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1. The $\textit{Nu}$STAR Serendipitous Survey: The 40-month Catalog and the Properties of the Distant High-energy X-Ray Source Population $\textit{text}$

Author

Lansbury, GB, Stern, D, Aird, J, Alexander, DM, Fuentes, C, Harrison, FA, Treister, E, Bauer, FE, Tomsick, JA, Baloković, M, Moro, AD, Gandhi, P, Ajello, M, Annuar, A, Ballantyne, DR, Boggs, SE, Brandt, WN, Brightman, M, Chen, CTJ, Christensen, FE, Civano, F, Comastri, A, Craig, WW, Forster, K, Grefenstette, BW, Hailey, CJ, Hickox, RC, Jiang, B, Jun, HD, Koss, M, Marchesi, S, Melo, AD, Mullaney, Noirot, G, Schulze, S, Walton, DJ, Zappacosta, L, Zhang, WW, Lansbury, George [0000-0002-5328-9827], Aird, James [0000-0003-1908-8463], Walton, Dominic [0000-0001-5819-3552], and Apollo - University of Cambridge Repository

Subjects
surveys, Astrophysics::High Energy Astrophysical Phenomena, quasars: general, galaxies: active, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: nuclei, Xrays: general Supporting material: figure sets, Astrophysics::Galaxy Astrophysics, catalogs, machine-readable tables
Abstract

We present the first full catalog and science results for the $\textit{Nuclear Spectroscopic Telescope Array}$ ($\textit{Nu}$STAR) serendipitous survey. The catalog incorporates data taken during the first 40 months of $\textit{Nu}$STAR operation, which provide ≈20 Ms of effective exposure time over 331 fields, with an areal coverage of 13 deg$^{2}$, and 497 sources detected in total over the 3-24 keV energy range. There are 276 sources with spectroscopic redshifts and classifications, largely resulting from our extensive campaign of ground-based spectroscopic follow-up. We characterize the overall sample in terms of the X-ray, optical, and infrared source properties. The sample is primarily composed of active galactic nuclei (AGNs), detected over a large range in redshift from $z$ = 0.002 to 3.4 (median of $\langle z\rangle =0.56$) = 0.56), but also includes 16 spectroscopically confirmed Galactic sources. There is a large range in X-ray flux, from log(f$_{3-24keV}$/erg s$^{-1}$ cm$^{-2}$) ≈ -14 to -11, and in rest-frame 10-40 keV luminosity, from (L$_{10-40keV}$/erg s$^{-1}$) ≈ 39 to 46, with a median of 44.1. Approximately 79% of the $\textit{Nu}$STAR sources have lower-energy ( 10$^{44}$ erg s$^{-1}$) to ≈80% at the lowest luminosities (LX < 10$^{43}$ erg s$^{-1}$). Our optical spectroscopic analysis finds that the observed fraction of optically obscured AGNs (i.e., the type 2 fraction) is F$_{Type 2}$ = 53$^{+15}_{−14}$%, for a well-defined subset of the 8-24 keV selected sample. This is higher, albeit at a low significance level, than the type 2 fraction measured for redshift- and luminosity-matched AGNs selected by, Please visit the publisher's website.

Published
2017

2. GRS 1739-278 OBSERVED AT VERY LOW LUMINOSITY WITH $\small \textit{XMM-NEWTON}$ AND $\small \textit{NuSTAR}$

Author

Furst, F, Tomsick, JA, Yamaoka, K, Dauser, T, Miller, JM, Clavel, M, Corbel, S, Fabian, A, Garcia, J, Harrison, FA, Loh, A, Kaaret, P, Kalemci, E, Migliari, S, Miller-Jones, JCA, Pottschmidt, K, Rahoui, F, Rodriguez, J, Stern, D, Stuhlinger, M, Walton, DJ, Wilms, J, Fabian, Andrew [0000-0002-9378-4072], Walton, Dominic [0000-0001-5819-3552], and Apollo - University of Cambridge Repository

Subjects
X-rays: binaries, X-rays: individual (GRS 1739-278), accretion, Astrophysics::High Energy Astrophysical Phenomena, accretion disks, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, stars: black holes
Abstract

