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dc.contributor.authorNowak, Michael A.
dc.contributor.authorJuett, Adrienne M.
dc.contributor.authorHoman, Jeroen
dc.contributor.authorYao, Yangsen
dc.contributor.authorWilms, Jorn
dc.contributor.authorSchulz, Norbert S.
dc.contributor.authorCanizares, Claude R.
dc.date.accessioned2012-07-31T14:34:59Z
dc.date.available2012-07-31T14:34:59Z
dc.date.issued2008-12
dc.date.submitted2008-02
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357
dc.identifier.urihttp://hdl.handle.net/1721.1/71911
dc.description.abstractWe present simultaneous Chandra High-Energy Transmission Gratings (HETG) and Rossi X-ray Timing Explorer (RXTE) observations of a "soft state" of the black hole candidate 4U 1957+11. These spectra, having limited hard X-ray excess, are an excellent test of disk atmosphere models that include effects of black hole spin. The HETG data show, by modeling the broadband continuum and direct fitting of absorption edges, that the disk spectrum is only very mildly absorbed, with N[subscript H] = (1–2) × 10[superscript 21] cm−[superscript 2]. These data additionally reveal λλ13.449 Ne IX absorption consistent with the warm/hot phase of the interstellar medium. The fitted disk model implies an inclined disk around a low-mass black hole rotating with normalized spin a* ≈ 1. We show, however, that pure Schwarzschild models describe the data extremely well, albeit with large disk atmosphere ``color-correction'' factors. Standard correction factors can be attained if one incorporates mild Comptonization. We find that the Chandra observations do not uniquely determine spin, even with this otherwise extremely well-measured, nearly pure disk spectrum. XMM-Newton RXTE observations, taken only six weeks later, are equally unconstraining. This lack of constraint is partly driven by the unknown mass and distance of 4U 1957+11; however, it is also driven by the limited Chandra and XMM-Newton bandpasses. We therefore present a series of 48 RXTE observations taken at different brightness/hardness levels. These data prefer a spin of a* ≈ 1, even when including a mild Comptonization component; however, they also show evolution of the color-correction factors. If the rapid-spin models with standard correction factors are to be believed, then the RXTE observations predict that 4U 1957+11 can range from a 3 M[sun] black hole at 10 kpc with a* ≈ 0.83 to a 16 M[sun] black hole at 22 kpc with a* ≈ 1.en_US
dc.description.sponsorshipUnited States. National Aeronautics and Space Administration (Grant Number SV3-73016)en_US
dc.description.sponsorshipGerman Aerospace Center (DLR) (Grant Number 50OR0701)en_US
dc.language.isoen_US
dc.publisherIOP Publishingen_US
dc.relation.isversionofhttp://dx.doi.org/10.1086/592227en_US
dc.rightsArticle is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use.en_US
dc.sourcearVixen_US
dc.titleDisk-dominated States of 4U 1957+11: Chandra, XMM-Newton, and RXTE Observations of Ostensibly the Most Rapidly Spinning Galactic Black Holeen_US
dc.typeArticleen_US
dc.identifier.citationNowak, Michael A. et al. “Disk‐dominated States of 4U 1957+11: Chandra,XMM‐Newton,and RXTE Observations of Ostensibly the Most Rapidly Spinning Galactic Black Hole.” The Astrophysical Journal 689.2 (2008): 1199–1214.en_US
dc.contributor.departmentMIT Kavli Institute for Astrophysics and Space Researchen_US
dc.contributor.approverCanizares, Claude C.
dc.contributor.mitauthorNowak, Michael A.
dc.contributor.mitauthorHoman, Jeroen
dc.contributor.mitauthorYao, Yangsen
dc.contributor.mitauthorSchulz, Norbert S.
dc.contributor.mitauthorCanizares, Claude R.
dc.relation.journalAstrophysical Journalen_US
dc.eprint.versionAuthor's final manuscripten_US
dc.type.urihttp://purl.org/eprint/type/JournalArticleen_US
eprint.statushttp://purl.org/eprint/status/PeerRevieweden_US
dspace.orderedauthorsNowak, Michael A.; Juett, Adrienne; Homan, Jeroen; Yao, Yangsen; Wilms, Jörn; Schulz, Norbert S.; Canizares, Claude R.en
dc.identifier.orcidhttps://orcid.org/0000-0002-5769-8441
mit.licensePUBLISHER_POLICYen_US
mit.metadata.statusComplete


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