TY - JOUR
T1 - Suzaku broadband observations of galactic black hole binaries
T2 - 6th Integral Workshop - The Obscured Universe
AU - Takahashi, Hiromitsu
AU - Fukazawa, Yasushi
AU - Mizuno, Tsunefumi
AU - Hirasawa, Ayumi
AU - Kitamoto, Shunji
AU - Sudoh, Keisuke
AU - Ogita, Takayuki
AU - Kubota, Aya
AU - Makishima, Kazuo
AU - Kokubun, Motohide
AU - Itoh, Takeshi
AU - Parmar, Arvind N.
AU - Dotani, Tadayasu
AU - Ebisawa, Ken
AU - Naik, Sachindra
AU - Takahashi, Tadayuki
AU - Ohnuki, Kousuke
AU - Yaqoob, Tahir
AU - Angelini, Lorella
AU - Ueda, Yoshihiro
AU - Yamaoka, Kazutaka
AU - Kotani, Taro
AU - Kawai, Nobuyuki
AU - Namiki, Masaaki
AU - Kohmura, Takayoshi
AU - Negoro, Hitoshi
PY - 2006/7
Y1 - 2006/7
N2 - The Galactic black-hole binary GRO J1655-40 was observed with Suzaku on 2005 September 22-23, for a gross time span of ∼1 day.The source was detected over a wide and continuous energy range of 0.7-300 keV, with an intensity of ∼50 mCrab in the 1.5-12 keV band. At an assumed distance of 3.2 kpc, the 0.7-300 keV luminosity is calculated to be ∼ 4.4 × 10 36 ergs s-1. The source was in a typical low/hard state, since its overall spectrum was dominated by a power-law component with a photon index of ∼1.7. The source intensity gradually decreased by 20% during the observation, involving little spectral changes above ∼3 keV. However, at softer energies, the amplitude of variability was somewhat enhanced. This indicates the presence of an independent soft component. The spectra in the hard energy band reveal a high-energy spectral cutoff, with an e-folding energy of ∼200 keV which is suggested to be higher than those observed from typical black hole binaries in the low/hard state.
AB - The Galactic black-hole binary GRO J1655-40 was observed with Suzaku on 2005 September 22-23, for a gross time span of ∼1 day.The source was detected over a wide and continuous energy range of 0.7-300 keV, with an intensity of ∼50 mCrab in the 1.5-12 keV band. At an assumed distance of 3.2 kpc, the 0.7-300 keV luminosity is calculated to be ∼ 4.4 × 10 36 ergs s-1. The source was in a typical low/hard state, since its overall spectrum was dominated by a power-law component with a photon index of ∼1.7. The source intensity gradually decreased by 20% during the observation, involving little spectral changes above ∼3 keV. However, at softer energies, the amplitude of variability was somewhat enhanced. This indicates the presence of an independent soft component. The spectra in the hard energy band reveal a high-energy spectral cutoff, with an e-folding energy of ∼200 keV which is suggested to be higher than those observed from typical black hole binaries in the low/hard state.
KW - Accretion disks
KW - Black hole physics
KW - Stars: individual (GRO J1655-40)
KW - X-ray: binaries
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M3 - Conference article
AN - SCOPUS:45749146714
SN - 0379-6566
SP - 325
EP - 332
JO - European Space Agency, (Special Publication) ESA SP
JF - European Space Agency, (Special Publication) ESA SP
IS - 622 SP
Y2 - 2 July 2006 through 8 July 2006
ER -