マスタタイトルの書式設定. Beyond ALMA. ALMA: 何がわかったか 何が足りないか LST: 何をやりたいか どのような計画か ALMA へのボーナス効果 最後に :small developments が未来を切り開く. Ryohei Kawabe (NAOJ)

マスタタイトルの書式設定 Beyond ALMA ALMA: 何がわかったか 何が足りないか LST: 何をやりたいか どのような計画か ALMA へのボーナス効果 最後に :small developments が未来を切り開く Ryohei Kawabe (NAOJ)

I: Advent of ALMA 何がわかったか 何が足りないか

ALMA opens new era ALMA will contribute to elucidating galaxy formation and planet formation with exploiting extreme performance - High Angular Resolution, ~ 0.01 arcsec; sharp radio images - High Sensitivity to reach the early universe (also thanks to very unique characteristic of submillimeter emission in SMG) Hubble Deep Field and SCUBA map Gaps in Protoplanetary Disks Hughes et al. 3 1998

Cycle-0 unveiling exciting views of the universe, but still in starting point of climbing to the top. Imagine how splendid the view is at the top! Y+ Config (max. BL) Band 10 ACA ALMA Goal: 0.01 resolution.. Band-5, 1 Bands 4 & 8 Polarization ALMA cycle-0 4

ALMA Science Goals ALMA will contribute to elucidating galaxy formation and planet formation with exploiting extreme performance Dreams - High Angular come true! Resolution, ~ 0.01 arcsec; sharp radio images - High Sensitivity to reach the early universe (also thanks to very unique characteristic of submillimeter emission in SMG) Hubble Deep Field and SCUBA map Gaps in Protoplanetary Disks 5

[OIII] detection at z=7.21! Inoue, Tamura+2016

Line-Emitter/redshift Search :ALMA is not so powerful? ASPECS: ALMA SPECtroscopiC Survey in HDF (PI:F. Walter) To unveil cosmic gas density evolution etc. preliminary results with ~ 20 hours - B-3: 10 emitter cand. - B-6: 11 candidates => one/ hour Walter+2016

Dust gaps unveiled in disks :gas/pol imagings are still challenging? Dust Gaps in Class-II source TW-Hya (d=54 pc) Dust filtration due to a formed planet? - dust-β and pol. imaging constraints on grain size - gas gap image needed for planet mass estimate 37 au gap 22 au gap B4+B6 Continuum Image Tsukagosi, Nomura, Muto + 16 Cyc-4 observations - 0.14 polarimetry ~ 6 hours PI: Muto Kataoka+ 15, 17-0.1 (~5.4 au) & 0.2 km/s 13 CO & C 18 O imaging (requested ~8 hours) Central hole PI: Nomura Kanagawa+ 15 x 2-3 resolution needs x ~10 more in time

Needs More for ALMA? Sensitivity, especially in spectral line & Polarimetry Spatial Resolution, especially in continuum Spectral/Frequency Coverage for e.g., spec-z Field of View Time-domain Science? How can be improved in the future plans?

Synergy among ALMA, ngvla, and SKA Cosmic Star Formation, Co-Evolution of Galaxies and SMBH, Large Scale Structure ALMA: Challenges to z~10 EoR with [CII], [OIII], dust etc. ngvla: Challenges to z>5 with CO ladders SKA: Challenges to large scale structure at z> 10 and star formation beyond z>5 Special Note: multi-wavelength astronomy!

ngvla is only array to detect CO at z=5?

ngvla is only array to detect CO at z=5? NGC6240/Mrk231 CO(8-7) CO(7-6) CI ALMA B4+B5 ALMA still powerful!

Inevitable Barriers for Large Arrays Brightness Temperature Barrier Spatial Resolution Barrier Freq. coverage Barrier ALMA can go deeper and finer in the cool (thermal) universe Not easy for ALMA to overcome wide-field & wide freq coverage, time-domain problems

10000000 Brightness Temperature Sensitivity (R-J) : 1000000 continuum case (0.01 beam/fixed hours assumed) 10000 1000 100 10 1 SKA 100000 10000 1000 100 10 ngvla ALMA b6 b7 Beam Size : 1 K sensitivity assumed ALMA B6/7 1 1 is at the best 0.1 1 10 100 1000 0.1 100 mas 0.01 10 mas 0.1 1 10 100 1000 Freq. (GHz) 0.001

M82 (10 Msun/yr) x 5 at z= 10 (EoR) ngvla=5-10 x JVLA 20 hours ALMA 20 hours 5σ ~ 34 ujy Line 5σ Continuum 5σ 1 µjy 10 cm 1 cm λ obs 1mm

