Class IX Right ascension 16 23 35.22 Distance 7.2 kly (2.2 kpc) | Constellation Scorpius Declination –26° 31′ 32.7″ Apparent magnitude (V) +5.9 | |
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Messier 4 or M4 (also designated NGC 6121) is a globular cluster in the constellation of Scorpius. It was discovered by Philippe Loys de Chéseaux in 1745 and catalogued by Charles Messier in 1764. It was the first globular cluster in which individual stars were resolved.
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Visibility
M4 is conspicuous in even the smallest of telescopes as a fuzzy ball of light. It appears about the same size as the Moon in the sky. It is one of the easiest globular clusters to find, being located only 1.3 degrees west of the bright star Antares, with both objects being visible in a wide-field telescope. Modestly sized telescopes will begin to resolve individual stars, of which the brightest in M4 are of apparent magnitude 10.8.
Characteristics
M4 is a rather loosely concentrated cluster of class IX and measures 75 light years across. It features a characteristic "bar" structure across its core, visible to moderate sized telescopes. The structure consists of 11th magnitude stars and is approximately 2.5' long and was first noted by William Herschel in 1783. At least 43 variable stars have been observed within M4.
M4 is approximately 7,200 light years away, the same distance as NGC 6397, making these the two closest globular clusters to the Solar System. It has an estimated age of 12.2 billion years.
In astronomy, the abundance of elements other than hydrogen and helium is called the metallicity, and it is usually denoted by the abundance ratio of iron to hydrogen as compared to the Sun. For this cluster, the measured abundance of iron is equal to:
This value is the logarithm of the ratio of iron to hydrogen relative to the same ratio in the Sun. Thus the cluster has an abundance of iron equal to 8.5% of the iron abundance in the Sun. Based upon the abundance measurements, there is evidence that this cluster hosts two distinct stellar populations. Each of the populations is a group of stars that all formed at about the same time. Thus the cluster may have undergone at least two separate cycles of star formation.
The space velocity components of this cluster are (U, V, W) = (–57 ± 3, –193 ± 22, –8 ± 5) km/s. It is following an orbit through the Milky Way that has a period of (116 ± 3) million years and an eccentricity of 0.80 ± 0.03. During periapsis it comes within (0.6 ± 0.1) kpc from the galactic core, while at apoapsis it travels out to a distance of (5.9 ± 0.3) kpc. The orbital inclination is at an angle of 23° ± 6° from the galactic plane, carrying it as much as (1.5 ± 0.4) kpc above the disk. When passing through the disk, this cluster does so at distances of less than 5 kpc from the galactic nucleus. The cluster undergoes tidal shock during each passage, which can cause the repeated shedding of stars. Thus the cluster may have been much more massive in the past.
Notable stars
Photographs taken with the Hubble Space Telescope in 1995 have revealed white dwarf stars in M4 that are among the oldest known stars in the Milky Way Galaxy at an age of 13 billion years. One such white dwarf has been found to be a binary star with a pulsar companion, PSR B1620-26 and a planet orbiting it with a mass of 2.5 times that of Jupiter.
In 1987 a millisecond pulsar was discovered in M4 with a period of 3.0 milliseconds, or about ten times faster than the Crab Pulsar.
CX-1 Is located in M4. It is known as a possible millisecond pulsar/neutron star binary. It orbits in 6.31 hours.