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17 results on '"Tomsick, JA"'

1. Nustar and integral observations of a low/hard state of 1E1740.7-2942

Author

Natalucci, L, Tomsick, JA, Bazzano, A, Smith, DM, Bachetti, M, Barret, D, Boggs, SE, Christensen, FE, Craig, WW, Fiocchi, M, Fürst, F, Grefenstette, BW, Hailey, CJ, Harrison, FA, Krivonos, R, Kuulkers, E, Miller, JM, Pottschmidt, K, Stern, D, Ubertini, P, Walton, DJ, and Zhang, WW

Subjects
accretion, accretion disks, black hole physics, X-rays: binaries, X-rays: individual, astro-ph.HE, accretion, accretion disks, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract

The microquasar 1E1740.7-2942, also known as the "Great Annihilator," was observed by NuSTAR in the summer of 2012. We have analyzed in detail two observations taken ∼2 weeks apart, for which we measure hard and smooth spectra typical of the low/hard state. A few weeks later the source flux declined significantly. Nearly simultaneous coverage by INTEGRAL is available from its Galactic Center monitoring campaign lasting ∼2.5 months. These data probe the hard state spectrum from 1E1740.7-2942 before the flux decline. We find good agreement between the spectra taken with IBIS/ISGRI and NuSTAR, with the measurements being compatible with a change in flux with no spectral variability. We present a detailed analysis of the NuSTAR spectral and timing data and upper limits for reflection of the high energy emission. We show that the high energy spectrum of this X-ray binary is well described by thermal Comptonization. © 2014. The American Astronomical Society. All rights reserved.

Published
2014

3. Discovery of thermonuclear (Type I) X-ray bursts in the X-ray binary Swift J1858.6–0814 observed with NICER and NuSTAR

Author

MIT Kavli Institute for Astrophysics and Space Research, Buisson, DJK, Altamirano, D, Bult, P, Mancuso, GC, Güver, T, Jaisawal, GK, Hare, J, Albayati, AC, Arzoumanian, Z, Castro Segura, N, Chakrabarty, D, Gandhi, P, Guillot, S, Homan, J, Gendreau, KC, Jiang, J, Malacaria, C, Miller, JM, Özbey Arabacı, M, Remillard, R, Strohmayer, TE, Tombesi, F, Tomsick, JA, Vincentelli, FM, Walton, DJ, MIT Kavli Institute for Astrophysics and Space Research, Buisson, DJK, Altamirano, D, Bult, P, Mancuso, GC, Güver, T, Jaisawal, GK, Hare, J, Albayati, AC, Arzoumanian, Z, Castro Segura, N, Chakrabarty, D, Gandhi, P, Guillot, S, Homan, J, Gendreau, KC, Jiang, J, Malacaria, C, Miller, JM, Özbey Arabacı, M, Remillard, R, Strohmayer, TE, Tombesi, F, Tomsick, JA, Vincentelli, FM, and Walton, DJ

Abstract

© 2020 Oxford University Press. All rights reserved. Swift J1858.6-0814 is a recently discovered X-ray binary notable for extremely strong variability (by factors of >100 in soft X-rays) in its discovery state. We present the detection of five thermonuclear (Type I) X-ray bursts from Swift J1858.6-0814, implying that the compact object in the system is a neutron star (NS). Some of the bursts show photospheric radius expansion, so their peak flux can be used to estimate the distance to the system. The peak luminosity, and hence distance, can depend on several system parameters; for the most likely values, a high inclination and a helium atmosphere, D = 12.8+0.8-0.6kpc, although systematic effects allow a conservative range of 9-18 kpc. Before one burst, we detect a QPO at 9.6 ± 0.5 mHz with a fractional rms amplitude of 2.2 ± 0.2 per cent (0.5-10 keV), likely due to marginally stable burning of helium; similar oscillations may be present before the other bursts but the light curves are not long enough to allow their detection. We also search for burst oscillations but do not detect any, with an upper limit in the best case of 15 per cent fractional amplitude (over 1-8 keV). Finally, we discuss the implications of the NS accretor and this distance on other inferences which have been made about the system. In particular, we find that Swift J1858.6-0814 was observed at super-Eddington luminosities at least during bright flares during the variable stage of its outburst.

