... We will consider the rms, (K), for observations with a receiver of system temperature, T , frequency resolution, per polarization, and total integration time per observing cycle, . ... For ``in-band'' frequency switching, the line under investigation is always in the observing band. ... Position Switching or ``Out-of-Band'' Frequency Switching: Here the line is only observed for one half of the time, with noise being present all of the time. ...

The potential of masers to act as probes of their environment has long been recognised, but to date has proven very difficult to realise. ... 2001, Sutton et al. 2001). Masers are variable on timescales of weeks to months and one of the major limitations in previous attempts at multi-transition analysis has been the uncertainties introduced by combining observations made over many years using a variety of instruments with differing spectral and spatial resolutions and polarisation properties. ...

... Limitations on the Calibration Accuracy for COS/FUV Observations of Extended Targets and for COS/FUV BOA Observations in Cycle 23 . ... Cycle 23 Results . ... Extended targets with COS/FUV . ... Combined with the aperture vignetting, these effects may result in an unreliable flux calibration for COS/FUV/LP3 observations of extended targets (larger than 0.6? ... Users should make themselves aware of the limitations in the calibration of COS/FUV observations of extended targets or with the BOA at LP3....

... High spectral, spatial and temporal resolution UV observations of the quiet Sun transition region show a highly structured and dynamical environment where transient supersonic flows are commonly observed. ... Estimates of the kinetic and enthalpy fluxes associated with these events show that explosive events are not important so far as solar coronal heating is concerned. ... In some cases, non-Gaussian line profiles are associated with supersonic flows in small magnetic loops. ...

On April 27 the large sunspot in Active Region 8970 was observed using the Adaptive Optics system at the Swedish Vacuum Solar Telescope at La Palma. ... It showed to give a significant improvement of the image quality under less favorable conditions. Click on the image to get a high resolution version. ... The data cube is cut in three pieces to get manageable file sizes, you can glue them together to restore the whole 108 images cube. gband_ao.01_36.cube.fits 36.5 Mb: image 1 - 36 . ...

... 227Wink This paper containes an investigation of 91 sources which appear to be point sources when observed with the angular resolution of the 100-m telescope at 4.9 GHz, teta_a = 2.6', and which we expected to be HII regions. The basic search list was prepared from the 4.9 GHz survey of the galactic plane by Altenhoff et al. ... In the present paper we list 4.9 GHz flux densities only for sources for sources for which we present new observations. ... source structure indicated . ...

Next: Radial velocity of the Up: Optical spectrum of IRAS04296 Previous: Observations and spectra reduction . ... However, molecular emission features are only very rarely observed in the optical spectra of PPNe. ... On the other hand, it is well known that cometary nuclei spectra show prominent Swan band emission. In both spectra of IRAS04296 we have discovered strong emission in the (0;0) and (0;1) bands of the Swan system of the molecule. ... Now consider the case of IRAS04296. ...

... Science Users Information > Science and Technical Meetings > Conferences 2010 > The Origin and Fate of the Sun: Evolution of Solar-mass Stars Observed with High Angular Resolution . ... Observing Facilities . ... Observing with ESO Telescopes . ... The goal of this workshop is to review recent results on solar-mass stars obtained with infrared and millimeter interferometers, and to discuss their importance for our understanding of stellar evolution from star formation to stellar end products. ...

The problem of solar wind data correlation for the observations onboard several spacecraft is very important for three points of view: . ... This problem is studied now in detail by systematic determination of ion flux and ion velocity data correlations by INTERBALL-1 (IKI group), WIND and IMP 8 (both - MIT group). ... Solar wind plasma correlation lengths from IMP 8, WIND and INTERBALL-1. ... Correlation of solar wind observations onboard several spacecraft: INTERBALL-1, IMP 8 and WIND data. ...

... Contacts . 2012: . ... We refined the fundamental parameters of the components, the orbital periods, and the conditions of photospheric heating of the secondary component by the ultraviolet radiation of the hot component. ... The observations of the star clusters associated with ultra-luminous x-ray sources (ULXs) in four galaxies on the 6-meter and VLT telescopes have shown that all the ULXs are located within 200pc of very young star clusters (younger than 5 million years). ... Archive . ...

