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This is an incomplete list of problems people have had while observing (actually it's a list of problems i've worked on and got around to documenting). 12dec05: 9 level wapp pulsar folding is doing the 9 level correction incorrectly. 17apr05 sband bistatic radar run had pointing problems. 31jan05: single Pol/channel setups for spectral line wapp observing only provides 1 polarization. 02aug04: ripples in lbw around 1390,1400 Mhz. seen a1861(may04), p1914(aug04) . ...

... A similar level of effort is anticipated for HDF-S. We are maintaining a `clearinghouse' for supporting and follow-up observations of the HDF-S. Test observations of the HDF-S field were obtained in October, 1997. ... Simultaneous, parallel observations were made with the three HST instruments STIS, WFPC2 and NICMOS of separate, neighboring fields. ... Additional flanking field observations were made surrounding the deep STIS, WFPC2 and NICMOS fields. ... The red field is the main HDF-S WFPC2 field....

... ATNF Home . About ATNF . ... About ATNF overview . ... Australia Telescope Steering Committee . ... Australia Telescope User Committee . ... Murchison Radio-astronomy Observatory . ... Parkes radio telescope . Australia Telescope Compact Array . Mopra radio telescope . ... Australia Telescope Online Archive (ATOA) . ... Spectrum management . Spectrum management overview . ... CSIRO ATNF Data Archives . ... Visiting Parkes radio telescope . ... Parkes radio telescope webcam . ...

... Exposure Time Calculator (ETC) . ... ESO - Public Surveys . ... the recommended values to use for DIT, . ... Detector on-chip integration (DIT): seconds. to your chosen value - a separate page gives recommended values to use for DIT - for modes 1 and 2 below you may wish to start with the maximum recommended values as these will minimize the effect of read noise (a total object exposure of Y secs with DIT=X secs will produce Y/X lots of read noise) and give you a lower limit on the time needed. ...

... The file contains median maps, noise maps and an offset correction table used in low energy noise reduction of the PN. ... NOISE_MAP_INDEX . An index which gives the name of the extension containing the correct noise map for a given mode, ccd and rawx value. Attributes: . ... The noise map for ccd nn and mode mm, consisting of a single image. ... The median map for ccd nn and mode mm, consisting of a single image. ... Master offset map for ccd nn and mode mm, consisting of a single image. ...

... The first step to improve the FORS calibration is therefore to obtain data to allow a computation of the illumination correction across the field. ... Another limitation on the calibration accuracy has been the brightness of the Landolt standards which have forced the use of extremely short exposures introducing small but non-negligible shutter-time errors and also resulting in a very small number of useful standards per frame. ...

The problem of solar wind data correlation for the observations onboard several spacecraft is very important for three points of view: . ... This problem is studied now in detail by systematic determination of ion flux and ion velocity data correlations by INTERBALL-1 (IKI group), WIND and IMP 8 (both - MIT group). ... Solar wind plasma correlation lengths from IMP 8, WIND and INTERBALL-1. ... Correlation of solar wind observations onboard several spacecraft: INTERBALL-1, IMP 8 and WIND data. ...

... They are concerned with Attitude Control System of the spacecraft, satellite visibility from tracking stations, limits on the satellite autonomous operations during the orbit, and needs for auxiliary operations with the spacecraft. ... Among the operational constraints the most important one is the number of programmed slews per orbit, which determines the maximum number of radio sources to be observed during one orbit. ... System temperature (K) . ... Progress of the RadioAstron Project in Pictures...

Text of these problems is available also in other languages : . ... What can one see in the Moon's sky more often - the Sun or the Earth? ... There are about of 250 millions of stars in the elliptical galaxy M32 (a satellite of Andromeda galaxy). ... The masses of Capella's components. ... You are proposed to estimate the masses of Capella's components, using our observational data. ... A galaxy's mass. ... Estimate the mass of FGC 1908 and compare it to the mass of our galaxy. ...

