709 research outputs found
Ocular Refraction at Birth and Its Development During the First Year of Life in a Large Cohort of Babies in a Single Center in Northern Italy
The purpose of this study was to investigate refraction at birth and during the first year of life in a large cohort of babies born in a single center in Northern Italy. We also aimed to analyze refractive errors in relation to the gestational age at birth. An observational ophthalmological assessment was performed within 24 h of birth on 12,427 newborns. Refraction was examined using streak retinoscopy after the administration of tropicamide (1%). Values in the range of between +0.50 †D †+4.00 were defined as physiological refraction at birth. Newborns with refraction values outside of the physiological range were followed up during the first year of life. Comparative analyses were conducted in a subgroup of babies with known gestational ages. The following distribution of refraction at birth was recorded: 88.03% of the babies had physiological refraction, 5.03% had moderate hyperopia, 2.14% had severe hyperopia, 3.4%, had emmetropia, 0.45%, had myopia, 0.94% had astigmatism, and 0.01% had anisometropia. By the end of the first year of life, we observed reductions in hyperopia and astigmatism, and stabilization of myopia. Preterm babies had a four-fold higher risk of congenital myopia and a three-fold higher risk of congenital emmetropia as compared to term babies. Refraction profiles obtained at birth changed during the first year of life, leading to a normalization of the refraction values. Gestational age at birth affected the incidence of refractive errors and amblyopia
A survey of HC_3N in extragalactic sources: Is HC_3N a tracer of activity in ULIRGs?
Context. HC_3N is a molecule that is mainly associated with Galactic star-forming regions, but it has also been detected in extragalactic environments.
Aims. To present the first extragalactic survey of HC_3N, when combining earlier data from the literature with six new single-dish detections, and to compare HC_3N with other molecular tracers (HCN, HNC), as well as other properties (silicate absorption strength, IR flux density ratios, C_(II) flux, and megamaser activity).
Methods. We present mm IRAM 30 m, OSO 20 m, and SEST observations of HC_3N rotational lines (mainly the J = 10â9 transition) and of the J = 1â0 transitions of HCN and HNC. Our combined HC_3N data account for 13 galaxies (excluding the upper limits reported for the non-detections), while we have HCN and HNC data for more than 20 galaxies.
Results. A preliminary definition âHC_3N-luminous galaxyâ is made based upon the HC_3N/HCN ratio. Most (~80%) HC_3N-luminous galaxies seem to be deeply obscured galaxies and (U)LIRGs. A majority (~60% or more) of the HC3N-luminous galaxies in the sample present OH mega- or strong kilomaser activity. A possible explanation is that both HC_3N and OH megamasers need warm dust for their excitation. Alternatively, the dust that excites the OH megamaser offers protection against UV destruction of HC_3N. A high silicate absorption strength is also found in several of the HC_3N-luminous objects, which may help the HC3N to survive. Finally, we find that a high HC_3N/HCN ratio is related to a high dust temperature and a low C_(II) flux
Evidence for a chemically differentiated outflow in Mrk 231
Aims: Our goal is to study the chemical composition of the outflows of active
galactic nuclei and starburst galaxies.
Methods: We obtained high-resolution interferometric observations of HCN and
HCO and of the ultraluminous infrared
galaxy Mrk~231 with the IRAM Plateau de Bure Interferometer. We also use
previously published observations of HCN and HCO and
, and HNC in the same source.
Results: In the line wings of the HCN, HCO, and HNC emission, we find
that these three molecular species exhibit features at distinct velocities
which differ between the species. The features are not consistent with emission
lines of other molecular species. Through radiative transfer modelling of the
HCN and HCO outflow emission we find an average abundance ratio
. Assuming a clumpy outflow,
modelling of the HCN and HCO emission produces strongly inconsistent
outflow masses.
