2010A&A...512A..75S


C.D.S. - SIMBAD4 rel 1.7 - 2019.09.17CEST13:31:24

2010A&A...512A..75S - Astronomy and Astrophysics, volume 512, A75-75 (2010/3-1)

A long hard look at the minimum state of PG 2112+059 with XMM-Newton.

SCHARTEL N., RODRIGUEZ-PASCUAL P.M., SANTOS-LLEO M., JIMENEZ-BAILON E., BALLO L. and PICONCELLI E.

Abstract (from CDS):

Our observational aim is to perform a long X-ray observation of the quasar PG 2112+059 in its low or minimum state. Starting form this very peculiar emission state, we intend to constrain the intrinsic emission mechanism by comparing new and old data, corresponding to different source states. XMM-Newton successfully detected the minimum state of PG 2112+059 during a short snapshot observation and performed a long follow-up observation. The high signal-to-noise spectra are modelled assuming different emission scenarios and compared with archival spectra taken by XMM-Newton and Chandra. The PG 2112+059 X-ray spectra acquired in May 2007 allowed the detection of a weak iron fluorescent line, which is interpreted as being caused by reflection from neutral material at some distance from the primary X-ray emitting source. The X-ray spectra of PG 2112+059 taken at five different epochs during different flux states can be interpreted within two different scenarios. The first consists of two layers of ionised material with column densities of NH∼5x1022cm–2 and NH∼3.5x1023cm–2, respectively. The first layer is moderately ionised and its ionisation levels follow the flux changes, while the other layer is highly ionised and does not show any correlation with the flux of the source. The spectra can also be interpreted assuming reflection by an ionised accretion disk seen behind a warm absorber. The warm absorber ionisation is consistent with being correlated with the flux of the source, which provides an additional degree of self-consistency with the overall reflection-based model. We explain the spectral variability with light bending according to the models of Miniutti and Fabian and constrain the black hole spin to be a/M>0.86. Both scenarios also assume that a distant cold reflector is responsible for the FeK α emission line. Light bending provides an attractive explanation of the different states of PG 2112+059 and may also describe the physical cause of the observed properties of other X-ray weak quasars. The observations of PG 2112+059 in different states provide valuable constraints, although are unable to break the degeneracy between complex absorption scenarios and reflection from an ionised disk.

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Journal keyword(s): galaxies: active - quasars: individual: PG 2112+059

Simbad objects: 9

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Number of rows : 9

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 Mrk 335 Sy1 00 06 19.5371542746 +20 12 10.617456059   14.19 13.85     ~ 1053 0
2 3XMM J003915.8-511701 Sy1 00 39 15.8341273306 -51 17 01.480962252   15.77 15.28 15.66   ~ 116 0
3 2XMM J013955.7+061922 Sy1 01 39 55.7698488494 +06 19 22.518916337   16.80 17.00     ~ 151 0
4 NGC 1365 Sy1 03 33 36.458 -36 08 26.37 10.48 10.08 9.63 8.79 9.7 ~ 1464 2
5 4U 0708-49 Sy1 07 08 41.4887418009 -49 33 06.308287663   16.02 15.7 12.7   ~ 410 0
6 Mrk 486 Sy1 15 36 38.4013129866 +54 33 33.214684833   15.21 14.78     ~ 242 0
7 QSO B1544+4855 Sy1 15 45 30.2362003284 +48 46 08.978296070   16.92 16.73     ~ 212 0
8 2MASS J21145258+0607423 Sy1 21 14 52.5774242314 +06 07 42.435724828   16.06 15.77     ~ 195 0
9 QSO J2155-0922 Sy1 21 55 01.5123415724 -09 22 24.351917710   13.9 16.8 14.1   ~ 152 0

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2019.09.17-13:31:24

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