Target: Jupiter Date: 2012-11-05 Time : 03:38:10 Telescope: CDK20N Camera: Apogee U16M Filters: griz Exposure time : Satellites: z' at 0.2 seconds full frame Disk: g' at 0.008 seconds 256x256 subframe r' at 0.006 seconds i' at 0.006 seconds z' at 0.20 seconds Observer: John Kielkopf Processing: John Kielkopf ...

Next: AXAF Recipes Up: ROSAT HRI Recipes Previous: Quantum Efficiency Correction (a.k.a. For some observations, a significant amount of data may have been rejected during SASS processing because the background level was higher than the calculated threshold for rejection. ... REJECTED EVENTS . ... The recipe will allow the user to include rejected events in the generation of a new qpoe file and filter on the background level. ... This creates a qpoe file with standard + rejected events. ...

adapted from Observe: Eclipses, published in 1979 by the Astronomical League and "Safe Solar Filters," by B. Ralph Chou, Sky and Telescope, August 1981) . ... Tape TWO pieces of film together into a sandwich, and tape this over the opening in the cardboard. ... The cardboard frame will act as a shade from the bright Sun, while you safely observe through the film sandwich. ... Undeveloped film is not safe. ... tape . ... At the end of one of the tubes, tape the aluminum foil, and make a tiny pinhole. ...

... Note on Filters: . ... NGC 3351 is a mostly face-on late type spiral galaxy. It is marked by a bar like feature in its central regions and a strong inner ring of star formation. ... The galaxy was imaged through the A1,B1 and B5 filters over a total exposure time of 1936 seconds. ... The galaxy was imaged through the A1 filter for 450 seconds and the B1 filter for 1084 seconds. ... The galaxy was imaged through the A1 and V1 filters over a total exposure time of 1200 seconds. ...

... A test was done with the alfa filter bank on 07dec11 to see how well the filter bank settled. ... This centered the high freq band at 1450 MHz. The low freq band at 1300 MHz was not used for the test. ... While the mock spectrometers were taking data, the alfa filterbank was switched between the wide band filter (300 MHz) and the narrow band filter (100 MHz centered at 1440 MHz). ... The alfa filter has has trouble switching between narrow band and wide band observing for most of the alfa beams. ...

... ATNF Home . About ATNF . ... About ATNF overview . ... Australia Telescope Steering Committee . ... Australia Telescope User Committee . ... Murchison Radio-astronomy Observatory . ... Parkes radio telescope . Australia Telescope Compact Array . Mopra radio telescope . ... Australia Telescope Online Archive (ATOA) . ... ATCA | ... Australia Telescope 20GHz Survey . ... Visiting Parkes radio telescope . Visiting Australia Telescope Compact Array . ... Parkes radio telescope webcam . ...

... Near Infrared Camera and Multi-Object Spectrometer Instrument Handbook for Cycle 17 > Chapter 10: Overheads andOrbit Time Determination > 10.3 Orbit Use Determination . ... The second example describes a coronagraphic acquisition and subsequent observations. ... The F222M filter is used in each of the two cameras in turn. The observer requires exposure times of 128 seconds in each exposure, in MULTIACCUM mode. ... 128 seconds exposure time on target . ... 128 seconds exposure time on background . ...

... Exposure Time Calculator (ETC) . ... ESO - Public Surveys . ... the recommended values to use for DIT, . ... Detector on-chip integration (DIT): seconds. to your chosen value - a separate page gives recommended values to use for DIT - for modes 1 and 2 below you may wish to start with the maximum recommended values as these will minimize the effect of read noise (a total object exposure of Y secs with DIT=X secs will produce Y/X lots of read noise) and give you a lower limit on the time needed. ...

... omichain (omichain-1.50) [xmmsas_20070708_1801-7.1.0] . ... The omichain then cycles through each filter in the filter list and processes each exposures in the exposure list for that filter. ... First it checks to see if the exposure is a full-frame low resolution mode, and if so it runs omcomb to combine the four separate image segments into a single full-frame image, which is then processed instead of the individual image segments. ...

... Meade Instruments Corporation . ... Meade Pictor 616A Color Filter System Instruction Manual . ... Remove the Meade Pictor 616A Color Filter System from the telescope or camera. Use the supplied hex wrench to remove the three screws from the telescope side of the Meade Pictor 616A Color Filter System. Position your Meade Pictor 616A Color Filter System to align with the diagram below. ... Carefully screw each filter into the wheel, and re-assemble the Meade Pictor 616A Color Filter System. ...

