In this gallery are many images of Low Surface Brightness Galaxies which have recently been discovered and analyzed. ... The central surface brightness of this galaxy is 24.28 . Malin 2 This galaxy is another huge disk galaxy with a scale length of 15 kpc and a redshift of 15000 km/a. The high surface brightness knot in one of its spiral arms actually has the same color, luminosity and H-alpha equivalent width as the entire Large Magellanic Cloud . ... Truly it is a Low Surface Brightness Galaxy. ...

Target Acquisition Reference Information . ... In almost all cases where an onboard acquisition will not work (because the object is in a crowded field, or is variable, or is a moving target), it is sufficient to use an early acquisition to get a WFPC2 or FOC image a few weeks in advance of the GHRS observation. ... Explicit BRIGHT and FAINT limits may be specified if you desire, although there is an increased risk of a failed acquisition unless you are confident of those fluxes. ... MAPs . ...

Subject, Problems and Objects of Theoretical Astrophysics. ... Stellar Photospheres, Their Features. ... Physics of Continuous Radiation Absorption in Stellar Photospheres. ... Continuous Radiation Absorption in Stellar Photospheres of Various Spectral Classes. Solar Type Photospheres. ... Characterisics of Absorption Lines. ... Interstellar Absorption Lines, Their Features. ... Physical and Dynamic Features of Interstellar Medium, Which Follows from Observations of Interstellar Absorption Lines. ...

... Column 1 gives the object name from the Case or Markarian catalogs. ... For Markarian galaxies the errors of coordinates usually lie inside 2'' (Lipovetsky [ 1983 ]). Column 4 gives the eye-estimated apparent blue magnitudes according to the same sources. ... Other names of a galaxy we give in column 7. ... In column 3 we cite the original emission-line code of the galaxy for the strength of [O III ] doublet according to the Case catalog (s - strong, m - medium, w - weak). ...

... A new IRAF task has been developed that automatically identifies linear (line-like) features in an image or set of images. ... In order to automatically detect linear features, the first step is to select pixels in the image (Fig. 1 , left panel) that fall within a given data value range. ... Another aspect of extended linear features is that the image space pixels that describe them are in some way adjacent to one another and have a minimum and maximum length. ...

... 3D structure rings , spots filaments · Application to Cygnus A and 3C 317 Radio cocoon and shaped Xray gas (contours) in Cygnus A Cygnus A (Chandra archive, courtesy P. Strub) large cocoon width elliptically shaped cluster gas marks bow shock axis ratio: 1.2 Outline · · · ­ Pretty data: Cygnus A Parameters of jet simulations in the history Extension to very low ... L g[ = -2 ] Parameter Study: Axis Ratio Small jets have spherical bow shocks! critical radius depends on . ...

PCA Calibration Status · Calibration of the Rossi X-ray Timing Explorer Proportional Counter Array Jahoda, Markwardt, Radeva, Rots, Stark, Strohmayer, Swank, and Zhang, 2006, ApJS, 163, 401 ­ Energy : residuals 1% (E 10 keV ); 2% (below 20 keV ) ­ Background: (excess variance)1/2 2%/channel on time scales 1600 sec · ~ 1% (2-10 keV ); ~ 0.7% (10-20 keV ) ­ Timing: ...

... Armagh Observatory, College Hill, Armagh BT61 9DG, +44 (0)28 3752 2928 . ... The interface between the lower solar atmosphere where energy is generated by subsurface convection and the corona comprises the chromosphere, which is dominated by jet-like, dynamic structures, called mottles when found in quiet regions, fibrils when found in active regions and spicules when observed at the solar limb. ... In addition, how they affect the coronal heating and solar wind need to be further explored. ...

The problem of solar wind data correlation for the observations onboard several spacecraft is very important for three points of view: . ... This problem is studied now in detail by systematic determination of ion flux and ion velocity data correlations by INTERBALL-1 (IKI group), WIND and IMP 8 (both - MIT group). ... Solar wind plasma correlation lengths from IMP 8, WIND and INTERBALL-1. ... Correlation of solar wind observations onboard several spacecraft: INTERBALL-1, IMP 8 and WIND data. ...

