J/MNRAS/485/2710 Radio jets associated with galactic outflows (Jarvis+, 2019)
Prevalence of radio jets associated with galactic outflows and feedback from
quasars.
Jarvis M.E., Harrison C.M., Thomson A.P., Circosta C., Mainieri V.,
Alexander D.M., Edge A.C., Lansbury G.B., Molyneux S.J., Mullaney J.R.
<Mon. Not. R. Astron. Soc., 485, 2710-2730 (2019)>
=2019MNRAS.485.2710J 2019MNRAS.485.2710J (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, radio ; Active gal. nuclei ; QSOs ; Radio sources
Keywords: galaxy: evolution - galaxies: active - galaxies: jets -
quasars: general
Abstract:
We present 1-7GHz high-resolution radio imaging (VLA and e-MERLIN) and
spatially resolved ionized gas kinematics for 10 z<0.2 type 2
'obscured' quasars (log[LAGN/erg.s-1]≳45) with moderate radio
luminosities (log[L1.4GHz/W.Hz-1]=23.3-24.4). These targets were
selected to have known ionized outflows based on broad [OIII]
emission-line components (full width at half-maximum∼800-1800km/s).
Although 'radio-quiet' and not 'radio AGN' by many traditional
criteria, we show that for nine of the targets, star formation likely
accounts for ~<10 per cent of the radio emission. We find that ∼80-90
per cent of these nine targets exhibit extended radio structures on
1-25kpc scales. The quasars' radio morphologies, spectral indices, and
position on the radio size-luminosity relationship reveals that these
sources are consistent with being low power compact radio galaxies.
Therefore, we favour radio jets as dominating the radio emission in
the majority of these quasars. The radio jets we observe are
associated with morphologically and kinematically distinct features in
the ionized gas, such as increased turbulence and outflowing bubbles,
revealing jet-gas interaction on galactic scales. Importantly, such
conclusions could not have been drawn from current low-resolution
radio surveys such as FIRST. Our observations support a scenario where
compact radio jets, with modest radio luminosities, are a crucial
feedback mechanism for massive galaxies during a quasar phase.
Description:
In this work, we focus on 10 type 2 ('obscured') z<0.2AGN, which have
quasar-like luminosities (i.e. L[OIII]>1042erg/s; Reyes et al.
2008AJ....136.2373R 2008AJ....136.2373R, Cat. J/AJ/136/2373). These were originally
selected by Harrison et al. (2014MNRAS.441.3306H 2014MNRAS.441.3306H) from our parent
sample of 24264 z<0.4 spectroscopically identified AGN presented in
Mullaney et al. (2013MNRAS.433..622M 2013MNRAS.433..622M).
We observed with VLA under two proposals: programme 13B-127, with
observations carried out on 2013 December 1-2014 May 13 and programme
16A-182 with observations carried out on 2016 May 30-2017 January 20.
For 13B-127, we observed nine targets, from our primary sample of 10,
in four configuration-frequency combinations: (1) A-array in L band
(1-2GHz; ∼1.3arcsec resolution); (2) A-array in C band (4-8GHz;
∼0.3arcsec resolution); (3) B-array in L band (1-2GHz; ∼4.3arcsec
resolution), and (4) B-array in C band (4-8GHz; ∼1.0arcsec
resolution). The final target in our primary sample (J1338+1503) was
observed by VLA during our 16A-182 project. Due to incomplete
observations, this was only observed in one configuration-frequency
combination: B-array in the C band (i.e. 4-8GHz; ∼1.0arcsec
resolution).We also gathered archival data from the UV to FIR to
derive the stellar masses.
The positions, redshifts, [OIII] properties, and radio properties
(from the FIRST Survey; Becker, White & Helfand 1995ApJ...450..559B 1995ApJ...450..559B,
Cat. VIII/92) of the 10 targets studied in this paper are presented in
Table 1. We use SED fitting from the UV to FIR to isolate the FIR
luminosity associated with star formation (LIR, SF) in addition to
getting stellar masses and AGN bolometric luminosities (LAGN) (see
Table 2). The final flux densities (or 5σ upper limits) and
their 1σ uncertainties at 1.5, 5.2, and 7.2GHz are presented in
Table 4.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 78 10 Target list and basic properties
table2.dat 95 10 Galaxy and AGN parameters derived from SED
fitting for the primary sample
table4.dat 107 52 Radio properties of the morphological structures
extracted from resolution matched e-MERLIN and
VLA images
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See also:
VIII/92 : The FIRST Survey Catalog, Version 2014Dec17 (Helfand+ 2015)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name Object name (JHHMM+DDMM)
12- 13 I2 h RAh Right ascension (J2000) (1)
15- 16 I2 min RAm Right ascension (J2000) (1)
18- 22 F5.2 s RAs Right ascension (J2000) (1)
24 A1 --- DE- Declination sign (J2000) (1)
25- 26 I2 deg DEd Declination (J2000) (1)
28- 29 I2 arcmin DEm Declination (J2000) (1)
31- 34 F4.1 arcsec DEs Declination (J2000) (1)
36- 41 F6.4 --- z Systemic redshift from the GMOS data
43- 47 F5.2 [10-7W] logLOIII Total observed [OIII] λ5007
luminosity from Mullaney et al.
(2013MNRAS.433..622M 2013MNRAS.433..622M) (2)
49- 52 I4 km/s FWHM Full width at half-maximum (FWHM) of the
broad component of the [OIII] line fit from
Mullaney et al. (2013MNRAS.433..622M 2013MNRAS.433..622M)
54- 57 F4.1 mJy S1.4 1.4GHz flux densities obtained from the
FIRST survey (Becker et al.
