... A demonstration of HST WFPC image restoration has been made using both empirical and simulated PSFs. Empirical PSFs are obtained from the WFPC PSF library and also extracted from the image to be restored. ... The best results obtained thus far rely upon being able to determine a high S/N empirical PSF from the data frame. In order to achieve accurate restorations of data with high dynamic range excellent PSF models are required. ... Keywords: image restoration, HST WFPC image, PSFs . ...

Physica C 1 PHYSICA C C ELSEVIER CONDUCTIVITY and Antiferromagnetism of CaCuO2 Thin Films Doped by Sr Gennady A. Ovsyannikova,b*, Viktor V. Demidovb, Yuli V. Kislinskib, Philippe V. Komissinskia,b, Dag Winklera a Chalmers ... revised date here; accepted date here Abstract The results of electrical and magnetic investigations of epitaxial CaxSr1-xCuO2 ( CSCO ) thin films grown by pulsed laser deposition are presented ... Temperature dependence EPR amplitude for two CSCO films with =0.15 ...

... 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. ...

We present simultaneous ultraviolet and optical observations of five flares on the very late type M dwarf Gl 866 (dM5.5e). A procedure to estimate the physical parameters of the flaring plasma has been developed using a simplified model of the flare and a comparison of observed and computed Balmer decrements. With this procedure we have determined the optical thickness, electron temperature and electron density of the flaring plasma at flare maximum for three spectroscopically observed flares. ...

... We will consider the rms, (K), for observations with a receiver of system temperature, T , frequency resolution, per polarization, and total integration time per observing cycle, . ... For ``in-band'' frequency switching, the line under investigation is always in the observing band. ... Position Switching or ``Out-of-Band'' Frequency Switching: Here the line is only observed for one half of the time, with noise being present all of the time. ...

... Test T1: Creation of the transfer/linearity table. The table will contain 5 columns: column 1 for the exposure time of the first of each sets (frames 1) (label :Exp_tim1); column 2 the exposure time of the second frames (frames 2) (:Exp_tim2); column 3 the median pixel intensities over the selected frame sections in frames 1 (:Med_cnt1); column 4 the median pixel intensities over the selected area in frames 2 (:Med_cnt2) ; column 5 the variance of the difference of the frames 1 and 2 (:Variance). ...

... Contacts . 2012: . ... We refined the fundamental parameters of the components, the orbital periods, and the conditions of photospheric heating of the secondary component by the ultraviolet radiation of the hot component. ... The observations of the star clusters associated with ultra-luminous x-ray sources (ULXs) in four galaxies on the 6-meter and VLT telescopes have shown that all the ULXs are located within 200pc of very young star clusters (younger than 5 million years). ... Archive . ...

IBIS Data Analysis . ... IBIS . ... Flat Fielding - Introduction . The images obtained by IBIS will have intensity variations across the field of view that are not due to the solar image, but rather caused by instrumental effects that alter the observed intensity in each point of the field of view. ... IBIS Flat Fielding Techniques . ... Therefore, it is desirable to obtain the flat field measurements center on a point along the equator near the heliographic center of the solar disk. ...

... The x-ray spectral analysis consists of a comparison between the observed pulse height spectrum and a pulse height spectrum calculated using a given spectral model. ... To obtain the spectral parameters for an x-ray source, several steps need to be followed. For each source: . ... obtain the best fit parameters for a spectral model - repeated for each model of interest . obtain a 1-D or 2-D grid of values around the best fit values - this can be done for as many models as desired . ...

... The package AMPLE (Adaptable Minor Planet Ephemerides) is dedicated to solving a number of problems concerning minor planets with the aid of IBM-type personal computer. ... Obtaining selection of orbital elements and/ or photometric parameters of minor planets in conformity with imposed restrictions. ... The orbital elements of all minor planets used in AMPLE for 2015 have been determined in IAA on the ground of available observations in the catalogue of observations of the Minor Planet Center. ...

... Phys. (U.S.S.R. ) 42, 1416-1418 (May, 1962) A series of size effects , which are determined by the relationships between the size of electron orbits and the size of a metallic sample, can be observed when a sample having a long fre e path is placed in a constant magnetic field. ... When the field is increased the radius of the electron orbit decreases, and the numbe r of return s of the electron throug h the skin layer durin g the fre e path time increases. ... The sample had a thickness of 0.54 mm ...

... About ATNF overview . ... Australia Telescope Steering Committee . ... Parkes radio telescope . Australia Telescope Compact Array . ... Information & tools for observers . ... Virtual Radio Interferometer . ... The ratio above is called the resolution of the telescope. ... An interferometer works most efficiently, in the sense of returning the most information about the intensity and size of the source being observed, for a source whose size is comparable with the telescope's resolution. ...

Next: Radial velocity of the Up: Optical spectrum of IRAS04296 Previous: Observations and spectra reduction . ... However, molecular emission features are only very rarely observed in the optical spectra of PPNe. ... On the other hand, it is well known that cometary nuclei spectra show prominent Swan band emission. In both spectra of IRAS04296 we have discovered strong emission in the (0;0) and (0;1) bands of the Swan system of the molecule. ... Now consider the case of IRAS04296. ...

... the time of observation . ... Observing the Changing Position of the Sun To Establish Cardinal Directions . ... Observations of the Sun's apparent movement across the sky and its pattern of rising and setting in the east and west horizon helped to establish the cardinal directions. ... The final stage of the Sun's return was marked by the observation that the Sun had reached its highest altitude when the full width of your mitted hand could fill the gap between the Sun and the horizon. ...

... Science Users Information > Science and Technical Meetings > Conferences 2010 > The Origin and Fate of the Sun: Evolution of Solar-mass Stars Observed with High Angular Resolution . ... Observing Facilities . ... Observing with ESO Telescopes . ... The goal of this workshop is to review recent results on solar-mass stars obtained with infrared and millimeter interferometers, and to discuss their importance for our understanding of stellar evolution from star formation to stellar end products. ...

... 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: . ...

... 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. ...

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Next: NICMOS/HST H-band (F160W) Images Up: NICMOS Science Previous: HST NICMOS Observations of . ... Observations of P . ... The NICMOS team has devised a comprehensive program of observations of the Galactic Center. ... Data in hand give a first look at variability and a detailed look at the search for the tip of the main sequence will be discussed where NICMOS has demonstrated adequate sensitivity and photometric precision to identify likely O8-B1 stars at the Galactic Center. ...