Questt too understanddthee originn off thee Solarr system
Namii Sakaii (CPR,, RIKEN)
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KAKENHI: Grant-in-Aid for Transformative Research AreasʤAʥFY2020-FY2024
RIKEN Pioneering Research Project |Evolution of Matter in the Universe (r-EMU)| FY2019-FY2023

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History of formationof Matter
Structure Formation

llion years
ye
138 Billion
10 Billion years

Chemistry/Material Science

4 Billion years
The Dark Ages
Big Bang

Quantum
Gravity /Superstring Theory

380
Thousand years

History of Structure Formation

10-35m10-32mNeutrino

10-15mQuark-Gluon
PlasmaCosmicSupersymmetry/
Microwave
Grand Unified
Background First Generation
TheoryStar

Origin of life /Astrobiology
CosmicReionizationGalaxySupermassive
Black HoleStar
Formation

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Molecules in Space (~300 species)

2 Atoms (42 Species)
H2, CO, AlF, AlCl, C2, CH, CH+, CN, CO+, CP, SiC, HCl, KCl, NH, NO, NO+(?), NS, NS+, NaCl, OH, PN, SO, SO+, SiN, SiO, SiS, CS, HF, HD, FeOര;͍Ϳ͕O2, CF+,
SiHര;͍Ϳ͕WK͕WK+, AlO, OH+, CN–, SH+, SH, HCl+, TiO, ArH+, HeH+, NO+ (?), N2
3 Atoms (40 Species)
C3, C2H, C2O, C2S, CH2, HCN, HCO, HCO+, HCS+, HOC+, H2O, H2S, HNC, HNO, MgCN, MgNC, N2H+, N2O, NaCN, OCS, SO2, c-SiC2,
CO2, NH2, H3+, SiCN, AlNC, SiNC, HCP, CCP, AlOH, H2O+, H2Cl+, KCN, FeCN, HO2, TiO2, C2N, Si2C, HS2, HCS, HSC, HNO, CaNC, NCS
4 Atoms (27 Species)
c-C3H, l-C3H, C3N, C3O, C3S, C2H2, NH3, HCCN, HCNH+, HNCO, HNCS, HOCO+, H2CO, H2CN, H2CS, H3O+, c-SiC3, CH3, C3N–, PH3,
HCNO, HOCN, HSCN, H2O2, C3H+, HMgNC, HCCO, CNCN, HONO, MgC2H, HCCS, HNCN, H2NC, HCCS+
5 Atoms (23 Species)
C5, C4H, C4Si, l-C3H2, c-C3H2, H2CCN, CH4, HC3N, HC2NC, HCOOH, H2CNH, H2C2O, H2NCN, HNC3 , SiH4, H2COH+, C4H–, HC(O)CN,
HNCNH, CH3O, NH4+, H2NCO+ , NCCNH+, CH3Cl, MgC3N, NH2OH, HC3O+, HC3S+, H2C2S, C4S, HC(O)SH, HC(S)CN, HCCCO

Highly unsaturated species (Carbon-chain molecules: CCMs)

љiCOMs (interstellar “Complex” Organic Molecules)

