J/MNRAS/458/2221 ATLAS3D Project. XXXI (Nyland+, 2016)
The ATLAS3D Project.
XXXI. Nuclear radio emission in nearby early-type galaxies.
Nyland K., Young L.M., Wrobel J.M., Sarzi M., Morganti R., Alatalo K.,
Blitz L., Bournaud F., Bureau M., Cappellari M., Crocker A.F., Davies R.L.,
Davis T.A., De Zeeuw P.T., Duc P.-A., Emsellem E., Khochfar S.,
Krajnovic D., Kuntschner H., McDermid R.M., Naab T., Oosterloo T.,
Scott N., Serra P., Weijmans A.-M.
<Mon. Not. R. Astron. Soc., 458, 2221-2268 (2016)>
=2016MNRAS.458.2221N 2016MNRAS.458.2221N (SIMBAD/NED BibCode)
ADC_Keywords: Galaxy catalogs ; Galaxies, nearby ; Radio continuum ; Morphology
Keywords: galaxies: active - galaxies: nuclei - radio continuum: galaxies
Abstract:
We present the results of a high-resolution, 5GHz, Karl G. Jansky
Very Large Array study of the nuclear radio emission in a
representative subset of the atlas3D survey of early-type galaxies
(ETGs). We find that 51±4 per cent of the ETGs in our sample contain
nuclear radio emission with luminosities as low as 1018W/Hz.
Most of the nuclear radio sources have compact (≲25-110pc)
morphologies, although ∼10 per cent display multicomponent core+jet
or extended jet/lobe structures. Based on the radio continuum
properties, as well as optical emission line diagnostics and the
nuclear X-ray properties, we conclude that the majority of the central
5GHz sources detected in the atlas3D galaxies are associated with
the presence of an active galactic nucleus (AGN). However, even at
subarcsecond spatial resolution, the nuclear radio emission in some
cases appears to arise from low-level nuclear star formation rather
than an AGN, particularly when molecular gas and a young central
stellar population is present. This is in contrast to popular
assumptions in the literature that the presence of a compact,
unresolved, nuclear radio continuum source universally signifies the
presence of an AGN. Additionally, we examine the relationships between
the 5 GHz luminosity and various galaxy properties including the
molecular gas mass and - for the first time - the global kinematic
state. We discuss implications for the growth, triggering, and
fuelling of radio AGNs, as well as AGN-driven feedback in the
continued evolution of nearby ETGs.
Description:
The 125 ETGs included in our new high-resolution 5GHz VLA
observations are selected from the atlas3D survey (Paper I, 2011, Cat.
J/MNRAS/413/813). A list of these ETGs is provided in Table A1. Since
one of our goals is to probe the relationship between LLAGN-driven
radio emission and molecular gas content, we included as many of the
56 IRAM single-dish CO detections as possible. We excluded only four
CO-detected ETGs from our new VLA observations (NGC 3245, NGC 4203,
NGC 4476, and NGC 5866). NGC 4476 was excluded due to its proximity
(12.6 arcmin) to the bright radio source hosted by NGC 4486 (M87). The
other three CO-detected sources (NGC 3245, NGC 4203, and NGC 5866)
were not included in our new observations based on the availability of
archival VLA data with similar properties.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 76 125 VLA 5GHz sample and flux density measurements
tablea2.dat 108 53 5GHz spatial parameters of detections
tablea3.dat 82 16 5GHz image properties of sources with multiple
components
tablea4.dat 80 16 5GHz spatial properties of sources with
multiple components
tablea5.dat 76 29 *Archival high-resolution radio continuum data
tablea6.dat 59 148 Additional galaxy properties
tablec1.dat 55 53 Relative contour levels in the 5GHz continuum maps
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Note on tablea5.dat: The additional atlas3D galaxies included in this study with
radio continuum observations at high spatial resolution
(θFWHM≲1-arcsec) and near a frequency of 5GHz in the literature.
