869 research outputs found
Galactic and Cosmic Type Ia SN rates: is it possible to impose constraints on SNIa progenitors?
We compute the Type Ia supernova rates in typical elliptical galaxies by
varying the progenitor models for Type Ia supernovae. To do that a formalism
which takes into account the delay distribution function (DTD) of the explosion
times and a given star formation history is adopted. Then the chemical
evolution for ellipticals with baryonic initial masses , and
is computed, and the mass of Fe produced by each galaxy is
precisely estimated. We also compute the expected Fe mass ejected by
ellipticals in typical galaxy clusters (e.g. Coma and Virgo), under different
assumptions about Type Ia SN progenitors. As a last step, we compute the cosmic
Type Ia SN rate in an unitary volume of the Universe by adopting several cosmic
star formation rates and compare it with the available and recent observational
data. Unfortunately, no firm conclusions can be derived only from the cosmic
SNIa rate, neither on SNIa progenitors nor on the cosmic star formation rate.
Finally, by analysing all our results together, and by taking into account
previous chemical evolution results, we try to constrain the best Type Ia
progenitor model. We conclude that the best progenitor models for Type Ia SNe
are still the single degenerate model, the double degenerate wide model, and
the empirical bimodal model. All these models require the existence of prompt
Type Ia supernovae, exploding in the first 100 Myr since the beginning of star
formation, although their fraction should not exceed 15-20% in order to fit
chemical abundances in galaxies.Comment: 17 pages, 11 figures, Submitted to MNRA
Galaxy Evolution, Deep Galaxy Counts and the Near-IR Cosmic Infrared Background
Accurate synthetic models of stellar populations are constructed and used in
evolutionary models of stellar populations in forming galaxies. Following their
formation, the late type galaxies are assumed to follow the Schmidt law for
star formation, while early type galaxies are normalized to the present-day
fundamental plane relations assumed to mimic the metallicity variations along
their luminosity sequence. We then compute predictions of these models for the
observational data at early epochs for various cosmological parameters and . We find good match to the metallicity data from the
damped systems and the evolution of the luminosity density out to
. Likewise, our models provide good fits for low values of
to the deep number counts of galaxies in all bands where data is available;
this is done without assuming existence of extra populations of galaxies at
high . Our models also match the data on the redshift distribution of galaxy
counts in and bands. We compute the predicted mean levels and angular
distribution of the cosmic infrared background produced from the early
evolution of galaxies. The predicted fluxes and fluctuations are still below
the current observational limits, but not by a large factor. Finally, we find
that the recent detection of the diffuse extragalactic light in the visible
bands requires for our models high redshift of galaxy formation, (3-4); otherwise the produced flux of the extragalactic light at optical
bands exceeds the current observational limits.Comment: Accepted to Ap
A Search for the Damped Ly-alpha Absorber at z=1.86 toward QSO 1244+3443 with NICMOS
We have carried out a high-resolution imaging search for the galaxy
associated with the damped Lyman-alpha (DLA) absorber at z=1.859 toward the
z_{em}=2.48 quasar QSO 1244+3443, using the HST and the NICMOS. Images were
obtained in the broad filter F160W and the narrow filter F187N with camera 2 on
NICMOS with the goal of detecting the rest-frame optical continuum and the
H-alpha line emission from the DLA. After PSF subtraction, two weak features
are seen at projected separations of 0.16-0.24" from the quasar. Parts of these
features may be associated with the DLA absorber, although we cannot completely
rule out that they could be artifacts of the point spread function (PSF). If
associated with the DLA, the objects would be ~1-2 h_{70}^{-1} kpc in size with
integrated flux densities of 2.5 and 3.3 mu Jy in the F160W filter, implying
luminosities at lambda_{central}=5600 A in the DLA rest frame of 4.4-5.9 x
10^{9} h_{70}^{-2} L_{solar} at z=1.86, for q0=0.5. However, no significant
H-alpha line emission is seen from these objects, suggesting low star formation
rates (SFRs). Our 3 sigma upper limit on the SFR in the DLA is 1.3 h_{70}^{-2}
M_{solar}/yr for q0 = 0.5 (2.4 h_{70}^{-2} M_{solar} yr^{-1} for q0 = 0.1).
