... 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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• High-resolution Herschel spectroscopy reveals the proto-planetary disk around
• Algorithm
• Descrizione tecnica NICS

... HST . Using Multiple FP-POS positions with COS observations . ... Data . ... HST Peer Review Process . ... HST Overview . Overview . ... Phase I Proposing . ... Retrieving HST Data . ... COS Data Handbook . ... The use of multiple FP-POS positions for each CENWAVE position of the COS FUV detector was strongly encouraged in the Cycle 19 Call for Proposals, Primer, and COS Instrument Handbook, as this improves the limiting S/N and allows the effects of flat-field artifacts to be minimized. ...

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• Fine Guidance Sensor Instrument Handbook
• CCD Position and Orientation on Sky
• COS FUV Spectra Shifted to New Lifetime Position.

Next: Primary Catalog Up: Observations and Analysis Previous: Source Positions . ... This energy selection allows direct comparison with previous EGRET, COS-B and SAS-2 results. ... The energy spectra shown in the catalog are taken largely from previous EGRET publications (or those currently in the publication process), which discuss the details of source identifications, time variability, and energy spectra. ... Such sources are identified in the catalog. ...

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• Source Positions
• Results and Discussion
• Optical spectroscopy

... Advises . Contact Advises . As an advise for amateurs we would like to underline: if it's possible, try to observe 3 asteroid positions per night and do not neglect to observe the Numbered Minor Planets in your telescope field of view as a "by product" of your observational programs. ... We think such estimations ought to be produced every morning after CCD observations of the moving celestial objects by observer himself. ...

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The software package ERA (Ephemerides for Research in Astronomy) is a problem-oriented software system for solving heterogeneous calculating tasks of Ephemeris and Dynamical Astronomy. The package makes it possible to produce ephemeris calculations needed for both planning various observational programs and processing the resulting observations. ... The system includes packages of processing the position observations by both the Least Squares Method and by Kalman filtering. ...

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• (Untitled)

CONSTRAINING LONG-TERM AND SPATIAL VARIABILITY OF THE PN LOW ENERGY RESPONSE WITH RXJ1856 (IUSS Pavia; INAF, IASF-Milano) In collaboration with: N. Sartore, S. Mereghetti, A. De Luca, R. Turolla, F. Haberl Andrea Tiengo RX J1856.5-3754 (RXJ1856) Brightest of the "Magnificent Seven", or X-ray Dim Isolated Neutron Stars (XDINSs) (e.g. Turolla 2009 f or a review) The closest known neutron star: d ~120 pc (W alter et al. ... 2011) Why studying RXJ1856 variability? ...

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• Description
• Generation from In-Orbit Data

Proposal Identi cation No.: A1864 Date Received: 2004-Sep-30 15:58:29 Technical Page Proposal Type: Regular General Category: Astronomy Sub-Category: Spectroscopy Observation Category: Galactic Total Time Requested: 30 Hours Proposal Title: Mapping OH Emission near OH Zeeman Positions ABSTRACT: We were granted approximately 500 hours for Zeeman e ect observations of 1665 and 1667 MHz OH emission lines from molecular cloud cores (project a1457). ... X Maybe Part of the observing run. ...

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• ON/OFF (Position Switching)
• AO Spectral Line Position Search Database.

... Flux density at 1 GHz (/Jy): 130 . ... X-ray: Brightest to the E. Point sources: Central possible pulsating X-ray source. ... Molonglo at 408 MHz (3': S=198?20 Jy). ADS . ... 1982, ApJ, 258, 22. Einstein observations. ... IR observations. ... Possible pulsation detection from central X-ray source. ... X-ray observations of central source. ... ATCA at 1.4 GHz (90'') for H I near central X-ray source. ... Chandra observations of E edge. ... Chandra proper motion study of central X-ray source. ...

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• G327.6+14.6
• G189.1+3.0
• G292.0+1.8

Program: TRACE Purpose: TRACE plots image values at user given positions as function of distance to a plot centre (in 2-d (sub)sets). Category: ANALYSIS, PLOTTING File: trace.c Author: M.G.R. Vogelaar Keywords: INSET= Give set (, subset): Only one subset is allowed. ... XYBOX= Give size of box around one pixel: [3,3] The resulting value at a selected position is an average of the pixels in the defined box around that position. ... POSITION= Give position x, y: Physical values are allowed. ...

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• Archive of VLBI Observations Majordomo List

The close position of main satellite and subsatellite (distance between them about 1000 km) and using the similar sets of Faraday cups (VDP and VDP-S) with high resolution measurements (up to 16 Hz for the main satellite and up to 10 Hz for the subsatellite) allow us to determine the small-scale variations of the magnetopause shape and position and to estimate the velocity of the magnetopause motion. ... Two point observation of the magnetopause motion: the INTERBALL project. ...

