Polarization the Central Calibration of Pixel of ALFA Hands-on Project AO-6 Outline Motivation Observational Setup Calibration Data Analysis Results Future W ork 1 M o ti v a ti o n Determine the flux and % polarization of 3C286 Determine instrumental polarization of ALFA beam zero without assumi ng source parameters Characterize i nstrumental polarization so that it can be removed i n future ...

... The analysis of NICMOS polarization images is aimed at determining the Stokes' Parameters, and from those the polarization angle and degree for each pixel. NICMOS Camera 1 and Camera 2 each contain three polarizers, whose principal axes of transmission are separated by 120 degrees. ... The images in the three filters need to be compared, in order to produce the Stokes' parameters. ... The Stokes parameters can then be combined to yield the polarized intensity, I p: . ...

... Previous: Pipeline Processing and Quality Control for Echelle Data . ... On-the-fly re-calibration of HST data (OTF) has now been available at the CADC and ST-ECF for about 18 months. ... The calibration can only be executed using the calibration reference files which are available at that time. ... On-the-fly re-calibration has another advantage for our archive sites: we only need to keep the raw data and calibration reference files on-line for the process to be automatic. ...

... The miriad Front-End . ... Miriad Datasets . ... Inside Datasets . Scratch Files . Miriad Data Disks at Epping . Visibility Data Concepts . Miriad Visibility File Format . Miriad 's Calibration Model . ... Selecting UV Data in Miriad . Spectral Window Selection . ... Image Data Concepts . Image Datasets . ... Getting Data In and Out of Miriad . ... Reading Visibility FITS Files . ... Writing Visibility FITS Files . ... Flagging, Manipulating and Examining Visibility Data . ...

... Based on the measurements of the Stokes parameters in the continuum and in the broad 0.6563 nm hydrogen emission line obtained with the 6-m telescope for the Seyfert galaxy Mkn 6, secular variability of the hydrogen line profile polarization was discovered; a time lag of less than 2 days between the continuum flux and the polarized continuum emission was determined which corresponds to the size of the region where the polarization of the continuum occurs, less than 0.001 pc. ...

... The Earth orientation parameters UT1 and polar motion (x pol ; y pol ) are relat­ ed with the values of UT0 and VOL obtained from the LLR analysis for a station with geocentric longitude and latitude (–; OE) by the following expression: 7 UT0 \Gamma UTC = UT1 \Gamma UTC + (x pol sin – + y pol cos –) tan OE 15 V OL = x pol cos – \Gamma y pol sin – At least four normal points for each station--reflector pair at one day were accepted for the diurnal UT0 estimations. ...

Peremennye Zvezdy ( Variable Stars ) 32 , No. ... We report on a new episode of decretion disk formation in the IGR J06074+2205 system. ... From a study of three HeI lines, the rotational velocity of the star was determined as km/s. After five years of spectroscopic monitoring of IGR J06074+2205 (Reig et al. 2010), a reversion from emission to absorption of the H line and hence disappearance of the equatorial disk was reported. ... Reig P., 2011, Astrophys.& ...

... Here we address the issue of how to determine what calibration files make up the current calibration file for a given observation time. Each calibration file has a validity start date and a validity end date. ... In the simplest case (no end of validity date), a new version of the calibration file -- call it , will have and (figure 1 ). ... Within this scheme, at any time the applicable issue of the calibration file is obtained by selecting among all files the one with the higher issue number. ...

Next: Primary Catalog Up: Observations and Analysis Previous: Source Positions . ... This energy selection allows direct comparison with previous EGRET, COS-B and SAS-2 results. ... The energy spectra shown in the catalog are taken largely from previous EGRET publications (or those currently in the publication process), which discuss the details of source identifications, time variability, and energy spectra. ... Such sources are identified in the catalog. ...

The close position of main satellite and subsatellite (distance between them about 1000 km) and using the similar sets of Faraday cups (VDP and VDP-S) with high resolution measurements (up to 16 Hz for the main satellite and up to 10 Hz for the subsatellite) allow us to determine the small-scale variations of the magnetopause shape and position and to estimate the velocity of the magnetopause motion. ... Two point observation of the magnetopause motion: the INTERBALL project. ...

... Determining the nominal roll angle for stable intervals . ... We found the necessary information in a file 'rh*.ao', which has a binary extension table for each obi. ... Unlike the question of determining the nominal roll angle, we know of no a priori indication of this problem (although the guide star configuration may be the cause, or at least associated with this condition): it is necessary to examine the source position for each obi. ... The guide star record is at the end of the 'anc file'. ...

