Galaxy properties as revealed by MaNGA – II. Differences in stellar populations of slow and fast rotator ellipticals and dependence on environment

Bernardi, Mariangela; Sánchez, H. Domínguez; Brownstein, Joel R.; Drory, Niv; Sheth, Ravi K.

doi:10.1093/mnras/stz2413

Cited by 42 publications

(37 citation statements)

References 75 publications

(124 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Figure 3 shows the star formation histories from the galaxy centre and the outer shell region. As expected from fast-rotating, low-mass galaxies in low-density environment (Kauffmann et al 2004;McDermid et al 2015;Bernardi et al 2019), we obtain evidence of extended star formation from both regions of NGC 474. The galaxy centre formed half of its stellar mass within the first ∼3 Gyr while it took a more extended period of ∼5 Gyr for the outer shell to build up half its stellar mass.…”

Section: Stellar Age Metallicity and Star Formation History Of Ngc 474supporting

confidence: 83%

NGC 474 as viewed with KCWI: diagnosing a shell galaxy

Alabi

Ferré-Mateu

Forbes

et al. 2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Abstract We present new spectra obtained using Keck/KCWI and perform kinematics and stellar population analyses of the shell galaxy NGC 474, from both the galaxy centre and a region from the outer shell. We show that both regions have similarly extended star formation histories although with different stellar population properties. The central region of NGC 474 is dominated by intermediate-aged stars (8.3 ± 0.3 Gyr) with subsolar metallicity ([Z/H]=−0.24 ± 0.07 dex) while the observed shell region, which hosts a substantial population of younger stars, has a mean luminosity-weighted age of 4.0 ± 0.5 Gyr with solar metallicities ([Z/H]=−0.03 ± 0.09 dex). Our results are consistent with a scenario in which NGC 474 experienced a major to intermediate merger with a log$(M_*/\rm M_\odot )\mathord {\sim }10$ mass satellite galaxy at least $\mathord {\sim }2$ Gyr ago which produced its shell system. This work shows that the direct spectroscopic study of low-surface brightness stellar features, such as shells, is now feasible and opens up a new window to understanding galaxy formation and evolution.

show abstract

Section: Stellar Age Metallicity and Star Formation History Of Ngc 474supporting

confidence: 83%

NGC 474 as viewed with KCWI: diagnosing a shell galaxy

Alabi

Ferré-Mateu

Forbes

et al. 2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…Although early-type and passive galaxies in observations are consistent with flat (or even inverted) stellar age and [α/Fe] radial profiles (e.g. Kuntschner et al 2010;Greene et al 2015;Li et al 2018a;Bernardi et al 2019;Barsanti et al 2020;Santucci et al 2020), late-type galaxies tend to have stellar age profiles consistent with the inner parts being older (e.g. González Delgado et al 2015;Barsanti et al 2020).…”

Section: The Stellar Populations Of Slow Rotatorsmentioning

confidence: 92%

“…Weijmans et al (2014); Foster et al (2017); Li et al (2018a); Krajnović et al (2018) find that SRs tend to have a higher occurrence of triaxial or prolate intrinsic shapes compared to fast rotators, which are mostly oblate, axisymmetric systems (often with bars). The intrinsic stellar populations of SRs indicate flat α/Fe metallicity radial profiles, uniform old stellar ages, and declining metallicity radial profiles (where the central parts are more metalrich than the outer parts; Kuntschner et al 2010;Bernardi et al 2019;Krajnović et al 2020).…”

Section: Introductionmentioning

confidence: 98%

The diverse nature and formation paths of slow rotator galaxies in the eagle simulations

