396 research outputs found
Refrigeration System for the ATLAS Experiment
The proposed ATLAS detector for the 27 km circumference LHC collider is of unprecedented size and complexity. The magnet configuration is based on an inner superconducting solenoid and large superconducting air-core toroids (barrel and two end-caps) each made of eight coils symmetrically arranged outside the calorimetry. The total cold mass approaches 600 tons and the stored energy is 1.7Â GJ. The cryogenic infrastructure will include a 6Â kW @ 4.5Â K refrigerator, a precooling unit and distribution systems and permits flexible operation during cool-down, normal running and quench recovery. A dedicated LN2 refrigeration system is proposed for the three liquid argon calorimeters (84 m3 of LAr). Magnets and calorimeters will be individually tested prior to their definitive installation in a large scale cryogenic test area on the surface. The experiment is scheduled to be operational in 2005
Classification and Management of Pontecerebellar-Petrosal Bridging Veins
The risks and benefits of coagulating intradural venous elements during a retrosigmoid approach for trigeminal neurovascular decompression has not been accurately established. The objectives of this study were to identify the veins that drain into the superior petrosal sinus, classify them in relation to the suprameatal tubercle, and determine the implication of their coagulation
Gaia Focused Product Release: Spatial distribution of two diffuse interstellar bands
Diffuse interstellar bands (DIBs) are absorption features seen in optical and
infrared spectra of stars that are probably caused by large and complex
molecules in the ISM. Here we investigate the Galactic distribution and
properties of two DIBs identified in almost six million stellar spectra
collected by the Gaia Radial Velocity Spectrometer. These measurements
constitute a part of the Gaia Focused Product Release to be made public between
the Gaia DR3 and DR4 data releases. In order to isolate the DIB signal from the
stellar features in each individual spectrum, we identified a set of 160 000
spectra at high Galactic latitudes which we consider to be the DIB-free
reference sample. Matching each target spectrum to its closest reference
spectra in stellar parameter space allowed us to remove the stellar spectrum
empirically, without reference to stellar models, leaving a set of six million
ISM spectra. Identifying the two DIBs at 862.1 nm and 864.8 nm in the stacked
spectra, we modelled their shapes and report the depth, central wavelength,
width, and equivalent width (EW) for each, along with confidence bounds on
these measurements. Our main results are as follows: (1) the strength and
spatial distribution of the DIB 862.1 are very consistent with what
was found in Gaia DR3, but for this work we attained a higher signal-to-noise
ratio in the stacked spectra to larger distances, which allowed us to trace
DIBs in the outer spiral arm and beyond the Scutum--Centaurus spiral arm; (2)
we produced an all-sky map below of Galactic latitude to
4000 pc of both DIB features and their correlations; (3) we detected the
signals of DIB\,862.1 inside the Local Bubble; and (4) there is a
reasonable correlation with the dust reddening found from stellar absorption
and EWs of both DIBs.Comment: 29 pages, accepted for publication in A&
<i>Gaia</i> Data Release 1. Summary of the astrometric, photometric, and survey properties
Context. At about 1000 days after the launch of Gaia we present the first Gaia data release, Gaia DR1, consisting of astrometry and photometry for over 1 billion sources brighter than magnitude 20.7.
Aims. A summary of Gaia DR1 is presented along with illustrations of the scientific quality of the data, followed by a discussion of the limitations due to the preliminary nature of this release.
Methods. The raw data collected by Gaia during the first 14 months of the mission have been processed by the Gaia Data Processing and Analysis Consortium (DPAC) and turned into an astrometric and photometric catalogue.
Results. Gaia DR1 consists of three components: a primary astrometric data set which contains the positions, parallaxes, and mean proper motions for about 2 million of the brightest stars in common with the HIPPARCOS and Tycho-2 catalogues â a realisation of the Tycho-Gaia Astrometric Solution (TGAS) â and a secondary astrometric data set containing the positions for an additional 1.1 billion sources. The second component is the photometric data set, consisting of mean G-band magnitudes for all sources. The G-band light curves and the characteristics of âŒ3000 Cepheid and RR-Lyrae stars, observed at high cadence around the south ecliptic pole, form the third component. For the primary astrometric data set the typical uncertainty is about 0.3 mas for the positions and parallaxes, and about 1 mas yrâ1 for the proper motions. A systematic component of âŒ0.3 mas should be added to the parallax uncertainties. For the subset of âŒ94 000 HIPPARCOS stars in the primary data set, the proper motions are much more precise at about 0.06 mas yrâ1. For the secondary astrometric data set, the typical uncertainty of the positions is âŒ10 mas. The median uncertainties on the mean G-band magnitudes range from the mmag level to âŒ0.03 mag over the magnitude range 5 to 20.7.
