CCD Performance . ... The dark current appears to have two components: one from electronic sources in the CCD, and a second component whose strength correlates with the cosmic ray flux. ... As of this writing, the " DARKTIME" keyword in the WFPC2 image headers does not reflect correctly the actual time during which the CCD collects dark current. ... External exposures of 180s or longer made with the serial clocks off (CLOCKS=NO; the default setting) suffer an additional 60s of darktime (restart=1). ...

... Primordial theory review : Dick Bond . Defects and the CMB review : Andy Albrecht . ... Gravitational wave contribution to CMB anisotropies : V.B. Lukash and E.V. Mikheeva . C_l from cosmic strings : Lloyd Knox . Some aspects of CMB anisotropies induced from topological defects : Mairi Sakellariadou . ... CMB anisotropies from scaling sources : Ruth Durrer . ... SZ observations I : Sarah Church . ... Holes in the microwave sky? ... Detecting cosmic strings in the CMB : James Robinson . ...

Cosmic Ray laboratory of . ... Neutron Monitor (Cosmic Ray Observations) . is situated in Irkutsk (Russia) . ... Height - location above sea level . ... Height: . ... For recording the CR (Cosmic Rays) neutron component at Irkutsk, . neutron monitor NM-64 is used, which is an installation with 18 two-meter proportional counters filled with BF 3 (boron trifluoride gas) in which the B 10 90 per cent of the total boron. ... The neutron monitor is located at 475m above sea level. ...

... 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. ...

... Minute Values of Geomagnetic Field Components . ... AA 1868 - Present (3 hourly and daily) (monthly) (yearly) (Lists and histograms of geomagnetic disturbance and Solar Sunspots) KP_AP 1932 - Present (3 hourly and daily) (Lists and histograms of geomagnetic disturbance and Solar Sunspots) AE_HV 1957-75, 78-88 (hourly) AE_MIN 1978-881-6;198903;1990-94 (minute) DST 1957 - Present (hourly) PC 1975 - Present (15-minute) AMANAS 1959 - Present (3 hourly and daily) KMKNKS 1983 - Present (3 hourly) . ...

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. This artist s impression shows how photons in the cosmic microwave background (CMB) are deflected by the gravitational lensing effect of massive cosmic structures as they travel across the universe. Gravitational lensing creates tiny, additional distortions to the mottled pattern of the CMB temperature fluctuations. A small fraction of the CMB is polarized; one component of this polarized light, B-modes, have been given an additional signature by gravitational lensing. ESA/Planck Collaboration

Next: Order Extraction Up: Background Definition Previous: Background estimate by . ... The sky background component can be measured in spectra taken with an extended slit using the two commands DEFINE/SKY and EXTRACT/SKY . ... The command EXTRACT/ECHELLE performs an average extraction of the sky background using these offsets, optionally fiters for cosmics, and provides an extracted spectrum in a format similar to the one resulting from EXTRACT/ECHELLE . ...

... Partial matching is allowed Cone Search Right ascension Right Ascension measurement in hh:mm:ss.ss (J2000) Declination Declination measurement dd:mm:ss.ss (J2000) Search window Field of view to search around the RA/Dec measurement (arcmin) Project ID This is the OPAL project ID in which an observation was observed Observation date (DD MMM YYYY) Allows searching for pulsar observations by observation date in dd mmm yyyy format ...

... It is notoriously difficult to identify weak cosmic ray events in long exposure observations. ... The method is to compare the probability distribution function (PDF) of cosmic ray events between an observation and a dark frame matched in exposure time. We illustrate the basic idea using dark exposures from a Tek 1024 1024 CCD with varying exposure lengths and read-out times. ... Figure: Histogram of cosmic ray events in a two hour dark frame. ... Original PostScript figure (78 kB) . ...

... Report on Cosmic Call 1999 . ... Cosmic Call Sessions . ... This Report outlines methodology, hard- and software, which were developed to transmit first public Interstellar messages from Evpatoria Deep Space Center (EDSC), and describes four Cosmic Call Sessions, which were fulfilled in EDSC on May 24 and June 30 - July 1, 1999. ... Each Cosmic Call consists of two parts. ... Dutil Message, . ... The software for gathering all messages and creating the Cosmic Call stream, was written on C language. ...

