J/AJ/156/94 APOGEE and Gaia DR2 analysis of IC 166 (Schiappacasse-Ulloa+, 2018)
A chemical and kinematical analysis of the intermediate-age open cluster IC 166
from APOGEE and Gaia DR2.
Schiappacasse-Ulloa J., Tang B., Fernandez-Trincado J.G., Zamora O.,
Geisler D., Frinchaboy P., Schultheis M., Dell'Agli F., Villanova S.,
Masseron T., Meszaros S., Souto D., Hasselquist S., Cunha K., Smith V.V.,
Garcia-Hernandez D.A., Vieira K., Robin A.C., Minniti D., Zasowski G.,
Moreno E., Perez-Villegas A., Lane R.R., Ivans I.I., Pan K., Nitschelm C.,
Santana F.A., Carrera R., Roman-Lopes A.
<Astron. J., 156, 94-94 (2018)>
=2018AJ....156...94S 2018AJ....156...94S (SIMBAD/NED BibCode)
ADC_Keywords: Milky Way ; Clusters, open ; Populations, stellar ;
Photometry, infrared ; Effective temperatures ; Abundances ;
Parallaxes, trigonometric ; Radial velocities ; Proper motions
Keywords: Galaxy: abundances - Galaxy: kinematics and dynamics -
open clusters and associations: individual: IC 166
Abstract:
IC 166 is an intermediate-age open cluster (OC) (∼1 Gyr) that lies in
the transition zone of the metallicity gradient in the outer disk. Its
location, combined with our very limited knowledge of its salient
features, make it an interesting object of study. We present the first
high-resolution spectroscopic and precise kinematical analysis of IC 166,
which lies in the outer disk with RGC∼12.7 kpc. High-resolution
H-band spectra were analyzed using observations from the SDSS-IV Apache
Point Observatory Galactic Evolution Experiment survey. We made use of
the Brussels Automatic Stellar Parameter code to provide chemical
abundances based on a line-by-line approach for up to eight chemical
elements (Mg, Si, Ca, Ti, Al, K, Mn, and Fe). The α-element (Mg,
Si, Ca, and whenever available Ti) abundances, and their trends with
Fe abundances have been analyzed for a total of 13 high-likelihood
cluster members. No significant abundance scatter was found in any of
the chemical species studied. Combining the positional, heliocentric
distance, and kinematic information, we derive, for the first time,
the probable orbit of IC 166 within a Galactic model including a rotating
boxy bar, and found that it is likely that IC 166 formed in the Galactic
disk, supporting its nature as an unremarkable Galactic OC with an orbit
bound to the Galactic plane.
Description:
In this work, we provide an independent abundance determination of
several chemical species in the OC IC 166 using the Brussels Automatic
Code for Characterizing High accUracy Spectra (BACCHUS; Masseron et al.
2016ascl.soft05004M), and compare them with the Apogee Stellar Parameter
and Chemical Abundances Pipeline (ASPCAP; Garcia Perez et al. 2016,
J/AJ/151/144).
The APOGEE (Majewski et al. 2017AJ....154...94M 2017AJ....154...94M) is one of the projects
operating as part of the Sloan Digital Sky Survey IV (Blanton et al.
2017AJ....154...28B 2017AJ....154...28B; Abolfathi et al. 2018ApJS..235...42A 2018ApJS..235...42A), aiming to
characterize the MW Galaxy's formation and evolution through a precise,
systematic and large-scale kinematic and chemical study. The APOGEE
instrument is a near-infrared (λ=1.51-1.70 µm) high-resolution
(R∼22500) multi-object spectrograph (Wilson et al. 2012SPIE.8446E..0HW)
mounted at the SDSS 2.5 m telescope (Gunn et al. 2006AJ....131.2332G 2006AJ....131.2332G),
with a copy now operating in the South at Las Campanas Observatory - the
2.5 m Irenee du Pont telescope. The APOGEE survey has observed more than
270000 stars across all of the main components of the MW (Zasowski et al.