Lagos

Emsellem

Sande

et al. 2021

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We use a sample of z = 0 galaxies visually classified as slow rotators (SRs) in the eagle hydrodynamical simulations to explore the effect of galaxy mergers on their formation, characterise their intrinsic galaxy properties, and study the connection between quenching and kinematic transformation. SRs that have had major or minor mergers (mass ratios ≥0.3 and 0.1 − 0.3, respectively) tend to have a higher triaxiality parameter and ex-situ stellar fractions than those that had exclusively very minor mergers or formed in the absence of mergers (“no-merger” SRs). No-merger SRs are more compact, have lower black hole-to-stellar mass ratios and quenched later than other SRs, leaving imprints on their z = 0 chemical composition. For the vast majority of SRs we find that quenching, driven by active galactic nuclei feedback, precedes kinematic transformation, except for satellite SRs, in which these processes happen in tandem. However, in ≈50 per cent of these satellites, satellite-satellite mergers are responsible for their SR fate, while environment (i.e. tidal field and interactions with the central) can account for the transformation in the rest. By splitting SRs into kinematic sub-classes, we find that flat SRs prefer major mergers; round SRs prefer minor or very minor mergers; prolate SRs prefer gas-poor mergers. Flat and prolate SRs are more common among satellites hosted by massive haloes ($>10^{13.6}\, \rm M_{\odot }$) and centrals of high masses ($M_{\star } > 10^{10.5}\, \rm M_{\odot }$). Although eagle galaxies display kinematic properties that broadly agree with observations, there are areas of disagreement, such as inverted stellar age and velocity dispersion profiles. We discuss these and how upcoming simulations can solve them.

show abstract

“…Figure 7 shows the λ R e − diagram (Emsellem et al 2007(Emsellem et al , 2011 for the kinematic classification of our samples of morphological E galaxies. See, for example, Graham et al (2018), Smethurst et al (2018), Bernardi et al (2019), andTabor et al (2019) for information about this kinematic classification for MaNGA galaxies. The galaxies enclosed by the black lines correspond to non-regular rotators (i.e., slow rotators), according to Cappellari (2016).…”

Section: Classification Of Elliptical Galaxies Based On Their Integra...mentioning

confidence: 99%

SDSS-IV MaNGA: Global and local stellar population properties of elliptical galaxies

Lacerna

Ibarra-Medel

Ávila-Reese

et al. 2020

A&A

View full text Add to dashboard Cite

Context. We study the spatially resolved properties of 343 elliptical galaxies with the Mapping Nearby Galaxies at the Apache Point Observatory (MaNGA) survey. Aims. Our goal is to understand the fundamental processes of formation and quenching of elliptical galaxies. Methods. We used the DESI Legacy Imaging Surveys for accurate morphological classification. Based on integrated spectroscopic properties and colors, we classified seven classes of elliptical galaxies. We inferred the stellar age and metallicity gradients out to a 1.5 effective radius (Reff) of classical “red and dead”, recently quenched, and blue star-forming ellipticals (CLEs, RQEs, and BSFs), corresponding to 73%, 10%, and 4% of the sample, respectively. Additionally, we reconstructed their global and radial histories of star formation and mass growth. Results. The mass- and luminosity-weighted age gradients of CLEs are nearly flat or mildly negative, with small differences between both ages. The respective metallicity gradients are negative (∇log[Zmw] = −0.11−0.08+0.07 dex/Reff and ∇log[Zlw] = −0.11−0.07+0.06 dex/Reff, respectively), being flatter as the mass is smaller. The more massive CLEs formed stars earlier and quenched faster than the less massive ones. The CLEs show a weak inside-out growth and a clear inside-out quenching. They finished their quenching globally 3.8 ± 1.2 Gyr ago on average, with quenching time-scales of 3.4 ± 0.8 Gyr. At M⋆ < 1011 M⊙, the age and Z gradients of the RQEs and BSFs are flatter than those of the CLEs, but with larger scatters. They show very weak inside-out growth and quenching, which is slow and not even completed at z ∼ 0 for the BSFs. Instead, the massive RQEs show an outside-in quenching and positive gradients in the luminosity-weighted age and stellar metallicities. The RQEs of all masses quenched 1.2 ± 0.9 Gyr ago on average. Conclusions. Our results for the CLEs are consistent with a two-phase scenario where their inner parts formed by an early and coeval dissipative collapse with a consequent burst of star formation and further quenching, whereas the outer parts continued their assembly, likely by dry mergers. We also discuss some evolutionary scenarios for the RQE and BSF galaxies that would agree with the generic results.

show abstract

Galaxy properties as revealed by MaNGA – II. Differences in stellar populations of slow and fast rotator ellipticals and dependence on environment

Cited by 42 publications

References 75 publications

NGC 474 as viewed with KCWI: diagnosing a shell galaxy

NGC 474 as viewed with KCWI: diagnosing a shell galaxy

The diverse nature and formation paths of slow rotator galaxies in the eagle simulations

SDSS-IV MaNGA: Global and local stellar population properties of elliptical galaxies

Contact Info

Product

Resources

About