2015.12.14-12.20

12月14日（月）13：30～15：00　　太陽系小天体セミナー　　　南棟2階会議室
Dec 14 Mon　　　Solar System Minor Body Seminar　　　Conference Room, South Bldg.2F

12月15日（火）15：00～16：00 　　VLBIコロキウム　　中央棟（南）2F VLBIセミナー室
Dec 15 Tue　　　VLBI Colloquium　　　　VLBI Seminar Room, Main Bldg. (South) 2F

12月15日（火）15：00～16：00　　国立天文台野辺山談話会　　　野辺山観測所本館 輪講室
Dec 15 Tue　　　Nobeyama NAOJ Seminar　　　　　　　Seminar Room, Main building, NRO

12月16日（水）10：00～12：00　　総研大コロキウム　　　中央棟（東）輪講室
Dec 16 Wed　　　SOKENDAI colloquium　　　　　　　　　Rinko-shitsu,Main Bldg.(East)

12月16日（水）14：10～15：10　　理論コロキウム　　　　中央棟（北）1F講義室
Dec 16 Wed　　　DTA Colloquium　　　　　　　　　　　Lecture Room

12月18日（金）13：30～15：00　　太陽天体プラズマセミナー　　コスモス会館 会議室
Dec 18 Fri　　　Solar and Space Plasma (SSP) Seminar　　　　Conference Room, Cosmos Lodge

12月18日（金）16：00～17：00　　国立天文台談話会　　　大セミナー室
Dec 18 Fri　　　NAOJ Seminar　　　　　　　 　　Large Seminar Room

詳細は以下をご覧下さい。

12月14日(月)

キャンパス

三鷹

セミナー名

太陽系小天体セミナー

臨時・定例の別

定例

日時

12月14日（月曜日）13時30分～15時

場所

南棟２階会議室

講演者

松村行博

連絡先

　名前：渡部潤一

備考

テレビ会議またはスカイプによる参加も可

12月15日(火)

キャンパス

三鷹

セミナー名

VLBIコロキウム

臨時・定例の別

臨時

日時

　12月15日（火曜日）15:00　～　16:00

場所

　中央棟(南)2階VLBIセミナー室

講演者1

Monica Orienti

所属

　INAF-IRA

タイトル

Radio and gamma-ray properties of the nearby radio galaxy 3C 84

Abstract

We present results of multifrequency high resolution Very Long Baseline Interferometry (VLBI) observations of the nearby radio galaxy 3C 84.This object is one of the closest and thus best-studied misaligned active galactic nuclei. Despite gamma-ray silent during the EGRET-era, 3C84 has been detected during high-energy flares by Fermi and MAGIC telescopes. Recent high-resolution observations point out a limb-brightened structure on parsec scale. In this talk we present an overview of this peculiar object, and we discuss the connection between the radio and gamma-ray properties.

講演者2

Filippo D’Ammando

所属

　INAF-IRA

タイトル

Seven years of gamma-ray and multiwavelength observations of powerful relativistic jets in narrow-line Seyfert 1 galaxies

Abstract

Before the launch of the Fermi satellite only two classes of AGN were known to generate relativistic jets and thus to emit electromagnetic radiation up to the gamma-ray energy range: blazars and radio galaxies, both hosted in giant elliptical galaxies. The first six years of observations by Fermi-LAT confirmed that these two are the most numerous classes of identified sources in the extragalactic gamma-ray sky, but the discovery of variable gamma-ray emission from radio-loud Narrow-Line Seyfert 1 galaxies (NLSy1) revealed the presence of an emerging third class of AGN with relativistic jets. By considering that NLSy1 are commonly hosted in spiral galaxies, this finding poses intriguing questions about the nature of these objects, the formation of relativistic jets, and the evolution of radio-loud AGN.

I report on a systematic investigation of the gamma-ray properties of a complete sample of radio-loud NLSy1, including the detection of new objects, using 7 years of Fermi-LAT data with the new Pass 8 event-level analysis. In addition I discuss new results about the radio-to-very-high-energy properties of the gamma-ray emitting NLSy1 in the context of the blazar scenario.

Language

English

連絡先

　名前：酒井 大裕

備考

テレビ参加可

12月15日(火)

キャンパス

野辺山

セミナー名

国立天文台野辺山　談話会

臨時・定例の別

定例

日時

12月15日（火曜日）　15:00 ～ 16:00

場所

野辺山宇宙電波観測所　本館　輪講室

講演者

松澤歩 氏

所属

総合研究大学院大学

タイトル

Study on the Verification Method of Pointing Performance of Submillimeter Wavelength Antenna through the ALMA

Abstract

ALMA (Atacama Large Millimeter/Submillimeter Array) is an astronomical radio interferometer of millimeter/submillimeter wavelength composed of 66 antennas. All the ALMA antennas are required to meet high pointing performance which is better than 0.6 arcsec in tracking a star under the primary operating conditions. In this presentation, the detailed verification measurements of the pointing performance in tracking a star of the ALMA ACA antennas were performed with an optical pointing telescope and angular encoders. In particular, the estimation method of the pointing error due to optical seeing is investigated. As a result, the method to estimate contribution of the pointing error due to optical seeing is improved by developing a relation between the pointing error due to optical seeing, integration time and averaged wind velocity.

