Deep extragalactic survey
with Tsukuba 10m THz
telescope

Yoichi Tamura (IoA, UTokyo)
Antarctic THz Workshop
NAOJ-Mitaka
18-19 November 20151

Outline❖ Continuum imaging survey❖❖❖❖

Introduction
Sensitivity estimate
Brief comments on science cases
Summary and requirements❖ Mid-z SF galaxies seen in FIR fine structure lines❖❖❖

Introduction[OIII]/[CII] survey
Sensitivity estimate

2

前提❖❖

10m 望遠鏡のサイエンスに特化します❖

どこに discovery space があるか？→ まずは feasibility study をしたい❖

GLT/CCAT との住み分け？ (Hirashita et al. 2015, arxiv:1511.00839)

30m 望遠鏡のサイエンスについては、関連する大口径望遠鏡 (LST) の検討資料をご覧ください❖ WS on “Large Aperture Millimeter/Submillimeter Telescope in the ALMA Era”
❖ LSTWS2011: http://www.ioa.s.u-tokyo.ac.jp/~ytamura/WS/WS2011❖ LSTWS2012: http://www.ioa.s.u-tokyo.ac.jp/~kkohno/ALMA/index.php?Workshop120929❖ LSTWS2015: http://www.ioa.s.u-tokyo.ac.jp/~ytamura/WS/LSTWS2015❖ New Trends in Radio Astronomy in the ALMA Era: The 30th Anniversary of Nobeyama (2012)❖ http://www.nro.nao.ac.jp/~nro30/html/Symposium2012❖ 宇電懇シンポジウム❖ 田村 (2012) http://www.ioa.s.u-tokyo.ac.jp/~ytamura/Wiki/?
plugin=attach&pcmd=open&file=ytamura_asteII_121222.pdf&refer=ASTE
川辺 (2015) http://alma-intweb.mtk.nao.ac.jp/~udencon/symp/symp2014/symp2014-kawabe.pdf❖❖ 田村 (2015) http://alma-intweb.mtk.nao.ac.jp/~udencon/symp/symp2014/symp2014-tamura1.pdf❖ 野辺山ユーザーズミーティング❖ 田村 (2011) http://www.ioa.s.u-tokyo.ac.jp/~ytamura/Wiki/?
❖plugin=attach&pcmd=open&file=ytamura_ct_110728.pdf&refer=ASTE
川辺, 河野, 田村他 (2012) http://www.ioa.s.u-tokyo.ac.jp/~ytamura/Wiki/?

❖plugin=attach&pcmd=open&file=ytamura_asteII_120726.pdf&refer=ASTE河野 (2013) http://www.nro.nao.ac.jp/~nroum/html/data/25b/NROUM-LargeTelescope-Kohno130725-toLOC.pdf❖ ASTE/ALMA Future Development Workshop❖ 田村 (2013) http://alma-intweb.mtk.nao.ac.jp/~diono/meetings/EA_Development_Meeting/Program_files/Tamura.pdf❖ 河野 (2014) http://alma-intweb.mtk.nao.ac.jp/~diono/meetings/ASTE_ALMA_2014/astealma-devws-kohno140618.pdf❖ 田村 (2014) http://alma-intweb.mtk.nao.ac.jp/~diono/meetings/ASTE_ALMA_2014/ytamura_astews_140617.pdf❖ 遠藤 (2014) http://alma-intweb.mtk.nao.ac.jp/~diono/meetings/ASTE_ALMA_2014/endo_aste_ws_dist.pdf

3Viewgraph from LSTWS 2015

RSD Redshift Space Distortion
CO/[CII] Tomography

Verify	  GR	  by	  estimating	  the	  growth	  rate	  of	  structure,	  dark	  energy	  problem

LSS Cosmic Large-Scale Structure
Investigate	  the	  correlation	  between	  dark	  and	  baryonic	  matters	  from	  clustering	  analysis,	  dark	  matter	  problem

EoR Epoch of Reionization
Search	  for	  earliest	  “hidden”	  galaxies,	  ﬁrst	  generation	  galaxiesEvolution ofGalaxies

Cosmic	  evolution	  of	  galaxies	  proved	  through	  properties	  of	  interstellar	  medium

CSFH Cosmic Star-formation History
Investigate	  mass/luminosity	  function	  of	  molecular	  gas	  as	  a	  function	  of	  redshift,	  “hidden”	  history	  of	  baryonic	  matter... and serendipitous discoveries
Line	  emitters,	  transient	  and	  variables,	  ...
Yoichi Tamura / Large Aperture Sub/mm Single Dish Telescopes in the ALMA Era

Continuum imaging survey

5Cosmic star formation history:
Roles of dusty galaxy population

Burgarella+...?

