2,510 research outputs found
Testing Verlinde's emergent gravity in early-type galaxies
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 3D 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
velocity dispersion, and the light distribution in a sample of 4260
massive and local early-type galaxies (ETGs) from the SPIDER sample. Our
results remain unaltered if we consider the sample of 807 roundest field
galaxies. 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) DM-based models, b) 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-,
and bottom-heavier IMFs at larger . 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 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. (abridged)Comment: 12 pages, 2 figures, submitted to MNRAS. The updated manuscript
presents significantly altered conclusions, after discovering an internal bug
in an older version of the Mathematica package, leading to incorrect
numerical results when calculating the derivatives of Gamma function
MOND and IMF variations in early-type galaxies from ATLAS3D
MOdified Newtonian dynamics (MOND) represents a phenomenological alternative
to dark matter (DM) for the missing mass problem in galaxies and clusters of
galaxies. We analyze the central regions of a local sample of
early-type galaxies from the survey, to see if the data can be
reproduced without recourse to DM. We estimate dynamical masses in the MOND
context through Jeans analysis, and compare to stellar masses
from stellar population synthesis. We find that the observed stellar
mass--velocity dispersion relation is steeper than expected assuming MOND with
a fixed stellar initial mass function (IMF) and a standard value for the
acceleration parameter . Turning from the space of observables to
model space, a) fixing the IMF, a universal value for cannot be
fitted, while, b) fixing and leaving the IMF free to vary, we find
that it is "lighter" (Chabrier-like) for low-dispersion galaxies, and "heavier"
(Salpeter-like) for high dispersions. This MOND-based trend matches inferences
from Newtonian dynamics with DM, and from detailed analysis of spectral
absorption lines, adding to the converging lines of evidence for a
systematically-varying IMF.Comment: 6 pages, 3 figures, accepted for publication on MNRAS Letters, typos
corrected and further references adde
Dark matter scaling relations in intermediate z haloes
We investigate scaling relations between the dark matter (DM) halo model parameters for a sample of intermediate-redshift early-type galaxies (ETGs) resorting to a combined analysis of Einstein radii and aperture velocity dispersions. Modelling the dark halo with a Navarro-Frenk-White profile and assuming a Salpeter initial mass function (IMF) to estimate stellar masses, we find that the column density and the Newtonian acceleration within the halo characteristic radius rs and effective radius Reff are not universal quantities, but correlate with the luminosity LV, the stellar mass M★ and the halo mass M200, contrary to recent claims in the literature. We finally discuss a tight correlation among the DM mass MDM(Reff) within the effective radius Reff, the stellar mass M★(Reff) and Reff itself. The slopes of the scaling relations discussed here strongly depend, however, on the DM halo model and the IMF adopted so that these ingredients have to be better constrained in order to draw definitive conclusions on the DM scaling relations for ETG
Galaxy evolution within the Kilo-Degree Survey
The ESO Public Kilo-Degree Survey (KiDS) is an optical wide-field imaging
survey carried out with the VLT Survey Telescope and the OmegaCAM camera. KiDS
will scan 1500 square degrees in four optical filters (u, g, r, i). Designed to
be a weak lensing survey, it is ideal for galaxy evolution studies, thanks to
the high spatial resolution of VST, the good seeing and the photometric depth.
