J/ApJ/808/103 Kapteyn moving group star abundances (Navarrete+, 2015)
The Kapteyn moving group is not tidal debris from ω Centauri.
Navarrete C., Chaname J., Ramirez I., Meza A., Anglada-Escude G.,
Shkolnik E.
<Astrophys. J., 808, 103 (2015)>
=2015ApJ...808..103N 2015ApJ...808..103N (SIMBAD/NED BibCode)
ADC_Keywords: Abundances ; Equivalent widths ; Clusters, globular ;
Radial velocities
Keywords: Galaxy: halo; globular clusters: individual: NGC 5139;
stars: abundances
Abstract:
The Kapteyn moving group has been postulated as tidal debris from
ω Centauri. If true, members of the group should show some of
the chemical abundance patterns known for stars in the cluster. We
present an optical and near-infrared high-resolution,
high-signal-to-noise ratio spectroscopic study of 14 stars of the
Kapteyn group, plus 10 additional stars (the ω Cen group) that,
while not listed as members of the Kapteyn group as originally
defined, have nevertheless been associated dynamically with ω
Centauri. Abundances for Na, O, Mg, Al, Ca, and Ba were derived from
the optical spectra, while the strength of the chromospheric
HeI10830Å line is studied as a possible helium abundance indicator.
The resulting Na-O and Mg-Al patterns for stars of the combined
Kapteyn and ω Cen group samples do not resemble those of ω
Centauri, and are not different from those of field stars of the
Galactic halo. The distribution of equivalent widths of the
HeI10830Å line is consistent with that found among non-active field
stars. Therefore, no evidence is found for second-generation stars
within our samples, which most likely rules out a globular-cluster
origin. Moreover, no hint of the unique barium overabundance at the
metal-rich end, well established for ω Centauri stars, is seen
among stars of the combined samples. Because this specific Ba pattern
is present in ω Centauri irrespective of stellar generation,
this would rule out the possibility that our entire sample might be
composed of only first-generation stars from the cluster. Finally, for
the stars of the Kapteyn group, the possibility of an origin in the
hypothetical parent galaxy of ω Centauri is disfavored by the
different run of α-elements with metallicity between our targets
and stars from present-day dwarf galaxies.
Description:
Optical spectroscopic observations of our sample stars were carried
out using the MIKE spectrograph on the 6.5m Magellan/Clay Telescope
at Las Campanas Observatory (R∼83000 and 65000 in the blue and red
CCDs, respectively). The full wavelength range covered by the standard
setup of the MIKE spectrograph is 320-1000nm. The S/N of our spectra
varies from star to star, but it is typically in the range from 150 to
200 per pixel at 6000Å.
High-resolution, high-S/N near-infrared spectra for the target stars
were collected using the CRIRES mounted on the VLT UT1 telescope. The
observations were carried out in Service Mode (Program 090.B-0605(B),
29hr, P.I. J.C.) from 2011 October through 2012 March (R∼50000).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 58 45 Spectroscopic stellar parameters of our target stars
table4.dat 267 166 List of atomic transitions and equivalent width
measurements for our target stars
table5.dat 96 45 Chemical abundances for our sample stars
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See also:
B/pastel : The PASTEL catalogue (Soubiran+, 2010-)
III/260 : General Catalogue of Ap and Am stars (Renson+ 2009)
I/311 : Hipparcos, the New Reduction (van Leeuwen, 2007)
J/A+A/583/A76 : Ome Cen candidates RAVE-selected (Fernandez-Trincado+, 2015)
J/MNRAS/437/1609 : NGC 2808 HB stars abundances (Marino+, 2014)
J/ApJ/771/67 : Abundances for 97 metal-poor stars. II. (Ishigaki+, 2013)
J/A+A/552/A64 : Gaia-RVS standards (Soubiran+, 2013)
