The Kinematics and Physical Conditions of the Ionized Gas in Markarian 509. I. Chandra High-Energy Grating Spectroscopy

Details The Kinematics and Physical Conditions of the Ionized Gas in Markarian 509. I. Chandra High-Energy Grating Spectroscopy The Kinematics and Physical Conditions of the Ionized Gas in Markarian 509. I. Chandra High-Energy Grating Spectroscopy

2002-08-29

arxiv.org/abs/astro-ph/0208530v1

Astrophys.J. 582 (2003) 105-124

Astronomy and Astrophysics

Astrophysics

Accepted for publication in the Astrophysical Journal. 66 pages, 14 figures, six of them color. Abstract is abridged

Scientific paper

10.1086/344541

We observed the Seyfert 1 galaxy Mrk 509 simultaneously with Chandra/HETG, HST/STIS and RXTE. We measure strong absorption lines from He-like Ne and Mg, and from H-like N, O, and Ne. The lines are unresolved except for Ne Lya and Ne IX(r). The absorption-line profiles are blueshifted by ~200 km/s with respect to the systemic velocity of Mrk 509, and there is a hint of another component near systemic. The soft X-ray spectrum can be described in remarkable detail with a simple, single-zone photoionized absorber with a column density of 2.06 (+0.39,-0.45) x 10^21 cm^-2 and an ionization parameter of log{xi} = 1.76 (+0.13,-0.14) (or log{U}=0.27). The UV data, on the other hand, can easily detect eight kinematic components, covering roughly the same velocities as the X-ray absorption profiles. Even though the X-ray and UV absorbers share the same velocity space, the UV absorbers have a much smaller column density and ionization state. We show that models of the X-ray data do not predict significant UV absorption and are therefore consistent with the UV data. The UV absorbers could be embedded in the X-ray absorber, as a multiphase medium. Finally, we do not detect any soft X-ray emission lines.

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