Messier 79

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Messier 79
NGC1904 M79.png
Observation data (J2000 epoch)
Class V[1]
Constellation Lepus
Right ascension 05h 24m 10.59s[2]
Declination −24° 31′ 27.3″[2]
Distance 41 kly (13 kpc)[citation needed]
Apparent magnitude (V) +8.56[2]
Apparent dimensions (V) 8.7'
Physical characteristics
Metallicity  = –1.55[3] dex
Estimated age 11.7 Gyr[3]
Other designations M79, NGC 1904, GCl 10[2]
See also: Globular cluster, List of globular clusters

Messier 79 (also known as M79 or NGC 1904) is a globular cluster in the Lepus constellation. It was discovered by Pierre Méchain in 1780 and is at a distance of about 41,000 light years away from Earth and 60,000 light years away from the Galactic Center.

Like Messier 54 (the other extragalactic globular on Messier's list), it is thought that M79 is not native to the Milky Way galaxy at all, but instead to the putative Canis Major Dwarf Galaxy, which is currently experiencing a very close encounter with the Milky Way. This is, however, a contentious subject as astronomers are still debating the nature of the Canis Major dwarf galaxy itself.[4]

Color-magnitude diagram[edit]

An infrared color-magnitude diagram of Messier 79.

This color-magnitude diagram was made using infrared images of Messier 79 in two bands - J and K. J-band magnitude is plotted along y-axis and color, J-K, is plotted along x-axis. The image was created using Peter Stetson standard for clouded-field photometry, Daophot.[5]

Based on the diagram, it is evident that most of the stars in this cluster are red giants. The elongated branch is Red giant branch. Stars in the upper left sequence extending outwards from the branch and some stars at the very low temperature end are actually foreground stars.

Altogether three regions of HRD are present here: low mass end of the main sequence, complete red giant branch and horizontal branch. In infrared red stars are brighter, that's why red stars are brighter in this diagram making the lower main sequence shallower than usual. On the other hand, the horizontal branch becomes steeper in this diagram due to IR effects (on the HB the blue end is fainter and the red end is brighter).


  1. ^ Shapley, Harlow; Sawyer, Helen B. (August 1927), "A Classification of Globular Clusters", Harvard College Observatory Bulletin (849): 11–14, Bibcode:1927BHarO.849...11S 
  2. ^ a b c d "SIMBAD Astronomical Database". Results for NGC 1904. Retrieved 2006-11-17. 
  3. ^ a b Koleva, M.; et al. (April 2008), "Spectroscopic ages and metallicities of stellar populations: validation of full spectrum fitting", Monthly Notices of the Royal Astronomical Society, 385 (4): 1998–2010, arXiv:0801.0871Freely accessible, Bibcode:2008MNRAS.385.1998K, doi:10.1111/j.1365-2966.2008.12908.x 
  4. ^ López-Corredoira, M.; Momany, Y.; Zaggia, S.; Cabrera-Lavers, A. (2007). "Re-affirming the connection between the Galactic stellar warp and the Canis Major over-density". Astronomy and Astrophysics. 472 (3): l47. arXiv:0707.4440Freely accessible. Bibcode:2007A&A...472L..47L. doi:10.1051/0004-6361:20077813. 
  5. ^ This diagram is made by Astromundus students attending the lectures and workshop of Peter Stetson, the writer of Daophot, standard codes for clouded-filed photometry. Date: June 2011, University of Rome Tor Vergata

External links[edit]

Coordinates: Sky map 05h 24m 10.59s, −24° 31′ 27.3″