The roles of the new 30 – 50 m class single dish telescope: (1) deep & wide continuum imaging Deep and wide surveys at short-millimeter to long- submillimeter wavelengths –Target frequency range: 70 – 420 GHz (4.3 – 0.71 mm) Option (under illumination): up to ~1.2 THz (250μm) ??? –Wide field of view: 0.5 deg diameter (circular) >> ALMA –Equipped with large format arrays to fill FoV a few 1,000 – a few 100,000 pixels per band x 4 ~ 6 bands?  “mm-submm version Suprime-Cam” –Greater survey efficiency than ALMA !!!

Survey efficiency: New 30-50m vs ALMA 1.1mm (270 GHz) 1.2 million pointings (!!) will be needed for ALMA/Band 6 to fully cover a 10-deg 2 region. D=35mD=50m (option) By Yoichi Tamura A deep survey of 10deg 2 area using 500 hours. Bandwidth: 8 GHz for ALMA 50 GHz for 35/50m Num. of pixels 1 for ALMA > 10^4 for 35/50m !

The roles of the new 30 – 50 m class single dish telescope: (2) ultra-wide band & multi-pixel spectroscopy Wide area, spectral surveys at short-millimeter to long-submillimeter wavelengths –Specification on the instantaneous bandwidth and the number of pixels is under discussion. A case study: CO tomography assuming D = 50m, instantaneous coverage = 70 – 346 GHz, dual polarization, 1000 pixels (Y. Tamura et al.) (very challenging, more study!) Large instantaneous bandwidth (>a few 10 GHz; cf. 8 GHz in ALMA) and/or large number of pixels (> a few 10 – 100; cf. single pixel in ALMA) will be crucial.

Target frequency/wavelength coverage Frequency [GHz] Transmission [%] 1.0Wavelength [mm] GHz 3.3mm 150GHz 2.0mm 225GHz 1.3mm 275GHz 1.1mm 350GHz 0.86mm 405GHz 0.74mm PWV=0.5mm -SZ Kinetic SZ only +SZ SMGs

Band definition and beam properties for continuum camera (D=35m) Band center 90 GHz 3.3 mm 150 GHz 2.0 mm 225 GHz 1.3 mm 275 GHz 1.1 mm 350 GHz 0.86 mm 405 GHz 0.74 mm Coverage [GHz] [mm] Beam size [arcsec] Num. of beams(TBD) 5,80016,20036,40054,40088,100118,000 Assumed field of view: circular, diameter = 0.5 deg = 707 arcmin^2 =0.196 deg^2 Beam size: 1.2×λ/D Number of beams: to fill the FoV (beam spacing = beam size) (Option)

Band definition and beam properties for continuum camera (D=50m) Band center 90 GHz 3.3 mm 150 GHz 2.0 mm 225 GHz 1.3 mm 275 GHz 1.1 mm 350 GHz 0.86 mm 405 GHz 0.74 mm Coverage [GHz] [mm] Beam size [arcsec] Num. of beams(TBD) 11,90033,00074,300111,000180,000241,000 Assumed field of view: circular, diameter = 0.5 deg = 707 arcmin^2 =0.196 deg^2 Beam size: 1.2×λ/D Number of beams: to fill the FoV (beam spacing = beam size) (Option)

Confusion limit (5σ) for D=35m Based on: Takeuchi et al. 2001, PASP, 113, 586 WavelengthBeam size [arcsec] Confusion limit [mJy] 0.86 mm mJy 1.3 mm mJy 3.3 mm mJy 0.25 mJy mJy 0.15 mJy 5σ Memo: beam size = 30  confusion limit ~ 0.7 mJy ⇔ ~1.4 mm : consistent with AzTEC/ASTE deep survey experience ×5 deeper than AzTEC/ASTE Large dish is essential to reduce the confusion!

Confusion limit (5σ) for D=50m WavelengthBeam size [arcsec] Confusion limit [mJy] 0.86 mm mJy 1.3 mm mJy 3.3 mm mJy 0.15 mJy mJy 0.09 mJy 5σ Memo: beam size = 30  confusion limit ~ 0.7 mJy ⇔ ~1.4 mm : consistent with AzTEC/ASTE deep survey experience ×8 deeper than AzTEC/ASTE Based on: Takeuchi et al. 2001, PASP, 113, 586 Large dish is essential to reduce the confusion!

AzTEC/ASTE10m ADF-S 3σ AKARI Deep Field South (ADF-S) 3σ Confusion limits (5σ) for 35m 0.86mm 1.3mm 3.3mm HerMES Confusion 5σ 35m telescope Confusion 5σ SED: Bunyo Hatsukade

Confusion limits (5σ) for 50m 0.86mm 1.3mm 3.3mm AKARI Deep Field South (ADF-S) 3σ HerMES Confusion 5σ AzTEC/ASTE10m ADF-S 3σ 50m telescope Confusion 5σ SED: Bunyo Hatsukade

Memo: Confusion limit (5σ) for SPIRE Based on: Takeuchi et al. 2001, PASP, 113, 586 ~13 mJy from a model by Takeuchi et al SPIRE on Herschel Beam = 36.2 arcsec Estimated confusion noise (5σ) = 30.5 Oliver et al. 2012, MNRAS, 424, μm Mostly consistent?