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| Miscellaneous :
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:
- NH = 1022 at/cm2
- Short period binary (?)
- dipping behavior (~30% dips; ~5 min duration) (Markwardt and Swank 2003 Atel 156)
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Walter et al. 2006:
- soft excess explained by partially covered absorber and marginal K-alpha line (EW < 10 eV)
- NH = 4.5(+-0.7)x1022 at/cm2, or 2.70(+-0.15)x1022 at/cm2 if partial-covering absorber included
- IR counterpart (4.9 arcsec away) has a K-band magnitude of 12.9 (SEE HOWEVER CHATY ET
AL. 2008)
- unabsorbed flux (2-100 keV) is 3.4x10-10 ergs/cm2/s
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Bazzano et al. 2006 (ApJ):
- 43/-0.5 mCrab in 100-150 keV.
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Brandt et al. 2007: <
ATel
1054
- Detection of 2 X-ray bursts with JEM-X
- Bursts shape are FRED-like, e-folding time of about 5 seconds.
- Confirms IGR J17597-2201 is a burst source
- Current burst recurrence time could be of 3-10 hours.
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Chaty et al. 2008: - Optical and infrared observations
- 2MASS candidate is outside the XMM error
- 1 bright and 2 faint candidates in error box, plus 2 additional at the
bborder.
- No definite answer to which is true counterpart. Analysis of the
brightest is presented
- Discussion on type of the source, and LMXB suggested
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Ratti et al. 2010:
- Chandra and Optical observations
- Single optical counterpart in Chandra error box
- Position consistent with candidate 1 of Chaty et al.
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Bodaghee et al. 2012 (ApJ) :
- Non detection with Chandra => 2-10 keV 3-σ upper limit = 1.5E-12 erg/cm2/s
- Boundary on quiescent flux
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Zolotukhin & Revnivtsev 2015 (MNRAS) :
- Counterpart in UKIDSS, GLIMPSE (G007.5695+00.7703) catalogues
- J=16.58; H=14.87; K=13.89; m3.6=13.224; m4.5=13.230;
m5.8=12.93; m4.5>12.6
- Accretion from a stellar wind in an LMXB => source is a Symbiotic XRB
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