The star cluster is situated in the highly crowded area of Milky Way near Gamma Cygni, at a distance of 7,200 (most sources including Mallas/Kreimer and Burnham, and agreeing with early estimates or R.J. Trumpler 1930) or 4,000 light years (the latter from Kenneth Glyn Jones and the Sky Catalogue 2000.0). The Night Sky Observer's Guide by Kepple and Sanner gives a deviating value of 6,000 light years – the uncertainty due to poorly known absorption of the cluster's light.
According to the Sky Catalog 2000, Messier 29 is included in the Cygnus OB1 association, and is approaching us at 28 km/s. Its age is estimated at 10 million years, as its five hottest stars are all giants of spectral class B0. The Night Sky Observer's Guide gives the apparent brightness of the brightest star as 8.59 visual magnitudes. The absolute magnitude may be an impressive -8.2 mag, or a luminosity of 160,000 Suns. The linear diameter was estimated at only 11 light years. Its Trumpler class is III,3,p,n (as it is associated with nebulosity), although Götz gives, differently, II,3,m, and Kepple/Sanner gives I,2,m,n. The Sky Catalogue 2000.0 lists it with 50 member stars; earlier Becvar gave only the number of 20 members.
This cluster can be seen in binoculars. In telescopes, lowest powers are best. The brightest stars of Messier 29 form a "stubby dipper", as Mallas says it. The four brightest stars form a quadrilateral, and another three, a triangle north of them. It is often known as the "cooling tower" due to its resemblance to the hyperboloid-shaped structures. A few fainter stars are around them, but the cluster appears quite isolated, especially in smaller telescopes. In photographs, a large number of very faint Milky Way background stars shows up.
Messier 29 can be found quite easily as it is about 1.7 degrees south and little east of Gamma or 37 Cygni (Sadr). In the vicinity of Messier 29, there is some diffuse nebulosity which can be detected in photographs.
The open cluster Messier 29
|Observation data (J2000 epoch)|
|Right ascension||20h 23m 56s|
|Declination||+38° 31′ 24″|
|Distance||3,740 ly (1,148 pc)|
|Apparent magnitude (V)||6.6|
|Apparent dimensions (V)||7.0′|
|Estimated age||13.2 Myr|
|Other designations||M29, NGC 6913, OCl 168|
Gliese 806 is a red dwarf star in the constellation of Cygnus, located roughly 41 light years from the Sun. The star is suspected to host a substellar companion yet unconfirmed.HD 185435
HD 185435 is a star in the constellation Cygnus. Its apparent magnitude is 6.42.HD 189276
HD 189276 is a star in the constellation Cygnus. Its apparent magnitude is 4.96.HD 197036
HD 197036 is a 7th magnitude star in the constellation Cygnus, approximately 2000 light years away from Earth. It is a bluish white subgiant star of the spectral type B5IV, meaning it possesses a surface temperature of 11,000 to 25,000 kelvins. It is therefore hotter, larger, and brighter than our Sun. It can be found within one degree of the star Deneb.HD 203857
HD 203857 is a late type K giant star in the constellation Cygnus, located nearly 920 light years away from the Sun. The star is thought to form a visual binary system with the F-type bright giant BDS 10966 A, though it's likely they are actually not gravitationally bound. The star likely hosts an extrasolar planet, though yet unconfirmed.KOI-74
KOI-74 (KIC 6889235) is an eclipsing binary star in the constellation of Cygnus. The primary star is an A-type main-sequence star with a temperature of 9,400 K (9,130 °C; 16,460 °F). It lies in the field of view of the Kepler Mission and was determined to have a companion object in orbit around it which is smaller and hotter than the main star.Kepler-15
Kepler-15 is a star that is host to the planet Kepler-15b. It is a G-type main sequence star with a mass of 1.018 M☉. It is also known as KOI-128, or KIC 11359879.Kepler-17
Kepler-17 is main-sequence yellow dwarf star. This star is known to host one exoplanet, Kepler-17b, in orbit around it.Kepler-18
Kepler-18 is a star with almost the same mass as the Sun in the Cygnus constellation with 3 confirmed planets, announced in 2011.Kepler-35
Kepler-35 is a binary star system in the constellation of Cygnus. These stars, called Kepler-35A and Kepler-35B have masses of 89% and 81% solar masses respectively, therefore both are spectral class G. They are separated by 0.176 AU, and complete an eccentric orbit around a common center of mass every 20.73 days.Kepler-36
Kepler-36 is a star in the constellation of Cygnus with two known planets. It has an anomalously large radius, meaning that it is a subgiant.Kepler-43
Kepler-43,formerly known as KOI-135, is a star in the northern constellation of Cygnus. It is located at the celestial coordinates: Right Ascension 19h 00m 57.8034s, Declination +46° 40′ 05.665″. With an apparent visual magnitude of 13.996, this star is too faint to be seen with the naked eye.Kepler-44
Kepler-44,formerly known as KOI-204, is a star in the northern constellation of Cygnus. It is located at the celestial coordinates: Right Ascension 20h 00m 24.564s, Declination +45° 45′ 43.71″. With an apparent visual magnitude of 16, this star is too faint to be seen with the naked eye.Kepler-66
Kepler-66 is a star with slightly more mass than the Sun in the NGC 6811 open cluster in the Cygnus constellation. It has one confirmed planet, slightly smaller than Neptune, announced in 2013.Kepler-67
Kepler-67 is a star with slightly less mass than the Sun in the NGC 6811 open cluster in the Cygnus constellation and has one confirmed planet, slightly smaller than Neptune, announced in 2013.V1057 Cygni
V1057 Cygni (V1057 Cyg) is a FU Orionis-type variable star in the constellation of Cygnus. It has a spectral type of F and an apparent visual magnitude of approximately 11.660. It was the second FU Orionis-type variable discovered.V1668 Cygni
V1668 Cygni was a nova that appeared in the constellation Cygnus in 1978 with a maximum brightness of 6th apparent magnitude.V1974 Cygni
V1974 Cygni or Nova Cygni 1992 was a relatively bright nova in the constellation Cygnus.
It was discovered on February 19, 1992, by Peter Collins. At that time it was magnitude 6, the maximum magnitude reached was 4.4. The hydrogen burning on the white dwarf ended two years later, in 1994. This nova was a neon nova. It is the first nova observed from onset to completion, and can be calculated to be 10,430 light years away from Earth.
It was also studied with the Hubble Space Telescope instrument the High Speed Photometer. The instrument recorded a short amount of ultraviolet photometry. The nova was also observed in the far-ultraviolet by Voyager 2.V476 Cygni
V476 Cygni or Nova Cygni 1920 was a nova which occurred in the constellation Cygnus in 1920. It reached a brightness of 2.0 mag. Nowadays its brightness is 17.09 mag.