Published
2022

4. The Soft State of the Black Hole Transient Source MAXI J1820+070: Emission from the Edge of the Plunge Region?

Author

Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Fabian, AC, Buisson, DJ, Kosec, P, Reynolds, CS, Wilkins, DR, Tomsick, JA, Walton, DJ, Gandhi, P, Altamirano, D, Arzoumanian, Z, Cackett, EM, Dyda, S, Garcia, JA, Gendreau, KC, Grefenstette, BW, Homan, J, Kara, Erin A, Ludlam, RM, Miller, JM, Steiner, JF, Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Fabian, AC, Buisson, DJ, Kosec, P, Reynolds, CS, Wilkins, DR, Tomsick, JA, Walton, DJ, Gandhi, P, Altamirano, D, Arzoumanian, Z, Cackett, EM, Dyda, S, Garcia, JA, Gendreau, KC, Grefenstette, BW, Homan, J, Kara, Erin A, Ludlam, RM, Miller, JM, and Steiner, JF

Abstract

The Galactic black hole X-ray binary MAXI J1820+070 had a bright outburst in 2018 when it became the second brightest X-ray source in the sky. It was too bright for X-ray CCD instruments such as XMM–Newton and Chandra, but was well observed by photon-counting instruments such as Neutron star Inner Composition Explorer (NICER) and Nuclear Spectroscopic Telescope Array(NuSTAR). We report here on the discovery of an excess-emission component during the soft state. It is best modelled with a blackbody spectrum in addition to the regular disc emission, modelled as either diskbb or kerrbb. Its temperature varies from about 0.9 to 1.1 keV, which is about 30–80 per cent higher than the inner disc temperature of diskbb. Its flux varies between 4 and 12 per cent of the disc flux. Simulations of magnetized accretion discs have predicted the possibility of excess emission associated with a non-zero torque at the innermost stable circular orbit (ISCO) about the black hole, which, from other NuSTAR studies, lies at about 5 gravitational radii or about 60 km (for a black hole, mass is $8\, {\rm M}_{\odot }$). In this case, the emitting region at the ISCO has a width varying between 1.3 and 4.6 km and would encompass the start of the plunge region where matter begins to fall freely into the black hole.

Published
2022

5. Simultaneous NICER and NuSTAR Observations of the Ultracompact X-Ray Binary 4U 1543–624

Author

Ludlam, RM, Jaodand, AD, García, JA, Degenaar, N, Tomsick, JA, Cackett, EM, Fabian, AC, Gandhi, P, Buisson, DJK, Shaw, AW, Chakrabarty, D, Ludlam, RM, Jaodand, AD, García, JA, Degenaar, N, Tomsick, JA, Cackett, EM, Fabian, AC, Gandhi, P, Buisson, DJK, Shaw, AW, and Chakrabarty, D

Abstract

Abstract We present the first joint NuSTAR and NICER observations of the ultracompact X-ray binary (UCXB) 4U 1543−624 obtained in 2020 April. The source was at a luminosity of L 0.5−50 keV = 4.9(D/7 kpc)2 × 1036 erg s−1 and showed evidence of reflected emission in the form of an O viii line, Fe K line, and Compton hump within the spectrum. We used a full reflection model, known as xillverCO, that is tailored for the atypical abundances found in UCXBs, to account for the reflected emission. We tested the emission radii of the O and Fe line components and conclude that they originate from a common disk radius in the innermost region of the accretion disk (R in ≤ 1.07 R ISCO). Assuming that the compact accretor is a neutron star (NS) and the position of the inner disk is the Alfvén radius, we placed an upper limit on the magnetic field strength to be B ≤ 0.7(D/7 kpc) × 108 G at the poles. Given the lack of pulsations detected and position of R in, it was likely that a boundary layer region had formed between the NS surface and inner edge of the accretion disk with an extent of 1.2 km. This implies a maximum radius of the neutron star accretor of R NS ≤ 12.1 km when assuming a canonical NS mass of 1.4 M ⊙.

