Kimiaki Kawara

Excitation mechanism of forbidden Fe II 1. 644 micron emission in Seyfert and starburst galaxies

The excitation mechanism of the forbidden Fe II emission in AGN and starbust nuclei (SBN) is studied by comparing the intensity of the forbidden Fe II 1.644 micron emission with those of low-ionization optical lines. A linear correlation is found between the line ratio of forbidden Fe II/Br-gamma and forbidden O I /H-alpha, while the correlation between forbidden Fe II/Br-gamma and forbidden N II/H-alpha is poor. The forbidden O I lines is radiated from hydrogen transition regions while the forbidden N II line comes from fully ionized regions. It is concluded that the forbidden Fe II emission is excited by electron collisions in extended transition regions. In SBN, the forbidden Fe II emission is due to shock heating caused by starburst winds rather than photoionization. The forbidden Fe II emission is stronger in Seyfert and composite galaxies than in pure starburst galaxies. 66 refs.

The University of Tokyo Atacama Observatory 6.5m telescope: project overview and current status

The University of Tokyo Atacama Observatory Project is to construct and operate a 6.5m infrared telescope at the summit of Co. Chajnantor (5640m altitude) in northern Chile, promoted by the Institute of Astronomy of the University of Tokyo. Thanks to the dry climate (PWV~0.5mm) and the high altitude, excellent observation condition in the NIR to MIR wavelengths is achieved. The telescope has two Nasmyth foci where two facility instruments, SWIMS for the near-infrared and MIMIZUKU for the mid-infrared, are installed and two folded- Cassegrain foci for carry-in instruments. All these four foci can be switched by rotating a tertiary mirror. The final focal ratio is 12.2 and the foci have large field-of-view of 25 arcmin in diameter. We adopted a 6.5-m F/1.25 light-weighted borosilicate honeycomb primary mirror and its support system that are developed by Steward Observatory Richard F. Caris Mirror Lab. An enclosure has the shape of carousel, and large ventilation windows with shutters control the wind to flush heat inside the enclosure. A support building with a control room, a mirror coating system and maintenance facilities is located at the side of the enclosure. The mirror coating system consists of a large aluminizing chamber and a mirror washing facility. The operation of the telescope will be remotely carried out from a base facility at San Pedro de Atacama, 50km away from the summit. Development of the two facility instruments has already been completed and they are transported to Hilo, Hawaii in 2017. We are going to carry out engineering observations of those instruments on the Subaru telescope for clearing up technical issues and verifying their performance. The existing summit access road from the ALMA concession area was laid in 2006, however, it is too narrow to carry large components of the telescope and the ancillary facilities such as the primary mirror, its cell, and the aluminizing chamber. The road is being expanded so that it has the width of <5m for straight portion and <7m for curved portion.. The telescope mount and the enclosure are being pre-assembled for functional and performance tests in Japan. All telescope system will be assembled at the summit and see the engineering first light early 2019.