1. The 3 rd workshop on Large Mm/Submm Telescopes in the ALMA Era March 10, 09:00 – 18:10 March 11, 09:00 – 17:40 COSMOS Lodge Conference Room

2. Background of the workshop ALMA, the most powerful mm/submm facility with high angular resolution imaging capability coupled with unprecedentedly high sensitivity, has been producing a growing number of impressive and compelling results. It is also evident that many outstanding ALMA results often rely on wide area surveys using existing ground- based and space telescopes such as Nobeyama, Nanten, IRAM, JCMT, CSO, Mopra, SPT, ASTE, APEX, Herschel, and so on, emphasizing the importance of next generation large mm/submm survey telescopes, which will have large FoV (> 0.5 deg) and large instantaneous frequency coverage with large format bolometer/heterodyne arrays, to exploit ALMA capabilities. Observing freq.[GHz] Flux density [mJy] z=5.656 J=5-4 J=6-5 Weiss et al. 2013, ApJ, 767, 88 e.g., Vieira et al. 2013, Nature, 495, 344

3. Background of the workshop It is also evident that many outstanding ALMA results often rely on wide area surveys using existing ground-based and space telescopes such as Nobeyama, Nanten, IRAM, JCMT, CSO, Mopra, SPT, ASTE, APEX, Herschel, and so on  emphasizing the importance of next generation large mm/submm survey telescopes, which will have large FoV (> 0.5 deg) and large instantaneous frequency coverage with large format bolometer/heterodyne arrays, to exploit ALMA capabilities.

4. Goals of the workshop (1) to explore the astrophysical potential of such next generation large single dish telescopes at mm/submm wavelengths, (2) to share current status and running and planned mm/submm telescopes such as NRO 45m, LMT, GLT, CCAT, SST, and LST, (3) to discuss about state-of-the-art technologies of detectors/receivers/telescopes, which shall be essential for the next generation mm/submm telescopes, and (4) to discuss about the synergies with related survey missions at other wavelengths such as Subaru, TAO, SPICA, WISH, and SKA.

5. So many large single dish projects ! Showing the richness of science cases, and..? How can we widen and sharpen the science cases ? How can we make our projects more competitive ?

6. Exploring new parameter space Example 1Example 2Example 3Example 4 Area1 deg 2 10 deg 2 600 deg 2 100 deg 2 Cadence 4 epochs per month 2 epochs per month (×3 months) 25 epochs per month (Single epoch) Integration time per epoch 70 hours (~7 nights) 35 hours/deg 2 × 10 deg 2 ~ 15 full- days 1 min/deg 2 × 600 deg 2 = 10 hours ~ 1 night 22 hours/deg 2 (2 nights/deg 2 ) × 100 deg 2 ~ 200 nights Sensitivity (5σ) per epoch 0.2 mJy @1.1mm 0.1 mJy @2mm13 mJy @1.1mm 0.36 mJy @1.1mm Total observing time 70 hours × 4 epochs = 280 hours 350 hours × 6 epochs = 2100 hours 10 hours × 25 epochs = 250 hours 2200 hours comments For wondering BH survey ?? For Orphan GRB afterglow survey ??? After 25 epochs, sensitivity reaches 2.6 mJy (5σ)  2.4×10 5 sources For confusion- limited deep and wide surveys  1.9×10 6 sources - some survey plans using LST -

7. LOC announcement Lunch: cafeteria of COSMOS-Lodge Banquet: same place, just after the session – Please pay in advance if you want to join Wifi is available (but not to concentrate on your e-mails!) Discuss, and enjoy!