&lt;title&gt;Data analysis environment (DASH2000) for the Subaru telescope&lt;/title&gt;

We found a very large, ∼ 35 kpc, emission-line region around the Seyfert type 2 galaxy NGC 4388, using deep narrow-band imaging with the prime focus camera (Suprime-Cam) of the Subaru telescope. This region consists of many faint gas clouds or filaments, and extends northeastwards from the galaxy. The typical Hα luminosity L(Hα) of the clouds is ∼ 10 37 erg s −1 , and the total L(Hα) of the region within 10 kpc from the nucleus is ∼ 2 × 10 38 erg s −1 , which corresponds to an ionized gas mass of ∼ 10 5 M . The map of the emission-line intensity ratio I([O III])/I (Hα) indicates that the inner (r < 12 kpc) region of the VEELR may be excited by nuclear ionizing radiation. The excitation mechanism of the outer (r > 12 kpc) region is unclear, but it is likely that the nuclear radiation is also a dominant source of its ionization. We discuss the origin of the ionized gas. Two plausible origins of the gas in the VEELR are (i) the tidal debris resulting from a past interaction with a gas-rich dwarf galaxy, i.e., a minor merger, or (ii) the interstellar medium of NGC 4388, stripped by the ram pressure of the hot intracluster medium of the Virgo cluster.

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Discovery of a Very Extended Emission‐Line Region around the Seyfert 2 Galaxy NGC 4388

Yoshida

Yagi

Okamura

et al. 2002

ApJ

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100

121

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A Differential Abundance Analysis of the Wide Binary Pair HD 219542 A and B

Sadakane¹,

Ohkubo²,

Honda³

2003

Publications of the Astronomical Society of Japan

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The abundances of 22 elements (Li through Zr) in the A and B components of the visual pair HD 219542 were determined and compared using a differential analysis technique. Both components were found to be metal rich, $[\mathrm{Fe/H}] = +0.13$, in the brighter component (A) and $[\mathrm{Fe/H}] = +0.08$ in the fainter component (B). The abundances of three elements (Sc, Ti, and Fe) are definitely higher (by 0.05 dex) in component A than in component B. On the other hand, both components have nearly identical abundances of the light element Si. No evidence has been found for differences in the abundances for C, O, Na, Mg, Al, S, Ca, V, Cr, Mn, Co, Ni, Cu, Zn, Sr, Y, and Zr. No clear correlation has been found between the differences in the abundance between the two components and the condensation temperature ($T_\mathrm{c}$).

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Current Performance and On-Going Improvements of the 8.2 m Subaru Telescope

Iye

Karoji²,

Ando

et al. 2004

Publications of the Astronomical Society of Japan

143

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An overview of the current status of the 8.2 m Subaru Telescope constructed and operated at Mauna Kea, Hawaii, by the National Astronomical Observatory of Japan is presented. The basic design concept and the verified performance of the telescope system are described. Also given are the status of the instrument package offered to the astronomical community, the status of operation, and some of the future plans. The status of the telescope reported in a number of SPIE papers as of the summer of 2002 are incorporated with some updates included as of 2004 February. However, readers are encouraged to check the most updated status of the telescope through the home page, http://subarutelescope.org/index.html, and/or the direct contact with the observatory staff.

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<title>Data analysis environment (DASH2000) for the Subaru telescope</title>

Cited by 4 publications

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Discovery of a Very Extended Emission‐Line Region around the Seyfert 2 Galaxy NGC 4388

Discovery of a Very Extended Emission‐Line Region around the Seyfert 2 Galaxy NGC 4388

A Differential Abundance Analysis of the Wide Binary Pair HD 219542 A and B

Current Performance and On-Going Improvements of the 8.2 m Subaru Telescope

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