ALMA Cycle 2 Capability Jongsoo Kim ALMA EA Korea node

Locations of ALMA and GMT ALMA GMT

Antennas 50x12m-Array + 12x7m- Array m-TP Array Longest baseline: 16 km Current: 66 delivered Completed in 2013(?)

Resolution and Sensitivity Comparison

ALMA Atacama Large Millimeter/Submillimeter Array

C2: Antennas 34 12m-Array ACA Array: complement to 12m-Array –9 7m-Array Shorter baselines No WVR (Water Vapor Radiometer) –2 12-m TP Array Single dish observations Spectral line (no continuum) observations in Band 3-8 (no 9)

Atmospheric Transparency

C2: Receivers B2,4,6,7: 1.5km, B8,9: 1km B2,4,6,7,8,9: dual pol, XX,YY

7-m, 12-m Array Configurations 7 configurations  Most compact confi. with max baseline 160m  Most extended conf. with max baselines, 1.5km for B3,4,6,7, 1.0km for B8,9

12-m Array configurations

7-m Array Configuration, TP Low elevation m TP

Time Estimates for mult-conf. Rule of thumb –estimate dt_ex, for 12-m extended configuration (C34-4,5,6,7) –4*dt_ex for TP –2*dt_ex for 7-m Array –0.5*dt_ex for 12-m compact configuration (C34- 1,2,3) Use OT Total time (12-m+ACA) < 100 hours

Spectral Capability Number of BBs in 2SB in each sideband: 0, 1, 2, 4 Number of BBs in DSB (B9): no restriction Spw in each BB: up to 4, share correlator resource among them Should have same correlator mode with a BB Binning of data of power 2 mainly due to limitation of data rate, maximum 60MB/s, average 6MB/s

Correlator mode

Polarization Single Polarization, XX: more bandwidth or more spectral resolution Dual Polarization XX, YY: improve sensitivity of sqrt(2) compared with single pol case Full polarization XX, XY, YX, YY: –continuum obs in Band 3,6,7 –LAS < 1/3 12-m primary beam, single field –Fixed frequencies

Source restrictions “SG(Science Goal): single angular resolution, sensitivity, LAS, receiver band No restriction on number of SG per proposal Total # of positions with 10 deg < 150 per SG per array One mosaic observing mode < 150 positions per SG

Calibration Absolute Amplitude calibration –Better than 5% in B 3,4 –Better than 10% in B 6,7 –Better than 20% in B 8,9 due to high opacity and DSB of B9

ToO Only 12-m array < 2 weeks monitoring projects are unlikely fully observed within 2 weeks contact can not be guaranteed

ALMA Partnership The Atacama Large Millimeter/submillimeter Array (ALMA), an international astronomy facility, is a partnership of Europe, North America and East Asia in cooperation with the Republic of Chile. ALMA is funded in Europe by the European Organization for Astronomical Research in the Southern Hemisphere (ESO), in North America by the U.S. National Science Foundation (NSF) in cooperation with the National Research Council of Canada (NRC) and the National Science Council of Taiwan (NSC) and in East Asia by the National Institutes of Natural Sciences (NINS) of Japan in cooperation with the Academia Sinica (AS) in Taiwan.

Maercker (Oct-11), Nature Cyclo 0 December 2011, data delivered CO(J=3- 2) 345GHz 1.3’’x10’’ beam 50’’x50’’ map, 45-point mosaic CASA Large Mass Loss from R Sculptoris, an AGB Star

ALMA survey of SMGs in ECDFS (Extended Chandra Deep Field South) Hodge+ 2013, ApJ, Cycle 0 ALMA band 7 (344GHz, 870  m) Primary beam: 17.3 arcsec Angular resolution: 1.5 arcsec (125m) Observed 126 subm sources detected in LESS (LABOCA ECDFS Submillimeter Survey) by 12m APEX 2 minutes integration time for each source 3x sensitivity 200x resolution  Resolve previously blended sources  Main 99 SMGs+ supplementary 32 SMGs