J/MNRAS/475/1633 Photometric study of globular clusters (Meszaros+, 2018)
A photometric study of globular clusters observed by the APOGEE survey.
Meszaros S., Garcia-Hernandez D.A., Cassisi S., Monelli M., Szigeti L.,
Dell'Agli F., Derekas A., Masseron T., Shetrone M., Stetson P., Zamora O.
<Mon. Not. R. Astron. Soc., 475, 1633-1645 (2018)>
=2018MNRAS.475.1633M 2018MNRAS.475.1633M (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, globular ; Photometry, UBVRI ; Abundances
Keywords: stars: abundances - stars: AGB and post-AGB -
globular clusters: general
Abstract:
In this paper, we describe the photometric and spectroscopic
properties of multiple populations in seven northern globular
clusters. In this study, we employ precise ground-based photometry
from the private collection of Stetson, space photometry from the
Hubble Space Telescope (HST), literature abundances of Na and O, and
Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey
abundances for Mg, Al, C, and N. Multiple populations are identified
by their position in the CU,B,I-V pseudo colour-magnitude diagram
(pseudo-CMD) and confirmed with their chemical composition determined
using abundances. We confirm the expectation from previous studies
that the red giant branches (RGBs) in all seven clusters are split and
the different branches have different chemical compositions. The Mg-Al
anticorrelations were well explored by the APOGEE and Gaia-ESO surveys
for most globular clusters, some clusters showing bimodal
distributions, while others continuous distributions. Even though the
structure (i.e. bimodal versus continuous) of Mg-Al can greatly vary,
the Al-rich and Al-poor populations do not seem to have very different
photometric properties, agreeing with theoretical calculations. There
is no one-to-one correspondence between the Mg-Al anticorrelation
shape (bimodal versus continuous) and the structure of the RGB seen in
the HST pseudo-CMDs, with the HSTphotometric information usually
implying more complex formation/evolution histories than the
spectroscopic ones. We report on finding two second-generation
horizontal branch (HB) stars in M5, and five second-generation
asymptotic giant branch (AGB) stars in M92, which is the most
metal-poor cluster to date in which second-generation AGB stars have
been observed.
Description:
The ground-based U, B, V, R, I photometry was taken from the private
collection of Peter Stetson and is precise to the level of
<0.002mag in the U band and to <0.001mag for the other bands.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 128 357 Ground-based photometry and atmospheric
parameters and abundances from
Meszaros et al., 2015, Cat. J/AJ/149/153
table3.dat 76 329 Photometric and abundances parameters collected
from the literature
table5.dat 88 37 HST photometry and abundances from
Meszaros et al., 2015, J/AJ/149/153
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See also:
J/AJ/149/153 : Abundances of red giants in 10 globular clusters
(Meszaros+, 2015)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- --- [2M]
3- 18 A16 --- 2MASS 2MASS ID, HHMMSSss+DDMMSSs
20- 22 A3 --- Cluster Cluster ID
24- 29 I6 --- PhotID Photometric ID
31- 36 F6.3 mag Umag U magnitude
38- 43 F6.3 mag Bmag B magnitude
45- 50 F6.3 mag Vmag V magnitude
52- 57 F6.3 mag Rmag ?=99.999 R magnitude
59- 64 F6.3 mag Imag I magnitude
66- 69 I4 K Teff Effective temperature
71- 74 F4.2 [cm/s2] logg Surface gravity
76- 80 F5.2 [-] [Fe/H] Metallicity
82- 86 F5.2 [-] [C/Fe] ?=99.99 Abundance [C/Fe]
88- 92 F5.2 [-] [N/Fe] ?=99.99 Abundance [N/Fe]
94- 98 F5.2 [-] [O/Fe] ?=99.99 Abundance [O/Fe]
100-104 F5.2 [-] [Mg/Fe] ?=99.99 Abundance [Mg/Fe]
106-110 F5.2 [-] [Al/Fe] ?=99.99 Abundance [Al/Fe]
112-116 F5.2 [-] [Si/Fe] ?=99.99 Abundance [Si/Fe]
118-122 F5.2 [-] [Ca/Fe] ?=99.99 Abundance [Ca/Fe]
124-128 F5.2 [-] [Ti/Fe] ?=99.99 Abundance [Ti/Fe]
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 A2 --- --- [2M]
3- 18 A16 --- 2MASS 2MASS ID, HHMMSSss+DDMMSSs
20- 25 F6.3 mag Umag U magnitude
27- 32 F6.3 mag Bmag B magnitude
34- 39 F6.3 mag Vmag V magnitude
41- 46 F6.3 mag Rmag ?=99.999 R magnitude
48- 53 F6.3 mag Imag I magnitude
55- 60 F6.3 [-] [Fe/H] Metallicity
62- 67 F6.3 [-] [O/Fe] ?=99.99 Abundance [O/Fe]
69- 74 F6.3 [-] [Na/Fe] ?=99.99 Abundance [Na/Fe], NLTE corrected when
it is available in the source
76 A1 --- Ref Literature source (1)
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Note (1): Literature source as follows:
a = Carretta et al. (2009A&A...505..117C 2009A&A...505..117C, Cat. J/A+A/505/117)
b = Sneden et al. (1997AJ....114.1964S 1997AJ....114.1964S)
c = Sobeck et al. (2011AJ....141..175S 2011AJ....141..175S, Cat. J/AJ/141/175)
d = Meszaros et al. (2015AJ....149..153M 2015AJ....149..153M, Cat. J/AJ/149/153)
e = Johnson & Pilachowski (2012ApJ...754L..38J 2012ApJ...754L..38J, Cat. J/ApJ/754/L38)
f = Cohen & Melendez (2005AJ....129..303C 2005AJ....129..303C, Cat. J/AJ/129/303)
g = Kraft et al. (1992AJ....104..645K 1992AJ....104..645K)
h = Sneden et al. (2004AJ....127.2162S 2004AJ....127.2162S)
i = Cavallo & Nagar (2000AJ....120.1364C 2000AJ....120.1364C, Cat. J/AJ/120/1364)
j = Sneden et al. (1992AJ....104.2121S 1992AJ....104.2121S)
k = Ivans et al. (2001AJ....122.1438I 2001AJ....122.1438I)
l = Lai et al. (2011AJ....141...62L 2011AJ....141...62L, Cat. J/AJ/141/62)
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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- 2 A2 --- --- [2M]
3- 18 A16 --- 2MASS 2MASS ID, HHMMSSss+DDMMSSs
20- 24 A5 --- Cluster Cluster ID
26- 31 F6.3 mag F275W HST F275W magnitude
33- 38 F6.3 mag F335W HST F335W magnitude
40- 45 F6.3 mag F438W HST F438W magnitude
47- 52 I6 --- HST HST ID
54- 58 F5.2 [-] [Fe/H] Metallicity
60- 64 F5.2 [-] [C/Fe] ?=99.99 Abundance [C/Fe]
66- 70 F5.2 [-] [N/Fe] ?=99.99 Abundance [N/Fe]
72- 76 F5.2 [-] [O/Fe] ?=99.99 Abundance [O/Fe]
78- 82 F5.2 [-] [Mg/Fe] Abundance [Mg/Fe]
84- 88 F5.2 [-] [Al/Fe] Abundance [Al/Fe]
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 06-Apr-2021