J/ApJ/886/150 VRI and K-band light curves of type 1 AGNs (Minezaki+, 2019)
Reverberation measurements of the inner radii of the dust tori in quasars.
Minezaki T., Yoshii Y., Kobayashi Y., Sugawara S., Sakata Yu, Enya K.,
Koshida S., Tomita H., Suganuma M., Aoki T., Peterson B.A.
<Astrophys. J., 886, 150 (2019)>
=2019ApJ...886..150M 2019ApJ...886..150M
ADC_Keywords: Active gal. nuclei; QSOs; Photometry, VRI; Photometry, infrared
Keywords: Active galactic nuclei ; Quasars ; Dust continuum emission ;
Cosmological parameters
Abstract:
We present the results of a dust-reverberation survey of quasars at
redshifts z<0.6. We found a delayed response of the K-band flux
variation after the optical flux variation in 25 out of 31 targets,
and obtained the lag time between them for 22 targets. Combined with
the results for nearby Seyfert galaxies, we provide the largest
homogeneous collection of K-band dust-reverberation data for 36 type 1
active galactic nuclei (AGNs). This doubles the sample and includes
the most distant AGN and the largest lag so far measured. We estimated
the optical luminosity of the AGN component of each target using three
different methods: spectral decomposition, the flux-variation-gradient
method, and image decomposition. We found a strong correlation between
the reverberation radius for the innermost dust torus and the optical
luminosity over a range of approximately four orders of magnitude in
luminosity, as is already known for Seyfert galaxies. We estimated the
luminosity distances of the AGNs based on their dust-reverberation
lags, and found that the data in the redshift-distance diagram are
consistent with the current standard estimates of the cosmological
parameters. We also present the radius-luminosity relations for
isotropic luminosity indicators such as the hard X-ray (14-195keV),
[OIV]25.89µm, and mid-infrared (12µm) continuum luminosities,
which are applicable to obscured AGNs.
Description:
In this paper, we report the results for 31 type 1 AGNs monitored by
the Multicolor Active Galactic Nuclei (MAGNUM) project
(Yoshii 2002ntto.conf..235Y and Yoshii+ 2003AAS...202.3803Y 2003AAS...202.3803Y).
We conducted monitoring observations using a multicolor imaging
photometer (MIP) mounted on the MAGNUM 2m telescope at the Haleakala
Observatories in Hawaii. The MIP is capable of simultaneous imaging in
one optical band (selected from among U, B, V, R, and I) and one
near-infrared band (selected from among Y, J, H, and K).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 108 31 List of targets and monitoring parameters
table2.dat 42 2981 Light curve data
table5.dat 58 31 Optical AGN fluxes and luminosities
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See also:
II/183 : UBVRI Photometric Standards (Landolt 1992)
VII/223 : The 2dF QSO Redshift Survey. V. The 10k catalogue (Croom+ 2001)
J/ApJ/269/352 : Quasar evolution (Schmidt+, 1983)
J/AJ/109/1498 : Large Bright Quasar Survey VI (LBQS) (Hewett+, 1995)
J/ApJ/663/81 : SED of hard X-ray selected AGN in XMDS (Polletta+, 2007)
J/ApJ/698/895 : Variations in QSOs optical flux (Kelly+, 2009)
J/ApJ/709/1257 : Spitzer-IRS spectra of Seyfert galaxies. II. (Tommasin+, 2010)
J/ApJS/207/19 : Hard X-ray survey from Swift-BAT 6yrs (Baumgartner+, 2013)
J/ApJS/206/4 : SED & bolometric corrections for QSOs (Krawczyk+, 2013)
J/MNRAS/439/1648 : Subarcsecond mid-infrared atlas of local AGN (Asmus+, 2014)
J/ApJ/788/159 : 17 Seyfert 1 galaxies light curves (Koshida+, 2014)
J/A+A/561/L8 : BRJK photometry of Seyfert galaxy WPVS48 (Pozo Nunez+, 2014)
J/ApJ/801/127 : 3.6um, 4.5um, B & V light curves of NGC 6418 (Vazquez+, 2015)
J/ApJS/233/17 : Swift/BAT AGN spectroscopic survey. V. X-ray (Ricci+, 2017)
J/A+A/620/A137 : CCD B,V,R,I,Ha photometry of 3C120 (Ramolla+, 2018)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- ID Identifier (Truncated name)
18- 19 I2 h RAh Hour of right ascension (J2000)
21- 22 I2 min RAm Minute of right ascension (J2000)
24- 29 F6.3 s RAs Second of right ascension (J2000)
31 A1 --- DE- Sign of declination (J2000)
32- 33 I2 deg DEd Degree of declination (J2000)
35- 36 I2 arcmin DEm Arcminute of declination (J2000)
38- 42 F5.2 arcsec DEs Arcsecond of declination (J2000)
44- 49 F6.4 --- z [0.06/0.6] Heliocentric redshift from NED
51 A1 --- Opt Optical observing band (V, R or I) (1)
53 A1 --- NIR NIR observing band (always K) (1)
55- 64 A10 "Y/M/D" Start Starting date of observation (UT)
65 A1 --- --- [-]
66- 75 A10 "Y/M/D" End Ending date of observation (UT)
77- 79 I3 --- Nobs [12/134] Number of observations
81- 83 I3 d Tint [6/112] Median monitoring interval
85- 108 A24 --- Name Full name of the source
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Note (1): Observing photometric bands to measure the dust-reverberation lag.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- ID Identifier (Truncated name)
18 A1 --- Band Observing band (V, R, I or K)
20- 27 F8.2 d MJD [52117.45/54330.62] Observation Date
29- 35 F7.1 uJy Flux [44/19712] Flux in Band (1)
37- 42 F6.1 uJy e_Flux [0.4/324] Uncertainty in Flux
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Note (1): Galactic extinction has been corrected for, and the fluxes from the
host galaxy have not been subtracted.
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- ID Identifier (Truncated name)
18 A1 --- Band Optical band (V, R or I) for Flux
20 A1 --- f_Band Flag on Band (2)
22- 27 F6.1 uJy Flux [10/5878]? Optical flux of the AGN in Band
29- 33 F5.1 uJy e_Flux [0.4/161]? Flux downwards uncertainty
35- 39 F5.1 uJy E_Flux [0.4/161]? Flux upwards uncertainty
41- 46 F6.3 [10-7W] logL [42.6/45.43]? Log of the V-band luminosity
of the AGN in erg/s units
48- 52 F5.3 [10-7W] e_logL [0.005/0.3]? LogL downwards uncertainty
54- 58 F5.3 [10-7W] E_logL [0.005/0.4]? LogL upwards uncertainty
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Note (2): Flag as follows:
a = In the case of SDSS J1720+6128, the emission in the rest-frame V band
is in fact closer to that in the observer-frame R band, although the
monitoring observations for the dust reverberation were conducted in
the I band (owing to a mistake in the filter selection at the start of
observation). We therefore converted the I-band AGN flux into an
R-band flux based on the slope of the linear regression of the
multi-epoch flux data in the R and I bands. See Section 4.2.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 20-Apr-2021