The MASSIVE Survey. XII. Connecting Stellar Populations of Early-type Galaxies to Kinematics and Environment

Greene, Jenny E.; Veale, Melanie; Ma, Chung‐Pei; Thomas, Jens; Quenneville, Matthew E.; Blakeslee, John P.; Walsh, Jonelle L.; Goulding, A. D.; Ito, Jennifer

doi:10.3847/1538-4357/ab01e3

Cited by 50 publications

(41 citation statements)

References 111 publications

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“…We have obtained comprehensive spectroscopic data using IFS on both sub-arcsecond and arc-minute scales and performed uniform measurements of the spatiallyresolved kinematics. Many results on the stellar kinematics and stellar populations of MASSIVE galaxies out to a few effective radii from our wide-field IFS observations can be found in Veale et al (2017bVeale et al ( ,a, 2018; Ene et al (2018); Greene et al (2015Greene et al ( , 2019. Results from finely-resolved stellar kinematics in the central ∼ 2 kpc regions of 20 MASSIVE galaxies are presented in Ene et al (2019); Ene et al (2020).…”

Section: Introductionmentioning

confidence: 83%

The MASSIVE Survey. XV. A Stellar Dynamical Mass Measurement of the Supermassive Black Hole in Massive Elliptical Galaxy NGC 1453

Liepold

Quenneville

et al. 2020

ApJ

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We present a new stellar dynamical mass measurement (M BH ) of the supermassive black hole (SMBH) in NGC 1453, a fast-rotating massive elliptical galaxy in the MASSIVE survey. We measure stellar kinematics in 135 spatial bins in the central 1.5 kpc by 2 kpc region of the galaxy using high signal-to-noise (S/N ∼ 130) spectra from the Gemini-North GMOS integral-field spectrograph (IFS). Combining with wide-field IFS kinematics out to ∼ 3 effective radii and stellar light distributions from Hubble Space Telescope (HST ) WFC3 images, we perform Schwarzschild orbit-based mass modeling in the axisymmetric limit to constrain the mass components in NGC 1453. The best-fit black hole mass is M BH = (2.9 ± 0.4) × 10 9 M ; the mass models without a central black hole are excluded at the 8.7σ level. The NGC 1453 black hole lies within the intrinsic scatter of the SMBH and galaxy scaling relations, unlike three other galaxies hosting 10 10 M SMBHs in the MASSIVE sample. The high-S/N GMOS spectra enable us to determine 8 moments of the Gauss-Hermite expansion of the line-of-sight velocity distributions (LOSVDs), which are used as constraints in the orbit modeling. The stellar orbits in the mass models are further constrained to produce negligible h 9 through h 12 to minimize spurious behavior in the LOSVDs. We show that truncating the series at h 4 , as was often done in prior work, leads to a much weaker constraint on the inferred M BH for NGC 1453. Furthermore, we discuss precautions and modifications that are needed to achieve axisymmetry in triaxial orbit codes that use the Schwarzschild method to sample the start space of stellar orbits in triaxial gravitational potentials.

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Section: Introductionmentioning

confidence: 83%

The MASSIVE Survey. XV. A Stellar Dynamical Mass Measurement of the Supermassive Black Hole in Massive Elliptical Galaxy NGC 1453

Liepold

Quenneville

et al. 2020

ApJ

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“…Moreover, galaxy assembly history is not only expected to depend on the total M * or morphology of galaxies, but also on their environment (e.g. Greene et al 2015Greene et al , 2019. We will study second order trends in the metallicity profiles of ETGs in follow-up work.…”

Section: Estimating the Ex-situ Stellar Mass Fractionmentioning

confidence: 99%

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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“…Relationships among stellar mass,[Mg/Fe], and [Fe/H] for MRG-M0138 (black and blue diamonds, corresponding to the MOSFIRE and FIRE measurements), COSMOS-11494 at z = 2.1 (green circle;Kriek et al 2016), and the centers of local massive ETGs (light blue circles;Greene et al 2019). Red pentagons show measurements derived from the SDSS stacks ofConroy et al (2014).…”

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confidence: 99%

Resolved Multi-element Stellar Chemical Abundances in the Brightest Quiescent Galaxy at z ∼ 2

Jafariyazani

Newman

Mobasher

et al. 2020

ApJL

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Measuring the chemical composition of galaxies is crucial to our understanding of galaxy formation and evolution models. However, such measurements are extremely challenging for quiescent galaxies at high redshifts, which have faint stellar continua and compact sizes, making it difficult to detect absorption lines and nearly impossible to spatially resolve them. Gravitational lensing offers the opportunity to study these galaxies with detailed spectroscopy that can be spatially resolved. In this work, we analyze deep spectra of MRG-M0138, a lensed quiescent galaxy at z = 1.98 which is the brightest of its kind, with an H-band magnitude of 17.1. Taking advantage of full spectral fitting, we measure [Mg/Fe] = 0.51 ± 0.05, [Fe/H] = 0.26 ± 0.04, and, for the first time, the stellar abundances of 6 other elements in this galaxy. We further constrained, also for the first time in a z ∼ 2 galaxy, radial gradients in stellar age, [Fe/H], and [Mg/Fe]. We detect no gradient in age or [Mg/Fe] and a slightly negative gradient in [Fe/H], which has a slope comparable to that seen in local early-type galaxies. Our measurements show that not only is MRG-M0138 very Mg-enhanced compared to the centers of local massive early-type galaxies, it is also very iron rich. These dissimilar abundances suggest that even the inner regions of massive galaxies have experienced significant mixing of stars in mergers, in contrast to a purely inside-out growth model. The abundance pattern observed in MRG-M0138 challenges simple galactic chemical evolution models that vary only the star formation timescale and shows the need for more elaborate models.

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The MASSIVE Survey. XII. Connecting Stellar Populations of Early-type Galaxies to Kinematics and Environment

Cited by 50 publications

References 111 publications

The MASSIVE Survey. XV. A Stellar Dynamical Mass Measurement of the Supermassive Black Hole in Massive Elliptical Galaxy NGC 1453

The MASSIVE Survey. XV. A Stellar Dynamical Mass Measurement of the Supermassive Black Hole in Massive Elliptical Galaxy NGC 1453

Signatures of Stellar Accretion in MaNGA Early-type Galaxies

Resolved Multi-element Stellar Chemical Abundances in the Brightest Quiescent Galaxy at z ∼ 2

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