2,548 research outputs found
On the formation of dwarf galaxies and stellar halos
Using analytic arguments and a suite of very high resolution (10^3 Msun per
particle) cosmological hydro-dynamical simulations, we argue that high
redshift, z ~ 10, M ~ 10^8 Msun halos, form the smallest `baryonic building
block' (BBB) for galaxy formation. These halos are just massive enough to
efficiently form stars through atomic line cooling and to hold onto their gas
in the presence of supernovae winds and reionisation. These combined effects,
in particular that of the supernovae feedback, create a sharp transition: over
the mass range 3-10x10^7 Msun, the BBBs drop two orders ofmagnitude in stellar
mass. Below ~2x10^7 Msun, galaxies will be dark with almost no stars and no
gas. Above this scale is the smallest unit of galaxy formation: the BBB.
A small fraction (~100) of these gas rich BBBs fall in to a galaxy the size
of the Milky Way. Ten percent of these survive to become the observed LG dwarf
galaxies at the present epoch. Those in-falling halos on benign orbits which
keep them far away from the Milky Way or Andromeda manage to retain their gas
and slowly form stars - these become the smallest dwarf irregular galax ies;
those on more severe orbits lose their gas faster than they can form stars and
become the dwarf spheroidals. The remaining 90% of the BBBs will be accreted.
We show that this gives a metallicity and total stellar mass consistent with
the Milky Way old stellar halo (abridged).Comment: 15 pages, 7 figures, one figure added to match accepted version. Some
typos fixed. MNRAS in pres
The effect of neutrinos on the matter distribution as probed by the Intergalactic Medium
We present a suite of full hydrodynamical cosmological simulations that
quantitatively address the impact of neutrinos on the (mildly non-linear)
spatial distribution of matter and in particular on the neutral hydrogen
distribution in the Intergalactic Medium (IGM), which is responsible for the
intervening Lyman-alpha absorption in quasar spectra. The free-streaming of
neutrinos results in a (non-linear) scale-dependent suppression of power
spectrum of the total matter distribution at scales probed by Lyman-alpha
forest data which is larger than the linear theory prediction by about 25% and
strongly redshift dependent. By extracting a set of realistic mock quasar
spectra, we quantify the effect of neutrinos on the flux probability
distribution function and flux power spectrum. The differences in the matter
power spectra translate into a ~2.5% (5%) difference in the flux power spectrum
for neutrino masses with Sigma m_{\nu} = 0.3 eV (0.6 eV). This rather small
effect is difficult to detect from present Lyman-alpha forest data and nearly
perfectly degenerate with the overall amplitude of the matter power spectrum as
characterised by sigma_8. If the results of the numerical simulations are
normalized to have the same sigma_8 in the initial conditions, then neutrinos
produce a smaller suppression in the flux power of about 3% (5%) for Sigma
m_{\nu} = 0.6 eV (2
sigma C.L.), comparable to constraints obtained from the cosmic microwave
background data or other large scale structure probes.Comment: 38 pages, 21 figures. One section and references added. JCAP in pres
On the formation of dwarf galaxies and stellar haloes
Using analytic arguments and a suite of very high resolution (∼103 M⊙ per particle) cosmological hydrodynamical simulations, we argue that high-redshift, z∼ 10, M∼ 108 M⊙ haloes, form the smallest ‘baryonic building block' (BBB) for galaxy formation. These haloes are just massive enough to efficiently form stars through atomic line cooling and to hold on to their gas in the presence of supernova (SN) winds and reionization. These combined effects, in particular that of the SN feedback, create a sharp transition: over the mass range 3-10 × 107 M⊙, the BBBs drop two orders of magnitude in stellar mass. Below ∼2 × 107 M⊙, galaxies will be dark with almost no stars and no gas. Above this scale is the smallest unit of galaxy formation: the BBB. We show that the BBBs have stellar distributions which are spheroidal, of low rotational velocity, old and metal poor: they resemble the dwarf spheroidal galaxies (dSphs) of the Local Group (LG). Unlike the LG dSphs, however, they contain significant gas fractions. We connect these high-redshift BBBs to the smallest dwarf galaxies observed at z= 0 using linear theory. A small fraction (∼100) of these gas-rich BBBs at high redshift fall in to a galaxy the size of the Milky Way (MW). We suggest that 10 per cent of these survive to become the observed LG dwarf galaxies at the present epoch. This is consistent with recent numerical estimates. Those infalling haloes on benign orbits which keep them far away from the MW or Andromeda manage to retain their gas and slowly form stars - these become the smallest dwarf irregular galaxies; those on more severe orbits lose their gas faster than they can form stars and become the dwarf spheroidals. The remaining 90 per cent of the BBBs will be accreted. We show that this gives a metallicity and total stellar mass consistent with the MW old stellar hal
