J/A+A/647/A152 Tully-Fisher relation in MAGIC groups (Abril-Melgarejo+, 2021)
The Tully-Fisher relation in dense groups at z∼0.7 in the MAGIC survey.
Abril-Melgarejo V., Epinat B., Mercier W., Contini T., Boogaard L.A.,
Brinchmann J., Finley H., Michel-Dansac L., Ventou E., Amram P.,
Krajnovic D., Mahler G., Pineda J.C.B., Richard J.
<Astron. Astrophys. 647, A152 (2021)>
=2021A&A...647A.152A 2021A&A...647A.152A (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Galaxy catalogs ; Galaxies, rotation ;
Redshifts ; Rotational velocities ; Velocity dispersion
Keywords: galaxies: evolution - galaxies: kinematics and dynamics -
galaxies: groups: general - galaxies: high-redshift
Abstract:
Galaxies in dense environments are subject to interactions and
mechanisms that directly affect their evolution by lowering their gas
fractions and consequently reducing their star-forming capacity
earlier than their isolated counterparts. The aim of our project is to
get new insights into the role of environment in the stellar and
baryonic content of galaxies using a kinematic approach, through the
study of the Tully-Fisher relation (TFR).
We study a sample of galaxies in eight groups, over-dense by a factor
larger than 25 with respect to the average projected density, spanning
a redshift range of 0.5<z<0.8 and located in ten pointings of the
MAGIC MUSE Guaranteed Time Observations program. We perform a
morpho-kinematics analysis of this sample and set up a selection based
on galaxy size, [OII]λλ3727,3729 emission line doublet
signal-to-noise ratio, bulge-to-disk ratio, and nuclear activity to
construct a robust kinematic sample of 67 star-forming galaxies.
We show that this selection considerably reduces the number of
outliers in the TFR, which are predominantly dispersion-dominated
galaxies. Similar to other studies, we find that including the
velocity dispersion in the velocity budget mainly affects galaxies
with low rotation velocities, reduces the scatter in the relation,
increases its slope, and decreases its zero-point. Including gas
masses is more significant for low-mass galaxies due to a larger gas
fraction, and thus decreases the slope and increases the zero-point of
the relation. Our results suggest a significant offset of the TFR
zero-point between galaxies in low- and high-density environments,
regardless of the kinematics estimator used. This can be interpreted
as a decrease in either stellar mass by ∼0.05-0.3dex or an increase in
rotation velocity by ∼0.02-0.06dex for galaxies in groups, depending
on the samples used for comparison. We also studied the stellar and
baryon mass fractions within stellar disks and found they both
increase with stellar mass, the trend being more pronounced for the
stellar component alone. These fractions do not exceed 50%. We show
that this evolution of the TFR is consistent either with a decrease in
star formation or with a contraction of the mass distribution due to
the environment. These two effects probably act together, with their
relative contribution depending on the mass regime.
Description:
Eight dense galaxy groups in the COSMOS field at intermediate
redshifts (z∼0.7) were studied using IFU and high resolution
photometry data to determine morphological and kinematic properties of
the disk star-forming galaxies inside these dense structures. The
results of the morpho-kinematic modeling are presented in two tables.
