Following are instructions to build and install the programs in this distribution. Make sure that you have all necessary tools for building executables. ... The automatic build process expects a configuration file called Config.local . ... The configuration file specifies the directory in which to install the binaries, as well as control over the generation of debugging code and reference clock support. ... Cleans out object files, programs and temporary files. make distclean . ...

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. ... Wavelengths are based on experimental level energies where available; wavelengths calculated from theoretical energies are less accurate and are given as negative values. References: %observed energy levels: Kelly, R.L., 1987, J.Phys.Chem.Ref.Data 16, Suppl. ...

... the dark tail just above the actual trap, which can be treated with wfixup or fixpix , . cases where real objects cross the bad column, such as the object just above 2-637 in Figure 5 , . ... The standard technique for removing the effects of traps (i.e., "bad columns") is to use the . ... c1h images. ... Note that trap 2-637 from Figure 1 and Figure 5 appears to be the only trap which leaks a small amount of charge in an "upstream" direction, thus we chose a more typical trap for this example.) ...

... Sources found in the local detection step (task eboxdetect ) at significance levels (column SIGMA of eboxdetect source list) exceeding a user-specifiable threshold (input parameter mlmin ) in the respective energy band are removed from the image using a suitable PSF and source brightness dependent cut-out radius (determined to be the radius at which each source contributes more than a user-specifiable number of counts/arcsec to the background; parameter scut ; default value: 0.01). ...

Neptunes in the Noise: Improved Precision in Exoplanet Transit Detection AimИe Hall , Simon Hodgkin , Gabor Kovacs and Don Pollacco 1 1 1 1 2 Institute of Astronomy, University of Cambridge 2 Department of Physics, University of Warwick Figure 2 (right): Distribution of radii of all known exoplanets (grey), with those from Kepler (green) and SuperWASP (blue) also shown. We present early results from a new analysis of raw data taken with the SuperWASP telescope[1]. ...

... 2000 . ... Abstract: I present the distribution of the brightest galaxies in the southern sky as obtained from the H I Parkes All-Sky Survey (HIPASS). ... A histogram of the systemic velocities of the brightest HIPASS galaxies is shown in Fig. ... It peaks, as expected, in the interval 800 to 2000 km/s. No bright galaxies were found with systemic velocities of less than -350 or more than 5500 km/s. Figure 2: Histogram of the H I systemic velocities of the brightest galaxies obtained from HIPASS. ...

... 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. ...

... The removal of the bright sky background from your IR images is one of the key steps in the data reduction process. Once bad pixels have been removed from all the astronomical frames, the object frames must have the matching sky background images subtracted from them. ... The simplest sky subtraction is where you have separate sky and object frames taken a short time apart. ... The resulting sky subtracted images should be examined to make sure that sky subtraction has been properly achieved. ...

... A2584 used the cband receiver and the mock spectrometers to cover a 1 ghz band at cband. ... Of the 14 bands, some were 11 Mhz and others were 86 Mhz. the digital filtering and offsetting was used. 01-17nov10 : gortex cover comes loose from cband horn mouth. moisture get ins horn, causes tsys to go up . 22feb11: the wideband H2CO line did not line up with the narrow band H2CO line. ... The plots for 22feb11 below have jumps across the band in Tsys. ... Plots were made of: . ... cntsToK and Tsys . ...

... Stellar Evolution is driven entirely by the never ending battle between Pressure and Gravity . As imbalances are reached, the star is driven to find a new Energy source. ... Pressure and gravitational forces are equal, the star is stable and its core is sufficiently hot to fuse Hydrogen into Helium More about main sequence stars . ... The luminosity generated by the core fusion of Helium into Carbon is far greater than the shell luminosity associated with the fusion of Hydrogen into Helium. ...

