2020A&A...634A.114C

Query : 2020A&A...634A.114C

2020A&A...634A.114C - Astronomy and Astrophysics, volume 634A114-114 (2020/2-1)

LLAMA: The MBH-σ relation of the most luminous local AGNs.

CAGLAR T., BURTSCHER L., BRANDL B., BRINCHMANN J., DAVIES R.I., HICKS E.K.S., KOSS M., LIN M.-Y., MACIEJEWSKI W., MULLER-SANCHEZ F., RIFFEL R.A., RIFFEL R., ROSARIO D.J., SCHARTMANN M., SCHNORR-MULLER A., SHIMIZU T.T., STORCHI-BERGMANN T., VEILLEUX S., DE XIVRY G.O. and BENNERT V.N.

Abstract (from CDS):

Context. The MBH-σ* relation is considered a result of coevolution between the host galaxies and their supermassive black holes. For elliptical bulge hosting inactive galaxies, this relation is well established, but there is still discussion concerning whether active galaxies follow the same relation. Aims. In this paper, we estimate black hole masses for a sample of 19 local luminous active galactic nuclei (AGNs; LLAMA) to test their location on the MBH-σ* relation. In addition, we test how robustly we can determine the stellar velocity dispersion in the presence of an AGN continuum and AGN emission lines, and as a function of signal-to-noise ratio. Methods. Supermassive black hole masses (MBH) were derived from the broad-line-based relations for Hα, Hβ, and Paβ emission line profiles for Type 1 AGNs. We compared the bulge stellar velocity dispersion (σ*) as determined from the Ca II triplet (CaT) with the dispersion measured from the near-infrared CO (2-0) absorption features for each AGN and find them to be consistent with each other. We applied an extinction correction to the observed broad-line fluxes and we corrected the stellar velocity dispersion by an average rotation contribution as determined from spatially resolved stellar kinematic maps. Results. The Hα-based black hole masses of our sample of AGNs were estimated in the range 6.34≤logMBH≤7.75M☉ and the σ*CaT estimates range between 73≤σ*CaT≤227km/s. From the so-constructed MBH-σ* relation for our Type 1 AGNs, we estimate the black hole masses for the Type 2 AGNs and the inactive galaxies in our sample.Conclusions. We find that our sample of local luminous AGNs is consistent with the MBH-σ* relation of lower luminosity AGNs and inactive galaxies, after correcting for dust extinction and the rotational contribution to the stellar velocity dispersion.

Abstract Copyright: © ESO 2020

Journal keyword(s): accretion - accretion disks - black hole physics - galaxies: active - galaxies: bulges - galaxies: evolution - galaxies: Seyfert