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See also:
J/MNRAS/413/813 : ATLAS3D project. I (Cappellari+, 2011)
J/MNRAS/414/888 : ATLAS3D project. III (Emsellem+, 2011)
J/MNRAS/414/940 : ATLAS3D project. IV (Young+, 2011)
J/MNRAS/416/1680 : ATLAS3D project. VII (Cappellari+, 2011)
J/MNRAS/433/2812 : ATLAS3D project. XXIII (Krajnovic+, 2013)
J/MNRAS/446/120 : ATLAS3D project. XXIX (Duc+, 2015)
J/MNRAS/448/3484 : ATLAS3D Project. XXX (McDermid+, 2015)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1 A1 --- f_Name [a] Flag on Name (1)
2- 10 A9 --- Name Galaxy name
11 A1 --- n_Name [b] Note on Name (1)
13- 16 F4.1 Mpc Dist Atlas3D distance (Paper I,
Cappellari et al. 2011, Cat. J/MNRAS/413/813)
18 I1 --- Virgo [0/1] Virgo membership
20 A1 --- F/S kinematic class (Paper III, Emsellem et al.,
2011, Cat. J/MNRAS/414/888) (G1)
22- 26 F5.2 [Msun] logMJAM ?=- Dynamically modelled stellar mass
(Paper XV, Cappellari et al.,
2013MNRAS.432.1709C 2013MNRAS.432.1709C)
28 A1 --- l_logMH2 Limit flag on logMH2
29- 32 F4.2 [Msun] logMH2 Molecular hydrogen mass (Paper IV,
Young et al., 2011, Cat. J/MNRAS/414/940)
34 A1 --- l_SW91 Limit flag on SW91
35- 38 F4.1 mJy SW91 ?=- Integrated flux density from the 5GHz
study of nearby ETGs carried-out by
Wrobel & Heeschen (1991AJ....101..148W 1991AJ....101..148W)
at 5 arcsec resolution
40- 42 F3.1 mJy e_SW91 ? rms uncertainty on SW91
44- 45 I2 uJy/beam rms ?=- Average rms noise (3)
47 A1 --- l_Speak Limit flag on Speak (3)
48- 52 F5.2 mJy/beam Speak ?=- Peak flux density (3)
54- 57 F4.2 mJy/beam e_Speak ? rms uncertainty on Speak (3)
60- 64 F5.2 mJy Sint ?=- Integrated flux density (3)(4)
66- 69 F4.2 mJy e_Sint ? rms uncertainty on Sint (3)
71 A1 --- l_logL Limit flag on logL (3)
72- 76 F5.2 [W/Hz] logL ?=- 5 GHz radio luminosity (3)(5)
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Note (1): Notes as follows:
a = Extended source not well represented by a single two-dimensional Gaussian
model. The peak and integrated flux densities were calculated by drawing
an aperture at the 3xrms level around the source in the casa Viewer
and then using the IMSTAT task to determine the flux parameters.
b = Multicomponent source. The integrated flux density refers to the sum of
all components. See Table A3 for information on the properties of
individual components.
Note (3): refer to data from our new high-resolution 5GHz VLA observations.
Note (4): Note that measurements of the integrated flux density are only given
for sources that are formally resolved by JMFIT.
Note (5): When an integrated flux density is given, L is based on the integrated
flux density. If only a peak flux density is given (either a measurement or
an upper limit), then L is based on the peak flux density.