2013AJ....146...81Z 2013AJ....146...81Z, 2017AJ....154..198Z 2017AJ....154..198Z), achieving a typical spectral
signal-to-noise ratio (S/N)>100 per pixel. The latest data release (DR14;
Abolfathi et al. 2018ApJS..235...42A 2018ApJS..235...42A) includes all of the APOGEE-1 data
and APOGEE data taken between 2014 July and 2016 July. A number of
candidate member stars of the OC IC 166 were observed by the APOGEE
survey, and their spectra were released for the first time as part of
the DR14 (Abolfathi et al. 2018ApJS..235...42A 2018ApJS..235...42A).
Objects:
----------------------------------------------------
RA (ICRS) DE Designation(s)
----------------------------------------------------
01 52 23 +61 51.9 IC 166 = Cl Tombaugh 3
----------------------------------------------------
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 58 13 Summary table of likely members of IC 166
table2.dat 44 13 Stellar parameters obtained from FERRE/MARCS
table5.dat 96 13 IC 166 data sample from Gaia DR2 and APOGEE
table7.dat 159 49 Atomic lines used and derived abundances
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See also:
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
J/AJ/144/95 : Abundance in stars of the outer galactic disk. IV.
(Yong+, 2012)
J/PAZh/38/571 : Astrophysical parameters for 593 open clusters
(Gozha+, 2012)
J/A+A/564/A79 : Proper motions of open clusters from UCAC4 (Dias+, 2014)
J/A+A/585/A101 : Milky Way global survey of star clusters. V.
(Kharchenko+, 2016)
J/AJ/151/144 : ASPCAP weights for the 15 APOGEE chemical elements
(Garcia+, 2016)
J/AZh/93/49 : Abundances in Galactic open clusters (Marsakov+, 2016)
J/A+A/618/A93 : Gaia DR2 open clusters in the Milky Way (Cantat-Gaudin+, 2018)
J/A+A/619/A155 : Open cluster kinematics with Gaia DR2 (Soubiran+, 2018)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 18 A18 --- APOGEE APOGEE identifier (2MHHMMSSss+DDMMSSs)
20- 21 I2 --- Star [1/13] Star number
23- 31 F9.6 deg RAdeg Right Ascension in decimal degrees (J2000)
33- 41 F9.6 deg DEdeg Declination in decimal degrees (J2000)
43- 48 F6.3 mag Jmag [12.649/13.487] 2MASS J band magnitude
50- 55 F6.3 mag Ksmag [11.603/12.503] 2MASS Ks band magnitude
57- 58 I2 % Memb [63/96]? Membership probability from Dias et al.
(2014, J/A+A/564/A79)
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Star [1/13] Star number
4- 7 I4 K Teff [4825/5170] Effective temperature from this work
9- 12 F4.2 [cm/s2] logg [2.87/3.22] Surface gravity from this work
14- 18 F5.2 [-] [Fe/H] [-0.11/-0.01] Metallicity from this work
20- 23 F4.2 km/s ksi [0.93/1.69] Microturbulent velocity from this
work ξ
25- 28 I4 K TeffA [4775/5175] Effective temperature from ASPCAP
30- 33 F4.2 [cm/s2] loggA [2.75/3.15] Surface gravity from ASPCAP
35- 39 F5.2 [-] [Fe/H]A [-0.09/-0.03] Metallicity from ASPCAP
41- 44 F4.2 km/s ksiA [1.1/1.7] Microturbulent velocity from ASPCAP
ξ