THE PHOTOMETRIC RESEARCHS OF THE MERCURY'S SURFACE BY MEANS OF DIGITAL MODELS. ... The surface brightness of Mercury was measured Danjon (1933, 1949, 1953) and Harris (1961) in phase angle 3o-123o. The analysis of the various data of the integral photometric gives the results of determination of the main photometric constants for Mercury. ... THE PHOTOMETRIC RESEARCHS OF THE MERCURY'S SURFACE: S.G. Pugacheva The surface brightness of the Mercurian images was established on the geologic map Mercury. ...

... 8, ``Celestial Mechanics'', 2002 Parameterization of the Solar Radiation Pressure model for GPS satellites I. S. Gayazov Institute of Applied Astronomy, St. Petersburg, Russia The treatment of solar radiation pressure (SRP) effect until now is the main problem in precise modeling of GPS satellite orbits. ... In practice, however, all seven parameters of the empirical model cannot be confidently determined from phase observations. ... Bar­Sever Y. E. A new model for GPS yaw attitude. ...

... 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...

Above is an image of a Chandra Low Energy Transmission Grating (LETG) spectrum of a very bright X-ray source, the nova XTE J1118+480, showing only the shortest wavelengths. ... Bright spot in center = the source (i.e., 0th order of the spectrum) . Bright diagonal line extending corner to corner = the main dispersed spectrum (1st and higher orders) . Bright line perpendicular to the main spectrum = cross-dispersion spectrum of 0th order, caused by the LETG fine-support structure . ...

... The HH flow associated with young stellar object HL Tau has an exciting history and even until now the origin of some its features is not clear yet. ... Knotty structures of Herbig-Haro jets are common phenomena and knowing the origin of such structures is essential for understanding the processes of jet formation. ... In the flow detected compact knots with high (-150 km/s) and bow shape structures in front of those, with low radial velocities (-50 km/s). ...

... northern O and early B stars whose spectra could be obtained with the parameters required to look for variability at the using the CEGS echelle spectrograph, maintained at the coude focus of the 1-m Northern Caucasus Special Astrophysical Observatory (SAO) telescope (Musaev 1996). The list of the program stars includes 29 obiects. When choosing appropriate dates of observations, the program stars can be observed for almost the entire night. ...

... Apache HTTP Server Version 2.4 . ... macro_module . ... These macros have parameters. ... macro definition within a <Macro> section, following the apache style. user defined names for the macro and its parameters. macro names are case-insensitive, like apache directives. macro parameter names are case sensitive. macro parameters must have distinct names. error on empty parameter names. redefining a macro generates a warning. macro definitions can be nested... (but what for?) . ... Use of a macro: . ...

... We are using Canadian Galactic Plane Survey l 74.2њ, -3.6њ < b This poster gives preliminary results for a full-fledged analysis of the gas properties and distribution of HISA features in the CGPS. ... where T ON and T OFF are observed brightnesses on and off the HISA feature, T S is the spin or excitation temperature of the HISA gas, tau is its optical depth, T C is the continuum intensity, and p is the fraction of H I emission lying behind the HISA feature. ... GIF | ...

Statistical methods and HI in the Magellanic Bridge Erik Muller ATNF Preamble Using numerical simulations to assist in the interpretation of observational data. ... Numerical simulations of the Mag. ... Some statistical methods for HI · Spatial Power spectrum (SPS) · Spectral Correlation Function (SCF) The Magellanic System. ... N-Body Numerical simulations High velocity spur SMC LMC SMC Wing Peak intensity, RA-Vel [K] (Bruns 2003 ­ Parkes data only) Some conclusions from SPS 1. ...

... 11 Yellow-Green (78% transmission): Contrasts well with the red and blue characteristics of surface features on Jupiter and Saturn. ... 82A Light Blue (73% transmission): Useful on the Moon, Mars, Jupiter, and Saturn, this subtle pale blue filter enhances areas of low contrast while avoiding significant reduction of overall image brightness. ... Meade Series 4000 Photo-Visual Color Filters may be ordered individually or in the following sets: . ... Meade Series 4000 Broadband Nebular Filters . ...

The night sky brightness, together with number of clear nights, seeing, transparency, photometric stability and humidity, are some of the most important parameters that qualify a site for front-line ground--based astronomy. ... Night sky at ESO-Paranal (Chile). ... Night sky brightness data . ... UBVRI night sky brightness at ESO-Paranal during sunspot maximum (A 2003, PDF) . ... The Dancing Sky: six years of night sky observations at Cerro Paranal (Starlight 2007 conference proceedings, PDF) . ...