2024.2.5-2024.2.11

February 6 Tue 10:00-11:30
太陽系小天体セミナー
Zoom


February 7 Wed 14:00-15:00
ALMA-J seminar
hybrid; Small seminar room in the Subaru building and Zoom


February 7 Wed 15:30-16:30
NAOJ Science Colloquium
hybrid; Large Seminar Room in Subaru Building and Zoom


February 9 Fri 10:30-12:00
Solar and Space Plasma Seminar
Zoom


February 9 Fri 16:00-17:00
NAOJ Seminar
hybrid; Large Seminar Room in Subaru Building and Zoom


詳細は下記からご覧ください。

=============== February 6 Tue ===============

キャンパス:三鷹
セミナー名:太陽系小天体セミナー
定例・臨時の別:定例
日時:2月6日(火曜日)10時00分~11時30分
場所:zoom
講演者:和田 空大
所属:東京大学
タイトル:Tomo-e Gozen NEO 探査改善プロジェクトの現状共有と今後の展望
Abstract:東京大学木曽観測所では2019年から地球接近小惑星 (NEOs)
の探査を開始し、現在までで多数の小惑星の発見や物理量の測定を行ってきました。
探査を行うにつれ現在のプロセスの課題が浮き彫りになっており、私が主導して改善を試みている最中です。
今回の発表では、プロセス全体の中でも特に移動天体検出に使っている機械学習モデルについて、その改善の方針と現状共有をします。

世話人の連絡先
 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

=============== February 7 Wed ===============

Campus: Mitaka
Seminar: ALMA-J seminar
Date and time: February 7 (Wed) 14:00-15:00
Place: hybrid (Small seminar room in the Subaru building and Zoom)

Speaker: Yuhito Shibaike
Affiliation: NAOJ
Title: Constrains on the properties of forming planets from the dust continuum emission of the circumplanetary disks

Abstract:
Although there have been a lot of theoretical research on the formation of gas planets, observational supports have still been very rare. The young T Tauri star PDS 70 has two gas accreting planets sharing one large gap in a pre-transitional disk, which is a valuable system to obtain observational constraints. Recently, dust continuum emission from PDS 70 c has been detected by ALMA Band 7, considered as the evidence of a circumplanetary disk (CPD), a small gas (and dust) disk formed around the planet as a byproduct of the gas accretion. To obtain constraints on the planet properties, we introduce a model of dust evolution in the CPD and reproduce the detection of the dust continuum emission. We find positive correlations between the intensity of the dust emission and three important planet properties, the planet mass, gas accretion rate, and their product called MMdot. We then find that the MMdot of PDS 70 c must be larger than 0.4 MJ^2 /yr, corresponding to the lower limits of the planet mass and the gas accretion rate, 5 MJ and 0.02 MJ/yr. This is the first case to succeed in obtaining constraints on planet properties from the dust continuum emission of a CPD. We also find some loose constraints on the properties of PDS 70 b from the non-detection of its dust emission. We propose possible scenarios for the PDS 70 b and c explaining the non-detection respectively detection of the dust emission from their CPDs. I will also discuss my future plans to obtain constraints on other gas accreting planets if there is enough time.

=============== February 7 Wed===============

Campus: Mitaka
Seminar: NAOJ Science Colloquium
Date and time: 2023 Feb. 7 (Wed.), 15:30-16:30
Place: the large seminar room / Zoom (hybrid)

Speaker: Yui Kawashima
Affiliation: ISAS/JAXA
Title: Subaru/IRD high-resolution spectroscopy of a T-type brown dwarf and investigation of its atmospheric properties with high-resolution spectrum model ExoJAX
Abstract:
While brown dwarf atmospheres share composition and temperature with those of extrasolar gas giant planets, in general, brown dwarfs are observable with a higher signal-to-noise ratio when compared to exoplanets. Thus, the observation of brown dwarf atmospheres helps us establish our understanding of various processes in the atmospheres of such temperature and composition, including chemistry, thermal structure, dynamics, and cloud formation. Also, their high-resolution spectra serve as excellent templates for the observational validation of the molecular line lists at such high temperatures. The accuracy of molecular line lists holds the key to detecting chemical species in exoplanet atmospheres, which are often observed with a lower signal-to-noise ratio.

