Messier 20 (M20), also known as the Trifid Nebula, is a famous star-forming region located in the constellation Sagittarius. The nebula’s designation in the New General Catalogue is NGC 6514. The name Trifid refers to its three-lobed appearance. Messier 20 consists of several different objects: an emission nebula, a reflection nebula, a dark nebula and an open star cluster.
The dark nebula, catalogued as Barnard 85, consists of dust clouds that absorb and block light from the bright objects behind them. It is responsible for the apparent gaps in the larger emission nebula that give M20 its trifurcated look. The other two types of nebulae – emission and reflection – make M20 glow in different colours in images.
Emission nebulae are energised by the ultraviolet light of nearby stars and usually appear red in photographs. These nebulae are clouds of extremely hot hydrogen gas and usually regions where new stars are being formed. The light of the stars illuminates the surrounding clouds, ionizing photons in large portions of the clouds.
Reflection nebulae, which typically appear blue in images, consist mostly of clouds of interstellar dust. They are also usually star-forming regions, but unlike emission nebulae, which emit spectral line radiation from ionized hydrogen, reflection nebulae do not emit any light of their own, but simply reflect the light of nearby stars.
Messier 20 is a popular target for amateur astronomers as it is quite bright, even when seen through a small telescope. It has an apparent magnitude of 6.3 and lies at an approximate distance of 5,200 light years, or 1,600 parsecs, from Earth. M20 has a linear diameter of over 40 light years and is only 300,000 years old.
The Trifid Nebula can be found about 2 degrees to the northwest of the larger and brighter Lagoon Nebula (Messier 8) and appears in the same field of view as the open cluster Messier 21. M20 can be located in the same way as the Lagoon, using the Teapot asterism in Sagittarius. It lies a few degrees to the west of Lambda Sagittarii, the star at the top of the Teapot. The larger Lagoon Nebula is visible to the naked eye on clear, moonless nights and the Trifid appears as a hazy patch of light only 2 degrees away.
The open cluster at the centre of M20 is catalogued as C 1759-230. The cluster is surrounded by the red emission nebula which, in turn, is surrounded by the blue reflection nebula. The reflection nebula is particularly prominent in the northern part of M20.
Messier 20 was famously photographed by the Hubble Space Telescope in 1997. The images revealed a dense cloud of gas and dust in the process of forming new stars. Many embryonic stars were found within the cloud, which lies roughly 8 light years from M20’s central star. The stellar jet protruding from the stellar nursery stretches across 0.75 light years. It is the radiation from the central star that makes the jet glow.
An evaporating gas globule (EGG) was found in the vicinity of the jet. EGGs are knots of hydrogen gas, finger-like in shape and dense enough to prevent the star’s radiation from eroding the dust and gas in its path.
Images taken by NASA’s Spitzer Space Telescope, an infrared space observatory, in January 2005 revealed 30 embryonic stars and 120 newly formed stars that had not been seen in visible light images of M20. Some of the stars found within the Trifid Nebula are only a few hundred thousand years old, possibly making the open cluster in M20 one of the youngest open clusters known. Some of the extremely young and massive stars that formed in the region may have already ended their lives in supernova explosions. These supernova events may be responsible for the appearance of the dust lanes in M20.
These embryos are indicated with arrows in the false-color Spitzer picture (right), taken by the telescope’s infrared array camera. The same embryos cannot be seen in the visible-light pictures (left). Spitzer found clusters of embryos in two of the cores and only single embryos in the other two. This is one of the first times that multiple embryos have been observed in individual cores at this early stage of stellar development. Image: NASA/JPL-Caltech/J. Rho (SSC/Caltech)
The brightest star in the Trifid Nebula, designated HD 196692 (ADS 10991), is a triple star system composed of three extremely hot stars located on the west side of the open cluster. The three components have apparent magnitudes of 7.6, 10.7 and 8.7. The brightest of the three stars has a spectral type of O5 to O7. The system may contain additional, fainter components.
Another extremely luminous star is found on the northern edge of the cluster. Designated HD 164514, the star is a white supergiant with the stellar classification A5 Ia. It has a visual magnitude of 7.42.
A survey with the European Southern Observatory’s (ESO) VISTA telescope in 2015 revealed two entirely new categories of Cepheid variables stars, the first stars of this kind to be found in the centre of our galaxy. These stars exhibit variations in size and temperature and, as a result, their brightness changes over a period of about 11 days. The Cepheids only appear to be just behind M20, but are really located some 37,000 light years away, on the other side of the Milky Way.
Messier 20 is difficult to see from locations too far to the north. The best time of year to observe it is in the summer months, when Sagittarius rises over the southern horizon in the evening. The nebula’s features can only be seen in large telescopes and the object itself doesn’t appear particularly notable in visible light.
Charles Messier discovered the nebula on June 5, 1764 and described it as a “cluster of stars, a little above the Ecliptic, between the bow of Sagittarius & the right foot of Ophiuchus.”
William Herschel observed M20 on July 12, 1784 and noted that “three nebulae, faintly joined, form a triangle. In the middle is a double st[ar], vF [very faint], and of great extent.” When Herschel catalogued M20, he assigned the object four different numbers: H IV.41 (added on May 26, 1786) and H V.10, H V.11 and H V.12 (added on July 12, 1784.)
John Herschel viewed the object on July 1, 1826 and was the first to call it Trifid. He noted, “vL [very large]; trifid, three nebulae with a vacuity in the midst, in which is centrally situated the double star Sh 379, neb == 7′ in extent. A most remarkable object.”
Edward Emerson Barnard catalogued the dark nebula in M20 as Barnard 85 (B 85). B 85 appeared on the list of Barnard objects in the first Barnard Catalogue of Dark Markings in the Sky, published in 1919.
Astronomers can actually count the individual embryos tucked inside the cores by looking closely at the Spitzer image taken by its infrared array camera (top right). This instrument has the highest spatial resolution of Spitzer’s imaging cameras. The Spitzer image from the multiband imaging photometer (bottom right), on the other hand, specializes in detecting cooler materials. Its view highlights the relatively cool core material falling onto the Trifid’s growing embryos. The middle panel is a combination of Spitzer data from both of these instruments.
The embryos are thought to have been triggered by a massive “type O” star, which can be seen as a white spot at the center of the nebula in all four images. Type O stars are the most massive stars, ending their brief lives in explosive supernovas. The small newborn stars probably arose at the same time as the O star, and from the same original cloud of gas and dust. Image: NASA/JPL-Caltech/J. Rho (SSC/Caltech)
FACTS
| Object: Nebula with an open cluster |
| Type: Emission, reflection, dark |
| Designations: Messier 20, M20, Trifid Nebula, NGC 6514, Sharpless 30, RCW 147, Gum 76, C 1759-230, Collinder 360, LBN 27, MWSC 2789, OCl 23.0 |
| Constellation: Sagittarius |
| Right ascension: 18h 02m 23s |
| Declination: -23°01’48” |
| Distance: 5,200 light years (1,600 parsecs) |
| Age: 300,000 years |
| Apparent magnitude: +6.3 |
| Apparent dimensions: 28′ |
| Radius: 21 light years |
LOCATION
