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Reflection Spectroscopy of the Black Hole Binary XTE J1752−223 in Its Long-stable Hard State

García, Javier A. and Steiner, James F. and Grinberg, Victoria and Dauser, Thomas and Connors, Riley M. T. and McClintock, Jeffrey E. and Remillard, Ronald A. and Wilms, Jörn and Harrison, Fiona A. and Tomsick, John A. (2018) Reflection Spectroscopy of the Black Hole Binary XTE J1752−223 in Its Long-stable Hard State. Astrophysical Journal, 864 (1). Art. No. 25. ISSN 1538-4357. http://resolver.caltech.edu/CaltechAUTHORS:20180827-144724340

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Abstract

We present a detailed spectral analysis of the black hole binary XTE J1752−223 in the hard state of its 2009 outburst. Regular monitoring of this source by the Rossi X-ray Timing Explorer mission provided high signal-to-noise spectra along the outburst rise and decay. During one full month this source stalled at ~30% of its peak count rate at a constant hardness and intensity. By combining all the data in this exceptionally stable hard state, we obtained an aggregate proportional counter array spectrum (3–45 keV) with 100 million counts, and a corresponding high energy X-ray timing experiment spectrum (20–140 keV) with 5.8 million counts. Implementing a version of our reflection code with a physical model for Comptonization, we obtain tight constraints on important physical parameters for this system. In particular, the inner accretion disk is measured very close in, at R_(in) = 1.7 ± 0.4 R_g . Assuming R_(in_ = R_(ISCO), we find a relatively high black hole spin (a_* = 0.92 ± 0.06). Imposing a lamppost geometry, we obtain a low inclination (i = 35° ± 4°), which agrees with the upper limit found in the radio (i < 49°). However, we note that this model cannot be statistically distinguished from a non-lamppost model with a free emissivity index, for which the inclination is markedly higher. Additionally, we find a relatively cool corona (57–70 keV) and large iron abundance (3.3–3.7 solar). We further find that properly accounting for Comptonization of the reflection emission improves the fit significantly and causes an otherwise low reflection fraction (~0.2–0.3) to increase by an order of magnitude, in line with geometrical expectations for a lamppost corona. We compare these results with similar investigations reported for GX 339−4 in its bright hard state.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/aad231DOIArticle
https://arxiv.org/abs/1807.01949arXivDiscussion Paper
ORCID:
AuthorORCID
García, Javier A.0000-0003-3828-2448
Steiner, James F.0000-0002-5872-6061
Grinberg, Victoria0000-0003-2538-0188
Connors, Riley M. T.0000-0002-8908-759X
Remillard, Ronald A.0000-0003-4815-0481
Wilms, Jörn0000-0003-2065-5410
Harrison, Fiona A.0000-0003-2992-8024
Tomsick, John A.0000-0001-5506-9855
Additional Information:© 2018. The American Astronomical Society. Received 2018 May 11; revised 2018 July 2; accepted 2018 July 5; published 2018 August 27. The authors dedicate the present work to the memory of our friend, colleague, and mentor Jeffrey E. McClintock, who passed on 2017 November 8. This paper grew from a program to explore black hole systems using RXTE under Jeff's leadership. We thank Jeff for his mentorship, his always open door, and for his friendship. Jeff's love for science inspired us, his relentless curiosity was a joy to share, and we miss him greatly. This work was partially supported under NASA Contract No. NNG08FD60C. J.A.G. and R.M.T.C. acknowledge support from NASA Grant No. 80NSSC177K0515. J.A.G also acknowledges support from the Alexander von Humboldt Foundation. J.F.S has been supported by the NASA Einstein Fellowship, Grant No. PF5-160144. V.G. is supported through the Margarethe von Wrangell fellowship by the ESF and the Ministry of Science, Research and the Arts Baden-Württemberg.
Group:Space Radiation Laboratory
Funders:
Funding AgencyGrant Number
NASANNG08FD60C
NASA80NSSC177K0515
Alexander von Humboldt FoundationUNSPECIFIED
NASA Einstein FellowshipPF5-160144
European Science FoundationUNSPECIFIED
Ministry of Science, Research and the Arts (Baden-Württemberg)UNSPECIFIED
Subject Keywords:accretion, accretion disks; atomic processes; black hole physics; line: formation; X-rays: individual (XTE J1752−223)
Record Number:CaltechAUTHORS:20180827-144724340
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20180827-144724340
Official Citation:Javier A. García et al 2018 ApJ 864 25
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:89180
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:27 Aug 2018 22:49
Last Modified:27 Aug 2018 22:49

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