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 . ...

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. ...

Next: *imcnts* - Radial Profile Up: Radial Profiles and Projections Previous: *tabplot* - Displaying a . ... Input a spatially blocked and energy filtered image from above and use with the background determined from the broad-band background map. cl xray xr xspatial xs imcnts addbkg=no # Do not add the background error Source image file : xdata$snr.qp Source region descripter: c 503 513 50 p 503 513 0 360 n=10 # circular region centered on point ...

... This paper describes the main algorithms used by the Einstein Level One processing to create the exposure masks and the background maps for Einstein IPC images, and how these algorithms were recreated in the IRAF environment. Our goal was to recreate the algorithms used by the Level One Processing to create exposure masks and background maps for Einstein Image Proportional Counter (IPC) data (cf. sections 2.5 and 2.7 of Harnden et al. ...

HI source finding: 2 novel approaches ATNF, December 2010 Outline · Background · What is source finding? ... Motivation for developing new HI source finding methods · Novel source finding methods · · · · General idea Iterative 3-D median smoothing Characterised noise method Wavelet method · Summary Background What is source finding? ... 3-D median smoothing: Purpose · Goal: Reduce noise while preserving shape · Particularly edges · Median works because it's non-linear · Consider this, Iter. ...

... comparison of the system performance for alfa and lbw at OH (.ps) ( .pdf ) (no amps in) . comparison of the system performance for alfa and lbw at OH (.ps) ( .pdf ) (with amps in) . ... On 01apr05 the system performance was measured using the continuum source CTA21 (B0316+162. ... The plots show the comparison of the system performance for alfa and lbw at OH (.ps) ( .pdf ) (no amps installed). ... Black is polA, red is polB. ... G/T alfa)/(G/T lbw) . ... The polB/polA performance ratios are: . ...

Family ASTRO Event Leaders can follow the links below to find a number of resources and more background reading to help them with their Astronomy Events and expand their knowledge on the topics covered in our series of Leader Kits for educators. ... Print and Web Resources on the Night Sky . ... If you have questions about Family ASTRO, see our Frequently Asked Questions for Educators and Astronomers page , or our Frequently Asked Questions for Families and Friends page. ...

The Astronomy Net . Articles | AstroGuide | ... Forums . ... H ere you can find resouces to help understand perhaps the grandest of all sciences. ... Upcoming Sky Events . ... This site includes lists of manufacturers, vendors, software, etc. organized in the AstroGuide to help when you are looking to purchase your tools. ... Astronomy Articles . ... Are you interested in writing an article for the Astronomy Net? ... www.astronomy.net . ... dbHTML," "AstroGuide," "ASTRONOMY.NET" & "VA.NET" . ...

SIMPLE = T / file does conform to FITS standard BITPIX = 8 / number of bits per data pixel NAXIS = 0 / number of data axes EXTEND = T / FITS dataset may contain extensions COMMENT FITS (Flexible Image Transport System) format is defined in 'AstronomyCOMMENT and Astrophysics', volume 376, page 359; bibcode: 2001A .. ... IMAGEW = 4256 / image width IMAGEH = 2832 / image height ANRUN = T / Solve this field! ...

lsst.tcc љ 1.2.2-3-g89ecb63 . ... Files . ... python . ... cmd . showInstrument.py . ... 35 љ kwStrs.append( "Inst=%s; InstPos=%s; GCView=%s" % ( . ... 48 љ kwStrs.append( "IImScale=%0.4f, %0.4f; IImCtr=%0.2f, %0.2f; IImLim=%0.2f, %0.2f, %0.2f, %0.2f" % ( . ... 61 љ kwStrs.append( "GImScale=%0.4f, %0.4f; GImCtr=%0.2f, %0.2f; GImLim=%0.2f, %0.2f, %0.2f, %0.2f" % ( . ... 69 љ kwStrs.append( "GImScale=NaN, NaN; GImCtr=NaN, NaN; GImLim=NaN, NaN, NaN, NaN" ) . ... tcc.cmd.showFocus.showFocus . ...

... 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. ...

... A patch exist for tsearch to regenerate oids when a dump file is loaded into a new database. Future versions of tsearch will not have a problem with dumping and reloading. For now to apply the patch, download the following file to the root of your PostgreSQL source tree (not contrib/tsearch2). http://www.sai.msu.su/~megera/postgres/gist/tsearch/V2/regprocedure_7.4.patch.gz In the root of your PostgreSQL source tree, it's assumed that you have run configure with the options you want. ...

