... A SPYBAL is executed to center the spectrum in the cross-dispersion (or GHRS ydirection) on the diode array. ... A SPYBAL actually produces science data consisting of a wavelength calibration exposure. ... This means that as long as the grating does not change, no new SPYBAL will be inserted, unless one has several exposures and the total alignment time (not real orbital time) exceeds 90 minutes. ...

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• Polarization Observations
• GHRS Observations of Diffuse Clouds in the Local Bubble
• HST Spectral Maps of Accretion Disks in Cataclysmic Binaries

... Up: Proposal Processing . ... ESO is prototyping a distributed ``Phase II'' system that will allow astronomers to prepare their observations at their home institutions, while maintaining a central repository for all observation data. ... ESO is developing a Phase II Proposal Preparation system (P2PP) to collect detailed scientific programme descriptions, in the form of observation blocks (OB). ... ESO's Phase II Proposal Preparation system is an integral part of the VLT Data Flow System (DFS). ...

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• Distributed Software for Observations in the Near Infrared
• ETCs and Observations Simulation at the VLT
• VLT Data Quality Control

... The most precisely determined characteristic for accreting neutron stars (NS's) is their period. ... Period changes show fluctuations. ... Some applications of stochastic processes in astrophysics especially in accreting systems were discussed in Lipunov (1987),Hoshino Takeshima (1993) and Lipunov (1992).In Hoshino Takeshima (1993) the authors, using simple models of MHD turbulence, try to explain aperiodic changes in X-ray luminosity of X-ray pulsars. ... Here, -constant angular momentum. ...

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• Initial Distributions of Binary Parameters
• State of the problem
• Old neutron star distribution in the Galaxy

Next: How to get Up: Introduction Previous: Introduction . ... However, we cannot make all our observations at the same time, or at the same place in the sky. ... To do this, we must distribute the observations so that the main independent variables (such as airmass, star color, and instrumental temperature) are uncorrelated with each other. ... As some (like temperature) are inherently likely to be correlated with time, it is doubly important that others (like airmass) be uncorrelated. ...

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• Equations of condition
• Introduction
• A 20 cm VLA survey of Abell clusters of galaxies

... The dayside auroral precipitation consist of magnetosheath related boundary layer precipitation, and plasma sheet related BPS/CPS precipitation (extensions of the nightside precipitation regions). ... For example, the much lower fluxes from the LLBL region when compared to the cusp are compensated by the bidirectional electron beams found in the LLBL: the precipitating energy fluxes in the LLBL and the cusp are not that different. ... directly through the cusp and plasma mantle . ...

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• Current Solar Wind Conditions
• Field-aligned potential drops [Oulu]
• Radar aurora [Oulu]

... Let us first find out which way -- rise in spectral resolution with some loss in the S/N ratio or increase in the S/N ratio with a fixed spectral resolution -- is better for the purpose of reduction of equivalent width determination errors. ... N -- number of counts for 1 ? ... line equivalent width, . ... Thus if the spectral resolution is managed to be increased (i.e. to decrease )without loss in the number of counts falling at 1 ?, the equivalent width measurement error is then proportional to . ...

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• Laboratory for the Stellar Magnetism Study of SAO of the RAS - Home
• Fabry-Perot Interferometer: Data cubes
• Emission molecular bands

Subject, Problems and Objects of Theoretical Astrophysics. ... Stellar Photospheres, Their Features. ... Physics of Continuous Radiation Absorption in Stellar Photospheres. ... Continuous Radiation Absorption in Stellar Photospheres of Various Spectral Classes. Solar Type Photospheres. ... Characterisics of Absorption Lines. ... Interstellar Absorption Lines, Their Features. ... Physical and Dynamic Features of Interstellar Medium, Which Follows from Observations of Interstellar Absorption Lines. ...

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• Extragalactic Astronomy
• Physics of Heliosphere
• General Astrophysics

... Posts tagged ?regularity condition? ... 3, 2007? Tags: identifiability , likelihood ratio test , mixture , regularity condition . ... Data-Driven Goodness-of-Fit Tests by L. Mikhail . ... ArXiv] Data-Driven Goodness-of-Fit Tests, Aug. ... Chi-square function, chi-square statistics, chi-square goodness-of-fit test are the words that serve different data analysis purposes but under the same prefix. ... Tags: chi-square , degrees-of-freedom , optimization , regularity condition , test . ...

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• Project Tanagra
• The AstroStat Slog Blog Archive [ArXiv] An unbiased estimator, May 29, 2007
• The AstroStat Slog Pareto distribution

Molecular Lines in Star Formation Regions ­ the ALMA Challenge Paul Jones University of New South Wales Universidad de Chile 1 Molecular Lines in Star Formation Regions - Molecular lines trace the kinematics and chemistry (composition) of molecular clouds. ... The lines also trace physical conditions such as temperature and density, complementary to mm/sub-mm dust continuum data e.g. ATLASGAL and ALMA continuum. ... Simple molecules (eg. ... More complex molecules (eg. ...

