1130 I/130 LDS Catalogue: Doubles with Common Proper Motion W J Luyten Publ. Astr. Obs. Univ. Minnesota III, part 3 35 1969 1969PMMin..21....1L W J Luyten Publ. Astr. Obs. Univ. Minnesota III, part 3 35 1970 1970PMMin..25....1L W J Luyten Publ. Astr. Obs. Univ. Minnesota III, part 3 35 1972 1972PMMin..29....1L W J Luyten Publ. Astr. Obs. Univ. Minnesota III, part 3 35 1975 1975PMMin..40....1L W J Luyten Publ. Astr. Obs. Univ. Minnesota III, part 3 35 1977 1977PMMin..50....1L W J Luyten Publ. Astr. Obs. Univ. Minnesota III, part 3 35 1980 1980PMMin..55....1L W J Luyten Publ. Astr. Obs. Univ. Minnesota III, part 3 35 1983 1983PMMin..64....1L W J Luyten Publ. Astr. Obs. Univ. Minnesota III, part 3 35 1987 1987PMMin..71....1L Proper motions Stars, double and multiple This catalogue contains all double stars with common proper motion discovered by Luyten since 1940 up to 1987 (references below). When Luyten had noticed that an entry was duplicated (ref. 8 and 9), only the former LDS number was kept in the data file but with the data given for the latter. The unique exception is LDS 6166, which is a duplicate of LDS 5662, but with an additional component. The systems classified as optical by Luyten were also rejected from the main data files. All the rejected data were put together in a separate file. All coordinates are for the equinox 1950; when the original publication gave another equinox (this is the case for ref. 1), the 1950-coordinates were calculated. The catalogue contains all the systems, sorted by increasing LDS numbers. Duplicate entries and optical systems listed by Luyten were rejected. The catalogue contains 6121 systems, including 87 triple and 1 quadruple systems. The number of records is thus 6210, since each triple system occupies 2 records and the quadruple system 3.

LDS LDS number number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. --- Mult 't' indicates a system is triple and 'q' it is quadruple. Then, the LDS number is the same for all entries. number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. --- RAh Right Ascension 1950 (hours) number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. h RAm Right Ascension 1950 (minutes) number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. min RAs Right Ascension 1950 (seconds) number=1 When the seconds are provided, the RAm fractional part is blank s DE- Declination 1950 (sign) number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. --- DEd Declination 1950 (degrees) number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. deg DEm Declination 1950 (minutes) number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. arcmin mR1 Photographic R magnitude of the primary component (99.9 = unknown) number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. mag u_mR1 Uncertainty flag on mR1 number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. --- mB1 Photographic magnitude of the primary component (99.9 = unknown) number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. mag u_mB1 Uncertainty flag on mB1 number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. --- color1 Color class of the primary component number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. --- mR2 photographic R magnitude of the secondary component (99.9 = unknown) number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. mag u_mR2 Uncertainty flag on mR2 number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. --- mB2 photographic magnitude of the secondary component (99.9 = unknown) number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. mag u_mB2 Uncertainty flag on mB2 number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. --- color2 Color class of the secondary component number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. --- pm Annual proper motion, number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. arcsec/a pmPA Direction (N to E) of the proper motion number=2 LDS 3543 has a value of 403deg (outside standard limits) deg Theta Position angle, see also Quadrant number=4 Theta, sep and Quadrant blank for LDS 149. LDS 1170 has a value of 440deg (outside standard limits) deg Sep Separation between components number=4 Theta, sep and Quadrant blank for LDS 149. LDS 1170 has a value of 440deg (outside standard limits) arcsec Quadrant Quadrant designation for ref.1 number=4 Theta, sep and Quadrant blank for LDS 149. LDS 1170 has a value of 440deg (outside standard limits) --- Remark Short remark and/or other identification number=3 the reasons for rejection are in bytes 81-91 in file "reject". A '*' refers to a remark (see 'Individual Remarks' below) The {Lambda} identifications given in ref.1 were not keypunched. --- Ref Reference code (see References section) number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. --- J.-L. Halbwachs, F. Ochsenbein CDS 1997Feb04 UNKNOWN UNKNOWN Keypunched at CDS in 1987 * 15-Jun-1994: Corrected a few errors (existing in the publication) LDS 3593: third decimal place of proper motion (pm) set to blank LDS 4309: "+" embedded in DEm LDS 4871: RAm was -1 LDS 5644: secondary magnitudes were 18.,0 19.1 LDS 5679: third decimal place of proper motion (pm) set to blank LDS 5999: third decimal place of proper motion (pm) set to blank * 04-Feb-1997: ReadMe file standardized, and disentangled Quadrant from Theta values in data files * 19-Sep-1997: a few bad magnitude values (above 90.0) corrected in both main and rejected files. I_130.xml