271 research outputs found
Dicrocoeliosis in Cats and Dogs
This paper is the first report of clinical cases of dicrocoeliosis in cats and dogs. In cats, symptoms manifested as inappetence, diarrhoea, loss of weight, changes of hair coat, and, in particular, conjunctivitis with mucoserous discharge and prolapse of the third eyelid. In dogs, clinical symptoms manifested with alteration of the digestive apparatus (anorexia, increased peristalsis, vomiting and diarrhoea), loss of weight, jaundice and skin lesions (pruritus, alopecia and dermatitis interdigitalis). The performance of all working dogs was reduced significantly. Both in dogs and cats, a reliable diagnosis is only possible through repeated coprological examination and demonstration of Dicrocoelium eggs. As far as the therapeutic procedures are concerned, albendazole administered for four days was only found fully effective in the cat as well as in the dog, in which praziquantel for 4-5 days was also sufficient
The dynamics of the ionized and molecular ISM in powerful obscured quasars at z>=3.5
We present an analysis of the kinematics and excitation of the warm ionized
gas in two obscured, powerful quasars at z>=3.5 from the SWIRE survey, SWIRE
J022513.90-043419.9 and SWIRE J022550.67-042142, based on imaging spectroscopy
on the VLT. Line ratios in both targets are consistent with luminous
narrow-line regions of AGN. SWIRE J022550.67-042142 has very broad (FWHM=2000
km/s), spatially compact [OIII] line emission. SWIRE J022513.90-043419.9 is
spatially resolved, has complex line profiles of H-beta and [OIII], including
broad wings with blueshifts of up to -1500 km/s relative to the narrow
[OIII]5007 component, and widths of up to FWHM=5000 km/s. Estimating the
systemic redshift from the narrow H-beta line, as is standard for AGN host
galaxies, implies that a significant fraction of the molecular gas is
blueshifted by up to ~ -1000 km/s relative to the systemic velocity. Thus the
molecular gas could be participating in the outflow. Significant fractions of
the ionized and molecular gas reach velocities greater than the escape
velocity. We compare empirical and modeling constraints for different energy
injection mechanisms, such as merging, star formation, and momentum-driven AGN
winds. We argue that the radio source is the most likely culprit, in spite of
the sources rather modest radio power of 10^25 W/Hz. Such a radio power is not
uncommon for intense starburst galaxies at z~2. We discuss these results in
light of the co-evolution of AGN and their host galaxy.Comment: Accepted by MNRA
Method and apparatus for selection of content from a stream of data
A main stream contains successive content elements of video and/or audio information that encode video and/or audio information at a first data rate. A computation circuit (144) computes main fingerprints from the successive content elements. A reference stream is received having a second data rate lower than the first data rate. The reference stream defines a sequence of the reference fingerprints. A comparator unit (144) compares the main fingerprints with the reference fingerprints. The main stream is monitored for the presence of inserted content elements between original content elements, where the original content elements have main fingerprints that match successive reference fingerprints and the inserted content elements have main fingerprints that do not match reference fingerprints. Rendering of inserted content elements to be skipped. In an embodiment when more than one content element matches only one is rendered. In another embodiment matching is used to control zapping to or from the main stream. In another embodiment matching is used to control linking of separately received mark-up information such as subtitles to points in the main strea
Defying jet-gas alignment in two radio galaxies at z~2 with extended light profiles: Similarities to brightest cluster galaxies
