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 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
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
l Reionization:z~20-6(tuniv~200Myr-1Gyr)l Hydrogenionizingphoton(LyC:λ<912ÅorE>13.6eV)l Keyquestions
-Whatisthemaindriverofreionization?!Recentconsensus:abundantUVstar-forminggalaxies aresufficientwithoutdemandingPopIIIstars(e.g.,Robertson+15)
TheBigBang
Fullyionizedneutralized
Recombination
firststars/galaxies Reionization Fullyionizzed
YearsaftertheBigBang0 13.8billion100Myr 1billion
1+z1000 100 10 1
©NAOJ
cf.,bluecompactgalaxies
CosmicReionization
l Reionization:z~20-6(tuniv~200Myr-1Gyr)l Hydrogenionizingphoton(LyC:λ<912ÅorE>13.6eV)l Keyquestions
-Whatisthemaindriverofreionization?-How,whenandwherereionizationhasprocessed? àfuture21cmobservationsintheEoR(割愛)
TheBigBang
Fullyionizedneutralized
Recombination
firststars/galaxies Reionization Fullyionizzed
YearsaftertheBigBang0 13.8billion100Myr 1billion
1+z1000 100 10 1
©NAOJ
l Galaxycandidatesatz≈8-11owingtoHSTandSpitzerl Statisticalproperties(UVLF,SFRD)
TheBigBang
Fullyionizedneutralized
Recombination
firststars/galaxies Reionization Fullyionizzed
YearsaftertheBigBang0 13.8billion100Myr 1billion
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
Fullyionizedneutralized
Recombination
firststars/galaxies Reionization Fullyionizzed
YearsaftertheBigBang0 13.8billion100Myr 1billion
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
A.K.Inoueetal.2016,Science
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
A.K.Inoueetal.2016,Science
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
A.K.Inoueetal.2016,Science
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
A.K.Inoueetal.2016,Science
5.4σ
Inoue+16Carniani+17Laporte+17Hashimoto+18LAELAELAE/LBGLAE/LBG
Hashimoto+19aTamura+19Marrone+18Walter+18Hashimoto+19bLAE/LBG LBGpair-SMGSMGandQSO2QSOs
alsoHarikane+19;Sunaga+inprep.
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
• 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
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
[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
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
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