|Right Ascension||09 : 55.6 (h:m)
|Declination||+69 : 04 (deg:m)
|Visual Brightness||6.9 (mag)
|Apparent Dimension||21x10 (arc min)
Discovered by Johan Elert Bode in 1774.
M81 is one of the easiest and most rewarding galaxies to observe for the amateur astronomer on the northern hemisphere, because with its total visual brightness of about 6.8 magnitudes it can be found with small instruments. Brian Skiff of Lowell Observatory reports that he could see M81 with the unaided naked eye under exceptionally good viewing conditions (i.e., clear dark skies), and is at least the fourth observer who reported to have done so !
The pronounced grand-design spiral galaxy M81 forms a most conspicuous physical pair with its neighbor, M82, and is the brightest and probably dominant galaxy of a nearby group called M81 group. A few tens of million years ago, which is semi-recently on the cosmic time scale, a close encounter occurred between the galaxies M81 and M82. During this event, larger and more massive M81 has dramatically deformed M82 by gravitational interaction. The encounter has also left traces in the spiral pattern of the brighter and larger galaxy M81, first making it overall more pronounced, and second in the form of the dark linear feature in the lower left of the nuclear region. The galaxies are still close together, their centers separated by a linear distance of only about 150,000 light years.
Using the Hubble Space Telescope, a team under Wendy Freedman of the Carnegie Institution of Washington has investigated 32 Cepheid variables in M81 and determined the distance to be 11.0 million light years, in 1993 well before the HST was refurbished. Together with the new distance scale correction implied by the results of ESA's Hipparcos satellite, the true distance of M81 is probably closer to 12.0 million light years. See the H0 Key Project Team's work on M81 (article 1, Freedman et.al. 1994, and article 2, Hughes et.al. 1994).
On Sunday, March 28, 1993, a type II supernova (1993J) occured in M81, which was discovered by the Spanish amateur astronomer Francisco Garcia Diaz from Lugo (Spain), and reached a brightness of about mag 10.5 in its maximum. The remnant of this supernova was imaged in the radio light at 3.6 cm wavelength from roughly six to 18 months after the explosion, with a global Very Long Baseline Interferometer (VLBI) array of radio telescopes in Europe and North America.
Investigations performed in 1994 have indicated that M81 has probably only little dark matter, as its rotation curve was found to fall off in the outer regions; this is in contrast to many galaxies, including our own Milky Way, for which the rotation curve increases outward. To explain the velocity of the stars in these regions, the galaxy must have a certain amount of mass. However, the total mass observed in luminous matter - stars and nebulae - is insufficient to explain this behaviour; thus it is assumed that there is a significant portion of mass in galaxies is non-luminous, dark matter (or at least low-luminosity matter).
In December 1990, the ASTRO-1 Space Shuttle mission (STS-35) transported telescopes into the Earth's orbit, including the UIT (Ultraviolet Imaging Telescope) which obtained images of M81 (in the ultraviolet light; these were compared with the visible light image, and combined to an interesting and informative overlay; an animation [433 k MPG] showing a morphing from the UV to visual image of M81 is available). Previously, M81's UV radiation had been investigated by the Soviet Astron orbital observatory. Bill Keel has assembled a series of images of M81 in the different parts of the electromagnetic spectrum from the radio part to the X-rays region.
Last Modification: 9 Dec 1999, 22:59 MET