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J/A+A/598/A68       Gaia-ESO Survey. Trumpler 23             (Overbeek+, 2017)

The Gaia-ESO Survey: the inner disk, intermediate-age open cluster Trumpler 23. Overbeek J.C., Friel E.D., Donati P., Smiljanic R., Jacobson H.R., Hatzidimitriou D., Held E.V., Magrini L., Bragaglia A., Randich S., Vallenari A., Cantat-Gaudin T., Tautvaisiene G., Jimenez-Esteban F., Frasca A., Geisler D., Villanova S., Tang B., Munoz C., Marconi G., Carraro G., San Roman I., Drazdauskas A., Zenoviene R., Gilmore G., Jeffries R.D., Flaccomio E., Pancino E., Bayo A., Costado M.T., Damiani F., Jofre P., Monaco L., Prisinzano L., Sousa S.G., Zaggia S. <Astron. Astrophys., 598, A68-68 (2017)> =2017A&A...598A..68O (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, open ; Abundances ; Effective temperatures ; Radial velocities Keywords: Galaxy: formation - Galaxy: abundances - Galaxy: disk - open clusters and associations: individual: Trumpler 23 - stars: abundances Abstract: Trumpler 23 is a moderately populated, intermediate-age open cluster within the solar circle at a RGC∼6kpc. It is in a crowded field very close to the Galactic plane and the color-magnitude diagram shows significant field contamination and possible differential reddening; it is a relatively understudied cluster for these reasons, but its location makes it a key object for determining Galactic abundance distributions. New data from the Gaia-ESO Survey enable the first ever radial velocity and spectroscopic metallicity measurements for this cluster. We aim to use velocities to isolate cluster members, providing more leverage for determining cluster parameters. Gaia-ESO Survey data for 167 potential members have yielded radial velocity measurements, which were used to determine the systemic velocity of the cluster and membership of individual stars. Atmospheric parameters were also used as a check on membership when available. Literature photometry was used to re-determine cluster parameters based on radial velocity member stars only; theoretical isochrones are fit in the V, V-I diagram. Cluster abundance measurements of ten radial-velocity member stars with high-resolution spectroscopy are presented for 24 elements. These abundances have been compared to local disk stars, and where possible placed within the context of literature gradient studies. We find Trumpler 23 to have an age of 0.80±0.10Gyr, significant differential reddening with an estimated mean cluster E(V-I) of 1.02+0.14-0.09, and an apparent distance modulus of 14.15±0.20. We find an average cluster metallicity of [Fe/H]=0.14±0.03dex, a solar [α/Fe] abundance, and notably subsolar [s-process/Fe] abundances. Description: Data for GES are taken with the Fiber Large Array Multi-Element Spectrograph (FLAMES) on the VLT at the European Southern Observatory. FLAMES has two instruments, the medium-resolution multi-object spectrograph GIRAFFE and the high-resolution Ultraviolet and Visual Echelle Spectrograph (UVES). For intermediate-age OCs with prominent red clumps, GES targets are selected as follows: likely clump stars are observed with UVES, so that the most time-intensive targets are most likely to be members, followed by probable red giants if the clump is sparse. Main sequence stars down to V=19 are observed with GIRAFFE, using the HR9B setup primarily for stars of spectral type A to F and the HR15N setup for cooler stars. General GES target selection methods are outlined in Bragaglia et al. (in prep.). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file tablea1.dat 107 60 Parameters for Trumpler 23 radial velocity members with GIRAFFE data tablea2.dat 107 91 Parameters for Trumpler 23 radial velocity non-members with GIRAFFE data tablea3.dat 111 16 Parameters for Trumpler 23 targets with UVES data tablea4.dat 94 10 UVES target light and alpha-element abundances tablea5.dat 84 10 UVES target Fe-peak abundances tablea6.dat 84 10 UVES target neutron-capture element abundances
Byte-by-byte Description of file: tablea1.dat tablea2.dat
Bytes Format Units Label Explanations
1- 4 I4 --- Star Identification number (G1) 6- 21 A16 --- GES GES identification (HHMMSSss+DDMMSSs) 23- 28 F6.3 mag Vmag V magnitude (G1) 30- 34 F5.3 mag V-I V-I colour index (G1) 36- 44 F9.5 deg RAdeg Right ascension (J2000) 46- 54 F9.5 deg DEdeg Declination (J2000) 56- 59 I4 K Teff ?=- Effective temperature 61- 63 I3 K e_Teff ? rms uncertainty on Teff 65- 68 F4.2 [cm/s2] logg ?=- Surface gravity 70- 73 F4.2 [cm/s2] e_logg ? rms uncertainty on logg 75- 78 F4.2 km/s xi ?=- Microturbulent velocity 80- 83 F4.2 km/s e_xi ? rms uncertainty on xi 85- 89 F5.2 [-] [Fe/H] ?=- Metallicity 91- 94 F4.2 [-] e_[Fe/H] ? rms uncertainty on [Fe/H] 96-102 F7.2 km/s RV Radial velocity 104-107 F4.2 km/s e_RV rms uncertainty on RV
Byte-by-byte Description of file: tablea3.dat
Bytes Format Units Label Explanations
1- 4 I4 --- Star Identification number (G1) 6- 21 A16 --- GES GES identification (HHMMSSss+DDMMSSs) 23- 28 F6.3 mag Vmag V magnitude (G1) 30- 34 F5.3 mag V-I V-I colour index (G1) 36- 44 F9.5 deg RAdeg Right ascension (J2000) 46- 54 F9.5 deg DEdeg Declination (J2000) 56- 58 I3 --- S/N Signal-to-noise ratio 60- 65 F6.2 km/s RV Radial velocity 67- 70 F4.2 km/s e_RV rms uncertainty on RV 72- 75 I4 K Teff ?=- Effective temperature 77- 79 I3 K e_Teff ? rms uncertainty on Teff 81- 84 F4.2 [cm/s2] logg ?=- Surface gravity 86- 89 F4.2 [cm/s2] e_logg ? rms uncertainty on logg 91- 94 F4.2 km/s xi ?=- Microturbulent velocity 96- 99 F4.2 km/s e_xi ? rms uncertainty on xi 101-104 F4.2 [-] [Fe/H] ?=- Metallicity 106-109 F4.2 [-] e_[Fe/H] ? rms uncertainty on [Fe/H] 111 A1 --- Memb? [Y/N] Radial velocity membership ?
