... 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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• Flat Fielding GPI Data Pipeline 1.0 documentation
• Persistence GPI Data Pipeline 1.0 documentation
• Initial Hypotheses

... 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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Home . ... Observing . Exposure Time Calculator (ETC) . Survey processing . ... ESO - Public Surveys . near IR surveys . ... Exposure Time Calculator . ... Survey Area Definition Tool . Recommended values for Detector Integration Time (DIT) . ... Detector Properties . ... Filter properties . ... ESO ][ VISTA Home ] ...

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• VISTA ETC - Exposure Time Calculator
• VISTA Integration Time DIT Recommendations
• VISTA - Visible and Infrared Survey Telescope for Astronomy

... We will consider the rms, (K), for observations with a receiver of system temperature, T , frequency resolution, per polarization, and total integration time per observing cycle, . ... For ``in-band'' frequency switching, the line under investigation is always in the observing band. ... Position Switching or ``Out-of-Band'' Frequency Switching: Here the line is only observed for one half of the time, with noise being present all of the time. ...

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• CIMA Auto-Observing
• Spectral Line Observations at AO
• INTRODUCTION to Spectral Line Observing at AO

These observations are aimed at fully charactering FORS1 photometric system (UBVRI zero-points, color-terms and extinction coefficients) for the Tektronix 2048x2048 pixel CCD (24µm px) . To this aim, the two Landolt/Stetson photometric fields SA95 and SA101 will be observed on a number of epochs and at different airmasses during February and March 2007. ... SA101 . ... OBs for SA101 have to be observed during evenigh twilight (exceptions are expected for the second half of March) . ...

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• ESO - Thesis Topic: Foreground emission and Cosmic Microwave background
• ESO - Guaranteed Time Observations
• ESO - How do I find out the exposure time for a given observation?

... You are here: start €Ё lbaops €Ё lbamar2008 €Ё v255a . ... VLBI Schedule . ... Observer's Wiki . ... Other VLBI . ... lbaops:lbamar2008:v255a . V255a Setup: . ... Channel 1 . IFP#1-LO 6641 - 6657 MHz USB RCP . ... Ftp: ftp://ftp.atnf.csiro.au/pub/people/vlbi/v255/v255a . ... For Hobart the LOs should be set to 468 MHz (IFP#1) and 809 MHz (IFP#2) for the 4 x 16 MHz setup and 809 MHz for the 2 x 16 MHz setup. ... lbaops/lbamar2008/v255a.txt €§ Last modified: 2015/12/18 16:38 (external edit) . ...

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• VLBI Wiki | LBAMar2008 / V255A
• PPTA Wiki | Observing / Details
• VLBI Wiki | LBAFeb2009 / V255D

... Galaxies 99 Cosmic background with model of cloudy interstellar medium Yu. ... Figure 1: Averaged spectrum of the cosmic background I f in frequency range 0.25 200 MHz for the Galactic poles. ... First interpretation of the cosmic noise background spectrum at broad band frequency range 0.25 200 MHz with a model of the cloudy interstellar medium ISM is presented here. ... Synthesized background spectra I f for regions of the Galactic poles at the frequency range 0.25 200 MHz is presented in Fig. ...

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• Pulkovo NEO Page: Estimation of Accuracy of the Observations
• Pulkovo NEO Page: Ephemeris Support

... In the three intervening decades there have been many observations of this diffuse emission over a wide range of x-ray energies. ... During the 1970's researchers at the University of Wisconsin, lead by Dr. William Kraushaar, used a series of sounding rocket flights to map the diffuse x-ray emission from the sky in several bands. ... University of Wisconsin Sky Survey map of the B-band (0.13-0.188 keV) x-ray intensity. ... University of Wisconsin Sky Survey map of the 2-6 keV band x-ray intensity. ...

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• Infrared Data
• Champlane Observation: Magellan/IMACS June 6-9, 2005
• Chandra Images for G184.6-05.8

... The R , I photometric observations of SBS 0335-052W were obtained occasionally during the study of SBS 0335-052 with the 3.5m telescope in Calar Alto on 1991 October 6. ... Aperture photometry was performed on the standard star observations using MAGNITUDE/CIRCLE task with the same aperture for all stars. ... For photometry of extended objects, we used the package SURFPHOT as well as dedicated software for adaptive filtering developed at the Astrophysical Institute of Potsdam (Lorenz et al. ...

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• The GB/NAIC 5GHz Survey
• Optical spectroscopy
• The sample description

... 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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• Mutual Events of the Uranian Satellites
• Observations with the Faulkes Telescopes
• First CCD Observations of Asteroids from Armagh

. Next: Ground calibration Up: RGS_TEMPLATEBCKGND Previous: Purpose Contents . Background spectrum templates are accumulated in intervals of background rate. A background spectrum for an individual observation is then synthesised from a combination of the templates weighted according to the variations of the observed background rate. Michael Smith 2011-09-20

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• XMM-Newton Further EPIC Background Scripts
• XMM-Newton OM Response Files Page
• XMM-Newton Current Calibration Files

... They are concerned with Attitude Control System of the spacecraft, satellite visibility from tracking stations, limits on the satellite autonomous operations during the orbit, and needs for auxiliary operations with the spacecraft. ... Among the operational constraints the most important one is the number of programmed slews per orbit, which determines the maximum number of radio sources to be observed during one orbit. ... System temperature (K) . ... Progress of the RadioAstron Project in Pictures...

