[Speaker 1]
Ayumu Matsuzawa
M2, SOKENDAI, Mitaka（supervisor : Satoru Iguchi）
[Title]
Evaluation of pointing error on ALMA ACA antenna
[Abstract]
The pointing error is difference between actual direction and directed direction of the antenna. I evaluate the activity of scientific performance by pointing error for ALMA antenna. The pointing error of ALMA antenna has three components: The components of antenna, the component of the optical pointing telescope and the components of the atmosphere. The purpose of my research is extract and evaluates the only component of radio antenna. Because, the component of antenna specification be established.
Therefore, the component of antenna can correctly evaluate rather than other two components.
For evaluate the pointing error, I estimate the pointing error from measurement data. The measurement of pointing error uses the optical pointing telescope (OPT). OPT installed in surface of antenna, and shooting a star by CCD in OPT. In the image of CCD, the pointing error assumed the difference center of image between centroid of star. But, this image included same noise. I made a program for remove the noise in image. I confirm that this program perform in ideal image as expected.
The component of antenna has some components (wind, thermal, servo, meterology). For extract these components, I measure the pointing error by Long tracking (measure the pointing error when tracking the one source over 15min). It can extract using the data of resolver and thermocouple. Now, I measure the pointing error by many long tracking, also I will measure the pointing error by Fast switching (measure the pointing error when the antenna is moving fast). After this, I will evaluate the component of radio antenna from pointing error. By this research, I expect improve the precision of pointing error for ALMA antenna.
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[Speaker 2]
Nagisa Shino
D1, SOKENDAI, Mitaka（supervisor : Mareki Honma）
[Title]
Testing the formation scenario of massive star by CH3OH maser
[Abstract]
Now classⅠ CH3OH maser is thought to be associated with outflow, while classⅡ CH3OH maser is thought to be associated with accretion disc.
If this is true, classⅠ CH3OH maser is expected to be distributed perpendicularly with respect to rotating disk.
Detecting (or rejecting) this will play a major role in understanding the scenario of massive star formation.
To do this, we plan to observe distributions of two classes of CH3OH masers with VLBI. For that purpose, first we have to look fortarget sources in which both of classes are detected.
We performed the single-dish observations of both classes of CH3OH maser using Nobeyama 45m and Yamagucchi 32m telescopes.
As a result, we discovered 89 sources detected in both classes.