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http://xray.sai.msu.ru/~mystery/articles/review/node84.html.

1. Extragalactic Gravitational Wave Background
Next: Gravitational Wave Background from Previous: Galactic Gravitational Wave Background . ... It is intuitively clear that at frequencies above the critical ones for our Galaxy, one will detect rare bright jerks produced by coalescing white dwarfs   (at a rate of 1 per 100 year) and NS (at a rate of 1 per - year) in our Galaxy, against a background of the extragalactic stochastic GW. ... Firstly we consider GWB from close individual galaxies, and then will discuss overall extragalactic GWB. ...
[ Сохраненная копия ]  Ссылки http://xray.sai.msu.ru/~mystery/articles/review/node83.html -- 4.5 Кб -- 04.03.1997
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2. http://www.atnf.csiro.au/research/pulsar/ppta/uploads/Main2/PPTA_Angular_2012Oct_v1.pdf
... 2011) What is Mathematica? Slide 5 of 13 Notation & Assumptions Assuming: GW distance R >> pulsar distance D, = 0, pulsar sky direction precisely known independent noise between frequency bins and across different pulsars (OK for high f) Ignoring O x 2 curvature term in r x see however Deng, X . et al 2011 on the effect GW n Pulsar k Earth x 0 Pulsar p r (x) R 0 Earth GW What is Mathematica? ... n , rL 1 pulsars Earth L, M, J, K 1, 2, .. ... Np pulsars , IJ XI A XI ,IJ rI d00,I rJ . ...
[ Текст ]  Ссылки http://www.atnf.csiro.au/research/pulsar/ppta/uploads/Main2/PPTA_Angular_2012Oct_v1.pdf -- 817.9 Кб -- 17.10.2012
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3. SAO RAS home page
... Дни открытых дверей к юбилею САО РАН (12-14 апреля 2016 г.) . Международная конференция "Dark Ages and White Nights (Spectroscopy of the CMB)" (20-24 июня 2016 г.) . ... Международная конференция MULTI-SPIN GALAXIES - 2016 (26-30 сентября 2016 г.) . Международная астрономическая конференция "Физика звезд: от коллапса до коллапса" (3-7 октября 2016 г.) Архив . ... Подробнее.. ... 10.02.16 . ... БТА в реальном времени . ... Цейсс-1000 в реальном времени . ... Последнее обновление: 22/03/2016 ...
[ Сохраненная копия ]  Ссылки http://www.sao.ru/ -- 11.4 Кб -- 09.04.2016
[ Сохраненная копия ]  Ссылки http://mavr.sao.ru/ -- 11.4 Кб -- 09.04.2016
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4. Background
Next: Optimal Combination Up: Optimal Combination of Sub-Stepped Previous: Optimal Combination of Sub-Stepped . The diodes of both GHRS detectors are spaced on 50 m centers. ... The spectrum projected on the 500 diodes is therefore not well sampled, with only one diode per resolution element. ... This procedure, which can also be accomplished together with sampling of the adjacent background, is fast and efficient in terms of observing time. ... where Dn refers to diode n and sn to substep n . ...
[ Сохраненная копия ]  Ссылки http://www.stsci.edu/stsci/meetings/irw/proceedings/walshj.dir/section3_1.html -- 3.9 Кб -- 15.06.1994
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5. Wavelength Calibration at Moderately High Resolution
... The calibration of astrophysical spectra in wavelength based on calibration lamp data suffers from different kinds of uncertainties. Besides inaccuracies in the observational phase, common data reduction practice adds ``pixelation'' errors, due to the fact that the centering method does not use the correct PSF. These model mismatch errors depend, for a given feature, on the sub-pixel location of the line center (David & Verschueren, private communication). ...