Possible evidence for an inverted temperature-density relation in the intergalactic medium from the flux distribution of the Lyman-alpha forest
We compare the improved measurement of the Lya forest flux probability
distribution at 1.7<z<3.2 presented by Kim et al. (2007) to a large set of
hydrodynamical simulations of the Lya forest with different cosmological
parameters and thermal histories. The simulations are in good agreement with
the observational data if the temperature-density relation for the low density
intergalactic medium (IGM), T=T_0 Delta^{gamma-1}, is either close to
isothermal or inverted (gamma<1). Our results suggest that the voids in the IGM
may be significantly hotter and the thermal state of the low density IGM may be
substantially more complex than is usually assumed at these redshifts. We
discuss radiative transfer effects which alter the spectral shape of ionising
radiation during the epoch of HeII reionisation as a possible physical
mechanism for achieving an inverted temperature-density relation at z~3.Comment: 16 pages, 6 figures, accepted for publication in MNRAS following
minor revision. The accepted version includes an expanded discussion of the
flux power spectru
Diferenciação de rochas vulcânicas da formação serra geral utilizando gamaespectrometria terrestre na região vitivinícola Serra Gaúcha, RS - Brasil.
A Região Vitivinícola Serra Gaúcha (RVSG) possui fatores naturais e culturais aliados à geodiversidade da região que implica na formação de solos e relevos diferenciados. Essa particularidade, por sua vez, acarreta em respostas agronômicas específicas da videira e possibilita a valorização da produção de vinhos com distintas qualidades que caracterizam, consequentemente, diferentes terroírs. A área de estudo se situa no contexto de áreas de indicações geográficas para vinhos finos (Vale do Rio das Antas), no limite das unidades geomorfológicas Serra Geral e Planalto dos Campos Gerais, esculpidas sobre rochas da Formação Serra Geral. Na área ocorrem as Fácies Gramado e Caxias. Na primeira, têm-se basaltos de 132 milhões de anos, granulares finos a médios, melanocráticos; na segunda têm-se rochas intermediárias a ácidas (riodacíticas) de 131 milhões de anos, mesocráticas, granulares finas a microfaneríticas. Os horizontes superiores apresentam disjunção tabular bem desenvolvida e as partes centrais dos derrames são maciças, podendo apresentar estruturas de fluxo laminar e dobras. O relevo foi originado na era mesozóica por intenso vulcanismo fissural, havendo platôs com escarpas íngremes e o arcabouço estrutural mostra fraturas e falhas que condicionam a padrões de drenagem angulares e o entalhe das vertentes retilíneas. As áreas cultivadas com vinhedos na RVSG situam-se sobre zonas de maior altitude e menor declividade, relativas aos topos dos platôs, onde predominam rochas ácidas a intermediárias (Fácies Caxias), contendo argissolos, cambissolos e nitossolos. Nas áreas íngremes sobre rochas básicas (Fácies Gramado), ocorrem alissolos e chernossolos situados nos patamares inferiores. O objetivo deste trabalho foi testar um método rápido de distinção de rochas ácidas e básicas, por meio de gamaespectrometria terrestre. As medições foram adquiridas em uma área de 800 Km2 com orientação NE-SW, num perfil transversal da RVSG. O método utilizado empregou o amaespectrometro portátil da marca Radiation Solutíons, modelo super Spec RS-125 de 1024 canais espectrais, cedido pela UNISINOS/NEAP e GPS Garmin Montana 650, sendo o trabalho de campo apoiado pela Embrapa Uva e Vinho. Foram analisadas 83 medidas de rochas, sendo 59 da Fácies Caxias e 24 da Fácies Gramado, em sua maioria de rochas sãs. A classificação dessas rochas foi realizada utilizando critérios descritivos de campo. As medidas de K, eU e eTh foram comparadas na forma de gráficos, relativamente aos valores encontrados na literatura para esses tipos de rochas. Os resultados demonstraram que o método é eficaz na discriminação entre as rochas vulcânicas ácidas e básicas da Formação Serra Geral. Para a Fácies Caxias as concentrações médias foram de 3,7%, 5,5 ppm e 17,4 ppm, para K, eU e eTh, respectivamente. Já para a Fácies Gramado os valores médios de K foram de 2%, de eU foram de 2 ppm e de eTh de 9,2 ppm. O estudo também ratificou que as concentrações de K e eU são mais sensíveis ao grau de intemperismo das rochas do que as concentrações de eTh. Os dados estão organizados em um SIG e, na próxima etapa, o estudo buscará agregar dados de sensoriamento remoto hiperespectral para integrar com os dados gamaespectrométrico e geológicos
Constraining Warm Dark Matter candidates including sterile neutrinos and light gravitinos with WMAP and the Lyman-alpha forest
The matter power spectrum at comoving scales of (1-40) h^{-1} Mpc is very
sensitive to the presence of Warm Dark Matter (WDM) particles with large free
streaming lengths. We present constraints on the mass of WDM particles from a
combined analysis of the matter power spectrum inferred from the large samples
of high resolution high signal-to-noise Lyman-alpha forest data of Kim et al.
