In this article we discuss the possibility of using the observations by GLAST of standard gamma sources, as the Crab Nebula, to calibrate imaging air Cherenkov detectors, MAGIC in particular, and ...optimise their energy resolution. We show that at around 100
GeV the absolute energy calibration uncertainty of Cherenkov telescopes can be reduced to ≲10% by means of such cross-calibration procedure.
We are developing a novel Transition Radiation Detector (SiTRD) based on silicon strip detectors (SSDs) operated in a magnetic field region. In this way the trajectory of the radiating particle is ...deflected with respect to the Transition Radiation X-rays that are absorbed in a detector region far away from the particle track. The SiTRD combines the particle identification performance of a traditional TRD with the high-precision tracking capability of SSDs, and it can be suitable for both accelerator and cosmic ray experiments, whenever particle identification and momentum reconstruction are required. In this paper we will show the experimental results obtained with a reduced scale SiTRD prototype exposed to an electron–pion beam.
CALCO, the Conference on Algebra and Coalgebra in Computer Science, is a high-level, bi-annual conference formed by joining CMCS (the International ...WorkshoponCoalgebraicMethodsinComputerScience)andWADT(theWo- shoponAlgebraicDevelopmentTechniques).CALCObringstogetherresearchers and practitioners to exchange new results related to foundational aspects and both traditional and emerging uses of algebras and coalgebras in computer s- ence. The study of algebra and coalgebra relates to the data, process and str- tural aspects of software systems. CALCO is supervised by the Steering C- mittee, co-chaired by Jos´ e Luiz Fiadeiro and Jan Rutten. The ?rst two CALCO conferences took place in 2005 in Swansea, Wales, and in 2007 in Bergen, Norway. CALCO 2009, the third event in the series, took place in Udine, Italy, during September 7-10, 2009. CALCO 2009 received 42 submissions, out of which 23 were selected for presentationattheconference.Inspiteofarelativelylownumberofsubmissions, their standard was generally very high. The selection process was carried out by the Program Committee, taking into account the originality, quality and relevance of the material presented in each submission, based on the opinions of expert reviewers, four for each submission. The selected and revised papers are included in this volume, together with the contributions from the invited speakersMaiGehrke,ConorMcBride,PrakashPanangadenandGordonPlotkin.
With its diameter of 17m, the MAGIC telescope is the largest Cherenkov detector for gamma ray astrophysics. It is sensitive to photons above an energy of 30 GeV. MAGIC started operations in October ...2003 and is currently taking data. This report summarizes its main characteristics, its first results and its potential for physics.
Astropart.Phys. 23 (2005) 572-576 In this article we discuss the possibility of using the observations by GLAST
of standard gamma sources, as the Crab Nebula, to calibrate Imaging Air
Cherenkov ...detectors, MAGIC in particular, and optimise their energy resolution.
We show that at around 100 GeV the absolute energy calibration uncertainty of
Cherenkov telescopes can be reduced to <10% by means of such cross-calibration
procedure.
With its diameter of 17m, the MAGIC telescope is the largest Cherenkov
detector for gamma ray astrophysics. It is sensitive to photons above an energy
of 30 GeV. MAGIC started operations in October ...2003 and is currently taking
data. This report summarizes its main characteristics, its rst results and its
potential for physics.
Astrophys.J.642:L119-L122,2006 The MAGIC collaboration has studied the high peaked BL-Lac object
1ES1218+30.4 at a redshift z = 0.182, using the MAGIC imaging air Cherenkov
telescope located on the ...Canary island of La Palma. A gamma-ray signal was
observed with 6.4sigma significance. The differential energy spectrum for an
energy threshold of 120GeV can be fitted by a simple power law yielding F_E(E)
= (8.1+-2.1)*10^-7 (E/250GeV)^(-3.0+-0.4) TeV^-1 m^-2 s^-1. During the six days
of observation in January 2005 no time variability on time scales of days was
found within the statistical errors. The observed integral flux above 350GeV is
nearly a factor two below the the upper limit reported by the Whipple
Collaboration in 2003.
In this article we discuss the possibility of using the observations by GLAST of standard gamma sources, as the Crab Nebula, to calibrate Imaging Air Cherenkov detectors, MAGIC in particular, and ...optimise their energy resolution. We show that at around 100 GeV the absolute energy calibration uncertainty of Cherenkov telescopes can be reduced to <10% by means of such cross-calibration procedure.
With its diameter of 17m, the MAGIC telescope is the largest Cherenkov detector for gamma ray astrophysics. It is sensitive to photons above an energy of 30 GeV. MAGIC started operations in October ...2003 and is currently taking data. This report summarizes its main characteristics, its rst results and its potential for physics.
Astrophys.J.641:L9-L12,2006 The long-duration GRB050713a was observed by the MAGIC Telescope, 40 seconds
after the burst onset, and followed up for 37 minutes, until twilight. The
observation, ...triggered by a SWIFT alert, covered energies above ~175 GeV. Using
standard MAGIC analysis, no evidence for a gamma signal was found. As the
redshift of the GRB was not measured directly, the flux upper limit, estimated
by MAGIC, is still compatible with the assumption of an unbroken power-law
spectrum extending from a few hundred keV to our energy range.
PDF