NGC 3982
| NGC 3982 | |
|---|---|
| Constellation | Ursa Major |
| Apparent magnitude (V) | 12.0[1] |
| Apparent diameter | 1′.7 × 1′.5[1] |
| Classification | SAB (r)b[1] |
| Position Epoch: J2000.0 | |
| Right ascension (RA,α) | 11h 56m 28.1s [1] |
| Declination (Dec,δ) | + 55° 07′ 31″[1] |
| Red shift | 1,109+-6km/s [1] |
| Distance | 68.1 ± 2.5*106 light-year [2] |
| The other name | |
| The other name | |
| ■Project ■ Template | |
NGC 3982 is the middle eddy Milky Way at the approximately 68 million light-year away position in the direction of Ursa Major. I am known as UGC 6918. William Hershel discovered it on April 14, 1789 and classified it as a planetary nebula mistakenly [3]. NGC 3982 is a member of the M109 Milky Way group.
The apparent magnitude is 12.0, and a telescope is necessary for observation of NGC 3982. This Milky Way is seen as the spherical irregularity-formed light that is very gloomy, and is thin that some central domains are spirited when I use a small telescope.
Table of contents
Summary
NGC 3982 spreads through galactic approximately 300,000 light-year equal to approximately a one-third in the Seyfert type 2 Milky Way. It goes away at speed of approximately 1,109km/s from us. This Milky Way is the typical eddy Milky Way similar to the galaxy, and a super large mass black hole exists in the center, and the star formation is prosperous by the bright arm. In this domain, the supernova is observed, too.
In the arm of NGC 3982, a fixed star is born rapidly. Light Milky Way nucleus attracts old fixed stars, and density rises as the center. The star formation is prosperous in the nuclear fringe area and is estimated to be 0.52 sun mass per one year. With the image with the Hubble Space Telescope, it is shown between star formation domain and the Milky Way nuclei around the nucleus that a small whirlpool exists, and, as for this, it is the channel which gas metastasizes to in a black hole from the star formation domain.
NGC 3982 is located in Ursa Major and is a member of the M109 Milky Way group including the more than 50 Milky Way. This Milky Way group was named by brightest eddy Milky Way M109 [4]; [5] [6].
In this Milky Way, it can be help to measure distance out of the galaxy to include both two tools to measure a supernova and the distance of the heavenly bodies called Cepheid and I am interested and am studied.
Supernova SN 1998aq
In 1998, the light from a supernova of NGC 3982 reached the earth, and British amateur astronomer mark Armstrong discovered it (this supernova was named SN 1998aq later). Apparent magnitude was discovered at the time of 14.9, and two days increase shined it, and this supernova reached the up to 14.0 class. When this explosion comes from the binary system which a white dwarf catches the metastasis of the mass from a subordinate star, and a white dwarf acquires enough mass and can no longer support oneself, the fixed star wakes up an explosion bright intensely. Because a supernova explosion is generated in the typical eddy Milky Way every approximately 100 years, I am looking for the fixed star which seems to wake up a supernova using a high-resolution image of NGC 3982 and other Milky Way.
Source
- ^ a b c d e f g h "NASA/IPAC Extragalactic Database". Results for NGC 3982. November 16, 2006 reading.
- ^ Riess, Adam G.; Li, Weidong; Stetson, Peter B.; Filippenko, Alexei V.; Jha, Saurabh; Kirshner, Robert P.; Challis, Peter M.; Garnavich, Peter M.; Chornock, Ryan (2005). "Cepheid Calibrations from the Hubble Space Telescope of the Luminosity of Two Recent Type Ia Supernovae and a Redetermination of the Hubble Constant." Astrophysical Journal 627 (2): 579-607. arXiv:astro-ph/0503159. Bibcode 2005ApJ...627..579R. doi: 10.1086/430497.
- ^ NGC 3982. Students for the Exploration and Development of Space. Retrieved March 3, 2009
- ^ R. B. Tully (1988). Nearby Galaxies Catalog. Cambridge: Cambridge University Press. ISBN 0-521-35299-1.
- ^ P. Fouque, E. Gourgoulhon, P. Chamaraux, G. Paturel (1992). "Groups of galaxies within 80 Mpc. II - The catalogue of groups and group members." It is 211-233 Astronomy and Astrophysics Supplement 93. Bibcode 1992A&AS...93..211F.
- ^ G. Giuricin, C. Marinoni, L. Ceriani, A. Pisani (2000). "Nearby Optical Galaxies: Selection of the Sample and Identification of Groups." Astrophysical Journal 543 (1): 178-194. arXiv:astro-ph/0001140. Bibcode 2000ApJ...543..178G. doi: 10.1086/317070.
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