... Archives . ... The PCA and ICA is used for separating mixed components with some assumptions. ... The need of source separation methods in astronomy has led various adaptations of decomposition methods available. ... I rarely come up with a paper which gathered and summarized component separation methods applicable to astronomical data. In that regards, the following paper seems useful to overview methods of reducing dimensionality for astronomers. [arxiv:0805.0269] . ... Chandra Blog . ...

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• The AstroStat Slog component separation
• Comments on: [ArXiv] component separation methods By: hlee By: Sam Leach
• The AstroStat Slog maximum entropy

A New Mass Model For The JVAS Gravitational Lens B1030+074. ... University of Manchester, Jodrell Bank, U.K. B1030+074 is a double image gravitational lens, which was dis- covered during the Jodrell Bank VLA Astrometric Survey (JVAS). ... HST WFPC2 observations have revealed the lensing galaxy, which lies close to component B. The redshifts of the lensing galaxy and the background source have also been obtained and are 0.599 and 1.535 respectively. ...

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• G263.9-3.3
• G327.6+14.6
• G41.1-0.3

... The PSF image (after tapering/weighting) and weights image. ... Directory listing: total 145G -rw-r--r-- 1 whi550 at-astro 534M 2010-12-11 23:22 ASKAPsim.FLASH.cont.catalogue.dat - rw-rw-r -- 1 whi550 at-astro 50M 2010-12-10 15:10 ASKAPsim.FLASH.cont. image .restored.fits - rw-rw-r -- 1 whi550 at-astro 50M 2010-12-10 15:10 ASKAPsim.FLASH.cont.imagemodel.fits - rw-rw-r -- 1 whi550 at-astro 127M 2010-12-14 10:15 ASKAPsim.FLASH.cont. model .input.fits - rw-rw-r -- 1 whi550 ...

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• http://www.atnf.csiro.au/research/masermeeting/web_papers/309_Goss.pdf
• http://www.atnf.csiro.au/pub/people/atzioumi/vsop_ao2/stj_ao2_gps.ps
• http://www.atnf.csiro.au/pub/people/atzioumi/iau164/tziou.ps

Text of these problems is available also in other languages : . ... What can one see in the Moon's sky more often - the Sun or the Earth? ... There are about of 250 millions of stars in the elliptical galaxy M32 (a satellite of Andromeda galaxy). ... The masses of Capella's components. ... You are proposed to estimate the masses of Capella's components, using our observational data. ... A galaxy's mass. ... Estimate the mass of FGC 1908 and compare it to the mass of our galaxy. ...

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... 2008 December 1 . Massive Stars Resolved in the Carina Nebula . ... Explanation: How massive can stars be? ... Such was the case for two of the brightest objects visible in the open star cluster Trumpler 16 , located in the southern Carina Nebula . ... The Carina Nebula , home to unusually shaped dust clouds and the famous variable star Eta Carina , lies about 7,500 light years away toward the constellation of Ship's Keel ( Carina ). ... About APOD | ... A service of: ASD at NASA / GSFC . ...

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• APOD: 2015 September 16 - Bright Spots Resolved in Occator Crater on Ceres
• APOD: 2009 August 5 - Betelgeuse Resolved
• APOD: 2012 June 28 - In the Glare of Alpha Centauri

... We have made observations of the Perseus cluster with the Westerbork Telescope at 610 MHz. ... Several newly detected sources are identified with cluster galaxies. ... No evidence is found for the existence of the previously reported ~ 65'x25' cluster halo, 3C 84B. Key words: radio galaxies - clusters - tailed radio sources buoyancy The Perseus Cluster of galaxies is one of the most fascinating systems accessible to extragalactic astronomers. ...

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• The 7C(G) survey
• RATAN-600 NCP bright radio sources
• A fast-scan extragalactic source survey at 4.755 GHz

... 2009: . ... New Wolf-Rayet Type Star. ... It was discovered that the peculiar velocity of the star is about 50km/s, and that it was discarded from a young star cluster. ... Based on the observational data from the 6-m telescope and from other sources, it was shown with high reliability that chemically peculiar stars with strong depressions in their continuum energy distributions possess the magnetic fields and rotation periods 2 and 3 times larger, respectively, than the stars with weak depressions....

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• CH Cyg
• Detection of unique bright radio flare of X-ray binary
• Optical component of GRB080319B

... Bright Spots Resolved in Occator Crater on Ceres . ... Credit Copyright: NASA , JPL-Caltech , UCLA , MPS/DLR/IDA Explanation: What created these bright spots on Ceres? ... Dawn is scheduled to continue to spiral down toward Ceres and scan the dwarf planet in several new ways that, it is hoped, will determine the chemical composition of the region and finally reveal the nature and history of the spots. ... Dwarf Planet, Bright Spot . Dark Craters and Bright Spots Revealed on Asteroid Ceres . ...

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• Massive Stars Resolved in the Carina Nebula
• Астронет > Massive Stars Resolved in the Carina Nebula
• Betelgeuse Resolved

Orbital elements of binary components in a hierachical system can be fit to either the visibility data directly or to the separation and position angle data. ... Then use Data|Astrometry to read a previously prepared file ("zetuma.psn") containing the positional data. ... Semi-major axis = 8.4214471 . Semi-minor axis = 4.7663976 . ... We can now use the Thiele-Innes method to estimate the orbital elements from this apparent ellipse and the data, as implemented with the Util|Orbit button. ...

