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. ...

... 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 . ...

... 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 ...

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 . ...

... 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). ...

... 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). ...

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. ...

... 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. ...

... 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)...

... 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 . ...

... 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 . ...

... 6.02.2002 . ... Credit: A. Kashlinsky ( SSAI ) S. Odenwald ( Raytheon ), 2MASS , NSF , NASA Explanation: What cosmic wallpaper is on the sky? ... Recently, however, the background in near infrared light was imaged at high resolution by the 2MASS telescope , and confirmed earlier estimates that it is over twice as bright as originally expected. ... Visible is light emitted from the very first stars and galaxies in the universe , emitted when the universe was less than half its current age. ...

To main of Laboratory . The research work and design of optical and optical-electronic devices are carries out by laboratory staff: . ... Lens: . ... In the layout 1 prism systems perform functions of dispersive element, corrector of aberrations, optical reducer. ... Spectral range 200 - 400 nm; . ... Back Forward . ... The main corrector's function are compensation of field aberrations of the main spherical mirror of a telescope (diameter of 600 mm, f'=1200 mm) and increase aperture ratio. ...

To see a Russian version of this page, click here . ... Graduated from Moscow State University (MSU), Faculty of Physics in 1976. Ph.D. degree - 1988, MSU. Main field of scientific activities: photometric investigations of various stars, close binary stellar systems and other astronomical objects, including research with use of fast photoelectric photometry with a high time resolution till 1 millisecond. ... New portable photometer . ... Send your mail to: tem@sai.msu.ru ...

... Data was taken with lbw and the mock spectrometers on 05may09 to investigate the problem with higher time resolution and bandwidth. ... 6 172 Mhz bands were taken centered at: 1200,1300,1400,1500,1600, and 1700 Mhz. 8192 channels (20Khz resolution) was used for the low time resolution (.1 second dumps). 4096 channels (40Khz resolution) was used for the high time resolution (.001 second dumps). ... The total power was computed for each 172 Mhz band and then plotted vs time (.1 second resolution). ...

... Therefore, we see that some spectral resolution is achieved by selection of the wavelet size, and some temporal resolution follows from the location of the wavelet relative to the signal (Fig. ... Figure 6: Contour line representation of the wavelet transform for a near-continuum of durations. We can identify the individual peaks and troughs of the cosine wave as well as their frequency: this compromise between the temporal domain and the spectral domain is the hallmark of wavelet transforms. ...

We present observational radial velocity curves for 12 chromospherically active binary systems and individual measurements for a further 5 systems. ... Six of our target binaries do not agree with published ephemerides or orbital parameters. We also present a rigourous derivation of the resolution limit for binary star cross-correlation radial velocities. ... Key Words: stars:binaries:close-stars:binaries:spectroscopic-techniques: radical velocities. ...

Limiting Resolution . The terms MTF cutoff frequency, limiting resolution, and resolving power have all been used interchangeably to define the smallest target that can be resolved with an imaging system. Although the term 'limiting resolution' is often used to describe the smallest target length that can be imaged. ... For example, high frequency targets can be reproduced from their low frequency fundamentals and phase errors can produce 'phantom' images that resemble high frequencies. ...

... Science Users Information > Science Publications > Science Announcements > Improvement to FLAMES Spectral Resolution and Sensitivity . ... The FLAMES GIRAFFE spectrograph is not kept at a controlled temperature, and thus, at the beginning of every observing block, GIRAFFE is re-focussed to take account of collimator temperature. ... The updated values lead to a substantial increase in spectral resolution and sensitivity across all settings, particularly for the high resolution ( HR ) settings. ...

Some recent results ( see ) attracted the attentions of astronomers working on field which could benefits from photon counting techniques with high speed and spatial resolutions as adaptive optics. ... Fasti has been designed to be fast and largerly configurable. ... The data rate attined in the best case (30 Mhz), give no impossible load to the digital acquisition in the photon counting mode, since data are 1 bit only, they can be parallelized, giving a maximum speed of about 940.000 32 bit word/sec. ...