J/MNRAS/492/1641 APOGEE southern GCs with the BACCHUS code (Meszaros+, 2020)
Homogeneous analysis of globular clusters from the APOGEE survey with the
BACCHUS code - II. The Southern clusters and overview.
Meszaros S., Masseron T., Garcia-Hernandez D.A., Allende Prieto C.,
Beers T.C., Bizyaev D., Chojnowski D., Cohen R.E., Cunha K., Dell'Agli F.,
Ebelke G., Fernandez-Trincado J.G., Frinchaboy P., Geisler D.,
Hasselquist S., Hearty F., Holtzman J., Johnson J., Lane R.R., Lacerna I.,
Longa-Pena P., Majewski S.R., Martell S.L., Minniti D., Nataf D.,
Nidever D.L., Pan K., Schiavon R.P., Shetrone M., Smith V.V., Sobeck J.S.,
Stringfellow G.S., Szigeti L., Tang B., Wilson J.C., Zamora O.
<Mon. Not. R. Astron. Soc., 492, 1641-1670 (2020)>
=2020MNRAS.492.1641M 2020MNRAS.492.1641M (SIMBAD/NED BibCode)
ADC_Keywords: Stars, late-type ; Stars, giant ; Clusters, globular ;
Abundances, [Fe/H] ; Abundances, peculiar ; Milky Way ;
Spectra, infrared
Keywords: astronomical data bases: miscellaneous - surveys -
stars, galaxies: abundances - stars: late-type -
globular clusters: general - galaxies: fundamental parameters
Abstract:
We investigate the Fe, C, N, O, Mg, Al, Si, K, Ca, Ce, and Nd
abundances of 2283 red giant stars in 31 globular clusters from
high-resolution spectra observed in both the northern and Southern
hemisphere by the SDSS-IV APOGEE-2 survey. This unprecedented
homogeneous data set, largest to date, allows us to discuss the
intrinsic Fe spread, the shape, and statistics of Al-Mg and N-C
anti-correlations as a function of cluster mass, luminosity, age, and
metallicity for all 31 clusters. We find that the Fe spread does not
depend on these parameters within our uncertainties including cluster
metallicity, contradicting earlier observations. We do not confirm the
metallicity variations previously observed in M22 and NGC 1851. Some
clusters show a bimodal Al distribution, while others exhibit a
continuous distribution as has been previously reported in the
literature. We confirm more than two populations in ω Cen and
NGC 6752, and find new ones in M79. We discuss the scatter of Al by
implementing a correction to the standard chemical evolution of Al in
the Milky Way. After correction, its dependence on cluster mass is
increased suggesting that the extent of Al enrichment as a function of
mass was suppressed before the correction. We observe a turnover in
the Mg-Al anticorrelation at very low Mg in ω Cen, similar to
the pattern previously reported in M15 and M92. ω Cen may also
have a weak K-Mg anticorrelation, and if confirmed, it would be only
the third cluster known to show such a pattern.
Description:
Our target selection follows that of Meszaros et al.
(2015AJ....149..153M 2015AJ....149..153M, Cat. J/AJ/149/153) and Masseron et al.
(2019A&A...622A.191M 2019A&A...622A.191M, Cat. J/A+A/622/A191). We select stars based on
their radial velocity first, their distance from cluster centre
second, and their metallicity third. In radial velocity, we required
stars to be within three times the velocity dispersion of the mean
cluster velocity, and in distance we required stars to be within the
tidal radius. The metallicity cut was usually set to ±0.5dex around
the cluster average, except for clusters with suspected intrinsic Fe
spread for which the metallicity cut was skipped, or only obvious
field stars were deleted (for example, stars with solar-like
metallicity in otherwise metal-poor clusters). For this paper we made
important updates by selecting the average cluster radial velocity and
its scatter from Gaia DR2 (Baumgardt & Hilker 2018MNRAS.478.1520B 2018MNRAS.478.1520B,
Cat. J/MNRAS/478/1520) rather than from Harris (1996AJ....112.1487H 1996AJ....112.1487H,
Cat. VII/195, 2010 edition). In addition, we introduced a fourth step
that is based upon selecting stars that have proper motion within a
1.5-2.5mas/yr range (depending on the cluster) around the cluster
average proper motion from the Gaia DR2 catalogue (Gaia Collaboration
2018A&A...616A...1G 2018A&A...616A...1G, Cat. I/345).
