ALMA による z = 6-9 銀河の性質と南極 THz 望遠鏡への期待nakai/astroobs/pdf/Hashimoto...2019/12/21 · ALMA による z = 6-9 銀河の性質と南極 THz 望遠鏡への期待

ALMAによるz=6-9銀河の性質と南極THz望遠鏡への期待

橋本拓也

筑波大学宇宙史研究センターテニュアトラック助教(卓越研究員)

Outline

l  Introduction-Cosmicreionization-Galaxiesintheepochofreionization(EoR) -Spectroscopy

l  Rest-frameFIRpropertiesatz>7withALMA-Casestudy: propertiesofaz=9.1[OIII]88μmemitter-Statistics: HighratiosofL[OIII]88μm/L[CII]158μm inhigh-zLAEs/LBGs

l  (SomethoughtsonAAT)

Outline



l  SomethoughtsonAAT

CosmicReionization

l  Reionization:z~20-6(tuniv~200Myr-1Gyr)l  Hydrogenionizingphoton(LyC:λ<912ÅorE>13.6eV)l  Keyquestions

-Whatisthemaindriverofreionization?-How,whenandwherereionizationhasprocessed?

TheBigBang

Fullyionizedneutralized

Recombination

firststars/galaxies Reionization Fullyionizzed

YearsaftertheBigBang0 13.8billion100Myr 1billion

1＋z1000 100 10 1

©NAOJ

CosmicReionization


-Whatisthemaindriverofreionization?!Recentconsensus:abundantUVstar-forminggalaxies aresufficientwithoutdemandingPopIIIstars(e.g.,Robertson+15)

TheBigBang


Recombination



1＋z1000 100 10 1

©NAOJ

cf.,bluecompactgalaxies

CosmicReionization


-Whatisthemaindriverofreionization?-How,whenandwherereionizationhasprocessed? àfuture21cmobservationsintheEoR(割愛)

TheBigBang


Recombination



1＋z1000 100 10 1

©NAOJ

l  Galaxycandidatesatz≈8-11owingtoHSTandSpitzerl  Statisticalproperties(UVLF,SFRD)

TheBigBang


Recombination



1＋z1000 100 10 1

©NAOJ

GalaxiesintheEpochofReionization

GalaxiesintheEpochofReionization

l  SpectroscopicpropertiesintheEoRareyettobeconstrained(redshiftidentification,Z,U,ne)

l  Galaxyformationandevolution•  Ancestorsofpresent-daygalaxies•  Originofheavyelements(O,C,Netc.)andcosmicdust•  Starformingactivity&ISMproperties(e.g.fesc,Z,U,ne)

TheBigBang


Recombination



1＋z1000 100 10 1

©NAOJ

Spectroscopyatz>7

A.K.Inoueetal.2016,Science

Harikane+18観測波長[Å]=(1+z)x静止系波長

l  Lyαispowerfulatzupto~7(e.g.VLT/MUSE:Bacon+17,Hashimoto+17b)l  butstronglyattenuatedbytheIGMatz>7(e.g.Stark+10,Pentericci+12)!Alternativeemissionlineisessential

[OIII]88μm

[CII]158μm

[NII]122μm

1216Å

ALMAobservationsatz>7


Harikane+18

[OIII]88μm

[CII]158μm

[NII]122μm

l  Far-infraredfinestructurelinesareuseful•  metallicity,U,ne(Nagao+12,Pereira-Santaella+18)

l  Dustcontinuumcanbesimultaneouslyobserved•  star-formationactivity(dustproduction/growth/destruction)

NOEMA

ObservedWavelength[Å]=(1+z)xλrest10/51

l  ~20[CII]detectionsatz~5-7galaxies(e.g.Carniani+17,Smit+18)Manydetectionsinhigh-zQSOsl  Non-detectionsarereportedatz>7(Ouchi+13,Ota+14)

Atraditionaltoolathigh-z:[CII]158μm

z=6.8LBGSmitetal.2018Nature

z=5.5LBGCapaketal.2015Nature

ALMA[CII]HSTUV

11

[OIII]88μminthelocalUniverse


l  ISOmetalrichspirals,L[OIII]≈0.5xL[CII](e.g.Malhotra+01,Brauher+08)l  Herscheldwarfgalaxies,L[OIII]≈2xL[CII](e.g.Madden+12,Cormier+15)SomeobjectshaveL[OIII]≈10xL[CII]

[OIII]/[CII]luminosity

ratio

10

1

localmetalrichspirals

10610810101012

LIR[Lsun]

Madden+12

Thefirst[OIII]88μmdetectionintheEoR


l  LAEatzLya=7.21withEW0(Lyα)=33Å(Shibuya+12)•  ALMABand8follow-upobservations(PI.A.K.Inoue)

Contours:ALMA[OIII]bkg:SubaruLyα

5.4σ

l  Band6[CII]isundetected;L[OIII]/L[CII]>12(3σ:laterdiscussion)l  Thispioneeringworkopensanewwindowinstudiesofreionization

Inoue,Tamura,Matsuo+16Science

5.4σ

MorethanN>15[OIII]88μmintheEoR


5.4σ

Inoue+16Carniani+17Laporte+17Hashimoto+18LAELAELAE/LBGLAE/LBG

Hashimoto+19aTamura+19Marrone+18Walter+18Hashimoto+19bLAE/LBG LBGpair-SMGSMGandQSO2QSOs

alsoHarikane+19;Sunaga+inprep.