Conclusions. Gaia DR1 is an important milestone ahead of the next Gaia data release, which will feature five-parameter astrometry for all sources. Extensive validation shows that Gaia DR1 represents a major advance in the mapping of the heavens and the availability of basic stellar data that underpin observational astrophysics. Nevertheless, the very preliminary nature of this first Gaia data release does lead to a number of important limitations to the data quality which should be carefully considered before drawing conclusions from the data
Derivatization of estrogens enhances specificity and sensitivity of analysis of human plasma and serum by liquid chromatography tandem mass spectrometry
AbstractEstrogens circulate at concentrations less than 20pg/mL in men and postmenopausal women, presenting analytical challenges. Quantitation by immunoassay is unreliable at these low concentrations. Liquid chromatography tandem mass spectrometry (LCâMS/MS) offers greater specificity and sometimes greater sensitivity, but ionization of estrogens is inefficient. Introduction of charged moieties may enhance ionization, but many such derivatives of estrogens generate non-specific product ions originating from the âreagentâ group. Therefore an approach generating derivatives with product ions specific to individual estrogens was sought.Estrogens were extracted from human plasma and serum using solid phase extraction and derivatized using 2-fluoro-1-methylpyridinium-p-toluenesulfonate (FMP-TS). Electrospray in positive mode with multiple reaction monitoring using a QTrap 5500 mass spectrometer was used to quantify âFMPâ derivatives of estrogens, following LC separation.Transitions for the FMP derivatives of estrone (E1) and estradiol (E2) were compound specific (m/z 362â238 and m/z 364â128, respectively). The limits of detection and quantitation were 0.2pg on-column and the method was linear from 1â400pg/sample. Measures of intra- and inter-assay variability, precision and accuracy were acceptable (<20%). The derivatives were stable over 24h at 10°C (7â9% degradation). Using this approach, E1 and E2, respectively were detected in human plasma and serum: pre-menopausal female serum (0.5mL) 135â473, 193â722pmol/L; male plasma (1mL) 25â111, 60â180pmol/L and post-menopausal female plasma (2mL), 22â78, 29â50pmol/L.Thus FMP derivatization, in conjunction with LCâMS/MS, is suitable for quantitative analysis of estrogens in low abundance in plasma and serum, offering advantages in specificity over immunoassay and existing MS techniques
Solid confirmation of the broad DIB around 864.8 nm using stacked GaiaâRVS spectra
Context. Studies of the correlation between different diffuse interstellar bands (DIBs) are important for exploring their origins. However, the GaiaâRVS spectral window between 846 and 870 nm contains few DIBs, the strong DIB at 862 nm being the only convincingly confirmed one. /
Aims. Here we attempt to confirm the existence of a broad DIB around 864.8 nm and estimate its characteristics using the stacked GaiaâRVS spectra of a large number of stars. We study the correlations between the two DIBs at 862 nm (λ862) and 864.8 nm (λ864.8), as well as the interstellar extinction. /
Methods. We obtained spectra of the interstellar medium (ISM) absorption by subtracting the stellar components using templates constructed from real spectra at high Galactic latitudes with low extinctions. We then stacked the ISM spectra in Galactic coordinates (â,ââb) â pixelized by the HEALPix scheme â to measure the DIBs. The stacked spectrum is modeled by the profiles of the two DIBs, Gaussian for λ862 and Lorentzian for λ864.8, and a linear continuum. We report the fitted central depth (CD), central wavelength, equivalent width (EW), and their uncertainties for the two DIBs. /
Results. We obtain 8458 stacked spectra in total, of which 1103 (13%) have reliable fitting results after applying numerous conservative filters. This work is the first of its kind to fit and measure λ862 and λ864.8 simultaneously in cool-star spectra. Based on these measurements, we find that the EWs and CDs of λ862 and λ864.8 are well correlated with each other, with Pearson coefficients (rp) of 0.78 and 0.87, respectively. The full width at half maximum (FWHM) of λ864.8 is estimated as 1.62â
