Nucleosynthesis: the origin of elements,
Milky Way, & distant galaxies

from z=5 to 0

https://www.youtube.com/watch?v=jk5bLrVI8Tw

Metallicity [O/H] = –5 (blue) to -1 (red); > -1 (white)

Chiaki Kobayashi(Univ. of Hertfordshire, UK)Galactic Archaeology
Nomoto, CK, Tominaga 2013 ARAA

(SNIbc)Q [Fe/H] and [X/Fe] evolve in a galaxy: fossils that retain theevolution history of the galaxy → Galactic Archaeology
Q With IFU surveys/ALMA/JWST, Extra-galactic Archaeology

Galactic Chemical Evolution (GCE)(1) One-zone model (instantaneous mixing): Tinsley 80, Timmes+95,
Pagel 97, Matteucci 01, Prantzos+93, Ferrini+92 (Molla, Travaglio, Magrini), Chiappini+97,CK+ 00…, Vincenzo+14, Cote+16d(Zfg )= ESW + ESNcc + ESNIa − Zψ + Z inflow Rinflow − ZRoutflow
dt
Metal ejection rates••••

Inflow

Outflow

decreased bynucleosynthesis yields
star formation
initial mass function (IMF)
binaries, SNIa progenitors
nuclear reaction rates
given from hydrodynamics in(3) Chemodynamical simulation
Burkert & Hensler 87, Katz 92, Steinmetz &(2) Stochastic model
Ishimaru+99; Argast+02;
Cescutti+08; Wehmeyer+15

Müller 94, Mihos & Hernquist 96, CK 04,…,FIRE, EAGLE, Horizon, Illustris→ inhomogeneous enrichment

Core-collapse SNe 25M , Mösta +14

18M8, Müller+178← ν-driven SNII & failed SN
Hypernovae (mechanism?) →In GCE, 50-1% at >20M803dh51

Kinetic energy [10 erg]

Mezzacappa+ 100
Burrows+
Kotake+98bw

Takiwaki+Obergaulinger& Aloy
03lw

97ef

1008D02ap
06aj

103bg
05bf

93J
94I

87A

99br
97D

Nomoto et al. 2002, 20130.1
10(single stars)

15

20
2530
35
40
Main-sequence mass [M! ]4550

Nucleosynthesis Yields
Nomoto, CK, Tominaga 2013, ARAA (1D, no rotation, single)

core-collapse SNAGB
super AGB
ECSN

Also, Woosley & Heger; Limongi & Chieffi; NuGrid; PUSH

Nucleosynthesis Yields
Nomoto, CK, Tominaga 2013, ARAA (1D, no rotation, single)

PPISN

PISN
BH?

core-collapse SN

Also, Woosley & Heger; Takahashi & Umeda

Thermonuclear (Type Ia) Supernovae
Thermonuclear explosion in a binary with C+O white dwarf
Chandrasekhar (Ch)
Sub-Ch mass explosion,vsmass explosion, expected inshowed in Double Degenerate (DD)Single Degenerate (SD)simulations, also possible in SD

companion star observed! (McCully+14)

[O/Fe]-[Fe/H] relation~TimePopIII?

EMP

M,rotation

SNII
M,E,ZPopII

SNIa

PopI

Lifetime, Z
NLTE obs.

SNII↑

oldage↑↓SNIa↓youngage

Solar Neighborhood

in MW, Ch dominant (WD+WD mergers <25%)← old W7

CK, Leung, Nomoto 2020

Neutron-capture processes
AGB star

Neutron Star Merger
Yields: Wanajo+14
Rates: Mennekens &Vanbeveren 2014

Electron Capture
Supernovae
Yields: Wanajo+13
Mass: Doherty+15

CK, Karakas, Lugaro 2020

Magnetorotational
Supernovae
Yields: Nishimura+15

time

CK, Karakas, Lugaro 2020

The Origin of Elements
CK, Karakas, Lugaro 2020, ApJ※Purely theoretical, no empirical equations.

