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Detection of Very Low-frequency, Quasi-periodic Oscillations in the 2015 Outburst of V404 Cygni

Huppenkothen, D. and Younes, G. and Ingram, A. and Kouveliotou, C. and Göğüş, E. and Bachetti, M. and Sánchez-Fernández, C. and Chenevez, J. and Motta, S. and van der Klis, M. and Granot, J. and Gehrels, N. and Kuulkers, E. and Tomsick, J. A. and Walton, D. J. (2017) Detection of Very Low-frequency, Quasi-periodic Oscillations in the 2015 Outburst of V404 Cygni. Astrophysical Journal, 934 (1). Art. No. 90. ISSN 0004-637X. http://resolver.caltech.edu/CaltechAUTHORS:20161028-100132024

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Abstract

In 2015 June, the black hole X-ray binary (BHXRB) V404 Cygni went into outburst for the first time since 1989. Here, we present a comprehensive search for quasi-periodic oscillations (QPOs) of V404 Cygni during its recent outburst, utilizing data from six instruments on board five different X-ray missions: Swift/XRT, Fermi/GBM, Chandra/ACIS, INTEGRAL's IBIS/ISGRI and JEM-X, and NuSTAR. We report the detection of a QPO at 18 mHz simultaneously with both Fermi/GBM and Swift/XRT, another example of a rare but slowly growing new class of mHz-QPOs in BHXRBs linked to sources with a high orbital inclination. Additionally, we find a duo of QPOs in a Chandra/ACIS observation at 73 mHz and 1.03 Hz, as well as a QPO at 136 mHz in a single Swift/XRT observation that can be interpreted as standard Type-C QPOs. Aside from the detected QPOs, there is significant structure in the broadband power, with a strong feature observable in the Chandra observations between 0.1 and 1 Hz. We discuss our results in the context of current models for QPO formation.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.3847/1538-4357/834/1/90DOIArticle
http://iopscience.iop.org/article/10.3847/1538-4357/834/1/90/metaPublisherArticle
http://arxiv.org/abs/1610.08653arXivDiscussion Paper
ORCID:
AuthorORCID
Bachetti, M.0000-0002-4576-9337
Walton, D. J.0000-0001-5819-3552
Additional Information:© 2017. The American Astronomical Society. Received 2016 May 12; revised 2016 October 24; accepted 2016 October 26; published 2017 January 4. We thank the anonymous referee for very helpful comments and suggestions. We thank Victoria Grinberg for very informative and useful discussions on INTEGRAL calibration and timing with IBIS/ISGRI. D.H. acknowledges support by the Moore-Sloan Data Science Environment at NYU. Partly based on observations with INTEGRAL, an ESA project with instruments and science data centre funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Switzerland, Spain) and with the participation of Russia and the USA. AI acknowledges support from the Netherlands Organization for Scientific Research (NWO) Veni Fellowship, grant number 639.041.437. M.B. was supported in part by the Sardinian Region, in the framework of the Regional Fundamental Research funds (L.R. 7/2007). J.C. thanks financial support from ESA/PRODEX Nr. 90057.
Group:NuSTAR
Funders:
Funding AgencyGrant Number
New York University (NYU)UNSPECIFIED
Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)639.041.437
Sardinian RegionL.R. 7/2007
ESA/PRODEX90057
Subject Keywords:methods: statistical; relativistic processes; stars: black holes; X-rays: binaries
Record Number:CaltechAUTHORS:20161028-100132024
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20161028-100132024
Official Citation:D. Huppenkothen et al 2017 ApJ 834 90
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:71568
Collection:CaltechAUTHORS
Deposited By: Joy Painter
Deposited On:28 Oct 2016 19:34
Last Modified:29 Nov 2017 05:15

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