...?

Bouwens+

Burgarella et al. 2013❖❖

Cosmic SFR density (SFRD) peaks at z = 1-3.
What is the role of dusty galaxies at z > 4?

Madau & Dickinson 2014❖❖

Cosmic evolution of extinction.
What is the role of dust in z > 4 galaxies?

cosmic “obscured” star-formation throughthe cosmic time is still unknown.

6

AzTEC/ASTE 1.1-mm Survey❖❖❖

AzTEC 1.1mm camera (Wilson et al. 2008) on ASTE, in 2007/2008.
2 deg2, σ ~ 0.5–1 mJy/B, ~1400 SMGs, ~20 papers published (-2014 Aug.)❖1.1 mm number counts (Hatsukade+10; Scott+12), clustering(Hatsukade+, in prep.), relation with LSSs (Tamura+09; Aretxaga+11;Umehata+14, Umehata+15)❖Case studies: lensed SMGs (Wilson+08; Ikarashi+11; Takekoshi+13;
Tamura+15), SMGs w/ X-ray sources (proto-QSOs) (Tamura+10;Humphyley+11; Johnson+13)❖

Photo-z’s, redshift distribution (Yun+12; Umehata+14; Ikarashi+15)

ALMA follow-up observations on-going (Ikarashi+, Umehata+, Kohno+, Suzuki+for Cy1; Hatsukade+, Umehata+, Kohno+, Lee+ for Cy2; many for Cy 3)~2 deg2 in total
COSMOS
0.72 deg2

SXDS
0.25 deg2

ADF-S
0.2 deg2

SSA22GOODS-S
0.27 deg2 0.08 deg27

THz to ~1mm color(photo-z with dust SEDs)

Redshifted SEDs of dusty starbursts

20cm

1cm

5'cm'(JVLA/C%band)

1.3mm

870µm

Hershel'
SPIRE

~1 mm

Spitzer'IRAC'
3.6μm

Herschel / SPIRE

Spitzer'
MIPS'
24μm

Observing Wavelength (µm)
Viewgraph prepared by Kohno-san8

Sensitivity: Calculation❖ We consider ❖ 1) Ab-initio noise estimate to account for MKID and opticalefficiencies (Endo+2016, de Visser+2014);❖ 2) Ruze formula to account for primary aperture efficiency;❖ 3) Atmospheric model to account for atmospheric transmission
and photon noise at the Antarctic and Chajnantor (Paine+2012);❖ 4) Optimally filtered image with an appropriate beam size at anarbitrary observing frequency to mimic the actual map-making
procedure which maximizes the point source sensitivity.

❖ The estimates are consistent with those prepared by Nakaisan/Kuno-san and actually observed with ASTE/AzTEC.

9Sensitivity: Assumptions❖ Tsukuba 10-m Telescope❖❖❖❖

Surface error = 10, 20, 30 micron
N_pix = 6000 pixels (350 um)
R = 12 (ΔB = 80 GHz @1 THz)
Antarctic: PWV = 140 um, T_atm = 200 K❖ Other telescopes (for reference)
❖❖
❖
❖
❖

ASTE/AzTEC: D=10m, surface=20 um, Npix=100 pix
CCAT: D=25m, surface=15um, Npix=0.1 Mpix
LST: D=50m, surface=45um, Npix=1 Mpix
R = 12 (ΔB = 80 GHz @1 THz)
Chajnantor: PWV = 600 um, T_atm = 273 K❖ Fiducial model survey❖ Area = 1 sq-deg❖ t_on-source = 1000 hr
10

Sensitivity: 1 sq-deg survey

log σ (Jy/beam)

850um

450um 350um

250um

Tsukuba (30um)
Tsukuba (20um)
Tsukuba (10um)
ASTE/AzTEC

σconf(Herschel)
σconf (10m)Tsukuba 10m

Frequency (THz)11Sensitivity: 1 sq-deg survey

log σ (Jy/beam)

850um

450um 350um

Tsukuba (30um)
Tsukuba (20um)
Tsukuba (10um)
ASTE/AzTEC
CCAT/0.1Mpix
LST/1Mpix

250um

σconf(Herschel)
σconf (10m)σconf (50m)

Tsukuba 10m

Frequency (THz)12Sensitivity: Limiting IR luminosity“Tsukuba” source
Herschel source

Deeper-than-ALMA sources

350-um dropouts

13

Brief comment on science cases❖ 1. Connecting “single-dish selected” and “ALMAdetected” populations at z ~ 1–4❖ (i) Cross-calibration of Herschel results❖ Confusion is always bad for extragalactic studies.
❖ Resolving Herschel sources at deeper limit will drasticallychange of the statistical aspect of Herschel results (just like
ALMA has changed the picture we obtained with SCUBA/AzTEC).

