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. ...

... 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. ...

Next: Quantum Efficiency Correction (a.k.a. Up: ROSAT HRI Recipes Previous: Appearance of new HRI . The mean pulse height analyzer channel (PHA) of a spectral distribution will vary depending on its location on the detector. Below is a method to compare observed data with that of preflight calibration measurements. ... For temporal gain variations, see The HRI Calbration Report . ... Retrieve the gain maps (mean PHA) from anonymous ftp at SAO. ... But don't forget temporal gain variations!] ...

... In most cases it will however be necessary to compute an appropriate airmass using the COMPUTE/AIRMASS . ... It is important to keep in mind that ``mean airmass'' and ``mean atmospheric extinction correction'' are different from the values at mid-exposure, especially for larger zenith distances. ... For reasonable combinations of exposure time and zenith distance, the weighted mean airmass supplied by COMPUTE/AIRMASS should be appropriate. ...

The following tasks belong to the category CALCULATION: . Calculations with set data'' In parentheses the name of the source file is given. ... Apply a flat field correction to a map by fitting a 2-D polynomial to the background. ( flat.c ) . ... Program to calculate flux in user defined box. ( flux.c ) . ... RESWRI derives the kinematical parameters from the observed velocity field by fitting tilted-rings to the velocity field and fits harmonic terms after convergence of the ROTCUR part of code. ...

... 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. ...

... HST . What is (epsilon_Nspix)' and how is the spectroscopic S/N calculated? ... Missions . ... Data . ... HST Overview . ... Retrieving HST Data . ... epsilon_Nspix)' is the fraction of the point source energy within N_spix pixels in the spatial direction. For spectroscopic observations, S/N calculations are performed over N_spix x N_lpix pixels, where N_spix is already defined and N_lpix is the number of pixels for a resolution element in the dispersion direction, i.e. 2 px for STIS and ACS. ...

... The RA_PNT , DEC_PNT and PA_PNT keywords, together with the AVRG_PNT keyword which records the type of average used, are meant to describe the average value of the spacecraft attitude during the exposure. ... attsource =`binned': whatever values of the PNT keywords calculated by attbin and stored in the inbinnedattset dataset are simply copied over. attsource =`odf': PNT values are sought from the header of the dataset pointed to by pntkwdset . ... In this case AVRG_PNT is set to `FIXED'. ...

... Correlation between ratio of peak fluxes of flare microwave bursts at 8.8 and 15.4 GHz (parameter S 9 /S 15 ) and spectral index of solar proton fluxes (parameter ?= lg (J 10 /J 100 ) calculated by measurements near the Earth in the >10 MeV and >100 MeV channels. ... The following events are marked by numbers (numeration according to Main Table): 41 - 14.07.2000, 43 - 12.09.2000, 59 - 26.12.2001, 63 - 15.07.2002, 81 - 20.01.2005. ...

Download Izmccd (~2.7 MB). ... a) a choice of the best mode of measurements of stars and objects ("Properties/Measurement"), . b) a choice of reference stars. ... 1) necessity of presence on an image of a plenty of stars (we recommend to apply this mode, if on the frame of reference stars is more 100) . ... Sx and Sy depend from residuals at all reference stars (reference stars are marked by blue color). ... These residuals are the image of the star a minus function of a profile for each pixel. ...

... The accuracy of calculation of both INTERBALL spacecraft (SC) motion has been estimated at the IKI. ... The 30 days measuring intervals were used during the Tail probe (TP) orbital data treatment, and 15 days intervals - during the Auroral probe (AP) orbit determination. ... http://www.iki.rssi.ru/vprokhor/indap.htm for the Auroral probe; . http://www.iki.rssi.ru/vprokhor/indtp.htm for the Tail probe . ... http://www.iki.rssi.ru/vprokhor/ssc.htm , or http://www.iki.rssi.ru/vprokhor/amisan.htm . ...

... Hartmann Test Using a Screen With Four Holes 2 Hartmann test with four holes screen The theoretical concept of the primary aberrations measurement by four apertures Hartmann test introduced by "Malacara" * and "SalasPeimbert et. al. ... Black curve show the calculated coefficients for phase screens which have 8 modes of Zernike aberrations and red curve show the calculated coefficient for original phase screen. (a) astigmatism 45 (b) astigmatism 090 14 Coma Coma modes of Zernike aberration. ...

... Theoretical and experimental investigations electrodynamical characteristics of RATAN-600. Calculation of the two- and thee-mirror periscopic systems of RATAN-600 and optimization their characteristics. Measurements and calculation of the antenna noise temperature of the RATAN-600 radio telescope. ... Calculation and experimental investigation of the characteristics of the radio telescope RATAN-600 when the primary feed is shifted from the focus. ... The "radio-Schmidt telescope" mode. ...

As it is in Ephemerides task, O–C can be calculated with different accuracy. ... It presents three modes of accuracy. One can calculate position of a minor planet by the formulae of elliptic motion starting from the fundamental set of elements for given minor planet. ... Also there is possibility to calculate positions taking into account perturbations from different sets of perturbing bodies by numerical integration ( Integration mode). ... Accuracy of integration is equal to 10**(–10) AU. ...

... The SDSS 2.5-m primary mirror is supported in a manner similar to the Apache Point Observatory 3.5-m telescope primary. ... The axial support is provided by 48 air pistons. The pistons have the same diameter thereby applying equal forces with the same air pressure. ... Each group supports a 120њ sector of the mirror. ... Figure 1: CAD drawing showing the 2.5-m primary mirror and the locations of actuators (green circles) These actuators apply forces (10*cos2 N) to correct astigmatism. ...

... Fitting the observed dependence includes calculations of the polarization cross-sections averaged over particles orientation and size distribution, their normalization and the comparison of obtained dependencies with Serkowski's curve representing observational data for a chosen star. ... Variations of the polarization factors with wavelength are shown in Fig. 16 for homogeneous spheroidal particles with PF orientation. ... The distinction between prolate and oblate spheroids is also clearly seen. ...

... The cross entropy for this complex image is given by ( 16 ) and ( 17 ). ... Differentiating ( 31 ) with respect to and , we find the gradient of is given by . and upon differentiating once more we find the Hessian (curvature) matrix of has the form . ... and its Hessian matrix reads . ... From ( 16 ) and ( 17 ), we find the components of the gradient vector of the cross entropy are given by . ... Differentiating once more we find the components of the Hessian of the cross entropy to be given by . ...

... The plot widgets as shown below are created using Calibrate|Visibility|PLOT . The one on the left is the general plot selection widget, the one on the right, the (data) index selection widget, is created when additional input is required as to the indices of the selected data. ... The calibration is applied to all stars selected in the plot selection widget. ... Below is the screen print after clicking on "Calibrate". Solution calculated for OB= 1, Bl= 1, Ch= 2. RMS [%] = 1.876) . ...

Plot of Pulse broadening time at 1 GHz vs. dispersion measure DM for 196 pulsars. ... A similar plot with fewer pulsars appears in Nature , 354 , 121, 1991 (Cordes, Weisberg, Frail, Spangler & Ryan). ... Dynamic Spectra from Pulsar B1919+21 in 1980-1981. These data obtained at the Arecibo Observatory were reported by Cordes, Weisberg & Boriakoff 1985, ApJ , 288 , 221 and Cordes 1986, ApJ , 311 , 183. Dynamic Spectra from Pulsar B0329+54. ... Dynamic Spectra from Pulsar B1933+16. ...