Lacerta was created by the Polish astronomer Johannes Hevelius in 1687. It is a small, faint constellation that is sometimes referred to as Little Cassiopeia because its brightest stars form a “W” shape, just like the stars in the considerably larger Cassiopeia constellation.
The brightest stars in Lacerta are only of fourth magnitude and none of them have proper names. There are no myths associated with the constellation.
FACTS, LOCATION & MAPLacerta is the 68th constellation in size, occupying an area of 201 square degrees.
It is located in the fourth quadrant of the northern hemisphere (NQ4) and can be seen at latitudes between +90° and -40°.
Lacerta has one star with known planets and contains no Messier objects. The brightest star in the constellation is Alpha Lacertae, with an apparent magnitude of 3.76. There are no meteor showers associated with the constellation.
The name Lacerta does not come from mythology. Johannes Hevelius introduced the constellation in Firmamentum Sobiescianum, his star atlas published in 1690.
He gave the constellation an alternative name, Stellio, after a type of lizard known as a starred agama, but this name was not used much and soon fell into oblivion.
MAJOR STARS IN LACERTA
α Lacertae (Alpha Lacertae)
Alpha Lacertae is a main sequence star with the stellar classification A1 V. It has an apparent visual magnitude of 3.777 and is about 102 light years distant from the solar system. It is the brightest star in the constellation.
Alpha Lacertae has a visual, line-of-sight companion with an apparent magnitude of 11.8, belonging to the spectral class A. The companion, CCDM J22313+5017B, is located about 36 arc seconds away from Alpha Lacertae.
β Lacertae (Beta Lacertae)
Beta Lacertae is only the fourth brightest star in the constellation. It has a visual magnitude of 4.43 and is approximately 170 light years distant fom the Sun.
Beta Lacertae is a giant star with the stellar classification G8.5IIIb.EV Lacertae
EV Lacertae is a red dwarf only 16.5 light years from Earth.
It has an apparent magnitude of 10.09 and is not easily seen in binoculars.
The star belongs to the spectral class M3.5 and is classified as a flare star that emits X-rays.
It is a fast spinner and, as a result, it has a very strong magnetic field, which in turn plays a part in the star’s ability to produce very bright flares.
The brightest flare from the star was recorded by NASA in April 2008. It was thousands of times more powerful than the largest recorded flare coming from the Sun.
Roe 47 is a star system consisting of five components with apparent visual magnitudes of 5.8, 9.8, 10.1, 9.4, and 9.8.
ADS 16402 is a double star with a confirmed extrasolar planet in its orbit.
The planet, named HAT P-1b, orbits the secondary star (HAT P-1) in the ADS 16402 system.
The planet is similar to Jupiter in size and exhibits an extremely low density.
The binary system ADS 16402 consists of two stars similar to the Sun, approximately 450 light years distant. They have apparent visual magnitudes of 10.0 and 10.4, and stellar classifications F8/G0V. The system is believed to be about 3.6 billion years old.
DEEP SKY OBJECTS IN LACERTA
NGC 7243 (Caldwell 16)
NGC 7243 is an open star cluster in Lacerta. It has an apparent visual magnitude of 6.4 and is approximately 2,800 light years distant from the solar system. It lies in the vicinity of Alpha Lacertae. The cluster has an estimated age of just over a billion years. Most of the stars in it are white and blue in colour.
BL Lacertae is a core of a galaxy, originally thought to be a star, which is why it still has a variable star designation. It is a highly variable extragalactic AGN (active galactic nucleus).
BL Lacertae was first discovered by the German astronomer Cuno Hoffmeister in 1929. In 1968, John Schmitt at the David Dunlap University identified the object as a bright, variable radio source.
Today, an entire group of celestial objects are called the BL Lacertae objects, referring to a subtype of blazar.