J/ApJ/896/1 SEAMBHs. XI. Mrk 142 X-ray to optical light curves (Cackett+, 2020)
Supermassive black holes with high accretion rates in active galactic nuclei.
XI. Accretion disk reverberation mapping of Mrk 142.
Cackett E.M., Gelbord J., Li Y.-R., Horne K., Wang J.-M., Barth A.J.,
Bai J.-M., Bian W.-H., Carroll R.W., Du P., Edelson R., Goad M.R., Ho L.C.,
Hu C., Khatu V.C., Luo B., Miller J., Yuan Y.-F.
<Astrophys. J., 896, 1 (2020)>
=2020ApJ...896....1C 2020ApJ...896....1C
ADC_Keywords: Active gal. nuclei; X-ray sources; Photometry, ugriz;
Photometry, ultraviolet
Keywords: Active galactic nuclei ; Accretion
Abstract:
We performed an intensive accretion disk reverberation mapping
campaign on the high accretion rate active galactic nucleus Mrk142 in
early 2019. Mrk 142 was monitored with the Neil Gehrels Swift
Observatory for four months in X-rays and six different UV/optical
filters. Ground-based photometric monitoring was obtained from the Las
Cumbres Observatory, the Liverpool Telescope, and the Dan Zowada
Memorial Observatory in ugriz filters, as well as from the Yunnan
Astronomical Observatory in V. Mrk 142 was highly variable throughout,
displaying correlated variability across all wavelengths. We measure
significant time lags between the different wavelength lightcurves. In
the UV and optical, we find that the wavelength-dependent lags,
τ(λ), generally follow the relation
τ(λ)∝λ4/3, as expected for the
T∝R-3/4 profile of a steady-state, optically thick,
geometrically thin accretion disk, though they can also be fit by
τ(λ)∝λ2, as expected for a slim disk. The
exceptions are the u and U bands, where an excess lag is observed, as
has been observed in other active galactic nuclei and attributed to
continuum emission arising in the broad-line region. Furthermore, we
perform a flux-flux analysis to separate the constant and variable
components of the spectral energy distribution, finding that the flux
dependence of the variable component is consistent with the
fν∝ν1/3 spectrum expected for a geometrically thin
accretion disk. Moreover, the X-ray to UV lag is significantly offset
from an extrapolation of the UV/optical trend, with the X-rays showing
a poorer correlation with the UV than the UV does with the optical.
The magnitude of the UV/optical lags is consistent with a highly
super-Eddington accretion rate.
Description:
A large, coordinated monitoring campaign on Mrk 142 took place from
2018 October-2019 June. The core of the campaign was centered around
X-ray and UV/optical observations taken with Swift. In addition, we
obtained further X-ray observations with NICER, as well as supporting
ground-based photometric and spectroscopic monitoring from multiple
telescope sites.
Here, we focus only on the Swift and ground-based photometric data.
The ground-based monitoring involved the Las Cumbres Observatory (LCO),
the Liverpool Telescope, the Dan Zowada Memorial Observatory, and the
Yunnan Astronomical Observatory.
Mrk 142 was monitored by Swift from 2019 January 1 to 2019 April 30
through Cycle 14 proposal 1417139 (PI: E. M. Cackett). In total, 185
epochs of observations were obtained. See Section 2.1. LCO is a global
network of robotic telescopes.
As part of an LCO Key Project (KEY-2018B-001, PI: R. Edelson),
monitoring was obtained in Sloan u, g, r, i, and PanSTARRS z filters
from both the 2m Faulkes Telescope North at the Haleakala Observatory
(OGG), and the 1m telescope at the McDonald Observatory (ELP).
Observations with LCO took place between 2018 December 15 and 2019
June 19. See Section 2.2.
Photometric monitoring was obtained with the robotic 2m Liverpool
Telescope (LT) located on La Palma, Spain through program PL19A01
(PI: M. Goad). Observations were taken using the IO:O instrument in u,
g, r, i, and z filters and took place between 2019 January 3 and
2019 April 22.
The Zowada Observatory is a robotic 20 inch f/6.8 PlaneWave telescope
located near Rodeo, New Mexico, and is owned and operated by Wayne
State University. Observations began on 2018 October 31 and continued
daily (when possible) until 2019 May 30. Images were obtained using u,
g, r, i, and z filters.
Observations at the Lijiang Station of the Yunnan Observatories,
Chinese Academy of Sciences, were obtained with the 2.4m telescope.
