... The concerns here are similar to those for observing bright targets; saturation and blooming of the bright companion PSF must not impact the faint target. Also, one may need to consider subtracting the PSF of the bright object, and effects which limit the accuracy of that subtraction. If the bright companion will saturate and bloom, it will be necessary to rotate the CCD so that blooming along the CCD columns does not obliterate the faint target. ...

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• Making HST Pictures: Illustrations
• NICMOS Proposing Example - 3
• Example of Deconvolution: The HST Image of SN1987A

... Next: Star Finding and Up: Image Restoration and Previous: Multiresolution and Astronomical . ... Design improvements continue to be made in the filter developed using mathematical morphology principles for the Infrared Astronomical Satellite ( IRAS ) images. The purpose of this filter is to eliminate Galactic cirrus emission from extragalactic fields. ... With an appropriate normalization, the filter curve was applied to each pixel in the image to remove the Galactic cirrus. ...

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• Application of a Kalman Filter at UKIRT
• Spatial Structure of NGC 6822: An Example for Statistical Modeling of
• Titan Image Processing

. unfiltered . PC 1 - average . PC 2+3 - annual . PC 2 . PC 3 . PC 4 - secular . PC 5 . PC 6 . Sum of nine first PC's 1-10 . Difference between the initial signal and ten first PC 1-10 .

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• IDL programs

... This experiment makes use of a novel an sophisticated CCD imaging design whereby by 4 2048x2048 detectors are butted together to form a single 4096x4096 pixel detector system. ... Figure 4 (1.1 Megs) shows an example image from one of the LMC fields that is searched for gravitational microlensing amplification of stellar brightness. ... Figure 5 (124 Kbytes) shows an image of NGC 253, taken with this camera and a 320x512 RCA CCD which has 30 micron size pixels. ... Page 5 . ...

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• Galaxy Gallery Page III
• CCD Astronomy Magazine Article Page 3
• Astro-2 and the UIT Experiment

... Meta Index / Home Page / Description / How to use Slew data is particularly susceptible to problems caused by background flares, low-energy noise and halos around bright sources. For a practical guide of the issues to be aware of when interpreting slew data please see Saxton et al. ... In this image, problems due to low-energy noise and optical loading can readily be seen. It is worth checking this image for problems before interpreting interesting features in the scientific images. ...

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• Stage Three: ``filter''
• Examples.

... 11 Yellow-Green (78% transmission): Contrasts well with the red and blue characteristics of surface features on Jupiter and Saturn. ... 82A Light Blue (73% transmission): Useful on the Moon, Mars, Jupiter, and Saturn, this subtle pale blue filter enhances areas of low contrast while avoiding significant reduction of overall image brightness. ... Meade Series 4000 Photo-Visual Color Filters may be ordered individually or in the following sets: . ... Meade Series 4000 Broadband Nebular Filters . ...

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... We have defined a set of rules for classifying SUSI exposures according to the exposure type (BIAS, FF, SCI) and a set of rules for classifying them according to the optical path. ... The MIDAS session shown in Table creates these rules and applies them to our set of SUSI exposures (Table ). The result of the classification process is illustrated in Table . ... The table must contain the following columns: . ... Table: Classification Table for SUSI exposures (susi_rule.tbl) . ...

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• Digital Filters
• Magnitudes and Colors
• WSRT deep surveys

... Animation . Background . ... I created the first animation entirely within the GIMP, using Filters / Distort / Map Object for mapping an image to a box, and Script-Fu / Shadow / Drop Shadow for the shadow effect. If you are curious about the parameters to Map Object, here they are: I set the X angle to 30 degrees, the Z angle to 0 degrees, and I changed the Y angle from 0 to 90 degrees in eight steps, in order to get the rotating box effect. ... We can of course do more with this animation.. ...

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• GIMP animations: merge-anim example 5
• Using Channel Ops with GIMP
• GIMP animations: merge-anim example 2

Figure 2 Microcalorimeter resolution example. The two pannels in the plot show histograms of the filtered pulse heights that result from left: random samples of the microcalorimeter voltage (a measure of the intrinsic detector resolution) and right: pulses from the absorption of Mn K-alpha x-rays. The smooth curves are gaussian profiles with the FWHM as labeled; in the right pannel the gaussian profile has been convolved with the shape of the Mn K-alpha x-ray line doublet. ... 617) 495-7062 . ...

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• Spatial Region Boundaries
• The AstroStat Slog Kalman filter
• Table Filtering with Indexes

... HIPASS results . ... Of the BGC galaxies, 138 have redshifts for the first time. ... We really need ALFA to address that faint end. ... This estimate accounts for the smaller beam size, the number of pixels, and the available solid angle. ... HIPASS (with an integration time of 250 sec per pixel) was complete only for M * galaxies at cz ALFA (with the same intergration time) would be complete to 15,000 km/s . ... The integration time would be only 1 sec per beam for a total time of about 2.6 hours. ...

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• alfa x102 calibrations may15
• alfabmmaps
• alfa x102 calibrations apr12

splitxyz - filter to divide (x,y,z[, distance ,heading]) data into (x,y,z) track segments . splitxyz [ xyz [ dh ] file ] -C course _ change [ -A azimuth / tolerance ] [ -D minimum _ distance ] [ -F xy _ filter / z _ filter ] [ -G gap _ distance ] [ -H [ nrec ] ] [ -M ] [ -N namestem ] [ -S ] [ -V ] [ -Z ] [ -: ] [ -bi [ s ][ n ] ] [ -bo [ s ] ] ... If xy _ filter is non-zero, the data is first divided into segments and then the x,y values of each segment are filtered separately. ...

