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A joint NICER and XMM-Newton view of the "Magnificent" thermally emitting X-ray Isolated Neutron Star RX J1605.3+3249

A joint NICER and XMM-Newton view of the "Magnificent" thermally emitting X-ray Isolated Neutron Star RX J1605.3+3249
A joint NICER and XMM-Newton view of the "Magnificent" thermally emitting X-ray Isolated Neutron Star RX J1605.3+3249
Thermally emitting X-ray isolated neutron stars represent excellent targets for testing cooling surface emission and atmosphere models, which are used to infer physical parameters of the neutron star. Among the seven known members of this class, RX J1605.3+3249 is the only one that still lacks confirmation of its spin period. Here we analyze NICER and XMM-Newton observations of RX J1605.3+3249, in order to address its timing and spectral behavior. Contrary to a previous tentative detection, but in agreement with the recent work by Pires et al. (2019), we find no significant pulsation with pulsed fraction higher than 1.3% (3sigma) for periods above 150 ms. We also find a limit of 2.6% for periods above 2 ms, despite searches in different energy bands. The X-ray spectrum can be fit by either a double-blackbody model or by a single-temperature magnetized atmosphere model, both modified by a Gaussian absorption line at ~0.44 keV. The origin of the absorption feature as a proton cyclotron line or as an atomic transition in the neutron star atmosphere is discussed. The predictions of the best-fit X-ray models extended to IR, optical and UV bands are compared with archival data. Our results are interpreted in the framework of a fallback disk scenario.
1538-4357
1-11
Malacaria, Christian
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Bogdanov, Slavko
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Ho, Wynn C.G.
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Enoto, Teruaki
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Ray, Paul S.
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Arzoumanian, Zaven
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Cazeau, Thoniel
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Gendreau, Keith C.
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Guillot, Sebastien
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Guver, Tolga
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Jaisawal, Gaurava K.
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Wolff, Michael T.
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Malacaria, Christian
309a8f91-28a7-4365-b0a3-633171fc2e51
Bogdanov, Slavko
39f20582-4d71-4b1a-ae2a-b266367341ef
Ho, Wynn C.G.
d78d4c52-8f92-4846-876f-e04a8f803a45
Enoto, Teruaki
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Ray, Paul S.
773c1940-2b53-4871-8176-c363521bb83f
Arzoumanian, Zaven
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Cazeau, Thoniel
c8dabdca-97d9-4583-84b1-40d504710cad
Gendreau, Keith C.
cad26609-b22d-4c1d-ada3-4af51e2cd780
Guillot, Sebastien
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Guver, Tolga
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Jaisawal, Gaurava K.
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Wolff, Michael T.
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Malacaria, Christian, Bogdanov, Slavko, Ho, Wynn C.G., Enoto, Teruaki, Ray, Paul S., Arzoumanian, Zaven, Cazeau, Thoniel, Gendreau, Keith C., Guillot, Sebastien, Guver, Tolga, Jaisawal, Gaurava K. and Wolff, Michael T. (2019) A joint NICER and XMM-Newton view of the "Magnificent" thermally emitting X-ray Isolated Neutron Star RX J1605.3+3249. The Astrophysical Journal, 880 (2), 1-11, [74]. (doi:10.3847/1538-4357/ab2875).

Record type: Article

Abstract

Thermally emitting X-ray isolated neutron stars represent excellent targets for testing cooling surface emission and atmosphere models, which are used to infer physical parameters of the neutron star. Among the seven known members of this class, RX J1605.3+3249 is the only one that still lacks confirmation of its spin period. Here we analyze NICER and XMM-Newton observations of RX J1605.3+3249, in order to address its timing and spectral behavior. Contrary to a previous tentative detection, but in agreement with the recent work by Pires et al. (2019), we find no significant pulsation with pulsed fraction higher than 1.3% (3sigma) for periods above 150 ms. We also find a limit of 2.6% for periods above 2 ms, despite searches in different energy bands. The X-ray spectrum can be fit by either a double-blackbody model or by a single-temperature magnetized atmosphere model, both modified by a Gaussian absorption line at ~0.44 keV. The origin of the absorption feature as a proton cyclotron line or as an atomic transition in the neutron star atmosphere is discussed. The predictions of the best-fit X-ray models extended to IR, optical and UV bands are compared with archival data. Our results are interpreted in the framework of a fallback disk scenario.

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1906.02806 - Accepted Manuscript
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Accepted/In Press date: 6 June 2019
e-pub ahead of print date: 26 July 2019
Published date: 1 August 2019

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Local EPrints ID: 431693
URI: http://eprints.soton.ac.uk/id/eprint/431693
ISSN: 1538-4357
PURE UUID: 66539847-94db-4abb-998b-c3a1c6b53f1b
ORCID for Wynn C.G. Ho: ORCID iD orcid.org/0000-0002-6089-6836

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Date deposited: 13 Jun 2019 16:30
Last modified: 28 Nov 2019 01:34

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