Exp osure Time and S/N calculated by the ETC for the G130M/1055 and G130M/1096 Settings are not correct The focus of the G130M/1055 and G130M/1096 settings were recently adjusted to increase their resolution. As a consequence, the sp ectral height and size of the resolution element (resel) have changed. ... The ETC assumes a resel of 30 pixels and an extraction height of 47 pixels, but the true resels are smaller and dep end on wavelength; the true extraction heights are larger. ...

... We present a computer program for modelling energy flux distribution and light curves of eclipsing binaries from far ultraviolet to infrared regions. The Roche model is assumed. Proximity effects of components (reflection of radiation and surface gravity darkening) are taken into account. ... Figure 1: The surface temperature distribution for Algol A-B system before (upper plot) and after (lower plot) correction for temperature due to the irradiation effect. ...

... The task calculates an average RMF over the spatial region used to extract the source spectrum. ... Essentially a grid is placed over the source region and the redistribution parameters calculated at each point. ... By means of command line parameters the averaging may be performed assuming that the flux distribution is that of the point spread function (PSF), a flat uniform distribution or it may be defined explicitly by supplying the task with an image containing the source region. ...

... The remote planet Pluto and its moon Charon orbit the Sun at a mean distance of almost 6,000 million kilometres, or nearly fourty times farther out than the Earth. During a recent investigation by an international group of astronomers [1], the best picture ever of Pluto and Charon [2] was secured with the European Space Agency's Faint Object Camera at the Hubble Space Telescope (HST). ... The new HST image was taken when Charon was near its maximum elongation from Pluto (0.9 arcseconds). ...

... Read in a hires optical spectrum and mask out lines to be ignored ! ... a) just calculate a spectrum with fixed abundances ! ... c) Solve for all light elements abundances { 1 8.53 0.0 2 11.54 0.0 5 0.10 0.0 6 8.00 1.0 7 7.81 1.0 8 7.10 1.0 12 7.01 1.0 13 5.73 1.0 14 6.94 1.0 15 5.50 1.0 16 6.75 1.0 18 6.10 1.0 20 5.10 1.0 21 1.70 0.0 22 3.84 0.0 23 2.82 0.0 24 4.06 0.0 25 3.71 0.0 26 6.18 0.0 27 4.26 0.0 28 5.05 0.0 29 3.20 0.0 30 4.34 0.0 39 1.42 0.0 40 2.40 0.0 -1 0 0 } synth save end ...

... Let us assume that table OBSERVP.tbl contains observations of a periodic phenomenon. ... SET/CONTEXT TSA ! Enable TSA package . NORMALIZE/TSA OBSERVP :VALUE ! ... BAND/TSA OBSERVP ! ... Inspect corresponding settings . POWER/TSA OBSERVP POWERSPEC ! Compute power spectrum and . ... PLOT/ROW POWERSPEC ! ... PLOT/ROW AOVSPEC ! ... POWER/TSA ? LINESPEC 20 .01 501 ! Compute detail of power spec. PLOT/ROW LINESPEC ! ... WIDTH/TSA LINESPEC ! ... SINEFIT/TSA OBSERVP CLNOBS 23 1 ! ...

... In combining the data, it is assumed that the low resolution image better represents the short spacing data, whereas the high resolution best represents the fine structure. ... Key: out The output image. ... Key: factor The flux calibration factor. ... In practise, the calibration may not be perfect, and an extra calibration factor will be required to align the flux scales. "factor" gives the factor to scale the low resolution image to put it on the same flux scale as the high resolution image. ...

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. ...

... Äíè îòêðûòûõ äâåðåé ê þáèëåþ ÑÀÎ ÐÀÍ (12-14 àïðåëÿ 2016 ã.) . Ìåæäóíàðîäíàÿ êîíôåðåíöèÿ "Dark Ages and White Nights (Spectroscopy of the CMB)" (20-24 èþíÿ 2016 ã.) . ... Ìåæäóíàðîäíàÿ êîíôåðåíöèÿ MULTI-SPIN GALAXIES - 2016 (26-30 ñåíòÿáðÿ 2016 ã.) . Ìåæäóíàðîäíàÿ àñòðîíîìè÷åñêàÿ êîíôåðåíöèÿ "Ôèçèêà çâåçä: îò êîëëàïñà äî êîëëàïñà" (3-7 îêòÿáðÿ 2016 ã.) Àðõèâ . ... Ïîäðîáíåå.. ... 10.02.16 . ... ÁÒÀ â ðåàëüíîì âðåìåíè . ... Öåéññ-1000 â ðåàëüíîì âðåìåíè . ... Ïîñëåäíåå îáíîâëåíèå: 22/03/2016 ...

