61 research outputs found
A Search for Stars of Very Low Metal Abundance. V. Photoelectric UBV Photometry of Metal-Weak Candidates from the Northern HK Survey
We report photoelectric UBV data for 268 metal-poor candidates chosen from
the northern HK objective-prism/interference-filter survey of Beers and
colleagues. Over 40 % of the stars have been observed on more than one night,
and most have at least several sets of photometric measurements. Reddening
estimates, preliminary spectroscopic measurements of abundance, and type
classifications are reported.Comment: To Appear in the Astronomical Journal, October 200
UVES radial velocity accuracy from asteroid observations. Implications for the fine structure constant variability
High resolution observations of the asteroids Iris and Juno have been
performed by means of the UVES spectrograph at the ESO VLT to obtain the
effective accurac y of the spectrograph's radial velocity. The knowledge of
this quantity has impo rtant bearings on studies searching for a variability of
the fine structure cons tant carried on with this instrument. Asteroids provide
a precise radial velocit y reference at the level of 1 m/s which allows
instrumental calibration and the recognition of small instrumental drifts and
calibration systematics. In particu lar, radial velocity drifts due to non
uniform slit illumination and slit optica l misalignment in the two UVES
spectrograph arms can be investigated. The positi on of the solar spectrum
reflected by the asteroids are compared with the solar wavelength positions or
with that of asteroid observations at other epochs or wi th the twilight to
asses UVES instrumental accuracy . Radial velocities offsets in the range
10--50 m/s are generally observed likely due to a non uniform slit
illumination. However, no radial velocity patterns with wavelength are detected
and the two UVES arms provide consistent radial velocities. These results
suggest that the detected alpha variability by Levshakov et al. (2007) deduced
from a drift of -180 (+/- 85) m/s at z =1.84, between two sets of FeII lines
falling in the two UVES arms may be real or induced by other kinds of
systematics than those investigated here. The proposed technique allows real
time quality check of the spectrograph and should be followed for very accurate
measurements.Comment: Accepted A&
Multi-sensor analysis of extreme events in North-Eastern Italy
International audienceThe North-eastern part of Italy is known to be one of the most rainy regions in Europe. In this paper three extreme events are analysed, using a multi-sensor observing system including a weather radar and a dense telemetric network of surface stations, recording precipitation, wind, temperature and relative humidity. The cases examined comprise two long lasting rainfall events impacting two distinct areas, and a vigorous hail-producing thunderstorm event over the plains. In all cases, inter-comparison between remotely sensed and surface observations, including estimates and measures of precipitation and wind, helps to better understand the behaviour of the atmosphere, thus supporting operational fore- and now-casting. In the case of widespread precipitation, a relation is suggested between the wind speed and direction at medium/low levels with the location of the maximum precipitation relative to the mountains. This reflects the dynamical interaction between the mountain barrier and the atmospheric flux impinging upon it. This flux can be estimated by the automatic weather station of Mt. Cesen, a focal point for a now-casting of the rain in the Veneto Region. Analysis of strong thunderstorm activity makes extensive use of radar data. In the examined case the interaction of a sea breeze-like circulation with a mesoscale trough gave rise to a distinct convergence line that triggered a severe and long-lived hail-producing multi-cell thunderstorm. The hail was successfully detected by the radar's hail detection algorithm
A Frequency Comb calibrated Solar Atlas
The solar spectrum is a primary reference for the study of physical processes
in stars and their variation during activity cycles. In Nov 2010 an experiment
with a prototype of a Laser Frequency Comb (LFC) calibration system was
performed with the HARPS spectrograph of the 3.6m ESO telescope at La Silla
during which high signal-to-noise spectra of the Moon were obtained. We exploit
those Echelle spectra to study the optical integrated solar spectrum . The
DAOSPEC program is used to measure solar line positions through gaussian
fitting in an automatic way. We first apply the LFC solar spectrum to
characterize the CCDs of the HARPS spectrograph. The comparison of the LFC and
Th-Ar calibrated spectra reveals S-type distortions on each order along the
whole spectral range with an amplitude of +/-40 m/s. This confirms the pattern
found by Wilken et al. (2010) on a single order and extends the detection of
the distortions to the whole analyzed region revealing that the precise shape
varies with wavelength. A new data reduction is implemented to deal with CCD
pixel inequalities to obtain a wavelength corrected solar spectrum. By using
this spectrum we provide a new LFC calibrated solar atlas with 400 line
positions in the range of 476-530, and 175 lines in the 534-585 nm range. The
new LFC atlas improves the accuracy of individual lines by a significant factor
reaching a mean value of about 10 m/s. The LFC--based solar line wavelengths
are essentially free of major instrumental effects and provide a reference for
absolute solar line positions. We suggest that future LFC observations could be
used to trace small radial velocity changes of the whole solar photospheric
spectrum in connection with the solar cycle and for direct comparison with the
predicted line positions of 3D radiative hydrodynamical models of the solar
photosphere.Comment: Accept on the 15th of October 2013. 9 pages, 10 figures. ON-lINE data
A&A 201
Climate and atmospheric models of rocky planets: habitability and observational properties
The quest for atmospheric spectral signatures that may witness biological
activity in exoplanets is focused on rocky planets. The best targets for
future, challenging spectroscopic observations will be selected among
potentially habitable planets. Surface habitability can be quantified and
explored with climate and atmospheric models according to temperature-based
criteria. The conceptual, modellistic, technological and interpretative
