Van Biesbroeck's star catalog
Encyclopedia
In 1961 the astronomer George Van Biesbroeck
published a catalog of low luminosity stars discovered using the 82 in (2.1 m) Otto Struve refractor telescope
of the McDonald Observatory
in Texas
. This survey is similar to earlier dim star surveys that were done by Max Wolf
and Frank Elmore Ross
but using later equipment and techniques that could detect even fainter stars. The stars in this catalog are all low luminosity stars that appear near known high proper motion
stars in the telescope's field of view. The high proper motion indicates that the stars are close enough to Earth
for a dim star to be seen with a large telescope. Presuming that these high proper motion stars might be binary stars with dim, previously undetected, companions. He took astrophotographs
of the space around these stars looking for low luminosity stars that shared the high proper motions of the primary star. In general, the primary stars were too dim for a direct measurement of their distance by measuring their parallax
at that time.
The stars in this catalog are identified by the designation; VB.
The original list ended at 12 with most identified as gravitationally bound in a binary or multiple star system. He also identified an additional 17 known high proper motion
stars he later found to have low luminosity stars in the field of view of the bright star. Many of these stars were found to be optical double stars, not gravitationally bound to another star, and not known to be part of a binary system.
Most of the stars in this catalog are type K and M
, red dwarf
, stars, some with exceptionally low mass and luminosity. Three of the stars are type DC, white dwarf
, stars.
The star from this catalog that is known to be closest to Earth is VB 10
, at about 19 light years distance.
The original 1961 catalog has been updated for this table using the latest coordinates from SIMBAD
as many of these objects have moved a considerable distance away from their 1961 positions. The original object designations for the primary stars are used but modified to be consistent with SIMBAD
standards where necessary. One primary star was incorrectly identified and two primary stars could not be positively identified from the original catalog.
. These low mass, low luminosity stars close by are uniquely situated for exo-planetary searches using astrometry
or optical methods. The low mass of the star enables observers on Earth
to see a large motion of the star for a given planetary mass. The low luminosity of the stars makes a direct optical or infrared telescopic survey for orbiting objects, such as planets, near the star possible.
A notable member of this group is VB 10
, discovered in 1944. This star was the least massive and dimmest star known at the time of its discovery. Based on a discovery claim made in 2009, VB 10
would have become the first star to have an extrasolar planet detected using astrometry
, however this clam was later refuted.
George Van Biesbroeck
George A. Van Biesbroeck was a Belgian-American astronomer. He worked at observatories in Belgium, Germany and the United States. He specialized in the observation of double stars, asteroids and comets...
published a catalog of low luminosity stars discovered using the 82 in (2.1 m) Otto Struve refractor telescope
Otto Struve Telescope
The Otto Struve Telescope was the first major telescope to be built at McDonald Observatory. Located in the Davis Mountains in West Texas, the Otto Struve Telescope was designed by Warner & Swasey Company and constructed between 1933 and 1939 by the Paterson-Leitch Company. Its 2.1 meter mirror...
of the McDonald Observatory
McDonald Observatory
The McDonald Observatory is an astronomical observatory located near the unincorporated community of Fort Davis in Jeff Davis County, Texas, United States. The facility is located on Mount Fowlkes and Mount Locke in the Davis Mountains of West Texas...
in Texas
Texas
Texas is the second largest U.S. state by both area and population, and the largest state by area in the contiguous United States.The name, based on the Caddo word "Tejas" meaning "friends" or "allies", was applied by the Spanish to the Caddo themselves and to the region of their settlement in...
. This survey is similar to earlier dim star surveys that were done by Max Wolf
Max Wolf
Maximilian Franz Joseph Cornelius Wolf was a German astronomer and a pioneer in the field of astrophotography...
and Frank Elmore Ross
Frank Elmore Ross
Frank Elmore Ross was an American astronomer and physicist. He was born in San Francisco, California and died in Altadena, California. In 1901 he received his doctorate from the University of California. In 1905 he became director of the International Latitude Observatory station at Gaithersburg,...
but using later equipment and techniques that could detect even fainter stars. The stars in this catalog are all low luminosity stars that appear near known high proper motion
Proper motion
The proper motion of a star is its angular change in position over time as seen from the center of mass of the solar system. It is measured in seconds of arc per year, arcsec/yr, where 3600 arcseconds equal one degree. This contrasts with radial velocity, which is the time rate of change in...
stars in the telescope's field of view. The high proper motion indicates that the stars are close enough to Earth
Earth
Earth is the third planet from the Sun, and the densest and fifth-largest of the eight planets in the Solar System. It is also the largest of the Solar System's four terrestrial planets...
for a dim star to be seen with a large telescope. Presuming that these high proper motion stars might be binary stars with dim, previously undetected, companions. He took astrophotographs
Astrophotography
Astrophotography is a specialized type of photography that entails recording images of astronomical objects and large areas of the night sky. The first photographs of an astronomical object were taken in the 1840s, but it was not until the late 19th century that advances in technology allowed for...
of the space around these stars looking for low luminosity stars that shared the high proper motions of the primary star. In general, the primary stars were too dim for a direct measurement of their distance by measuring their parallax
Parallax
Parallax is a displacement or difference in the apparent position of an object viewed along two different lines of sight, and is measured by the angle or semi-angle of inclination between those two lines. The term is derived from the Greek παράλλαξις , meaning "alteration"...
at that time.
