Next: Identification loop Up: Wavelength Calibration Previous: The Echelle Relation . As a consequence of the cross-disperser dispersion relation, a given line repeated in two overlapped regions of the spectrum must be found at the same y position if spectrum and detector are perfectly aligned. ... The above condition provides a geometrical way to estimate the angle, as: , with the difference in y position of the two occurences of the pairs and the difference of their x positions. ...

... This paper describes distortion calibration procedures for the SOHO /LASCO-C2 Coronagraph, based on in-orbit data and extensive image processing methods. ... C2 suffers from moderate optical distortion, which must be corrected in order to properly locate the stars crossing its field-of-view (which are subsequently used for photometric calibrations), to retrieve critical attitude parameters, and to insure a correct overlapping of the region common to the C2 and C3 instruments. ...

Next: Imaging Polarimetry with NICMOS Up: NICMOS Data Calibration and Previous: The Photometric Performance of . ... NICMOSlook and Calnic C . ... Extracting spectra from a large number of NICMOS grism images requires a convenient interactive tool which allows a user to manipulate direct/grism image pairs. ... NICMOSlook and Calnic-C are two programs that were designed to take advantage of the fact that the NICMOS grism mode typically consists of taking both a direct and a grism image. ...

... LABORATORY OF RADIO ASTRONOMICAL OBSERVATIONS . Radio sources identification is one of the most important tasks of the current radio astrophysics. ... Optical idetification. ... Optical identifications of subsample of steep spectra radio sources from RC catalog using 6m SAO telescope of SAO RAS: optical observations. ... Astronomy Reports. ... Identification of radio sources with data of various radio catalogs allows one to construct continual spectrum of the object and its radio structure. ...

... Hanisch provided me with the ``right'' answers for the stars in the simulated cluster, so it's easy to determine the error of each magnitude determination: find the star in the truth file that falls nearest to the position of each star in my photometric output, and compute the difference between their magnitudes. The question of how to encapsulate these magnitude differences in an overall figure of merit for the reduction procedure deserves some thought. ...

Next: Identifications and Efficiency Up: THE DEEP X-RAY RADIO Previous: Source Classification . ... For some sources which did not have NVSS positions before the time of optical observations, arcsecond positions from the Texas survey (Douglas et al. 1996) and NED (typically based on VLA data) were used. ... All X-ray/radio sources without counterparts on the survey plates were imaged at either the KPNO 0.9m or the CTIO 0.9m telescopes. ... Previously Identified Sources . Sample Properties . ...

Anemic Galaxy NGC 4921 at the Edge . ... Credit Copyright: NASA , ESA , K. Cook ( LLNL ) Explanation: How far away is spiral galaxy NGC 4921? ... Toward this goal, this image was taken by the Hubble Space Telescope in order to help identify key stellar distance markers know as Cepheid variable stars. Since NGC 4921 is a member of the Coma Cluster of Galaxies , refining its distance would also allow a better distance determination to one of the largest nearby clusters in the local universe. ...

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... For each observed position the table contains designation of object as in file of observations, the time of observation, the number and name/ preliminary designation of minor planet supposedly identical with observed object, the values of O – C (observed position minus computed one) in right ascension and declination expressed in arcsec, the difference O – C between observed magnitude and computed one, the code of observatory in the Observatory list (see Observatories section). ...

... 09sep15: calibration run shows that problem is not the cal values. 28sep15: TsysLoad, antenna show that large Tsys Difference only occurs on antenna . ... Their ratio cancels the cal value. bottom: Ratios polB/polA . ... Comparing the ratio of sefdA,B to the ratio of TsysA,B shows that the Tsys difference is independent of the cal value (so the problem is not a problem with the cal values) . Tsys on load,antenna from 28sep15 showed that the large pola,B difference only occurs on antenna. ...

