... Classes . Files . ... File List . File Members . measures . ... It is a simple 00060 // container with the selected method, and the mean epoch . br 00061 // The method is selected from one of the following: 00062 // ul 00063 // li Aberration ::STANDARD (at 1995/09/04 the IAU1980 definition) 00064 // li Aberration ::NONE 00065 // li Aberration ::B1950 00066 // /ul 00067 // Epochs can be specified as the MJD (with defined constants MeasData::MJD2000 00068 // and MeasData ...

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• casacore: measures/Measures/SolarPos.h Source File
• casacore: casa::Aberration Class Reference
• casacore: casa::SolarPos Class Reference

Instrument Science Report WFC3 2005-14 Results of WFC3 Thermal Vacuum Testing: IR Channel Gain B. Hilbert April 11, 2005 ABSTRACT Thermal vacuum testing in September - October of 2004 provided the fist opportunity to measure the gain of FPA64 since its integration into the instrument. Gain values derived from this data are between 2.43 e-/ADU and 2.50 e-/ADU, roughly 5% lower than those calculated for FPA64 at the Detector Characterization Lab (DCL). ... Gain values for each quadrant of FPA64. ...

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• GigaCAM -Figure 2.
• FOC Exposure Simulator - FOCSIM
• ALUMINUM SUPERCONDUCTING HOT-ELECTRON BOLOMETER MIXERS FOR THz APPLICATIONS -

... Archives . ... Magnitude [Eqn] . ... Differential Emission Measures (DEMs) are a summary of the temperature structure of the outer atmospheres (aka coronae) of stars, and are usually derived from a select subset of line fluxes. ... is called the Differential Emission Measure and is a very useful summary of the temperature structure of stellar coronae. ... Tags: DEM , Differential Emission Measure , EotW , Equation , Equation of the Week , stellar coronae . ... Comment ( RSS ) | ... Chandra Blog . ...

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• The AstroStat Slog DEM
• The AstroStat Slog stellar coronae
• The AstroStat Slog Differential Emission Measure

This section is on a higher level than the rest, and is primarily meant for advanced users, who may wonder how orbital motion is actually derived. ... As stated earlier, the motion of a satellite (or of a planet) in its elliptical orbit is given by 3 "orbital elements": . ... 3) The mean anomaly M , an angle growing at a steady rate, increasing by 360 degrees each orbit . ... In polar coordinates ( r,f ) describing the satellite's motion in its orbital plane, f is the polar angle. ... The angles: . ...

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• Frames of Reference: The Basics
• Trigonometry--what it is good for?
• Magnetometers [Oulu]

Collection of the orbital elements | ... The errors of the spacecraft motion extrapolation outside the measuring time interval were estimated by using the comparison of SC positions calclulated by the forward integration ( extrapolation method) and backward integration ( interpolation methods). ... The character of these time shift of the ascending nodes ( D Tn) corresponds to the orbiting period errors, which arise during SC motion extrapolation outside the measuring intervals. ... INTERBALL mission ...

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• The INTERBALL Tail PROBE orbital elements
• How Orbital Motion is Calculated
• About modification of the INTERBALL orbital elements

Next: Calling Parameters Up: CAL_getRFCdefocus Previous: CAL_getRFCdefocus Contents . ... The angle of incidence on the facets of the gratings . where is the blaze angle, which is available from CCF MiscData , item BLAZE_ANGLE , and is the angle of incidence measured from the grating surface for an on axis source. is available from CCF MiscData , item INCIDENCE_ANGLE , or from CCF Lincoord , item G_ALPHA . ... with the radius of the Rowland circle available from CCF MiscData item ROWLAND . ...

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• Comments on Individual Table Columns
• The contour method of calculating source region shape

These are very prominent absorption lines is most all galaxies. ... These pair of absorption lines will appear in all the spectra and they should be your principle source for determining the redshift. ... When this applet opens you will see an iconic representation of galaxies in the left hand side of the applet and a target area in the right side of the applet. ... Note: What you are doing in this excercise is identical to what Hubble did in the 1920's and you are using the same galaxies. ...

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• Energy From the Wind
• Basics of Wind Energy

... Matching the Surface of Best Focus . ... The plug-plates of SDSS project are responsible for locating the optical-fiber plugs spatially and for defining the plug tilt with respect to the surface of best focus. ... Approximately 670 holes are drilled in each plate. ... In the first attempts to match the curvature of the plug-plates to that of the best focal surface, the bending fixture was set upon 3 6.630mm metal supports that were affixed to a table top and spaced 120 apart. ...

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• Astigmatism II
• Appendix B
• Dan Long

Magnification (Power) And Using Eyepieces . ... To determine power in a telescope, divide the focal length of the telescope by the focal length of the eyepiece. By exchanging an eyepiece of one focal length for another, you can increase or decrease the power of the telescope. For example, a 25mm eyepiece used on a telescope with a 1000mm focal length would yield a power of 40x (1000 / 25 = 40) and a 10mm eyepiece used on the same telescope would yield a power of 100x (1000 / 10 = 100). ...

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• Astronomy Terms - To Help You Study The Universe - an Astronomy Net Article
• Resolution - an Astronomy Net ATM Forum Message
• So How Can We Calculate The Mass Of The BH? - an Astronomy Net Blackholes Forum

The ESA/ESO Astronomy Exercise Series 2 . The Distance to Messier 100 as Determined by Cepheid Variable Stars . ... The small variations in distance to the individual Cepheid variable stars in the Cloud are negligible compared with the much larger distance to the SMC. ... In this way Cepheid variable stars can be used as one of the 'standard candles' in the Universe that act either as distance indicators themselves or can be used to calibrate (or set the zero point for) other distance indicators. ...

