... We have been using it to analyze PC images of known gravitational lenses and QSOs which are candidates for lensing (Falco 1993). ... Fig. 1 plots the higher contours of the PC image of 0142 in the upper left, and its power spectrum in the upper right. ... If we fit the envelope of the power spectrum with a binary model, we find that best fit gives a separation of the two components of 1.3 PC pixels or about 58 mas. ... The lower two curves are cuts through the 0142 power spectrum. ...

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• Fine Guidance Sensor Instrument Handbook
• Stellar Photometry
• Which Instrument to Use: WFPC2, FOC, NICMOS, or STIS?

... The sample of the Local Volume galaxies (distance smaller than 10 Mpc) gives a unique opportunity to study the properties of galaxies including the weakest objects: the absolute magnitude M B -10 and the virial mass M vir 10 9 M x263C;. ... Luminosity function of the Local Volume galaxies. ... The luminosity functions for galaxies are presented: red dashed line - from the 2dFGRS survey (Norberg et al. 2002); blue dash-dotted line - from the SDSS survey (Blanton et al. ...

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• Solar system sector, archive 1994
• Optical component of GRB080319B
• Galaxy sector, archive 1994

... OCR by H.Andernach 1/96, to be proof-read) This is the first of a series of papers presenting results of a 10-GHz radio continuum survey of the galactic plane region using the 45-m telescope at Nobeyama. ... Weak Nonthermal Sources: A comparison with the Bonn S-GHz survey reveals a number of weak nonthermal sources near the galactic plane. ... For this reason we conducted a survey of the galactic plane region at 10 GHz using the 45-m radio telescope at the Nobeyama Radio Observatory (NRO). ...

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• Principal Components Analysis
• Introduction
• A 20 cm VLA survey of Abell clusters of galaxies

... About ATNF overview . ... Australia Telescope Steering Committee . ... Murchison Radio-astronomy Observatory . ... Parkes radio telescope . ... Australia Telescope 20GHz Survey . ... Bright prospects: Comparing the H Survey with large-scale radio continuum emission . ... Prospects for comparisons between the AAO/UKST H \ survey and large-scale radio continuum emission are considered, with particular reference to the recently completed Parkes 2.4-GHz survey of the southern Galactic Plane. ...

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• casacore: components/ComponentModels.h Source File
• casacore: components package (libcasa_components)
• casacore: ComponentModels_module

XMM-Newton CCF Release Note XMM- CCF -REL-176 RGS QUANTUMEF Shortest-Wavelength Correction Factors A.M.T. Pollock July 27, 2004 1 CCF components Name of CCF VALDATE List of Blocks changed XSCS ag RGS1 QUANTUMEF 0013 1998-01-01T00:00:00 RGA EFFAREACORR NO SI1 SI2 SI3 SI4 SI7 RGS2 QUANTUMEF 0014 1998-01-01T00:00:00 RGA EFFAREACORR NO SI1 SI2 SI3 SI4 SI5 SI7 2 Changes Near the short-wavelength end of the RGS bandpass, the instrument ... The best- t power-law indices, , are shown. ...

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• http://xmm.vilspa.esa.es/calibration/documentation/epic_cal_meetings/201504/Maitra_Cal_2015.pdf
• http://xmm.vilspa.esa.es/docs/documents/CAL-SRN-0055-1-0.ps.gz
• http://xmm.vilspa.esa.es/sas/6.5.0/doc/esrcselect.ps.gz

... 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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• ADASS 2003 Conference Proceedings
• GIM2D: An IRAF package for the Quantitative Morphology Analysis of Distant
• A Computer-Based Technique for Automatic Description and Classification of

The ESA/ESO Astronomy Exercise Series 2 . The Distance to Messier 100 as Determined by Cepheid Variable Stars . ... The small variations in distance to the individual Cepheid variable stars in the Cloud are negligible compared with the much larger distance to the SMC. ... In this way Cepheid variable stars can be used as one of the 'standard candles' in the Universe that act either as distance indicators themselves or can be used to calibrate (or set the zero point for) other distance indicators. ...

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• ASP: Star Science in the Autumn Sky
• ASP: Accidental Astrophysics: The Devil's In the Magnitudes, Part II

... 22.02.2011 . ... Credit Copyright: morn1415 (YouTube) Explanation: How big is our Sun compared to other stars? In a dramatic and popular video featured on YouTube , the relative sizes of planets and stars are shown from smallest to largest. ... Note that the true sizes of most stars outside of the Sun and Betelgeuse are not known by direct observation, but rather inferred by measurements of their perceived brightness , temperature , and distance. ... Publications with keywords: star - planet . ...

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• Journal "Peremennye Zvezdy"
• Light from a Extra Solar Planet
• XWare > APOD

Star formation is often best manifested by bright H II regions.These are regions of hydrogen which have been ionized by ultraviolet photons which are emitted from massive stars (typically stars more than 20 times the mass of the Sun). ... A narrowband filter image centered on this wavelength will then readily reveal these H II regions and hence the current sites of star formation in a galaxy, The luminous blobs that can be seen here are all H II regions . ... NGC 3558 Visual . NGC 3558 Infrared . ...

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• Low Surface Brightness Galaxy Gallery
• Evidence for Dark Matter
• HST Deep Field Data

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. ...

