2012A&A...547A..31G


C.D.S. - SIMBAD4 rel 1.7 - 2020.01.19CET13:43:36

2012A&A...547A..31G - Astronomy and Astrophysics, volume 547A, 31-31 (2012/11-1)

The X-ray variability history of Markarian 3.

GUAINAZZI M., LA PAROLA V., MINIUTTI G., SEGRETO A. and LONGINOTTI A.L.

Abstract (from CDS):

The unified scenario for active galactic nuclei (AGN) postulates that our orientation with respect to a parsec-scale azimuthally-symmetric gas and dust system causes the difference in their phenomenology in the optical/UV and X-ray bands. Only recently have high-resolution radio (VLBI) and IR interferometric observations provided direct constraints on the size and structure of this obscuring system (known historically as the ``torus''). On the other hand, variability in optically-thick X-ray absorption and reprocessing in heavily obscured AGN often probe smaller scales, down to the broad line region and beyond. We aim at constraining the geometry of the reprocessing matter in the nearby prototypical Seyfert 2 Galaxy Markarian 3 by studying the time evolution of the spectral components associated to the primary AGN emission and to its Compton-scattering. We analyzed archival spectroscopic observations of Markarian 3 taken over the last ≃12 years with the XMM-Newton, Suzaku and Swift observatories, as well as data taken during a monitoring campaign activated by us in 2012. The timescale of the Compton-reflection component variability (originally discovered by ASCA in the mid-'90s) is ≲64 days. This upper limit improves by more than a factor of 15 on previous estimates of the Compton-reflection variability timescale for this source. When the light curve of the Compton-reflection continuum in the 4-5keV band is correlated with the 15-150 keV Swift/BAT curve, a delay >1200 days is found. The cross-correlation results depend on the model used to fit the spectra, although the detection of the Compton-reflection component variability is independent of the range of models employed to fit the data. Reanalysis of an archival Chandra image of Markarian 3 indicates that the Compton-reflection and the Fe Kα emitting regions are extended to the north up to ≃300pc. The combination of these findings suggests that the optically-thick reprocessor in Markarian 3 is clumpy. There is mounting experimental evidence that the structure of the optically-thick gas and dust in the nuclear environment of nearby heavily obscured AGN is extended and complex. We discuss possible modifications to the standard unification scenarios encompassing this complexity. Markarian 3, which exhibits X-ray absorption and reprocessing on widely different spatial scales, is an ideal laboratory to test these models.

Abstract Copyright:

Journal keyword(s): galaxies: active - galaxies: nuclei - galaxies: Seyfert - galaxies: groups: individual: Markarian 3 - X-rays: galaxies

Simbad objects: 11

goto Full paper

goto View the reference in ADS

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 NGC 449 Sy2 01 16 07.2096682810 +33 05 21.651153340   15.90 14.96     ~ 265 4
2 Mrk 573 Sy2 01 43 57.7763654544 +02 20 59.525472345   14.90 14.07     ~ 471 0
3 M 77 GiP 02 42 40.771 -00 00 47.84 9.70 9.61 8.87 10.1 9.9 ~ 4016 2
4 2XMM J061515.0+710203 AGN 06 15 15.1 +71 02 03           ~ 13 1
5 Mrk 3 Sy2 06 15 36.458 +71 02 15.24 14.21 14.03 12.97     ~ 831 3
6 NGC 2992 Sy2 09 45 42.045 -14 19 34.90 13.54 13.14 12.18 12.6 12.2 ~ 772 3
7 NGC 4151 Sy1 12 10 32.5771747733 +39 24 21.057727323   12.18 11.48     ~ 3333 2
8 NGC 4945 Sy2 13 05 27.279 -49 28 04.44   9.31 14.40 7.55   ~ 1236 2
9 NAME Circinus Galaxy Sy2 14 13 09.906 -65 20 20.47   10.89 9.84 10.6 10.0 ~ 979 2
10 NGC 5506 AGN 14 13 14.901 -03 12 27.22   15.25 14.38     ~ 975 0
11 NGC 7213 Sy1 22 09 16.2106632887 -47 10 00.082166299   10.97 12.08 10.50 10.6 ~ 578 0

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2012A&A...547A..31G and select 'bookmark this link' or equivalent in the popup menu


2020.01.19-13:43:36

© Université de Strasbourg/CNRS

    • Contact