Published
2022

6. The Soft State of the Black Hole Transient Source MAXI J1820+070: Emission from the Edge of the Plunge Region?

Author

Fabian, AC, Buisson, DJ, Kosec, P, Reynolds, CS, Wilkins, DR, Tomsick, JA, Walton, DJ, Gandhi, P, Altamirano, D, Arzoumanian, Z, Cackett, EM, Dyda, S, Garcia, JA, Gendreau, KC, Grefenstette, BW, Homan, J, Kara, E, Ludlam, RM, Miller, JM, Steiner, JF, Fabian, AC, Buisson, DJ, Kosec, P, Reynolds, CS, Wilkins, DR, Tomsick, JA, Walton, DJ, Gandhi, P, Altamirano, D, Arzoumanian, Z, Cackett, EM, Dyda, S, Garcia, JA, Gendreau, KC, Grefenstette, BW, Homan, J, Kara, E, Ludlam, RM, Miller, JM, and Steiner, JF

Abstract

ABSTRACT The Galactic black hole X-ray binary MAXI J1820+070 had a bright outburst in 2018 when it became the second brightest X-ray source in the sky. It was too bright for X-ray CCD instruments such as XMM–Newton and Chandra, but was well observed by photon-counting instruments such as Neutron star Inner Composition Explorer (NICER) and Nuclear Spectroscopic Telescope Array(NuSTAR). We report here on the discovery of an excess-emission component during the soft state. It is best modelled with a blackbody spectrum in addition to the regular disc emission, modelled as either diskbb or kerrbb. Its temperature varies from about 0.9 to 1.1 keV, which is about 30–80 per cent higher than the inner disc temperature of diskbb. Its flux varies between 4 and 12 per cent of the disc flux. Simulations of magnetized accretion discs have predicted the possibility of excess emission associated with a non-zero torque at the innermost stable circular orbit (ISCO) about the black hole, which, from other NuSTAR studies, lies at about 5 gravitational radii or about 60 km (for a black hole, mass is $8\, {\rm M}_{\odot }$). In this case, the emitting region at the ISCO has a width varying between 1.3 and 4.6 km and would encompass the start of the plunge region where matter begins to fall freely into the black hole.

Published
2021

7. 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

8. 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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9. 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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10. 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.

11. 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

12. 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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13. Characterizing hole trap production due to proton irradiation in germanium cross-strip detectors.

Author

Pike SN, Boggs SE, Brewster G, Haight SE, Roberts JM, Shih AY, Szornel J, Tomsick JA, and Zoglauer A

Abstract

We present an investigation into the effects of high-energy proton damage on charge trapping in germanium cross-strip detectors with the goal of accomplishing three important measurements. First, we calibrated and characterized the spectral resolution of a spare COSI-balloon detector in order to determine the effects of intrinsic trapping, finding that electron trapping due to impurities dominates over hole trapping in the undamaged detector. Second, we performed two rounds of proton irradiation of the detector in order to quantify, for the first time, the rate at which charge traps are produced by proton irradiation. We find that the product of the hole trap density and cross-sectional area, [ n σ ] h , follows a linear relationship with the proton fluence, F p , with a slope of ( 5.4 ± 0.4 ) × 10 - 11 cm / p + . Third, by utilizing our measurements of physical trapping parameters, we performed calibrations which corrected for the effects of trapping and mitigated degradation to the spectral resolution of the detector., Competing Interests: Competing interestsThe authors declare no competing interests., (© The Author(s) 2025.)

Published
2025
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14. Design and modeling of a Laue lens for radiation therapy with hard x-ray photons.

Author

Girou D, Ford E, Wade C, van Aarle C, Uliyanov A, Hanlon L, Tomsick JA, Zoglauer A, Collon MJ, Beijersbergen MW, and Barrière NM

Subjects
Monte Carlo Method, Phantoms, Imaging, Radiometry, X-Rays, Photons therapeutic use, Silicon
Abstract

We have designed and modeled a novel optical system composed of a Laue lens coupled to an x-ray tube that produces a focused beam in an energy range near 100 keV ( λ = 12.4 picometer). One application of this system is radiation therapy where it could enable treatment units that are considerably simpler and lower in cost than present technologies relying on linear accelerators. The Laue lens is made of Silicon Laue components which exploit the silicon pore optics technology. The lens concentrates photons to a small region thus allowing high dose rates at the focal area with very much lower dose rates at the skin and superficial regions. Monte Carlo simulations with Geant4 indicate a dose deposition rate of 0.2 Gy min -1 in a cylindrical volume of 0.7 mm diameter and 10 mm length, and a dose ratio of 72 at the surface (skin) compared to the focus placed 10 cm within a water phantom. Work is ongoing to newer generation crystal technologies to increase dose rate., (Creative Commons Attribution license.)

