J/A+A/665/A54 MAGIC morpho-kinematics MS catalogue (Mercier+, 2022)
Scaling relations of z ∼ 0.25-1.5 galaxies in various environments from the
morpho-kinematics analysis of the MAGIC sample.
Mercier W., Epinat B., Contini T., Abril-Melgarejo V., Boogaard L.,
Brinchmann J., Finley H., Krajnovic D., Michel-Dansac L., Ventou E.,
Bouche N., Dumoulin J., Pineda J.C.B.
<Astron. Astrophys. 665, A54 (2022)>
=2022A&A...665A..54M 2022A&A...665A..54M (SIMBAD/NED BibCode)
ADC_Keywords: Galaxy catalogs ; Galaxies, rotation ; Models ; Morphology ;
Velocity dispersion
Keywords: galaxies: evolution - galaxies: kinematics and dynamics -
galaxies: clusters: general - galaxies: groups: general -
galaxies: high-redshift
Abstract:
The evolution of galaxies is influenced by many physical processes,
which may vary depending on their environment.
We combine Hubble Space Telescope (HST) and Multi-Unit Spectroscopic
Explorer (MUSE) data of galaxies at 0.25≲z≲1.5 to probe the impact
of environment on the size-mass relation, the main sequence (MS)
relation, and the Tully-Fisher relation (TFR).
We perform a morpho-kinematics modelling of 593 [OII] emitters in
various environments in the COSMOS area from the MUSE-gAlaxy Groups In
Cosmos survey. The HST F814W images are modelled with a bulge-disk
decomposition to estimate their bulge-disk ratio, effective radius,
and disk inclination. We use the [OII]λλ3727,3729
doublet to extract the galaxies' ionised gas kinematics maps from
the MUSE cubes, and we model those maps for a sample of 146 [OII]
emitters, including bulge and disk components constrained from
morphology and a dark matter halo.
We find an offset of 0.03dex (1σ significant) on the size-mass
relation zero point between the field and the large structure
sub-samples, with a richness threshold of N=10 to separate between
small and large structures, and of 0.06dex (2σ) with N=20.
Similarly, we find a 0.1dex (2σ) difference on the MS relation
with N=10 and 0.15dex (3σ) with N=20. These results suggest that
galaxies in massive structures are smaller by 14% and have star
formation rates reduced by a factor of 1.3-1.5 with respect to field
galaxies at z≃0.7. Finally, we do not find any impact of the
environment on the TFR, except when using N=20 with an offset of
0.04dex (1σ). We discard the effect of quenching for the largest
structures, which would lead to an offset in the opposite direction.
We find that, at z≃0.7, if quenching impacts the mass budget of
galaxies in structures, these galaxies would have been affected quite
recently and for roughly 0.7-1.5Gyr. This result holds when including
the gas mass but vanishes once we include the asymmetric drift
correction.
Description:
The MAGIC morpho-kinematics MS catalogue contains the main
morpho-kinematics and physical properties for Main Sequence galaxies.
This corresponds to 447 galaxies on the MS.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablef1.dat 462 447 Morpho-kinematics params for MS galaxies in MAGIC
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Byte-by-byte Description of file: tablef1.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- ID MUSE galaxy ID (1)
12- 30 F19.17 --- z Spectroscopic systemic redshift derived
from kinematics modelling
32- 49 F18.14 deg RAdeg Right Ascension (J2000) of
morphological centre
51- 68 F18.16 deg DEdeg Declination (J2000) of
morphological centre
70- 72 I3 --- N ?=-99 Number of galaxies in structures with
more than three members
74- 93 F20.17 kpc Reffd Disk effective radius
95-114 F20.17 kpc Reffb Bulge effective radius
116-135 F20.17 kpc Reff Global effective radius
137-158 F22.18 --- logBD Logarithm of the bulge-to-disk ratio
at Reff
160-165 F6.4 --- q Axis ratio of the disk
167-173 F7.2 deg PAm Morphological position angle of the
major axis
175-193 F19.17 arcsec FWHM Median PSF FWHM, corresponding to narrow
band OII MUSE observations in arcsecond
195-205 F11.5 10-24W/m2 OIIflux(R22) OII flux derived from MUSE flux maps
at R22 (2)
207-217 F11.4 10-24W/m2 OIIflux OII] flux derived from MUSE flux maps
at 3"
219-228 F10.6 --- SNR Total OII signal-to-noise ratio
230-247 F18.15 deg i Disk inclination corrected for thickness
249-269 F21.16 deg PAk Kinematic position angle of the
major axis
271-289 F19.16 kpc rs NFW halo scale radius
291-312 F22.18 km/s Vhmax Maximum rotation velocity of the
NFW rotation curve
314-332 F19.15 km/s Vr22 Rotation velocity at R22
334-353 F20.16 km/s sigma Median velocity dispersion
355-373 F19.15 km/s Vc22 Corrected rotation velocity at R22
375-379 F5.2 Msun logM* Logarithm of the stellar mass within an
aperture of 3"
381-399 F19.16 Msun logM*(R22) Logarithm of the corrected stellar mass
inside R22
401-422 F22.19 Msun/yr logSFR Logarithm of the SFR at 3" using Gilbank
et al. (2010MNRAS.405.2594G 2010MNRAS.405.2594G,
2011AJ....141...94G 2011AJ....141...94G or
2011MNRAS.414..304G 2011MNRAS.414..304G) prescription
424-442 F19.16 Msun logMg Logarithm of the gas mass computed from
the Schmidt-Kennicutt law and OII flux
measured at R22
444-462 F19.16 Msun logMdyn Logarithm of the dynamical mass computed
at R22 from the mass model
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Note (1): IDs are in the form X-CGrY, where X refers to the galaxy
identification number within the field targeting COSMOS group CGrY
Note (2): R22 = 1.311 x Reffd
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Acknowledgements:
Wilfried Mercier, wilfried.mercier(at)irap.omp.eu
(End) Wilfried Mercier [IRAP], Patricia Vannier [CDS] 21-Apr-2022