Next: Star Formation Rate and Up: No Title Previous: Calculation of Evolutionary Tracks . To start calculations, we choose the distributions of the initial binary parameters: the mass of the primary ZAMS component, , binary mass ratio, , orbital separation a . ... whereas the mass ratio distribution is not. ... The zero assumption often made is that the mass ratio distribution has a flat shape, that is binaries with a high mass ratio occur as frequently as those with equal masses. ...

... In brief: the frequency-dependent radiative transfer equation is solved for a dust under assumption of spherically-symmetric geometry for its distribution taking into account particle size distribution and quantum heating effects for the very small dust particles. ... Table: Model parameters for IRAS04296+3429. ... parameter . ... hot dust shell) . ... The best fit to the spectral energy distribution of IRAS04296 is shown by heavy solid line (see Table2 for details concerning parameters of the model...

... I slept on my image of SN1999cq and decided to revisit my initial analysis, using "Submarine Sonar Subjective Analysis Techniques" (or whatever that means for - e.g. do we have a target or not ?) ... 1) LEHMANN's Image is great and matches Circular# 7209. ... 3) KERESZTY-ZOLT's Image shows only the very slightest hint for resolution of SN1999cq, in the generally diffused central area of UGX11268. 99.9% of what is marked as the ID for the supernova is actually the upper object shown in LEHMANN's...

... Primary mirror actuators . Secondary mirror actuators . ... Consequently, the resolution of the secondary mirror actuators must be fine enough to not contribute significant astrometric error. ... The resolution of the axial actuators for the primary mirror is set by the criterion that the tilt quantization error not produce significant decollimation. The quantization error of the primary actuators can be compensated by the finer tilt and lateral motions of the secondary actuators. ... mas . ...

Next: *upspecrdf, downspecrdf* - Transform Up: Spectral Analysis Previous: *grid_plot* - Plot Results . The conversion of count rate to flux depends on the intrinsic spectrum of the source, so xflux must be used in conjunction with fit . Fit generates a table of the best fit intrinsic spectrum ( _int.tab extension). xflux uses this table to calculate either the integrated flux between two energy limits or the flux density at a specific energy. ... This produces ``..._obs.tab'' file. ...

... 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 Co­Addition Technique Applied to Images of Galaxy Cores W. W. Zeilinger Institut f˜ur Astronomie, University of Vienna, T˜urkenschanzstraúe 17, A­1180 Wien, Austria P. Crane, P. GrosbÜl and A. Renzini European Southern Observatory, Karl­Schwarzschild Straúe 2, D­85748 Garching, Germany Abstract. ... One may therefore take full advantage of the high resolution FOC images by co­adding them with (high signal­to­noise) ground­ based data. ... References Crane, P. et al. ...

IBIS Data Analysis . ... IBIS . ... Flat Fielding - Introduction . The images obtained by IBIS will have intensity variations across the field of view that are not due to the solar image, but rather caused by instrumental effects that alter the observed intensity in each point of the field of view. ... IBIS Flat Fielding Techniques . ... Therefore, it is desirable to obtain the flat field measurements center on a point along the equator near the heliographic center of the solar disk. ...

OptInt PmWiki . MROI Fast Tip Tilt / . Tech Meet 9 . ... Page History | ... MROI Delay Line Design Contract . ... Design Documentation . ... MROI DL Production SW Contract . ... Preliminary Design Review . Software Design Documentation . ... MROI Fast Tip-Tilt Contract . ... Meetings . ... MROI FTT Contract Private Material . ... MROI DL Design Contract Private Material . ... Return to Tech Meet 9 ( Edit ) . ... Nasmyth Optical Table . ... XS analysis: Attach:FTT_mount_analysis_05.pdf . ...

... Take a particularly simple signal: a cosine wave. ... Now, we are going to stretch and shrink the wavelet along the time axis (we assume the data is in the time domain), and at each time compare the shape of the signal to that of the wavelet. ... Figure 3: The wavelet (dotted line) is translated rela tive to the signal (solid line). ... Figure 4: The dashed line plots the `match' between the wavelets (dotted line) and the signal (solid line) as a function of time. ...

ATM Forum Message . Forums: . ... Post . ... Resolution . Forum List | ... Post Message | ... Posted by Rick Crockett on April 25, 2007 08:46:54 UTC . ... resolution - aschilli - April 30, 2007 - 00:08 UTC . Indoor resolution - rick_crockett - June 2, 2007 - 07:04 UTC . ... www.astronomy.net . About Astronomy Net | Advertise on Astronomy Net | ... Forum posts are Copyright their authors as specified in the heading above the post. "dbHTML," "AstroGuide," "ASTRONOMY.NET" & "VA.NET" . ...