The telescope is equipped with the Yunnan Faint Object Spectrograph
and Camera (YFOSC), which is a versatile instrument usable both for
photometry and spectroscopy. While the Lijiang telescope was primarily
used for spectroscopy, images in the V filter were also obtained as
part of the program. Observations span from 2018 October 22 to
2019 June 21.
Objects:
----------------------------------------------------------
RA (ICRS) DE Designation(s)
----------------------------------------------------------
10 25 31.28 +51 40 34.9 Mrk 142 = PG 1022+519
----------------------------------------------------------
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 48 2617 Mrk 142 lightcurves
--------------------------------------------------------------------------------
See also:
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
J/ApJ/613/682 : AGN central masses & broad-line region sizes (Peterson+, 2004)
J/MNRAS/397/1177 : Swift-XRT observations of GRBs (Evans+, 2009)
J/ApJ/782/45 : SEAMBHs. I. Mrk 142, Mrk 335, and IRAS F12397+3333 (Du+, 2014)
J/ApJ/806/22 : SEAMBHs IV. Hβ time lags (Du+, 2015)
J/ApJ/806/129 : Space telescope RM project. II. Swift data (Edelson+, 2015)
J/ApJ/825/126 : SEAMBHs. V. The third year (Du+, 2016)
J/ApJ/821/56 : HST RM project. III. NGC 5548 LCs (Fausnaugh+, 2016)
J/ApJ/840/41 : X-ray/UV Swift monitoring of NGC 4151 (Edelson+, 2017)
J/ApJ/856/6 : SEAMBHs IX. 10 new Hβ light curves (Du+, 2018)
J/ApJ/870/123 : Swift optical & UV flux of four AGNs (Edelson+, 2019)
J/ApJ/877/23 : SEAMBHs. X. RM campaign compilation (Lu+, 2019)
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 F9.3 d MJD [58413.934/58655.583] Modified Julian Date
11- 15 A5 --- Filt Filter name
17- 21 F5.3 --- Flux [0.025/9.1] Flux
23- 27 F5.3 --- e_Flux [0.002/0.5] Uncertainty in Flux
29- 35 A7 --- Tel Telescope identifier (1)
37- 48 A12 --- x_Flux Flux units (2)
--------------------------------------------------------------------------------
Note (1): Telescope as follows:
Swift = The Neil Gehrels Swift Observatory with UVOT and XRT
(1112 occurrences)
Zowada = Zowada Observatory robotic PlaneWave telescope located near Rodeo,
New Mexico (506 occurrences)
OGG = The 2m Faulkes Telescope North at the Haleakala Observatory (OGG)
at Las Cumbres Observatory (LCO; 412 occurrences)
ELP = The 1m telescope at the McDonald Observatory (ELP)
at Las Cumbres Observatory (LCO; 277 occurrences)
LT = The robotic 2m Liverpool Telescope located on La Palma, Spain
(248 occurrences)
Lijiang = The Lijiang 2.4m telescope with YFOSC at Yunnan Observatory
(62 occurrences)
Note (2): The X-ray fluxes are given as count rates (ct/s), while the
Swift/UVOT and optical fluxes are given in units of 10-15erg/cm2/s/Å.
The exception is the Lijiang V light curve, which is given in
arbitrary flux units normalized to a mean of 1.
--------------------------------------------------------------------------------
History:
From electronic version of the journal
References:
Du et al. Paper I. 2014ApJ...782...45D 2014ApJ...782...45D Cat. J/ApJ/782/45
Wang et al. Paper II. 2014ApJ...793..108W 2014ApJ...793..108W Cat. J/ApJ/793/108
Hu et al. Paper III. 2015ApJ...804..138H 2015ApJ...804..138H
Du et al. Paper IV. 2015ApJ...806...22D 2015ApJ...806...22D Cat. J/ApJ/806/22
Du et al. Paper V. 2016ApJ...825..126D 2016ApJ...825..126D Cat. J/ApJ/825/126
Du et al. Paper VI. 2016ApJ...820...27D 2016ApJ...820...27D
Xiao et al. Paper VII. 2018ApJ...864..109X 2018ApJ...864..109X
Li et al. Paper VIII. 2018ApJ...869..137L 2018ApJ...869..137L
Du et al. Paper IX. 2018ApJ...856....6D 2018ApJ...856....6D Cat. J/ApJ/856/6
Lu et al. Paper X. 2019ApJ...877...23L 2019ApJ...877...23L Cat. J/ApJ/877/23
Cackett et al. Paper XI. 2020ApJ...896....1C 2020ApJ...896....1C This catalog
Hu et al. Paper XII. 2021ApJS..253...20H 2021ApJS..253...20H Cat. J/ApJS/253/20
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 03-May-2021