True Color Image Gallery: Galactic SNR | Magellanic Cloud SNR . ... parameters were derived from bright shell at N . Abundance of O-like element was set to zero asumming Typ1 I SN( Hughes et al., 1995 ). source=(xswabs * xsvraymond) . reduce chi^2 = 7.41398 . ... DataSet 1: 153 data points -- 144 degrees of freedom. Statistic value = 1067.61 . ... DataSet 3: 90 data points -- 76 degrees of freedom. ... Back to SNR J0519.5-6902 Index . Chandra Supernova Remnant Catalog . ...

... Initial mass function and binary stars . ... The principal goal of this study is to show that the real shape of the initial mass function for low- and intermediate-mass stars differs from the observed one. In particular, comparison of radii of eclipsing binary components and single stars shows a noticeable difference for B0V-G0V components of eclipsing binaries and single stars of the corresponding spectral type. ...

... The hot component shows very spectacular activity: irregular outbursts accompanied by fast, massive outflows and jets. ... Diffraction-limited images for both components of CH Cyg binary system were reconstructed using visible speckle interferometry at BTA 6-m telescope (Fig.1). The orbital period 15.6 years and masses: 2.0 Msun and 0.7 Msun for red giant and white dwarf, respectively were derived from angular distance (0.042") and magnitude difference (2 m ) of the components. ... Fig.1. ...

The preliminary version of documentation of the format for the interchange of calibrated optical/IR data being developed by Tom Pauls of NRL and John Young of COAST was presented and a number of issues discussed. The proposed format is in the general form of a relational database with different components stored in FITS binary tables. ... Should there be a single data table type that includes all data types, or multiple table types, one per data type? What data types are needed? ...

FGS Instrument Handbook for Cycle 24 . ... Fine Guidance Sensor Instrument Handbook for Cycle 24 > Chapter 4: Observing with the FGS > 4.4 Transfer Mode Overview . ... 4.4.1 The FGS Response to a Binary . ... Figure 4.3 shows the changes in the observed FGS1r interferogram due to binary systems of varied separations and magnitude differences. In Figure 4.3 a we display the interferogram of a wide binary pair with component separations and magnitude differences of (200 mas, 1.0) respectively. ...

CIMA is more than just the observing tool - in fact, the observing tool is just a part of a bigger package called the CIMA software package. ... There is also a another package called the CIMA WAPP software which contains the WAPP software, the special Tcl/Tk interpreter used by CIMA and support libraries. ... All CIMA software components recognize the following general options that are part of the CIMA version selection system: . ... The select_cima script can be used to set up a default version. ...

We present model fits to spectral energy distributions in the optical and NIR of >100 flat-spectrum radio quasars from the Parkes Half-Jansky Flat-spectrum Sample. We find that ~40% of the sources have power-law SEDs, while a similar number show evidence for two primary components: a blue power law and optical synchrotron emission. ... The sources with power law SEDs show evidence for an excess number of red power law slopes compared to optically-selected quasars. ...

... In collaborative work with David Garc?a Alvarez (an Observatory PhD student now at Harvard) and John Butler, an extensive study of the RS CVn binary HR1099 was completed leading to two papers; the first on Doppler imaging and the second on flare activity. Spectra for the Doppler imaging were taken at two different sites, Kitt Peak National Observatory (KPNO), Arizona, and Mount Stromlo Observatory (MSO), Australia, during the 1998 MUltiSIte COntinuous Spectroscopic (MUSICOS) campaign. ...

... astro-ph . ... Whitespace-separated words are treated as AND ed. Show 10 50 100 articles per page in Full Compact mode . ... Quasar Variability in the Framework of Poissonian Models . ... It is shown that in this very general framework the well established anti-correlation between variability amplitude and wavelength can only be understood as an effect of an underlying spectral component which remains stable on long time-scales, and is redder than the variable component. ...

Text of these problems is available also in other languages : . ... What can one see in the Moon's sky more often - the Sun or the Earth? ... There are about of 250 millions of stars in the elliptical galaxy M32 (a satellite of Andromeda galaxy). ... The masses of Capella's components. ... You are proposed to estimate the masses of Capella's components, using our observational data. ... A galaxy's mass. ... Estimate the mass of FGC 1908 and compare it to the mass of our galaxy. ...

... 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. ...

The CHIANTI database consists of 4 primary ASCII files for each ion in the database. contains the energy levels in cm^(-1) It includes both experimental data and theoretical values of the levels energies. ... The 24 configuration model used to derive the transition probabilities in the ".wgfa" file, gave energy levels which were slightly different from the observed levels. ... contains the spline fits to the electron collision strengths scaled according to Burgess and Tully (1992). ...

Abstract -- Calculations are performed for the linear polarization of starlight due to extinction by aligned dust grains when the starlight traverses a medium with irregular magnetic fields. This medium is intended to represent the optically thick components of interstellar clouds which are observed to make little, if any, contribution to the polarization of starlight. ...

Next: Extinction efficiencies: general behaviour Up: Optical properties of cosmic Previous: Optical properties of cosmic . It is now evident that observed interstellar extinction cannot be explain using particles of only one kind. ... The intensity of radiation after passing a dust cloud is equal to . ... The interstellar extinction is . ... Next: Extinction efficiencies: general behaviour Up: Optical properties of cosmic Previous: Optical properties of cosmic root 2003-04-09 ...

Geomagnetic disturbances can be monitored by ground-based magnetic observatories recording the three magnetic field components. The global Kp index is obtained as the mean value of the disturbance levels in the two horizontal field components, observed at 13 selected, subauroral stations . ... Geomagnetic activity is the occurrence of K variations. ... But K still remains a local index, describing disturbances in the vicinity of each observatory. ...

... The HST uses an onboard model of its orbit to perform in real-time various control functions relating to spacecraft operations and observation support. ... New coefficients for the ephemeris are updated every other day, and are archived as FITS keywords for each HST observation data set. Using these coefficients,an observer can perform a variety of calibration and characterization calculations relating to the orbital position and velocity of the telescope. ...

... Here some data observed on the 6m telescope with IFP installed in the OLD focal reducer are presented. ... Mkn 3: velocity field . ... NGC 5252: [OIII] image . ... NGC 5252 was observed 23 Feb. 1998 in the [OIII]5007 emission line with CCD TK1024 as detector. ... We observed the ionized gas velocity fields of the spiral galaxies with two purpose. ... Restored velocity field of NGC 157 in the reference frame rotating with the pattern speed overlaid on the Ha image of the galaxy . ... NGC 4100 . ...

... 105Lawrence+ Nearly 1000 sources from the 5 GHz MIT-Green Bank (MG) survey have been observed with the VLA. ... About 1000 sources, selected as described in IIa from a prelimenary version of the MIT-GB I catalog, have been observed with VLA. ... About 20 sources observed at the VLA are within the MG sky area and above the 106 mJy completeness limit, even allowing for the large flux-density errors in the preliminary list, but do not appear in the MG catalog. ... 1 Source name in IAU B1950.0 format. ...

NMW survey overview . Access image archive . ... The New Milky Way survey aims to detect bright (V<13.5) optical transients near the Galactic plane using an automated wide-field (8x6 deg.) system capable of surveying the whole Milky Way area visible from the observing site in one night. ... All images obtained during the transient search survey are available online (please use the image archive access form ). ... Images per field: . ... Images per night: . ... Milky Way imaging time: . ...

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