Quest to understandthe origin of the Solar system
Nami Sakai (CPR, RIKEN)
Supported by
KAKENHI: Grant-in-Aid for Transformative Research Areas（A）FY2020-FY2024
RIKEN Pioneering Research Project ”Evolution of Matter in the Universe (r-EMU)” FY2019-FY2023

Existence of “life”
Common or Miracle?

(From PIXTA)(From NASA)“Where do we come from?” ”How did we get here?”(From PIXTA)Why Baryon?
Matter in the Universe

Dark energy

O

Dark matter

68 %

27 %

N

5 %

Baryon(~“Atom”)

H

71 %
27 %
2%

Heavy elements

HeNeCHistory of formationof Matter
Structure Formation

138 Billion years
10 Billion years

Chemistry/Material Science

4 Billion years
The Dark Ages
Big Bang

380
Thousand years-35
Quantum 10 m
10-32mGravity /10-15mNeutrino
Superstrin
Quark-Gluong Theory
PlasmaCosmicSupersymmetry/
Microwave
Grand Unified
Background First Generation
TheoryStar

History of Structure Formation

Origin of life /Astrobiology
CosmicReionization

GalaxySupermassive
Black HoleStar
Formation

PlanetFormation(The Solarsystem)INTEGRAL(107 K)

Herschel

JWSTSubaru
TMTALMA(10 K)

XRISM

AKARI

EVLA

Hyperfine spectra,
Heavy moleculesRotationalTransitionsof simple molecules

Vibrational
Transitions

ElectronicTransitions

NuclearReaction

Molecules in Space (~275 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, FeO (?), O2, CF+,SiH (?), PO, PO+, 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)↓iCOMs (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, CH2CHCHO , CH2CCHCN, H2NCH2CN, CH3CHNH, CH3SiH3, H2NC(O)NH2, HCCCH2CN,
HC5NH+, CH2CHCCH, MgC6H, C2H3NH2, (CHOH)2
9 Atoms (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(The Cologne Database for Molecular Spectroscopy (CDMS): June. 2022)

GBT Observations of TMC-1:
Hunting Aromatic Molecules (GOTHAM)

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)QUIJOTE: Q-band Ultrasensitive Inspection
Journey to the Obscure TMC-1 Enviroment:
Discovering the limits of chemical complexity

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Formation of atoms(Nucleosynthesis in stars)
Formation of dust
(M/C Giants, SN)

Diffuse Ionized gas T ~ 100 K
HI cloud (Neutral atoms)
Molecular CloudAtomH3+, H2Ce.g. O  OH  COa) diffuse atomic cloud0) death of stars

Ice(dust)surface

T ~ 10K
Density>105cm-3・ Depletionb) molecular cloud (gas and dust)・ Hydrogenation

e.g. CO  CH3OHf) matured system(star and planetary system)

Evaporation
Gas-phase reactionsc) dense cloud coree) protostar and protpplanetary disk

dust surface

Chemical Evolution

8/22

20K < T< 100K
Dynamical change of physicald) protostar, protostellarenvelope/disk, and outflow/jet
condition, Diffusion of heavier
elements on dust, Gas-dust
Ice(dust)surface
interaction 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-C3H

Rich in saturated COMs (Hot Corino Chemistry)

NGC1333IRAS4A: Lefloch,,,,NS+ (2018) Mon. Not. Astron. Soc.

CH2DOH

CH3NH

13CS

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 pc
20 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)

Radio Telescope：Lower Spatial Resolution
Single-Dish： a few 10s arcsec cf; SUBARU (Infrared-Optical)：0.2-0.02 arcsec

ドイツ: MPIfR 100 m電波望遠鏡

14

ALMA: Atacama Large Millimeter/sub-millimeter ArrayHigh angular resolution
1”  <0.01”-0.1”

Altitude: 5000 m

High sensitivity
100 hours  10 min.