❖ Number counts, cosmic SFR density, counterpart
identifications, etc.

❖ (ii) Statistical studies of “sub-mJy” sources❖ ALMA FoV is too small.
❖ Multi-λ understanding of more “normal” galaxies that are
responsible for cosmic SF.

❖ 2. Extracting THz-dropouts to explore the z > 5
population of SMGs

14

Summary (continuum imaging survey)❖ Science goals❖ extend the Herschel results out to z ~ 5 (cf. Herschel z < 3)
and cover the era of the cosmic high-noon.

❖ high-z (z > 5) sources will be extracted by combining ~1mmresults, which is more efficient than Herschel/SPIRE bands.

❖ Sensitivity❖ will reach confusion limit (σconf(350um) ~ 1 mJy) in reasonableamount of time (~1000 hr).

❖ It is essential to have (1) kilo-pix array cameras and (2)transparent sky in THz bands.

❖ Requirements / Recommendations❖ Multi-color photometry❖ Surface error < 20 um to surpass Herschel and CCAT(Atacama, 5000m) at 1.3 THz❖ Low EL angles to access the equator δ ~ 0° (or at least
GOODS-South at δ = –35°)❖ Tight coordination with SPICA (e.g. SEP/ADF-South)
15

SSP-HSC survey regions

from SSP proposal

Three-layer survey (wedding-cake-style)
Wide: Fall (~640 deg2), Spring (~680 deg2), North (~55 deg2)~1400 deg2 in total
Deep: ~7 deg2 (4 FoVs) x 4 regions = ~28 deg2 in totalaround COSMOS, SXDS, ELAIS-N1, & DEEP2-3
Ultradeep: ~1.75 deg2 (1 FoV) x 2 regions = ~3.5 deg2 in totalaround COSMOS & SXDS

Viewgraph prepared by Nagao-san

16Antarctic vs. Atacama

Tsukuba (10um, EL=30°; PWV=140um, Tgr=200K)Tsukuba (10um, EL=90°; PWV=140um, Tgr=200K)
Atacama (10um, EL=70°; PWV=600um, Tgr=273K)*Telescope/camera spec and survey design are the same.

17

Mid-z SF galaxies
seen in FIR fine structure (FS) lines

18

# of detections FS lines is growing...
References[CII]157 detections- Maiolino+2005 (SDSS1148)- Iono+2006 (BR1202)- Maiolino+2009 (BRI0952)- Walter+2009 (SDSS1148)- Hailey_Dunsheath+2010 (MIPS1428)- Ivison+2010 (Eyelash*)- Stacey+2010 (z~1)- Wagg+2010 (BRI1335)- Cox+2011 (SDP141)- De Breuck+2011 (LESS0332)- Valtchanov+2011 (SDP81*)- Carilli+2012 (BR1202)- Gallerani+2012 (BRI0952)- Maiolino+2012 (SDSS1148)- Salome+2012 (BR1202)- Swinbank+2012 (ALESS SMGs)- Venemans+2012 (ULAS1120)- Wagg+2012 (BR1202, LAEs)- Carniani+2013 (BR1202)- Rawle+2013 (HLS0918)- Riechers+2013 (FLS3)- Wang+2013 (z~6 QSOs, deficit, Mdyn, LF)- Willott+2013 (J2329)- De Breuck+2014 (LESS0332)- Decarli+2014 (BR1202)- Ferkinhoff+2014 (SDP11)- Riechers+2014 (Az3, LBG)
- Williams+2014 (BR1202, LAEs)[NII]205 detections- Bradford+2011 (APM08279)- Combes+2012 (HLS0918)- Decarli+2012 (APM08279, MM18423)- Nagao+2012 (LESS0332)- Decarli+2014 (BR1202)[NII]122 detections- Ferkinhoff+2011 (SMM02399, Cloverleaf)[OIII]88 detections- Ferkinhoff+2010 (APM08279)- Valtchanov+2011 (SDP81*)[OIII]52 detections- Sturm+2010 (MIPS1428*)[OI]63 detections- Sturm+2010 (MIPS1428*)- Ferkinhoff+2014 (SDP11*)---@ Simple interpretation[CII]/FIR deficit[CII] as SF tracer- de Looze+2011*[CII] morphology and dynamics[CII]/CO PDR analysis[CII] luminosity function- Swinbank+2012- Wang+2011@ Photoionization / PDR analysis[NII]/[CII] metallicity, PDR-HII- Nagao+2012- Decarli+2014[OIII]/[NII] UV hardness- Ferkinhoff+2010- Ferkinhoff+2011*) Herschel results

