For efficient spectroscopic redshift identification of early galaxies in the northern hemisphere, we aim to combine the Large Millimeter Telescope (LMT) with a wide-band heterodyne receiver, FINER, which will cover radio frequencies of 120–360 GHz and offer a 3–21 GHz intermediate frequency (IF) per sideband and polarization. To take full advantage of such wide IFs, we present a novel 10.24-GHz-wide digital spectrometer, DRS4 (Elecs Industry Co., Ltd.). It incorporates 20.48 Gsps samplers with an FPGA-based digital signal processing module. To mitigate the noise contamination from the image sideband, it is equipped with a digital sideband separation function to improve the sideband rejection up to 25 dB. Laboratory performance evaluations show that it exhibits an Allan time of at least ~ 100 s and a total power dynamic range of at least 7 dB. These results demonstrate its capability of instantaneously wide-band spectroscopy toward high-redshift galaxies with position-switching observations.
We present an archive system named "Adria", which have been developed and maintained by ALMA project team of National Astronomical Observatory of Japan (NAOJ). Adria aims to store and open to the public various science data. Adria is composed of an object storage to store the observation data, the access control by "ticket", JSON format metadata, JavaScript APIs and html documents. The combination has the advantages of flexibility and solidity, which are important to store various telescope data in the same platform and to be maintained with small cost for a long time. Firstly, we have applied Adria to the observation data (since July 2013) of Nobeyama Radio Observatory (NRO) 45m, and then we have added the data (since June 2019) of Atacama Submillimeter Telescope Experiment (ASTE) to the same platform.
We installed a new Band10 receiver cartridge (790 − 940 GHz) on ASTE and carried out its Commissioning and Science Verification. We repeated observations toward IRC+10216 with HCN maser line (1110)-(0400), J=10-9, determined the cartridge-specific offsets of sub-reflector position and telescope pointing, and then, obtained beam patterns. The beam size was estimated to be 10.9″ × 10.0″ from the beam patterns. For science verification, we performed observations of an 8′ × 4′ area around Orion-KL of the Orion Molecular Cloud 1 region with CO (J=7-6) line in the on-the-fly method, verified that our images were consistent with past results, and confirmed the capability of ASTE Band10 observations toward bright and extended objects like Giant Molecular Clouds.
A new 790 – 940 GHz heterodyne receiver, ASTE Band 10, was installed in October 2019 on ASTE (Atacama Submillimeter Telescope Experiment), a 10 m submillimeter telescope near of the ALMA site in Chile. An ALMA Band 10 prototype receiver was upgraded with SIS mixers employing high-Jc junctions. The receiver noise temperature (TDSB) measured in the laboratory is between 175 K and 344 K. The achieved system noise temperature on ASTE toward the zenith was 2400 K (PWV <1.0 mm). Their Allan variances were less than 2.0 x 10-6 for timescales in the range of 0.05 sec < T <100 sec.
KEYWORDS: Receivers, Polarization, Heterodyning, Telescopes, Superconductors, Temperature metrology, Single sideband modulation, Radio telescopes, Astronomy, Clouds
The ASTE (Atacama Submillimeter Telescope Experiment) is a 10-m submillimeter telescope located near the ALMA (Atacama Large Millimeter/submillimeter Array) site in Chile. Recently, the ASTE heterodyne receiver system has been upgraded with a new cryostat and two sub-mm-wave heterodyne receivers. The cryostat has three receiver ports. Its cooling capacity is improved with new design compared to a previous three-cartridge cryostat. The two new receivers are dual polarization Superconductor-Insulator-Superconductor (SIS) sideband-separating receivers in 345 GHz and 460 GHz bands. The 345 GHz band receiver has 55 GHz bandwidth. The single-sideband noise temperature TSSB measured in the laboratory is between 62 K and 440 K. The 460 GHz band receiver was originally an engineering qualification model of the ALMA Band 8 cartridge. The design of SIS mixer devices has been optimized for full coverage of ALMA Band 8 frequency (385-500 GHz). TSSB of the receiver is between 98 K and 257 K. The receiver system was installed on ASTE in March 2017. We have started to provide it for open-use observations after our CSV (Commissioning and Science Verification) activities.
Alain Baudry, Richard Lacasse, Ray Escoffier, John Webber, Joseph Greenberg, Laurence Platt, Robert Treacy, Alejandro Saez, Philippe Cais, Giovanni Comoretto, Benjamin Quertier, Sachiko Okumura, Takeshi Kamazaki, Yoshihiro Chikada, Manabu Watanabe, Takeshi Okuda, Yasutake Kurono, Satoru Iguchi
Two large correlators have been constructed to combine the signals captured by the ALMA antennas deployed on the
Atacama Desert in Chile at an elevation of 5050 meters. The Baseline correlator was fabricated by a NRAO/European
team to process up to 64 antennas for 16 GHz bandwidth in two polarizations and another correlator, the Atacama
Compact Array (ACA) correlator, was fabricated by a Japanese team to process up to 16 antennas. Both correlators meet
the same specifications except for the number of processed antennas. The main architectural differences between these
two large machines will be underlined. Selected features of the Baseline and ACA correlators as well as the main
technical challenges met by the designers will be briefly discussed. The Baseline correlator is the largest correlator ever
built for radio astronomy. Its digital hybrid architecture provides a wide variety of observing modes including the ability
to divide each input baseband into 32 frequency-mobile sub-bands for high spectral resolution and to be operated as a
conventional 'lag' correlator for high time resolution. The various observing modes offered by the ALMA correlators to
the science community for 'Early Science' are presented, as well as future observing modes. Coherently phasing the
array to provide VLBI maps of extremely compact sources is another feature of the ALMA correlators. Finally, the status
and availability of these large machines will be presented.
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