J/ApJ/905/77 Monitoring AGNs with Hβ Asymmetry. II. (Brotherton+, 2020)
Monitoring AGNs with Hβ Asymmetry (MAHA).
II. Reverberation mapping of three Seyfert galaxies historically displaying
Hβ profiles with changing asymmetry: Mrk 79, NGC 3227, and Mrk 841.
Brotherton M.S., Du P., Xiao M., Bao D.-W., Zhao B., McLane J.N.,
Olson K.A., Wang K., Huang Z.-P., Hu C., Kasper D.H., Chick W.T.,
Nguyen M.L., Maithil J., Hand D., Li Y.-R., Ho L.C., Bai J.-M., Bian W.-H.,
Wang J.-M., the MAHA Collaboration.
<Astrophys. J., 905, 77 (2020)>
=2020ApJ...905...77B 2020ApJ...905...77B
ADC_Keywords: Active gal. nuclei; Spectra, optical; Black holes; Redshifts;
Galaxies, Seyfert
Keywords: Seyfert galaxies ; Supermassive black holes ; Reverberation mapping
Abstract:
We report the results of reverberation mapping of three bright Seyfert
galaxies, Mrk 79, NGC 3227, and Mrk 841, from a campaign conducted
from 2016 December to 2017 May with the Wyoming Infrared Observatory
(WIRO) 2.3m telescope. All three of these targets have shown
asymmetric broad Hβ emission lines in the past, although their
emission lines were relatively symmetric during our observations. We
measured Hβ time lags for all three targets and estimated masses
of their black holes-for the first time in the case of Mrk 841. For
Mrk 79 and NGC 3227, the data are of sufficient quality to resolve
distinct time lags as a function of velocity and to compute
two-dimensional velocity-delay maps. Mrk 79 shows smaller time lags
for high-velocity gas, but the distribution is not symmetric, and its
complex velocity-delay map could result from the combination of both
inflowing and outflowing Hβ emitting disks that may be part of a
single larger structure. NGC 3227 shows the largest time lags for
blueshifted gas, and the two-dimensional velocity-delay map suggests a
disk with some inflow. We compare our results with previous work and
find evidence for different time lags despite similar luminosities, as
well as evolving broad-line region structures.
Description:
We conducted our observations between late 2016-December and late
2017-May. We used the Wyoming Infrared Observatory (WIRO) 2.3m
telescope and its Long Slit Spectrograph in the range ∼4000-7000Å.
Figure 2 and Table 3 provide the 5100Å continuum and Hβ
emission-line light curves. We measure continuum and Hβ
emission-line fluxes from our calibrated spectra. See Section 2.2.
Given that our targets are relatively bright, we follow our Paper I
(Du+ 2018, J/ApJ/869/142) in supplementing our continuum light curves
with available survey data. The All-Sky Automated Survey for
Supernovae (ASAS-SN) provides photometric light curves for relatively
isolated objects down to ∼17mag, including our targets during our
campaign. This was especially useful for Mrk 841. See Section 2.3.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 43 3 Targets
table3.dat 42 105 Light curves
table5.dat 85 3 *Hβ width measurements and black hole masses
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Note on table5.dat: We have corrected for the line-spread function caused
by the instrument and seeing.
