... Surface Brightness of Background Light . Home . ... Data . ... WFPC2 Home . ... Instrument Home . WFPC2 History . ... LRF Data . ... Data Analysis Home . ... Instrument Handbook . Data Handbook . ... Input the surface brightness in magnitudes per square arcsecond. ... Galaxy U-B and B-V colors are drawn from Longo and deVaucouleurs 1983 for representative objects;V-R and R-I are estimated from WFPC2 Handbook Table 6.1. ... AB_xxxxx are AB magnitudes at the standard WFPC2 filter bands. ...

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• Sky Background
• Surface Brightness
• WFPC2 Instrument Handbook Update

... 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. ...

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• Automated Software for Slitless Spectroscopy Analysis and Quasar Selection
• Refining the Guide Star Catalog: Plate Evaluations
• ADASS 2002 Conference Proceedings

XMM-Newton Science Analysis System . ... A different approach is done via the setting withctisrcpos =Y: all event energy corrections do not use the actual RAWY coordinate but the corresponding RAWY location of the source ( SRCPOS ) as determined by the task epframes (either automatically or via setting withsrccoords =Y). ... The task epchain may be used with the setting ccds =4 withctisrcpos =Y to process only the CCD 4 where usually the bright source is located that causes the Out-of-Time events. ...

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• The contour method of calculating source region shape

. Please standby and you will be automatically connected to the new location of the unframed Supernova page. Or, click on the link above. If you have questions or problems, please email me at David Bishop dbishop@vhdl.org . Last modified: Mon Aug 27 12:40:15 EDT 2001

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• Bright Supernova Bright Supernova - links

... User Guide ] Task: moment Purpose: Calculate moments of a Miriad image. ... Key: in The input image. No default. ... Key: mom -3: Velocity at peak intensity using a three-point quadratic fit around the peak (km/s). 2: Peak intensity using a three-point quadratic fit (units same as individual channels). ... The moments are calculated independently for each pixel using spectral channels with intensity satisfying the specified clip range. ... Key: axis Axis for which the moment is calculated. ...

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• The HIPASS Bright Galaxy Catalog
• The HIPASS Bright Galaxy Survey

In this gallery are many images of Low Surface Brightness Galaxies which have recently been discovered and analyzed. ... The central surface brightness of this galaxy is 24.28 . Malin 2 This galaxy is another huge disk galaxy with a scale length of 15 kpc and a redshift of 15000 km/a. The high surface brightness knot in one of its spiral arms actually has the same color, luminosity and H-alpha equivalent width as the entire Large Magellanic Cloud . ... Truly it is a Low Surface Brightness Galaxy. ...

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• Galaxy Gallery Page III

... We present the ROSAT All-Sky Survey Bright Source Catalogue (RASS-BSC, revision 1RXS) derived from the all-sky survey performed during the first half year of the ROSAT mission in 1990/91. 18,811 sources are catalogued, with a limiting ROSAT PSPC countrate of 0.05 cts/s in the 0.1-2.4 keV energy band. ... Broad band images are available for a subset of the flagged sources. ... Retrieving the full catalogue The ROSAT All-Sky Survey Bright Source Catalogue can be retrieved via your WWW browser: 1. ...

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• The Parkes 6 cm Galactic Survey
• HyperLEDA documentation: compilation of surface brightness (a105)
• HyperLEDA documentation: parameter: bt

The ESA/ESO Astronomy Exercise Series 2 . The Distance to Messier 100 as Determined by Cepheid Variable Stars . ... The small variations in distance to the individual Cepheid variable stars in the Cloud are negligible compared with the much larger distance to the SMC. ... In this way Cepheid variable stars can be used as one of the 'standard candles' in the Universe that act either as distance indicators themselves or can be used to calibrate (or set the zero point for) other distance indicators. ...

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• ASP: Star Science in the Autumn Sky
• ASP: Monster Comet Promises Big Show
• ASP: Accidental Astrophysics: The Devil's In the Magnitudes, Part II

Next: Photometry Up: Regions and Source Parameters Previous: *imcnts* - Find counts . This task (developed for use with optical images, but also useful with x-ray data) will quickly compute location, size, ellipticity, and position angle of sources. ... User can generate contour plots of any portion of the image and count rates in slices through the image. The program is advertised as ``quick [optical] photometry''. input file: rp110590_im1.imh . output file: logfile . ... Photometry . ...

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• Notes on IPC and PSPC Spectral Fitting
• Spatial Analysis
• Radial Profiles and Projections

Sternberg Astronomical Institute, Moscow University, . Moscow, Russia . Supernovae make us brighter .. Search russian astronomical resources . Mirror of International Supernovae Network ( Original site ) . Catalogue of Supernovae Stars . HTTP access to SAI Catalogue of Supernovae Stars . SAI SN Light Curves Online . ... Sternberg Astronomical Institute ( in Russian ) . ... Astronet - Russian Astronomical Network . ... Russian Foundation for Basic Research . ...

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• Creating a watermark effect
• Bright Sn in NGC 3877
• SN 1989B Light Curve Analysis.

