J/MNRAS/491/92 Young radio AGNs study based on SDSS spectroscopy (Liao+, 2020)
Investigation on young radio AGNs based on SDSS spectroscopy.
Liao M., Gu M.
<Mon. Not. R. Astron. Soc., 491, 92-112 (2020)>
=2020MNRAS.491...92L 2020MNRAS.491...92L (SIMBAD/NED BibCode)
ADC_Keywords: Active gal. nuclei ; Black holes ; Accretion ; Radio sources ;
Galaxies ; Spectra, optical ; Equivalent widths ; Redshifts
Keywords: accretion; accretion discs - galaxies: active - galaxies: evolution -
quasars: emission lines - quasars: supermassive black holes
Abstract:
The gigahertz peaked spectrum (GPS) sources, compact steep spectrum
(CSS) radio sources, and high-frequency peaker (HFP) radio sources are
thought to be young radio active galactic nuclei (AGNs) at the early
stage of AGN evolution. We investigated the optical properties of the
largest sample of 126 young radio AGNs based on the spectra in SDSS
DR12. We find that the black hole masses MBH range from 107.32 to
109.84M☉ and the Eddington ratios Redd vary from 10-4.93
to 100.37, suggesting that young radio AGNs have various accretion
activities and not all are accreting at high accretion rate. Our young
radio sources generally follow the evolutionary trend towards
large-scale radio galaxies with increasing linear size and decreasing
accretion rate in the radio power-linear size diagram. The radio
properties of low-luminosity young radio AGNs with low Redd are
discussed. The line width of [OIII]λ5007 core (σ[OIII])
is found to be a good surrogate of stellar velocity dispersion
σ*. The radio luminosity L{5GHz} correlates strongly with
[OIII] core luminosity L[OIII], suggesting that radio activity and
accretion are closely related in young radio sources. We find one
object that can be defined as a narrow-line Seyfert 1 galaxy,
representing a population of young AGNs with both young jet and early
accretion activity. The optical variabilities of 15 quasars with
multi-epoch spectroscopy were investigated. Our results show that the
optical variability in young AGN quasars presents low variations (=<60
per cent) similar to the normal radio-quiet quasars.
Description:
To systematically study the optical properties of the largest possible
sample of young radio AGNs, we first collected all available
radio-selected samples of young radio AGNs in the literature.
The CSS sources were collected from Spencer et al.
(1989MNRAS.240..657S 1989MNRAS.240..657S), Fanti et al. (1990A&A...231..333F 1990A&A...231..333F), Fanti et
al. (2001A&A...369..380F 2001A&A...369..380F, Cat. J/A+A/369/380), Kunert et al.
(2002A&A...391...47K 2002A&A...391...47K), Edwards & Tingay (2004A&A...424...91E 2004A&A...424...91E), Snellen
et al. (2004MNRAS.348..227S 2004MNRAS.348..227S), and Kunert-Bajraszewska et al.
(2010MNRAS.408.2261K 2010MNRAS.408.2261K, Cat. J/MNRAS/408/2261). For GPS sources, the
radio-selected samples of Stanghellini et al. (1998A&AS..131..303S 1998A&AS..131..303S,
Cat. J/A+AS/131/303), Snellen et al. (1998A&AS..131..435S 1998A&AS..131..435S), Snellen et
al. (2002MNRAS.337..981S 2002MNRAS.337..981S), Edwards & Tingay (2004A&A...424...91E 2004A&A...424...91E), and
Snellen et al. (2004MNRAS.348..227S 2004MNRAS.348..227S) were included. We collected HFP
sources from Dallacasa et al. (2000A&A...363..887D 2000A&A...363..887D, Cat.
J/A+A/363/887) and Stanghellini, Dallacasa & Orienti
(2009AN....330..223S 2009AN....330..223S, Cat. J/AN/330/223), and CSO sources from Peck &
Taylor (2000ApJ...534...90P 2000ApJ...534...90P), Snellen et al. (2004MNRAS.348..227S 2004MNRAS.348..227S),
and An & Baan (2012ApJ...760...77A 2012ApJ...760...77A). This selection produces a sample
of 250 CSS, 148 GPS, 116 HFP, and 80 CSO radio sources. After removing
the overlap sources in the literature, the sample consists of 545
radio sources, which is the parent sample of our study.