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• ASP: Star Science in the Autumn Sky
• ASP: Indiana Jones and the Astronomers of Yore
• ASP: Good Astronomy Activities on the WWW

... The time taken for 10 full swings of a long pendulum performing small angle oscillations is measured seven times. The results (in seconds) are: 34.63, 34.80, 34.71, 34.80, 38.21, 34.54, 34.77 (a) Estimate the error in making a timing measurement. [3] (b) Estimate of the period of the pendulum and the error in this estimate. 3] The pendulum is now left to swing and two experiments are made in which the time is measured for many complete swings using the same method as for one swing. ...

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• http://www.mrao.cam.ac.uk/~kjbg1/exams/2009_paper.pdf
• http://www.mrao.cam.ac.uk/~kjbg1/exams/2006_paper.pdf
• A Calculation of derivatives

Electron Bombarded, Back-Illuminated CCD Sensors . ... EBCCD PERFORMANCE: EBS Gain . ... To the first order, the signal gain in the EBCCD is proportional to the kinetic energy of the photoelectrons prior to their impinging on the CCD back surface. ... To obtain EBS gain in the active material, it is necessary for the photoelectron to enter the pixel from the back surface of the CCD -- away from the gate structures that dissipate the electron energy. ... The EBCCD EBS gain was tested using two methods. ...

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• Current star formation rate
• Faraday Rotation Measures
• Measuring aperture

Problem Set 2 - Cosmology­A3002 ­Due on or before November 7th. Can be sent via internal mail (Brian Schmidt, RSAA) use H0=70 km/s/Mpc, M=0.27, =0.73, w=-1 for all problems. ... Finish off your Monte Carlo simulation by selecting objects at random redshifts from 0<z<0.1, assuming that they have a mean absolute magnitude of M=-19.5 with a dispersion 0.2 magnitudes. ... Problem 2.1 (2 pt): In class we described the scale at which material can collapse in the Universe as the Jeans' length. ...

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• Pink Black Holes: Frequently Asked Questions
• Paul Francis -- Astronomical Constants
• GSAOI Bulk Motions Science Page

... We have calculated the binary coalescence rate with time using the ``Scenario Machine'' code, which allows us to simulate evolution of large ensembles of binary stars in an artificial galaxy using a Monte Carlo method (see Lipunov 1992, Lipunov et al 1994, 1995 and references therein). ... The source evolution in a galaxy with given star formation rate is thus calculated as , where is the redshift at the turn-on of star formation, which is the second important parameter of the model. ...

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• The COOC Criterion (Criterion of Observations versus Calculations)
• Normal star evolution
• Calculation of Binary Neutron Star Coalescence Rates

Организаторы: Michel Balazard (CNRS, Лаборатория Понселе) , Михаил Цфасман (CNRS, Лаборатория Понселе, ИППИ РАН) , Алексей Зыкин (Лаборатория Понселе, ГУ ВШЭ) . О конференции . ... In the set of all lattices I define subset of principial unstable lattices. Their Haar measure can be easely calculated. Comparing this with the measure of all lattices we get some inequality between regulator and discriminant of number field. ... Страница Лаборатории Понселе . ...

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• Arithmetic groups (Spring 1997)

QED calculations of H2 molecule Vladimir A. Yerokhin St. Petersburg State Polytechnical University in collaboration with Krzysztof Pachucki Warsaw University FFK 2013, Pulkovo, St. Petersburg, October 7-11 Do we need QED for H2? ... 150, 51 (2011) An order of magnitude in precision every 14 years QED : -0.1964 (9) 5, 3039 (2009) Theory: J. Chem. ... Wave function is represented by a linear combination of basis functions Choice of the basis functions: · · Explicitly correlated basis set. ...

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• Structure of the database files
• Datafile structure

... The HST uses an onboard model of its orbit to perform in real-time various control functions relating to spacecraft operations and observation support. ... New coefficients for the ephemeris are updated every other day, and are archived as FITS keywords for each HST observation data set. Using these coefficients,an observer can perform a variety of calibration and characterization calculations relating to the orbital position and velocity of the telescope. ...

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• A New Entropy Measure Based on Multiple Resolution and Noise Modeling
• A New PROS Task for Calculating HRI Source Intensities or Upper Limits
• MEM Task for Image Restoration in IRAF

Download Izmccd (~2.7 MB). ... If you want to calculate equatorial coordinates of object: . Click the " File " menu, and then click " Open " ; or press  on toolbar. Choose a file with image. ... Also see section " Viewing of image ". ... Before, if it is necessary, you must make an account dark current and flat field (See section " Preliminary processing of images ".) ... Measure the marked stars. ... Click the " Calculations " menu, and then click " Coordinates " or . ...

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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. ...

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• http://www.naic.edu/~phil/temp/pfg_obs_opt_depth.ps
• http://www.naic.edu/~gibson/asph405/dry/drylab.pdf
• INTERSTELLAR SCATTERING DISPERSION PLOTS

New reduction of minor planets photographic plates obtained with Pulkovo Normal Astrograph A.A. Berezhnoy Pulkovo Observatory of RAS, Saint-Petersburg, Russia Minor Planet observations at Pulkovo Periodical observations of 14 bright asteroids named Selected Minor Planets (SMP) were performed at Pulkovo since 1948 within the international framework started by works of B.V. Numerov and D. Brouwer. ... 108 133 113 74 124 67 97 88 14 84 64 5 20 19 Epochs (YYYY.MM) 1200 Mean values of total obs. ...

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