We report the detection of extended warm ionized gas in two powerful
high-redshift radio galaxies, NVSS J210626-314003 at z=2.10 and TXS 2353-003 at
z=1.49, that does not appear to be associated with the radio jets. This is
contrary to what would be expected from the alignment effect, a characteristic
feature of distant, powerful radio galaxies at z> 0.6. The gas also has smaller
velocity gradients and line widths than most other high-z radio galaxies with
similar data. Both galaxies are part of a systematic study of 50 high-redshift
radio galaxies with SINFONI, and are the only two that are characterized by the
presence of high surface-brightness gas not associated with the jet axis and by
the absence of such gas aligned with the jet. Both galaxies are spatially
resolved with ISAAC broadband imaging covering the rest-frame R band, and have
extended wings that cannot be attributed to line contamination. We argue that
the gas and stellar properties of these galaxies are more akin to gas-rich
brightest cluster galaxies in cool-core clusters than the general population of
high-redshift radio galaxies at z>2. In support of this interpretation, one of
our sources, TXS 2353-003, for which we have H\alpha\ narrowband imaging, is
associated with an overdensity of candidate H\alpha\ emitters by a factor of 8
relative to the field at z=1.5. We discuss possible scenarios of the
evolutionary state of these galaxies and the nature of their emission line gas
within the context of cyclical AGN feedback.Comment: A&A in pres
A SINFONI view of flies in the Spiderweb: a galaxy cluster in the making
The environment of the high-z radio galaxy PKS 1138-262 at z~2.2 is a prime
example of a forming galaxy cluster. We use deep SINFONI data to perform a
detailed study of the kinematics of the galaxies within 60 kpc of the radio
core and we link this to the kinematics of the protocluster on the megaparsec
scale. Identification of optical emission lines shows that 11 galaxies are at
the redshift of the protocluster. The density of line emitters is more than an
order of magnitude higher in the core of the protocluster than the larger scale
environment. This implies a matter overdensity in the core of delta_m~70 which
is similar to the outskirts of local galaxy clusters. The velocity distribution
of the confirmed satellite galaxies shows a broad, double-peaked velocity
structure with sigma=1360+/-206 km/s. A similar broad, double-peaked
distribution was found in a previous study targeting the large scale
protocluster structure, indicating that a common process is acting on both
small and large scales. Including all spectroscopically confirmed protocluster
galaxies, a velocity dispersion of 1013+/-87 km/s is found. We show that the
protocluster has likely decoupled from the Hubble flow and is a dynamically
evolved structure. Comparison to the Millenium simulation indicates that the
protocluster velocity distribution is consistent with that of the most massive
haloes at z~2, but we rule out that the protocluster is a fully virialized
structure based on dynamical arguments and its X-ray luminosity. Comparison to
merging haloes in the Millennium simulation shows that the structure as
observed in and around the Spiderweb galaxy is best interpreted as being the
result of a merger between two massive haloes. We propose that this merger can
result in an increase in star formation and AGN activity in the protocluster
core and is possibly an important stage in the evolution of massive cD
galaxies.Comment: 12 pages, 7 figures. Accepted for publication in MNRA
Gas kinematics in powerful radio galaxies at z ∼2: Energy supply from star formation, AGN, and radio jets⋆
We compare the kinetic energy and momentum injection rates from intense star
formation, bolometric AGN radiation, and radio jets with the kinetic energy and
momentum observed in the warm ionized gas in 24 powerful radio galaxies at z~2.