Needs More for ALMA? Sensitivity, especially in spectral line & Polarimetry Spatial Resolution, especially in continuum Spectral/Frequency Coverage for e.g., spec-z Field of View Time-domain Science? How can be improved in the future plans? Band-1 and -3 sensitivity can be improved by ngvla

Needs More for ALMA? Sensitivity, especially in spectral line & Polarimetry Spatial Resolution, especially in continuum Spectral/Frequency Coverage for e.g., spec-z Field of View Time-domain Science? How can be improved in the future plans? Band-1 and -3 sensitivity can be improved by ngvla LST can develop new discovery space complementary to ALMA

II: LST 何をやりたいか, どのような計画か, ALMA へのボーナス効果

New Challenges in 2030- Unveiling EoR & formation of first star, Galaxies, SMBH through the cosmic time Time-domain Science - GRB, Magneters, Pulsars - FRB, GW-counter parts - Flares from stars, Extreme Physics in the Universe - Resolving BH shadow - CMB B-mode

New Challenges in 2030- Unveiling EoR & formation of first star, Galaxies, SMBH through the cosmic time Time-domain Science - GRB, Magneters, Pulsars - FRB, GW-counter parts - Flares from stars, Planet Formation & Life in Space Extreme Physics in the Universe - Resolving BH shadow - CMB B-mode LST

Basic Concept :Tentative Specifications Large Aperture: Diameter = ~ 50 m less confusion, confident counterpart ID, high sensitivity for line emitter search and point-like sources & transients such as GRB: Large FOV : F.O.V = 30 arcmin. diameter, Goal = 1.0 deg cosmological deep and wide-field survey & high cadence Main Frequency Range = 70 420 GHz well fit to Atm windows & Major Science Case covers up to ~ THz with the limited use of surface to maximize synergy with ALMA total surface rms 45 μm (El = 30-80 deg) with Active surface Control Possible site; ALMA site

Key Science of LST Exploration of Cosmic Star Formation History and Large Scale Structures via two kinds of surveys - Multi-band Deep Continuum Survey over ~10 3 deg 2 - Blind CO/CII line emitter search (Tomography) up to z~ 8, EoR, using imaging spectrograph (Blind vs multi-target spectroscopy still needs to be investigated, but blind can provide us with census of non-biased line emitters, in which strong-line but continuum-weak emitters will be included) Time-domain science via high cadence performance Covers wide range: SZ cosmology, VLBI, chemistry RK+ in SPIE proceedings; White paper by Kohno, RK in prep

CO/[CII] Tomography Evolution of Galaxies EoR Epoch of Reionization.,, / / /. /, /., RSD Redshift Space Distortion. / /., / LSS Cosmic Large-Scale Structure /,,. /, CSFH Cosmic Star-formation History /.. /..,.,,.... and serendipitous discoveries, Yoichi Tamura / Large Aperture Sub/mm Single Dish Telescopes in the ALMA Era

CO/CII vs HI Tomography 10000 hrs SKA 1 surveys (SKA 1: 10% of full SKA) 1000 hrs LST+ super-deshima (300 pix) survey Deep 2 deg 2 70-400 4-15 ~ 100,000? (7~9) Y.Tamura+ in prep. GHz >1,000 (z>6)

SKA HI Blue: Medium wide Green: Med. deep Red: Deep LST CO/[CII] EoR

Why LST/sDESHIMA so powerful? s-deshima 370 GHz [CII] 70 GHz

Time-Domain Science Case GRB Orphan Afterglow (Totani+2002) GRB Reverse Shock at extremly high-z (Inoue+2007) - Absorption detection in GRB environments & intervening gas? LST can contribute to quick location determination & WB spectroscopy at same time Inoue+2007 LST z=20 GRB

Simulation of GRB afterglow z = 30 GRB afterglow (1-12hr, 300GHz) 5 arcmin Movie is available on the LST web site LST 50m 1.0 Flux density (mjy/b) 0.0 0.1 ALMA (mosaic) ALMA FoV (Band 7) CCAT 25m ASTE 10m Swift/BAT error circle Yoichi Tamura / Large Aperture Sub/mm Single Dish Telescopes in the ALMA Era

LST covers wide range of Science Develop new discovery space complementary to ALMA Wide-Field Spectroscopic Imaging Time-domain Science

LST Sky Coverage El > 25 deg LST ~ 4 arcsec. ~ 60 µk RJ Planck 3.5 arcmin.