The surface photometry have provided with structural parameters (e.g. size and
S\'ersic index), aperture and total magnitudes have been used to derive
photometric redshifts from Machine learning methods and stellar
masses/luminositites from stellar population synthesis. Our project aimed at
investigating the evolution of the colour and structural properties of galaxies
with mass and environment up to redshift and more, to put
constraints on galaxy evolution processes, as galaxy mergers.Comment: 4 pages, 2 figures, to appear on the refereed Proceeding of the "The
Universe of Digital Sky Surveys" conference held at the INAF--OAC, Naples, on
25th-28th november 2014, to be published on Astrophysics and Space Science
Proceedings, edited by Longo, Napolitano, Marconi, Paolillo, Iodic
Colour and stellar population gradients in galaxies
We discuss the colour, age and metallicity gradients in a wide sample of
local SDSS early- and late-type galaxies. From the fitting of stellar
population models we find that metallicity is the main driver of colour
gradients and the age in the central regions is a dominant parameter which
rules the scatter in both metallicity and age gradients. We find a consistency
with independent observations and a set of simulations. From the comparison
with simulations and theoretical considerations we are able to depict a general
picture of a formation scenario.Comment: 4 pages, 4 figures. Proceedings of 54th Congresso Nazionale della
SAIt, Napoli 4-7 May 201
Dynamical and gravitational lensing properties of a new phenomenological model of elliptical galaxies
Recent observations of the line of sight velocity profile of elliptical galaxies have furnished controversial results with some works favouring the presence of a large amount of dark matter in the outer regions and others arguing in favour of no dark matter at all. In order to shed new light on this controversy, we propose here a new phenomenological description of the total mass profile of galaxies. Under the hypothesis of spherical symmetry, we assume a double power-law expression for the global M/L ratio Upsilon(r)= Upsilon_0(r/r_0) ^{alpha}(1+r/r_0)^{beta}. In particular, Upsilon propto r^{alpha} for r/r_01 so that alpha1), Upsilon propto r^{alpha+beta} thus showing that models with alpha+beta=0 have an asymptotically constant M/L ratio. A wide range of possibilities is obtained by varying the slope parameters in the range we determine on the basis of physical considerations. Choosing a general expression for the luminosity density profile j(r), we work out an effective galaxy model that accounts for all the phenomenology observed in real elliptical galaxies. We derive the main dynamics and lensing properties of such an effective model. We analyze a general class of models, able to take into account different dynamical trends. We are able to obtain analytical expressions for the main dynamical and lensing quantities. We show that constraining the values of alpha+beta makes it possible to analyze the problem of the dark matter in elliptical galaxies. Indeed, positive values of alpha+beta would be a strong evidence for dark matter. Finally we indicate possible future approaches in order to face the observational data, in particular using velocity dispersion profiles and lensed quasar events
Dark matter scaling relations in intermediate z haloes
We investigate scaling relations between the dark matter (DM) halo model
parameters for a sample of intermediate redshift early - type galaxies (ETGs)
resorting to a combined analysis of Einstein radii and aperture velocity
dispersions. Modeling the dark halo with a Navarro - Frenk - White profile and
assuming a Salpeter initial mass function (IMF) to estimate stellar masses, we
find that the column density and the Newtonian acceleration within
the halo characteristic radius and effective radius are not
universal quantities, but correlate with the luminosity , the stellar mass
and the halo mass , contrary to recent claims in the
literature. We finally discuss a tight correlation among the DM mass
within the effective radius , the stellar mass
and itself. The slopes of the scaling relations
discussed here strongly depend, however, on the DM halo model and the IMF
adopted so that these ingredients have to be better constrained in order to
draw definitive conclusions on the DM scaling relations for ETGs.Comment: 8 pages, 1 figure, 4 tables, MNRAS submitted version (including
corrections after the referee report
KiDS0239-3211: A new gravitational quadruple lens candidate
We report the discovery of a candidate to quadrupole gravitationally lensed
system KiDS0239-3211 based on the public data release 3 of the KiDS survey and
machine learning techniques
Tribological behaviour of Ti or Ti alloy vs. zirconia in presence of artificial saliva
Abutment is the transmucosal component in a dental implant system and its eventual appearance has a major impact on aesthetics: use of zirconia abutments can be greatly advantageous in avoiding this problem. Both in the case of one and two-piece zirconia abutments, a critical issue is severe wear between the zirconia and titanium components. High friction at this interface can induce loosening of the abutment connection, production of titanium wear debris, and finally, peri-implant gingivitis, gingival discoloration, or marginal bone adsorption can occur. As in vivo wear measurements are highly complex and time-consuming, wear analysis is usually performed in simulators in the presence of artificial saliva. Different commercial products and recipes for artificial saliva are available and the effects of the different mixtures on the tribological behaviour is not widely explored. The specific purpose of this research was to compare two types of artificial saliva as a lubricant in titanium-zirconia contact by using the ball on disc test as a standard tribological test for materials characterisation. Moreover, a new methodology is suggested by using electrokinetic zeta potential titration and contact angle measurements to investigate the chemical stability at the titanium-lubricant interface. This investigation is of relevance both in the case of using zirconia abutments and artificial saliva against chronic dry mouth. Results suggest that an artificial saliva containing organic corrosion inhibitors is able to be firmly mechanically and chemically adsorb on the surface of the Ti c.p. or Ti6Al4V alloy and form a protective film with high wettability. This type of artificial saliva can significantly reduce the friction coefficient and wear of both the titanium and zirconia surfaces. The use of this type of artificial saliva in standard wear tests has to be carefully considered because the wear resistance of the materials can be overestimated while it can be useful in some specific clinical applications. When saliva is free from organic corrosion inhibitors, wear occurs with a galling mechanism. The occurrence of a super-hydrophilic saliva film that is not firmly adsorbed on the surface is not efficient in order to reduce wear. The results give both suggestions about the experimental conditions for lab testing and in vivo performance of components of dental implants when artificial saliva is used
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