Performance and operation of the CMS electromagnetic calorimeter

The operation and general performance of the CMS electromagnetic calorimeter using cosmic-ray muons are described. These muons were recorded after the closure of the CMS detector in late 2008. The calorimeter is made of lead tungstate crystals and the overall status of the 75 848 channels corresponding to the barrel and endcap detectors is reported. The stability of crucial operational parameters, such as high voltage, temperature and electronic noise, is summarised and the performance of the light monitoring system is presented. © 2010 IOP Publishing Ltd and SISSA.

Time reconstruction and performance of the CMS electromagnetic calorimeter

The resolution and the linearity of time measurements made with the CMS electromagnetic calorimeter are studied with samples of data from test beam electrons, cosmic rays, and beam-produced muons. The resulting time resolution measured by lead tungstate crystals is better than 100 ps for energy deposits larger than 10 GeV. Crystal-to-crystal synchronization with a precision of 500 ps is performed using muons produced with the first LHC beams in 2008. © 2010 IOP Publishing Ltd and SISSA.

Performance of the CMS hadron calorimeter with cosmic ray muons and LHC beam data

The CMS Hadron Calorimeter in the barrel, endcap and forward regions is fully commissioned. Cosmic ray data were taken with and without magnetic field at the surface hall and after installation in the experimental hall, hundred meters underground. Various measurements were also performed during the few days of beam in the LHC in September 2008. Calibration parameters were extracted, and the energy response of the HCAL determined from test beam data has been checked. © 2010 IOP Publishing Ltd and SISSA.

Performance of CMS hadron calorimeter timing and synchronization using test beam, cosmic ray, and LHC beam data

This paper discusses the design and performance of the time measurement technique and of the synchronization systems of the CMS hadron calorimeter. Time measurement performance results are presented from test beam data taken in the years 2004 and 2006. For hadronic showers of energy greater than 100 GeV, the timing resolution is measured to be about 1.2 ns. Time synchronization and out-of-time background rejection results are presented from the Cosmic Run At Four Tesla and LHC beam runs taken in the Autumn of 2008. The inter-channel synchronization is measured to be within 2 ns. © 2010 IOP Publishing Ltd and SISSA.

Identification and filtering of uncharacteristic noise in the CMS hadron calorimeter

Commissioning studies of the CMS hadron calorimeter have identified sporadic uncharacteristic noise and a small number of malfunctioning calorimeter channels. Algorithms have been developed to identify and address these problems in the data. The methods have been tested on cosmic ray muon data, calorimeter noise data, and single beam data collected with CMS in 2008. The noise rejection algorithms can be applied to LHC collision data at the trigger level or in the offline analysis. The application of the algorithms at the trigger level is shown to remove 90% of noise events with fake missing transverse energy above 100 GeV, which is sufficient for the CMS physics trigger operation. © 2010 IOP Publishing Ltd and SISSA.

Performance of the CMS drift tube chambers with cosmic rays

Studies of the performance of the CMS drift tube barrel muon system are described, with results based on data collected during the CMS Cosmic Run at Four Tesla. For most of these data, the solenoidal magnet was operated with a central field of 3.8 T. The analysis of data from 246 out of a total of 250 chambers indicates a very good muon reconstruction capability, with a coordinate resolution for a single hit of about 260 μm, and a nearly 100% efficiency for the drift tube cells. The resolution of the track direction measured in the bending plane is about 1.8 mrad, and the efficiency to reconstruct a segment in a single chamber is higher than 99%. The CMS simulation of cosmic rays reproduces well the performance of the barrel muon detector. © 2010 IOP Publishing Ltd and SISSA.

Performance study of the CMS barrel resistive plate chambers with cosmic rays

In October and November 2008, the CMS collaboration conducted a programme of cosmic ray data taking, which has recorded about 270 million events. The Resistive Plate Chamber system, which is part of the CMS muon detection system, was successfully operated in the full barrel. More than 98% of the channels were operational during the exercise with typical detection efficiency of 90%. In this paper, the performance of the detector during these dedicated runs is reported. © 2010 IOP Publishing Ltd and SISSA.

Performance of the CMS cathode strip chambers with cosmic rays

The Cathode Strip Chambers (CSCs) constitute the primary muon tracking device in the CMS endcaps. Their performance has been evaluated using data taken during a cosmic ray run in fall 2008. Measured noise levels are low, with the number of noisy channels well below 1%. Coordinate resolution was measured for all types of chambers, and fall in the range 47μm to 243μm. The efficiencies for local charged track triggers, for hit and for segments reconstruction were measured, and are above 99%. The timing resolution per layer is approximately 5 ns. © 2010 IOP Publishing Ltd and SISSA.

