# 2007A&A...466...23P

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 Query : 2007A&A...466...23P

2007A&A...466...23P - Astronomy and Astrophysics, volume 466, 23-30 (2007/4-4)

An XMM-Newton view of the X-ray flat radio-quiet quasar PG1416-129.

PORQUET D., REEVES J.N., MARKOWITZ A., TURNER T.J., MILLER L. and NANDRA K.

Abstract (from CDS):

The radio-quiet quasar PG1416-129 (z=0.129) exhibits atypical optical and X-ray properties. Between 1990 and 2000, in response to its optical continuum decrease, the classical'' broad component of Hβ almost completely disappeared, with a factor of 10 decrease in the line flux. In addition, the width of the broad component of the Hβ line decreased significantly from 4000km/s to 1450km/s. In the X-ray band, this object was observed by Ginga in 1988 to have the hardest quasar photon index, with Γ=1.1 ±0.1. We present an XMM-Newton/EPIC observation of PG1416-129 performed in July 2004. We analyze the time-averaged pn spectrum of this quasar, as well as perform time-resolved spectroscopy. We find that during the present XMM-Newton observation, PG1416-129 still has a rather hard photon index, both in the soft (0.2-2keV) and hard (2-12keV) energy ranges, compared to radio-quiet quasars (BLS1 and NLS1) but compatible with the photon index value found for radio-loud quasars. This object also shows long-term luminosity variability over 16 years by a factor of three with a variation of photon index from ∼1.2 to ∼1.8. In the soft energy band (0.2-2keV), we found a very weak soft X-ray excess compared to other RQ quasars. The whole time averaged spectrum is fit very well either by X-ray ionized reflection from the accretion disk surface, by a warm absorber-emitter plus power-law, or by a smeared absorption/emission from a relativistic outflow. While no constant narrow FeK line at 6.4keV is observed, we find the possible presence of two non-simultaneous transient iron lines: a redshifted narrow iron line at about 5.5keV (96.4% confidence level according to multi-trial Monte-Carlo simulations) at the beginning of this observation and the appearance of a line at 6.3-6.4keV (99.1% c.l.) at the end of the observation. These variable lines could be generated by discrete hot-spots on the accretion disk surface.

Journal keyword(s): galaxies: active - X-rays: galaxies - accretion, accretion discs - quasars: individual: PG 1416-129

Full paper

 Number of rows : 8
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 ESO 113-10 Sy1 01 05 16.8746925168 -58 26 15.260456148   14.63 14.6 13.35   ~ 59 0
2 Mrk 359 Sy1 01 27 32.5217343720 +19 10 43.839069600   14.89 14.22     ~ 295 0
3 2MASS J04474860-0628131 AGN 04 47 48.6206159976 -06 28 13.067923584   18.4       ~ 12 0
4 LEDA 88588 Sy1 07 08 41.4886614696 -49 33 06.308921700   16.02 15.7 12.7   ~ 488 0
5 NGC 3516 Sy1 11 06 47.4632200800 +72 34 07.298374656   13.12 12.40     ~ 1497 0
6 NGC 4253 Sy1 12 18 26.5163572920 +29 48 46.531535472   14.34 13.57     ~ 1010 1
7 NAME OKM2018 SWIFT J1419.0-1323 Sy1 14 19 03.8170514760 -13 10 44.785212600   16.46 16.10 16.50   ~ 229 0
8 Ton 202 Sy1 14 27 35.6076948744 +26 32 14.541190476   15.96 16.00     ~ 290 1

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2023.02.08-12:27:59