J/ApJ/876/49 A 10yr reverberation mapping campaign for 3C273 (Zhang+, 2019)
Kinematics of the broad-line region of 3C 273 from a 10yr reverberation mapping
campaign.
Zhang Z.-X., Du P., Smith P.S., Zhao Y., Hu C., Xiao M., Li Y.-R.,
Huang Y.-K., Wang K., Bai J.-M., Ho L.C., Wang J.-M.
<Astrophys. J., 876, 49 (2019)>
=2019ApJ...876...49Z 2019ApJ...876...49Z
ADC_Keywords: Active gal. nuclei; Photometry; Spectra, optical
Keywords: galaxies: active ; galaxies: individual (3C 273) ; galaxies: nuclei
Abstract:
Despite many decades of study, the kinematics of the broad-line region
of 3C 273 are still poorly understood. We report a new, high
signal-to-noise, reverberation mapping campaign carried out from 2008
November to 2018 March that allows the determination of time lags
between emission lines and the variable continuum with high precision.
The time lag of variations in Hβ relative to those of the
5100Å continuum is 146.8-12.1+8.3days in the rest frame, which
agrees very well with the Paschen-α region measured by the
GRAVITY at The Very Large Telescope Interferometer. The time lag of
the Hγ emission line is found to be nearly the same as that for
Hβ. The lag of the FeII emission is 322.0-57.9+55.5days,
longer by a factor of ∼2 than that of the Balmer lines. The
velocity-resolved lag measurements of the Hβ line show a complex
structure that can be possibly explained by a rotation-dominated disk
with some inflowing radial velocity in the Hβ-emitting region.
Taking the virial factor of fBLR=1.3, we derive a BH mass of
dM/dt=4.1-0.4+0.3x108M☉ and an accretion rate of
9.3LEddc-2 from the Hβ line. The decomposition of its Hubble
Space Telescope images yields a host stellar mass of
M*=1011.3±0.7M☉, and a ratio of dM/dt/M*∼2.0x10-3 in
agreement with the Magorrian relation. In the near future, it is
expected to compare the geometrically thick BLR discovered by the
GRAVITY in 3C 273 with its spatially resolved torus in order to
understand the potential connection between the BLR and the torus.
Description:
The spectroscopic and photometric data of 3C 273 used in this paper
are mainly derived from the Steward Observatory (SO) spectropolarimetric
monitoring project, which is a long-term optical program to support
the Fermi Gamma-ray Space Telescope. The project began just after the
launch of Fermi in 2008 and provides almost a decade of
spectropolarimetric, photometric, and spectroscopic data for more than
70 blazars (Smith+ 2009, 0912.3621).
The SO campaign utilizes both the 2.3m Bok Telescope on Kitt Peak and
the 1.54m Kuiper Telescope on Mt. Bigelow in Arizona. All of the
observations are carried out using the SPOL spectropolarimeter.
There are a total of 374 spectroscopic epochs for 3C 273 up until 2018
March from the SO program.
3C 273 has 297 V-band photometric epochs. For the 374 spectroscopic
observations, there are only 291 spectra that have the photometric
observations in the same nights.
We monitored 3C 273 from 2016 December 28 to 2017 June 13 using the
2.4m telescope at the Lijiang Station of the Yunnan Observatories,
Chinese Academy of Sciences. It is mounted with the Yunnan Faint
Object Spectrograph and Camera (YFOSC), which is a multifunctional
instrument both for photometry and spectroscopy (wavelength coverage
is 3800-7200Å). See Section 2.2.
For comparison, we also show the V-band light curve of 3C 273 from the
ASAS-SNs project (Shappee+ 2014, J/ApJ/788/48 and
Kochanek+ 2017PASP..129j4502K 2017PASP..129j4502K). See Section 2.3.
Objects:
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RA (ICRS) DE Designation(s)
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12 29 06.70 +02 03 08.6 3C 273 = LEDA 41121
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 79 700 Continuum and emission-line fluxes of 3C 273
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See also:
J/ApJ/613/682 : AGN central masses & broad-line regions (Peterson+, 2004)
J/ApJ/687/78 : FeII emission in quasars (Hu+, 2008)
J/AJ/136/2373 : Type 2 quasars from SDSS (Reyes+, 2008)
J/ApJ/716/993 : LAMP: reverberation mapping of H and He lines (Bentz+, 2010)
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 and IRAS F12397+3333 (Du+, 2014)
J/ApJ/788/48 : X-ray through NIR photometry of NGC 2617 (Shappee+, 2014)
J/ApJ/793/108 : SEAMBHs. II. Continuum and Hbeta LCs (Wang+, 2014)
J/ApJS/217/26 : Lick AGN monitoring 2011: light curves (Barth+, 2015)
J/ApJ/806/128 : Space telescope RM project. I. NGC5548 (De Rosa+, 2015)
J/ApJ/806/22 : SEAMBHs IV. Hβ time lags (Du+, 2015)
J/ApJ/825/126 : SEAMBHs. V. The third year (Du+, 2016)
J/ApJ/827/118 : A new reverberation mapping campaign on NGC 5548 (Lu+, 2016)
J/ApJ/818/30 : Lag measurements for 15 z<0.8 QSOs from SDSS-RM (Shen+, 2016)
J/ApJ/837/131 : Space telescope RM project. V. NGC5548 (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/AJ/159/259 : Opt-NIR light curves of the quasar 3C 273 (Figaredo+, 2020)
http://www.astronomy.ohio-state.edu/asassn : ASAS-SN home page
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 10 F10.2 d JD1 [2454795/2458195]? Julian Date of spectra
12- 16 F5.2 10-17W/m2/nm F5100 [14/24.1]? Continuum flux at 5100Å,
in 10-15erg/s/cm2/Å
18- 21 F4.2 10-17W/m2/nm e_F5100 [0.2/0.3]? Uncertainty in F5100
23- 27 F5.2 10-16W/m2 FHbeta [15.5/19.7]? Hβ emission-line flux,
in 10-13erg/s/cm2
29- 32 F4.2 10-16W/m2 e_FHbeta [0.15/0.3]? Uncertainty in FHbeta
34- 37 F4.2 10-16W/m2 FHgamma [4.9/7.2]? Hγ emission-line flux
39- 42 F4.2 10-16W/m2 e_FHgamma [0.1/0.2]? Uncertainty in FHgamma
44- 48 F5.2 10-16W/m2 FFe [12.9/16]? Fe emission-line flux
50- 53 F4.2 10-16W/m2 e_FFe [0.2/0.5]? Uncertainty in FFe
55- 55 A1 --- Obs1 ? Spectrum observatory (1)
57- 66 F10.2 d JD2 [2454795/2458218.7] Julian Date
of V band photometry
68- 72 F5.2 mag Vmag [12.5/13.3] V band magnitude
74- 77 F4.2 mag e_Vmag [0.01/0.11] Uncertainty in Vmag
79- 79 A1 --- Obs2 Photometry observatory (1)
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Note (1): Observatory codes for spectrum and photometric monitoring as follows:
S = Steward Observatory (SO) spectropolarimetric monitoring project1;
L = Lijiang Observatory;
A = All-Sky Automated Survey for Supernovae (ASAS-SN) project.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 02-Oct-2020