6 Atomsoms (17 Species)
C5H, l-C4H2, C2H4, CH3CN, CH3NC, CH3OH, CH3SH, HC3NH+, HC2CHO, NH2CHO, C5N, l-HC4H, l-HC4N, c-H2C3O, H2CCNH, C5N–,HNCHCN,
HCN, SiH3CN, C5S, MgC4H, CH3CO+, C3H3, H2C3S, HCCCHS, C5O, C5H+, HCCNCH+
7 Atomsoms (10 Species)
C6H, CH2CHCN, CH3C2H, HC5N, CH3CHO, CH3NH2, c-C2H4O, H2CCHOH, C6H–, CH3NCO, HC5O, HOCH2CN, HCCCHNH, HC4NC,
c-C3HCCH, l-C5H2, MgC5N, CH2C3N
8 Atomsoms (11 Species)
CH3C3N, HC(O)OCH3, CH3COOH, C7H, C6H2, CH2OHCHO, l-HC6H, CH2,,Kര͕,2CCHCN, H2NCH2CN, CH3CHNH, CH3SiH3, H2NC(
NC(O)NH2, HCCCH2CN,+
HC5NH
H , CH2CHCCH, MgC6H, C2H3NH2, (CHOH)2
9 Atomsms (10 Species)
CH3C4H, CH3CH2CN, (CH3)2O, CH3CH2OH, HC7N, C8H, CH3C(O)NH2, C8H–, C3H6, CH3CH2SH, CH3CH2SH, CH3NHCHO, HC7O, HCCCHCHCN, H2CCHC3N,
H2CCCHCCH, HOCHCHCHO(?)
10 Atoms (5 Species)
CH3C5N, (CH3)2CO, (CH2OH)2, CH3CH2CHO, CH3CHCH2O, CH3OCH2OH, c-C6H4, H2CCCHC3N, C2H5NCO, C2H5NH2(?), HC7NH+
11 Atoms (4 Species)
HC9N, CH3C6H, C2H5OCHO, CH3OC(O)CH3, CH3C(O)CH2OH, c-C5H6, HOCH2CH2NH2
12 Atoms (4 Species)
c-C6H6, n-C3H7CN, i-C3H7CN, C2H5OCH3, 1-c-C5H5CN, 2-c-C5H5CN, CH3C7N(?), n-C3H7OH, i-C3H7OH
Mainly detected by radio observations>12 Atoms (3 Species)(Gray: Detected only toward AGB stars)
C60, C70, C60+, c-C6H5CN, HC11N, 1-C10H7CN, 2-C10H7CN, c-C9H8, 1-c-C5H5CCH, 2-c-C5H5CCH

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(The Cologne Database for Molecular Spectroscopy (CDMS): June. 2022)

GBT Observations of TMC-1:
Hunting Aromatic Molecules (GOTHAM)QUIJOTE: Q-band Ultrasensitive Inspection
Journey to the Obscure TMC-1 Enviroment:
Discovering the limits of chemical complexity

PI: Brett A. McGuire(e.g. McGuire, B. A., et al. 2020, ApJ, 900, L10;
McCarthy, M. C., et al. 2021, Natur., 5, 176
Loomis, R. A., et al. 2021, Natur. Astro., 5, 188)

Robert C. Byrd Green Bank Telescope (GBT)

PI: Jose Cernicharo(Guélin, Michel & Cernicharo, Jose, 2022, Frontiers in Astronomy andSpace Sciences, vol. 9, id. 787567, and references therein)

The 40-m Yebes telescope –credit: Pablo deVicente

Molecules in Space (~300 species)

2 Atoms (42 Species)
H2, CO, AlF, AlCl, C2, CH, CH+, CN, CO+, CP, SiC, HCl, KCl, NH, NO, NO+(?), NS, NS+, NaCl, OH, PN, SO, SO+, SiN, SiO, SiS, CS, HF, HD, FeOര;͍Ϳ͕O2, CF+,
SiHര;͍Ϳ͕WK͕WK͍Ϳ͕ WK
WK͕ WK+, AlO,AlO OH+, CN–, SH+, SH, HCl+, TiO
TiO,
O, ArH+, HeH+, NO+ (?), N2
3 Atoms
toms (40 Species)
C3, C2H, C2O, C2S, CH2, HCN, HCO, HCO+, HCS+, HOC+, H2O, H2S, HNC, HNO, MgCN, MgNC, N2H+, N2O, NaCN, OCS, SO2, c-SiC2,
CO2, NH2, H3+, SiCN, AlNC, SiNC, HCP, CCP, AlOH, H2O+, H2Cl+, KCN, FeCN, HO2, TiO2, C2N, Si2C, HS2, HCS, HSC, HNO, CaNC, NCS
4 Atoms
toms (27 Species)
c-C3H, l-C3H, C3N, C3O, C3S, C2H2, NH3, HCCN, HCNH+, HNCO, HNCS, HOCO+, H2CO, H2CN, H2CS, H3O+, c-SiC3, CH3, C3N–, PH3,
HCNO,
NO, HOCN, HSCN, H2O2, C3H+, HMgNC, HCCO, CNCN, HONO, MgC2H, HCCS, HNCN, H2NC, HCCS+
5 Atoms
toms (23 Species)
C5, C4H, C4Si, l-C3H2, c-C3H2, H2CCN, CH4, HC3N, HC2NC, HCOOH, H2CNH, H2C2O, H2NCN, HNC3 , SiH4, H2COH+, C4H–, HC(O)CN,
HNCNH,
NH, CH3O, NH4+, H2NCO+ , NCCNH+, CH3Cl, MgC3N, NH2OH, HC3O+, HC3S+, H2C2S, C4S, HC(O)SH, HC(S)CN, HCCCO

