J/ApJS/262/14 AGNs with Hβ asymmetry. III. 15 PG quasars (Bao+, 2022)
Monitoring AGNs with Hβ asymmetry.
III. Long-term reverberation mapping results of 15 Palomar-Green quasars.
Bao D.-W., Brotherton M.S., Du Pu, McLane J.N., Zastrocky T.E., Olson K.A.,
Fang F.-N., Zhai S., Huang Z.-P., Wang K., Zhao B.-X., Li S.-S., Yang S.,
Chen Y.-J., Liu J.-R., Yao Z.-H., Peng Y.-C., Guo W.-J., Songsheng Y.-Y.,
Li Y.-R., Jiang B.-W., Kasper D.H., Chick W.T., Nguyen My L., Maithil J.,
Kobulnicky H.A., Dale D.A., Hand D., Adelman C., Carter Z., Murphree A.M.,
Oeur M., Schonsberg S., Roth T., Winkler H., Marziani P., D'Onofrio M.,
Hu C., Xiao M., Xue S., Czerny B., Aceituno J., Ho L.C., Bai J.-M.,
Wang J.-M., The MAHA Collaboration.
<Astrophys. J. Suppl. Ser., 262, 14 (2022)>
=2022ApJS..262...14B 2022ApJS..262...14B
ADC_Keywords: Active gal. nuclei; QSOs; Spectra, optical; Redshifts
Keywords: Reverberation mapping ; Active galactic nuclei ;
Active galaxies ; Supermassive black holes ; Quasars
Abstract:
In this third paper of the series reporting on the reverberation
mapping campaign of active galactic nuclei with asymmetric Hβ
emission-line profiles, we present results for 15 Palomar-Green
quasars using spectra obtained between the end of 2016-2021 May. This
campaign combines long time spans with relatively high cadence. For
eight objects, both the time lags obtained from the entire light
curves and the measurements from individual observing seasons are
provided. Reverberation mapping of nine of our targets has been
attempted for the first time, while the results for six others can be
compared with previous campaigns. We measure the Hβ time lags
over periods of years and estimate their black hole masses. The long
duration of the campaign enables us to investigate their broad-line
region (BLR) geometry and kinematics for different years by using
velocity-resolved lags, which demonstrate signatures of diverse BLR
geometry and kinematics. The BLR geometry and kinematics of individual
objects are discussed. In this sample, the BLR kinematics of
Keplerian/virialized motion and inflow is more common than that of
outflow.
Description:
The spectroscopic observations were carried out using the 2.3m
telescope of the Wyoming Infrared Observatory (WIRO) in the United
States, the Lijiang 2.4m telescope of the Yunnan Observatories of the
Chinese Academy of Sciences in China, the 2.2m telescope of the Calar
Alto Astronomical Observatory of Centro Astronomico Hispano-Aleman
(CAHA) in Spain, the Copernico 1.82m telescope of the Italian National
Institute for Astrophysics (INAF) at Mount Ekar in Italy, and the
Sutherland 1.9m telescope at the South African Astronomical
Observatory (SAAO) in South Africa.
For PG 0007+106, PG 1100+772, PG 1202+281, and PG 1501+106, some of
the data points come from the Asiago 1.82m telescope. The spectra
were taken using the Asiago Faint Object Spectrograph and Camera
(AFOSC). See Section 2.2.4.
Observations for some objects date back to 2016 December and continued
until the northern spring of 2021 for all targets except PG 1211+143
(for which observations concluded in 2017 July). We monitored most of
the objects for more than one year.
The Lijiang/YFOSC and CAHA/CAFOS instruments can also perform imaging
observations.
To improve the cadence and extend the temporal coverage of the
continuum light curves, we also employ archival time-domain
photometric data from the All-Sky Automated Survey for SuperNovae
(ASAS-SN) and the Zwicky Transient Facility (ZTF).
See Section 2.3.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 99 15 Basic information of the 15 Palomar-Green (PG)
targets
table5.dat 79 10313 Light curves
--------------------------------------------------------------------------------
See also:
J/ApJ/269/352 : Quasar evolution (Schmidt+, 1983)
J/A+A/369/57 : Monitoring Mkn 279 in BVRI and Hβ (Santos-Lleo+, 2001)
J/ApJS/145/199 : Opt. spectroscopic atlas of low-redshift AGN (Marziani+, 2003)
J/ApJ/613/682 : AGN central masses & broad-line region sizes (Peterson+, 2004)
J/A+A/440/409 : Extragalactic sources at 22 and 37GHz (Terasranta+, 2005)
J/ApJ/687/78 : FeII emission in quasars (Hu+, 2008)
J/ApJS/201/23 : Spectroscopy of 88 z<0.7 SDSS QSOs (Eracleous+, 2012)
J/ApJ/755/60 : Reverberation mapping for 5 Seyfert 1 galaxies (Grier+, 2012)
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/ApJS/217/26 : Lick AGN monitoring 2011: light curves (Barth+, 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/840/97 : Optical RM campaign of 5 AGNs (Fausnaugh+, 2017)
J/ApJ/851/21 : SDSS RM project first year of observations (Grier+, 2017)
J/ApJ/866/133 : Continuum-Hβ light curves 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/865/56 : Emission line & R-band continuum LCs of 17 QSOs (Lira+, 2018)
J/ApJ/880/46 : Spectroscopy & V-band monitoring of CTS C30.10 (Czerny+, 2019)