Published
2021
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15. Extended hard-X-ray emission in the inner few parsecs of the Galaxy.

Author

Perez K, Hailey CJ, Bauer FE, Krivonos RA, Mori K, Baganoff FK, Barrière NM, Boggs SE, Christensen FE, Craig WW, Grefenstette BW, Grindlay JE, Harrison FA, Hong J, Madsen KK, Nynka M, Stern D, Tomsick JA, Wik DR, Zhang S, Zhang WW, and Zoglauer A

Abstract

The Galactic Centre hosts a puzzling stellar population in its inner few parsecs, with a high abundance of surprisingly young, relatively massive stars bound within the deep potential well of the central supermassive black hole, Sagittarius A* (ref. 1). Previous studies suggest that the population of objects emitting soft X-rays (less than 10 kiloelectronvolts) within the surrounding hundreds of parsecs, as well as the population responsible for unresolved X-ray emission extending along the Galactic plane, is dominated by accreting white dwarf systems. Observations of diffuse hard-X-ray (more than 10 kiloelectronvolts) emission in the inner 10 parsecs, however, have been hampered by the limited spatial resolution of previous instruments. Here we report the presence of a distinct hard-X-ray component within the central 4 × 8 parsecs, as revealed by subarcminute-resolution images in the 20-40 kiloelectronvolt range. This emission is more sharply peaked towards the Galactic Centre than is the surface brightness of the soft-X-ray population. This could indicate a significantly more massive population of accreting white dwarfs, large populations of low-mass X-ray binaries or millisecond pulsars, or particle outflows interacting with the surrounding radiation field, dense molecular material or magnetic fields. However, all these interpretations pose significant challenges to our understanding of stellar evolution, binary formation, and cosmic-ray production in the Galactic Centre.

Published
2015
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16. Modulated high-energy gamma-ray emission from the microquasar Cygnus X-3.

Author

Abdo AA, Ackermann M, Ajello M, Axelsson M, Baldini L, 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, do Couto e Silva E, 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, Jóhannesson G, Johnson AS, Johnson TJ, Johnson WN, Kamae T, Katagiri H, Kawai N, Kerr M, Knödlseder 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, Rainò S, Rando R, Ray PS, Razzano M, Rea N, Readhead A, Reimer A, Reimer O, Richards JL, Rochester LS, Rodriguez J, Rodriguez AY, Romani RW, Ryde F, Sadrozinski HF, Sander A, Saz Parkinson PM, Sgrò 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, and Ziegler M

Abstract

Microquasars are accreting black holes or neutron stars in binary systems with associated relativistic jets. Despite their frequent outburst activity, they have never been unambiguously detected emitting high-energy gamma rays. The Fermi Large Area Telescope (LAT) has detected a variable high-energy source coinciding with the position of the x-ray binary and microquasar Cygnus X-3. Its identification with Cygnus X-3 is secured by the detection of its orbital period in gamma rays, as well as the correlation of the LAT flux with radio emission from the relativistic jets of Cygnus X-3. The gamma-ray emission probably originates from within the binary system, opening new areas in which to study the formation of relativistic jets.

Published
2009
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17. Large-scale, decelerating, relativistic x-ray jets from the microquasar XTE J1550-564.

Author

Corbel S, Fender RP, Tzioumis AK, Tomsick JA, Orosz JA, Miller JM, Wijnands R, and Kaaret P

Abstract

We have detected, at x-ray and radio wavelengths, large-scale moving jets from the microquasar XTE J1550-564. Plasma ejected from near the black hole traveled at relativistic velocities for at least 4 years. We present direct evidence for gradual deceleration in a relativistic jet. The broadband spectrum of the jets is consistent with synchrotron emission from high-energy (up to 10 tera-electron volts) particles that were accelerated in the shock waves formed within the relativistic ejecta or by the interaction of the jets with the interstellar medium. XTE J1550-564 offers a rare opportunity to study the dynamical evolution of relativistic jets on time scales inaccessible for active galactic nuclei jets, with implications for our understanding of relativistic jets from Galactic x-ray binaries and active galactic nuclei.

Published
2002
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