The MUSE Hubble ultra deep field survey

• Verfasst von: Bouché, Nicolas F. [VerfasserIn]
• Verfasst von: Genel, Shy [VerfasserIn]
• Verfasst von: Pellissier, Alisson [VerfasserIn]
• Verfasst von: Dubois, Cédric [VerfasserIn]
• Verfasst von: Contini, Thierry [VerfasserIn]
• Verfasst von: Epinat, Benoît [VerfasserIn]
• Verfasst von: Pillepich, Annalisa [VerfasserIn]
• Verfasst von: Krajnović, Davor [VerfasserIn]
• Verfasst von: Nelson, Dylan [VerfasserIn]
• Verfasst von: Abril-Melgarejo, Valentina [VerfasserIn]
• Verfasst von: Richard, Johan [VerfasserIn]
• Verfasst von: Boogaard, Leindert [VerfasserIn]
• Verfasst von: Maseda, Michael [VerfasserIn]
• Verfasst von: Mercier, Wilfried [VerfasserIn]
• Verfasst von: Bacon, Roland [VerfasserIn]
• Verfasst von: Steinmetz, Matthias [VerfasserIn]
• Verfasst von: Vogelsberger, Mark [VerfasserIn]
• Titel: The MUSE Hubble ultra deep field survey
• Titelzusatz: XVI. The angular momentum of low-mass star-forming galaxies - a cautionary tale and insights from TNG50
• Verf.angabe: Nicolas F. Bouché, Shy Genel, Alisson Pellissier, Cédric Dubois, Thierry Contini, Benoît Epinat, Annalisa Pillepich, Davor Krajnović, Dylan Nelson, Valentina Abril-Melgarejo, Johan Richard, Leindert Boogaard, Michael Maseda, Wilfried Mercier, Roland Bacon, Matthias Steinmetz, and Mark Vogelsberger
• E-Jahr: 2021
• Jahr: 08 October 2021
• Umfang: 21 S.
• Fussnoten: Gesehen am 27.01.2022
• Titel Quelle: Enthalten in: Astronomy and astrophysics
• Ort Quelle: Les Ulis : EDP Sciences, 1969
• Jahr Quelle: 2021
• Band/Heft Quelle: 654(2021), Artikel-ID A49, Seite 1-21
• ISSN Quelle: 1432-0746
• DOI: doi:10.1051/0004-6361/202040225
• Datenträger: Online-Ressource
• Sprache: eng
• K10plus-PPN: 1787302016

Abstract

We investigate the specific angular momentum (sAM) <i>j<i/>(< <i>r<i/>) profiles of intermediate redshift (0.4 < <i>z<i/> < 1.4) star-forming galaxies (SFGs) in the relatively unexplored regime of low masses (down to <i>M<i/><sub>⋆<sub/> ∼ 10<sup>8<sup/> <i>M<i/><sub>⊙<sub/>) and small sizes (down to <i>R<i/><sub>e<sub/> ∼ 1.5 kpc), and we characterize the sAM scaling relation (i.e., Fall relation) and its redshift evolution. We have developed a 3D methodology to constrain sAM profiles of the star-forming gas using a forward modeling approach with GAlPAK<sup>3D<sup/> that incorporates the effects of beam smearing, yielding the intrinsic morpho-kinematic properties even with limited spatial resolution data. Using mock observations from the TNG50 simulation, we find that our 3D methodology robustly recovers the star formation rate (SFR)-weighted profiles down to a low effective signal-to-noise ratio of ⪆3. We applied our methodology blindly to a sample of 494 [O II]-selected SFGs in the MUSE Ultra Deep Field (UDF) 9 arcmin<sup>2<sup/> mosaic data, covering the unexplored 8 < log <i>M<i/><sub>⋆<sub/>/<i>M<i/><sub>⊙<sub/> < 9 mass range. We find that the (SFR-weighted) sAM relation follows with an index <i>α<i/> varying from <i>α<i/> = 0.3 to <i>α<i/> = 0.5, from log <i>M<i/><sub>⋆<sub/>/<i>M<i/><sub>⊙<sub/> = 8 to log <i>M<i/><sub>⋆<sub/>/<i>M<i/><sub>⊙<sub/> = 10.5. The UDF sample supports a redshift evolution , with which is consistent with the (1 + <i>z<i/>)<sup>−0.5<sup/> expectation from a universe in expansion. The scatter of the sAM sequence is a strong function of the dynamical state with , where <i>σ<i/> is the velocity dispersion at 2<i>R<i/><sub>e<sub/>. In TNG50, SFGs also form a plane, but it correlates more with galaxy size than with morphological parameters. Our results suggest that SFGs might experience a dynamical transformation, and lose their sAM, before their morphological transformation to becoming passive via either merging or secular evolution.