632 research outputs found
The DPOSS II distant compact group survey: the EMMI-NTT spectroscopic sample
This paper presents the results of the redshift survey of 138 candidate
compact groups from the DPOSS II catalog (Iovino et al., 2003; de Carvalho et
al. 2005), which extends the available redshift range of spectroscopically
confirmed compact groups of galaxies to z~0.2. The aims of the survey are to
confirm group membership via spectroscopic redshift information, to measure the
characteristic parameters of the confirmed groups, namely mass, radius,
luminosity, velocity dispersion and crossing time, and to compare them with
those of nearby compact groups. Using available information from the
literature, we also studied the surrounding group environment and searched for
additional, previously unknown, group members, or larger scale structures to
whom the group might be associated. Of the 138 observed groups, 96 had three or
more concordant galaxies, i.e. a 70% success rate. Of these 96, 62 are isolated
on the sky, while the other 34 are close on the sky to a larger scale
structure. The remaining objects turned out to be couple of pairs or chance
projection of galaxies on the sky. Group environment and the characteristics
parameters (mass, crossing time, velocity dispersion) are evaluated and
discussed.Comment: Accepted on A&A, version updated to match the printed one. The paper
will read well even without printing figures 8 and
Photometric and spectroscopic study of the intermediate age open cluster NGC 3960
We present CCD UBVI photometry and high-resolution spectroscopy of the
intermediate age open cluster NGC 3960. The colour - magnitude diagrams (CMDs)
derived from the photometric data and interpreted with the synthetic CMD method
allow us to estimate the cluster parameters. We derive: age = 0.9 or 0.6 Gyr
(depending on whether or not overshooting from convective regions is included
in the adopted stellar models), distance (m-M)0 = 11.6 +/- 0.1, reddening
E(B-V) = 0.29 +/- 0.02, differential reddening Delta E(B-V) = 0.05 and
approximate metallicity between solar and half of solar. We obtained high
resolution spectra of three clump stars, and derived an average [Fe/H] = -0.12
(rms 0.04 dex), in very good agreement with the photometric determination. We
also obtained abundances of alpha-elements, Fe-peak elements, and of Ba. The
reddenings toward individual stars derived from the spectroscopic temperatures
and the Alonso et al. calibrations give further support to the existence of
significative variations across the cluster.Comment: Accepted for publication on MNRAS; fig. 3, 4, 5, 6 at degraded
resolutio
The pseudobulge of NGC 1292
The photometric and kinematic properties of Sb NGC 1292 suggest it hosts a
pseudobulge. The properties of the stellar population of such a pseudobulge are
consistent with a slow buildup within a scenario of secular evolution.Comment: 2 pages, 1 figure to appear in the proceedings of "Formation and
Evolution of Galaxy Disks", Rome, October 2007, Eds. J. Funes and E. M.
Corsin
Magnetic losses in Si-Fe alloys for avionic applications
This paper presents an experimental analysis of the rotational power losses of the magnetic materials of transformers, motors and actuators used in avionic environment. A large frequency range is investigated using a suitable experimental test frame developed to measure the power losses for a circular magnetization. The results about different silicon iron alloys with different textures and thickness are considered and compared
Recovering star formation histories: Integrated-light analyses vs stellar colour-magnitude diagrams
Accurate star formation histories (SFHs) of galaxies are fundamental for
understanding the build-up of their stellar content. However, the most accurate
SFHs - those obtained from colour-magnitude diagrams (CMDs) of resolved stars
reaching the oldest main sequence turnoffs (oMSTO) - are presently limited to a
few systems in the Local Group. It is therefore crucial to determine the
reliability and range of applicability of SFHs derived from integrated light
spectroscopy, as this affects our understanding of unresolved galaxies from low
to high redshift.
To evaluate the reliability of current full spectral fitting techniques in
deriving SFHs from integrated light spectroscopy by comparing SFHs from
integrated spectra to those obtained from deep CMDs of resolved stars.
We have obtained a high signal--to--noise (S/N 36.3 per \AA)
integrated spectrum of a field in the bar of the Large Magellanic Cloud (LMC)
using EFOSC2 at the 3.6 meter telescope at La Silla Observatory. For this same
field, resolved stellar data reaching the oMSTO are available. We have compared
the star formation rate (SFR) as a function of time and the age-metallicity
relation (AMR) obtained from the integrated spectrum using {\tt STECKMAP}, and
the CMD using the IAC-star/MinnIAC/IAC-pop set of routines. For the sake of
completeness we also use and discuss other synthesis codes ({\tt STARLIGHT} and
{\tt ULySS}) to derive the SFR and AMR from the integrated LMC spectrum.
