Quiescent NIR and optical counterparts to candidate black hole X-ray binaries

Creators: López, K. M.; Jonker, P. G.; Torres, M. A. P.; Heida, M.; Rau, A.; Steeghs, D.

Abstract

We present near-infrared and optical imaging of 15 candidate black hole X-ray binaries. In addition to quiescent observations for all sources, we also observed two of these sources (IGR J17451−3022 and XTE J1818−245) in outburst. We detect the quiescent counterpart for 12 out of 15 sources, and for the remaining 3, we report limiting magnitudes. The magnitudes of the detected counterparts range between K_s = 17.59 and K_s = 22.29 mag. We provide (limits on) the absolute magnitudes and finding charts of all sources. Of these 12 detections in quiescence, 7 detections represent the first quiescent reported values (for MAXI J1543−564, XTE J1726−476, IGR J17451−3022, XTE J1818−245, MAXI J1828−249, MAXI J1836−194, Swift J1910.2−0546), and 2 detections show fainter counterparts to XTE J1752−223 and XTE J2012+381 than previously reported. We used theoretical arguments and observed trends, for instance between the outburst and quiescent X-ray luminosity and orbital period P_(orb) to derive an expected trend between ΔK_s and P_(orb) of ΔK_s ∝ log P^(0.565)_(orb)⁠. Comparing this to observations, we find a different behaviour. We discuss possible explanations for this result.

Additional Information

© 2018 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 2018 October 12. Received 2018 October 12; in original form 2018 August 7. Published: 16 October 2018. This study is based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programmes 099.A-9025(A) and 1101.D-0105(A). PGJ and KML acknowledge funding from the European Research Council under ERC Consolidator Grant agreement no 647208. Part of the funding for GROND (both hardware as well as personnel) was generously granted from the Deutsche Forschungsgemeinschaft Gottfried Wilhelm Leibniz Prize to Prof. G. Hasinger (DFG grant HA 1850/28-1). MAPT acknowledges support via a Ramón y Cajal Fellowship (RYC-2015-17854). MAPT also acknowledges support by the Spanish Ministry of Economy, Industry and Competitiveness under grant AYA2017-83216-P. This research is based on observations made with the William Herschel Telescope operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias; with the Keck Telescope at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. We have made use of the SIMBAD data base, operated at CDS, Strasbourg, France, of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.

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