J/ApJ/764/78 : Oxygen abundances in nearby FGK stars (Ramirez+, 2013)
J/A+A/549/A147 : Microlensed Bulge dwarf stars abundances. V. (Bensby+, 2013)
J/ApJ/757/164 : Oxygen abundances of dwarf stars (Ramirez+, 2012)
J/A+A/534/A136 : Halo red giants from the SEGUE survey (Martell+, 2011)
J/A+A/531/A88 : Optical spectra of 12 Miras (Uttenthaler+, 2011)
J/ApJ/731/64 : Spectroscopy of 300 RGBs in ω Cen (Marino+, 2011)
J/ApJ/722/1373 : ω Centauri giants abundances (Johnson+, 2010)
J/AJ/140/631 : HST WFC3/UVIS photometry of omega Cen core (Bellini+, 2010)
J/ApJ/705/328 : Abundance measurements in Sculptor dSph (Kirby+, 2009)
J/A+A/505/139 : Abundances of red giants in 17 GCs (Carretta+, 2009)
J/A+A/505/117 : Abundances of red giants in 15 GCs (Carretta+, 2009)
J/A+A/497/563 : Chemical abundances of 451 stars (Neves+, 2009)
J/AJ/135/1580 : Element abundances in 10 Car dSph red giants (Koch+, 2008)
J/ApJ/667/911 : Abundances on the MS of ω Cen (Stanford+, 2007)
J/A+A/465/815 : Abundances of Sgr dSph stars (Sbordone+, 2007)
J/A+A/465/271 : Oxygen abundances in nearby stars (Ramirez+, 2007)
J/A+A/464/939 : Abundances of red giants in NGC 6218 (Carretta+, 2007)
J/MNRAS/367/1329 : Elemental abundances for 176 stars (Reddy+, 2006)
J/ApJ/647/1075 : Age-metallicity relation of ω Cen (Stanford+, 2006)
J/AJ/128/1177 : Galactic stellar abundances (Venn+, 2004)
J/A+A/404/187 : Equivalent widths for metal-poor stars (Gratton+, 2003)
J/MNRAS/340/304 : [X/Fe] of Galactic disc F and G dwarfs (Reddy+, 2003)
J/ApJS/141/503 : Radial Velocities for 889 late-type stars (Nidever+, 2002)
J/A+A/390/235 : OI and FeII EWs in metal-poor stars (Nissen+ 2002)
J/AJ/119/2866 : Proper motions of metal-poor stars (Beers+, 2000)
J/A+AS/141/491 : Chemical composition of halo and disk stars (Nissen+, 2000)
J/PASP/107/1042 : Infrared Arcturus Atlas (Hinkle+ 1995)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1 A1 --- Group Star group (G1)
3- 12 A10 --- Name Star name
14 A1 --- f_Name [a] a: Reference star (see section 3 and
table 3)
16- 22 F7.2 km/s HRV [-398/311] Heliocentric velocity
24- 27 F4.2 km/s e_HRV [0.3/0.5] HRV uncertainty
29- 32 I4 K Teff [4396/6288] Effective temperature
34- 36 I3 K e_Teff [43/195]? Teff uncertainty
38- 41 F4.2 [cm/s2] logg [0.6/4.6] Log of surface gravity
43- 46 F4.2 [cm/s2] e_logg [0.1/0.3]? logg uncertainty
48- 53 F6.3 [Sun] [Fe/H] [-2.5/-0.7] Metallicity
55- 58 F4.2 [Sun] e_[Fe/H] [0.04/0.09]? [Fe/H] uncertainty
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Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 F7.2 0.1nm lambda [4491.4/7836.2] Wavelength in Angstroms
9- 12 F4.1 --- Sp [8/56.1] Species code (1)
14- 17 F4.2 eV ExPot [0/9.2] Excitation potential
19- 23 F5.2 [-] log(gf) [-5/2.3] Log of the oscillator strength
25- 28 F4.1 10-13m EW1 [5/94]? The CD-30 1121 equivalent width
30- 34 F5.1 10-13m EW2 [4/232]? The CD-62 1346 equivalent width (2)
36- 39 F4.1 10-13m EW3 [4/56]? The HD 110621 equivalent width (2)
41- 45 F5.1 10-13m EW4 [4/111]? The HD 111721 equivalent width (2)
47- 50 F4.1 10-13m EW5 [3/44]? The HD 13979 equivalent width (2)
52- 56 F5.1 10-13m EW6 [3/117]? The HD 181007 equivalent width (2)
58- 61 F4.1 10-13m EW7 [1/33]? The HD 181743 equivalent width (2)
63- 66 F4.1 10-13m EW8 [2/99]? The HD 186478 equivalent width (2)
68- 71 F4.1 10-13m EW9 [3/39]? The HD 188031 equivalent width (2)
73- 76 F4.1 10-13m EW10 [3/95]? The HD 193242 equivalent width (2)
78- 81 F4.1 10-13m EW11 [3/85]? The HD 208069 equivalent width (2)
83- 87 F5.1 10-13m EW12 [4/131]? The HD 21022 equivalent width (2)
89- 93 F5.1 10-13m EW13 [2/154]? The HD 215601 equivalent width (2)
95- 98 F4.1 10-13m EW14 [1/20]? The HD 215801 equivalent width (2)
100-103 F4.1 10-13m EW15 [2/17]? The BD+02 3375 equivalent width (2)
