... The sky distribution of the BCGs from the HSS sample is shown in Fig. 6 together with BCGs from the SBS and Case surveys (Izotov et al. [ 1993b ]; Pustilnik et al. ... First, we compare the apparent magnitude distributions of the three samples. ... The similar behaviour of the faint end of the apparent magnitude distributions infers that the Northern BCG sample may have a similar completeness down to this limiting magnitude. ...

... Fitting the observed dependence includes calculations of the polarization cross-sections averaged over particles orientation and size distribution, their normalization and the comparison of obtained dependencies with Serkowski's curve representing observational data for a chosen star. ... Variations of the polarization factors with wavelength are shown in Fig. 16 for homogeneous spheroidal particles with PF orientation. ... The distinction between prolate and oblate spheroids is also clearly seen. ...

Next: Redshift Distribution Up: Sample Identification Previous: Previously Identified Sources . ... In Figure 3, we plot the redshift distribution of DXRBS FSRQs opposite that of the 1 Jy and S4 samples. In Figure 4, we plot the redshift distribution of DXRBS BL Lacs opposite the Slew and 1 Jy samples. ... The apparent deficit of objects at the very highest luminosities is a result of the smaller area of sky covered by DXRBS compared to, e.g., the Slew and 1 Jy samples. ...

... In order to compare the number of different evolutionary stages obtained and X-ray luminosity of the chosen X-ray sources with the observed galactic values we use the sum of C/O+O/C , where C and O are the calculated and observed values of a given binary type, respectively. If we make comparison for a number of different binary species (for example, we compare the number of CV, number of X-ray pulsars,   total X-ray luminosity of LMXB, etc.), we write this criterion in the form: . ...

Next: Discussion Up: Iterative/Recursive Deconvolution with Application Previous: Test Results . There have been several investigations of the photometric properties of HST image restoration techniques utilizing a range of different algorithms. ... They used that technique to restore a simulated image of a crowded field. ... Cohen (1991) investigated the reliability of the Maximum Entropy method (Skilling 1989, Gull 1989) in restoring astronomical images while preserving photometric accuracy. ...

Next: The Chemical Evolution of Up: Stellar Astrophysics Previous: Stellar Astrophysics . Simon Jeffery has used a novel camera attached to the William Herschel Telescope (WHT) to obtain the best light curves ever obtained for pulsating subdwarf B stars. These stars pulsate non-radially in several modes with different frequencies and enable astronomers to establish their overall properties and internal structure with unusual precision. ...

... The nebular spectra of SNeIa can be used to determine the mass, density, and distribution of the SN ejecta, and the distance and reddening to the SN. Synthetic spectra can very rapidly be computed in NLTE and compared to the observed ones. Given the relatively large number of parameters, it is convenient to explore the parameter space in an automated form. The nebular spectrum synthesis code can be run in parallel on a workstation cluster. ...

... ATNF Home . About ATNF . ... About ATNF overview . ... Australia Telescope Steering Committee . ... Australia Telescope User Committee . ... Murchison Radio-astronomy Observatory . ... Parkes radio telescope . Australia Telescope Compact Array . Mopra radio telescope . ... Parkes | ... Visiting Parkes radio telescope . ... Parkes radio telescope webcam . ... The first claim that HI could be associated with a dSph-like system was for the dIrr/dSph system Phoenix (Carignan, Demers & CУДtУ? ...

... R2422 Date Received: 2008­May­30 13:02:35 Technical Page Proposal Type: Regular General Category: Planetary Radar Sub­Category: Radar Observation Category: Solar System Total Time Requested: 22 Hours Minimum Useful Time: 2h Proposal Title: Continuation of Long­term Survey of Main­Belt M and X­class Asteroids. ... Zwetana is of special interest because it shows the largest rotational variation in radar albedo of any asteroid observed, ranging from a low of 0.10 to a high of 0.60. ...

... Abstract: We present Monte Carlo radiative transfer simulations for spiral galaxies modelled as a stellar disk and a two-phase clumpy dust distribution. ... As a general result, clumpy models are less opaque than the corresponding homogeneous models. ... 0.00 0.15 0.50 0.1 0.5 1.0 2.0 5.0 10.0 0.25 X . ... We have also produced several homogeneous models, to compare to the clumpy models. ... Homogeneous and clumpy models with the same tauV have the same dust mass. ...

... We publish 16 Doppler imaging temperature maps for the years 1994-2002 of the active RS CVn star II Peg. ... Through Doppler imaging we want to study the spot evolution of the star and in particular compare this with previous results showing a cyclic spot behaviour and persistent active lo