Recently, we observed the high-resolution spectrum of a T6.5-type brown dwarf Gl 229B with the InfraRed Doppler (IRD) spectrograph mounted on the Subaru Telescope. We have constrained its atmospheric properties, such as the molecular abundances and thermal structure, using an inverse-problem approach with our high-resolution spectrum model ExoJAX (Kawahara, Kawashima et al. 2022). We have also investigated the possibility of inferring the object mass using the embedded information on collision-induced absorption uniquely accessible by high-resolution spectroscopy. Furthermore, we have revealed that in some wavelength regions, specific molecular line lists do not match the observed absorption features.

Facilitator
-Name: Kazumasa Ohno

Comment: English

=============== February 9 Fri==============

Campus: Mitaka
Seminar: Solar and Space Plasma Seminar
Regularly Scheduled/Sporadic: Sporadic
Date and time:9 February (Fri), 10:30-12:00
Place: Zoom

Speaker:Dr. Tetsu Anan
Affiliation:The National Solar Observatory
Title:Measurements of a reconnection electric field in the solar chromosphere

Abstract:The efficient release of magnetic energy in astrophysical plasmas can be achieved through magnetic-field diffusion, the rate of which is directly tied to the associated electric field. However, there have been only a
few attempts to measure electric fields in the solar atmosphere, because of the common assumption that electric fields must vanish quickly or only exist at unresolvable spatial scales. Using the newly commissioned National Science Foundation’s Daniel K. Inouye Solar Telescope (DKIST), we observed NOAA active region 12995 on February 23rd, 2022, in three spectral bands 397 nm, 630 nm, and 854 nm using the Visible SpectroPolarimeter (ViSP). We successfully obtained Stokes spectra of an Ellerman bomb, which is brightening in the lower chromosphere and are thought to be associated with magnetic reconnection. At the Ellerman bomb, we discovered a broadband circular polarization in a Balmer line of the neutral hydrogen at 397 nm, H epsilon, that can only be explained by the presence of an electric field. Moreover, we found that the measured signal filled a region up to ~1000 km, which is three orders of
magnitude larger than that expected in theory. In this talk, we will present our findings and discuss why the diffusion region is so large, and what is the next step.

Facilitator
-Name:Akiko Tei

Comment:English

=============== February 9 Fri==============

Campus:Mitaka
Seminar:NAOJ Seminar
Regularly Scheduled/Sporadic:Regular
Date and time:February 9, 2024 16:00-17:00
Place:Zoom/Large Seminar Room (hybrid)

Speaker:Dr. Eleonora Di Valentino
Affiliation:University of Sheffield

Title:Unresolved Anomalies and Tensions in the Standard Cosmological Model

Abstract: The standard Lambda Cold Dark Matter cosmological model has been incredibly successful in explaining a wide range of observational data, from the cosmic microwave background radiation to the large-scale structure of the universe. However, recent observations have revealed a number of inconsistencies among the model’s key cosmological parameters, which have different levels of statistical significance. These include discrepancies in measurements of the Hubble constant, the S8 tension, and the CMB tension. While some of these inconsistencies could be due to systematic errors, the persistence of such tensions across various probes suggests a potential failure of the canonical LCDM model. I will examine these inconsistencies and discuss possible explanations, including modifications to the standard model, that could potentially alleviate them. However, I will also discuss the limitations of these proposed solutions and note that none of them have successfully resolved the discrepancies.

Facilitator
-Name:Takashi Moriya

2024.1.29-2024.2.4

January 30 Tue 10:00-16:40
SOKENDAI Progress Report Defense in the second semester, AY2023
2023年度後期 総研大研究中間レポート発表会
hybrid; 中央棟(北)1階 講義室およびZoom


January 30 Tue 10:00-11:30
太陽系小天体セミナー
Zoom


January 31 Wed 10:00-12:00
SOKENDAI Doctoral Thesis Dissertation review
総研大博士学位論文予備審査会
hybrid; Lecture Room and Zoom


January 31 Wed 10:30-12:00
SOKENDAI Colloquium
hybrid; Large Seminar Room in Subaru Building and Zoom


January 31 Wed 15:30-16:30
NAOJ Science Colloquium
hybrid; the 3F seminar room in Instrument Development Building No.3 and Zoom


February 1 Thu 14:00-15:00
Tea Talk
Zoom


詳細は下記からご覧ください。

=============== January 30 Tue ===============

キャンパス:三鷹
セミナー名:2023年度後期 総研大研究中間レポート発表会
(SOKENDAI Progress Report Defense in the second semester, AY2023)
定例・臨時の別:臨時
日時:2023年1月30日(火) 10:00~16:40
場所:中央棟(北)1階 講義室およびZoom