連絡先

　名前：西村淳

備考

テレビ参加可

12月16日(水)

Campus

Mitaka

Seminar Name

SOKENDAI colloquium

Regular/Irregular

Regular

Date

10:00-12:00, Dec 16, 2015

Place

輪講室 (IP: 133.40.2.203)

Speaker 1

Koki OKUTOMI

Affiliation

D1, SOKENDAI( supervisor: Yoichi ASO, Raffaele FLAMINIO, Tomotada AKUTSU )

Title

Installation and Control of The Mirror Suspension System for KAGRA

Abstract

Japanese gravitational-wave telescope KAGRA is now under installation of instruments toward the test run in next March. The suspension system of the mirror is one of the key instruments to activate the laser interferometer and to achieve expected sensitivity. Today I’ll present a current status of the installation work and some measurement results of the suspension control system.

Speaker 2

Shogo ISHIKAWA

Affiliation

D2, SOKENDAI( supervisor: Nobunari Kashikawa )

Title

TBA

Speaker 3

Ryosuke NAGASAWA

Affiliation

D1, SOKENDAI( supervisor: Hideo Hanada )

Title

Software development for precise determination of lunar orbit and rotation using Lunar Laser Ranging data analysis

Organizer

Name : Ryosuke Nagasawa

Comment

TV conference connection is available from Hawaii, Nobeyama, Mizusawa and Okayama.

12月16日(水)

Campus

Mitaka

Seminar

DTA colloquium

Regular/Irregular

Regular

Date

16 Dec 2015, 14:10-15:10

Place

Lecture Room

Speaker

Lucie Jilkova

Affiliation

Leiden Observatory

Title

Mass transfer between debris discs during close stellar encounters

Abstract

Stars are born in clustered environment and planetary systems are born around stars. Stars in clusters gravitationally interact and experience close encounters that have a direct influence on their planetary systems. I will present results on simulations of mass transfer among debris (planetesimal) discs during close stellar encounters that happen in star clusters. We explored the parameter space of the encounters and mapped the orbits of the transferred planetesimals around their parent star as well as around their new host. Depending on encounter parameters, a substantial part of the disc can be captured by the other star and the captured objects have specific orbits. We expect that many stars experienced transfer among their debris discs and planetary systems in their birth environment and I will present the implications of this process for the Solar system.

Facilitator

-Name: Tsuyoshi Inoue

12月18日(金)

Campus

Mitaka

Seminar

Solar and Space Plasma Seminar

Regular/Irregular

Regular

Date

13:30-15:00, 18 December (Fri)

Place

Seminar Room, Cosmos Kaikan

Speaker

Yukio Katsukawa (NAOJ) and Sunrise-J team

Affiliation

National Astronomical Observatory of Japan

Title

Sunrise-III for high-resolution and -sensitivity spectro-polarimetric observations of the chromosphere

Abstract

We’ve just started a study to participate in the Sunrise balloon-borne observatory project which was so far conducted by Germany and Spain, and to make a spectro-polarimetric observation of the chromosphere. The Sunrise observatory carries a 1 m aperture optical telescope, and allows us to perform seeing-free visible-IR observations as well as observations in the 200 – 300 nm UV range from an altitude higher than 35 km. So far, imaging observations were done by filtergraph instruments SuFI and IMaX mainly observing photospheric lines in the previous flights. In the third flight, a new spectro-polarimeter is expected to be implemented for observing chromospheric lines as well as upgrading the existing instruments. Targets of the spectro-polarimeter are to study driving mechanisms of spicules and jets in the chromosphere and to clarify an energy flow along chromospheric structures based on the spectro-polarimetric observations combined with the imaging ones.
For doing them, the spectro-polarimeter is designed to observe both Ca II 854 nm and Na I D 589 nm lines simultaneously, as a baseline, to have good magnetic sensitivity from the photosphere to the middle chromosphere. The spatial resolution and FOV are 0.2″ and 50″x50″, respectively, and 3e-4 polarimetric sensitivity can be achieved within 15 sec integration. The instrument is to be developed as maximum use of existing heritage developed for Solar-C and CLASP and acquiring and demonstrating new techniques for Solar-C. The third flight is desired to be in the 2019-2020 time frame not to significantly fall behind DKIST.

Facilitator

-Name： Shin Toriumi

12月18日(金)

キャンパス

三鷹

セミナー名

国立天文台談話会

臨時・定例の別

定例

日時

12月18日 (金) 16:00-17:00

場所

大セミナー室

講演者

Jean-Luc Starck

所属

CEA Saclay

タイトル

Morphological Diversities in Astrophysics

Abstract

We present the concept of Morphological Diversity, which is based on sparsity and allows us to separate blindly one data set into several components, each one being sparse in a given representation.
This method has been extended to multichannel data.
We show how this idea allows us to analyze differently astrophysical data set such as cosmic microwave background data provided by WMAP and PLANCK satellites.

連絡先

名前：田中　雅臣

以上