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THE SUBMILLIMETER ARRAY: CURRENT STATUS AND FUTURE PLAN
OHASHI NAGAYOSHI The Korean Astronomical Society 2005 Journal of The Korean Astronomical Society Vol.38 No.2
The Submillimeter Array (SMA), a collaborative project of the Smithsonian Astrophysical Observatory (SAO) and the Academia Sinica Institute of Astronomy & Astrophysics (ASIAA), has begun operation on Mauna Kea in Hawaii. A total of eight 6-m radio telescopes comprise the array with currently working receiver bands at 230, 345, and 690 GHz. The array will have 8 receiver bands covering the frequency range of 180-900 GHz. The backend is flexible analog-digital correlator with a full bandwidth of 2GHz, which is very powerful to cover several line emissions simultaneously. The current status and future plans of the SMA are described with emphasis on Taiwanese efforts.
MILLIMETER OBSERVATIONS OF THE TRANSITION DISK AROUND HD 135344B (SAO 206462)
Lyo, A-Ran,Ohashi, Nagayoshi,Qi, Chunhua,Wilner, David J.,Su, Yu-Nung American Institute of Physics 2011 The Astronomical journal Vol.142 No.5
<P>We present ~1'' resolution 1.3 mm dust continuum and spectral line (<SUP>12</SUP>CO and <SUP>13</SUP>CO J = 2-1) observations of the transitional disk system HD 135344B obtained with the Submillimeter Array. The disk shows a Keplerian rotation pattern with an inclination of ~11°, based on the spatially and spectrally resolved <SUP>12</SUP>CO and <SUP>13</SUP>CO emission. The data show clear evidence for both dust and gas surface density reductions in the inner region of the disk (radius <img entity='lsim' SRC='http://ej.iop.org/icons/Entities/lsim.gif' ALT='lsim' ALIGN='BASELINE' /> 50 AU) from the continuum and <SUP>13</SUP>CO J = 2-1 data, respectively. The presence of this inner cavity in both the dust and gas is more consistent with clearing by giant planet formation than by photoevaporation or by grain growth. There is also an indication of global CO gas depletion in the disk, as the mass estimated from <SUP>13</SUP>CO emission (~3.8 × 10<SUP>–4</SUP> M<SUB>☉</SUB>) is about two orders of magnitude lower than that derived from the 1.3 mm continuum (~2.8 × 10<SUP>–2</SUP> M<SUB>☉</SUB>).</P>