We present a detailed spectral analysis of $\small \textit{XMM-Newton}$ and $\small \textit{NuSTAR}$ observations of the accreting transient black hole GRS 1739−278 during a very faint low hard state at ~0.02% of the Eddington luminosity (for a distance of 8.5 kpc and a mass of 10 $M_\odot$). The broadband X-ray spectrum between 0.5 and 60 keV can be well-described by a power-law continuum with an exponential cutoff. The continuum is unusually hard for such a low luminosity, with a photon index of $\Gamma$ = 1.39 ± 0.04. We find evidence for an additional reflection component from an optically thick accretion disk at the 98% likelihood level. The reflection fraction is low, with $\mathcal{R}_\text{refl}$ = 0.043$^\text{+0.033}_\text{ -0.023}$. In combination with measurements of the spin and inclination parameters made with $\small \textit{NuSTAR}$ during a brighter hard state by Miller et al., we seek to constrain the accretion disk geometry. Depending on the assumed emissivity profile of the accretion disk, we find a truncation radius of 15–35 $R_\text{g}$ (5–12 $R_\text{ISCO}$) at the 90% confidence limit. These values depend strongly on the assumptions and we discuss possible systematic uncertainties., We thank the schedulers and SOC of XMM-Newton and NuSTAR for making these observations possible. Based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This work is based upon work supported by NASA under award No. NNX16AH17G. J.A.T. acknowledges partial support from NASA under Swift Guest Observer grants NNX15AB81G and NNX15AR52G. E.K. acknowledges support of TUBITAK Project No 115F488. S.C. and A.L. acknowledge funding support from the French Research National Agency: CHAOS project ANR-12-BS05-0009 and the UnivEarthS Labex program of Sorbonne Paris Cité (ANR-10-LABX-0023 and ANR-11-IDEX-0005-02). J.C.A. M.-J. is the recipient of an Australian Research Council Future Fellowship (FT140101082). This work was supported under NASA contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). We would like to thank John E. Davis for the slxfig module, which was used to produce all figures in this work. This research has made use of MAXI data provided by RIKEN, JAXA and the MAXI team. The Swift/BAT transient monitor results were provided by the Swift/BAT team. This research has made use of a collection of ISIS functions (ISISscripts) provided by ECAP/Remeis observatory and MIT.

Published
2017
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3. Modulated high-energy gamma-ray emission from the microquasar Cygnus X-3

