scripts · Made a comparison with SCISIM ray trace that replicates each observation Main Analysis Steps · Select regions for each camera and run esas · Extract spectra and background · Made an . arf that is a guess for typical off axis angle ( fn(E) knowing only a single reflection occurs ) · Assume source spectrum of a LMXRB e.g. const*phabs*(diskbb+comptt) probably the detailed spectrum doesn't matter to 1st order · Also require an ...

... December 21, 1997 . ... Advantages are briefly discussed of gaining in spectral resolution, which is accompanied by losses in signal level, as compared with the attempts to improve the accuracy of measurement of line parameters by means of rising the S/N ratio alone with increasing the exposure time. To partially solve the problem of observations of faint objects at the BTA a new design echelle spectrometer is proposed. high resolution spectroscopy . ...

... Delivery Procedures . ... File Structure . Reference Files . ... The procedure compares two FITS reference files tables. ... The compared elements are limited to those specified in the COLUMNS parameter (which is necessary for this program to run). ... The parameter COLUMNS is an n-element array of strings with the names of the columns to compare within the table. ... When a combination is missing (in the new_file ;or in the old_file) the procedure will flag it in the standard output. ...

Crater Gassendi . ... I made this drawing was made on the 26th of november 2001. If you compare this one with the previous drawing of Gassendi (below) the differences are clear. ... This drawing was made on the 28th of september 2001. After nearly a full month without observations I had a one hour gap between the thicker clouds. ... This drawing was made on the 29th of august 2001. ... This drawing was made on the 27th of august 2001. ... This drawing was made on the 25th of august 2001. ...

... In order to compare the number of different evolutionary stages obtained and X-ray luminosity of the chosen X-ray sources with the observed galactic values we use the sum of C/O+O/C , where C and O are the calculated and observed values of a given binary type, respectively. If we make comparison for a number of different binary species (for example, we compare the number of CV, number of X-ray pulsars,   total X-ray luminosity of LMXB, etc.), we write this criterion in the form: . ...

. You can use the diff command to compare the contents of two directories: diff directory1 directory2 . The information given by the command tells you what to do to make the directories match. If there is no difference between the directories you are returned to the shell prompt . diff reports if a file or directory is only to be found in directory1 or directory2 . It also reports any line by line differences for files that are common to each directory. Example .

... The sample of the Local Volume galaxies (distance smaller than 10 Mpc) gives a unique opportunity to study the properties of galaxies including the weakest objects: the absolute magnitude M B -10 and the virial mass M vir 10 9 M x263C;. ... Luminosity function of the Local Volume galaxies. ... The luminosity functions for galaxies are presented: red dashed line - from the 2dFGRS survey (Norberg et al. 2002); blue dash-dotted line - from the SDSS survey (Blanton et al. ...

... These measurements have invariably been interpreted as evidence for significant wide-spread small-scale structure in the HI distribution with volume densities orders of magnitude higher ($n_{HI}\sim 10^4-10^5$ cm$^{-3}$) than those implied by the parsec-scale component. Naturally, there are serious difficulties about such structures being in equilibrium with the other components of the medium, and hence about how to generate and maintain such apparently commonly encountered structures. ...

Once students get the hang of it, they can find and measure the brightness of Delta Cephei in a few minutes. ... of Delta Cephei . ... Oct. ... The following table lists the measurements of Delta Cephei made by one amateur astronomer in autumn 1990. ... 4.0 . ... This activity is a simplified version of one that appeared in Hands-On Astrophysics, a series of activities prepared by the American Association of Variable Star Observers with support from the National Science Foundation. << previous page | ...

... Basic Observables: Zero-differenced phase and code ionosphere-free combinations of global GNSS network stations, corrected by P1-C1 satellite code biases (cc2noncc), daily observations with 30 seconds sampling rate Sites coordinates : IGb08 reference frame coordinates and velocities Displacements: solid tides, ocean loading, pole tide loading (IERS 2010) Geometric model : Receivers antennas eccentricities, absolute receiver and ...