The VLTI Calibrator Selector Tool is a tool intended to assist in the selection of suitable interferometric calibrators for VLTI observations with MIDI and AMBER. It uses a model of the VLTI and its instruments to assess the fringe visibility, given the observed bandpass, the geometry, spectrum, and coordinates of the target and the time at which the observations are to be made. ... The tool offers an HTML/Java based interface and consists of two pages. ... The quality flag depends on LDD_chi2. ...

For solar wind dials without any explanatory text, see this page . ... There are three logs, one for each condition index ( K P , Solar Wind ,and NOAA/SEC .) ... More about the solar wind's recent behavior can be found on my Current Solar Wind Conditions page. ... Other items of interest include NOAA/SEC Current Conditions , my composite current Auroral Images page, Windows on the Universe: Space Weather , and Public Outreach Index, Department of Space Physics and Astronomy, Rice University . ...

... Aloisi, A. The Old Stellar Population . Alonso-Herrero, A. HST /NICMOS Observations of the . ... Balcells, M. HST-NICMOS Observations of Galactic . ... Baum, S.A. Investigating the Evolution of . ... Becklin, E.E. A Coronagraphic Search for . ... Clampin, M. The Old Stellar Population . ... Close, L. HST NICMOS Observations of . ... The Stellar Population in . Geballe, T.R. HST NICMOS Observations of . ... Greggio, L. The Old Stellar Population . ... Leitherer, C. The Old Stellar Population . ...

... Field of interest: data analysis and interpretation of X-ray observations of BHC and NS systems, astrophysics of compact objects and related phenomena: X-ray , optical and radio observations , shocks and stellar winds, emission mechanism, the spectral and timing analysis of the X-ray emission from microquasars ( signature of accreting BH), atoll- and Z-sources ( signature of accreting NS), modeling of INTEGRAL images % . ...

SN 1989B Light Curve Analysis. ... In the light curve depicting their observations, definite trends are noted, here is a "thumb-nail" analysis of the the magnitude estimations of the bright SN (1989B) in the galaxy NGC 3627 (M66). ... The observations were inserted against the V magnitude templete of BL, CCD photometric data, (Wells et. al, (1994) and a color trend (B-V) histogram of the mean type Ia SN (BL)(nutemp.gif). Key Words: Amateur Observations, Supernova, Magnitude Estimates, 1989B . ...

... Old World First Asteroid Radar Echo. ... It testifies that 4179 Toutatis is a double object like asteroid 4769 Castalia. ... Interference of Radar Echo from the Binary Asteroid 4179 Toutatis. ... An analysis of the 6-cm radar data revealed quasi-harmonic oscillation of the echo’s “central” Doppler frequency with a period of about 14 sec and a deviation of about (0.7*B) Hz, where B is the echo bandwidth, which for 4179 Toutatis was equal to 2.1 Hz and 1.9 Hz for 1992 Dec 8 and 9, respectively. ...

... PUL VLBI Analysis Center . ... Pulkovo EOP and Reference Systems Analysis Center (PERSAC) is located at the Pulkovo Observatory . ... Processing of VLBI , GPS, and optical observations aimed at analysis of the Earth rotation, station displacement, and celestial reference system. ... Celestial Pole Offset (CPO) and Free Core Nutation (FCN) . Four daily updated CPO and FCN series (models) are provided. ... File fcn1.dat contains the ZM1 FCN model with variable amplitude and phase. ...

... Primordial theory review : Dick Bond . Defects and the CMB review : Andy Albrecht . ... Gravitational wave contribution to CMB anisotropies : V.B. Lukash and E.V. Mikheeva . C_l from cosmic strings : Lloyd Knox . Some aspects of CMB anisotropies induced from topological defects : Mairi Sakellariadou . ... CMB anisotropies from scaling sources : Ruth Durrer . ... SZ observations I : Sarah Church . ... Holes in the microwave sky? ... Detecting cosmic strings in the CMB : James Robinson . ...

... We present an analysis of an optical blue spectrum of the pulsating helium star V652 Her (=BD+13 3224$) in order to determine its effective temperature, surface gravity and chemical composition. ... The surface composition is characterised by abundances of nH=0.009, He=0.988, nC~0.000040, nN=0.0025 and nO=0.00010 (number fractions). ... If V652 Her was formed by the merger of two white dwarfs, its surface composition demands that they should both be helium white dwarfs. ...