2011A&A...534A..39M


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.02CEST15:20:47

2011A&A...534A..39M - Astronomy and Astrophysics, volume 534A, 39-39 (2011/10-1)

Multiwavelength campaign on Mrk 509. IV. Optical-UV-X-ray variability and the nature of the soft X-ray excess.

MEHDIPOUR M., BRANDUARDI-RAYMONT G., KAASTRA J.S., PETRUCCI P.O., KRISS G.A., PONTI G., BLUSTIN A.J., PALTANI S., CAPPI M., DETMERS R.G. and STEENBRUGGE K.C.

Abstract (from CDS):

We present the analysis of XMM-Newton and Swift optical-UV and X-ray observations of the Seyfert-1/QSO Mrk 509, part of an unprecedented multi-wavelength campaign, investigating the nuclear environment of this AGN. The XMM-Newton data are from a series of 10 observations of about 60ks each, spaced from each other by about 4 days, taken in Oct.-Nov. 2009. During our campaign, Mrk 509 was also observed with Swift for a period of about 100 days, monitoring the behaviour of the source before and after the XMM-Newton observations. With these data we have established the continuum spectrum in the optical-UV and X-ray bands and investigated its variability on the timescale of our campaign with a resolution time of a few days. In order to measure and model the continuum as far as possible into the UV, we also made use of Hubble Space Telescope (HST ) cosmic origin spectrograph (COS) observations of Mrk 509 (part of our coordinated campaign) and of an archival Far Ultraviolet Spectroscopic Explorer (FUSE ) observation. We have found that in addition to an X-ray power-law, the spectrum displays soft X-ray excess emission below 2keV, which interestingly varies in association with the thermal optical-UV emission from the accretion disc. The change in the X-ray power-law component flux (albeit smaller than that of the soft excess), on the other hand, is uncorrelated to the flux variability of the soft X-ray excess and the disc component on the probed timescale. The results of our simultaneous broad-band spectral and timing analysis suggest that, on a resolution time of a few days, the soft X-ray excess of Mrk 509 is produced by the Comptonisation of the thermal optical-UV photons from the accretion disc by a warm (0.2keV) optically thick (τ∼17) corona surrounding the inner regions of the disc. This makes Mrk 509, with a black hole mass of about 1-3x108M, the highest mass known system to display such behaviour and origin for the soft X-ray excess.

Abstract Copyright:

Journal keyword(s): galaxies: active - galaxies: nuclei - galaxies: Seyfert - quasars: individual: Mrk 509 - X-rays: galaxies

Simbad objects: 11

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Number of rows : 11

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 2MASS J01365444-3509524 Sy1 01 36 54.4577149075 -35 09 52.330090067   18.80 18.0 17.80   ~ 42 0
2 HZ 2 WD* 04 12 43.5549840231 +11 51 48.973557049 12.903 13.787 13.877 13.984 14.094 DA2.3 90 0
3 7C 103144.10+395402.00 Sy1 10 34 38.5975589813 +39 38 28.181434249   17.37 16.90     ~ 303 1
4 NGC 4151 Sy1 12 10 32.5771747733 +39 24 21.057727323   12.18 11.48     ~ 3379 2
5 GD 153 WD* 12 57 02.3224875106 +22 01 52.634392478 11.883 13.060 13.349 13.488 13.669 DA1.2 312 0
6 NGC 5548 Sy1 14 17 59.5401093128 +25 08 12.600227883   14.35 13.73     ~ 2391 0
7 Mrk 841 Sy1 15 04 01.1935077982 +10 26 15.778741853   14.50 14.27     ~ 583 0
8 V* V381 Nor HXB 15 50 58.6520652623 -56 28 35.309070422   17.95 16.6     K3III 1021 0
9 Granat 1915+105 LXB 19 15 11.54938 +10 56 44.7585           ~ 2281 0
10 Mrk 509 Sy1 20 44 09.7504131334 -10 43 24.724854084   13.35 13.12 10.7   ~ 1128 0
11 NGC 7469 Sy1 23 03 15.674 +08 52 25.28 12.60 13.00 12.34     ~ 1885 3

    Equat.    Gal    SGal    Ecl

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2020.07.02-15:20:47

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