... The target area that we are concerned with in this study has a few problems....in that there isn't an abundance of literature available for the individual to access in search of photographs of the target galaxies, and magnitude sequencing of stars around these galaxies. ... The Rev. Robert O. Evans of Coonabarabran, Australia. ... Reference photographs (no sequencing) of the target galaxies (with the exception of 27 galaxies) can be found in the Deep Space CCD Atlas: North, by John C. Vickers.( ...

The radial velocity corrected to the galactic center vgsr (cz in km/s) is obtained by a correction of the motion of the Sun with respect to the local standard of rest (LSR) and a correction of the LSR motion with respect to the galactic center. The resulting correction is: vgsr = v + 232 sin(al2) cos(ab2) + 9 cos(al2) cos(ab2) + 7 sin (ab2) Where al2 and ab2 are the Galactic coordinates (longitude and latitude) and v is the radial (cz) velocity in km/s given as parameter v . ...

K-band Arcetri Obscured Supernova Search . What is the KAOSS Project? W hat is the KAOSS Project? Some recent surveys aimed at detecting Supernovae (SNe) in the optical have found that starburst galaxies do not show evidence for an enhanced SN rate, with respect to quiescent galaxies (Richmond et al. ... A similar result was obtained by Navasardyan et al. (2001) who looked for SNe in interacting galaxies, finding no evidence for correlations between SN rate and galaxy properties. ...

... To be read in conjunction with Chapter 5 of the WFPC2 Instrument -Handbook, Version 4.0. Here we supplement the Instrument Handbook with short discussions of the use of PSF subtraction to maximize image dynamic range and to obtain accurate stellar photometry. We also discuss a source of error in the published values of the HST aperture correction. ... Thus faint objects near bright objects can be difficult to detect and to distinguish from PSF artifacts. ... Last updated: 06/16/98 10:38:00 . ...

... Armagh Observatory, College Hill, Armagh BT61 9DG, +44 (0)28 3752 2928 . ... Circular polarization of the bright side of Iapetus versus wavelength, obtained with FORS2 at the ESO VLT during the night 2011-03-28 at a phase angle of 0.77 . ... It can be noted that a change in signal occurs in circular polarization observations that are taken after rotating the instrument by 90 degree with respect to the intial position angle on the sky. ...

New reduction of minor planets photographic plates obtained with Pulkovo Normal Astrograph A.A. Berezhnoy Pulkovo Observatory of RAS, Saint-Petersburg, Russia Minor Planet observations at Pulkovo Periodical observations of 14 bright asteroids named Selected Minor Planets (SMP) were performed at Pulkovo since 1948 within the international framework started by works of B.V. Numerov and D. Brouwer. ... 108 133 113 74 124 67 97 88 14 84 64 5 20 19 Epochs (YYYY.MM) 1200 Mean values of total obs. ...

... Two additional extensions contain the polynomial coefficients describing the distortion for all the filters. FILTER-U . ... Each extension FILTER-FilterId holds a binary table sampling the detector distortion of a specific filter at a coarse resolution ( 1 datapoint every 25 subpixel). ... The filter element is found in the column FILTER_ID. The required binary table entry is identified by matching the value of the column FILTER_ID with the State Variable FilterID. ... not applicable . ...

... This is the famous Orion nebula which is centered on the middle star of the sword of Orion (this is a 4th magnitude star). ... Here we present two CCD images of it. The black and white image was obtained using an ST6 Camera on a small telescope. The color image was obtained on the 48-inch telescope at Mt. ... The obtainer, Nelson Caldwell, took CCD images through Red, Green and Blue filters and later combined them to produce this image. ...

RTT150 . ... One of the image, obtained in the May, 2003, with Andor DW436 CCD. Cluster 1541+6626, filter R, exposure 15 minutes, the resolution is 1", limiting star magnitude is 23m, the field of view is 8' x 8'. At the left: image of cluster 0720+7132 (z=0.268) obtained in the beginning of November, 2002 with RTT-150 and AP-47P CCD. 25 minutes exposure in R. The resolution is 0.7" (angular size of the image element - 0.23"), limiting stellar magnitude is 23.5-24. ...