Next: NICMOS/HST H-band (F160W) Images Up: NICMOS Science Previous: HST NICMOS Observations of . ... Observations of P . ... The NICMOS team has devised a comprehensive program of observations of the Galactic Center. ... Data in hand give a first look at variability and a detailed look at the search for the tip of the main sequence will be discussed where NICMOS has demonstrated adequate sensitivity and photometric precision to identify likely O8-B1 stars at the Galactic Center. ...

Magnetic Fields around Radio Galaxies Robert Laing (ESO) Laing et al. ... 2008) Negligible depolarization and 2 rotation Almost all Faraday effects must be due to foreground material How to fit depolarization caused by foreground Faraday rotation Complex polarization Rotation measure Integrate over a beam Observed RM for 0 2 rotation and depolarization Faraday rotation and depolarization 5.5 arcsec FWHM Faraday effects at high resolution FWHM = 1.5 ...

... Galaxies 99 Cosmic background with model of cloudy interstellar medium Yu. ... Figure 1: Averaged spectrum of the cosmic background I f in frequency range 0.25 200 MHz for the Galactic poles. ... First interpretation of the cosmic noise background spectrum at broad band frequency range 0.25 200 MHz with a model of the cloudy interstellar medium ISM is presented here. ... Synthesized background spectra I f for regions of the Galactic poles at the frequency range 0.25 200 MHz is presented in Fig. ...

... In order to compare the number of different evolutionary stages obtained and X-ray luminosity of the chosen X-ray sources with the observed galactic values we use the sum of C/O+O/C , where C and O are the calculated and observed values of a given binary type, respectively. If we make comparison for a number of different binary species (for example, we compare the number of CV, number of X-ray pulsars,   total X-ray luminosity of LMXB, etc.), we write this criterion in the form: . ...

Next: Rotation Periods of ZAMS stars Previous: T Tauri Stars . ... The first attempts to directly measure periodic modulation of T Tauri stars occurred in the early 1980s. Rydgren & Vrba (1983) observed four PMS stars using photoelectric photometry over a period of seven consecutive photometric nights. ... Because the spot lifetime is much longer than the rotational period, the observed effect will be a modulation of the light from the star synchronously with the rotation period. ...

RADIOASTROPHYSICAL DEPARTMENT • INSTITUTE OF SOLAR-TERRESTRIAL PHYSICS RAS SB . General information Main characteristics of the Radio telescope Observing programs General view of the antenna array Main research areas Principle of generation of radio images Radio telescope 's beam Receiving systems Main characteristics of the base receiving-recording complex Calibrations Data archive and databases Publication SSRT - Siberian Solar Radio Telescope . ...

... The study of the Large-scale structure of the Universe and measurements of the Dark Energy equation of state; The exploration of the growth and cosmological evolution of supermassive Black holes in the Universe. ... In course of the all sky survey SRG will discover about 100 000 galaxy clusters and 3 million AGNs. Galaxy clusters are the largest gravitationally bounded objects in the Universe and are best explored through the study of X-ray emission from the hot intergalactic gas. ... 2016 IKI RAN ...

... Up: Data Analysis and Processing Techniques . ... Also, a method for quality control of CCD observations is suggested. ... Everyone who observes a celestial object using a CCD detects moving celestial objects as a ``by product''. ... We hope that our investigations may be useful for near-Earth space control and also for searches of the moving celestial objects through analysis of old and new CCD frames obtained at any amateur or professional astronomical observatory. ...

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. ...

We report here on those proposed UIT targets that, in fact, were successfully acquired. ... Note on Filters: . A1 centered at 2500 angstroms with a width of 1200 angstroms . ... Sextans A is a low mass dwarf companion to the Milky Way Galaxy. It is sufficiently close that it is easily resolved into its individual stars. ... An exposure of 1100 seconds through the A1 and B1 filters was obtained. NGC 2903 Is a relatively nearby mostly face-on galaxy with active star formation. ...