PHYSICAL CONDITIONS IN THE X-RAY EMISSION-LINE GAS IN NGC 1068

• Published in: The Astrophysical journal Vol. 798; no. 1; pp. 53 - 12
• Main Authors: Kraemer, S. B., Sharma, N., Turner, T. J., George, Ian M., Crenshaw, D. Michael
• Format: Journal Article
• Language: English
• Published: United States 01.01.2015
• Subjects: ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; CARBON; COMPUTERIZED SIMULATION; Diffraction gratings; ELECTRON TEMPERATURE; Emission spectroscopy; Gratings (spectra); INFRARED SPECTRA; IRON; L SHELL; MASS; NEON; NITROGEN; OXYGEN; PHOTOIONIZATION; Physical properties; RADIAL VELOCITY; RECOMBINATION; REFLECTION; SEYFERT GALAXIES; SOFT X RADIATION; STAR CLUSTERS; STARS; X-RAY GALAXIES; X-rays; XMM (spacecraft)
• ISSN: 1538-4357; 0004-637X; 1538-4357
• DOI: 10.1088/0004-637X/798/1/53

We present a detailed, photo-ionization modeling analysis of XMM-Newton/Reflection Grating Spectrometer observations of the Seyfert 2 galaxy NGC 1068. The spectrum, previously analyzed by Kinkhabwala et al., reveals a myriad of soft X-ray emission lines, including those from H- and He-like carbon, nitrogen, oxygen, and neon, and M- and L-shell iron. The total mass of the X-ray gas is roughly an order of magnitude greater than the mass of ionized gas determined from optical and near-IR spectroscopy, which indicates that it may be the dominant component of the narrow-line region. Furthermore, we suggest that the medium that produces the scattered/polarized optical emission in NGC 1068 possesses similar physical characteristics to those of the more highly ionized of the X-ray model components.