The density of dark matter haloes of early-type galaxies in low-density environments

Corsini, E. M.; Wegner, Gary A.; Thomas, Jens; Saglia, R. P.; Bender, R.

doi:10.1093/mnras/stw2935

Cited by 19 publications

(24 citation statements)

References 96 publications

(144 reference statements)

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“…It results to be unreliable in the analysis of the faintest outskirts of large galaxies like ours (Hyde & Bernardi 2009;Méndez-Abreu et al 2017). Therefore, we measured the sky level in the surroundings of each sample galaxy following the procedure proposed by Pohlen & Trujillo (2006) as applied in Corsini et al (2017) and Morelli et al (2016). We masked all the foreground stars, companion and background galaxies, and spurious sources like residual cosmic rays and bad pixels close to the galaxy and measured its surfacebrightness radial profile with the ellipse task in IRAF 1 (Jedrzejewski 1987).…”

Section: Data Reductionmentioning

confidence: 99%

No evidence for small disk-like bulges in a sample of late-type spirals

Costantin

Méndez-Abreu

Corsini

et al. 2017

A&A

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Context. About 20% of low-redshift galaxies are late-type spirals with a small or no bulge component. Although they are the simplest disk galaxies in terms of structure and dynamics, the role of the different physical processes driving their formation and evolution is not yet fully understood. Aims. We investigated whether small bulges of late-type spirals follow the same scaling relations traced by ellipticals and large bulges and if they are disk-like or classical bulges. Methods. We derived the photometric and kinematic properties of 9 nearby late-type spirals. To this aim, we analyzed the surfacebrightness distribution from the i-band images of the Sloan Digital Sky Survey and obtained the structural parameters of the galaxies from a two-dimensional photometric decomposition. We found a bulge component in 7 galaxies of the sample, while the remaining 2 resulted to be pure disk galaxies. We measured the line-of-sight stellar velocity distribution within the bulge effective radius from the long-slit spectra taken with high spectral resolution at the Telescopio Nazionale Galileo. We used the photometric and kinematic properties of the sample bulges to study their location in the Fundamental Plane, Kormendy, and Faber-Jackson relations defined for ellipticals and large bulges. Results. We found that our sample bulges satisfy some of the photometric and kinematic prescriptions for being considered disk-like bulges such as small sizes and masses with nearly exponential light profiles, small bulge-to-total luminosity ratios, low stellar velocity dispersions, and ongoing star formation. However, each of them follows the same scaling relations of ellipticals, massive bulges, and compact early-type galaxies so they cannot be classified as disk-like systems. Conclusions. We found a single population of galaxy spheroids that follow the same scaling relations, where the mass seems to lead to a smooth transition in the photometric and kinematic properties from less massive bulges to more massive bulges and ellipticals.

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Section: Data Reductionmentioning

confidence: 99%

No evidence for small disk-like bulges in a sample of late-type spirals

Costantin

Méndez-Abreu

Corsini

et al. 2017

A&A

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“…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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The density of dark matter haloes of early-type galaxies in low-density environments

Cited by 19 publications

References 96 publications

No evidence for small disk-like bulges in a sample of late-type spirals

No evidence for small disk-like bulges in a sample of late-type spirals

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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