SDSS-IV MaNGA: global stellar population and gradients for about 2000 early-type and spiral galaxies on the mass–size plane

Li, Hongyu; Mao, Shude; Cappellari, Michele; Ge, Junqiang; Long, R. J.; Li, Ran; Mo, H. J.; Li, Cheng; Zhang, Zheng; Bundy, Kevin; Thomas, Daniel; Brownstein, Joel R.; Roman-Lopes, Alexandre; Law, David R.; Drory, Niv

doi:10.1093/mnras/sty334

Cited by 136 publications

(159 citation statements)

References 86 publications

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“…Using data from the same survey, Goddard et al (2017a) find that gradients are steeper with increasing M * , although with low significance. Though also based on MaNGA, Li et al (2018) find shallower gradients at higher central velocity dispersions (σ * > 100km/s). There are several possible sources for these discrepancies, from stellar population synthesis approach (see Conroy 2013) to fitting method.…”

Section: Introductionmentioning

confidence: 74%

Signatures of Stellar Accretion in MaNGA Early-type Galaxies

Oyarzún

Bundy

Westfall

et al. 2019

ApJ

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The late assembly of massive galaxies is thought to be dominated by stellar accretion in their outskirts (beyond 2 effective radii R e ) due to dry, minor galaxy mergers. We use observations of 1010 passive early-type galaxies (ETGs) within z < 0.15 from SDSS IV MaNGA to search for evidence of this accretion. The outputs from the stellar population fitting codes FIREFLY, pPXF, and Prospector are compared to control for systematic errors in stellar metallicity (Z) estimation. We find that the average radial logZ/Z profiles of ETGs in various stellar mass (M * ) bins are not linear. As a result, these profiles are poorly characterized by a single gradient value, explaining why weak trends reported in previous work can be difficult to interpret. Instead, we examine the full radial extent of stellar metallicity profiles and find them to flatten in the outskirts of M * 10 11 M ETGs. This is a signature of stellar accretion. Based on a toy model for stellar metallicity profiles, we infer the ex-situ stellar mass fraction in ETGs as a function of M * and galactocentric radius. We find that ex-situ stars at R∼2R e make up 20% of the projected stellar mass of M * 10 10.5 M ETGs, rising up to 80% for M * 10 11.5 M ETGs. 5 pPXF

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Section: Introductionmentioning

confidence: 74%

Signatures of Stellar Accretion in MaNGA Early-type Galaxies

Oyarzún

Bundy

Westfall

et al. 2019

ApJ

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“…1 suggests that this gas temperature is ultimately determined by the mass (or virial temperature) of the galaxy plus the additional energetic input from the central super-massive black hole. The apparent trends between stellar population properties and galaxy velocity dispersion (McDermid et al 2015;Scott et al 2017;Li et al 2018) would be then just a consequence of the fact that σ strongly depends on both halo and black hole mass, while the stellar mass of a galaxy is mostly just probing the mass of its dark Figure 1 and Figure 2, lines of constant σ can be approximated as lines of constant M•, and therefore of constant gas temperature (as labeled on each diagonal line). We hypothesize that the physical mechanism behind the observed stellar population trends in the mass -size plane is actually a combination of potentially accreting gas being shockheated to the virial temperature of the halo and the additional energy released from the central super-massive black hole.…”

Section: Re-thinking the Mass-size Planementioning

confidence: 99%

Black hole feedback and the evolution of massive early-type galaxies

Martín-Navarro

Burchett

Mezcua

2019

Monthly Notices of the Royal Astronomical Society

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Observationally, constraining the baryonic cycle within massive galaxies has proven to be quite difficult. In particular, the role of black hole feedback in regulating star formation, a key process in our theoretical understanding of galaxy formation, remains highly debated. We present here observational evidence showing that, at fixed stellar velocity dispersion, the temperature of the hot gas is higher for those galaxies hosting more massive black holes in their centers. Analyzed in the context of well-established scaling relations, particularly the mass-size plane, the relation between the mass of the black hole and the temperature of the hot gas around massive galaxies provides further observational support to the idea that baryonic processes within massive galaxies are regulated by the combined effects of the galaxy halo virial temperature and black hole feedback, in agreement with the expectations from the EAGLE cosmological numerical simulation.

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“…There is now general agreement that metallicity increases towards the central regions of early-type galaxies (e.g. Scott et al 2009;González Delgado et al 2014;McDermid et al 2015;González Delgado et al 2015;Greene et al 2015;Boardman et al 2017;van de Sande et al 2018;Li et al 2018;Parikh et al 2019;Zhuang et al 2019;Zibetti et al 2019;Ferreras et al 2019), whereas age gradients are less pronounced. In addition, recent studies of IMF gradients (Martín-Navarro et al 2015a;Martín-Navarro et al 2015c,b;La Barbera et al 2016;Vaughan et al 2018a,b;Sarzi et al 2018) consistently find that the central regions of galaxies favour a bottom-heavy IMF.…”

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confidence: 92%

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

Bernardi

Sánchez

Brownstein

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present estimates of stellar population (SP) gradients from stacked spectra of slow (SR) and fast (FR) rotator elliptical galaxies from the MaNGA-DR15 survey. We find that: 1) FRs are ∼ 5 Gyrs younger, more metal rich, less α-enhanced and smaller than SRs of the same luminosity L r and central velocity dispersion σ 0 . This explains why when one combines SRs and FRs, objects which are small for their L r and σ 0 tend to be younger. Their SP gradients are also different. 2) Ignoring the FR/SR dichotomy leads one to conclude that compact galaxies are older than their larger counterparts of the same mass, even though almost the opposite is true for FRs and SRs individually. 3) SRs with σ 0 ≤ 250 km s −1 are remarkably homogeneous within ∼ R e : they are old, α-enhanced and only slightly super-solar in metallicity. These SRs show no gradients in age and M * /L r , negative gradients in metallicity, and slightly positive gradients in [α/Fe] (the latter are model dependent). SRs with σ 0 ≥ 250 km s −1 are slightly younger and more metal rich, contradicting previous work suggesting that age increases with σ 0 . They also show larger M * /L r gradients. 4) Self-consistently accounting for M * /L gradients yields M dyn ≈ M * because gradients reduce M dyn by ∼ 0.2 dex while only slightly increasing the M * inferred using a Kroupa (not Salpeter) IMF. 5) The FR population all but disappears above M * ≥ 3 × 10 11 M ; this is the same scale at which the size-mass correlation and other scaling relations change. Our results support the finding that this is an important mass scale which correlates with the environment and above which mergers matter.

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SDSS-IV MaNGA: global stellar population and gradients for about 2000 early-type and spiral galaxies on the mass–size plane

Cited by 136 publications

References 86 publications

Signatures of Stellar Accretion in MaNGA Early-type Galaxies

Signatures of Stellar Accretion in MaNGA Early-type Galaxies

Black hole feedback and the evolution of massive early-type galaxies

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

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