J/AJ/156/142 Precision cluster abund. for APOGEE using SDSS DR14 (Donor+, 2018)
The Open Cluster Chemical Abundances and Mapping survey.
II. Precision cluster abundances for APOGEE using SDSS DR14.
Donor J., Frinchaboy P.M., Cunha K., Thompson B., O'Connell J., Zasowski G.,
Jackson K.M., McGrath B.M., Almeida A., Bizyaev D., Carrera R.,
Garcia-Hernandez D.A., Nitschelm C., Pan K., Zamora O.
<Astron. J., 156, 142 (2018)>
=2018AJ....156..142D 2018AJ....156..142D (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, open ; Populations, stellar ; Radial velocities ;
Abundances ; Proper motions ; Milky Way
Keywords: Galaxy: abundances - Galaxy: disk - Galaxy: evolution -
open clusters and associations: general
Abstract:
The Open Cluster Chemical Abundances and Mapping (OCCAM) survey aims
to produce a comprehensive, uniform, infrared-based spectroscopic data set
for hundreds of open clusters, and to constrain key Galactic dynamical
and chemical parameters from this sample. This second contribution from
the OCCAM survey presents analysis of 259 member stars with [Fe/H]
determinations in 19 open clusters, using Sloan Digital Sky Survey Data
Release 14 (SDSS/DR14) data from the Apache Point Observatory Galactic
Evolution Experiment and ESA Gaia. This analysis, which includes clusters
with RGC ranging from 7 to 13 kpc, measures an [Fe/H] gradient of
-0.061±0.004 dex/kpc. We also confirm evidence of a significant positive
gradient in the α-elements ([O/Fe], [Mg/Fe], and [Si/Fe]) and
present evidence for a significant negative gradient in iron-peak elements
([Mn/Fe] and [Ni/Fe]).
Description:
The primary spectroscopic data for OCCAM comes from the APOGEE
(Majewski et al. 2017AJ....154...94M 2017AJ....154...94M), which is part of the Sloan Digital
Sky Survey-III and IV surveys (SDSS; Eisenstein et al. 2011AJ....142...72E 2011AJ....142...72E;
Blanton et al. 2017AJ....154...28B 2017AJ....154...28B), utilizing the 2.5 m Sloan Foundation
telescope (Gunn et al. 2006AJ....131.2332G 2006AJ....131.2332G) at Apache Point Observatory.
APOGEE is a near-infrared (1.514-1.696 µm) spectroscopic survey,
primarily focusing on the Galactic disk (Zasowski et al.
2013AJ....146...81Z 2013AJ....146...81Z, 2017AJ....154..198Z 2017AJ....154..198Z). The survey uses multi-fiber
spectrographs (Wilson et al. 2012SPIE.8446E..0HW), allowing for
simultaneous observations of 300 stars.
The targets selected for analysis were observed from 2011 August to
2014 July (APOGEE-1), and from 2014 July to 2016 July (APOGEE-2). These
data were released as part of the 14th Data Release of SDSS (DR14;
Abolfathi et al. 2018ApJS..235...42A 2018ApJS..235...42A), which included APOGEE data for over
250000 stars. For this study, we analyzed all stars within 2x the cluster
radius (Kharchenko et al. 2013, J/A+A/558/A53) for 19 clusters that
resulted in a sample of 1361 stars.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 93 19 OCCAM data sample
table3.dat 35 19 RGC calculated using different distance sources
table5.dat 161 19 OCCAM DR14 cluster abundances
table1.dat 99 1361 OCCAM sample from APOGEE data used for membership
analysis
table6.dat 161 260 DR14 OCAAM open cluster member star abundances
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See also:
B/ocl : Optically visible open clusters and Candidates (Dias+ 2002-2015)
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
I/347 : Distances to 1.33 billion stars in Gaia DR2 (Bailer-Jones+, 2018)
J/AJ/125/1397 : Kinematics, age and abundances of open clusters (Chen+, 2003)
J/A+A/431/933 : Abundances of NGC 7789 evolved stars (Tautvaisiene+, 2005)
J/AJ/136/118 : Open clusters as galactic disk tracers. I. (Frinchaboy+, 2008)
J/A+A/511/A56 : Abundances of five open clusters (Pancino+, 2010)
J/AJ/142/59 : Chemical abundance in 10 open clusters (Jacobson+, 2011)
J/A+A/558/A53 : Milky Way global survey of star clusters. II.
