Science Observatory Branch Report SOB-93-12-06 A determination of the pointing history during FOS scans of Mars Colin Cox and Matt Lallo December 1993 We have used pointing software, developed earlier for a comparison with the PASS software, to analyze scans of Mars performed at intervals since June 1992. ... For these sets of data the V2 V3 positions are those of the Faint Object Spectrograph's paired apertures as recorded in the Science Instrument Aperture File in the Project Data Base. ...

... This task operates on event data in an event list. ... In the first two cases, the celestial coordinates of the reference point are taken respectively as the values of the RA_NOM , DEC_NOM or RA_OBJ , DEC_OBJ values in the input event file header. ... Although the OM attitude information may be more accurate, it will not be present throughout part of the observation, and as such, the default source for the attitude data should be "ahf". ...

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... The alfa rotation angle was set to 0 degrees. ... Beam 0 was sampled more often than the others to get a better measure of the pointing offsets. ... Page 5: Pointing error. beam 2 had large za errors. ... Compute the change in the pointing error if the alfa rotation error was off by -5 to +5 degrees in .1 degree steps. ... Top: rms pointing error vs rotation angle offset. ... Red: Az rms pointing error . ... rotating by + 1.1 degrees reduces the non beam 0 rms from 13 to 12 asecs. rms Error asecs . ...

... Restrictions ) are used. If specified form of output is EMP then astrometric equatorial coordinates are printed in the form usual for Ephemerides of Minor Planets, with formal precision of 0.01 minute of time in R.A. and 0.1 minute of arc in declination. ... It should be noted that the near-opposition ephemerides are not calculated for bodies/ points with numbers from –12 to 0 (in case they are included into task for computation of such ephemerides only their names are displayed in the results). ...

... The ROSAT Consortium (the Max-Planck-Institut fuer extraterrestrische Physik, the Goddard Space Flight Center, the Smithsonian Astrophysical Observatory, Leicester University, and the Astrophysikalisches Institut Potsdam) announces the release of the completed source catalogs of all ROSAT pointed observations. ... Detailed information about the catalog and methods of access to the catalog and data products can be obtained from the ROSAT Results Archive web pages in Germany, in the US, and in the UK:...

Next: First Catalog Sources Up: The Second EGRET Catalog Previous: Catalog Construction . ... For each observation with 3, the excess is presented as a flux with its uncertainty. ... For all except the brightest sources or those in confused regions, the statistical uncertainty is larger than any systematic uncertainties. ... The primary catalog is Table 4. ... Other names -- the source name from the first EGRET catalog ([ Fichtel et al. 1994b ]) or other gamma-ray references. ...

... Two algorithms have been used to simultaneously solve for the sky, gain, and offset for simulated sets of dithered images. ... When solving for sky and gain, achieves machine precision on noiseless data; for noisy data, solution within noise. ... When solving for sky and gain, achieves machine precision on noiseless data; for noisy data, solution slightly different from Fixsen-Arendt solution, but within noise. ... Figure 2: MIPS truth image, and full MIPS dither pattern . ...

... This program was created for correlating chosen regions in the series of fts images. ... Chosen regions' . ... In this section the program counts the integral for each region of the grid for each image. ... As a matter of fact, the integral is total brightness of the region and it is counted by 'int_tabulated' IDL function. ... In addition, the program will show the count of the regions which correlate with the corresponding region (the brighter region means the bigger count) and its contour. ...

Program: HIFLUX Purpose: derive fluxes and standard deviations from HIRAS images File: hiflux.src Category: IRAS Author: Do Kester Keywords: *** MAPS= Max number of maps to be processed simultaneously [4] All maps should be of the same size, and presumably of the same field. ... COLIND= Color index for plot colours [standard] *** LOCAL= Calculate local background [No] The background is determined as the median of the points within the form selected with SELECT=. ... But see also RADIUS=). ...

