A Wide Energy Band Compound Pixelated Photon Detector A Wide Energy Band Compound Pixelated Photon Detector Upendra Desai, Larry Orwig Code 682, NASA/GSFC We present a new concept of a stacked detector that provides high spectral resolution over a wide energy band (keV-MeV). ... For the energy range from sub keV to 20 keV we use silicon PIN detectors. To cover energies from 20 keV to 60 keV we use a 2-mm-thick CZT detector beneath the "Si" PIN detector. ...

... References: %Observed energy levels (2-5): Kucera et al., 2000, ApJ , 538, 424 % Observed energy levels (6-15): Edlen, B., 1984, Pysica Scripta, 30, 135 % Observed energy levels (n=3): identifications from the X-ray line list by Landi Phillips 2005 , ApJ , in press % Observed energy levels (n=4,5): Shirai,T., Sugar,J., Musgrove,A., Wiese,W.L., 2000, J.Phys.Chem.Ref.Data, Monograph 8 % Observed energy ...

Next: Early searches at other Up: The discovery of pulsars Previous: The Nature letter of . ... Gold (1968) [ 12 ], Pacini (1968) [ 28 ] . White dwarfs no longer viable . Vela pulsar (P=89ms) discovered [ 17 ] . Crab pulsar (P=33ms) [ 33 ] . Vibration of neutron stars no longer viable . slow down of Crab pulsar observed [ 32 ] . Age of Crab pulsar age of Crab nebula . Crab pulsar and nebula . ...

... For example, as pointed out by Perlman et al. (1996b), the lack of a Ca II H & K break strength criterion in the 1 Jy, S4 and S5 samples of BL Lacs, has caused numerous objects to be misclassified as radio galaxies instead of BL Lacs (see also March? Browne 1995, 1996). ... While one may argue that some of these objects fall in the expanded region of the (H & K break strength, equivalent width) diagram that March? et al. (1996) allot to the BL Lacs, several, for example 1 Jy 1308+326, do not. ...

The database contains references to the papers, data files and links to the Internet resources related to measurements and calculations of the optical constants in the wavelength interval from X-rays to radio domain. ... References to some useful books and reviews on the subject (e.g. the classical handbooks edited by E.D.Palik) and links to Internet collections of optical constants and personal WWW pages with related software were also placed in the database. You have arrived at our welcome page. ...

April 4, 2008 (Friday) Maxim Pospelov, Victoria University . ... Fall 2007 . Winter 2008 . Fall 2006 . Winter 2007 . Spring 2007 . ... A new generation cosmic ray detector, the Pierre Auger Observatory, has been designed to study cosmic rays with energy above 10 18 eV and answer the crucial questions of ultra high energy cosmic ray physics. ... Oscillating scalar fields, with an oscillation frequency much greater than the expansion rate, have been proposed as models for dark energy. ...

... The low energy plasma composition spectrometer AMEI-2 is built to be able to find in the low energy range of the phase space (E, q, j) and separate the fluxes of the major ion species in the magnetotail - H+, He++, He+ and O+, and analyse their energy and angular distributions. ... Electrostatic angular scanning in one direction and the use of the spin of the satellite to sample the other angle give the ability to measure 2-D distributions for each ion specie several times per spin. ...

... The bandpass in which the measurement is made must be identified. The bandpass name is recorded in a column labelled BAND. This name, combined with the information in the instrument file, is used to identify the detector in multichannel instruments.) Standard passband names should be used: 'V', 'B', 'U', 'URL', 'R', 'I', 'u', 'v', 'b', 'y', 'betaW', etc. ... Such information must be decoded to a standard band name in the observation-table file. ...

. eng || rus . Home . Projects . Research . Publications . Astronomy Letters . Conferences . SRG Project . RSDC . Contacts . Theory and observations . INTEGRAL All-sky survey . Bright X-Ray pulsars with INTEGRAL . X-ray survey for galaxy clusters using archival ROSAT observations 400 deg 2 cluster survey . Observations of gamma-ray burst afterglows with RTT150 telescope . Optical identifications of hard X-ray sources . 2016 IKI RAN

... RECOMMENDED VALUES OF PHYSICAL CONSTANTS AND CONVERSION FACTORS. ... This reference must be included when these constants are used in a context where their full accuracy is important. ... elementary charge (of proton) . ... gravitational constant . ... unified atomic mass constant . ... of electron . ... of proton . ... Planck constant . ... Rydberg constant, m 0 2 m e e 4 c 3 /8h 3 . ... fine structure constant, m 0 e 2 c/2h . ... Bohr radius, h 2 ( pm 0 c 2 m e e 2 ) . ... Bohr magneton, e h /2m e...