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1 A1 --- f_Name [a] Flag on Name (1)
2- 10 A9 --- Name galaxy name
11 A1 --- n_Name [b] Note on Name (1)
13 A1 --- Morph [RU] Radio morphology based on the output of
the JMFIT task in aips (G2)
15- 16 I2 h RAh Right ascension (J2000) of the emission at
the peak flux density (G3)
18- 19 I2 min RAm Right ascension (J2000) of the emission
at the peak flux density (G3)
21- 26 F6.3 s RAs Right ascension (J2000) of the emission
at the peak flux density (G3)
28 A1 --- DE- Declination sign (J2000) of the central
position of the emission (G3)
29- 30 I2 deg DEd Declination of the central position of
the emission (G3)
32- 33 I2 arcmin DEm Declination of the central position of
the emission (G3)
35- 39 F5.2 arcsec DEs Declination of the central position of
the emission (G3)
41- 44 F4.2 arcsec Beam1 Angular dimension of the synthesized beam
(major axis)
45 A1 --- --- [x]
46- 49 F4.2 arcsec Beam2 Angular dimension of the synthesized beam
(minor axis)
51- 56 F6.2 deg BPA Beam position angle, measured anti clockwise
from North
58 A1 --- l_thetaM Limit flag on thetaM
59- 63 F5.2 arcsec thetaM Radius upper limit or major axis of the
emission (4)
65- 68 F4.2 arcsec e_thetaM ? rms uncertainty on thetaM
69 A1 --- --- [x]
70- 73 F4.2 arcsec thetam ? Minor axis of the emission (4)
75- 78 F4.2 arcsec e_thetam ? rms uncertainty on thetam
80- 85 F6.2 deg PA ?=- Position angle of the emission from JMFIT
87- 91 F5.2 deg e_PA ? rms uncertainty on PA
93 A1 --- l_Maj Limit flag on Maj
94-100 F7.2 pc Maj Linear radius upper limit or major axis of
the emission in physical units
101 A1 --- --- [x]
102-108 F7.2 pc Min ? Linear minor axis of the emission
in physical units
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Note (1): Notes as follows:
a = Extended source not well-represented by a two-dimensional Gaussian model.
The source dimensions were measured using the casa Viewer.
b = Multicomponent source. The spatial dimensions refer to the source closest
to the centre of the galaxy based on ground-based optical measurements.
See Table A4 for information on individual components.
Note (4): Angular dimensions of the emission (major x minor axis). If JMFIT
was only able to deconvolve the major axis of the source, then the minor
axis extent is given as 0.00. The errors are from JMFIT and are only given
if the emission was successfully deconvolved in at least one dimension and
categorized as resolved. For non-Gaussian sources, source dimensions were
determined using the casa Viewer and no error is reported.
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Byte-by-byte Description of file: tablea3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Name Galaxy name
10- 28 A19 --- Comp Radio component name. The brightest
component in each galaxy is listed first
30- 31 I2 h RAh Right ascension (J2000) at the location of
the peak flux density
33- 34 I2 min RAm Right ascension (J2000) at the location of
the peak flux density
36- 41 F6.3 s RAs Right ascension (J2000) at the location of
the peak flux density
43 A1 --- DE- Declination sign (J2000) at the location of
the peak flux density
44- 45 I2 deg DEd Declination (J2000) at the location of the
peak flux density
47- 48 I2 arcmin DEm Declination (J2000) at the location of the
peak flux density
50- 54 F5.2 arcsec DEs Declination (J2000) at the location of the
peak flux density
56- 60 F5.2 mJy/beam Speak Peak flux density
62- 65 F4.2 mJy/beam e_Speak rms uncertainty on Speak
67- 71 F5.2 mJy Sint ?=- Integrated flux density
73- 76 F4.2 mJy e_Sint ? rms uncertainty on Sint
78- 82 F5.2 [W/Hz] logL Radio luminosity (1)
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Note (1): When an integrated flux density is given, L is based on the integrated
flux density. If only a peak flux density is given (either a measurement or
an upper limit), then L is based on the peak flux density.