[ Сохраненная копия ]  Ссылки http://www.adass.org/adass/proceedings/adass94/decuyperjp.html -- 12.1 Кб -- 03.11.2000
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6. Background: motivation for developing this procedure
... Meta Index / Home Page / Description / Soft flare rejection for . The EPIC-pn fast timing mode was designed so that a time resolution of 0.029 milliseconds can be achieved. ... Below this energy the data is affected by so-called soft flares which are caused by stack overflows generated by high energy particles. These so-called soft flares have sharp rise (from 0 counts/sec to several thousand counts/sec in 0.10-0.15 sec) then decaying back 0 counts/sec slightly slower in about 0.3-0.4 sec). ...
[ Сохраненная копия ]  Ссылки http://xmm.vilspa.esa.es/sas/6.5.0/doc/epreject/node7.html -- 5.2 Кб -- 15.08.2005
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7. http://zebu.uoregon.edu/~uochep/talks/talks05/trackrecon.pdf
SiD Tracking using VXD Nick Sinev, University of Oregon Plan Motivation Track reconstruction algorithm Performance for single tracks Does it have any limits ? With backgrounds To do Motivation Tracking in SiD is a challenge, especially pattern recognition. ... Limitations caused by reconstruction speed consideration In the presence of high number of background hits, number of 3-point combinations used as track seed became enormous if we consider all combinations. ...
[ Текст ]  Ссылки http://zebu.uoregon.edu/~uochep/talks/talks05/trackrecon.pdf -- 174.2 Кб -- 29.03.2005
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8. NICMOS and the VLT: A New Era of High Resolution Near Infrared Imaging and
... ST-ECF, ESO, STScI and the NICMOS IDT organized a workshop on near infrared imaging from space and ground was held in Pula on May 26-27, 1998. ... The meeting was held in May 1998, about one year after science observations started with NICMOS, and about half a year before the Infrared Spectrometer and Array Camera (ISAAC) starts to operate on the VLT. Currently, it is expected that NICMOS will operate until the end of 1998. ...
[ Сохраненная копия ]  Ссылки http://www.stecf.org/conferences/meeting/ -- 4.8 Кб -- 13.06.2006
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9. Astrophysics Group VSA
... Astrophysics Group . ... VSA . ... CAT . ... The Very Small Array is a custom-built radio telescope (operating between 26-36 GHz), designed expressly to make high resolution observations of the cosmic microwave background (CMB) radiation on angular scales around and below one degree. ... The VSA has been operated in ?compact array? and ?extended array? configurations (see the technical description below) and data collected to achieve high sensitivity in both regimes have been analysed. ... 1.75 GHz)...
[ Сохраненная копия ]  Ссылки http://www.mrao.cam.ac.uk/outreach/radio-telescopes/vsa/ -- 20.2 Кб -- 10.04.2016
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10. ASP: The New and Improved Hubble Space Telescope
... We can help students grasp the significance of Hubble's extremely keen eye, and learn a bit about angles and math in the process, with the following in-class activity. ... Looking through binoculars or telescopes allows us to magnify a small section of the sky. To measure sizes or distances in that small section, astronomers divide a degree into 60 smaller pieces called arcminutes, and further subdivide minutes into 60 smaller sections called arcseconds. ... 30 feet = . ... 36 seconds . ...
[ Сохраненная копия ]  Ссылки http://www.astrosociety.org/edu/publications/tnl/26/hubble2.html -- 16.0 Кб -- 02.10.2012
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11. *imcalc* - Obtain a background subtracted image for ROSAT PSPC Data
... Use the ROSAT broad band background which is a array file at 1/30 the *.qp file resolution, and contains data from PI bins 7-240. input files: xdata$rp110590.qp; xdata$rp110590_bk1.imh . ... xr> ximages xi> imcalc input file ('-' for STDIN) or imcalc commands: - # Interactive mode IMC) IMC) rp90_a.imh = xdata$rp110590.qp[bl=30,pi=7:240] - xdata$rp110590_bkl.imh # Select same size and channels as the background map # and subtract the background IMC) quit # To exit the interactive mode and imcalc . ...
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