pdf/2308.02645">pdf</a>, <a href="https://arxiv.org/format/2308.02645">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> High-mass X-ray Binaries </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</a>, <a href="/search/?searchtype=author&query=Antoniou%2C+V">Vallia Antoniou</a>, <a href="/search/?searchtype=author&query=Dubus%2C+G">Guillaume Dubus</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2308.02645v1-abstract-short" style="display: inline;"> Binary systems in which a neutron star or black hole accretes material from a high-mass star are known as high-mass X-ray binaries (HMXBs). This chapter provides a brief introduction to the physics of wind accretion and an observational view of HMXBs, including their classification, X-ray spectra, X-ray variability, orbital and compact object properties, as well as studies of Galactic and Magellan… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.02645v1-abstract-full').style.display = 'inline'; document.getElementById('2308.02645v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.02645v1-abstract-full" style="display: none;"> Binary systems in which a neutron star or black hole accretes material from a high-mass star are known as high-mass X-ray binaries (HMXBs). This chapter provides a brief introduction to the physics of wind accretion and an observational view of HMXBs, including their classification, X-ray spectra, X-ray variability, orbital and compact object properties, as well as studies of Galactic and Magellanic HMXB populations. Two classes of X-ray sources whose possible connections to HMXBs have been debated, ultraluminous X-ray sources and gamma-ray binaries, are also discussed. Approximately 300 HMXBs residing either in the Milky Way or the Magellanic Clouds have been discovered. The majority of these HMXBs host wind-accreting neutron stars. Their X-ray properties depend both on the interaction of the accreting material with the neutron star's strong magnetic field and the properties of the donor star's wind. Most HMXBs are classified as either supergiant XBs or Be XBs based on the spectral type of the donor star; these classes exhibit different patterns of X-ray variability and occupy different phase space in diagrams of neutron star spin versus orbital period. While studies of HMXBs in the Milky Way and Magellanic Clouds find that their luminosity functions have similar shapes, an overabundance of Be XBs in the Small Magellanic Cloud points to important variations of the HMXB population with metallicity and age. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.02645v1-abstract-full').style.display = 'none'; document.getElementById('2308.02645v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Invited chapter for Handbook of X-ray and Gamma-ray Astrophysics, 44 pages of text, 11 pages of references, 18 figures, 1 table</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.04691">arXiv:2306.04691</a> <span> [<a href="https://arxiv.org/pdf/2306.04691">pdf</a>, <a href="https://arxiv.org/format/2306.04691">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stad1729">10.1093/mnras/stad1729 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Classifying IGR J15038-6021 as a magnetic CV with a massive white dwarf </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=Kumar%2C+S+G">Snehaa Ganesh Kumar</a>, <a href="/search/?searchtype=author&query=Coughenour%2C+B+M">Benjamin M. Coughenour</a>, <a href="/search/?searchtype=author&query=Shaw%2C+A+W">Aarran W. Shaw</a>, <a href="/search/?searchtype=author&query=Mukai%2C+K">Koji Mukai</a>, <a href="/search/?searchtype=author&query=Hare%2C+J">Jeremy Hare</a>, <a href="/search/?searchtype=author&query=Clavel%2C+M">Maica Clavel</a>, <a href="/search/?searchtype=author&query=Krivonos%2C+R">Roman Krivonos</a>, <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</a>, <a href="/search/?searchtype=author&query=Gerber%2C+J">Julian Gerber</a>, <a href="/search/?searchtype=author&query=Joens%2C+A">Alyson Joens</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.04691v1-abstract-short" style="display: inline;"> Cataclysmic variables (CVs) are binary systems consisting of a white dwarf (WD) accreting matter from a companion star. Observations of CVs provide an opportunity to learn about accretion disks, the physics of compact objects, classical novae, and the evolution of the binary and the WD that may ultimately end in a type Ia supernova (SN). As type Ia SNe involve a WD reaching the Chandrasekhar limit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.04691v1-abstract-full').style.display = 'inline'; document.getElementById('2306.04691v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.04691v1-abstract-full" style="display: none;"> Cataclysmic variables (CVs) are binary systems consisting of a white dwarf (WD) accreting matter from a companion star. Observations of CVs provide an opportunity to learn about accretion disks, the physics of compact objects, classical novae, and the evolution of the binary and the WD that may ultimately end in a type Ia supernova (SN). As type Ia SNe involve a WD reaching the Chandrasekhar limit or merging WDs, WD mass measurements are particularly important for elucidating the path from CV to type Ia SN. For intermediate polar (IP) type CVs, the WD mass is related to the bremsstrahlung temperature of material in the accretion column, which typically peaks at X-ray energies. Thus, the IPs with the strongest hard X-ray emission, such as those discovered by the INTEGRAL satellite, are expected to have the highest masses. Here, we report on XMM-Newton, NuSTAR, and optical observations of IGR J15038-6021. We find an X-ray periodicity of 1678+/-2s, which we interpret as the WD spin period. From fitting the 0.3-79 keV spectrum with a model that uses the relationship between the WD mass and the post-shock temperature, we measure a WD mass of 1.36+0.04-0.11 Msun. This follows an earlier study of IGR J14091-6108, which also has a WD with a mass approaching the Chandrasekhar limit. We demonstrate that these are both outliers among IPs in having massive WDs and discuss the results in the context of WD mass studies as well as the implications for WD mass evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.04691v1-abstract-full').style.display = 'none'; document.getElementById('2306.04691v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">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/2206.14812">arXiv:2206.14812</a> <span> [<a href="https://arxiv.org/pdf/2206.14812">pdf</a>, <a href="https://arxiv.org/format/2206.14812">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/stac2402">10.1093/mnras/stac2402 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MOSDEF Survey: Towards a Complete Census of the z ~ 2.3 Star-forming Galaxy Population </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Runco%2C+J+N">Jordan N. Runco</a>, <a href="/search/?searchtype=author&query=Shapley%2C+A+E">Alice E. Shapley</a>, <a href="/search/?searchtype=author&query=Sanders%2C+R+L">Ryan L. Sanders</a>, <a href="/search/?searchtype=author&query=Kriek%2C+M">Mariska Kriek</a>, <a href="/search/?searchtype=author&query=Reddy%2C+N+A">Naveen A. Reddy</a>, <a href="/search/?searchtype=author&query=Coil%2C+A+L">Alison L. Coil</a>, <a href="/search/?searchtype=author&query=Mobasher%2C+B">Bahram Mobasher</a>, <a href="/search/?searchtype=author&query=Siana%2C+B">Brian Siana</a>, <a href="/search/?searchtype=author&query=Topping%2C+M+W">Michael W. Topping</a>, <a href="/search/?searchtype=author&query=Freeman%2C+W+R">William R. Freeman</a>, <a href="/search/?searchtype=author&query=Shivaei%2C+I">Irene Shivaei</a>, <a href="/search/?searchtype=author&query=Azadi%2C+M">Mojegan Azadi</a>, <a href="/search/?searchtype=author&query=Price%2C+S+H">Sedona H. Price</a>, <a href="/search/?searchtype=author&query=Leung%2C+G+C+K">Gene C. K. Leung</a>, <a href="/search/?searchtype=author&query=Fetherolf%2C+T">Tara Fetherolf</a>, <a href="/search/?searchtype=author&query=de+Groot%2C+L">Laura de Groot</a>, <a href="/search/?searchtype=author&query=Zick%2C+T">Tom Zick</a>, <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</a>, <a href="/search/?searchtype=author&query=Barro%2C+G">Guillermo Barro</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2206.14812v2-abstract-short" style="display: inline;"> We analyze the completeness of the MOSDEF survey, in which z ~ 2 galaxies were selected for rest-optical spectroscopy from well-studied HST extragalactic legacy fields down to a fixed rest-optical magnitude limit (H_AB = 24.5). The subset of z ~ 2 MOSDEF galaxies with high signal-to-noise (S/N) emission-line detections analyzed in previous work represents a small minority (<10%) of possible z ~ 2… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.14812v2-abstract-full').style.display = 'inline'; document.getElementById('2206.14812v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.14812v2-abstract-full" style="display: none;"> We analyze the completeness of the MOSDEF survey, in which z ~ 2 galaxies were selected for rest-optical spectroscopy from well-studied HST extragalactic legacy fields down to a fixed rest-optical magnitude limit (H_AB = 24.5). The subset of z ~ 2 MOSDEF galaxies with high signal-to-noise (S/N) emission-line detections analyzed in previous work represents a small minority (<10%) of possible z ~ 2 MOSDEF targets. It is therefore crucial to understand how representative this high S/N subsample is, while also more fully exploiting the MOSDEF spectroscopic sample. Using spectral-energy-distribution (SED) models and rest-optical spectral stacking, we compare the MOSDEF z ~ 2 high S/N subsample with the full MOSDEF sample of z ~ 2 star-forming galaxies with redshifts, the latter representing an increase in sample size of more than a factor of three. We find that both samples have similar emission-line properties, in particular in terms of the magnitude of the offset from the local star-forming sequence on the [N II] BPT diagram. There are small differences in median host galaxy properties, including the stellar mass (M_*), star-formation rate (SFR) and specific SFR (sSFR), and UVJ colors; however, these offsets are minor considering the wide spread of the distributions. Using SED modeling, we also demonstrate that the sample of z ~ 2 star-forming galaxies observed by the MOSDEF survey is representative of the parent catalog of available such targets. We conclude that previous MOSDEF results on the evolution of star-forming galaxy emission-line properties were unbiased relative to the parent z ~ 2 galaxy population. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.14812v2-abstract-full').style.display = 'none'; document.getElementById('2206.14812v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 10 figures, 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/2204.13140">arXiv:2204.13140</a> <span> [<a href="https://arxiv.org/pdf/2204.13140">pdf</a>, <a href="https://arxiv.org/ps/2204.13140">ps</a>, <a href="https://arxiv.org/format/2204.13140">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/ac694d">10.3847/1538-4357/ac694d <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Termination Shocks and the Extended X-ray Emission in MRK 78 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</a>, <a href="/search/?searchtype=author&query=Elvis%2C+M">Martin Elvis</a>, <a href="/search/?searchtype=author&query=Maksym%2C+W+P">W. Peter Maksym</a>, <a href="/search/?searchtype=author&query=Fabbiano%2C+G">Giuseppina Fabbiano</a>, <a href="/search/?searchtype=author&query=Bergmann%2C+T+S">Thaisa Storchi Bergmann</a>, <a href="/search/?searchtype=author&query=Gandhi%2C+P">Poshak Gandhi</a>, <a href="/search/?searchtype=author&query=Whittle%2C+M">Mark Whittle</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="2204.13140v1-abstract-short" style="display: inline;"> Sub-arcsecond imaging of the X-ray emission in the type 2 AGN Mrk 78 with Chandra shows complex structure with spectral variations on scales from $\sim$200 pc to $\sim$ 2 kpc. Overall the X-ray emission is aligned E-W with the radio (3.6 cm) and narrow emission line region as mapped in [OIII], with a marked E-W asymmetry. The Eastern X-ray emission is mostly in a compact knot coincident with the l… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.13140v1-abstract-full').style.display = 'inline'; document.getElementById('2204.13140v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.13140v1-abstract-full" style="display: none;"> Sub-arcsecond imaging of the X-ray emission in the type 2 AGN Mrk 78 with Chandra shows complex structure with spectral variations on scales from $\sim$200 pc to $\sim$ 2 kpc. Overall the X-ray emission is aligned E-W with the radio (3.6 cm) and narrow emission line region as mapped in [OIII], with a marked E-W asymmetry. The Eastern X-ray emission is mostly in a compact knot coincident with the location where the radio source is deflected, while the Western X-ray emission forms a loop or shell $\sim$2 kpc from the nucleus with radius $\sim$0.7 kpc. There is suggestive evidence of shocks in both the Eastern knot and the Western arc. Both these positions coincide with large changes in the velocities of the [OIII] outflow. We discuss possible reasons why the X-ray shocks on the Western side occur $\sim1$ kpc farther out than on the Eastern side. We estimate that the thermal energy injected by the shocks into the interstellar medium corresponds to $0.05-0.6$% of the AGN bolometric luminosity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.13140v1-abstract-full').style.display = 'none'; document.getElementById('2204.13140v1-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 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 14 figures, 6 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/2201.11170">arXiv:2201.11170</a> <span> [<a href="https://arxiv.org/pdf/2201.11170">pdf</a>, <a href="https://arxiv.org/format/2201.11170">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/stac263">10.1093/mnras/stac263 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Classifying IGR J18007-4146 as an intermediate polar using XMM and NuSTAR </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Coughenour%2C+B+M">Benjamin M. Coughenour</a>, <a href="/search/?searchtype=author&query=Tomsick%2C+J+A">John A. Tomsick</a>, <a href="/search/?searchtype=author&query=Shaw%2C+A+W">Aarran W. Shaw</a>, <a href="/search/?searchtype=author&query=Mukai%2C+K">Koji Mukai</a>, <a href="/search/?searchtype=author&query=Clavel%2C+M">Ma茂ca Clavel</a>, <a href="/search/?searchtype=author&query=Hare%2C+J">Jeremy Hare</a>, <a href="/search/?searchtype=author&query=Krivonos%2C+R">Roman Krivonos</a>, <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</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="2201.11170v1-abstract-short" style="display: inline;"> Many new and unidentified Galactic sources have recently been revealed by ongoing hard X-ray surveys. A significant fraction of these have been shown to be the type of accreting white dwarfs known as cataclysmic variables (CVs). Follow-up observations are often required to categorize and classify these sources, and may also identify potentially unique or interesting cases. One such case is IGR J18… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.11170v1-abstract-full').style.display = 'inline'; document.getElementById('2201.11170v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.11170v1-abstract-full" style="display: none;"> Many new and unidentified Galactic sources have recently been revealed by ongoing hard X-ray surveys. A significant fraction of these have been shown to be the type of accreting white dwarfs known as cataclysmic variables (CVs). Follow-up observations are often required to categorize and classify these sources, and may also identify potentially unique or interesting cases. One such case is IGR J18007-4146, which is likely a CV based on follow-up Chandra observations and constraints from optical/IR catalogs. Utilizing simultaneous XMM-Newton and NuSTAR observations, as well as the available optical/IR data, we confirm the nature of IGR J18007-4146 as an intermediate polar type CV. Timing analysis of the XMM data reveals a periodic signal at 424.4 +/- 0.7 s that we interpret as the spin period of the white dwarf. Modeling the 0.3-78 keV spectrum, we use a thermal bremsstrahlung continuum but require intrinsic absorption as well as a soft component and strong Fe lines between 6 and 7 keV. We model the soft component using a single-temperature blackbody with kT = 73 +8/-6 eV. From the X-ray spectrum, we are able to measure the mass of the white dwarf to be 1.06 +0.19/-0.10 Msun, which means IGR J18007-4146 is more massive than the average for magnetic CVs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.11170v1-abstract-full').style.display = 'none'; document.getElementById('2201.11170v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 January, 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">9 pages, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.09715">arXiv:2112.09715</a> <span> [<a href="https://arxiv.org/pdf/2112.09715">pdf</a>, <a href="https://arxiv.org/format/2112.09715">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/stac1115">10.1093/mnras/stac1115 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Reconciling the Results of the z~2 MOSDEF and KBSS-MOSFIRE Surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Runco%2C+J+N">Jordan N. Runco</a>, <a href="/search/?searchtype=author&query=Reddy%2C+N+A">Naveen A. Reddy</a>, <a href="/search/?searchtype=author&query=Shapley%2C+A+E">Alice E. Shapley</a>, <a href="/search/?searchtype=author&query=Steidel%2C+C+C">Charles C. Steidel</a>, <a href="/search/?searchtype=author&query=Sanders%2C+R+L">Ryan L. Sanders</a>, <a href="/search/?searchtype=author&query=Strom%2C+A+L">Allison L. Strom</a>, <a href="/search/?searchtype=author&query=Coil%2C+A+L">Alison L. Coil</a>, <a href="/search/?searchtype=author&query=Kriek%2C+M">Mariska Kriek</a>, <a