Aligning the CMS muon chambers with the muon alignment system during an extended cosmic ray run

The alignment system for the muon spectrometer of the CMS detector comprises three independent subsystems of optical and analog position sensors. It aligns muon chambers with respect to each other and to the central silicon tracker. System commissioning at full magnetic field began in 2008 during an extended cosmic ray run. The system succeeded in tracking muon detector movements of up to 18 mm and rotations of several milliradians under magnetic forces. Depending on coordinate and subsystem, the system achieved chamber alignment precisions of 140-350 μm and 30-200 μrad, close to the precision requirements of the experiment. Systematic errors on absolute positions are estimated to be 340-590 μm based on comparisons with independent photogrammetry measurements. © 2010 IOP Publishing Ltd and SISSA.

Precise mapping of the magnetic field in the CMS barrel yoke using cosmic rays

The CMS detector is designed around a large 4 T superconducting solenoid, enclosed in a 12 000-tonne steel return yoke. A detailed map of the magnetic field is required for the accurate simulation and reconstruction of physics events in the CMS detector, not only in the inner tracking region inside the solenoid but also in the large and complex structure of the steel yoke, which is instrumented with muon chambers. Using a large sample of cosmic muon events collected by CMS in 2008, the field in the steel of the barrel yoke has been determined with a precision of 3 to 8% depending on the location. © 2010 IOP Publishing Ltd and SISSA.

Performance of CMS muon reconstruction in cosmic-ray events

The performance of muon reconstruction in CMS is evaluated using a large data sample of cosmic-ray muons recorded in 2008. Efficiencies of various high-level trigger, identification, and reconstruction algorithms have been measured for a broad range of muon momenta, and were found to be in good agreement with expectations from Monte Carlo simulation. The relative momentum resolution for muons crossing the barrel part of the detector is better than 1% at 10 GeV/c and is about 8% at 500 GeV/c, the latter being only a factor of two worse than expected with ideal alignment conditions. Muon charge misassignment ranges from less than 0.01% at 10GeV/c to about 1% at 500 GeV/c. © 2010 IOP Publishing Ltd and SISSA.

L'Amour dácadent em dramas de Villiers de L'Isle-Adam e Maurice Maeterlinck

Pós-graduação em Estudos Literários - FCLAR

Radiative transfer analyses of Titan's tropical atmosphere

Titan's optical and near-IR spectra result primarily from the scattering of sunlight by haze and its absorption by methane. With a column abundance of 92 km amagat (11 times that of Earth), Titan's atmosphere is optically thick and only similar to 10% of the incident solar radiation reaches the surface, compared to 57% on Earth. Such a formidable atmosphere obstructs investigations of the moon's lower troposphere and surface, which are highly sensitive to the radiative transfer treatment of methane absorption and haze scattering. The absorption and scattering characteristics of Titan's atmosphere have been constrained by the Huygens Probe Descent Imager/Spectral Radiometer (DISR) experiment for conditions at the probe landing site (Tomasko, M.G., Bezard, B., Doose, L., Engel, S., Karkoschka, E. 120084 Planet. Space Sci. 56, 624-247: Tomasko, M.G. et al. [2008b] Planet. Space Sci. 56, 669-707). Cassini's Visual and Infrared Mapping Spectrometer (VIMS) data indicate that the rest of the atmosphere (except for the polar regions) can be understood with small perturbations in the high haze structure determined at the landing site (Penteado, P.F., Griffith, CA., Tomasko, M.G., Engel, S., See, C., Doose, L, Baines, K.H., Brown, R.H., Buratti, B.J., Clark, R., Nicholson, P., Sotin, C. [2010]. Icarus 206, 352-365). However the in situ measurements were analyzed with a doubling and adding radiative transfer calculation that differs considerably from the discrete ordinates codes used to interpret remote data from Cassini and ground-based measurements. In addition, the calibration of the VIMS data with respect to the DISR data has not yet been tested. Here, VIMS data of the probe landing site are analyzed with the DISR radiative transfer method and the faster discrete ordinates radiative transfer calculation; both models are consistent (to within 0.3%) and reproduce the scattering and absorption characteristics derived from in situ measurements. Constraints on the atmospheric opacity at wavelengths outside those measured by DISR, that is from 1.6 to 5.0 mu m, are derived using clouds as diffuse reflectors in order to derive Titan's surface albedo to within a few percent error and cloud altitudes to within 5 km error. VIMS spectra of Titan at 2.6-3.2 mu m indicate not only spectral features due to CH4 and CH3D (Rannou, P., Cours, T., Le Mouelic, S., Rodriguez, S., Sotin, C., Drossart, P., Brown, R. [2010]. Icarus 208, 850-867), but also a fairly uniform absorption of unknown source, equivalent to the effects of a darkening of the haze to a single scattering albedo of 0.63 +/- 0.05. Titan's 4.8 mu m spectrum point to a haze optical depth of 0.2 at that wavelength. Cloud spectra at 2 mu m indicate that the far wings of the Voigt profile extend 460 cm(-1) from methane line centers. This paper releases the doubling and adding radiative transfer code developed by the DISR team, so that future studies of Titan's atmosphere and surface are consistent with the findings by the Huygens Probe. We derive the surface albedo at eight spectral regions of the 8 x 12 km(2) area surrounding the Huygens landing site. Within the 0.4-1.6 mu m spectral region our surface albedos match DISR measurements, indicating that DISR and VIMS measurements are consistently calibrated. These values together with albedos at longer 1.9-5.0 mu m wavelengths, not sampled by DISR, resemble a dark version of the spectrum of Ganymede's icy leading hemisphere. The eight surface albedos of the landing site are consistent with, but not deterministic of, exposed water ice with dark impurities. (C) 2011 Elsevier Inc. All rights reserved.