Conclusions: Both the anti-correlated outflow features of HCN and HCO and
the different outflow masses calculated from the radiative transfer models of
the HCN and HCO emission suggest that the outflow is chemically
differentiated. The separation between HCN and HCO could be an indicator of
shock fronts present in the outflow, since the HCN/HCO ratio is expected to
be elevated in shocked regions. Our result shows that studies of the chemistry
in large-scale galactic outflows can be used to better understand the physical
properties of these outflows and their effects on the interstellar medium (ISM)
in the galaxy.Comment: 12 pages, 8 figures, accepted for publication in A&
Molecular gas in the northern nucleus of Mrk273: Physical and chemical properties of the disk and its outflow
Aiming to characterise the properties of the molecular gas in the
ultraluminous infrared galaxy Mrk273 and its outflow, we used the NOEMA
interferometer to image the dense gas molecular tracers HCN, HCO+, HNC, HOC+
and HC3N at 86GHz and 256GHz with angular resolutions of 4.9x4.5 arcsec
(3.7x3.4 kpc) and 0.61x0.55 arcsec (460x420 pc). We also modelled the flux of
several H2O lines observed with Herschel using a radiative transfer code that
includes excitation by collisions as well as by far-infrared photons. The disk
of the Mrk273 north nucleus has two components with decoupled kinematics. The
gas in the outer parts (1.5 kpc) rotates with a south-east to north-west
direction, while in the inner disk (300 pc) follows a north-east to south-west
rotation. The central 300 pc, which hosts a compact starburst region, is filled
with dense and warm gas, contains a dynamical mass of (4-5)x10^9M_sun, a
luminosity of L'_HCN=(3-4)x10^8 K km/s pc^2, and a dust temperature of 55 K. At
the very centre, a compact core with R~50 pc has a luminosity of
L_IR=4x10^11L_sun (30% of the total infrared luminosity), and a dust
temperature of 95 K. The core is expanding at low velocities ~50-100 km/s,
probably affected by the outflowing gas. We detect the blue-shifted component
of the outflow, while the red-shifted counterpart remains undetected in our
data. Its cold and dense phase reaches fast velocities up to ~1000 km/s, while
the warm outflowing gas has more moderate maximum velocities of ~600 km/s. The
outflow is detected as far as 460 pc from the centre in the northern direction,
and has a mass of dense gas <8x10^8M_sun. The difference between the position
angles of the inner disk (~70 degree) and the outflow (~10 degree) indicates
that the outflow is likely powered by the AGN, and not by the starburst.
Regarding the chemistry, we measure an extremely low HCO+/HOC+ ratio of 10+-5
in the inner disk of Mrk273.Comment: Accepted for publication in A&A. 21 pages, 17 figures, 7 tables, and
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Localization of orexin B and receptor 2 for orexins in testicular cytotypes of the camelid alpaca (Vicugna pacos).
The orexins A (OxA) and B (OxB) are two hypothalamic peptides involved in many physiological functions of the mammalian body. They act through the binding of two G-coupled receptors named receptor 1 (OX1 ) and receptor 2 (OX2 ) for orexins. The first receptor is specific for OxA, while the second binds both the substances with equal affinity. The orexins and the relative receptors have been traced by means of different techniques also at the periphery of the body and particularly in the adrenals, and in gastrointestinal and genital organs. Aim of this work was to investigate the presence of OxB and OX2 by means of immunohistochemistry and Western blotting analysis in the testis of the South American camelid alpaca, a species primarily breed in Chile and Ecuador and recently diffused in Europe where the quality of its wool is particularly appreciated. OxB immunoreactivity (IR) was found in the tubular compartment of the testis where spermatogonia (resting), zygotene and pachytene spermatocytes, and spermatids clearly showed differently sized and shaped cytoplasmic positive structures. OX2 -IR was found both in the interstitial and tubular compartments of the testis and particularly in Leydig cells and round and elongated spermatids. Western blotting analysis of testis lysates showed the presence of a protein band whose molecular weight corresponded to that currently assigned to OX2 . Such findings easily translate the hypothesis that OxB and its receptor 2 play a functional role both in the interstitial and tubular compartments of the alpaca testis
The Dense Molecular Gas and Nuclear Activity in the ULIRG IRAS 13120-5453
We present new ALMA Band 7 ( GHz) observations of the dense gas
tracers HCN, HCO, and CS in the local, single-nucleus, ultraluminous
infrared galaxy IRAS 13120-5453. We find centrally enhanced HCN (4-3) emission,
relative to HCO (4-3), but do not find evidence for radiative pumping of
HCN. Considering the size of the starburst (0.5 kpc) and the estimated
supernovae rate of yr, the high HCN/HCO ratio can be