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Highly unsaturated species (Carbon-chain molecules: CCMs)

љiCOMs (interstellar “Complex” Organic Molecules)

6 Atoms (17 Species)
C5H, l-C4H2, C2H4, CH3CN, CH3NC, CH3OH, CH3SH, HC3NH+, HC2CHO, NH2CHO, C5N, l-HC4H, l-HC4N, c-H2C3O, H2CCNH, C5N–,HNCHCN, SiH3CN, C5S, MgC4H, CH3CO+, C3H3, H2C3S, HCCCHS, C5O, C5H+, HCCNCH+
7 Atoms (10 Species)
C6H, CH2CHCN, CH3C2H, HC5N, CH3CHO, CH3NH2, c-C2H4O, H2CCHOH, C6H–, CH3NCO, HC5O, HOCH2CN, HCCCHNH, HC4NC,
c-C3HCCH, l-C5H2, MgC5N, CH2C3N
8 Atoms (11 Species)
CH3C3N, HC(O)OCH3, CH3COOH, C7H, C6H2, CH2OHCHO, l-HC6H, CH2,,Kര͕,2CCHCN, H2NCH2CN, CH3CHNH, CH3SiH3, H2NC(O)NH2, HCCCH2CN,
HC5NH+, CH2CHCCH, MgC6H, C2H3NH2, (CHOH)2
9 Atoms (1010 Species)
CH3C4H, CH3CH2CN, (CH3)2O, CH3CH2OH, HC7N, C8H, CH3C(O)NH2, C8H–, C3H6, CH3CH2SH, CH3CH2SH, CH3NHCHO, HC7O, H
HCCCHCHCN, H2CCHC3N,
H2CCCHCCH,
CH, HOCHCHCHO(?)
10 Atomss (5 Species)
CH3C5N, (CHCH3)2CO, (CH2OH)2, CH3CH2CHO, CH3CHCH2O, CH3OCH2OH, c-C6H4, H2CCCHC3N, C2H5NCO, C2H5NH2(?), HC7NH+
11 Atomss (4 Species)
HC9N, CH3C6H, C2H5OCHO, CH3OC(O)CH3, CH3C(O)CH2OH, c-C5H6, HOCH2CH2NH2
12 Atomss (4 Species)
c-C6H6, n-C
C3H7CN, i-C3H7CN, C2H5OCH3, 1-c-C5H5CN, 2-c-C5H5CN, CH3C7N(?), n-C3H7OH, i-C3H7OH
H
Mainly detected by radio observations>12 Atomss (3 Species)(Gray: Detected only toward AGB stars)
C60, C70, C60+, c-C6H5CN, HC11N, 1-C10H7CN, 2-C10H7CN, c-C9H8, 1-c-C5H5CCH, 2-c-C5H5CCH+RZWKH\IRUPHGDORQJVWDUIRUPDWLRQ"+RZWKH\GHOLYHUHGWRSODQHWV"$Q\UHODWLRQWRWKHELUWKRIOLIH"

(The Cologne Database for Molecular Spectroscopy (CDMS): June. 2022)

安宲宵宰室宷宬宲宱季宲宩季室宷宲宰家
孫宑宸宦宯宨宲家宼宱宷宫宨家宬家季宬宱季家宷室宵家孬
安宲宵宰室宷宬宲宱季宲宩季宧宸家宷孫宐孲宆季宊宬室宱宷家孯季宖宑孬

Diffuse Ionized gas T ~ 100 K
ÆHI cloud (Neutral atoms)ÆMolecular CloudAtom

H3+, H2

C

e.g. O Æ OH Æ CO

室孬季宧宬宩宩宸家宨季室宷宲宰宬宦季宦宯宲宸宧孳孬季宧宨室宷宫 宲宩季家宷室宵家

Ice(dust)surface

T ~ 10K
Density>105cm-3
䞉 Depletion宥孬季宰宲宯宨宦宸宯室宵季宦宯宲宸宧季孫宪室家季室宱宧季宧宸家宷孬䞉 Hydrogenation
e.g. CO Æ CH3OH

