The Massive Survey. Ii. Stellar Population Trends Out to Large Radius in Massive Early-Type Galaxies

Greene, Jenny E.; Janish, Ryan; Pei, Chung; McConnell, Nicholas J.; Blakeslee, John P.; Thomas, Jens; Murphy, J.H.

doi:10.1088/0004-637x/807/1/11

Cited by 145 publications

(200 citation statements)

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“…Thus the breaks at 1R e are interpreted as transition from the in situ to the accreted stellar populations, and are observed in other giant ellipticals from the MASSIVE survey (Greene et al 2013(Greene et al , 2015. In NGC 3311, this type of break in the stellar properties of the inner galaxy and the external halo correlates with variations in the velocity dispersion profile.…”

Section: Correspondence Among Stellar Populationsmentioning

confidence: 63%

The Hydra I cluster core

Barbosa

Arnaboldi

Coccato

et al. 2016

A&A

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Context. The history of the mass assembly of brightest cluster galaxies may be studied by mapping the stellar populations at large radial distances from the galaxy centre, where the dynamical times are long and preserve the chemodynamical signatures of the accretion events. Aims. We provide extended and robust measurements of the stellar population parameters in NGC 3311, the cD galaxy at the centre of the Hydra I cluster, and out to three effective radii. We wish to characterize the processes that drove the build-up of the stellar light at all these radii. Methods. We obtained the spectra from several regions in NGC 3311 covering an area of ∼3 arcmin 2 in the wavelength range 4800 λ(Å) 5800, using the FORS2 spectrograph at the Very Large Telescope in the Mask exchange unit (MXU) mode. We measured the equivalent widths of seven absorption-features defined in the Lick/IDS system, which were modelled by single stellar populations, to provide luminosity-weighted ages, metallicities, and alpha element abundances. Results. The trends in the Lick indices and the distribution of the stellar population parameters indicate that the stars of NGC 3311 may be divided in two radial regimes, one within and the another beyond one effective radius, R e = 8.4 kpc, similar to the distinction between the inner galaxy and the external halo derived from the NGC 3311 velocity dispersion profile. The inner galaxy (R ≤ R e ) is old (age ∼14 Gyr), has negative metallicity gradients and positive alpha element gradients. The external halo is also very old, but has a negative age gradient. The metal and element abundances of the external halo both have a large scatter, indicating that stars from a variety of satellites with different masses have been accreted. The region in the extended halo associated with the off-centred envelope at 0• < PA < 90• has higher metallicity with respect to the symmetric external halo. Conclusions. The different stellar populations in the inner galaxy and extended halo reflect the dominance of in situ stars in the former and the accreted origin for the large majority of the stars in the latter. The low value of the velocity dispersion in the inner galaxy indicates that its stars are bound to the galaxy's gravitational potential, and the abundances and gradients suggest that the inner galaxy is formed in an outside-in scenario of merging gas-rich lumps, reminiscent of the first phase of galaxy formation. The external halo has a higher velocity dispersion, it is dynamically hotter than the galaxy and its stars are gravitationally driven by the cluster's gravitational potential. The stars in the external halo were removed from their parent galaxies, either disks with truncated star formation, or the outer regions of early-type galaxies. Late mass accretion at large radii is now coming from the tidal stripping of stars from dwarfs and S0 galaxies. These results provide supporting evidence for the recent theoretical models of formation of massive ellipticals as a two-phase process.

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Section: Correspondence Among Stellar Populationsmentioning

confidence: 63%

The Hydra I cluster core

Barbosa

Arnaboldi

Coccato

et al. 2016

A&A

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“…To date, we have IFU spectroscopy for 70 of the 116 galaxies in the MASSIVE survey. With these data we are measuring stellar population gradients (Greene et al 2013(Greene et al , 2015, molecular gas masses and star formation efficiencies (Davis et al 2016), stellar kinematic fields (M. Veale et al 2016, in preparation), and, when combined with modeling, the enclosed dark matter halo mass (e.g., Thomas et al 2011). …”