The stars in this catalog are identified by the designation; VB.
The original list ended at 12 with most identified as gravitationally bound in a binary or multiple star system. He also identified an additional 17 known high proper motion
Proper motion
The proper motion of a star is its angular change in position over time as seen from the center of mass of the solar system. It is measured in seconds of arc per year, arcsec/yr, where 3600 arcseconds equal one degree. This contrasts with radial velocity, which is the time rate of change in...
stars he later found to have low luminosity stars in the field of view of the bright star. Many of these stars were found to be optical double stars, not gravitationally bound to another star, and not known to be part of a binary system.
Most of the stars in this catalog are type K and M
Stellar classification
In astronomy, stellar classification is a classification of stars based on their spectral characteristics. The spectral class of a star is a designated class of a star describing the ionization of its chromosphere, what atomic excitations are most prominent in the light, giving an objective measure...
, red dwarf
Red dwarf
According to the Hertzsprung-Russell diagram, a red dwarf star is a small and relatively cool star, of the main sequence, either late K or M spectral type....
, stars, some with exceptionally low mass and luminosity. Three of the stars are type DC, white dwarf
White dwarf
A white dwarf, also called a degenerate dwarf, is a small star composed mostly of electron-degenerate matter. They are very dense; a white dwarf's mass is comparable to that of the Sun and its volume is comparable to that of the Earth. Its faint luminosity comes from the emission of stored...
, stars.
The star from this catalog that is known to be closest to Earth is VB 10
VB 10
VB 10, also referred to as Van Biesbroeck's star, is a very small and very dim M-type red dwarf star located in the constellation Aquila...
, at about 19 light years distance.
| Low-luminosity stars discovered | ||||||||
|---|---|---|---|---|---|---|---|---|
| Number | Magnitude Apparent magnitude The apparent magnitude of a celestial body is a measure of its brightness as seen by an observer on Earth, adjusted to the value it would have in the absence of the atmosphere... |
Type Stellar classification In astronomy, stellar classification is a classification of stars based on their spectral characteristics. The spectral class of a star is a designated class of a star describing the ionization of its chromosphere, what atomic excitations are most prominent in the light, giving an objective measure... |
Right Ascension Right ascension Right ascension is the astronomical term for one of the two coordinates of a point on the celestial sphere when using the equatorial coordinate system. The other coordinate is the declination.-Explanation:... |
Declination Declination In astronomy, declination is one of the two coordinates of the equatorial coordinate system, the other being either right ascension or hour angle. Declination in astronomy is comparable to geographic latitude, but projected onto the celestial sphere. Declination is measured in degrees north and... |
Primary Star | Proper Motion Proper motion The proper motion of a star is its angular change in position over time as seen from the center of mass of the solar system. It is measured in seconds of arc per year, arcsec/yr, where 3600 arcseconds equal one degree. This contrasts with radial velocity, which is the time rate of change in... |
Parallax Parallax Parallax is a displacement or difference in the apparent position of an object viewed along two different lines of sight, and is measured by the angle or semi-angle of inclination between those two lines. The term is derived from the Greek παράλλαξις , meaning "alteration"... |
Notes |
| VB 1 | 16.0 | M6V | 05 45 43.22 | -22 20 03.5 | gamma Leporis | -237 -580 | ||
| VB 2 | 14.86 | M | 06 06 30.57 | +04 30 32.7 | Ross 413 | 155 -790 | ||
| VB 3 | 16.59 | DC | 07 45 38.73 | -33 47 50.0 | GC 10473 | -271 1668 | 65.79 | |
| VB 4 | 15 | DC | 11 34 29.74 | -32 49 56.6 | GC 15873 | -591 731 | 104.5 | |
| VB 5 | 15.43 | M4 | 11 46 32.70 | -40 29 47.7 | GC 16149 | -1530 403 | ||
| VB 6 | 16 | 11 58 26.54 | -41 55 06.3 | CD-41 6879 | -643 -367 | |||
| VB 7 | 15.23 | M7V | 14 00 26.62 | +47 39 59.1 | Ross 1027 | -619 -301 | ||
| VB 8 | 16.7 | M6.5V | 16 55 35.29 | -08 23 40.1 | Wolf 629 | -771 -871 | 153.96 | |
