Further Evidence for Large Central Mass-to-Light Ratios in Early-Type Galaxies: The Case of Ellipticals and Lenticulars in the A262 Cluster

Wegner, Gary A.; Corsini, E. M.; Thomas, Jens; Saglia, R.; Bender, R.; Pu, S. B.

doi:10.1088/0004-6256/144/3/78

Cited by 56 publications

(78 citation statements)

References 104 publications

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“…In order to determine these M/L ratios, the central (if available, otherwise the galaxy) V − I colours (Table 4) initial mass function (IMF). Recent works suggest that the IMF may vary with velocity dispersion for early-type galaxies but there is a significant scatter in this relation (e.g., Cappellari et al 2012Cappellari et al , 2013Conroy & van Dokkum 2012;Spiniello et al 2012;Wegner et al 2012;Ferreras et al 2013;Zaritsky et al 2014). Galaxies with low-velocity dispersions require a Kroupa (2001, or a Chabrier 2003) IMF, while high-velocity dispersion galaxies (σ > ∼ 200 km s −1 ) may prefer a "bottom-heavy" IMF having a steeper slope than that of Salpeter (1955), although Cappellari et al (2013, their Fig.…”

Section: Central Stellar Mass Deficitsmentioning

confidence: 99%

Depleted cores, multicomponent fits, and structural parameter relations for luminous early-type galaxies

Dullo¹,

Graham²

2014

Monthly Notices of the Royal Astronomical Society

147

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New surface brightness profiles from 26 early-type galaxies with suspected partially depleted cores have been extracted from the full radial extent of Hubble Space Telescope images. We have carefully quantified the radial stellar distributions of the elliptical galaxies using the core-Sérsic model whereas for the lenticular galaxies a core-Sérsic bulge plus an exponential disc model gives the best representation. We additionally caution about the use of excessive multiple Sérsic functions for decomposing galaxies and compare with past fits in the literature. The structural parameters obtained from our fitted models are in general, in good agreement with our initial study using radially limited (R < ∼ 10 ′′ ) profiles, and are used here to update several "central" as well as "global" galaxy scaling relations. We find near-linear relations between the break radius R b and the spheroid luminosity L such that R b ∝ L 1.13±0.13 , and with the supermassive black hole mass. This is internally consistent with the notion that major, dry mergers add the stellar and black hole mass in equal proportion, i.e., M BH ∝ L. In addition, we observe a linear relation R b ∝ R 0.98±0.15 e for the core-Sérsic elliptical galaxies-where R e is the galaxies' effective half light radii-which is collectively consistent with the approximately-linear, bright-end of the curved L − R e relation. Finally, we measure accurate stellar mass deficits M def that are in general 0.5−4 M BH , and we identify two galaxies (NGC 1399, NGC 5061) that, due to their high M def /M BH ratio, may have experienced oscillatory core-passage by a (gravitational radiation)-kicked black hole. The galaxy scaling relations and stellar mass deficits favor core-Sérsic galaxy formation through a few "dry" major merger events involving supermassive black holes such that M def ∝ M 3.70±0.76 BH , for M BH > ∼ 2 × 10 8 M ⊙ .

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Section: Central Stellar Mass Deficitsmentioning

confidence: 99%

Depleted cores, multicomponent fits, and structural parameter relations for luminous early-type galaxies

Dullo¹,

Graham²

2014

Monthly Notices of the Royal Astronomical Society

147

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“…The IMF has been initially considered as universal across galaxy types and cosmic time, mostly because of a lack of evidence of variations among stellar clusters and OB associations in the Milky Way (see Bastian et al 2010 for a review about IMF studies). This assumption has been recently questioned by different dynamical, lensing, and stellar population studies, finding evidence for systematic IMF variations in ETGs Thomas et al 2011;Conroy & van Dokkum 2012;Cappellari et al 2012Cappellari et al , 2013Spiniello et al 2012;Wegner et al 2012;Dutton et al 2013;Ferreras et al 2013;Goudfrooij & Kruijssen 2013;La Barbera et al 2013;Tortora et al 2013;Weidner et al 2013;Goudfrooij & Kruijssen 2014;Shu et al 2015;Tortora et al 2014a,c;Martín-Navarro et al 2015;Lyubenova et al 2016;Tortora et al 2016;Corsini et al 2017;Li et al 2017;Sonnenfeld et al 2017).…”

Section: Constraining the Imfmentioning

confidence: 99%

“…The scenario is even more complicated if one takes into account the effect of a non universal IMF (van Dokkum & Conroy 2010;Treu et al 2010;Thomas et al 2011;Conroy & van Dokkum 2012;Cappellari et al 2012Cappellari et al , 2013Spiniello et al 2012;Wegner et al 2012;Barnabè et al 2013;Dutton et al 2013;Ferreras et al 2013;Goudfrooij & Kruijssen 2013;La Barbera et al 2013;Tortora et al 2013;Weidner et al 2013;Goudfrooij & Kruijssen 2014;Shu et al 2015;McDermid et al 2014;Tortora et al 2014a,c;Martín-Navarro et al 2015;Spiniello et al 2015;Lyubenova et al 2016;Tortora et al 2016;Corsini et al 2017;Li et al 2017;Sonnenfeld et al 2017;Tortora et al 2017). Indeed, the IMF remains the largest source of uncertainty to quantify the stellar and DM mass budget in the central galactic regions.…”