Outline




•  AlensedJ-banddropoutgalaxy(Zheng+12,Nature)•  Bright(H=25.7)withamagnificationfactor(μg)~10•  Oneofthehighest-zgalaxycandidateaccessiblew.ALMA

Zheng+17

JD1

(1)MACS1149-JD1

4”.6

W.Zheng+17

HSTandSpitzer/IRACimagesofJD1

JD1detected

JD1undetected

3.6μm4.5μm

•  zph=9.6±0.2(Zheng+12)•  Lateratzph≈9.0-9.8(Bouwens+14,Huang+16,Kawamata+16,McLeod+16,Zheng+17)

Zheng+17

SEDofJD1

J125

JH140 H160

Spitzer/IRAC[3.6]&[4.5]

18

l  zOIII=9.1096±0.0006

l  SED(K.Mawatari)analysesshowage≈300Myratz=9!zform≈15±2

-白色の等高線:酸素-背景の画像：紫外光(HST)

7.4σ

7.4σ

Contours:ALMA[OIII]Bkg:HSTF160Wrest-UV

Hashimoto+18Nature

[OIII]88μmdetectionatz=9.11

FWHM=154±39kms-1

•  ALMABand7inCy3Ttot≈8.7hrs(PI:A.K.Inoue)•  Wecoveredthezphrange(9.0–9.8)with4ALMAtunings

7.4σ<3σ

l M*≈1x109x(10/μg)M¤　fromSED-fitl  log(Md-to-M*)<-4to-3(3σ)forTd=60-30K(c.f.,Popping+17)cf.,log(Md-to-M*)≈-4to-1@M*≈1x109M¤atz=0"Usefulconstraintfortheoreticaldustmodels(e.g.,Calura+17)

Dustcontinuum@90μm

Sν,90μm<5.3x(10/μg)μJy/B(3σ)

DustcontinuumisundetectedinJD1

MBB:

l  Deepfollow-upobservationsfor[CII]158μm(PI:N.Laporte)l  Similarbeamsizeasusedin[OIII]88μmobservations

Laporteincl.TH+19

l  L[OIII]/L[CII]>18.5(3σ;thehighestratiotodate:laterdiscussion)

green![OIII]88μmblue![CII]158μm

21

[CII]158isundetectedinMACS1149-JD1

Outline




[OIII]88/[CII]158luminosityratio@z=6-9

ForLAEs/LBGs:Td=50Kβ=1.5isassumed

[OIII]35eV[CII]11eVhighly-ionizedISMhasalinehighratio

Hashimoto+19aseealsoTH+19b

l  Anti-correlationbetween[OIII]/[CII]andLbol.

[OIII]88/[CII]158luminosityratio@z=6-9

l  Anti-correlationbetween[OIII]/[CII]andLbol.

[OIII]35eV[CII]11eVhighly-ionizedISMhasalinehighratio

Bakxincl.TH+20inprep

SMGsLBGs

LBG/LAELAE

LAE

JD1

YD4

Y1LBG

ForLAEs/LBGs:Td=50Kβ=1.5isassumed

Ubiquitouslyhigh[OIII]/[CII]ratiosatz>6

l  CMBsupressionon[CII]?-TCMB>20Kcf.,[CII]Tex≈92K(dashed-line:insufficient)

l  High-ionizationparameterintheISM?(Inoue+16,TH+19a)-[OIII]Pion(35eV)vs.[CII]Pion(11eV) !LyCescape??

l  SomecluesonO/C?(needionizationcorrection)è Detailedmodelingwillbeperformed(seealsoHarikane+19)　è InitialresultshighlighttheunusualISMconditionsintheEoR

Laporteincl.TH+19

25

◯localgalaxies●Simulations(Lagache+18,0.1Z¤)

High-zgalaxies

OngoingWorksofOurTeam

①Morpho-kinematicpropertiesatz=8-92ALMACy6projectswith“A”(PIs:Hashimoto,Tamura)àAreferencestudyforfutureJWSTandELTsscience

>10σ

Cycle3+4+6(θ~0”.3)

Tokuoka,TH+inprep

Combineddatahaveintrinsicresolutionof~500x400pc2

Moriwaki+18

OngoingWorksofOurTeam

②[OIII]88μmforfivez~10candidates2ALMACy7projectswith“A”-33hrs(PIs:Hashimoto,Tamura)àHST+Spitzerで得られる現在最高のサンプルà2supplementaryVLTobservationsongoing(PI:Hashimoto)

rest-frameUVlinesàIfconfirmed,strong(est)JWSTandELTtargets

③Multiplelinestudyfor“BigThreeDragons”atz=7.15[OIII]52,[NII]122,CO(7-6)&CO(6-5)&[CI](2-1)

3ALMACy7projects“B”(PIs:Matsuo,Inoue,Hashimoto)!AcomprehensiveunderstandingofISMintheEoR　　　criticaldensity;nitrogenabundance,metallicity,gasproperties

Outline




DustemissionintheEoRz=6.90lensedSMG(s)Marrone+18Nature

Originallydiscoveredasabright2.0and1.4mmsourcebythe2500deg2SPTsurvey

~10mJy!!

