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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Astronomical Data Analysis Software and Systems IV ASP Conference Series, Vol. ... The user interface is organized as widget­based X11 client. ... Design The design of a data acquisition package is, as always, a long struggle between many different and contrasting needs. ... 1993; Di Giacomo et al. ... In our case we have to differentiate between a number of tasks: (1) a graph­ ical user interface, (2) the display of images, (3) the hardware interface, and (4) data transfer between computers. ...

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... The SF does not contain all the information required to process the ODF with the SAS. odfingest extends the SF with data extracted from the instrument housekeeping data files and the calibration database. It creates a new summary file: the SAS ODF Summary File (SOSF). ... The user need not have write access to the ODF directory. odfingest uses the parameter outdir to learn where to write the SOSF. ... Alternatively, the name of the SOSF can be passed to odfingest with the parameter summaryfile . ...

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FGS Instrument Handbook for Cycle 24 . ... Fine Guidance Sensor Instrument Handbook for Cycle 24 > Chapter 7: FGS AstrometryData Processing > 7.2 Exposure-Level Processing . ... 7.2.2 Observing Mode Dependent Processing . ... After pipeline initialization and data quality assessments, successful observations (i.e., those that acquired the target), are processed according to the FGS observation mode: Position or Transfer. ... The corrections applied to the FGS data are as follows: . ... Transfer mode . ...

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... Stellar Evolution is driven entirely by the never ending battle between Pressure and Gravity . As imbalances are reached, the star is driven to find a new Energy source. ... Pressure and gravitational forces are equal, the star is stable and its core is sufficiently hot to fuse Hydrogen into Helium More about main sequence stars . ... The luminosity generated by the core fusion of Helium into Carbon is far greater than the shell luminosity associated with the fusion of Hydrogen into Helium. ...

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... XmTel is a telescope control interface designed to to communicate with Elwood Downey's XEphem. It will also operate as a free-standing program for control of telescopes that use the NexStar, LX200 or RCOS command sets. XmTel is accompanied by routines which support the necessary communication and commands for running Meade Instruments LX200, Celestron NexStar telescopes. A version for RC Optical Systems Professional Series mounting is available from the manufacturer. ...

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... You are here: start €Ё difx €Ё difxmpi . ... difx:difxmpi . The DiFX software correlator uses MPI for organizing the spawning of processes on different computers and for transmitting data from one process to another. MPI is used only for communication between mpifxcorr processes. ... MPI assigns each process that it starts an integer identifier (called rank) that is used to refer back to that process. ... A vast majority of known DiFX installations use OpenMPI (available at www.openmpi.org ). ...

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... Science . ... Science Users Information > Science Publications > Science Announcements > Processed Calibration Files for VLT instruments Now Available . ... ESO Data . ... ESOReflex data reduction workflows can be used to customize the generation of the processed and co-added calibration frames and to apply them to the science files. A detailed step-by-step guide on how to automatically associate the appropriate calibrations, raw or processed, to the science files of interest is available . ...

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... It was designed to observe the solar wind approaching Earth, from a position near the Lagrangian point L1, and it is part of the International Solar-Terrestrial Physics (ISTP) Initiative . ... The original plan called for "Wind" to approach its final station over two years, undergoing two close encounters with the Moon to boost its speed. ... If however the object is moving , the encounter is not symmetric, and in the end the spacecraft may have gained or lost speed, depending on its trajectory. ...

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... Posts tagged ?Pareto distribution? ... Posted by hlee . ... Tags: Classification , covariance , FARIMA , Fisher information , GL , GRB , Levy , light curve , limb darkening , ML , Pareto distribution , quasars , solar flare , standard candle , tessellation , time series , VO , void . ... 1 Comment . ... ArXiv] Pareto Distribution? ... 4 Comments . ... From arxiv/astro-ph, arXiv:0706.2590v1 Extreme Value Theory and the Solar Cycle by Ramos, A. This paper might drag a large attention from CHASC...

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Chiaki Kobayashi, Ralph Sutherland How galaxies did form and evolution? - to answer this unsolved problem, we are simulating the formation and evolutionary history of galaxies in the Universe, including star formation, supernovae feedback, and chemical enrichment. Comparing the spacial distribution of elements within galaxies with observations, we will examine fundamental physical processes that drive galaxy formation. ... COALA : Universe Galaxy AGN Star Planet ...

