V4197 Sagittarii

data from SKY2000 - Master Star Catalog (Myers+ 1997)

position, motion, parallax:

position (J2000)	RA: 19h 5min 57.869sec	DEC: -19° 28' 52.61''	ą0.18 arcsec	source: 16
position (2000.73)	RA: 19h 6min 1sec	DEC: -19° 28' 49''	JD: 2451810.12
proper motion (J2000)	RA: 0.0008 arcsec/a	DEC: 0.004 arcsec/a		source: 16
radial velocity	-27 km/s			source: 11
galactic coord. (B1950)	longitude: 16.95°	latitude: -11.84°

magnitude:

visual	8.1 (observed)	source: 20
photovisual	8.6	source: 16

spectral information:

spectral class	B5		source: 96
Morgan-Keenan	B2/3V(n)		source: 23
B-magnitude	8.11 ą0.02	B-V-magnitude	0.01
U-magnitude	7.45 ą0.02	U-B-magnitude	-0.66

variability information:

source of data: 28

variability type	9
var. amplitude	0.2

sources:

11	General Catalogue of Stellar Radial Velocities
Wilson, R.E., General Catalogue of Stellar of Stellar Radial Radial Velocities, Washington, DC: Carnegie Institute of Washington, 1953
16	PPM North and PPM South Catalogs and PPM Supplement
Roser, S., and U. Bastian, "Catalogue of Positions and Proper Motions," A&AS, Vol. 74, p. 449, 1988, and Bastian, U., et al., "Catalogue of Positions and Proper Motions - South," 1993
20	Catalogue of Homogeneous Means in the UBV System
Mermilliod, J.C., Catalogue of Homogeneous Means in the UBV System, Institut d'Astronomie, Universite de Lausanne, 1994
23	Michigan Catalog of 2-Dimensional Spectral Types, Volume IV
Houk, N. and Smith-Moore, D., Michigan Catalogue of 2-Dimensional Spectral Types for the HD Stars, Vol. 4, (Zones -25 to -12 Degrees), Ann Arbor: The University of Michigan, 1988
96	SAO or HD/HDE Catalog
Reference from Value 1 or Reference from Value 2

data from Smithsonian Astrophysical Observatory Star Catalog (SAO Staff 1966; USNO, ADC 1990)

position and proper motion:

position (B1950)	RA: 19h 3min 1.336sec	DEC: -19° 33' 31.11''	ą0.027 arcsec
position (2000.73)	RA: 19h 6min 0sec	DEC: -19° 28' 49''	JD: 2451810.12
position (J2000)	RA: 19h 5min 58.033sec	DEC: -19° 28' 52.09''
proper motion B1950 (FK4)	RA: 0.003 arcsec/a	DEC: 0.013 arcsec/a	ą0.015 arcsec/a in RA ą0.011 arcsec/a in DEC
proper motion J2000 (FK5)	RA: 0.0031 arcsec/a	DEC: 0.013 arcsec/a
source of proper motion data	Determined by source catalog

magnitude:

visual	8.8 (accuracy: 1 decimal)
source of visual magnitude data	Taken from AGK1.

spectral information:

spectral class	B5
source of spectral data	Taken from the HD with M stars reclassified by Miss Cannon.

catalogues

source catalogue	Yale Transactions 12 Part II, catalogue number: 8080
Durchmusterung	BD-19 5292
Henry Draper Catalogue	177559

data from Combined General Catalogue of Variable Stars (Vol. I-III) (Kholopov+ 1998)

position:

position (equinox 1950.0)

RA: 19h 3min 1.3sec

DEC: -19° 33' 31''

variability informations:

variability type	EW/KE	close binary eclipsing system
magnitute at max. brightness	7.95
magnitute at min. brightness	8.7
photometric system	visual, photovisual or Johnson's V

references

to a study	E.M.Halbedel, IBVS No.3420, 1990.
to a chart/photograph	no chart is avaible, but the star is contained in the 'Bonner Durchmusterung'

miscanellous

ID in the GCVS catalogue	72/4197
constellation	Sagittarius
notes on existence	The star is equivalent to '71383'.

variability type description

variability type	description
EW	Eclipsing binary systems. These are binary systems with orbital planes so close to the observer's line of sight (the inclination i of the orbital plane to the plane orthogonal to the line of sight is close to 90 deg) that the components periodically eclipse each other. Consequently, the observer finds changes of the apparent combined brightness of the system with the period coincident with that of the components' orbital motion. EA Algol (Beta Persei)-type eclipsing systems. Binaries with spherical or slightly ellipsoidal components. It is possible to specify, for their light curves, the moments of the beginning and end of the eclipses. Between eclipses the light remains almost constant or varies insignificantly because of reflection effects, slight ellipsoidality of components, or physical variations. Secondary minima may be absent. An extremely wide range of periods is observed, from 0.2 to >= 10000 days. Light amplitudes are also quite different and may reach several magnitudes. EB Beta Lyrae-type eclipsing systems. These are eclipsing systems having ellipsoidal components and light curves for which it is impossible to specify the exact times of onset and end of eclipses because of a continuous change of a system's apparent combined brightness between eclipses; secondary minimum is observed in all cases, its depth usually being considerably smaller than that of the primary minimum; periods are mainly longer than 1 day. The components generally belong to early spectral types (B-A). Light amplitudes are usually <2 mag in V. EW W Ursae Majoris-type eclipsing variables. These are eclipsers with periods shorter than 1 days, consisting of ellipsoidal components almost in contact and having light curves for which it is impossible to specify the exact times of onset and end of eclipses. The depths of the primary and secondary minima are almost equal or differ insignificantly. Light amplitudes are usually <0.8 mag in V. The components generally belong to spectral types F-G and later.
KE	Contact systems of early (O-A) spectral type, both components being close in size to their inner critical surfaces.