The individual atmospheric parameters and the derived abundances are
listed in Table 2, while the abundance averages and RMS scatters for
each cluster are presented in Table 3. Table 2 contains results for
all stars and clusters that were analysed, altogether 3382 stars in 44
clusters.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 261 3382 Atmospheric parameters and abundances of
individual stars
table3.dat 140 31 Abundance averages and scatter
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See also:
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
III/284 : APOGEE-2 data from DR16 (Johnsson+, 2020)
J/AJ/149/153 : Abundances of red giants in 10 globular clusters
(Meszaros+, 2015)
J/MNRAS/478/1520 : Milky Way globular clusters data (Baumgardt+, 2018)
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 18 A18 --- Name Star name (2MHHMMSSss+DDMMSSs)
20- 27 A8 --- Cluster Cluster name
29- 32 A4 --- Status [HB/RGB/eAGB/ ] Star status (1)
34- 38 I5 K Teff Effective temperature
40- 44 F5.2 [cm/s2] logg Surface gravity
46- 51 F6.3 [-] [Fe/H] ? Iron to hydrogen abundance ratio
53- 57 F5.3 [-] e_[Fe/H] ? Error on [Fe/H]
59- 64 F6.3 [-] [C/Fe] ? C/Fe abundance ratio
66 I1 --- limitC Number of C lines used in the abundances
analysis from BACCHUS (2)
68- 72 F5.3 [-] e_[C/Fe] ? Error on [C/Fe]
74 I1 --- o_[C/Fe] Number of C lines observed
76- 81 F6.3 [-] [N/Fe] ? N/Fe abundance ratio
83 I1 --- limitN Number of N lines used in the abundances
analysis from BACCHUS (2)
85- 89 F5.3 [-] e_[N/Fe] ? Error on [N/Fe]
91- 92 I2 --- o_[N/Fe] Number of N lines observed
94- 99 F6.3 [-] [O/Fe] ? O/Fe abundance ratio
101 I1 --- limitO Number of O lines used in the abundances
analysis from BACCHUS (2)
103-107 F5.3 [-] e_[O/Fe] ? Error on [O/Fe]
109-110 I2 --- o_[O/Fe] Number of O lines observed
112-117 F6.3 [-] [Na/Fe] ? Na/Fe abundance ratio
119 I1 --- limitNa Number of Na lines used in the abundances
analysis from BACCHUS (2)
121-125 F5.3 [-] e_[Na/Fe] ? Error on [Na/Fe]
127 I1 --- o_[Na/Fe] Number of Na lines observed
129-134 F6.3 [-] [Mg/Fe] ? Mg/Fe abundance ratio
136 I1 --- limitMg Number of Mg lines used in the abundances
analysis from BACCHUS (2)
138-142 F5.3 [-] e_[Mg/Fe] ? Error on [Mg/Fe]
144-145 I2 --- o_[Mg/Fe] Number of Mg lines observed
147-152 F6.3 [-] [Al/Fe] ? Al/Fe abundance ratio
154 I1 --- limitAl Number of Al lines used in the abundances
analysis from BACCHUS (2)
156-160 F5.3 [-] e_[Al/Fe] ? Error on [Al/Fe]
162 I1 --- o_[Al/Fe] Number of Al lines observed
164-169 F6.3 [-] [Si/Fe] ? Si/Fe abundance ratio
171 I1 --- limitSi Number of Si lines used in the abundances
analysis from BACCHUS (2)
173-177 F5.3 [-] e_[Si/Fe] ? Error on [Si/Fe]
179-180 I2 --- o_[Si/Fe] Number of Si lines observed
182-187 F6.3 [-] [K/Fe] ? K/Fe abundance ratio
189 I1 --- limitK Number of K lines used in the abundances
analysis from BACCHUS (2)
191-195 F5.3 [-] e_[K/Fe] ? Error on [K/Fe]
197 I1 --- o_[K/Fe] Number of K lines observed
199-204 F6.3 [-] [Ca/Fe] ? Ca/Fe abundance ratio
206 I1 --- limitCa Number of Ca lines used in the abundances
analysis from BACCHUS (2)
208-212 F5.3 [-] e_[Ca/Fe] ? Error on [Ca/Fe]
214 I1 --- o_[Ca/Fe] Number of Ca lines observed
216-221 F6.3 [-] [Ce/Fe] ? Ce/Fe abundance ratio
223 I1 --- limitCe Number of Ce lines used in the abundances
analysis from BACCHUS (2)
225-229 F5.3 [-] e_[Ce/Fe] ? Error on [Ce/Fe]
231 I1 --- o_[Ce/Fe] Number of Ce lines observed
233-238 F6.3 [-] [Nd/Fe] ? Nd/Fe abundance ratio
240 I1 --- limitNd Number of Nd lines used in the abundances
analysis from BACCHUS (2)
242-246 F5.3 [-] e_[Nd/Fe] ? Error on [Nd/Fe]
248 I1 --- o_[Nd/Fe] Number of Nd lines observed
250-253 I4 --- S/N Signal to noise ratio
255-261 I7 --- OName ? Object identifier from Carretta et al.
