Fast and slow rotators: the build-up of the red sequence

Emsellem, Éric; Cappellari, Michele; Krajnović, Davor; Ven, Glenn van de; Bacon, Roland; Bureau, Martin; Davies, Roger L.; Zeeuw, P. T. de; Falcón-Barroso, J.; Küntschner, H.; McDermid, Richard M.; Peletier, Reynier F.; Sarzi, Marc; Bosch, Remco C. E. van den

doi:10.1017/s1743921308017158

Cited by 3 publications

(3 citation statements)

References 26 publications

(19 reference statements)

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“…For example, in local galaxies Cortese et al (2016) (using SAMI) and Lagos et al (2016) (using the EAGLE galaxy formation model) show that the disk stability and galaxy spin, λR (as defined in Emsellem et al 2007) are strongly correlated with V / σ and define a continious sequence in the specific angular momentum-stellar mass plane, where galaxies with high specific angular momentum are the most stable with high V / σ and λR. Moreover, Stevens et al (2016) (see also Obreschkow et al 2015) suggest that specific angular momentum plays a defining role in defining the disk stability.…”

Section: Disk Stabilitymentioning

confidence: 99%

Angular momentum evolution of galaxies over the past 10 Gyr: A MUSE and KMOS dynamical survey of 400 star-forming galaxies from $z$ = 0.3–1.7

Swinbank

Harrison

Trayford

et al. 2017

Mon. Not. R. Astron. Soc.

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(2017) 'Angular momentum evolution of galaxies over the past 10 Gyr : a MUSE and KMOS dynamical survey of 400 star-forming galaxies from z = 0.3 to 1.7.', Monthly notices of the Royal Astronomical Society., 467 (3). pp. 3140-3159.Further information on publisher's website: Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-pro t purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. ABSTRACTWe present a MUSE and KMOS dynamical study 405 star-forming galaxies at redshift z = 0.28-1.65 (median redshiftz = 0.84). Our sample is representative of the star-forming "main-sequence", with star-formation rates of SFR = 0.1-30 M ⊙ yr −1 and stellar masses M ⋆ = 10 8 -10 11 M ⊙ . For 49 ± 4% of our sample, the dynamics suggest rotational support, 24 ± 3% are unresolved systems and 5 ± 2% appear to be early-stage major mergers with components on 8-30 kpc scales. The remaining 22 ± 5% appear to be dynamically complex, irregular (or face-on systems). For galaxies whose dynamics suggest rotational support, we derive inclination corrected rotational velocities and show these systems lie on a similar scaling between stellar mass and specific angular momentum as local spirals with⋆ but with a redshift evolution that scales as j ⋆ ∝ M 2/3 ⋆ (1 + z) −1 . We also identify a correlation between specific angular momentum and disk stability such that galaxies with the highest specific angular momentum (log(j ⋆ / M 2/3 ⋆ ) > 2.5) are the most stable, with Toomre Q = 1.10 ± 0.18, compared to Q = 0.53 ± 0.22 for galaxies with log(j ⋆ / M 2/3 ⋆ ) < 2.5. At a fixed mass, the HST morphologies of galaxies with the highest specific angular momentum resemble spiral galaxies, whilst those with low specific angular momentum are morphologically complex and dominated by several bright star-forming regions. This suggests that angular momentum plays a major role in defining the stability of gas disks: at z ∼ 1, massive galaxies that have disks with low specific angular momentum, are globally unstable, clumpy and turbulent systems. In contrast, galaxies with high specific angular have evolved in to stable disks with spiral structure where star formation is a local (rather than global) process.

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Section: Disk Stabilitymentioning

confidence: 99%

Angular momentum evolution of galaxies over the past 10 Gyr: A MUSE and KMOS dynamical survey of 400 star-forming galaxies from $z$ = 0.3–1.7

Swinbank

Harrison

Trayford

et al. 2017

Mon. Not. R. Astron. Soc.