LST Sky Coverage shared with SUBARU, TMT, JVLA/ngVLA LST ~ 4 arcsec Planck 3.5 arcmin. ~ 60 µk RJ

LST Galactic Plane Survey Wide Survey 1.1 mm with 1 deg FOV, 2 mjy/b 30 shallower than confusion limit 10^4 deg^2 870 hours Deep 1.1 mm with 1 deg FOV, 0.7 mjy/b x10 shallower than confusion limit 10^3 deg^2 870 hours Contamination expected - 10^6 bight SMGs - > 1000 lensed SMGs

Technical Feasibility Study Science Requirement & Technical Specification Operation condition & Operation Planning Optics Design Conceptual Design of Telescope Structure Surface Accuracy Budget Analysis (Very Preliminary) Cost Estimate AO application or Millimeter-wave AO (MAO) under discussion

Optical Design for wide FOV very preliminary Richey-Chretien Optics for D= 50 m main reflector Lyot-Stop at Sub-refrector: D effective ~ 46.7 m FOV ~ 0.7 deg. in diameter at 850 micron achievable But - large mirrors D sub-ref ~ 6.2 m #3 mirror ~ 7 m diameter - huge RX cabin needed (big impact on telescope mechanical structure?) - No aperture plane @main reflector Takekoshi, Oshima + in prep.

Conceptual Design Double Sector Gears Receiver Cabin Tertiary & Forth Mirrors Collimator Tower The First Drawing of LST Conceptual Design; Major req. accommodated. Elevator Image Courtesy of Mitsubishi Electric Company

Conceptual Design Top View #3, & #4 mirrors limit the minimal size of receiver cabin.. Back View Image Courtesy of Mitsubishi Electric Company

Active Surface Control Required 45 µm rms needs careful mech/thermal design as well ~ 2m x 1m 2 m

Tentative Surface Error Budget for LST & comparison with IRAM 30m Telescope Error budgets for Gravity and Thermal Deformation can be smaller Wind-Load is current headache, some correction etc. needed RK+ in SPIE proceedings; White paper by RK, Kohno, in prep

Key Instruments Ultra-Wideband Medium-Resolution Imaging Spectrometer Array: Blind CO/[CII] Tomography Freq= 70-420 GHz & N pix of > 300 (~ 1000) Multi-Chroic Wide-Field Camera covering 2, 1.1, 0.85 mm, (+0.45, 0.35 mm) Multiple-band Heterodyne Array Receivers (~ 100 beams) + Ultra-wideband Spectrometers (for line survey) => Super DESHIMA <= or Super MOSAIC Mm/submm multi-object spectrograph MOSAIC Delft SRON High-Z Mapper

Combined Array: ALMA+LST 1 ~ 40% increase in correcting area 2 ~ keeping F.O.V. area with multiple beam or x2 increase only for 12m-LST correlat. 1+2 => > x2 increase in observing speed - F.O.V. 12m-LST ~ sqrt(p 12m )*sqrt(p LST )

International Collaboration? Discussion via workshops - LSTWS2015: Large millimeter/submillimeter telescope in the ALMA era - Status of Other Telescopes updated e.g., Caltech ~ 30m survey telescope Recent Progress - European perspective: ~ 40m class similar to LST : A good-sign toward a future 40-50 m class submm single disk telescope in Chile as a single international project, although it will be hard to project and secure construction budget

III: 最後に Small is beautiful! Small developmentsの積み上げが将来を切り開く (+ALMAを使い倒す)

Examples of Small developments New Detector Technologies - TES Camera/Multiple- chroic TES - DESHIMA/DESHIMA 49 - Tsukuba-cam, Super-resolution Imaging by Sparse Model. - Application to ALMA Data Millimeter-wave Adaptive Optics (MAO)

Super-resolution Imaging Conventional Imaging: CLEAN, λ/d limit Super-resolution by Sparse Modeling Applications to ALMA underway - continuum imaging - pol. Imaging - Spectral line imaging - selfcal, mfs etc Honma+2014 Akiyama+2017 See Poster by M. Yamaguchi

Original data: 0.51 x 0.43 Sparse Modeling: ALMA HD142527 Image by Sparse Modeling x 2-3 higher resolution Super-res w. small CB Comparison Consistent! High-res. data: 0.18 x 013

Millimeter-wave Adaptive Optics PI: Y. Tamura

まとめ ALMA は本当に powerful ALMA は将来を映す鏡 : ALMA で観測を進めると 将来何が必要かがだんだん見えて来る LST は ALMA を補佐しつつ新たな地平を目指す ( 中型 ) 計画 サイエンス 装置技術の検討を進めて行きたい Small projects (+ アイデアを試すことも ) are essential for our future.