4,683 research outputs found
The Excess Far-Infrared Emission of AGN in the Local Universe
We have cross-correlated the Sloan Digital Sky Survey (SDSS) second data
release spectroscopic galaxy sample with the IRAS faint-source catalogue (FSC).
Optical emission line ratios are used to classify the galaxies with reliable
IRAS 60 and 100 microns detections into AGN and normal star-forming galaxies.
We then create subsamples of normal galaxies and AGN that are very closely
matched in terms of key physical properties such as stellar mass, redshift,
size, concentration and mean stellar age (as measured by absorption line
indicators in the SDSS spectra). We then quantify whether there are systematic
differences between the IR luminosities of the galaxies and the AGN in the
matched subsamples. We find that the AGN exhibit a significant excess in far-IR
emission relative to the star-forming galaxies in our sample. The excesses at
60 and 100 microns are 0.21 +/- 0.03 dex and 0.12 +/- 0.035 dex in
log[L(60)/M*] and log[L(100)/M*], respectively. We then discuss whether the
far-IR excess is produced by radiation from the active nucleus that is absorbed
by dust or alternatively, by an extra population of young stars that is not
detectable at optical wavelengths.Comment: 12 pages, 14 figures, accepted by MNRA
Thermal conductivity of lipidic emulsions and its use for production and quality control
Thermal conductivity of lipidic emulsions has been experimentally determined by the probe method. To this purpose a special probe has been designed and built in laboratory, with small diameter (0.6 mm) and a high length to diameter ratio (100). The temperature sensor of the probe (type T thermocouple) and the heater (Pt wire) were properly calibrated. Moreover, the probe performance has been tested by means of a pure liquid (glycerin) having well known thermal conductivity by literature. Differences of about 1.5% at ambient temperature in thermal conductivity values between literature and experiments were found.
On lipidic emulsions first thermal conductivity has been measured in the temperature range 1040°C, second the same property as a function of time at constant temperature (40°C), then the values after freezing at –15°C and reheating at 20 °C; and last the kinetics of degeneration. Results show a significant difference between thermal conductivity values of a new emulsion (0.51 W/m K), compared with the creamed one (0.62 W/m K), and the decayed one (0.68 W/m K ). It has also put into evidence why the frozen emulsion cannot be used for intravenous injection, i.e. viscosity increases because of breaking of the oil particles. Finally information about the kinetics of the degeneration process have been obtained. The uncertainty resulting from the calibration and tests justifies the possible use of the measurement technique for process control of production, and also for quality control in the clinical practice
Mono- and Biexponential Luminescence Decays of Individual Single-Walled Carbon Nanotubes
We have studied the exciton recombination dynamics of individual (6,4) and (6,5) single-walled carbon nanotubes embedded in aqueous gels or deposited on glass surfaces. CoMoCat nanotubes systematically display short monoexponential photoluminescence (PL) decays presumably due to defects introduced during their synthesis. In contrast HiPco nanotubes can either display mono- or biexponential PL decays depending on the environmental conditions. Transition from bi- to monoexponential decays can be reproduced by a simple three level model taking into account defect-dependent nonradiative decay mechanisms
Fluctuation-induced interactions between dielectrics in general geometries
We study thermal Casimir and quantum non-retarded Lifshitz interactions
between dielectrics in general geometries. We map the calculation of the
classical partition function onto a determinant which we discretize and
evaluate with the help of Cholesky factorization. The quantum partition
function is treated by path integral quantization of a set of interacting
dipoles and reduces to a product of determinants. We compare the approximations
of pairwise additivity and proximity force with our numerical methods. We
propose a ``factorization approximation'' which gives rather good numerical
results in the geometries that we study
The Fermi-Pasta-Ulam problem and its underlying integrable dynamics: an approach through Lyapunov Exponents
FPU models, in dimension one, are perturbations either of the linear model or
of the Toda model; perturbations of the linear model include the usual
-model, perturbations of Toda include the usual model. In
this paper we explore and compare two families, or hierarchies, of FPU models,
closer and closer to either the linear or the Toda model, by computing
numerically, for each model, the maximal Lyapunov exponent . We study the
asymptotics of for large (the number of particles) and small
(the specific energy ), and find, for all models, asymptotic
power laws , and depending on the model. The
asymptotics turns out to be, in general, rather slow, and producing accurate
results requires a great computational effort. We also revisit and extend the
analytic computation of introduced by Casetti, Livi and Pettini,
originally formulated for the -model. With great evidence the theory
extends successfully to all models of the linear hierarchy, but not to models
close to Toda
The excess far-infrared emission of active galactic nuclei in the local Universe
We have cross-correlated the Sloan Digital Sky Survey (SDSS) second data release spectroscopic galaxy sample with the IRAS Faint Source Catalogue (FSC). Optical emission line ratios are used to classify the galaxies with reliable IRAS 60- and 100-μm detections into active galactic nuclei (AGN) and normal star-forming galaxies. We then create subsamples of normal galaxies and AGN that are very closely matched in terms of key physical properties such as stellar mass, redshift, size, concentration and mean stellar age (as measured by absorption line indicators in the SDSS spectra). We then quantify whether there are systematic differences between the infrared (IR) luminosities of the galaxies and the AGN in the matched subsamples. We find that the AGN exhibit a significant excess in far-infrared (FIR) emission relative to the star-forming galaxies in our sample. The excesses at 60 and 100 μm are 0.21 ± 0.03 and 0.12 ± 0.035 dex in log L60/M★ and log L100/M★, respectively. We then discuss whether the FIR excess is produced by radiation from the active nucleus that is absorbed by dust or, alternatively, by an extra population of young stars that is not detectable at optical wavelength
SPIDER X - Environmental effects in central and satellite early-type galaxies through the stellar fossil record
A detailed analysis of how environment affects the star formation history of
early-type galaxies (ETGs) is undertaken via high signal to noise ratio stacked
spectra obtained from a sample of 20,977 ETGs (morphologically selected) from
the SDSS-based SPIDER survey. Two major parameters are considered for the
study: the central velocity dispersion (sigma), which relates to local drivers
of star formation, and the mass of the host halo, which relates to
environment-related effects. In addition, we separate the sample between
centrals (the most massive galaxy in a halo) and satellites. We derive trends
of age, metallicity, and [alpha/Fe] enhancement, with sigma. We confirm that
the major driver of stellar population properties in ETGs is velocity
dispersion, with a second-order effect associated to the central/satellite
nature of the galaxy. No environmental dependence is detected for satellite
ETGs, except at low sigma - where satellites in groups or in the outskirts of
clusters tend to be younger than those in the central regions of clusters. In
contrast, the trends for centrals show a significant dependence on halo mass.
Central ETGs in groups (i.e. with a halo mass >10^12.5 M_Sun) have younger
ages, lower [alpha/Fe], and higher internal reddening, than "isolated" systems
(i.e. centrals residing in low-mass, <10^12.5 M_Sun, halos). Our findings imply
that central ETGs in groups formed their stellar component over longer time
scales than "isolated" centrals, mainly because of gas-rich interactions with
their companion galaxies.Comment: 22 pages, 19 figures, accepted for publication in MNRA
Numerical methods for fluctuation driven interactions between dielectrics
We develop a discretized theory of thermal Casimir interactions to
numerically calculate the interactions between fluctuating dielectrics. From a
constrained partition function we derive a surface free energy, while handling
divergences that depend on system size and discretization. We derive analytic
results for parallel plate geometry in order to check the convergence of the
numerical methods. We use the method to calculate vertical and lateral Casimir
forces for a set of grooves.Comment: revtex, 20 page
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