... BLUE STRAGGLER STARS are unusually hot and bright stars found in the cores of ancient star clusters known as globulars. ... BACKGROUND (from wikipedia): Blue straggler stars are stars in open or globular clusters that are hotter and bluer than other cluster stars having the same luminosity. ... There is evidence in favor of this view, notably that blue straggler stars appear to be much more common in dense regions of clusters, especially in the cores of globular clusters. ...

Next: *display, xdisplay, xexamine* - Up: Image Display in Xwindows Previous: A Region mask for . In order to view a large image/qp file with the SAOimage display, it is necessary to block or section that image. The SAOimage pixel readout is not in original image/qp coordinates (physical) but in blocked and perhaps sectioned coordinates (logical). ... In the output file, your original region has been commented out and the same region in physical coordinates has been inserted. ...

... To save time, I will only provide ephemerides in 2000 coordinates. ... Note: most the orbital elements used to create these ephemerides were obtained from the International Astronomical Union Circulars (IAUCs), Minor Planet Circulars (MPCs) or the ICQ Comet Handbook. ... The following 1-day ephemeris (March 1, 1997 - October 1, 1997) is from Donald Yeomans of JPL and is based on Reference Orbit #55 (March 4, 1997). 2000 coordinates (March - September, 1997) [3/4/97] . ... Epoch: 1997 Feb. 1.0 . ...

... Shortly after its discovery it was determined to be in a highly elliptical path near Jupiter and on a collision course. ... T he size and mass of the original body and the individual fragments is as of this writing still highly uncertain. ... B etween 16 July 1994 and 22 July 1994 the fragments impacted the upper atmosphere of Jupiter. ... T he pictures were posted to the Net within hours of the impacts and caused severe overloading on some ftp and WWW sites. ... JPL's SL9 page . ... Small Bodies .....

... For more distant stars we must use other techniques. ... Hence if we see a distant galaxy and can pick out any cepheids lying within it, we can calculate its distance. ... Here then is another method to gauge the size of the Universe and there are yet more. volume at high enough temperature a nuclear fusion reaction sweeps across the white dwarf's surface and eventually we will see a spectacularly bright new star (hence nova) in our skies. ... Why is this relevant to the size of the Universe? ...

The revision of the MASS/DIMM star catalogue N. Shatsky, V. Kornilov March 16, 2008 Abstract The compilation of the (updated) version of the MASS (MASS/DIMM) device target catalogue is described. ... Then the list was cleaned according to following criteria: I. Remove stars too faint for a MASS device. ... Here the color equation of the Sternb erg device was taken: M AS S mag = V mag + 0.45 (B - V ); stars with M AS S mag > 3.2 were removed. ... This was made based on the GCVS4.2 catalogue data. ...

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]. ...

Modeling of atmospheres of the brightest stars belonging to the Cyg OB2 association O LGA M A RY E VA , V. G . K L O C H K OVA , E.L. C H E N T S OV Special Astrophysical Observatory RAS; olga.maryeva@gmail.com We present the results of modeling of the spectrum of the brightest stars belonging to the Cyg OB2 association ­ Cyg OB2 #7 (O3If ) and Cyg OB2 #11 (O5Ifc). ... The lines in Cyg OB2 #7 spectrum are divided into three groups which can not be described with a single model. ...

Kholtygin A.F., Burlakova T.E., Fabrika S.N., Valyavin G.G., Yushkin M.V. Microvariability of Line Profiles in the Spectra of OB Stars: delta Ori A . ... We have studied variability of the spectral lines of the OB star delta Ori A -the brightest component of the delta Ori triple system. ... However, some of the variable features go outside the band, presumably due to either imhomogeneities in the stellar wind from .Ori Aa1 or non-radial pulsations of the weaker components of the system, Aa 2 or Ab. ...

The WISP field position as originally planned, shown on a reproduction of O filter (blue) Palomar Sky Survey prints of the Pleiades region. ... WISP1, WISP2, and Bj 50% transmission bandwidths are shown at bottom. ... Regions 6-11 select more general parts of the larger nebulosity and are shown connected to Alcyone, which is presumed to illuminate them for the discussion in \S\ref{Sec:schmidt_results}. ... The same field shown in Fig. \ref{Fig:schmidt_bloom}, with saturation bloom lines removed. ...