This together with our earlier result for LBQS 1210+1731 mark a significant
improvement over previous constraints on the star formation rates of DLAs. A
combination of low SFR and some dust extinction is likely to be responsible for
the lack of H-alpha emission. Alternatively, the objects, may be associated
with the quasar host galaxy. In any case, our observations suggest that the DLA
is not a large bright proto-disk, but a compact object or a low-surface
brightness galaxy. If the two features are PSF artifacts then the constraints
on DLA properties are even more severe.Comment: 28 pages, 9 figures. Accepted for publication in The Astrophysical
Journal. Figures are given at a slightly lower resolution here, to decrease
file sizes. The higher resolution versions can be found in the Ap
Stellar populations in gas-rich galaxy mergers II. Feedback effects of Type Ia and II supernovae
We numerically investigate chemodynamical evolution of major disk-disk galaxy
mergers in order to explore the origin of mass-dependent chemical, photometric,
and spectroscopic properties observed in elliptical galaxies. We particularly
investigate the dependence of the fundamental properties on merger progenitor
disk mass (M_d). Main results obtained in this study are the following three.
(1) More massive (luminous) ellipticals formed by galaxy mergers between more
massive spirals have larger metallicity (Z) and thus show redder colors: The
typical metallicity ranges from ~ 1.0 solar abundance (Z~ 0.02) for ellipticals
formed by mergers with M_d = 10^10 M_solar to ~ 2.0 solar (Z ~ 0.04) for those
with M_d = 10^12 M_solar. (2) The absolute magnitude of negative metallicity
gradients developed in galaxy mergers is more likely to be larger for massive
ellipticals.
Absolute magnitude of metallicity gradient correlates with that of age
gradient in ellipticals in the sense that an elliptical with steeper negative
metallicity gradient is more likely to show steeper age gradient. (3) Both
M/L_B and M/L_K, where M, L_B, and L_K are total stellar mass of galaxy
mergers, B-band luminosity, and K-band one, respectively, depend on galactic
mass in such a way that more massive ellipticals have larger M/L_B and smaller
M/L_K.Comment: 58 pages 16 figures, ApJ in press (March 1999 issue
High Redshift Quasars and Star Formation in the Early Universe
In order to derive information on the star formation history in the early
universe we observed 6 high-redshift (z=3.4) quasars in the near-infrared to
measure the relative iron and \mgii emission strengths. A detailed comparison
of the resulting spectra with those of low-redshift quasars show essentially
the same FeII/MgII emission ratios and very similar continuum and line spectral
properties, indicating a lack of evolution of the relative iron to magnesium
abundance of the gas since z=3.4 in bright quasars. On the basis of current
chemical evolution scenarios of galaxies, where magnesium is produced in
massive stars ending in type II SNe, while iron is formed predominantly in SNe
of type Ia with a delay of ~1 Gyr and assuming as cosmological parameters H_o =
72 km/s Mpc, Omega_M = 0.3, and Omega_Lambda = 0.7$, we conclude that major
star formation activity in the host galaxies of our z=3.4 quasars must have
started already at an epoch corresponding to z_f ~= 10, when the age of the
universe was less than 0.5 Gyrs.Comment: 29 pages, 5 figures, ApJ in pres
Closing the loop of SIEM analysis to Secure Critical Infrastructures
Critical Infrastructure Protection is one of the main challenges of last years. Security Information and Event Management (SIEM) systems are widely used for coping with this challenge. However, they currently present several limitations that have to be overcome. In this paper we propose an enhanced SIEM system in which we have introduced novel components to i) enable multiple layer data analysis; ii) resolve conflicts among security policies, and discover unauthorized data paths in such a way to be able to reconfigure network devices. Furthermore, the system is enriched by a Resilient Event Storage that ensures integrity and unforgeability of events stored
A Mechanism for the Oxygen and Iron Bimodal Radial Distribution Formation in the Disc of our Galaxy
Recently it has been proposed that there are two types of SN Ia progenitors
-- short-lived and long-lived. On the basis of this idea, we develope a theory
of a unified mechanism for the formation of the bimodal radial distribution of
iron and oxygen in the Galactic disc. The underlying cause for the formation of
the fine structure of the radial abundance pattern is the influence of spiral
