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 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:
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FileName Lrecl Records Explanations
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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
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Byte-by-byte Description of file: tablea1.dat tablea2.dat
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Bytes Format Units Label Explanations
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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
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Byte-by-byte Description of file: tablea3.dat
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Bytes Format Units Label Explanations
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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 ?
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Byte-by-byte Description of file: tablea4.dat
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Bytes Format Units Label Explanations
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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
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Byte-by-byte Description of file: tablea5.dat
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Bytes Format Units Label Explanations
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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
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Byte-by-byte Description of file: tablea6.dat
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Bytes Format Units Label Explanations
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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
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Global notes:
Note (G1): ID numbers and photometry from Carraro et al. (2006MNRAS.368.1078C 2006MNRAS.368.1078C).
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History:
From electronic version of the journal
References:
(End) Patricia Vannier [CDS] 24-May-2017