The collisional and photoionized plasma in the polarized NLS1 galaxy Mrk 1239

Author:

Buhariwalla Margaret Z1,Gallo Luigi C1,Mao J23ORCID,Komossa S4,Jiang J5,Gonzalez A1,Grupe D6

Affiliation:

1. Department of Astronomy and Physics, Saint Mary’s University , 923 Robie Street, Halifax, NS B3H 3C3, Canada

2. Department of Astronomy, Tsinghua Univerisity , 30 Shuangqing Road, Beijing 100084, China

3. Department of Physics, Hiroshima University , 1-3-1 Kagamiyama, Higashi-Hiroshima City, Hiroshima 739-8526, Japan

4. Max-Planck-Institut für Radioastronomie , Auf dem Hügel 69, D-53121 Bonn, Germany

5. Institute of Astronomy, University of Cambridge , Madingley Road, Cambridge CB3 0HA, UK

6. Department of Physics, Geology, and Engineering Technology Science Center, Northern Kentucky University , 1 Nunn Drive, Highland Heights, KY 41099, USA

Abstract

ABSTRACTMrk 1239 is a highly polarized NLS1 in the optical band, whose 0.3–3 keV spectrum has remained remarkably consistent over more than two decades of observation. Previous analysis of this object suggested that the soft X-ray band was dominated by emission lines (collisionally and/or photoionized) from the distant host galaxy as the X-ray emission from the central engine was highly obscured. New XMM–Newton data of Mrk 1239 are presented here to investigate the soft X-ray band of this galaxy with high resolution. The first RGS spectra of this source reveal a plethora of ionized emission lines originating from two distinct plasmas, one collisionally ionized and the other photoionized at approximately equal brightness. The best-fitting model uses apec and xstar grids to account for the collisionally ionized and photoionized components, respectively. The fit improves significantly if the photoionized material is allowed to outflow at ≈500 km s−1, matching the outflow velocity of the forbidden O vii emission line. From constraints on the ionization and density of the photoionized material, we can estimate the location of it to be no further than a few pc from the central source, around the outer radius of the torus, which is consistent with the O vii(f) emission line. Properties of the collisionally ionized plasma are consistent with star formation rate (SFR) of $\approx 3 \hbox{$\rm \, M_{\odot }$}\textrm {yr}^{-1}$, which is comparable with several previous measurements of the SFR in this galaxy.

Funder

Leverhulme Trust

Isaac Newton Trust

St. Edmund’s College, University of Cambridge

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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