dotted lines: solar values

It is necessary to have the r-process
associated with core-collapse SNe,such as MRSNe (or collapsars)...
Is there any observational evidence?
• 26000 SkyMapper photometric candidates• 2618 EMP candidates with ANU 2.3m spectra (Da Costa+19)• 479 stars in SkyMapper DR1.1 (Yong+21b) with Magellan/VLT/Kech• SMSS J200322.54-114203.3, [Fe/H]= -3.5, 2.3kpc away, Halo orbit

Magneto-rotational Hypernova!
a3.0

Yong, CK, Da Costa+ 21, Nature
MRHN
NSM+GCE

SMSS 2003−1142

2.0[X/Fe]

NZn

1.00.0[Fe/H]= -3.5

−1.0b1.5∆ [X/Fe]

1.0Mg
SiCrZnCoMo

Ce Eu Ho Lu
Ba Nd Tb Tm OsUZrSr Ru

La Sm Dy Yb
Pr Gd Er HfThY

0.50.0−0.5−1.0−1.5AlCa20

NiMn

4060
Atomic Number80

Galactic Archaeology surveysof Milky Way and local dwarf galaxies❖ Motions of one billion stars are measured with Gaia.
❖ Ages from asteroseismology COROT, Kepler, K2, TESS…
❖ Elemental Abundances (from Li to Eu) of one million stars
will be measured with multi-object spectrographs:
uSEGUE (Resolution~1800) on SDSSu RAVE (R~7500) on 1.2m UKSTu HERMES on AAT (R~28000/50000)
u APOGEE (R~20000, IR) on SDSSu GAIA-ESO with VLT (R~20000/40000)
u WFMOS on Subaru
u WEAVE on WHT (R~5000/20000)
u 4MOST on VISTA (R~5000/18000)
u PFS on Subaru (R~2300-5000)
u MSE (R~2000/6500/20000)❖ The origin of sub-structures? The merging history of MW?
Gaia spacecraft http://sci.esa.int/gaia/

MW-type galaxy zoom-in simulation

https://star.herts.ac.uk/~chiaki/works/Aq-C-5-kro2.mpg

Gadget3-based code (CK+ 2007)
Aquila Initial Condition (Scannapieco+12), 3x105M8, 0.5kpc(CK 2015; Haynes & CK 2019; Vincenzo & CK 2020; CK 2022)

[X/Fe] in Gaia Satellites

Aguado, Belokurov, ..CK+ 2021

CK 2016,
Nature News&Views

4 Nov 2021
⋀Fluorine

3800

10HF (1-0)

12

H2O 220-211

4000

H2O 321-312

14

H2O 312-221

Stacked ALMA Band 6
HF absorption line
Gemini-K band

CO(10-9)24 1504200❖ N(H2)=2.1±0.4 1024 cm2 (from [C I])❖ H2 + F → H + HF (stable, dominant)Flux density [mJy]Dec (J2000)❖ Lensed dusty star-forming galaxy
NGP-190387 at z = 4.420

aArp 220

NGP-190387

8636002”13h33m37.6s

37.4s
RA (J2000)

37.2s

1150

1160
1230
1240
Frequency (rest-frame) [GHz]Wolf-Rayet stars!? (or ν-process)
100a1024

10010 1

NHF/NH2864 2

Fluorinecontribution

1.4 Gyrs after Big Bang, 0.7 Gyrs after re-ionization

27101010 810 910 1010 1110 1210 13bWR
AGB

SNe
Solar neighborhood

SNe

SNe+AGB+WR
SNe+AGB

Model ⌧ = 0.1 Gyr
Model ⌧ = 0.3 Gyr
Model ⌧ = 0.5 Gyr

3Franco et al. 2021, Nature Astronomy

45Redshift

67Redshift evolutionVincenzoof CNO
ratios& CK 2018a, A&A, 610, 16×109(a) galaxyAAGalaxy
6z = 0.5z=1z=22z=4z=6dM⋆(z = 0)/dt [M⊙ Gyr−1 ]40×1010(b) galaxyBBGalaxy
0.80.60.40.20.0×109

Galaxy(c) galaxy CC642014 13 12 11 109876543210age [Gyr]C: low-mass AGB, <4M8
N: massive AGB, >4M8
O: core-collapse SNe
Currently, N/O (z<2.5),
C/O (z>2), but C/N with
JWST/NIRSpec!