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See also:
J/ApJS/126/331 : Spectrophotometry of nearby field galaxies (Jansen+ 2000)
J/ApJ/613/682 : AGN central masses & broad-line regions (Peterson+, 2004)
J/MNRAS/426/416 : Mrk 6 Hα, Hβ and Hγ sp. (Doroshenko+, 2012)
J/ApJ/779/109 : Long-term monitoring of NGC 5548 (Peterson+, 2013)
J/MNRAS/431/836 : Type 1 AGN at low z. III. (Stern+, 2013)
J/ApJ/782/45 : SEAMBHs. I. Mrk 142, Mrk 335 & IRAS F12397+3333 (Du+, 2014)
J/ApJ/788/48 : X-ray through NIR photometry of NGC 2617 (Shappee+, 2014)
J/ApJS/217/26 : Lick AGN monitoring 2011: light curves (Barth+, 2015)
J/ApJ/806/22 : SEAMBHs IV. Hβ time lags (Du+, 2015)
J/ApJ/827/118 : A new reverberation mapping campaign on NGC 5548 (Lu+, 2016)
J/ApJ/840/97 : Optical RM campaign of 5 AGNs (Fausnaugh+, 2017)
J/ApJ/837/131 : Space telescope RM project. V. NGC5548 sp. (Pei+, 2017)
J/ApJ/866/133 : Continuum-Hβ LCs of 5 Seyfert 1 (De Rosa+, 2018)
J/ApJ/869/142 : Monitoring AGNs with Hβ Asymmetry (MAHA). I. (Du+, 2018)
J/ApJ/856/6 : SEAMBHs IX. 10 new Hβ light curves (Du+, 2018)
J/ApJ/887/135 : V-band, 5100Å and broad emission LCs of Mrk 79 (Lu+, 2019)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Name AGN name
10- 11 I2 h RAh Hour of right ascension (J2000)
13- 14 I2 min RAm Minute of right ascension (J2000)
16- 19 F4.1 s RAs Second of right ascension (J2000)
21 A1 --- DE- Sign of declination (J2000)
22- 23 I2 deg DEd Degree of declination (J2000)
25- 26 I2 arcmin DEm Arcminute of declination (J2000)
28- 29 I2 arcsec DEs Arcsecond of declination (J2000)
31- 36 F6.4 --- z [0.0039/0.04] Redshift
38- 39 I2 --- Nsp [17/48] Number of spectra
41- 43 F3.1 --- Cad [3.1/6.4] Average cadence
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Name AGN name
10- 17 F8.4 d JD [46.8/202] Julian date; JD-2457700
19- 24 F6.3 10-15cW/m2/nm F5100 [2.3/14.8] Continuum flux at 5100Å (1)
26- 30 F5.3 10-15cW/m2/nm e_F5100 [0.004/0.3] Uncertainty in F5100 (1)
32- 36 F5.3 10-13mW/m2 FHb [1.29/5.6] Hβ line flux (2)
38- 42 F5.3 10-13mW/m2 e_FHb [0.006/0.1] Uncertainty in FHb (2)
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Note (1): In units of 10-15erg/s/cm2/Angstroms.
Note (2): In units of 10-13erg/s/cm2.
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Byte-by-byte Description of file: table5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Name AGN name
10- 13 I4 km/s vFWHM [4032/6191] FWHM (VFWHM) from mean
spectra
15- 16 I2 km/s e_vFWHM [45/78] vFWHM uncertainty
18- 21 I4 km/s sig [3370/3505] Line dispersion
(σline) from mean spectra
23- 24 I2 km/s e_sig [16/33] sig uncertainty
26- 29 I4 km/s vFWHMrms [2476/5087] FWHM (VFWHM) from rms spectra
31- 32 I2 km/s e_vFWHMrms [21/27] vFWHMrms uncertainty
34- 37 I4 km/s sigrms [1502/2092] Line dispersion
(σline) from rms spectra
39- 40 I2 km/s e_sigrms [18/24] sigrms uncertainty
42- 45 F4.2 10+7Msun MVP [0.91/8.19] Virial product MVP measured
from the rms spectrum,
RHβ.V2FWHM/G
47- 50 F4.2 10+7Msun e_MVP [0.12/1.86] Lower uncertainty on MVP
52- 55 F4.2 10+7Msun E_MVP [0.12/1.67] Upper uncertainty on MVP
57- 60 F4.2 10+7Msun MBH1 [1.02/9.17] Black hole mass (M{dot})
from the rms spectra,
1.12xRHβ.V2FWHM/G (1)
62- 65 F4.2 10+7Msun e_MBH1 [0.14/2.08] Lower uncertainty on MBH1
67- 70 F4.2 10+7Msun E_MBH1 [0.14/1.87] Upper uncertainty on MBH1
72- 75 F4.2 10+7Msun MBH4 [1.5/6.19] Black hole mass (M{dot}) from
the rms spectra,
4.47xRHβ.σ2line/G (1)
77- 80 F4.2 10+7Msun e_MBH4 [0.2/1.77] Lower uncertainty on MBH4
82- 85 F4.2 10+7Msun E_MBH4 [0.2/1.59] Upper uncertainty on MBH4
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Note (1): The black hole masses (M{dot}) are calculated from the rms spectra
using the fBLR factors from Woo+ (2015ApJ...801...38W 2015ApJ...801...38W).
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History:
From electronic version of the journal
References:
Du et al. Paper I. 2018ApJ...869..142D 2018ApJ...869..142D Cat. J/ApJ/869/142
Brotherton et al. Paper II. 2020ApJ...905...77B 2020ApJ...905...77B This catalog
Bao et al. Paper III. 2022ApJS..262...14B 2022ApJS..262...14B Cat. J/ApJS/262/14
Zastrocky et al. Paper IV. 2024ApJS..272...29Z 2024ApJS..272...29Z Cat. J/ApJS/272/29
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 26-Jul-2022