Next: Results & Discussion Up: Coronal Hole Diagnostics out Previous: Introduction . ... The dates of the observations discussed here, their locations, pointing, slit sizes and exposure times are given in BTDW. ... Line fits are given by the dotted line. ... An estimation of the errors in the derived parameters was obtained using the GA-derived parameters as an input for a ``classical'' IDL-CURVEFIT procedure (Peter, 1999; Peter & Judge, 1999). ...

... HST . GHRS ISR 071: . Results for Side 1 (1100-1350 ) . ... HST Overview . Overview . ... Cycle 24 Announcement . Cycle 23 Results . ... In order to find evidence for any sensitivity variations with time, we used the first post-COSTAR observation of BD+28D4211 on SMS 94098 as a reference point for the 1200 data and divided all subsequent observations by this spectrum. ... Plots of individual ratioed spectra obtained early in the cycle which include error bars were shown in GHRS ISR 69. ...

XMM-Newton OM Response Files Page . ... Data Analysis SAS News What is SAS? ... The response files have the name om_effarea_<filter>_v2.0.rsp. The response files should be used in conjunction with a spectral data file containing the filter count rate. Such a data file may be created by editing the template filter file om_filter_default.pi with a fits editor such as 'fv' and changing the "RATE" and "STAT_ERR" entries in the SPECTRUM extension to the filter count rate and error. ...

... The fitting package in STSDAS (Space Telescope Science Data Analysis System) relies on two basic techniques (one linear and one non-linear) for fitting functions to data. ... Results show that both methods may generate biased coefficients (at the ~few percent level), and over or under-estimate error bars (at the ~10 percent level), in particular from low signal-to-noise data. ... Function coefficient errors are computed directly from the covariance matrix. ... Abscissa is signal-to-noise. ...

The 90 GHz continuum spectra displayed below have been obtained on July 10, 2001, with the one baseline (CA03-CA04: 30m) 3mm prototype system of the Australia Telescope Compact Array . ... Calibrated 90 GHz continuum spectra of Eta Carina. The centre frequencies of the two IFs are 90.560 GHz and 90.688 GHz, each with a bandwidth of 128 MHz, divided into 64 channels (config ant234ac_128_64_2p-2f). The displayed spectra are Hanning smoothed (hann=3). ... 12-07-2001 * B?rbel Koribalski ...

New reduction of minor planets photographic plates obtained with Pulkovo Normal Astrograph A.A. Berezhnoy Pulkovo Observatory of RAS, Saint-Petersburg, Russia Minor Planet observations at Pulkovo Periodical observations of 14 bright asteroids named Selected Minor Planets (SMP) were performed at Pulkovo since 1948 within the international framework started by works of B.V. Numerov and D. Brouwer. ... 108 133 113 74 124 67 97 88 14 84 64 5 20 19 Epochs (YYYY.MM) 1200 Mean values of total obs. ...

... Spider scans ( heiles calibration scans ) were taken with alfa on 02nov09 using beam 0 and 03nov09 using beams 0,2,3,4,5 to test its performance. ... Page 5: Pointing error. beam 2 had large za errors. beam 3 had large az errors. ... Plot the rms error and mean error for these newly computed series. ... Plots showing the pointing error vs rotation angle offset (.ps) ( .pdf ): . ... rotating by + 2 degrees reduces the non beam 0 rms from 18.7 to 14.8 asecs. rms Error asecs . mean error asecs . ...

For a sample of 16 people, the error would be 4/16 = 25%. This a large error since the range of YES vs NO is from 0-100% if 12 people answered yes and 4 people answered no then your result would be: . Percentage yes = 75 +/- 25% . ... For a sample fo 1000 people, the error would be SQRT(1000)/1000 = 33/1000 = 3%. If 750 answered yes and 250 answered no then your result would be: . ... Conclusion: Always ask what the measuring errors are!! Previous Lecture Next Lecture Course Page ...

... The PROS system provides the capability to keep track of the uncertainties in image files through error arrays. ... There is a task, errcreate , that will estimate the errors in an image and produce an error array. ... Some tasks that transform images, such as imsmooth, imcompress , and imreplicate have the option to produce a resultant error array, derived from the original image's error array. Note, however, that the imcalc task does not produce an error array. ...

... 1.7 GSC 084 Pulkovo Obs., 0.33 15 x 15' 1.0" 7 34 0.179 0.307 Normal Asgr. 3.0 UCAC 118 Slovakia, 0.57 14 x 10' 1.7" 3 12 0.090 0.145 Modra 3.3 USNO 127 Germany, 0.19 30 x 20' 2.4" 3 15 0.151 0.087 Bornheim 0.8 GSC 168 34 200 0.282 0.315 291 USA,Kitt Peak, 1.8 390 x 30' 1.0" 1 5 0.143 0.144 Spacewatch II 4.7 USNO 300 Japan, 0.5 78 x 78' 2.3" 7 36 0.420 0.447 Bisei Center 1.3 ACT 461 Hungary, JATE 0.60 28 x 19' 1.1" 6 22 0.124 0.153 Asteroid Surv. ... Polynesia 1.0 UCAC F85 Tiki Obs., ...