Simbad objects: 40

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Number of rows : 40
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 NGC 718 GiC 01 53 13.2842245224 +04 11 44.843164296   12.52 11.67 11.10 10.29 ~ 165 0
2 NGC 1079 Sy2 02 43 44.3354434608 -29 00 11.748886668   12.17 11.37 10.86 11.5 ~ 146 0
3 NGC 1315 GiP 03 23 06.5986714536 -21 22 30.696768948   13.46   12.23   ~ 55 0
4 NGC 1365 Sy1 03 33 36.458 -36 08 26.37 10.48 10.08 9.63 8.79 9.7 ~ 1987 2
5 NGC 1947 GiG 05 26 47.613 -63 45 36.08   11.76 10.80 10.06   ~ 141 0
6 MCG-05-14-012 Sy2 05 43 32.9579928216 -27 39 05.070354192   14.28   13.14 13.8 ~ 54 0
7 NGC 2110 Sy2 05 52 11.3768668776 -07 27 22.507465392   14.77 13.51 11.86   ~ 712 1
8 ESO 208-21 GiG 07 33 56.2880839056 -50 26 35.057648832   12.01   10.39   ~ 82 0
9 NGC 2775 AG? 09 10 20.1334093488 +07 02 16.874157048   11.417 10.481 9.920 8.994 ~ 377 0
10 NGC 2992 Sy2 09 45 42.045 -14 19 34.90 13.54 13.14 12.18 12.6 12.2 ~ 951 3
11 MCG-05-23-016 Sy2 09 47 40.1332188528 -30 56 55.960779696   14.10 13.69 12.44   ~ 611 0
12 NGC 3081 Sy2 09 59 29.5437024336 -22 49 34.747341960   13.06 13.55 11.67 12.1 ~ 509 0
13 NGC 3175 EmG 10 14 42.1304335632 -28 52 19.628995332   12.14   11.7 11.2 ~ 110 0
14 M 95 GiP 10 43 57.7313485800 +11 42 13.301191332 10.71 10.51 9.73 9.48   ~ 1238 2
15 ESO 93-3 AG? 10 59 26.0621043696 -66 19 58.317477456   13.9   13.4 12.9 ~ 41 0
16 NGC 3717 EmG 11 31 31.992 -30 18 27.86   12.21   10.56 11.0 ~ 107 1
17 NGC 3749 EmG 11 35 53.203 -37 59 50.39   13.22   11.54 12.3 ~ 54 1
18 NGC 3783 Sy1 11 39 01.7096819040 -37 44 19.009642992   12.46 13.43 11.33 12.1 ~ 1765 1
19 NGC 4224 GiG 12 16 33.7856435496 +07 27 43.527631068   13.3       ~ 167 0
20 NGC 4235 Sy1 12 17 09.8818997904 +07 11 29.673389004   14.70 13.60     ~ 441 0
21 M 99 H2G 12 18 49.625 +14 24 59.36 10.45 10.44 9.87     ~ 1004 2
22 NGC 4260 GiP 12 19 22.2401274336 +06 05 55.291593192   13.1       ~ 174 0
23 NGC 4388 Sy2 12 25 46.820 +12 39 43.45 11.91 11.76 11.02     ~ 1433 2
24 3C 273 BLL 12 29 06.6998257176 +02 03 08.597629980   13.05 14.830 14.11   ~ 6022 1
25 NGC 4593 Sy1 12 39 39.4435107024 -05 20 39.034988448   13.95 13.15     ~ 1179 0
26 NGC 5037 GiP 13 14 59.381 -16 35 25.16   13.0   11.78   ~ 67 0
27 NAME Centaurus A BLL 13 25 27.61521044 -43 01 08.8050291   8.18 6.84 6.66   ~ 4774 3
28 ESO 21-4 Sy2 13 32 40.5938806776 -77 50 40.532334072   12.7   12.8 12.2 ~ 49 0
29 MCG-06-30-015 Sy1 13 35 53.7691256160 -34 17 44.160716796   13.89 13.61 8.9   ~ 1559 0
30 NGC 5506 Bla 14 13 14.8761010056 -03 12 27.556909272   15.25 14.38     ~ 1173 1
31 NGC 5728 Sy2 14 42 23.8918506576 -17 15 11.240783784   14.34 13.40     ~ 679 1
32 NGC 5845 GiG 15 06 00.7823239488 +01 38 01.704838596   13.8 11.20 12.06 9.94 ~ 403 0
33 NGC 5921 AG? 15 21 56.561 +05 04 13.94   12.7       ~ 286 0
34 ESO 137-34 Sy2 16 35 14.114 -58 04 48.10   12.20   10.84 11.6 ~ 165 0
35 IC 4653 AG? 17 27 06.9284687544 -60 52 44.153863320   13.25   12.00   ~ 34 0
36 NGC 6814 Sy1 19 42 40.5862186152 -10 19 25.108718844   15.33 14.21 11.7 11.3 ~ 866 0
37 NGC 7172 Sy2 22 02 01.897 -31 52 11.60   12.72 13.61 11.15 25.10 ~ 572 2
38 NGC 7213 Bla 22 09 16.2100443720 -47 10 00.115999716   10.97 12.08 10.50 10.6 ~ 700 1
39 NGC 7582 Sy2 23 18 23.60 -42 22 13.3 11.62 10.92 10.62     ~ 978 3
40 NGC 7727 EmG 23 39 53.870 -12 17 34.84   11   10.55   ~ 183 0

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