Next: EPN_BADPIX Up: EMOS_BADPIX Previous: Generation from Ground Calibration Contents . Bad pixel lists are derived mostly from the internal calibration exposures, acquired at regular intervals since the beginning of the mission via dedicated automatic monitoring scripts at the SOC. ... Diagnostic and science exposures can also be used to identify bad pixels. Diagnostic exposures can also be used to confirm the presence of previously identified and up-linked bad pixels. ...

Next: Redshift Distribution Up: Sample Identification Previous: Previously Identified Sources . ... In Figure 3, we plot the redshift distribution of DXRBS FSRQs opposite that of the 1 Jy and S4 samples. In Figure 4, we plot the redshift distribution of DXRBS BL Lacs opposite the Slew and 1 Jy samples. ... The apparent deficit of objects at the very highest luminosities is a result of the smaller area of sky covered by DXRBS compared to, e.g., the Slew and 1 Jy samples. ...

The Spitzer Infrared Nearby Galaxies Survey (SINGS) is carrying out a comprehensive multiwavelength survey on a sample of 75 nearby galaxies. The 1-850 ЮМm spectral energy distributions (SEDs) are presented using broadband imaging data from Spitzer, 2MASS, ISO, IRAS, and SCUBA. ... Spitzer's excellent sensitivity and resolution also allow a detailed investigation of the infrared SEDs for various locations within the three large, nearby galaxies NGC 3031 (M81), NGC 5194 (M51), and NGC 7331. ...

... Bojan Nikolic web pages (r. 329) . ... The OOF data reduction software is made available under the terms of the GPL V2 or (at licensee?s option) latter licences. ... Also, please note that this is primarily a research system that has grown during investigation and application of the OOF technique. ... The first generation of the OOF system that I wrote was designed to work within the software package that J. S. Richer wrote for reduction of with-phase holography for the JCMT. ... Build system: . ...

... APPLY/DISPERSION in out [y] [coef] . Apply the dispersion relation to a 1D spectrum and generates a table . BATCH/LONG . ... CALIBRA/FLUX in out [resp] . Correct an image for the instrumental response function . ... Wavelength calibration of 1D and long-slit spectra . ... LINADD/LONG in w,bin [y] [mtd] [mode] [line] . ... PLOT/CALIBRATE [mode] . ... Plots a 1D spectrum in table format, as supplied by APPLY/DISPERSION . ... RESPONSE/LONG [plot] [fit] [deg] [smo] [table] [image] [visu] . ...

Next: Identification and Analysis of Binary Star Systems using Probability Theory . ... We present a computing code for modelling energy flux distributions, photometric indices and spectral line profiles of (non-)radially pulsating Main-Sequence stars. ... In the case of slowly rotating stars one can use the zero-rotation approximation to describe stellar pulsations. Such a model was used already by Cugier, Dziembowski & Pamyatnykh (1994) to study nonadiabatic observables of Cephei stars. ...

... ATNF Home . About ATNF . ... About ATNF overview . ... Australia Telescope Steering Committee . ... Australia Telescope User Committee . ... Murchison Radio-astronomy Observatory . ... Parkes radio telescope . Australia Telescope Compact Array . Mopra radio telescope . ... Parkes | ... Visiting Parkes radio telescope . ... Parkes radio telescope webcam . ... The first claim that HI could be associated with a dSph-like system was for the dIrr/dSph system Phoenix (Carignan, Demers & CУДtУ? ...

... The power can be converted to the probability that the period found is not true, the false alarm probability (FAP). Scargle (1982) showed that the probability distribution returned by this method is exponential, and thus the probability of a false alarm is defined as , where z is the power at a given frequency and N is the number of frequencies sampled. Unfortunately, the formulation for calculating the FAP is only valid in the case where the data are not clumped in their sampling. ...

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. ...

... In brief: the frequency-dependent radiative transfer equation is solved for a dust under assumption of spherically-symmetric geometry for its distribution taking into account particle size distribution and quantum heating effects for the very small dust particles. ... Table: Model parameters for IRAS04296+3429. ... parameter . ... hot dust shell) . ... The best fit to the spectral energy distribution of IRAS04296 is shown by heavy solid line (see Table2 for details concerning parameters of the model...

2007 Jan 08) Bright comet C/2006 P1 (McNaught) . 2005 Jan 20) Tornado near Coonabarabran . 2005 Jan 16) Major upgrade in progress . 2005 Jan 16) Near Earth Comet 162P/Siding Spring . 2004 Apr) 2004 CB identified as a comet . 2004 Apr) Systematic surveying commenced 2004 March 16 . 2004 Apr) Media Releases on commencement of survey . 2004 Jan) 'Accidental' discovery of 2003 XB22 . ... Siding Spring Survey Main Page . ... Previous News Items . ...

Next: Galactic distribution and absolute Up: BASIC PROPERTIES Previous: BASIC PROPERTIES . ... RCB stars have a spectrum which resembles that of an F or G supergiant. The Balmer lines of hydrogen are unusually weak or absent, there are many lines of neutral atomic carbon and strong bands of molecular carbon (C and CN). ... Clayton 1996 ], [ Jeffery et al. 1996 ]). There is a small group of early-type stars reputed to show RCB-type light curves and also have weak Balmer lines. ...

... One of the most widely used tools of Fourier analysis is the Parseval theorem. It enables the experimentalist to view how the `energy' in the signal is distributed among frequencies. The Fast Fourier Transform (FFT) algorithms have made power spectra one of the obvious diagnostics tools during data acquisition, and energy maps are a versatile alternative. ... The result is an energy map (Fig. 9), showing the distribution of energy corresponding to the wavelet map (Fig. ...

Looking back on the universeтАЩs history for a specific patch of the sky observed by Herschel and Keck to reveal many previously unseen starburst galaxies. This graphic shows a representation of the distribution of nearly 300 galaxies in one 1.4 x 1.4 degree field of view. In total, Keck identified 767 galaxies found by Herschel. Five starburst galaxies (as seen by the ESA/NASA Hubble Space Telescope) are shown as insets. ...

Next: Pilot Survey Up: Minutes of the 1st Previous: GALFA Surveys . ... The minimum integration time required to achieve a given mass sensitivity scales as distance to 4th power so the depth of survey increases only as t int to the 1/4. ... To predict what ALFA might see for several surveys, I have performed a set of simulations governed by the following: . ... ZOA survey: Assuming integration time of 300 sec, covering 10 (more than pulsar survey suggested), within the AO limits . ...

This module uses cookies to provide for a clickstream log of user activity on a site. ... In Apache 1.2 and later this module has been renamed the "user tracking" module, mod_usertrack. ... Instead, a configurable log format file should be used to log user click-streams. ... When used, this directive determines whether the cookie used for user tracking is created using the default ("normal") format (eg: decimal values for items like the PID) or using a more compact format (eg: hexidecimal values). ...

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... The Network Time Protocol (NTP) is used to synchronize the time of a computer client or server to another server or reference time source, such as a radio or satellite receiver or modem. ... Information on the NTP architecture, protocol and algorithms can be found in the Further Information and Bibliography page. The Building and Installing the Distribution page presents an overview of the procedures for compiling the distribution and installing it on a typical client or server. ...

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... 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. ...