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http://www.adass.org/adass/proceedings/adass02/P4-10/.

1. APOD: 2001 March 8 - Bright Venus
... 2001 March 8 . Bright Venus . ... That's no star, that's planet Venus the second "rock" from the Sun . Blazing at -4.6 magnitude , Venus, after the Sun and Moon, is the third brightest celestial body in planet Earth's sky . ... This causes Venus to look brighter as it looms large in its crescent phases than when it is smaller and nearly full. Taken on January 28th, this dramatic picture finds a crescent Venus near its brightest to the right of a crescent Moon. ... About APOD | ...
[ Сохраненная копия ]  Ссылки http://www.sai.msu.su/apod/ap010308.html -- 4.7 Кб -- 01.10.2012
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2. http://www.adass.org/adass/proceedings/adass02/reprints/P4-10.pdf
... Classifiers We apply machine learning methods to generate classifiers from `training' data sets, each set being a particular sample of ob jects with pre-assigned class names that have measured X-ray fluxes and, wherever possible, data from other wavelength bands. ... Figure 1. ... With ClassX, one can isolate sources with a greater degree of class name ambiguity and look into why their classification in the training set differs from the OC1 classification (see Figure 2). ...
[ Текст ]  Ссылки http://www.adass.org/adass/proceedings/adass02/reprints/P4-10.pdf -- 390.6 Кб -- 11.03.2003
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3. Observing Faint Targets Near Bright Objects
... The concerns here are similar to those for observing bright targets; saturation and blooming of the bright companion PSF must not impact the faint target. Also, one may need to consider subtracting the PSF of the bright object, and effects which limit the accuracy of that subtraction. If the bright companion will saturate and bloom, it will be necessary to rotate the CCD so that blooming along the CCD columns does not obliterate the faint target. ...
[ Сохраненная копия ]  Ссылки http://www.stsci.edu/instrument-news/handbooks/wfpc2/W2_69.html -- 8.9 Кб -- 24.07.1996
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4. Low Surface Brightness Galaxy Gallery
In this gallery are many images of Low Surface Brightness Galaxies which have recently been discovered and analyzed. ... The central surface brightness of this galaxy is 24.28 . Malin 2 This galaxy is another huge disk galaxy with a scale length of 15 kpc and a redshift of 15000 km/a. The high surface brightness knot in one of its spiral arms actually has the same color, luminosity and H-alpha equivalent width as the entire Large Magellanic Cloud . ... Truly it is a Low Surface Brightness Galaxy. ...
[ Сохраненная копия ]  Ссылки http://zebu.uoregon.edu/sb2.html -- 4.8 Кб -- 26.05.2000
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5. Analysis of very bright sources
XMM-Newton Science Analysis System . ... A different approach is done via the setting withctisrcpos =Y: all event energy corrections do not use the actual RAWY coordinate but the corresponding RAWY location of the source ( SRCPOS ) as determined by the task epframes (either automatically or via setting withsrccoords =Y). ... The task epchain may be used with the setting ccds =4 withctisrcpos =Y to process only the CCD 4 where usually the bright source is located that causes the Out-of-Time events. ...
[ Сохраненная копия ]  Ссылки http://xmm.vilspa.esa.es/sas/7.0.0/doc/epevents/node8.html -- 4.8 Кб -- 28.06.2006
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6. Астронет > Albireo: A Bright and Beautiful Double
... Albireo: A Bright and Beautiful Double . ... Such is the case of the bright double star Albireo . Seen at even slight magnification, Albireo unfolds from a bright single point into a beautiful double star of strikingly different colors. ... The brighter yellow star is itself a binary star system, but too close together to be resolved even with a telescope. ... Публикации с ключевыми словами: star system - двойные звезды . Публикации со словами: star system - двойные звезды . ...
