KNIFE, KAshima Nobeyama InterFErometer

By connecting two antennas, Kashima 34~m and Nobeyama 45~m, an east-west baseline of 200~km is formed. At that time, because Nobeyama 45~m had the world's number one sensitivity in the 43~GHz band, and also Kashima 34~m was the world's third-largest one, the Kashima-Nobeyama baseline provided the highest sensitivity at 43~GHz VLBI (Figure 1). The construction of the Kashima 34~m antenna began in 1988, also almost at the same time, a domestic project of mm-VLBI (KNIFE, Kashima Nobeyama INterFrermeter) started. Nobeyama Radio Observatory provided the first cooled-HEMT 43~GHz receiver in the world to the Kashima 34~m. In October 1989, the first fringe at 43~GHz was detected. We here review the achievements of the KNIFE at that time.Comment: 5 pages, 5 figures, manuscript in Proceedings of the 18th NICT TDC Symposium (Kashima, October 1, 2020

Observations of SiO Maser Sources within a Few Parsec from the Galactic Center

Mapping and monitoring observations of SiO maser sources near the Galactic center were made with the Nobeyama 45-m telescope at 43 GHz. Rectangular mapping an area of approximately 200'' x 100''$ in a 30'' grid, and triangular mapping in a 20'' grid toward the Galactic center, resulted in 15 detections of SiO sources; the positions of the sources were obtained with errors of 5--10'', except for a few weak sources. Three-year monitoring observations found that the component at V_lsr=-27 km/s of IRS 10 EE flared to about 1.5 Jy during 2000 March--May, which was a factor of more than 5 brighter than its normal intensity. Using the radial velocities and positions of the SiO sources, we identified 5 which are counterparts of previously observed OH 1612 MHz sources. The other 10 SiO sources have no OH counterparts, but two were previously detected with VLA, and four are located close to the positions of large-amplitude variables observed at near-infrared wavelengths. A least-squares fit to a plot of velocities versus Galactic longitudes gives a rather high speed for the rotation of the star cluster around the Galactic center. The observed radial-velocity dispersion is roughly consistent with a value obtained before. It was found that all of the SiO sources with OH 1612 MHz counterparts have periods of light variation longer than 450 days, while SiO sources without OH masers often have periods shorter than 450 days. This fact suggests that lower-mass AGB stars are more often detected in SiO masers than in the OH 1612 MHz line.Comment: 9 pages, 7 figures. PASJ 54, No. 1 (2002) in pres

THE ELEMENTS OF THE CLINICAL SUPERVISION: EXPORTING CONCEPTS TO JAPAN

The current Japanese counseling profession is in the process of reforming and uniting the system and training together for counseling and related professions. Supervision is one of significant training piece in this profession; however, its familiarity among Japanese counseling professionals is very unclear. This study explored how Japanese counseling professionals conceptualize the ideal figure of a clinical supervisor based on the identified fundamental elements of clinical supervision in the US. The preliminary analysis indicates that each aspect of the U.S. clinical supervision models might be adoptable to Japanese counseling professionals. Yet the small sample size does not confirm the conceptual framework of the ideal clinical supervisor for Japanese counseling professionals, the main analysis indicated an alternative culturally appropriate conceptual framework. Further research embracing Japanese cultural characteristics and sound ethical manner in the professional counseling and supervisory relationship would enrich the clinical supervision in Japan