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Infrared Spectroscopy of the Black Hole Candidate GRO J1655-40

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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Infrared Spectroscopy of the Black Hole Candidate GRO J1655-40

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  1. Infrared Spectroscopy of theBlack Hole CandidateGRO J1655-40 Francis T. O’Donovan based on

  2. 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.

  3. GRO J1655-40 • Discovered in July 1994 by CGRO. • X-ray Transient. Harbors a BH? • Superluminal jets. Model for AGN?!

  4. 166”x166” CTIO CIRIM image (K-band, 30s exposure)

  5. Observations Made • Keck II NIRSPEC spectrograph. • First high S/N ratio K-band (IR) spectrum of a BH XT system. • Looking for disk emission.

  6. 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.

  7. Spectroscopic Data Analysis • Spectra of isolated stars from spectral atlas of Wallace & Hinkle (1997).

  8. 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.

  9. 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!

  10. Modeling Mx ~ 7 Ms.

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

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