Author

Abdo, Aa, Ackermann, M, Ajello, M, Axelsson, M, Baldini, Luca, Ballet, J, Barbiellini, G, Bastieri, D, Baughman, Bm, Bechtol, K, Bellazzini, R, Berenji, B, Blandford, Rd, Bloom, Ed, Bonamente, E, Borgland, Aw, Brez, A, Brigida, M, Bruel, P, Burnett, Th, Buson, S, Caliandro, Ga, Cameron, Ra, Caraveo, Pa, Casandjian, Jm, Cecchi, C, Celik, O, Chaty, S, Cheung, Cc, Chiang, J, Ciprini, S, Claus, R, Cohen Tanugi, J, Cominsky, Lr, Conrad, J, Corbel, S, Corbet, R, Dermer, Cd, de Palma, F, Digel, Sw, Silva, Ede, Drell, Ps, Dubois, R, Dubus, G, Dumora, D, Farnier, C, Favuzzi, C, Fegan, Sj, Focke, Wb, Fortin, P, Frailis, M, Fusco, P, Gargano, F, Gehrels, N, Germani, S, Giavitto, G, Giebels, B, Giglietto, N, Giordano, F, Glanzman, T, Godfrey, G, Grenier, Ia, Grondin, Mh, Grove, Je, Guillemot, L, Guiriec, S, Hanabata, Y, Harding, Ak, Hayashida, M, Hays, E, Hill, Ab, Hjalmarsdotter, L, Horan, D, Hughes, Re, Jackson, Ms, Johannesson, G, Johnson, As, Johnson, Tj, Johnson, Wn, Kamae, T, Katagiri, H, Kawai, N, Kerr, M, Knodlseder, J, Kocian, Ml, Koerding, E, Kuss, M, Lande, J, Latronico, L, Lemoine Goumard, M, Longo, F, Loparco, F, Lott, B, Lovellette, Mn, Lubrano, P, Madejski, Gm, Makeev, A, Marchand, L, Marelli, M, Max Moerbeck, W, Mazziotta, Mn, Mccoll, N, Mcenery, Je, Meurer, C, Michelson, Pf, Migliari, S, Mitthumsiri, W, Mizuno, T, Monte, C, Monzani, Me, Morselli, A, Moskalenko, Iv, Murgia, S, Nolan, Pl, Norris, Jp, Nuss, E, Ohsugi, T, Omodei, N, Ong, Ra, Ormes, Jf, Paneque, D, Parent, D, Pelassa, V, Pepe, M, Pesce Rollins, M, Piron, F, Pooley, G, Porter, Ta, Pottschmidt, K, Raino, S, Rando, R, Ray, Ps, Razzano, Massimiliano, Rea, N, Readhead, A, Reimer, A, Reimer, O, Richards, Jl, Rochester, Ls, Rodriguez, J, Rodriguez, Ay, Romani, Rw, Ryde, F, Sadrozinski, Hfw, Sander, A, Parkinson, Pms, Sgro, C, Siskind, Ej, Smith, Da, Smith, Pd, Spinelli, P, Starck, Jl, Stevenson, M, Strickman, Ms, Suson, Dj, Takahashi, H, Tanaka, T, Thayer, Jb, Thompson, Dj, Tibaldo, L, Tomsick, Ja, Torres, Df, Tosti, G, Tramacere, A, Uchiyama, Y, Usher, Tl, Vasileiou, V, Vilchez, N, Vitale, V, Waite, Ap, Wang, P, Wilms, J, Winer, Bl, Wood, Ks, Ylinen, T, Ziegler, M., High Energy Astrophys. & Astropart. Phys (API, FNWI), A. A., Abdo, M., Ackermann, M., Ajello, M., Axelsson, L., Baldini, J., Ballet, G., Barbiellini, D., Bastieri, B. M., Baughman, K., Bechtol, R., Bellazzini, B., Berenji, R. D., Blandford, E. D., Bloom, E., Bonamente, A. W., Borgland, A., Brez, M., Brigida, P., Bruel, T. H., Burnett, S., Buson, G. A., Caliandro, R. A., Cameron, P. A., Caraveo, J. M., Casandjian, C., Cecchi, O., Celik, S., Chaty, C. C., Cheung, J., Chiang, S., Ciprini, R., Clau, J., Cohen Tanugi, L. R., Cominsky, J., Conrad, S., Corbel, R., Corbet, C. D., Dermer, F. d., Palma, S. W., Digel, E. D. E., Silva, P. S., Drell, R., Duboi, G., Dubu, D., Dumora, C., Farnier, C., Favuzzi, S. J., Fegan, W. B., Focke, P., Fortin, M., Fraili, P., Fusco, F., Gargano, N., Gehrel, S., Germani, G., Giavitto, B., Giebel, N., Giglietto, F., Giordano, T., Glanzman, G., Godfrey, I. A., Grenier, M. H., Grondin, J. E., Grove, L., Guillemot, S., Guiriec, Y., Hanabata, A. K., Harding, M., Hayashida, E., Hay, A. B., Hill, L., Hjalmarsdotter, D., Horan, R. E., Hughe, M. S., Jackson, G., Johannesson, A. S., Johnson, T. J., Johnson, W. N., Johnson, T., Kamae, H., Katagiri, N., Kawai, M., Kerr, J., Knodlseder, M. L., Kocian, E., Koerding, M., Ku, J., Lande, L., Latronico, M., Lemoine Goumard, Longo, Francesco, F., Loparco, B., Lott, M. N., Lovellette, P., Lubrano, G. M., Madejski, A., Makeev, L., Marchand, M., Marelli, W., Max Moerbeck, M. N., Mazziotta, N., Mccoll, J. E., Mcenery, C., Meurer, P. F., Michelson, S., Migliari, W., Mitthumsiri, T., Mizuno, C., Monte, M. E., Monzani, A., Morselli, I. V., Moskalenko, S., Murgia, P. L., Nolan, J. P., Norri, E., Nu, T., Ohsugi, N., Omodei, R. A., Ong, J. F., Orme, D., Paneque, D., Parent, V., Pelassa, M., Pepe, M., Pesce Rollin, F., Piron, G., Pooley, T. A., Porter, K., Pottschmidt, S., Raino, R., Rando, P. S., Ray, M., Razzano, N., Rea, A., Readhead, A., Reimer, O., Reimer, J. L., Richard, L. S., Rochester, J., Rodriguez, A. Y., Rodriguez, R. W., Romani, F., Ryde, H. F. W., Sadrozinski, A., Sander, P. M. S., Parkinson, C., Sgro, E. J., Siskind, D. A., Smith, P. D., Smith, P., Spinelli, J. L., Starck, M., Stevenson, M. S., Strickman, D. J., Suson, H., Takahashi, T., Tanaka, J. B., Thayer, D. J., Thompson, L., Tibaldo, J. A., Tomsick, D. F., Torre, G., Tosti, A., Tramacere, Y., Uchiyama, T. L., Usher, V., Vasileiou, N., Vilchez, V., Vitale, A. P., Waite, P., Wang, J., Wilm, B. L., Winer, K. S., Wood, T., Ylinen, M., Ziegler, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Fermi-LAT, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), and Université Fédérale Toulouse Midi-Pyrénées