Next: Colours and magnitudes Up: The ESO Red Sky Previous: Project history . ... Plate overlaps are used for the calibrations. ... Galaxy counts on several plates near the SGP as a function of local background densities yield a good average correction curve for the magnitudes. ... Magnitudes from the J- and R-plates are labeled b_J and r_F, the symbols indicating the blue and red passbands and the photographic emulsions Kodak IIIa-J and Kodak IIIa-F, used in combination with filters. ...

... HI Observations of Interacting Galaxy Pair NGC 4038/9 . ... We present the results of new radio interferometer HI line observations for the merging galaxy pair NGC 4038/9 (`The Antennae'), obtained using the Australia Telescope Compact Array. ... Radio continuum images at 20 and 13cm are also presented, showing the discs in detail. ... Optical image of the central disks taken with the 4-m AAT by Dave Malin ( AAO ) . ... A 13-cm radio image of the central disks taken with the ATCA by B. Koribalski . ...

... Use the ROSAT broad band background which is a array file at 1/30 the *.qp file resolution, and contains data from PI bins 7-240. input files: xdata$rp110590.qp; xdata$rp110590_bk1.imh . ... xr> ximages xi> imcalc input file ('-' for STDIN) or imcalc commands: - # Interactive mode IMC) IMC) rp90_a.imh = xdata$rp110590.qp[bl=30,pi=7:240] - xdata$rp110590_bkl.imh # Select same size and channels as the background map # and subtract the background IMC) quit # To exit the interactive mode and imcalc . ...

... We report on our ongoing project ``Infrared Study of HII Regions Associated with Small Clouds.' ... These IR data, combined with optical imaging (which will be obtained from the IAC-80 telescope), IRAS survey maps, and existing CO observations of the associated clouds, will allow us to undertake a detailed investigation of the gas-to-dust mass ratio, initial mass function and the star-formation efficiency in these complexes. ... CHECKPSF: check the PSF (Point Spread Function) model, . ...

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... Tpram - time of the PRAM instrument (aquisition computer) . ... Bx - DC magnetic field with a fixed amplitude calibration; X component . ... The color lines present FFT from the AC magnetic field (Waveform); Bwx, Bwy, Bwz - from the bottom. ...

... Tpram - time of the PRAM instrument (aquisition computer) . ... Bx - DC magnetic field with a fixed amplitude calibration; X component . ... The color lines present FFT from the AC magnetic field (Waveform); Bwx, Bwy, Bwz - from the bottom. ...

The .out files contain the data displayed in plots of the wide spectral scans of High-CAL and the respective bets-fits obtained. Each of the 14 pipelines has a separate file. What to expect inside this file ? ... These files are made available for interested people to download. ... Note: Since the measurements for the beam0-pol_1, beam 5 (both pol.s) were missed from the set on tJD:53228 (due to the pre-amp and WAPP problems respectively), the corresponding fits & .out files missing. ...

D. Suprunenko Institute of Mathematics, National Academy of Sciences of Belarus Minsk, Belarus suprunenko@im.bas-net.by Lower estimates for the maximal weight multiplicities in irreducible representations of the classical algebraic groups The goal of this talk is to discuss some results on lower estimates for the maximal weight multiplicities in irreducible representations of the classical algebraic ... For groups of type An the situation is substantially more difficult. ...

Peremennye Zvezdy", . ... USNO-B1.0 0610-0600707 . ... USNO-B1.0 0608-0607099, 2MASS J17455451-2908127 . ... The star is too faint to be detected in the W2 band. It is difficult to unambiguously match the star with a 2MASS catalog object. ... The variable is the brighter southern star. It was not possible to measure the stars separately using UVOT U and W1 images, so the light curves and the variability amplitudes in these two bands refer to the combination of two stars. ...

... 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. ...