New activity in the large circumstellar disk of the Be-shell star 48 Librae

Aims. Spectroscopic, polarimetric, and high spectral resolution interferometric data covering the period 1995-2011 are analyzed to document the transition into a new phase of circumstellar disk activity in the classical Be-shell star 48 Lib. The objective is to use this broad data set to additionally test disk oscillations as the basic underlying dynamical process. Methods. The long-term disk evolution is described using the V/R ratio of the violet and red emission components of H alpha and Br gamma, radial velocities and profiles of He I and optical metal shell lines, as well as multi-band BVRI polarimetry. Single-epoch broad-band and high-resolution interferometric visibilities and phases are discussed with respect to a classical disk model and the given baseline orientations. Results. Spectroscopic signatures of disk asymmetries in 48 Lib vanished in the late nineties but recovered some time between 2004 and 2007, as shown by a new large-amplitude and long-duration V/R cycle. Variations in the radial velocity and line profile of conventional shell lines correlate with the V/R behavior. They are shared by narrow absorption cores superimposed on otherwise seemingly photospheric He I lines, which may form in high-density gas at the inner disk close to the photosphere. Large radial velocity variations continued also during the V/R-quiet years, suggesting that V/R may not always be a good indicator of global density waves in the disk. The comparison of the polarization after the recovery of the V/R activity shows a slight increase, while the polarization angle has been constant for more than 20 years, placing tight limits on any 3-D precession or warping of the disk. The broad H-band interferometry gives a disk diameter of (1.72 +/- 0.2) mas (equivalent to 15 stellar radii), position angle of the disk (50 +/- 9)degrees and a relatively low disk flattening of 1.66 +/- 0.3. Within the errors the same disk position angle is derived from polarimetric observations and from photocenter shifts across Br gamma. The high-resolution interferometric visibility and phase profiles show a double or even multiple-component structure. A preliminary estimate based on the size of the Br gamma emitting region indicates a large diameter for the disk (tens of stellar radii). Overall, no serious contradiction between the observations and the disk-oscillation model could be construed.

