A CENSUS OF X-RAY GAS IN NGC 1068: RESULTS FROM 450 ks of CHANDRA HIGH ENERGY TRANSMISSION GRATING OBSERVATIONS

We present models for the X-ray spectrum of the Seyfert 2 galaxy NGC 1068. These are fitted to data obtained using the High Energy Transmission Grating on Chandra. The data show line and radiative recombination continuum emission from a broad range of ions and elements. The models explore the import...

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Main Authors: Kallman, T. R. (Author), Evans, Daniel A. (Author), Longinotti, Anna Lia (Author), Marshall, Herman Lee (Contributor), Canizares, Claude R. (Contributor), Nowak, Michael A. (Contributor), Schulz, Norbert S. (Contributor)
Other Authors: MIT Kavli Institute for Astrophysics and Space Research (Contributor)
Format: Article
Language:English
Published: IOP Publishing, 2015-02-17T14:45:52Z.
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Online Access:Get fulltext
LEADER 02369 am a22002773u 4500
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042 |a dc 
100 1 0 |a Kallman, T. R.  |e author 
100 1 0 |a MIT Kavli Institute for Astrophysics and Space Research  |e contributor 
100 1 0 |a Marshall, Herman Lee  |e contributor 
100 1 0 |a Canizares, Claude R.  |e contributor 
100 1 0 |a Nowak, Michael A.  |e contributor 
100 1 0 |a Schulz, Norbert S.  |e contributor 
700 1 0 |a Evans, Daniel A.  |e author 
700 1 0 |a Longinotti, Anna Lia  |e author 
700 1 0 |a Marshall, Herman Lee  |e author 
700 1 0 |a Canizares, Claude R.  |e author 
700 1 0 |a Nowak, Michael A.  |e author 
700 1 0 |a Schulz, Norbert S.  |e author 
245 0 0 |a A CENSUS OF X-RAY GAS IN NGC 1068: RESULTS FROM 450 ks of CHANDRA HIGH ENERGY TRANSMISSION GRATING OBSERVATIONS 
260 |b IOP Publishing,   |c 2015-02-17T14:45:52Z. 
856 |z Get fulltext  |u http://hdl.handle.net/1721.1/94546 
520 |a We present models for the X-ray spectrum of the Seyfert 2 galaxy NGC 1068. These are fitted to data obtained using the High Energy Transmission Grating on Chandra. The data show line and radiative recombination continuum emission from a broad range of ions and elements. The models explore the importance of excitation processes for these lines including photoionization followed by recombination, radiative excitation by absorption of continuum radiation, and inner shell fluorescence. The models show that the relative importance of these processes depends on the conditions in the emitting gas and that no single emitting component can fit the entire spectrum. In particular, the relative importance of radiative excitation and photoionization/recombination differs according to the element and ion stage emitting the line. This in turn implies a diversity of values for the ionization parameter of the various components of gas responsible for the emission, ranging from log(ξ) = 1 to 3. Using this, we obtain an estimate for the total amount of gas responsible for the observed emission. The mass flux through the region included in the HETG extraction region is approximately 0.3 M [subscript ☉] yr[superscript -1], assuming ordered flow at the speed characterizing the line widths. This can be compared with what is known about this object from other techniques. 
546 |a en_US 
655 7 |a Article 
773 |t The Astrophysical Journal