Next: HST Science: Structure Up: Scientific Results from Deconvolved Previous: Introduction . A major question in the minds of most astronomical users was discussed by Ivan King at this workshop - the issue of validation of the output from deconvolution. ... Fig. 1 shows an example of cross-validation, using data taken from Keel (1993). The image is of the faint radio galaxy 53W044 at redshift . ... For galaxies with smooth, symmetric structure, modelling allows an independent comparison. ...

... GCN 8471 | ... TITLE: GCN CIRCULAR NUMBER: 8516 SUBJECT: GRB 081102: MASTER refind and final results DATE: 08/11/11 15:50:10 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina, D.Kuvshinov, P.Balanutsa Sternberg Astronomical Institute, Moscow State University A. Tlatov, A.Parkhomenko Kislovodsk Solar Station of the Pulkovo Observatory V.Krushinski, I.Zalognikh Ural State GCN Circ 8470, Lipunov et al., ...

... Apache HTTP Server Version 2.2 . Apache > HTTP Server > Documentation > Version 2.2 . ... This document explains some of the directives provided by the core server which are used to configure the basic operations of the server. ... Related Modules . ... The ServerAdmin and ServerTokens directives control what information about the server will be presented in server-generated documents such as error messages. ... The ThreadStackSize directive is used with some platforms to control the stack size. ...

Hide Zen home . ... GIN . ... contains: value_array @> query_array . ... An example for a Gin opclass can be found in ginarayproc.c. Datum * extractValue( Datum inputValue, uint32* nentries) Returns an array of Datum of entries of the value to be indexed. nentries should contain the number of returned entries . int compareEntry( Datum a, Datum b) Compares two entries (not the indexing values) Datum * extractQuery( Datum query , uint32* nentries, StrategyNumber n) Returns an ...

... Bojan Nikolic web pages (r. 329) . ... Using high-resolution three-dimensional realisations of turbulent fields, we investigate the limits on achievable performance of atmospheric phase correction using water-vapour radiometers arising from following effects: the incoherent measurement of power from water by the radiometers (in contrast to coherent detection of the astronomical signal); the different tapers of the response patterns of the astronomical and radiometer receivers; and, the ...

... Posts tagged ?central limit theorem? ... Tags: Bayesian , central limit theorem , confidence bounds , error bar , Frequentist , highest posterior density , HPD , likelihoodist , sigma . ... 3 Comments . ... Entries RSS . ... Algorithms arXiv Astro Bad AstroStat Bayesian CHASC Cross-Cultural Data Processing Fitting Frequentist Galaxies gamma-ray High-Energy Imaging Jargon Job Languages MC MCMC Meta Methods Misc News Nuggets Objects Optical Physics Quotes Spectral Stars Stat Timing Uncertainty X-ray ....

Next: Acknowledgements Up: World Wide Web version Previous: Page contents . ... Part of the table and a cartoon figure of the track calculated for the default set of the initial parameters are shown in Fig. 1 and 2. In the future, we intend to made available calculations of a large number of binary systems assuming different intial distributions, chemical composition, etc., to construct a "Galaxy at will", as well as various interface facilities. ... Fri Jun 21 19:17:07 MSD 1996 ...

Comment on the International Jubilee Symposium . ... The usefulness of the Internet as a method of holding international meetings without the expense of travel is also clear, but this new medium is not yet well established in this role. ... How can we move on with international cooperation in the World Wide Web era? I would like to suggest that NASA's Planetary Data System is a good model. ... At the same time, much might be done with older images, by scanning prints to create new digital files. ...

... Archive 2003: . As a result of development of image slicers, polarization analyzers and reduction technique, the limiting magnitude of spectral observations at BTA with high spectral resolution (up to R=80000) has been increased by 3 times, the limiting magnitude of spectropolarimetric observations increased from 3 to 8 times (in the red and UV ranges, respectively). ... Archive . ...

... ATNF Home . ... About ATNF overview . ... Australia Telescope Steering Committee . ... Australia Telescope User Committee . ... Astrophysics graduate student programs . ... Australian Square Kilometre Array Pathfinder . Murchison Radio-astronomy Observatory . ... Parkes radio telescope . Australia Telescope Compact Array . Mopra radio telescope . ... ATCA . ... Visiting Parkes radio telescope . Visiting Australia Telescope Compact Array . ... Parkes radio telescope webcam . ...

