Next: Catalog Construction Up: Observations and Analysis Previous: Source Detections . ... It was assumed that the highest signal gives the most likely position of the source. ... Comparing the summed map with the maps from the individual energy ranges, the one which produced the smallest error box was chosen to represent the source position, as long as was greater than 4, a level chosen to reflect a reasonable degree of confidence in the detection. ...

... Miriad has a couple of tasks available for finding positions of sources (see also cgcurs in Chapter 17 ). ... It fits a 2-D parabola to the image intensities in a 3 by 3 pixel box centred on the brightest pixel in a specified region and reports the fitted location and intensity. ... Input image . ... The quality of your fit can improve significantly by selecting a snug region, and/or using the clip keyword to keep pixel values with little signal (e.g. sidelobes and noise) out of the fitting process....

The offsets (in focal plane and sky) are shown for various configurations (.ps) ( .pdf ): . Each plot shows the location of the 19 dipoles in various positions. ... On 29jun10 i switched to use the measured center locations on the sky.. but: . ... Page 1,2 have the dipoles as they are mounted on the positioner with no rotation. ... Page 3: Dipoles at center (focal plane) . ... Page 5: Dipoles at center and positions A1-A6 (focal plane) . Page 6: Dipoles at center and positions A1-A6 (on sky) . ...

... The exact directions of the offsets are parallel to the rows and columns of the CCD on which the aperture is specified. ... It is often useful to explicitly specify the desired rotation of the WFPC2 field-of-view on the sky. ... Figure 7.8 shows the CCD orientation and aperture locations relative to the U3 axis. ... Obtain the Position Angle (PA) of the source axis on the sky, measured in the standard way, North through East. ... desired source angle in field-of-view measured CW from +U3 axis) . ...

A bright supernova, 1998S, has been found on March 3 by Chinese astronomers at Beijing Observatory. 1998S is located in NGC 3877 an UMa galaxy at R.A. = 11h46m06s, Decl. = +47o29'.0. ... Recent magnitude estimates show the star at around magn 12. ... It covers a field of 35'x35' and shows stars down to magnitude 15 and is mainly based on the GSC and USNO catalogues. ... Below follows a list of field and sequence stars located within ~20' from SN 1998S in NGC 3877: . ... TI (b-r)=+0.5 . ...

XMM-Newton Science Analysis System . ... A different approach is done via the setting withctisrcpos =Y: all event energy corrections do not use the actual RAWY coordinate but the corresponding RAWY location of the source ( SRCPOS ) as determined by the task epframes (either automatically or via setting withsrccoords =Y). ... The task epchain may be used with the setting ccds =4 withctisrcpos =Y to process only the CCD 4 where usually the bright source is located that causes the Out-of-Time events. ...

. Please standby and you will be automatically connected to the new location of the unframed Supernova page. Or, click on the link above. If you have questions or problems, please email me at David Bishop dbishop@vhdl.org . Last modified: Mon Aug 27 12:40:15 EDT 2001

... Tonight's Sky . ... The Magazine . ... Observing . ... The double star 54 Leonis, spiral galaxy NGC 3198, and emission nebula NGC 3199 . ... Astronomy for Kids . ... Observing springtime deep-sky objects with a large telescope . ... Bright planets meet at dusk . ... Astronomy magazine subscribers can read the full article for free. ... Get instant access to subscriber content on Astronomy.com! ... Receive news, sky-event information, observing tips, and more from Astronomy's weekly email newsletter....

... Slit-plate Deflection . ... One end of the approximately 2m long fiber is inserted into a hole in an aluminum plug-plate, and the other end is fed into and supported by a slit-plate. ... Since the fibers are to be calibrated from a fixed position, it will be necessary to know how much the slit-plate deflects under its own weight due to gravity, as well as how much it deflects under the weight of the fibers and harnesses. The deflection of two plates of thickness 3.175 and 3.607mm was tested. ...

Locating Uranus and Neptune in the constellation Capricornus for fall 1999 Alpha Theta Beta Rho Pi Omicron Sigma Key: Magnitudes 3 4 5 6 7 8 Uranus (mag 5.7) Neptune (mag 7.9) Shown for 5-Oct-99, but positions wont change much until mid-November Using binoculars, you should be able to locate Uranus and possibly Neptune using the chart above, even from the light polluted suburbs of Boston. ... Once you find Sigma, look further in the same direction and youll see Neptune. ...