These galaxies are amongst our best candidates for being massive galaxies near
the end of their active formation period, when intense star formation, quasar
activity, and powerful radio jets all co-exist. All galaxies have VLT/SINFONI
imaging spectroscopy of the rest-frame optical line emission, showing
emission-line regions with large velocity offsets (up to 1500 km/s) and line
widths (typically 800-1000 km/s) consistent with very turbulent, often
outflowing gas. As part of the HeRGE sample, they also have FIR estimates of
the star formation and quasar activity obtained with Herschel/PACS and SPIRE,
which enables us to measure the relative energy and momentum release from each
of the three main sources of feedback in massive, star-forming AGN host
galaxies during their most rapid formation phase. We find that star formation
falls short by factors 10-1000 of providing the energy and momentum necessary
to power the observed gas kinematics. The obscured quasars in the nuclei of
these galaxies provide enough energy and momentum in about half of the sample,
however, only if these are transfered to the gas relatively efficiently. We
compare with theoretical and observational constraints on the efficiency of the
energy and momentum transfer from jet and AGN radiation, which advocates that
the radio jet is the main driver of the gas kinematics.Comment: A&A accepted. Comments welcom
Intense Star-formation and Feedback at High Redshift: Spatially-resolved Properties of the z=2.6 Submillimeter Galaxy SMMJ14011+0252
We present a detailed analysis of the spatially-resolved properties of the
lensed submillimeter galaxy SMMJ14011+0252 at z=2.56, combining deep
near-infrared integral-field data obtained with SPIFFI on the VLT with other
multi-wavelength data sets. The broad characteristics of SMMJ14011+0252 are in
agreement with what is expected for the early evolution of local massive
spheroidal galaxies. From continuum and line flux, velocity, and dispersion
maps, we measure the kinematics, star-formation rates, gas densities, and
extinction for individual subcomponents. The star formation intensity is
similar to low-redshift ``maximal starbursts'', while the line fluxes and the
dynamics of the emission line gas provide direct evidence for a
starburst-driven wind with physical properties very similar to local
superwinds. We also find circumstantial evidence for "self-regulated" star
formation within J1. The relative velocity of the bluer companion J2 yields a
dynamical mass estimate for J1 within about 20 kpc, M_dyn \sim 1\times 10^{11}
M_sun. The relative metallicity of J2 is 0.4 dex lower than in J1n/s,
suggesting different star formation histories. SED fitting of the continuum
peak J1c confirms and substantiates previous suggestions that this component is
a z=0.25 interloper. When removing J1c, the stellar continuum and H-alpha line
emission appear well aligned spatially in two individual components J1n and
J1s, and coincide with two kinematically distinct regions in the velocity map,
which might well indicate a merging system. This highlights the close
similarity between SMGs and ULIRGs, which are often merger-driven maximal
starbursts, and suggests that the intrinsic mechanisms of star-formation and
related feedback are similar to low-redshift strongly star-forming systems.Comment: Some of the figures changed from b/w to colo
Disk, merger, or outflow ? Molecular gas kinematics in two powerful obscured QSOs at z>3.4
We report on the detection of bright CO(4-3) line emission in two powerful,
obscured quasars discovered in the SWIRE survey, SW022513 and SW022550 at
z>3.4. We analyze the line strength and profile to determine the gas mass,
dynamical mass and the gas dynamics for both galaxies. In SW022513 we may have
found the first evidence for a molecular, AGN-driven wind in the early
Universe. The line profile in SW022513 is broad (FWHM = 1000 km/s) and
blueshifted by -200 km/s relative to systemic (where the systemic velocity is
estimated from the narrow components of ionized gas lines, as is commonly done
for AGN at low and high redshifts). SW022550 has a more regular, double-peaked
profile, which is marginally spatially resolved in our data, consistent with
either a merger or an extended disk. The molecular gas masses, 4x10^10 Msun,
are large and account for <30% of the stellar mass, making these obscured QSOs
as gas rich as other powerful CO emitting galaxies at high redshift, i.e.,
submillimeter galaxies. Our sources exhibit relatively lower star-formation
efficiencies compared to other dusty, powerful starburst galaxies at high
redshift. We speculate that this could be a consequence of the AGN perturbing
the molecular gas.Comment: Accepted for publication in A&
Populations of OB-type stars in galaxies
One of the challenges for stellar astrophysics is to reach the point at which
we can undertake reliable spectral synthesis of unresolved populations in
young, star-forming galaxies at high redshift. Here I summarise recent studies
of massive stars in the Galaxy and Magellanic Clouds, which span a range of
metallicities commensurate with those in high-redshift systems, thus providing
an excellent laboratory in which to study the role of environment on stellar
evolution. I also give an overview of observations of luminous supergiants in
external galaxies out to a remarkable 6.7 Mpc, in which we can exploit our
understanding of stellar evolution to study the chemistry and dynamics of the
host systems.Comment: 9 pages, 3 figures, invited review at IAU Symposium 272 (eds Neiner,
Wade, Meynet & Peters
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