... Light curves resulting from electron scattering absorption in this envelope were computed and compared with observed IBIS/ISGRI and BATSE light curves. ... Assuming approximately 10-6 solar mass/year for the rate of the WR-wind, the observed light curves and accretion luminosity can be re-produced (assuming Thomson scattering opacity in the ionized He-rich envelope). ... Reduced 2-values between the models and ISGRI light curves vs inclination, for different mass ratios and wind velocities. ...

... ATNF Home . ... About ATNF overview . ... Australia Telescope Steering Committee . ... Australia Telescope User Committee . ... Murchison Radio-astronomy Observatory . ... Parkes radio telescope . Australia Telescope Compact Array . ... Visiting Parkes radio telescope . ... Parkes radio telescope webcam . ... PULSE@Parkes . ... The project does not assume any detailed prior knowledge of pulsar astronomy though students should have studied astronomy as a component of Stage 4 Science (Years 7-8). ...

function flux _to_em, emis , flux = flux , logT = logT , wvl = wvl ,Z=Z,NH=NH,defEM=defEM,$ noph=noph, thresh = thresh , _extra=e ;+ ;function flux _to_em ; return emission measures (-1 where undeterminable) at various ; temperatures consistent with given line fluxes and line emissivities. ; ; for each temperature, assume a delta-function emission measure, ; compute ...

... The first task assumes the searching for chemical composition and sizes of particles which give the wavelength dependence of the extinction efficiencies close to the observed dependence of . Figure 7: Wavelength dependence of the extinction efficiency factors for homogeneous spherical particles of different sizes consisting of astronomical silicate and amorphous carbon. The dashed segment shows the approximate wavelength dependence of the mean galactic extinction curve at optical wavelengths. ...

... 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. ...

... Using simulated clusters and Markov Chain Monte Carlo sampling of the probability distribution functions, we show that estimates of the MF slope, ЮБ, are unbiased and that the uncertainty, Ю?ЮБ, depends primarily on the number of observed stars and on the range of stellar masses they span, assuming that the uncertainties on individual masses and the completeness are both well characterized. ...

... commands . ... data_spectrum <name> : data in "spectrum" format . ... Repeat command to add additional mask regions. sigma is the s.d. to apply to the data within the region to be masked. ... Repeat command to add additiona continuum regions. ... cont_reg_clear : Clear current continuum regions . ... The observed spectrum is then multipled by this filter to obtain a new spectrum for use by SFIT. cont_sigma : Computes standard deviation of data in continuum regions and applies it to current data . ...

... The group of radio emitting X-ray binaries (XRB's), such as SS433, Cyg X-3, LSI , Cir X-1, etc., exhibit highly variable bursting radio emission interpreted as synchrotron radiation from relativistic electrons. ... In this paper, a numerical model for radio outbursts in XRB's is developed. The model is based on a process of continuous injection of relativistic particles into a spherical expanding plasmon, ejected following a transitory supercritical accretion event onto the compact star. ...

... The scheduling routines assist in creating an observing list (stored in the startable) from scratch or from another list stored on disk, and computing the visibility of the stars in a specific night and array configuration. The date of observation is taken from the variable date , and the array name from the variable systemid . If these are not defined, defaults are used for date (the next night) and for array (NPOI). ... addstar , stars _char Add one or more stars to the startable. ...

... COMPUTER SIMULATION OF RADIOWAVE MULTIPLE SCATTERING EFFECTS IN IONOSPHERE USING MONTE-CARLO METHOD . ... Distribution of reflected radiation on the ground is computed. ... Such influence can be remarkable if the scattering is multiple, i.e. the optical thickness for the scattering process is considerably greater than a unit. ... Radiation energy transfer in the slab is modeled by distribution of some particles carring small portions of radiation energy. ... The isotropic plasma approximation is...