Introduction This catalogue contains mainly the atomic data needed in the astrophysical investigations of low-density plasma. It is a revised and extended version of the "Catalogue of Atomic Data for the Rarefied Astrophysical Plasma" (Golovatyj et al. ... Low-density plasma. ... In the present study we represent only the atomic data for computation of sp ectra of low-density astrophysical plasma (most known kinds of it are gaseous nebulae), their thermal and ionization structure. ...

... 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...

You can also see this page in Russian with using KOI8 (X Windows) or CP1251 (MS Windows) Cyrillic coding. The Laboratory supports the space TV experiments, mainly in the planetary exploration missions. ... Image Co-registration . ... PHOBOS mission - Martian satellites investigations. Phobos on the Martian limb, the image from Phobos-2 probe from 02/28/89. ... Russian Space Bulletin. ... Last modified at June,26 1997 Alexey Kuzmin: akuzmin@mx.iki.rssi.ru . Back to IKI home page ...

... As piles of ash are removed, the courtyard haтАж . Sidebar Left . Sidebar Top . No Sidebar . Sidebar Bottom . Sidebar Right . ... Title: As piles of ash are removed, the courtyard has the top few cm of contaminated soil removed as well. Description: NOTE: All images and movies are copyright and must not be reproduced or mirrored in any form without written permission. ... As piles of ash are removed, the courtyard has the top few cm of contaminated soil removed as well. ...

... Spherical aberration, coma, and astigmatism are also easily observed using the star test. ... Off-axis images are complex. ... Fig. ... Diffraction by a circular aperture as a function of defocus for no aberration Airy Disk 1 wave defocus Less than 1 wave defocus Fig. ... Diffraction by a circular aperture as a function of defocus for third-order spherical aberration Paraxial Focus Small distance inside paraxial focus Moderate distance from marginal focus Immediate neighborhood of marginal focus Fig...

Next: ST-6 Data Collection Up: Data Acquisition Previous: Data Acquisition with . ... The tracking software is extremely important to data collection, and will be presented here. The tracking software is run from the CPU box. ... The exposure adjust will set the exposure time. ... After the drive is calibrated, the track button will set the ST-4 in a mode where it will track the star until it either loses track or the operator stops the track. ...

... A three-cell test section roughly representative of the primary mirror was provided for this test by the Steward Mirror Lab. ... Additionally, the tests are intended to determine relative airflow vs. pressure drop characteristics for each of the air flow patterns so the results can be evaluated both as a function of flow rate and of pressure drop along the flow path. ... The bottom (top as installed) was cut out so it could close the chamber for heating and be removed for the cooling tests. ...

Bright Supernova - Archives On these pages you will find references to Supernovae which have faded into oblivion. ... Finally, in 1999, when I took over the International Supernova Network's Latest Supernovae page I retitled the main page "Latest Supernovae", BUT, it's the "Latest Supernovae" page of the "Bright Supernovae" pages which are also sub-pages of ISN. ... Brightest supernova in 2005 . ... Brightest supernova in 2002 . ... Brightest supernova in 2000 . ... Brightest supernova in 1999 . ...

ION AND ELECTRON ENERGY DETECTOR PAN-2 . ... The energy and angular distributions of charged particles can bring further information on the nature and spatial scales of magnetospheres processes. ... It permits the fast measurements of energy and angular parameters of charged particles in the range 40eV-40keV. ... The sensor unit is an electron electrostatic, axially symmetrical, toroidal analyzer. ... The energy range for both types of charged particles must stepped according to the logarithmic scale. ...

Gaussian Multiplicative Chaos and Applications R и M I R H O D E S , U N I V E R S I T и PA R I S - DAU P H I N E Motivations in turbulence In fluid dynamics, turbulence is a flow regime in which the velocity field presents unsteady vortices on many scales. ... Such flows arise when the source of kinetic energy making the fluid move is much greater than viscosity forces of the fluid. ... 2) In 1941, Kolmogorov suggested a statistical approach of the local dissipation of energy, called the K41 theory. ...