Messier 53

Messier 53
Globular cluster Messier 53 in Coma Berenices
Observation data (J2000 epoch)
ClassV[1]
ConstellationComa Berenices
Right ascension13h 12m 55.25s[2]
Declination+18° 10′ 05.4″[2]
Distance58×10^3 ly (18 kpc)[3]
Apparent magnitude (V)7.6[4]
Apparent dimensions (V)13.0′[4]
Physical characteristics
Mass8.26×105[5] M☉
Metallicity = –1.86[6] dex
Estimated age12.67 Gyr[6]
Other designationsM53, NGC 5024, GCl 22, C 1310+184[7]
See also: Globular cluster, List of globular clusters

Messier 53 (also known as M53 or NGC 5024) is a globular cluster in the Coma Berenices constellation.[a] It was discovered by Johann Elert Bode in 1775. M53 is one of the more outlying globular clusters, being about 60,000 light-years (18.4 kpc) light-years away from the Galactic Center, and almost the same distance (about 58,000 light-years (17.9 kpc)) from the Solar System. The cluster has a core radius (rc) of 2.18 pc, a half-light radius (rh) of 5.84 pc, and a tidal radius (rtr) of 239.9 pc.[8]

This is considered a metal-poor cluster and at one time was thought to be the most metal-poor cluster in the Milky Way.[8] Abundance measurements of cluster members on the red giant branch show that most are first-generation stars. That is, they did not form from gas recycled from previous generations of stars. This differs from the majority of globular clusters that are more dominated by second generation stars. The second generation stars in NGC 5024 tend to be more concentrated in the core region. Overall, the stellar composition of cluster members is similar to members of the Milky Way halo.[9]

The cluster displays various tidal-like features including clumps and ripples around the cluster, and tails along the cluster's orbit in an east–west direction. A tidal bridge-like structure appears to connect M53 with the close, very diffuse neighbor NGC 5053, as well as an envelope surrounding both clusters. These may indicate a dynamic tidal interaction has occurred between the two clusters; a possibly unique occurrence within the Milky Way since there are no known binary clusters within the galaxy.[10] In addition, M53 is a candidate member of the Sagittarius dwarf galaxy tidal stream.[8]

Among the variable star population in the cluster, there are 55 known to be RR Lyrae variables. Of these, a majority of 34 display behavior typical of the Blazhko effect, including 23 of type RRc – the largest known population of the latter in any globular cluster.[11] There are also at least three variables of type SX Phe and a semi-regular red giant.[12]

  1. ^ Cite error: The named reference hcob849_11 was invoked but never defined (see the help page).
  2. ^ a b Cite error: The named reference aj140_6_1830 was invoked but never defined (see the help page).
  3. ^ Cite error: The named reference apj670_1_363 was invoked but never defined (see the help page).
  4. ^ a b "Messier 53". SEDS Messier Catalog. Retrieved 29 April 2022.
  5. ^ Cite error: The named reference apj742_1_51 was invoked but never defined (see the help page).
  6. ^ a b Cite error: The named reference mnras404_3_1203 was invoked but never defined (see the help page).
  7. ^ Cite error: The named reference simbad was invoked but never defined (see the help page).
  8. ^ a b c Cite error: The named reference Bomberg2015 was invoked but never defined (see the help page).
  9. ^ Cite error: The named reference Boberg2016 was invoked but never defined (see the help page).
  10. ^ Cite error: The named reference Chun2010 was invoked but never defined (see the help page).
  11. ^ Cite error: The named reference ArellanoFerro2012 was invoked but never defined (see the help page).
  12. ^ Cite error: The named reference Bramich2012 was invoked but never defined (see the help page).


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