Canes Venatici I (dwarf galaxy)

Canes Venatici Dwarf Galaxy[1]
Observation data (J2000 epoch)
Constellation Canes Venatici
Right ascension 13h 28m 03.5s<[1]
Declination +33° 33′ 21″[1]
Distance

711 ± 33 kly (218 ± 10 kpc)
[2]

685+23
−16 kly (210+7
−5 kpc)[3]
Type dSph
Apparent dimensions (V) 17.8 ± 0.8′[4]
Apparent magnitude (V) 13.9 ± 0.5[5]
Other designations
CVn Dwarf Galaxy[1]
See also: Galaxy, List of galaxies

Canes Venatici I or CVn I is a dwarf spheroidal galaxy situated in the Canes Venatici constellation and discovered in 2006 in the data obtained by Sloan Digital Sky Survey.[5] It is one the most distant satellites of the Milky Way as of 2011 together with Leo I and Leo II.[5] The galaxy is located at the distance of about 220 kpc from the Sun and moves away from the Sun with the velocity of about 31 km/s.[6] It is classified as a dwarf spheroidal galaxy (dSph) meaning that it has an elliptical (ratio of axes ~ 2.5:1) shape with the half-light radius of about 550 pc.[5][4]

CVn I is a relatively faint satellite of the Milky Way—its integrated luminosity is about 230,000 times that of the Sun (absolute visible magnitude of about −8.6).[4] However, its mass is about 27 million solar masses, which means that galaxy's mass to light ratio is around 220. A high mass to light ratio implies that CVn I is dominated by the dark matter.[6]

The stellar population of CVn I consists mainly of old stars formed more than 10 billion years ago. The metallicity of these old stars is also very low at [Fe/H] ≈ −2.08 ± 0.02, which means that they contain 110 times less heavy elements than the Sun.[7] There are also about 60 RR Lyrae stars.[3] The galaxy also contains a small fraction of younger (1–2 billion years old) more metal rich ( [Fe/H] ≈ −1.5) stars, which account for about 5% of its mass and 10% of its light. These younger stars are concentrated in the center of the galaxy.[2] There is currently no star formation in CVn I and the measurements have so far failed to detect neutral hydrogen in it—the upper limit is 30,000 solar masses.[8]

References

  1. ^ a b c d "SIMBAD Astronomical Database". Results for Canes Venatici Dwarf. http://simbad.u-strasbg.fr/Simbad. Retrieved 2011-11-21. 
  2. ^ a b Martin, N. F.; Coleman, M. G.; De Jong, J. T. A.; Rix, H. W.; Bell, E. F.; Sand, D. J.; Hill, J. M.; Thompson, D. et al. (2008). "A Deep Large Binocular Telescope View of the Canes Venatici I Dwarf Galaxy". The Astrophysical Journal 672: L13. doi:10.1086/525559.  edit
  3. ^ a b Kuehn, C.; Kinemuchi, K.; Ripepi, V.; Clementini, G.; Dall'Ora, M.; Di Fabrizio, L.; Rodgers, C. T.; Greco, C. et al. (2008). "Variable Stars in the Newly Discovered Milky Way Dwarf Spheroidal Satellite Canes Venatici I". The Astrophysical Journal 674 (2): L81. doi:10.1086/529137.  edit
  4. ^ a b c Martin, N. F.; De Jong, J. T. A.; Rix, H. W. (2008). "A Comprehensive Maximum Likelihood Analysis of the Structural Properties of Faint Milky Way Satellites". The Astrophysical Journal 684 (2): 1075. doi:10.1086/590336.  edit
  5. ^ a b c d Zucker, D. B.; Belokurov, V.; Evans, N. W.; Wilkinson, M. I.; Irwin, M. J.; Sivarani, T.; Hodgkin, S.; Bramich, D. M. et al. (2006). "A New Milky Way Dwarf Satellite in Canes Venatici". The Astrophysical Journal 643 (2): L103. doi:10.1086/505216.  edit
  6. ^ a b Simon, J. D.; Geha, M. (2007). "The Kinematics of the Ultra‐faint Milky Way Satellites: Solving the Missing Satellite Problem". The Astrophysical Journal 670: 313. doi:10.1086/521816.  edit
  7. ^ Kirby, E. N.; Simon, J. D.; Geha, M.; Guhathakurta, P.; Frebel, A. (2008). "Uncovering Extremely Metal-Poor Stars in the Milky Way's Ultrafaint Dwarf Spheroidal Satellite Galaxies". The Astrophysical Journal 685: L43. doi:10.1086/592432.  edit
  8. ^ Grcevich, J.; Putman, M. E. (2009). "H I in Local Group Dwarf Galaxies and Stripping by the Galactic Halo". The Astrophysical Journal 696: 385. doi:10.1088/0004-637X/696/1/385.  edit

External links

Location
Galactic core
Spiral arms
Satellite galaxies
Other

Coordinates: 13h 28m 03.5s, +33° 33′ 21″

References