Then, we searched for the spectra of the young radio AGNs in SDSS
spectroscopic data release 12 (SDSS DR12, Alam et al.
2015ApJS..219...12A 2015ApJS..219...12A, Cat. V/147) within 2arcsec from the NASA/IPAC
Extragalactic Database (NED) position for all the objects in the
parent sample. This results in our optical sample, consisting of 147
sources.
After removing the blazar-type sources from the parent and optical
samples, it results in 126 sources in our final optical sample.
Many young radio AGNs do not have optical spectral data in SDSS or
other archives. In order to increase available spectrum, we observed
two GPS sources HB89 1127-145 and CGRaBS J1424+2256 on 2012 May 11 and
12, respectively, by using the Yunnan Faint Object Spectrograph Camera
(YFOSC) installed on the Lijiang 2.4m telescope at Yunnan Observatory
(Bai & Liu 2010gfss.conf...63B), Chinese Academy of Sciences.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 102 128 Sample
table2.dat 130 128 Emission line properties
table3.dat 114 30 The optical variability
table4.dat 83 39 Radio and spectroscopic classification
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Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 A19 --- Name Object name
21- 25 F5.3 --- z Redshift
27- 29 A3 --- Type Object type (1)
31- 34 A4 --- r_Type Reference for Type (2)
36 A1 --- Class [GQ] Source classification (3)
38- 42 F5.2 [W/Hz] P5GHz Radio power at 5GHz
44- 46 A3 --- r_P5GHz Reference for P5GHz (2)
48- 54 F7.4 pc LS ? Linear size
56 A1 --- f_LS [a] Flag on LS (4)
58- 60 A3 --- r_LS Reference for LS (2)
62- 65 F4.2 [Msun] logMBH ? Logarithm of the black hole mass
67- 72 A6 --- metMBH Method adopted to obtain logMBH
74- 78 F5.2 [10-7W] logLbol ? Bolometric luminosity
80- 91 A12 --- metLbol Method adopted to obtain logLbol
93- 97 F5.2 [-] logRedd ? Logarithm of the Eddington ratio
(Redd=Lbol/Ledd)
99-102 F4.1 --- S/N Median signal to noise ratio of the spectrum
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Note (1): Object type as follows:
CSO = Compact symmetric object (6/128)
CSS = Compact steep spectrum radio source (82/128)
GPS = Gigahertz peaked spectrum source (21/128)
HFP = High-frequency peaker radio source (19/128)
Note (2): References as follows:
A12 = An & Baan (2012ApJ...760...77A 2012ApJ...760...77A)
B91 = Becker, White & Edwards (1991ApJS...75....1B 1991ApJS...75....1B, Cat. VIII/13)
C10 = Cui et al. (2010A&A...518A..23C 2010A&A...518A..23C)
D00 = Dallacasa et al. (2000A&A...363..887D 2000A&A...363..887D, Cat. J/A+A/363/887)
D09 = de Vries et al. (2009A&A...498..641D 2009A&A...498..641D)
E04 = Edwards & Tingay (2004A&A...424...91E 2004A&A...424...91E)
F01 = Fanti et al. (2001A&A...369..380F 2001A&A...369..380F, Cat. J/A+A/369/380)
H04 = Horiuchi et al. (2004ApJ...616..110H 2004ApJ...616..110H, Cat. J/ApJ/616/110)
H07 = Helmboldt et al. (2007ApJ...658..203H 2007ApJ...658..203H, Cat. J/ApJ/658/203)
K02 = Kunert et al. (2002A&A...391...47K 2002A&A...391...47K)
K10 = Kunert-Bajraszewska et al. (2010MNRAS.408.2261K 2010MNRAS.408.2261K, Cat. J/MNRAS/408/2261)
