... Meta Index / Home Page This task creates a sensitivity map giving point source detection upper limits (vignetting corrected source count rate corresponding to the likelihood of detection as specified in the parameter file) for each image pixel. ... The upper limits are calculated by assuming Poissonian count statistics in each 3 3 pixel detection cell, using the exposure and background values read from the input images. ...

... Correcting ETC Calculations of CCD Spectral Observations for CTE Effects . ... HST Overview . Overview . ... Post-Observation . ... ETC . ... ID: CL Script for Applying CTE Loss to Output of Spectroscopic ETC . ... However, the STIS ETC calculations do not incorporate these CTE effects as yet. ... The output from this script should then be used to calculate the appropriate input flux level for a second run of the ETC, which will then yield output which is corrected for the CTE effect. ...

... The star formation rate (SFR) of the current SF episode can be estimated from the total H luminosity. ... For the derived total flux F (H )=5.8 erg s -1 cm -2 we obtain a total H luminosity of 10 39 erg s -1 . ... The total mass of ionized gas can be obtained from the average mass density inside the H II region and its volume. An average mass density corresponding to the average electron density of 1 cm -3 within a volume with a diameter of 0.5 kpc yields a total ionized gas mass of 10 6 . ...

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. ...

Astrophysics 405 Homework Assignment 4 Tully­Fisher Galaxies in the Expanding Universe Due 1999 April 15 This assignment is a ``dry lab'' simulation of a galaxy observation project. ... Images, spectra, and apparent magnitudes mB for a collection of nearby galaxies have been provided. ... For those galaxies you are unable to classify, assume type Sc. (g) Compute the T­F distance for each galaxy. ... 2 Galaxy Data Use the following data in your calculations. There are 32 galaxies in this sample. ...

... User Guide ] Task: gpscal Purpose: Self-calibration for arrays with linear feeds Categories: calibration, map making GPSCAL is a MIRIAD task to perform self-calibration of visibility data, where the visibility data is produced by linear feeds, and the source is moderately or strongly polarised. Either phase only or amplitude and phase calibration can be performed. The inputs to GPSCAL include a visibility data file, and model images. ... Key: vis Name of input visibility data file. ...

... Next: The PROS Big Up: Software Systems Previous: Data Reduction Software . ... The srcinten task provides PROS users with a tool to compute count rates for point sources in the ROSAT High Resolution Imager (HRI). ... Corrected upper limits are cited at locations where the count rate falls below the source detection threshold. ... Srcinten is a new PROS task that computes and applies the above correction factors to the net counts in a user-specified aperture. ...

... Team . ... The main goal of observations of GRB host galaxies is accumulation of statistics of their spectroscopic and photometric properties. ... The Hubble diagram for 22 GRB host galaxies with known magnitudes and redshifts (GRB 970228, GRB 970508, GRB 970828, GRB 971214, GRB 980613, GRB 980703, GRB 990123, GRB 990510, GRB 990712, GRB 9912008, GRB 991216, GRB 000131, GRB 000210, GRB 000301C, GRB 000418, GRB 000911, GRB 000926, GRB 001109, GRB 010222, GRB 010921, GRB 011121 and GRB011211). ... 600...

... Column (1): Source name from NED. ... Column (8): Log star formation rate, from SDSS. {\it Detected sources:} (1) (2) (3) (4) (5) (6) (7) IC0159 0.58±0.10 8.31 ± 0.07 8.25 ± 0.07 9.55 9.70 8.89 -0.06 UGC2004 5.98±0.65 9.32 ± 0.04 9.03 ± 0.04 9.83 9.61 9.15 0.36 NGC1234 0.24±0.06 7.92 ± 0.09 7.80 ± 0.09 9.67 9.58 8.98 -0.68 2MASJ0839+03 2.30±0.54 8.91 ± 0.09 8.69 ± 0.09 --- 9.94 9.08 0.58 2MASJ0846+02 2.75±0.47 8.98 ± 0.07 8.85 ± 0.07 --- 9.84 8.99 ...

On' failures in the NIRSpec MEMS ST-ECF Instrument Science Report NGST 2002-02 The effects of `on' failures in a MEMS array for the NGST NIRSpec Santiago Arribas, Robert Fosbury Peter Jakobsen --1-- ST-ECF Instrument Science Report NGST 2002-02 The effects of `on' failures in a MEMS array for the NGST ... Assuming that the spectrum of a single facet uses 2000 detector pixels, only 0.01% of `on' failures is acceptable (i.e., 400 facets in a 2k в 2K MEMS array). ...

