J/MNRAS/449/3889 Detailed abundances of 15 stars in NGC 4833 (Roederer+, 2015)
Detailed abundances of 15 stars in the metal-poor globular cluster NGC 4833.
Roederer I.U., Thompson I.B.
<Mon. Not. R. Astron. Soc., 449, 3889-3910 (2015)>
=2015MNRAS.449.3889R 2015MNRAS.449.3889R (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, globular ; Stars, giant ; Equivalent widths ; Abundances
Keywords: nuclear reactions, nucleosynthesis, abundances - stars: abundances -
stars: Population II - globular clusters: individual (NGC 4833)
Abstract:
We have observed 15 red giant stars in the relatively massive, metal-poor
globular cluster NGC 4833 using the Magellan Inamori Kyocera Echelle
spectrograph at Magellan. We calculate stellar parameters for each star
and perform a standard abundance analysis to derive abundances of
43 species of 39 elements, including 20 elements heavier than the iron
group. We derive <[Fe/H]≥-2.25±0.02 from FeI lines and
<[Fe/H]≥-2.19±0.013 from FeII lines. We confirm earlier results that
found no internal metallicity spread in NGC 4833, and there are no
significant star-to-star abundance dispersions among any elements in
the iron group (19=<Z=<30). We recover the usual abundance variations
among the light elements C, N, O, Na, Mg, Al, and possibly Si. The
heavy-element distribution reflects enrichment by r-process
nucleosynthesis ([Eu/Fe]=+0.36±0.03), as found in many other metal-poor
globular clusters. We investigate small star-to-star variations found
among the neutron-capture elements, and we conclude that these are
probably not real variations. Upper limits on the Th abundance,
logε (Th/Eu)←0.47±0.09, indicate that NGC 4833, like other
globular clusters where Th has been studied, did not experience a
so-called actinide boost.
Description:
We have observed 15 probable members of NGC 4833 with the Magellan
Inamori Kyocera Echelle (MIKE) spectrograph (Bernstein et al.
2003SPIE.4841.1694B 2003SPIE.4841.1694B) on the 6.5 m Landon Clay (Magellan II) Telescope
at Las Campanas Observatory. Thorium-argon (ThAr) comparison lamp spectra
have been taken immediately preceding or following each observation.
The red and blue arms of MIKE are split by a dichroic at ∼4950 Å.
This setup provides complete wavelength coverage from 3350-9150 Å.
Data reduction, extraction, and wavelength calibration have been performed
using the carpy MIKE data reduction pipeline written by D. Kelson (see
also Kelson 2003PASP..115..688K 2003PASP..115..688K).
Objects:
-----------------------------------------------
RA (ICRS) DE Designation(s)
-----------------------------------------------
12 59 33.92 -70 52 35.4 NGC 4833 = GCl 21
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 38 17 Observing log
table4.dat 132 354 Atomic data and equivalent widths
table5.dat 33 3391 Abundances derived from individual lines
table6.dat 51 735 Mean abundances in each star
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See also:
J/A+AS/109/479 : NGC 4833 BV photometry (Samus+, 1995)
J/ApJ/645/613 : Abundances of HD 221170 (Ivans+, 2006)
J/ApJS/162/227 : Transition probabilities for SmII (Lawler+, 2006)
J/ApJS/167/292 : Laboratory transition probabilities for Gd II
(Den Hartog+, 2006)
J/ApJ/667/1267 : CrI transition probabilities (Sobeck+, 2007)
J/ApJS/169/120 : Transition probabilities for HfII and Hf (Lawler+, 2007)
J/ApJS/182/51 : Transition probabilities of rare earth elements
(Lawler+, 2009)
J/ApJS/182/80 : Rare earth abundances (Sneden+, 2009)
J/ApJ/742/37 : Abundances of six RGB stars in M22 (Roederer+, 2011)