[ Сохраненная копия ]  Ссылки http://www.astronet.ru/db/msg/1207743/eng/ -- 21.4 Кб -- 30.08.2005
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7. HIPASS Bright Galaxy Catalog
... The two plots below illustrate two of the selection criteria: velocity width (limited by the channel width) and the HIPASS peak flux. Zoom-in on Figure 3a. The two plots below give some idea of the shape of the HI spectra. ... For Gaussian HI spectra the difference is slightly more, but for irrgeular galaxies, pairs and groups many different shapes are observed. ... Some trend towards detecting more narrow-width galaxies at higher velocities is visible. ...
[ Сохраненная копия ]  Ссылки http://www.atnf.csiro.au/people/bkoribal/BGals/comparisons.html -- 2.8 Кб -- 23.12.2007
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8. ASP: Star Science in the Autumn Sky
Once students get the hang of it, they can find and measure the brightness of Delta Cephei in a few minutes. ... of Delta Cephei . ... Oct. ... The following table lists the measurements of Delta Cephei made by one amateur astronomer in autumn 1990. ... 4.0 . ... This activity is a simplified version of one that appeared in Hands-On Astrophysics, a series of activities prepared by the American Association of Variable Star Observers with support from the National Science Foundation. << previous page | ...
[ Сохраненная копия ]  Ссылки http://www.astrosociety.org/edu/publications/tnl/32/starscience4.html -- 18.8 Кб -- 02.10.2012
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9. Why can I only see six of the ``Seven Sisters''?
Two major reasons: the number of stars isn't really seven (it's many more), and they all have different brightnesses, so that you see more or fewer of them depending on viewing conditions. The brightness of stars is measured on the magnitude scale, where the most prominent stars in the sky are around 1st magnitude, and the faintest you can see with your eye are about 6th. ... I think this makes it quite likely that the list will be truncated at Taygeta, giving six visible stars. ...
[ Сохраненная копия ]  Ссылки http://www.naic.edu/~gibson/pleiades/pleiades_see.html -- 7.7 Кб -- 05.04.2007
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10. The AstroStat Slog Blog Archive Magnitude [Eqn]
... Archives . ... Differential Emission Measure [Eqn] . ... Astro 301, class 1, and it took all of 20 minutes of talk about stellar magnitudes to put that notion to permanent rest. ... Now, it turns out that the human eye perceives brightness on a log scale, so magnitudes are numerically similar to log (brightness). ... frac{5}{2}\log_{10}\left(\frac{f_{object}}{f_{standard}}\right) \,,$$ . ... frac{5}{2}\log_{10}\left(\frac{L_{object}}{4 \pi d^2}\frac{1}{f_{standard}}\right) \,.$ ... Chandra Blog . ...
[ Сохраненная копия ]  Ссылки http://hea-www.harvard.edu/AstroStat/slog/groundtruth.info/AstroStat/slog/2008/eotw-magnitude/index.html -- 22.9 Кб -- 01.03.2014
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11. Nova in M31 2000 3
Nova in M31 2000 3 . ... From Giovanni Sostero (Remanzacco Observatory): at the end we have found a good Nova candidate in the course of our monitoring program in M31. ... Remanzacco Observatory Light curve This is a preliminary lightcurve of Nova M31-3 from the images we collected and those provided by others. ... vsnet-alert 5346 ] [FWD] Suspected Nova in M 31 . ... vsnet-alert 5349 ] (fwd) M31 possible nova . ... vsnet-alert 5355 ] [FWD] New image of the possible Nova in M31 (GSo) . ...
[ Сохраненная копия ]  Ссылки http://www.sai.msu.su/mirrors/isn/sn2000/nm313.html -- 8.8 Кб -- 22.12.2007
[ Сохраненная копия ]  Ссылки http://www.rochesterastronomy.org/sn2000/nm313.html -- 8.8 Кб -- 19.04.2014
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12. Phil Plait's Bad Astronomy: Misconceptions
... Bad Astronomy . ... Bad Astronomy: The North Star, Polaris, is a very bright star. Good Astronomy: Polaris is a middling-bright star, easily missed. ... He said it was close to Polaris, the North Star, but he also said it was in the East. ... It's natural,