Section: Introductionmentioning

confidence: 99%

The last 6 Gyr of dark matter assembly in massive galaxies from the Kilo Degree Survey

Tortora

Napolitano

Roy

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We study the dark matter (DM) assembly in the central regions of massive early-type galaxies up to z ∼ 0.65. We use a sample of ∼ 3800 massive (log M /M > 11.2) galaxies with photometry and structural parameters from 156 sq. deg. of the Kilo Degree Survey, and spectroscopic redshifts and velocity dispersions from SDSS. We obtain central total-to-stellar mass ratios, M dyn /M , and DM fractions, by determining dynamical masses, M dyn , from Jeans modelling of SDSS aperture velocity dispersions and stellar masses, M , from KiDS galaxy colours. We first show how the central DM fraction correlates with structural parameters, mass and density proxies, and demonstrate that most of the local correlations are still observed up to z ∼ 0.65; at fixed M , local galaxies have larger DM fraction, on average, than their counterparts at larger redshift. We also interpret these trends with a non universal Initial Mass Function (IMF), finding a strong evolution with redshift, which contrast independent observations and is at odds with the effect of galaxy mergers. For a fixed IMF, the galaxy assembly can be explained, realistically, by mass and size accretion, which can be physically achieved by a series of minor mergers. We reproduce both the R e -M and M dyn /M -M evolution with stellar and dark mass changing at a different rate. This result suggests that the main progenitor galaxy is merging with less massive systems, characterized by a smaller M dyn /M , consistently with results from halo abundance matching.

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“…Chabrier-or Kroupa-like IMFs have been usually adopted in most types of galaxies, environments and redshifts. Recently, this hypothesis has been questioned by different lines of observational evidence (van Dokkum & Conroy 2010;Treu et al 2010; Thomas et al 2011;Conroy & van Dokkum 2012;Cappellari et al 2012Cappellari et al , 2013Spiniello et al 2012;Wegner et al 2012;Barnabè et al 2013;Dutton et al 2013;Ferreras et al 2013;Goudfrooij & Kruijssen 2013;La Barbera et al 2013;Tortora et al 2013;Weidner et al 2013;Goudfrooij & Kruijssen 2014;Shu et al 2015;McDermid et al 2014;Tortora et al 2014a,c;Martín-Navarro et al 2015;Spiniello et al 2015;Lyubenova et al 2016;Tortora et al 2016;Corsini et al 2017;Li et al 2017;Sonnenfeld et al 2017). In the current analysis we will express our results in terms of stellar M/L and the associated IMF, discussing whether these are realistic within different gravity frameworks.…”

Section: Introductionmentioning

confidence: 99%

Testing Verlinde's emergent gravity in early-type galaxies

Tortora

Koopmans

Napolitano

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Verlinde derived gravity as an emergent force from the information flow, through two-dimensional surfaces and recently, by a priori postulating the entanglement of information in three-dimensional space, he derived the effect of the gravitational potential from dark matter (DM) as the entropy displacement of dark energy by baryonic matter. In Emergent Gravity (EG) this apparent DM depends only on the baryonic mass distribution and the present-day value of the Hubble parameter. In this paper we test the EG proposition, formalized by Verlinde for a spherical and isolated mass distribution, using the central dynamics (SDSS velocity dispersion, σ) and the K-band light distribution in a sample of 4260 massive (M > ∼ 10 10 M ) and local early-type galaxies (ETGs) from the SPIDER datasample. Our results remain unaltered if we consider the sample of 807 roundest field galaxies. Using these observations we derive the predictions by EG for the stellar mass-to-light ratio (M/L) and the Initial Mass Function (IMF), and compare them with the same inferences derived from a) the standard DM-based models, b) an alternative description of the missing mass (i.e. MOND) and c) stellar population models. We demonstrate that, consistently with a classical Newtonian framework with a DM halo component, or alternative theories of gravity as MOND, the central dynamics can be fitted if the IMF is assumed non-universal. The results can be interpreted with a IMF lighter than a standard Chabrier at low-σ, and bottom-heavier IMFs at larger σ. We find lower, but still acceptable, stellar M/L in EG theory, if compared with the DM-based NFW model and with MOND. The results from EG are comparable to what is found if the DM haloes are adiabatically contracted and also with expectations from spectral gravity-sensitive features. If the strain caused by the entropy displacement would be not maximal, as adopted in the current formulation, then the dynamics of ETGs could be reproduced with larger M/L.

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Further Evidence for Large Central Mass-to-Light Ratios in Early-Type Galaxies: The Case of Ellipticals and Lenticulars in the A262 Cluster

Cited by 56 publications

References 104 publications

Depleted cores, multicomponent fits, and structural parameter relations for luminous early-type galaxies

Depleted cores, multicomponent fits, and structural parameter relations for luminous early-type galaxies

The last 6 Gyr of dark matter assembly in massive galaxies from the Kilo Degree Survey

Testing Verlinde's emergent gravity in early-type galaxies

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