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Adding the s-‐Process to the APOGEE Stellar Popula8ons
(Apache Point Observatory Galac8c Evolu8on Experiment)
Verne V. Smith NOAO, Tucson, Arizona USA + APOGEE & ASPCAP Teams
APOGEE Stellar Parameters & Abundance Pipeline
APOGEE: “The Big Picture” • Galac8c Cartography • Part of SDSS III & IV • R=22,400 NIR H-‐band
(λ1.52-‐1.69μm) 300-‐fibers • Kinema8c (~100 m/s) • Chemical (~0.1 dex) • ~15 elements per star à
f(Teff, log g, [m/H]) • 140,000 stars in DR12 • 500,000 stars by 2020 • APOGEE-‐1 (2011 – 2014) • APOGEE-‐2 will add • Data Release 13 (DR13)
Majewski et al. 2016
H hydrogen
Li lithium
Na sodium
K potassium
Rb rubidium
Cs caesium
Fr francium
Be beryllium
Mg magnesium
Ca calcium
Sr strontium
Ba barium
Ra radium
Sc scandium
Y yttrium
Ti titanium
Zr zirconium
Hf hafnium
V vanadium
Nb niobium
Cr chromium
Mo molybdenum
Mn manganese
Tc technetium
Fe iron
Ru ruthenium
Co cobalt
Rh rhodium
Ni nickel
Pd palladium
Cu copper
Ag silver
Zn zinc
Cd cadminium
Ta tantalum
W tungsten
Re rhenium
Os osminium
Ir iridium
Pt platinum
Au gold
Hg mercury
B boron
Si silicon
Ge geramanium
As arsenic
Sb antimoney
Te tellurium
Po polonium
C carbon
P phosphorous
N nitrogen
O oxygen
S sulphur
Se selenium
Al aluminium
Ga galium
In indium
Tl thallium
Sn tin
Pb lead
Bi bismuth
F fluorine
Cl chlorine
Br bromine
I iodine
At astatine
He helium
Ne neon
Ar argon
Kr krypton
Xe xenon
Rn radon
1 2
3
11
19
37
55
La Lanthanum
Ce cerium
Pr praseodymium
Pm promethium
Sm samarium
Eu europium
Gd gadolinium
Tb terbium
Dy dysprosium
Ho holmium
Re erbium
Tm thulium
Yb ytterbium
Lu lutetium
Nd neodymium
Ac actinium
Pa protactinium
U uranium
Np neptunium
Pu plutonium
Am americium
Cm curium
Bk berkelium
Cf californium
Es einsteinium
Fm fermium
Md mendelevium
Th thorium
No nobelium
Lr lawrencium
87
4
12
20
38
56
88
39
22 21
40
72
23
41
73
24
42
74
25
43
74
26
44
76
27
45
77
28
46
78
29
47
79
30
48
80
31
49
81
5
13
32
50
82
14
33
51
83
7
15
34
52
84
8
16
35
53
85
9
17
36
54
86
10
18
57 59 61 62 63 64 65 66 67 68 69 70 71
89 90 91 92 93 94 95 96 97 98 99 100 101 102 103
The APOGEE Periodic Table
6
� λ1.51 – 1.69μm � C, N, O determined (mostly) from molecular transi8ons: CO, OH, CN � Everything elseà atomic lines, almost all neutral. Ti II � Note lack of heavy elements (Z>30) � Stellar parameters and chemical abundances all hang on the APOGEE line list
Already in, but may need work
Also lines in current list from Ge I and Y II, but very weak. Some doubly ionized lines ( Ce III) but not visible in red giants
Elemental Abundances
Test Slide
Plus Kurucz compila8ons & molecules Con8nuing to improve on iden8fying missing lines from the most recent line lists; can add addi8onal elements from these previously unknown lines
Informa8on in a moderately metal-‐poor K-‐giant
• Teff=4300K • [Fe/H]= -‐1.3 • Log g = 1.5 • Informa8on
content • Molecular gf-‐
values from literature
• Atomic gf-‐values allowed to vary within 2σ via synthesis of Sun and Arcturus
What do ASPCAP results look like?