The HyperNews Linux KHG Discussion Pages . Forum: The Linux Kernel Hackers' Guide . Re : Linux SMP Scheduling (Angela) . Date: Mon, 16 Mar 1998 16:34:54 GMT . From: Felix Rauch < rauch@inf.ethz.ch > . The definition of NO_PROC_ID can be fount by, e.g., the following command: . find . -name "*.[ch]" -print | xargs grep NO_PROC_ID | grep #define . (assuming you are in the Linux-source-directory). This will show that NO_PROC_ID is defined as follows: . #define NO_PROC_ID 0xFF .

... 13-Aug-2014 12:13 106K lk_20140815_0905.tar.. 15-Aug-2014 09:06 106K lk_20140901_0823.tar.. 01-Sep-2014 08:23 103K lk_20141016_1324.tar.. 16-Oct-2014 13:25 103K lk_20141211_1708.tar.. 11-Dec-2014 17:08 103K lk_20150430_0315.tar.. 30-Apr-2015 03:15 103K lk_20150430_0420.tar.. 30-Apr-2015 04:20 103K lk_20150818_1511.tar.. 18-Aug-2015 15:11 104K lk_20151113_1903.tar.. 13-Nov-2015 19:04 105K lk_20160314_0610.tar.. 14-Mar-2016 06:11 105K . ...

These pages collect together references to many pictures of the solar system that can be found on the Net. ... Since I originally compiled this list the number of relevant images has grown tremendously. ... http://www.jpl.nasa.gov/pictures/ . ... ftp://dftnic.gsfc.nasa.gov/images/gifs/ . ... http://www.jpl.nasa.gov/galileo/images.html . http://www.jpl.nasa.gov/magellan/images.html . ... http://nssdc.gsfc.nasa.gov/image/planetary/ . ... NASA Image Access Homepage (Planetary Photojournal) . ...

Stellarium 0.12.3 . ... Renderer . FileљStructure . FileљList . FileљMembers . core . renderer . StelTextureParams.hpp . ... 6 љ * modify it under the terms of the GNU General Public License . ... 8 љ * of the License, or (at your option) any later version. ... 13 љ * GNU General Public License for more details. ... 64 љ struct TextureParams . ... 70 љ : autoGenerateMipmaps (false) . ... 84 љ TextureParams & filtering ( const TextureFiltering filtering ) . ...

ESO Phase 3 Data Release Description Please start from this template when preparing the documentation for your ESO Phase 3 data release. ... Finally, the release description will be published as submitted - without further editing by ESO - to support the user community in utilizing the data. ... Please indicate if this is a catalogue data release. ... Data Reduction and Calibration Please address the following questions for scientific catalogue data, particularly in case of source catalogues: . ...

... R-band images obtained at 0.8 arcsec seeing conditions have allowed us to separate foreground star from point-like extragalactic source and estimate their brightness separately. ... To study the nature and properties of the source, we observed it under high spatial resolution. ... CONCLUSION RTT150 optical observations with sub-arcsecond seeing and low resolution spectra confirm the hypothesis of superposition of a radio source onto a `normal' F/G galactic star proposed by [1]. ...

In calculating the NIFS sensitivity, we adopt a read noise of 5 e - , a dark current of 0.01 e - s -1 pix -1 , and a maximum exposure time of 3600 s. Grating . ... e/pix) . ... OH Cont. (e/pix) . ... NIFS should achieve signal-to-noise ratios of ~ 10 per spectral pixel in a 0.1" 0.1" aperture for single 1800 s exposures on uniform, extended, continuum sources with surface brightnesses of J = 15.4, J = 15.0, H = 14.8, and K = 13.5 mag arcsec -2 using the Z , J , H , and K gratings, respectively. ...

The Ryle Telescope was used for some years for monitoring variable sources (in addition to its role in source-surveys related to the Sunyaev-Zeldovitch studies). The instrument is now transformed into the "AMI large array": see the AMI pages for details. ... The rebuild took place between 2006 June and mid-2008; between these dates there is no useful data available. ... For some sources there are many plots, organised by date: . ...