... Science Activities > PhD Thesis Topics offered by ESO Faculty Members > Thesis Topic: Foreground emission and Cosmic Microwave background intrinsic anisotropies . ... Since its discovery the Cosmic Microwave Radiation (CMB) has been one of the pillars of modern Cosmology. ... Further development of this work is the application of already tested algorithms to disentangle the foreground emission from the CMB maps and the determination of the CMB intrinsic emission. ... Return to list of thesis topics ...

Main research interests: . 1) Structure and geometry of the circumnuclear medium of AGN, particularly through hard X-ray observations of obscured sources. ... 3) Physics of Ultraluminous Infrared Galaxies (ULIRGs): analysis of the AGN and starburst components through hard X-ray and infrared (with ground-based 3-5 micron spectroscopy, and with Spitzer in the 5-30 micron band) imaging and spectroscopy. ...

Peremennye Zvezdy", . ... Star Name: . GSC 3710-00312, USNO-A2.0 1425-04252279 . ... Variability type: . ... USNO-A2.0 1425-04252279 is located at the distance of 15?.7 from the X-ray source 1RXS J031707.9+572942, which is larger than the position error of the source (12?), but its hardness ratio HR1 = 0.03 0.29, typical of chromospherically active stars, and its character of variability allow us to assume that the star is related to the X-ray source. ... Eclipsing variability . Sine wave 1 . ...

The space between the planets is far from empty. It contains: electromagnetic radiation (photons); hot plasma (electrons, protons and other ions) a.k.a. the solar wind ; cosmic rays; microscopic dust particles; and magnetic fields (primarily the Sun's). While the Sun 's radiation is obvious, the other components of the interplanetary medium were not discovered until very recently. ... Except near some of the planets, interplanetary space is filled with the Sun's magnetic field. ... Sun .. ...

... 27 мая . ... Заседание в Малом зале . ... Председатель Мингалиев М.Г. 14:00 Акъюз А. Preliminary Results from RTT150 Observations of Supernova Remnants in Two Spiral Galaxies . ... 15:00 Желенкова О.П. Application of IVOA Software Tools for Radio Sources Investigation . ... 16:00 Шарина М.Е. Results from the 6m Telescope Observations of Globular Clusters in Dwarf Galaxies . ... Кратов Д. The "MARS-3" Matrix Radiometric System for RATAN-600 Radio Telescope: Trial Observations . ...

... It contains: electromagnetic radiation (photons); hot plasma (electrons, protons and other ions) a.k.a. the solar wind ; cosmic rays; microscopic dust particles; and magnetic fields (primarily the Sun's). W hile the Sun 's radiation is obvious, the other components of the interplanetary medium were not discovered until very recently. ... Within a few solar radii of the Sun the magnetic field determines the flow of the solar wind; much of the flow is trapped in magnetic loops. ... Sun .. ...

CONTENTS Volume 23 Number 2 (July 1996) . ... ENVIRONMENTS OF ACTIVE CLOSE BINARY STARS . A. G. Gunn . ... K-BAND OBSERVATIONS OF THE FLARE STAR UV CET . A. D. Andrews & P. M. Panagi . ... Elma S. Parsamian & A. D. Andrews . ... ASTRONOMICAL CLOCKS AT ARMAGH OBSERVATORY . ... JOHN BIRMINGHAM ON ``COGGIA'S COMET. ... 1995-1999 Irish Astronomical Journal, Downshay, 12 Heather Lea Avenue, Dore, Sheffield S17 3DJ, S. Yorkshire, United Kingdom WWW Contact: Alastair G Gunn Back to IAJ Home Page ...

Next: Limiting Energy Channels Input Up: *fit* - Fit Data Previous: Raymond Model . The model is a two-temperature Raymond thermal spectrum, low temperature range is 0.55 to 0.65 keV, high temperature range is 1 to 2 keV, element abundance table is cosmic, abundance of heavy elements (atomic number >2 ) is 50% of the value in the table. Note that 0.7 = log(5.0), specifies that the second component normalization will be 5 times the normalization of the first component. ...

Next: Polarization efficiency: size/shape/orientation effects Up: Optical properties of cosmic Previous: The 2175? feature . To model the interstellar polarization one needs to calculate the forward-transmitted radiation for an ensemble of non-spherical aligned dust grains. ... Let non-polarized stellar radiation passes through a dusty cloud with a homogeneous magnetic field. ... The angle between the line of sight and the magnetic field is ( ). ... where the angle is connected with and ( ). ...