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J/A+A/466/931       UBVI photometry of NGC 1901                 (Carraro+, 2007)

Observational templates of star cluster disruption. The stellar group NGC 1901 in front of the Large Magellanic Cloud. Carraro G., de la Fuente Marcos R., Villanova S., Moni Bidin C., de la Fuente Marcos C., Baumgardt H., Solivella G. <Astron. Astrophys. 466, 931 (2007)> =2007A&A...466..931C
ADC_Keywords: Clusters, open ; Photometry, CCD ; Photometry, UBVRI Keywords: Galaxy: open clusters and associations: individual: NGC 1901 - Galaxy: evolution Abstract: Observations indicate that present-day star formation in the Milky Way disk takes place in stellar ensembles or clusters rather than in isolation. Bound, long-lived stellar groups are known as open clusters. They gradually lose stars and are severely disrupted in their final evolutionary stages, leaving an open cluster remnant made up of a few stars. In this paper, we study in detail the stellar content and kinematics of the poorly populated star cluster NGC 1901. This object appears projected against the Large Magellanic Cloud. The aim of the present work is to derive the current evolutionary status, binary fraction, age, and mass of this stellar group. These are fundamental quantities to compare with those from N-body models in order to study the most general topic of star cluster evolution and dissolution. The analysis is performed using wide-field photometry in the UBVI pass-band, proper motions from the UCAC.2 catalog, and 3 epochs of high-resolution spectroscopy, as well as results from extensive N-body calculations. The star group NGC 1901 is found to be an ensemble of solar metallicity stars, 400±100Myr old, with a core radius of 0.23pc, a tidal radius of 1.0pc, and a location at 400±50pc from the Sun. Out of 13 confirmed members, only 5 single stars have been found. Its estimated present-day binary fraction is at least 62%. The calculated heliocentric space motion of the cluster is not compatible with possible membership in the Hyades stream. Our results show that NGC 1901 is a clear prototype of an open cluster remnant characterized by a high value of the binary fraction and a significant depletion of low-mass stars. In light of numerical simulations, this is compatible with NGC 1901 being what remains of a larger system initially made of 500-750 stars. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 94 50000 Photometry of NGC 1901
Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 5 I5 --- Seq [1/50000] Sequential number 7- 8 I2 h RAh Right ascension (J2000.0) 9 A1 --- --- [:] 10- 11 I2 min RAm Right ascension (J2000.0) 12 A1 --- --- [:] 13- 17 F5.2 s RAs Right ascension (J2000.0) 19 A1 --- DE- Declination sign (J2000.0) 20- 21 I2 deg DEd Declination (J2000.0) 22 A1 --- --- [:] 23- 24 I2 arcmin DEm Declination (J2000.0) 25 A1 --- --- [:] 26- 30 F5.2 arcsec DEs Declination (J2000.0) 32- 38 F7.4 mag Umag ?=99.9999 U magnitude 40- 46 F7.4 mag e_Umag ?=99.9999 error in U magnitude 48- 54 F7.4 mag Bmag ?=99.9999 B magnitude 56- 62 F7.4 mag e_Bmag ?=99.9999 Error in B magnitude 64- 70 F7.4 mag Vmag ?=99.9999 V magnitude 72- 78 F7.4 mag e_Vmag ?=99.9999 error in V magnitude 80- 86 F7.4 mag Imag ?=99.9999 I magnitude 88- 94 F7.4 mag e_Imag ?=99.9999 error in I magnitude
Acknowledgements: Giovanni Carraro, giovanni.carraro(at)
(End) Giovanni Carraro [Padova, Italy], Patricia Vannier [CDS] 06-Mar-2007
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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