... News Latest News News Archive Newsletter Quarterly Status Report . ... Data Analysis SAS News What is SAS? ... Other Links Project Related Links Research Projects Other X-ray Missions Space Weather Links . This page contains links to four sorted lists of observations planned or performed as of 12 March 2003. ... Planned Observations (sorted by type. ... Planned Observations (sorted by RA/DEC) . Performed Observations (sorted by RA/DEC) . Planned Performed Observations (sorted by RA/DEC) . ...

... DPERSC-CP34SE: ...and 0 packets were found to have segments without Reed Solomon corrections CPEEND- DATA EDITING ENDED 26-APR-95 18:05:56 FOR W1DR0806T . CPE0EN--------------------------------------------- DATA EDITING COMPLETED ----------------------------------------------------- CPG0VS--------------------------------------------- DATA EVALUATION STARTED ----------------------------------------------- DPVSTR- DATA EVALUATION STARTED 26-APR-95 18:16:57 FOR ...

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. ...

Next: Results of follow-up spectroscopy Up: Spectral observations and data Previous: Spectral observations and data . ... The reduction of the originally two-dimensional CCD data included standard steps such as: bias and dark subtraction, flat-fielding, cosmic-ray removal. ... In the final spectra showing emission lines, redshifts and line fluxes are measured applying Gaussian fitting. ... The line [O II ] 3727 ? ... For all spectra, the individual emission line fluxes of the H , [N II ] 6548,6583 ? ...

... The results are used in quasireal time by the observing process, but also as input by hardware quality control, by the dynamical scheduler, and by the Science Pipeline. Among processing operations are the calibration of the atmospheric absorption, of phase radiometric correction, of pointing scans, of phase and amplitude reference measurements, .. ... Using the last few measurements, we will determine a provisional amplitude calibration curve (to be also used by the Quick Look pipeline). ...

... The next step after loading is to apply a number of ``fixes'' that are important for 3-mm data. ... By default atfix applies the ``standard'' gain/elevation model for the antennas. ... As mentioned above, the ATCA uses the chopper wheel method to measure an above atmosphere system temperature. ... On the night of an ATCA reconfiguration, a solution for the antenna positions is derived. ... Task atfix corrects the data for an improved antenna location solution via the dantpos parameter. ... ATFIX . ...

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). ...

Peremennye Zvezdy ( Variable Stars ) 32 , No. ... We report on our photometric analysis of the poorly studied cataclysmic variable in Ophiuchus, 1RXS J174320.1-042953 (DDE 11). ... The long-term behavior of J1743-0429 shows that it is a probable magnetic cataclysmic variable (polar), with a large difference between its low and high states. The orbital period obtained from our observations is 0 0866, or 2 08, close to the lower boundary of the period gap of cataclysmic variables. ... Fig. ...

... The Science Operation Department is composed of Astronomers, Telescope Instruments Operators(TIOs) and Data Handling Administrators(DHAs). ... Astronomers have proposed several methods to quantitatively measure the amount of turbulence above the telescope, which the most common ones is Differential Image Motion Monitor (DIMM). In optical testing, the Hartmann test is the common method to test the quality of optical components. ... Hartmann mask consists of 48 lenses. ...

... Equivalent widths of Ca I absorption lines at 6122?, 6162?, and 6494? and Fe I at 6103?, 6200?, and 6574? were measured for several spectral standards. ... The spectral types of the target stars were determined by comparing source line ratios to those of standard stars. ... The uncertainty in the spectral type is about one and a half sub--types. ... Northwest of the belt, again all but one source shows Li in absorption, but only one star (out of 13 = 7.7%) shows an H emission line. ...

Observation of the Sunyaev-Zel'dovich E ect toward CL0016+16 at 43 GHz M. Tsuboi et al. Ibaraki University, Japan We performed a mapping observation of the Sunyaev-Zel'dovich e ect toward a distant cluster of galaxies, CL0016+16, at 43 GHz using a newly developed 6-beam SIS receiver installed in the Nobeyama 45-m telescope. The temperature decrement of the cosmic microwave background radiation was measured to be
T  A = 0:490:05 mK at the central position of the cluster. ...

