The reduction of a given magnitude m to bt is given by: . bt = a.m + b + c.(logr25 - <logr25>) . ... e.(logd25 - <logd25>) . f.(de1950 - <de1950>) . where a, b, c, d, e, f, <logr25>, <t>, <logd25> and <de1950> are constant values given in the table here below for each reference taken into account. The mean bt magnitude is calculated as a weighted mean where the weight (last column) is derived from each source of magnitude as the inverse square of the mean standard deviation. ...

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• HyperLEDA documentation : parameter: bvt
• Documentation: LEDA: parameter:
• Documentation: LEDA: raw data : flux

The beam pattern and the polarization characteristics . of the radio telescope RATAN-600 . The Mueller matrix elements was computed via formulas [1]: . ... The BP were computed by the aperture method, proceeding from the fild distribution in the aperture of the primary mirror. The components of the main and cross-polarization components of the electric field in the vertical aperture of the primary mirror was computed in Frenel diffraction approximation. ...

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• SCORPIO parameters
• shmidt_e

... Computing the true count rates for digital data. ... The following equation is used to find the count rate. x = ( raw counts / sample time ) . ... True count rates for digital data are corrected by using the first equation for a point source and the second for an extended source. a = ( y - pre_amp - darkrate ) / ( highvolt x pt_effic ) . ... True photocurrents (count rates for analog data) are corrected by the first equation for point sources and the second equation for extended sources. ...

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• Obsolescent Acquisition Parameters
• covar2ellipse.pro (JWST Pipeline routines in IDL)
• HSP Data Handbook

The pitch, roll, and focus errors of the telescope (measured and computed in AO9 survey and tilt sensor pitch,roll ) can be corrected by using the tiedowns. ... Tiedown positions to correct the pitch,roll, focus errors versus azimuth for za 2 through 20 degrees. ... The pitch, roll, and focus errors are plotted versus azimuth for za 1 to 20 degrees (the color changes every two degrees) . ... The pitch error is on the top and the roll error is on the bottom. ... The pitch and roll errors versus za. ...

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• http://www.naic.edu/~phil/hardware/vertex/hagenDocmemos/klaus/ATA1A/GUI_CFG.txt
• HIPASS parameters Barnes et al (2001), Ryan-Weber et al. (2002), Zwaan et al
• Wapp Home Page

... CentralProcessor 0.11 documentation . Calibration and Imaging Documentation . The cmodel pipeline task is responsible for extracting a local sky model (LSM) from the global sky model (GSM) and building an image from the components and/or images resulting from the request. ... MPI wrapper> cmodel -c config.in . ... None . ... If Cmodel.gsm.database is set to asciitable then a row/column (space separated) file is used as the global sky model source. ... cmodel (Model Image Generator) . ...

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• ccontsubtract CentralProcessor 0.11 documentation
• Parameter Set CentralProcessor 0.11 documentation
• User Parameters - Pipeline & job control CentralProcessor 0.11 documentation

XMM-Newton Science Analysis System Page: 1 ommag July 2, 2008 Abstract Converts from count rates to magnitudes in the instrumental system. ... Please note that no magnitude is computed for corrected count-rates greater than 1000- for such bright sources the count rate is wrong because it is out of coincidence-loss correction. ... MAG The instrumental magnitude computed using the corrected count rate and using the appropriate calibration constants for the lter. ... Convert this to a limiting magnitude. ...

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• http://xmm.vilspa.esa.es/sas/7.0.0/doc/ommag.ps.gz
• http://xmm.vilspa.esa.es/sas/6.5.0/doc/ommag.ps.gz
• http://xmm.vilspa.esa.es/sas/7.1.0/doc/ommag.ps.gz

ESO Phase 3 Data Release Description Please start from this template when preparing the documentation for your ESO Phase 3 data release. ... Finally, the release description will be published as submitted - without further editing by ESO - to support the user community in utilizing the data. ... Please indicate if this is a catalogue data release. ... Data Reduction and Calibration Please address the following questions for scientific catalogue data, particularly in case of source catalogues: . ...

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• Stellar parameters from calibrations of spectral types
• CONSTRICTOR parameters for astrometric reductions
• Parameters

Stellarium 0.12.3 . ... FileљStructure . ... SphericalRegion . DrawParams . ... SphericalRegion::DrawParams Struct Reference . Parameters specifying how to draw a SphericalRegion . More... #include < StelSphereGeometry.hpp > . DrawParams (class StelProjector *projector) . Construct DrawParams with default parameters and specified projector. ... Do not subdivide the region to follow projection distortions. ... class StelProjector * SphericalRegion::DrawParams::projector_ . ...

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• Stellarium: Extinction Class Reference
• Stellarium: gSatTEME Class Reference
• Stellarium: Skybright Class Reference

... 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 ...

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• OptInt PmWiki : Url Approvals
• OptInt PmWiki : MROIDelayLine / Trolley Software
• OptInt PmWiki : PmWiki / Url Approvals

lsst.tcc љ 1.2.2-3-g89ecb63 . ... Namespaces . ... tcc.mov.fullSlew Namespace Reference . ... Compute a jerk-limited trapezoidal slew. ... tJerk , . ... dp position of starting point at time t = 0 (deg) . ... dp velocity of starting point at time t = 0 (deg/sec) . ... dp sets maximum allowed jerk and minimum slew duration (deg/sec^3) (see Details for more information) . ... Rounding extends for a time (tJerk / 2) (or less if required) symmetrically to both sides of each trapezoidal slew node. ...