Optical observations of comet P/Tempel 1 Heike Rauer, JЖrg Knollenberg, Michael Weiler DLR, Institut fЭr Planetenforschung Berlin-Adlershof Observations of comet P/Tempel 1 at optical wavelengths Before and after impact : monitoring · Gas production rates -,,classical optical long- slit spectroscopy: CN, C3, C2, NH2 - variation along heliocentric distance : difference before ­ after? - compare with measurements of parent species at radio, IR · ...

We report first results of a multifrequency campaign from radio to hard X-ray energies of the prominent gamma-ray blazar 3C 279 during the first year of the INTEGRAL mission. The variable blazar was found at a low activity level, but was detected by all participating instruments. Subsequently a multifrequency spectrum could be compiled. ... In addition, this 2003 broadband spectrum is compared to one measured in 1999 during a high activity period of 3C 279. | ...

... This thread uses PINTofALE to generate a simulated Chandra spectrum. ... define a DEM . ... pset marx .par ExposureTime=50000 OutputDir='sim_ marx ' \ ; GratingType='NONE' DetectorType=' ACIS-I ' SourceFlux=-1 \ ; SpectrumType='FILE' SpectrumFile='spec_ marx .dat' \ ; SourceType='POINT' DitherModel='INTERNAL' ; marx TSTART=2006.46 ; marx2fits sim_ marx / spec_ marx .evt ; dmextract infile= spec_ marx .evt[EVENTS][(x,y)=circle(4018,4141,10)] ; [bin pi=1:1024:1] outfile= spec_ ...

... Mass . 17a. Measuring Mass . ... A medium-size (1.25 inch wide) binder clip, as is used in offices to hold papers together--the type made of flat blue steel, with two wire handles. ... The theory predicts that the oscillation period should be proportional to the square root of the oscillating mass, including the mass of the clip. Note that gravity plays no part here: the oscillation period would be the same on the Moon or in zero-g. Denoting square root by SQRT, we have . ...

Chiaki Kobayashi, Ralph Sutherland How galaxies did form and evolution? - to answer this unsolved problem, we are simulating the formation and evolutionary history of galaxies in the Universe, including star formation, supernovae feedback, and chemical enrichment. Comparing the spacial distribution of elements within galaxies with observations, we will examine fundamental physical processes that drive galaxy formation. ... COALA : Universe Galaxy AGN Star Planet ...

Next: Summary and conclusions Up: Preliminary analysis of the Previous: Sky and redshift distribution . To get an estimate of the external accuracy of IPCS redshifts we compared our results for common galaxies with the redshifts from CfA catalog (Huchra et al. ... For 18 galaxies in common we have mean difference = -27 km s -1 with the error 16 km s -1 and the standard deviation = 64 km s -1 . This comparison indicates that most of IPCS redshifts have uncertainty less than 100 km s -1 . ...

Next: GOCG Post-Observation Products . ... Reconstructed Orbit . JPL MMNAV Reconstructed Orbit . ... The JPL MMNAV files will be made available on the JPL MMNAV FTP site in directory [RAstron.ODDATA.JPLICV.TRACK] (note the capital letters). back to top . ... What: X-band Doppler tracking data will be transmitted in near real-time from the DSN GTS to the JPL MMNAV team and from the Pushchino GTS to the ASC navigation team, and post-pass (via FTP) from the GBTS to the JPL MMNAV team. ...

... 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: . ...

G1.9+0.3 has been recently identified as the youngest known Galactic supernova remnant, about 150 years old at most. ... The Youngest Galactic Supernova Remnant: G1.9+0.3 . ... X-ray spectral variations in the youngest Galactic Supernova Remnant G1.9+0.3 . ... Radioactive Scandium in the Youngest Galactic Supernova Remnant G1.9+0.3 . ... Expansion of the Youngest Galactic Supernova Remnant G1.9+0.3 . ... Supernova Ejecta in the Youngest Galactic Supernova Remnant G1.9+0.3 . ...

The above image is a computer simulation of the distribution of mass in a Dark Matter dominated Universe. ... Structure (\eg density enhancements) clearly forms at the intersection of these filaments. ... What is Dark Matter? ... Testing for the presence of dark matter in the solar neighborhood now becomes an accounting problem The possible sources of this mass in the solar neighborhood are 1) luminous stars, 2) interstellar gas, 3) stellar remnants (mostly white dwarfs) and 4) dark matter: . ...