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J/A+A/601/A112      GES iDR4 Mg-Al anticorrelation in GCs       (Pancino+, 2017)

The Gaia-ESO Survey. Mg-Al anti-correlation in iDR4 globular clusters. Pancino E., Romano D., Tang B., Tautvaisiene G., Casey A.R., Gruyters P., Geisler D., San Roman I., Randich S., Alfaro E.J., Bragaglia A., Flaccomio E., Korn A.J., Recio-Blanco A., Smiljanic R., Carraro G., Bayo A., Costado M.T., Damiani F., Jofre P., Lardo C., de Laverny P., Monaco L., Morbidelli L., Sbordone L., Sousa S.G., Villanova S. <Astron. Astrophys. 601, A112 (2017)> =2017A&A...601A.112P (SIMBAD/NED BibCode)
ADC_Keywords: Surveys ; Clusters, globular ; Abundances ; Effective temperatures Keywords: surveys - stars: abundances - globular clusters: general - globular clusters: individual: NGC 5927 Abstract: We use Gaia-ESO Survey iDR4 data to explore the Mg-Al anti-correlation in globular clusters, that were observed as calibrators, as a demonstration of the quality of Gaia-ESO Survey data and analysis. The results compare well with the available literature, within 0.1~[-] or less, after a small (compared to the Minternal spreads) offset between the UVES and the GIRAFFE data of 0.10-0.15dex was taken into account. In particular, we present for the first time data for NGC 5927, one of the most metal-rich globular clusters studied in the literature so far with [Fe/H]=-0.49dex, that was included to connect with the open cluster regime in the Gaia-ESO Survey internal calibration. The extent and shape of the Mg-Al anti-correlation provide strong constraints on the multiple population phenomenon in globular clusters. In particular, we studied the dependency of the Mg-Al anti-correlation extension with metallicity, present-day mass, and age of the clusters, using GES data in combination with a large set of homogenized literature measurements. We find a dependency with both metallicity and mass, that is evident when fitting for the two parameters simultaneously, but no significant dependency with age. We confirm that the Mg-Al anti-correlation is not seen in all clusters, but disappears for the less massive or most metal-rich ones. We also use our dataset to see whether a normal anti-correlation would explain the low [Mg/α] observed in some extragalactic globular clusters, but find that none of the clusters in our sample can reproduce it, and more extreme chemical compositions (like the one of NGC 2419) would be required. We conclude that GES iDR4 data already meet the requirements set by the main survey goals, and can be used to study in detail globular clusters even if the analysis procedures were not specifically designed for them. Description: List of globular clusters analyzed in this paper, with basic properties. List of the 510 stars that were selected from GES iDR4 as probable members and analyzed in this paper. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 66 9 Globular clusters list with basic properties table2.dat 76 510 Member stars with parameters and abundances
See also: J/A+A/598/A5 : Gaia-ESO Survey iDR4 calibrators (Pancino+, 2017) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 7 A7 --- NGC NGC cluster identification 8- 13 A6 --- AName Cluster alternate name 15- 19 F5.2 [-] [Fe/H]H Cluster metallicity from Harris, 1996AJ....112.1487H, Cat. VII/195 21- 26 F6.1 km/s RV Cluster radial velocity from Harris, 1996AJ....112.1487H, Cat. VII/195 29- 32 F4.2 [Msun] logM Cluster logarithmic mass 34- 37 F4.2 [Msun] e_logM Error on cluster mass 39 A1 --- r_logM [a/b] Reference for cluster mass (1) 42- 46 F5.2 [-] [Fe/H]G Cluster metallicity from Gaia-ESO survey 48- 51 F4.2 [-] e_[Fe/H]G Error on cluster metallicity 53- 58 F6.1 km/s RVG Radial velocity from Gaia-ESO survey 60- 62 F3.1 km/s e_RVG Error on radial velocity 64- 66 I3 --- Nstar Number of member stars analyzed
Note (1): The present-day mass is from: a = McLaughlin & van der Marel (2005, Cat. J/ApJS/161.304) b = Mandushev et al. (1991A&A...252...94M)
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 16 A16 --- GES GES star ID based on sexagesimal coordinates, HHMMSSss+DDMMSSs 18- 24 A7 --- NGC NGC cluster of which the star is member 26- 29 I4 K Teff Effective temperature 31- 33 I3 K e_Teff Error on the effective temperature 35- 37 F3.1 [cm2/s] logg Logarithm of surface gravity in cgs units 39- 41 F3.1 [cm2/s] e_logg Error on surface gravity 43- 47 F5.2 [-] [Fe/H] Metallicity based on iron abundance 49- 52 F4.2 [-] e_[Fe/H] Error on metallicity 54- 58 F5.2 [-] logAMg ?=-9.99 Mg abundance 60- 64 F5.2 [-] e_logAMg ?=-9.99 Error on Mg abundance 66- 70 F5.2 [-] logAAl ?=-9.99 Al abundance 72- 76 F5.2 [-] e_logAAl ?=-9.99 Error on Al abundance
Acknowledgements: Elena Pancino, pancino(at)
(End) Elena Pancino [INAF-OAA, ASDC], Patricia Vannier [CDS] 23-Feb-2017
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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