Subjects
Physics, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Multidisciplinary, Black Holes, 010308 nuclear & particles physics, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::High Energy Astrophysical Phenomena, X-ray binary, Gamma ray, Astronomy, Cosmic ray, Quasar, Fermi satellite, Astrophysics, 01 natural sciences, High Energy Gamma-ray Astronomy, Neutron star, Relativistic beaming, Astrophysical jet, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Fermi Gamma-ray Space Telescope
Abstract

Microquasar Spotted Microquasars are binary star systems where a normal star sheds matter onto a neutron star or a black hole, generating x-ray radiation and jets of material moving at relativistic speeds. Microquasars have proved difficult to detect in high-energy gamma rays (> 100 megaelectron volts). Using the Fermi Large Area Telescope, Abdo et al. (p. 1512 , published online 26 November; see the Perspective by Bignami ) now report the detection of variable gamma-ray emission from the microquasar Cygnus X-3. The gamma-ray flux is modulated at the orbital period of Cygnus X-3, and its variation is correlated with the radio emission originating from the microquasar's relativistic jets.

Published
2009
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4. Living on a Flare: Relativistic Reflection in V404 Cyg Observed by NuSTAR during Its Summer 2015 Outburst

Author

Walton, DJ, Mooley, K, King, AL, Tomsick, JA, Miller, JM, Dauser, T, García, JA, Bachetti, M, Brightman, M, Fabian, AC, Forster, K, Fürst, F, Gandhi, P, Grefenstette, BW, Harrison, FA, Madsen, KK, Meier, DL, Middleton, MJ, Natalucci, L, Rahoui, F, Rana, V, and Stern, D

Subjects
X-rays: binaries, 13. Climate action, Astrophysics::High Energy Astrophysical Phenomena, black hole physics, Astrophysics::Solar and Stellar Astrophysics, X-rays: individual (V404 Cyg)
Abstract

We present first results from a series of $\textit{NuSTAR}$ observations of the black hole X-ray binary V404 Cyg obtained during its summer 2015 outburst, primarily focusing on observations during the height of this outburst activity. The $\textit{NuSTAR}$ data show extreme variability in both the flux and spectral properties of the source. This is partly driven by strong and variable line-of-sight absorption, similar to previous outbursts. The latter stages of this observation are dominated by strong flares, reaching luminosities close to Eddington. During these flares, the central source appears to be relatively unobscured and the data show clear evidence for a strong contribution from relativistic reflection, providing a means to probe the geometry of the innermost accretion flow. Based on the flare properties, analogies with other Galactic black hole binaries, and also the simultaneous onset of radio activity, we argue that this intense X-ray flaring is related to transient jet activity during which the ejected plasma is the primary source of illumination for the accretion disk. If this is the case, then our reflection modeling implies that these jets are launched in close proximity to the black hole (as close as a few gravitational radii), consistent with expectations for jet launching models that tap either the spin of the central black hole, or the very innermost accretion disk. Our analysis also allows us to place the first constraints on the black hole spin for this source, which we find to be ${a}^{* }\gt 0.92$ (99% statistical uncertainty, based on an idealized lamp-post geometry)., D.J.W., P.G., and M.J.M. acknowledge support from STFC Ernest Rutherford fellowships (grant ST/J003697/2). K.P.M. acknowledges support from the Hintze Foundation. A.L.K. acknowledges support from NASA through an Einstein Postdoctoral Fellowship (grant number PF4-150125) awarded by the Chandra X-ray Center, operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. A.C.F. acknowledges support from ERC Advanced Grant 340442. L.N. wishes to acknowledge the Italian Space Agency (ASI) for Financial support by ASI/INAF grant I/037/12/0-011/13. This research has made use of data obtained with NuSTAR, a project led by Caltech, funded by NASA and managed by NASA/JPL, and has utilized the NUSTARDAS software package, jointly developed by the ASDC (Italy) and Caltech (USA). This research has also made use of data from AMI, which is supported by the ERC, and we thank the AMI staff for scheduling these radio observations.

