Discussions about the observing strategy for the HDF-S focussed primarily on the questions: . What filters/gratings to use for each instrument ? What exposure time to use for each filter/grating ? ... Different areas of the Version 1 output image correspond to variable amounts of exposure time, due to the relatively large pointing shifts necessitated by the multi-instrument observing strategy. ... WFPC-2 Filters, exposure times and limiting AB magnitudes for Version 1 images . Filter . ...

... 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. ...

... Calculated exposure times do not take into account instrument and telescope overheads. ... The exposure time calculator consists of two pages. ... An instrument description for HAWK-I is available on the instrument page . ... begin{equation} \mathit{FWHM}_{\text{IQ}} = \sqrt{\mathit{FWHM}_{\text{atm}}^2(\mathit{s},x,\lambda)+\mathit{FWHM}_{\text{tel}}^2(\mathit{D},\lambda)+\mathit{FWHM}_{\text{ins}}^2(\lambda)} \end{equation} } \) . ... F_{\text{Kolb}} = \frac {1}{1+300 {\text{ }} D/L_{0}}-1$$ . ...

... NICS will be the only infrared instrument for the first light of the TNG; as a consequence, we decided to incorporate a sufficient degree of operation flexibility by providing the instrument with six different observing modes, three aimed at imaging and three at spectroscopy: . ... It will be possible to use the narrow band filters as order sorters; this will allow to perform high resolution long-slit spectroscopy in the wavelength ranges covered by the available narrow band filters. ...

... Second, the observatory can control the configuration, test data analysis procedures, and provide calibration solutions with the help of instrument models. This paper presents the VLT object-oriented framework for the development of ETCs (Exposure Time Calculators) and data simulators. ... Instrument simulations are being developed for the purpose of predictive calibration, instrument configuration control, and evaluation of data analysis procedures. ...

... Parameter . ... Type . ... data set . ... The name of the observation-wide attitude time series data set created by atthkgen . ... name of existing D -type column in attset . The name of the column in the attitude data set containing the time tags - passed to tabgtigen in parameter timecolumn . ... A selection switch which determines the type of selection expression that the attitude time series is filtered with. cone and pyramid select the fixed cone- and pyramid filters (see above) respectively. ...

... 11 Yellow-Green (78% transmission): Contrasts well with the red and blue characteristics of surface features on Jupiter and Saturn. ... 82A Light Blue (73% transmission): Useful on the Moon, Mars, Jupiter, and Saturn, this subtle pale blue filter enhances areas of low contrast while avoiding significant reduction of overall image brightness. ... Meade Series 4000 Photo-Visual Color Filters may be ordered individually or in the following sets: . ... Meade Series 4000 Broadband Nebular Filters . ...

Contact Russet McMillan (primary) or your Observing Specialists (secondary) for additional information. Contact Jack Dembicky for web page errors, corrections, ommisions, or additions. This page last updated: July 6, 2004 - JMD . This page last checked: September 14, 2003 - JMD . Configuring TUI to use the Echelle . Setting up the Echelle exposure parameters . Taking your Calibration lamps . ... Setting up multiple exposures . ... Stopping an exposure (discarding data) . ...

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. ...

... Finally, the individual observations themselves are reduced, using the parameters from the extinction solution. ... That is, the extinction solution can in principle produce results if we observe extinction star 1 only in passband A and star 2 in passband B on night 1, and star 1 only in passband B and star 2 in passband A on night 2. ... Even if the passbands are linked by color terms in the extinction, the solution is possible, because we do obtain mean colors for each star. ...

Next: RECEIVER CHOICE Up: Spectral-Line Observing at AO Previous: Spectral-Line Observing at AO . ... This involves deciding which receiver you wish to use, the observing procedure and parameters you wish to employ, what frequency range and set-up for the correlator boards you want, integration length, any equipment you may need to deal with RFI (filters, radar blankers, etc.), etc. ... These files are automatically saved into your project area on the ``observer'' computer. ...

... The Miriad task uvgen can be used to simulate a variety of observing modes. ... Simulating a telescope approximately, let alone in some detail, requires a good many parameters. uvgen takes an appreciable number of parameters and input files to describe the telescope, correlator and source. Fortunately keyword and set-up files for some common situations exist ( e.g. simulating the ATCA and VLA). ... For example, to load typical parameters for the ATCA, use miriad% source $MIRCAT/uvgen.def.atca . ...

... Parameters . Filters . ... Direct images . ... The SCORPIO-2 project: . Spectral Camera with Optical Reducer for Photometric and Interferometric Observations - 2 . The broad-band glass filters made in SAO RAS are used for the observation in the Johnson-Cousins (UBVRI) photometric system in the direct images mode. The glass filters transmission curves are shown by solid line. ... The filters transmission curves of the `comets' filters measured with the SCORPIO-2 in the F/4 beam. ...

Next: AXAF Recipes Up: ROSAT HRI Recipes Previous: Quantum Efficiency Correction (a.k.a. For some observations, a significant amount of data may have been rejected during SASS processing because the background level was higher than the calculated threshold for rejection. ... REJECTED EVENTS . ... The recipe will allow the user to include rejected events in the generation of a new qpoe file and filter on the background level. ... This creates a qpoe file with standard + rejected events. ...

... commands . ... data_spectrum <name> : data in "spectrum" format . ... Repeat command to add additional mask regions. sigma is the s.d. to apply to the data within the region to be masked. ... Repeat command to add additiona continuum regions. ... cont_reg_clear : Clear current continuum regions . ... The observed spectrum is then multipled by this filter to obtain a new spectrum for use by SFIT. cont_sigma : Computes standard deviation of data in continuum regions and applies it to current data . ...

Next: NICMOS/HST H-band (F160W) Images Up: NICMOS Science Previous: HST NICMOS Observations of . ... Observations of P . ... The NICMOS team has devised a comprehensive program of observations of the Galactic Center. ... Data in hand give a first look at variability and a detailed look at the search for the tip of the main sequence will be discussed where NICMOS has demonstrated adequate sensitivity and photometric precision to identify likely O8-B1 stars at the Galactic Center. ...

Static Fourier spectrometers are often used for spectral measurements of the ionosphere emissions. There are two main advantages of Fourier spectrometers (FS) - large geometric factor and high spectral resolution; these parameters are two orders better than for grating spectral instruments. ... In scanning Fourier spectrometer optical and electric modulation of signal is used to avoid this problem, for static Fourier spectrometer there are no such ways. ...

RTT150 . ... This search system is designed for generating the necessary information on series of pointings (observations of each source consist of sets of exposures with different filters and sometimes with different exposure times) for observed sources. Search results appear at the separate page as a table with the following data: . DATE - real (not evening!) observations date (in YYYY-MM-DD format); . ... Bin - minimal CCD binning mode (may vary during the observations); . ...

Next: Star Formation Rate and Up: No Title Previous: Calculation of Evolutionary Tracks . To start calculations, we choose the distributions of the initial binary parameters: the mass of the primary ZAMS component, , binary mass ratio, , orbital separation a . ... whereas the mass ratio distribution is not. ... The zero assumption often made is that the mass ratio distribution has a flat shape, that is binaries with a high mass ratio occur as frequently as those with equal masses. ...

... 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...