3

Viewgraph from ALMA WS 系外微細構造線勉強会 2014（田村）19

Photodissociation region++
O(35.1 eV)+C (11.3 eV)O0(13.6 eV)
Tielens & Hollenbach 2005, Phys. Rev.
9

Viewgraph from ALMA WS 系外微細構造線勉強会 2014（田村）2013.6 eVPDRHIIAGN

CoronaSpinoglio+2012

20Viewgraph from ALMA WS 系外微細構造線勉強会 2014（田村）21

SMG stacks

山口, 田村ほか (2015) 日本天文学会秋季年会

22Cormier+2015

Herschel Dwarf Galaxy Survey
Dwarfs1% of L_TIR❖

Local dwarfs (i.e. low metallicity SF galaxies)
as low-z analogs of typical SF galaxies at highredshift.

❖[OIII]88 is the brightest❖
Normal SF galaxies(Brauer+08)❖

L_[OIII]88 / L_[CII]158 > 1 (up to ~10).

High ionization state and/or “truncated” PDRs
(matter-bounded Stromgren sphere)?

U/LIRGs(Farrah+13; Gracia-Carpio+11)[OIII] is moreimportant
1% of L_TIR

Normal SF galaxies[CII] is more important(Brauer+08)

23

Stars

N_H

N_WNM
1cm-3, 5000K

N_CNM
50cm-3, 250K

[CII]158[OI]63

LyA

Ionized gas([NII]122)[CII]
Vallini+2013

z = 7.1 LAE with
ALMA/[CII](Maiolino+2015)

24

[OIII]88/[CII]158 Survey❖ Window to “primordial” galaxies in the early universe❖ will help us answer the fundamental (and longstanding)question: Did z > 6 SF galaxies (e.g. LAEs) generate FUV
photons enough to fully re-ionize the Universe?

❖ THz telescopes are not very good at doing z > 6, but

lower-redshift calibration should be extremely importantfor opening low-metallicity universe at mid-z (e.g.
primordial pocket) and “calibrating z > 6 results” as well.

❖ However, [OIII] observations are very limited to only
two... (Ferkinhoff+2010)25

Sensitivity
850um

450um

350um

250um

5"

[CII]158"[OIII]88"

4"[CII]158"[OIII]88"[OI63]"[OI63]"

1200"

1400"

Redshift

3"

2"

1"

0"
200"

400"

600"

800"

1000"

Frequency (GHz)26

Sensitivity: Low-Z galaxies
R = 1000; t(on-source) = 20 hr
z = 0.1[CII]158z = 0.5z=1z=2z=3z=5[OIII]88[OI]63
LTIR = 5 x 10^12 LSun(application: e.g. lensed LBGs)

27

Sensitivity: Z_Sun galaxies
R = 1000; t(on-source) = 20 hrz = 0.3z = 0.5z=1z=2[CII]158[OIII]88

z=3z=5[OI]63

LTIR = 5 x 10^13 LSun(application: e.g. SPT sources)28

Summary (FS lines)❖ Science goals❖ Observations of mid-z SF galaxies in FS lines of [OIII]88 and[CII]158 will❖ Sensitivities❖ The 10m will detect both [OIII]88 and [CII]158 in❖ (1) lensed SMGs with ~Z_Sun (Lir ~ 5e13 L_Sun)❖ (2) lensed UV-selected galaxies with sub-Z_Sun (Lir ~ 5e12L_Sun) at 1 < z < 4.

❖ Requirements / Recommendation❖ Surface error < 20 um to surpass Herschel and CCAT
(Atacama, 5000m) at 1.5 THz❖ Transparent sky at > 1 THz❖ You can start even with ASTE/DESHIMA, which offers a good
opportunity to prepare good science cases with Tsukuba 10mTHz telescope.

❖ Tight coordination with SPICA29