Section: The Massive Surveymentioning

confidence: 99%

“…The other possible second parameter is metallicity. More massive early-type galaxies are also more metal-rich (e.g., Trager et al 2000;McDermid et al 2014;Greene et al 2015), which naturally leads to more mass loss per unit mass. Thus, one possible explanation for the mismatch between the expected luminosity due to mass loss and that observed simply arises due to our presumed model of mass loss.…”

Section: The Role Of Galaxy Rotation In X-ray Gas Heatingmentioning

confidence: 99%

“…Complementary to these previous multiwavelength studies, here we focus our study on the hot-gas emission present in the volume-limited MASSIVE survey (Ma et al 2014; M14 hereafter) of the 116 most massive early-type galaxies within 108 Mpc. Similar to ATLAS 3D , MASSIVE uses integral field spectroscopy (IFS) combined with uniform K-band imaging to study the stellar populations (Greene et al 2015) and stellar kinematics (M. Veale et al 2016, in preparation) of the MASSIVE galaxies.…”

Section: Introductionmentioning

confidence: 99%

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The Massive Survey. Iv. The X-Ray Halos of the Most Massive Early-Type Galaxies in the Nearby Universe

Goulding

Greene

et al. 2016

ApJ

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112

156

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Studies of the physical properties of local elliptical galaxies are shedding new light on galaxy formation. Here we present the hot-gas properties of 33 early-type systems within the MASSIVE galaxy survey that have archival Chandra X-ray observations, and we use these data to derive X-ray luminosities (L X,gas ) and plasma temperatures (T gas ) for the diffuse gas components. We combine this with the ATLAS 3D survey to investigate the X-ray-optical properties of a statistically significant sample of early-type galaxies across a wide range of environments. When X-ray measurements are performed consistently in apertures set by the galaxy stellar content, we deduce that all early types (independent of galaxy mass, environment, and rotational support) follow a universal scaling law such that µL T X,gas gas 4.5 . We further demonstrate that the scatter in L X,gas around both K-band luminosity (L K ) and the galaxy stellar velocity dispersion (s e ) is primarily driven by T gas , with no clear trends with halo mass, radio power, or angular momentum of the stars. It is not trivial to tie the gas origin directly to either stellar mass or galaxy potential. Indeed, our data require a steeper relation between L L , K X,gas , and s e than predicted by standard mass-loss models. Finally, we find that T gas is set by the galaxy potential inside the optical effective radius. We conclude that within the innermost 10-30 kpc region, early types maintain pressure-supported hot gas, with a minimum T gas set by the virial temperature, but the majority show evidence for additional heating.

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“…Indeed, either traditional long-slit or integral field absorption line spectroscopy require long integration times to go beyond 2 effective radii (e.g., Coccato et al 2010aCoccato et al ,b, 2011Greene et al 2012Greene et al , 2015. This is particularly challenging for early-type galaxies because, contrarily to their spiral counterparts, they do not contain as much gas to be used as kinematic tracer in their outskirts.…”

Section: Introductionmentioning

confidence: 99%

Planetary nebulae as kinematic tracers of galaxy stellar halos

Coccato

2016

Proc. IAU

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Abstract. The kinematic and dynamical properties of galaxy stellar halos are difficult to measure because of the faint surface brightness that characterizes these regions. Spiral galaxies can be probed using the radio Hi emission; on the contrary, early-type galaxies contain less gas, therefore alternative kinematic tracers need to be used. Planetary nebulae (PNe) can be easily detected far out in the halo thanks to their bright emission lines. It is therefore possible to map the halo kinematics also in early-type galaxies, typically out to 5 effective radii or beyond. Thanks to the recent spectroscopic surveys targeting extra-galactic PNe, we can now rely on a few tens of galaxies where the kinematics of the stellar halos are measured. Here, I will review the main results obtained in this field in the last decades.

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The Massive Survey. Ii. Stellar Population Trends Out to Large Radius in Massive Early-Type Galaxies

Cited by 145 publications

References 153 publications

The Hydra I cluster core

The Hydra I cluster core

The Massive Survey. Iv. The X-Ray Halos of the Most Massive Early-Type Galaxies in the Nearby Universe

Planetary nebulae as kinematic tracers of galaxy stellar halos

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