explained by an enhanced HCN abundance as a result of mechanical heating by the
supernovae, though the active galactic nucleus and winds may also contribute
additional mechanical heating. The starburst size implies a high
of kpc, slightly below predictions of
radiation-pressure limited starbursts. The HCN line profile has low-level
wings, which we tentatively interpret as evidence for outflowing dense
molecular gas. However, the dense molecular outflow seen in the HCN line wings
is unlikely to escape the galaxy and is destined to return to the nucleus and
fuel future star formation. We also present modeling of Herschel observations
of the HO lines and find a nuclear dust temperature of K. IRAS
13120-5453 has a lower dust temperature and than is inferred for
the systems termed "compact obscured nuclei" (such as Arp 220 and Mrk 231). If
IRAS 13120-5453 has undergone a compact obscured nucleus phase, we are likely
witnessing it at a time when the feedback has already inflated the nuclear ISM
and diluted star formation in the starburst/AGN core.Comment: accepted for publication in ApJ, 21 pages, 11 figure
Central serous chorioretinopathy: Pathogenesis and management
Central serous chorioretinopathy (CSC) is a common retina disease and has a relative high recurrence rate, etiology, and pathogenesis of which remains largely ambiguous. The effects on the retina are usually self-limited, although some people are left with permanent vision loss due to progressive and irreversible photoreceptor damage or retinal pigment epithelium atrophy. There have been a number of interventions used in CSC, including, but not limited to, laser treatment, photodynamic therapy (PDT), intravitreal injection of anti-vascular endothelial growth factor agents, and subthreshold lasers. It is not clear whether there is a clinically important benefit to treating acute CSC, which often resolves spontaneously as part of its natural history. Of the interventions studied to date, PDT and micropulse laser treatment appear the most promising
The influence of cosmic rays in the circumnuclear molecular gas of NGC1068
We surveyed the circumnuclear disk of the Seyfert galaxy NGC1068 between the
frequencies 86.2 GHz and 115.6 GHz, and identified 17 different molecules.
Using a time and depth dependent chemical model we reproduced the observational
results, and show that the column densities of most of the species are better
reproduced if the molecular gas is heavily pervaded by a high cosmic ray
ionization rate of about 1000 times that of the Milky Way. We discuss how
molecules in the NGC1068 nucleus may be influenced by this external radiation,
as well as by UV radiation fields.Comment: 6 pages. Conference proceeding for the workshop on "Cosmic-ray
induced phenomenology in star-forming environments" held in Sant Cugat,
Spain, on April 16-19, 201
Luminous, pc-scale CO 6-5 emission in the obscured nucleus of NGC1377
High resolution submm observations are important in probing the morphology,
column density and dynamics of obscured active galactic nuclei (AGNs). With
high resolution (0.06 x 0.05) ALMA 690 GHz observations we have found bright
(TB >80 K) and compact (FWHM 10x7 pc) CO 6-5 line emission in the nucleus of
the extremely radio-quiet galaxy NGC1377. The integrated CO 6-5 intensity is
aligned with the previously discovered jet/outflow of NGC1377 and is tracing
the dense (n>1e4 cm-3), hot gas at the base of the outflow. The velocity
structure is complex and shifts across the jet/outflow are discussed in terms
of jet-rotation or separate, overlapping kinematical components. High velocity
gas (deltaV +-145 km/s) is detected inside r<2-3 pc and we suggest that it is
emerging from an inclined rotating disk or torus of position angle PA=140+-20
deg with a dynamical mass of approx 3e6 Msun. This mass is consistent with that
of a supermassive black hole (SMBH), as inferred from the M-sigma relation. The
gas mass of the proposed disk/torus constitutes <3% of the nuclear dynamical
mass. In contrast to the intense CO 6-5 line emission, we do not detect dust
continuum with an upper limit of S(690GHz)<2mJy. The corresponding, 5 pc, H2
column density is estimated to N(H2)<3e23 cm-2, which is inconsistent with a
Compton Thick (CT) source. We discuss the possibility that CT obscuration may
be occuring on small (subparsec) or larger scales. From SED fitting we suggest
that half of the IR emission of NGC1377 is nuclear and the rest (mostly the
far-infrared (FIR)) is more extended. The extreme radio quietness, and the lack
of emission from other star formation tracers, raise questions on the origin of
the FIR emission. We discuss the possibility that it is arising from the
dissipation of shocks in the molecular jet/outflow or from irradiation by the
nuclear source along the poles.Comment: 7 pages, 5 figures, submitted to Astronomy and Astrophysic
Outcomes in antiretroviral-naive HIV-infected patients initiating therapy with TDF/FTC plus either atazanavir/r or another third recommended drug
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