J/ApJS/194/35 : Atomic transition probabilities of Mn (Den Hartog+, 2011)
J/ApJ/750/76 : r-process peaks elements in HD 160617 (Roederer+, 2012)
J/ApJS/208/27 : Sun and HD 84937 TiII log(gf) and abundances (Wood+, 2013)
J/A+A/564/A60 : NGC 4833 Na-O measured with FLAMES (Carretta+, 2014)
J/ApJS/211/20 : NiI transition probability measurements (Wood+, 2014)
J/ApJS/214/18 : VII log(gf) values, and V abundance in HD 84937 (Wood+ 2014)
J/MNRAS/441/3127 : FeI oscillator strengths for Gaia-ESO (Ruffoni+, 2014)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- Name Star name
8- 10 F3.1 arcsec Slit [0.7/1] Slit width
12- 21 A10 "date" Date Date of observation
23- 27 A5 "h:m:s" Time Start of the exposure, UT (hh:mm)
29- 32 I4 s Texp [1200/7200] Exposure time
34- 38 F5.1 km/s HRV [187.9/297.6] Heliocentric radial velocity
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Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 F7.2 0.1nm Wave [3694.2/7836.13] Wavelength (Å)
9- 12 F4.1 --- ID [3/90.1] Species (1)
14- 17 F4.2 eV ExPot [0/9.14] Excitation potential
19- 23 F5.2 [-] log(gf) [-9.78/0.65] Log of degeneracy times
oscillator strength
25- 26 I2 --- r_log(gf) [1/40] Literature reference for log(gf) (2)
28- 32 F5.1 0.1pm EW(2-185) [5.6/176.5]? Equivalent width in milli
Angstroms for star 2-185
33 A1 --- n_EW(2-185) [ls] Note on EW(2-185) (3)
35- 39 F5.1 0.1pm EW(2-277) [6.2/155.4]? Equivalent width in milli
Angstroms for star 2-277
40 A1 --- n_EW(2-277) [ls] Note on EW(2-277) (3)
43- 47 F5.1 0.1pm EW(2-882) [9.5/165.3]? Equivalent width in milli
Angstroms for star 2-882
48 A1 --- n_EW(2-882) [ls] Note on EW(2-882) (3)
50- 54 F5.1 0.1pm EW(2-918) [4.3/165.3]? Equivalent width in milli
Angstroms for star 2-918
55 A1 --- n_EW(2-918) [ls] Note on EW(2-918) (3)
57- 61 F5.1 0.1pm EW(2-1578) [6.6/176.7]? Equivalent width in milli
Angstroms for star 2-1578
62 A1 --- n_EW(2-1578) [ls] Note on EW(2-1578) (3)
64- 68 F5.1 0.1pm EW(2-1664) [6.3/178.8]? Equivalent width in milli
Angstroms for star 2-1664
69 A1 --- n_EW(2-1664) [ls] Note on EW(2-1664) (3)
71- 75 F5.1 0.1pm EW(3-742) [7/222.2]? Equivalent width in milli
Angstroms for star 3-742
76 A1 --- n_EW(3-742) [ls] Note on EW(3-742) (3)
78- 82 F5.1 0.1pm EW(3-772) [14.4/178.3]? Equivalent width in milli
Angstroms for star 3-772
83 A1 --- n_EW(3-772) [ls] Note on EW(3-772) (3)
85- 89 F5.1 0.1pm EW(3-1509) [6.2/184]? Equivalent width in milli
Angstroms for star 3-1509
90 A1 --- n_EW(3-1509) [ls] Note on EW(3-1509) (3)
92- 96 F5.1 0.1pm EW(4-224) [5/198]? Equivalent width in milli Angstroms
for star 4-224
97 A1 --- n_EW(4-224) [ls] Note on EW(4-224) (3)
99-103 F5.1 0.1pm EW(4-341) [5/195.1]? Equivalent width in milli
Angstroms for star 4-341
104 A1 --- n_EW(4-341) [ls] Note on EW(4-341) (3)
106-110 F5.1 0.1pm EW(4-464) [7.7/166.6]? Equivalent width in milli
Angstroms for star 4-464
111 A1 --- n_EW(4-464) [ls] Note on EW(4-464) (3)
113-117 F5.1 0.1pm EW(4-1255) [4.4/213.7]? Equivalent width in milli
Angstroms for star 4-1255
118 A1 --- n_EW(4-1255) [ls] Note on EW(4-1255) (3)
120-124 F5.1 0.1pm EW(4-1398) [4.4/186.6]? Equivalent width in milli
Angstroms for star 4-1398
125 A1 --- n_EW(4-1398) [ls] Note on EW(4-1398) (3)
127-131 F5.1 0.1pm EW(4-1706) [6.9/150.6]? Equivalent width in milli
Angstroms for star 4-1706
132 A1 --- n_EW(4-1706) [ls] Note on EW(4-1706) (3)
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Note (1): The number to the left of the decimal point indicates the atomic
number, and the number to the right of the decimal point indicates the
ionization state (0=neutral, 1=first ion).
