X-Ray and Near-Infrared Observations of GX 339-4 in the Low/Hard State with Suzaku and IRSF

X-ray and near-infrared ($J$-$H$-$K_{\rm s}$) observations of the Galactic black hole binary GX 339--4 in the low/hard state were performed with Suzaku and IRSF in 2009 March. The spectrum in the 0.5--300 keV band is dominated by thermal Comptonization of multicolor disk photons, with a small contribution from a direct disk component, indicating that the inner disk is almost fully covered by hot corona with an electron temperature of $\approx$175 keV. The Comptonizing corona has at least two optical depths, $\tau \approx 1,0.4$. Analysis of the iron-K line profile yields an inner disk radius of $(13.3^{+6.4}_{-6.0}) R_{\rm g}$ ($R_{\rm g}$ represents the gravitational radius $GM/c^2$), with the best-fit inclination angle of $\approx50^\circ$. This radius is consistent with that estimated from the continuum fit by assuming the conservation of photon numbers in Comptonization. Our results suggest that the standard disk of GX 339--4 is likely truncated before reaching the innermost stable circular orbit (for a non rotating black hole) in the low/hard state at $\sim$1% of the Eddington luminosity. The one-day averaged near-infrared light curves are found to be correlated with hard X-ray flux with $F_{\rm Ks} \propto F_{\rm X}^{0.45}$. The flatter near infrared $\nu F_{\nu}$ spectrum than the radio one suggests that the optically thin synchrotron radiation from the compact jets dominates the near-infrared flux. Based on a simple analysis, we estimate the magnetic field and size of the jet base to be $5\times10^4$ G and $6\times 10^8$ cm, respectively. The synchrotron self Compton component is estimated to be approximately 0.4% of the total X-ray flux.Comment: 17pages, 15 figures, accepted for publication in PASJ (Suzaku and MAXI Special Issue

Spectroscopically identified intermediate age stars at 0.5–3 pc distance from Sagittarius A*

Context. Nuclear star clusters (NSCs) at the dynamical center of galaxies appear to have a complex star formation history. This suggests repeated star formation, even in the influence of the strong tidal field from supermassive black holes. Although the central region of our Galaxy is an ideal target for studies of the star formation history in the NSCs, most studies in the past have concentrated on a projected distance of RSgr A ∗ ~ 0.5 pc from the supermassive black hole Sgr A*. Aims. In our previous study, we detected 31 so far unknown early-type star candidates throughout the Galactic NSC (at RSgr A ∗ = 0.5–3 pc). They were found via near-infrared (NIR) imaging observations with narrow-band filters which are sensitive to CO absorption lines at ~2.3 μm, a prominent feature for old, late-type stars. The aim of this study is to confirm the spectral type for the early-type star candidates. Methods. We have carried out NIR spectroscopic observations of the early-type star candidates using Subaru/IRCS/AO188 and the laser guide star system. K-band spectra for 20 out of the 31 candidates and reference late-type stars were obtained. By determining an equivalent width, EW(CO), of the 12CO absorption feature at ≈2.294 μm, we have derived an effective temperature and a bolometric magnitude for each candidate and late-type star, and then constructed an HR diagram. Results. No young (~Myr) massive stars are included in the 20 candidates we observed; however, 13 candidates are most likely intermediate-age giants (50–500 Myr). Two other sources have ages of ~1 Gyr and the remaining five sources are old (>1 Gyr), late-type giants. Conclusions. Although none of the early-type star candidates from our previous narrow-band imaging observations can be confirmed as a young star, we find that the photometric technique can distinguish old, late-type giants from young and intermediate-age populations. From the 20 spectroscopically observed candidates, 65% of them are confirmed as being younger than 500 Myr. The intermediate-age stars could be as yet unknown members of a population formed in a starburst ~100 Myr ago. Finding no young (~a few Myr) stars at RSgr A ∗ = 0.5–3 pc favors the in situ formation scenario for the presence of the young stars at RSgr A ∗< 0.5 pc, although we do not completely exclude the possible existence of unknown young, massive stars in the region from our observations. Furthermore, the different spatial distributions of the young and the intermediate-age stars imply that the Galactic NSC is an aggregate of stars that were born in different places and under a variety of physical conditions