infrared spectroscopy of the black hole candidate gro j1655 40 n.
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Infrared Spectroscopy of the Black Hole Candidate GRO J1655-40. Francis T. O’Donovan based on. Ay 101. BH = remnant from death of a massive star. How observe? - Binary star systems! X-ray binaries. XT - X-ray Transient system. Light curve - Ellipsoidal variability. GRO J1655-40.

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Presentation Transcript
ay 101
Ay 101
  • BH = remnant from death of a massive star.
  • How observe? - Binary star systems!
  • X-ray binaries.
  • XT - X-ray Transient system.
  • Light curve - Ellipsoidal variability.
gro j1655 40
GRO J1655-40
  • Discovered in July 1994 by CGRO.
  • X-ray Transient. Harbors a BH?
  • Superluminal jets. Model for AGN?!
observations made
Observations Made
  • Keck II NIRSPEC spectrograph.
  • First high S/N ratio K-band (IR) spectrum of a BH XT system.
  • Looking for disk emission.
atomic spectral line
Atomic Spectral Line
  • Br- or HI (4-7) @  = 21661.20Å.
  • HeI (0-1) @  = 20586.900Å.
  • FeI (5-4) @  = 20701.122Å.
  • SiI (2-1) @  = 21360.055Å.
  • TiI] (2-3) @  = 21890.0Å.
spectroscopic data analysis
Spectroscopic Data Analysis
  • Spectra of isolated stars from spectral atlas of Wallace & Hinkle (1997).
spectroscopic data analysis1
Spectroscopic Data Analysis
  • Spectra of isolated stars from spectral atlas of Wallace & Hinkle (1997).
  • Equivalent widths: Absorption spectrum similar to that ofa F5-F7 III-IV star.
spectroscopic data analysis2
Spectroscopic Data Analysis
  • Spectra of isolated stars from spectral atlas of Wallace & Hinkle (1997).
  • Equivalent widths: Absorption spectrum similar to that ofa F5-F7 III-IV star.
  • No emission  negligible disk contribution!
modeling
Modeling

Mx ~ 7 Ms.

comments and conclusions
Comments and Conclusions
  • Derived values comparable with previous studies.
  • But a unique determination of disk contribution.