J/MNRAS/511/214 Study of CSS/GPS/MPS radio sources (Nascimento+, 2022)
Optical properties of Peaked Spectrum radio sources.
Nascimento R.S., Rodriguez-Ardila A., Dahmer-Hahn L., Fonseca-Faria M.A.,
Riffel R., Marinello M., Beuchert T., Callingham J.R.
<Mon. Not. R. Astron. Soc., 511, 214-230 (2022)>
=2022MNRAS.511..214N 2022MNRAS.511..214N (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies ; Active gal. nuclei ; Radio sources ; Infrared ;
Optical ; Photometry ; Spectroscopy ; Populations, stellar ;
Radio continuum ; Positional data ; Redshifts ; Extinction ;
Morphology ; Stars, ages ; Abundances ; Stars, masses ;
Star Forming Region
Keywords: galaxies: active - galaxies: ISM - galaxies: nuclei
Abstract:
In this work, we study the optical properties of compact radio sources
selected from the literature in order to determine the impact of the
radio-jet in their circumnuclear environment. Our sample includes 58
Compact Steep Spectrum (CSS) and GigaHertz Peaked Spectrum (GPS) and
14 Megahertz-Peaked spectrum (MPS) radio sources located at z ≤ 1.
The radio luminosity (LR) of the sample varies between Log LR ∼ 23.2
and 27.7 W.Hz-1. We obtained optical spectra for all sources from
SDSS-DR12 and performed a stellar population synthesis using the
STARLIGHT code. We derived stellar masses (M*), ages <t*>, star
formation rates (SFR), metallicities <Z*> and internal reddening AV
for all young AGNs of our sample. A visual inspection of the SDSS
images was made to assign a morphological class for each source. Our
results indicate that the sample is dominated by intermediate to old
stellar populations and there is no strong correlation between optical
and radio properties of these sources. Also, we found that young AGNs
can be hosted by elliptical, spiral and interacting galaxies,
confirming recent findings. When comparing the optical properties of
CSS/GPS and MPS sources, we do not find any significant difference.
Finally, the Mid-Infrared WISE colours analysis suggests that the
compact radio sources defined as powerful AGNs are, in general,
gas-rich systems.
Description:
With the increasing availability of powerful stellar population
synthesis codes (i.e starlight, pPXF) and optical spectroscopy for a
sizeable number of objects from public surveys as the Sloan Digital
Sky Survey the stellar content of CSS/GPS can now be studied in
detail. In this work, we carry out a detailed study of the stellar
population in a sample of CSS/GPS galaxies limited by volume in order
to determine the general properties of the stellar population in these
sources and investigate the impact of the radio-jet on the
circumnuclear environment of these objects, (i.e see section
Introduction).
Based on selected catalogues publicly available in the literature
(using surveys that observed the sky around or above 1 GHz) as exposed
in the section 2 Peaked-spectrum sample selection, we constructed a
sample of 204 objects with redshift range restricted to z < 1. This
choice was made in order to include narrow lines from [O II] to
[Ar III] (3727 Å - 7136 Å in the rest frame) in the observed
wavelength range covered by SDSS. We looked for optical counterparts
from the SDSS-DR12 (Alam et al. 2015ApJS..219...12A 2015ApJS..219...12A, Cat. V/147) for
these objects. A maximum search radius of 8 arcseconds was adopted to
match the sources in both FIRST and SDSS catalogs. Of the 204 sources,
84 have a SDSS spectroscopic counterpart and out of these, 75 have
spectra with signal-to-noise ratio (SNR) higher than 10. We also
included low-frequency sources in our sample in order to see whether
they have similar properties to those of well-known CSS and GPS. For
this purpose, we used a sample of MPS sources (Callingham et al.
2017ApJ...836..174C 2017ApJ...836..174C, Cat. J/ApJ/836/174) identified from the GLEAM
survey (Hurley-Walker et al. 2017MNRAS.464.1146H 2017MNRAS.464.1146H, Cat. VIII/100) with
flux density measurements around 1.4 GHz. Of these, 154 are located
at z < 1 and 23 have SDSS-DR12 optical spectra.
