430 research outputs found
The assembly of massive galaxies from NIR observations of the Hubble Deep Field South
We use a deep K(AB)<25 galaxy sample in the Hubble Deep Field South to trace
the evolution of the cosmological stellar mass density from z~ 0.5 to z~3. We
find clear evidence for a decrease of the average stellar mass density at high
redshift, 2<z<3.2, that is 15^{+25}_{-5}% of the local value, two times higher
than what observed in the Hubble Deep Field North. To take into account for the
selection effects, we define a homogeneous subsample of galaxies with
10^{10}M_\odot \leq M_* \leq 10^{11}M_\odot: in this sample, the mass density
at z>2 is 20^{+20}_{-5} % of the local value. In the mass--limited subsample at
z>2, the fraction of passively fading galaxies is at most 25%, although they
can contribute up to about 40% of the stellar mass density. On the other hand,
star--forming galaxies at z>2 form stars with an average specific rate at least
~4 x10^{-10} yr, 3 times higher than the z<~1 value. This
implies that UV bright star--forming galaxies are substancial contributors to
the rise of the stellar mass density with cosmic time. Although these results
are globally consistent with --CDM scenarios, the present rendition of
semi analytic models fails to match the stellar mass density produced by more
massive galaxies present at z>2.Comment: Accepted for publication on ApJLetter
Strongly star-forming rotating disks in a complex merging system at z = 4,7 as revealed by ALMA
We performed a kinematical analysis of the [CII] line emission of the BR
1202-0725 system at z~4,7 using ALMA observations. The most prominent sources
of this system are a quasar and a submillimeter galaxy, separated by a
projected distance of about 24 kpc and characterized by very high SFR, higher
than 1000 Msun/yr. However, the ALMA observations reveal that these galaxies
apparently have undisturbed rotating disks, which is at variance with the
commonly accepted scenario in which strong star formation activity is induced
by a major merger. We also detected faint components which, after spectral
deblending, were spatially resolved from the main QSO and SMG emissions. The
relative velocities and positions of these components are compatible with
orbital motions within the gravitational potentials generated by the QSO host
galaxy and the SMG, suggesting that they are smaller galaxies in interaction or
gas clouds in accretion flows of tidal streams. We did not find any clear
spectral evidence for outflows caused by AGN or stellar feedback. This suggests
that the high star formation rates might be induced by interactions or minor
mergers with these companions, which do not affect the large-scale kinematics
of the disks, however. Our kinematical analysis also indicates that the QSO and
the SMG have similar Mdyn, mostly in the form of molecular gas, and that the
QSO host galaxy and the SMG are seen close to face-on with slightly different
disk inclinations: the QSO host galaxy is seen almost face-on (i~15), while the
SMG is seen at higher inclinations (i~25). Finally, the ratio between the black
hole mass of the QSO, obtained from XShooter spectroscopy, and the Mdyn of the
host galaxy is similar to value found in very massive local galaxies,
suggesting that the evolution of black hole galaxy relations is probably better
studied with dynamical than with stellar host galaxy masses.Comment: Accepted for publication in Astronomy and Astrophysic
The evolution of the galaxy luminosity function in the rest frame blue band up to z=3.5
We present an estimate of the cosmological evolution of the field galaxy
luminosity function (LF) in the rest frame 4400 Angstrom B -band up to redshift
z=3.5. To this purpose, we use a composite sample of 1541 I--selected galaxies
selected down to I_(AB)=27.2 and 138 galaxies selected down to K_(AB)=25 from
ground-based and HST multicolor surveys, most notably the new deep JHK images
in the Hubble Deep Field South (HDF-S) taken with the ISAAC instrument at the
ESO-VLT telescope. About 21% of the sample has spectroscopic redshifts, and the
remaining fraction well calibrated photometric redshifts. The resulting blue LF
shows little density evolution at the faint end with respect to the local
values, while at the bright end (M_B(AB)<-20) a brightening increasing with
redshift is apparent with respect to the local LF. Hierarchical CDM models
overpredict the number of faint galaxies by about a factor 3 at z=1. At the
bright end the predicted LFs are in reasonable agreement only at low and
intermediate redshifts (z=1), but fail to reproduce the pronounced brightening
observed in the high redshift (z=2-3) LF. This brightening could mark the epoch
where a major star formation activity is present in the galaxy evolution.Comment: 14 pages, 2 figures, Astrophysical Journal Letters, in pres
New Orientia tsutsugamushi strain from scrub typhus in Australia.
In a recent case of scrub typhus in Australia, Orientia tsutsugamushi isolated from the patient's blood was tested by sequence analysis of the 16S rDNA gene. The sequence showed a strain of O. tsutsugamushi that was quite different from the classic Karp, Kato, and Gilliam strains. The new strain has been designated Litchfield
Cholecystojejunostomy varices demonstrated by enteroclysis
Varices in unusual sites constitute a minor but significant cause of gastrointestinal bleeding in patients with liver disease. We report a case of varices across the anastomotic line between the jejunum and gallbladder after cholecystojejunostomy. Although such varices have been demonstrated by angiography, to our knowledge they have never been demonstrated by small bowel enema (enteroclysis). We report a case and describe the findings on enteroclysis.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/42391/1/261-22-5-474_22n5p474.pd
A study of the nuclear medium influence on transverse momentum of hadrons produced in deep inelastic neutrino scattering
The influence of nuclear effects on the transverse momentum
distributions of neutrinoproduced hadrons is investigated using the data
obtained with SKAT propane-freon bubble chamber irradiated in the neutrino beam
(with = 3-30 GeV) at Serpukhov accelerator. Dependences of of hadrons (more pronounced for the
positively charged ones) produced in the target fragmentation region at low
invariant mass of the hadronic system (2 4 GeV) or at low energies
transferred to the current quark (2 GeV). At higher or ,
no influence of nuclear effects on is observed. Measurement results
are compared with predictions of a simple model, incorporating secondary
intranuclear interactions of hadrons (with a formation length extracted from
the Lund fragmentation model), which qualitatively reproduces the main features
of the data.Comment: 23 pages, 7 figure
BlueGroups: Middleware para Construção de Aplicações Distribuídas em Dispositivos Móveis
Equipados com diversos recursos e preços mais baixos, dispositivos móveis atingiram grande popularidade, aumentando a demanda por aplicações móveis. Entretanto, o desenvolvimento de tais aplicações com o suporte atual de linguagens de programação exige habilidades de programação avançadas. Ao lidar com dispositivos distribuídos e dados compartilhados em redes sem fio, um sólido conhecimento sobre problemas relacionados pode também ser requerido. Para facilitar o desenvolvimento, este trabalho introduz um middleware que implementa primitivas de comunicação em grupo sobre Bluetooth e permite gerenciamento de dados usando mecanismos de controle de versão
Isoscalar resonances with J^{PC}=1^{--} in e^+e^-annihilation
The analysis of the vector isoscalar excitations in the energy range between
1 and 2 GeV of the annihilation is presented for the final states
, , , and
. The effects of both the resonance mixing and the
successive opening of multiparticle channels, with the energy dependent partial
widths, are taken into account. The work extends our previous analysis
hep-ph/9609216 of the vector isovector excitations and is aimed to compare the
existing data with the predictions of the model. It is shown that
this hypothesis does not contradict the data.Comment: 16 pages, revtex, 6 ps figures. Clarifying remarks, a table, and
references are added. Accepted in Phys. Rev.
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