Investigating the ultra-compact x-ray binary candidate SLX 1735-269 with NICER and NuSTAR
Investigating the ultra-compact x-ray binary candidate SLX 1735-269 with NICER and NuSTAR
e present two simultaneous NICER and NuSTAR observations of the ultracompact X-ray binary (UCXB) candidate SLX 1735−269 while the source was in two different spectral states. Using various reflection modeling techniques, we find that xillverCO, a model used for fitting X-ray spectra of UCXBs with high carbon and oxygen abundances is an improvement over relxill or relxillNS, which instead contains solar-like chemical abundances. This provides indirect evidence in support of the source being ultracompact. We also use this reflection model to get a preliminary measurement of the inclination of the system, i=57+23−7 degrees. This is consistent with our timing analysis, where a lack of eclipses indicates an inclination of i < 80°. The timing analysis is otherwise inconclusive, and we cannot confidently measure the orbital period of the system.
astro-ph.HE
Moutard, D.L.
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Ludlam, R.M.
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Sudha, Malu
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Cackett, E.M.
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Degenaar, N.
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Fabian, A.C.
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Gandhi, P.
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Garcia, J.A.
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Shaw, A.W.
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Tomsick, J.A.
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11 June 2024
Moutard, D.L.
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Ludlam, R.M.
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Sudha, Malu
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Cackett, E.M.
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Degenaar, N.
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Fabian, A.C.
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Gandhi, P.
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Garcia, J.A.
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Shaw, A.W.
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Tomsick, J.A.
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Moutard, D.L., Ludlam, R.M., Sudha, Malu, Cackett, E.M., Degenaar, N., Fabian, A.C., Gandhi, P., Garcia, J.A., Shaw, A.W. and Tomsick, J.A.
(2024)
Investigating the ultra-compact x-ray binary candidate SLX 1735-269 with NICER and NuSTAR.
The Astrophysical Journal, 968, [51].
(doi:10.48550/arXiv.2401.12371).
Abstract
e present two simultaneous NICER and NuSTAR observations of the ultracompact X-ray binary (UCXB) candidate SLX 1735−269 while the source was in two different spectral states. Using various reflection modeling techniques, we find that xillverCO, a model used for fitting X-ray spectra of UCXBs with high carbon and oxygen abundances is an improvement over relxill or relxillNS, which instead contains solar-like chemical abundances. This provides indirect evidence in support of the source being ultracompact. We also use this reflection model to get a preliminary measurement of the inclination of the system, i=57+23−7 degrees. This is consistent with our timing analysis, where a lack of eclipses indicates an inclination of i < 80°. The timing analysis is otherwise inconclusive, and we cannot confidently measure the orbital period of the system.
Text
2401.12371v1
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Available under License Other.
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2401.12371v2
- Accepted Manuscript
Available under License Other.
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Moutard_2024_ApJ_968_51
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More information
Submitted date: 22 January 2024
Accepted/In Press date: 10 May 2024
e-pub ahead of print date: 11 June 2024
Published date: 11 June 2024
Additional Information:
Douglas JK Buisson was a co-author on the original submitted paper, available on ArXiv.
Keywords:
astro-ph.HE
Identifiers
Local EPrints ID: 487409
URI: http://eprints.soton.ac.uk/id/eprint/487409
ISSN: 0004-637X
PURE UUID: 9bb8b26e-2c44-4e3b-8473-e3a402471b41
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Date deposited: 20 Feb 2024 12:45
Last modified: 22 Aug 2025 02:12
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Contributors
Author:
D.L. Moutard
Author:
R.M. Ludlam
Author:
Malu Sudha
Author:
E.M. Cackett
Author:
N. Degenaar
Author:
A.C. Fabian
Author:
J.A. Garcia
Author:
A.W. Shaw
Author:
J.A. Tomsick
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