宩孬季宰室宷宸宵宨宧季家宼家宷宨宰
孫家宷室宵季室宱宧季害宯室宱宨宷室宵宼季家宼家宷宨宰孬宦孬季宧宨宱家宨季宦宯宲宸宧季宦宲宵宨Evaporation
Gas-phase reactions
宨孬季害宵宲宷宲家宷室宵 室宱宧季害宵宲宷害害宯室宱宨宷室宵宼 宧宬家宮

dust surface&KHPLFDO(YROXWLRQ

20K < T< 100K
Dynamical change of physical宧孬季害宵宲宷宲家宷室宵孯季害宵宲宷宲家宷宨宯宯室宵孰宨宱容宨宯宲害宨孲宧宬家宮孯季室宱宧季宲宸宷宩宯宲宺孲宭宨宷condition, Diffusion of heavier
elements on dust, Gas-dust
Ice(dust)surface
interactionÎ Complex organics

Chemical Composition in Cloud-Core (Envelope) Scale
Rich in unsaturated COMs (Warm Carbon-Chain Chemistry)

L1527: Yoshida, NS+ (2019) Pub. Astron. Soc. Japan

Parent Cloudc-C3H

Dense Core(Protostellar Core)

DC3N

N2H

c-C3H2c-C3HRich in saturated COMs (Hot Corino Chemistry)
NGC1333IRAS4A: Lefloch,,,,NS+ (2018) Mon. Not. Astron. Soc.
13CS

CH3NH
CH2DOH

HDCS

Protostar

Envelope

CH3OH
SO2

CH3OH

CH3CHO

S18O

CH3OH

Jet/Outflow

Which is the dominant case ? Which is the case for our solar system??

Perseus Chemical Survey
Exploring core (~5,000 au) scale diversity(Nobeyama 45 m + IRAM 30 m survey toward Class0/I sources@2014-2016)

10
0 pc
20
0 pc

Orange: Dust, Green Contour: CO(Hatchell et al. 2005, A&A, 440, 141; 2007, A&A, 468, 1009)(Higuchi, NS et al. 2018, ApJS, 236, 52)

Chemical Diversity in Perseus

Narrow dV component

Diversity in envelope size scale (~5,000 au)
Hot Corino

HybridWCCC

How about in protoplanetary-disk size scale ?
~100 au(Higuchi, NS et al. 2018, ApJS, 236, 52)㻾㼍㼐㼕㼛㻌㼀㼑㼘㼑㼟㼏㼛㼜㼑䠖㻸㼛㼣㼑㼞㻌㻿㼜㼍㼠㼕㼍㼘㻌㻾㼑㼟㼛㼘㼡㼠㼕㼛㼚㻿㼕㼚㼓㼘㼑㻙㻰㼕㼟㼔䠖 㼍㻌㼒㼑㼣㻌㻝㻜㼟㻌㼍㼞㼏㼟㼑㼏 㼏㼒㻧㻌㻿㼁㻮㻭㻾㼁㻌㻔㻵㼚㼒㼞㼍㼞㼑㼐㻙㻻㼜㼠㼕㼏㼍㼘㻕䠖㻜㻚㻞㻙㻜㻚㻜㻞㻌㼍㼞㼏㼟㼑㼏㻭㻸㻹㻭㻦㻌㻭㼠㼍㼏㼍㼙㼍㻌㻸㼍㼞㼓㼑㻌㻹㼕㼘㼘㼕㼙㼑㼠㼑㼞㻛㼟㼡㼎㻙㼙㼕㼘㼘㼕㼙㼑㼠㼑㼞㻌㻭㼞㼞㼍㼥High angular resolution
1” Æ <0.01”-0.1”

Altitude: 5000 m

High sensitivity
100 hours Æ 10 min.

