Keck observations of the black-hole candidate GRO J0422+32

Details Keck observations of the black-hole candidate GRO J0422+32 Keck observations of the black-hole candidate GRO J0422+32

Jan 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999a%26a...341..491h&link_type=abstract

Astronomy and Astrophysics, v.341, p.491-498 (1999)

Physics

31

Black Hole Physics, Stars: Binaries: Close, Stars: Individual: Gro J0422+32, Stars: Novae, Cataclysmic Variables, X-Rays: Stars

Scientific paper

Keck observations of the black-hole candidate GRO J0422+32 in quiescence have been used by Filippenko, Matheson, & Ho (1995) to determine a mass function f(M_x) = 1.21 +/- 0.06 Msun for the compact object. Reanalysis of the data shows that the mass ratio, q = M_c/M_x, is q = 0.116(+0.079}_{-0.071) from the rotational broadening of the companion star upsilon sin i = 90(+22}_{-27) km s(-1) (1sigma ). From q and the mass function (slightly revised to 1.13 +/- 0.09 Msun), we derive the mass of the compact object, M_x = (1.4 +/- 0.2) sin (-3) i Msun. The companion star (M2(+2}_{-1) spectral type) contributes 61 +/- 4% of the light at red wavelengths. An Hα Doppler image of the system shows the typical ring-like distribution of an accretion disk. Emissivity laws for Hα in black-hole binaries roughly follow an R(-1.5) law, which is also supported by GRO J0422+32. The LiI <~mbda6708 absorption line is not detected (1sigma equivalent width limit of 0.13 Angstroms), in contrast to four other X-ray binaries. Based on observations obtained at the W.M. Keck Observatory

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