J/AJ/158/14 Stellar populations of globular clusters using APOGEE (Nataf+, 2019)
The relationship between globular cluster mass, metallicity, and light-element
abundance variations.
Nataf D.M., Wyse R.F.G., Schiavon R.P., Ting Y.-S., Minniti D., Cohen R.E.,
Fernandez-Trincado J.G., Geisler D., Nitschelm C., Frinchaboy P.M.
<Astron. J., 158, 14 (2019)>
=2019AJ....158...14N 2019AJ....158...14N (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, globular ; Stellar distribution ; Abundances ;
Radial velocities ; Effective temperatures ; Proper motions
Keywords: globular clusters: individual (47 Tuc, M4, Terzan 5)
Abstract:
We investigate aluminum abundance variations in the stellar populations
of globular clusters using both literature measurements of sodium and
aluminum and APOGEE measurements of nitrogen and aluminum abundances.
For the latter, we show that the Payne is the most suitable of the five
available abundance pipelines for our purposes. Our combined sample of
42 globular clusters spans approximately 2 dex in [Fe/H] and 1.5 dex
in logMGC/M☉. We find no fewer than five globular clusters with
significant internal variations in nitrogen and/or sodium with little
to no corresponding variation in aluminum, and that the minimum
present-day cluster mass for aluminum enrichment in metal-rich systems
is logMGC/M☉∼4.50+2.17([Fe/H]+1.30). We demonstrate that the
slopes of the [Al/Fe] versus [Na/Fe] and [Al/Fe] versus [N/Fe] relations
for stars without field-like abundances are approximately log-linearly
dependent on both the metallicity and the stellar mass of the globular
clusters. In contrast, the relationship between [Na/Fe] and [N/Fe] shows
no evidence of such dependencies. This suggests that there were (at least)
two classes of non-supernova chemical polluters that were common in
the early universe, and that their relative contributions within globular
clusters somehow scaled with the metallicity and mass of globular clusters.
The first of these classes is predominantly responsible for the CNO and
NeNa abundance variations, and likewise the second for the MgAl abundance
variations. Particularly striking examples of this dichotomy include 47 Tuc
and M4. As an auxiliary finding, we argue that abundance variations among
Terzan 5 stars are consistent with it being a normal globular cluster.
Description:
We use APOGEE and APOGEE-2 (Majewski et al. 2017AJ....154...94M 2017AJ....154...94M) data
products (stellar atmosphere parameters and abundances) from Data
Release 14 (DR14; Abolfathi et al. 2018ApJS..235...42A 2018ApJS..235...42A) of the Sloan
Digital Sky Survey (SDSS; Gunn et al. 2006AJ....131.2332G 2006AJ....131.2332G). APOGEE was
a component of SDSS-III (Eisenstein et al. 2011AJ....142...72E 2011AJ....142...72E), and
APOGEE-2 is part of SDSS-IV (Blanton et al. 2017AJ....154...28B 2017AJ....154...28B).
Observations were taken from the 2.5 m Sloan Telescope at Apache Point
Observatory (Gunn et al. 2006AJ....131.2332G 2006AJ....131.2332G), which is coupled to a
300-fiber, high-resolution (R∼22000) H-band spectrograph (Wilson et al.