... spectrum . ... SPECTRUM will compute synthetic spectra, line profiles equivalent widths, specific intensities, assuming LTE, from model atmospheres of early-type stars. ... sterne models . file containing model atmosphere in 2006 Sterne format . ... T=25000, log g=4.0, vt=0, 1400-1415A. a) NLTE model atmosphere, spectrum computed with SYNSPECv25 (black). b) LTE model atmosphere, same linelist in converted format, spectrum computed with SPECTRUM (red) using this input file and this linelist . ...

... The models provided are: . abs - absorption of x-rays by neutral gas with solar abundances. parameter 1 = . ... parameter 2 = . ... normalization - logarithmic value of the flux density at 1 keV in units of keV cm -2 s -1 keV -1 . ... normalization - logarithmic value of the normalization of the gaussian in units of keV cm -2 s -1 . ... absorption ( params )* model ( params ) . ... A single value for the normalization (i.e., fixed normalization) will force the program to use that value. ...

Astrophysical implications of external triggers, GRB030329 in particular External Triggers subgroup · · GRB astrophysics is still very uncertain Associated GW emission: even more uncertain Interpret our observations in the simplest terms Easy to re-cast in terms of specific models Provides some astrophysical context which is readily interpretable Probable: The GRB field will need GW observations to fully understand GRB progenitor astrophysics Nov 10, 2003 Frey 1 Short and Long GRBs.. ...

Astronomy Discussion Forums . ... God and Science ћ SETI ћ Software ћ UFO ћ XEphem . ... SETI Assumes ET Doesnot Care About Can Being Detected What If . ... Post Message | ... My search on how to go undetected in space and SETI Search for Extraterrestrial Intelligence SETI. ... www.astronomy.net . About Astronomy Net | Advertise on Astronomy Net | ... Forum posts are Copyright their authors as specified in the heading above the post. "dbHTML," "AstroGuide," "ASTRONOMY.NET" & "VA.NET" . ...

... FTP access the basic models is here . ... Below, we put short descriptions of the used SED models for the photometric redshifts providing by the current server . ... The uniqueness of this model consists in expanding to the near IR (NIR) of Rocca-Volmerange and Guiderdoni's (1988) atlas of synthetic spectra with a revised stellar library, which includes parameters of cool stars. ... Homepage of the GISSEL model). ... Another model used earlier is the model of synthetic spectra of Poggianti (1997). ...

... Exposure Time Calculator (ETC) . Survey processing . ... VISTA is a 4-m class wide field survey telescope for the southern hemisphere, equipped with a near infrared camera (1.65 degree diameter field of view at VISTA's nominal pixel size) containing 67 million pixels of mean size 0.34 arcsec and available broad band filters at Z,Y,J,H,K s and a narrow band filter at 1.18 micron. A wide field visible camera, if constructed, could also be used on VISTA. ... Tile . ... ESO VISTA Public Surveys . ...

... Let $M$ be a K3 surface or a 2-dimensional compact torus, $B$ a stable bundle on $M$, and $X$ the coarse moduli of stable deformations of $B$. The Fourier-Mukai transform is a functor $FM:\; D_b(M) \arrow D_b(X)$, where $D_b(M)$, $D_b(X)$ denotes the derived category of coherent sheaves on $M$, $X$. Consider a stable bundle $B_1$ on $M$, and let $FM(B_1)$ be the corresponding complex of coherent sheaves on $X$. ... We prove it for arbitrary stable bundles $B$, $B_1$. ...

... Calculated exposure times do not take into account instrument and telescope overheads. ... The reference area for the S/N is circular with a radius equal to FWHM of the Image Quality PSF at the airmass and wavelength of observation. ... 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} } \) . ... The Exposure Time is the product of DIT and NDIT . ...

... VaST is a software tool for finding variable objects on a series of astronomical images. ... VaST performs object detection and aperture photometry using SExtractor on each image, cross-matches lists of detected stars, performs magnitude calibration with respect to the first (reference) image and constructs a lightcurve for each object. ... VaST FITS image viewer ./pgfv . ... Part I" PZP, vol. ... K. V. Sokolovsky, S. A. Korotkiy; "New Variable Stars Discovered by the NMW Survey" PZP, vol. ...

... 13, Moscow 119992, Russian Federation, e-mail: busarev@sai.msu.ru; 2 Research Institute Crimean Astrophysical Observatory, p/o Nauchnyi, Crimea 334413, Ukraine, e-mail: prok@crao.crimea.ua Summary: We propose a combined method of astronomical investigations of small or distant planets incorporating registration of a set of integral spectra of an object and their frequency analysis. ... An application of the method is shown on example of asteroid 21 Lutetia. ... 6] Busarev V. V. (2002), Solar Sys. ...