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. ...

... Values have been scaled arbitrarily. High ratios are shown in blue, corresponding to blue colors, and low ratios are shown in red, corresponding to red colors. ... Noise combined with background subtraction difficulties in the lower left quadrant of the WISP1 data (see Fig. \ref{Fig:wisp_snr_mskd}) make colors in this area very unreliable. ... The values shown here are typically a factor of ~3 less than those calculated for the Schmidt data, shown in Figure \ref{Fig:bj_alpha}. ...

This is how a typical dispersion modeling result looks when shown as a map. ... Their numerical values are shown at the top. White normally means no data, but high values may be also shown as white if above the fixed high limit (that is, if no automatic normalization is used for colors). Note that calculations were done both for cell positions and for station positions, so both are colored. PO territories are filled by color corresponding to the average value of cells overlaying them. ...

... The file names' construction . The flight (m) stage's file set . ... the orbital data used for the flight operation monthly (m) long-term planning, . ... The orbital calculations are based on the initial orbital data determined by KIAM RAN using the orbital radio- measurement treatment. The determined initial orbital data are presented as a state vector (satellite position and velocity) in the J2000 reference. ... Accept the file with extension '.bgr', where the Moscow time (MT=UT+3h) is used. ...

. XMM-Newton Science Analysis System . imrebin (tools-1.63) [xmmsas_20060628_1801-7.0.0] . Meta Index / Home Page / Description . Three options are available: . newvaluestyle =`sum': the values of the corresponding input pixels are simply added. newvaluestyle =`average': the values of the corresponding input pixels are averaged. newvaluestyle =`rms': the output value is calculated as the root mean square of the cooresponding input pixels. XMM-Newton SOC/SSC -- 2006-06-28

Taking into account the result by Watanabe P=2.5 days in outburst, I reconstruct old set of photographic observations being partly lost, and add some new observations. ... The periodogram calculated with the method by Lafler and Kinman is shown. ... The last periodogram indicates peaks corresponding following possible periods with the double-wave light curve: 0.4236, 0.4650, 0.5379, 0.6064, 0.7365, 0.871, 1.168, 1.5437, 2.8173, and 6.89 days. ...

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. ...

... It is precisely these values that are displayed as O – C. In case computed positions of minor planet for all or some part of moments are found without accounting for perturbations, the corresponding moments are followed by asterisk (without perturbations are computed positions for all minor planets if moments of their observations lie outside the basic interval of 16 months or for ordinary ... The coordinate system and type of computed positions are indicated in status bar. ...

... Categories: calibration, map making SELFCAL is a MIRIAD task to perform self-calibration of visibility data. ... The input to SELCAL are a visibility data file, and model images. ... Key: vis Name of input visibility data file. ... Several models can be given, which can cover different channel ranges and different pointing and sources of the input visibility data. ... NOTE: When you give SELFCAL a model, it will, by default, select the data associated with this model from the visibility data- set. ...

... Armagh Observatory, College Hill, Armagh BT61 9DG, +44 (0)28 3752 2928 . ... First three columns show base-difference images of the evolution of the wave in 3 EUV channels (211 , 193 , 171 ) of AIA in which the wave is clearly visible. ... From our study we have quantitatively confirmed previous results that during wave passage the plasma visible in the Atmospheric Imaging Assembly (AIA) 171 channel is getting heated to higher temperatures corresponding to AIA 193 and 211 channels. ...

My colleagues and I have recently completed a series of observations of SN1999an. ... The telescope is located at Martin Observatory in Blacksburg, VA, and is operated by the Physics Department of Virginia Tech. Our IAU Minor Planet Center Observatory Code is 841. ... Attached you will find a copy of one of our images (in .jpg format) with the supernova indicated. ... Virginia Tech Department of Physics . Back to Bright Supernovae . Back to Supernova 1999an . ...

... Bojan Nikolic web pages (r. 329) . Out-Of-Focus (OOF) Holography . The circle polynomials of Zernike, or Zernike polynomials, are an infinite set of polynomials orthonormal on the unit circle. ... The code used by the OOF system to calculate Zernike polynomials is available under the terms of the GPL. ... The first column in the table shows some of the labels that are used for the Zernike polynomial shown. ... The GBT= label is the label used by the GBT control software. ... Label . ...

The following figures show the behaviour of the efficiency factors Q ext , Q sca , Q abs as well as albedo and asymmetry parameter g for porous particles. ... These optical characteristics are compared with results of Lorenz-Mie calculations for corresponding n -layered spheres. ... factors . Qext(x) . Qsca(x) . ... Qabs (x) . ... albedo (x) . ... Henning, Modelling the optical properties of composite and porous interstellar grains, Astronomy and Astrophysics , 429 , 371-381, 2005. ...

... Basic Observables: Zero-differenced phase and code ionosphere-free combinations of global GNSS network stations, corrected by P1-C1 satellite code biases (cc2noncc), daily observations with 30 seconds sampling rate Sites coordinates : IGb08 reference frame coordinates and velocities Displacements: solid tides, ocean loading, pole tide loading (IERS 2010) Geometric model : Receivers antennas eccentricities, absolute receiver and ...

Next: *upspecrdf, downspecrdf* - Transform Up: Spectral Analysis Previous: *grid_plot* - Plot Results . The conversion of count rate to flux depends on the intrinsic spectrum of the source, so xflux must be used in conjunction with fit . Fit generates a table of the best fit intrinsic spectrum ( _int.tab extension). xflux uses this table to calculate either the integrated flux between two energy limits or the flux density at a specific energy. ... This produces ``..._obs.tab'' file. ...

Next: Beam procedures and functions Up: Introduction Previous: Introduction Contents . A collection of procedures capable of imaging interferometric data. ... In the latter, a model (list of CLEAN components) is built-up incrementally between phase self-calibrations. ... PEARL will work with the complex visibilities, which have to be initialized with the observed visibility and closure phase data using the set_complexvis procedure. ...

Next: MOUNTING= 'GERMAN' Up: MOUNTING= 'FORK' Previous: Column label: OBSW . The values in this column are the corresponding hour angles of the western ``moonlight'' limits, in decimal degrees. A simple sanity check on the tabular data is that the ``moonlight'' limits should always be closer to the horizon (i.e., farther from the meridian) than the ``observing'' limits, at every declination. ... Tue Mar 28 16:52:29 MET DST 1995 ...

Colorful Moon Mosaic . ... Credit Copyright: Noel Carboni Explanation: No single exposure can easily capture faint stars along with the subtle colors of the Moon. ... The fascinating color differences along the lunar surface are real, though highly exaggerated, corresponding to regions with different chemical compositions . And while these color differences are not visible to the eye even with a telescope, moon watchers can still see a dramatic lunar presentation tonight. ...

Next: Identification and Analysis of Binary Star Systems using Probability Theory . ... We present a computing code for modelling energy flux distributions, photometric indices and spectral line profiles of (non-)radially pulsating Main-Sequence stars. ... In the case of slowly rotating stars one can use the zero-rotation approximation to describe stellar pulsations. Such a model was used already by Cugier, Dziembowski & Pamyatnykh (1994) to study nonadiabatic observables of Cephei stars. ...

... The SDSS 2.5-m primary mirror is supported in a manner similar to the Apache Point Observatory 3.5-m telescope primary. ... The axial support is provided by 48 air pistons. The pistons have the same diameter thereby applying equal forces with the same air pressure. ... Each group supports a 120њ sector of the mirror. ... Figure 1: CAD drawing showing the 2.5-m primary mirror and the locations of actuators (green circles) These actuators apply forces (10*cos2 N) to correct astigmatism. ...