... People . Posts tagged ?identification? ... As far as I know SUSY is the abbreviation of SUperSYmetricity in particle physics. ... I?ll not go into the details of particle physics and the standard model. ... Comment . ... Entries RSS . Comments RSS . ... General comments . ... vlk on [MADS] Parallel Coordinates . upvc windows on [MADS] Parallel Coordinates . ... Alfred Inselberg on [MADS] Parallel Coordinates . ... nestor on People . ... Entries (RSS) and Comments (RSS) . ...

... We present a computer program for modelling energy flux distribution and light curves of eclipsing binaries from far ultraviolet to infrared regions. The Roche model is assumed. Proximity effects of components (reflection of radiation and surface gravity darkening) are taken into account. ... Figure 1: The surface temperature distribution for Algol A-B system before (upper plot) and after (lower plot) correction for temperature due to the irradiation effect. ...

... LABORATORY OF RADIO ASTRONOMICAL OBSERVATIONS . Radio sources identification is one of the most important tasks of the current radio astrophysics. ... Optical idetification. ... Optical identifications of subsample of steep spectra radio sources from RC catalog using 6m SAO telescope of SAO RAS: optical observations. ... Astronomy Reports. ... Identification of radio sources with data of various radio catalogs allows one to construct continual spectrum of the object and its radio structure. ...

We present optical, ultraviolet (UV) and extreme ultraviolet (EUV) results for a new active late-type dwarf star discovered by the Extreme Ultraviolet Explorer (EUVE). A large flare with an energy in excess of 1E35 erg and duration of ~1.1 days was detected in the EUVE Lex/B band (60--200AA). ... The `quiescent' EUV emission of the source is similar to the most active flare stars with the `quiescent' optical spectrum showing strong H alpha, Ca II H Mg II h emission and Li I 6707.8A absorption. ...

Fermi s Gamma ray Pulsars . ... Traditionally identified and studied by observing their regular radio pulsations , two dozen pulsars have now been detected at extreme gamma-ray energies by the Fermi Gamma-ray Space Telescope . ... This gamma-ray all-sky map, aligned with the plane of our Milky Way Galaxy, shows the pulsar positions, with the 16 new Fermi pulsars circled in yellow (8 previously known radio pulsars are in magenta). ... NASA Web Site Statements, Warnings, and Disclaimers . ...

... Energy . ... The free ions and electrons in a plasma behave the same way. Knowing the temperature of the high atmosphere of Earth, or that of the Sun, we can calculate energies expected of ions and electrons found there. However, ions and electrons actually observed in space are often much, much more energetic, and may move at a respectable fraction of the velocity of light (300,000 km/sec or 186,000 miles/sec). ... Typical energy of an electron in the polar aurora. 40,000 ev . ... 50,000 ev . ...

Next: Feature enhancement: filtering Up: No Title Previous: Commentary . A sharp contrast is seen between the `crowded' energy map of the modulated oscillations (individual minima and maxima of the signal identified by the Mexican hat wavelet) in section 13 and and the `smooth' presentation of the norm-Morlet transforms of the same data in section 15. ... construct an energy map based on individual events. smooth the map by merging the events that are `close enough' to each other. ...

... A2119 Date Received: 2005-May-27 23:29:33 Technical Page Proposal Type: General Category: Sub-Category: Observation Category: Total Time Requested: Prop osal Title: Regular Astronomy Spectroscopy Extragalactic 75.6 Hours OH Megamasers in ULIRGs: The Mega-Obvious Place to Look for Zeeman Splitting! ... We prop ose to use 75.6 hours of Arecib o time to observe 6 of the brightest OH megamasers in full-Stokes mo de in order to detect Zeeman splitting of the 1667 MHz transition. ...