Main antenna : 12 m x 50
ACA antenna: 12 m x 4, 7 m x 12
Total:66㻣㻌㼙㼙㻌㻙 㻜㻚㻠 㼙㼙㻌㻔㻠㻜㻌㻙 㻥㻠㻜 㻳㻴㼦㻕㻌㻞㻜㻝㻠㻘㻌㼒㼡㼘㼘㻌㼛㼜㼑㼞㼍㼠㼕㼛㼚㻌㼟㼠㼍㼞㼠㼑㼐Europe, North America, and East Asia in cooperation with ChileFormation of Planetary System & Observational Challenges
Molecular Cloud

Dense
Core

Star formationSt
form
mationProtoplanetary Disk

Planetary System

Protostar~100 auEnve
Envelope
velopee
OutflowOu
utflow

Cloud Core

Envelope

c-C3H2c-C3H2 & SO

Disk Substructure
Planet Formation

Disk

0.7 cm dust continuum

CCH

3000 au
Association/ Infall
Sakai+ (2010)
Astrophys. J.

PdBI

500 auCentrifugal Barrier
Sakai+ (2014)
Nature100 auALMA

Accretion (soft) shock
Sakai+ (2017)
Mon. Not. R. Astron. Soc.
Mo

15 au
Gap/Ring :Nakatani, Sakai+ (2020)
Astrophys. J., 895. L2
Warped : Sakai+ (2019) Nature,565, 206

VLA

PErseus ALMA CHEmical Survey
ALMA data:
PI Sakai~50 YSOs Weakest cont.
in Perseus
d~300 pc
Strong cont.
COMs non-detection(SO/SO2 detection)

Strongest cont.

Contours: Continuum@1.3mm
0.0006, 0.003, 0.015, 0.03, 0.06 [Jy/beam](Yang, Y-L, NS+2021, ApJ, 910, 20.)

PErseus ALMA CHEmical Survey

ALMA data:
PI Sakai~50 YSOs
in Perseus
d~300 pc

Zhang, Yichen
Continuum
Outflows

Yang, Yao-Lun
COMs analysis
Higuchi, Aya
Calibrations

Zeng, Shaoshan.
D/H ratios
N-bearing
Mullio, Nadia
Multiplicity
Chem.Calc

Zhang, Ziwei Artur de la Villarmois,
Elizabeth
SO
SO/SO2Excit.
O/S
Calc.
S-bearing(Yang, Y-L, NS+2021, ApJ, 910, 20.)

Oxygen vs Nitrogen Chemistry
ALMA data:
PI Sakai~50 YSOs
in Perseus
d~300 pc

Normalized by
Tb,cont, Tb,contLbol, Tb,contTbol

Beautiful correlation between CH3OH and CH3CN
Chem. relation & Large abundance range (>102 times).
(Yang, Y-L, NS+2021, ApJ, 910, 20.)

Chemistry in Gaseous Envelope/Diskʀ How common is the WCCC & Hot-Corino Chemistry ?
Semi-statistical chemical surveys in disk forming scale (100-300 au)
PEACHES (50 YSOs in Perseus): e.g. Yang, Y.-L., Sakai+2021, ApJ, 910, 20
ORANGES (19 YSOs in Orion): e.g. Bouvier, M.,,Sakai+2022, ApJ, 929, 10
ALMASOP (56 YSOs in Orion): e.g. Hsu, S.-Y.,, Yang,Y.-L.+2022, ApJ, 927, 218
Ophiucus (12 YSOs in Oph.): Artur de la Villarmois, E.,Sakai+2019, A&A, 626, A71--Diversity in disk forming region is confirmed. Regional difference is significant.
--”Hybrid” type sources are commonly seen.
Perseus (PEACHES) 58% /Orion (ORANGES/ALMASOP) 26-40% /Ophiuchus 0%
ORANGESʀ What is the origin of the diversity? (branching?)
Large dynamic range observations vs chemical/physical models
WCCC become active @ low T or low Av during starless phase
Chem. network model (e.,g, Aikawa,Y.,,NS+2020, ApJ, 897, 110)

ʀ Any other axis on chemical diversity?
Detailed chemical compositions in <a few 10s au scale
ALMA Large Project FAUST (~70 members)
Co-PIs: Yamamoto, S., Ceccarelli, C., Chandler, C., Codella, C., and Sakai, N.

