2,159 research outputs found
The Chemical Evolution of the Galaxy: the two-infall model
In this paper we present a new chemical evolution model for the Galaxy which
assumes two main infall episodes for the formation of halo-thick disk and thin
disk, respectively. We do not try to take into account explicitly the evolution
of the halo but we implicitly assume that the timescale for the formation of
the halo was of the same order as the timescale for the formation of the thick
disk. The formation of the thin-disk is much longer than that of the thick
disk, implying that the infalling gas forming the thin-disk comes not only from
the thick disk but mainly from the intergalactic medium. The timescale for the
formation of the thin-disk is assumed to be a function of the galactocentric
distance, leading to an inside-out picture for the Galaxy building. The model
takes into account the most up to date nucleosynthesis prescriptions and adopts
a threshold in the star formation process which naturally produces a hiatus in
the star formation rate at the end of the thick disk phase, as suggested by
recent observations. The model results are compared with an extended set of
observational constraints. Among these constraints, the tightest one is the
metallicity distribution of the G-dwarf stars for which new data are now
available. Our model fits very well these new data. We show that in order to
reproduce most of these constraints a timescale Gyr for the
(halo)-thick-disk and of 8 Gyr for the thin-disk formation in the solar
vicinity are required. We predict that the radial abundance gradients in the
inner regions of the disk () are steeper than in the outer
regions, a result confirmed by recent abundance determinations, and that the
inner ones steepen in time during the Galactic lifetime.Comment: 48 pages, 20 Postscript figures, AASTex v.4.0, to be published in
Astrophysical Journa
K dwarfs and the chemical evolution of the Solar cylinder
K-dwarfs have life-times older than the present age of the Galactic disc, and
are thus ideal stars to investigate the disc's chemical evolution. We have
developed several photometric metallicity indicators for K dwarfs, based an a
sample of accurate spectroscopic metallicities for 34 disc and halo G and K
dwarfs. The photometric metallicities lead us to develop a metallicity index
for K dwarfs based only on their position in the colour absolute-magnitude
diagram. Metallicities have been determined for 431 single K dwarfs drawn from
the Hipparcos catalog, selecting the stars by absolute magnitude and removing
multiple systems. The sample is essentially a complete reckoning of the metal
content in nearby K dwarfs. We use stellar isochrones to mark the stars by
mass, and select a subset of 220 of the stars which is complete in a narrow
mass interval. We fit the data with a model of the chemical evolution of the
Solar cylinder. We find that only a modest cosmic scatter is required to fit
our age metallicity relation. The model assumes two main infall episodes for
the formation of the halo-thick disc and thin disc respectively. The new data
confirms that the solar neighbourhood formed on a long timescale of order 7
Gyr.Comment: 14 pages, 15 figures, accepted by MNRA
Colour gradients of high-redshift Early-Type Galaxies from hydrodynamical monolithic models
We analyze the evolution of colour gradients predicted by the hydrodynamical
models of early type galaxies (ETGs) in Pipino et al. (2008), which reproduce
fairly well the chemical abundance pattern and the metallicity gradients of
local ETGs. We convert the star formation (SF) and metal content into colours
by means of stellar population synthetic model and investigate the role of
different physical ingredients, as the initial gas distribution and content,
and eps_SF, i.e. the normalization of SF rate. From the comparison with high
redshift data, a full agreement with optical rest-frame observations at z < 1
is found, for models with low eps_SF, whereas some discrepancies emerge at 1 <
z < 2, despite our models reproduce quite well the data scatter at these
redshifts. To reconcile the prediction of these high eps_SF systems with the
shallower colour gradients observed at lower z we suggest intervention of 1-2
dry mergers. We suggest that future studies should explore the impact of wet
galaxy mergings, interactions with environment, dust content and a variation of
the Initial Mass Function from the galactic centers to the peripheries.Comment: 13 pages, 7 figures, 1 table, accepted for publication on MNRA
The impact of stellar rotation on the CNO abundance patterns in the Milky Way at low metallicities
We investigate the effect of new stellar models, which take rotation into
account, computed for very low metallicities on the chemical evolution of the
earliest phases of the Milky Way. We check the impact of these new stellar
yields on a model for the halo of the Milky Way that can reproduce the observed
halo metallicity distribution. In this way we try to better constrain the ISM