The N/O-O/H relation
Vincenzo & CK 2018b, MNRAS, 478, 155
obs. of stars & gas❖ Local relation reflects metallicity radial gradients.
❖ Global relation is caused by the mass-metallicity relation.
❖ for 33 star-forming galaxies in cosmological simulations

The N/O-O/H relation

KLEVER survey:
Hayden-Pawson, Curti,
Maiolino ...CK+ 21, submitted

Stellar [α/Fe]-mass relation of ETGs
Not solved yet in any (proper) cosmological simulations...

Kriek+16@z=2.1

z=2
longer SF
more SNe Ia

Taylor & CK 2015, MNRAS, 448, 1835

~ Mass of galaxies

More [α/Fe] observations❖ NIRVANDELS survey on gasphase O/H and stellar Fe/H of 33
star-forming galaxies 2.95 < z <3.80 (Cullen+21)❖ EMPRESS survey, local young
low-mass galaxies (Kojima+20,Isobe+21)#There was a long history until MW stars’ [α/Fe] settle down...

Extra-galactic Archaeology❖ Chemodynamical structures of galaxies, i.e., kinematics
and 2D map of gas, stars, chemical abundances, aremeasured with Integral Field Units (SAURON, CALIFA,MaNGA, SAMI, KMOS, MUSE, Hector, NIRSpec/JWST…)❖ Time evolution and scaling relations with larger sample(e.g., SDSS, MOSFIRE, VMOS, FMOS, MOONS, PFS)
❖ Evolution of mass-metallicity relations, metallicity
gradients? Proof of galactic ecosystem?
JWST http://www.jwst.nasa.gov

The topic not mentioned,
but absolutely beautiful...

X-ray Intracluster medium (ICM)
Perseus cluster (Hitomi collaboration 2017)
Soft X-ray Spectrometer (SXS) on Hitomi∆E ≈ 5 eV in the 2–10 keV bandX-ray Intracluster medium (ICM)

How to translate line ratios into abundance ratios?

Distant galaxies, DLA, IGM
to witness time evolution

star-forming galaxies,
How to translate line ratios into abundance ratios?

DLA

The need for UV spectra of stars

GALAH, CUBES, HST

The need for HRMOS:⋀Isotopic ratios!
for accurate/true abundances &3D/NLTE analyses are essential.

in starsIncomplete list (correct me, I will update the slide)references

KAGRA

GW

NS/BH merger-Super-K, Hyper-K

MeV ν, backgroundSN-

KamLAND

low E νSN, pp-chain-IceCube-Gen2

high E νSN

2033

XRISM

Xray high-res spec

SNRMn,Cr etc

2022

FORCE

high E Xray 1-80keV

AGN

44Ti

mid 2020s

Mori+

HiZ-GUNDAM

Xray 0.5-4keV

high-z GRB

late 2020s

Yonetoku+20

ATHENA

Xray IFU

ICM

2031

ESA

SuperDIOS

Xray

redshifted OVII,
OVIII

2030s

Yamada+18

LAPYUTA, 60cm

UV 115-190nm?

?

2029-31

Tsuchiya+

Subaru-HDS

opticalstars

Li to U

-Subaru-PFS

optical MOS (HR/IFU?)

stars, galaxies

Fe, α

2023

TMT-HROS

opticalstars

Li to U??

ULTIMATE-Subaru

0.9-1.8μm (IFU MOS?)

galaxies

JASMINE

1.1-1.6μm astrometry

GREX-PLUS, 1.2m

10-20μm, 30000A

ATT10@南極

300μm / 1THz

ALMA

0.3mm-1cm / 31.3-950GHz

LST, merged to AtLAST

0.8-4mm / 70-420 GHz[OIII]@z=7-9; some
[CII],[NII]EAVN/VERA

10-100mm

AGB mass-loss

ngVLA@北米

0.3-20cm / 1.2-116 GHz

SKA

3cm-4m /70MGz-10 GHz

C to Ni??
dynamics[OIII],[NII]

Akiyama+

2022/30s
2030s

Inoue+?

2032

Kuno+

CNOF

-?

2031?

Kohno+21-

Imai+20

2030s

NRAO

H

2027-