True Color Image Gallery: Galactic SNR | Magellanic Cloud SNR . ... Description: large, diffuse, X-ray and radio brighter in northern half . Radio . ... Radio Images Page . ... Exposure uf . ... Exposure uf Exposure time of unfiltered event file . Exposure f Exposure time of filtered event file . ... Event 2 FITS File . ... AUX file . ... 0.3 - 10.0 . ... see fit detail page for more about the fit. see chandra spectrum page for region used. ... True Color Image . ... Radio Images . ...

Next: Catalog Construction Up: Observations and Analysis Previous: Source Detections . ... It was assumed that the highest signal gives the most likely position of the source. ... Comparing the summed map with the maps from the individual energy ranges, the one which produced the smallest error box was chosen to represent the source position, as long as was greater than 4, a level chosen to reflect a reasonable degree of confidence in the detection. ...

... ATNF Home . ... About ATNF overview . ... Australia Telescope Steering Committee . ... Murchison Radio-astronomy Observatory . ... Parkes radio telescope . ... Mopra radio telescope . ... Online Resources . ... A Comparison of Discrete Sources in Radio and H surveys of the Magellanic Clouds - and the Potential for the New H Survey . ... Previous Section: Discrete Sources towards the . ... The comparison of the radio and H surveys resulted in the discovery of 180 sources common to both surveys. ...

... ESO is building what will be the World's largest optical telescope array, The Very Large Telescope (VLT). The VLT Project organisation is responsible for the design and construction of the Unit Telescopes, including enclosures, optics, adapter-rotators and coating unit. ... Unit Telescopes Overview - This page is outdated, an update is in process. ... Secondary mirror (M2 Unit) - This page is outdated, an update is in process. ... Coating Unit - This page is outdated, an update is in process. ...

WFC3 Instrument Handbook for Cycle 24 . ... Wide Field Camera 3 Instrument Handbook for Cycle 24 > Appendix A: WFC3 Filter Throughputs > A.2 Throughputs and S/N Ratio Data . ... Note that the plots show the S/N as a function of source magnitude for exposure times as short as 0.1 s, although the minimum exposure time for the UVIS channel is actually 0.5 s. Wide Field Camera 3 Instrument Handbook for Cycle 24 > Appendix A: WFC3 Filter Throughputs > A.2 Throughputs and S/N Ratio Data . ...

On 1 February 2002 this Mirror was upgraded from NVSSlist v2.10 to NVSSlist v2.17 . ... This form searches the source catalog produced by the NRAO/VLA Sky Survey (NVSS). ... Object name [optional] : . ... Search radius and verification halfwidth in arcseconds [Optional] : . ... Enter a list of positions to search: . ... The contents of the NVSS source catalog and the techniques used by NVSSlist to derive error estimates and other parameters are described here. ...

... Up: Science Data Pipelines . ... We designed and developed a package which simulates extragalactic point source data within a given field of view and SIRTF band. ... The simulator is modular and extensible to enable multi-wavelength simulations, has been optimized by utilizing parallel processing capabilities, and will be used to test pipeline software. ... The extragalactic simulator is capable of generating large numbers of galaxies within a given patch of sky for SIRTF pipeline testing. ...

... list of all files with drifts 15apr03 to 27may03 baseband mixer chassis was tested on the bench and the tubular lowpass filters (k&E) (100 mhz) after the mixer were causing the problem. ... 10apr03 shows drift of sbc1B with the outputs of the IF2 switched sbc1B, sbc2b. The drift remains in sbc1B so the problem is after this switch (in the correlator). 14apr03 The cables leaving the attenuator box in the correlator were switched (sbc1b and sbc2b). ... At sample 4600 i retightened the switched cables....

... This is followed by astrometric columns - ie columns for the Right Ascension, declination, position error, galactic longitude and galactic latitude. There then follows columns for the computed significance (signal-to-noise) of each source for each of the filters present. Columns for the instrumental magnitudes and colours for each filter, follow. ... Columns for the standard magnitudes and errors, for each filter, follow. ... Standard colours and errors then follow. ...

. Previous . Next . Because an index has not been defined, the previous query is searching using a sequential scan over each row. This will be slow for large tables. Seq Scan on ts_readme (cost=0.00..7.63 rows=1 width=89) (actual time=0.117..0.391 rows=11 loops=1) Filter: (ts_vec @@ '\'databas\' | \'queri\''::tsquery) Total runtime: 0.516 ms

. Comment on J1146-3328 . The derived position here is about 20" from that of the PMN survey position (Griffith & Wright 1993). The source is only detected on the shorter baselines and is probably resolved, although some smearing may be caused by the large position offset. VLBApls home page . Last modified: 16 Oct 2000

... Exposure Time Calculator (ETC) . Survey processing . ... VISTA is a 4-m class wide field survey telescope for the southern hemisphere, equipped with a near infrared camera (1.65 degree diameter field of view at VISTA's nominal pixel size) containing 67 million pixels of mean