J/MNRAS/476/1765 MaNGA E and S galaxies properties (Li+, 2018)
SDSS-IV MaNGA: global stellar population and gradients for about 2000
early-type and spiral galaxies on the mass-size plane.
Li H., Mao S., Cappellari M., Ge J., Long R.J., Li R., Mo H.J., Li C.,
Zheng Z., Bundy K., Thomas D., Brownstein J.R., Roman Lopes A., Law D.R.,
Drory N.
<Mon. Not. R. Astron. Soc., 476, 1765-1775 (2018)>
=2018MNRAS.476.1765L 2018MNRAS.476.1765L (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies ; Morphology ; Velocity dispersion
Keywords: galaxies: evolution - galaxies: formation -
galaxies: kinematics and dynamics - galaxies: structure
Abstract:
We perform full spectrum fitting stellar population analysis and Jeans
Anisotropic modelling of the stellar kinematics for about 2000
early-type galaxies (ETGs) and spiral galaxies from the MaNGA DR14
sample. Galaxies with different morphologies are found to be located
on a remarkably tight mass plane which is close to the prediction of
the virial theorem, extending previous results for ETGs. By examining
an inclined projection ('the mass-size' plane), we find that spiral
and early-type galaxies occupy different regions on the plane, and
their stellar population properties (i.e. age, metallicity, and
stellar mass-to-light ratio) vary systematically along roughly the
direction of velocity dispersion, which is a proxy for the bulge
fraction. Galaxies with higher velocity dispersions have typically
older ages, larger stellar mass-to-light ratios and are more metal
rich, which indicates that galaxies increase their bulge fractions as
their stellar populations age and become enriched chemically. The age
and stellar mass-to-light ratio gradients for low-mass galaxies in our
sample tend to be positive (centre<outer), while the gradients for
most massive galaxies are negative. The metallicity gradients show a
clear peak around velocity dispersion log10σe~=2.0, which
corresponds to the critical mass ∼3x1010M☉ of the break in the
mass-size relation. Spiral galaxies with large mass and size have the
steepest gradients, while the most massive ETGs, especially above the
critical mass Mcrit≥2x 1011M☉, where slow rotator ETGs
start dominating, have much flatter gradients. This may be due to
differences in their evolution histories, e.g. mergers.
Description:
The galaxies in this study are from the MaNGA Product Launch 5 (MPL5)
catalogue (internal release, nearly identical to SDSS-DR14, Abolfathi
et al., 2018ApJS..235...42A 2018ApJS..235...42A), which includes 2778 galaxies of
different morphologies.
We perform Jeans Anisotropic modelling (JAM, Cappellari,
2008MNRAS.390...71C 2008MNRAS.390...71C) for all the galaxies in our sample.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 64 2110 Properties of all the galaxies in the sample
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See also:
J/AJ/154/86 : MaNGA catalog, DR15 (Wake+, 2017)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- MaNGA MaNGA ID of the galaxy
11 A1 --- Morph [SE] Galaxy morphology,
E for ETGs, S for spiral galaxies
12- 16 F5.2 [km/s] logsigmae Velocity dispersion within 1Re, as defined
in equation (2) in the paper
18- 22 F5.2 [Msun] logM1/2 Enclosed total mass within
three-dimensional half-light radius
from dynamical model
24- 28 F5.2 [kpc] logRe Major axis of the half-light isophote for
the best-fitting MGE model
30- 34 F5.2 [yr] logAge Mean logAge within the effective radius
36- 40 F5.2 [-] [Z/H] Mean metallicity within the effective
radius
42- 46 F5.2 [Msun/Lsun] logM*/L Mean stellar mass-to-light ratio within the
effective radius in SDSS r band
48- 52 F5.2 [-] DlogAge Age gradient
54- 58 F5.2 [-] D[Z/H] Metallicity gradient
60- 64 F5.2 [-] DlogM*/L Stellar mass-to-light ratio gradient in
SDSS r band
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 23-Apr-2021