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• http://xray.sai.msu.ru/~ivan/gmt/man/filter1d.html
• http://xray.sai.msu.ru/~ivan/gmt/man/grdfilter.html
• #tex2html_wrap_inline12527#-#tex2html_wrap_inline12529# for Supernova...

Here is an image a supernova in UGC3683. 11.4.1998. 0.08 UT, CCD ST-7, 520s. Track and Accumulate exposure (13x40s), no filter, dark and flat corrected, temp -20c, telescope used 152/2063 refractor. The image have been taken at the center of our city, Jyvaskyla. The weather was horrible (a full moon was shining and there was clouds on the sky during exposure), so I had stopped imaging in that night. ... Iґll wait for a next clear night and send a better image then. ...

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• Nove in M31 2, 1998
• Supernova 1998aq in NGC 3982
• Supernova 1998ab in NGC 4704

... GCN 8471 | ... TITLE: GCN CIRCULAR NUMBER: 8516 SUBJECT: GRB 081102: MASTER refind and final results DATE: 08/11/11 15:50:10 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina, D.Kuvshinov, P.Balanutsa Sternberg Astronomical Institute, Moscow State University A. Tlatov, A.Parkhomenko Kislovodsk Solar Station of the Pulkovo Observatory V.Krushinski, I.Zalognikh Ural State GCN Circ 8470, Lipunov et al., ...

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... CentralProcessor 0.11 documentation . ... This allows flexible logging to stdout, file, or other sinks. Here is an example of a typical log output: . ... Log level . ... DOCTYPE log4j: configuration SYSTEM log4j.dtd log4j: configuration xmlns:log4j= http://jakarta.apache.org/log4j/ appender name = console class= org.apache.log4j.ConsoleAppender param name = Target value = System.out / layout class= org.apache.log4j.PatternLayout param name = ConversionPattern ...

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• The high quality H interference filter
• cmodel (Model Image Generator) CentralProcessor 0.11 documentation
• casacore: casa::LogSinkInterface Class Reference

Measurement of Sky Brightness at the Iranian National Observatory Davoud Afshari1 and Sadollah Nasiri1,2 1Physics Department, Zanjan University, Zanjan 45195-313, Iran; Institute for Advanced studies in Basic Science (IASBS), Zanjan 45195-1159, Iran; Measurement of light pollution 2 Introduction Among 34 candidate sites at the central part of the country, 5 sites namely Garkesh (in Kashan ), Kolahbarfi(in Kashan ), Deynava (in ... One of these is light pollution. ...

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• Results of recent and ongoing site programs

2009-05-20 O.Hainaut There are many steps between the data coming out of a camera on a professional telescope and the final image that appears in magazines or on our web sites. ... preliminary: from the telescope to Photoshop. cleaning: remove the artifacts remaining in the image . ... In each filter, several images are acquired. ... Fig 1: a raw image (click for full scale) . ... At this stage, the images are still in FITS, the astronomical format, with one FITS file per filter. ... The final image. ...

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• VLTI Calibrator Selection Help Page
• IRAF/STECF imaging linear polarimetry simulation and reduction package
• Homepages of Christian A. Hummel

The aim of this assignment is to teach you how to carry out a very common programming task: reading in a bunch of data from a text file, doing something with it then writing the results out again. ... The goal of the assignment is to write a computer program which will select this sample for you. You will pick the micro-quasars to observe from a rather large catalogue, which can be found here: The catalogue is an ASCII (text) file - you can inspect it with a normal text editor. ...

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• Gemini South Adaptive Optics Imager Performance Calculator
• Brad's Data
• Course Info

OptInt PmWiki . Pm Wiki / . ... Wiki Group . Results of search for PmWiki/ : . ... To limit your search to a single group, enter the group name followed by a slash at the beginning of the search string (e.g., "PmWiki/" or "Site/"). ... apple pie . ... apple' in the PmWiki group of pages . ... the phrase 'pmwiki/apple' in all groups of pages . ... For advanced searches , page list parameters (count, name, group, fmt, link, list, order, and trail) can be entered together with the search string. ...

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• OptInt PmWiki : Page Actions | Search Results
• Astrophysics Group COAST Astronomical Results
• OptInt PmWiki : Test Results | History

Peremennye Zvezdy ( Variable Stars ) 33 , No. ... The new variable star HD 305629, with a Cepheid-like light curve, is demonstrated, from our optical observations and ASAS-3 data, to actually be an ellipsoidal variable star on a highly eccentric orbit. ... During a systematic search of variable stars in the publicly available ASAS-3 database (Pojmanski 2002), apparent variability was found in the star HD 305629 (10 51 34 35, -60 47 57 4, J2000.0; Fig. ... The light curve and color curves of HD 305629. ...

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• XWare > APOD

RTT150 . ... This search system is designed for generating the necessary information on series of pointings (observations of each source consist of sets of exposures with different filters and sometimes with different exposure times) for observed sources. Search results appear at the separate page as a table with the following data: . DATE - real (not evening!) observations date (in YYYY-MM-DD format); . ... Bin - minimal CCD binning mode (may vary during the observations); . ...

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• High Energy Astrophysics Department at IKI RAN