13 representative YSOs: e.g. Codella, C.,, Sakai+2021, Frontiers in A.S.S. 8, 782006

&KHPLVWU\LQ,F\*UDLQ0DQWOHVCORINOS Project Lead by Dr.. Yao-lun Yang.
(Yang, Y.-L,,,Sakai+2022, ApJ, 941, L13)
-Press released-Focused by “Nature Astronomy”

JWST MIRI MRS spectrum of a Class 0 protostar IRAS 15398-3359

/RFDWHRXU6RODUV\VWHPLQWKHGLYHUVLW\

Case for the Solarsystem?

Molecular Cloud
Protostellar System
Protoplanetary Disks
Time
21

Spectrum taken toward NGC2264CMM3A(0.2” resolution with ALMA)(20” resolution with ASTE)

Observing Gas Cell instead of the Sky(PLVVLRQQ6SHFWURPHWHU

CMB 2.7 K Interstellar Clouds(>10 K)
Protostellar hot core (~300 K)
77 K

Telescope
SIS/HEB
B
mixer

;

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dryy pumpsampleὉWide
e frequencyy coverageὉReliable
e intensityὉNarrow
w linee widthAuto-correlators

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Spectrometers

Disadvantage: low sensitivity for 1 line detection&RQYHQWLRQDOO$EVRUSWLRQ
Q6SHFWURPHWHU;~

Detector(InSb,, etc.)

dryy pumpMOD

samplePSD

(Watanabe, Y.,,,Sakai,N+2021, PASJ, 73, 372)

SUMIRE “Observing” gas-cell instead of the sky

SSpectrometer Using superconductor MIxer REceiver in RIKEN

Gas Cell
XFFTS
ALM
ALMA
MAM
A-ty
type
y
ype
Cartridge
Cartrid
Cartr
ridg
idge
id
dge ReceiverRe
eceiver
eceiveec(in collab./w UEC&NAOJ)

Liquid N2

Receivers- 215-265 GHz band (ALMA-B6, SIS)
- 270-500 GHz band (ALMA-B7+8, SIS)
clock Rb-GPS

XFFTS

Freq. accuracy: ~ 1 kHz
Int. accuracy: 5-10%
Determine
accurate frequency &absolute intensity (Sǌ2)

CH3OH Spectrum taken by SUMIRE(Watanabe, Y., Chiba, M., Sakai,T., Tamanai, A., Suzuki, R., & Sakai, N. 2021, PASJ, 73, 372)

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1*&&00$(Shibayama,Watanabe,,NS+2021, ApJ, 918, 32)

Intensity-Calibrated Spectroscopy
Workss lead byy Dr.. Oyama,, T.

CH2DOH13
3CH
H2DO
DOH 
D
experimentexperiment

preliminaryEstimation 
R branch

Q branchby JPL program

R-branch

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Q-branch

by JPL program



IUHTXHQF\0+](Ohno, Y., Oyama, T., ,NS+2022, ApJ, 932, 101)

(Oyama, T., NS+2023, in press.)

In JPL(NASA) web site

Formation of Interstellar Molecules
Gass Phase

Grainn Surface

102 – 108 cm-3, 10 – 100 K
A+BÆC+D
A + B Æ AB
B˕

Mdustt//M
Mggas 㹼 0.01
Size 㹼 0.1
0 ǌP

ʹSilicate core

- Binary reaction- Exothermic- No reaction barrier

Ice mantle

ex. H3+ + C Æ CH+ + H2
Photo:: Tauruss Molecularr Cloud- Hydrogenation- Condensation
ex. O + H Æ OH
+ H Æ H2 O
CO+H Æ HCO
ÆÆ CH3OH

Gas-Solid Interaction could be the KEY for COMs Formation
Cloud

Star Formation
matio

Dense
Core

Chemistry in
Low T & n

Envelopw

Protostar~100 au

Sensitive toreactiondynamics

Surface diffusion

Quiescent chemistry

Planetary System line
our Solar system)