August 3, 1998 . ... An example of the EUV large-scale chains revealed by the modified TRACE EUV images. (a) - The original TRACE EUV (171 A) mosaic image of August 3, 1998. Some thin chains and threads are seen inside the active complexes A and B in the north-west and south-west sectors of the disk. Large-scale structures outside the complexes are hardy visible. (b) - The same TRACE image, but after a modification. ... Back to the page of the TRACE chains . ... Last update: 9 August 1998 . ...

... I. Mean Surface Brightnesses and Integral Color Indices for Bars Gusev A.S. ================================================================================ Abstract: UBVRIJHK surface brightnesses and color indices of bars of galaxies are determined using surface photometry data for 100 barred galaxies (table1.dat). ... J0 Mean surface J0 brightness 46 A1 --- CI- CI sign 47 -50 F1.2 magn/sq.arcsec. U-B)0 (U-B)0 color index 52 -55 F1.2 magn/sq.arcsec. ...

... 50 Weirdest Objects . ... Observing springtime deep-sky objects with a large telescope . ... What is the baseline for determining the magnitude scale of celestial objects? Why do brighter objects have negative numbers? ... He called the brightest 1st magnitude and the faintest 6th magnitude. ... Also, to assign a magnitude to the brightest planets, the Moon, and especially the Sun, scientists would have to work with negative numbers. Get instant access to subscriber content on Astronomy.com! ...

You Can Make Stellar Images Brighter . Articles | ... A few months ago I wrote an article titled "You Can’t Make Them Brighter". So why am I now writing that you can make them brighter. ... The image of a focused star is actually a small disk called the Airy disk, named after the 19 th century scientist Sir George Airy. ... For a given aperture, a smaller Airy disk means that the light is focused to a smaller disk and is therefore brighter. ... www.astronomy.net . About Astronomy Net | ...

April 17, 2007 1:00 UTC (approx) Nikon D200 on CDK20 at Moore Observatory 30 second exposure 85mm f/1.4 lens (stopped to f/2) ISO 400. It's a 30 second exposure, tracking with the CDK20, in noise reduction (dark subtraction) mode. I've scaled the original 10 megapixel image down by a half in each dimension here, so it would be about 2.5 MB uncompressed. The compressed file is 1 MB. ... Except for rotating the image and scaling down, its unaltered from the file out of the camera. ...

... Submitted by Sidney Johnston on 03/14/2013 01:01:35 . 2013 comet Panstarrs on 13 March 2013 . ... We took this image with a Canon 40D, 135 mm setting on a zoom lens (28 mm - 135 mm) on 13 March 2013, at about 19:50 EDT (18:50 EST) (23:50 UTC). The image was stretched by Photoshop to adjust brightness. The pesky aircraft contrail shows in the original camera image and also in the stretched image “with contrail”. ... Copyright (c) Amateur Telescope Makers of Boston, Inc. ...

... Bad Astronomy . ... Mad Science . ... Universe Today . ... Keep Bad Astronomy close to your heart, and help make me filthy rich. ... type 1a supernovae seem most useful . ... This is a bright, massive star that explodes after fusing all the light elements in its core. ... That means we can calculate how far away it is. ... This is exactly what we are trying to do with these supernovae; look far enough away that any deviations from flatness of the Universe can be seen. ... Phil Plait . ...

On' failures in the NIRSpec MEMS ST-ECF Instrument Science Report NGST 2002-02 The effects of `on' failures in a MEMS array for the NGST NIRSpec Santiago Arribas, Robert Fosbury Peter Jakobsen --1-- ST-ECF Instrument Science Report NGST 2002-02 The effects of `on' failures in a MEMS array for the NGST ... Assuming that the spectrum of a single facet uses 2000 detector pixels, only 0.01% of `on' failures is acceptable (i.e., 400 facets in a 2k в 2K MEMS array). ...

Physical and dynamical parameters of particles in outbursting Comet 17 P/Holmes . ... The time depending offset between the center of brightness and center of mass of the comet nucleus has been determined on the ground of positional observations of the comet. ... The motion of these particles allowed subsequent offset between the center of brightness and center of mass of the comet nucleus to be obtained from positional observations. ... comet, dynamical model, outburst, brightness. ...

... The catalog contains SAO number; the right ascension and declination with a B1950.0 equinox and epoch; annual proper motion and its standard deviation, photographic and visual magnitudes; spectral type; references to sources; the Durchmusterung (DM) identifier if the star is listed in the Bonner DM (BD), Cordoba DM (CD), or Cape Photographic DM (CP); component identification; The Henry Draper (Extension) (HD or HDE) number; and J2000 positions and proper motions. ...