Detection of Highly Ionized O and Ne Absorption Lines in the X-Ray Spectrum of 4U 1820–303 in the Globular Cluster NGC 6624

• Published in: The Astrophysical journal 2004-04, Vol.605 (2), p.793-799
• Main Authors: Futamoto, Kazuo, Mitsuda, Kazuhisa, Takei, Yoh, Fujimoto, Ryuichi, Yamasaki, Noriko Y
• Format: Article
• Language: English
• ISSN: 0004-637X; 1538-4357
• DOI: 10.1086/381087

We searched for absorption lines of highly ionized O and Ne in the energy spectra of two low-mass X-ray binaries, 4U 1820-303 in the globular cluster NGC 6624 and Cyg X-2, observed with the Chandra LETG, and detected O VII, O VIII, and Ne IX absorption lines for 4U 1820-303. The equivalent width of the O VII Kalpha line was 1.19[image] eV (90% errors), and the significance was 6.5 capital sigma . Absorption lines were not detected for Cyg X-2 with a 90% upper limit on the equivalent width of 1.06 eV for O VII Kalpha. The intrinsic line width was not resolved, and an upper limit corresponding to a velocity dispersion of b = 420 km s super(-1) was obtained for the O VII Kalpha line of 4U 1820-303. The ion column densities were estimated from the curve-of-growth analysis, assuming several different values of b. The absorption lines observed in 4U 1820-303 are likely due to hot interstellar medium, because O will be fully photoionized if the absorbing column is located close to the binary system. The velocity dispersion is restricted to b = 200-420 km s super(-1) from consistency between O VII Kalpha and K beta lines, the Ne/O abundance ratio, and H column density. The average temperature and the O VII density are estimated to be log T(K) = 6.2-6.3 and n[image] = (0.7-2.3) x 10 super(-6) cm super(-3), respectively. The difference of O VII column densities for the two sources may be connected to the enhancement of the soft X-ray background (SXB) toward the Galactic bulge region. Using the polytrope model of hot gas to account for the SXB, we corrected for the density gradient and estimated the midplane O VII density at the solar neighborhood. The scale height of hot gas is then estimated using the active galactic nuclei (AGN) absorption lines. It is suggested that a significant portion of both the AGN absorption lines and the high-latitude SXB emission lines can be explained by the hot gas in our Galaxy.