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• The Brightness of the Night Sky
• The Very Large Telescope Project
• ESO - Newsletter January 2016

... Armagh Observatory, College Hill, Armagh BT61 9DG, +44 (0)28 3752 2928 . ... Lightcurve of HW Vir from images obtained using the Faulkes Telescope South, operated by Las Cumbres Observatory . The blue triangles show the difference between two stars whose brightness is constant. ... This shows the value of the Faulkes Telescopes in the follow-up observations of eclipsing binaries with the aim to detect and characterise additional circumbinary companions. ...

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• Armagh Observatory
• Explosive Events
• Doppler Imaging and Flare Activity on HR1099

Role in the Universe IAU Symposium 209, 2002 M. Dopita, S. Kwok and R.S. Sutherland, eds. Near-infrared monitoring of the carbon star IRC +10 216 : A high spatial-resolution time sequence of dust -shell evolution G. Weigelt , T. Blocker, K.-H. Hofmann, A. Men'shchikov, J.M. Winters Max{Planck{Institut fur Radioastronomie, 53121 Bonn, Germany Y. Balega Special Astrophysical Observatory, Nizhnij Arkhyz, 35147, Russia The carbon star IRC +10 ... 2000, Tuthill et al. 2000). ...

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• http://mavr.sao.ru/hq/balega/PUBL_BAL/PUB_2006/malogolovets.ps
• Bispectrum speckle interferometry and future long-baseline interferometry of
• GRB follow-up team

. Back to A.Zasov's homepage.

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... W e study the SPS for each of regions in the Bridge, as a function of velocity and of velocity integrated width. ( v): There is considerable variation in the HI structure throughout the MB. W e probe the power spectra for four different regions in the Bridge (see Figure 1). ... W e find that the northern regions have a peak value of (v) which is ver y distinct from the sout her n regio ns. ( dv): The variation of the power spectrum index, as a function of velocity is shown in Figure 3. ...

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• GRB030329
• CIMA Software Components

NMW survey overview . Access image archive . ... The New Milky Way survey aims to detect bright (V<13.5) optical transients near the Galactic plane using an automated wide-field (8x6 deg.) system capable of surveying the whole Milky Way area visible from the observing site in one night. ... All images obtained during the transient search survey are available online (please use the image archive access form ). ... Images per field: . ... Images per night: . ... Milky Way imaging time: . ...

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... 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. ...

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• http://www.gao.spb.ru/english/publ-s/viii-rfs/p091.pdf
• Conferences

... The HST uses an onboard model of its orbit to perform in real-time various control functions relating to spacecraft operations and observation support. ... New coefficients for the ephemeris are updated every other day, and are archived as FITS keywords for each HST observation data set. Using these coefficients,an observer can perform a variety of calibration and characterization calculations relating to the orbital position and velocity of the telescope. ...

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• ETCs and Observations Simulation at the VLT
• See Spike Run... Run, Spike, Run
• ADASS 2003 Conference Proceedings

... The bright supernova (hereafter SN) in the galaxy NGC 4527 was first sighted by S. Knight (USA) on April 13.17UT at magnitude ~14.0v. The report of the sighting was subsequently forwarded by phone to the AAVSO. ... SN 1991T. The galaxy NGC 4527 is an Sb(s)II type galaxy with an apparent Blue magnitude of 11.32 (Shapley-Ames, 1981). ... An analysis of this event utilizing visual observations by amateurs, plus a light curve is presented.. ... THE LIGHT CURVE: . ... ISN SN 1991T web page . ...

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• Bright Supernova Bright Supernova
• Supernova 2000db in NGC 3949
• Supernova 2002fk in NGC 1309

... arXiv.org . astro-ph . ... We fit the near-infrared to radio spectral energy distributions of 30 luminous and ultra-luminous infrared galaxies with pure starburst models or models that include both starburst and AGN components to determine important physical parameters for this population of objects. In particular we constrain the optical depth towards the luminosity source, the star formation rate, the star formation efficiency and the AGN fraction. ...

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. Additional settings . Number of observations found: . 17 . ADS number: . 03353 . WDS number: . 04385+2656 . Components: . AB . All (17) . Photo (15) . CCD (2) . Epoch . JD . Separation . e(S) . N(S) . e1(S) . Pos.angle . e(P) . N(P) . e1(P) . N . Orient. Meas.code . Detector . Back . Abbreviations . Main Page .

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... Called Gliese 623b or Gl623b, the diminutive star (right of center) is ten times less massive than the Sun and 60,000 times fainter. ... The image file is on oposite.stsci.edu in the directory /pubinfo/gif: PR# GIF File Caption text Object STScI-PRC94-54 Gl623b.gif G1623b.txt Dwarf Star Gliese 623b The photo release text is in the directory /pubinfo/press-releases: PR# PR text STScI-PRC94-54 PR-54.txt Another directory, /pubinfo/latest, contains all of the files relevant to the latest releases. ...

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• Procedures for Observations
• The puzzling core of the Phoenix cluster: deep X-ray observations
• Youngest Brown Dwarf Yet in Multiple Stellar System (ESO Press Release 16/00)