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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- 18 A18 --- APOGEE APOGEE identifier (2MHHMMSSss+DDMMSSs)
20- 21 I2 --- Star [1/13] Star number (from Table 1)
23- 24 I2 h RAh Hour of Right Ascension (J2000)
26- 27 I2 min RAm Minute of Right Ascension (J2000)
29- 33 F5.2 s RAs Second of Right Ascension (J2000)
35 A1 --- DE- Sign of the Declination (J2000)
36- 37 I2 deg DEd Degree of Declination (J2000)
39- 40 I2 arcmin DEm Arcminute of Declination (J2000)
42- 45 F4.1 arcsec DEs Arcsecond of Declination (J2000)
47- 51 F5.3 mas Plx [0.092/0.305] Parallax
53- 57 F5.3 mas e_Plx [0.034/0.059] Uncertainty in Plx
59- 65 F7.3 km/s RV [-44.142/-37.449] Radial velocity
67- 71 F5.3 km/s e_RV [0.033/0.688] Uncertainty in RV
73- 78 F6.3 mas/yr pmRA [-1.58/-1.236] Proper motion in right ascension
direction (pmRA*cosDE)
80- 84 F5.3 mas/yr e_pmRA [0.036/0.065] Uncertainty in pmRA
86- 90 F5.3 mas/yr pmDE [0.996/1.291] Proper motion in declination
direction
92- 96 F5.3 mas/yr e_pmDE [0.05/0.088] Uncertainty in pmDE
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- El Element(s)
9- 16 F8.2 0.1nm lambda [15159.2/16828.2]? Wavelength in air
λair (Å)
18- 22 F5.2 [-] Abund1 [-0.16/7.64]? Abundance for star 1
24- 27 F4.2 [-] e_Abund1 [0.01/0.14]? Uncertainty in Abund1
29- 33 F5.2 [-] Abund2 [-0.25/7.73]? Abundance for star 2
35- 38 F4.2 [-] e_Abund2 [0.03/0.14]? Uncertainty in Abund2
40- 44 F5.2 [-] Abund3 [-0.16/7.55]? Abundance for star 3
46- 49 F4.2 [-] e_Abund3 [0.01/0.18]? Uncertainty in Abund3
51- 55 F5.2 [-] Abund4 [-0.23/7.79]? Abundance for star 4
57- 60 F4.2 [-] e_Abund4 [0.04/0.15]? Uncertainty in Abund4
62- 66 F5.2 [-] Abund5 [-0.19/7.73]? Abundance for star 5
68- 71 F4.2 [-] e_Abund5 [0.02/0.1]? Uncertainty in Abund5
73- 77 F5.2 [-] Abund6 [-0.19/7.73]? Abundance for star 6
79- 82 F4.2 [-] e_Abund6 [0.01/0.13]? Uncertainty in Abund6
84- 88 F5.2 [-] Abund7 [-0.17/7.59]? Abundance for star 7
90- 93 F4.2 [-] e_Abund7 [0.04/0.1]? Uncertainty in Abund7
95- 99 F5.2 [-] Abund8 [-0.23/7.55]? Abundance for star 8
101-104 F4.2 [-] e_Abund8 [0.03/0.14]? Uncertainty in Abund8
106-110 F5.2 [-] Abund9 [-0.22/7.56]? Abundance for star 9
112-115 F4.2 [-] e_Abund9 [0.04/0.18]? Uncertainty in Abund9
117-121 F5.2 [-] Abund10 [-0.18/7.74]? Abundance for star 10
123-126 F4.2 [-] e_Abund10 [0.01/0.11]? Uncertainty in Abund10
128-132 F5.2 [-] Abund11 [-0.17/7.66]? Abundance for star 11
134-137 F4.2 [-] e_Abund11 [0.02/0.13]? Uncertainty in Abund11
139-143 F5.2 [-] Abund12 [-0.13/7.88]? Abundance for star 12
145-148 F4.2 [-] e_Abund12 [0.01/0.2]? Uncertainty in Abund12
150-154 F5.2 [-] Abund13 [-0.17/7.55]? Abundance for star 13
156-159 F4.2 [-] e_Abund13 [0.04/0.13]? Uncertainty in Abund13
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History:
From electronic version of the journal
(End) Tiphaine Pouvreau [CDS] 01-Mar-2019