Status of the Korean ALMA project

Jongsoo Kim

Korea Astronomy and Space Science Institute

ALMA activities be-fore 2014 in Korea

• 2012-03-19– MOU bew. NAOJ and KASI

• 2012-09-13,14– ALMA EA Science Workshop

• 2012, 2013– Reports of Planning Study for the ALMA project

were submitted to the KASI– Last December, a report was finally approved in

the KASI

Preparation of Cycle 2 CfP

• Survey Science Group, KIAS– 2013-10-04, Cycle 2 CfP

• Town Meeting at KASI– 2013-10-28, 64 participants– Cycle 2 Capability, OT, CASA Simulator

• SNU Colloquium– 2013-11-21, Cycle 2 CfP

• ALMA proposals from Korea: 17

Classification of 17 proposals

• Fields– Cosmology and the high redshift Universe: 2– Galaxies and galactic nuclei: 2– Interstellar medium, star formation and astrochemistry:

11 – Circumstellar disks, exoplanets and the Solar System: 1– Stellar evolution and the Sun: 1

• Institutions– KASI: Universities = 12:5

ALMA Korean ProjectARC: Jongsoo Kim, A-Ran Lyo, Ji-Hyun Kang, Kyung-Hee Kim, Chan-dreyee Sengupta

Development: Jungwon Lee, Do-Hung Je, Ji-Man Kang, Seung-Lae Kim

ALMA Korean Project

• budget: 15MUSD/11years +

20MUSD (2020~2023years)• ARC

– Proposals, observing scripts, reductions, sciences

• Development plan– Multi-Beam Receivers (ASTE ALMA TP)– Spectrometer/Correlator (ASTE ALMA TP)

Multi-beam Receiver for ASTE

• Frequency band: 345 GHz or 460 GHz (or wide band to cover both bands)

• Number of beams: 9~64 beams• RF/IF Specifications: follow the ALMA speci-

fication (except polarization)

Software Spectrometer for an ASTE Multi-beam Receiver

• goal specification for a multi-beam receiver (ALMA specification): 4 basebands with 2GHz bandwidth, dual polarisation, 16 beams

• performance requirement: ~ 20 Tflops• input and output data rates: 1.6Tb/s, 200MB/sec

• A software spectrometer based on a 16-node cluster with 64 40GE ports

and 32 GPU cards is proposed.

2-band quasi-optics for ASTE

• Simultaneous observations using two receivers– CATS345, 324-372 GHz– ALMA B8QM, 400-500GHz

• Need modifications of the current spectrometers, – MAC– WHSF