enrichment timescale, which was not done in our previous work. The stellar
models adopted in this work were computed under the assumption that the ratio
of the initial rotation velocity to the critical velocity of stars is roughly
constant with metallicity. This naturally leads to faster rotation at lower
metallicity, as metal poor stars are more compact than metal rich ones. We find
that the new Z = 10-8 stellar yields computed for large rotational velocities
have a tremendous impact on the interstellar medium nitrogen enrichment for
log(O/H)+12 < 7 (or [Fe/H]< -3). We show that upon the inclusion of the new
stellar calculations in a chemical evolution model for the galactic halo with
infall and outflow, both high N/O and C/O ratios are obtained in the very-metal
poor metallicity range in agreement with observations. Our results give further
support to the idea that stars at very low metallicities could have initial
rotational velocities of the order of 600-800kms-1. An important contribution
to N from AGB stars is still needed in order to explain the observations at
intermediate metallicities. One possibility is that AGB stars at very low
metallicities also rotate fast. This could be tested in the future, once
stellar evolution models for fast rotating AGB stars will be available.Comment: Contribution to Nuclei in the Cosmos IX (Proceedings of Science - 9
pages, 4 figs., accepted) - Version 2: one reference added in the caption of
Fig.
The dust content of QSO hosts at high redshift
Infrared observations of high-z quasar (QSO) hosts indicate the presence of
large masses of dust in the early universe. When combined with other
observables, such as neutral gas masses and star formation rates, the dust
content of z~6 QSO hosts may help constraining their star formation history. We
have collected a database of 58 sources from the literature discovered by
various surveys and observed in the FIR. We have interpreted the available data
by means of chemical evolution models for forming proto-spheroids,
investigating the role of the major parameters regulating star formation and
dust production. For a few systems, given the derived small dynamical masses,
the observed dust content can be explained only assuming a top-heavy initial
mass function, an enhanced star formation efficiency and an increased rate of
dust accretion. However, the possibility that, for some systems, the dynamical
mass has been underestimated cannot be excluded. If this were the case, the
dust mass can be accounted for by standard model assumptions. We provide
predictions regarding the abundance of the descendants of QSO hosts; albeit
rare, such systems should be present and detectable by future deep surveys such
as Euclid already at z>4.Comment: 22 pages, 8 figures, MNRAS, accepte
IUE observations of oxygen-rich supernova remnants
The IUE observations were used to determine the composition of the ejecta (especially C and Si abundances) and to test models for the ionization and excitation of the ejecta of two oxygen-rich supernova remnants (N132D in the Large Magellanic Cloud and 1E 0102-7219 in the Small Magellanic Cloud). Time-dependent photoionization by the EUV and X-ray radiation from 1E 0102-7219 can qualitatively explain its UV and optical line emission, but the density and ionization structures are complex and prevent a unique model from being specified. Many model parameters are poorly constrained, including the time dependence and shape of the ionizing spectrum. Moreover, the models presented are not self-consistent in that the volumes and densities of the optically emitting gas imply optical depths of order unity in the EUV, but absorption of the ionizing radiation was ignored. It is possible that these shortcomings reflect a more fundamental limitation of the model assumptions. It is assumed that the electron velocity distribution is Maxwellian and that the energy deposited by photoionization heats the electrons directly. The 500 eV electrons produced by the Auger process may excite or ionize other ions before they slow down enough to share their energy with other electrons. Many of the excitations would produce photons that could ionize lower ionization stages
Retrotransposon-Encoded Reverse Transcriptase in the Genesis, Progression and Cellular Plasticity of Human Cancer
LINE-1 (Long Interspersed Nuclear Elements) and HERVs (Human Endogenous Retroviruses) are two families of autonomously replicating retrotransposons that together account for about 28% of the human genome. Genes harbored within LINE-1 and HERV retrotransposons, particularly those encoding the reverse transcriptase (RT) enzyme, are generally expressed at low levels in differentiated cells, but their expression is upregulated in transformed cells and embryonic tissues. Here we discuss a recently discovered RT-dependent mechanism that operates in tumorigenesis and reversibly modulates phenotypic and functional variations associated with tumor progression. Downregulation of active LINE-1 elements drastically reduces the tumorigenic potential of cancer cells, paralleled by reduced proliferation and increased differentiation. Pharmacological RT inhibitors (e.g., nevirapine and efavirenz) exert similar effects on tumorigenic cell lines, both in culture and in animal models. The HERV-K family play a distinct complementary role in stress-dependent transition of melanoma cells from an adherent, non-aggressive, to a non-adherent, highly malignant, growth phenotype. In synthesis, the retrotransposon-encoded RT is increasingly emerging as a key regulator of tumor progression and a promising target in a novel anti-cancer therapy
