J/MNRAS/477/4711 Stellar angular momentum for MaNGA galaxies (Graham+, 2018)
SDSS-IV MaNGA: stellar angular momentum of about 2300 galaxies:
unveiling the bimodality of massive galaxy properties.
Graham M.T., Cappellari M., Li H., Mao S., Bershady M.A., Bizyaev D.,
Brinkmann J., Brownstein J.R., Bundy K., Drory N., Law D.R., Pan K.,
Thomas D., Wake D.A., Weijmans A.-M., Westfall K.B., Yan R.
<Mon. Not. R. Astron. Soc., 477, 4711-4737 (2018)>
=2018MNRAS.477.4711G 2018MNRAS.477.4711G (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies ; Morphology
Keywords: galaxies: elliptical and lenticular, cD - galaxies: evolution -
galaxies: formation - galaxies: kinematics and dynamics -
galaxies: spiral
Abstract:
We measure λRe, a proxy for galaxy specific stellar angular
momentum within one effective radius, and the ellipticity, ε,
for about 2300 galaxies of all morphological types observed with
integral field spectroscopy as part of the Mapping Nearby Galaxies at
Apache Point Observatory survey, the largest such sample to date. We
use the (λRe, ε) diagram to separate early-type
galaxies into fast and slow rotators. We also visually classify each
galaxy according to its optical morphology and two-dimensional stellar
velocity field. Comparing these classifications to quantitative
λRe measurements reveals tight relationships between angular
momentum and galaxy structure. In order to account for atmospheric
seeing, we use realistic models of galaxy kinematics to derive a
general approximate analytic correction for λRe. Thanks to
the size of the sample and the large number of massive galaxies, we
unambiguously detect a clear bimodality in the (λRe,
ε) diagram which may result from fundamental differences in
galaxy assembly history. There is a sharp secondary density peak
inside the region of the diagram with low λRe and
ε<0.4, previously suggested as the definition for slow
rotators. Most of these galaxies are visually classified as
non-regular rotators and have high velocity dispersion. The intrinsic
bimodality must be stronger, as it tends to be smoothed by noise and
inclination. The large sample of slow rotators allows us for the first
time to unveil a secondary peak at ±90° in their distribution of
the misalignments between the photometric and kinematic position
angles. We confirm that genuine slow rotators start appearing above
M≥2x1011M☉ where a significant number of high-mass fast
rotators also exist.
Description:
We have measured the stellar angular momentum parametrized by
λRe from the kinematics of 2286 galaxies in the MaNGA sample,
the largest sample with IFS observations to date.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 100 2722 All the quantities and properties required to
plot all the figures in Section 4
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- MaNGA MaNGA-ID associated with a unique MaNGA
galaxy
11 A1 --- Clean [Y/N] In clean sample?
13- 16 A4 --- Mtype Hubble classification type (1)
18- 21 A4 --- Classkin Kinematic classification (F = flagged)
23- 28 F6.3 [deg] log(Re)c circular effective radius
30- 35 F6.3 [kpc] log(Re)l semimajor axis
37- 39 F3.1 arcsec PSF FWHM of the PSF
41- 48 F8.3 --- lambdaRe ?=-999 Proxy for galaxy specific stellar
angular momentum within one effective radius
50- 54 F5.3 --- Ell Final ellipticity
56- 60 F5.1 --- PAph Final photometric position angle
(East of North)
62- 67 F6.1 deg PAkin ?=-999 Knematic position angle
(East of North)
69- 74 F6.1 deg e_PAkin ?=-999 rms uncertainty on PAkin
76- 80 F5.2 [Msun] log(M*) Stellar mass
82- 89 F8.3 [km/s] log(sigmae) ?=-999 Effective velocity dispersion
90 A1 --- u_log(sigmae) [I] I for infinity
91- 96 F6.4 --- z Redshift
98-100 F3.1 --- n Sersic index
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Note (1): Hubble classification:
U for unclassified and M/CP for merger or close pair.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 15-Jun-2021