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Byte-by-byte Description of file: tablea4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Name Galaxy name
10- 28 A19 --- Comp Radio component name. The brightest component
in each galaxy is listed first
30 A1 --- Morph [RU] Radio morphology as reported by JMFIT (G2)
32 A1 --- l_thetaM Limit flag on thetaM
33- 36 F4.2 arcsec thetaM Radius upper limit or major axis of the
emission (G3)
38- 41 F4.2 arcsec e_thetaM ? rms uncertainty on thetaM
42 A1 --- --- [x]
43- 46 F4.2 arcsec thetam ? Minor axis of the emission (G3)
48- 51 F4.2 arcsec e_thetam ? rms uncertainty on thetam
53- 58 F6.2 deg PA ?=- Position angle of the emission from JMFIT
60- 64 F5.2 deg e_PA ? rms uncertainty on PA
66 A1 --- l_Maj Limit flag on Maj
67- 73 F7.2 pc Maj Linear radius upper limit or major axis of
the emission in physical units
74 A1 --- --- [x]
75- 80 F6.2 pc Min ? Linear minor axis of the emission in
physical units
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Byte-by-byte Description of file: tablea5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Name Galaxy name
9 A1 --- n_Name [abc] Note on Name (1)
11- 14 F4.1 Mpc Dist Atlas3D distance (Paper I,
Cappellari et al. 2011, Cat. J/MNRAS/413/813))
16 I1 --- Virgo [0/1] Virgo membership
18 A1 --- F/S Kinematic class (Paper III, Emsellem et al.,
2011, Cat. J/MNRAS/414/888) (G1)
20- 24 F5.2 [Msun] logMJAM ?=- Dynamically modelled stellar mass
(Paper XV, Cappellari et al.,
2013MNRAS.432.1709C 2013MNRAS.432.1709C))
26 A1 --- l_logMH2 Limit flag on logMH2
27- 30 F4.2 [Msun] logMH2 Molecular hydrogen mass (Paper IV,
Young et al., 2011, Cat. J/MNRAS/414/940)
32- 36 F5.2 mJy SW91 ?=- Integrated flux density from the 5GHz study
of nearby ETGs carried-out by Wrobel &
Heeschen (1991AJ....101..148W 1991AJ....101..148W)
at 5 arcsec resolution
38- 41 F4.2 mJy e_SW91 ? rms uncertainty on SW91
43- 46 F4.1 GHz Freq Original observing frequency
48- 52 F5.3 arcsec Res Approximate synthesized beam major axis
54 A1 --- l_S5GHz Limit flag on S5GHz
55- 61 F7.2 mJy S5GHz ?=- Integrated nuclear flux density at 5GHz (2)
63- 67 F5.2 mJy/beam e_S5GHz ? rms uncertainty on S5GHz
69 A1 --- l_logL Limit flag on logL
70- 74 F5.2 [W/Hz] logL ?=- Nuclear radio luminosity at 5GHz
76 A1 --- Ref References (3)
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Note (1): Notes as follows:
a = For NGC 4261, a milliarcsecond-scale spatial resolution VLBA radio flux
density is reported.
b = Although NGC 4697 and NGC 4477 were included in our new 5GHz VLA
observations, the sensitivity and quality of the final images were not
sufficient to detect them. We include a literature detection of NGC 4697
(Wrobel et al., 2008ApJ...686..838W 2008ApJ...686..838W) as well as a detection of NGC 4477
from project 12B-191 based on our own independent analysis.
c = For NGC 5846, the flux density has been extrapolated from to 5GHz using
a spectral index of -0.03. This spectral index was calculated based on
high-resolution measurements at 8.4 and 15GHz in Filho et al.
(2004A&A...418..429F 2004A&A...418..429F) and Nagar et al. (2005, Cat. J/A+A/435/521),
respectively.
Note (2): For measurements originally at frequencies other than 5GHz, the flux
densities listed here have been scaled to 5GHz using the source spectral
index reported in the literature. If no such spectral index information is
available, the flux density is scaled to 5GHz assuming a flat spectral index
of α=-0.1, where S~ν^α. Uncertainties are reported as given in
the literature when possible. If errors were not reported in the literature,
we estimate the flux density uncertainty as described in Section 5.