We find very good agreement (average differences 4.1 ) between the
SFR(t) and the AMR obtained using {\tt STECKMAP} on the integrated light
spectrum, and the CMD analysis. {\tt STECKMAP} minimizes the impact of the
age-metallicity degeneracy and has the advantage of preferring smooth solutions
to recover complex SFHs by means of a penalized . [abridged]Comment: 23 pages, 24 figures. Accepted for publication in A&A (6 Sep 2015
Kinematic and stellar population properties of the counter-rotating components in the S0 galaxy NGC 1366
Context. Many disk galaxies host two extended stellar components that rotate in opposite directions. The analysis of the stellar populations of the counter-rotating components provides constraints on the environmental and internal processes that drive their formation. Aims. The S0 NGC 1366 in the Fornax cluster is known to host a stellar component that is kinematically decoupled from the main body of the galaxy. Here we successfully separated the two counter-rotating stellar components to independently measure the kinematics and properties of their stellar populations. Methods. We performed a spectroscopic decomposition of the spectrum obtained along the galaxy major axis and separated the relative contribution of the two counter-rotating stellar components and of the ionized-gas component. We measured the line-strength indices of the two counter-rotating stellar components and modeled each of them with single stellar population models that account for the \u3b1/Fe overabundance. Results. We found that the counter-rotating stellar component is younger, has nearly the same metallicity, and is less \u3b1/Fe enhanced than the corotating component. Unlike most of the counter-rotating galaxies, the ionized gas detected in NGC 1366 is neither associated with the counter-rotating stellar component nor with the main galaxy body. On the contrary, it has a disordered distribution and a disturbed kinematics with multiple velocity components observed along the minor axis of the galaxy. Conclusions. The different properties of the counter-rotating stellar components and the kinematic peculiarities of the ionized gas suggest that NGC 1366 is at an intermediate stage of the acquisition process, building the counter-rotating components with some gas clouds still falling onto the galaxy. \ua9 ESO 2017
Optical and radio survey of Southern Compact Groups of galaxies. I. Pilot study of six groups
Multi-wavelength observations of Hickson's Compact Groups (HCGs) have shown
that many of these groups are physical bound structures and are in different
stage of evolution, from spiral-dominated systems to almost merged objects.
Very few studies have analysed the Southern Compact Groups (SCGs) sample, which
is though to be younger that HCGs, due to an on average higher number of spiral
galaxies. We present here the first results from optical and radio observations
on a pilot sample of SCGs.Comment: accepted on A&A on July 19, 2007. Figures 1 and 3-12 will be
available only in electronic for
DEPOSIZIONE AUTOCATALITICA DI COMPOSITI A MATRICE NI-P
Nel presente lavoro è stata studiata la deposizione autocatalitica di compositi Ni-P-B4C, Ni-P-CNT e Ni-PAl2O3 attraverso l’impiego di un elettrolita a base di sodio ipofosfito in cui sono state disperse particelle nanometriche di B4C, CNT e Al2O3. La dimensione delle particelle di Al2O3 e B4C è compresa rispettivamente tra 50-70 nm e 25-30 nm. I nanotubi di carbonio presentano un diametro compreso tra 10-30 nm. Per ciascun tipo di composito, sono state effettuate prove con concentrazioni comprese tra 0 e 4 g/l. Sono stati studiati gli effetti della concentrazione di particelle all’interno del bagno sulla velocità di deposizione, sulle caratteristiche meccaniche e sulle proprietà tribologiche dei depositi
The XXL Survey VIII: MUSE characterisation of intracluster light in a z0.53 cluster of galaxies
Within a cluster, gravitational effects can lead to the removal of stars from
their parent galaxies. Gas hydrodynamical effects can additionally strip gas
and dust from galaxies. The properties of the ICL can therefore help constrain
the physical processes at work in clusters by serving as a fossil record of the
interaction history. The present study is designed to characterise this ICL in
a ~10^14 M_odot and z~0.53 cluster of galaxies from imaging and spectroscopic
points of view. By applying a wavelet-based method to CFHT Megacam and WIRCAM
images, we detect significant quantities of diffuse light. These sources were
then spectroscopically characterised with MUSE. MUSE data were also used to
compute redshifts of 24 cluster galaxies and search for cluster substructures.
An atypically large amount of ICL has been detected in this cluster. Part of
the detected diffuse light has a very weak optical stellar component and
apparently consists mainly of gas emission, while other diffuse light sources
are clearly dominated by old stars. Furthermore, emission lines were detected
in several places of diffuse light. Our spectral analysis shows that this
emission likely originates from low-excitation parameter gas. The stellar
contribution to the ICL is about 2.3x10^9 yrs old even though the ICL is not
currently forming a large number of stars. On the other hand, the contribution
of the gas emission to the ICL in the optical is much greater than the stellar
contribution in some regions, but the gas density is likely too low to form
stars. These observations favour ram pressure stripping, turbulent viscous
stripping, or supernovae winds as the origin of the large amount of
intracluster light. Since the cluster appears not to be in a major merging
phase, we conclude that ram pressure stripping is the most plausible process
that generates the observed ICL sources.Comment: Accepted in A&A, english enhanced, figure location different than in
the A&A version due to different style files, shortened abstrac
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