... GCN 8471 | ... TITLE: GCN CIRCULAR NUMBER: 8516 SUBJECT: GRB 081102: MASTER refind and final results DATE: 08/11/11 15:50:10 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina, D.Kuvshinov, P.Balanutsa Sternberg Astronomical Institute, Moscow State University A. Tlatov, A.Parkhomenko Kislovodsk Solar Station of the Pulkovo Observatory V.Krushinski, I.Zalognikh Ural State GCN Circ 8470, Lipunov et al., ...

... U. Amsterdam Explanation: The GRB distance scale controversy may have just ended with a flash . Gamma Ray Bursts (GRBs) are powerful explosions occurring in seemingly random positions on the sky. ... There they found a faint but variable optical source : a potential counterpart to the gamma-ray burst that was getting brighter. Most importantly, continued scrutiny showed that this optical transient had absorption lines with a redshift of about 0.8 - the distance scale of galaxies and quasars . ...

Lab . Main page News People . ASA . Master . Master net Homepage . ... Lomonosov Moscow State University Sternberg Astronomical Institute . ... MASTER . ... Lomonosov (ShOK) . ... About Space Monitoring Laboratory, scientific directions, instruments, contacts . People, who work in lab . Latest news and news archive . ... Bright MASTER OT105123.02+672528.3 discovery at Optical/X-ray/radio source position ATel3845, ATel3849 ATel3889 . ... All news ...

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Once students get the hang of it, they can find and measure the brightness of Delta Cephei in a few minutes. ... of Delta Cephei . ... Oct. ... The following table lists the measurements of Delta Cephei made by one amateur astronomer in autumn 1990. ... 4.0 . ... This activity is a simplified version of one that appeared in Hands-On Astrophysics, a series of activities prepared by the American Association of Variable Star Observers with support from the National Science Foundation. << previous page | ...

1) Find the variable star and the comparison stars marked in the map. 2) Seeing the the variable star, try to imagine its location in the brightness interval between the reference stars. 3) Looking at the specially prepared scale, try to reproduce the location of variable in the brightness scale from memory. ... The grades of arbitrary scale are marked relative to brightness intervals between the reference stars. ...

Finding Himalia, The Fifth Brightest Moon Of Jupiter . Articles | ... Himalia is the only moon other than the Galilean moons of Jupiter that is visible in an amateur size telescope. ... I normally use “The Sky” from Software Bisque for planning my observing sessions and in helping me find objects, but it only has the Galilean moons for Jupiter so I used Red Shift (version 3 at the time) which I also had on my computer. ... www.astronomy.net . ... dbHTML," "AstroGuide," "ASTRONOMY.NET" & "VA.NET" . ...

... Using a simple 2-D Gaussian Point Spread Function (PSF) on a constant (flat) sky background, I derive a theoretical photometric and astrometric performance model for analytical and digital PSF-fitting stellar photometry. ... The photometric performance is maximized when either the effective background area or the effective-background-level measurement error is minimized. ... An important, but frequently ignored, noise source is the uncertainty of the measurement of the effective background level ( )...

image collection >> physical phenomena >> vortices . Image ers0205130118 . ... Cyclonic eddies on the front of the Soya Warm Current, La Perouse Strait. In the SAR image, the narrow bright band ~1 km wide is caused by current shift and starts near Kamen Opasnosti (Rock of Danger) where cold waters are located (see AVHRR image ). ... The third eddy also has the cold central area with SST equal to 5°C. The coldest waters (4°C) form a band to the southeast off the eddy's centre. ... Image . ...

True Color Image Gallery: Galactic SNR | ... Common Name: SGR 1900+14 . ... Description: bright SGR located well outside shell of remnant . ... Exposure uf . ... Exposure uf Exposure time of unfiltered event file . Exposure f Exposure time of filtered event file . not clear if SGR and remnant are associated . ... Event 2 FITS File . ... Pileup model used to correct spectrum but index probably uncertain. see fit detail page for more about the fit. see chandra spectrum page for region used. ...