... The J, H and K bands are characterized by a bright background, such a background is mainly due to the emission of atmospheric lines and of thermal radiation. ... If the source cover a large fraction of the slit, spectra off-source must be observed to adequately sample the sky background. ... The on chip integration time (time spent in each position of the slit) must not exceed 40 seconds in J and H bands and 60 seconds in K band. ... We suggest a sequence of 10 for each elementary integration time. ...

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... GPI Data Pipeline 1.0 documentation . ... Thermal/Sky Backgrounds . ... Using Thermal/Sky Backgrounds in GPI Data Reduction: . Creating Calibrations: . ... Thermal emission (from sky or telescope) becomes an important background source for wavelengths longer than 2 microns. ... The pipeline treats thermal/sky backgrounds similar to dark frames and is designed to subtract a thermal/sky background, scaled to the integration time of the science image, from K-band observations. ...

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• HDF-S Data Products
• STIS Instrument Handbook
• NICMOS Background

Next: Results of follow-up spectroscopy Up: Spectral observations and data Previous: Spectral observations and data . ... The reduction of the originally two-dimensional CCD data included standard steps such as: bias and dark subtraction, flat-fielding, cosmic-ray removal. ... In the final spectra showing emission lines, redshifts and line fluxes are measured applying Gaussian fitting. ... The line [O II ] 3727 ? ... For all spectra, the individual emission line fluxes of the H , [N II ] 6548,6583 ? ...

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• Reduction of long-slit spectra
• Optical spectroscopy
• Background Estimates

Next: SAS processing Up: Maintenance procedures Previous: Maintenance procedures Contents . Suitable observations should be longer than about 20 ksec, cover all the considered time period, and have different background levels, in particular the highest ones, so the sample should include observations taken at the beginning and end of the science window. It is helpful to consider objects for which no RGS spectrum is expected or to look at the RGS monitor pages. ... Michael Smith 2011-09-20 ...

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• Maintenance procedures
• Combination of the selected observations to make the templates and build CCFs
• Description

... Flux density at 1 GHz (/Jy): 19 . ... Notes: This is the remnant of the SN of AD 1006. ... Optical: Filaments to the NW, with broad H component. ... Point sources: The background Schweizer Middleditch star is near the middle of the remnant. ... van den Bergh 1976, ApJ, 208, L17. Optical observations. ADS . ... X-ray spectroscopy. ... Schweizer & Middleditch 1980, ApJ, 241, 1039. ... Optical spectroscopy of the Schweizer Middleditch star. ... Optical spectroscopy. ... 2013, A&A, 552, A9. ...

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• G263.9-3.3
• G189.1+3.0

Next: Infrared Imaging Data Reduction Software and Techniques . ... Economou, F., Jenness, T., Cavanagh, B., Wright, G. S., Bridger, A. B., Kerr, T. H., Hirst, P., & Adamson, A. J. 2001, in ASP Conf. ... ORAC-DR is a flexible and extensible data reduction pipeline suitable for both on-line and off-line use. ... The ORAC-DR pipeline design was presented previously by Economou et al (1998) and Jenness & Economou (1999) and makes extensive reuse of existing data reduction packages (Economou et al. ...

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• PICsIM - the INTEGRAL/IBIS/PICsIT Observation Simulation Tool for Prototype
• ADASS 2003 Conference Proceedings
• Automated Software for Slitless Spectroscopy Analysis and Quasar Selection

... Background scans are automatically loaded with the get_data procedure, but can be manually loaded, for example after computing the biases when the background has been zeroed before, using the following procedure. get_bgdata Backgroundtable created. ... We flag these data manually (just plot channel 11 and then use Util|Edit to flag; re-plot to check whether all the data has been flagged); when OYSTER averages point data, any data without valid background scans will be discarded. ...

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• Help for Night Report / Progress Pages
• ESO - Thesis Topic: Foreground emission and Cosmic Microwave background
• GOODS

Next: stecf.impol - an IRAF Up: The ``stecf" IRAF Layered Previous: stecf.nictools - NICMOS GRISM . Slitless is an IRAF task originally written to allow the ``quicklook" extraction of spectra from STIS direct/grism HST image pairs. ... Optionally, a Data Quality image extension can be used to avoid extracting flagged pixels. Slitless is configured to work primarily with the STIS G750L grism mode, but more modes can be defined by the user using a simple grism dispersion configuration file. ...

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• ST-ECF Grism Spectrum Software for NICMOS Grism Data
• NICMOS and the VLT: A New Era of High Resolution Near Infrared Imaging and
• NICMOS Data Calibration and Analysis

... A1767 Date Received: 2003-Feb-03 23:27:54 Technical Page Proposal Type: Regular General Category: Astronomy Sub-Category: Spectroscopy Observation Category: Galactic Total Time Requested: 27 Hours Proposal Title: HI and H 2 CO Observations of IVCs with Strong Continuum Background Sources ABSTRACT: We propose the mapping at 21cm of a sample of Intermediate-Velocity Clouds (IVCs) that have been selected because they are compact and have strong continuum background sources along their lines of sight. ...

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• Standard On

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. ...