Chemistry in Protoplanetary disk forming
Regions

H

Dust

Protoplantary Disk

Dust

1 au : Averaged distance
between the Suns and the Earth

Chemistry in
Terrestrial Condition

Branching ratios
Energy barrier
Depletion Desorption
Surface Diffusion

Dust

Classical view
T~300, normal density

H, O, C, N, S ї OH, CO, HCO+ … ї CCH, CH3OH, CH3CN … ї HCOOCH3,
NH2CHO … Amino-achid, more Complent values ÆRIKEN-Pioneering Projectࠕr-EMU: Evolution of
Matter in the UniverseࠖQuantum chemical calc.
Takayanagi (Saitama-Univ.)
Yamasaki (Hirosaki-Univ.)

r-EMU Team: Nucleus
r-EMU Team: Atoms
A03 Team: Theory

Cosmic ray ionization Chemical network calc.
Isotope/Element Ratios Physical evolution model.
r-EMU Team: Molecules
Aikawa, Y. (Univ. of Tokyo)
Energetic events
THz, Excitation Analysis, Dust evolution Evolved stars/Dying stars

ModelsChemical Evolution
Physical Evolution

A01 Team: Observation

Observations

Sakai, N (RIKEN, CPR)
Spectroscopy: in collab. w. NAOJ/UEC
Observation

A02 Team: Analysis
Distribution
Abundance
Spectroscopy

Gas-Phase
Reaction
A04 Team: Gas-Phase Reaction

Planetary
Science
Mineralogy, Link to
HAYABUSA 2-636ָढ़รַ྘Ү$)<
3,1DPL6DNDLBranching Ratio
Reaction Rate
Reaction Barrier

The Solar System

Return Samples
Tachibana, S. (Univ. of Tokyo)

Depletion,
Desorption,
Dissociation,
Dispersion

Surface
Reaction

Ion - neutral-Atom: Nakano, Y. (Rikkyo Univ.)
Ion - polar-Mol.: Okada, K. (Sophia Univ.)
A05 Team: Surface Reaction
Ion – isomers: Tanuma, H. (Tokyo Met. Univ.)
Micro: Imada, H., Kim, Y. (RIKEN, CPR)(яNeutral-Neutral: I. Sims (Rennes1, France) ) Macro: Watanabe, N. (Hokkaido Univ.)

Hopping

Rotation

Reactionex) Innovation Originates from “Astrochemistry”
Carbon-chain molecules

HC5N

New field of nanoscience(1990~)
C60

Graphene

L. W. Avery, N. W. Broten, J. M. MacLeod,
T. Oka, and H. W. Kroto, ApJ, 205 (1976), L173

Formation of HC5N in the laboratory. Measuring rest
frequencies ofrotational transitions of HC5N

A.J. Alexander, H.W. Kroto, D.R.M. Walton
J. Mol. Spectrosc., 62 (1976), pp. 175–180

FullereneSuperconductivity,, Photoo Absorbent,, Catalyst,
w Thermall Conductivity,, Freee radicall
Low
Scavenger,, Cagee Structure,, Electronn Accepter,, etc.
c.

Carbon nanotube(ÆFuel Cell, Conductive Transparent Thin Film, Electronic Conductive
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Themes & Members
Chief Scientist: Nami Sakai
Theme (A) Chemical Evolution from Clouds to Planets
Yao-lun Yang, Ziwei Zhang, Shaoshan Zeng,
Yuki Okoda, Yui Kawashima, (Shota Notsu@UT)

Theme (B) Star and Planet Formation

Naida Murillo, Ross Burns, Ryota Tominaga,(Riouhei Nakatani@JPL), (Yichen Zhang@UVA), (Satoshi Ohashi @NAOJ)

Theme (C) Tools: Spectroscopy & Dust Experiments

Takahiro Oyama, Akemi Tamanai, (Satoshi Ohashi @NAOJ),(Yoshimasa Watanabe @SIT & Students), (Takeshi Sakai @UEC & Students)
S d)
As of Apr. 2023 PI, Sub-leader (Staff Scientist), PD, SPDR, (Visiting-Staff)

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Main Collaborators