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 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:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
catalog.dat 135 204 Catalogue of high-proper motion stars
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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
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Bytes Format Units Label Explanations
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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)
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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)
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Acknowledgements: Ralf Scholz
(End) Patricia Bauer [CDS] 27-Jan-2000