2009MNRAS.399.1553V


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.31CET12:28:03

2009MNRAS.399.1553V - Mon. Not. R. Astron. Soc., 399, 1553-1575 (2009/November-1)

Optical-to-X-ray emission in low-absorption AGN: results from the Swift-BAT 9-month catalogue.

VASUDEVAN R.V., MUSHOTZKY R.F., WINTER L.M. and FABIAN A.C.

Abstract (from CDS):

We present simultaneous optical-to-X-ray spectral energy distributions (SEDs) from Swift's X-ray and UV-optical telescopes (XRTs and UVOTs) for a well-selected sample of 26 low-redshift (z < 0.1) active galactic nuclei (AGN) from the Swift/Burst Alert Telescope 9-month catalogue, the largest well-studied, hard X-ray-selected survey of local AGN to date. Our sub-sample consists of AGN with low intrinsic X-ray absorption (NH< 1022/cm2) and minimal spectral complexity, to more accurately recover the intrinsic accretion luminosity in these sources. We perform a correction for host galaxy contamination in all available UVOT filter images to recover the intrinsic AGN emission and estimate intrinsic dust extinction from the resultant nuclear SEDs. Black hole mass estimates are determined from the host galaxy Two-Micron All-Sky Survey K-band bulge luminosity. Accretion rates determined from our SEDs are on average low (Eddington ratios λEdd≲ 0.1) and hard X-ray bolometric corrections cluster at ∼10-20, in contrast with the higher values seen for quasars. An average SED for the 22 low accretion rate (λEdd< 0.1) objects is presented, with and without correction for extinction. Significant dust reddening is found in some objects despite the selection of low NHobjects, emphasizing the complex relationship between these two types of absorption. We do not find a correlation of the optical-to-X-ray spectral index with the Eddington ratio, regardless of the optical reference wavelength chosen for defining the spectral index. An anticorrelation of bolometric correction with black hole mass may reinforce `cosmic downsizing' scenarios, since the higher bolometric corrections at low mass would boost accretion rates in local, lower mass black holes. We also perform a basic analysis of the UVOT-derived host galaxy colours for our sample and find hosts cluster near the `green valley' of the colour-magnitude diagram, but better quality images are needed for a more definitive analysis. The low accretion rates and bolometric corrections found for this representative low-redshift sample are of particular importance for studies of AGN accretion history.

Abstract Copyright: © 2009 The Authors. Journal compilation © 2009 RAS

Journal keyword(s): black hole physics - galaxies: active - galaxies: Seyfert

Simbad objects: 36

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Number of rows : 36

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 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9566 1
2 Mrk 352 Sy1 00 59 53.2853410350 +31 49 37.252347536   15.25 14.81     ~ 193 0
3 Mrk 1018 Sy1 02 06 15.9897977200 -00 17 29.219372130   15.90 15.50 10.3   ~ 248 0
4 2MASS J02093740+5226396 Sy1 02 09 37.4068484247 +52 26 39.659946835     14.9     ~ 40 0
5 NGC 863 Sy1 02 14 33.5610949475 -00 46 00.180128181   14.48 13.81 17.9   ~ 581 0
6 NGC 985 Sy1 02 34 37.882 -08 47 17.02   14.64 14.28 12.9   ~ 348 0
7 NAME Extended Chandra Deep Field South reg 03 32 30.0 -27 48 20           ~ 623 0
8 ESO 548-81 Sy1 03 42 03.7180399342 -21 14 39.646540303   12.84 13.68 11.57   ~ 101 0
9 Mrk 1506 Sy1 04 33 11.0958197353 +05 21 15.617543663   15.72 15.05 10.08   ~ 1856 2
10 2MASX J04520479+4932446 Sy1 04 52 04.7737592166 +49 32 44.738797125     17.1     ~ 56 0
11 Mrk 1095 Sy1 05 16 11.4093760763 -00 08 59.158774578   14.30 13.92     ~ 787 1
12 QSO B0521-365 BLL 05 22 57.9839686440 -36 27 30.847737786   15.26 14.62 14.48   ~ 723 2
13 QSO B0548-322 BLL 05 50 40.5706739558 -32 16 16.488658537   16.07 15.5     ~ 369 1
14 RX J0602.1+2828 Sy1 06 02 10.4708588399 +28 28 19.409846103   15.0       ~ 56 0
15 ESO 490-26 Sy1 06 40 11.6917875755 -25 53 43.063876738   14.08   12.60   ~ 63 0
16 2MASS J07594181-3843560 Sy1 07 59 41.8249712970 -38 43 56.041977918           ~ 51 0
17 [VV96] J091609.5-621929 Sy1 09 16 09.3662174299 -62 19 29.559790552   12.51 12.26 11.5   ~ 105 0
18 MCG+04-22-042 Sy1 09 23 43.0006235873 +22 54 32.569231798   16.23 15.82     ~ 103 0
19 2MASX J11390898+5911547 Sy1 11 39 08.9706766632 +59 11 54.771163685   15.88 15.77     ~ 69 0
20 UGC 6728 Sy1 11 45 15.9440557865 +79 40 53.378480801   14.8 15.2     ~ 83 0
21 NGC 4253 Sy1 12 18 26.5155239433 +29 48 46.518670434   14.34 13.57     ~ 938 1
22 3C 273 BLL 12 29 06.6996828061 +02 03 08.598846466   13.05 14.830 14.11   ~ 5352 1
23 NGC 4593 Sy1 12 39 39.4435521178 -05 20 39.035028119   13.95 13.15     ~ 959 0
24 2MASX J12412572-5750038 Sy2 12 41 25.7672413457 -57 50 03.481040498   17.4 16.9     ~ 62 0
25 MCG+09-21-096 Sy1 13 03 59.4958127580 +53 47 29.917551961   17   12.9   ~ 53 0
26 ESO 383-35 Sy1 13 35 53.7686909139 -34 17 44.139127597   13.89 13.61 8.9   ~ 1386 0
27 Mrk 279 Sy1 13 53 03.4356451470 +69 18 29.410672989   15.15 14.46     ~ 697 0
28 NGC 5548 Sy1 14 17 59.5401093128 +25 08 12.600227883   14.35 13.73     ~ 2416 0
29 Mrk 841 Sy1 15 04 01.1935077982 +10 26 15.778741853   14.50 14.27     ~ 587 0
30 4C 39.49 BLL 16 53 52.21668494 +39 45 36.6089458 14.09 14.15 13.29 8.26   ~ 1936 2
31 ICRF J184208.9+794617 Sy1 18 42 08.9910523393 +79 46 17.129210139   16.06 15.38     ~ 1218 0
32 QSO B1959+650 BLL 19 59 59.8525497024 +65 08 54.651170114     12.8 11.21   ~ 509 2
33 Mrk 509 Sy1 20 44 09.7504131334 -10 43 24.724854084   13.35 13.12 10.7   ~ 1135 0
34 2MAXI J2115+821 Sy1 21 14 01.1716311384 +82 04 48.338015583           ~ 107 1
35 IRAS 21262+5643 Sy1 21 27 45.3943647524 +56 56 34.913660916       16.6   ~ 130 0
36 NGC 7469 Sy1 23 03 15.674 +08 52 25.28 12.60 13.00 12.34     ~ 1903 3

    Equat.    Gal    SGal    Ecl

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2020.10.31-12:28:03

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