... 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. ...

... V.G. Kurt, V.V. Sokolov, S.V. Zharikov, G.G. Pavlov, B.V. Komberg: "BVRI observations of PSR0656+14 with the 6-meter telescope" (astro-ph/9706076), 1998, A&A, 333, 547 . ... A. Shibanov, A. B. Koptsevich, V.V. Sokolov, S.V. Zharikov, G.G. Pavlov, V.G. Kurt, V.N. Komarova: "Optical photometry of the PSR B0656+14 and its neigbourhood", 2000, Abstracts of JENAM-2001, 99 . ... A. Shibanov, V.V. Sokolov, V.G. Kurt: "Optical photometry of PSR B0656+14 and its neigbourhood", 2001, A&A, 370 , 1004 . ...

... Limit of star magnitude. If you want to obtain best results, you should use reference stars not more dimly than limiting star magnitude of your telescope. Limiting star magnitude depends on time of an exposition also.) This value should be set as " maximum of star magnitude " in a dialog box " Extraction from catalogue". To find darkest stars in the frame, make the following: . ... Two star magnitudes (m1, m2 in two photometric systems) will be outputted in the window "Information". ...

... In this activity, students will observe that the faintest stars which they can see in the sky are affected by many things: the adaptation of their eyes to the dark, the presence of clouds or haze, the time of year, and the presence of light pollution. General Information . ... After completing this activity, students should have a better understanding of the practical processes for dealing with the light pollution problem and with other environmental and societal issues. << previous page | ...

Next: HIMF Up: Minutes of the 1st Previous: HIPASS . ... HIDEEP is a deep, blind survey with Parkes over a small patch of sky. ... 9000 sec per beam . ... HIDEEP optical follow up: . ... HIDEEP galaxy properties: . ... HI column densities: . ... To figure out the actual HIDEEP sensitivity, you have to decide how to derive the limits on the column density when the beam is large (unresolved sources). ... In terms of your column density, you are assuming filled beam and then adopting an optical size. ...

... Meta Index / Home Page / Output Files / Summary File specification from Finally there will be a data quality record for each instrument exposure and one for the spacecraft data. ... Number of telemetry drops . ... Number of OOLs These items will be stored on a per exposure basis for each instrument and on a per observation basis for the spacecraft telemetry. ... Note . ... Comment . ... Number of telemetry packets associated with the instrument/ spacecraft that failed reception during the period. ...

... Accurate identification of physical binary star systems has become of increasing interest in recent years. ... Identification of physical binary star systems, with an estimated reliability of such identifications based on the theory of probability, is also important for current and future efforts to find binary star systems that are candidates for observations with the aim of determining their orbits and component masses. ... probability of the proximity of proper motions and ; . ...

... We have used the VLA to survey the inner Galaxy (|b| < 0.4^o, l=350-40^o) at 5 GHz to a limiting sensitivity of between 2.5 and 10 mJy. ... Zoonematkermani S., Helfand D., Becker R.H., White R.L., Perley R.L. Astrophys. ... 1990) Paper I. Becker R. H., White R. L., McLean B.J., Helfand D.J., Zoonematkermani, S. 1990, Ap. ... Paper II. ... Paper III. ... Paper V. Table 2 contains the complete list of VLA sources within the 5 GHz survey area from both the 5GHz and 1.4 GHz catalogs. ...

DISCLAIMER: The larger the aperture, the more light a telescope will gather and the fainter the object you can see. Here is a range of magnitudes you might expect to see. Given excellent sky conditions and good optics, a well trained eye can sometimes add up to 0.8 magnitude to these values. Limiting Magnitude depends on much more than the instruments aperture. ... One formula is for aperture in inches the other is for aperture in millimeters. ... Aperture (inches) . ... 15.2 . ...

An example of the AKR (Auroral Kilometric Radiation) recorded by the POLRAD radio-spectro-polarimeter. The 3 perpendicular components of the electric field are presented in the range from 4 kHz to 1 MHz , while crossing the morning sector of the auroral region (3.00 - 5.40 MLT) at the altitudes from 14441 to 18392 km. The lower limit of the AKR was at 150 kHz, while the maximum power was received at a typical range from 200 to 400 kHz. ...