The kinematic sample was selected using limits on the S/N of the [OII]
emission and the ratio Reff/PSF that relates the size (effective
radius) of the stellar disk and the PSF of the IFU data. Kinematic and
morphological model parameters and their uncertainties are presented
in Table B.1. Physical properties derived from these models are given
in Table B.2.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tableb1.dat 113 77 Kinematic and morphological parameters
(corrected version on 09-May-2023)
tableb2.dat 124 77 Physical properties
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Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- GrID COSMOS group ID
8- 10 I3 --- ID Galaxy ID (G1)
12- 18 F7.5 --- z Spectroscopic redshift
20- 22 I3 deg RAd Right Ascension (J2000)
24- 25 I2 arcmin RAm Right Ascension (J2000)
27- 30 F4.1 arcsec RAs Right Ascension (J2000)
32 A1 --- DE- Declination sign (J2000)
33 I1 deg DEd Declination (J2000)
35- 36 I2 arcmin DEm Declination (J2000)
38- 41 F4.1 arcsec DEs Declination (J2000)
43- 47 F5.3 arcsec FWHM Median PSF FWHM, corresponding to narrow
band [OII] MUSE observations
49- 53 I5 10-24W/m2 F[OII] Flux from [OII] derived from MUSE flux maps
(in 10-21erg/s/cm2)
55- 57 I3 10-24W/m2 e_F[OII] rms uncertainty on F[OII]
59- 62 F4.2 --- q Axis ratio
64- 67 F4.2 --- e_q rms uncertainty on axis ratio
69- 71 I3 deg PAm Morphological position angle of the major
axis
73- 74 I2 deg e_PAm rms uncertainty on PAm
76- 79 F4.2 kpc Rd Disk scale length
81- 84 F4.2 kpc e_Rd rms uncertainty on Rd
86- 88 I3 deg PAk Kinematic position angle of the major axis
90- 91 I2 deg e_PAk rms uncertainty on PAk
93- 96 F4.1 kpc rt Radius at which the plateau velocity is
98-102 E5.3 kpc e_rt rms uncertainty on rt (2)
105-107 I3 km/s Vt Velocity of the plateau
109-113 E5.3 km/s e_Vt rms uncertainty on Vt (2)
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Note (2): Galaxies with large uncertainties on both rt and Vt are those for
which the plateau is not reached within the data, nevertheless their slope
might be well constrained (see section 3.5 of the paper).
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Byte-by-byte Description of file: tableb2.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- GrID COSMOS group ID
8- 10 I3 --- ID Galaxy ID (G1)
12- 15 F4.2 kpc Reff Global effective radius
17- 21 F5.2 [-] logBD logarithm of the bulge-to-disk ratio
at R22
23- 24 I2 deg i Disk inclination
26 I1 deg e_i rms uncertainty on i
28- 30 I3 km/s Vr22 Rotation velocity at R22 (2)
32- 33 I2 km/s e_Vr22 rms uncertainty on Vr22
35- 37 I3 km/s sigma Median velocity dispersion
39- 40 I2 km/s e_sigma rms uncertainty on sigma
42- 44 I3 km/s Vc22 Corrected rotation velocity at R22 (2)
46- 48 I3 km/s e_Vc22 rms uncertainty on e_sigma
50- 54 F5.2 [Msun] logM* logarithm of the stellar mass within an
aperture of 3"
56- 59 F4.2 [Msun] E_logM* Error on logM* (upper value)
61- 64 F4.2 [Msun] e_logM* Error on logM* (lower value)
66- 70 F5.2 [Msun] logM*R22 logarithm of the corrected stellar mass
inside R22 (2)
72- 75 F4.2 [Msun] e_logM*R22 rms uncertainty on logM*R22
77- 81 F5.2 [Msun/yr] logSFR logarithm of the SFR from the SED fitting
83- 86 F4.2 [Msun/yr] E_logSFR Error on logSFR (upper value)
88- 91 F4.2 [Msun/yr] e_logSFR Error on logSFR (lower value)
93- 97 F5.2 [Msun] logMg logarithm of the gas mass computed from
the Kennicutt-Schmidt law and from SED
SFRs
99-102 F4.2 [Msun] e_logMg rms uncertainty on logMg
104-108 F5.2 [Msun] logMdynVr22 logarithm of the dynamical mass computed
from Vr22
110-113 F4.2 [Msun] e_logMdynVr22 rms uncertainty on logMdynVr22
115-119 F5.2 [Msun] logMdynVc22 logarithm of the dynamical mass computed
from Vc22
121-124 F4.2 [Msun] e_logMdynVc22 rms uncertainty on logMdynVc22
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Note (2): R22 corresponds to 2.2 times the disk scale length radius (2.2xRd).
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Global notes:
Note (G1): The table is split in three parts to identify
(i) the final kinematic sample (67 galaxies),
(ii) galaxies having their kinematics biased by an AGN
(2 galaxies, CGr32-268, CGr32-454), and
(iii) those with a dominant bulge within the effective radius
(8 galaxies with logB/D>0).
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Acknowledgements:
Valentina Abril-Melgarejo, vl.abril57(at)uniandes.edu.co
Benoit Epinat, bepinat(at)lam.fr
Histoty:
26-Mar-2021: on-line version
09-May-2023: positions corrected in table B1 (from author)
(End) V. Abril-Melgarejo [LAM, France], P. Vannier [CDS] 04-Feb-2021