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• ISOGAL YSO Candidates (Abstract)
• Cannibal Stars Cause Giant Explosions in Fornax Cluster Galaxy (ESO Press
• A homogeneous chemical analysis of the inner Galactic disk from the first data

On March 29, 2003, an exceptionally bright Gamma-Ray Burst (GRB) was discovered by the HETE-2 satellite (Vanderspek et al. ... 2003, GCN, 2020, 1), GRB 030329 is the nearest cosmological burst detected to date, and its extreme brightness can be attributed to its proximity. ... In the fourth epoch, 51 days after the burst, GRB 030329 appeared resolved at 15 GHz with a component appearing to the north east at 0.28 +/- 0.05 mas from the main component (Fig. a). ... days after the burst. ...

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• NGC7674.html
• Thesis Figures

... I happened to observe a surge of principle component analysis (PCA) and independent component analysis (ICA) applications in astronomy. ... Category: Algorithms , arXiv , Astro , Cross-Cultural , Data Processing , Jargon | ... Algorithms arXiv Astro Bad AstroStat Bayesian CHASC Cross-Cultural Data Processing Fitting Frequentist Galaxies gamma-ray High-Energy Imaging Jargon Job Languages MC MCMC Meta Methods Misc News Nuggets Objects Optical Physics Quotes Spectral Stars Stat Timing Uncertainty X-ray...

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• The AstroStat Slog principle component analysis
• The AstroStat Slog Blog Archive [ArXiv] component separation methods
• The AstroStat Slog component separation

... A detailed study of two consecutive bright points observed simultaneously with CDS, EIT and MDI is presented. The analysis of the evolution of the photospheric magnetic features and their coronal counterpart shows that there is a linear dependence between the EIT Fe XII 195? flux and the total magnetic flux of the photospheric bipolarity. ... In a follow-up study, we used wide slit (90arcsec240arcsec) movies of four EIT coronal bright points (BPs) obtained with CDS. ...

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• Terry Mosely's Bulletins
• Observations with the Faulkes Telescopes
• Armagh Observatory

... Flux density at 1 GHz (/Jy): 25 . ... ADS . ... Caswell et al. 1975, A&A, 45, 239. ... Arecibo S 430 MHz =82?51 Jy, also Algonquin 46-m at 10.6 GHz (3': S=12?2 Jy), and Haystack 36-m at 15.5 GHz (2'.3: S=8.5?3.0 Jy). ... 1985, ApJ, 296, 461. VLA at 1.4 and 5 GHz (8''), plus Einstein observations. ... VLA at 327 MHz (3'.5?3'.6: S=46.3 Jy). ... ASCA and ROSAT observations. ... VLA at 1.5 GHz (6".9?6".6) and 4.8 GHz (46".4?5".6), including polarisation and comparison with ROSAT image. ...

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• Inference of Coefficients for Use in Phase Correction
• G327.6+14.6
• G111.7-2.1

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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. Comment on J1130-1449 . There are two dominant components in our image. Comparison with the 15 GHz image of Kellermann et al. (1998) reveals that the western component is brighter at the higher frequency, indicating that the brighter (eastern) component in our image may have a steep spectrum. VLBApls home page . Last modified: 16 Oct 2000

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... 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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• Supernova 2000ch in NGC 3432
• Common problems
• Bright Supernova Bright Supernova

... 2005 April 5 . Light From A Distant Planet . Illustration Credit: R. Hurt ( SSC-Caltech ), JPL-Caltech , NASA . Explanation: Light emitted by a planet far beyond our Solar System has been identified for the first time. The planet, illustrated in the above drawing , had its light detected by comparing the brightness of only the parent star, when the planet was behind the star, to the light emitted when both the planet and its parent star were visible. ... About APOD | ...

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• APOD: 2013 June 6 - Star Size Comparisons
• APOD: 2011 February 22 - Star Size Comparisons
• APOD: 2007 February 27 - Atmospheres Detected on Two Extrasolar Planets

To appear in "Fourth Workshop on Robotic Autonomous Observatories (2015)"RevMexAA(SC) METEOR OBSERVATIONS WITH MINI-MEGATORTORA WIDE-FIELD MONITORING SYSTEM S. Karpov, 1, 3 N. Orekhova2 G. Beskin, 1, 3 A. Biryukov3,4 S. Bondar,2 E. Ivanov,2 E. Katkova,2 A. Perkov, and V. Sasyuk3 RESUMEN 2 Favor de prop orcionar un resumen en espanol. ... The faintest detected meteors has the peak brightness about 10 mag, while the ma jority - from 4 to 8 mag. ... 2010; Karpov et al. 2013; Beskin et al. ...

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• astro-ph

... The components have a steady phase but variations of 303 Gilcreek 2460 2272 2454 2448 2268 2442 2436 2264 1985 1990 1995 2000 2005 2390 2388 2386 2384 1985 1990 1995 2000 2005 Kashima 2132 2128 2124 2120 2116 Kokee-Kauai 1985 1990 1995 2000 2005 2390 2388 2386 2384 1985 1990 1995 2000 2005 1985 1990 1995 2000 2005 Onsala Westford 2240 2238 2236 Wettzell 1985 1990 1995 2000 2005 Figure 1. ... 2246 2244 2242 2240 2238 2236 2234 1985 1990 1995 2000 2005 BKG GSF IAA MAO IVS Figure 3. ...

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• http://www.gao.spb.ru/english/personal/malkin/publ/zm07c.pdf
• http://www.gao.spb.ru/english/as/j2014/presentations/brzezinski.pdf
• http://www.gao.spb.ru/english/personal/malkin/publ/zm12m.pdf