2014A&A...563A...1G


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.04CEST15:19:52

2014A&A...563A...1G - Astronomy and Astrophysics, volume 563A, 1-1 (2014/3-1)

Orbit and properties of the massive X-ray binary BD+6073 = IGR J00370+6122.

GRUNHUT J.H., BOLTON C.T. and McSWAIN M.V.

Abstract (from CDS):

High-energy X-rays generated in massive binary systems can arise from several different mechanisms. Constraints on the orbital parameters of these systems are therefore necessary to properly understand and interpret the X-ray phenomena. In this study we aim to determine a spectroscopic orbit for the high-mass X-ray binary system BD+60 73=IGR J00370+6122, to infer the properties of the optical and compact companion, and to interpret the characteristics of the X-ray light curve within the context of our findings. We acquired 123 spectroscopic observations with the David Dunlap Observatory and Kitt Peak National Observatory telescopes in the optical domain. Using a cross-correlation technique, we measured the radial velocity of each of these spectra relative to the heliocentric rest-frame. An orbital solution was obtained from the resulting radial velocity measurements. Spectra of several spectral standards were also acquired to reassess the spectral classification of the optical companion. The best-fit orbital parameters suggest an eccentricity of e=0.48+0.02–0.03 and a mass-function of f(M)=0.009±0.002, lending further support to the assumption that the companion is a low-mass compact star. We find that the X-ray maximum occurs just after the time of periastron passage, but before the time of superior conjunction when the optical companion could eclipse the compact companion. The spectrum of the optical companion is best matched by the B1Ib spectral standard HD24398, which reaffirms the original classification. The mass-function combined with a plausible range of possible masses for a neutron star companion yields primary masses within the range expected for the spectral type of BD+60 73 for high orbital inclinations. The compact companion cannot be a black hole unless the supergiant has an exceptionally high mass for its B1Ib spectral type or if the inclination of its orbit is very low. The X-ray timing and characteristics can potentially be explained by accretion variations on the compact object; but this would require the companion to be a magnetar.

Abstract Copyright:

Journal keyword(s): techniques: radial velocities - techniques: spectroscopic - ephemerides - stars: magnetars - binaries: general - stars: individual: BD+60 73

Simbad objects: 14

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Number of rows : 14

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 Ass Cas OB 4 As* 00 27 +62.4           ~ 41 0
2 BD+60 73 HXB 00 37 09.6358465128 +61 21 36.485521705 9.79 10.14 9.66     B1Ib 62 0
3 Ass Cas OB 7 As* 00 50 14 +64 04.3           ~ 59 0
4 Ass Cas OB 1 As* 01 00 +61.5           ~ 38 0
5 * omi Per ** 03 44 19.13204 +32 17 17.6929 3.13 3.88 3.83 3.71 3.71 B1III 572 0
6 * zet Per V* 03 54 07.9224751 +31 53 01.081262 2.19 2.97 2.85 2.71 2.62 B1Ib 812 0
7 * eps Per bC* 03 57 51.2320472 +40 00 36.775143 1.71 2.71 2.89 2.96 3.14 B1.5III 494 0
8 HD 35648 * 05 24 52.5432912928 -31 47 10.141773591   10.28 8.84     K3(III) 3 0
9 * tet01 Ori B Al* 05 35 16.112 -05 23 06.89 7.71 8.20 7.96     B1V 340 2
10 * kap Ori s*b 05 47 45.3888404 -09 40 10.577707 0.87 1.88 2.06 2.09 2.27 B0.5Ia 545 0
11 * chi02 Ori s*b 06 03 55.1848402263 +20 08 18.441609669 4.24 4.91 4.63 4.32 4.10 B2Ia 428 0
12 GSC 03588-00834 HXB 21 03 35.7101268891 +45 45 05.568943629   15.34 14.20 13.49 12.75 B0Ve 147 0
13 * 1 Cas * 23 06 36.8178557 +59 25 11.135698 3.93 4.771 4.840     B0.5III 228 0
14 Ass Cas OB 5 As* 23 54 +61.6           ~ 68 0

    Equat.    Gal    SGal    Ecl

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2020.07.04-15:19:52

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