IGR J00370+6122

Other names =

1 RXS J003709.6+612131

Type Orbital/Spin periods Radio Counterpart Infrared/Optical Counterpart
R.A. (J2000) Dec. (J2000) References R.A. (J2000) Dec. (J2000) References
HMXB (BN0.7Ib star) + pulsar 15.667 d / 359 s BD +60 73
00h 37m 09.63s 61° 21' 36.501"
Published Papers
Miscellaneous :
Neguerela et al. 2004 Atel 385:
    BN0.5II-IIIb supergiant with V=9.64. Leads to D~3.0 kpc
den Hartog et al. 2004 Atel 281:
    Orbital period 15.665 days
Cameron et al. 2004 Atel 312:
    No radio detection at 4 frequency down to relatively low levels
Reig et al. 2005 (A&A):
    eccentric orbit needed to explain the production of X-rays
Wen et al. 2006 (ApJS):
    Orbital period of 15.670 days with RXTE/ASM
den Hartog et al. 2006 (A&A):
  • further associates the IGR and Rosat sources.
  • the source was detected in 4 occasions by Beppo-SAX. Brightest observation =>spectral fit with Gamma=2.6
  • RXTE ToO => power law shaped spectra with gamma=2.74.
  • Comparison between INTEGRAL, Beppo-SAX and RXTE => source is highly variable from orbit to orbit.
  • Nh by RXTE and Beppo-SAX varies from 7e22 to 13e22, while the measured flux vary from 3e-10erg/s/cm2 (2-20 keV) to 1.8e-11 erg/s/cm2 (3-30 keV).
in't Zand et al. 2007 (A&A):
  • Refinement of orbital period and ephemeris to
    with RXTE/ASM
  • Period in INTEGRAL 20-45 and 45-89 keV folded light curves.
  • Spectral analysis performed with PCA and ISGRI=> average spectrum during the flare shows Nh~9.1 e22 cm-2 and Gamma=2.14 (PCA), while the ISGRI spectrum is somewhat harder with Gamma=1.84
  • Possible detection of a coherent signal at 359s => associate to the pulsar spin period.
  • Pulse period and orbital period=> wind accretion regime in the Corbet diagram.
Grunhut et al. (A&A):
  • Determination of orbital solution through spectroscopic observations of BD +60 73 optical companion.
  • Eccentricity =0.48-0.03+0.02 and mass function f(M)=0.009 => low mass compact object.
  • Spectrum of companion is best matched by B1Ib spectral type
  • Not a black hole unless the companion has an exceptionnaly high mass for this spectral type
González-Galán et al. 2014 (A&A):
  • High resolution spectra at different epoch
  • BD +60 73 is a low luminosity sg (BN0.7 Ib) star
  • Teff=24 000 K, d~ 3.1 kpc, eccentricity ~ 0.56
  • Intermediate supergiant X-ray transient will likely evolve towards persistent Sg binary

Last updated 25 April 2014

Jerome Rodriguez