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REM (Rapid Eye Mount) is a fully robotized fast slewing telescope equipped with a high throughput Near InfraRed (Z′, J, H, K′) camera (REMIR) and an optical slitless spectrograph (ROSS). A dedicated software for data reduction and software (AQuA) has been developed to extract scientific information from REM images without any human intervent. REM is installed in La Silla (Chile) and dedicated to detect and study the prompt optical/IR afterglow of Gamma Ray Bursts with the ambitious project of discovering objects at extremely high redshift. The synergy between REMIR camera and ROSS makes REM a powerful observing tool for any kind of fast transient phenomena.
Centaurus A (NGC 5128) is a giant early-type galaxy containing the nearest radio-bright AGN. The high-angular resolution Chandra images of Cen A reveal multi-scale X-ray structures with unprecedented detail and clarity. We present results from our study of X-ray structures surrounding the Cen A nuclear region, including the discovery of giant arc-like structures, extending to about 8 kpc in the direction perpendicular to the jet. We compare the X-ray structures with observations in other wavelengths and discuss their implication for a global understanding of the morphology of Cen A.
We present a study of X-ray column density variability in Seyfert 2 galaxies. We show that variations in NH are observed in almost all the objects with multiple hard X-ray observations. Variation timescales (as short as a few months in several cases) are not in agreement with the standard scenario of a parsec-scale toroidal absorber. We propose that the X-ray absorber in Seyfert galaxies is located much nearer to the centre than previously assumed, on the broad line region scale. An extension of the model by M. Elvis (2000) can explain the observed variability. We also show preliminary results of NH variability search inside single X-ray observations, which suggest that variations can occur on timescales of a few 104 s.
The BaR-SPOrt experiment is designed to measure the E-mode
power spectrum of the Cosmic Microwave Background Polarization (CMBP)
in the multipole range 50 < l < 1000.
In the current configuration at 32 GHz
it can explore up to l = 400.
Recent low frequency observations of the target region show that
the synchrotron emission should not contamine the CMBP already at 32 GHz.
A 6-month observation of a 6° × 6° sky area
during the polar night, in ideal
environmental conditions, will allow the Italian-French collaboration
to both measure the E–mode power spectrum with appropriate sensitivity
and perform important tests of the anomalous dust emission.
The BaR-SPOrt 32 GHz instrument, now under test and ready
for operations by Spring 2005, is proposed
for 1–2 years Winter operations at Dome C.
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