The table1.dat and table2.dat list, respectively, the main properties
of the 84 CSS/GPS and the 21 MPS sources in our sample. The radio and
MIR data were obtained from Faint Images of the Radio Sky at Twenty-cm
survey (FIRST, Helfand et al. 2015ApJ...801...26H 2015ApJ...801...26H, Cat. VIII/92) and
Wide-field Infrared Survey Explorer (WISE, Cutri et al.
2012wise.rept....1C, Cat. II/311), respectively, (i.e see section 2).
Hereafter, we remove from the subsequent analysis objects with z > 1,
those dominated by a power-law continuum and those with poor SNR (SNR
< 10). Our final sample is composed of 58 CSS/GPS and 14 MPS sources.
Next, as explained in the section 3 Stellar population synthesis, we
characterize the stellar properties of the radio-sources, we carry out
a stellar population synthesis using the starlight spectral synthesis
code. The table3.dat and table4.dat presents the results from this
code, also SFR*, M*, radio luminosity LR and visual morphology types
(i.e see section 4 and 5) for our CSS/GPS and the MPS sources in our
sample respectively.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 74 84 Properties of CSS/GPS sources in our sample
table2.dat 76 22 Properties of MPS sources in our sample
table3.dat 101 58 Stellar Population Synthesis Results for CSS/GPS
sources in our sample
table4.dat 104 14 Stellar Population Synthesis Results for MPS
sources in our sample
--------------------------------------------------------------------------------
See also:
V/147 : The SDSS Photometric Catalogue, Release 12 (Alam+, 2015)
J/A+A/369/380 : CSS/GPS radio sources VLA observations (Fanti+, 2001)
J/A+AS/131/303 : GHz-Peaked-Spectrum radio sources (Stanghellini+ 1998)
J/MNRAS/458/3786 : CSS and GPS radio sources sample (Jeyakumar, 2016)
J/MNRAS/485/2710 : Radio jets associated with galactic outflows (Jarvis+, 2019)
J/ApJ/836/174 : Extragalactic peaked-spectrum radio sources
(Callingham+, 2017)
VIII/100 : GaLactic and Extragalactic All-sky MWA survey
(Hurley-Walker+, 2016)
VIII/92 : The FIRST Survey Catalog, Version 2014Dec17 (Helfand+ 2015)
II/311 : WISE All-Sky Data Release (Cutri+ 2012)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Source Source object name (Source)
13 A1 --- n_Source Note on typical source objects (G1)
15- 16 I2 h RAh Right ascension (J2000)
18- 19 I2 min RAm Right ascension (J2000)
21- 25 F5.2 s RAs Right ascension (J2000)
27 A1 --- DE- Declination sign (J2000)
28- 29 I2 deg DEd Declination (J2000)
31- 32 I2 arcmin DEm Declination (J2000)
34- 38 F5.2 arcsec DEs Declination (J2000)
40- 43 F4.2 --- z Redshift (z)
45- 52 F8.2 mJy/beam S1.4 ? Peak flux per beam area derived by fitting
an elliptical Gaussian model to the source
from FIRST survey at 1.4 GHz in the L-band
(PeakFlux) (G2)
54- 61 F8.2 mJy I1.4 ? Intensity flux derived by fitting an
elliptical Gaussian model to the source from
FIRST survey at 1.4 GHz in the L-band
(Int.Flux) (G2)
63- 67 F5.2 mag W1-W2 WISE colours from MIR centered at 3.4 µm
and 4.6 µm (W1-W2)
69- 72 F4.2 mag W2-W3 ? WISE colours from MIR centered at
4.6 µm and 12 µm (W2-W3)
74 A1 --- AGN [S W] AGN classification of the source
according to the position in the WISE colour
diagram see section 6 MID-Infrared
photometry (AGNclass) (1)
--------------------------------------------------------------------------------
Note (1): AGN classification is as follows:
S = strong AGN morphological class, 41 sources in our sample