complexity of the problem requires to develop flexible climate and atmospheric
models suited for a comprehensive exploration of observationally unconstrained
parameters, and to simulate and interpret definitely non-terrestrial
conditions. We present a summary and preliminary results on the work we are
performing on multi-parametric explorations of the habitability and
observational properties of rocky planets.Comment: to appear on MemSAIt, vol 94. Proceedings of the Hack100 Conference:
Past, Present and Future of Astrophysical Spectroscopy, 6-10 June 2022,
Trieste, Ital
A search for Interstellar absorptions towards Sgr dSph
We searched for Na I D1,D2 interstellar absorption lines towards 12 giant
stars of the Sgr dwarf spheroidal and 3 stars of the associated globular
cluster Terzan 7, observed at high resolution with the UVES spectrograph at the
8.2 m Kueyen VLT telescope. These stars are not an ideal background source for
the analysis of interstellar (IS) absorption lines since they have been
observed in the framework of a stellar abundances study. However they are
sufficiently luminous to allow a decent S/N ratio at a resolution of about
43000, i.e. ~7 km/s, which allows an exploratory study. We detected two
distinct groups of IS absorptions, a ``local'' group, with radial velocities
ranging from -43 km/s to 50 km/s, and a high velocity group with radial
velocities ranging from 150 km/s to 165 km/s. Likely the high velocity
components are due to gas falling on the Sgr dSph since have been observed only
in 2 stars which are separated by only 1.5' in the sky. We argue that the
observations suggest a stripping of gas due to the passage of Sgr through the
Galactic disc.Comment: accepted by Astronomy & Astrophysic
A wide angle view of the Sagittarius dwarf Spheroidal Galaxy. I: VIMOS photometry and radial velocities across Sgr dSph major and minor axis
The Sagittarius dwarf Spheroidal Galaxy (Sgr dSph) provides us with a unique
possibility of studying a dwarf galaxy merging event while still in progress.
Due to its low distance (25 kpc), the main body of Sgr dSph covers a vast area
in the sky (roughly 15 x 7 degrees). Available photometric and spectroscopic
studies have concentrated either on the central part of the galaxy or on the
stellar stream, but the overwhelming majority of the galaxy body has never been
probed. The aim of the present study is twofold. On the one hand, to produce
color magnitude diagrams across the extension of Sgr dSph to study its stellar
populations, searching for age and/or composition gradients (or lack thereof).
On the other hand, to derive spectroscopic low-resolution radial velocities for
a subsample of stars to determine membership to Sgr dSph for the purpose of
high resolution spectroscopic follow-up. We used VIMOS-VLT to produce V and I
photometry and spectroscopy on 7 fields across the Sgr dSph minor and major
axis, plus 3 more centered on the associated globular clusters Terzan 7, Terzan
8 and Arp 2. A last field has been centered on M 54, lying in the center of Sgr
dSph. We present photometry for 320,000 stars across the main body of Sgr dSph,
one of the richest, and safely the most wide-angle sampling ever produced for
this fundamental object. We also provide robust memberships for more than one
hundred stars, whose high resolution spectroscopic analysis will be the object
of forthcoming papers. Sgr dSph appears remarkably uniform among the observed
fields. We confirm the presence of a main Sgr dSph population characterized
roughly by the same metallicity of 47 Tuc, but we also found the presence of
multiple populations on the peripheral fields of the galaxy, with a metallicity
spanning from [Fe/H]=-2.3 to a nearly solar value.Comment: 10 pages, 12 figures, accepted for publication in A&
Neuronal networks provide rapid neuroprotection against spreading toxicity
Acute secondary neuronal cell death, as seen in neurodegenerative disease, cerebral ischemia (stroke) and traumatic brain injury (TBI), drives spreading neurotoxicity into surrounding, undamaged, brain areas. This spreading toxicity occurs via two mechanisms, synaptic toxicity through hyperactivity, and excitotoxicity following the accumulation of extracellular glutamate. To date, there are no fast-acting therapeutic tools capable of terminating secondary spreading toxicity within a time frame relevant to the emergency treatment of stroke or TBI patients. Here, using hippocampal neurons (DIV 15-20) cultured in microfluidic devices in order to deliver a localized excitotoxic insult, we replicate secondary spreading toxicity and demonstrate that this process is driven by GluN2B receptors. In addition to the modeling of spreading toxicity, this approach has uncovered a previously unknown, fast acting, GluN2A-dependent neuroprotective signaling mechanism. This mechanism utilizes the innate capacity of surrounding neuronal networks to provide protection against both forms of spreading neuronal toxicity, synaptic hyperactivity and direct glutamate excitotoxicity. Importantly, network neuroprotection against spreading toxicity can be effectively stimulated after an excitotoxic insult has been delivered, and may identify a new therapeutic window to limit brain damage
Solar atlas revised
Context. Present knowledge of the solar spectrum is limited because it is very difficult to observe the integrated solar spectrum at high resolution. The reflected solar light from asteroids has been shown to provide a relatively straightforward integrated and unmodified solar spectrum.
Aims. We exploit this methodology to improve our knowledge of solar photospheric line positions both in terms of line number and precision with respect to the available solar line atlas.
Methods. We used the DAOSPEC program to measure solar line positions automatically in high signal-to-noise spectra of Ceres obtained with HARPS at the 3.6Â m ESOÂ telescope. The line positions were then verified with the solar HARPSÂ spectra of Ganymede and daylight as well as with a new FTSÂ solar spectra.
Results. A new atlas with 2334 lines in the range 4000â6859Â Ă
is provided. The new atlas is consistent with that based on FTS solar spectra but the new line list improves the precision of individual lines by at least a factor 3 â 5.
Conclusions. The new atlas provides a benchmark for 3DÂ models of the solar photosphere and can be used to trace possible line drifts related to solar activity or to calibrate space and ground spectrographs
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