年別アーカイブ: 2014年

Development of Software for Precise LLR Data Analysis / Black-Hole Mass Measurements Using mm-wave Interferometric Observations / Optical Seeing Properties on the Pointing Verification for ALMA Antenna

RyosukeNagasawa, M2, SOKENDAI, Mitaka(supervisor: Hideo Hanada)
Development of Software for Precise LLR Data Analysis

Kyoko Onishi, D1, SOKENDAI, Mitaka(supervisor: Satoru Iguchi)
Black-Hole Mass Measurements Using mm-wave Interferometric Observations

Ayumu Matsuzawa, D2, SOKENDAI, Mitaka(supervisor: Satoru Iguchi)
Optical Seeing Properties on the Pointing Verification for ALMA Antenna

Searching for Protoclusters / Probabilistic Selection of z>6 Quasars: Initial Results from the First HSC SSP Data

Jun Toshikawa, D3, SOKENDAI, Mitaka(supervisor: Nobunari Kashikawa)
Searching for Protoclusters

Masafusa Onoue, M2, SOKENDAI, Mitaka(supervisor: Nobunari Kashikawa)
Probabilistic Selection of z>6 Quasars: Initial Results from the First HSC SSP Data
I will present my high-z quasar selection method using SED fitting and its application to the first HSC-SSP data.
While it is a well-known problem that the classical quasar selection based on two colors suffers from contaminating sources such as brown dwarfs, photometric redshift with multi-color photometry is a complementary way to effectively isolate high-z quasars. Since photo-z for AGN has been less explored comparing with photo-z for galaxies, I have developed template SED fitting method by myself to construct the largest z>6 quasar sample with the HSC survey.
In this talk, I will show how our selection works on the existing quasar samples such as z>3 quasars in the COSMOS field, and then report the result of the first application to the HSC-SSP data products, which results in five z>6 quasar candidates including one possible highest-redshift (z_photo=7.3) quasar.

Observation ExperimentⅠA [ Experiment by Subaru ] Report English ver.

Graduate students from SOKENDAI (The Graduate University for Advanced Studies, Japan) conducted observation during the first half night of November 6, 2014 using Subaru Telescope. With the guidance and advices from the staff of the Subaru Telescope, they studied the surroundings of a quasar with Multi-Object InfraRed Camera and Spectrograph (MOIRCS). A faculty of SOKENDAI reports how the observation went.

Figure 1: Subaru Telescope’s enclosure at dusk. As the Sun goes down, the shutters of the Subaru Telescope enclosure started to open into a crisp air of about 4150 meter altitude (above 13,000 feet). Ventilators at the side and the rear of the telescope also start to open, to help equalize the temperature inside and outside of the building to ensure delivering sharp image into the observation instrument. (Credit: NAOJ,SOKENDAI)


The target of the night is a quasar of which luminosity is as much as 100 times greater than the entire Milky Way Galaxy. The source of energy is attributed to a super massive black hole in the nucleus of a galaxy in a great distance. Due to the large amount of their energy, it is possible to observe quasars even though they are far away.

How the quasars came to be? One of the mechanisms that might have contributed to them is the active star formation in their host galaxies. The indicator of such activity is the ionized hydrogen gas and the distribution of such gas can be detected in the specific emission lines in the spectrum, such as the one called H-alpha line. This line is in the visible wavelength, but shifts into the near infrared because the object is at the redshift z of 2.2. Use of MOIRCS, which has a wide field view as a near infrared imager, helps find such active star forming regions.

The observers of the night are the graduate students from SOKENDAI. SOKENDAI is a unique education-research facility in Japan, with only graduate course and bases on national institutions. National Astronomical Observatory of Japan serves as the Department of the Astronomical Science in SOKENDAI. It is important for a research facility to help grow the next generation researchers. Hence the staffs at Subaru Telescope assist and give advice to the graduate students’ learning.

The students took turns to intently monitor the observational condition, evaluate the data quality, and quickly adjust the integration time accordingly. By conducting observation at Subaru Telescope, they get credits for their course work. The faint signal from the distant universe is not readily noticeable in the quick look data. The high cloud somewhat diminished the signal, but never the enthusiasm of the observers.

Figure 2: (Top) Checking the telescope and the instrument condition during the daytime. (Bottom) Observation at nighttime. (Credit: NAOJ,SOKENDAI)

Toward the end of the observation, the students became confident about the quality of data. They describe their observation experience as precious and unique opportunity of learning, and call out “Come join us at SOKENDAI or other astronomy course, and together let’s explore the universe further.”



Subaru Telescope

天文科学実習IA(すばる実習)報告 日本語ver.

 総合研究大学院大学 (総研大) の大学院生による、すばる望遠鏡を用いた観測実習が2014年11月6日の前半夜に行われました。ハワイ観測所のスタッフのアドバイスも得ながら、赤外線多天体撮像分光装置 MOIRCS を使い、クエーサーの環境を調べる観測に取り組みました。ハワイ観測所の総研大教員がレポートします。


 クエーサーのエネルギー源は遠方銀河の中心にある巨大なブラックホールと考えられ、銀河全体の 100 倍以上もの光度を放っているため、宇宙で最も明るい天体現象です。天の川銀河系の中心にもブラックホールがありますが、クエーサーは放射しているエネルギー量が桁違いです。このためクエーサーは遠方にあっても検出できるのです。

 さてそのようなクエーサー生成の手がかりの一つが、クエーサーを含む銀河での星形成です。大規模な星形成があれば、生まれたばかりの星々が自分の周囲や近くにある星間雲の主成分である水素ガスを大量に電離させます。その電離した水素イオンが電子と再結合してもとの中性状態に戻るときに、特徴的なスペクトル線、たとえば Hα と呼ばれる輝線を出します。Hα 輝線はもともと可視光の波長域で出る輝線ですが、今回の対象天体のように赤方偏移 z=2.2 にあると、この輝線が赤外線の波長で観測されるようになります。クエーサー周辺で Hα 輝線を特に多く出している領域の分布を調べるため、ある程度広い視野を持つ近赤外線用の撮像装置として MOIRCS を使いました。



写真2:観測の前に望遠鏡や観測に使う装置をじっくり見学 (上)。昼の間にドーム側の寒いところで、ハワイ観測所のスタッフが行う様々な作業についても理解しました。夜は観測管制室で予め準備したファイルを使い、しかしその夜の気象条件と合わせ見て調整をしながら観測 (下)。(クレジット:国立天文台、総研大)




データ解析 春の学校