J/A+A/557/A138 Detailed chemical abundances in the GlC NGC 362 (Carretta+ 2013)
NGC 362: another globular cluster with a split red giant branch.
Carretta E., Bragaglia A., Gratton R.G., Lucatello S., D'Orazi V.,
Bellazzini M., Catanzaro G., Leone F., Momany Y., Sollima A.
<Astron. Astrophys. 557, A138 (2013)>
=2013A&A...557A.138C 2013A&A...557A.138C
ADC_Keywords: Clusters, globular ; Stars, population II ; Abundances
Keywords: stars: Population II - globular clusters - stars: abundances -
stars: atmospheres - globular clusters: individual: NGC 362
Abstract:
We obtained FLAMES GIRAFFE+UVES spectra for both first and
second-generation red giant branch (RGB) stars in the globular cluster
(GC) NGC 362 and used them to derive abundances of 21 atomic species
for a sample of 92 stars. The surveyed elements include proton-capture
(O, Na, Mg, Al, Si), alpha-capture (Ca, Ti), Fe-peak (Sc, V, Mn, Co,
Ni, Cu), and neutron-capture elements (Y, Zr, Ba, La, Ce, Nd, Eu, Dy).
The analysis is fully consistent with that presented for twenty GCs in
previous papers of this series. Stars in NGC 362 seem to be clustered
into two discrete groups along the Na-O anti-correlation, with a gap
at [O/Na]∼0dex. Na-rich, second generation stars show a trend to be
more centrally concentrated, although the level of confidence is not
very high. When compared to the classical second-parameter twin NGC
288, with similar metallicity, but different horizontal branch type
and much lower total mass, the proton-capture processing in stars of
NGC 362 seems to be more extreme, confirming previous analysis. We
discovered the presence of a secondary RGB sequence, redder than the
bulk of the RGB: a preliminary estimate shows that this sequence
comprises about 6% of RGB stars. Our spectroscopic data and literature
photometry indicate that this sequence is populated almost exclusively
by giants rich in Ba, and probably rich in all s-process elements, as
found in other clusters. In this regards, NGC 362 joins previously
studied GCs like NGC 1851, NGC 6656 (M 22), and NGC 7089 (M 2).
Description:
Results of the abundance analysis are given in several separate
tables, for GIRAFFE and UVES targets.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 69 92 ID, coordinates, magnitudes, RV
table3.dat 58 92 Teff, logg, [A/H], Vt, [FeI/H], [FeII/H]
table4.dat 61 92 [O/Fe], [Na/Fe], [Mg/Fe], [Al/Fe]
table5.dat 55 92 [Si/Fe], [Ca/Fe], [TiI/Fe], [TiII/Fe]
table6.dat 99 92 [ScII/Fe], [V/Fe], [CrI/Fe], [Mn/Fe], [Co/Fe],
[Ni/Fe], [Cu/Fe]
table7.dat 97 14 [YII/Fe], [ZrII/Fe], [LaII/Fe], [CeII/Fe],
[NdII/Fe], [EuII/Fe], [DyII/Fe] (UVES targets)
table8.dat 20 92 [BaII/Fe]
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See also:
J/A+A/455/271 : NGC 6441 red giant abundances (Gratton+, 2006)
J/A+A/464/927 : NGC 6752 red giant abundances (Carretta+, 2007)
J/A+A/464/939 : NGC 6218 red giant abundances (Carretta+, 2007)
J/A+A/464/953 : NGC 6441 red giant abundances (Gratton+, 2007)
J/A+A/464/967 : NGC 6388 red giant abundances (Carretta+, 2007)
J/A+A/505/117 : 15 globular clusters red giant abundances (Carretta+, 009)