Note (3): References as follows:
1 = Filho, Barthel & Ho (2006A&A...451...71F 2006A&A...451...71F)
2 = Filho et al. (2004A&A...418..429F 2004A&A...418..429F)
3 = Kharb et al. (2012AJ....143...78K 2012AJ....143...78K)
4 = Nagar et al. (2001ApJ...559L..87N 2001ApJ...559L..87N)
5 = Nagar et al. (2005, Cat. J/A+A/435/521)
6 = Project 12B-191
7 = Wrobel et al. (2008ApJ...686..838W 2008ApJ...686..838W)
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Byte-by-byte Description of file: tablea6.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 A9 --- Name Galaxy name
11- 14 F4.2 [Msun] logMBH Black hole mass
16- 17 I2 --- r_logMBH ? Black hole mass reference (1)
19 A1 --- l_logLX Limit flag on logLX
20- 24 F5.2 [10-7W] logLX ?=- 2-10keV X-ray luminosity from
the literature
26- 27 I2 --- r_logLX ?=- X-ray luminosity reference (2)
29 A1 --- l_log(LBol/LEdd) Limit flag on log(LBol/LEdd)
30- 34 F5.2 --- log(LBol/LEdd) ?=- Eddington ratio (3)
36 A1 --- l_logRX Limit flag on logRX
37- 41 F5.2 [-] logRX ?=- Radio-X-ray ratio as defined in
Terashima & Wilson
(2003ApJ...583..145T 2003ApJ...583..145T)
43- 47 F5.2 [10-7J] logL[OIII] ?=- Nuclear [OIII] luminosity
49- 53 F5.2 0.1nm EW[OIII] ?=- Nuclear [OIII] equivalent width
55- 59 A5 --- Class Nuclear emission line classification
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Note (1): for galaxies with dynamical mass estimates available in the
literature. If no reference is given, the black hole mass is estimated from
the MBH-σ* relation (McConnell & Ma, 2013ApJ...764..184M 2013ApJ...764..184M).
References as follows:
1 = Krajnovic et al. (2002A&A...390..423K 2002A&A...390..423K)
2 = Schulze & Gebhardt (2011ApJ...729...21S 2011ApJ...729...21S)
3 = Bower et al. (2001ApJ...550...75B 2001ApJ...550...75B)
4 = Barth et al. (2001ApJ...555..685B 2001ApJ...555..685B)
5 = van den Bosch & de Zeeuw (2010MNRAS.401.1770V 2010MNRAS.401.1770V)
6 = Nowak et al. (2010MNRAS.403..646N 2010MNRAS.403..646N)
7 = Gultekin et al. (2009ApJ...695.1577G 2009ApJ...695.1577G)
8 = Walsh et al. (2012ApJ...753...79W 2012ApJ...753...79W)
9 = Ferrarese, Ford & Jaffe (1996ApJ...470..444F 1996ApJ...470..444F)
10 = Walsh, Barth & Sarzi (2010ApJ...721..762W 2010ApJ...721..762W)
11 = Sarzi et al. (2001ApJ...550...65S 2001ApJ...550...65S)
12 = Rusli et al. (2013AJ....146..160R 2013AJ....146..160R)
13 = Gebhardt et al. (2011ApJ...729..119G 2011ApJ...729..119G)
14 = Davis et al. (2014MNRAS.444.3427D 2014MNRAS.444.3427D)
Note (2): Details on the computation of this parameter are provided in
Section 6.3.2.