Byte-by-byte Description of file: tablea4.dat
Bytes Format Units Label Explanations
1- 4 I4 --- Star Identification number (G1) 6- 9 F4.2 --- CI CI abundance 11- 14 F4.2 --- e_CI rms uncertainty on CI 16- 19 F4.2 --- OI OI abundance 21- 24 F4.2 --- e_OI rms uncertainty on OI 26- 29 F4.2 --- NaI NaI abundance 31- 34 F4.2 --- e_NaI rms uncertainty on NaI 36- 39 F4.2 --- MgI MgI abundance 41- 44 F4.2 --- e_MgI rms uncertainty on MgI 46- 49 F4.2 --- AlI AlI abundance 51- 54 F4.2 --- e_AlI rms uncertainty on AlI 56- 59 F4.2 --- SiI SiI abundance 61- 64 F4.2 --- e_SiI rms uncertainty on SiI 66- 69 F4.2 --- SI SI abundance 71- 74 F4.2 --- e_SI rms uncertainty on SI 76- 79 F4.2 --- CaI CaI abundance 81- 84 F4.2 --- e_CaI rms uncertainty on CaI 86- 89 F4.2 --- TiI TiI abundance 91- 94 F4.2 --- e_TiI rms uncertainty on TiI
Byte-by-byte Description of file: tablea5.dat
Bytes Format Units Label Explanations
1- 4 I4 --- Star Identification number (G1) 6- 9 F4.2 --- ScI ScI abundance 11- 14 F4.2 --- e_ScI rms uncertainty on ScI 16- 19 F4.2 --- VI VI abundance 21- 24 F4.2 --- e_VI rms uncertainty on VI 26- 29 F4.2 --- CrI CrI abundance 31- 34 F4.2 --- e_CrI rms uncertainty on CrI 36- 39 F4.2 --- MnI MnI abundance 41- 44 F4.2 --- e_MnI rms uncertainty on MnI 46- 49 F4.2 --- FeI FeI abundance 51- 54 F4.2 --- e_FeI rms uncertainty on FeI 56- 59 F4.2 --- FeII FeII abundance 61- 64 F4.2 --- e_FeII rms uncertainty on FeII 66- 69 F4.2 --- CoI CoI abundance 71- 74 F4.2 --- e_CoI rms uncertainty on CoI 76- 79 F4.2 --- NiI NiI abundance 81- 84 F4.2 --- e_NiI rms uncertainty on NiI
Byte-by-byte Description of file: tablea6.dat
Bytes Format Units Label Explanations
1- 4 I4 --- Star Identification number (G1) 6- 9 F4.2 --- YII YII abundance 11- 14 F4.2 --- e_YII rms uncertainty on YII 16- 19 F4.2 --- ZrI ZrI abundance 21- 24 F4.2 --- e_ZrI rms uncertainty on ZrI 26- 29 F4.2 --- MoI MoI abundance 31- 34 F4.2 --- e_MoI rms uncertainty on MoI 36- 39 F4.2 --- BaII BaII abundance 41- 44 F4.2 --- e_BaII rms uncertainty on BaII 46- 49 F4.2 --- LaII LaII abundance 51- 54 F4.2 --- e_LaII rms uncertainty on LaII 56- 59 F4.2 --- CeII CeII abundance 61- 64 F4.2 --- e_CeII rms uncertainty on CeII 66- 69 F4.2 --- NdII NdII abundance 71- 74 F4.2 --- e_NdII rms uncertainty on NdII 76- 79 F4.2 --- EuII EuII abundance 81- 84 F4.2 --- e_EuII rms uncertainty on EuII
Global notes: Note (G1): ID numbers and photometry from Carraro et al. (2006MNRAS.368.1078C).
History: From electronic version of the journal References:
(End) Patricia Vannier [CDS] 24-May-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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