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• Lagrangian Points
• Satellite position in the SE and GSM coordinate systems
• Events on January 10-11, 1997 - INTERBALL observations

True Color Image Gallery: Galactic SNR | Magellanic Cloud SNR . ... Description: large, diffuse, X-ray and radio brighter in northern half . Radio . ... Radio Images Page . ... Exposure uf . ... Exposure uf Exposure time of unfiltered event file . Exposure f Exposure time of filtered event file . ... Event 2 FITS File . ... AUX file . ... 0.3 - 10.0 . ... see fit detail page for more about the fit. see chandra spectrum page for region used. ... True Color Image . ... Radio Images . ...

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• Chandra Images for SNRJ 0540.1-6919
• Chandra Images for G189.1+03.0C
• Chandra Images for G309.9-02.5

... In order to maximise the information which may be extracted from the PICsIT data, we have designed a prototyping environment which consists of a GUI to a highly structured and modular set of procedures which allows the easy simulation of observations from the data collection phase through to the final image production and analysis. ... The PICsIM simulation tool is written entirely using the IDL 1 language and runs under both Windows NT and Linux operating systems. ...

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• Robust Data Analysis Methods for Spectroscopy
• Calculating the Position and Velocity Components of HST
• Identification and Analysis of Binary Star Systems using Probability Theory

... Over the course of a week two secondary students James Hadnett and Liam Fields observed NEAs using one of two 2-Metre telescopes courtesy of the Faulkes Telescope Project which are positioned in the Northern and Southern Hemisphere. This was made possible with the aid of Las Cumbres Observatory who, with their Global Telescope Network, give educational establishments the chance to observe with a high grade telescope. ... Comet C/2012 F6 (Lemmon) observed on 2013 July 1st. ... 2013 July 5th . ...

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• Armagh Observatory
• Postgraduate Positions
• Observations with the Faulkes Telescope North

Computer Ephemeris for 2014 from DE200/LE200. Longitude of central meridian of Uranus. ...

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• Central meridian positions for physical observations of Saturn for Computer
• Central meridian positions for physical observations of Neptune for Computer
• Lunar physical observations. Explanations for Computer Ephemeris.

Large-Scale Structure of the local Universe with INTEGRAL observatory >200-300 , . ... It is now widely accepted, that practically every galaxy in the local Universe has supermassive black hole and some of these black holes are AGNs. ... 136 ( ) 49- . ... The map of the survey is shown on the left. ... Using Hard X-ray all-sky survey such important properties of nearby Universe as energetics of accretion to the supermassive black holes and large-scale mass distribution of matter were studied. ...

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• http://hea.iki.rssi.ru/integral06/papers/D32_Khamitov01-04Oct06_10:26:31.pdf
• http://hea.iki.rssi.ru/integral06/papers/E30_Karasev01-27Mar07_15:40:32.pdf
• http://hea.iki.rssi.ru/integral06/papers/J33_Segreto01-28Mar07_22:36:14.pdf

... With enough velocity, a spacecraft can break loose from the Earth's gravity and enter an orbit around the Sun, like that of a planet. If it then orbits the Sun with the same period as the Earth--one year--it may keep a fixed position relative to Earth. ... If the distance is just right--about 4 times the distance to the Moon or 1/100 the distance to the Sun--the spacecraft, too, will need just one year to go around the Sun, and will keep its position between the Sun and the Earth. ...

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• Saturn's Possible New Moons
• Carrington's Flare
• The Wind Spacecraft

.

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• Astrometry

Natural Satellites Service. ... Apparent Encounters . of the Tycho-2 Catalogue stars and the main natural planetary satellites . ... Suggestions . ... Here we present the precalculated circumstances of the apparent encounters of the stars of the Tycho-2 Catalogue with the main satellites of Saturn (S1-S8) for the period from November 2004 to February 2010, and with the Galilean satellites of Jupiter for the period from November 2004 to October 2010. ...

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• jg0007
• jg0008
• jo0053

... 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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• http://zebu.uoregon.edu/2003/hum399/brahesum.html
• http://zebu.uoregon.edu/~uochep/talks/talks03/lscv2.pdf
• Orbital Properties of the Solar System

Pulkovo NEO Page . ... NEA Accuracy Estimation . ... The estimation of accuracy of the current CCD observations of asteroids and comets is constantly performed at Pulkovo Observatory. ... The (O-C) values, so called "Observed" minus "Calculated" positions, characterize numerically the observations of any observatory, both professional and amateur, during a short period (one or several close nights). ... So the (O-C) values for these objects nearly entirely define the errors of observations. ...

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• Pulkovo NEO Page: Apparent Close Approaches to the Stars
• Pulkovo NEO Page: Ephemeris Support
• Pulkovo NEO Page: Estimation of Observational Accuracy