L97 = Laurent-Muehleisen et al. (1997A&AS..122..235L 1997A&AS..122..235L, Cat. J/A+AS/122/235)
L07 = Labiano et al. (2007A&A...463...97L 2007A&A...463...97L, Cat. J/A+A/463/97)
O98 = O'Dea (1998PASP..110..493O 1998PASP..110..493O)
O10 = Orienti et al. (2010MNRAS.408.1075O 2010MNRAS.408.1075O)
O12 = Orienti & Dallacasa (2012MNRAS.424..532O 2012MNRAS.424..532O)
S89 = Spencer et al. (1989MNRAS.240..657S 1989MNRAS.240..657S)
S98 = Stanghellini et al. (1998A&AS..131..303S 1998A&AS..131..303S, Cat. J/A+AS/131/303)
SW98 = Snellen et al. (1998A&AS..131..435S 1998A&AS..131..435S)
S02 = Snellen et al. (2002MNRAS.337..981S 2002MNRAS.337..981S)
S03 = Snellen et al. (2003MNRAS.342..889S 2003MNRAS.342..889S)
S04 = Snellen et al. (2004MNRAS.348..227S 2004MNRAS.348..227S)
S09 = Stanghellini et al. (2009AN....330..223S 2009AN....330..223S, Cat. J/AN/330/223)
T20 = Peck & Taylor (2000ApJ...534...90P 2000ApJ...534...90P)
Note (3): Classification as follows:
G = Galaxy (55/128)
Q = Quasar (73/128)
Note (4): Flag as follows:
a = The upper limit of LS is given in column LS
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 A19 --- Name Object name
21- 25 I5 km/s FWHMCIV ? Full width at half-maximum for broad
CIV
27- 30 I4 km/s e_FWHMCIV ? Error on FWHMCIV
32- 35 I4 10-20W/m2 FCIV ? Flux for broad CIV
37- 39 I3 10-20W/m2 e_FCIV ? Error on FCIV
41- 44 I4 km/s FWHMMgII ? Full width at half-maximum for broad
MgII
46- 49 I4 km/s e_FWHMMgII ? Error on FWHMMgII
51- 54 I4 10-20W/m2 FMgII ? Flux for broad MgII
56- 57 I2 10-20W/m2 e_FMgII ? Error on FMgII
59- 62 I4 km/s FWHMHbeta ? Full width at half-maximum for broad
Hβ
64- 66 I3 km/s e_FWHMHbeta ? Error on FWHMHbeta
68- 72 I5 10-20W/m2 FHbeta ? Flux for broad Hβ
74- 76 I3 10-20W/m2 e_FHbeta ? Error on FHbeta
78- 80 I3 km/s FWHM[OIII] ? Full width at half-maximum for [OIII]
core line
82- 84 I3 km/s e_FWHM[OIII] ? Error on FWHM[OIII]
86- 89 I4 10-20W/m2 F[OIII] ? Flux for [OIII] core line
91- 93 I3 10-20W/m2 e_F[OIII] ? Error on F[OIII]
95- 98 I4 km/s FWHMHalpha ? Full width at half-maximum for broad
Hα
100-102 I3 km/s e_FWHMHalpha ? Error on FWHMHalpha
104-108 I5 10-20W/m2 FHalpha ? Flux for broad Hα
110-113 I4 10-20W/m2 e_FHalpha ? Error on FHalpha
115-117 I3 km/s FWHM[SII] ? Full width at half-maximum for [SII]
λ6716
119-121 I3 km/s e_FWHM[SII] ? Error on FWHM[SII]
123-125 I3 10-20W/m2 F[SII] ? Flux for [SII]λ6716
127-130 F4.1 10-20W/m2 e_F[SII] ? Error on F[SII]
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Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 A19 --- Name Object name (JHHMMSS.ss+DDMMSS.s)
21- 23 A3 --- Type Object type (1)
25- 29 F5.3 --- z Redshift
31- 34 I4 --- Plate SDSS Plate identifier
36- 40 I5 d MJD SDSS MJD
42- 44 I3 --- Fibre SDSS Fiber identifier
46- 49 F4.1 --- S/N Median signal to noise ratio of the
spectrum
51- 54 F4.1 % Df ? Variability Δf (2)
56- 58 A3 --- Da Colour variation (BWB - bluer when lighter)
60- 64 F5.2 --- alphal Spectral index of power-law continuum
66- 69 F4.2 --- e_alphal Error on alphal
71- 74 I4 km/s FWHMCIV ? Full width at half-maximum for broad CIV
76- 78 I3 km/s e_FWHMCIV ? Error on FWHMCIV