J/ApJ/886/42 : Reverberation mapping & opt. spectra data of AGNs (Du+, 2019)
J/ApJ/886/150 : VRI and K-band light curves of type 1 AGNs (Minezaki+, 2019)
J/ApJ/886/93 : SAMP. III. Opt. LCs and spectra of two AGNs (Rakshit+, 2019)
J/ApJ/876/49 : A 10yr reverberation mapping campaign for 3C273 (Zhang+, 2019)
J/ApJ/905/77 : AGNs with Hβ Asymmetry. II. (Brotherton+, 2020)
J/ApJ/903/112 : SDSS Hb & CIV reverberation mapped AGNs (Dalla Bonta+, 2020)
J/ApJ/905/75 : 3yrs spectroscopic light curves of PG0026+129 (Hu+, 2020)
J/ApJ/890/71 : 5100Å cont. & emission lines LCs of PG2130+099 (Hu+, 2020)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 A2 --- --- [PG]
4- 11 A8 --- PG Palomar Bright Quasar identifier
13- 30 A18 --- OName Other name(s)
32- 33 I2 h RAh [0/16] Hour of Right Ascension (J2000)
35- 36 I2 min RAm Minute of Right Ascension (J2000)
38- 41 F4.1 s RAs Second of Right Ascension (J2000)
43 A1 --- DE- Sign of the Declination (J2000)
44- 45 I2 deg DEd [5/76] Degree of Declination (J2000)
47- 48 I2 arcmin DEm Arcminute of Declination (J2000)
50- 51 I2 arcsec DEs Arcsecond of Declination (J2000)
53- 58 F6.4 --- z [0.028/0.32] Spectroscopic redshift
60- 65 F6.3 --- A [-0.23/0.07] Dimensionless asymmetry parameter (1)
67- 72 F6.3 --- A-B92 [-0.3/0.14]? Boroson & Green (1992ApJS...80..109B 1992ApJS...80..109B)
asymmetry parameter (2)
74- 91 A18 --- Obs Observatories
93- 97 A5 --- Ref Previous reverberation mapping campaign
reference(s) (3)
99 A1 --- f_Ref Flag on previous RM campaign (3)
--------------------------------------------------------------------------------
Note (1): This is measured from our campaign (see Section 2.1).
Note (2): Boroson & Green (1992ApJS...80..109B 1992ApJS...80..109B) adopted the line asymmetry
parameter:
A=[λc(3/4)-λc(1/4)]/Δλ(1/2), Equation (1)
defined by De Robertis (1985ApJ...289...67D 1985ApJ...289...67D), and measured the
asymmetries of the Hβ emission lines in PG quasars, where
λc(3/4) and λc(1/4) are the central wavelengths
where the profiles are 3/4 and 1/4 of the peak value, respectively,
and Δλ(1/2) is the FWHM of emission line. A<0 indicates
that the emission line has a profile with a more pronounced red wing,
while A>0 means the line has a stronger blue wing (see Figure 1 in
Paper I (Du+ 2018, J/ApJ/869/142)). See Section 2.1.
Note (3): References and Flag as follows:
1 = Grier et al. (2012, J/ApJ/755/60);
2 = Kaspi et al. (2000ApJ...533..631K 2000ApJ...533..631K);
3 = Maoz et al. (1990ApJ...351...75M 1990ApJ...351...75M);
4 = Santos-Lleo et al. (2001, J/A+A/369/57);
5 = Barth et al. (2015ApJS..217...26S 2015ApJS..217...26S);
6 = Brotherton et al. (2020, J/ApJ/905/77);
7 = Denney et al. (2010ApJ...721..715D 2010ApJ...721..715D);
8 = Minezaki et al. (2019, J/ApJ/886/150).
* = the previous RM campaign did not successfully measure the
time lag of Hβ.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 A2 --- --- [PG]
4- 11 A8 --- PG Palomar Bright Quasar identifier
13- 24 A12 --- Tel Telescope identifier (1)
26- 32 A7 --- Data Data type; continuum or Hβ line
34- 43 F10.5 d JD [477/2374.5] Julian Date of the observation;
JD-2457000
45- 49 F5.3 --- Flux [0.3/7.3] Measured flux (2)
51- 55 F5.3 --- e_Flux [0.001/0.6] Uncertainty in Flux (3)
57- 79 A23 --- x_Flux Flux units (2)
--------------------------------------------------------------------------------
Note (1): Telescope as follows:
ZTF = the Zwicky Transient Facility (4018 occurrences)
ASAS-SN = the All-Sky Automated Survey for SuperNovae (3160 occurrences)
WIRO = the Wyoming Infrared Observatory (WIRO) in the United States
(See section 2.2.1; 2598 occurrences)
Lijiang Spec = the Lijiang 2.4m telescope of the Yunnan Observatories of
the Chinese Academy of Sciences in China (See section 2.2.2;
296 occurrences)
Lijiang Phot = the Lijiang 2.4m telescope of the Yunnan Observatories of
the Chinese Academy of Sciences in China (See section 2.3;
150 occurrences)
Asiago = the Asiago 1.82m telescope (See section 2.2.4; 38 occurrences)
SAAO = the Sutherland 1.9m telescope at the South African Astronomical
Observatory in South Africa (See section 2.2.5; 30 occurrences)
CAHA Spec = the CAHA 2.2m telescope using the Calar Alto Faint Object
Spectrograph (CAFOS; See section 2.2.3; 14 occurrences)
CAHA Phot = the CAHA 2.2m telescope using CAFOS (See section 2.3;
9 occurrences)
Note (2): The units for continuum and Hβ are 10-15erg/s/cm2/Å
and 10-13erg/s/cm2, respectively.
Note (3): The uncertainty doesn't include the systematic errors measured
from median filter method (see Section 3.2).
--------------------------------------------------------------------------------
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 Cat. J/ApJ/905/77
Bao et al. Paper III. 2022ApJS..262...14B 2022ApJS..262...14B This catalog
Zastrocky et al. Paper IV. 2024ApJS..272...29Z 2024ApJS..272...29Z Cat. J/ApJS/272/29
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 16-Nov-2022