2022A&A...657A.122K


Query : 2022A&A...657A.122K

2022A&A...657A.122K - Astronomy and Astrophysics, volume 657A, 122-122 (2022/1-1)

The Great Slump: Mrk 926 reveals discrete and varying Balmer line satellite components during a drastic phase of decline.

KOLLATSCHNY W., OCHMANN M.W., KASPI S., SCHUMACHER C., BEHAR E., CHELOUCHE D., HORNE K., MULLER B., RAFTER S.E., CHINI R., HAAS M. and PROBST M.A.

Abstract (from CDS):


Aims. Mrk 926 is known to be a highly variable active galactic nucleus. Furthermore, it is known to show very broad line profiles. We intended to study the continuum and line profile variations of this object with high temporal resolution in order to determine its broad-line region structure and to derive its black hole mass.
Methods. We carried out a high-cadence spectroscopic variability campaign of Mrk 926 with the 10m HET telescope, aided by photometric V-band data taken with the C18 telescope at the Wise Observatory, over a period of about five months. We extracted spectroscopic continuum and line light curves, and computed cross-correlation functions (CCFs) as well as velocity-resolved CCFs with respect to the combined spectroscopic and photometric V-band light curve.
Results. The continuum luminosity of Mrk 926 showed a drastic decrease during our campaign. The luminosity dropped to less than 50% of its original luminosity within only 2.5 months. Furthermore, the spectra of Mrk 926 show complex and very broad Balmer line profiles, including outer Balmer satellites ranging from ±5000 to ±13 000 km/s. The integrated Hα, Hβ, and HeIλ5876 line light curves are delayed relative to the continuum light curve. The Hα and Hβ lines show two velocity-delay structures in the central part of their line profile (within ±5000 km/s), at ∼10 and ∼57 light-days and at ∼5 and ∼48 light-days, respectively. These structures might be interpreted as the upper and lower halves of an ellipse in the velocity-delay plane, which might be the signature of a line-emitting ring, inclined by ∼50° to the line of sight and orbiting the black hole at radii, R, of 33.5 and 26.5 light-days. We determined continuum luminosities, log(λLλ/(erg/s)), of 43.68-44.13, which are in good agreement with the established RBLR - LAGN relation. Adopting delays of 33.5 and 26.5 days for Hα and Hβ, respectively, we derive a black hole mass of (1.1 ±0.2)x108 M; this indicates a low Eddington ratio, which decreased from 8 to 3 percent during our campaign. The Balmer satellite components show a higher correlation coefficient with respect to the continuum than the central line profile, and their response to the continuum variations is on the order of only 3 - 5 days. We attribute this to the central line segment and the Balmer satellites having different, spatially distinct regions of origin.

Abstract Copyright: © ESO 2022

Journal keyword(s): galaxies: active - galaxies: Seyfert - galaxies: nuclei - galaxies: individual: Mrk926 - quasars: emission lines

VizieR on-line data: <Available at CDS (J/A+A/657/A122): wisevmod.dat list.dat fits/*>

Simbad objects: 23

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Number of rows : 23
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 Mrk 335 Sy1 00 06 19.5372339024 +20 12 10.617404076   14.19 13.85     ~ 1203 0
2 Mrk 1501 Sy1 00 10 31.00590413 +10 58 29.5042981   15.96 15.40 12.22   ~ 689 0
3 ESO 113-45 Sy1 01 23 45.7631533440 -58 48 20.808928944   14.08 13.83 13.34   ~ 835 0
4 Mrk 1044 Sy1 02 30 05.5225590096 -08 59 53.207139372   14.74 14.29 13.981 13.585 ~ 261 0
5 Mrk 1506 Sy1 04 33 11.0956735296 +05 21 15.619461552   15.72 15.05 10.08   ~ 1947 2
6 Mrk 1095 Sy1 05 16 11.4092471904 -00 08 59.157166920   14.30 13.92     ~ 848 1
7 HD 289002 * 06 45 13.3725491952 +02 08 14.685250596 10.06 10.62 10.44     B1 248 0
8 TYC 5392-2148-1 Em* 06 57 17.9770922520 -14 05 26.598368436   11.59 11.12     ~ 10 0
9 Mrk 110 Sy1 09 25 12.8479065576 +52 17 10.386311208   16.82 16.41     ~ 566 0
10 Mrk 142 Sy1 10 25 31.2786898344 +51 40 34.867889004   16.33 16.12     ~ 268 0
11 Mrk 40 Sy1 11 25 36.1539761184 +54 22 57.113791824   17.06 16.47     ~ 252 0
12 2MASX J11385104-2321353 SyG 11 38 51.0052630080 -23 21 35.346868704   17.4       ~ 42 0
13 NGC 4593 Sy1 12 39 39.4435107024 -05 20 39.034988448   13.95 13.15     ~ 1041 0
14 NGC 5548 Sy1 14 17 59.5400291832 +25 08 12.603122268   14.35 13.73     ~ 2589 0
15 3C 332.0 Sy1 16 17 42.5380089648 +32 22 34.372277976   18.25 17.45     ~ 245 1
16 ICRF J171914.4+485849 Sy1 17 19 14.4925971408 +48 58 49.423205136   15.86 14.81 9.44   ~ 303 1
17 ICRF J183503.3+324146 Sy1 18 35 03.3896172576 +32 41 46.855964616   16.50 15.39 10.50   ~ 620 1
18 ICRF J184208.9+794617 Sy1 18 42 08.9904975672 +79 46 17.127835104   16.06 15.38     ~ 1275 0
19 Mrk 1513 Sy1 21 32 27.8162556672 +10 08 19.252365396   14.92 14.64     ~ 580 0
20 Mrk 926 Sy1 23 04 43.4776098480 -08 41 08.629476864   16.20 15.91 9.4   ~ 433 0
21 2MASX J23044397-0842114 AGN 23 04 43.9816590792 -08 42 11.603475540   16.58   15.27   ~ 9 0
22 NGC 7603 Sy1 23 18 56.6538277656 +00 14 37.977066096   14.73 14.01     ~ 384 0
23 2MASX J23252420-3826492 Sy1 23 25 24.1886501280 -38 26 49.177796028   14.84 14.24     ~ 60 0

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2023.01.27-19:14:11

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