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J/A+A/464/495       UBVI photometry of NGC 45 star clusters  (Mora+, 2007)

Imaging of star clusters in unperturbed spiral galaxies with the Advanced Camera for Surveys. I. The low luminosity galaxy NGC 45. Mora M.D., Larsen S.S., Kissler-Patig M. <Astron. Astrophys., 464, 495-505 (2007)> =2007A&A...464..495M
ADC_Keywords: Galaxies, nearby ; Associations, stellar ; Photometry, UBVRI Keywords: galaxies: individual: NGC 45 - galaxies: star clusters - galaxies: photometry Abstract: Star clusters are present in almost all types of galaxies. Here we investigate the star cluster population in the low-luminosity, unperturbed spiral galaxy NGC 45, which is located in the nearby Sculptor group. Both the old (globular) and young star-cluster populations are studied. Previous ground-based observations have suggested that NGC 45 has few if any "massive" young star clusters. We aim to study the population of lower-mass "open" star clusters and also identify old globular clusters that could not be distinguished from foreground stars in the ground-based data. Star clusters were identified using UBVI imaging from the Advanced Camera for Surveys (ACS) and the Wide Field Planetary Camera 2 (WFPC2) on board the Hubble Space Telescope. From broad band colors and comparison with simple stellar population (SSP) models assuming a fixed metallicity, we derived the age, mass, and extinction. We also measured the radius for each star cluster candidate. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file tables.dat 165 47 Young star clusters (tables 2-4 of the paper)
Byte-by-byte Description of file: tables.dat
Bytes Format Units Label Explanations
1- 2 I2 -- [MLK2007] Sequential number 4 I1 h RAh Right ascension (J2000) 5 A1 --- --- [:] 6- 7 I2 min RAm Right ascension (J2000) 8 A1 --- --- [:] 9- 13 F5.2 s RAs [0:100] Right ascension (J2000) (1) 15 A1 --- DE- Declination sign (J2000) 16- 17 I2 deg DEd Declination sign (J2000) 18 A1 --- --- [:] 19- 20 I2 arcmin DEm Declination sign (J2000) 21 A1 --- --- [:] 22- 26 F5.2 arcsec DEs Declination sign (J2000) 28- 33 F6.3 mag Bmag B (F435W) magnitude 35- 39 F5.3 mag e_Bmag rms uncertainty on Bmag 41- 46 F6.3 mag Vmag V (F555W) magnitude 48- 52 F5.3 mag e_Vmag rms uncertainty in Vmag 54- 59 F6.3 mag Imag I (F814W) magnitude 61- 65 F5.3 mag e_Imag rms uncertainty on Imag 67- 72 F6.3 mag Umag ? U (F336W) magnitude 74- 78 F5.3 mag e_Umag ? rms uncertainty on Umag 80- 85 F6.3 pix FWHM FWHM derived using SExtractor for F435W band 87- 91 F5.3 pix FWHMB FWHM derived using ISHAPE for F435W band 93- 97 F5.3 pix FWHMV FWHM derived using ISHAPE for F555W band 99-103 F5.3 pix FWHMI FWHM derived using ISHAPE for F814W band 105-108 F4.2 mag AV1 ? Extinction derived for metallicity model 1 109 A1 --- n_AV1 [*] *: best fit value derived using SExtractor 110-113 F4.2 mag AV2 ? Extinction derived for metallicity model 2 114 A1 --- n_AV2 [*] *: best fit value derived using SExtractor 115-118 F4.2 mag AV3 ? Extinction derived for metallicity model 3 119 A1 --- n_AV3 [*] *: best fit value derived using SExtractor 120-123 F4.2 mag AV4 ? Extinction derived for metallicity model 4 124 A1 --- n_AV4 [*] *: best fit value derived using SExtractor 125-128 F4.2 [yr] logAge1 ? Cluster age derived for metallicity model 1 129 A1 --- n_logAge1 [*] *: best fit value derived using SExtractor 130-133 F4.2 [yr] logAge2 ? Cluster age derived for metallicity model 2 134 A1 --- n_logAge2 [*] *: best fit value derived using SExtractor 135-139 F5.2 [yr] logAge3 ? Cluster age derived for metallicity model 3 140 A1 --- n_logAge3 [*] *: best fit value derived using SExtractor 141-144 F4.2 [yr] logAge4 ? Cluster age derived for metallicity model 4 145 A1 --- n_logAge4 [*] *: best fit value derived using SExtractor 146-149 F4.2 [solMass] logM1 ? Cluster mass derived for metallicity model 1 150 A1 --- n_logM1 [*] *: best fit value derived using SExtractor 151-154 F4.2 [solMass] logM2 ? Cluster mass derived for metallicity model 2 155 A1 --- n_logM2 [*] *: best fit value derived using SExtractor 156-159 F4.2 [solMass] logM3 ? Cluster mass derived for metallicity model 3 160 A1 --- n_logM3 [*] *: best fit value derived using SExtractor 161-164 F4.2 [solMass] logM4 ? Cluster mass derived for metallicity model 4 165 A1 --- n_logM4 [*] *: best fit value derived using SExtractor
Note (1): For [MLK2007] 10, the printed position is erroneous. It has been corrected into 0:14:04.67 -23:09:22.27 (from author)
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 28-Sep-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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