105-108 F4.1 10-13m EW16 [3/69]? The CD-61 0282 equivalent width (2)
110-113 F4.1 10-13m EW17 [2/89]? The HD 113083 equivalent width (2)
115-118 F4.1 10-13m EW18 [4/99]? The HD 121004 equivalent width (2)
120-123 F4.1 10-13m EW19 [1/19]? The HD 140283 equivalent width (2)
125-128 F4.1 10-13m EW20 [2/89]? The HD 148816 equivalent width (2)
130-133 F4.1 10-13m EW21 [2/82]? The HD 193901 equivalent width (2)
135-138 F4.1 10-13m EW22 [3/68]? The HD 194598 equivalent width (2)
140-143 F4.1 10-13m EW23 [1/72]? The HD 3567 equivalent width (2)
145-148 F4.1 10-13m EW24 [1/21]? The HD 84937 equivalent width (2)
150-153 F4.1 10-13m EW25 [4/63]? The HD 102200 equivalent width (2)
155-158 F4.1 10-13m EW26 [2/30]? The HD 116064 equivalent width (2)
160-163 F4.1 10-13m EW27 [3/49]? The HD 128279 equivalent width (2)
165-169 F5.1 10-13m EW28 [2/127]? The HD 134439 equivalent width (2)
171-175 F5.1 10-13m EW29 [4/146]? The HD 134440 equivalent width (2)
177-181 F5.1 10-13m EW30 [8/142]? The HD 142948 equivalent width (2)
183-187 F5.1 10-13m EW31 [3/122]? The HD 145417 equivalent width (2)
189-193 F5.1 10-13m EW32 [5/141]? The HD 151559 equivalent width (2)
195-199 F5.1 10-13m EW33 [2/156]? The HD 17072 equivalent width (2)
201-205 F5.1 10-13m EW34 [5/125]? The HD 184266 equivalent width (2)
207-211 F5.1 10-13m EW35 [3/103]? The HD 190287 equivalent width (2)
213-216 F4.1 10-13m EW36 [3/74]? The HD 199289 equivalent width (2)
218-221 F4.1 10-13m EW37 [3/82]? The HD 211998 equivalent width (2)
223-226 F4.1 10-13m EW38 [2/54]? The HD 219617 equivalent width (2)
228-232 F5.1 10-13m EW39 [6/137]? The HD 221580 equivalent width (2)
234-238 F5.1 10-13m EW40 [3/156]? The HD 222434 equivalent width (2)
240-244 F5.1 10-13m EW41 [5/169]? The HD 222925 equivalent width (2)
246-250 F5.1 10-13m EW42 [2/145]? The HD 23798 equivalent width (2)
252-255 F4.1 10-13m EW43 [2/57]? The HD 26169 equivalent width (2)
257-261 F5.1 10-13m EW44 [2/183]? The HD 83212 equivalent width (2)
263-267 F5.1 10-13m EW45 [5/124]? The HD 9051 equivalent width (2)
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Note (1): Using the format XX.Y where XX is the atomic number and Y is the
ionization level, e.g. 26.1 is Fe II.
Note (2): In units of milli-Angstroms.
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Byte-by-byte Description of file: table5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1 A1 --- Group Star group (G1)
3- 12 A10 --- Name Star name
14- 19 F6.3 --- [Fe/H] [-2.5/-0.7] Metallicity
21- 24 F4.2 --- [O/Fe] ? Abundance of [O/Fe]
25 A1 --- f_[O/Fe] [*] Flag on [O/Fe]
27- 30 F4.2 --- e_[O/Fe] [0.04/0.2]? [O/Fe] uncertainty
32 I1 --- oe[O/Fe] [2/3]? Number of lines used for e_[O/Fe]
34- 38 F5.2 --- [Na/Fe] [-0.4/0.4]? [Na/Fe] abundance
40- 43 F4.2 --- e_[Na/Fe] [0.05/0.2]? [Na/Fe] uncertainty
45 I1 --- oe[Na/Fe] [1/6]? Number of lines used for e_[O/Fe]
47- 50 F4.2 --- [Mg/Fe] [0.02/0.6] [Mg/Fe] abundance
52- 55 F4.2 --- e_[Mg/Fe] [0.04/0.3]? [Mg/Fe] uncertainty
57 I1 --- oe[Mg/Fe] [1/5]? Number of lines used for e_[O/Fe]
59- 63 F5.2 --- [Al/Fe] [-0.02/0.4]? [Al/Fe] abundance
65- 68 F4.2 --- e_[Al/Fe] [0.04/0.3]? [Al/Fe] uncertainty
70 I1 --- oe[Al/Fe] [1/5]? Number of lines used for e_[O/Fe]
72- 75 F4.2 --- [Ca/Fe] [0.1/0.6] [Ca/Fe] abundance
77- 80 F4.2 --- e_[Ca/Fe] [0.05/0.2]? [Ca/Fe] uncertainty
82- 83 I2 --- oe[Ca/Fe] [6/15]? Number of lines used for e_[O/Fe]
85- 89 F5.2 --- [Ba/Fe] [-1/1.6] [Ba/Fe] abundance
91- 94 F4.2 --- e_[Ba/Fe] [0.04/0.4]? [Ba/Fe] uncertainty
96 I1 --- oe[Ba/Fe] [2/3]? Number of lines used for e_[O/Fe]
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Global note:
Note (G1): Code as follows:
K = Kapteyn group stars
O = ω Cen group stars
F = Field stars
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 20-Nov-2015