href="/search/?searchtype=author&query=Mobasher%2C+B">Bahram Mobasher</a>, <a href="/search/?searchtype=author&query=Pettini%2C+M">Max Pettini</a>, <a href="/search/?searchtype=author&query=Rudie%2C+G+C">Gwen C. Rudie</a>, <a href="/search/?searchtype=author&query=Siana%2C+B">Brian Siana</a>, <a href="/search/?searchtype=author&query=Topping%2C+M+W">Michael W. Topping</a>, <a href="/search/?searchtype=author&query=Trainor%2C+R+F">Ryan F. Trainor</a>, <a href="/search/?searchtype=author&query=Freeman%2C+W+R">William R. Freeman</a>, <a href="/search/?searchtype=author&query=Shivaei%2C+I">Irene Shivaei</a>, <a href="/search/?searchtype=author&query=Azadi%2C+M">Mojegan Azadi</a>, <a href="/search/?searchtype=author&query=Price%2C+S+H">Sedona H. Price</a>, <a href="/search/?searchtype=author&query=Leung%2C+G+C+K">Gene C. K. Leung</a>, <a href="/search/?searchtype=author&query=Fetherolf%2C+T">Tara Fetherolf</a>, <a href="/search/?searchtype=author&query=de+Groot%2C+L">Laura de Groot</a>, <a href="/search/?searchtype=author&query=Zick%2C+T">Tom Zick</a>, <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</a>, <a href="/search/?searchtype=author&query=Barro%2C+G">Guillermo Barro</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2112.09715v2-abstract-short" style="display: inline;"> The combination of the MOSDEF and KBSS-MOSFIRE surveys represents the largest joint investment of Keck/MOSFIRE time to date, with ~3000 galaxies at 1.4<=z<=3.8, roughly half of which are at z~2. MOSDEF is photometric- and spectroscopic-redshift selected with a rest-optical magnitude limit, while KBSS-MOSFIRE is primarily selected based on rest-UV colors and a rest-UV magnitude limit. Analyzing bot… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.09715v2-abstract-full').style.display = 'inline'; document.getElementById('2112.09715v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.09715v2-abstract-full" style="display: none;"> The combination of the MOSDEF and KBSS-MOSFIRE surveys represents the largest joint investment of Keck/MOSFIRE time to date, with ~3000 galaxies at 1.4<=z<=3.8, roughly half of which are at z~2. MOSDEF is photometric- and spectroscopic-redshift selected with a rest-optical magnitude limit, while KBSS-MOSFIRE is primarily selected based on rest-UV colors and a rest-UV magnitude limit. Analyzing both surveys in a uniform manner with consistent spectral-energy-distribution (SED) models, we find that the MOSDEF z~2 targeted sample has a higher median M_* and redder rest U-V color than the KBSS-MOSFIRE z~2 targeted sample, and a smaller median SED-based SFR and sSFR (SFR(SED) and sSFR(SED)). Specifically, MOSDEF targeted a larger population of red galaxies with U-V and V-J >=1.25, while KBSS-MOSFIRE contains more young galaxies with intense star formation. Despite these differences in the z~2 targeted samples, the subsets of the surveys with multiple emission lines detected and analyzed in previously published work are much more similar. All median host-galaxy properties with the exception of stellar population age -- i.e., M_*, SFR(SED), sSFR(SED), A_V, and UVJ colors -- agree within the uncertainties. Additionally, when uniform emission-line fitting and stellar Balmer absorption correction techniques are applied, there is no significant offset between the two samples in the [OIII]$位$5008/H$尾$ vs. [NII]$位$6585/H$伪$ diagnostic diagram, in contrast to previously-reported discrepancies. We can now combine the MOSDEF and KBSS-MOSFIRE surveys to form the largest z~2 sample with moderate-resolution rest-optical spectra and construct the fundamental scaling relations of star-forming galaxies during this important epoch. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.09715v2-abstract-full').style.display = 'none'; document.getElementById('2112.09715v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 14 figures, published in MNRAS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> MNRAS, 513, 3871 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.13839">arXiv:2109.13839</a> <span> [<a href="https://arxiv.org/pdf/2109.13839">pdf</a>, <a href="https://arxiv.org/format/2109.13839">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/stab2885">10.1093/mnras/stab2885 <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 of the James Webb Space Telescope North Ecliptic Pole Time-Domain Field </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Zhao%2C+X">X. Zhao</a>, <a href="/search/?searchtype=author&query=Civano%2C+F">F. Civano</a>, <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">F. M. Fornasini</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/?searchtype=author&query=Cappelluti%2C+N">N. Cappelluti</a>, <a href="/search/?searchtype=author&query=Chen%2C+C+T">C. T. Chen</a>, <a href="/search/?searchtype=author&query=Cohen%2C+S+H">S. H. Cohen</a>, <a href="/search/?searchtype=author&query=Elvis%2C+M">M. Elvis</a>, <a href="/search/?searchtype=author&query=Gandhi%2C+P">P. Gandhi</a>, <a href="/search/?searchtype=author&query=Grogin%2C+N+A">N. A. Grogin</a>, <a href="/search/?searchtype=author&query=Hickox%2C+R+C">R. C. Hickox</a>, <a href="/search/?searchtype=author&query=Jansen%2C+R+A">R. A. Jansen</a>, <a href="/search/?searchtype=author&query=Koekemoer%2C+A">A. Koekemoer</a>, <a href="/search/?searchtype=author&query=Lanzuisi%2C+G">G. Lanzuisi</a>, <a href="/search/?searchtype=author&query=Maksym%2C+W+P">W. P. Maksym</a>, <a href="/search/?searchtype=author&query=Masini%2C+A">A. Masini</a>, <a href="/search/?searchtype=author&query=Rosario%2C+D+J">D. J. Rosario</a>, <a href="/search/?searchtype=author&query=Ward%2C+M+J">M. J. Ward</a>, <a href="/search/?searchtype=author&query=Willmer%2C+C+N+A">C. N. A. Willmer</a>, <a href="/search/?searchtype=author&query=Windhorst%2C+R+A">R. A. Windhorst</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2109.13839v2-abstract-short" style="display: inline;"> We present the $NuSTAR$ extragalactic survey of the $James$ $Webb$ $Space$ $Telescope$ ($JWST$) North Ecliptic Pole (NEP) Time-Domain Field. The survey covers a $\sim$0.16 deg$^2$ area with a total exposure of 681 ks acquired in a total of nine observations from three epochs. The survey sensitivities at 20% of the area are 2.39, 1.14, 2.76, 1.52, and 5.20 $\times$ 10$^{-14}$ erg cm$^{-2}$ s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.13839v2-abstract-full').style.display = 'inline'; document.getElementById('2109.13839v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.13839v2-abstract-full" style="display: none;"> We present the $NuSTAR$ extragalactic survey of the $James$ $Webb$ $Space$ $Telescope$ ($JWST$) North Ecliptic Pole (NEP) Time-Domain Field. The survey covers a $\sim$0.16 deg$^2$ area with a total exposure of 681 ks acquired in a total of nine observations from three epochs. The survey sensitivities at 20% of the area are 2.39, 1.14, 2.76, 1.52, and 5.20 $\times$ 10$^{-14}$ erg cm$^{-2}$ s$^{-1}$ in the 3-24, 3-8, 8-24, 8-16, and 16-24 keV bands, respectively. The NEP survey is one of the most sensitive extragalactic surveys with $NuSTAR$ so far. A total of 33 sources were detected above 95% reliability in at least one of the five bands. We present the number counts, log$N$-log$S$, measured in the hard X-ray 8-24 and 8-16 keV bands, uniquely accessible by $NuSTAR$ down to such faint fluxes. We performed source detection on the XMM-$Newton$ and $Chandra$ observations of the same field to search for soft X-ray counterparts of each $NuSTAR$ detection. The soft band positions were used to identify optical and infrared associations. We present the X-ray properties (hardness ratio and luminosity) and optical-to-X-ray properties of the detected sources. The measured fraction of candidate Compton-thick (N$\rm _H\ge10^{24} cm^{-2}$) active galactic nuclei, derived from the hardness ratio, is between 3% to 27%. As this survey was designed to have variability as its primary focus, we present preliminary results on multi-epoch flux variability in the 3-24 keV band. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.13839v2-abstract-full').style.display = 'none'; document.getElementById('2109.13839v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 17 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/2104.09646">arXiv:2104.09646</a> <span> [<a href="https://arxiv.org/pdf/2104.09646">pdf</a>, <a href="https://arxiv.org/format/2104.09646">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/abfa1a">10.3847/1538-4357/abfa1a <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Using Chandra Localizations and Gaia Distances and Proper Motions to Classify Hard X-ray Sources Discovered by INTEGRAL </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=Coughenour%2C+B+M">Benjamin M. Coughenour</a>, <a href="/search/?searchtype=author&query=Hare%2C+J">Jeremy Hare</a>, <a href="/search/?searchtype=author&query=Krivonos%2C+R">Roman Krivonos</a>, <a href="/search/?searchtype=author&query=Bodaghee%2C+A">Arash Bodaghee</a>, <a href="/search/?searchtype=author&query=Chaty%2C+S">Sylvain Chaty</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=Rodriguez%2C+J">Jerome Rodriguez</a>, <a href="/search/?searchtype=author&query=Shaw%2C+A+W">Aarran W. Shaw</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="2104.09646v1-abstract-short" style="display: inline;"> Here we report on X-ray observations of ten 17-60 keV sources discovered by the INTEGRAL satellite. The primary new information is sub-arcsecond positions obtained by the Chandra X-ray Observatory. In six cases (IGR J17040-4305, IGR J18017-3542, IGR J18112-2641, IGR J18434-0508, IGR J19504+3318, and IGR J20084+3221), a unique Chandra counterpart is identified with a high degree of certainty, and f… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.09646v1-abstract-full').style.display = 'inline'; document.getElementById('2104.09646v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.09646v1-abstract-full" style="display: none;"> Here we report on X-ray observations of ten 17-60 keV sources discovered by the INTEGRAL satellite. The primary new information is sub-arcsecond positions obtained by the Chandra X-ray Observatory. In six cases (IGR J17040-4305, IGR J18017-3542, IGR J18112-2641, IGR J18434-0508, IGR J19504+3318, and IGR J20084+3221), a unique Chandra counterpart is identified with a high degree of certainty, and for five of these sources (all but J19504), Gaia distances or proper motions indicate that they are Galactic sources. For four of these, the most likely classifications are that the sources are magnetic Cataclysmic Variables (CVs). J20084 could be either a magnetic CV or a High Mass X-ray Binary. We classify the sixth source (J19504) as a likely Active Galactic Nucleus (AGN). In addition, we find likely Chandra counterparts to IGR J18010-3045 and IGR J19577+3339, and the latter is a bright radio source and probable AGN. The other two sources, IGR J12529-6351 and IGR J18013-3222 do not have likely Chandra counterparts, indicating that they are transient, highly variable, or highly absorbed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.09646v1-abstract-full').style.display = 'none'; document.getElementById('2104.09646v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 9 tables, 4 figures, accepted by ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2103.09245">arXiv:2103.09245</a> <span> [<a href="https://arxiv.org/pdf/2103.09245">pdf</a>, <a href="https://arxiv.org/format/2103.09245">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/stab1793">10.1093/mnras/stab1793 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MOSDEF Survey: The Mass-Metallicity relationship and the existence of the FMR at z~1.5 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Topping%2C+M+W">Michael W. Topping</a>, <a href="/search/?searchtype=author&query=Shapley%2C+A+E">Alice E. Shapley</a>, <a href="/search/?searchtype=author&query=Sanders%2C+R+L">Ryan L. Sanders</a>, <a href="/search/?searchtype=author&query=Kriek%2C+M">Mariska Kriek</a>, <a href="/search/?searchtype=author&query=Reddy%2C+N+A">Naveen A. Reddy</a>, <a href="/search/?searchtype=author&query=Coil%2C+A+L">Alison L. Coil</a>, <a href="/search/?searchtype=author&query=Mobasher%2C+B">Bahram Mobasher</a>, <a href="/search/?searchtype=author&query=Siana%2C+B">Brian Siana</a>, <a href="/search/?searchtype=author&query=Freeman%2C+W+R">William R. Freeman</a>, <a href="/search/?searchtype=author&query=Shivaei%2C+I">Irene Shivaei</a>, <a href="/search/?searchtype=author&query=Azadi%2C+M">Mojegan Azadi</a>, <a href="/search/?searchtype=author&query=Price%2C+S+H">Sedona H. Price</a>, <a href="/search/?searchtype=author&query=Leung%2C+G+C+K">Gene C. K. Leung</a>, <a href="/search/?searchtype=author&query=Fetherolf%2C+T">Tara Fetherolf</a>, <a href="/search/?searchtype=author&query=de+Groot%2C+L">Laura de Groot</a>, <a href="/search/?searchtype=author&query=Zick%2C+T">Tom Zick</a>, <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</a>, <a href="/search/?searchtype=author&query=Barro%2C+G">Guillermo Barro</a>, <a href="/search/?searchtype=author&query=Runco%2C+J+N">Jordan N. Runco</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="2103.09245v2-abstract-short" style="display: inline;"> We analyze the rest-optical emission-line ratios of z~1.5 galaxies drawn from the MOSFIRE Deep Evolution Field (MOSDEF) survey. Using composite spectra we investigate the mass-metallicity relation (MZR) at z~1.5 and measure its evolution to z=0. When using gas-phase metallicities based on the N2 line ratio, we find that the MZR evolution from z~1.5 to z=0 depends on stellar mass, evolving by… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.09245v2-abstract-full').style.display = 'inline'; document.getElementById('2103.09245v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.09245v2-abstract-full" style="display: none;"> We analyze the rest-optical emission-line ratios of z~1.5 galaxies drawn from the MOSFIRE Deep Evolution Field (MOSDEF) survey. Using composite spectra we investigate the mass-metallicity relation (MZR) at z~1.5 and measure its evolution to z=0. When using gas-phase metallicities based on the N2 line ratio, we find that the MZR evolution from z~1.5 to z=0 depends on stellar mass, evolving by $螖\rm log(\rm O/H)\sim0.25$ dex at $M_*<10^{9.75}M_{\odot}$ down to $螖\rm log(\rm O/H)\sim0.05$ at $M_*>10^{10.5}M_{\odot}$. In contrast, the O3N2-based MZR shows a constant offset of $螖\rm log(\rm O/H)\sim0.30$ across all masses, consistent with previous MOSDEF results based on independent metallicity indicators, and suggesting that O3N2 provides a more robust metallicity calibration for our z~1.5 sample. We investigated the secondary dependence of the MZR on SFR by measuring correlated scatter about the mean $M_*$-specific SFR and $M_*-\log(\rm O3N2)$ relations. We find an anti-correlation between $\log(\rm O/H)$ and sSFR offsets, indicating the presence of a $M_*$-SFR-Z relation, though with limited significance. Additionally, we find that our z~1.5 stacks lie along the z=0 metallicity sequence at fixed $渭=\log(M_*/M_{\odot})-0.6\times\log(\rm SFR / M_{\odot} yr^{-1})$ suggesting that the z~1.5 stacks can be described by the z=0 fundamental metallicity relation (FMR). However, using different calibrations can shift the calculated metallicities off of the local FMR, indicating that appropriate calibrations are essential for understanding metallicity evolution with redshift. Finally, understanding how [NII]/H$伪$ scales with galaxy properties is crucial to accurately describe the effects of blended [NII] and H$伪$ on redshift and H$伪$ flux measurements in future large surveys utilizing low-resolution spectra such as with Euclid and the Roman Space Telescope. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.09245v2-abstract-full').style.display = 'none'; document.getElementById('2103.09245v2-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 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 March, 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">14 Pages, 9 figures, Accepted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2008.08831">arXiv:2008.08831</a> <span> [<a href="https://arxiv.org/pdf/2008.08831">pdf</a>, <a href="https://arxiv.org/format/2008.08831">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/abba7a">10.3847/2041-8213/abba7a <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MOSDEF Survey: Neon as a Probe of ISM Physical Conditions at High Redshift </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Jeong%2C+M">Moon-Seong Jeong</a>, <a href="/search/?searchtype=author&query=Shapley%2C+A+E">Alice E. Shapley</a>, <a href="/search/?searchtype=author&query=Sanders%2C+R+L">Ryan L. Sanders</a>, <a href="/search/?searchtype=author&query=Runco%2C+J+N">Jordan N. Runco</a>, <a href="/search/?searchtype=author&query=Topping%2C+M+W">Michael W. Topping</a>, <a href="/search/?searchtype=author&query=Reddy%2C+N+A">Naveen A. Reddy</a>, <a href="/search/?searchtype=author&query=Kriek%2C+M">Mariska Kriek</a>, <a href="/search/?searchtype=author&query=Coil%2C+A+L">Alison L. Coil</a>, <a href="/search/?searchtype=author&query=Mobasher%2C+B">Bahram Mobasher</a>, <a href="/search/?searchtype=author&query=Siana%2C+B">Brian Siana</a>, <a href="/search/?searchtype=author&query=Shivaei%2C+I">Irene Shivaei</a>, <a href="/search/?searchtype=author&query=Freeman%2C+W+R">William R. Freeman</a>, <a href="/search/?searchtype=author&query=Azadi%2C+M">Mojegan Azadi</a>, <a href="/search/?searchtype=author&query=Price%2C+S+H">Sedona H. Price</a>, <a href="/search/?searchtype=author&query=Leung%2C+G+C+K">Gene C. K. Leung</a>, <a href="/search/?searchtype=author&query=Fetherolf%2C+T">Tara Fetherolf</a>, <a href="/search/?searchtype=author&query=de+Groot%2C+L">Laura de Groot</a>, <a href="/search/?searchtype=author&query=Zick%2C+T">Tom Zick</a>, <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</a>, <a href="/search/?searchtype=author&query=Barro%2C+G">Guillermo Barro</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="2008.08831v2-abstract-short" style="display: inline;"> We present results on the properties of neon emission in $z\sim2$ star-forming galaxies drawn from the MOSFIRE Deep Evolution Field (MOSDEF) survey. Doubly-ionized neon ([NeIII]3869) is detected at $\geq3蟽$ in 61 galaxies, representing $\sim$25% of the MOSDEF sample with H$伪$, H$尾$, and [OIII]$5007$ detections at similar redshifts. We consider the neon emission-line properties of both individual g… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.08831v2-abstract-full').style.display = 'inline'; document.getElementById('2008.08831v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.08831v2-abstract-full" style="display: none;"> We present results on the properties of neon emission in $z\sim2$ star-forming galaxies drawn from the MOSFIRE Deep Evolution Field (MOSDEF) survey. Doubly-ionized neon ([NeIII]3869) is detected at $\geq3蟽$ in 61 galaxies, representing $\sim$25% of the MOSDEF sample with H$伪$, H$尾$, and [OIII]$5007$ detections at similar redshifts. We consider the neon emission-line properties of both individual galaxies with [NeIII]3869 detections and composite $z\sim2$ spectra binned by stellar mass. With no requirement of [NeIII]3869 detection, the latter provide a more representative picture of neon emission-line properties in the MOSDEF sample. The [NeIII]3869/[OII]3727 ratio (Ne3O2) is anti-correlated with stellar mass in $z\sim2$ galaxies, as expected based on the mass-metallicity relation. It is also positively correlated with the [OIII]$5007$/[OII]$3727$ ratio (O32), but $z\sim2$ line ratios are offset towards higher Ne3O2 at fixed O32, compared with both local star-forming galaxies and individual H~II regions. Despite the offset towards higher Ne3O2 at fixed O32 at $z\sim2$, biases in inferred Ne3O2-based metallicity are small. Accordingly, Ne3O2 may serve as an important metallicity indicator deep into the reionization epoch. Analyzing additional rest-optical line ratios including [NeIII]$3869$/[OIII]$5007$ (Ne3O3) and [OIII]$5007$/H$尾$ (O3H$尾$), we conclude that the nebular emission-line ratios of $z\sim2$ star-forming galaxies suggest a harder ionizing spectrum (lower stellar metallicity, i.e., Fe/H) at fixed gas-phase oxygen abundance, compared to systems at $z\sim0$. These new results based on neon lend support to the physical picture painted by oxygen, nitrogen, hydrogen, and sulfur emission, of an ionized ISM in high-redshift star-forming galaxies irradiated by chemically young, $伪$-enhanced massive stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.08831v2-abstract-full').style.display = 'none'; document.getElementById('2008.08831v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">7 pages, 5 figures, accepted to ApJ Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2008.04924">arXiv:2008.04924</a> <span> [<a href="https://arxiv.org/pdf/2008.04924">pdf</a>, <a href="https://arxiv.org/format/2008.04924">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/stab119">10.1093/mnras/stab119 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MOSDEF Survey: A Comprehensive Analysis of the Rest-optical Emission-line Properties of $z\sim 2.3$ Star-forming Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Runco%2C+J+N">Jordan N. Runco</a>, <a href="/search/?searchtype=author&query=Shapley%2C+A+E">Alice E. Shapley</a>, <a href="/search/?searchtype=author&query=Sanders%2C+R+L">Ryan L. Sanders</a>, <a href="/search/?searchtype=author&query=Topping%2C+M+W">Michael W. Topping</a>, <a href="/search/?searchtype=author&query=Kriek%2C+M">Mariska Kriek</a>, <a href="/search/?searchtype=author&query=Reddy%2C+N+A">Naveen A. Reddy</a>, <a href="/search/?searchtype=author&query=Coil%2C+A+L">Alison L. Coil</a>, <a href="/search/?searchtype=author&query=Mobasher%2C+B">Bahram Mobasher</a>, <a href="/search/?searchtype=author&query=Siana%2C+B">Brian Siana</a>, <a href="/search/?searchtype=author&query=Freeman%2C+W+R">William R. Freeman</a>, <a href="/search/?searchtype=author&query=Shivaei%2C+I">Irene Shivaei</a>, <a href="/search/?searchtype=author&query=Azadi%2C+M">Mojegan Azadi</a>, <a href="/search/?searchtype=author&query=Price%2C+S+H">Sedona H. Price</a>, <a href="/search/?searchtype=author&query=Leung%2C+G+C+K">Gene C. K. Leung</a>, <a href="/search/?searchtype=author&query=Fetherolf%2C+T">Tara Fetherolf</a>, <a href="/search/?searchtype=author&query=de+Groot%2C+L">Laura de Groot</a>, <a href="/search/?searchtype=author&query=Zick%2C+T">Tom Zick</a>, <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</a>, <a href="/search/?searchtype=author&query=Barro%2C+G">Guillermo Barro</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="2008.04924v2-abstract-short" style="display: inline;"> We analyze the rest-optical emission-line spectra of $z\sim2.3$ star-forming galaxies in the complete MOSFIRE Deep Evolution Field (MOSDEF) survey. In investigating the origin of the well-known offset between the sequences of high-redshift and local galaxies in the [O III]5008/H$尾$ vs. [N II]6585/H$伪$ ("[N II] BPT") diagram, we define two populations of $z\sim2.3$ MOSDEF galaxies. These include th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.04924v2-abstract-full').style.display = 'inline'; document.getElementById('2008.04924v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.04924v2-abstract-full" style="display: none;"> We analyze the rest-optical emission-line spectra of $z\sim2.3$ star-forming galaxies in the complete MOSFIRE Deep Evolution Field (MOSDEF) survey. In investigating the origin of the well-known offset between the sequences of high-redshift and local galaxies in the [O III]5008/H$尾$ vs. [N II]6585/H$伪$ ("[N II] BPT") diagram, we define two populations of $z\sim2.3$ MOSDEF galaxies. These include the "high" population that is offset towards higher [O III]5008/H$尾$ and/or [N II]6585/H$伪$ with respect to the local SDSS sequence and the "low" population that overlaps the SDSS sequence. These two groups are also segregated within the [O III]5008/H$尾$ vs. [S II]6718,6733/H$伪$ and the [O III]4960,5008/[O II]3727,3730 (O$_{32}$) vs. ([O III]4960,5008+[O II]3727,3730)/H$尾$ (R$_{23}$) diagram, which suggests qualitatively that star-forming regions in the more offset galaxies are characterized by harder ionizing spectra at fixed nebular oxygen abundance. We also investigate many galaxy properties of the split sample and find that the "high" sample is on average smaller in size and less massive, but has higher specific star-formation rate and star-formation-rate surface density values and is slightly younger compared to the "low" population. From Cloudy+BPASS photoionization models, we estimate that the "high" population has a lower stellar metallicity (i.e., harder ionizing spectrum) but slightly higher nebular metallicity and higher ionization parameter compared to the "low" population. While the "high" population is more $伪$-enhanced (i.e., higher $伪$/Fe) than the "low" population, both samples are significantly more $伪$-enhanced compared to local star-forming galaxies with similar rest-optical line ratios. These differences must be accounted for in all high-redshift star-forming galaxies -- not only those "offset" from local excitation sequences. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.04924v2-abstract-full').style.display = 'none'; document.getElementById('2008.04924v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 7 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/2008.04327">arXiv:2008.04327</a> <span> [<a href="https://arxiv.org/pdf/2008.04327">pdf</a>, <a href="https://arxiv.org/format/2008.04327">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/staa3502">10.1093/mnras/staa3502 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MOSDEF Survey: Differences in SFR and Metallicity for Morphologically-Selected Mergers at z~2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Horstman%2C+K">Katelyn Horstman</a>, <a href="/search/?searchtype=author&query=Shapley%2C+A+E">Alice E. Shapley</a>, <a href="/search/?searchtype=author&query=Sanders%2C+R+L">Ryan L. Sanders</a>, <a href="/search/?searchtype=author&query=Mobasher%2C+B">Bahram Mobasher</a>, <a href="/search/?searchtype=author&query=Reddy%2C+N+A">Naveen A. Reddy</a>, <a href="/search/?searchtype=author&query=Kriek%2C+M">Mariska Kriek</a>, <a href="/search/?searchtype=author&query=Coil%2C+A+L">Alison L. Coil</a>, <a href="/search/?searchtype=author&query=Siana%2C+B">Brian Siana</a>, <a href="/search/?searchtype=author&query=Shivaei%2C+I">Irene Shivaei</a>, <a href="/search/?searchtype=author&query=Freeman%2C+W+R">William R. Freeman</a>, <a href="/search/?searchtype=author&query=Azadi%2C+M">Mojegan Azadi</a>, <a href="/search/?searchtype=author&query=Price%2C+S+H">Sedona H. Price</a>, <a href="/search/?searchtype=author&query=Leung%2C+G+C+K">Gene C. K. Leung</a>, <a href="/search/?searchtype=author&query=Fetherolf%2C+T">Tara Fetherolf</a>, <a href="/search/?searchtype=author&query=de+Groot%2C+L">Laura de Groot</a>, <a href="/search/?searchtype=author&query=Zick%2C+T">Tom Zick</a>, <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</a>, <a href="/search/?searchtype=author&query=Barro%2C+G">Guillermo Barro</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="2008.04327v2-abstract-short" style="display: inline;"> We study the properties of 55 morphologically-identified merging galaxy systems at z~2. These systems are flagged as mergers based on features such as tidal tails, double nuclei, and asymmetry. Our sample is drawn from the MOSFIRE Deep Evolution Field (MOSDEF) survey, along with a control sample of isolated galaxies at the same redshift. We consider the relationships between stellar mass, star for… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.04327v2-abstract-full').style.display = 'inline'; document.getElementById('2008.04327v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.04327v2-abstract-full" style="display: none;"> We study the properties of 55 morphologically-identified merging galaxy systems at z~2. These systems are flagged as mergers based on features such as tidal tails, double nuclei, and asymmetry. Our sample is drawn from the MOSFIRE Deep Evolution Field (MOSDEF) survey, along with a control sample of isolated galaxies at the same redshift. We consider the relationships between stellar mass, star formation rate (SFR), and gas-phase metallicity for both merging and non-merging systems. In the local universe, merging systems are characterized by an elevated SFR and depressed metallicity compared to isolated systems at a given mass. Our results indicate SFR enhancement and metallicity deficit for merging systems relative to non-merging systems for a fixed stellar mass at z~2, though larger samples are required to establish these preliminary results with higher statistical significance. In future work, it will be important to establish if the enhanced SFR and depressed metallicity in high-redshift mergers deviate from the "fundamental metallicity relation," as is observed in mergers in the local universe, and therefore shed light on gas flows during galaxy interactions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.04327v2-abstract-full').style.display = 'none'; document.getElementById('2008.04327v2-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 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 5 figures, 5 figures, accepted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2004.13033">arXiv:2004.13033</a> <span> [<a href="https://arxiv.org/pdf/2004.13033">pdf</a>, <a href="https://arxiv.org/ps/2004.13033">ps</a>, <a href="https://arxiv.org/format/2004.13033">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/staa1211">10.1093/mnras/staa1211 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Connecting the metallicity dependence and redshift evolution of high-mass X-ray binaries </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</a>, <a href="/search/?searchtype=author&query=Civano%2C+F">Francesca Civano</a>, <a href="/search/?searchtype=author&query=Suh%2C+H">Hyewon Suh</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="2004.13033v1-abstract-short" style="display: inline;"> The integrated X-ray luminosity ($L_{\mathrm{X}}$) of high-mass X-ray binaries (HMXBs) in a galaxy is correlated with its star formation rate (SFR), and the normalization of this correlation increases with redshift. Population synthesis models suggest that the redshift evolution of $L_{\mathrm{X}}$/SFR is driven by the metallicity ($Z$) dependence of HMXBs, and the first direct evidence of this co… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.13033v1-abstract-full').style.display = 'inline'; document.getElementById('2004.13033v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2004.13033v1-abstract-full" style="display: none;"> The integrated X-ray luminosity ($L_{\mathrm{X}}$) of high-mass X-ray binaries (HMXBs) in a galaxy is correlated with its star formation rate (SFR), and the normalization of this correlation increases with redshift. Population synthesis models suggest that the redshift evolution of $L_{\mathrm{X}}$/SFR is driven by the metallicity ($Z$) dependence of HMXBs, and the first direct evidence of this connection was recently presented using galaxies at $z\sim2$. To confirm this result with more robust measurements and better constrain the $L_{\mathrm{X}}$-SFR-$Z$ relation, we have studied the $Z$ dependence of $L_{\mathrm{X}}$/SFR at lower redshifts. Using samples of star-forming galaxies at $z=0.1-0.9$ with optical spectra from the hCOSMOS and zCOSMOS surveys, we stacked \textit{Chandra} data from the COSMOS Legacy survey to measure the average $L_{\mathrm{X}}$/SFR as a function of $Z$ in three redshift ranges: $z=0.1-0.25$, $0.25-0.4$, and $0.5-0.9$. We find no significant variation of the $L_{\mathrm{X}}$-SFR-$Z$ relation with redshift. Our results provide further evidence that the $Z$ dependence of HMXBs is responsible for the redshift evolution of $L_{\mathrm{X}}$/SFR. Combining all available $z>0$ measurements together, we derive a best-fitting $L_{\mathrm{X}}$-SFR-$Z$ relation and assess how different population synthesis models describe the data. These results provide the strongest constraints to date on the $L_{\mathrm{X}}$-SFR-$Z$ relation in the range of $8.0<$12+log(O/H)$<9.0$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.13033v1-abstract-full').style.display = 'none'; document.getElementById('2004.13033v1-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 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 7 figures, 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/1912.03315">arXiv:1912.03315</a> <span> [<a href="https://arxiv.org/pdf/1912.03315">pdf</a>, <a href="https://arxiv.org/ps/1912.03315">ps</a>, <a href="https://arxiv.org/format/1912.03315">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/ab5fd2">10.3847/1538-4357/ab5fd2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Chandra Observations of High Energy X-ray Sources Discovered by INTEGRAL </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=Bodaghee%2C+A">Arash Bodaghee</a>, <a href="/search/?searchtype=author&query=Chaty%2C+S">Sylvain Chaty</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=Hare%2C+J">Jeremy Hare</a>, <a href="/search/?searchtype=author&query=Krivonos%2C+R">Roman Krivonos</a>, <a href="/search/?searchtype=author&query=Rahoui%2C+F">Farid Rahoui</a>, <a href="/search/?searchtype=author&query=Rodriguez%2C+J">Jerome Rodriguez</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1912.03315v1-abstract-short" style="display: inline;"> The International Gamma-Ray Astrophysics Laboratory (INTEGRAL) satellite has detected in excess of 1000 sources in the ~20-100 keV band during its surveys of the sky over the past 17 years. We obtained 5 ks observations of 15 unclassified IGR sources with the Chandra X-ray Observatory in order to localize them, to identify optical/IR counterparts, to measure their soft X-ray spectra, and to classi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.03315v1-abstract-full').style.display = 'inline'; document.getElementById('1912.03315v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1912.03315v1-abstract-full" style="display: none;"> The International Gamma-Ray Astrophysics Laboratory (INTEGRAL) satellite has detected in excess of 1000 sources in the ~20-100 keV band during its surveys of the sky over the past 17 years. We obtained 5 ks observations of 15 unclassified IGR sources with the Chandra X-ray Observatory in order to localize them, to identify optical/IR counterparts, to measure their soft X-ray spectra, and to classify them. For 10 of the IGR sources, we detect Chandra sources that are likely (or in some cases certain) to be the counterparts. IGR J18007-4146 and IGR J15038-6021 both have Gaia parallax distances, placing them at 2.5+0.5-0.4 and 1.1+1.5-0.4 kpc, respectively. We tentatively classify both of them as intermediate polar-type Cataclysmic Variables. Also, IGR J17508-3219 is likely to be a Galactic source, but it is unclear if it is a Dwarf Nova or another type of transient. For IGR J17118-3155, we provide a Chandra localization, but it is unclear if the source is Galactic or extragalactic. Based on either near-IR/IR colors or the presence of extended near-IR emission, we classify four sources as Active Galactic Nuclei (IGR J16181-5407, IGR J16246-4556, IGR J17096-2527, and IGR J19294+1327), and IGR J20310+3835 and IGR J15541-5613 are AGN candidates. In addition, we identified an AGN in the INTEGRAL error circle of IGR J16120-3543 that is a possible counterpart. