Please use this identifier to cite or link to this item:
|Title:||Swift J201424.9+152930: discovery of a new deeply eclipsing binary with 491-s and 3.4-h modulations||Authors:||Esposito, P.
ISRAEL, Gian Luca
DE MARTINO, Domitilla
Di Stefano, R.
RODRIGUEZ CASTILLO, Guillermo Andres
|Issue Date:||2015||Journal:||MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY||Number:||450||Issue:||2||First Page:||1705||Abstract:||We report on the discovery of a new X-ray pulsator, Swift J201424.9+152930 (Sw J2014). Owing to its X-ray modulation at 491 s, it was discovered in a systematic search for coherent signals in the archival data of the Swift X-ray Telescope. To investigate the nature of Sw J2014, we performed multiwavelength follow-up observations with space-borne (Swift and XMM-Newton) and ground-based (the 1.5-m Loiano Telescope and the 3.6-m Telescopio Nazionale Galileo) instruments. The X-ray spectrum of Sw J2014 can be described by a hard and highly absorbed (N<SUB>H</SUB> ∼ 5 × 10<SUP>22</SUP> cm<SUP>-2</SUP>) power law (Γ ∼ 1). The optical observations made it possible to single out the optical counterpart to this source, which displays several variable emission lines and total eclipses lasting ≈20 min. Total eclipses of similar length were observed also in X-rays. The study of the eclipses, allowed us to infer a second periodicity of 3.44 h, which we interpret as the orbital period of a close binary system. We also found that the period has not significantly changed over a ∼7 yr timespan. Based on the timing signatures of Sw J2014, and its optical and X-ray spectral properties, we suggest that it is a close binary hosting an accreting magnetic white dwarf. The system is therefore a cataclysmic variable of the intermediate polar type and one of the very few showing deep eclipses.||Acknowledgments:||This research is based on observations obtained with Swift and XMM–Newton . Swift is a NASA mission with participation of the Italian Space Agency and the UK Space Agency. XMM–Newton is an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. We also made use of observations collected at the Astronomical Observatory of Bologna in Loiano and of TNG operated on the island of La Palma by the Fundación Galileo Galilei of the INAF. The iraf software package is distributed by the NOAO, which is operated by AURA, Inc., under cooperative agreement with the NSF. We thank the anonymous referee for valuable comments on the manuscript and constructive suggestions. PE acknowledges a Fulbright Research Scholar grant administered by the US – Italy Fulbright Commission and is grateful to the Harvard–Smithsonian Center for Astrophysics for hosting him during his Fulbright exchange. (The Fulbright Scholar Program is sponsored by the US Department of State and administered by CIES, a division of IIE.) MM acknowledges financial support from the Italian Ministry of Education, University and Research (MIUR) through grant FIRB 2012 RBFR12PM1F, and from INAF through grant PRIN-2011-1. This work was partially supported by the following contracts and grants: ASI/INAF I/004/11/0 and I/037/12/0, SAO/CXC GO3-14093X, NSF AST-1211843, and NASA NNX12AE39G.||URI:||http://hdl.handle.net/20.500.12386/23462||URL:||http://arxiv.org/abs/1503.08830v2
|Appears in Collections:||1.01 Articoli in rivista|
Show full item record
Files in This Item:
|Esposito_2015.pdf||PDF editoriale||1.88 MB||Adobe PDF||View/Open|
checked on Sep 20, 2020
checked on Sep 20, 2020
Items in DSpace are published in Open Access, unless otherwise indicated.