1995ApJ...450..559B 1995ApJ...450..559B, Cat. VIII/92)
59- 61 F3.1 mJy e_S1.4 Error on S1.4 (3)
63- 66 F4.1 W/Hz logL1.4 Rest-frame radio luminosities using a
spectral index of α=-0.7 and assuming
Sν∝να (4)
68- 72 F5.3 --- Theta Radio morphology parameter (5)
74- 78 F5.3 --- e_Theta Error on Theta
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Note (1): Coordinates taken from SDSS (DR7) (Adelman-McCarthy et al.
2009ApJS..182..543A 2009ApJS..182..543A, Cat. II/294)
Note (2): Absorption corrections would increase the values by on average 0.6dex
(with a maximum increase of 1.4dex)
Note (3): S1.4 uncertainties are defined as 3x the RMS noise of the radio image
at the source position
Note (4): We note that a range of α=-0.2 to -1.5 introduces a spread of
±0.1dex on the radio luminosity
Note (5): Sources with Theta>1.06 are classified as extended in the 1.4GHz
FIRST data (Harrison et al. 2014MNRAS.441.3306H 2014MNRAS.441.3306H)
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name Object name (JHHMM+DDMM)
12 A1 --- f_Name Flag on name (1)
14- 17 F4.1 [10-7W] logLAGN Bolometric AGN luminosity
19- 23 F5.2 [Msun] logM ? Stellar mass
25- 28 F4.2 [Msun] E_logM ? Upper error on logM
30- 33 F4.2 [Msun] e_logM ? Lower error on logM
35 A1 --- f_logM Flag on logM (2)
37- 41 F5.2 [10-7W] logLIR Infrared luminosity from star formation in
the range 8-1000µm
43- 46 F4.2 [10-7W] E_logLIR Upper error on logLIR
48- 51 F4.2 [10-7W] e_logLIR Lower error on logLIR
53- 56 F4.1 Msun/yr SFR Star formation rate
58- 61 F4.1 Msun/yr e_SFR Error on SFR
63- 65 F3.1 mJy S1.4 1.4GHz flux predicted from star formation
following the radio-LIR relation
(Bell 2003ApJ...586..794B 2003ApJ...586..794B,
Cat. J/ApJ/586/794)
67- 69 F3.1 mJy e_S1.4 Error on S1.4
71- 74 F4.1 --- perctSF ? Percentage of the FIRST luminosity
accounted for by star formation in the
radio excess sources
76- 78 F3.1 --- e_perctSF ? Error on perctSF
80- 83 F4.2 --- qIR qIR ('radio excess') parameter, where
qIR=<1.8 denotes radio excess
85- 88 F4.2 --- E_qIR Upper error on qIR
90- 93 F4.2 --- e_qIR Lower error on qIR
95 A1 --- Excess [YPN] Flag to define if the target is radio
excess (3)
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Note (1): Flag as follows:
a = These sources do not have photometric measurements at wavelengths longer
than 60µm, with J1316+1753 having no photometry above 22µm
Note (2): Flag as follows:
b = For this target, the AGN contribution is particularly high in the NIR
regime and the estimate of the stellar mass is unconstrained, with an
uncertainty larger than the parameter value itself. We therefore do not
report a value of logMsun.
Note (3): Excess as follows:
Y = radio excess
P = probably radio excess
N = not radio excess
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name Object name (JHHMM+DDMM)
12- 15 F4.1 mJy SFIRST Flux density from the FIRST survey
17- 19 F3.1 mJy e_SFIRST Error on SFIRST
21- 28 A8 --- Struc Name of structure
30 A1 --- f_Struc [ab] Flag on structure (1)
32- 53 A22 --- Interp Interpretation of structure or largest linear
size observed at that resolution in kpc
55 A1 --- f_Interp Flag on Interp (2)
57 A1 --- l_S1.5 Limit flag on S1.5
59- 63 F5.2 mJy S1.5 ? Flux density in at 1.5GHz (3)
65- 68 F4.1 mJy e_S1.5 ? Error on S1.5 (4)
70 A1 --- l_S5.2 Limit flag on S5.2
72- 76 F5.2 mJy S5.2 Flux density in at 5.2GHz (3)
78- 81 F4.2 mJy e_S5.2 ? Error on S5.2 (4)
83 A1 --- l_S7.2 Limit flag on S7.2
85- 89 F5.2 mJy S7.2 Flux density in at 7.2GHz (3)
91- 94 F4.2 mJy e_S7.2 ? Error on S7.2 (4)
96-101 F6.3 --- alpha ? Spectral index (5)
103-107 F5.3 --- e_alpha ? Error on alpha
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Note (1): Flag as follows:
a = Although this component is not detected at 5σ significance in any
individual band, it is detected in all three at 3σ resulting in a
spectral index of -0.5
b = Due to the fitting constraints needed to get this component to be well
fit by a Gaussian in all the three images, the fluxes and spectral
index for this source are unreliable
Note (2): Flag as follows:
c = We determine that HR:B is either a high S/N beam artefact or a variable
component, which then determines if LR:A is a composite or not
Note (3): 5σ upper limits are given for non-detections
Note (4): The errors given are a combination of 1σ random errors and a
10 per cent systematic
Note (5): Spectral index α defined as Sν∝να and
found by fitting a line through all detected points between 1.5 and
7.2GHz
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History:
From electronic version of the journal
(End) Ana Fiallos [CDS] 22-Sep-2022