(Kharchenko+, 2013)
J/AJ/149/15 : Spectroscopy of NGC 7789 (Overbeek+, 2015)
J/AJ/149/121 : WOCS. LXV. Abundances in NGC 6819 (Lee-Brown+, 2015)
J/A+A/585/A150 : On the metallicity of open clusters. III. (Netopil+, 2016)
J/ApJ/824/75 : Abundances in 23 open clusters. I. (Overbeek+, 2016)
J/AZh/93/49 : Abundances in Galactic open clusters (Marsakov+, 2016)
J/AJ/156/94 : APOGEE and Gaia DR2 analysis of IC 166
(Schiappacasse- Ulloa+, 2018)
J/A+A/623/A80 : Open clusters in APOGEE and GALAH surveys (Carrera+, 2019)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Name Cluster name
12 A1 --- f_Name [*] Flag on Name (1)
14- 21 F8.4 deg GLON [69.9658/215.691] Galactic longitude
23- 30 F8.4 deg GLAT [-8.9081/31.9221] Galactic latitude
32- 35 F4.1 arcmin Rad [2.7/33] Cluster radius (2)
37- 40 F4.2 Gyr Age [0.53/4.47] Cluster age (2)
42- 46 F5.2 kpc RGC [7.7/12.5] Distance to the Galactic center RGC
(3)
48- 53 F6.2 mas/yr pmRA [-10.97/2.55] Proper motion along RA
(pmRA*cosDE) (4)
55- 58 F4.2 mas/yr e_pmRA [0.15/0.61] 1σ uncertainty in pmRA (4)
60- 64 F5.2 mas/yr pmDE [-8.78/1.13] Proper motion along DE (4)
66- 69 F4.2 mas/yr e_pmDE [0.16/0.69] 1σ uncertainty in pmDE (4)
71- 75 F5.1 km/s RV [-73.4/74.2] Radial velocity
77- 79 F3.1 km/s e_RV [0.3/2.3] Uncertainty in RV
81- 85 F5.2 [-] [Fe/H] [-0.28/0.42] Metallicity (in dex)
87- 90 F4.2 [-] e_[Fe/H] [0.02/0.05] Uncertainty in [Fe/H] (in dex)
92- 93 I2 --- NSt6 [4/36] Number of member stars (see Table 6)
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Note (1): Flag as follows:
* = A separate analysis of APOGEE data for the open cluster IC 166 found 13
member stars and an average [Fe/H] of -0.08±0.05. These results can be
found in Schiappacasse-Ulloa et al. (2018, J/AJ/156/94).
Note (2): From Kharchenko et al. (2013, J/A+A/558/A53).
Note (3): Calculated using Bailer-Jones et al. (2018, Cat. I/347) with a solar
RGC=8 kpc.
Note (4): Proper motions and their 1σ uncertainties are those of the 2D
Gaussian fit, discussed in Section 3.2.
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Name Cluster name
13- 17 F5.2 kpc R(Dias) [7.69/13.05] Distance to the Galactic center using
the Dias Catalog (Dias et al. 2002, Cat. B/ocl)
19- 23 F5.2 kpc R(MWSC) [7.69/14.08] Distance to the Galactic center using
the MWSC Catalog (Kharchenko et al. 2013,
J/A+A/558/A53)
25- 29 F5.2 kpc R(Plx) [7.57/11.7] Distance to the Galactic center using
the inverse-parallax (1)
31- 35 F5.2 kpc R(B-J) [7.7/12.5] Distance to the Galactic center using
the Bailer-Jones catalog (Bailer-Jones et al.
2018, Cat. I/347)
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Note (1): From Gaia Collaboration et al. 2018A&A...616A...1G 2018A&A...616A...1G; Lindegren et al.
2018A&A...616A...2L 2018A&A...616A...2L, Cat. I/345, accounting for a 0.08 mas offset
(Stassun & Torres 2018ApJ...862...61S 2018ApJ...862...61S).