... Background modeling is ALSO connected to response , because any hard X-ray measurements are always background dominated See how the HXD data looks like The HXD design FOVs - BGO active shield 4.5o FOV /anti-coincidence - PSnCu passive collimator 0.55o fine FOV cross section view Well Unit ... view Side Anti Unit 60 57 10 40 Passive Fine Collimator BGO Corner Anti Unit 320 60 57 380mm 340mm Diode Energy range -2 mm Si- PIN diode (64 sig.) 10-60 keV -5 mmt ...

... We proposed that information retrieved from the local surface photometric behavior of the Moon could be used for guiding the remote sensing analyses of specific geological targets. ... The value of the difference of intensities mentioned above may be used as a photometric parameter I of the local surface roughness. ... 7] Apollo 11 Prelim. ... Figure 5 represents the diagram of relationship between photometric roughness parameter and local thorium content in different lunar regions. ...

... The requirements contained in the current National Electrical Code and NFPA Standard for Electrical Requirements for Employee Workplaces apply to all electrical equipment, installations, and usage's at APO. ... do not use defective electrical equipment. ... the Site Safety Officer is to be notified of overloaded circuits in order to replace fuses and reset circuit breakers. ... the only multiple outlet adapter, other than extension cords, allowed are those have internal circuit breakers. ...

. Please standby and you will be automatically connected to the new location of the unframed Supernova page. Or, click on the link above. If you have questions or problems, please email me at David Bishop dbishopx@gmail.com . Last modified: Mon Aug 27 12:40:15 EDT 2001

... Pre-main sequence stars at low metallicity . Identifying and estimating the properties of metal-poor pre-main sequence stars in essential to understand the role of increasing metallicity in star and planet formation, and the formation of the first stars. ... Photometric determination of pre-main sequence accretion rates . The disc accretion rate of pre-main sequence stars is an important parameter in pre-main sequence evolution, but requires time- expensive spectra to be measured accurately. ...

Next: Miriad Subroutine Library Up: Program Development Previous: Code History . The first executable statement of a program should be to print out a version identification. ... character version*(*) parameter(version='Clean: version 1.0 26-jan-90') . call output(version) This gives a version and the date when the task CLEAN was last modified. Additionally, this version identification should be included in any history generated by the task. Miriad manager . 2011-08-19 ...

. You can display the line by line difference between two files with the diff command. diff file1 file2 . The information given by the command tells you what changes need to be made for file1 and file2 to match. If there is no difference between the files you are returned to the shell prompt . diff indicates which lines need be added ( a ), deleted ( d ) or changed ( c ). Lines in file1 are identified with a ( < ) symbol: lines in file2 with a ( > ) symbol. Examples . Did You Know? .

... Chapter 1. ... Problems of observational radio cosmology (6) . ... Analysis of radio astronomical data (32) . ... Data analysis system (33) . ... Actuality, goals and results to depend (45) . ... Interactive processing of continuum radio spectra of radio sources (72) . ... Creation of the astrophysical catalogs data base CATS and its application for selection and analysis of radio galaxy samples (112) . ... Data and methods (176) . ... Results of analysis of known radio galaxies data (179) . ...

... Archives . ... ArXiv] Gamma-ray albedo of the moon, Aug. 15, 2007 . ArXiv] Data-Driven Goodness-of-Fit Tests, Aug. ... Aug 17th, 2007| 06:15 pm | ... From arxiv/math.st:0708.2153v1 . Estimating the number of classes by Mao and Lindsay . This study could be linked to identifying the number of lines from Poisson nature x-ray count data, one of the key interests for astronomers. ... The authors have been working on the Poisson mixture models on genetic data. ... Chandra Blog . ...

... Orienting Mir and modules . ... one on top, one on the left side) . ... Solar arrays can help to differ top from bottom - upper side is blue and flat, lower is light and ribbed. ... There are 4 long and 2 short radiators (pointed with yellow arrow on this photo ) on each module. ... So, if you see short radiators between long ones - you see module side. ... Top of each module is marked by 2 small antennas (pointed with green arrow on the photo ) in the middle of its length near ends of long...