J/A+A/505/139 : 17 globular clusters red giant abundances (Carretta+, 2009)
J/A+A/533/A69 : Spectroscopy of 124 RGB stars (Carretta+, 2011)
J/A+A/550/A34 : M4 and 47 Tuc red giant abundances (Carretta+, 2013)
J/A+A/520/A95 : M54 and Sgr dSph red giant abundances (Carretta+, 2010)
J/AJ/122/2569 : VI photometry of NGC 288, 362 and 1851 (Bellazzini+, 2001)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 5 I5 --- Star [986/20950] Star identification
7- 8 I2 h RAh Right ascension (J2000.0)
10- 11 I2 min RAm Right ascension (J2000.0)
13- 18 F6.3 s RAs Right ascension (J2000.0)
20 A1 --- DE- Declination sign (J2000.0)
21- 22 I2 deg DEd Declination (J2000.0)
24- 25 I2 arcmin DEm Declination (J2000.0)
27- 31 F5.2 arcsec DEs Declination (J2000.0)
33- 38 F6.3 mag Bmag B magnitude
40- 45 F6.3 mag Vmag V magnitude
47- 52 F6.3 mag Kmag 2MASS Ks magnitude
54- 59 F6.2 km/s HRV Heliocentric radial velocity
61- 69 A9 --- Inst Origin of spectra: Giraffe (HR11 and/or HR13)
and/or UVES
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 5 I5 --- Star [986/20950] Star identification
7- 10 I4 K Teff Teff
12- 15 F4.2 [cm/s2] logg Surface gravity
17- 21 F5.2 [Sun] [A/H] Metallicity
23- 26 F4.2 km/s vt Microturbulent velocity
28- 29 I2 --- nFeI Number of FeI lines
31- 36 F6.3 [Sun] [FeI/H] Abundance [Fe/H]I
38- 42 F5.3 [Sun] e_[FeI/H] rms of [FeI/H]
44- 45 I2 --- nFeII ? Number of FeII lines
47- 52 F6.3 [Sun] [FeII/H] ? Abundance [FeII/H]
54- 58 F5.3 [Sun] e_[FeII/H] ? rms of [Fe/H]II
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 5 I5 --- Star [986/20950] Star identification
7 I1 --- nO ? Number of O lines
9- 13 F5.2 [Sun] [O/Fe] ? Abundance [O/Fe]
15- 18 F4.2 [Sun] e_[O/Fe] ? rms of [O/Fe]
20 I1 --- nNa Number of Na lines
22- 26 F5.2 [Sun] [Na/Fe] Abundance [Na/Fe]
28- 31 F4.2 [Sun] e_[Na/Fe] ? rms of [Na/Fe]
33 I1 --- nMg ? Number of Mg lines
35- 39 F5.2 [Sun] [Mg/Fe] ? Abundance [Mg/Fe]
41- 44 F4.2 [Sun] e_[Mg/Fe] ? rms of [Mg/Fe]
46 I1 --- nAl ? Number of Al lines
48- 52 F5.2 [Sun] [Al/Fe] ? Abundance [Al/Fe]
54- 57 F4.2 [Sun] e_[Al/Fe] ? rms of [Al/Fe]
59 I1 --- O [0/1] is value of O a limit? 0=limit (1)
61 I1 --- Al [0/1]? is value of Al a limit? 0=limit (1)
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Note (1): limit in O, Al : 1 means actual measure, 0 upper limit
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 5 I5 --- Star [986/20950] Star identification
7- 8 I2 --- nSi ? Number of Si lines
10- 14 F5.2 [Sun] [Si/Fe] ? Abundance [Si/Fe]
16- 19 F4.2 [Sun] e_[Si/Fe] ? rms of [Si/Fe]
21- 22 I2 --- nCa ? Number of Ca lines
24- 28 F5.2 [Sun] [Ca/Fe] ? Abundance [Ca/Fe]
30- 33 F4.2 [Sun] e_[Ca/Fe] ? rms of [Ca/Fe]
35- 36 I2 --- nTiI ? Number of TiI lines
38- 42 F5.2 [Sun] [Ti/FeI] ? Abundance [Ti/FeI]
44- 47 F4.2 [Sun] e_[Ti/FeI] ? rms of [Ti/FeI]
49 I1 --- nTiII ? Number of TiII lines
51- 55 F5.2 [Sun] [Ti/FeII] ? Abundance [Ti/FeII]
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 5 I5 --- Star [986/20950] Star identification
7 I1 --- nSc Number of Sc lines
9- 13 F5.2 [Sun] [Sc/Fe] Abundance [Sc/Fe]
15- 18 F4.2 [Sun] e_[Sc/Fe] ? Error of [Sc/Fe]
20- 21 I2 --- nV ? Number of V lines
23- 27 F5.2 [Sun] [V/Fe] ? Abundance [V/Fe]