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• Spatial Corrections of ROSAT HRI Observations from Wobble-related Aspect
• The Diffuse X-Ray Background
• Background Corrections

... Copyrightї1997 Bob Yen (byen@ix.netcom.com) (http://www.comet-track.com/hb/hb.html) . ... Information on Comet Hale-Bopp for the Non-Astronomer Hale-Bopp rotates about twice a day (3/14/97) . ... The Comet Observation Home Page was been selected to receive the Griffith Observatory Star Award for the week of February 2 - 8, 1997 for excellence in promoting astronomy to the public through the World Wide Web. ... Typically, about 1,000 individual users/computers access this page every day. ...

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An astronomer by training, I currently work at the Australia Telescope National Facility , part of the CSIRO . I am part of the computing group for the Australian Square Kilometre Array Pathfinder (ASKAP), where my job is to develop science analysis software for the ASKAP processing pipeline. The huge volumes of data that ASKAP will produce mean that all observations will be processed automatically in pipelines. ... Matthew Whiting . ... Australia . ... Matthew.Whiting <at> csiro.au . ...

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• lbaops:lbamar2008:v255a [ATNF VLBI Wiki]
• VLBI Wiki | LBAMar2008 / V255A
• Recording Systems History and Background

... Figure 8: Can you detect the motion of the near-Earth asteroid 2000PH against the background stars during its close approach to Earth around 27 July 2004? ... Down) observed and imaged the unusual near-Earth asteroid 2000PH during its close approach to the Earth around 27 July 2004. The observations were carried out remotely using the new 2m aperture Faulkes telescope situated on the 10,000-foot summit of Haleakala, on the island of Maui in Hawaii. ...

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• Observations and Data Reduction
• An Overview of the Coupled Earth-Sun System PPARC Introductory Solar System
• Historical Background

Twilight observations with MASS/DIMM B. Safonov Sternberg Astronomical Institute Moscow State University Comprehensive Characterization of Astronomical Sites, 2010 B. Safonov (Moscow State University) Twilight observations with MASS/DIMM SITE 2010 1 / 17 Why observe in twilight with MASS/DIMM? ... ASM includes 3 devices sensitive to background: guider, DIMM and MASS. B. Safonov (Moscow State University) Twilight observations with MASS/DIMM SITE 2010 2 / 17 Background in guider. ...

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. Previous slide . Next slide . Back to first slide . View graphic version .

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• Siding Spring Survey
• COALA - Computational Astrophysics Laboratory

Next: Gravitational Wave Background from Previous: Galactic Gravitational Wave Background . ... It is intuitively clear that at frequencies above the critical ones for our Galaxy, one will detect rare bright jerks produced by coalescing white dwarfs   (at a rate of 1 per 100 year) and NS (at a rate of 1 per - year) in our Galaxy, against a background of the extragalactic stochastic GW. ... Firstly we consider GWB from close individual galaxies, and then will discuss overall extragalactic GWB. ...

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• Critical Frequencies and Gravitational Wave Detector Halfwidth for
• fields
• AXAF-Chandra

... 2.3 Establishing the Extragalactic Distance Scale . ... 2.3.2 The Second Rung: Distances to stellar clusters . ... 2.3.4 Distances to Local Group Galaxies . ... The Luminosity Function of Planetary Nebulae . ... 3.2.2 Clusters of Galaxies . ... 4.2 Evidence for Dark Matter as a Function of Scale Size . ... 4.3 Other Dark Matter Indicators for Galaxies . ... What is the nature of the large-scale distribution of matter in the universe as traced by the three-dimensional galaxy distribution? ...

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• Thermal History of the Universe
• Foundations of the Big Bang
• Physics 410/510 Observational Cosmology

. Departement of Quantum Astrophysics . Head: Kurt V.G. , Prof. ultraviolet spectroscopy of planetary upper atmospheres and interplanetary/interstellar medium; . observations of gamma-bursts and optical identification of their sources; . long-base optical interferometry. Staff: .

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• DPC Post-Observations Products
• Description of the RadioAstron project, english version
• Appendix B: Map of the Document

... MOUSER Over View . The design of a new generation fast spectrograph MOUSER (Multi Object Universal Spectrograph for Extragalactic Research) to be installed at the 6 m telescope is proposed. ... photometric observations in broad and narrow spectral bands with a 6'x6' field of view and an image scale of 0".30/pixel; . ... The spectrograph is to be installed on the field rotator of the 6 m telescope prime focus without a standard field corrector. ... Back to Laboratory Home Page . ...

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• A. Moiseev's scientific interests
• On the problem of high spectral resolution observations of faint objects
• The spectrograph design and the observing procedure

RTT150 . ... HEAD IKI . This page is a search interface through RTT150 observationsdatabase which is stored at IKI. According to the agreement between participantsof RTT150 project, observational data fully belong to the institution which hascarried out this observation for one year, are available to all three partiesinvolved (IKI, KSU and TUG) during the second year and become freely accessibleto the whole astronomical community starting two years after observation date. ...

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• GRANAT Home Page
• Observations of gamma-ray burst afterglows with RTT150 telescope