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Constraining the nature of the accreting binary in CXOGBS J174623.5−310550

Torres, M. A. P. and Repetto, S. and Wevers, T. and Heida, M. and Jonker, P. G. and Hynes, R. I. and Nelemans, G. and Kostrzewa-Rutkowska, Z. and Wyrzykowski, L. and Britt, C. T. and Heinke, C. O. and Casares, J. and Johnson, C. B. and Maccarone, T. J. and Steeghs, D. T. H. (2019) Constraining the nature of the accreting binary in CXOGBS J174623.5−310550. Monthly Notices of the Royal Astronomical Society, 487 (2). pp. 2296-2306. ISSN 0035-8711. https://resolver.caltech.edu/CaltechAUTHORS:20190614-111556752

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Abstract

We report optical and infrared observations of the X-ray source CXOGBS J174623.5−310550. This Galactic object was identified as a potential quiescent low-mass X-ray binary accreting from an M-type donor on the basis of optical spectroscopy and the broad H α emission line. The analysis of X-shooter spectroscopy covering three consecutive nights supports an M2/3-type spectral classification. Neither radial velocity variations nor rotational broadening is detected in the photospheric lines. No periodic variability is found in I- and r′-band light curves. We derive r′ = 20.8, I = 19.2, and K_s ≈ 16.6 for the optical and infrared counterparts with the M-type star contributing ≈90 per cent to the I-band light. We estimate its distance to be 1.3–1.8 kpc. The lack of radial velocity variations implies that the M-type star is not the donor star in the X-ray binary. This could be an interloper or the outer body in a hierarchical triple. We constrain the accreting binary to be a ≲2.2 h orbital period eclipsing cataclysmic variable or a low-mass X-ray binary lying in the foreground of the Galactic bulge.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/stz1405DOIArticle
https://arxiv.org/abs/1905.08107arXivDiscussion Paper
ORCID:
AuthorORCID
Repetto, S.0000-0001-5029-0059
Heida, M.0000-0002-1082-7496
Jonker, P. G.0000-0001-5679-0695
Heinke, C. O.0000-0003-3944-6109
Maccarone, T. J.0000-0003-0976-4755
Additional Information:© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model) Accepted 2019 May 16. Received 2019 April 23; in original form 2018 November 5. Published: 05 June 2019. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 088.D-0096(A) and 095.D-0973(A). This research has used the SIMBAD data base, operated at CDS, Strasbourg, France, and of the NASA’s Astrophysics Data System. IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. Tom Marsh is thanked for developing and sharing his package MOLLY. We thank the anonymous referee for constructive comments. MAPT and JC acknowledge support by the Spanish Ministry of Economy, Industry, and Competitiveness (MINECO) under grant AYA2017-83216-P. MAPT also acknowledges support via a Ramón y Cajal Fellowship (RYC-2015-17854). The work of SR was supported by the Netherlands Research School for Astronomy (NOVA). PGJ and ZKR acknowledge support from European Research Council Consolidator grant 647208. RIH and CBJ acknowledge support from NASA through Chandra Award Number AR3-14002X issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. The work of LW has been supported by the Polish National Science Centre grant no.DEC-2011/03/B/ST9/02573. The OGLE project has received funding from the National Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 and 2015/18/M/ST9/00544 to Andrzej Udalski. COH is supported by NSERC Discovery grant RGPIN-2016-04602, and a Discovery Accelerator Supplement. SR is thankful to Hagai Perets for his insights on the triple scenario.
Group:Space Radiation Laboratory
Funders:
Funding AgencyGrant Number
Ministerio de Economía, Industria y Competitividad (MINECO)AYA2017-83216-P
Ramón y Cajal ProgrammeRYC-2015-17854
Nederlandse Onderzoekschool Voor Astronomie (NOVA)UNSPECIFIED
European Research Council (ERC)647208
NASAAR3-14002X
NASANAS8-03060
National Science Centre (Poland)DEC-2011/03/B/ST9/02573
National Science Centre (Poland)2014/14/A/ST9/00121
National Science Centre (Poland)2015/18/M/ST9/00544
Natural Sciences and Engineering Research Council of Canada (NSERC)RGPIN-2016-04602
Subject Keywords:binaries: close, stars: individual: CXOGBS J174623.5−310550, X-rays: binaries
Issue or Number:2
Record Number:CaltechAUTHORS:20190614-111556752
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20190614-111556752
Official Citation:M A P Torres, S Repetto, T Wevers, M Heida, P G Jonker, R I Hynes, G Nelemans, Z Kostrzewa-Rutkowska, L Wyrzykowski, C T Britt, C O Heinke, J Casares, C B Johnson, T J Maccarone, D T H Steeghs, Constraining the nature of the accreting binary in CXOGBS J174623.5−310550, Monthly Notices of the Royal Astronomical Society, Volume 487, Issue 2, August 2019, Pages 2296–2306, https://doi.org/10.1093/mnras/stz1405
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:96446
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:14 Jun 2019 22:11
Last Modified:09 Mar 2020 13:19

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