Since the light from galaxies represents the integrated contribution of its consitutient stars, then we can learn about stellar populations in galaxies by modelling their light by summing up individual stellar spectra for different kinds of stars. ... The data cover the wavelength range 3500 - 9000 angstroms. ... Retrieve Digital Stellar Spectra Click on the appropriate spectral type. ... Note that the designation V means main sequence, IV means subgiants, III means giants, I means supergiant. ...

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• Astronomy HyperText Book: Stellar Clusters

Results from a series of long-term numerical integrations of orbits centred on that of C/1995 O1 (Hale-Bopp) are presented. Initially, 33 orbits taken from various sources were integrated in realistic models of the solar system for various time-scales about the present in the range (-3, +2) Myr and analyzed to assess the probability of different dynamical outcomes, such as a sungrazing state or the number of orbits since it was captured from a long-period orbit in the Oort cloud. ...

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• Armagh Observatory

... NRL . ... STScI . ... GSFC: Aerospace Building, 10210 Greenbelt Rd. ... Note that visitor badges for NRL need to be requested several days prior to the talk. ... The talks will be in room 408 of the Aerospace building, about 3/4 miles west of the GSFC main entrance at 10210 Greenbelt Rd (193). To get there, go out of the GSFC main gate and turn left, or continue past the main gate when coming from the BW Parkway. ... The visitor center is in the building just before (and outside) the gate. ...

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• Herschel Images and Results for the Magellanic Clouds
• The Astronomy Thesaurus and UDC - Present and Future (Group Discussion for
• Mathematical Analysis of the Iterative/Recursive Algorithm

... The visibility datasets possibly contain correlations for different polarizations and Stokes parameters. There are two basic ways that polarization characteristics can be measured: firstly, two orthogonal feeds can be present on the antennas, and the four different polarization correlations from a baseline can be taken and recorded. ... There are two ways the user can determine which polarizations he or she wants to process, either with the select parameter, or with the stokes parameter. ...

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• Unix Shell and Text Editor
• immerge
• Input Parameters to the Self-Calibration Tasks

ERS -1,2 SAR . ... SIR-C/X SAR . ... European Remote Sensing Satellite (ERS-1) was launched on 17 July 1991, and the follow mission ERS-2 (with the same sensors and an Ozone monitoring instrument added) was launched on 21 April 1995. ... The Spaceborne Imaging Radar-C/X-band Synthetic Radar (SIR-C/X-SAR), carried in the cargo bay of the Space Shuttle Endeavour in April and October of 1994, simultaneously recorded SAR data at three wavelengths (L-, C-, and X-bands; 23.5, 5.8, and 3.1 cm, respectively). ...

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• Radar aurora [Oulu]
• Formulas
• Magnetic field models[Oulu]

As it is in Ephemerides task, O?C can be calculated with different accuracy. ... It presents three modes of accuracy. One can calculate position of a minor planet by the formulae of elliptic motion starting from the fundamental set of elements for given minor planet. ... Also there is possibility to calculate positions taking into account perturbations from different sets of perturbing bodies by numerical integration ( Integration mode). ... Accuracy of integration is equal to 10**(?10) AU. ...

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• Asteroid and Comet Hazard
• Keywords_54
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Cryogenic Phase Locking Loop System for Superconducting Integrated Receiver Andrey Khudchenko1, Valery Koshelets1, Pavel Dmitriev1, Andrey Ermakov Pavel Yagoubov2, ... Institute for Space Research, the Netherlands Research Center of Superconducting Electronics Iceberg , Ukraine 1, Abstract A bandwidth of the typical Phase Locking Loop ( PLL ) system for the Superconducting Integrated Receiver ( To overcome this limitation we propose Cryogenic Phase Locking Loop (CPLL). ...

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• http://www.cplire.ru/html/lab234/pubs/2007_08.pdf
• http://www.cplire.ru/html/lab234/pubs/2010-13.pdf
• http://www.cplire.ru/html/lab234/pubs/2013_24.pdf

... 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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• RFI Issues at AO
• M42 Color Images
• NAIC-IRIDIUM Coordination Agreement

... Each day a different image or photograph of our fascinating universe is featured, along with a brief explanation written by a professional astronomer. August 11, 1998 . Sun Dance . ... Explanation: Hot gas dances across the surface of the Sun in this picture from the orbiting TRACE satellite . The temperature of the gas is color coded so that blue represents hundreds of thousands of Kelvin , while red represents extreme temperatures in the millions of Kelvin. ... About APOD > . ...

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• SAI Supernova catalog
• APOD: 2008 May 12 - The M81 Galaxy Group Through the Integrated Flux Nebula
• APOD: 2012 March 13 - The M81 Galaxy Group Through the Integrated Flux Nebula

... Fortran 66 . ... Fixed form . ... Whole Fortran 66 . ... Continuation line indicated in column 6 . ... Blank line as comment . ... Extension in Unix .f .f .f .f90 .f .f90 . Extension in DOS .FOR .FOR .FOR .F90 .FOR .F90 . ... This applies to both fixed form and free form source code. ... Fixed form of the source code is discouraged in Fortran 95! ... In UNIX there is no concept called extension, and the extensions are not specified in the Fortran standard, but in informal manufacturer standards. ...