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“…The quantity in equation 1 is a measure of the surface brightness extent in the x-axis direction. This definition is taken from Emsellem et al (2007); Cappellari et al (2007). We rotated each galaxy to align the major axis with the x-axis prior to calculating the moments.…”

Section: The Stellar and The Ionized Gas Distributionsmentioning

confidence: 99%

SDSS IV MaNGA: Characteristics of Edge-on Galaxies with a Counter-rotating Gaseous Disk

Beom,

Bizyaev,

Walterbos

et al. 2022

Preprint

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Counter-rotating components in galaxies are one of the most direct forms of evidence for past gas accretion or merging. We discovered ten edge-on disk gaseous counter-rotators in a sample of 523 edge-on galaxies identified in the final MaNGA (Mapping Nearby Galaxies at APO) IFU sample. The counter-rotators tend to located in small groups. The gaseous counter-rotators have intermediate stellar masses and and located in the green valley and red sequence of the color magnitude diagram. The average vertical extents of the stellar and ionized gas disks are the same as for the rest of the sample while their radial gas and stellar distributions are more centrally concentrated. This may point at angular momentum loss during the formation process of the counter-rotating disks. The counter-rotators have low gas and dust content, weak emission line strengths, and low star formation rates. This suggests that the formation of counter-rotators may be an efficient way to quench galaxies. One counter-rotator, SDSS J080016.09+292817.1 (Galaxy F), has a post starburst region and a possible AGN at the center. Another counter-rotator, SDSS J131234.03+482159.8 (Galaxy H), is identified as a potential on-going galaxy interaction with its companion satellite galaxy, a gas rich spiral galaxy. This may be representative case of a gaseous counter-rotator forming through a merger origin. However, tidal distortions expected in mergers are only found in a few of the galaxies and we cannot rule out direct gas accretion as another formation mechanism.

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“…To this end, we build our sample starting from the list of Galletta (1996) and Corsini & Bertola (1998) As a final step we checked also the SAURON (de Zeeuw et al 2002;Emsellem et al 2007) and ATLAS-3D Krajnović et al 2011) samples. The only selection criterium is the presence of both stars-gas and/or stars-stars CR.…”

Section: The Counter-rotating Galaxy Sample With Uv Emissionmentioning

confidence: 99%

The UV window on counter rotating ETGs: insight from SPH simulations with chemo-photometric implementation

Bettoni

Mazzei

Rampazzo

et al. 2014

Astrophys Space Sci

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The Galaxy Evolution Explorer (GALEX) detected ultraviolet emission in about 50% of multi-spin early-type galaxies (ETGs), suggesting the occurrence of a recent rejuvenation episode connected to the formation of these kinematical features. With the aim at investigating the complex evolutionary scenario leading to the formation of counter rotating ETGs (CR-ETGs) we use our Smooth Particle Hydrodynamic (SPH) code with chemo-photometric implementation. We discuss here the UV evolutionary path of two CR-ETGs, NGC 3593 and NGC 5173, concurrently best fitting their global observed properties, i.e., morphology, dynamics, as well as their total B-band absolute magnitude and spectral energy distribution (SED) extended over three orders of magnitude in wavelength. These simulations correspond to our predictions about the target evolution which we follow in the color-magnitude diagram (CMD), near-UV (N U V ) versus r-band absolute magnitude, as a powerful diagnostic tool to emphasize rejuvenation episodes.

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Fast and slow rotators: the build-up of the red sequence

Cited by 3 publications

References 26 publications

Angular momentum evolution of galaxies over the past 10 Gyr: A MUSE and KMOS dynamical survey of 400 star-forming galaxies from $z$ = 0.3–1.7

Angular momentum evolution of galaxies over the past 10 Gyr: A MUSE and KMOS dynamical survey of 400 star-forming galaxies from $z$ = 0.3–1.7

SDSS IV MaNGA: Characteristics of Edge-on Galaxies with a Counter-rotating Gaseous Disk

The UV window on counter rotating ETGs: insight from SPH simulations with chemo-photometric implementation

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