The kinematics and physical conditions of the ionized gas in markarian 509. I. Chandra high energy grating spectroscopy

Tahir Yaqoob, Barry McKernan, Steven B. Kraemer, D. Michael Crenshaw, Jack Gabel, Ian M. George, T. Jane Turner

Research output: Contribution to journalArticle

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Abstract

We observed the Seyfert 1 galaxy Mrk 509 for ∼59 ks with the Chandra high-energy transmission gratings, simultaneously with HST/STIS and RXTE. Here we present a detailed analysis of the soft X-ray spectrum observed with Chandra. We measure strong absorption lines from He-like Ne and Mg and from H-like N, O, and Ne. Weaker absorption lines may also be present. The lines are unresolved except for Ne x Lyα (λ12.134) and Ne IX 1s2-1s2p (λ13.447), which appear to be marginally resolved. The profiles are blueshifted with respect to the systemic velocity of Mrk 509, indicating an outflow of ∼-200 km s-1. There is also a hint that the profiles may have a velocity component near systemic. The soft X-ray spectrum can be described in remarkable detail with a simple, single-zone photoionized absorber having an equivalent neutral hydrogen column density of 2.06 +0.45 +0.39 × 1021 cm-2 and an ionization parameter of log U = 1.76-0.14 +0.13 (or log U = 0.27). Although the photoionized gas almost certainly is comprised of matter in more than one ionization state and may consist of several kinematic components, data with better spectral resolution and signal-to-noise ratio would be required to justify a more complex model. The UV data, on the other hand, have a velocity resolution of ∼10 km s-1 and 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. Finally, we do not detect any soft X-ray emission lines.

Original languageEnglish
Pages (from-to)105-124
Number of pages20
JournalAstrophysical Journal
Volume582
Issue number1 I
DOIs
StatePublished - Jan 1 2003
Externally publishedYes

Fingerprint

ionized gases
kinematics
spectroscopy
gratings
gas
energy
absorbers
ionization
x rays
profiles
X Ray Timing Explorer
spectral resolution
signal-to-noise ratio
physical conditions
coverings
signal to noise ratios
outflow
hydrogen
galaxies
gases

All Science Journal Classification (ASJC) codes

  • Nuclear and High Energy Physics
  • Space and Planetary Science

Cite this

Yaqoob, T., McKernan, B., Kraemer, S. B., Crenshaw, D. M., Gabel, J., George, I. M., & Turner, T. J. (2003). The kinematics and physical conditions of the ionized gas in markarian 509. I. Chandra high energy grating spectroscopy. Astrophysical Journal, 582(1 I), 105-124. https://doi.org/10.1086/344541

The kinematics and physical conditions of the ionized gas in markarian 509. I. Chandra high energy grating spectroscopy. / Yaqoob, Tahir; McKernan, Barry; Kraemer, Steven B.; Crenshaw, D. Michael; Gabel, Jack; George, Ian M.; Turner, T. Jane.

In: Astrophysical Journal, Vol. 582, No. 1 I, 01.01.2003, p. 105-124.

Research output: Contribution to journalArticle

Yaqoob, Tahir ; McKernan, Barry ; Kraemer, Steven B. ; Crenshaw, D. Michael ; Gabel, Jack ; George, Ian M. ; Turner, T. Jane. / The kinematics and physical conditions of the ionized gas in markarian 509. I. Chandra high energy grating spectroscopy. In: Astrophysical Journal. 2003 ; Vol. 582, No. 1 I. pp. 105-124.
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AU - Yaqoob, Tahir

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