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• Introduction
• Media types
• I. Daubechies, 1992, 10 Lectures on Wavelets, S.I.A.M.

On Systematic Differences in Individual Solutions and IERS Products Zinovy Malkin Institute of Applied Astronomy RAS, St. Petersburg, Russia 1 Present status Proper determination, modelling, and accounting for systematic differences between contributed series is of the great importance in compilation of the IERS products. ... Possible sources of systematic differences are: Ї Different reference systems (e.g. TRF, CRF, geopotential, time scale). ... 87 IERS Technical Note No. ...

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• http://www.gao.spb.ru/english/publ-s/viii-rfs/p099.pdf

... Colours of stars and galaxies hold information on intrinsic and extrinsic parameters, such as stellar temperatures and galaxy populations, selective absorption and colour changes due different dust contents and inclination angles of galaxies, as well as galaxy redshifts and evolution. ... The colour magnitude diagram of 65000 galaxies to which all above-mentioned quantities and others contribute can only be explained by comparison with simulations. ... Colours are also of technical help. ...

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• Different X-ray Spectra
• DFS group delivery procedure
• PAM Bulletin

... Because of the low conductivity, the magnetic coupling is weak and depends critically on density, temperature, ionisation rate and charged species. ... Implications When the Hall regime dominates near the midplane and ambipolar diffusion is dominant closer to the surface, a thicker layer of the disc is unstable to MRI perturbations and modes grow faster than under the ambipolar diffusion approximation. ... Right panel: For weak coupling, Hall limit perturbations grow until vA/cs ~ 2.9. ...

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• Student Briefing
• The Music of the Spheres
• The Electromagnetic Spectrum

... We can investigate projection of this distribution onto the celestial sphere in two ways: in terms of lines of constant SN frequencies per one square degree for all galaxies from the sample (Figure 36 ), and in terms of constant GW amplitudes at a given SN frequency per square degree (Figure 44 ). ... Figure 45: The sky distribution of the total supernova frequency from nearby galaxies in terms of lines of equal frequencies per square degree. ...

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• Detection rate of binary compact star merging
• Concluding Remarks and Future Prospects
• Art Gallery

. Figure 3. The SOHO/EIT derotated fixed-difference images with 6-hour time intervals in four channels of 304, 171, 195, and 284 illustrating the dimmings in different-temperature lines for two events of the 1st rotation (October 26, 2003 (a-d), November 4, 2003 (e-h)) and one event of the 2nd rotation (November 17, 2003 (i-l)). In frame d, the difference image with a 12-hour interval is presented because the 284 heliogram belonging to October 26, 19 UT is not available. To the parent page .

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• [INTERBALL] pr-7
• CMEs and Space Weather

... We present the results of an interferometric and single-dish study of G24.78+0.08, a region associated with high-mass star formation. ... We suggest that the embedded stars might be too young to have affected the surrounding molecular cloud significantly on a large scale. ... We assess that the (proto)stellar cluster lies at the center of a molecular clump with diameter of ~2 pc: to a good approximation this may be described as a spherically symmetric clump with density profile of the type n~R^(-1.8...

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• Arcetri Guaranteed Time
• CHIANTI atomic database

... ALMA has the potential to detect and resolve CO rotational line emission in debris disks, potentially providing key information to determine its provenance. " " (e.g. LTE, CO/H2 abundance ratio) do not necessarily apply in low gas density environments such as debris disks, and can lead to orders of magnitude errors in CO mass estimations. The 3 upper limit on the total CO mass for the Fomalhaut system is of 5.8 x 10-5 Mearth. ... Different colours represent different gas kinetic temperatures. ...

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• http://www.mrao.cam.ac.uk/projects/OAS/pmwiki/uploads/MROIFastTipTilt.DocMan/PreliminaryDesignReportOutline.pdf
• Data Format Session at 2001 IAU WG Meeting
• Samantha Thompson - Research

Next: Radial velocity of the Up: Optical spectrum of IRAS04296 Previous: Observations and spectra reduction . ... However, molecular emission features are only very rarely observed in the optical spectra of PPNe. ... On the other hand, it is well known that cometary nuclei spectra show prominent Swan band emission. In both spectra of IRAS04296 we have discovered strong emission in the (0;0) and (0;1) bands of the Swan system of the molecule. ... Now consider the case of IRAS04296. ...

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• harak_e
• di_eks
• From Power Up To Bash Prompt: The Filesystem

. Christmas History Traditions Carols Celebration in UK Celebration in USA яhristmas Menu .

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• education

... Up: Algorithms . ... Iterative algorithms with non-linear constraints are very attractive in image reconstruction with only a few strip-integrated projections. We present research into various versions of the iterative CLEAN algorithm for the solution of this problem. ... where is the object brightness distribution, is the fan (dirty) beam, and is the dirty (summary) image. ... We carried out the study of TC-CLEAN applied to image reconstruction with few projections. ...

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• ADASS 2002 Conference Proceedings
• Modelling Spectro-photometric Characteristics of Nonradially Pulsating Stars
• Automated Programming and Simulations of Signal Compression from the Cosmic