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J/A+A/501/949    Star cluster properties in five spiral galaxies   (Mora+, 2009)

Imaging of star clusters in unperturbed spiral galaxies with the Advanced Camera for Surveys. II. A comparison of star cluster systems in five late type spirals. Mora M.D., Larsen S.S, Kissler-Patig M., Brodie J.P., Richtler T. <Astron. Astrophys. 501, 949 (2009)> =2009A&A...501..949M
ADC_Keywords: Galaxies, photometry Keywords: galaxies: star clusters - galaxies: photometry Abstract: Aims: Our goal is to investigate the formation of star clusters in relatively unperturbed environments. To do this, we studied the five nearby spiral galaxies: NGC 45, NGC 1313, NGC 4395, NGC 5236, and NGC 7793. Methods: We obtained images of the galaxies and their star cluster systems in UBVI using the Advanced Camera for Surveys (ACS) and the Wide Field Planetary Camera 2 (WFPC2) on board the Hubble Space Telescope. From a comparison of the broad-band colours with simple stellar population (SSP) models, we derived individual properties for each galaxy for the clusters such such as masses, ages, and sizes, as well as global star cluster system properties such as the age distribution, luminosity function, and disruption time for clusters. Results. We identified about 600 star cluster candidates in the five galaxies, typically spanning ages from 3.9Myr up to 1Gyr and masses from 102M up to 105M. We used the cluster age distribution to reconstruct the recent star formation history of each galaxy and observed significant variations from galaxy to galaxy. We went on to derive the luminosity function of the young star clusters and found slopes around α~-2 (similar to the ones found in previous studies) and the brightest star cluster magnitudes consistent with a random sampling of the luminosity function without involving an upper luminosity cut off. Finally, the sample includes only a handful of old globular clusters in each galaxy from which we derive low globular cluster specific frequencies. Description: The galaxies were observed with the HST ACS Wide Field Channel and the WFPC2. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table.dat 251 580 Derived star cluster properties for all galaxies
See also: J/A+A/464/495 : UBVI photometry of NGC 45 star clusters (Mora+, 2007) Byte-by-byte Description of file: table.dat
Bytes Format Units Label Explanations
1- 13 A13 --- Name Cluster ID (1) 15- 16 I2 h RAh Hour Right Ascension J2000 (hours) 17 A1 --- --- [:] 18- 19 I2 min RAm Right Ascension J2000 (minutes) 20 A1 --- --- [:] 21- 27 F7.4 s RAs Right Ascension J2000 (seconds) 29 A1 --- DE- Declination J2000 (sign) 30- 31 I2 deg DEd Declination J2000 (degrees) 32 A1 --- --- [:] 33- 34 I2 arcmin DEm Declination J2000 (minutes) 35 A1 --- --- [:] 36- 41 F6.3 arcsec DEs Declination J2000 (seconds) 43- 50 F8.3 pix Xpos X position on the CCD according to the image 52- 59 F8.3 pix Ypos Y position on the CCD according to the image 61- 66 F6.3 mag Bmag B(F435W) photometry 68- 72 F5.3 mag e_Bmag Photometry error of F435W (Sigma_F435W) 74- 79 F6.3 mag Vmag V(F555W) photometry 81- 85 F5.3 mag e_Vmag Photometry error of F555W (Sigma_F555W) 87- 92 F6.3 mag Imag I(F814W) photometry 94- 98 F5.3 mag e_Imag Photometry error of F814W (Sigma_F814W) 100-105 F6.3 mag Umag U(F336W) photometry 107-111 F5.3 mag e_Umag Photometry error of F336W (Sigma_F336W) 113-119 F7.3 pix BfwhmS FWHM in pixels measured in the B(F435W) images according to SExtractor 121-127 F7.3 pix Bfwhm FWHM in pixels measured in the B(F435W) images according to ISHAPE 129-135 F7.3 pix Vfwhm FWHM in pixels measured in the V(F555W) images according to ISHAPE 137-143 F7.3 pix Ifwhm FWHM in pixels measured in the I(F814W) images according to ISHAPE 145-149 F5.3 mag E(B-V)1 Color excess calculated with Z=0.004 GALEV 151-155 F5.3 mag E(B-V)2 Color excess calculated with Z=0.008 GALEV 157-161 F5.3 mag E(B-V)3 Color excess calculated with Z=0.02 GALEV 163-167 F5.3 mag E(B-V)4 Color excess calculated with Z=0.05 GALEV 169-173 F5.3 mag E(B-V)5 Color excess calculated with Z=0.004 Girardi 175-179 F5.3 mag E(B-V)6 Color excess calculated with Z=0.019 Girardi 181-185 F5.3 [yr] Age1 log(Age) calculated with Z=0.004 GALEV 187-191 F5.3 [yr] Age2 log(Age) calculated with Z=0.008 GALEV 193-197 F5.3 [yr] Age3 log(Age) calculated with Z=0.02 GALEV 199-203 F5.3 [yr] Age4 log(Age) calculated with Z=0.05 GALEV 205-209 F5.3 [yr] Age5 log(Age) calculated with Z=0.004 Girardi 211-215 F5.3 [yr] Age6 log(Age) calculated with Z=0.019 Girardi 217-221 F5.3 [solMass] Mass1 log(Mass) calculated with Z=0.004 GALEV 223-227 F5.3 [solMass] Mass2 log(Mass) calculated with Z=0.008 GALEV 229-233 F5.3 [solMass] Mass3 log(Mass) calculated with Z=0.02 GALEV 235-239 F5.3 [solMass] Mass4 log(Mass) calculated with Z=0.05 GALEV 241-245 F5.3 [solMass] Mass5 log(Mass) calculated with Z=0.004 Girardi 247-251 F5.3 [solMass] Mass6 log(Mass) calculated with Z=0.019 Girardi
Note (1): Galaxy ID: NameFieldN
Acknowledgements: Marcelo Mora, mmora(at)dfa.uv.cl References: Mora et al., Paper I 2007A&A...464..495M, Cat. J/A+A/464/495
(End) M.D. Mora [Univ. de Valparaiso], Francois Ochsenbein [CDS] 28-Jul-2009
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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