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Optical spectroscopy and photometry of SAX J1808.4−3658 in outburst

dc.contributor.authorElebert, P.en_US
dc.contributor.authorReynolds, Mark T.en_US
dc.contributor.authorCallanan, P. J.en_US
dc.contributor.authorHurley, D. J.en_US
dc.contributor.authorRamsay, G.en_US
dc.contributor.authorLewis, F.en_US
dc.contributor.authorRussell, D. M.en_US
dc.contributor.authorNord, Brian D.en_US
dc.contributor.authorKane, S. R.en_US
dc.contributor.authorDePoy, D. L.en_US
dc.contributor.authorHakala, P.en_US
dc.date.accessioned2010-06-01T21:51:21Z
dc.date.available2010-06-01T21:51:21Z
dc.date.issued2009-05-11en_US
dc.identifier.citationElebert, P.; Reynolds, M. T.; Callanan, P. J.; Hurley, D. J.; Ramsay, G.; Lewis, F.; Russell, D. M.; Nord, B.; Kane, S. R.; DePoy, D. L.; Hakala, P. (2009). "Optical spectroscopy and photometry of SAX J1808.4−3658 in outburst." Monthly Notices of the Royal Astronomical Society 395(2): 884-894. <http://hdl.handle.net/2027.42/74893>en_US
dc.identifier.issn0035-8711en_US
dc.identifier.issn1365-2966en_US
dc.identifier.urihttps://hdl.handle.net/2027.42/74893
dc.description.abstractWe present phase resolved optical spectroscopy and photometry of V4580 Sagittarii, the optical counterpart to the accretion powered millisecond pulsar SAX J1808.4−3658, obtained during the 2008 September/October outburst. Doppler tomography of the N iiiΛ4640.64 Bowen blend emission line reveals a focused spot of emission at a location consistent with the secondary star. The velocity of this emission occurs at 324 ± 15 km s −1 ; applying a ‘ K -correction’, we find the velocity of the secondary star projected on to the line of sight to be 370 ± 40 km s −1 . Based on existing pulse timing measurements, this constrains the mass ratio of the system to be 0.044 +0.005 −0.004 , and the mass function for the pulsar to be 0.44 +0.16 −0.13  M ⊙ . Combining this mass function with various inclination estimates from other authors, we find no evidence to suggest that the neutron star in SAX J1808.4−3658 is more massive than the canonical value of 1.4 M ⊙ . Our optical light curves exhibit a possible superhump modulation, expected for a system with such a low mass ratio. The equivalent width of the Ca ii H and K interstellar absorption lines suggest that the distance to the source is ∼2.5 kpc. This is consistent with previous distance estimates based on type-I X-ray bursts which assume cosmic abundances of hydrogen, but lower than more recent estimates which assume helium-rich bursts.en_US
dc.format.extent1613691 bytes
dc.format.extent3109 bytes
dc.format.mimetypeapplication/pdf
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dc.publisherBlackwell Publishing Ltden_US
dc.rightsJournal compilation © 2009 RASen_US
dc.subject.otherAccretion, Accretion Discsen_US
dc.subject.otherBinaries: Closeen_US
dc.subject.otherStars: Individual: V4580 Sagittariien_US
dc.subject.otherStars: Neutronen_US
dc.subject.otherPulsars: Individual: SAX J1808.4−3658en_US
dc.subject.otherX-rays: Binariesen_US
dc.titleOptical spectroscopy and photometry of SAX J1808.4−3658 in outbursten_US
dc.typeArticleen_US
dc.subject.hlbsecondlevelAstronomyen_US
dc.subject.hlbtoplevelScienceen_US
dc.description.peerreviewedPeer Revieweden_US
dc.contributor.affiliationumDepartment of Astronomy, University of Michigan, 500 Church Street, Ann Arbor, MI 48109-1042, USAen_US
dc.contributor.affiliationumPhysics Department, University of Michigan, 450 Church Street, Ann Arbor, MI 48109-1040, USAen_US
dc.contributor.affiliationotherDepartment of Physics, University College Cork, Cork, Irelanden_US
dc.contributor.affiliationotherArmagh Observatory, College Hill, Armagh BT61 9DGen_US
dc.contributor.affiliationotherFaulkes Telescope Project, School of Physics and Astronomy, Cardiff University, 5, The Parade, Cardiff CF24 3AAen_US
dc.contributor.affiliationotherDepartment of Physics and Astronomy, The Open University, Walton Hall, Milton Keynes MK7 6AAen_US
dc.contributor.affiliationotherLas Cumbres Observatory Global Telescope, 6740 Cortona Drive, Goleta, CA 93117, USAen_US
dc.contributor.affiliationotherAstronomical Institute ‘Anton Pannekoek’, Kruislaan 403, 1098 SJ Amsterdam, the Netherlandsen_US
dc.contributor.affiliationotherNASA Exoplanet Science Institute, Caltech, MS 100-22, 770 South Wilson Avenue, Pasadena, CA 91125, USAen_US
dc.contributor.affiliationotherDepartment of Physics, Texas A&M University, 4242 TAMU, College Station, TX 77843-4242, USAen_US
dc.contributor.affiliationotherTuorla Observatory, University of Turku, VÄisÄlÄntie 20, FIN-21500 PiikkiÖ, Finlanden_US
dc.description.bitstreamurlhttp://deepblue.lib.umich.edu/bitstream/2027.42/74893/1/j.1365-2966.2009.14562.x.pdf
dc.identifier.doi10.1111/j.1365-2966.2009.14562.xen_US
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