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• lsst.tcc: tcc.axis.computeSlew Namespace Reference
• Astrophysical Research Consortium - Apache Point Observatory
• Telescope Parameters

There are six possible ways of object description: . a) by number(s) . ... d) by list . e) by orbital elements . ... They should be introduced as year, month, day with tenth (e.g. 20021104.1). d) Computations are performed for all objects listed in the file whose path and name should be introduced into assigned data field. ... On pressing Edit file button user has a possibility to look through the list of object elements or their coordinates and velocities to add or to change it. ...

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• ENGAMPLE

parameter estimates and variances Bayesian Gaussian Aperture Photometry -- updated notes · Model Selection Model Selection · · · · · p-values and Hypothesis Tests Type I, Type II, and other errors Analysis Design Upper Limits Hypothesis Tests , Likelihood Ratio Tests , and posterior predictive pvalues Odds ratios, Bayes Factors AIC/BIC/DIC/WAIC/HQIC/MDL · · p-values · · p=Pr(T T(D)|H) What ... The difference between significant and not significant is not significant." ...

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• http://hea-www.harvard.edu/AstroStat/astro193/VLK_slides_feb25.pdf
• The AstroStat Slog central limit theorem
• The AstroStat Slog computer vision

... Field size . Object name . ... Map size . ... Field size: the approximate size of the map in the Y direction. ... Galaxies: . ... Galaxies, which size exceeds some value depending on the field and map sizes, are displayed with their real positional angles and sizes by 25m isophote. ... In the "tools" fields there are links to the several famous AVO (Astrophysical Virtual Observatory) resources: NED and Simbad databases and DSS2 (Palomar Digitized Sky Survey) images of the corresponding sky area. ...

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... After the edit, recompile the kernel and recompile the Apache server then reboot. ... If you're running a really busy BSD Apache server, the following are useful things to do if the system is acting sluggish: . ... Maximum # of processes . ... This machine is a server that handles lots of traffic, # so we crank that value. options NMBCLUSTERS=4096 # mbuf clusters at 4096 # # Misc. options # options CHILD_MAX=512 # maximum number of child processes options OPEN_MAX=512 # maximum fds (breaks RPC svcs)...

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• Apache module mod_isapi
• Descriptors and Apache

... We demonstrate through numerical simulations that model parameters estimated with our technique are essentially bias-free, even when the average number of counts per bin is 1. ... The IW technique avoids such biases by estimating through successive iterations, where for each iteration, j, , and the best-fit parameters are determined by minimization of . ... In our sample, we find that the minimum values and best-fit parameters converge after about 6 iterations. ...

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• A New PROS Task for Calculating HRI Source Intensities or Upper Limits
• In-Orbit Calibration of the Distortion of the SOHO/LASCO-C2 Coronagraph
• Indexing and Searching Distributed Astronomical Data Archives

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. ...

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• Initial parameters of compact stars
• The Effect of Relativistic Wind on Accretion Flow Parameters
• Parameters of binary compact star evolution

Follow-up astrometry and recoveries are made with the ANU 40 inch (1.0-m) f/8 reflector at Siding Spring Observatory (IAU code 413). ... A routine follow-up of 2003 WY153 on 2003 Dec 15 became much more than routine when a faint object with unusual motion vector was found close to the target asteroid. ... During routine astrometry with the 1.0-m to improve the orbit of the Apollo asteroid 2004 CB, the asteroid was found on March 30 to have a short tail! ... Siding Spring Survey Main Page . ...

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• Emma Kirby - Science

.

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• THE HUBBLE LAW JAVA APPLET
• Potential Energy
• Evidence for Dark Matter

... SFIT is a general-purpose code designed to optimize theoretical stellar spectra to an observed spectrum. ... While the programme expects input from "stdio", it is more natural to save commands in a file (eg "sfit_input") and run the code simply by . ... If the spectra to be fitted have a filename "star_spectrum", then the best fit spectrum will be written out, together with the renormalized input spectrum, to a file called "star_spectrum.fit". ... sets up model spectrum grid (and for 2nd star) . ...

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• SCL Sfit SLV Commands
• SCL Sfit SYN Commands
• SFIT2 - Command Syntax

Computer Ephemeris for 2014 from DE200/LE200. Orbital parameters of the Sun. Date Mean Perigee Mean Paral Aberrat Epsilon Nutat longitude longitude anomaly Dec 24 272.6887 283.1787 349.5100 8.941 20.832 2326 6.72 -8.19 Jan 3 282.5451 283.1792 359.3660 8.943 20.837 6.71 -8.18 13 292.4016 283.1796 9.2220 8.942 20.834 6.76 -8.11 23 302.2581 283.1801 19.0780 8.935 20.818 6.87 -7.99 Feb 2 ...

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• Sun orbital parameters for Computer Ephemeris for 2015 (DE200/LE200).
• Optical static Fourier spectrometer
• Sun orbital parameters for Computer Ephemeris for 2016 (DE200/LE200).