80- 83 I4 10-20W/m2 FCIV ? Flux for broad CIV
85- 87 I3 10-20W/m2 e_FCIV ? Error on FCIV
89- 92 I4 km/s FWHMMgII ? Full width at half-maximum for broad MgII
94- 97 I4 km/s e_FWHMMgII ? Error on FWHMMgII
99 A1 --- f_FWHMMgII [*] Flag on FWHMMgII (3)
101-106 F6.1 10-20W/m2 FMgII ? Flux for broad MgII
108-112 F5.1 10-20W/m2 e_FMgII ? Error on FMgII
114 A1 --- f_FMgII [*] Flag on FMgII (3)
--------------------------------------------------------------------------------
Note (1): Object type as follows:
CSO = Compact symmetric object (2/30)
CSS = Compact steep spectrum radio source (16/30)
GPS = Gigahertz peaked spectrum source (2/30)
HFP = High-frequency peaker radio source (10/30)
Note (2): The source variability was determined by comparing the variation
between the brightest and faintest spectra as
Δf=(fint,b-fint,f)/fint,f, where fint,b and fint,f
are integrated flux at the brightest and faintest epochs,
respectively (e.g. Guo & Gu 2016ApJ...822...26G 2016ApJ...822...26G)
Note (3): Flag as follows:
* = For this source, the FWHM and flux correspond to Hβ instead of MgII
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Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 A19 --- Name Object name (JHHMMSS.ss+DDMMSS.s)
21- 23 A3 --- Type Object type (1)
25 A1 --- Class [GQ] Source classification (2)
27- 28 I2 --- S/N Median signal to noise ratio of the
spectrum
30- 32 I3 10-20W/m2 FHbeta Flux for Hβ (3)
34- 37 I4 10-20W/m2 F[OIII] Flux for [OIII] (3)
39- 41 I3 10-20W/m2 F[OI] Flux for [OI] (3)
43- 46 I4 10-20W/m2 FHalpha Flux for Hα (3)
48- 51 I4 10-20W/m2 F[NII] Flux for [NII] (3)
53- 55 I3 10-20W/m2 F[SII]1 Flux for [SII]λ6717 (3)
57- 59 I3 10-20W/m2 F[SII]2 Flux for [SII]λ6731 (3)
61- 64 F4.2 --- EI Excitation index (4)
66- 68 A3 --- HEG/LEG HEG and LEG classification based on EI
index (5)
70- 74 F5.2 [-] logRedd Logarithm of the Eddington ratio
(Redd=Lbol/Ledd)
76- 81 A6 --- opttype Optical classification based on the
existence of the broad lines (6)
83 A1 --- f_opttype [ab] Flag on opttype (7)
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Note (1): Object type as follows:
CSO = Compact symmetric object (1/39)
CSS = Compact steep spectrum radio source (25/39)
GPS = Gigahertz peaked spectrum source (11/39)
HFP = High-frequency peaker radio source (2/39)
Note (2): Classification as follows:
G = Galaxy (23/39)
Q = Quasar (16/39)
Note (3): The narrow emission line fluxes have typical uncertainties <10%
Note (4): The excitation index represents the overall ratio of high and low
excitation emission lines in each source
EI=log([OIII]/Hβ)-1/3[log([NII]/Hα)+log([SII]/Hα)+
log([OI]/Hα)]
Note (5): HEG/LEG classification as follows:
HEG = High-excitation galaxy (12/39)
LEG = Low-excitation galaxy (27/39)
Note (6): Optical type as follows:
Type 1 = (12/39)
Type 2 = (27/39)
Note (7): Flag as follows:
a = The source has broad lines and σ* measurements
b = The source has broad-line measurements but D4000>1 and S/N<10
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History:
From electronic version of the journal
(End) Ana Fiallos [CDS] 07-Feb-2023