... They worked out that first magnitude was on average 100 times brighter than the 6th magnitude star. ... This formed an equation of apparent magnitude Mv which is: Mv = -2.5 log f + constant were f is the flux of that star f = ( counts/ exposure) The images that we worked on were taken by the Polar Bear Telescope. ... One of these being that it will be combined with standard stars, which will be used to identify the area of stars and to also help identify other stars within the image. ...

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• Coronal Bright Points: Another Oscillating Environment
• Bright Point Studies
• HISTORICAL BACKGROUND

... Satellite data ] . SMIS ] . The program is designed to process the specific AVHRR instrument data for calculation and analysis of temperature fields on the sea surface and upper level of clouds. It performs brightness correction for visible channels with regards to clouds altitude. ... The program features a wide variety of classification algorithms (including two-dimensional histogram analysis) and enables to construct personal procedures for classification. ... Back to SMIS Home Page . ...

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• XV-IMAGE

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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• http://site2010.sai.msu.ru/static/doc/VOrlov_site2010.pdf

The Cosmic Microwave Background Radiation Temperature Work in groups of 2-4. ... Due 1999 April 15 In this laboratory exercise, you will use the radio telescope on the roof of Science B to measure the intensity of the Cosmic Microwave Background Radiation (CMBR). ... The output of the telescope when pointing at the sky will then be 2 Tsys = Trec + Tsky : The temperature of the sky can in principle arise from two sources, radiation from the atmosphere and radiation from outer space (the CMBR). ...

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• HISA Poster for the 197th Meeting of the AAS, January, 2001
• HISA Science Overview
• Shades and Apparitions: Toward an Inventory of Cold Hydrogen Clouds

... LMC Project Outline . NGC 1818 Initial Results . ... The Large Magellanic Cloud (LMC) is uniquely suitable for the study of massive star clusters at all stages of evolution. By combining HST observations of these clusters with N-body models we hope to understand the origin and evolution of rich star clusters in our own Galaxy, in the LMC, and beyond. ... We aim to combine our HST observations with N-body models to understand the formation and evolution of globular clusters. ...

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• NICMOS Data Calibration and Analysis
• The Stellar Population in the NICMOS Parallel Fields
• ST-ECF Grism Spectrum Software for NICMOS Grism Data

New reduction of minor planets photographic plates obtained with Pulkovo Normal Astrograph A.A. Berezhnoy Pulkovo Observatory of RAS, Saint-Petersburg, Russia Minor Planet observations at Pulkovo Periodical observations of 14 bright asteroids named Selected Minor Planets (SMP) were performed at Pulkovo since 1948 within the international framework started by works of B.V. Numerov and D. Brouwer. ... 108 133 113 74 124 67 97 88 14 84 64 5 20 19 Epochs (YYYY.MM) 1200 Mean values of total obs. ...

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... The Galactic low-mass X-ray binary GS 2023+338 was discovered during the burst on May 22, 1989 with the Japanise satellite Ginga (aka Galaxy). The flux reached 17 crabs (this unit of flux measurement is an bright X-ray source, Crab Nebula) at 10-35 keV. ... No other radio telescope worldwide carried out multi-frequency measurements. ... Upon 14 days the radio flux fell below the detection level at the RATAN-600 in relation to the decrease of the X-ray flux. ...

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• Solar system sector, archive 2006
• Galaxy sector, archive 2004
• Metagalaxy sector, archive 2000

Definitions of Magnitudes and Surface Brightness 1 The magnitude system 1.1 Apparent magnitude Astronomers are stuck with the antiquated old system of magnitudes and so a clear explanation of what this system is and how it relates to more sensible units is important. ... 1.2 Absolute magnitude Absolute magnitude is a logarithmic luminosity scale. ... One usually goes by the round about process of referring to the absolute magnitude of the sun. ... Magnitudes and surface brightness 6/6 ...

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• Sky Brightness
• Siding Spring Survey
• Blue Straggler Stars

... Science . ... Science Users Information > Data Handling and Products > Data Reduction FAQ > How can I run the pipeline when there are no bright objects in the individual image? ... Observing with ESO Telescopes . ... The default use of the visir_img_combine recipe of the VISIR pipeline is with the "ref" option set to false. ... The VISIR pipeline will create the combination of the nodded images using the ESO SEQ CUMOFFSETX and ESO SEQ CUMOFFSETY offset information in the fits file headers. ...

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• ESO - Final Data Release of zCOSMOS-bright Redshift Survey
• The Brightness of the Night Sky
• ESO - My data shows an extended, bright feature - what can this be?

... X Ray Moon . ... In this digital picture, pixel brightness corresponds to x-ray intensity. Consider the image in three parts: the bright hemisphere of the x-ray moon, the darker half of the moon, and the x-ray sky background. ... Still, the few x-ray photons which seem to come from the moon's dark half are currently thought to be caused by energetic particles in the solar wind bombarding the lunar surface. ... Publications with keywords: Moon - X-ray - cosmic rays - x-ray background . ...

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• Астронет > X Ray Moon
• X-Ray Moon
• Saturn: Bright Tethys and Ancient Rings