WFPC2 . Images: version1 , version2 . Catalogs: Version 1 HDF-S , HDF-N ;Version 2 HDF-S . STIS . ... NICMOS . Images: Camera 3 , V2 of psf-convolved STIS 50CCD on NICMOS . ... Images: WFPC2 FF , STIS FF ; Version2: WFPC2 FF , STIS FF , NICMOS FF . Catalogs: Version2 WFPC2 FF , STIS FF , NICMOS FF . ... Check the instrument specific technical pages for a description of the data products and the implemented data reduction steps: STIS , WFPC2 , NICMOS , Flanking Fields . ...

We report first results of a multifrequency campaign from radio to hard X-ray energies of the prominent gamma-ray blazar 3C 279 during the first year of the INTEGRAL mission. The variable blazar was found at a low activity level, but was detected by all participating instruments. Subsequently a multifrequency spectrum could be compiled. ... In addition, this 2003 broadband spectrum is compared to one measured in 1999 during a high activity period of 3C 279. | ...

Next: Results & Discussion Up: Coronal Hole Diagnostics out Previous: Introduction . ... The dates of the observations discussed here, their locations, pointing, slit sizes and exposure times are given in BTDW. ... Line fits are given by the dotted line. ... An estimation of the errors in the derived parameters was obtained using the GA-derived parameters as an input for a ``classical'' IDL-CURVEFIT procedure (Peter, 1999; Peter & Judge, 1999). ...

... A comparison of the computed and experimental relations F max ( H), as well as comparison of drift scans of point sources across different horizontal cross-sections of the BP with the corresponding computed cross-sections were made. ... The drift scans of the point source 3С84 (H=87 o ) at the wavelength 7.6 cm across the horizontal cross-sections of the BP (black lines) and the computed horizontal cross-sections of the BP corresponding to them (red lines). ...

... An interactive IRAF task for the analysis of Extreme Ultraviolet Explorer ( EUVE ) emission line spectra is presented. The line flux in extracted spectra may be measured by multiple techniques, including fitting individual lines. ... To aid in identifying lines, the positions of known lines may be marked on the spectrum during the fitting process. Also, model EUVE spectra may be constructed and overlaid using plasma emissivities and source emission measures supplied by the user. ...

... As a result of BTA observations of 23 chemically peculiar stars with strong magnetic fields, it was found that in 22 of them the longitudinal magnetic field, measured from the hydrogen line cores are considerably lower (by about 1/3) than the value measured from metal lines in the same spectra. ... New approaches need to be developed in order to interpret the data. ... The Zeeman spectrum of a star with a strong magnetic field, 53 Cam. ...

... P2205 Date Received: 2006­Feb­01 13:23:49 Technical Page Proposal Type: Regular General Category: Pulsars Observation Category: Total Time Requested: 21.5 Hours Proposal Title: Monitoring and Timing of RRAT Sources ABSTRACT: We have recently reported the discovery of a new class of Rotating RAdio Transients ( RRATs ), 11 objects characterized by repeated radio bursts with widths of 2 to 30 ms. While periods in the 0.4 to 7 s range have been measured from the arrival ...

Next: Results of follow-up spectroscopy Up: Spectral observations and data Previous: Calar Alto 2.2m observations . ... The context SPEC is adapted to the SAO data formats to perform an automatic reduction of the one-dimensional IPCS spectra (Kniazev [ 1994 ]). ... For the Calar Alto two-dimensional CCD data, the reduction included bias-dark correction, cosmic-ray removal and flat-field correction. ... Calar Alto CCD spectra are presented on an absolute flux scale. ...

XMM-Newton CCF Release Note XMM-CCF-REL-290 Implementation of the Variable Boresight for RGS R. Gonzґlez-Riestra a July 20, 2012 1 CCF comp onents Name of CCF XMM BORESIGHT 0023 VALDATE 2000-01-01T00:00:00 EVALDATE ­ Blocks changed RGS1 ANGVAR RGS2 ANGVAR XSCS flag NO 2 Changes Starting in SASv12.0, a variable b oresight is b eing used for the processing of data from the Optical Monitor and the EPIC cameras on-b oard XMM-Newton [1]. ... The scatter of the data is 1 mA smaller as well (see Fig. ...

The information path to prepare, perform and reduce a radioastronomical observation, using the Arcos correlator , is schematized in the figure: . The programs reside part on the computer network of the Arcetri Observatory, and part at the Medicina Radio Telescope . All programs running at Arcetri are written for a Sun workstation, and are public domain software, available upon request. Programs running at the telescope are written for a PC with DOS/Windows (or Linux).

... Simple X-ray Aperture Photometry Problem : Determine source intensity s and errors for an unresolved (point) x-ray source Know: · Number of counts , C, in source aperture (solid green ellipse) · Number of counts , B, in background aperture (dashed green elliptical annulus) · Areas As and Ab of source and background apertures · f = psf(x,y)dx dy over source aperture · g = psf(x,y)dx dy over background ... What happens if the single observation pdf 's are distinct? ...