A systematic study of photoionized emission and warm absorption signatures of the NLS1 Mrk 335
Name
2107.06851.pdf
Description
Accepted version
Size
947.46 KB
Format
Adobe PDF
Checksum (MD5)
d96a6da7593eff6245f6339338020663
Author(s)
Liu, H
Parker, ML
Jiang, J
Kara, E
Bambi, Cosimo
Grupe, D
Komossa, S
Date Issued
2021
Journal
Monthly Notices of the Royal Astronomical Society
Publisher
Oxford University Press (OUP)
Citation
Liu, H, Parker, ML, Jiang, J, Kara, E, Bambi, Cosimo et al. 2021. "A systematic study of photoionized emission and warm absorption signatures of the NLS1 Mrk 335." Monthly Notices of the Royal Astronomical Society, 506 (4).
Version
Author's final manuscript
Abstract
ABSTRACT
We present an analysis of all the archival high-resolution spectra of the narrow-line Seyfert 1 galaxy Mrk 335 obtained with Reflection Grating Spectrometer (RGS) onboard XMM–Newton. The spectra show rich emission and absorption features in low and intermediate flux intervals. We model the emission lines with the pion_xs grid and try to find any possible correlation between the properties of the emitting gas and the source flux. Current data do not allow detailed trace of the response of the line emitting gas to the X-ray flux of Mrk 335, but the flux of the X-ray lines is significantly less variable than the X-ray continuum. We also find that the warm absorber’s properties are not correlated with the flux variability. From the latest XMM–Newton observation in 2019 December, we find that the photoionized emission and distant reflection components have not responded to the flux drop of Mrk 335 from 2018 July. However, the possible existence of partial covering absorber in the 2018–2019 low state of Mrk 335 makes it difficult to constrain the scale of the emitting gas using this lack of response.
We present an analysis of all the archival high-resolution spectra of the narrow-line Seyfert 1 galaxy Mrk 335 obtained with Reflection Grating Spectrometer (RGS) onboard XMM–Newton. The spectra show rich emission and absorption features in low and intermediate flux intervals. We model the emission lines with the pion_xs grid and try to find any possible correlation between the properties of the emitting gas and the source flux. Current data do not allow detailed trace of the response of the line emitting gas to the X-ray flux of Mrk 335, but the flux of the X-ray lines is significantly less variable than the X-ray continuum. We also find that the warm absorber’s properties are not correlated with the flux variability. From the latest XMM–Newton observation in 2019 December, we find that the photoionized emission and distant reflection components have not responded to the flux drop of Mrk 335 from 2018 July. However, the possible existence of partial covering absorber in the 2018–2019 low state of Mrk 335 makes it difficult to constrain the scale of the emitting gas using this lack of response.
MIT Department
MIT Kavli Institute for Astrophysics and Space Research
Terms of Use
Creative Commons Attribution-Noncommercial-Share Alike
Persistent DSpace Link
DOI of Published Version
https://doi.org/10.1093/MNRAS/STAB2033
