Formation channels of slowly rotating early-type galaxies

Krajnović, Davor; Ural, Uğur; Küntschner, H.; Goudfrooij, Paul; Wolfe, M. A.; Cappellari, Michele; Davies, Roger L.; Zeeuw, Tim P. de; Duc, Pierre Alain; Emsellem, Éric; Karick, A. M.; McDermid, Richard M.; Mei, S.; Naab, Thorsten

doi:10.1051/0004-6361/201937040

Cited by 39 publications

(47 citation statements)

References 216 publications

(328 reference statements)

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“…Dry mergers lead to SRs that have flatter [Fe/H] profiles due to the effective redistribution of stellar mass during dry mergers (Lagos et al 2018b). Krajnović et al (2020) found that classical slow rotators (which they linked to the dissipation-less galaxy mergers; i.e. dry mergers) have flatter metallicity gradients than other slow rotators in ATLAS 3D , which is in qualitative agreement to what we find in .…”

Section: The Stellar Populations Of Slow Rotatorssupporting

confidence: 90%

“…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%

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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

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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.

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Section: The Stellar Populations Of Slow Rotatorssupporting

confidence: 90%

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

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“…Massive early-type galaxies and some BCGs can acquire cold gas through the cooling of hot gas and/or via cannibalism of a gas-rich satellite and they may undergo episodes of low level star formation at low redshift(Salomé & Combes 2003;O'Dea et al 2008;Hopkins & Hernquist 2009;Struve et al 2010;Young et al 2011;Zubovas & King 2012;Russell et al 2014;Smith & Edge 2017;Russell et al 2019;Krajnović et al 2020). …”

mentioning

confidence: 99%

The Black Hole Mass–Color Relations for Early- and Late-type Galaxies: Red and Blue Sequences

Dullo

Bouquin

Paz

et al. 2020

ApJ

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Tight correlations between supermassive black hole (SMBH) mass (M BH ) and the properties of the host galaxy have useful implications for our understanding of the growth of SMBHs and evolution of galaxies. Here, we present newly observed correlations between M BH and the host galaxy total UV− [3.6] color (C UV,tot , Pearson's r = 0.6 − 0.7) for a sample of 67 galaxies (20 early-type galaxies and 47 late-type galaxies) with directly measured M BH in the GALEX /S 4 G survey. The colors are carefully measured in a homogeneous manner using the galaxies' FUV, NUV and 3.6 µm magnitudes and their multi-component structural decompositions in the literature. We find that more massive SMBHs are hosted by (early-and late-type) galaxies with redder colors, but the M BH −C UV,tot relations for the two morphological types have slopes that differ at ∼ 2σ level. Early-type galaxies define a red sequence in the M BH − C UV,tot diagrams, while late-type galaxies trace a blue sequence. Within the assumption that the specific star formation rate of a galaxy (sSFR) is well traced by L UV /L 3.6 , it follows that the SMBH masses for late-type galaxies exhibit a steeper dependence on sSFR than those for early-type galaxies. The M BH − C UV,tot and M BH − L 3.6,tot relations for the sample galaxies reveal a comparable level of vertical scatter in the log M BH direction, roughly 5% − 27% more than the vertical scatter of the M BH − σ relation. Our M BH − C UV,tot relations suggest different channels of SMBH growth for early-and late-type galaxies, consistent with their distinct formation and evolution scenarios. These new relations offer the prospect of estimating SMBH masses reliably using only the galaxy color. Furthermore, we show that they are capable of estimating intermediate black hole masses in low-mass, early-and late-type galaxies.

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“…Numerous integral field spectroscopic surveys provide stellar metallicity gradient measurements. Most such surveys of nearby massive galaxies resolve well within once or twice the effective radii (e.g., SAURON, AT-LAS3D, MANGA, SAMI; Kuntschner et al 2010;Krajnović et al 2020;González Delgado et al 2015;Martín-Navarro et al 2018;Bernardi et al 2019;Ferreras et al 2019a;Oyarzún et al 2019), yet few probe beyond the cores because of the limited field of view. Thus we compare our integrated stellar metallicities with results from the MASSIVE and CALIFA surveys that provide gradient measurements to the largest spatial extent, out to ≈ 2.5 r eff .…”

Section: Descendantsmentioning

confidence: 99%

An exquisitely deep view of quenching galaxies through the gravitational lens: Stellar population, morphology, and ionized gas

Man,

Zabl,

Brammer

et al. 2021

Preprint

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This work presents an in-depth analysis of four gravitationally lensed red galaxies at z = 1.6 − 3.2. The sources are magnified by factors of 2.7 -30 by foreground clusters, enabling spectral and morphological measurements that are otherwise challenging. Our sample extends below the characteristic mass of the stellar mass function and is thus more representative of the quiescent galaxy population at z > 1 than previous spectroscopic studies. We analyze deep VLT/X-SHOOTER spectra and multiband Hubble Space Telescope photometry that cover the rest-frame UV-to-optical regime. The entire sample resembles stellar disks as inferred from lensing-reconstructed images. Through stellar population synthesis analysis we infer that the targets are young (median age = 0.1 -1.2 Gyr) and formed 80% of their stellar masses within 0.07 -0.47 Gyr. Mg II λλ 2796, 2803 absorption is detected across the sample. Blue-shifted absorption and/or redshifted emission of Mg II is found in the two youngest sources, indicative of a galactic-scale outflow of warm (T ∼ 10 4 K) gas. The [O III] λ5007 luminosity is higher for the two young sources (median age less than 0.4 Gyr) than the two older ones, perhaps suggesting a decline in nuclear activity as quenching proceeds. Despite high-velocity (v ≈ 1500 km s −1 ) galactic-scale outflows seen in the most recently quenched galaxies, warm gas is still present to some extent long after quenching. Altogether our results indicate that star formation quenching at highredshift must have been a rapid process (< 1 Gyr) that does not synchronize with bulge formation or complete gas removal. Substantial bulge growth is required if they are to evolve into the metal-rich cores of present-day slow-rotators.

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Formation channels of slowly rotating early-type galaxies

Cited by 39 publications

References 216 publications

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

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

The Black Hole Mass–Color Relations for Early- and Late-type Galaxies: Red and Blue Sequences

An exquisitely deep view of quenching galaxies through the gravitational lens: Stellar population, morphology, and ionized gas

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