Note (2): Reference as follows:
1 = Smith, Lambert, & Nissen (1998ApJ...506..405S 1998ApJ...506..405S) for both log(gf) value and
7Li HFS;
2 = Fuhr & Wiese (2010JPCRD..39a3101F 2010JPCRD..39a3101F);
3 = Aldenius, Lundberg, & Blackwell-Whitehead (2009A&A...502..989A 2009A&A...502..989A);
4 = Lawler & Dakin (1989JOSAB...6.1457L 1989JOSAB...6.1457L), using HFS from Kurucz & Bell (1995,
Cambridge, MA Smithsonian Astrophysical Observatory CD-ROM 23);
5 = Lawler et al. (2013ApJS..205...11L 2013ApJS..205...11L);
6 = Wood et al. (2013, J/ApJS/208/27);
7 = Doerr et al. (1985JQSRT..33...55D 1985JQSRT..33...55D), using HFS from Kurucz & Bell (1995,
Cambridge, MA Smithsonian Astrophysical Observatory CD-ROM 23);
8 = Wood et al. (2014, J/ApJS/214/18);
9 = Sobeck, Lawler, & Sneden (2007, J/ApJ/667/1267);
10 = Nilsson et al. (2006A&A...445.1165N 2006A&A...445.1165N);
11 = Den Hartog et al. (2011, J/ApJS/194/35) for both log(gf) value and HFS;
12 = Ruffoni et al. (2014, J/MNRAS/441/3127);
13 = Fuhr & Wiese (2010JPCRD..39a3101F 2010JPCRD..39a3101F), using HFS from Kurucz & Bell (1995,
Cambridge, MA Smithsonian Astrophysical Observatory CD-ROM 23);
14 = Wood et al. (2014, J/ApJS/211/20);
15 = Roederer & Lawler (2012, J/ApJ/750/76);
16 = Biemont et al. (2011MNRAS.414.3350B 2011MNRAS.414.3350B);
17 = Ljung et al. (2006A&A...456.1181L 2006A&A...456.1181L);
18 = Nilsson et al. (2010A&A...511A..16N 2010A&A...511A..16N);
19 = Palmeri et al. (2005MNRAS.363..452P 2005MNRAS.363..452P);
20 = Fuhr & Wiese (2010JPCRD..39a3101F 2010JPCRD..39a3101F), using HFS/IS from McWilliam
(1998AJ....115.1640M 1998AJ....115.1640M) when available;
21 = Lawler, Bonvallet, & Sneden (2001ApJ...556..452L 2001ApJ...556..452L), using HFS from
Ivans et al. (2006, J/ApJ/645/613);
22 = Roederer, Marino, & Sneden (2011, J/ApJ/742/37);
23 = Lawler et al. (2009, J/ApJS/182/51);
24 = Li et al. (2007PhyS...76..577L 2007PhyS...76..577L), using HFS from Sneden et al.