Note (3): References as follows:
15 = Pellegrini (2010ApJ...717..640P 2010ApJ...717..640P)
16 = Miller et al. (2012ApJ...747...57M 2012ApJ...747...57M)
17 = Kharb et al. (2012AJ....143...78K 2012AJ....143...78K)
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Byte-by-byte Description of file: tablec1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 A9 --- Name Galaxy name
11- 12 I2 uJy/beam rms rms noise
14- 55 A42 --- RC Relative contours
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Global notes:
Note (G1): F/S flag as follows:
F = fast rotator
S = slow rotator
Note (G2): Radio morphology flag as follows:
R = resolved
U = unresolved
Note (G3): For sources with multiple components denoted by a b symbol, the
position listed is that of the component closest to the optical position of
the nucleus.
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History:
From electronic version of the journal
References:
Cappellari et al., Paper I 2011MNRAS.413..813C 2011MNRAS.413..813C, Cat. J/MNRAS/413/813
Krajnovic et al., Paper II 2011MNRAS.414.2923K 2011MNRAS.414.2923K
Emsellem et al., Paper III 2011MNRAS.414..888E 2011MNRAS.414..888E, Cat. J/MNRAS/414/888
Young et al., Paper IV 2011MNRAS.414..940Y 2011MNRAS.414..940Y, Cat. J/MNRAS/414/940
Davis et al., Paper V 2011MNRAS.414..968D 2011MNRAS.414..968D
Bois et al., Paper VI 2011MNRAS.416.1654B 2011MNRAS.416.1654B
Cappellari et al., Paper VII 2011MNRAS.416.1680C 2011MNRAS.416.1680C, Cat. J/MNRAS/416/1680
Khochfar et al., Paper VIII 2011MNRAS.417..845K 2011MNRAS.417..845K
Duc et al., Paper IX 2011MNRAS.417..863D 2011MNRAS.417..863D
Davis et al., Paper X 2011MNRAS.417..882D 2011MNRAS.417..882D
Crocker et al., Paper XI 2012MNRAS.421.1298C 2012MNRAS.421.1298C
Lablanche et al., Paper XII 2012MNRAS.424.1495L 2012MNRAS.424.1495L
Serra et al., Paper XIII 2012MNRAS.422.1835S 2012MNRAS.422.1835S
Krajnovic et al., Paper XIV 2013MNRAS.432.1768K 2013MNRAS.432.1768K
Cappellari et al., Paper XV 2013MNRAS.432.1709C 2013MNRAS.432.1709C
Bayet et al., Paper XVI 2013MNRAS.432.1742B 2013MNRAS.432.1742B
Krajnovic et al., Paper XVII 2013MNRAS.432.1768K 2013MNRAS.432.1768K
Alatalo et al., Paper XVIII 2013MNRAS.432.1796A 2013MNRAS.432.1796A
Sarzi et al., Paper XIX 2013MNRAS.432.1845S 2013MNRAS.432.1845S
Cappellari et al., Paper XX 2013MNRAS.432.1862C 2013MNRAS.432.1862C
Scott et al., Paper XXI 2013MNRAS.432.1894S 2013MNRAS.432.1894S
Martig et al., Paper XXII 2013MNRAS.432.1914M 2013MNRAS.432.1914M
Krajnovic et al., Paper XXIII 2013MNRAS.433.2812K 2013MNRAS.433.2812K, Cat. J/MNRAS/433/2812
Davis et al., Paper XXIV 2013MNRAS.429..534D 2013MNRAS.429..534D
Cappellari et al., Paper XXV 2013MNRAS.432.1709C 2013MNRAS.432.1709C
Bayet et al., Paper XXVI 2013MNRAS.432.1742B 2013MNRAS.432.1742B
Krajnovic et al., Paper XXVII 2013MNRAS.432.1768K 2013MNRAS.432.1768K
Alatalo et al., Paper XXVIII 2013MNRAS.432.1796A 2013MNRAS.432.1796A
Duc et al., Paper XXIX 2015MNRAS.446..120D 2015MNRAS.446..120D
McDermid et al., Paper XXX 2015MNRAS.448.3484M 2015MNRAS.448.3484M, Cat. J/MNRAS/448/3484
(End) Patricia Vannier [CDS] 16-Nov-2017