J/A+A/688/A75 MUSE surveys intermediate-redshift galaxies (Munoz Lopez+, 2024)
Stellar angular momentum of intermediate-redshift galaxies in MUSE surveys.
Munoz Lopez C., Krajnovic D., Epinat B., Herrero-Alonso Y., Urrutia T.,
Mercier W., Bouche N.F., Boogaard L.A., Contini T., Michel-Dansac L.,
Pessa I.
<Astron. Astrophys. 688, A75 (2024)>
=2024A&A...688A..75M 2024A&A...688A..75M (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies ; Redshifts ; Morphology ; Photometry, HST ; Infrared
Keywords: galaxies: evolution - galaxies: formation -
galaxies: kinematics and dynamics
Abstract:
We quantify the stellar rotation of galaxies by computing the
λR parameter, a proxy for the stellar angular momentum in a
sample of 106 intermediate-redshift galaxies (0.1<z<0.8). The sample
is located in the CANDELS/GOODS-S and CANDELS/COSMOS regions, and it
was observed by various MUSE surveys. We created spatially resolved
stellar velocity and velocity dispersion maps using a full-spectrum
fitting technique, covering spatially ∼2Re for the galaxies. The
sample spans stellar masses from ∼107.5M☉ to 1011.8M☉
with star formation rates (SFRs) from log10(SFR)~-3M☉/yr to
∼1.7M☉/yr over a range of 6Gyr in cosmic time. We studied how
the atmospheric seeing, introduced by the instrumental point spread
function (PSF), affects the measured spin parameter, and we applied
corrections when pertinent. Through the analysis of the
λR-ε diagram, we note that the fraction of round and
massive galaxies increases with redshift. We did not measure any
galaxy with λR<0.1 in the sample, and we found only one
potential (but uncertain) low-mass slow rotator at z∼0.3, more similar
to the z=0 low-mass slow rotators characterized by counter-rotation
than to massive ellipticals. Moreover, we do not see an evident
evolution or trend in the stellar angular momentum with redshift. We
characterized the galaxy environment using two different indicators: a
local estimator based on the Voronoi tesselation method, and a global
estimator derived by the use of the friends-of-friends (FoF)
algorithm. We find no correlation between the environment and
λR given that we are not probing dense regions or massive
galaxy structures. We also analysed the kinematic maps of the sample
finding that about 40% of the galaxies are consistent with being
regular rotators (RRs), having rotating stellar discs with flat
velocity dispersion maps, while ∼20% have complex velocity maps and
can be identified as non-regular rotators in spite of their
λR values. For the remaining galaxies the classification is
uncertain. As we lack galaxies with λR<0.1 in the sample, we
are not able to identify when galaxies lose their angular momentum and
become slow rotators within the surveyed environments, area, and
redshift range.
Description:
We used data sets from the blind 3D spectroscopic survey MUSE-Wide
(Urrutia et al., 2019A&A...624A.141U 2019A&A...624A.141U, Cat. J/A+A/624/A141), which
targets 100 fields and/or pointings in the CANDELS/GOODS-S and
CANDELS/COSMOS regions.
The final sample is composed of 106 galaxies: 53 in the candels-cdfs
fields, 15 in the candels-cosmos fields, 16 in the udf-mosaic fields,
13 in the MXDF region, 5 in the HUDF09 parallels, and 4 in the UDF-10
fields. Table B.1 we list the properties of each galaxy in the sample.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tableb1.dat 112 106 Galaxy sample properties
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See also:
J/ApJS/214/24 : 3D-HST+CANDELS catalog (Skelton+, 2014)
J/A+A/624/A141 : MUSE-Wide Survey DR1 catalog (Urrutia+, 2019)
Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- N [1/106] Galaxy index
5- 9 I5 --- ID 3D-HST galaxy unique identifier within
a given field
11- 17 A7 --- Field Field
19- 23 F5.3 --- z MUSE spectroscopic redshift
25- 33 F9.5 deg RAdeg Right ascension (J2000) of
galaxy centre from 3D-HST survey
35- 43 F9.5 deg DEdeg Declination (J2000) of galaxy centre
from 3D-HST survey
45- 48 F4.1 mag F160W ?=- Magnitude in the F160W filter
from 3D-HST survey
50- 53 F4.2 arcsec Re Galaxy effective radius
55- 58 F4.2 arcsec sigmaPSF width of the Gaussian PSF (FWHMPSF/2.355)
60- 62 F3.1 --- epsilon Ellipticity
64- 66 F3.1 --- n Sersic inde
68- 72 F5.2 [Msun] log(M*) ?=- Galaxy stellar mass from 3D-HST survey
74- 78 F5.2 [Msun/yr] log(SFR) ?=- Galaxy star formation rate
from 3D-HST survey
80- 81 I2 --- S/N MUSE signal-to-noise ratio of the galaxy
measured within the effective radius
83 A1 --- n_lambdaR Note on lambdaR (1)
85- 89 F5.3 --- lambdaR Galaxy stellar angular momentum measured for
the half-light ellipse aperture
91- 95 F5.3 --- e_lambdaR rms uncertainty on galaxy stellar angular
momentum
97- 99 F3.1 --- Aperture Aperture in Re unit where lambdaR was
computed
101-112 A12 --- KC Our kinematic classification according to
the kinematics maps (2)
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Note (1): Note as follows:
f = galaxies where the correction was not applied, and thus indicate
measured values
r = galaxies with corrected values
Note (2): Classification as follows:
RR = regular rotators
NRR = non-regular rotators
RR* = galaxies with clues of regular rotation but are visually hard to
classify
NRR* = galaxies with clues of non-regular rotation, but are visually hard to
classify
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 06-Feb-2025