The 3rd workshop on Large Mm/Submm Telescopes in the ALMA Era

March 10, 09:00 – 18:10March 11, 09:00 – 17:40

COSMOS LodgeConference Room

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]

Flu

x de

nsit

y [m

Jy]

z=5.656

J=5-4J=6-5

Weiss et al. 2013, ApJ, 767, 88e.g., Vieira et al. 2013, Nature, 495, 344

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.

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.

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 ?

Exploring new parameter spaceExample 1 Example 2 Example 3 Example 4

Area 1 deg2 10 deg2 600 deg2 100 deg2

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/deg2 × 10 deg2 ~ 15 full-days

1 min/deg2 × 600 deg2 = 10 hours ~ 1 night

22 hours/deg2 (2 nights/deg2) × 100 deg2 ~ 200 nights

Sensitivity (5σ) per epoch

0.2 mJy @1.1mm

0.1 mJy @2mm 13 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) 2.4×105 sources

For confusion-limited deep and wide surveys 1.9×106 sources

- some survey plans using LST -

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!