Main antenna : 12 m x 50
ACA antenna: 12 m x 4, 7 m x 12Total:66

7 mm - 0.4 mm(40 - 940 GHz)

2014, full operation started
Europe, North America, and East Asia in cooperation with ChileFormation of Planetary System & Observational Challenges
Molecular Cloud

DenseCoreStar formation

Protoplanetary Disk

Planetary System

Protostar~100 auEnvelope
Outflow

Cloud Core

Envelope

c-C3H2c-C3H2 & SO

Disk Substructure
Planet Formation

Disk

0.7 cm dust continuum

CCH3000 auAssociation/ Infall
Sakai+ (2010)
Astrophys. J.

PdBI

500 auCentrifugal Barrier
Sakai+ (2014)
Nature100 auALMA

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

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]COMs are found in
58% of the sources!

(Yang, Y-L, NS+2021, ApJ, 910, 20.)

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

Normalized byTb,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.)

Locate our Solar system in the diversity

Case for the Solarsystem?

Molecular Cloud
Protostellar System

Protoplanetary DisksTime19

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

Required accuracy for Doppler analysis
c-C3H2 & SOFrequencyVelocity

Thermal line width ~ 0.1 km/s
<<250 kHz @ 800 GHz=0.8 THz(Various high excitation lines)
ALMA

500 auCentrifugal Barrier
Sakai+ (2014)
Nature <<50 kHz @ 160 GHz(iCOMs)
ALMA/NOEMA & IRAM-30m

Line of sight velocity ofc-C3H2 molecule [km/s]

 <<5 kHz @ 16 GHz(Larger iCOMs e.g. with rings)
VLA & GBT/Yabes-40m

Infrared Thermometers-Measure energy from stars

Check human body for a feverby measuring the heat energyIdeal for anyone who may have to worry
about cross contaminationsuch as infants.

Technology Developed for Astronomy
Meets
Molecular Science ?

Heterodyne Radio-Receiver-Observe molecules in space

Intensity Measurement ofLines from Molecules

Determine temperature and abundance
without direct interaction with the gas.

Observing Gas Cell instead of the Sky
Emission Spectrometer

CMB 2.7 K Interstellar Clouds(>10 K)
Protostellar hot core (~300 K)
77 K
200Φ

dry pump

sample・Wide frequency coverage
・Reliable intensity
・Narrow line width

Telescope
SIS/HEBmixerX

Auto-correlators

LNA........

~ Local Osc.
Rx--UEC, UT, NAOJ--

Spectrometers

Disadvantage: low sensitivity for 1 line detection

Conventional Absorption Spectrometer

X~Detector
dry pump

MODsample(InSb, etc.)

PSD

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

SUMIRE “Observing” gas-cell instead of the sky

Spectrometer Using superconductor MIxer REceiver in RIKEN

Gas Cell
XFFTS
Liquid N2

ALMA-type
Cartridge Receiver(in collab./w UEC&NAOJ)

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

clock Rb-GPS

XFFTSFreq. accuracy: ~ 1 kHz
Int. accuracy: 5-10%
Determine
accurate frequency &absolute intensity (Sμ2)

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

Origin of the “Weeds”: Torsionally Excited Lines (vt=1)

Observation toward the disk
around a protostar,
NGC2264CMM3A(Shibayama,Watanabe,,NS+2021, ApJ, 918, 32)

Intensity-Calibrated Spectroscopy
13CH DOH
2experiment

R branch

Q branch

Estimationby JPL program(Ohno, Y., Oyama, T., ,NS+2022, ApJ, 932, 101)

In JPL(NASA) web site

RIKEN-Pioneering Project「r-EMU: Evolution ofMatter in the Universe」

Quantum 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

Distribution
Abundance
Spectroscopy

Gas-Phase
Reaction
A04 Team: Gas-Phase Reaction

A02 Team: Analysis

PlanetaryScience
Mineralogy, Link to
HAYABUSA 2

JSPS 学術変革領域A
FY2020-2025
PI: Nami Sakai

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)(⇔Neutral-Neutral: I. Sims (Rennes1, France) ) Macro: Watanabe, N. (Hokkaido Univ.)

Hopping

Rotation

Reaction