HerschelSPIREFoV:8’x4’θ:18-36”

ALMA

AAT SPT

CombinationofAAT&SPTcanfindsuchextremelydustygalaxiesintheEoRTowardacompletepicture(UV+IR)ofSFRDevolution(Madau&Dickinson2014)

DustemissionintheEoRz=6.90lensedSMG(s)Marrone+18Nature

ALMAfollow-upobservationstargetingdust,[CII]158,[OIII]88

l  EandWcomponenthasLIR=(4.6±1.2)and(33±7)x1012L¤l  EandWcomponenthasMdust=(0.4±0.2)and(2.5±1.6)x109M¤

l  [OIII]/[CII]luminosityratiois~2.0and0.5l  [OIV]26μmwithATTorSPICA!AGNactivity

DustemissionintheEoR

l  4(normal)star-forminggalaxies(i.e.,LBGs)withdustcontinuumbeyondredshiftz=7uptoz=8.3allachievedwithALMA!

Object redshift λrest[μm] Sν[μJy] Ref.

A1689-zD1 ~7.5 90160

1670±360560±100

Inoue&Hashimoto+20subm.Watson+15Nature

B14-65666 7.15 90160

470±128130±25

Hashimoto+19a

A2744_YD4 8.38 90160

99±23<11(3σ)

Laporte+17Laporteincl.TH+19

MACS0416-Y1 8.31 90160

137±26<18(3σ)

Tamura,Mawatari,TH+19Bakx,Tamura,incl.TH+20

HighTdinhigh-zstar-forminggalaxies?

Object redshift Td Ref.A1689-zD1 ~7.5 63–92K Watson+15

Inoue&Hashimoto+20B14-65666 7.21 50–60K Bowler+18

Hashimoto+19aA2744_YD4 8.38 60–100K Behrens+18MACS0416-Y1 8.31 >90K Bakx,Tamura,incl.TH+20

l  Alargersampleiscrucialforadefitniveconclusionl  HighTdduetocompactstar-formation,strongUVradiation(e.g.,Inoue&TH+20)l  PartlyresolvetheIRX-βUVanddustmassbudgetproblems(Faisst+17,Behrens+18)

l  HighTdleadstoadustpeakathigherfrequency(shorterwavelength)!strategy

2020-2030年代に向けてl  多波長間の連携が極めて重要

l  Subaru/HSC(<0.6um)+WFIRST(mid2020:0.6-2um) 2000平方度

l  WISH(Inoue,Kodama,Iwata+)今後提案2-5um

100平方度27.5mag(5σ)cf.,JWSTは視野小l  AAT200um–1.5mm:広視野(1平方度)　　同程度(>100平方度) の探査領域が重要(後述)

NASA2020decadalsurvey

2020-2030年代に向けて①例えばz=15のLBG(紫外選択天体)を考えるLyman-breakat(1+15)*1216Å~20000Å=2um要は、2umまで見えない天体(深い未検出を確定するためデータは必要...HSC+WFIRST)

l WISH(2-5um)で静止系可視　　z=15LBGが選択可能になる

銀河の静止系紫外スペクトル

λrest=1216Å

λrest=912Å

2020-2030年代に向けてl  例えばz=15のLBG(紫外選択天体)を考えるl  AAT(200um–1.5mm)で静止系中間赤外 – 遠赤外線 (13-94um)z=15LBGのダスト連続光ピーク付近を抑えることが可能！重要輝線:H2分子輝線17/28um;[OIV]26um,[OIII]52/88umなど!個別で未検出でも多数スタックして平均像は得られる。②静止系紫外-可視で暗く赤外で明るいdustySB@z>10AAT(200um–1.5mm)+SPT(1.2–3.0mm)同様に、静止系紫外 – 可視(観測波長5um程度まで)データは必須多波長の2020-2030年代サーベイ予定を考慮しつつ、feasibility(感度、探査領域etc.) が重要。!ALMA2を通して詳細な分光フォローアップ

Documents

ALMA による z = 6-9 銀河の性質と 南極 THz 望遠鏡への期待nakai/astroobs/pdf/Hashimoto...2019/12/21 · ALMA による z = 6-9 銀河の性質と 南極 THz 望遠鏡への期待

ALMA による z = 6-9 銀河の性質と南極 THz 望遠鏡への期待nakai/astroobs/pdf/Hashimoto...2019/12/21 · ALMA による z = 6-9 銀河の性質と南極 THz 望遠鏡への期待