arms, specifically, the combined effect of the corotation resonance and
turbulent diffusion. From our modelling we conclude that to explain the bimodal
radial distributions simultaneously for oxygen and iron and to obtain
approximately equal total iron output from different types of supernovae, the
mean ejected iron mass per supernova event should be the same as quoted in
literature if maximum mass of stars, that eject heavy elements, is . For the upper mass limit of the production of iron
by a supernova II explosion should be increased by about 1.5 times.Comment: 7 pages, 6 figures, MNRAS submitte
VLT Spectroscopy of Globular Clusters in Low Surface Brightness Dwarf Galaxies
We present VLT/FORS2 spectroscopic observations of globular clusters (GCs) in
five low surface brightness (LSB) dwarf galaxies: KK211 and KK221, which are
both dwarf spheroidal satellites (dSph) of NGC 5128, dSph KK84 located close to
the isolated S0 galaxy NGC 3115, and two isolated dwarf irregular (dIrr)
galaxies UGC 3755 and ESO 490-17. Our sample is selected from the Sharina et
al. (2005) database of Hubble Space Telescope WFPC2 photometry of GC candidates
in dwarf galaxies. For objects with accurate radial velocity measurements we
confirm 26 as genuine GCs out of the 27 selected candidates from our WFPC2
survey. Lick absorption line indices in the spectra of confirmed GCs and the
subsequent comparison with SSP model predictions show that all confirmed GCs in
dSphs are old, except GC KK211-3-149 (6 +/- 2 Gyr), which we consider to be the
nucleus of KK211. GCs in UGC 3755 and ESO 490-17 show a large spread in ages
ranging from old objects (t > 10 Gyr) to clusters with ages around 1 Gyr. Most
of our sample GCs have low metallicities [Z/H] <= -1. Two relatively metal-rich
clusters with [Z/H] ~ -0.3 are likely to be associated with NGC 3115. Our
sample GCs show in general a complex distribution of alpha-element enhancement
with a mean [alpha/Fe]=0.19 +/-0.04 derived with the chi2 minimization
technique and 0.18+/-0.12 dex computed with the iterative approach. These
values are slightly lower than the mean [alpha/Fe]=0.29+/-0.01 for typical
Milky Way GCs. We compare other abundance ratios with those of Local Group GCs
and find indications for systematic differences in N and Ca abundance. The
specific frequencies, S_N, of our sample galaxies are in line with the
predictions of a simple mass-loss model for dwarf galaxies and compare well
with S_N values found for dwarf galaxies in nearby galaxy clusters.Comment: accepted for publication in Ap
A Near-Solar Metallicity, Nitrogen-Deficient Lyman Limit Absorber Associated with two S0 Galaxies
From UV spectra of the bright quasar PHL 1811 recorded by FUSE and the E140M
configuration on STIS, we have determined the abundances of various atomic
species in a Lyman limit system at z = 0.0809 with log N(H I) = 17.98.
Considerably more hydrogen may be in ionized form, since the abundances of C
II, Si II, S II and Fe II are very large compared to that of O I, when compared
to their respective solar abundance ratios. Our determination [O/H] = -0.19 in
the H I-bearing gas indicates that the chemical enrichment of the gas is
unusually high for an extragalactic QSO absorption system. However, this same
material has an unusually low abundance of nitrogen, [N/O] < -0.59, indicating
that there may not have been enough time during this enrichment for secondary
nitrogen to arise from low and intermediate mass stars. In an earlier
investigation we found two galaxies at nearly the same redshift as this
absorption system and displaced by 34 and 87 kpc from the line of sight. An
r-band image recorded by the ACS on HST indicates these are S0 galaxies. One or
both of these galaxies may be the source of the gas, which might have been
expelled in a fast wind, by tidal stripping, or by ram-pressure stripping.
Subtraction of the ACS point-spread function from the image of the QSO reveals
the presence of a face-on spiral galaxy under the glare of the quasar; although
it is possible that this galaxy may be responsible for the Lyman limit
absorption, the exact alignment of the QSO with the center of the galaxy
suggests that the spiral is the quasar host.Comment: 74 pages, 14 figures; to be published in the Astrophysical Journal
(Part 1) May 1, 2005 issue. A version of the paper with figures of better
quality may be found at http://www.astro.princeton.edu/~ebj/PHL1811_paper.ps
(postscript) or http://www.astro.princeton.edu/~ebj/PHL1811_paper.pdf (pdf
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