• [Ca/Fe] vs. [Fe/H] • DR12 • Teff > 3900K • Thin Disk / Thick Disk + Halo
• Includes F/G dwarfs from Bensby et al. (2014)
-2 -1.5 -1 -0.5 0 0.5
-0.5
0
0.5
[Fe/H]
H hydrogen
Li lithium
Na sodium
K potassium
Rb rubidium
Cs caesium
Fr francium
Be beryllium
Mg magnesium
Ca calcium
Sr strontium
Ba barium
Ra radium
Sc scandium
Y yttrium
Ti titanium
Zr zirconium
Hf hafnium
V vanadium
Nb niobium
Cr chromium
Mo molybdenum
Mn manganese
Tc technetium
Fe iron
Ru ruthenium
Co cobalt
Rh rhodium
Ni nickel
Pd palladium
Cu copper
Ag silver
Zn zinc
Cd cadminium
Ta tantalum
W tungsten
Re rhenium
Os osminium
Ir iridium
Pt platinum
Au gold
Hg mercury
B boron
Si silicon
Ge geramanium
As arsenic
Sb antimoney
Te tellurium
Po polonium
C carbon
P phosphorous
N nitrogen
O oxygen
S sulphur
Se selenium
Al aluminium
Ga galium
In indium
Tl thallium
Sn tin
Pb lead
Bi bismuth
F fluorine
Cl chlorine
Br bromine
I iodine
At astatine
He helium
Ne neon
Ar argon
Kr krypton
Xe xenon
Rn radon
1 2
3
11
19
37
55
La Lanthanum
Ce cerium
Pr praseodymium
Pm promethium
Sm samarium
Eu europium
Gd gadolinium
Tb terbium
Dy dysprosium
Ho holmium
Re erbium
Tm thulium
Yb ytterbium
Lu lutetium
Nd neodymium
Ac actinium
Pa protactinium
U uranium
Np neptunium
Pu plutonium
Am americium
Cm curium
Bk berkelium
Cf californium
Es einsteinium
Fm fermium
Md mendelevium
Th thorium
No nobelium
Lr lawrencium
87
4
12
20
38
56
88
39
22 21
40
72
23
41
73
24
42
74
25
43
74
26
44
76
27
45
77
28
46
78
29
47
79
30
48
80
31
49
81
5
13
32
50
82
14
33
51
83
7
15
34
52
84
8
16
35
53
85
9
17
36
54
86
10
18
57 59 61 62 63 64 65 66 67 68 69 70 71
89 90 91 92 93 94 95 96 97 98 99 100 101 102 103
The APOGEE Periodic Table
6
Already in, but may need work
Hasselquist et al. (2016)
Cunha et al. (2016)
Expanding the APOGEE Periodic Table
Focus on the heavy elements
Vetng the Lines • Iden8fy candidate lines based on atomic proper8es • In general, for heavy-‐element H-‐band lines, no laboratory gf-‐
values • Use combina8on of α Boo and the Sun to derive gf-‐values:
“astrophysical gf-‐values” – Also use chemically peculiar stars in APOGEE as tests ßImportant – Analysis that is self-‐consistent with ASPCAP
• Hasselquist et al. (2016) – submived – 5 Nd II lines – Required s-‐process rich stars to calibrate
• Cunha et al. (2016) – in prepara8on – 9 Ce II lines (1 falls in APOGEE chip gap) – Rests on op8cal analysis Ce II – gf-‐values from Lawler et al. (2009)
• For Ce II, es8mated internal scaver ~+/-‐0.05 dex • Adding the s-‐process as a rigorously determined quan8ty to
APOGEE
Why the s-‐Process is Interes8ng
• Thermally Pulsing AGB Phase: quan8fy AGB contribu8ons to chemical evolu8on
13C( α,n)16O
22Ne(α,n)25Mg
Lavanzio & Lugaro (2009)
Tests of Ce II Lines in APOGEE Window
• Cunha et al. (2016) • APOGEE Ce II lines with
astrophysical gf-‐values agrees with op8cal results
• Ce II lines detectable in large frac8on of the APOGEE red giants
• With Ce II & Nd II the ability to probe the s-‐process across the Galaxy
• Note s-‐process rich, N-‐rich, Al-‐rich star: Cunha et al. (2016) found Ce enhancement. Noted earlier by Fernandez-‐Trincado (2016) as N-‐ & Al-‐rich, retrograde orbit, suggested to be possible ω Cen escapee. Part of sample iden8fied by Schiavon et al. (2016) in the inner Galaxy
-1.5 -1 -0.5 0 0.5
-0.5
0
0.5
1
1.5
[Fe/H]
Summary: A work in progress
• Nd and Ce are being added • Rb I is there -‐ not clear yet how well ASPOGEE/ASPCAP can do. Always the op8mist
• Other lines are in there – maybe 1st-‐peak – Zr I (?) • In addi8on -‐ line list will con8nue to be improved: more complete lists, bever atomic data, in par8cular f-‐values, more molecules as needed
• Teff • Log g • ξ -‐ microturbulence • [M/H] • [α/M] • [C/M] • [N/M] • Spectral Libraries
are 1D models in LTE
• So far-‐ ATLAS9 + tests with MARCS
• Future releases will include MARCS
Atomic Line Illustra8on
• Sample Mn I with hfs shown
• δ Oph – M1 III • Teff= 3800K • [Fe/H]~0. • 0.1 dex increments in Mn
Some Scienceà Stellar evolu8on in open clusters: 12C/13C Along the NGC6791 RGB from APOGEE
• Cunha et al. (2016 – in prep.)
• MRGB~1.2MSun • [Fe/H]=+0.4 • From near luminosity bump, up RGB, down to Clump
• No change in 12C/13C
• Tes8ng mixing at high metallicity
3500 4000 4500 50000
10
20
30
1 1.5 2 2.5 30
10
20
30
21
“Bump” Clump
Clump