Goldfield Astronomical Observatory

Name: Messier 30
Brand: Globular Cluster
SKU: M250ASI094M30
Price: 0.81 USD
Availability: InStock

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Messier 30

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Product Details

Object: Messier 30, NGC 7099

Object Type: Globular Cluster

Type: Desktop

Telescope: Takahashi Mewlon250CRS

Camera: ZWO ASI094

Mount: ASA DDM60

Image Size: 7376 x 4928

Resolution: 0.4 arcsec/pixel

Field of View: 0.82º x 0.55º

Total Exposure: 1 Hour

RGB: 12x300s

Messier 30, NGC 7099, is a globular cluster in the southern constellation of Capricornus. It was discovered by the French astronomer Charles Messier in 1764 who described it as a circular nebula without a star. In the New General Catalogue, compiled during the 1880s, it was described as a "remarkable globular, bright, large, slightly oval." This cluster can be easily viewed with a pair of 10×50 binoculars, forming a patch of hazy light some 4 arcminutes wide that is slightly elongated along the east–west axis. With a larger instrument, individual stars can be resolved and the cluster will cover an angle of up to 12 arcminutes across with a compressed core one arcminute wide.

M30 is located at a distance of about 27,100 light-years from Earth and is about 93 light-years across. The estimated age is roughly 12.93 billion years and it has a combined mass of about 160,000 solar masses. The cluster is following a retrograde orbit through the inner galactic halo, suggesting that it was acquired from a satellite galaxy rather than forming within the Milky Way. It is currently located at a distance of about 22.2 kly (6.8 kpc) from the center of the galaxy, compared to an estimated 26 kly (8.0 kpc) for the Sun.

The M30 cluster has passed through a dynamic process called core collapse and now has a concentration of mass at its core of about a million times the Sun's mass per cubic parsec. This makes it one of the highest density regions in the Milky Way galaxy. Stars in such close proximity will experience a high rate of interactions that can create binary star systems, as well as a type of star called a blue straggler that is formed by mass transfer. A process of mass segregation may have caused the central region to gain a greater proportion of higher mass stars, creating a colour gradient with increasing blueness toward the middle of the cluster.