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• http://www.atnf.csiro.au/research/LVmeeting/magsys_pres/ruzicka.pdf
• OH_maser
• Reducing 3-mm ATCA observations

... Within SAS, a tool is available to check the pile-up fraction in the pn data: epatplot . This tool compares the observed pattern distributions (derived from a pn calibrated and concatenated even list) with the calibrated models. ... The lower panel is the key element for the evaluation of the pile-up fraction: it shows the observed distribution of pattern as a function of energy (PI channel in Analog-Digital Units ), using the same color code. ... Pages maintained by SAS librarian . ...

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• Selection of observations of empty RGS files
• Description

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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• http://site2010.sai.msu.ru/static/doc/Site2010-Summary.pdf
• http://site2010.sai.msu.ru/static/doc/AGusev_site2010.pdf

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 - Observing conditions: definitions
• Colours and magnitudes
• ESO - FLAMES Science Verification

... The Network Time Protocol (NTP) is used to synchronize the time of a computer client or server to another server or reference time source, such as a radio or satellite receiver or modem. ... Information on the NTP architecture, protocol and algorithms can be found in the Further Information and Bibliography page. The Building and Installing the Distribution page presents an overview of the procedures for compiling the distribution and installing it on a typical client or server. ...

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• APOD: 2002 August 20 - The Universe in Hot Gas
• Data gathering
• APOD: 2013 May 14 - Galaxy Collisions: Simulation vs Observations

Crater Gassendi . ... I made this drawing was made on the 26th of november 2001. If you compare this one with the previous drawing of Gassendi (below) the differences are clear. ... This drawing was made on the 28th of september 2001. After nearly a full month without observations I had a one hour gap between the thicker clouds. ... This drawing was made on the 29th of august 2001. ... This drawing was made on the 27th of august 2001. ... This drawing was made on the 25th of august 2001. ...

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Chair of solid state physics . ... The Physics of Phonons . ... In the first part of the course “The Physics of Phonons” the dynamics of atoms in one- and three- dimensional crystalline lattices is considered in detail. The quasiparticle conception in solids, taking phonons as an example, is discussed; creation and annihilation operators of phonons, main properties of acoustic and optical phonons dispersion laws, density of phonon states. ... Crystalline state. ... Acoustic and optical phonons. ...

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• Comet Observation Home Page (Chernogolovka)

Distribution of the analyzed SEPs with different >100 MeV proton fluxes ( J 100 ) at the microwave flux density plane ' S 9 vs. ... 1) General correspondence takes place between intensities of microwave bursts and proton fluxes - J 100 increases when S 9 and S 15 rise. ... 3) Powerful microwave bursts ( S 9 , S 15 >3000-10000 sfu ) with hard radio spectra ( S 9 < S 15 ) correspond to majority of powerful proton fluxes ( J 100 >10 pfu ). ...

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• APEX/Intro
• Ionospheric plasma-wave interaction
• projects

We model the spectral chanages of late oxygen-rich Miras observed in different pulsation phases. From a combination of variable near-IR spectra and UKIRT spectrophotometry of the 9.7 \mu m silicate dust emission feature in different phases we study the influence of the changing atmospherical circumstances on the conditions in the circumstellar dust shell. ... A comparision with the modelling results for another long period Mira U Ori is also provided. ...

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• Introduction
• Observations and Data Reduction
• Galactic distribution and absolute magnitudes

Distributed Software for Observations in Near Infrared V. Gavryusev 1 and C. Baffa Osservatorio Astrofisico di Arcetri E. Giani Dipartamento di Astronomia, Universit`a di Firenze Abstract. ... The processes denoted for control of hardware (telescope and other instruments) should be executed currently on PC dedicated for this task under DESQview/X, while all other components (user interface, tools for the data analysis, etc.) can work also under Unix. ... 1993, Di Giacomo et al. 1993). ...

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• Tracing Dust in Spiral Galaxies
• Water along the outflow from a young nearby protostar: a Herschel view
• NICMOS3 Detector for Spectroscopy

... We have studied scaling relations (virial mass versus CO luminosity, luminosity versus size, linewidth versus size) for molecular clouds in the 30 Dor and N 159 regions in the Large Magellanic Cloud. ... The study of molecular clouds in the Galaxy has resulted in a number of scaling relations between global cloud properties such as mass, density, luminosity, size and velocity dispersion (e.g. Larson (1981) , Scoville & Sanders (1987) , Solomon et al. ... Elmegreen B.G., 1989, ApJ , 338 , 178. ...

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• Determination of the relative orientation between radio and dynamical reference
• Introduction to phase correction for ALMA Bojan Nikolic web pages (r. 329)
• A CLEAN-based method for mosaic deconvolution

... It is reasonable to expect that UV part of the irradiating spectrum is most influenced by the grain evolution (growth and sedimentation ) which marks the very initial stage of planet formation. 2 log J [erg s­1 cm­2] 1 0 -1 -2 -3 1000 BB 40 0 0 (A5 ) BB 20 0 00 (A5) Drai ne (A5 ) BP Ta u (A5) BB 40 0 0 (GS) BB 20 0 00 (GS) Drai ne (GS) BP Ta u (GS) Disk Model Density distribution is based on a 1+1D disk ... Green lines are used for a model with dust growth and sedimentation. ...

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