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• RSOG Pre-Observation Products

... Here some data observed on the 6m telescope with IFP installed in the OLD focal reducer are presented. ... Mkn 3: velocity field . ... NGC 5252: [OIII] image . ... NGC 5252 was observed 23 Feb. 1998 in the [OIII]5007 emission line with CCD TK1024 as detector. ... We observed the ionized gas velocity fields of the spiral galaxies with two purpose. ... Restored velocity field of NGC 157 in the reference frame rotating with the pattern speed overlaid on the Ha image of the galaxy . ... NGC 4100 . ...

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• Observational data
• Observations and spectra reduction
• Emission molecular bands

The problem of solar wind data correlation for the observations onboard several spacecraft is very important for three points of view: . ... This problem is studied now in detail by systematic determination of ion flux and ion velocity data correlations by INTERBALL-1 (IKI group), WIND and IMP 8 (both - MIT group). ... Solar wind plasma correlation lengths from IMP 8, WIND and INTERBALL-1. ... Correlation of solar wind observations onboard several spacecraft: INTERBALL-1, IMP 8 and WIND data. ...

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• Spacecraft Observing the Sun and the Heavens above
• Interball Workshop Posters
• Events on January 10-11, 1997 - INTERBALL observations

Next: NICMOS/HST H-band (F160W) Images Up: NICMOS Science Previous: HST NICMOS Observations of . ... Observations of P . ... The NICMOS team has devised a comprehensive program of observations of the Galactic Center. ... Data in hand give a first look at variability and a detailed look at the search for the tip of the main sequence will be discussed where NICMOS has demonstrated adequate sensitivity and photometric precision to identify likely O8-B1 stars at the Galactic Center. ...

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• The Old Stellar Population of NGC 1569 from NICMOS data
• NICMOS/HST H-band (F160W) Images of the 30 Dor Starburst Cluster
• The STScI NICMOS Calibration Pipeline

... The Stellar Oscillations Network Group (SONG) seeks to study p-mode (acoustic) oscillations in solar type stars. ... The observation of many solar-like stars will also help us to understand how solar p-modes are excited and damped. ... Naively, the two or three orders of magnitude improvement over this provided by the normal 1 second time resolution of the KPNO CCD cameras should be quite sufficient for such a detection. ... Figure: Non-cadenced data-a free-running observing sequence. ...

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• NICMOS Calibration Pipeline: Processing Associations of Exposures
• NICMOS Software: An Observation Case Study
• Organizing Observational Data at the Telescope

GRANAT is the Russian x-ray sattelite launched to the high apogee orbit (200,000 km) and operated almost for 10 years (1989 -1999) , carrying out four major instruments: French SIGMA coded-mask hard x-ray telescope (30-1000 keV), Soviet ART-P coded-mask telescope (2??-60?? keV), all-sky monitor WATCH (6-150 keV), and a gamma-burst detector PHEBUS . ... Since September 1994, GRANAT is in the survey mode. ... Explore pages devoted to individual GRANAT instruments (including main scientific results): . ...

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• Fast search through RTT150 data archive
• RTT150 telescope: GRB 051028

We report here on those proposed UIT targets that, in fact, were successfully acquired. Where possible we provide an optical CCD image of the target or the field. Note on Filters: . A1 centered at 2500 angstroms with a width of 1200 angstroms . ... UGC 5675 is another Low Surface Brightness galaxy which is the center of the fourth deep A1 field. ... M32 a very high surface brightness dwarf elliptical companion was observed for 1561 seconds through the B5 filter. ...

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... In order to compare the number of different evolutionary stages obtained and X-ray luminosity of the chosen X-ray sources with the observed galactic values we use the sum of C/O+O/C , where C and O are the calculated and observed values of a given binary type, respectively. If we make comparison for a number of different binary species (for example, we compare the number of CV, number of X-ray pulsars,   total X-ray luminosity of LMXB, etc.), we write this criterion in the form: . ...

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• Galactic Gravitational Wave Background
• Extragalactic Gravitational Wave Background
• Transparency of the Stochastic Background

Program Id: . ... UTC End Time: . Astronomer/PI Name(s): . ... Observer Name(s): . Nightlog Day: Sunday Monday Tuesday Wednesday Thursday Friday Saturday Month: January Febuary March April May June July August September October November December Day (DD): Year (YYYY): Full Night A (First half) B (Second half) Special Schedule . ... Note: Open this weather logfile program in another browser window. Please copy and past the resultant info below at the end of the night) . ...

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• Observers Instructions for filling out the ARCSAT nightlog
• Spectrographic time budget
• APO Job Announcements