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... It allows observations of extended and starlike objects in different modes: CCD photometry, panoramic spectroscopy with the Fabry-Perot interferometer, spectroscopy and spectropolarimetry with a "long-slit", slit-free spectroscopy, multi-object spectroscopy. ... Digital servo drives that were installed have improved the reliability of the complex, extended the range severalfold, and reduced the telescope's speed control step. ... A software and hardware set for the BTA control system was implemented...

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Quasar VLBI network observatories as co-location sites A. Ipatov, I. Gayazov, S. Smolentsev Institute of Applied Astronomy, Saint Petersburg, Russia ... supposes: 1. installation of different observational techniques at sites (co-location) 2. combined processing of different types of observations (collocation) IAA activity in space geodesy · Quasar VLBI network : ­ VLBI observations ­ GPS /GLONASS observations ­ DORIS ( ...

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Next: Star Formation Rate and Up: No Title Previous: Calculation of Evolutionary Tracks . To start calculations, we choose the distributions of the initial binary parameters: the mass of the primary ZAMS component, , binary mass ratio, , orbital separation a . ... whereas the mass ratio distribution is not. ... The zero assumption often made is that the mass ratio distribution has a flat shape, that is binaries with a high mass ratio occur as frequently as those with equal masses. ...

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... The The ASC Data Archive for the AXAF Ground Calibration 393 T1 T1 replicate file (4GL) retrieve, ingest (4GL) search (SQL) replicate table retrieve, ingest (4GL) replicate file (RPC) search, store (SQL) search, store (SQL) replicate file (RPC) search (SQL) SAO Client SAO SQL Server Science Center, Cambridge MA Operations Center, Huntsville AL Databases Replication Server Replication Server SAO Archive Server XRCF Archive Files Server XRCF SQL Server Databases XRCF Client Files Figure 2. ...

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At Arecibo we have a variety of optical instruments that we use to study terrestrial airglow emissions. ... As a complement to the airglow instrumentation we also maintain a set of optical instruments, called lidars, used for "active" remote sensing of the atmosphere. That is, we generate our own source signal using lasers and measure the characteristics of the light scattered back from the atmosphere. ... An operations manual for the Optical Laboratories is currently under major revision. ...

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... Exposure Time Calculator (ETC) . ... ESO - Public Surveys . ... the recommended values to use for DIT, . ... Detector on-chip integration (DIT): seconds. to your chosen value - a separate page gives recommended values to use for DIT - for modes 1 and 2 below you may wish to start with the maximum recommended values as these will minimize the effect of read noise (a total object exposure of Y secs with DIT=X secs will produce Y/X lots of read noise) and give you a lower limit on the time needed. ...

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Below is a table of INTERBALL-2 experiments summary to remind you about specific features of each instrument. ... See bottom of the page for additional information. ... AURORAL PLASMA . ... Spectra of electrons and ions 0.03 < E < 15 keV; anisotropy of electrons and ions (M = 1, 4, 16), 30 < E < 500 keV/Q . ... IKI, Moscow, Russia . ... Electron and ion spectra and anisotropy (M = 1, 2, 4, 16), 0.005 < E < 20 keV/Q . ... Ion composition (M = 1-32) and 3-D energy distribution, 10 eV < E < 30 keV/Q . ...

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ROBOTIC OBSERVATIONS OF INTEGRAL SOURCES IN THE OPTICAL DOMAIN Д Д Petr Kubanek1,2,4 , Rene Hudec 1 , John French3,4 , Jan Strobl1 , Martin Nekola1 , and Filip Munz1 1 Astronomicky ustav Akademie ved Ceske republiky, Ondrejov, Czech Republic ДД Д 2 INTEGRAL Science Data Center, Chemin d'Ecogia 16, Versoix, Switzerland 3 University College Dublin, Dublin, Ireland 4 for the Watcher Collaboration ABSTRACT ... The sources are monitored with BART[3]. ... IGR J00234+6141 error box. ...

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... IRAF View . This is the orientation of the image as viewed in an image display via IRAF (e.g. ximtool, saoimage). Note: This is different from the orientation of the image as viewed on a Macintosh, via Remark . ... A +X, +Y instrument offset will move a star in the direction indicated by the arrows. ... Note: The offset direction depends upon which interface the offset command was issued in! ... Note: This is different from the orientation of the image as viewed by IRAF. ...

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