屉
0.33 nm which compares to 0.55â
屉
0.06 nm for λ862. We also measure the vacuum rest-frame wavelength of λ864.8 to be λ0â=â864.53â
屉
0.14 nm, smaller than previous estimates. /
Conclusions. We find solid confirmation of the existence of the DIB around 864.8 nm based on an exploration of its correlation with λ862 and estimation of its FWHM. The DIB λ864.8 is very broad and shallow. That at λ862 correlates better with E(BPâ
ââ
RP) than λ864.8. The profiles of the two DIBs could strongly overlap with each other, which contributes to the skew of the λ862 profile
Ultracool dwarfs in Gaia DR3
Aims. In this work we use the Gaia DR3 set of ultracool dwarf candidates and
complement the Gaia spectrophotometry with additional photometry in order to
characterise its global properties. This includes the inference of the
distances, their locus in the Gaia colour-absolute magnitude diagram and the
(biased through selection) luminosity function in the faint end of the Main
Sequence. We study the overall changes in the Gaia RP spectra as a function of
spectral type. We study the UCDs in binary systems, attempt to identify
low-mass members of nearby young associations, star forming regions and
clusters, and analyse their variability properties. Results. We detect 57
young, kinematically homogeneous groups some of which are identified as well
known star forming regions, associations and clusters of different ages. We
find that the primary members of 880 binary systems with a UCD belong mainly to
the thin and thick disk components of the Milky Way. We identify 1109 variable
UCDs using the variability tables in the Gaia archive, 728 of which belong to
the star forming regions defined by HMAC. We define two groups of variable UCDs
with extreme bright or faint outliers. Conclusions. The set of sources
identified as UCDs in the Gaia archive contains a wealth of information that
will require focused follow-up studies and observations. It will help to
advance our understanding of the nature of the faint end of the Main Sequence
and the stellar/substellar transition.Comment: Accepted by Astronomy and Astrophysics. 29 pages, 20 figures plus 3
appendice
Ăvolution de la contribution française Ă l'upgrade de LHCb
Ce document décrit l'évolution de la contribution française à l'upgrade de LHCb. Il s'inscrit dans le prolongement de la Lettre d'Intention [1], du Framework TDR [2], du document soumis au Conseil scientifique de l'IN2P3 le 21 juin 2012 [3], et des Technical Design Reports soumis au LHCC en novembre 2013 [4, 5]. Ces derniers concernent le détecteur de vertex et les détecteurs utilisés dans l'identification des particules. La contribution française s'est cristallisée autour de quatre grands projets : l'électronique front-end des calorimÚtres et du trajectographe à fibres scintillantes, le systÚme de déclenchement de premier niveau et la carte de lecture à 40MHz commune à l'ensemble des sous-systÚmes. Dans ce document nous décrivons les contributions envisagées et les ressources nécessaires pour mener à bien ces projets
Construction, assembly and tests of the ATLAS electromagnetic end-cap calorimeters
The construction and the assembly of the two end-caps of the ATLAS liquid argon electromagnetic calorimeter as well as their test and qualification programs are described. The work described here started at the beginning of 2001 and lasted for approximately three years. The results of the qualification tests performed before installation in the LHC ATLAS pit are given. The detectors are now installed in the ATLAS cavern, full of liquid argon and being commissioned. The complete detectors coverage is powered with high voltage and readout
A Purity Monitoring System for the H1 Liquid Argon Calorimeter
The ionization probes used for monitoring the liquid argon purity in the H1
calorimeter are described and results of their operation in tests at CERN and
during the period 1992 to the end of 1998 at HERA are given. The high
sensitivity of the charge measurements leads to refined charge collection
models, and to the observation of a variation of the ionization yield of our
electron sources with temperature.Comment: 26 pages, 14 figure
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