Shun Ishii

SXDF-ALMA 2 arcmin2 deep survey: Resolving and characterizing the infrared extragalactic background light down to 0.5 mJy

We present a multi-wavelength analysis of five submillimeter sources (S_1.1mm = 0.54-2.02 mJy) that were detected during our 1.1-mm-deep continuum survey in the SXDF-UDS-CANDELS field (2 arcmin^2, 1sigma = 0.055 mJy beam^-1) using the Atacama Large Millimeter/submillimeter Array (ALMA). The two brightest sources correspond to a known single-dish (AzTEC) selected bright submillimeter galaxy (SMG), whereas the remaining three are faint SMGs newly uncovered by ALMA. If we exclude the two brightest sources, the contribution of the ALMA-detected faint SMGs to the infrared extragalactic background light is estimated to be ~ 4.1^{+5.4}_{-3.0} Jy deg^{-2}, which corresponds to ~ 16^{+22}_{-12}% of the infrared extragalactic background light. This suggests that their contribution to the infrared extragalactic background light is as large as that of bright SMGs. We identified multi-wavelength counterparts of the five ALMA sources. One of the sources (SXDF-ALMA3) is extremely faint in the optical to near-infrared region despite its infrared luminosity (L_IR ~ 1e12 L_sun or SFR ~ 100 M_sun yr^{-1}). By fitting the spectral energy distributions (SEDs) at the optical-to-near-infrared wavelengths of the remaining four ALMA sources, we obtained the photometric redshifts (z_photo) and stellar masses (M_*): z_photo ~ 1.3-2.5, M_* ~ (3.5-9.5)e10 M_sun. We also derived their star formation rates (SFRs) and specific SFRs (sSFRs) as ~ 30-200 M_sun yr^{-1} and ~ 0.8-2 Gyr^{-1}, respectively. These values imply that they are main-sequence star-forming galaxies.

Hot ammonia in the center of the Seyfert 2 galaxy NGC 3079

We present the results of ammonia observations toward the center of NGC 3079. The NH3(J, K) = (1, 1) and (2, 2) inversion lines were detected in absorption with the Tsukuba 32-m telescope, and the NH3(1,1) through (6,6) lines with the VLA, although the profile of NH3(3,3) was in emission in contrast to the other transitions. The background continuum source, whose flux density was ~50 mJy, could not be resolved with the VLA beam of ~ ~ 175 K, tracing hot gas associated with the interaction of the fast nuclear outflow with dense molecular material around the nucleus.

Condition of Optical Systems Independent of Frequency for Wide Field-of-View Radio Telescopes

In this paper, we present a condition of optical systems to form images independent of frequency. The condition independent of frequency in case of a single Gaussian beam on an optical axis has been known, but that in case of a beam propagated off the axis or tilted beam, which appears in a wide field-of-view (FOV) telescope, has not been known. We first show relations between an arbitrary electric field on an object plane and an induced one on an image plane after passing through a lens with calculating Fresnel diffraction integrals. If the lens formula is met, there is a one-to-one correspondence between points on the object and image plane. This result enables to use geometrical optical methods. The condition and relations derived here are confirmed by simulations. We also applied them to a wide-FOV telescope.

The CARMA-NRO Orion Survey

We present the first results from a new, high resolution,

A Multi-Line Ammonia Survey of the Galactic Center Region with the Tsukuba 32-m Telescope - I. Observations and Data

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Dome Fuji in Antarctica as a Site for Infrared and Terahertz Astronomy

CO(1-0),

Expanding CO Shells in the Orion A Molecular Cloud

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Hot gas in the center of the Seyfert galaxy NGC 3079

CO(1-0), and C

Development of a 30-cm submillimeter-wave telescope for the operation at Dome Fuji in Antarctica

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Site testing at Dome Fuji for submillimeter and terahertz astronomy: 220 GHz atmospheric-transparency

O(1-0) molecular line survey of the Orion A cloud, hereafter referred to as the CARMA-NRO Orion Survey. CARMA observations have been combined with single-dish data from the Nobeyama 45m telescope to provide extended images at about 0.01 pc resolution, with a dynamic range of approximately 1200 in spatial scale. Here we describe the practical details of the data combination in uv space, including flux scale matching, the conversion of single dish data to visibilities, and joint deconvolution of single dish and interferometric data. A