Sculptor dwarf galaxy

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Galaxy
Sculptor dwarf galaxy
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Sculptor elliptical dwarf galaxy, imaged with the MPG / ESO 2.2 m telescope
Sculptor elliptical dwarf galaxy, imaged with the MPG / ESO 2.2 m telescope
AladinLite
Constellation sculptor
Position
equinox :  J2000.0 , epoch : J2000.0
Right ascension 01 h 00 m 09.3 s
declination -33 ° 42 ′ 33 ″
Appearance
Morphological type dE / dSph  
Brightness  (visual) 8.6 likes
Angular expansion 39.8 ′ × 30.9 ′
Physical data
Affiliation Local group  
Redshift (3.67 ± 0.05)  ·  10 −4  
Radial velocity (110 ± 1) km / s  
distance (280,000 ± 20,000) ly /
(86,000 ± 6,000) pc
Absolute brightness (−11.07 ± 0.51) mag
diameter (3200 ± 200) ly
Metallicity [Fe / H] −1.5
history
discovery Harlow Shapley
Discovery date 1937
Catalog names
PGC  3589 • ESO  351-G30 • MCG  -06-03-015 •

The Sculptor dwarf galaxy (also elliptical Sculptor dwarf galaxy or spheroidal Sculptor dwarf galaxy ) is a dwarf galaxy of early morphological type. It is a satellite of the Milky Way and is located in the constellation of the sculptor ( Latin Sculptor ). It was discovered by Harlow Shapley in 1937 . The galaxy is roughly 280,000 light years from our solar system .

The Sculptor dwarf galaxy contains only 4 percent of the carbon or other heavier elements compared to the Milky Way. This makes them comparable to the most pristine galaxies known to us in the universe .

Not to be confused with the Sculptor dwarf galaxy with the irregular Sculptor dwarf galaxy - PGC 621 - in the Sculptor group .


properties

In the year 1999 , the research group found Majewski et al. within the Sculptor dwarf galaxy a splitting into two different star populations with regard to their metallicity . One with a ratio [Fe / H] = −2.3 the other with [Fe / H] = −1.5.
Comparable to many of the other dwarf galaxies of the local group , a stronger concentration towards the center of the galaxy of the younger metal-rich population compared to the older, metal-poorer population was shown.

additional

Web links

Commons : Constellation Sculptor  - Collection of images, videos and audio files

Individual evidence

  1. ↑ a b c d e f g h i NASA / IPAC EXTRAGALACTIC DATABASE
  2. ↑ Karachentsev, ID; Kashibadze, OG: Masses of the local group and of the M81 group estimated from distortions in the local velocity field . In: Astrophysics . 49, No. 1, 2006, pp. 3-18. bibcode : 2006Ap ..... 49 .... 3K . doi : 10.1007 / s10511-006-0002-6 .
  3. ↑ Shapley, H. , (1938) Harvard Bull . 908 .
  4. ^ Shapley H: Two Stellar Systems of a New Kind . In: Nature . 142, No. 3598, 1938, pp. 715-6. bibcode : 1938Natur.142..715S . doi : 10.1038 / 142715b0 .
  5. ↑ Astronomers Detect Dust Around a Primitive Star, Shedding New Light on Universe's Origins Newswise, accessed January 19, 2008.
  6. ^ Sidney van den Bergh : Updated Information on the Local Group . In: The Publications of the Astronomical Society of the Pacific . 112, No. 770, April 2000, pp. 529-536. arxiv : astro-ph / 0001040 . bibcode : 2000PASP..112..529V . doi : 10.1086 / 316548 .