XMM-Newton CCF Release Note XMM-CCF-REL-297 Sun Angle correction to the RGS Wavelength scale R. Gonzґlez-Riestra a April 17, 2013 1 CCF comp onents Name of CCF RGS1 SAACORR 0001.CCF RGS2 SAACORR 0001.CCF VALDATE 2000-01-01T00:00:00 2000-01-01T00:00:00 EVALDATE ­ ­ Blocks changed SAACORR SAACORR XSCS flag NO NO 2 Intro duction Studies of RGS sp ... This correlation was confirmed indep endently by Kaastra et al. (2011) in their analysis of the RGS sp ectra of Mrk 509. ...

FOS/BLUE Wavelength-Zeropoint Correction Procedure Summary: A significant time-dependent systematic shift of up to 7 quarter-stepped pixels (1.75 diodes) in the zero-point of the FOS/BL wavelength scale has been confirmed in FOS Instrument Science Report (ISR) CAL/FOS-149 (Rosa, Kerber, and Keyes). ... Figures 1 and 2 (PDF - 14 Kbytes) illustrate the magnitude of the observed shifts and the effectiveness of the quick-fix algorithm provided here. ... Obtain the FOS ISR: CAL/FOS-149 (PDF - 53 Kbytes) . ...

... Many Miriad tasks support on-the-fly selection and averaging of the channels to be processed. ... Channel-0' data (data formed by averaging all spectral channels together) are also treated as continuum data. ... For the spectral data, if the channel number does not correspond reasonably directly with velocity ( e.g. if Doppler tracking was not used), then it might be desirable to resample the spectral data at equal increments in velocity. ... channel . This gives raw or averaged spectral channels. ...

Next: A Preliminary Investigation Up: Spatial Corrections of ROSAT Previous: Introduction . ... These tasks bin a time sorted photon event list based on an assigned phase that corresponds to the 402 second period of the wobble. ... The fundamental limitation of this method is how many source counts you have for centroiding each binned image section. ... Once the phase binned qpoes have been shifted in x,y so as to align the source centroid, they are restacked using 'qpappend_ftsi'. ...

... The plots show the average of 8 days of data (.ps) ( .pdf ) . A2708 is using carl heiles chzm2 routine to do freq switching on galactic oh lines. ... The freq switch is done by using two velocities for the same source: 7.5 AND 58.384 Km/sec . ... 240sec data . ... The full processing should eventually be done with carl's routines. find all of the 7.5 km/sec (freqOn) data as well as the 58.3384 km/sec (freqOff) scans . ... freqOn,freqOn, freqOff,freqOff .. this is 240secs*4 seconds of data . ...

... 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. ...

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The main steps in the reduction of NIR spectroscopic data are flat-field correction, subtraction of sky emission, wavelength calibration, correction for telluric absorption and correction for optical system plus detector efficency. ... Sky subtracted frames are corrected computing analitically the tilt angle from the instrumental calibration parameters or directly measuring it from the data. ... The same procedures are applied to the reference stars frames to obtain the calibration spectra. ...

... Below is the same model paraboloidal bow, C-type (i.e. the molecules are excited by the friction with streaming ions), shown moving at three different angles to the line of sight. ... Here is the 1-0 S(1) image and spec. for a bow moving tangentially to us: . Here is the 1-0 S(1) image and spec. for a bow moving at 60 degrees to us: . Here is the 1-0 S(1) image and spec. for a bow moving at 30 degrees to our line of sight: . ...

... Observers looking at an object that is moving away from them see light that has a longer wavelength than it had when it was emitted (a redshift), while observers looking at an approaching source see light that is shifted to shorter wavelength (a blueshift). ... By measuring the amount of the shift to the red, we can determine that the bright galaxy is moving away at 3,000 km/sec, which is 1 percent of the speed of light, because its lines are shifted in wavelength by 1 percent to the red. ... Part 2...

... 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. ...

spaceweb@oulu.fi - last update: 1 July 1998, 1200 UT (RR) . ... Relates the wave number k to the wave frequency. ... From the equation of motion , m d v /dt = q( v x B ) one can calculate that, in a presence of magnetic field B , a charged particle is accelerated in direction perpendicular to both v (perp) and B . ... The angle a between magnetic field B and velocity vector of a charged particle, v ., i.e., sin a = v(perp) / v(total), where v(perp) refers to the velocity component perpendicular to B . ...

... CI Cam (XTE J0421+560) is an X-ray transient and a binary system the optical companion, which shows the B[e] phenomenon. ... The centroid velocities of the following emission lines were measured: FeII (5 lines), [N II] 5754.59A (NIST Database), H_alpha, H_beta, HeI (5 lines), and [O III] 5006.843A. FeII and [N II] lines that form in the cool equatorial disk wind of B[e] star have stable sharp-edge profiles. ... All the FeII lines and the [N II] line in our spectra show a linear shift with time. ...

Allows you to specify a drift scan: motion at a constant velocity along a great circle. ... The path starts at the new object position (though the telescope actually intersects the path later, see Subtleties ). ... Note that the units are always /sec for both axes. ... The velocity along the path is 0.01 /sec. ... The path is assumed to start when you hit the Slew button (more precisely, when the TCC parses the command). However, it takes the telescope awhile to slew to meet the specified path. ...

... Data Handling and Products > Data Reduction FAQ > The spectrum of my MOS flux standard star is shifted in wavelength by several pixels. Why is that and how can I correct for it? ... Observing with ESO Telescopes . ... The shift of the flux standard spectrum is caused by a combination of bad centering within the slit and possible wavelength calibration issues. To align the spectrum to the tabulated flux, use the parameter --resp_shift in vmmosscience when determining the response curve. ...

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 medium solar time determined by the equatorial Sun's hour angle changing. The equatorial Sun is a false point, uniformly moving along the celestial equator having the average velocity of the Sun's moving along the ecliptic. Back .

... The Time shift for April, 17-18 20 April 1999 . ... The INTMINS April 1999 operations schedule was done on the base of the MIR ground track long-term prediction using the MIR's orbital elements status on 29/03/99 . ... The investigation of the time shift behaviour was began before 29/03/99 on the base of the different orbital elements determined (by KIAM RAN) 22/03/99, 25/03/99 and continued on the base of the orbital elements determined at 31/03/99, 5/04/99. ... Modified 20 April 1999  ...

... There are two main tasks in the package, XCSAO and EMSAO. XCSAO cross­correlates the Fourier transform of an object's spectrum against the transforms of a set of template spectra with known spectral shifts to obtain a velocity and error. EMSAO finds emission lines in a spectrum and computes the observed centers, getting individual shifts and errors for each line as well as a single velocity combining all of the lines. ... It combines spectra, shifting them to a common redshift. ...

... The OC "Mir" orbit parametres before the final burns . ... Orbit period (in min) . ... Mean orbit altitude (km) . ... solar F 10.7 flux . ... F 10.7 <= 100 - low level; 100 < F 10.7 < 150 - medium level; F 10.7 >= 150 - high level . Orbit 86328(15) - the first burn bulding the descent orbit  D V 1 =9.3 m/s. After burn altitude H min = 188.2 km, H max = 219.2 km. Orbit 86329(16) - the descent orbit second impulse D V 2 =10.4 m/s. After burn altitude H min = 158.9 km, H max = 218.5 km. ...