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dc.contributor.author
Contini, Thierry
dc.contributor.author
Épinat, Benoît
dc.contributor.author
Bouché, Nicolas
dc.contributor.author
Brinchmann, Jarle
dc.contributor.author
Boogaard, Leindert A.
dc.contributor.author
Ventou, Emmy
dc.contributor.author
Bacon, Roland
dc.contributor.author
Richard, Johan
dc.contributor.author
Weilbacher, Peter M.
dc.contributor.author
Wisotzki, Lutz
dc.contributor.author
Krajnović, Davor
dc.contributor.author
Vielfaure, J.B.
dc.contributor.author
Emsellem, Éric
dc.contributor.author
Finley, Hayley
dc.contributor.author
Inami, Hanae
dc.contributor.author
Schaye, Joop
dc.contributor.author
Swinbank, A. Mark
dc.contributor.author
Guérou, Adrien
dc.contributor.author
Martinsson, Thomas
dc.contributor.author
Michel-Dansac, Léo
dc.contributor.author
Schroetter, Ilane
dc.contributor.author
Shirazi, Maryam
dc.contributor.author
Soucail, Geneviève
dc.date.accessioned
2021-09-24T08:11:47Z
dc.date.available
2017-06-12T08:06:05Z
dc.date.available
2021-09-24T08:11:47Z
dc.date.issued
2016-07
dc.identifier.issn
0004-6361
dc.identifier.issn
1432-0746
dc.identifier.other
10.1051/0004-6361/201527866
en_US
dc.identifier.uri
http://hdl.handle.net/20.500.11850/117730
dc.description.abstract
Aims. Whereas the evolution of gas kinematics of massive galaxies is now relatively well established up to redshift z ~ 3, little is known about the kinematics of lower mass (M⋆≤ 1010M⊙) galaxies. We use MUSE, a powerful wide-field, optical integral-field spectrograph (IFS) recently mounted on the VLT, to characterize this galaxy population at intermediate redshift. Methods. We made use of the deepest MUSE observations performed so far on the Hubble Deep Field South (HDFS). This data cube, resulting from 27 h of integration time, covers a one arcmin2 field of view at an unprecedented depth (with a 1σ emission-line surface brightness limit of 1 × 10-19 erg s-1 cm-2 arcsec-2) and a final spatial resolution of ≈0.7′′. We identified a sample of 28 resolved emission-line galaxies, extending over an area that is at least twice the seeing disk, spread over a redshift interval of 0.2 <z< 1.4. More than half of the galaxies are at z ~ 0.3 − 0.7, which is a redshift range poorly studied so far with IFS kinematics. We used the public HST images and multiband photometry over the HDFS to constrain the stellar mass and star formation rate (SFR) of the galaxies and to perform a morphological analysis using GALFIT, providing estimates of the disk inclination, disk scale length, and position angle of the major axis. We derived the resolved ionized gas properties of these galaxies from the MUSE data and model the disk (both in 2D and in 3D with GALPAK3D) to retrieve their intrinsic gas kinematics, including the maximum rotation velocity and velocity dispersion. Results. We build a sample of resolved emission-line galaxies of much lower stellar mass and SFR (by ~1 − 2 orders of magnitude) than previous IFS surveys. The gas kinematics of most of the spatially resolved MUSE-HDFS galaxies is consistent with disk-like rotation, but about 20% have velocity dispersions that are larger than the rotation velocities and 30% are part of a close pair and/or show clear signs of recent gravitational interactions. These fractions are similar to what has been found in previous IFS surveys of more massive galaxies, indicating that the dynamical state of the ionized gas and the level of gravitational interactions of star-forming galaxies is not a strong function of their stellar mass. In the high-mass regime, the MUSE-HDFS galaxies follow the Tully-Fisher relation defined from previous IFS surveys in a similar redshift range. This scaling relation also extends to lower masses/velocities but with a higher dispersion. We find that 90% of the MUSE-HDFS galaxies with stellar masses below 109.5M⊙ have settled gas disks. The MUSE-HDFS galaxies follow the scaling relations defined in the local Universe between the specific angular momentum and stellar mass. However, we find that intermediate-redshift, star-forming galaxies fill a continuum transition from the spiral to elliptical local scaling relations, according to the dynamical state (i.e., rotation- or dispersion-dominated) of the gas. This indicates that some galaxies may lose their angular momentum and become dispersion-dominated prior to becoming passive.
en_US
dc.language.iso
en
en_US
dc.publisher
EDP Sciences
en_US
dc.subject
Galaxies: evolution
en_US
dc.subject
Galaxies: high-redshift
en_US
dc.subject
Galaxies: kinematics and dynamics
en_US
dc.title
Deep MUSE observations in the HDFS: Morpho-kinematics of distant star-forming galaxies down to 10 8M⊙
en_US
dc.type
Journal Article
dc.date.published
2016-06-10
ethz.journal.title
Astronomy & Astrophysics
ethz.journal.volume
591
en_US
ethz.journal.abbreviated
Astron. Astrophys.
ethz.pages.start
A49
en_US
ethz.size
26 p.
en_US
ethz.identifier.wos
ethz.identifier.scopus
ethz.publication.place
Les Ulis
en_US
ethz.publication.status
published
en_US
ethz.date.deposited
2017-06-12T08:11:52Z
ethz.source
ECIT
ethz.identifier.importid
imp5936547ee73c460872
ethz.ecitpid
pub:179647
ethz.eth
yes
en_US
ethz.availability
Metadata only
en_US
ethz.rosetta.installDate
2017-07-17T08:21:07Z
ethz.rosetta.lastUpdated
2022-03-29T13:31:23Z
ethz.rosetta.versionExported
true
ethz.COinS
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