2015 Fiscal Year Research-status Report
近赤外光束原理(cgs系)の設定と近赤外標準星ネットワークの構築
| Project/Area Number |
15K05019
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| Research Institution | The University of Tokyo |
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Principal Investigator |
福来 正孝 東京大学, カブリ数物連携宇宙研究機構, 特任教授 (40100820)
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| Co-Investigator(Kenkyū-buntansha) |
鈴木 尚孝 東京大学, カブリ数物連携宇宙研究機構, 特任助教 (20722804)
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| Project Period (FY) |
2015-04-01 – 2018-03-31
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| Keywords | cosmic dust / heavy metal abundance / Mg II clouds / galactic winds / DLA |
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| Outline of Annual Research Achievements |
The goal of the project is to set the zero point of near infrared photometry in cgs units (the AB system). The current project consists of a series of instrumentation and experiments towards this goal. This is not a project that directly produces science results, but a project indispensable to a vast variety of astronomical observations for near infrared bands to derive useful scientific results.The present project is purely of technical nature which becomes science only when we obtain the final results.
The first year is to prepare optical filters for the experimental device. After a number of iterations with Subaru Tele-scope in Hawaii and also with Asahi Spectra Co Ltd, the manufacturer of optical filters, we made a final design of the z-band optical filter and procured them by the end of March, with the preliminary transmission curve looked satisfactory.
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| Current Status of Research Progress |
Current Status of Research Progress
3: Progress in research has been slightly delayed.
Reason
According to the original plan, we measure the response of the MOIRCS detector in both i and z bands.While we have been studying their design, the Subaru team in Hawaii last autumn changed the specification of the MOIRCS detector. This sets back our original project, forced us to modify our strategy, discarding the i band measurement, which is now completely screened out by renewed MOIRCS optics. This was a bad news to us. This forces us to redesign our strategy, discarding the i band measurement, and at a technical level the characters of z band fiters, with understanding that we cannot ac- hieve a high accuracy as we originally aimed. After iterations with Asahi Spectra, we reached an optimal solution.
This procedure caused delay.
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| Strategy for Future Research Activity |
We first verify the transmission curves of procured filters. We then bring the filters to Hawaii and install them on the MOIRCS detectors, when they were brought to the room temperature, which is expected in August.
The support bench will be fabricated by summer, which will also be shipped to Hawaii.
We expect to carry out response measurements when MOIRCS is free from the observation use in Hawaii. As we were told, we expect it in late fall.
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| Causes of Carryover |
Procuremnet of filters were delayed, caused originally by the specification modification of the Subaru MOIRCS detector in the Hawaii observatory.
This caused a half year delay.
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| Expenditure Plan for Carryover Budget |
We purchase a few incandescent tungusten lamps, a few photodiode, and a power supply and connecting wires etc, after checking what are available in Hawaii Observatory.We will design (being done) and ask the NAOJ machine shop to fabricate supporting benches for the lamp.
The cost of extra liquid nitrogen needed for our work should also be paid.The rest is travel expenses to observatories, and also to various institutes to meet people.
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