... In the three intervening decades there have been many observations of this diffuse emission over a wide range of x-ray energies. ... During the 1970's researchers at the University of Wisconsin, lead by Dr. William Kraushaar, used a series of sounding rocket flights to map the diffuse x-ray emission from the sky in several bands. ... University of Wisconsin Sky Survey map of the B-band (0.13-0.188 keV) x-ray intensity. ... University of Wisconsin Sky Survey map of the 2-6 keV band x-ray intensity. ...

Next: The interstellar medium Up: An overview Previous: Radio pulse characteristics . Mostly the very youngest pulsars . Just 3 pulsars detected at Optical Wavelengths . Crab, Vela, B0540-69 . X-ray - 27 detected, 13 pulsed . Gamma ray - 6 detected all pulsed . Radio emission of spin down energy . ... Need radio ephemeris . 18000 pulse periods elapse between each EGRET photon detected from the Crab pulsar . ...

... The close X-ray binary with relativisic jest, contained probably a black hole, Cygnus X-3 has been detected in first time in Gamma-rays at enegries higher 100 МeV (AGILE, Tavani et al., ... Koljonen K.I.I.; Hannikainen D.C.; McCollough M.L.; Pooley G.G.; Trushkin S.A. The hardness-intensity diagram of Cygnus X-3: revisiting the radio/X-ray states 2010, MNRAS, 406, 307-319. ... X-ray image of Cygnus X-3 (Chandra) . ... Light curves Cygnus X-3 in gamma-rays (AGILE) and in radio cm-bands (Ryle tel., ...

... The close X-ray binary with relativisic jest, contained probably a black hole, Cygnus X-3 has been detected in first time in Gamma-rays at enegries higher 100 МeV (AGILE, Tavani et al., ... The bright radio flares from Cygnus X-3, caused by the massive ejections of matter with velocity close to speed of light accur in the certain ''huper-sort'' X-ray states (RXTE PCA), that was in the first time determined in the studies of HID -- ''hardness-intensity diagram'' [Fig.4]. ...

We present Spitzer Space Telescope images of the isolated dwarf galaxy UGC 10445. The galaxy is detected at all photometric bands (3.6-160 ЮМm), as well as in the Multiband Imaging Photometer for Spitzer (MIPS) spectral energy distribution mode (55-95 ЮМm). ... There is over 106 Msolar of cold dust (T~18 K) in the galaxy, represented by 160 ЮМm emission, which extends to a larger radius than the ultraviolet (UV), optical, and near-infrared light. ... ADS Citation Query . citations = 24 . ...

Astronomers Detect Coolest Radio Star . ... The new radio-star is much smaller and colder than our Sun.€а With a surface temperature not much higher than that of a giant planet, and a size comparable to JupiterтАЩs, it is scarcely visible in optical light.€а Yet the radio flares seen at Arecibo show it must have a strong magnetic field, implying that the same could be true of other similar stars. ...

... Credit Copyright: IceCube Collaboration , U. Wisconsin , NSF Explanation: From where do these neutrinos come? The IceCube Neutrino Observatory near the South Pole of the Earth has begun to detect nearly invisible particles of very high energy. Although these rarely-interacting neutrinos pass through much of the Earth just before being detected, where they started remains a mystery. ... NASA Web Site Statements, Warnings, and Disclaimers . ... Publications with keywords: Antarctica . ...

... 2015 September 1 . Distant Neutrinos Detected Below Antarctic Ice . Image Credit: IceCube Collaboration , U. Wisconsin , NSF . ... The IceCube Neutrino Observatory near the South Pole of the Earth has begun to detect nearly invisible particles of very high energy. ... Pictured here is IceCube's Antarctic lab accompanied by a cartoon depicting long strands of detectors frozen into the crystal clear ice below. ... About APOD | ... NASA Official: Phillip Newman Specific rights apply . ...

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. ...

... region (region-6.2.2) [xmmsas_20030110_1802-5.4.1] . ... The region task will automatically determine the optimal source and background extraction regions for a detected source in an XMM observation. ... The regions are defined in sky coordinates. region will attempt to maximise the area of the extraction region for each source, whilst ensuring that the extraction regions of neighbouring sources do not overlap, and that the background extraction region for a given source excludes neighbouring...

