Broad-band X-ray measurements of the black hole candidate XTE J1908+094

Free access article

Issue		A&A Volume 394, Number 2, November I 2002


Page(s)		553 - 560
Section		Formation, structure and evolution of stars
DOI		http://dx.doi.org/10.1051/0004-6361:20021123

A&A 394, 553-560 (2002)
DOI: 10.1051/0004-6361:20021123

Broad-band X-ray measurements of the black hole candidate XTE J1908+094

J. J. M. in 't Zand^{1, 2}, J. M. Miller³, T. Oosterbroek⁴ and A. N. Parmar⁴

¹ Astronomical Institute, Utrecht University, PO Box 80000, 3508 TA Utrecht, The Netherlands
² SRON National Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands
³ Center for Space Research and Department of Physics, Massachusetts Institute of Technology, Cambridge, MA 02139-4307, USA
⁴ Astrophysics Division, Research & Scientific Support Department, ESA, ESTEC SCI-SA, 2200 AG Noordwijk, The Netherlands

(Received 29 May 2002 / Accepted 1 August 2002 )

Abstract
XTE J1908+094 is an X-ray transient that went into outburst in February 2002. After two months it reached a 2-250 keV peak flux of 1 to $2\times10^{-8}$ erg cm ^-2 s ^-1. Circumstantial evidence points to an accreting galactic black hole as the origin of the X-radiation: pulsations nor thermonuclear flashes were detected that would identify a neutron star and the spectrum was unusually hard for a neutron star at the outburst onset. We report on BeppoSAX and RXTE All Sky Monitor observations of the broad-band spectrum of XTE J1908+094. The spectrum is consistent with a model consisting of a Comptonization component by a ~40 keV plasma,

a multicolor accretion disk blackbody component with a temperature just below 1 keV and a broad emission line at about 6 keV. The spectrum is heavily absorbed by cold interstellar matter with an equivalent hydrogen column density of $2.5\times10^{22}$ cm ^-2, which makes it difficult to study the black body component in detail. The black body component exhibits strong evolution about 6 weeks into the outburst. Two weeks later this is followed by a swift decay of the power law component. The broadness of the 6 keV feature may be due to relativistic broadening or Compton scattering of a narrow Fe-K line.

Key words: accretion, accretion disks -- binaries: close -- X-rays: individual: XTE J1908+094

Offprint request: J. J. M. in 't Zand, jeanz@sron.nl

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