(2009, J/ApJS/182/80);
25 = Ivarsson, Litzen, & Wahlgren (2001PhyS...64..455I 2001PhyS...64..455I), using HFS from
Sneden et al. (2009, J/ApJS/182/80);
26 = Den Hartog et al. (2003ApJS..148..543D 2003ApJS..148..543D), using HFS/IS from
Roederer et al. (2008ApJ...675..723R 2008ApJ...675..723R) when available;
27 = Lawler et al. (2006, J/ApJS/162/227), using HFS/IS from Roederer et al.
(2008ApJ...675..723R 2008ApJ...675..723R) when available;
28 = Lawler et al. (2001ApJ...563.1075L 2001ApJ...563.1075L), using HFS/IS from Ivans et al.
(2006, J/ApJ/645/613);
29 = Den Hartog et al. (2006, J/ApJS/167/292);
30 = Roederer et al. (2012ApJS..203...27R 2012ApJS..203...27R);
31 = Lawler et al. (2001ApJS..137..341L 2001ApJS..137..341L), using HFS from
Lawler, Wyart, & Blaise (2001ApJS..137..351L 2001ApJS..137..351L) when available;
32 = Wickliffe, Lawler, & Nave (2000JQSRT..66..363W 2000JQSRT..66..363W);
33 = Lawler, Sneden, & Cowan (2004ApJ...604..850L 2004ApJ...604..850L) for both log(gf) value and
HFS;
34 = Lawler et al. (2008ApJS..178...71L 2008ApJS..178...71L);
35 = Wickliffe & Lawler (1997JOSAB..14..737W 1997JOSAB..14..737W);
36 = Sneden et al. (2009, J/ApJS/182/80) for both log(gf) value and HFS/IS;
37 = Lawler et al. (2007, J/ApJS/169/120);
38 = Ivarsson et al. (2003A&A...409.1141I 2003A&A...409.1141I), using HFS/IS from Cowan et al.
(2005ApJ...627..238C 2005ApJ...627..238C), see note on log(gf) values there;
39 = Biemont et al. (2000MNRAS.312..116B 2000MNRAS.312..116B), using HFS/IS from Roederer et al.
(2012ApJS..203...27R 2012ApJS..203...27R);
40 = Nilsson et al. (2002A&A...382..368N 2002A&A...382..368N).
Note (3): Note as follows:
l = "limit": denotes lines used to derive an upper limit;
s = "synth": denotes lines used to derive an abundance via spectrum synthesis.
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Byte-by-byte Description of file: table5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- Name Star name
8- 12 A5 --- Species Species of the transition
14- 20 F7.2 0.1nm Wave [3694.2/7836.13] Wavelength (Å)
22 A1 --- l_logeps [<] Flag for upper limit on logeps
24- 28 F5.2 [-] logeps [-1.98/7.7] Log epsilon abundance
30- 33 F4.2 [-] e_logeps [0.08/1.61]? Error in log epsilon abundance
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- Name Star name
8- 13 A6 --- Species Species
15- 17 I3 --- Num [0/116] Number of lines used
19 A1 --- l_logeps [<] Flag for upper limit on logeps
21- 25 F5.2 [-] logeps [-1.98/7.33]? Log epsilon abundance
27- 31 F5.2 [-] [X/Fe] [-2.46/3.95]? Abundance relative to Fe I or
Fe II (1)
33- 36 F4.2 [-] s_[X/Fe] [0.02/1.31]? Statistical uncertainty in [X/Fe]
38- 41 F4.2 [-] e_[X/Fe] [0.08/1.31]? Total uncertainty in [X/Fe]
43- 46 F4.2 [-] e2_[X/Fe] [0/1.31]? Neutrals uncertainty in [X/Fe]
48- 51 F4.2 [-] e3_[X/Fe] [0/1.32]? Ions uncertainty in [X/Fe]
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Note (1): [Fe/H] is given for Fe I and Fe II.
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History:
From electronic version of the journal
(End) Tiphaine Pouvreau [CDS] 25-Nov-2019