La gestione di sorgenti multiple di disturbo in AMP: il caso delle Isole Tremiti

La gestione di sorgenti multiple di disturbo in AMP: il caso delle Isole Tremiti Il seguente lavoro di tesi valuta l’efficacia di protezione di un’area marina protetta (AMP) sui popolamenti di differenti habitat compresi in zone a diverso regime di tutela. Questo tema è molto sentito sia dal punto di vista scientifico, poiché le AMP rappresentano uno esperimento di esclusione delle attività antropiche ad ampia scala, sia dal punto di vista socio-economico per l’interesse che sono in grado di generare nelle comunità locali. Tuttavia, ad oggi, gli studi che abbiano dimostrato l’efficacia di protezione delle AMP sono pochi e sono per lo più diretti sulle specie di maggior interesse commerciale. In generale, c’è un’evidente mancanza di protezione in molte AMP del Mediterraneo e di aree extra-mediterranee che può essere attribuita a diversi fattori, tra cui le caratteristiche fisiche dei siti dove sono state istituite, le modalità di gestione e le numerose attività illegali che vengono svolte all’interno dei loro confini. Inoltre, nelle aree protette, spesso, anche le attività lecite non sono adeguatamente regolamentate, limitando ulteriormente il perseguimento degli obiettivi istitutivi e la tutela della biodiversità marina. Testare le ipotesi sull’efficacia di protezione delle AMP è, quindi, di fondamentale importanza per capire quali tipi di impatti sono maggiormente presenti e per poter fornire agli Enti gestori informazioni utili per migliorare l’amministrazione delle AMP. In particolare, l’AMP dell’arcipelago delle Isole Tremiti, istituita da oltre venti anni, è un’area protetta che presenta molte criticità, come dimostrato in precedenti campagne di monitoraggio condotte dal Consorzio Nazionale Interuniversitario per le Scienze del Mare (CoNISMa). In questo contesto, la presente tesi è stata sviluppata con lo scopo di quantificare l’effetto della regolamentazione di diverse attività umane sui popolamenti del subtidale, della frangia e delle praterie di Posidonia oceanica nell’AMP delle Isole Tremiti a diverse scale spaziali per un periodo di circa dieci anni. Questo lavoro, inoltre, rientra in un progetto finanziato dal Ministero dell’Ambiente e della Tutela del Territorio e del Mare al CoNISMa volto ad impostare un’attività di monitoraggio sperimentale e di mitigazione in questa AMP. I campionamenti sono stati condotti tra Giugno e Settembre 2010 e i dati raccolti sono stati integrati a quelli ottenuti nei precedenti monitoraggi svolti nelle Isole Tremiti. I risultati hanno mostrato che: 1) ci sono differenze significative consistenti nel tempo tra il subtidale dell’isola di Pianosa e quello delle altre isole dell’arcipelago; 2) i popolamenti nella frangia di Pianosa, di San Domino e di Caprara non presentano differenze significative; 3) c’è un’elevata variabilità a scala di sito nelle praterie di Posidonia oceanica, ma non si osserva una differenza tra località protette ed impattate. La differenza riscontrata nel subtidale tra zona a protezione integrale (Pianosa) e le altre isole dell’arcipelago (controlli) non è però attribuibile ad un effetto della protezione. Infatti, il subtidale di Pianosa è caratterizzato da un barren molto esteso con elevate percentuali di spugne rosse incrostanti, di alghe rodoficee incrostanti e di ricci di mare, mentre nelle isole di San Domino e di Caprara c’è una maggiore diversità data da alghe corallinacee articolate, alghe erette, idrozoi, ascidiacei e numerose spugne. Diversi fattori possono aver agito nel determinare questo risultato, ma molto probabilmente la cospicua attività di pesca illegale che viene praticata a Pianosa combinata all’attività di grazing degli erbivori, non controllati dai predatori, limita il recupero dei popolamenti. Al contrario, l’assenza di differenze nei popolamenti della frangia delle tre isole campionate fa ipotizzare la mancanza di impatti diretti (principalmente il calpestio) su questo habitat. Per quanto riguarda la Posidonia oceanica i risultati suggeriscono che si stia verificando un ancoraggio indiscriminato su tutte le praterie delle Isole Tremiti e che molto probabilmente si tratta di praterie in forte regressione, come indicano anche le ricerche condotte dall’Università di Bari. C’è bisogno, tuttavia, di ulteriori studi che aiutino a comprendere meglio la variabilità nella riposta dei popolamenti in relazione alle diverse condizioni ambientali e al diverso sforzo di gestione. In conclusione, dai risultati ottenuti, emerge chiaramente come anche nell’AMP delle Isole Tremiti, ci sia una scarsa efficacia di protezione, così come è stato rilevato per la maggior parte delle AMP italiane. Per risolvere le costanti conflittualità che perdurano nelle Isole Tremiti e che non permettono il raggiungimento degli obiettivi istitutivi dell’AMP, è assolutamente necessario, oltre che far rispettare la regolamentazione vigente incrementando il numero di guardacoste sull’isola durante tutto l’anno, procedere, eventualmente, ad una rizonizzazione dell’AMP e sviluppare un piano di gestione in accordo con la popolazione locale adeguatamente sensibilizzata. Solo in questo modo sarà possibile ridurre le numerose attività illegali all’interno dell’AMP, e, allo stesso tempo, rendere gli stessi cittadini una componente imprescindibile della conservazione di questo arcipelago.