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.03315v1-abstract-full').style.display = 'none'; document.getElementById('1912.03315v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 December, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">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/1910.13594">arXiv:1910.13594</a> <span> [<a href="https://arxiv.org/pdf/1910.13594">pdf</a>, <a href="https://arxiv.org/format/1910.13594">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The MOSDEF Survey: [SIII] as a New Probe of Evolving ISM Conditions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Sanders%2C+R+L">Ryan L. Sanders</a>, <a href="/search/?searchtype=author&query=Jones%2C+T">Tucker Jones</a>, <a href="/search/?searchtype=author&query=Shapley%2C+A+E">Alice E. Shapley</a>, <a href="/search/?searchtype=author&query=Reddy%2C+N+A">Naveen A. Reddy</a>, <a href="/search/?searchtype=author&query=Kriek%2C+M">Mariska Kriek</a>, <a href="/search/?searchtype=author&query=Coil%2C+A+L">Alison L. Coil</a>, <a href="/search/?searchtype=author&query=Siana%2C+B">Brian Siana</a>, <a href="/search/?searchtype=author&query=Mobasher%2C+B">Bahram Mobasher</a>, <a href="/search/?searchtype=author&query=Shivaei%2C+I">Irene Shivaei</a>, <a href="/search/?searchtype=author&query=Price%2C+S+H">Sedona H. Price</a>, <a href="/search/?searchtype=author&query=Freeman%2C+W+R">William R. Freeman</a>, <a href="/search/?searchtype=author&query=Azadi%2C+M">Mojegan Azadi</a>, <a href="/search/?searchtype=author&query=Leung%2C+G+C+K">Gene C. K. Leung</a>, <a href="/search/?searchtype=author&query=Fetherolf%2C+T">Tara Fetherolf</a>, <a href="/search/?searchtype=author&query=Zick%2C+T+O">Tom O. Zick</a>, <a href="/search/?searchtype=author&query=de+Groot%2C+L">Laura de Groot</a>, <a href="/search/?searchtype=author&query=Barro%2C+G">Guillermo Barro</a>, <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</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="1910.13594v2-abstract-short" style="display: inline;"> We present measurements of [SIII]$位位$9069,9531 for a sample of $z\sim1.5$ star-forming galaxies, the first sample with measurements of these lines at z>0.1. We employ the line ratio S$_{32}$$\equiv$[SIII]$位位$9069,9531/[SII]$位位$6716,6731 as a novel probe of evolving ISM conditions. Since this ratio includes the low-ionization line [SII], it is crucial that the effects of diffuse ionized gas (DIG) o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.13594v2-abstract-full').style.display = 'inline'; document.getElementById('1910.13594v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1910.13594v2-abstract-full" style="display: none;"> We present measurements of [SIII]$位位$9069,9531 for a sample of $z\sim1.5$ star-forming galaxies, the first sample with measurements of these lines at z>0.1. We employ the line ratio S$_{32}$$\equiv$[SIII]$位位$9069,9531/[SII]$位位$6716,6731 as a novel probe of evolving ISM conditions. Since this ratio includes the low-ionization line [SII], it is crucial that the effects of diffuse ionized gas (DIG) on emission-line ratios be accounted for in $z\sim0$ integrated galaxy spectra, or else that comparisons be made to samples of local HII regions in which DIG emission is not present. We find that S$_{32}$ decreases with increasing stellar mass at both $z\sim1.5$ and $z\sim0$, but that the dependence is weak suggesting S$_{32}$ has a very shallow anticorrelation with metallicity, in contrast with O$_{32}$ that displays a strong metallicity dependence. As a result, S$_{32}$ only mildly evolves with redshift at fixed stellar mass. The $z\sim1.5$ sample is systematicallty offset towards lower S$_{32}$ and higher [SII]/H$伪$ at fixed [OIII]/H$尾$ relative to $z=0$ HII regions. By comparing to photoionization model grids, we find that such trends can be explained by a scenario in which the ionizing spectrum is harder at fixed O/H with increasing redshift, but are inconsistent with an increase in ionization parameter at fixed O/H. This analysis demonstrates the advantages of expanding beyond the strongest rest-optical lines for evolutionary studies, and the particular utility of [SIII] for characterizing evolving ISM conditions and stellar compositions. These measurements provide a basis for estimating [SIII] line strengths for high-redshift galaxies, a line that the James Webb Space Telescope will measure out to z~5.5. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.13594v2-abstract-full').style.display = 'none'; document.getElementById('1910.13594v2-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 December, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 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">6 pages, 4 figures, accepted for publication in ApJ Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1909.11110">arXiv:1909.11110</a> <span> [<a href="https://arxiv.org/pdf/1909.11110">pdf</a>, <a href="https://arxiv.org/format/1909.11110">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/ab3f32">10.3847/1538-4357/ab3f32 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Neutron Stars and Black Holes in the Small Magellanic Cloud: The SMC NuSTAR Legacy Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lazzarini%2C+M">M. Lazzarini</a>, <a href="/search/?searchtype=author&query=Williams%2C+B+F">B. F. Williams</a>, <a href="/search/?searchtype=author&query=Hornschemeier%2C+A+E">A. E. Hornschemeier</a>, <a href="/search/?searchtype=author&query=Antoniou%2C+V">V. Antoniou</a>, <a href="/search/?searchtype=author&query=Vasilopoulos%2C+G">G. Vasilopoulos</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/?searchtype=author&query=Vulic%2C+N">N. Vulic</a>, <a href="/search/?searchtype=author&query=Yukita%2C+M">M. Yukita</a>, <a href="/search/?searchtype=author&query=Zezas%2C+A">A. Zezas</a>, <a href="/search/?searchtype=author&query=Bodaghee%2C+A">A. Bodaghee</a>, <a href="/search/?searchtype=author&query=Lehmer%2C+B+D">B. D. Lehmer</a>, <a href="/search/?searchtype=author&query=Maccarone%2C+T+J">T. J. Maccarone</a>, <a href="/search/?searchtype=author&query=Ptak%2C+A">A. Ptak</a>, <a href="/search/?searchtype=author&query=Wik%2C+D">D. Wik</a>, <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">F. M. Fornasini</a>, <a href="/search/?searchtype=author&query=Hong%2C+J">Jaesub Hong</a>, <a href="/search/?searchtype=author&query=Kennea%2C+J+A">J. A. Kennea</a>, <a href="/search/?searchtype=author&query=Tomsick%2C+J+A">J. A. Tomsick</a>, <a href="/search/?searchtype=author&query=Venters%2C+T">T. Venters</a>, <a href="/search/?searchtype=author&query=Udalski%2C+A">A. Udalski</a>, <a href="/search/?searchtype=author&query=Cassity%2C+A">A. Cassity</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="1909.11110v1-abstract-short" style="display: inline;"> We present a source catalog from the first deep hard X-ray ($E>10$ keV) survey of the Small Magellanic Cloud (SMC), the NuSTAR Legacy Survey of the SMC. We observed three fields, for a total exposure time of 1 Ms, along the bar of this nearby star-forming galaxy. Fields were chosen for their young stellar and accreting binary populations. We detected 10 sources above a 3$蟽$ significance level (4… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.11110v1-abstract-full').style.display = 'inline'; document.getElementById('1909.11110v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.11110v1-abstract-full" style="display: none;"> We present a source catalog from the first deep hard X-ray ($E>10$ keV) survey of the Small Magellanic Cloud (SMC), the NuSTAR Legacy Survey of the SMC. We observed three fields, for a total exposure time of 1 Ms, along the bar of this nearby star-forming galaxy. Fields were chosen for their young stellar and accreting binary populations. We detected 10 sources above a 3$蟽$ significance level (4$-$25 keV) and obtained upper limits on an additional 40 sources. We reached a 3$蟽$ limiting luminosity in the 4$-$25 keV band of $\sim$ $10^{35}$ erg s$^{-1}$, allowing us to probe fainter X-ray binary (XRB) populations than has been possible with other extragalactic NuSTAR surveys. We used hard X-ray colors and luminosities to constrain the compact-object type, exploiting the spectral differences between accreting black holes and neutron stars at $E>10$ keV. Several of our sources demonstrate variability consistent with previously observed behavior. We confirmed pulsations for seven pulsars in our 3$蟽$ sample. We present the first detection of pulsations from a Be-XRB, SXP305 (CXO J005215.4$-$73191), with an X-ray pulse period of $305.69\pm0.16$ seconds and a likely orbital period of $\sim$1160-1180 days. Bright sources ($\gtrsim 5\times 10^{36}$ erg s$^{-1}$) in our sample have compact-object classifications consistent with their previously reported types in the literature. Lower luminosity sources ($\lesssim 5\times 10^{36}$ erg s$^{-1}$) have X-ray colors and luminosities consistent with multiple classifications. We raise questions about possible spectral differences at low luminosity between SMC pulsars and the Galactic pulsars used to create the diagnostic diagrams. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.11110v1-abstract-full').style.display = 'none'; document.getElementById('1909.11110v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">8 tables, 18 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/1909.08635">arXiv:1909.08635</a> <span> [<a href="https://arxiv.org/pdf/1909.08635">pdf</a>, <a href="https://arxiv.org/ps/1909.08635">ps</a>, <a href="https://arxiv.org/format/1909.08635">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/ab4653">10.3847/1538-4357/ab4653 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MOSDEF Survey: The Metallicity Dependence of X-ray Binary Populations at $z\sim2$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</a>, <a href="/search/?searchtype=author&query=Kriek%2C+M">Mariska Kriek</a>, <a href="/search/?searchtype=author&query=Sanders%2C+R+L">Ryan L. Sanders</a>, <a href="/search/?searchtype=author&query=Shivaei%2C+I">Irene Shivaei</a>, <a href="/search/?searchtype=author&query=Civano%2C+F">Francesca Civano</a>, <a href="/search/?searchtype=author&query=Reddy%2C+N+A">Naveen A. Reddy</a>, <a href="/search/?searchtype=author&query=Shapley%2C+A+E">Alice E. Shapley</a>, <a href="/search/?searchtype=author&query=Coil%2C+A+L">Alison L. Coil</a>, <a href="/search/?searchtype=author&query=Mobasher%2C+B">Bahram Mobasher</a>, <a href="/search/?searchtype=author&query=Siana%2C+B">Brian Siana</a>, <a href="/search/?searchtype=author&query=Aird%2C+J">James Aird</a>, <a href="/search/?searchtype=author&query=Azadi%2C+M">Mojegan Azadi</a>, <a href="/search/?searchtype=author&query=Freeman%2C+W+R">William R. Freeman</a>, <a href="/search/?searchtype=author&query=Leung%2C+G+C+K">Gene C. K. Leung</a>, <a href="/search/?searchtype=author&query=Price%2C+S+H">Sedona H. Price</a>, <a href="/search/?searchtype=author&query=Fetherolf%2C+T">Tara Fetherolf</a>, <a href="/search/?searchtype=author&query=Zick%2C+T">Tom Zick</a>, <a href="/search/?searchtype=author&query=Barro%2C+G">Guillermo Barro</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="1909.08635v1-abstract-short" style="display: inline;"> Population synthesis models predict that high-mass X-ray binary (HMXB) populations produced in low metallicity environments should be more X-ray luminous, a trend supported by studies of nearby galaxies. This trend may be responsible for the observed increase of the X-ray luminosity ($L_{\mathrm{X}}$) per star formation rate (SFR) with redshift due to the decrease of metallicity ($Z$) at fixed ste… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.08635v1-abstract-full').style.display = 'inline'; document.getElementById('1909.08635v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.08635v1-abstract-full" style="display: none;"> Population synthesis models predict that high-mass X-ray binary (HMXB) populations produced in low metallicity environments should be more X-ray luminous, a trend supported by studies of nearby galaxies. This trend may be responsible for the observed increase of the X-ray luminosity ($L_{\mathrm{X}}$) per star formation rate (SFR) with redshift due to the decrease of metallicity ($Z$) at fixed stellar mass as a function of redshift. To test this hypothesis, we use a sample of 79 $z\sim2$ star-forming galaxies with oxygen abundance measurements from the MOSDEF survey, which obtained rest-frame optical spectra for $\sim1500$ galaxies in the CANDELS fields at $1.37<z<3.80$. Using Chandra data from the AEGIS-X Deep, Deep Field North, and Deep Field South surveys, we stack the X-ray data at the galaxy locations in bins of redshift and $Z$ because the galaxies are too faint to be individually detected. In agreement with previous studies, the average $L_{\mathrm{X}}$/SFR of our $z\sim2$ galaxy sample is enhanced by $\approx0.4-0.8$ dex relative to local HMXB $L_{\mathrm{X}}$-SFR scaling relations. Splitting our sample by $Z$, we find that $L_{\mathrm{X}}$/SFR and $Z$ are anti-correlated with 97% confidence. This observed $Z$ dependence for HMXB-dominated galaxies is consistent both with the local $L_{\mathrm{X}}$-SFR-$Z$ relation and a subset of population synthesis models. Although the statistical significance of the observed trends is weak due to the low X-ray statistics, these results constitute the first direct evidence connecting the redshift evolution of $L_{\mathrm{X}}$/SFR and the $Z$ dependence of HMXBs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.08635v1-abstract-full').style.display = 'none'; document.getElementById('1909.08635v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">22 pages, 8 figures, 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/1907.07189">arXiv:1907.07189</a> <span> [<a href="https://arxiv.org/pdf/1907.07189">pdf</a>, <a href="https://arxiv.org/format/1907.07189">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/ab385a">10.3847/2041-8213/ab385a <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MOSDEF Survey: Sulfur Emission-line Ratios Provide New Insights into Evolving ISM Conditions at High Redshift </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Shapley%2C+A+E">Alice E. Shapley</a>, <a href="/search/?searchtype=author&query=Sanders%2C+R+L">Ryan L. Sanders</a>, <a href="/search/?searchtype=author&query=Shao%2C+P">Peng Shao</a>, <a href="/search/?searchtype=author&query=Reddy%2C+N+A">Naveen A. Reddy</a>, <a href="/search/?searchtype=author&query=Kriek%2C+M">Mariska Kriek</a>, <a href="/search/?searchtype=author&query=Coil%2C+A+L">Alison L. Coil</a>, <a href="/search/?searchtype=author&query=Mobasher%2C+B">Bahram Mobasher</a>, <a href="/search/?searchtype=author&query=Siana%2C+B">Brian Siana</a>, <a href="/search/?searchtype=author&query=Shivaei%2C+I">Irene Shivaei</a>, <a href="/search/?searchtype=author&query=Freeman%2C+W+R">William R. Freeman</a>, <a href="/search/?searchtype=author&query=Azadi%2C+M">Mojegan Azadi</a>, <a href="/search/?searchtype=author&query=Price%2C+S+H">Sedona H. Price</a>, <a href="/search/?searchtype=author&query=Leung%2C+G+C+K">Gene C. K. Leung</a>, <a href="/search/?searchtype=author&query=Fetherolf%2C+T">Tara Fetherolf</a>, <a href="/search/?searchtype=author&query=de+Groot%2C+L">Laura de Groot</a>, <a href="/search/?searchtype=author&query=Zick%2C+T">Tom Zick</a>, <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</a>, <a href="/search/?searchtype=author&query=Barro%2C+G">Guillermo Barro</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="1907.07189v3-abstract-short" style="display: inline;"> We present results on the emission-line properties of 1.3<=z<=2.7 galaxies drawn from the complete MOSFIRE Deep Evolution Field (MOSDEF) survey. Specifically, we use observations of the emission-line diagnostic diagram of [OIII]5007/Hb vs. [SII]6717,6731/Ha, i.e., the "[SII] BPT diagram," to gain insight into the physical properties of high-redshift star-forming regions. High-redshift MOSDEF galax… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.07189v3-abstract-full').style.display = 'inline'; document.getElementById('1907.07189v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1907.07189v3-abstract-full" style="display: none;"> We present results on the emission-line properties of 1.3<=z<=2.7 galaxies drawn from the complete MOSFIRE Deep Evolution Field (MOSDEF) survey. Specifically, we use observations of the emission-line diagnostic diagram of [OIII]5007/Hb vs. [SII]6717,6731/Ha, i.e., the "[SII] BPT diagram," to gain insight into the physical properties of high-redshift star-forming regions. High-redshift MOSDEF galaxies are offset towards lower [SII]6717,6731/Ha at fixed [OIII]5007/Hb, relative to local galaxies from the Sloan Digital Sky Survey (SDSS). Furthermore, at fixed [OIII]5007/Hb, local SDSS galaxies follow a trend of decreasing [SII]6717,6731/Ha as the surface density of star formation (Sigma_SFR) increases. We explain this trend in terms of the decreasing fractional contribution from diffuse ionized gas (f_DIG) as Sigma_SFR increases in galaxies, which causes galaxy-integrated line ratios to shift towards the locus of pure HII-region emission. The z~0 relationship between f_DIG and Sigma_SFR implies that high-redshift galaxies have lower f_DIG values than typical local systems, given their significantly higher typical Sigma_SFR. When an appropriate low-redshift benchmark with zero or minimal f_DIG is used, high-redshift MOSDEF galaxies appear offset towards higher [SII]6717,6731/Ha and/or [OIII]5007/Hb. The joint shifts of high-redshift galaxies in the [SII] and [NII] BPT diagrams are best explained in terms of the harder spectra ionizing their star-forming regions at fixed nebular oxygen abundance (expected for chemically-young galaxies), as opposed to large variations in N/O ratios or higher ionization parameters. The evolving mixture of HII regions and DIG is an essential ingredient to our description of the ISM over cosmic time. