... Timeline . ... I had secured diagrams of all the groups and detached spots, and was engaged at the time in counting from the chronometer and recording the contacts of the spots with the cross-wires used in the observation, when within the area of the great north group (the size of which had previously excited great remark), two patches of intensely bright and white light broke out, in the positions indicated in fig. ... Click here for a text of Carrington's full article , including illustration.. ...

I-GALFA Survey Coverage Complete . ... The upper figure shows positions in equatorial coordinates: right ascension and declination, which are like extensions of the Earth's longitude and latitude coordinates on the sky. The lower figure shows positions in Galactic longitude and latitude, where Galactic latitude = 0 is the Galactic equator, or the plane of the Milky Way, and the center of the Galaxy lies in the Galactic plane in the direction where the Galactic longitude = 0. ... I-GALFA Main | ...

Tandis que je d butais la matin e du jeudi 1er septembre avec mes observations habituelles sur les formes et les positions des taches solaires, je fut t moin d'un ph nom ne que je crus extr mement rare. Comme d'habitude, l'image du disque solaire tait projet e sur une plaque de verre recouverte d'une peinture de couleur jaun tre, une distance et sous une puissance qui repr sentait une image d'environ 11 inches de diam tres. ... Je compris que j' tais le t moin d'un tout autre ph nom ne. ...

During the peak of the Leonid meteor shower on November 17, 1998, HST will be pointed near the anti-radiant for ten hours. Anyone who is interested can submit ideas to STScI for scientific observations during this time. ... At the time of the observations, the nominal V3 position angle is 248.3 degrees, and the STIS/CCD field is centered at RA=22 05 08.6, DEC=-23 25 59. ... There are no HST observations in the archives for objects in this field. ... No parallel observations may be requested. ...

Magnification (Power) And Using Eyepieces . ... To determine power in a telescope, divide the focal length of the telescope by the focal length of the eyepiece. By exchanging an eyepiece of one focal length for another, you can increase or decrease the power of the telescope. For example, a 25mm eyepiece used on a telescope with a 1000mm focal length would yield a power of 40x (1000 / 25 = 40) and a 10mm eyepiece used on the same telescope would yield a power of 100x (1000 / 10 = 100). ...

... Yu.A.Shokin Accurate positions of variable stars in the western part of the Large Magellanic Cloud bar (published in IBVS (No.5047, 14 March 2001) and SAI Proceedings) . B.S. Vozdvizhenskij The list of 2821 Venus positions (VINITI depository Oct 08 2007, N 956 B2007) . B.S. Vozdvizhenskij, E.N. Fedosseev The experience in processing long series of photographic observations of planetary positions (VINITI depository Apr 01 2008, N 274 B2007) . ...

Browse the articles below for new ideas for your classroom. Mercury September/October 2005: Astronomy Education and Public Outreach: Steps and Missteps Toward an Emerging Profession (pdf) . Focus on Education articles as they appeared in Mercury: . ... March/April 2000: . ... Education Newswire articles as they appeared in Mercury, by issue. ... January/February 2000 . November/December 1999 . ... March/April 1999 . ... November/December 1998 . ... November/December 1997 . ...

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. ...

... POLYNOM MAP NO | POLYNOM MAP2 NO 2 Changes The new distortion map is based in observations of the G153 eld. ... The previous map had been obtained by tting the measured o set (distorted position minus linear position, or detector minus sky positions) as a polynomial function of the linear (sky) position. ... Therefore what is needed is a function of the measured detector (distorted) position and this is how the new distortion map OM ASTROMET 0010 has been built. ...