2012SPIE.8446E..0HW). We make partial use of previously unpublished
APOGEE DR16 data. APOGEE targets were selected predominantly on the basis
of 2MASS photometry (Skrutskie et al. 2006, Cat. VII/233) to lie in the
brightness range 7~<H~<13.8.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 88 39 Parameters for the 28 globular clusters with
stars measured in APOGEE DR14 and 11 clusters
selected from DR16
table1.dat 98 1012 Parameters and abundances from the Payne for
the 1010 stars with spectra from APOGEE DR14 that
we associate with Galactic globular clusters
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See also:
VII/202 : Globular Clusters in the Milky Way (Harris, 1997)
VII/233 : The 2MASS Extended sources (IPAC/UMass, 2003-2006)
J/A+A/505/139 : Abundances of red giants in 17 globular clusters
(Carretta+, 2009)
J/AJ/146/133 : Stellar parameters from SDSS-III APOGEE DR10
(Meszaros+, 2013)
J/ApJ/808/16 : The Cannon: a new approach to determine abundances
(Ness+, 2015)
J/A+A/590/A9 : RGB stars in Galactic GC stellar parameters (Dias+, 2016)
J/AJ/151/144 : ASPCAP weights for the 15 APOGEE chemical elements
(Garcia+, 2016)
J/A+A/622/A191 : 885 globular cluster giants abundances (Masseron+, 2019)
J/MNRAS/482/5138 : Galactic GC mean proper motions & velocities
(Baumgardt+, 2019)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 A9 --- Cluster Cluster identifier
11 A1 --- n_Cluster [ab] Note on Cluster (1)
13- 18 A6 --- AName Alternative name of cluster
20- 24 F5.2 [-] [Fe/H] [-2.37/-0.11]? Metallicity
26- 32 F7.2 km/s RVmean [-244.4/494.3]? Mean radial velocity
34- 38 F5.2 km/s sigRV [0.6/19]? Radial velocity dispersion
40- 45 F6.2 mas/yr pmRA [-12.5/8.3]? Proper motion along RA
(µαcosδ)
47- 52 F6.2 mas/yr pmDE [-18.99/0.28]? Proper motion along DE
(µδ)
54- 57 F4.2 mas/yr e_pm [0.05/0.49]? Uncertainty in proper motion
59- 63 F5.2 arcmin rt [2.1/53.76]? Tidal radius
65- 68 F4.2 [Msun] logMGC [3.13/6.2]? Log globular cluster mass
log10(MGC/M☉)
70- 72 I3 --- NA [0/202]? Number of matches with a reported
[Fe/H] measurement from the APOGEE Stellar
Parameter and Abundances Pipeline (ASPCAP;
Garcia Perez et al. 2016, J/AJ/151/144)
74- 76 I3 --- NC [1/187]? Number of matches with a reported
[Fe/H] measurement from the Cannon pipeline
(Ness et al. 2015, J/ApJ/808/16; Casey et al.
2016arXiv160303040C 2016arXiv160303040C)
78- 80 I3 --- NP [0/214] Number of matches with a reported
[Fe/H] measurement from the Payne pipeline
(Ting et al. 2019ApJ...879...69T 2019ApJ...879...69T)
NP
82- 84 I3 --- NaNN [1/217]? Number of matches with a reported
[Fe/H] measurement from the AstroNN pipeline
(Leung & Bovy 2019MNRAS.483.3255L 2019MNRAS.483.3255L)
86- 88 I3 --- NB [26/218]? Number of matches with a reported
[Fe/H] measurement from the Brussels Automatic
Code for Characterizing HighaccUracy Spectra
pipeline (BACCHUS; Masseron et al.
2016ascl.soft05004M) (2)
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Note (1): Note as follows:
a = Total APOGEE DR14 values are: 844 (NA), 907 (NC), 659 (NP), 1012 (NaNN),
885 (NB);
b = Total APOGEE DR16 value is: 939 (NP).
Note (2): Similar applies for NB, for which the sample inclusion criteria are
different, and is described by Masseron et al. (2019, J/A+A/622/A191).
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Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 18 A18 --- APOGEE APOGEE identifier (2MHHMMSSss+DDMMSSs)
20- 30 F11.7 deg RAdeg Right Ascension in decimal degrees (J2000)
32- 42 F11.7 deg DEdeg Declination in decimal degrees (J2000)
44- 52 A9 --- Cluster Cluster identifier
54- 56 I3 --- S/N [5/888] Signal-to-noise ratio
58- 63 F6.1 K Teff [3255.9/7644.6]? Effective temperature (1)
65- 68 F4.2 [cm/s2] log(g) [0.33/4.33]? Log surface gravity (1)
70- 74 F5.2 [Sun] [Fe/H] [-1.45/0.24]? Metallicity (1)
76- 80 F5.2 [Sun] [C/H] [-2.24/0.39]? Log C/H abundance (1)
82- 86 F5.2 [Sun] [N/H] [-1.96/1.02]? Log N/H abundance (1)
88- 92 F5.2 [Sun] [O/H] [-2.09/0.79]? Log O/H abundance (1)
94- 98 F5.2 [Sun] [Al/H] [-2.48/0.48]? Log Al/H abundance (1)
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Note (1): Stars for which the Payne did not converge have parameters left blank.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 28-Aug-2019