The N/O Plateau of Blue Compact Galaxies: Monte Carlo Simulations of the Observed Scatter
Chemical evolution models and Monte Carlo simulation techniques have been
combined for the first time to study the distribution of blue compact galaxies
on the N/O plateau. Each simulation comprises 70 individual chemical evolution
models. For each model, input parameters relating to a galaxy's star formation
history (bursting or continuous star formation, star formation efficiency),
galaxy age, and outflow rate are chosen randomly from ranges predetermined to
be relevant. Predicted abundance ratios from each simulation are collectively
overplotted onto the data to test its viability. We present our results both
with and without observational scatter applied to the model points. Our study
shows that most trial combinations of input parameters, including a simulation
comprising only simple models with instantaneous recycling, are successful in
reproducing the observed morphology of the N/O plateau once observational
scatter is added. Therefore simulations which include delay of nitrogen
injection are no longer favored over those which propose that most nitrogen is
produced by massive stars, if only the plateau morphology is used as the
principal constraint. The one scenario which clearly cannot explain plateau
morphology is one in which galaxy ages are allowed to range below 250 Myr. We
conclude that the present data for the N/O plateau are insufficient by
themselves for identifying the portion of the stellar mass spectrum most
responsible for cosmic nitrogen production.Comment: 41 pages, 15 figures; accepted by ApJ, to appear Aug. 20, 200
The Earliest Phases of Galaxy Evolution
In this paper we study the very early phases of the evolution of our Galaxy
by means of a chemical evolution model which reproduces most of the
observational constraints in the solar vicinity and in the disk. We have
restricted our analysis to the solar neighborhood and present the predicted
abundances of several elements (C, N, O, Mg, Si, S, Ca, Fe) over an extended
range of metallicities to compared to previous
models. We adopted the most recent yield calculations for massive stars taken
from different authors (Woosley & Weaver 1995 and Thielemann et al. 1996) and
compared the results with a very large sample of data, one of the largest ever
used to this purpose. These data have been analysed with a new and powerful
statistical method which allows us to quantify the observational spread in
measured elemental abundances and obtain a more meaningful comparison with the
predictions from our chemical evolution model. Our analysis shows that the
``plateau'' observed for the [/Fe] ratios at low metallicities () is not perfectly constant but it shows a slope, especially for
oxygen. This slope is very well reproduced by our model with both sets of
yields. This is not surprising since realistic chemical evolution models,
taking into account in detail stellar lifetimes, never predicted a completely
flat plateau. This is due either to the fact that massive stars of different
mass produce a slightly different O/Fe ratio or to the often forgotten fact
that supernovae of type Ia, originating from white dwarfs, start appearing
already at a galactic age of 30 million years and reach their maximum at 1 Gyr.Comment: 32 pages, 9 figures, to be published in Ap
On Dwarf Galaxies as the Source of Intracluster Gas
Recent observational evidence for steep dwarf galaxy luminosity functions in
several rich clusters has led to speculation that their precursors may be the
source of the majority of gas and metals inferred from intracluster medium
(ICM) x-ray observations. Their deposition into the ICM is presumed to occur
through early supernovae-driven winds, the resultant systems reflecting the
photometric and chemical properties of the low luminosity dwarf spheroidals and
ellipticals we observe locally. We consider this scenario, utilising a
self-consistent model for spheroidal photo-chemical evolution and gas ejection
via galactic superwinds. Insisting that post-wind dwarfs obey the observed
colour-luminosity-metallicity relations, we conclude that the bulk of the ICM
gas and metals does not originate within their precursors.Comment: 43 pages, 8 figures, LaTeX, also available at
http://msowww.anu.edu.au/~gibson/publications.html, to appear in ApJ, Vol
473, 1997, in pres
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