• Publications of The Korean Astronomical Society
• /
• v.30 no.2
• /
• pp.655-657
• /
• 2015

The Australia Telescope National Facility (ATNF) consists of the Parkes and Mopra radio telescopes, and the Australia Telescope Compact Array, with the first elements of the wide-field Australian Square Kilometer Array Pathfinder (ASKAP), currently being commissioned. The capabilities of these facilities are described.

• The Bulletin of The Korean Astronomical Society
• /
• v.37 no.2
• /
• pp.63-63
• /
• 2012

The Square Kilometre Array (SKA) will be the world's largest and most sensitive radio telescope. It will address a wide range of fundamental questions in physics, astrophysics, cosmology and astrobiology. Australia, one of the two countries selected to host the SKA, has spent several years preparing by opening up the Murchison Radio-astronomy Observatory (MRO) as a uniquely radio quiet site in Western Australia, and by constructing the world's most powerful radio survey telescope, the Australian SKA Pathfinder (ASKAP). The SKA will be built in two phases. Phase I will include ASKAP, which will use novel phased-array feeds and grow to become "SKA-survey". Phase I will also include a dish array ("SKA-mid") in South Africa and a low-frequency array ("SKA-low") in Australia, and is slated for operation from about 2020. Phase II of the SKA will consist of further expansion of SKA-low and SKA-mid and is due for completion in the middle of the next decade.

• The Bulletin of The Korean Astronomical Society
• /
• v.11
• /
• pp.11.3-12
• /
• 1986

• Journal of the Korean Institute of Telematics and Electronics B
• /
• v.31B no.9
• /
• pp.67-75
• /
• 1994

In this paper, we manufactured the continuum receiver system for observing the continuum waves emitted from the continuum sources with using the 14m radio-telescope. The receiving system measures the total power of the continuum sources and consists of DC-amplifier, beam-chopper system. Phase-Locked Loop(PLL) circuit, blanking circuit and its period selection circuit, V/F converter, and counter part which are capable of interfacing with the computer which is used for a data acquisition and making the radio-telescope track the source. We compared the obsevation results which use the existing DVM method with the observation results which use the continuum receiver to measure the total power of the sources. Moreover, by method of beam switching observation which uses newly installed beam chopper system. We can significantly improve the observational efficiency more than the existing position switching observation method.

• Journal of Astronomy and Space Sciences
• /
• v.17 no.2
• /
• pp.221-232
• /
• 2000

A Gunn waveguide-oscillator, mechanically tunable from 60 to 70 GHz, has been developed for use as a local oscillator(LO) is millimeter radio telescope. Disc size, post size and characteristics of Gunn diode have an effect on the frequency tuning characteristics of Gunn oscillator. In this paper we report experimental results and design criteria for a wideband tunable Gunn oscillator. The developed Gunn oscillator has been used in the 100/150 GHz band dual channel receiver for the Taeduk Radio Astronomy Observatory.

• Bulletin of the Korean Space Science Society
• /
• 2010.04a
• /
• pp.34.3-34.3
• /
• 2010

We present the results of flux monitoring of BL Lac object 0716+71 and 0954+65 at 22GHz and 43GHz. Both of the flat spectrum radio sources are known as Intraday variables (IDVs) which are characterized by fast flux variation on time scales of a day or less. In general, the IDV phenomenon is interpreted as the effect of refractive scintillation in the interstellar medium or the evidence of source intrinsic flux variation. The observations were made simultaneously at 22GHz and 43GHz with KVN Yonsei 21m radio telescope.

• The Bulletin of The Korean Astronomical Society
• /
• v.31 no.1
• /
• pp.38.2-38.2
• /
• 2006

• The Bulletin of The Korean Astronomical Society
• /
• v.27 no.1
• /
• pp.61-61
• /
• 2002

• The Bulletin of The Korean Astronomical Society
• /
• v.14
• /
• pp.8.1-8.1
• /
• 1989

• Journal of Astronomy and Space Sciences
• /
• v.23 no.1
• /
• pp.19-28
• /
• 2006

The noise temperature of existing millimeter-wave receivers is already within two or three times quantum noise limit. One of practical ways to increase the observation speed of single dish radio telescope without longer integration time is use of multi-beam focal plane array receiver as demonstrated in several large single dish radio telescopes. In this context the TRAO (Taeduk Radio Astronomy Observatory), which operates a 143n Cassegrain radio telescope, is planning to develop a 4 x 4 beams focal plane array SIS receiver system for 86-115 GHz band. Even though millimeter-wave HEMT LNA-based receivers approach the noise temperature comparable to the SIS receiver at W-band, it is believed that the receiver based on SIS mixer seems to offer a bit more advantages. The critical part of the multi-beam array receiver will be sideband separating SIS mixers. Employing such a type of SIS mixer makes it possible to simplify the quasi-optics of receiver. Otherwise, an SSB filter should be used in front of the mixer or some sophisticated post-processing of observation data is needed. In this paper we will present a preliminary design concept and components needed for the development of a new 3 mm band multi-beam focal plane array receiver.