Andromeda II

Andromeda II
Observation data (J2000 epoch)
Constellation Andromeda
Right ascension 01h 16m 29.8s[1]
Declination +33° 25′ 09″[1]
Redshift -188 ± 3 km/s[1]
Distance 2.22 ± 0.07 Mly (680 ± 20 kpc)[2][3]
Type dSph[1]
Apparent dimensions (V) 3′.6 × 2′.52[1]
Apparent magnitude (V) 13.5[1]
Notable features satellite galaxy of M31
Other designations

Andromeda II Dwarf Spheroidal,[1]

PGC 4601,[1][4] And II[5]
See also: Galaxy, List of galaxies

Andromeda II (And II) is a dwarf spheroidal galaxy about 2.22 Mly away in the constellation Andromeda. It is part of the Local group of galaxies and is a satellite galaxy of the Andromeda Galaxy (M31) but it's also situated closely to the Triangulum Galaxy (M33), it is not quite clear if it is a satellite of the one or the other galaxy.

It was discovered by Sidney Van den Bergh[6] in a survey of photographic plates taken with the Palomar 48-inch (1.2 m) Schmidt telescope in 1970 and 1971, together with Andromeda I, Andromeda III, and the presumable non- or background galaxy Andromeda IV (Van den Bergh 1972).[7]

Contents

Spectra observations

Using the Keck telescope Côté et al. 1999 observed spectra for seven stars inside Andromeda II. From this data, they found an average velocity Vr of -188 ± 3 km/s and velocity dispersion of 9.2 ± 2.6 km/s. This gives a mass to light ratio of M/Lv of +21
−14 solar units which implies that And II contains a significant amount of dark matter. Also in 1999, Côté, Oke, & Cohen used the Keck to measure the spectra of 42 red giants. From this, they deduced an average metallicity of <[Fe/H]> = -1.47 ± 0.19 and a dispersion of 0.35 ± 0.10 dex.[5]

In 1999, Da Costa et al. studied the color-magnitude diagram of And II and discovered that most of stars in And II have ages between 6 and 9 Gyr. However, the observation of RR Lyrae variables and blue horizontal-branch stars demonstrates the existence of a population segment with an age greater than 10 Gyr. And II differs from And I in that it does not show a radial gradient in horizontal-branch morphology. Additionally, the dispersion in abundance is significantly larger in And II as compared to And I. This implies that these two dwarf spheroidal companions to the Andromeda galaxy have very different evolutionary histories. This raises the question of whether there is a correlation between a radial horizontal-branch gradient and the metallicity dispersion between dwarf spheroidal galaxies.[5]

See also

External links

References

  1. ^ a b c d e f g h "NASA/IPAC Extragalactic Database". Results for Andromeda II. http://nedwww.ipac.caltech.edu/. Retrieved 2006-11-29. 
  2. ^ I. D. Karachentsev, V. E. Karachentseva, W. K. Hutchmeier, D. I. Makarov (2004). "A Catalog of Neighboring Galaxies". Astronomical Journal 127 (4): 2031–2068. Bibcode 2004AJ....127.2031K. doi:10.1086/382905. 
  3. ^ Karachentsev, I. D.; Kashibadze, O. G. (2006). "Masses of the local group and of the M81 group estimated from distortions in the local velocity field". Astrophysics 49 (1): 3–18. Bibcode 2006Ap.....49....3K. doi:10.1007/s10511-006-0002-6. 
  4. ^ "SIMBAD Astronomical Database". Results for Andromeda II. http://simbad.u-strasbg.fr/Simbad. Retrieved 2006-11-29. 
  5. ^ a b c Van den Bergh, Sidney (April 2000). "Updated Information on the Local Group". The Publications of the Astronomical Society of the Pacific 112 (770): 533. arXiv:astro-ph/0001040. Bibcode 2000PASP..112..529V. doi:10.1086/316548 
  6. ^ McConnachie, A. W.; Irwin, M. J.; Ferguson, A. M. N.; Ibata, R. A.; Lewis, G. F.; Tanvir, N. (2005). "Distances and metallicities for 17 Local Group galaxies". Monthly Notices of the Royal Astronomical Society 356 (4): 979–997. arXiv:astro-ph/0410489. Bibcode 2005MNRAS.356..979M. doi:10.1111/j.1365-2966.2004.08514.x. 
  7. ^ Van den Bergh, Sydney (January 1972). "Search for Faint Companions to M31". Astrophysical Journal 171: L31. Bibcode 1972ApJ...171L..31V. doi:10.1086/180861 

Coordinates: 01h 16m 29.8s, +33° 25′ 09″