2006A&A...456...75C


Query : 2006A&A...456...75C

2006A&A...456...75C - Astronomy and Astrophysics, volume 456, 75-90 (2006/9-2)

Systematic effects in measurement of black hole masses. by emission-line reverberation of active galactic nuclei: Eddington ratio and inclination.

COLLIN S., KAWAGUCHI T., PETERSON B.M. and VESTERGAARD M.

Abstract (from CDS):

Scatter around the relationship between central black hole masses in active galactic nuclei (AGNs) obtained by reverberation-mapping methods and host-galaxy bulge velocity dispersion indicates that the masses are uncertain typically by a factor of about three. In this paper, we try to identify the sources and systematics of this uncertainty. We characterize the broad Hβ emission-line profiles by the ratio of their full-width at half maximum (FWHM) to their line dispersion, i.e., the second moment of the line profile. We use this parameter to separate the reverberation-mapped AGNs into two populations, the first with narrower Hβ lines that tend to have relatively extended wings, and the second with broader lines that are relatively flat-topped. The first population is characterized by higher Eddington ratios than the second. Within each population, we calibrate the black-hole mass scale by comparison of the reverberation-based mass with that predicted by the bulge velocity dispersion. We also use the distribution of ratios of the reverberation-based mass to the velocity-dispersion mass prediction in a comparison with a ``generalized thick disk'' model in order to see if inclination can plausibly account for the observed distribution. We find that the line dispersion is a less biased parameter in general than FWHM for black hole mass estimation, although we show that it is possible to empirically correct for the bias introduced by using FWHM to characterize the emission-line width. We also argue that inclination effects are apparent only in some small subset of the reverberation-based mass measurements; it is primarily the objects with the narrowest emission lines that seem to be most strongly affected. Our principal conclusion is that the Hβ profile is sensitive primarily to Eddington ratio, but that inclination effects play a role in some cases.

Abstract Copyright:

Journal keyword(s): galaxies: quasars: general - galaxies: nuclei - galaxies: Seyfert

Simbad objects: 34

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Number of rows : 34
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 Mrk 335 Sy1 00 06 19.5372339024 +20 12 10.617404076   14.19 13.85     ~ 1255 0
2 LEDA 1790 Sy1 00 29 13.7012449608 +13 16 03.947778264   15.70 15.41     ~ 446 0
3 LEDA 3237 Sy1 00 54 52.1183662680 +25 25 38.983241532     15.42     ~ 389 0
4 ESO 113-45 Sy1 01 23 45.7631533440 -58 48 20.808928944   14.08 13.83 13.34   ~ 882 0
5 NGC 863 Sy1 02 14 33.5604714720 -00 46 00.181845336   14.48 13.81 17.9   ~ 693 0
6 Mrk 1506 Sy1 04 33 11.0956735296 +05 21 15.619461552   15.72 15.05 10.08   ~ 2002 2
7 Mrk 1095 Sy1 05 16 11.4092471904 -00 08 59.157166920   14.30 13.92     ~ 891 1
8 Mrk 79 Sy1 07 42 32.8210670808 +49 48 34.783809768   14.74 14.27     ~ 714 1
9 2MASS J08105865+7602424 Sy1 08 10 58.6641543864 +76 02 42.450451260   15.03 14.71     ~ 471 0
10 Ton 951 Sy1 08 47 42.4485615096 +34 45 04.482515304   14.83 14.50     ~ 467 0
11 Mrk 110 Sy1 09 25 12.8479065576 +52 17 10.386311208   16.82 16.41     ~ 607 0
12 PG 0953+414 Sy1 09 56 52.3931554992 +41 15 22.211247636 14.710 15.611 15.546 15.294 14.720 ~ 454 0
13 NGC 3227 Sy1 10 23 30.5765149296 +19 51 54.282206700   12.61 11.79     ~ 1709 1
14 NGC 3516 Sy1 11 06 47.4632200800 +72 34 07.298374656   13.12 12.40     ~ 1545 0
15 NGC 3783 Sy1 11 39 01.7096819040 -37 44 19.009642992   12.46 13.43 11.33 12.1 ~ 1651 0
16 NGC 4051 Sy1 12 03 09.6101337312 +44 31 52.682601288   11.08 12.92 9.94   ~ 2167 1
17 NGC 4151 Sy1 12 10 32.5759813872 +39 24 21.063527532   12.18 11.48     ~ 3698 2
18 PB 3894 Sy1 12 14 17.6738687784 +14 03 13.182723144   14.46 14.19     ~ 823 0
19 3C 273 BLL 12 29 06.6998257176 +02 03 08.597629980   13.05 14.830 14.11   ~ 5811 1
20 NGC 4593 Sy1 12 39 39.4435107024 -05 20 39.034988448   13.95 13.15     ~ 1091 0
21 LEDA 45656 Sy1 13 09 47.0031619008 +08 19 48.212362524   16.04 15.89     ~ 391 0
22 ESO 445-50 Sy1 13 49 19.2601801224 -30 18 34.213815504   13.81 13.66 12.18 12.35 ~ 807 0
23 Mrk 279 Sy1 13 53 03.4348964112 +69 18 29.410910460   15.15 14.46     ~ 762 0
24 LEDA 50824 Sy1 14 13 48.3306274368 +44 00 14.003371296   14.99 14.99     ~ 385 0
25 NGC 5548 Sy1 14 17 59.5400291832 +25 08 12.603122268   14.35 13.73     ~ 2716 0
26 Mrk 1383 Sy1 14 29 06.5720038632 +01 17 06.155007252   15.21 14.87     ~ 463 0
27 Mrk 817 Sy1 14 36 22.0820611632 +58 47 39.394934844   14.19 13.79     ~ 523 0
28 Mrk 876 Sy1 16 13 57.1795021224 +65 43 09.952685328   16.03 15.49     ~ 584 0
29 Mrk 877 Sy1 16 20 11.2799789400 +17 24 27.515242152   15.79 15.39     ~ 273 0
30 IRAS 17002+5153 Sy1 17 01 24.8265469104 +51 49 20.447878836   15.49 15.12     ~ 386 0
31 ICRF J184208.9+794617 Sy1 18 42 08.9904975672 +79 46 17.127835104   16.06 15.38     ~ 1317 0
32 Mrk 509 Sy1 20 44 09.7504483224 -10 43 24.727155528   13.35 13.12 10.7   ~ 1279 0
33 Mrk 1513 Sy1 21 32 27.8162556672 +10 08 19.252365396   14.92 14.64     ~ 614 0
34 NGC 7469 Sy1 23 03 15.6 +08 52 26 12.60 13.00 12.34     ~ 2101 3

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