2018A&A...615A..72M


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.24CEST08:04:56

2018A&A...615A..72M - Astronomy and Astrophysics, volume 615A, 72-72 (2018/7-1)

Multi-wavelength campaign on NGC 7469. III. Spectral energy distribution and the AGN wind photoionisation modelling, plus detection of diffuse X-rays from the starburst with Chandra HETGS.

MEHDIPOUR M., KAASTRA J.S., COSTANTINI E., BEHAR E., KRISS G.A., BIANCHI S., BRANDUARDI-RAYMONT G., CAPPI M., EBRERO J., DI GESU L., KASPI S., MAO J., DE MARCO B., MIDDEI R., PERETZ U., PETRUCCI P.-O., PONTI G. and URSINI F.

Abstract (from CDS):

We investigate the physical structure of the active galactic nucleus (AGN) wind in the Seyfert-1 galaxy NGC 7469 through high-resolution X-ray spectroscopy with Chandra HETGS and photoionisation modelling. Contemporaneous data from Chandra, HST, and Swift are used to model the optical-UV-X-ray continuum and determine the spectral energy distribution (SED) at two epochs, 13yr apart. For our investigation we use new observations taken in December 2015-January 2016, and historical ones taken in December 2002. We study the impact of a change in the SED shape, seen between the two epochs, on the photoionisation of the wind. The HETGS spectroscopy shows that the AGN wind in NGC 7469 consists of four ionisation components, with their outflow velocities ranging from -400 to -1800km/s. From our modelling we find that the change in the ionising continuum shape between the two epochs results in some variation in the ionisation state of the wind components. However, for the main ions detected in X-rays, the sum of their column densities over all components remains in practice unchanged. For two of the four components, which are found to be thermally unstable in both epochs, we obtain 2<r<31pc and 12<r<29pc using the cooling and recombination timescales. For the other two thermally stable components, we obtain r<31pc and r<80pc from the recombination timescale. The results of our photoionisation modelling and thermal stability analysis suggest that the absorber components in NGC 7469 are consistent with being a thermally driven wind from the AGN torus. Finally, from analysis of the zeroth-order ACIS/HETG data, we discover that the X-ray emission in the range 0.2-1keV is spatially extended over 1.5-12''. This diffuse soft X-ray emission is explained by coronal emission from the nuclear starburst ring in NGC 7469. The star formation rate inferred from this diffuse soft X-ray emission is consistent with those found by far-infrared studies of NGC 7469.

Abstract Copyright: © ESO 2018

Journal keyword(s): X-rays: galaxies - galaxies: active - galaxies: Seyfert - galaxies: individual: NGC 7469 - techniques: spectroscopic

VizieR on-line data: <Available at CDS (J/A+A/615/A72): heg2002.dat heg2016.dat megstack.dat>

Simbad objects: 4

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Number of rows : 4

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 NGC 3783 Sy1 11 39 01.7095761008 -37 44 19.008597647   12.46 13.43 11.33 12.1 ~ 1445 0
2 NGC 5548 Sy1 14 17 59.5401093128 +25 08 12.600227883   14.35 13.73     ~ 2335 0
3 Mrk 509 Sy1 20 44 09.7504131334 -10 43 24.724854084   13.35 13.12 10.7   ~ 1093 0
4 NGC 7469 Sy1 23 03 15.674 +08 52 25.28 12.60 13.00 12.34     ~ 1843 3

    Equat.    Gal    SGal    Ecl

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2019.10.24-08:04:56

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