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Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Name Cluster name
13- 30 A18 --- 2MASS 2MASS identifier (2MHHMMSSss+DDMMSSs)
32- 37 F6.1 km/s HRV [-210.7/357.1] Heliocentric radial velocity
39- 43 F5.1 km/s e_HRV [0/103] Uncertainty in HRV
45- 49 F5.2 [Sun] [Fe/H] [-2.14/0.54] APOGEE [Fe/H]
51- 54 F4.2 [Sun] e_[Fe/H] [0.01/0.02] Uncertainty in [Fe/H]
56- 62 F7.2 mas/yr pmRA [-229.06/371.7] Gaia DR2 proper motion along RA
(pmRA*cosDE)
64- 67 F4.2 mas/yr e_pmRA [0.02/1.73] Uncertainty in pmRA
69- 75 F7.2 mas/yr pmDE [-215.79/99.82] Gaia DR2 proper motion along DE
77- 80 F4.2 mas/yr e_pmDE [0.02/1.99] Uncertainty in pmDE
82- 85 F4.2 --- P(RV) [0/1] Membership probability in RV
87- 91 F5.2 --- P(Fe/H) [-1/1] Membership probability in [Fe/H] (1)
93- 96 F4.2 --- P(pm) [0/1] Membership probability in proper motion
98- 99 A2 --- Memb OCCAM membership determination (2)
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Note (1): A [Fe/H] membership probability of -1 corresponds to a check against
log(g) for [Fe/H] reliability. Stars which failed may be members, but are
flagged because [Fe/H] is not a reliable membership discriminator for these
stars.
Note (2): Options for membership are as follows:
GM = Giant member;
DM = Dwarf member;
NM = Non-member.
We differentiate between giants and dwarfs due the log(g) cut mentioned: these
dwarfs may be members, but their metallicities may not be reliable.
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Byte-by-byte Description of file: table5.dat table6.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Name Cluster name
13- 30 A18 --- 2MASS 2MASS identifier (2MHHMMSSss+DDMMSSs) (only
in Table 6)
32- 36 F5.1 km/s HRV [-74.2/75.1]? Heliocentric radial velocity
(only in Table 6)
38- 40 F3.1 km/s e_HRV [0/6.8]? Uncertainty in HRV (only in Table 6)
42- 46 F5.2 [Sun] [Fe/H] [-0.32/0.54]? APOGEE [Fe/H] (only in Table 6)
48- 51 F4.2 [Sun] e_[Fe/H] [0.01/0.01]? Uncertainty in [Fe/H] (only in
Table 6)
53- 57 F5.2 [Sun] [O/Fe] [-0.17/0.24] APOGEE [O/Fe]
59- 62 F4.2 [Sun] e_[O/Fe] [0.01/0.1] Uncertainty in [O/Fe]
64- 68 F5.2 [Sun] [Mg/Fe] [-0.13/0.14] APOGEE [Mg/Fe]
70- 73 F4.2 [Sun] e_[Mg/Fe] [0.01/0.06] Uncertainty in [Mg/Fe]
75- 79 F5.2 [Sun] [Ca/Fe] [-0.07/0.27] APOGEE [Ca/Fe]
81- 84 F4.2 [Sun] e_[Ca/Fe] [0.01/0.06] Uncertainty in [Ca/Fe]
86- 90 F5.2 [Sun] [Si/Fe] [-0.16/0.22] APOGEE [Si/Fe]
92- 95 F4.2 [Sun] e_[Si/Fe] [0.01/0.06] Uncertainty in [Si/Fe]
97-101 F5.2 [Sun] [S/Fe] [-0.2/0.31] APOGEE [S/Fe]
103-106 F4.2 [Sun] e_[S/Fe] [0.04/0.14] Uncertainty in [S/Fe]
108-112 F5.2 [Sun] [V/Fe] [-0.57/0.53]?=-9.99 APOGEE [V/Fe]
114-117 F4.2 [Sun] e_[V/Fe] [0.04/0.27]?=9.99 Uncertainty in [V/Fe]
119-123 F5.2 [Sun] [Cr/Fe] [-0.27/0.15] APOGEE [Cr/Fe]
125-128 F4.2 [Sun] e_[Cr/Fe] [0.02/0.12] Uncertainty in [Cr/Fe]
130-134 F5.2 [Sun] [Mn/Fe] [-0.38/0.22] APOGEE [Mn/Fe]
136-139 F4.2 [Sun] e_[Mn/Fe] [0.01/0.14] Uncertainty in [Mn/Fe]
141-145 F5.2 [Sun] [Co/Fe] [-2.27/0.59]?=-9.99 APOGEE [Co/Fe]
147-150 F4.2 [Sun] e_[Co/Fe] [0.03/0.7]?=9.99 Uncertainty in [Co/Fe]
152-156 F5.2 [Sun] [Ni/Fe] [-0.12/0.09] APOGEE [Ni/Fe]
158-161 F4.2 [Sun] e_[Ni/Fe] [0.01/0.05] Uncertainty in [Ni/Fe]
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History:
From electronic version of the journal
References:
O'Connell et al. Paper III. 2018 AJ submitted
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 08-Mar-2019