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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.

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Presentation on theme: "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."— Presentation transcript:

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 deg 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 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 s!) Discuss, and enjoy!


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