... The results are used in quasireal time by the observing process, but also as input by hardware quality control, by the dynamical scheduler, and by the Science Pipeline. Among processing operations are the calibration of the atmospheric absorption, of phase radiometric correction, of pointing scans, of phase and amplitude reference measurements, .. ... Using the last few measurements, we will determine a provisional amplitude calibration curve (to be also used by the Quick Look pipeline). ...

... The following charts/text are intended as tools for monitoring the Type Ia supernovae ( SNe ) event visually or photographically (utilizing telescope equipped CCD equipment).The files include: A replication of The Type Ia SNe , V- magnitude (with data point checks from other cited references)and color index (B-V) templete (to indicate a general color-related trend of the type Ia ... I believe this might help alleviate some of the problems involving the making of acceptable amateur light curves...

... Most imaging systems contain intrinsic geometric distortions. Although they can often be disregarded for small field corrections they must be applied when image tubes or dispersive elements (e.g. in spectrographs) are used. ... A wavelength transformation for an image tube spectrum is shown in Figure where both resulting spectra with and without flux correction are given. ... The spectrum rebinned to wavelength is shown with (B1) and without the Jacobian determinant correction (B2). ...

... The choice of the spectrograph design (Fig.2) is determined by the quantity R, the overall dimensions of the PF cage and the restrictions on the rigidity of the structure of the device. ... As the camera's objective a fast 4-lens aplanat is used having a focal distance F cam =140 mm and a relative aperture of 1:1.8, the resolution at the centre is no less than 80 gr/mm, that over the field at a distance of 3 mm from the edge along the frame ( ) diagonal is 35 gr/mm. ...

... 2.3 Establishing the Extragalactic Distance Scale . ... 2.3.2 The Second Rung: Distances to stellar clusters . ... 2.3.4 Distances to Local Group Galaxies . ... The Luminosity Function of Planetary Nebulae . ... 3.2.2 Clusters of Galaxies . ... 4.2 Evidence for Dark Matter as a Function of Scale Size . ... 4.3 Other Dark Matter Indicators for Galaxies . ... What is the nature of the large-scale distribution of matter in the universe as traced by the three-dimensional galaxy distribution? ...

... Posts tagged ?change point problem? ... X-ray summer school is on going. ... Tags: ARCH , Bayesian Block , challenges , change point problem , GARCH , light curves , summer school , X-ray . ... 4 Comments . ... 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 . ...

... Astrophysics Group . ... VSA . ... CAT . ... The Very Small Array is a custom-built radio telescope (operating between 26-36 GHz), designed expressly to make high resolution observations of the cosmic microwave background (CMB) radiation on angular scales around and below one degree. ... The VSA has been operated in ?compact array? and ?extended array? configurations (see the technical description below) and data collected to achieve high sensitivity in both regimes have been analysed. ... 1.75 GHz)...

... Observing . ... The double star 54 Leonis, spiral galaxy NGC 3198, and emission nebula NGC 3199 . ... Problems posed by massive stars . ... These questions were at least part of the motivation when CУЕssio Barbosa of Brazil's University of SУ?o Paulo and Donald Figer of the Space Telescope Science Institute in Baltimore surveyed observers and theorists to see what they believed were the most pressing problems concerning massive stars. ... Get instant access to subscriber content on Astronomy.com! ...

... If you came here by a notice of this URL in some newsgroup article: Here is the toplevel of the XFree86/OS2 pages . ... The following is the list of recent file dates and sizes from the main archive at ftp.xfree86.org/pub/XFree86/3.3/binaries/OS2. ... Filelist of XFree86-3.3 The following link(s) refers to bugs known to be present in older releases. ... Double check that you really have the hardware which was sold to you We have found one case where Superprobe was right, and the dealer was lying. ...

... The J, H and K bands are characterized by a bright background, such a background is mainly due to the emission of atmospheric lines and of thermal radiation. ... If the source cover a large fraction of the slit, spectra off-source must be observed to adequately sample the sky background. ... The on chip integration time (time spent in each position of the slit) must not exceed 40 seconds in J and H bands and 60 seconds in K band. ... We suggest a sequence of 10 for each elementary integration time. ...