W = weak AGN morphological class, 43 sources in our sample
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 15 A15 --- Source Source object name (Source)
17 A1 --- n_Source Note on typical source objects (G1)
19- 20 I2 h RAh Right ascension (J2000)
22- 23 I2 min RAm Right ascension (J2000)
25- 30 F6.3 s RAs Right ascension (J2000)
32 A1 --- DE- Declination sign (J2000)
33- 34 I2 deg DEd Declination (J2000)
36- 37 I2 arcmin DEm Declination (J2000)
39- 43 F5.2 arcsec DEs Declination (J2000)
45- 48 F4.2 --- z Redshift (z)
50- 56 F7.2 mJy/beam S1.4 Peak flux per beam area derived by fitting
an elliptical Gaussian model to the source
from FIRST survey at 1.4 GHz in the L-band
(PeakFlux) (G2)
58- 64 F7.2 mJy I1.4 Intensity flux derived by fitting an
elliptical Gaussian model to the source from
FIRST survey at 1.4 GHz in the L-band
(Int.Flux) (G2)
66- 69 F4.2 mag W1-W2 WISE colours from MIR centered at 3.4 µm
and 4.6 µm (W1-W2)
71- 74 F4.2 mag W2-W3 WISE colours from MIR centered at 4.6 µm
and 12 µm (W2-W3)
76 A1 --- AGN [S W] AGN classification of the source
according to the position in the WISE colour
diagram see section 6 MID-Infrared
photometry (AGNclass) (1)
--------------------------------------------------------------------------------
Note (1): AGN classification is as follows:
S = strong AGN morphological class, 13 sources in our sample
W = weak AGN morphological class, 9 sources in our sample
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Source Source object name (Object)
13- 17 F5.2 % FC Percentage contribution of Featureless
Continuum to SSPs (FC)
19- 23 F5.2 % xy Percentage xy(t ≤ 50 Myr) Light-weighted
young age contribution to SSPs (xy)
25- 29 F5.2 % xi Percentage xi(50 Myr ≤ t ≤ 2 Gyr)
Light-weighted intermediate age contribution
to SSPs (xi)
31- 35 F5.2 % xo Percentage xo(t > 2 Gyr) Light-weighted
old age contribution to SSPs (xo)
37- 40 F4.2 % my Percentage my(t ≤ 50 Myr) Mass-weighted
young age contribution to SSPs (my)
42- 46 F5.2 % mi Percentage mi(50 Myr ≤ t ≤ 2 Gyr)
Mass-weighted intermediate age contribution
to SSPs (mi)
48- 52 F5.2 % mo Percentage mo(t > 2 Gyr) Mass-weighted old
age contribution to SSPs (mo)
54- 58 F5.2 mag Av Dust extinction in V band (AV)
60- 63 F4.2 [yr] logt*L The light-weighted mean age (<logt*>L) (G3)
65- 69 F5.2 [yr] logt*M The mass-weighted mean age ( (<logt*>M)
(G3)
71- 74 F4.2 --- Z*L The light-weighted mean metallicity (<Z*>L)
(G3)
76- 79 F4.2 --- Z*M The mass-weighted mean metallicity (<Z*>M)
(G3)
81- 85 F5.2 [Msun] logM* Logarithm of the present stellar mass of the
galaxy (M*) (G4)
87- 91 F5.2 Msun/yr SFR* Logarithm of the Star formation rate over
the last 50 Myr (SFR*) (G4)
93- 97 F5.2 [W/Hz] logL1.4 Radio uminosity estimated assuming
H0 = 69.8 km/s/Mpc as proposed by
Freedman et al. 2019ApJ...882...34F 2019ApJ...882...34F Hubble
Program (LogLR)
99- 101 A3 --- MType Morphology type determined visually from
SDSS images (Morph) (1)
--------------------------------------------------------------------------------
Note (1): Morphology class are as follows:
E = Elliptical galaxy, 15 sources in our sample
I/M = Irregular or merger galaxy, 12 sources in our sample
P = Point source galaxy, 13 sources in our sample
S = Spiral galaxy, 18 sources in our sample
Because the stellar population of a galaxy is very dependent on the
morphology (e.g. Cano-Diaz et al. 2019MNRAS.488.3929C 2019MNRAS.488.3929C), we obtained
SDSS images and performed a visual classification of these objects.
