... Values have been scaled arbitrarily. High ratios are shown in blue, corresponding to blue colors, and low ratios are shown in red, corresponding to red colors. ... Noise combined with background subtraction difficulties in the lower left quadrant of the WISP1 data (see Fig. \ref{Fig:wisp_snr_mskd}) make colors in this area very unreliable. ... The values shown here are typically a factor of ~3 less than those calculated for the Schmidt data, shown in Figure \ref{Fig:bj_alpha}. ...

... 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). ...

... 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 ...

... Set output projection (reference coordinate, pixel size) from the first input image Project corners of each input image into output frame to find the bounds of the output image Calculate size of output image in pixels from bounds and pixel size Check the POSCOROK keyword in the header of each input file and, if the value of this keyword is true then use the reference positions given by the ... Create output image Loop over input images Normalize each one by its exposure...

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. ...

... Bayesian and maximum entropy algorithms that use a constant balancing parameter present large residuals in the low or the high S/N regions depending on the value chosen for the parameter. ... This variation of the balancing parameter implies a variable resolution in the restoration, allowing high resolution with low bias in high S/N regions and a lower resolution with lower artifacts in poor S/N regions. We have applied the algorithm to the FOC and WF/PC cameras of the HST. ...

Next: Extragalactic Gravitational Wave Background Previous: Transparency of the Stochastic . Let the sky be observed with a detector having a pencil beam diagram across. The number of stars per frequency decade that is swept by the detector is a function of celestial coordinates (say, galactic coordinates l , b ): . ... It is clear from the figure that for an all-sky detector the Galaxy becomes transparent above the frequency  Hz. ...

Colorful Moon Mosaic . ... Credit Copyright: Noel Carboni Explanation: No single exposure can easily capture faint stars along with the subtle colors of the Moon. ... The fascinating color differences along the lunar surface are real, though highly exaggerated, corresponding to regions with different chemical compositions . And while these color differences are not visible to the eye even with a telescope, moon watchers can still see a dramatic lunar presentation tonight. ...

Fair" UV Coverage for a Multi-resolution John Bunton, CSIRO Telecommunications and Industrial Physics, Australia Introduction If we wish to have a multi-resolution telescope with equal point source sensitivity at all resolutions then we must accept that the baseline distribution of the correlations is predetermined. ... This occurs for each added step in resolution. ... It is seen that for the combined telescope the total number of correlations is 5.17 times the number needed for a single resolution. ...

The Library of Medium Resolution Spectra of Galaxies . HyperLeda home | Documentation | ... We have assembled in the frame of the HyperLeda FITS archive a Library of Medium Resolution Spectra of Galaxies. ... Spiral galaxies . ... 1998A .. ... Early-type galaxies . ... 131.. ... 1997A .. ... L98031HP1 Note: The observations of early-type galaxies from Jan. ... This library is supplemented with more recent spectra also taken with the CARELEC spectrograph, but with a EEV CCD 696x2048. ...

... 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. ...

... Instrument Status . Science Verification . ... CRIRES . ... SV observer shall submit their proposals using the Science Verification proposal template Proposers are asked to provide at least a short summary of the science goal, coordinates and magnitudes of GS and science target, a finding chart , the observing wavelength ID, as specified in appendix A of the UM and DIT, NDIT settings of science detectors as computed with the exposure time calculator (see below). ... with a 0.2 arcsec slit. ...

... 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 . ...

... NICS will be the only infrared instrument for the first light of the TNG; as a consequence, we decided to incorporate a sufficient degree of operation flexibility by providing the instrument with six different observing modes, three aimed at imaging and three at spectroscopy: . ... It will be possible to use the narrow band filters as order sorters; this will allow to perform high resolution long-slit spectroscopy in the wavelength ranges covered by the available narrow band filters. ...

... Research . ... I use interferometric arrays of telescopes to yield images with an angular resolution more than one hundred times better than that of the Hubble Space Telescope. ... As a result, the MROI will be able to image targets 10 times fainter than those accessible with any other interferometer, and it will be able to make images on timescales of hours instead of days (Buscher et al 2013). ...

... Let us first find out which way -- rise in spectral resolution with some loss in the S/N ratio or increase in the S/N ratio with a fixed spectral resolution -- is better for the purpose of reduction of equivalent width determination errors. ... N -- number of counts for 1 ? ... line equivalent width, . ... Thus if the spectral resolution is managed to be increased (i.e. to decrease )without loss in the number of counts falling at 1 ?, the equivalent width measurement error is then proportional to . ...

The next large instrument on a Gemini telescope, GHOST, is being built by a collaboration including AAO, ANU and NRC-Herzberg. It aims to be a high efficiency fiber fed Echelle spectrograph with a wide wavelength range. I will describe the designтАЩs background, including lenslet-based image slicing that reduces slit losses while maintaining high resolution, and why despite cost constraints, the spectrograph has several modes, including a precision radial velocity mode and a two object mode. ...

... 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 . ...

... This report provides background information about the Armagh Observatory and a summary of the Observatory's principal achievements in research and other areas during the reporting period, which is the Calendar Year 2002. ... Calendar Year . ... 66,000 . ... 134,000 . ... Apart from maintaining the level and quality of astronomical research carried out at the Observatory, the key task for the year is to continue to work with the DCAL to widen the Observatory's access to research development funds. ...

Armagh Planetarium Mars HiRISE Wallpapers . High Resolution Imaging Science Experiment (HiRISE) is flying onboard the Mars Reconnaissance Orbiter (MRO) mission. Mouse over the thumbnails for a larger view of the image. ... When the image has entirely loaded, right click on it and choose option 'Set as background' or 'Set as wallpaper' depending of your Windows version. ... Historical Images . ... Mars Wallpapers . 1024 x 768 px . 1600 x 1200 px . Image Info . ... 1600 x 1200 pix . ...