Volume 608, December 2017
|Number of page(s)||10|
|Published online||13 December 2017|
Chandra imaging of the ~kpc extended outflow in 1H 0419-577
1 Department of Astronomy, University of Geneva, 16 Ch. d’ Ecogia, 1290 Versoix, Switzerland
2 SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands
3 Osservatorio Astronomico di Roma (INAF), via Frascati 33, 00040 Monteporzio Catone (Roma), Italy
4 Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
Received: 29 August 2017
Accepted: 2 October 2017
The Seyfert 1 galaxy 1H 0419-577 hosts a ~kpc extended outflow that is evident in the [O iii] image and that is also detected as a warm absorber in the UV/X-ray spectrum. Here, we analyze a ~30 ks Chandra-ACIS X-ray image, with the aim of resolving the diffuse extranuclear X-ray emission and of investigating its relationship with the galactic outflow. Thanks to its sub-arcsecond spatial resolution, Chandra resolves the circumnuclear X-ray emission, which extends up to a projected distance of at least ~16 kpc from the center. The morphology of the diffuse X-ray emission is spherically symmetrical. We could not recover a morphological resemblance between the soft X-ray emission and the ionization bicone that is traced by the [O iii] outflow. Our spectral analysis indicates that one of the possible explanations for the extended emission is thermal emission from a low-density (nH ~ 10-3 cm-3) hot plasma (Te ~ 0.22 keV). If this is the case, we may be witnessing the cooling of a shock-heated wind bubble. In this scenario, the [O iii] emission line and the X-ray/UV absorption lines may trace cooler clumps that are entrained in the hot outflow. Alternatively, the extended emission could be to due to a blend of emission lines from a photoionized gas component having a hydrogen column density of NH ~ 2.1 × 1022 cm-2 and an ionization parameter of log ξ ~ 1.3. Because the source is viewed almost edge-on we argue that the photoionized gas nebula must be distributed mostly along the polar directions, outside our line of sight. In this geometry, the X-ray/UV warm absorber must trace a different gas component, physically disconnected from the emitting gas, and located closer to the equatorial plane.
Key words: quasars: general / quasars: emission lines / quasars: absorption lines / galaxies: individual: 1H 0419-577 / X-rays: galaxies
© ESO, 2017
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