... Flats : Properly exposed flats over all echelle orders require a two-step process. Flats are taken both with and without a CuSO4 (aka "blue") filter in the beam. ... Suggested exposures are 7 seconds ("red"; no filter) and 240 seconds ("blue", CuSO4 filter) yielding S/N values of ~480. The filter for "blue" flats is listed as "blue" in the Config window in Echelle control under Remark. ... Exposure times for objects can be derived from the following plot: . ...

... Up: Proposal Processing . ... An automated observing proposal processing system has been in use at KPNO during the past three years. ... Observer and proposal information fields in these files are well-marked with LaTeX tags, thus allowing automated extraction and importation to observatory databases. ... The Kitt Peak observing proposal handling system (Bell et al. 1996) is an automated system for distributing, receiving, and processing LaTeX observing forms and associated PostScript figures. ...

... The first step to improve the FORS calibration is therefore to obtain data to allow a computation of the illumination correction across the field. ... Another limitation on the calibration accuracy has been the brightness of the Landolt standards which have forced the use of extremely short exposures introducing small but non-negligible shutter-time errors and also resulting in a very small number of useful standards per frame. ...

... The three optical trains for the cameras, and the pupil reimaging system, are mounted on a wheel, accurately driven by an external motor. ... The low-resolution spectroscopic mode uses the wide field camera and a suitable set of grisms and order sorting filters that are inserted in the parallel beam after the pupil. ... One of the five grisms can operate at four different orders, depending on the filter selected on the first filter wheel that acts as order sorter. ...

... Apache HTTP Server Version 2.2 . ... This document describes the use of filters in Apache. ... The Filter Chain is available in Apache 2.0 and higher, and enables applications to process incoming and outgoing data in a highly flexible and configurable manner, regardless of where the data comes from. ... A wider range of applications are implemented by third-party filter modules available from modules.apache.org and elsewhere. ... There are two ways to use filtering: Simple and Dynamic. ...

... IC 1396 . IC 1396, better know as the Elephant's Trunk. ... LGB (no red)and H filters as follows: . L - 25 images, G and B - 15 images each, all with a subframe of 180 seconds. Halpha (Used Halpha in place of Red filter) - 20 images of subframe 360 seconds. Processed/stacked with CCDStack. Combined and stacked with PS CS5. ... Copyright (c) Amateur Telescope Makers of Boston, Inc. ...

M obile A stronomical Sy stem of TE lescope- R obots MASTER-II Kislovodsk Lomonosov Moscow State University, Sternberg Astronomical Institute , Moscow Union "Optic" , Kislovodsk Solar Station Latitude = 43 o љ44'.767љN; Longitude = 42 o љ31'.417љE; Altitude = 2067љm MASTERљIIљ(8љsquareљdegress) + MASTERљVWF(VeryљWideљFieldљCameras (FOV=800 square degrees, Timeљresolutionљupљtoљ150љms, with unfiltered m_lim=14m on 5 sec. exposure, and ~10.5m with 0.15 sec) . ... 11h 38m 38.0s , -09d 59m 59s) . ...

. unfiltered . GGM02C model . PC 1 . PC 2+3 . PC 2 . PC 3 . PC 4 . PC 5 . Sum of nine first PCs 2-10 . Difference between the initial signal and ten first PCs 1-10 . PC 1 . PC 2+3 . PC 2 . PC 3 . PC 4 . PC 5 . Sum of nine first PCs 2-10 . Difference between the initial signal and ten first PCs 1-10 . PC 1 . PC 2+3 . PC 2 . PC 3 . PC 4 . PC 5 . Sum of nine first PCs 2-10 . Difference between the initial signal and ten first PCs 1-10 .

Nova 1998 2 in M31 this image of the second Nova in M31 in 1998, was made from 38 exposures of 45 seconds integration time. It was made at September 21, 22h 20m UT. Telescope was a CG11 at f/6.3, no filters were used. The long list of processing steps caused the artefacts at the overexposed center of the galaxy and in many of the brighter stars. During the exposures thin clouds covered the sky but the CCD cuts through them, allowing me to obtain this result. ...

Peremennye Zvezdy", . ... GSC 04232-02059, NSVS 3145727, NSVS 3145773, NSVS 3173757 . ... 13.1-13.6 (R, NSVS); . ... To combine our unfiltered photometry with publicly available NSVS (Wozniak et al., 2004; http://skydot.lanl.gov/nsvs/nsvs.php) data, we shifted the zero point of our light curve to match its magnitude at maximum light to the magnitude at maximum of the NSVS light curve. ... Light Curve . The light curve of GSC 4232-02059 in the magnitude scale of NSVS 3145773. ...