... This thread contains a step-by-step recipe to extract MOS spectra of a point-like source observed in Imaging mode and to create associated response matrices, starting from a calibrated, concatenated event list (either produced with emproc or available as PPS product; here it has the assumed file name MOS.fits ). ... The users should note that the SAS metatask xmmselect allows them to interactively define source and background regions (via ds9) and to run backscale on the fly. ...

Photon/Particle Counting Image Measurement System : PIAS-TI . The PIAS-TI is an extremely sensitive image measurement device developed for imaging and quantification in ultimate levels with an extremely small number of photons, electrons and charged particles. ... The PIAS-TI is a measuring system that makes use of the technology of the photon counter to detect the input positions of individual photons or particles, and accumulate them to create an image. ...

Next: Star Formation Rate and Up: No Title Previous: Calculation of Evolutionary Tracks . To start calculations, we choose the distributions of the initial binary parameters: the mass of the primary ZAMS component, , binary mass ratio, , orbital separation a . ... whereas the mass ratio distribution is not. ... The zero assumption often made is that the mass ratio distribution has a flat shape, that is binaries with a high mass ratio occur as frequently as those with equal masses. ...

... Magnetic Storms . ... Cosmic Rays . ... Energetic Particles . ... Solar fast Particles . We cannot observe the way the distant universe accelerates cosmic rays or produces energetic photons, but acceleration processes also occur on our Sun , though on a much more moderate scale. ... That is why such events are often missed by cosmic ray detectors near the equator, where the lowest energies are excluded by the Earth's magnetic field. ... Should we be concerned about solar energetic radiation? ...

... Magnetic Storms . ... Cosmic Rays . ... Energetic Particles . ... Solar fast Particles . We cannot observe the way the distant universe accelerates cosmic rays or produces energetic photons, but acceleration processes also occur on our Sun , though on a much more moderate scale. ... That is why such events are often missed by cosmic ray detectors near the equator, where the lowest energies are excluded by the Earth's magnetic field. ... Should we be concerned about solar energetic radiation? ...

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. ...

Figure 3: Image showing the result of a vast number of computer simulations to reproduce the shape of Scheila's triple dust tails observed December 12, 2010. The researchers reasoned that the downrange plume and the conical impact ejecta produced the dust particles, which sunlight pushed away from the asteroid. ... The downrange plume explains the appearance of the prominent northern feature (1) while the conical impact ejecta explain the remaining two structures (2)(3). ...

lsst.tcc љ 1.2.2-3-g89ecb63 . ... Files . ... python . ... axis . coordConvWithFP.py . ... 22 љ def coordConvWithFP (fromCoordSys, fromPVTPair, fromPxPMRadVel, fromDir, toCoordSys, obj, inst, zeroPM, useGSWavelen): . 23 љ """!Convert a coord from one coordinate system to another . ... 35 љ @param[in] obj object block computed at desired desired TAI date of conversion . ... 50 љ obj = tcc.base.Obj(obj) # make a copy so I can change obj.site if useGSWavelen . ... tcc.axis.rotFromObs.rotFromObs . ...

... RVSAO 2.0 is the latest release of a package for calculating apparent radial velocities of celestial objects from observed spectral shifts. ... XCSAO cross-correlates the Fourier transform of an object's spectrum against the transforms of a set of template spectra with known spectral shifts to obtain a velocity and error. ... Full documentation of this software, including numerous examples of its use, is on-line at http://tdc-www.harvard.edu/iraf/rvsao/ . ...

... Staff . ... Cosmic dust has been observed both in emission and extinction everywhere in our Galaxy as well as in many other galaxies. ... Dust grains are classically thought to form in the winds of Asymptotic Giant Branch (AGB) stars. However, nowadays there is increasing observational evidence for notable dust formation in Supernovae (SNe). ... Hence the observed dust mass of 0.7вИТ0.9M вКЩ in this source can be safely considered as indicative of the mass of freshly formed dust in SN ejecta. ...