We present results of new Monte Carlo calculations made with the DIRTY code of radiative transfer of stellar and scattered radiation for a dusty giant late-type galaxy like the Milky Way, which illustrate the effect of the attenuation of stellar light by internal dust on the integrated photometry of the individual bulge and disk components. ... In addition, we find that the structure of the dusty ISM affects more sensitively the observed magnitudes than the observed colors of both bulge and disk. ...

... 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. ...

... 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. ...

... ATNF Home . About ATNF . ... About ATNF overview . ... Australia Telescope Steering Committee . ... Australia Telescope User Committee . ... Astrophysics graduate student programs . ... Australian Square Kilometre Array Pathfinder . Murchison Radio-astronomy Observatory . ... Parkes radio telescope . Australia Telescope Compact Array . Mopra radio telescope . ... Visiting Parkes radio telescope . Visiting Australia Telescope Compact Array . ... Parkes radio telescope webcam . ...

... Bojan Nikolic web pages (r. 329) . ... We present a Bayesian approach to calculating the coefficients that convert the outputs of ALMA 183 GHz water-vapour radiometers into estimates of path fluctuations that can be used to correct the observed interferometric visibilities. ... Inference of Coefficients for Use in Phase Correction . ... Simulating Atmospheric Phase Errors, Phase Correction and the Impact on ALMA Science . ... Copyright 2005 -- 2016, Bojan Nikolic feedback welcome ...

... The J, H and K bands are characterized by a bright background, such a background is mainly due to the emission of atmospheric lines and of thermal radiation. ... If the source cover a large fraction of the slit, spectra off-source must be observed to adequately sample the sky background. ... The on chip integration time (time spent in each position of the slit) must not exceed 40 seconds in J and H bands and 60 seconds in K band. ... We suggest a sequence of 10 for each elementary integration time. ...

... Fitting the observed dependence includes calculations of the polarization cross-sections averaged over particles orientation and size distribution, their normalization and the comparison of obtained dependencies with Serkowski's curve representing observational data for a chosen star. ... Variations of the polarization factors with wavelength are shown in Fig. 16 for homogeneous spheroidal particles with PF orientation. ... The distinction between prolate and oblate spheroids is also clearly seen. ...

... we show that the comparison between the calculated and observed numbers of the most ``fragile'' (from the point of view of the binary evolution scenario )   galactic binary types (such as X-ray low-mass X-ray binaries (LMXB), cataclysmic variables (CV),   Be-stars   with compact companions, relative number of visible binary radiopulsars   with normal and compact secondary components) impose certain constraints on the feasible initial ... Phenomenological Kick Velocity . ...

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. ...

... A technique allowing automatic representation by a relatively small number of independent parameters based on the principal component analysis of data sequences is presented. ... In recent years the spectrum of observed astronomical data can be characterized as greatly varied. ... In this instance, the problem of initial description and classification of newly-observed data becomes most urgent, especially if there is a lack of preliminary observational material and theoretical expectations. ...

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. ...

... 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 . ...

... 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 . ...

PENTICTON SOLAR RADIO FLUX VALUES (from SGD Explanation of Data Reports) Daily Solar Flux Values - Penticton -- Daily measurements of the integrated emission from the solar disc at 2800MHz (10.7cm wavelength) have been made by the National Research Council of Canada since 1947. ... The data are tabulated in two forms: the "observed flux" (S), and the "adjusted flux" (Sa). ... The "observed flux" values are useful in ionospheric physics and other terrestrial consequences of solar activity. ...

... The emission line galaxies observed are listed in Table 3 containing the following information: . column 1: The object's IAU-type name with the prefix HS. column 2: Right ascension for equinox B1950. column 3: Declination for equinox B1950. ... Two very faint objects (HS 1134+3640 and HS 1308+3845) are probably super-associations in the dwarf spiral NGC 3755 and in the Im galaxy UGC 8261. ... HS 1134+3639 : Probable low-mass companion of the galaxy NGC 3755 (the distance is 230 or 25 kpc). ...

... AMPLE (Adaptable Minor Planet Ephemerides) is integrated software package to deal with a number of problems concerning minor planets with the aid of IBM-type personal computer. ... compiling a list of all numbered minor planets which can be seen at certain moment within specified sky region and visualization of their mutual positions; . ... As AMPLE is able to reproduce virtually any table of "the Ephemerides of Minor Planets" , it may be considered as computer version of the EMP. ...

... Archives . ... The PCA and ICA is used for separating mixed components with some assumptions. ... The need of source separation methods in astronomy has led various adaptations of decomposition methods available. ... I rarely come up with a paper which gathered and summarized component separation methods applicable to astronomical data. In that regards, the following paper seems useful to overview methods of reducing dimensionality for astronomers. [arxiv:0805.0269] . ... Chandra Blog . ...

... For GK Hya excess emis­ sion was observed in the Balmer lines and Mg I b lines while TY Pyx showed excess emission in the Balmer lines and Ca II H & K lines. The emission from GK Hya arises from a global phenomenon associated solely with the secondary component. The lack of significant He I D 3 excess absorption and an analy­ sis of the flux ratio in the Balmer lines suggest that the emission originates in prominence­like material seen off the limb of the star. ...

Marc White . ... Turbulent entrainment processes may play an important role in the outflows from young stellar objects at all stages of their evolution. In particular, lateral entrainment of ambient material by high-velocity, well-collimated protostellar jets may be the cause of the multiple emission-line velocity components observed in the microjet-scale outflows driven by classical T Tauri stars. ... University of Amsterdam; STARPLAN, Copenhagen, Jul 2013 . ... E marc.white@anu.edu.au . ...

Next: General CCF Components Up: Calibration Access and Data Previous: List of CAL Routines Contents . This section contains descriptions of the structure of CCF constituents. ... The calibration team of the SOC is also providing additional CCF components where required in conjunction with data that were generated with SciSim. ... These CCF components are generated on a need basis and are identical in structure to the real life components. ... Generation from Ground Calibration Data . ...