| VB 9 | 13.02 | M3.5 | 18 35 27.23 | +45 45 40.3 | LFT 1421 | 460 361 | 63 | |
| VB 10 | 17.30 | M8V | 19 16 57.62 | +05 09 02.2 | Wolf 1055 | -614 -1368 | 164.3 | Primary is incorrectly listed as Wolf 1085. |
| VB 11 | 16.68 | DC | 20 56 47.79 | -04 50 39.8 | Ross 193 | 787.22 -218.69 | 56.56 | |
| VB 12 | 16.96 | sdM3 | 23 17 05.00 | -13 51 04.1 | GC 32412 | -525 -1168 | ||
| VB 13 | 15 | M | 00 55 49.48 | -11 38 03.6 | L 796-10 | 288 -114 | ||
| VB 14 | 14.2 | M1 | 01 52 50.90 | -10 34 13.7 | Ross 555 | 346 123 | ||
| VB 15 | 15 | 5 25 33.79 | -3 29 48.3 | BD -3 3110 | Primary coordinates do not agree. VB 15 is not listed in SIMBAD |
|||
| VB 16 | 13.77 | M4 | 06 49 05.42 | +37 06 53.4 | LFT 487 | 201 -1586 | 72 | |
| VB 17 | 15 | 07 33 11.03 | -42 49 31.3 | LFT 533 | 92 -552 | |||
| VB 18 | 17 | 10 57 14.97 | +41 57 56.5 | Fu 29 | -274 -262 | The primary is unidentified. | ||
| VB 19 | 18 | 11 16 05.66 | +07 57 43.0 | Wolf 373 | 167 -293 | |||
| VB 20 | 10.91 | 11 17 11.716 | +17 29 26.92 | LFT 789 | -304.84 -33.81 | 10.25 | ||
| VB 21 | 14 | 12 03 22.74 | +69 03 54.5 | LFT 880 | -265 44 | |||
| VB 22 | 15.5 | 13 36 59.29 | +07 51 54.5 | Ross 491 | 372 -14 | |||
| VB 23 | 15 | 14 50 38.26 | +07 20 52.3 | LFT 1146 | -202 55 | |||
| VB 24A | 12.48 | M3 | 15 40 03.53 | +43 29 39.7 | 1171 -317 | 74.2 | ||
| VB 24B | 13.80 | M3.5 | 15 40 03.74 | +43 29 35.5 | 1171 -317 | 74.2 | ||
| VB 25 | 14 | 16 45 47.58 | +33 26 34.8 | BD 33 2777 | -146 -366 | |||
| VB 26 | 14.05 | K | 16 55 13.76 | -08 07 58.7 | BD -8 4352 | -243 -664 | ||
| VB 27 | 15 | M | 18 23 17.66 | +72 41 55.6 | chi Draconis | -98 484 | ||
| VB 28 | 15 | 18 41 58.73 | +31 40 17.0 | Ross 145 | -116 -216 | |||
| VB 29 | 13 | M | 21 27 47.51 | +55 05 33.7 | Ross 198 | 492 193 |
The original 1961 catalog has been updated for this table using the latest coordinates from SIMBAD
SIMBAD
SIMBAD is an astronomical database of objects beyond the Solar System...
as many of these objects have moved a considerable distance away from their 1961 positions. The original object designations for the primary stars are used but modified to be consistent with SIMBAD
SIMBAD
SIMBAD is an astronomical database of objects beyond the Solar System...
standards where necessary. One primary star was incorrectly identified and two primary stars could not be positively identified from the original catalog.
Significance
This catalog of stars is significant not only for the intrinsic features of the stars themselves but also for the stars proximity to EarthEarth
Earth is the third planet from the Sun, and the densest and fifth-largest of the eight planets in the Solar System. It is also the largest of the Solar System's four terrestrial planets...
. These low mass, low luminosity stars close by are uniquely situated for exo-planetary searches using astrometry
Astrometry
Astrometry is the branch of astronomy that involves precise measurements of the positions and movements of stars and other celestial bodies. The information obtained by astrometric measurements provides information on the kinematics and physical origin of our Solar System and our Galaxy, the Milky...
or optical methods. The low mass of the star enables observers on Earth
Earth
Earth is the third planet from the Sun, and the densest and fifth-largest of the eight planets in the Solar System. It is also the largest of the Solar System's four terrestrial planets...
to see a large motion of the star for a given planetary mass. The low luminosity of the stars makes a direct optical or infrared telescopic survey for orbiting objects, such as planets, near the star possible.
A notable member of this group is VB 10
VB 10
VB 10, also referred to as Van Biesbroeck's star, is a very small and very dim M-type red dwarf star located in the constellation Aquila...
, discovered in 1944. This star was the least massive and dimmest star known at the time of its discovery. Based on a discovery claim made in 2009, VB 10
VB 10
VB 10, also referred to as Van Biesbroeck's star, is a very small and very dim M-type red dwarf star located in the constellation Aquila...
would have become the first star to have an extrasolar planet detected using astrometry
Astrometry
Astrometry is the branch of astronomy that involves precise measurements of the positions and movements of stars and other celestial bodies. The information obtained by astrometric measurements provides information on the kinematics and physical origin of our Solar System and our Galaxy, the Milky...
, however this clam was later refuted.