2019A&A...629A..34G


Query : 2019A&A...629A..34G

2019A&A...629A..34G - Astronomy and Astrophysics, volume 629A34-34 (2019/9-1)

Machine learning in APOGEE. Identification of stellar populations through chemical abundances.

GARCIA-DIAS R., ALLENDE PRIETO C., SANCHEZ ALMEIDA J. and PALICIO P.A.

Abstract (from CDS):


Context. The vast volume of data generated by modern astronomical surveys offers test beds for the application of machine-learning. In these exploratory applications, it is important to evaluate potential existing tools and determine those that are optimal for extracting scientific knowledge from the available observations.
Aims. We explore the possibility of using unsupervised clustering algorithms to separate stellar populations with distinct chemical patterns.
Methods. Star clusters are likely the most chemically homogeneous populations in the Galaxy, and therefore any practical approach to identifying distinct stellar populations should at least be able to separate clusters from each other. We have applied eight clustering algorithms combined with four dimensionality reduction strategies to automatically distinguish stellar clusters using chemical abundances of 13 elements. Our test-bed sample includes 18 stellar clusters with a total of 453 stars.
Results. We have applied statistical tests showing that some pairs of clusters (e.g., NGC 2458-NGC 2420) are indistinguishable from each other when chemical abundances from the Apache Point Galactic Evolution Experiment (APOGEE) are used. However, for most clusters we are able to automatically assign membership with metric scores similar to previous works. The confusion level of the automatically selected clusters is consistent with statistical tests that demonstrate the impossibility of perfectly distinguishing all the clusters from each other. These statistical tests and confusion levels establish a limit for the prospect of blindly identifying stars born in the same cluster based solely on chemical abundances. Conclusion. We find that some of the algorithms we explored are capable of blindly identify stellar populations with similar ages and chemical distributions in the APOGEE data. Even though we are not able to fully separate the clusters from each other, the main confusion arises from clusters with similar ages. Because some stellar clusters are chemically indistinguishable, our study supports the notion of extending weak chemical tagging that involves families of clusters instead of individual clusters.

Abstract Copyright: © ESO 2019

Journal keyword(s): open clusters and associations: general - globular clusters: general - Galaxy: abundances - methods: numerical - methods: statistical - methods: data analysis

VizieR on-line data: <Available at CDS (J/A+A/629/A34): table1.dat>

Status at CDS : All or part of tables of objects will not be ingested in SIMBAD.

Simbad objects: 31

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Number of rows : 31
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026
#notes
1 [FSR2007] 0494 OpC 00 25 38.2 +63 45 22           ~ 33 0
2 NGC 188 OpC 00 47 14.8 +85 14 42           ~ 990 0
3 Cl Berkeley 5 OpC 01 47 43.0 +62 56 23           ~ 17 0
4 IC 166 OpC 01 52 21.3 +61 51 29   13.0 11.7     ~ 98 0
5 Cl Berkeley 66 OpC 03 04 06.9 +58 44 14           ~ 74 0
6 Cl King 5 OpC 03 14 43.6 +52 41 52           ~ 84 0
7 NGC 1245 OpC 03 14 44.3 +47 14 06   9.16 8.4     ~ 171 0
8 Cl Melotte 22 OpC 03 46 38.0 +24 10 41           ~ 3679 0
9 Cl King 7 OpC 03 59 08.0 +51 47 11           ~ 74 0
10 NGC 1798 OpC 05 11 39.3 +47 41 28           ~ 85 0
11 Cl Berkeley 17 OpC 05 20 30.5 +30 34 20           ~ 192 0
12 Cl Berkeley 71 OpC 05 40 56.7 +32 16 11           ~ 49 0
13 NGC 2158 OpC 06 07 26.7 +24 05 53           ~ 317 0
14 NGC 2420 OpC 07 38 24.6 +21 34 26   9.0 8.3     ~ 523 0
15 NGC 2458 G 07 55 51.3884683920 +56 42 38.265036048   16       ~ 14 0
16 NGC 2682 OpC 08 51 23.5 +11 48 54           ~ 2528 0
17 M 3 GlC 13 42 11.62 +28 22 38.2     6.39     ~ 2593 0
18 M 5 GlC 15 18 33.22 +02 04 51.7     5.95     ~ 2095 0
19 M 107 GlC 16 32 31.86 -13 03 13.6           ~ 835 0
20 M 13 GlC 16 41 41.634 +36 27 40.75     5.8     ~ 2291 0
21 M 92 GlC 17 17 07.39 +43 08 09.4     6.52     ~ 2240 0
22 M 9 GlC 17 19 11.78 -18 30 58.5   9.36 8.42     ~ 348 0
23 NGC 6405 OpC 17 40 14.5 -32 14 16           ~ 235 0
24 NGC 6475 OpC 17 53 44.1 -34 49 36           ~ 413 0
25 NAME SDG G 18 55 19.0 -30 32 43   4.5 3.6     ~ 2438 2
26 NGC 6791 OpC 19 20 52.8 +37 46 40   10.52 9.5     ~ 1120 0
27 NGC 6819 OpC 19 41 18.3 +40 11 19   8.21 7.3     ~ 719 0
28 M 71 GlC 19 53 46.49 +18 46 45.1           ~ 1190 0
29 Cl Berkeley 53 OpC 20 55 54.8 +51 03 30           ~ 43 0
30 M 15 GlC 21 29 58.33 +12 10 01.2           ~ 3274 0
31 NGC 7789 OpC 23 57 19.4 +56 43 28   7.68 6.7     ~ 575 0

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