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.07189v3-abstract-full').style.display = 'none'; document.getElementById('1907.07189v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 August, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 July, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">6 pages, 4 figures, accepted to ApJ Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1907.00013">arXiv:1907.00013</a> <span> [<a href="https://arxiv.org/pdf/1907.00013">pdf</a>, <a href="https://arxiv.org/format/1907.00013">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/stz3032">10.1093/mnras/stz3032 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MOSDEF Survey: Direct-Method Metallicities and ISM Conditions at $z\sim1.5-3.5$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Sanders%2C+R+L">Ryan L. Sanders</a>, <a href="/search/?searchtype=author&query=Shapley%2C+A+E">Alice E. Shapley</a>, <a href="/search/?searchtype=author&query=Reddy%2C+N+A">Naveen A. Reddy</a>, <a href="/search/?searchtype=author&query=Kriek%2C+M">Mariska Kriek</a>, <a href="/search/?searchtype=author&query=Siana%2C+B">Brian Siana</a>, <a href="/search/?searchtype=author&query=Coil%2C+A+L">Alison L. Coil</a>, <a href="/search/?searchtype=author&query=Mobasher%2C+B">Bahram Mobasher</a>, <a href="/search/?searchtype=author&query=Shivaei%2C+I">Irene Shivaei</a>, <a href="/search/?searchtype=author&query=Freeman%2C+W+R">William R. Freeman</a>, <a href="/search/?searchtype=author&query=Azadi%2C+M">Mojegan Azadi</a>, <a href="/search/?searchtype=author&query=Price%2C+S+H">Sedona H. Price</a>, <a href="/search/?searchtype=author&query=Leung%2C+G">Gene Leung</a>, <a href="/search/?searchtype=author&query=Fetherolf%2C+T">Tara Fetherolf</a>, <a href="/search/?searchtype=author&query=de+Groot%2C+L">Laura de Groot</a>, <a href="/search/?searchtype=author&query=Zick%2C+T">Tom Zick</a>, <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</a>, <a href="/search/?searchtype=author&query=Barro%2C+G">Guillermo Barro</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="1907.00013v2-abstract-short" style="display: inline;"> We present detections of [OIII]$位$4363 and direct-method metallicities for star-forming galaxies at $z=1.7-3.6$. We combine new measurements from the MOSFIRE Deep Evolution Field (MOSDEF) survey with literature sources to construct a sample of 18 galaxies with direct-method metallicities at $z>1$, spanning $7.5<1$2+log(O/H$)<8.2$ and log(M$_*$/M$_{\odot})=7-10$. We find that strong-line calibratio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.00013v2-abstract-full').style.display = 'inline'; document.getElementById('1907.00013v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1907.00013v2-abstract-full" style="display: none;"> We present detections of [OIII]$位$4363 and direct-method metallicities for star-forming galaxies at $z=1.7-3.6$. We combine new measurements from the MOSFIRE Deep Evolution Field (MOSDEF) survey with literature sources to construct a sample of 18 galaxies with direct-method metallicities at $z>1$, spanning $7.5<1$2+log(O/H$)<8.2$ and log(M$_*$/M$_{\odot})=7-10$. We find that strong-line calibrations based on local analogs of high-redshift galaxies reliably reproduce the metallicity of the $z>1$ sample on average. We construct the first mass-metallicity relation at $z>1$ based purely on direct-method O/H, finding a slope that is consistent with strong-line results. Direct-method O/H evolves by $\lesssim0.1$ dex at fixed M$_*$ and SFR from $z\sim0-2.2$. We employ photoionization models to constrain the ionization parameter and ionizing spectrum in the high-redshift sample. Stellar models with super-solar O/Fe and binary evolution of massive stars are required to reproduce the observed strong-line ratios. We find that the $z>1$ sample falls on the $z\sim0$ relation between ionization parameter and O/H, suggesting no evolution of this relation from $z\sim0$ to $z\sim2$. These results suggest that the offset of the strong-line ratios of this sample from local excitation sequences is driven primarily by a harder ionizing spectrum at fixed nebular metallicity compared to what is typical at $z\sim0$, naturally explained by super-solar O/Fe at high redshift caused by rapid formation timescales. Given the extreme nature of our $z>1$ sample, the implications for representative $z\sim2$ galaxy samples at $\sim10^{10}$ M$_{\odot}$ are unclear, but similarities to $z>6$ galaxies suggest that these conclusions can be extended to galaxies in the epoch of reionization. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.00013v2-abstract-full').style.display = 'none'; document.getElementById('1907.00013v2-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">v1</span> submitted 28 June, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">27 pages + 4 page appendix, 18 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/1905.13338">arXiv:1905.13338</a> <span> [<a href="https://arxiv.org/pdf/1905.13338">pdf</a>, <a href="https://arxiv.org/format/1905.13338">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ab4a7c">10.3847/1538-4357/ab4a7c <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MOSDEF survey: a census of AGN-driven ionized outflows at $z = 1.4-3.8$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Leung%2C+G+C+K">Gene C. K. Leung</a>, <a href="/search/?searchtype=author&query=Coil%2C+A+L">Alison L. Coil</a>, <a href="/search/?searchtype=author&query=Aird%2C+J">James Aird</a>, <a href="/search/?searchtype=author&query=Azadi%2C+M">Mojegan Azadi</a>, <a href="/search/?searchtype=author&query=Kriek%2C+M">Mariska Kriek</a>, <a href="/search/?searchtype=author&query=Mobasher%2C+B">Bahram Mobasher</a>, <a href="/search/?searchtype=author&query=Reddy%2C+N">Naveen Reddy</a>, <a href="/search/?searchtype=author&query=Shapley%2C+A">Alice Shapley</a>, <a href="/search/?searchtype=author&query=Siana%2C+B">Brian Siana</a>, <a href="/search/?searchtype=author&query=Fetherolf%2C+T">Tara Fetherolf</a>, <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</a>, <a href="/search/?searchtype=author&query=Freeman%2C+W+R">William R. Freeman</a>, <a href="/search/?searchtype=author&query=Price%2C+S+H">Sedona H. Price</a>, <a href="/search/?searchtype=author&query=Sanders%2C+R+L">Ryan L. Sanders</a>, <a href="/search/?searchtype=author&query=Shivaei%2C+I">Irene Shivaei</a>, <a href="/search/?searchtype=author&query=Zick%2C+T">Tom Zick</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="1905.13338v3-abstract-short" style="display: inline;"> Using data from the MOSFIRE Deep Evolution Field (MOSDEF) survey, we present a census of AGN-driven ionized outflows in a sample of 159 AGNs at $1.4 \le z \le 3.8$. The sample spans AGN bolometric luminosities of $10^{44-47} \mathrm{~erg~s}^{-1}$ and includes both quiescent and star-forming galaxies extending across three orders of magnitude in stellar mass. We identify and characterize outflows f… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.13338v3-abstract-full').style.display = 'inline'; document.getElementById('1905.13338v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1905.13338v3-abstract-full" style="display: none;"> Using data from the MOSFIRE Deep Evolution Field (MOSDEF) survey, we present a census of AGN-driven ionized outflows in a sample of 159 AGNs at $1.4 \le z \le 3.8$. The sample spans AGN bolometric luminosities of $10^{44-47} \mathrm{~erg~s}^{-1}$ and includes both quiescent and star-forming galaxies extending across three orders of magnitude in stellar mass. We identify and characterize outflows from the \hbeta, [OIII], \halpha ~and [NII] emission line spectra. We detect outflows in $17\%$ of the AGNs, seven times more often than in a mass-matched sample of inactive galaxies in MOSDEF. The outflows are fast and galaxy-wide, with velocities of $\sim 400-3500 ~\mathrm{km~s}^{-1}$ and spatial extents of $0.3-11.0$ kpc. The incidence of outflows among AGNs is independent of the stellar mass of the host galaxy, with outflows detected in both star-forming and quiescent galaxies. This suggests that outflows exist across different phases in galaxy evolution. We investigate relations between outflow kinematic, spatial, and energetic properties and both AGN and host galaxy properties. Our results show that AGN-driven outflows are widespread in galaxies along the star-forming main sequence. The mass-loading factors of the outflows are typically $0.1-1$ and increase with AGN luminosity, capable of exceeding unity at $L_\mathrm{AGN} \gtrsim 10^{46.3} \mathrm{~erg~s}^{-1}$. In these more luminous sources the ionized outflow alone is likely sufficient to regulate star formation, and when combined with outflowing neutral and molecular gas may be able to quench star formation in their host galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.13338v3-abstract-full').style.display = 'none'; document.getElementById('1905.13338v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 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">24 pages, 12 figures, accepted for publication in the 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/1903.09858">arXiv:1903.09858</a> <span> [<a href="https://arxiv.org/pdf/1903.09858">pdf</a>, <a href="https://arxiv.org/ps/1903.09858">ps</a>, <a href="https://arxiv.org/format/1903.09858">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Astro 2020 Science White Paper: Time Domain Studies of Neutron Star and Black Hole Populations: X-ray Identification of Compact Object Types </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Vulic%2C+N">N. Vulic</a>, <a href="/search/?searchtype=author&query=Hornschemeier%2C+A+E">A. E. Hornschemeier</a>, <a href="/search/?searchtype=author&query=Antoniou%2C+V">V. Antoniou</a>, <a href="/search/?searchtype=author&query=Basu-Zych%2C+A+R">A. R. Basu-Zych</a>, <a href="/search/?searchtype=author&query=Binder%2C+B">B. Binder</a>, <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">F. M. Fornasini</a>, <a href="/search/?searchtype=author&query=Furst%2C+F">F. Furst</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/?searchtype=author&query=Heida%2C+M">M. Heida</a>, <a href="/search/?searchtype=author&query=Lehmer%2C+B+D">B. D. Lehmer</a>, <a href="/search/?searchtype=author&query=Maccarone%2C+T+J">T. J. Maccarone</a>, <a href="/search/?searchtype=author&query=Ptak%2C+A+F">A. F. Ptak</a>, <a href="/search/?searchtype=author&query=Sivakoff%2C+G+R">G. R. Sivakoff</a>, <a href="/search/?searchtype=author&query=Tzanavaris%2C+P">P. Tzanavaris</a>, <a href="/search/?searchtype=author&query=Wik%2C+D+R">D. R. Wik</a>, <a href="/search/?searchtype=author&query=Williams%2C+B+F">B. F. Williams</a>, <a href="/search/?searchtype=author&query=Wilms%2C+J">J. Wilms</a>, <a href="/search/?searchtype=author&query=Yukita%2C+M">M. Yukita</a>, <a href="/search/?searchtype=author&query=Zezas%2C+A">A. Zezas</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="1903.09858v1-abstract-short" style="display: inline;"> What are the most important conditions and processes governing the growth of stellar-origin compact objects? The identification of compact object type as either black hole (BH) or neutron star (NS) is fundamental to understanding their formation and evolution. To date, time-domain determination of compact object type remains a relatively untapped tool. Measurement of orbital periods, pulsations, a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.09858v1-abstract-full').style.display = 'inline'; document.getElementById('1903.09858v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1903.09858v1-abstract-full" style="display: none;"> What are the most important conditions and processes governing the growth of stellar-origin compact objects? The identification of compact object type as either black hole (BH) or neutron star (NS) is fundamental to understanding their formation and evolution. To date, time-domain determination of compact object type remains a relatively untapped tool. Measurement of orbital periods, pulsations, and bursts will lead to a revolution in the study of the demographics of NS and BH populations, linking source phenomena to accretion and galaxy parameters (e.g., star formation, metallicity). To perform these measurements over sufficient parameter space, a combination of a wide-field (>5000 deg^2) transient X-ray monitor over a dynamic energy range (~1-100 keV) and an X-ray telescope for deep surveys with <5 arcsec PSF half-energy width (HEW) angular resolution are required. Synergy with multiwavelength data for characterizing the underlying stellar population will transform our understanding of the time domain properties of transient sources, helping to explain details of supernova explosions and gravitational wave event rates. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.09858v1-abstract-full').style.display = 'none'; document.getElementById('1903.09858v1-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 March, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">9 pages, 2 figures. Submitted to the Astro2020 Decadal Survey</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1811.11767">arXiv:1811.11767</a> <span> [<a href="https://arxiv.org/pdf/1811.11767">pdf</a>, <a href="https://arxiv.org/format/1811.11767">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/aaed1e">10.3847/1538-4357/aaed1e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MOSDEF Survey: Significant Evolution in the Rest-Frame Optical Emission Line Equivalent Widths of Star-Forming Galaxies at z=1.4-3.8 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Reddy%2C+N+A">Naveen A. Reddy</a>, <a href="/search/?searchtype=author&query=Shapley%2C+A+E">Alice E. Shapley</a>, <a href="/search/?searchtype=author&query=Sanders%2C+R+L">Ryan L. Sanders</a>, <a href="/search/?searchtype=author&query=Kriek%2C+M">Mariska Kriek</a>, <a href="/search/?searchtype=author&query=Coil%2C+A+L">Alison L. Coil</a>, <a href="/search/?searchtype=author&query=Shivaei%2C+I">Irene Shivaei</a>, <a href="/search/?searchtype=author&query=Freeman%2C+W+R">William R. Freeman</a>, <a href="/search/?searchtype=author&query=Mobasher%2C+B">Bahram Mobasher</a>, <a href="/search/?searchtype=author&query=Siana%2C+B">Brian Siana</a>, <a href="/search/?searchtype=author&query=Azadi%2C+M">Mojegan Azadi</a>, <a href="/search/?searchtype=author&query=Fetherolf%2C+T">Tara Fetherolf</a>, <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</a>, <a href="/search/?searchtype=author&query=Leung%2C+G">Gene Leung</a>, <a href="/search/?searchtype=author&query=Price%2C+S+H">Sedona H. Price</a>, <a href="/search/?searchtype=author&query=Zick%2C+T">Tom Zick</a>, <a href="/search/?searchtype=author&query=Barro%2C+G">Guillermo Barro</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="1811.11767v1-abstract-short" style="display: inline;"> We use extensive spectroscopy from the MOSFIRE Deep Evolution Field (MOSDEF) survey to investigate the relationships between rest-frame optical emission line equivalent widths ($W$) and a number of galaxy and ISM characteristics for a sample of $1134$ star-forming galaxies at redshifts $1.4\lesssim z\lesssim 3.8$. We examine how the equivalent widths of [OII]$位位3727, 3730$, H$尾$, [OIII]… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.11767v1-abstract-full').style.display = 'inline'; document.getElementById('1811.11767v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1811.11767v1-abstract-full" style="display: none;"> We use extensive spectroscopy from the MOSFIRE Deep Evolution Field (MOSDEF) survey to investigate the relationships between rest-frame optical emission line equivalent widths ($W$) and a number of galaxy and ISM characteristics for a sample of $1134$ star-forming galaxies at redshifts $1.4\lesssim z\lesssim 3.8$. We examine how the equivalent widths of [OII]$位位3727, 3730$, H$尾$, [OIII]$位位4960, 5008$, [OIII]$+$H$尾$, H$伪$, and H$伪$+[NII]$位位6550, 6585$, depend on stellar mass, UV slope, age, star-formation rate (SFR) and specific SFR (sSFR), ionization parameter and excitation conditions (O32 and [OIII]/H$尾$), gas-phase metallicity, and ionizing photon production efficiency ($尉_{\rm ion}$). The trend of increasing $W$ with decreasing stellar mass is strongest for [OIII] (and [OIII]+H$尾$). More generally, the equivalent widths of all the lines increase with redshift at a fixed stellar mass or fixed gas-phase metallicity, suggesting that high equivalent width galaxies are common at high redshift. This redshift evolution in equivalent widths can be explained by the increase in SFR and decrease in metallicity with redshift at a fixed stellar mass. Consequently, the dependence of $W$ on sSFR is largely invariant with redshift, particularly when examined for galaxies of a given metallicity. Our results show that high equivalent width galaxies, specifically those with high $W({\rm [OIII]})$, have low stellar masses, blue UV slopes, young ages, high sSFRs, ISM line ratios indicative of high ionization parameters, high $尉_{\rm ion}$, and low metallicities. As these characteristics are often attributed to galaxies with high ionizing escape fractions, galaxies with high $W$ are likely candidates for the population that dominates cosmic reionization. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.11767v1-abstract-full').style.display = 'none'; document.getElementById('1811.11767v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 November, 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">34 pages, 8 tables, 28 figures; submitted 2018 August 23, accepted 2018 October 29 to the Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/1810.07204">arXiv:1810.07204</a> <span> [<a href="https://arxiv.org/pdf/1810.07204">pdf</a>, <a href="https://arxiv.org/format/1810.07204">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/aae887">10.3847/2041-8213/aae887 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MOSDEF Survey: Stellar Continuum Spectra and Star Formation Histories of Active, Transitional, and Quiescent Galaxies at 1.4$<$\lowercase{z}$<$2.6 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Zick%2C+T+O">Tom O. Zick</a>, <a href="/search/?searchtype=author&query=Kriek%2C+M">Mariska Kriek</a>, <a href="/search/?searchtype=author&query=Shapley%2C+A+E">Alice E. Shapley</a>, <a href="/search/?searchtype=author&query=Reddy%2C+N+A">Naveen A. Reddy</a>, <a href="/search/?searchtype=author&query=Freeman%2C+W+R">William R. Freeman</a>, <a href="/search/?searchtype=author&query=Siana%2C+B">Brian Siana</a>, <a href="/search/?searchtype=author&query=Coil%2C+A+L">Alison L. Coil</a>, <a href="/search/?searchtype=author&query=Azadi%2C+M">Mojegan Azadi</a>, <a href="/search/?searchtype=author&query=Barro%2C+G">Guillermo Barro</a>, <a href="/search/?searchtype=author&query=Fetherolf%2C+T">Tara Fetherolf</a>, <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</a>, <a href="/search/?searchtype=author&query=de+Groot%2C+L">Laura de Groot</a>, <a href="/search/?searchtype=author&query=Leung%2C+G">Gene Leung</a>, <a href="/search/?searchtype=author&query=Mobasher%2C+B">Bahram Mobasher</a>, <a href="/search/?searchtype=author&query=Price%2C+S+H">Sedona H. Price</a>, <a href="/search/?searchtype=author&query=Sanders%2C+R+L">Ryan L. Sanders</a>, <a href="/search/?searchtype=author&query=Shivaei%2C+I">Irene Shivaei</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="1810.07204v2-abstract-short" style="display: inline;"> Using the MOSDEF rest-frame optical spectroscopic survey, we investigate the star-formation histories (SFHs) of different galaxy types, ranging from actively star forming to quiescent at $1.4\leq~z\leq2.6$. SFHs are constrained utilizing stellar continuum spectroscopy, specifically through a combination of Balmer absorption lines, the 4000$脜$ break, and the equivalent width of the H$伪$ emission li… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.07204v2-abstract-full').style.display = 'inline'; document.getElementById('1810.07204v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1810.07204v2-abstract-full" style="display: none;"> Using the MOSDEF rest-frame optical spectroscopic survey, we investigate the star-formation histories (SFHs) of different galaxy types, ranging from actively star forming to quiescent at $1.4\leq~z\leq2.6$. SFHs are constrained utilizing stellar continuum spectroscopy, specifically through a combination of Balmer absorption lines, the 4000$脜$ break, and the equivalent width of the H$伪$ emission line. To attain a sufficiently high signal-to-noise ratio (S/N) to conduct these measurements we stack spectra of galaxies with similar spectral types, as determined from their rest-frame $U-V$ and $V-J$ colors. We bin the MOSDEF sample into five spectral types, subdividing the quiescent and star-forming bins to better explore galaxies transitioning between the two. We constrain the average SFHs for each type, finding that quiescent and transitional galaxies in the MOSDEF sample are dominated by an SFH with an average star-formation timescale of $蟿\sim0.1-0.2$~Gyr. These findings contrast with measurements from the low-redshift Universe where, on average, galaxies form their stars over a more extended time period ($蟿>1$~Gyr). Furthermore, our spectral index measurements correlate with mass surface density for all spectral types. Finally, we compare the average properties of the galaxies in our transitional bins to investigate possible paths to quiescence, and speculate on the viability of a dusty post-starburst phase. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.07204v2-abstract-full').style.display = 'none'; document.getElementById('1810.07204v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 October, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 October, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">Accepted to ApJ Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1808.09978">arXiv:1808.09978</a> <span> [<a href="https://arxiv.org/pdf/1808.09978">pdf</a>, <a href="https://arxiv.org/format/1808.09978">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ab06ee">10.3847/1538-4357/ab06ee <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MOSDEF Survey: No Significant Enhancement in Star Formation or Deficit in Metallicity in Merging Galaxy Pairs at 1.5<=z<=3.5 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Wilson%2C+T+J">Timothy J. Wilson</a>, <a href="/search/?searchtype=author&query=Shapley%2C+A+E">Alice E. Shapley</a>, <a href="/search/?searchtype=author&query=Sanders%2C+R+L">Ryan L. Sanders</a>, <a href="/search/?searchtype=author&query=Reddy%2C+N+A">Naveen A. Reddy</a>, <a href="/search/?searchtype=author&query=Freeman%2C+W+R">William R. Freeman</a>, <a href="/search/?searchtype=author&query=Kriek%2C+M">Mariska Kriek</a>, <a href="/search/?searchtype=author&query=Shivaei%2C+I">Irene Shivaei</a>, <a href="/search/?searchtype=author&query=Coil%2C+A+L">Alison L. Coil</a>, <a href="/search/?searchtype=author&query=Siana%2C+B">Brian Siana</a>, <a href="/search/?searchtype=author&query=Mobasher%2C+B">Bahram Mobasher</a>, <a href="/search/?searchtype=author&query=Price%2C+S+H">Sedona H. Price</a>, <a href="/search/?searchtype=author&query=Azadi%2C+M">Mojegan Azadi</a>, <a href="/search/?searchtype=author&query=Barro%2C+G">Guillermo Barro</a>, <a href="/search/?searchtype=author&query=de+Groot%2C+L">Laura de Groot</a>, <a href="/search/?searchtype=author&query=Fetherolf%2C+T">Tara Fetherolf</a>, <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</a>, <a href="/search/?searchtype=author&query=Leung%2C+G+C+K">Gene C. K. Leung</a>, <a href="/search/?searchtype=author&query=Zick%2C+T+O">Tom O. Zick</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="1808.09978v2-abstract-short" style="display: inline;"> We study the properties of 30 spectroscopically-identified pairs of galaxies observed during the peak epoch of star formation in the universe. These systems are drawn from the MOSFIRE Deep Evolution Field (MOSDEF) Survey at $1.4 \leq z \leq 3.8$, and are interpreted as early-stage galaxy mergers. Galaxy pairs in our sample are identified as two objects whose spectra were collected on the same Keck… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.09978v2-abstract-full').style.display = 'inline'; document.getElementById('1808.09978v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1808.09978v2-abstract-full" style="display: none;"> We study the properties of 30 spectroscopically-identified pairs of galaxies observed during the peak epoch of star formation in the universe. These systems are drawn from the MOSFIRE Deep Evolution Field (MOSDEF) Survey at $1.4 \leq z \leq 3.8$, and are interpreted as early-stage galaxy mergers. Galaxy pairs in our sample are identified as two objects whose spectra were collected on the same Keck/MOSFIRE spectroscopic slit. Accordingly, all pairs in the sample have projected separations $R_{\rm proj}\leq 60$ kpc. The velocity separation for pairs was required to be $螖v \leq 500 \mbox{ km s}^{-1}$, which is a standard threshold for defining interacting galaxy pairs at low redshift. Stellar mass ratios in our sample range from 1.1 to 550, with 12 ratios closer than or equal to 3:1, the common definition of a "major merger." Studies of merging pairs in the local universe indicate anenhancement in star-formation activity and deficit in gas-phase oxygen abundance relative to isolated galaxies of the same mass. We compare the MOSDEF pairs sample to a control sample of isolated galaxies at the same redshift, finding no measurable SFR enhancement or metallicity deficit at fixed stellar mass for the pairs sample. The lack of significant difference between the average properties of pairs and control samples appears in contrast to results from low-redshift studies, although the small sample size and lower signal-to-noise of the high-redshift data limit definitive conclusions on redshift evolution. These results are consistent with some theoretical works suggesting a reduced differential effect of pre-coalescence mergers on galaxy properties at high redshift -- specifically that pre-coalescence mergers do not drive strong starbursts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.09978v2-abstract-full').style.display = 'none'; document.getElementById('1808.09978v2-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 February, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 August, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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, 7 figures, 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/1808.05617">arXiv:1808.05617</a> <span> [<a href="https://arxiv.org/pdf/1808.05617">pdf</a>, <a href="https://arxiv.org/ps/1808.05617">ps</a>, <a href="https://arxiv.org/format/1808.05617">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/aad500">10.3847/1538-4357/aad500 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Black Holes and Neutron Stars in Nearby Galaxies: Insights from NuSTAR </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Vulic%2C+N">Neven Vulic</a>, <a href="/search/?searchtype=author&query=Hornschemeier%2C+A+E">Ann E. Hornschemeier</a>, <a href="/search/?searchtype=author&query=Wik%2C+D+R">Daniel R. Wik</a>, <a href="/search/?searchtype=author&query=Yukita%2C+M">Mihoko Yukita</a>, <a href="/search/?searchtype=author&query=Zezas%2C+A">Andreas Zezas</a>, <a href="/search/?searchtype=author&query=Ptak%2C+A+F">Andrew F. Ptak</a>, <a href="/search/?searchtype=author&query=Lehmer%2C+B+D">Bret D. Lehmer</a>, <a href="/search/?searchtype=author&query=Antoniou%2C+V">Valsamo Antoniou</a>, <a href="/search/?searchtype=author&query=Maccarone%2C+T+J">Thomas J. Maccarone</a>, <a href="/search/?searchtype=author&query=Williams%2C+B+F">Benjamin F. Williams</a>, <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</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="1808.05617v1-abstract-short" style="display: inline;"> Nearby galaxy surveys have long classified X-ray binaries (XRBs) by the mass category of their donor stars (high-mass and low-mass). The NuSTAR observatory, which provides imaging data at E $>10$ keV, has enabled the classification of extragalactic XRBs by their compact object type: neutron star (NS) or black hole (BH). We analyzed NuSTAR/Chandra/XMM-Newton observations from a NuSTAR-selected samp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.05617v1-abstract-full').style.display = 'inline'; document.getElementById('1808.05617v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1808.05617v1-abstract-full" style="display: none;"> Nearby galaxy surveys have long classified X-ray binaries (XRBs) by the mass category of their donor stars (high-mass and low-mass). The NuSTAR observatory, which provides imaging data at E $>10$ keV, has enabled the classification of extragalactic XRBs by their compact object type: neutron star (NS) or black hole (BH). We analyzed NuSTAR/Chandra/XMM-Newton observations from a NuSTAR-selected sample of 12 galaxies within 5 Mpc having stellar masses ($M_{\star}$) $10^{7-11}$ $M_{\odot}$ and star formation rates (SFR) $\approx0.01-15$ $M_{\odot}$ yr$^{-1}$. We detect 128 NuSTAR sources to a sensitivity of $\approx10^{38}$ erg s$^{-1}$. Using NuSTAR color-intensity and color-color diagrams we classify 43 of these sources as candidate NS and 47 as candidate BH. We further subdivide BH by accretion states (soft, intermediate, and hard) and NS by weak (Z/Atoll) and strong (accreting pulsar) magnetic field. Using 8 normal (Milky Way-type) galaxies in the sample, we confirm the relation between SFR and galaxy X-ray point source luminosity in the 4-25 and 12-25 keV energy bands. We also constrain galaxy X-ray point source luminosity using the relation $L_{\rm{X}}=伪M_{\star}+尾\text{SFR}$, finding agreement with previous work. The XLF of all sources in the 4-25 and 12-25 keV energy bands matches with the $伪=1.6$ slope for high-mass XRBs. We find that NS XLFs suggest a decline beginning at the Eddington limit for a 1.4 $M_{\odot}$ NS, whereas the BH fraction shows an approximate monotonic increase in the 4-25 and 12-25keV energy bands. We calculate the overall ratio of BH to NS to be $\approx1$ for 4-25 keV and $\approx2$ for 12-25 keV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.05617v1-abstract-full').style.display = 'none'; document.getElementById('1808.05617v1-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, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">38 pages, 12 figures, 8 tables. 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/1808.00970">arXiv:1808.00970</a> <span> [<a href="https://arxiv.org/pdf/1808.00970">pdf</a>, <a href="https://arxiv.org/format/1808.00970">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/aada4e">10.3847/1538-4357/aada4e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Low-luminosity AGN and X-ray binary populations in COSMOS star-forming galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</a>, <a href="/search/?searchtype=author&query=Civano%2C+F">Francesca Civano</a>, <a href="/search/?searchtype=author&query=Fabbiano%2C+G">Giuseppina Fabbiano</a>, <a href="/search/?searchtype=author&query=Elvis%2C+M">Martin Elvis</a>, <a href="/search/?searchtype=author&query=Marchesi%2C+S">Stefano Marchesi</a>, <a href="/search/?searchtype=author&query=Miyaji%2C+T">Takamitsu Miyaji</a>, <a href="/search/?searchtype=author&query=Zezas%2C+A">Andreas Zezas</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="1808.00970v1-abstract-short" style="display: inline;"> We present an X-ray stacking analysis of $\sim$75,000 star-forming galaxies between $0.1<z<5.0$ using the Chandra COSMOS Legacy survey to study the X-ray emission of low-luminosity active galactic nuclei (AGN) and its connection to host galaxy properties. The stacks at $z<0.9$ have luminosity limits as low as $10^{40}-10^{41}$ erg s$^{-1}$, a regime in which X-ray binaries (XRBs) can dominate the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.00970v1-abstract-full').style.display = 'inline'; document.getElementById('1808.00970v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1808.00970v1-abstract-full" style="display: none;"> We present an X-ray stacking analysis of $\sim$75,000 star-forming galaxies between $0.1<z<5.0$ using the Chandra COSMOS Legacy survey to study the X-ray emission of low-luminosity active galactic nuclei (AGN) and its connection to host galaxy properties. The stacks at $z<0.9$ have luminosity limits as low as $10^{40}-10^{41}$ erg s$^{-1}$, a regime in which X-ray binaries (XRBs) can dominate the X-ray emission. Comparing the measured luminosities to established XRB scaling relations, we find that the redshift evolution of the luminosity per star formation rate (SFR) of XRBs depends sensitively on the assumed obscuration and may be weaker than previously found. The XRB scaling relation based on stacks from the Chandra Deep Field South overestimates the XRB contribution to the COSMOS high specific SFR (sSFR) stacks, possibly due to a bias affecting the CDF-S stacks because of their small galaxy samples. After subtracting the estimated XRB contribution from the stacks, we find that most stacks at $z>1.3$ exhibit a significant X-ray excess indicating nuclear emission. The AGN emission is strongly correlated with stellar mass but does not exhibit an additional correlation with SFR. The hardness ratios of the high-redshift stacks indicate that the AGN are substantially obscured ($N_{\mathrm{H}}\sim10^{23}$ cm$^{-2}$). These obscured AGN are not identified by IRAC color selection and have $L_X\sim10^{41}-10^{43}$ erg s$^{-1}$, consistent with accretion at an Eddington rate of $\sim10^{-3}$ onto $10^7-10^8 M_{\odot}$ black holes. Combining our results with other X-ray studies suggests that AGN obscuration depends on stellar mass and an additional variable, possibly the Eddington rate. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.00970v1-abstract-full').style.display = 'none'; document.getElementById('1808.00970v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 August, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">24 pages, 12 figures, 3 tables (2 tables available in full online or by request)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1711.00224">arXiv:1711.00224</a> <span> [<a href="https://arxiv.org/pdf/1711.00224">pdf</a>, <a href="https://arxiv.org/format/1711.00224">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/aabcbd">10.3847/1538-4357/aabcbd <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MOSDEF survey: a stellar mass-SFR-metallicity relation exists at $z\sim2.3$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Sanders%2C+R+L">Ryan L. Sanders</a>, <a href="/search/?searchtype=author&query=Shapley%2C+A+E">Alice E. Shapley</a>, <a href="/search/?searchtype=author&query=Kriek%2C+M">Mariska Kriek</a>, <a href="/search/?searchtype=author&query=Freeman%2C+W+R">William R. Freeman</a>, <a href="/search/?searchtype=author&query=Reddy%2C+N+A">Naveen A. Reddy</a>, <a href="/search/?searchtype=author&query=Siana%2C+B">Brian Siana</a>, <a href="/search/?searchtype=author&query=Coil%2C+A+L">Alison L. Coil</a>, <a href="/search/?searchtype=author&query=Mobasher%2C+B">Bahram Mobasher</a>, <a href="/search/?searchtype=author&query=Dav%C3%A9%2C+R">Romeel Dav茅</a>, <a href="/search/?searchtype=author&query=Shivaei%2C+I">Irene Shivaei</a>, <a href="/search/?searchtype=author&query=Azadi%2C+M">Mojegan Azadi</a>, <a href="/search/?searchtype=author&query=Price%2C+S+H">Sedona H. Price</a>, <a href="/search/?searchtype=author&query=Leung%2C+G">Gene Leung</a>, <a href="/search/?searchtype=author&query=Fetherholf%2C+T">Tara Fetherholf</a>, <a href="/search/?searchtype=author&query=de+Groot%2C+L">Laura de Groot</a>, <a href="/search/?searchtype=author&query=Zick%2C+T">Tom Zick</a>, <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</a>, <a href="/search/?searchtype=author&query=Barro%2C+G">Guillermo Barro</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="1711.00224v2-abstract-short" style="display: inline;"> We investigate the nature of the relation among stellar mass, star-formation rate, and gas-phase metallicity (the M$_*$-SFR-Z relation) at high redshifts using a sample of 260 star-forming galaxies at $z\sim2.3$ from the MOSDEF survey. We present an analysis of the high-redshift M$_*$-SFR-Z relation based on several emission-line ratios for the first time. We show that a M$_*$-SFR-Z relation clear… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1711.00224v2-abstract-full').style.display = 'inline'; document.getElementById('1711.00224v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1711.00224v2-abstract-full" style="display: none;"> We investigate the nature of the relation among stellar mass, star-formation rate, and gas-phase metallicity (the M$_*$-SFR-Z relation) at high redshifts using a sample of 260 star-forming galaxies at $z\sim2.3$ from the MOSDEF survey. We present an analysis of the high-redshift M$_*$-SFR-Z relation based on several emission-line ratios for the first time. We show that a M$_*$-SFR-Z relation clearly exists at $z\sim2.3$. The strength of this relation is similar to predictions from cosmological hydrodynamical simulations. By performing a direct comparison of stacks of $z\sim0$ and $z\sim2.3$ galaxies, we find that $z\sim2.3$ galaxies have $\sim0.1$ dex lower metallicity at fixed M$_*$ and SFR. In the context of chemical evolution models, this evolution of the M$_*$-SFR-Z relation suggests an increase with redshift of the mass-loading factor at fixed M$_*$, as well as a decrease in the metallicity of infalling gas that is likely due to a lower importance of gas recycling relative to accretion from the intergalactic medium at high redshifts. Performing this analysis simultaneously with multiple metallicity-sensitive line ratios allows us to rule out the evolution in physical conditions (e.g., N/O ratio, ionization parameter, and hardness of the ionizing spectrum) at fixed metallicity as the source of the observed trends with redshift and with SFR at fixed M$_*$ at $z\sim2.3$. While this study highlights the promise of performing high-order tests of chemical evolution models at high redshifts, detailed quantitative comparisons ultimately await a full understanding of the evolution of metallicity calibrations with redshift. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1711.00224v2-abstract-full').style.display = 'none'; document.getElementById('1711.00224v2-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 June, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 November, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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, 8 figures, 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/1705.08902">arXiv:1705.08902</a> <span> [<a href="https://arxiv.org/pdf/1705.08902">pdf</a>, <a href="https://arxiv.org/ps/1705.08902">ps</a>, <a href="https://arxiv.org/format/1705.08902">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/aa6ff4">10.3847/1538-4357/aa6ff4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An XMM-Newton and NuSTAR study of IGR J18214-1318: a non-pulsating high-mass X-ray binary with a neutron star </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</a>, <a href="/search/?searchtype=author&query=Tomsick%2C+J+A">John A. Tomsick</a>, <a href="/search/?searchtype=author&query=Bachetti%2C+M">Matteo Bachetti</a>, <a href="/search/?searchtype=author&query=Krivonos%2C+R+A">Roman A. Krivonos</a>, <a href="/search/?searchtype=author&query=F%C3%BCrst%2C+F">Felix F眉rst</a>, <a href="/search/?searchtype=author&query=Natalucci%2C+L">Lorenzo Natalucci</a>, <a href="/search/?searchtype=author&query=Pottschmidt%2C+K">Katja Pottschmidt</a>, <a href="/search/?searchtype=author&query=Wilms%2C+J">J枚rn Wilms</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1705.08902v1-abstract-short" style="display: inline;"> IGR J18214-1318, a Galactic source discovered by the International Gamma-Ray Astrophysics Laboratory, is a high-mass X-ray binary (HMXB) with a supergiant O-type stellar donor. We report on the XMM-Newton and NuSTAR observations that were undertaken to determine the nature of the compact object in this system. This source exhibits high levels of aperiodic variability, but no periodic pulsations ar… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1705.08902v1-abstract-full').style.display = 'inline'; document.getElementById('1705.08902v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1705.08902v1-abstract-full" style="display: none;"> IGR J18214-1318, a Galactic source discovered by the International Gamma-Ray Astrophysics Laboratory, is a high-mass X-ray binary (HMXB) with a supergiant O-type stellar donor. We report on the XMM-Newton and NuSTAR observations that were undertaken to determine the nature of the compact object in this system. This source exhibits high levels of aperiodic variability, but no periodic pulsations are detected with a 90% confidence upper limit of 2% fractional rms between 0.00003-88 Hz, a frequency range that includes the typical pulse periods of neutron stars (NSs) in HMXBs (0.1-10$^3$ s). Although the lack of pulsations prevents us from definitively identifying the compact object in IGR J18214-1318, the presence of an exponential cutoff with e-folding energy $\lesssim30$ keV in its 0.3-79 keV spectrum strongly suggests that the compact object is an NS. The X-ray spectrum also shows a Fe K$伪$ emission line and a soft excess, which can be accounted for by either a partial-covering absorber with $N_{\mathrm{H}}\approx10^{23}$ cm$^{-2}$ which could be due to the inhomogeneous supergiant wind, or a blackbody component with $kT=1.74^{+0.04}_{-0.05}$ keV and $R_{BB}\approx0.3$ km, which may originate from NS hot spots. Although neither explanation for the soft excess can be excluded, the former is more consistent with the properties observed in other supergiant HMXBs. We compare IGR J18214-1318 to other HMXBs that lack pulsations or have long pulsation periods beyond the range covered by our observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1705.08902v1-abstract-full').style.display = 'none'; document.getElementById('1705.08902v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 May, 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">15 pages, 12 figures, 4 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/1703.00021">arXiv:1703.00021</a> <span> [<a href="https://arxiv.org/pdf/1703.00021">pdf</a>, <a href="https://arxiv.org/format/1703.00021">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/aa61fc">10.3847/1538-4365/aa61fc <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The NuSTAR Hard X-ray Survey of the Norma Arm Region </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</a>, <a href="/search/?searchtype=author&query=Tomsick%2C+J+A">John A. Tomsick</a>, <a href="/search/?searchtype=author&query=Hong%2C+J">JaeSub Hong</a>, <a href="/search/?searchtype=author&query=Gotthelf%2C+E+V">Eric V. Gotthelf</a>, <a href="/search/?searchtype=author&query=Bauer%2C+F">Franz Bauer</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=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=Clavel%2C+M">Ma茂ca Clavel</a>, <a href="/search/?searchtype=author&query=Corral-Santana%2C+J+M">Jes煤s M. Corral-Santana</a>, <a href="/search/?searchtype=author&query=Hailey%2C+C+J">Charles J. Hailey</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=Alexander%2C+D+M">David M. Alexander</a>, <a href="/search/?searchtype=author&query=Barret%2C+D">Didier Barret</a>, <a href="/search/?searchtype=author&query=Boggs%2C+S+E">Steven 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=Forster%2C+K">Karl Forster</a>, <a href="/search/?searchtype=author&query=Giommi%2C+P">Paolo Giommi</a>, <a href="/search/?searchtype=author&query=Grefenstette%2C+B+W">Brian W. Grefenstette</a>, <a href="/search/?searchtype=author&query=Harrison%2C+F+A">Fiona A. Harrison</a>, <a href="/search/?searchtype=author&query=Hornstrup%2C+A">Allan Hornstrup</a>, <a href="/search/?searchtype=author&query=Kitaguchi%2C+T">Takao Kitaguchi</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="1703.00021v1-abstract-short" style="display: inline;"> We present a catalog of hard X-ray sources in a square-degree region surveyed by NuSTAR in the direction of the Norma spiral arm. This survey has a total exposure time of 1.7 Ms, and typical and maximum exposure depths of 50 ks and 1 Ms, respectively. In the area of deepest coverage, sensitivity limits of $5\times10^{-14}$ and $4\times10^{-14}$ erg s$^{-1}$ cm$^{-2}$ in the 3-10 and 10-20 keV band… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.00021v1-abstract-full').style.display = 'inline'; document.getElementById('1703.00021v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1703.00021v1-abstract-full" style="display: none;"> We present a catalog of hard X-ray sources in a square-degree region surveyed by NuSTAR in the direction of the Norma spiral arm. This survey has a total exposure time of 1.7 Ms, and typical and maximum exposure depths of 50 ks and 1 Ms, respectively. In the area of deepest coverage, sensitivity limits of $5\times10^{-14}$ and $4\times10^{-14}$ erg s$^{-1}$ cm$^{-2}$ in the 3-10 and 10-20 keV bands, respectively, are reached. Twenty-eight sources are firmly detected and ten are detected with low significance; eight of the 38 sources are expected to be active galactic nuclei. The three brightest sources were previously identified as a low-mass X-ray binary, high-mass X-ray binary, and pulsar wind nebula. Based on their X-ray properties and multi-wavelength counterparts, we identify the likely nature of the other sources as two colliding wind binaries, three pulsar wind nebulae, a black hole binary, and a plurality of cataclysmic variables (CVs). The CV candidates in the Norma region have plasma temperatures of $\approx$10-20 keV, consistent with the Galactic Ridge X-ray emission spectrum but lower than temperatures of CVs near the Galactic Center. This temperature difference may indicate that the Norma region has a lower fraction of intermediate polars relative to other types of CVs compared to the Galactic Center. The NuSTAR log$N$-log$S$ distribution in the 10-20 keV band is consistent with the distribution measured by Chandra at 2-10 keV if the average source spectrum is assumed to be a thermal model with $kT\approx15$~keV, as observed for the CV candidates. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.00021v1-abstract-full').style.display = 'none'; document.getElementById('1703.00021v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 February, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">42 pages, 12 figures, 11 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/1605.08802">arXiv:1605.08802</a> <span> [<a href="https://arxiv.org/pdf/1605.08802">pdf</a>, <a href="https://arxiv.org/format/1605.08802">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/stw1330">10.1093/mnras/stw1330 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> IGR J18293-1213 is an eclipsing Cataclysmic Variable </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Clavel%2C+M">Ma茂ca Clavel</a>, <a href="/search/?searchtype=author&query=Tomsick%2C+J+A">J. A. Tomsick</a>, <a href="/search/?searchtype=author&query=Bodaghee%2C+A">A. Bodaghee</a>, <a href="/search/?searchtype=author&query=Chiu%2C+J+-">J. -L. Chiu</a>, <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">F. M. Fornasini</a>, <a href="/search/?searchtype=author&query=Hong%2C+J">J. Hong</a>, <a href="/search/?searchtype=author&query=Krivonos%2C+R">R. Krivonos</a>, <a href="/search/?searchtype=author&query=Ponti%2C+G">G. Ponti</a>, <a href="/search/?searchtype=author&query=Rahoui%2C+F">F. Rahoui</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="1605.08802v1-abstract-short" style="display: inline;"> Studying the population of faint hard X-ray sources along the plane of the Galaxy is challenging because of high-extinction and crowding, which make the identification of individual sources more difficult. IGR J18293-1213 is part of the population of persistent sources which have been discovered by the INTEGRAL satellite. We report on NuSTAR and Swift/XRT observations of this source, performed on… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.08802v1-abstract-full').style.display = 'inline'; document.getElementById('1605.08802v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1605.08802v1-abstract-full" style="display: none;"> Studying the population of faint hard X-ray sources along the plane of the Galaxy is challenging because of high-extinction and crowding, which make the identification of individual sources more difficult. IGR J18293-1213 is part of the population of persistent sources which have been discovered by the INTEGRAL satellite. We report on NuSTAR and Swift/XRT observations of this source, performed on 2015 September 11. We detected three eclipsing intervals in the NuSTAR light curve, allowing us to constrain the duration of these eclipses, $螖t = 30.8^{+6.3}_{-0.0}$ min, and the orbital period of the system, $T = 6.92\pm0.01$ hr. Even though we only report an upper limit on the amplitude of a putative spin modulation, the orbital period and the hard thermal Bremsstrahlung spectrum of IGR J18293-1213 provide strong evidence that this source is a magnetic Cataclysmic Variable (CV). Our NuSTAR and Swift/XRT joint spectral analysis places strong constraints on the white dwarf mass $M_{\rm wd} = 0.78^{+0.10}_{-0.09}$ M$_\odot$. Assuming that the mass to radius ratio of the companion star $M_* / R_* = 1$ (solar units) and using $T$, $螖t$ and $M_{\rm wd}$, we derived the mass of the companion star $M_* = 0.82\pm0.01$ M$_\odot$, the orbital separation of the binary system $a=2.14\pm0.04$ R$_\odot$, and its orbital inclination compared to the line of sight $i=(72.2^{+2.4}_{-0.0})\pm1.0^\circ$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.08802v1-abstract-full').style.display = 'none'; document.getElementById('1605.08802v1-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, 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">8 pages, 5 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/1605.03882">arXiv:1605.03882</a> <span> [<a href="https://arxiv.org/pdf/1605.03882">pdf</a>, <a href="https://arxiv.org/format/1605.03882">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/10.3847/0004-637X/825/2/132">10.3847/0004-637X/825/2/132 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> NuSTAR Hard X-ray Survey of the Galactic Center Region II: X-ray Point Sources </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Hong%2C+J">JaeSub Hong</a>, <a href="/search/?searchtype=author&query=Mori%2C+K">Kaya Mori</a>, <a href="/search/?searchtype=author&query=Hailey%2C+C+J">Charles J. Hailey</a>, <a href="/search/?searchtype=author&query=Nynka%2C+M">Melania Nynka</a>, <a href="/search/?searchtype=author&query=Zhang%2C+S">Shuo Zhang</a>, <a href="/search/?searchtype=author&query=Gotthelf%2C+E">Eric Gotthelf</a>, <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</a>, <a href="/search/?searchtype=author&query=Krivonos%2C+R">Roman Krivonos</a>, <a href="/search/?searchtype=author&query=Bauer%2C+F">Franz Bauer</a>, <a href="/search/?searchtype=author&query=Perez%2C+K">Kerstin Perez</a>, <a href="/search/?searchtype=author&query=Tomsick%2C+J+A">John A. Tomsick</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=Clavel%2C+M">Ma茂ca Clavel</a>, <a href="/search/?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/?searchtype=author&query=Grindlay%2C+J+E">Jonathan E. Grindlay</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+M">David M. Alexander</a>, <a href="/search/?searchtype=author&query=Aramaki%2C+T">Tsuguo Aramaki</a>, <a href="/search/?searchtype=author&query=Baganoff%2C+F+K">Frederick K. Baganoff</a>, <a href="/search/?searchtype=author&query=Barret%2C+D">David Barret</a>, <a href="/search/?searchtype=author&query=Barri%C3%A8re%2C+N">Nicolas Barri猫re</a>, <a href="/search/?searchtype=author&query=Boggs%2C+S+E">Steven E. Boggs</a>, <a href="/search/?searchtype=author&query=Canipe%2C+A+M">Alicia M. Canipe</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> , et al. (19 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="1605.03882v1-abstract-short" style="display: inline;"> We present the first survey results of hard X-ray point sources in the Galactic Center (GC) region by NuSTAR. We have discovered 70 hard (3-79 keV) X-ray point sources in a 0.6 deg^2 region around Sgr A* with a total exposure of 1.7 Ms, and 7 sources in the Sgr B2 field with 300 ks. We identify clear Chandra counterparts for 58 NuSTAR sources and assign candidate counterparts for the remaining 19.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.03882v1-abstract-full').style.display = 'inline'; document.getElementById('1605.03882v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1605.03882v1-abstract-full" style="display: none;"> We present the first survey results of hard X-ray point sources in the Galactic Center (GC) region by NuSTAR. We have discovered 70 hard (3-79 keV) X-ray point sources in a 0.6 deg^2 region around Sgr A* with a total exposure of 1.7 Ms, and 7 sources in the Sgr B2 field with 300 ks. We identify clear Chandra counterparts for 58 NuSTAR sources and assign candidate counterparts for the remaining 19. The NuSTAR survey reaches X-ray luminosities of ~4 x and ~8 x 10^32 erg s^-1 at the GC (8 kpc) in the 3-10 and 10-40 keV bands, respectively. The source list includes three persistent luminous X-ray binaries and the likely run-away pulsar called the Cannonball. New source-detection significance maps reveal a cluster of hard (>10 keV) X-ray sources near the Sgr A diffuse complex with no clear soft X-ray counterparts. The severe extinction observed in the Chandra spectra indicates that all the NuSTAR sources are in the central bulge or are of extragalactic origin. Spectral analysis of relatively bright NuSTAR sources suggests that magnetic cataclysmic variables constitute a large fraction (>40-60%). Both spectral analysis and logN-logS distributions of the NuSTAR sources indicate that the X-ray spectra of the NuSTAR sources should have kT > 20 keV on average for a single temperature thermal plasma model or an average photon index of Gamma = 1.5 - 2 for a power-law model. These findings suggest that the GC X-ray source population may contain a larger fraction of X-ray binaries with high plasma temperatures than the field population. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.03882v1-abstract-full').style.display = 'none'; document.getElementById('1605.03882v1-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 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">32 pages, 15 figures, 7 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/1512.00044">arXiv:1512.00044</a> <span> [<a href="https://arxiv.org/pdf/1512.00044">pdf</a>, <a href="https://arxiv.org/ps/1512.00044">ps</a>, <a href="https://arxiv.org/format/1512.00044">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/10.3847/0004-637X/816/1/38">10.3847/0004-637X/816/1/38 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Chandra Observations of Eight Sources Discovered by INTEGRAL </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=Krivonos%2C+R">Roman Krivonos</a>, <a href="/search/?searchtype=author&query=Wang%2C+Q">Qinan Wang</a>, <a href="/search/?searchtype=author&query=Bodaghee%2C+A">Arash Bodaghee</a>, <a href="/search/?searchtype=author&query=Chaty%2C+S">Sylvain Chaty</a>, <a href="/search/?searchtype=author&query=Rahoui%2C+F">Farid Rahoui</a>, <a href="/search/?searchtype=author&query=Rodriguez%2C+J">Jerome Rodriguez</a>, <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</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="1512.00044v1-abstract-short" style="display: inline;"> We report on 0.3-10 keV observations with the Chandra X-ray Observatory of eight hard X-ray sources discovered within 8 degrees of the Galactic plane by the INTEGRAL satellite. The short (5 ks) Chandra observations of the IGR source fields have yielded very likely identifications of X-ray counterparts for three of the IGR sources: IGR J14091-6108, IGR J18088-2741, and IGR J18381-0924. The first tw… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1512.00044v1-abstract-full').style.display = 'inline'; document.getElementById('1512.00044v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1512.00044v1-abstract-full" style="display: none;"> We report on 0.3-10 keV observations with the Chandra X-ray Observatory of eight hard X-ray sources discovered within 8 degrees of the Galactic plane by the INTEGRAL satellite. The short (5 ks) Chandra observations of the IGR source fields have yielded very likely identifications of X-ray counterparts for three of the IGR sources: IGR J14091-6108, IGR J18088-2741, and IGR J18381-0924. The first two have very hard spectra in the Chandra band that can be described by a power-law with photon indices of Gamma = 0.6+/-0.4 and -0.7(+0.4)(-0.3), respectively (90% confidence errors are given), and both have a unique near-IR counterpart consistent with the Chandra position. IGR J14091-6108 also displays a strong iron line and a relatively low X-ray luminosity, and we argue that the most likely source type is a Cataclysmic Variable (CV), although we do not completely rule out the possibility of a High Mass X-ray Binary. IGR J18088-2741 has an optical counterpart with a previously measured 6.84 hr periodicity, which may be the binary orbital period. We also detect five cycles of a possible 800-950 s period in the Chandra light curve, which may be the compact object spin period. We suggest that IGR J18088-2741 is also most likely a CV. For IGR J18381-0924, the spectrum is intrinsically softer with Gamma = 1.5(+0.5)(-0.4), and it is moderately absorbed, nH = (4+/-1)e22 cm-2. There are two near-IR sources consistent with the Chandra position, and they are both classified as galaxies, making it likely that IGR J18381-0924 is an Active Galactic Nucleus (AGN). For the other five IGR sources, we provide lists of nearby Chandra sources, which may be used along with further observations to identify the correct counterparts, and we discuss the implications of the low inferred Chandra count rates for these five sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1512.00044v1-abstract-full').style.display = 'none'; document.getElementById('1512.00044v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 November, 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">Accepted by ApJ, 14 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/1409.7701">arXiv:1409.7701</a> <span> [<a href="https://arxiv.org/pdf/1409.7701">pdf</a>, <a href="https://arxiv.org/ps/1409.7701">ps</a>, <a href="https://arxiv.org/format/1409.7701">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/796/2/105">10.1088/0004-637X/796/2/105 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Norma Arm Region Chandra Survey: X-ray Populations in the Spiral Arms </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</a>, <a href="/search/?searchtype=author&query=Tomsick%2C+J+A">John A. Tomsick</a>, <a href="/search/?searchtype=author&query=Bodaghee%2C+A">Arash Bodaghee</a>, <a href="/search/?searchtype=author&query=Krivonos%2C+R+A">Roman A. Krivonos</a>, <a href="/search/?searchtype=author&query=An%2C+H">Hongjun An</a>, <a href="/search/?searchtype=author&query=Rahoui%2C+F">Farid Rahoui</a>, <a href="/search/?searchtype=author&query=Gotthelf%2C+E+V">Eric V. Gotthelf</a>, <a href="/search/?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</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="1409.7701v1-abstract-short" style="display: inline;"> We present a catalog of 1415 X-ray sources identified in the Norma arm region Chandra survey (NARCS), which covers a 2 deg x 0.8 deg region in the direction of the Norma spiral arm to a depth of $\approx$20 ks. Of these sources, 1130 are point-like sources detected with $\geq3蟽$ confidence in at least one of three energy bands (0.5-10, 0.5-2, and 2-10 keV), five have extended emission, and the rem… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.7701v1-abstract-full').style.display = 'inline'; document.getElementById('1409.7701v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1409.7701v1-abstract-full" style="display: none;"> We present a catalog of 1415 X-ray sources identified in the Norma arm region Chandra survey (NARCS), which covers a 2 deg x 0.8 deg region in the direction of the Norma spiral arm to a depth of $\approx$20 ks. Of these sources, 1130 are point-like sources detected with $\geq3蟽$ confidence in at least one of three energy bands (0.5-10, 0.5-2, and 2-10 keV), five have extended emission, and the remainder are detected at low significance. Since most sources have too few counts to permit individual classification, they are divided into five spectral groups defined by their quantile properties. We analyze stacked spectra of X-ray sources within each group, in conjunction with their fluxes, variability, and infrared counterparts, to identify the dominant populations in our survey. We find that $\sim$50% of our sources are foreground sources located within 1-2 kpc, which is consistent with expectations from previous surveys. Approximately 20% of sources are likely located in the proximity of the Scutum-Crux and near Norma arm, while 30% are more distant, in the proximity of the far Norma arm or beyond. We argue that a mixture of magnetic and nonmagnetic CVs dominates the Scutum-Crux and near Norma arms, while intermediate polars (IPs) and high-mass stars (isolated or in binaries) dominate the far Norma arm. We also present the cumulative number count distribution for sources in our survey that are detected in the hard energy band. A population of very hard sources in the vicinity of the far Norma arm and active galactic nuclei dominate the hard X-ray emission down to $f_X\approx10^{-14}$ erg cm$^{-2}$ s$^{-1}$, but the distribution curve flattens at fainter fluxes. We find good agreement between the observed distribution and predictions based on other surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.7701v1-abstract-full').style.display = 'none'; document.getElementById('1409.7701v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 September, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">27 pages, 19 figures, 12 tables, catalog will be made available in published ApJ version and by personal request</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1406.4514">arXiv:1406.4514</a> <span> [<a href="https://arxiv.org/pdf/1406.4514">pdf</a>, <a href="https://arxiv.org/ps/1406.4514">ps</a>, <a href="https://arxiv.org/format/1406.4514">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201424006">10.1051/0004-6361/201424006 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Near-infrared spectroscopy of 20 new Chandra sources in the Norma Arm </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Rahoui%2C+F">Farid Rahoui</a>, <a href="/search/?searchtype=author&query=Tomsick%2C+J+A">John A. Tomsick</a>, <a href="/search/?searchtype=author&query=Fornasini%2C+F+M">Francesca M. Fornasini</a>, <a href="/search/?searchtype=author&query=Bodaghee%2C+A">Arash Bodaghee</a>, <a href="/search/?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</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="1406.4514v1-abstract-short" style="display: inline;"> We report on CTIO/NEWFIRM and CTIO/OSIRIS photometric and spectroscopic observations of 20 new X-ray (0.5-10 keV) emitters discovered in the Norma Arm Region Chandra Survey (NARCS). NEWFIRM photometry was obtained to pinpoint the near-infrared counterparts of NARCS sources, while OSIRIS spectroscopy was used to help identify 20 sources with possible high mass X-ray binary properties. We find that… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1406.4514v1-abstract-full').style.display = 'inline'; document.getElementById('1406.4514v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1406.4514v1-abstract-full" style="display: none;"> We report on CTIO/NEWFIRM and CTIO/OSIRIS photometric and spectroscopic observations of 20 new X-ray (0.5-10 keV) emitters discovered in the Norma Arm Region Chandra Survey (NARCS). NEWFIRM photometry was obtained to pinpoint the near-infrared counterparts of NARCS sources, while OSIRIS spectroscopy was used to help identify 20 sources with possible high mass X-ray binary properties. We find that (1) two sources are WN8 Wolf-Rayet stars, maybe in colliding wind binaries, part of the massive star cluster Mercer 81; (2) two are emission-line stars, possibly in X-ray binaries, that exhibit near- and mid-infrared excesses either due to free-free emission from the decretion discs of Be stars or warm dust in the stellar winds of peculiar massive stars such as B[e] supergiants or luminous blue variables; (3) one is a B8-A3 IV-V star that could be in a quiescent high mass X-ray binary system; (4) two are cataclysmic variables including one intermediate polar; (5) three may be neutron star symbiotic binaries; (6) five are most likely white dwarf symbiotic binaries; and (7) five exhibit properties more consistent with isolated giant/dwarf stars. The possible detection of one to three high mass X-ray binaries is in good agreement with our predictions. However, our study illustrates the difficulty of clearly differentiating quiescent or intermediate X-ray luminosity systems from isolated massive stars, which may lead to an underestimation of the number of known high mass X-ray binaries. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1406.4514v1-abstract-full').style.display = 'none'; document.getElementById('1406.4514v1-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, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">17 pages, 14 figures, 7 tables. Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 568, A54 (2014) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1402.2292">arXiv:1402.2292</a> <span> [<a href="https://arxiv.org/pdf/1402.2292">pdf</a>, <a href="https://arxiv.org/ps/1402.2292">ps</a>, <a href="https://arxiv.org/format/1402.2292">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/785/1/4">10.1088/0004-637X/785/1/4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> NuSTAR J163433-4738.7: A Fast X-ray Transient in 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=Gotthelf%2C+E+V">Eric V. Gotthelf</a>, <a href="/search/?searchtype=author&query=Rahoui%2C+F">Farid Rahoui</a>, <a href="/search/?searchtype=author&query=Assef%2C+R+J">Roberto J. Assef</a>, <a href="/search/?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/?searchtype=author&query=Bodaghee%2C+A">Arash Bodaghee</a>, <a href="/search/?searchtype=author&query=Boggs%2C+S+E">Steven 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=Fornasini%2C+F+M">Francesca M. Fornasini</a>, <a href="/search/?searchtype=author&query=Grindlay%2C+J">Jonathan 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">Roman Krivonos</a>, <a href="/search/?searchtype=author&query=Natalucci%2C+L">Lorenzo Natalucci</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="1402.2292v2-abstract-short" style="display: inline;"> During hard X-ray observations of the Norma spiral arm region by the Nuclear Spectroscopic Telescope Array (NuSTAR) in 2013 February, a new transient source, NuSTAR J163433-4738.7, was detected at a significance level of 8-sigma in the 3-10 keV bandpass. The source is consistent with having a constant NuSTAR count rate over a period of 40 ks and is also detected simultaneously by Swift at lower si… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1402.2292v2-abstract-full').style.display = 'inline'; document.getElementById('1402.2292v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1402.2292v2-abstract-full" style="display: none;"> During hard X-ray observations of the Norma spiral arm region by the Nuclear Spectroscopic Telescope Array (NuSTAR) in 2013 February, a new transient source, NuSTAR J163433-4738.7, was detected at a significance level of 8-sigma in the 3-10 keV bandpass. The source is consistent with having a constant NuSTAR count rate over a period of 40 ks and is also detected simultaneously by Swift at lower significance. The source is not significantly detected by NuSTAR, Swift, or Chandra in the days before or weeks after the discovery of the transient, indicating that the strong X-ray activity lasted for between ~0.5 and 1.5 days. Near-IR imaging observations were carried out before and after the X-ray activity, but we are not able to identify the counterpart. The combined NuSTAR and Swift energy spectrum is consistent with a power-law with a photon index of Gamma = 4.1(+1.5)(-1.0) (90% confidence errors), a blackbody with kT = 1.2+/-0.3 keV, or a bremsstrahlung model with kT = 3.0(+2.1)(-1.2) keV. The reduced-chi2 values for the three models are not significantly different, ranging from 1.23 to 1.44 for 8 degrees of freedom. The spectrum is strongly absorbed with NH = 2.8(+2.3)(-1.4)e23 cm-2, 9(+15)(-7)e22 cm-2, and 1.7(+1.7)(-0.9)e23 cm-2, for the power-law, blackbody, and bremsstrahlung models, respectively. Although the high column density could be due to material local to the source, it is consistent with absorption from interstellar material along the line of sight at a distance of 11 kpc, which would indicate an X-ray luminosity >1e34 erg/s. Although we do not reach a definitive determination of the nature of NuSTAR J163433-4738.7, we suggest that it may be an unusually bright active binary or a magnetar. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1402.2292v2-abstract-full').style.display = 'none'; document.getElementById('1402.2292v2-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 March, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 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">6 pages, 4 figures, published as ApJ, 785, 4. The name of the source has been revised to NuSTAR J163433-4738.7 in order to comply with the IAU format for NuSTAR sources</span> </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg> <a href="https://info.arxiv.org/help/contact.html"> Contact</a> </li> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>subscribe to arXiv mailings</title><desc>Click here to subscribe</desc><path d="M476 3.2L12.5 270.6c-18.1 10.4-15.8 35.6 2.2 43.2L121 358.4l287.3-253.2c5.5-4.9 13.3 2.6 8.6 8.3L176 407v80.5c0 23.6 28.5 32.9 42.5 15.8L282 426l124.6 52.2c14.2 6 30.4-2.9 33-18.2l72-432C515 7.8 493.3-6.8 476 3.2z"/></svg> <a href="https://info.arxiv.org/help/subscribe"> Subscribe</a> </li> </ul> </div> </div> </div>   <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/license/index.html">Copyright</a></li> <li><a href="https://info.arxiv.org/help/policies/privacy_policy.html">Privacy Policy</a></li> </ul> </div> <div class="column sorry-app-links"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/web_accessibility.html">Web Accessibility Assistance</a></li> <li> <p class="help"> <a class="a11y-main-link" href="https://status.arxiv.org" target="_blank">arXiv Operational Status <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 256 512" class="icon filter-dark_grey" role="presentation"><path d="M224.3 273l-136 136c-9.4 9.4-24.6 9.4-33.9 0l-22.6-22.6c-9.4-9.4-9.4-24.6 0-33.9l96.4-96.4-96.4-96.4c-9.4-9.4-9.4-24.6 0-33.9L54.3 103c9.4-9.4 24.6-9.4 33.9 0l136 136c9.5 9.4 9.5 24.6.1 34z"/></svg></a><br> Get status notifications via <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/email/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg>email</a> or <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/slack/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 448 512" class="icon filter-black" role="presentation"><path d="M94.12 315.1c0 25.9-21.16 47.06-47.06 47.06S0 341 0 315.1c0-25.9 21.16-47.06 47.06-47.06h47.06v47.06zm23.72 0c0-25.9 21.16-47.06 47.06-47.06s47.06 21.16 47.06 47.06v117.84c0 25.9-21.16 47.06-47.06 47.06s-47.06-21.16-47.06-47.06V315.1zm47.06-188.98c-25.9 0-47.06-21.16-47.06-47.06S139 32 164.9 32s47.06 21.16 47.06 47.06v47.06H164.9zm0 23.72c25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06H47.06C21.16 243.96 0 222.8 0 196.9s21.16-47.06 47.06-47.06H164.9zm188.98 47.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06h-47.06V196.9zm-23.72 0c0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06V79.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06V196.9zM283.1 385.88c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06v-47.06h47.06zm0-23.72c-25.9 0-47.06-21.16-47.06-47.06 0-25.9 21.16-47.06 47.06-47.06h117.84c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06H283.1z"/></svg>slack</a> </p> </li> </ul> </div> </div> </div>  </div> </footer> <script src="https://static.arxiv.org/static/base/1.0.0a5/js/member_acknowledgement.js"></script> </body> </html>

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