Pulkovo NEO Page . ... NEA Accuracy Estimation . ... The estimation of accuracy of the current CCD observations of asteroids and comets is constantly performed at Pulkovo Observatory. ... The (O-C) values, so called "Observed" minus "Calculated" positions, characterize numerically the observations of any observatory, both professional and amateur, during a short period (one or several close nights). ... So the (O-C) values for these objects nearly entirely define the errors of observations. ...

... A2193 Date Received: 2006-Jan-31 19:34:08 Technical Page Proposal Type: General Category: Sub-Category: Observation Category: Total Time Requested: Prop osal Title: Short Astronomy Spectroscopy Galactic 3 Hours Completion of a2004 Pro ject to Observe the Taurus Molecular Cloud Complex with GALFA. ... Name Marko Krco Institution Cornell University E-mail marko@astro.cornell.edu Phone 607-351-3589 Student G Service Observing Request Remot e Observing Request X None All of the observing run. ...

Next: NICMOS Science Up: NICMOS Data Calibration and Previous: NICMOS Software at the . ... Reference File Tools . Image Analysis and Reduction . ... These include the tasks used in the STScI pipeline, tools to generate the reference files used by the calibration pipeline tasks, and general image analysis, manipulation, and arithmetic tasks. ... Calnica is used to apply instrumental calibrations to individual datasets, while calnicb is used to process associated sets of NICMOS images. ...

... For high spectral resolution observations the devices permanently located at the N2 focus of the BTA are used (Klochkova, 1995, Panchuk, 1995). However for a number of tasks to be performed, it is needed to rule out the influence of the second and third mirrors, i.e. to realize the high spectral resolution ( ) directly at the prime focus. ... Examine the principal parameters of the PF echelle spectrometer, which is equivalent in spectral resolution to the CCD-equipped MSS (Panchuk, 1995). ...

... 8, ``Celestial Mechanics'', 2002 CCD observations of planetary satellites and occultations and close approachments of stars by asteroids with 26­ inch refractor of Pulkovo observatory T. P. Kiseleva, I. S. Izmailov, M. A. Mozhaev Pulkovo Observatory, St. Petersburg, Russia ST--6 CCD camera has been used with 26-- inch Refractor at Pulkovo for ob­ servations of ... These estimates are \Sigma0:015 arcsec and \Sigma0:014 arcsec for X and Y correspondingly. ...

. Next: Phase unwrapping Up: Pipeline Previous: Flag tables Contents . As usual, bias correction is based in incoherent scans and is performed separately for each interferometer configuration. First, bias correction fit coefficients are computed combining all observations (for each configuration) to make sure that a basic correction is performed. Second, bias corrections are updated for each star with the measurement obtained for this star only. Christian Hummel 2015-04-28

To appear in "Fourth Workshop on Robotic Autonomous Observatories (2015)"RevMexAA(SC) METEOR OBSERVATIONS WITH MINI-MEGATORTORA WIDE-FIELD MONITORING SYSTEM S. Karpov, 1, 3 N. Orekhova2 G. Beskin, 1, 3 A. Biryukov3,4 S. Bondar,2 E. Ivanov,2 E. Katkova,2 A. Perkov, and V. Sasyuk3 RESUMEN 2 Favor de prop orcionar un resumen en espanol. ... The faintest detected meteors has the peak brightness about 10 mag, while the ma jority - from 4 to 8 mag. ... 2010; Karpov et al. 2013; Beskin et al. ...

... Despite new observation methods provided by radar and satellite instrumentation , optical measurements are still important when studying auroras . ... Because of the monochromatic nature of the auroral light, photomultiplier tubes with very narrow band filters were used in the measurements. ... The spectra of the background emissions from atmospheric impurities (clouds, ice crystals, etc.) is rather continuous, and measurements just outside the auroral emission lines are valid for the line itself. ...

RTT150 . Russian-Turkish 1.5-m Telescope . ... Telescope has two main foci (Cassegrain and Coude ) and allows to use six optical systems based on Ritchey-Chretien system with a common main mirror . At present scientific observations are being performed at the Cassegrain focus in main optical scheme with focal ratio of 1:7.7. ... flat . ... To use the Coude focus the removable flat diagonal mirror is also needed in the crossing point of declination axis and main optical axis of telescope. ...