IRAF cl script to demonstrate the routines in the imaging polarimetry package # impol for WFPC2 # # Author; J. R. Walsh, ST-ECF. jwalsh@eso.org # # REQUIREMENTS: # An image display tool should be active. ... Create table of reflection nebula parameters from ascii file # ! ... Simply take # this as a fractional value of the linear polarization image # imarith operand1="reflneb1po.fits" op=* operand2=1.0E-4 result="reflneb1cir.fits" # # Form the set of input images for the positions of the polarizer. ...

... Impact of Covariance Information on the Orientation Parameters Between Radio Source Position Catalogs, IVS 2012 General Meeting Proceedings, p.339­341 http://ivscc.gsfc.nasa.gov/publications/gm2012/sokolova.pdf Impact of Covariance Information on the Orientation Parameters Between Radio Source ... IVS Analysis Centers provide these catalogs in a standard IERS format, where together with radio source positions and other relevant information, RA/DE correlations are reported. ...

... In polar coordinates, the point P is defined by its distance r from the origin O (see drawing) and by its polar angle ("azimuth" on a map) between the x-axis and the "radius" r = OA, measured counter-clockwise. ... When one or both are negative , the angle f is larger than 90 degrees, and such angles never appears in any right-angled triangle. ... There is a simple solution , though: use the above equations to re-define sin f and cos f for such larger angles! ... But it also works for larger angles....

Next: Discussion Up: Old neutron star distribution Previous: Galactic potential . It proves to be teachful to have a look at the calculated distribution (Fig. ... The galactic z -distribution of stars and peculiar velocities slightly smear out this narrow boundary. ... The final picture (Fig. ) of the old neutron star density distribution is obviously the sum of filled equipotential lobes with different weighted with the probability shown in the Fig. ...

... Positions in 2000 - Jan - Feb - Mar - Apr - May - Jun - Jul - Aug - Sep - Oct - Nov - Dec . Positions in 2001 - Jan - Feb - Mar - Apr - May - Jun - Jul - Aug - Sep - Oct - Nov - Dec . Positions in 2002 - Jan - Feb - Mar - Apr - May - Jun - Jul - Aug - Sep - Oct - Nov - Dec . Positions in 2003 - Jan - Feb - Mar - Apr - May - Jun - Jul - Aug - Sep - Oct - Nov - Dec . Positions in 2004 - Jan - Feb - Mar - Apr - May - Jun - Jul - Aug - Sep - Oct - Nov - Dec . ...

The beam pattern and the polarization characteristics . of the radio telescope RATAN-600 . The Mueller matrix elements was computed via formulas [1]: . ... The BP were computed by the aperture method, proceeding from the fild distribution in the aperture of the primary mirror. The components of the main and cross-polarization components of the electric field in the vertical aperture of the primary mirror was computed in Frenel diffraction approximation. ...

... astro-ph . ... We present the goals and preliminary results of an unbiased, near-infrared, narrow-band imaging survey of the First Galactic Quadrant (10deg<l<65deg ; -1.3deg<b<+1.3deg). ... 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 longitudes. ...

... sin f = y / r . cos f = x / r . ... They are now viewed as new definitions of the sine and cosine, for the polar angle f given by x and y ( a slightly different way of formulating this definition is described further below ). ... sin 2 f + cos 2 f = 1 . ... Angle . ... Many trigonometry texts define the sine and cosine slightly differently, using the so-called unit circle . ... Then the distance AB ("the sine line") equals sin a , and the distance OA ("the cosine line") equals cos a . ...

... The perceptron structure, on the basis of which the database is built, is defined by a number of the input and output parameters and a required accuracy. ... The output perceptron data are the expansion coefficients of the scattering matrix elements in series of the generalized spherical functions. ... As the cluster structure depends on the generation conditions the expansion coefficients were averaged over 5--7 realizations of the clusters (for N . ... is the coefficient number. ...

APAO is a relatively new Olympiad which was founded in the spring 2005 as an international regional programme in line with the International Astronomy Olympiad. The 8 th Asian-Pacific Astronomy Olympiad (VIII APAO) took place in November-December 2012 in town of Cox's Bazar ( South-East part of Bangladesh ). The Olympiad organized by Bangladesh Astronomical Association . ... Theoretical round, problems 1-6, group a : English , Russian . ... For the best result in all the rounds . ...