Disastrous earthquakes happen 100 to 200 times a year. ... There is a chance that the data of ionospheric plasma observations hold an answer to the latter question. Satellites and ground-based facilities may detect earthquake precursors in the ionosphere a few hours or days before the main shock. ... ULF "Hz"-oscillations have been recorded several hours before the main shock in a narrow magnetic field tube (40...100 km along the satellite trajectory) conjugated with epicenter of the earthquake. ...

. This plot shows the locations of 150 blazars (green dots) used in the EBL study. The background map shows the entire sky and was constructed from four years of gamma-rays with energies above 10 billion electron volts (GeV) detected by Fermi. The plane of our Milky Way Galaxy runs along the middle of the plot. The Fermi LAT instrument is the first to detect more than 500 sources in this energy range. // Credit: NASA/DOE/Fermi LAT Collaboration

... 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. ...

... Flux density at 1 GHz (/Jy): 15 . ... Molonglo at 408 MHz (3') and Parkes 64-m at 5 GHz (4'). ADS . ... FIRST at 1415 MHz (50''). ... Wilson 1986, ApJ, 302, 718. ... Whiteoak & Green 1996, A&AS, 118, 329. ... Green et al. ... ATCA at 1.4 GHz (16".5?19".5: S=14.3?0.1 Jy) and 4.5 GHz (2".0?1".5: S=12.5?0.2 Jy). ... ATCA and Parkes 64-m at 1.4 GHz (1'.8?2'.0), plus H I . ... ATCA at 19 GHz (6".1?7".7), including polarisation. ... ATCA at 1.4 GHz (5".8?7".0: S=13.8?0.4 Jy), plus XMM observations. ...

SKA-3 instrument consists of two energy-angle ( EA ) electrostatic analyzers and two energy-mass ( EM ) time-of-flight analyzers. ... Here you can find more details about SKA-3 instrumentation set. ... Case 218 . ... satellite's trajectory in geomagnetic frame ( blue coloured), UFSIPS scan location and observation moment ( red coloured), interval of the SKA-3 observations ( green coloured) . ... a view of the Nothern polar region at the moment of UFSIPS observations, the scan location is red coloured. ...

Next: SLIM: A Program to Simulate the ACS Spectroscopic Modes . ... Previous: On the Fly Bad Pixel Detection for the Chandra X-ray Observatory's Aspect Camera . ... We here present an overview of Celldetect , a source detection program for Chandra. ... Celldetect identifies point sources in the presence of background. ... At each point where a detection is attempted, celldetect uses an appropriately sized cell. ... The background statistics in celldetect change as the cell size increases. ...

Next: Unusual Emission near a Up: NICMOS Science Previous: The Stellar Population in . ... Three examples are presented of how ISOCAM 1 sees the process of stellar evolution. i) Standard staring and coronographic observations with ISOCAM towards BD+31 643 are presented. ... Position 4 is closest to the star; Position 6 coincides roughly with the minimum of emission seen in the images; position 7 with the ring. ... I presented three examples of the evolution of stars as seen with ISOCAM. ...

The Variable Gamma-Ray Source 2CG 135+01 ApJ, 497:L89-L91, 1998 7 h gamma AGN variability . gamma-radio-AGN-variability ADS query . ... Model for the High-Energy Emission from Blazars 1993ApJ.. ... Possible Production of High-Energy Gamma Rays from Proton Acceleration in the Extragalactic Radio Source Markarian 501 astro-ph/9803241 K.Mannheim . ... A theoretical unifying scheme for gamma-ray bright blazars astro-ph/9807317 G. Ghisellini, A. Celotti, G. Fossati, L. Maraschi, A. Comastri . ...

Class 1 Introduction, Background History of Modern Astronomy The Night Sky, Eclipses and the Seasons Kepler's Laws Newtonian Gravity General Relativity Matter and Light Telescopes Class 2 Solar System Characteristics Formation Exosolar Planets Class 3 Stars The Sun Stellar Evolution of Low and High Mass Stars Deaths of Stars Exotic Stars Class 4 Galaxies Galaxy Classification Formation of Galaxies Galactic Evolution ... So far, one planet has been studied by this method. ...

Detected Supernovae . The search have produced till now the detections of 4 SNe. ... This result highlights the power of infrared monitoring in detecting Obscured SNe and indicates that optical surveys are probably missing a significant fraction of SNe, especially in obscured systems such as starburst galaxies. ... In Fig. we show the archival SOFI image of NGC3256 (left) and the first image obtained in 2001 (right) where SN2001db has been detected. ...