(2004) and Croft et al. (2002) and the cosmic microwave background data of
WMAP. We obtain a lower limit of m_wdm > 550 eV (2 sigma for early decoupled
thermal relics and m_wdm > 2.0 keV (2 sigma) for sterile neutrinos. We also
investigate the case where in addition to cold dark matter a light thermal
gravitino with fixed effective temperature contributes significantly to the
matter density. In that case the gravitino density is proportional to its mass,
and we find an upper limit m_{3/2} < 16 eV (2 sigma). This translates into a
bound on the scale of supersymmetry breaking, Lambda_{susy} < 260 TeV, for
models of supersymmetric gauge mediation in which the gravitino is the lightest
supersymmetric particle.Comment: 10 pages, 5 figures, 1 table. PRD in pres
Integração de dados em SIG - geológicos e sensoriamento remoto na caracterização da IG Farroupilha para vinhos de qualidade, RS, Brasil.
Este trabalho visou elaborar uma base geológica da IG Farroupilha, a fim de contribuir com a delimitação da mesma, integrando e processando os dados num sistema de informações geográficas
Neutrinos in Non-linear Structure Formation - a Simple SPH Approach
We present a novel method for implementing massive neutrinos in N-body
simulations. Instead of sampling the neutrino velocity distribution by
individual point particles we take neutrino free-streaming into account by
treating it as an effective redshift dependent sound speed in a perfect
isothermal fluid, and assume a relation between the sound speed and velocity
dispersion of the neutrinos. Although the method fails to accurately model the
true neutrino power spectrum, it is able to calculate the total matter power
spectrum to the same accuracy as more complex hybrid neutrino methods, except
on very small scales. We also present an easy way to update the publicly
available Gadget-2 version with this neutrino approximation.Comment: 13 pages, 7 figure
Neutrino Halos in Clusters of Galaxies and their Weak Lensing Signature
We study whether non-linear gravitational effects of relic neutrinos on the
development of clustering and large-scale structure may be observable by weak
gravitational lensing. We compute the density profile of relic massive
neutrinos in a spherical model of a cluster of galaxies, for several neutrino
mass schemes and cluster masses. Relic neutrinos add a small perturbation to
the mass profile, making it more extended in the outer parts. In principle,
this non-linear neutrino perturbation is detectable in an all-sky weak lensing
survey such as EUCLID by averaging the shear profile of a large fraction of the
visible massive clusters in the universe, or from its signature in the general
weak lensing power spectrum or its cross-spectrum with galaxies. However,
correctly modeling the distribution of mass in baryons and cold dark matter and
suppressing any systematic errors to the accuracy required for detecting this
neutrino perturbation is severely challenging.Comment: 13 pages, 11 figures. Submitted to JCA
Gamma-ray spectrometry for distinguishing acid and basic rocks of the serra geral formation, in the serra gaúcha wine region, Brazil.
The gamma-ray spectrometric research has allowed for observation of the distribution of radioactive elements such as K, U and Th for recognizing the radioactive signatures of different rock types. The objective of this study was to evaluate the possibility to distinguish between acid and basic rocks of the Serra Geral Formation, in the Serra Gaúcha wine region in the state of Rio Grande do Sul (Brazil) through gamma-ray spectrometry techniques. This study contributed to geologically... Keywords: geophysical method, wine terroir, volcanic rock. A pesquisa por gamaespectrometria tem permitido observar a distribuição de elementos radioativos, tais como K, U e Th reconhecendo as assinaturas radioativas de diferentes tipos de rocha. O objetivo deste estudo foi avaliar a possibilidade de distinguir entre as rochas ácidas e básicas da Formação Serra Geral, na região vitivinícola Serra Gaúcha, no estado do Rio Grande do Sul (Brasil) por meio de técnicas de gamaespectrometria Palavras-chave: m´étodos geofísicos, terroir vitivinícola, rocha vulcânica
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