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The Disk Wind in the Rapidly Spinning Stellar-mass Black Hole 4U 1630–472 Observed with NuSTAR

King, Ashley L. and Walton, Dominic J. and Miller, Jon M. and Barret, Didier and Boggs, Steven E. and Christensen, Finn E. and Craig, William W. and Fabian, Andy C. and Fürst, Felix and Hailey, Charles J. and Harrison, Fiona A. and Krivonos, Roman and Mori, Kaya and Natalucci, Lorenzo and Stern, Daniel and Tomsick, John A. and Zhang, William W. (2014) The Disk Wind in the Rapidly Spinning Stellar-mass Black Hole 4U 1630–472 Observed with NuSTAR. Astrophysical Journal Letters, 784 (1). Art. No. L2. ISSN 2041-8205. http://resolver.caltech.edu/CaltechAUTHORS:20140429-083422136

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Abstract

We present an analysis of a short NuSTAR observation of the stellar-mass black hole and low-mass X-ray binary 4U 1630−472. Reflection from the inner accretion disk is clearly detected for the first time in this source, owing to the sensitivity of NuSTAR. With fits to the reflection spectrum, we find evidence for a rapidly spinning black hole, a∗ = 0.985^(+0.005)_(−0.014) (1σ statistical errors). However, archival data show that the source has relatively low radio luminosity. Recently claimed relationships between jet power and black hole spin would predict either a lower spin or a higher peak radio luminosity. We also report the clear detection of an absorption feature at 7.03 ± 0.03 keV, likely signaling a disk wind. If this line arises in dense, moderately ionized gas (log ξ = 3.6+0.2 −0.3) and is dominated by He-like Fe xxv, the wind has a velocity of v/c = 0.043^(+0.002)_(−0.007) (12900^(+600)_(−2100) km s^(−1)). If the line is instead associated with a more highly ionized gas (log ξ = 6.1+0.7 −0.6), and is dominated by Fe xxvi, evidence of a blueshift is only marginal, after taking systematic errors into account. Our analysis suggests the ionized wind may be launched within 200–1100 Rg, and may be magnetically driven.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/2041-8205/784/1/L2DOIArticle
http://iopscience.iop.org/2041-8205/784/1/L2PublisherArticle
http://arxiv.org/abs/1401.3646arXivDiscussion Paper
ORCID:
AuthorORCID
Boggs, Steven E.0000-0001-9567-4224
Harrison, Fiona A.0000-0003-2992-8024
Krivonos, Roman0000-0003-2737-5673
Mori, Kaya0000-0002-9709-5389
Stern, Daniel0000-0003-2686-9241
Additional Information:© 2014 American Astronomical Society. Received 2013 September 26; accepted 2014 January 15; published 2014 March 4. We would like to thank Julia Lee for her invaluable comments. 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 NASA. L.N. wishes to acknowledge the Italian Space Agency (ASI) for financial support by ASI/INAF grant I/037/12/0-011/13.
Group:NuSTAR, Space Radiation Laboratory
Funders:
Funding AgencyGrant Number
NASANNG08FD60C
Agenzia Spaziale Italiana (ASI)I/037/12/0-011/13
Subject Keywords:accretion, accretion disks – black hole physics – stars: winds, outflows – X-rays: binaries
Other Numbering System:
Other Numbering System NameOther Numbering System ID
Space Radiation Laboratory2014-66
Record Number:CaltechAUTHORS:20140429-083422136
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20140429-083422136
Official Citation:The Disk Wind in the Rapidly Spinning Stellar-mass Black Hole 4U 1630–472 Observed with NuSTAR Ashley L. King et al. 2014 ApJ 784 L2
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:45265
Collection:CaltechAUTHORS
Deposited By: Jason Perez
Deposited On:29 Apr 2014 20:36
Last Modified:10 Oct 2017 21:11

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