J/MNRAS/451/2723 Low-redshift clusters in the SAMI Pilot Survey (Scott+, 2015)
The SAMI Pilot Survey: the fundamental and mass planes in three low-redshift
clusters.
Scott N., Fogarty L.M.R., Owers M.S., Croom S.M., Colless M., Davies R.L.,
Brough S., Pracy M.B., Bland-Hawthorn J., Jones D.H., Allen J.T.,
Bryant J.J., Cortese L., Goodwin M., Green A.W., Konstantopoulos I.S.,
Lawrence J.S., Richards S., Sharp R.
<Mon. Not. R. Astron. Soc., 451, 2723-2734 (2015)>
=2015MNRAS.451.2723S 2015MNRAS.451.2723S (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Galaxy catalogs ; Redshifts ; Morphology ;
Velocity dispersion ; Surveys
Keywords: galaxies: elliptical and lenticular, cD - galaxies: evolution -
galaxies: formation
Abstract:
Using new integral field observations of 106 galaxies in three nearby
clusters, we investigate how the intrinsic scatter of the Fundamental
Plane depends on the way in which the velocity dispersion and effective
radius are measured. Our spatially resolved spectroscopy, combined with
a cluster sample with negligible relative distance errors, allows us
to derive a Fundamental Plane with minimal systematic uncertainties.
From the apertures we tested, we find that velocity dispersions measured
within a circular aperture with radius equal to one effective radius
minimizes the intrinsic scatter of the Fundamental Plane. Using simple
yet powerful Jeans dynamical models, we determine dynamical masses for
our galaxies. Replacing luminosity in the Fundamental Plane with dynamical
mass, we demonstrate that the resulting Mass Plane has further reduced
scatter, consistent with zero intrinsic scatter. Using these dynamical
models, we also find evidence for a possibly non-linear relationship
between dynamical mass-to-light ratio and velocity dispersion.
Description:
In this study, we use Integral Field Spectrograph (IFS) observations from
the Sydney-AAO Multi-Object IFS (SAMI) Pilot Survey (Fogarty et al.
2014MNRAS.443..485F 2014MNRAS.443..485F) to study the Fundamental Plane (FP) and Mass Plane (MP)
in three clusters at redshift ∼0.05. The SAMI Pilot Survey is a study
of 106 galaxies in three z∼0.05 clusters using the SAMI instrument
(Croom et al. 2012MNRAS.421..872C 2012MNRAS.421..872C) on the 3.9m Anglo-Australian Telescope
at Siding Spring Observatory. The pilot survey is a precursor to the SAMI
Galaxy Survey (SGS; Bryant et al. 2015MNRAS.447.2857B 2015MNRAS.447.2857B) of ∼3400 galaxies
with the same instrument.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 23 3 Properties of the three clusters from which our
sample is drawn
tablea1.dat 74 105 Fundamental Plane (FP) parameters and other
properties of the 106 galaxies in our sample
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See also:
V/147 : The SDSS Photometric Catalogue, Release 12 (Alam+, 2015)
J/AJ/111/42 : Galaxies in Abell 168 (Tomita+ 1996)
J/A+AS/128/67 : BVR photometry of Abell 85 (Slezak+ 1998)
J/A+AS/129/281 : ABCG 85 velocities catalogue (Durret+ 1998)
J/A+A/495/379 : Optical radial velocities in A85 (Bravo-Alfaro+, 2009)
J/MNRAS/446/1567 : SAMI Galaxy Survey: EDR (Allen+, 2015)
J/MNRAS/454/2050 : SAMI Pilot Survey (Fogarty+, 2015)
J/MNRAS/456/1299 : SAMI Galaxy Survey: gas streaming (Cecil+, 2016)
J/MNRAS/458/1590 : Deep spectroscopy of Abell 85 (Agulli+, 2016)
J/ApJ/835/104 : SAMI Galaxy Survey: rotators classification
(van de Sande+, 2017)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- --- [Abell]
7- 10 I4 --- Abell [85/2399] Cluster identifier (Abell NNNN)
12- 13 I2 --- N [23/44] Number of ETG targets
15- 19 F5.3 --- z [0.045/0.058] Redshift
21- 23 I3 Mpc Dist [179/243] Distance
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 19 A19 --- SDSS SDSS galaxy identifier (JHHMMSS.ss+DDMMSS.s)
21- 24 F4.1 Lsun Lum(r) [9.8/11.3] Total r-band luminosity
26- 29 F4.1 arcsec Re [1.2/14.2] Effective radius
31- 34 F4.2 --- e [0.01/0.77] Ellipticity
36- 38 I3 km/s sigmac [70/419] Velocity dispersion measured in
a central Re/8 circular aperture
40- 41 I2 km/s e_sigmac [2/19] Uncertainty in sigmac
43- 45 I3 km/s sigmae [67/429] Velocity dispersion measured in
a 1 Re circular aperture
47- 48 I2 km/s e_sigmae [1/14] Uncertainty in sigmae
50- 52 I3 km/s sigmaell [70/400] Velocity dispersion measured in
an elliptical aperture with ellipticity and
major axis radius
54- 55 I2 km/s e_sigmaell [1/12] Uncertainty in sigmae,ell
57- 60 F4.1 --- M/L [2.8/15.1] Dynamical mass-to-light ratio
derived from JAM modelling (1)
62- 64 F3.1 --- e_M/L [0.1/1.6] Uncertainty in M/L
66 I1 --- Qual [0/2]? Quality of JAM model fit (2)
68 A1 --- Type [FLS] Kinematic morphological type (3)
70- 73 I4 --- Abell [85/2399] Host cluster identifier (Abell NNNN)
74 A1 --- f_SDSS [d] Flag for galaxy subsequently identified
as non-member
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Note (1): Dynamical masses were determined using the Jeans Anisotropic MGE (JAM)
modelling method of Cappellari (2008MNRAS.390...71C 2008MNRAS.390...71C).
Note (2): Following Cappellari et al. (2013MNRAS.432.1709C 2013MNRAS.432.1709C), the JAM model fit
qualities were classified as follows:
2 = Good fit;
1 = Adequate fit;
0 = Poor fit or bad data.
Note (3): Kinematic morphological type as follows:
L = Late-type galaxy;
S = Slow rotator;
F = Fast rotator.
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History:
From electronic version of the journal
(End) Tiphaine Pouvreau [CDS] 29-Nov-2019