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J/A+A/353/958   New proper motions in 0<RA<7h, -63<DE←32°  (Scholz+, 2000)

New high-proper motion survey in the Southern sky Scholz R.-D., Irwin M., Ibata R., Jahreiss H., Malkov O.Yu. <Astron. Astrophys. 353, 958 (2000)> =2000A&A...353..958S
ADC_Keywords: Proper motions ; Stars, high-velocity ; Magnitudes Keywords: astrometry - stars: kinematics - stars: low-mass, brown dwarfs - stars: white dwarfs Abstract: We present the discovery of about 100 new high-proper motion stars in the region between 0h and 7h in right ascension and -63° and -32° in declination, with proper motions between 0.3 and 1.0arcsec/yr. In addition we have obtained improved coordinates and photographic photometry for another about 100 already known high-proper motion stars in the same region. In this study we have made use of APM measurements of UKST survey plates in 40 survey fields. Using all available information (position, proper motion, photographic R magnitude and BJ-R colour index), we draw some preliminary conclusions on the nature of the new high-proper motion stars, particularly of extreme cases. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file catalog.dat 135 204 Catalogue of high-proper motion stars
See also: I/98 : NLTT Catalogue (Luyten, 1979) I/87 : LHS Catalogue, 2nd Edition (Luyten 1979) J/A+AS/78/231 : New proper-motion stars DE←40, 0<RA<4h30 (Wroblewski+ 1989) J/A+AS/91/129 : New proper-motion stars DE←40, 4h30<RA<16h (Wroblewski+ 1991) J/A+AS/105/179 : New proper-motion stars DE←40, 16<RA<24h (Wroblewski+ 1994) J/A+AS/115/481 : New proper-motion stars -30<DE←5, 0<RA<9h (Wroblewski+ 1996) J/A+AS/122/447 : New proper-motion stars -30<DE←5, 9<RA<13h30m (Wroblewski+ Byte-by-byte Description of file: catalog.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq [1/204] Running number 5- 7 I3 --- oNum Original detection number (apm...) 9- 17 A9 --- APMPM APMPM Jxxxx-xxxx name corresponding to the J2000 coordinates 18 A1 --- m_APMPM Multiplicity index in APMPM for components of common proper motion stars 20- 30 A11 --- NLTT Name as given in Luyten's NLTT (Cat. <I/98>) catalogue or the Luyten ESO survey (Luyten & Hughes (1985)) (1) 35- 38 I4 --- LHS ? LHS (Cat. I/87) number 41- 43 I3 --- WT ? Number in Wroblewski & Torres catalogues (1) 45- 46 I2 h RAh Right ascension (J2000, epoch of UKST R plate) 48- 49 I2 min RAm Right ascension (J2000, epoch of UKST R plate) 51- 55 F5.2 s RAs Right ascension (J2000, epoch of UKST R plate) 57 A1 --- DE- Declination sign (J2000) 58- 59 I2 deg DEd Declination (J2000, epoch of UKST R plate) 61- 62 I2 arcmin DEm Declination (J2000, epoch of UKST R plate) 64- 67 F4.1 arcsec DEs Declination (J2000, epoch of UKST R plate) 69- 71 I3 ---- UKST UKST survey field number 73- 79 F7.2 yr Epoch Epoch of reference plate (= UKST R plate) 81- 85 F5.2 yr Depoch Epoch difference between UKST B_J and R plates 87- 91 F5.2 arcsec/yr pmX Proper motion component muα*cosδ 93- 97 F5.2 arcsec/yr pmY Proper motion component muδ 99-103 F5.2 mag Rmag R magnitude 105-109 F5.2 mag B-R BJ-R colour index 111 I1 --- Mult [1/2]? Flag for multiple detections (2) 113 I1 --- Qual [1/2]? flag for poor photometric quality (3) 115-134 A20 --- SpClass Rough and preliminary spectral classification from SAAO spectra (4)
Note (1): Luyten & Hughes, 1985, Proper motion survey with Schmidt telescopes. LXVII Proper motions for 210 faint stars. University of Minnesota Press, Minneapolis Wroblewski & Torres, Cat. J/A+AS/78/231, J/A+AS/91/129, J/A+AS/105/179, J/A+AS/115/481, J/A+AS/122/447 Note (2): 1: Multiple detections of the same star in different UKST fields 2: for one probable binary star (DSS2 was not yet available for a definitive confirmation) measured as a single object Note (3): 1: the star was located near the plate edge 2: the image of the star was disturbed by the diffraction spikes or halo of a bright stellar image in its vicinity Note (4): K/M star = K8..M1 M star = M2..M4 late M star = M5..M7 very late M star = M8.. For the cool WDs if DA then the less Balmer lines the cooler the type, however, it is impossible to tell the difference between DC and DA WDs for our faint WDs at the given signal-to-noise and resolution. Most of the WDs should have 5000∼K to 6000∼K)
Acknowledgements: Ralf Scholz
(End) Patricia Bauer [CDS] 27-Jan-2000
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