... Bojan Nikolic web pages (r. 329) . ALMA . We present a framework for modelling atmospheric phase errors and their correction by both the fast-switching and water vapour radiometeric techniques. ... We use this framework to simulate relative point source sensitivity and effective resolution for a range of atmospheric conditions, with and without phase correction. ... Published as ALMA Memo #582. ... Simulating Atmospheric Phase Errors, Phase Correction and the Impact on ALMA Science . ...

... In Fig. 2 the spectrum of the host galaxy HS1035+4758 is shown, in which typical HII-galaxy narrow emission lines are seen: H 4861, [OIII] 4959,5007, H 6562, [NII] 6548,6584 and [SII] 6716,6731 ?. ... The spectral evolution of SN 1998bv is illustrated in Fig. ... The change of the spectrum between April 6 and 19 with clear reddening shortward of H during these 2 weeks indicates seemingly that the 1st spectrum was observed in the period between the 20th and 30th days after the peak of the light curve...

ON THE IMPACT OF THE GALACTIC ABERRATION ON VLBI-DERIVED PRECESSION MODEL Z.M. MALKIN Pulkovo Observatory Pulkovskoe Ch. ... Corrections to adopted precession rate are usually computed from the linear trends in long-term time series of celestial pole offset (CPO), which are the differences between the measured and the theoretical coordinates of the celestial pole. ... CONCLUSIONS We have estimated the impact of GA on parameters of precession-nutation model derived from VLBI observations. ...

... The actual cross-correlations were done as follows: north of WGACAT was correlated with the GB6 catalog with a correlation radius of one arc minute. ... We therefore cross-correlated WGACAT with the GB6 and PMN radio catalogs with a 1.5 arcmin radius. ... As a result of this experiment, we then added to the WGACAT/PMN candidate list the 29 unclassified sources obtained from the 1.5 arcmin correlation and having PSPC offsets arcmin, ratio between X-ray/radio offset and positional error , and . ...

SKA-3 instrument consists of two energy-angle ( EA ) electrostatic analyzers and two energy-mass ( EM ) time-of-flight analyzers. ... Here you can find more details about SKA-3 instrumentation set. ... Case 218 . ... satellite's trajectory in geomagnetic frame ( blue coloured), UFSIPS scan location and observation moment ( red coloured), interval of the SKA-3 observations ( green coloured) . ... a view of the Nothern polar region at the moment of UFSIPS observations, the scan location is red coloured. ...

... First, we computed the mean errors of orbit parameters on the assumption of the linear connection of them with observation errors and then we compared obtained estimates with those resulting from the assumption of the nonlinearity of this connection. Secondly, we correlate orbital parameters and their errors obtained by the method of the least modulus with those obtained by the least-squares method. ...

Peremennye Zvezdy ( Variable Stars ) 32 , No. ... We report on a new episode of decretion disk formation in the IGR J06074+2205 system. ... From a study of three HeI lines, the rotational velocity of the star was determined as km/s. After five years of spectroscopic monitoring of IGR J06074+2205 (Reig et al. 2010), a reversion from emission to absorption of the H line and hence disappearance of the equatorial disk was reported. ... Reig P., 2011, Astrophys.& ...

... GCN 8471 | ... TITLE: GCN CIRCULAR NUMBER: 8516 SUBJECT: GRB 081102: MASTER refind and final results DATE: 08/11/11 15:50:10 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina, D.Kuvshinov, P.Balanutsa Sternberg Astronomical Institute, Moscow State University A. Tlatov, A.Parkhomenko Kislovodsk Solar Station of the Pulkovo Observatory V.Krushinski, I.Zalognikh Ural State GCN Circ 8470, Lipunov et al., ...

... Auroral Currents . ... 25c. Space tether . ... Aurora from Space . ... But the best view is still from space. ... The Canadian scientific satellite Isis-2 (1971) carried an auroral imaging camera and discovered the diffuse aurora, a broad ribbon around the auroral oval, too spread-out to be noticed from the ground. ... Currently, NASA's Polar (1996) collects images of the polar aurora using three cameras--in visible light (sometimes as frequently as 12 seconds apart), in ultra-violet and in x-rays. ...

... A comparison of the computed and experimental relations F max ( H), as well as comparison of drift scans of point sources across different horizontal cross-sections of the BP with the corresponding computed cross-sections were made. ... The drift scans of the point source 3С84 (H=87 o ) at the wavelength 7.6 cm across the horizontal cross-sections of the BP (black lines) and the computed horizontal cross-sections of the BP corresponding to them (red lines). ...