(2009A&A...505..117C 2009A&A...505..117C)
--------------------------------------------------------------------------------
Note (1): Status as follows:
HB = Horizontal branch star (183/3382)
RGB = Red giant branch star (2919/3382)
eAGB = Early-Asymptotic giant branch star (280/3382)
Note (2): Number of lines used in the abundances analysis from BACCHUS
(Masseron, Merle & Hawkins 2016ascl.soft05004M)
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Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Name Cluster name (NGC NNNN or Pal 5)
10- 16 A7 --- Oname Alternative name
18- 23 F6.3 [-] [Fe/H]C ? Fe/H abundance ration from
Carretta et al. (2009A&A...508..695C 2009A&A...508..695C)
25- 29 F5.2 [-] [Fe/H]P ? Fe/H abundance ration from
Pancino et al. (2017A&A...601A.112P 2017A&A...601A.112P,
Cat. J/A+A/601/A112)
31- 36 F6.1 10+3Msun Mass Cluster mass from
Baumgardt & Hilker (2018MNRAS.478.1520B 2018MNRAS.478.1520B,
Cat. J/MNRAS/478/1520)
38- 43 F6.2 mag VMAG Absolute visual magnitude
45- 48 F4.1 Gyr Age ? Cluster age from
Krause et al. (2016A&A...587A..53K 2016A&A...587A..53K)
50- 55 F6.3 [-] [Fe/H] Average Fe/H abundance ratio
57- 61 F5.3 [-] s_[Fe/H] Scatter on [Fe/H] (1)
63- 67 F5.3 [-] e_[Fe/H] Average uncertainty on [Fe/H]
69- 73 F5.3 [-] [Al/Fe] Average Al/Fe abundance ratio
75- 79 F5.3 [-] s_[Al/Fe] Scatter on [Al/Fe] (1)
81- 85 F5.3 [-] [Al/Fe]sup ? Average of [Al/Fe]>0.3dex abundances
87- 92 F6.3 [-] [Al/Fe]inf ? Average of [Al/Fe]<0.3dex abundances
94- 98 F5.3 [-] s_[Al/Fe]sup ? Scatter on [Al/Fe]sup (1)
100-104 F5.3 --- fenriched ? Extent of enrichment
fenriched=NSG/Ntot (2)
106-110 F5.3 [-] S1 Average (Mg+Al+Si)/Fe abundance ratio
112-116 F5.3 [-] s_S1 Scatter on S1 (1)
118-122 F5.3 [-] [N/Fe] ? Average N/Fe abundance ratio
124-128 F5.3 [-] s_[N/Fe] ? Scatter on [N/Fe]
130-134 F5.3 [-] S2 ? Average (C+N+O)/Fe abundance ratio
136-140 F5.3 [-] s_S2 ? Scatter on S2 (1)
--------------------------------------------------------------------------------
Note (1): The scatter is defined as the standard deviation around the mean
Note (2): fenriched is defined as the ratio of second-generation stars to the
total number of stars in each cluster
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History:
From electronic version of the journal
References:
Masseron et al., Paper I 2019A&A...622A.191M 2019A&A...622A.191M, Cat. J/A+A/622/A191
(End) Ana Fiallos [CDS] 14-Mar-2023