5. Reflection and Timing Study of the Transient Black Hole X-Ray Binary MAXI J1803-298 with NuSTAR

Author

Coughenour, Benjamin M., Tomsick, John A., Mastroserio, Guglielmo, Steiner, James M., Connors, Riley M. T., Jiang, Jiachen, Hare, Jeremy, Shaw, Aarran W., Ludlam, Renee M., Fabian, A. C., García, Javier, Coley, Joel B., Coughenour, BM [0000-0003-0870-6465], Tomsick, JA [0000-0001-5506-9855], Mastroserio, G [0000-0003-4216-7936], Steiner, JF [0000-0002-5872-6061], Connors, RMT [0000-0002-8908-759X], Jiang, J [0000-0002-9639-4352], Hare, J [0000-0002-8548-482X], Shaw, AW [0000-0002-8808-520X], Ludlam, RM [0000-0002-8961-939X], Fabian, AC [0000-0002-9378-4072], García, JA [0000-0003-3828-2448], Coley, JB [0000-0001-7532-8359], and Apollo - University of Cambridge Repository

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), 5101 Astronomical Sciences, FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 51 Physical Sciences
Abstract

The transient black hole X-ray binary MAXI J1803-298 was discovered on 2021 May 1, as it went into outburst from a quiescent state. As the source rose in flux it showed periodic absorption dips and fit the timing and spectral characteristics of a hard state accreting black hole. We report on the results of a Target-of-Opportunity observation with NuSTAR obtained near the peak outburst flux beginning on 2021 May 13, after the source had transitioned into an intermediate state. MAXI J1803-298 is variable across the observation, which we investigate by extracting spectral and timing products separately for different levels of flux throughout the observation. Our timing analysis reveals two distinct potential QPOs which are not harmonically related at 5.4+/-0.2 Hz and 9.4+/-0.3 Hz, present only during periods of lower flux. With clear relativistic reflection signatures detected in the source spectrum, we applied several different reflection models to the spectra of MAXI J1803-298. Here we report our results, utilizing high density reflection models to constrain the disk geometry, and assess changes in the spectrum dependent on the source flux. With a standard broken power-law emissivity, we find a near-maximal spin for the black hole, and we are able to constrain the inclination of the accretion disk at 75+/-2 degrees, which is expected for a source that has shown periodic absorption dips. We also significantly detect a narrow absorption feature at 6.91+/-0.06 keV with an equivalent width between 4 and 9 eV, which we interpret as the signature of a disk wind., Comment: 14 pages, 8 figures, accepted for publication (ApJ)

Published
2023

6. Chandra Observations of NuSTAR Serendipitous Sources near the Galactic Plane

Author

AnaSofija Cuturilo, L. Klindt, Daniel Stern, Farid Rahoui, Francesca M. Fornasini, John A. Tomsick, Jaesub Hong, David M. Alexander, George B. Lansbury, James Aird, Maïca Clavel, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Tomsick, JA [0000-0001-5506-9855], Lansbury, GB [0000-0002-5328-9827], Rahoui, F [0000-0001-7655-4120], Aird, J [0000-0003-1908-8463], Alexander, DM [0000-0002-5896-6313], Clavel, M [0000-0003-0724-2742], Fornasini, FM [0000-0002-9286-9963], Stern, D [0000-0003-2686-9241], Apollo - University of Cambridge Repository, Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), and Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)

Subjects
Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Cataclysmic variable star, X-rays: stars, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Magnetar, 01 natural sciences, law.invention, Telescope, stars: neutron, surveys, Observatory, law, 0103 physical sciences, Emission spectrum, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, white dwarfs, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, White dwarf, Astronomy and Astrophysics, Galactic plane, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], stars: black holes
Abstract

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., Comment: 16 pages, accepted by ApJ

Published
2018
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