29- 32 F4.2 [Sun] e_[V/Fe] ? Error of [V/Fe]
34- 35 I2 --- nCrI ? Number of CrI lines
37- 41 F5.2 [Sun] [CrI/Fe] ? Abundance [CrI/Fe]
43- 46 F4.2 [Sun] e_[CrI/Fe] ? Error of [CrI/Fe]
48 I1 --- nMn ? Number of Mn lines
50- 54 F5.2 [Sun] [Mn/Fe] ? Abundance [Mn/Fe]
56- 59 F4.2 [Sun] e_[Mn/Fe] ? Error of [Mn/Fe]
61 I1 --- nCo ? Number of Co lines
63- 67 F5.2 [Sun] [Co/Fe] ? Abundance [Co/Fe]
69- 72 F4.2 [Sun] e_[Co/Fe] ? Error of [Co/Fe]
74- 75 I2 --- nNi Number of Ni lines
77- 81 F5.2 [Sun] [Ni/Fe] Abundance [Ni/Fe]
83- 86 F4.2 [Sun] e_[Ni/Fe] ? Error of [Ni/Fe]
88 I1 --- nCu ? Number of Cu lines
90- 94 F5.2 [Sun] [Cu/Fe] ? Abundance [Cu/Fe]
96- 99 F4.2 [Sun] e_[Cu/Fe] ? Error of [Cu/Fe] (1)
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Note (1): For [Cu/Fe] the error is estimated by summing in quadrature the best
fit variation obtained by changing temperature, gravity, metal abundance and
microturbulent velocity in amounts corresponding to the errors in these
parameters. To this, we added a fit error of 0.05dex in quadrature.
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
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1- 5 I5 --- Star [986/20950] Star identification
7 I1 --- nYII Number of YII lines
9- 13 F5.2 [Sun] [YII/Fe] Abundance [YII/Fe] (1)
15- 18 F4.2 [Sun] e_[YII/Fe] Error of [YII/Fe]
20 I1 --- nZrII Number of ZrII lines
22- 26 F5.2 [Sun] [ZrII/Fe] Abundance [ZrII/Fe] (1)
28- 31 F4.2 [Sun] e_[ZrII/Fe] Error of [ZrII/Fe]
33 I1 --- nLaII Number of LaII lines
35- 39 F5.2 [Sun] [LaII/Fe] Abundance [LaII/Fe] (1)
41- 44 F4.2 [Sun] e_[LaII/Fe] Error of [LaII/Fe]
46 I1 --- nCeII Number of CeII lines
48- 52 F5.2 [Sun] [CeII/Fe] Abundance [CeII/Fe] (1)
54- 57 F4.2 [Sun] e_[CeII/Fe] Error of [CeII/Fe]
59- 60 I2 --- nNdII Number of NdII lines
62- 66 F5.2 [Sun] [NdII/Fe] Abundance [NdII/Fe] (1)
68- 71 F4.2 [Sun] e_[NdII/Fe] Error of [NdII/Fe]
73 I1 --- nEuII Number of EuII lines
75- 79 F5.2 [Sun] [EuII/Fe] Abundance [EuII/Fe] (1)
81- 84 F4.2 [Sun] e_[EuII/Fe] Error of [EuII/Fe]
86 I1 --- nDyII Number of DyII lines
88- 92 F5.2 [Sun] [DyII/Fe] Abundance [DyII/Fe] (1)
94- 97 F4.2 [Sun] e_[DyII/Fe] Error of [DyII/Fe]
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Note (1): For species with only one transition, the error is estimated by
summing in quadrature the best fit variation obtained by changing temperature,
gravity, metal abundance and microturbulent velocity in amounts corresponding
to the errors in these parameters. To this, we added a fit error of 0.05dex
in quadrature.
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Byte-by-byte Description of file: table8.dat
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Bytes Format Units Label Explanations
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1- 5 I5 --- Star [986/20950] Star identification
7 I1 --- nBa ? Number of BaII lines
9- 14 F6.3 [Sun] [BaII/Fe] ? Abundance [BaII/Fe]
16- 20 F5.3 [Sun] e_[BaII/Fe] ? rms of [BaII/Fe]
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Acknowledgements:
Eugenio Carretta, eugenio.carretta(at)oabo.inaf.it
(End) Patricia Vannier [CDS] 05-Aug-2013