This classification was made independently by three distinct
classifiers. When at least two of them agreed, the morphological
class was established. For objects where the three classifiers
disagreed, each classifier explained his choice and tried to convince
one of the other two into changing their classification.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 15 A15 --- Source Source object name (Object)
17- 21 F5.2 % FC Percentage contribution of Featureless
Continuum to SSPs (FC)
23- 27 F5.2 % xy Percentage xy(t ≤ 50 Myr) Light-weighted
young age contribution to SSPs (xy)
29- 33 F5.2 % xi Percentage xi(50 Myr ≤ t ≤ 2 Gyr)
Light-weighted intermediate age contribution
to SSPs (xi)
35- 39 F5.2 % xo Percentage xo(t > 2 Gyr) Light-weighted
old age contribution to SSPs (xo)
41- 44 F4.2 % my Percentage my(t ≤ 50 Myr) Mass-weighted
young age contribution to SSPs (my)
46- 50 F5.2 % mi Percentage mi(50 Myr ≤ t ≤ 2 Gyr)
Mass-weighted intermediate age contribution
to SSPs (mi)
52- 57 F6.2 % mo Percentage mo(t > 2 Gyr) Mass-weighted old
age contribution to SSPs (mo)
59- 62 F4.2 mag Av Dust extinction in V band (AV)
64- 67 F4.2 [yr] logt*L The light-weighted mean age
(<logt*>L) (G3)
69- 73 F5.2 [yr] logt*M The mass-weighted mean age ( (<logt*>M)
(G3)
75- 78 F4.2 --- Z*L The light-weighted mean metallicity
(<Z*>L) (G3)
80- 83 F4.2 --- Z*M The mass-weighted mean metallicity (<Z*>M)
(G3)
85- 89 F5.2 [Msun] logM* Logarithm of the present stellar mass of the
galaxy (M*) (G4)
91- 94 F4.2 Msun/yr SFR* Logarithm of the Star formation rate over
the last 50 Myr (SFR*) (G4)
96- 100 F5.2 [W/Hz] logL1.4 Radio uminosity estimated assuming
H0 = 69.8 km/s/Mpc as proposed by
Freedman et al. 2019ApJ...882...34F 2019ApJ...882...34F Hubble
Program (LogLR)
102- 104 A3 --- MType Morphology type determined visually from
SDSS images (Morph) (1)
--------------------------------------------------------------------------------
Note (1): Morphology class are as follows:
I/M = Irregular or merger galaxy, 4 sources in our sample
P = Point source galaxy, 8 sources in our sample
S = Spiral galaxy, 2 sources in our sample
Because the stellar population of a galaxy is very dependent on the
morphology (e.g. Cano-Diaz et al. 2019MNRAS.488.3929C 2019MNRAS.488.3929C), we obtained
SDSS images and performed a visual classification of these objects.
This classification was made independently by three distinct
classifiers. When at least two of them agreed, the morphological
class was established. For objects where the three classifiers
disagreed, each classifier explained his choice and tried to convince
one of the other two into changing their classification.
--------------------------------------------------------------------------------
Global notes:
Note (G1): The * symbol depicts the objects dominated by a non-stellar
continuum. These objects were removed from the stellar population
synthesis and will be analyzed in a forthcoming paper.
Note (G2): On the other hand, some sources are outside the FIRST survey coverage
area and, in these cases, the integrated flux was obtained from the
NRAO VLA Sky Survey (NVSS, 1.4GHz NRAO VLA Sky Survey Condon et al.
1998AJ....115.1693C 1998AJ....115.1693C, Cat. VIII/65). These name sources are
B2-0026+34, 3C 049, SDSSJ08382, SDSSJ08485, SDSSJ08531, 3C 237,
3C 268.3, B3-1402+415, B2-1542+39, and SDSSJ15504.
Note (G3): As explained in the section 3.1 Mean stellar age and metallicity,
the mean stellar age and metallicity are fundamental
parameters to describe the mixture of stellar population in a galaxy.
They can be defined in terms of light fraction or of mass fraction as
written in the equations 3 and 4 with light fraction population
vector components xj or with mass fraction population vector
components mj.
Note (G4): As seen in the section 4.2 Star formation rate and stellar mass, M*
and SFR are computed from the stellar population fitting process.
The equations 5 and 6 show details of these computations, then the
corrected M* and SFR are given by the expressions 7.
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History:
From electronic version of the journal
(End) Luc Trabelsi [CDS] 15-Jan-2025