The Inclination Angle and Mass of the Black Hole in XTE J1118+480 | Zendy

Dawn Gelino | Zendy; Ş. Balman | Zendy; Ü. Kızıloğlu | Zendy; Arda Yılmaz | Zendy; Emrah Kalemci | Zendy; John A. Tomsick | Zendy

AI Assistant Blog Pricing

Home ZAIA Blog

Open Access

The Inclination Angle and Mass of the Black Hole in XTE J1118+480

Author(s) -

Dawn Gelino,

Ş. Balman,

Ü. Kızıloğlu,

Arda Yılmaz,

Emrah Kalemci,

John A. Tomsick

Publication year - 2006

Publication title -

the astrophysical journal

Language(s) - English

Resource type - Journals

eISSN - 1538-4357

pISSN - 0004-637X

DOI - 10.1086/500924

Subject(s) - physics , orbital inclination , astrophysics , infrared , photometry (optics) , spectral energy distribution , black hole (networking) , inclination angle , mass ratio , accretion disc , light curve , optics , astronomy , stars , geometry , binary number , galaxy , computer network , routing protocol , routing (electronic design automation) , arithmetic , mathematics , computer science , link state routing protocol

We have obtained optical and infrared photometry of the quiescent soft X-raytransient XTE J1118+480. In addition to optical and J-band variations, wepresent the first observed H- and K_s-band ellipsoidal variations for thissystem. We model the variations in all bands simultaneously with the WD98 lightcurve modeling code. The infrared colors of the secondary star in this systemare consistent with a K7V, while there is evidence for light from the accretiondisk in the optical. Combining the models with the observed spectral energydistribution of the system, the most likely value for the orbital inclinationangle is 68 +/- 2 deg. This inclination angle corresponds to a primary blackhole mass of 8.53 +/- 0.60 M_sun. Based on the derived physical parameters andinfrared colors of the system, we determine a distance of 1.72 +/- 0.10 kpc toXTE J1118+480.Comment: 6 pages, 3 figures, To appear in ApJ 01 May 2006 issu

The content you want is available to Zendy users.

Already have an account? Click here to sign in.

Having issues? You can contact us here

Accelerating Research