講演者:柿元 拓実(10:00~)(Takumi Kakimoto)
所属:総研大 天文科学専攻 (the Department of Astronomical Science, SOKENDAI)
タイトル:The formation history of a massive quiescent galaxy in a group environment at z = 4.53

講演者:中野 すずか(10:50~)(Suzuka Nakano)
所属:総研大 天文科学専攻 (the Department of Astronomical Science, SOKENDAI)
タイトル:塵に埋もれた活動的な超巨大ブラックホールの発掘を可能とするサブミリ波帯熱源診断法の開発

講演者:渡辺 くりあ(13:00~)(Kuria Watanabe)
所属:総研大 天文科学専攻 (the Department of Astronomical Science, SOKENDAI)
タイトル:Uncovering the Physical Origin of Elemental Abundances in Early Galaxies Formation through Observations and Modeling

講演者:波多野 駿(13:50~)(Shun Hatano)
所属:総研大 天文科学専攻 (the Department of Astronomical Science, SOKENDAI)
タイトル:Exploring for Intermediate Mass Black Holes with Optical Spectra and Near-infrared Luminosity Variability Data.

講演者:内藤 由浩(15:00~)(Yoshihiro Naito)
所属:総研大 天文科学専攻 (the Department of Astronomical Science, SOKENDAI)
タイトル:Spectroscopic study of Alfvén waves in coronal holes as an energy source for the fast solar wind acceleration

講演者:佐藤 慶暉(15:50~)(Yoshiaki Sato)
所属:総研大 天文科学専攻 (the Department of Astronomical Science, SOKENDAI)
タイトル:Study of Electron Acceleration in Solar Flares with X-ray Focusing-Imaging Spectroscopy and Test-Particle Simulation

世話人の連絡先
-名前:大学院係 松田

=============== January 30 Tue ===============

キャンパス:三鷹
セミナー名:太陽系小天体セミナー
定例・臨時の別:定例
日時:1月30日(火曜日)10時00分~11時30分
場所:zoom
講演者:紅山仁
所属:東京大学
タイトル:地球接近小惑星の観測計画2024
Abstract:発表者が2024年に実施する二件の地球接近小惑星の観測計画について発表します。多くの方々のコメントを歓迎いたします。

世話人の連絡先
 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

=============== January 31 Wed===============

Campus:Mitaka
Seminar:SOKENDAI Doctoral Thesis Dissertation review 総研大博士学位論文予備審査会
Regularly Scheduled/Sporadic:Sporadic
Date and time:January 31, 2024 10:00-12:00
Place :Lecture Room and Zoom

Speaker:Yui Kasagi
Title:Unveiling Atmospheric Features of Faint Substellar Companions from High-Resolution Near-Infrared Spectra

Facilitator
-Name:Nozomu Tominaga, Hideyuki Kobayashi, Kaya Kitabayashi (Graduate Student Affairs Unit)

Comment:
https://guas-astronomy.jp/CampusLife/doctor_report.html

=============== January 31 Wed==============

Campus:Mitaka
Seminar:SOKENDAI Colloquium
Regularly Scheduled/Sporadic:Regular
Date and time:January 31, 2024 10:30-12:00
Place:Large Seminar Room in Subaru Building and Zoom

Speaker: Shubham Bhardwaj
Affiliation: SOKENDAI 4th year (D2) (Supervisor: Maria Dainotti, Nozomu Tominaga, Kazunari Iwasaki)
Title: GRB Redshift Estimation Using Machine Learning

Facilitator
-Name:Matsuda, Graduate Student Affairs Unit

=============== January 31 Wed==============

Campus: Mitaka
Seminar: NAOJ Science Colloquium
Date and time: 2023 Jan. 31 (Wed.), 15:30-16:30
Place: the 3F seminar room in Instrument Development Building No.3 / Zoom (hybrid)

Speaker: Shun Hatano
Affiliation: NAOJ (M2)
Title: Origin of high-ionization lines found in extremely metal poor galaxies.
Abstract:
The extreme metal poor galaxies (EMPG) exhibit intense high-ionization emission lines, such as He II4686, unexplained by stellar synthesis models. Umeda et al. (2022) employed CLOUDY and MCMC to reproduce the observed spectrum, revealing an unidentified non-thermal radiation source. In this study, we introduce [Ne V]3426 emission (97.1 eV) and estimate spectral indices and luminosities for EMPGs in the 54.4-97.1 eV range. Confirming that non-thermal radiation dominates the 54.4-97.1 eV range for all the galaxies with [Ne V]3426 detections, we discuss the origin of the non-thermal radiation.

Speaker: Ryota Hatami
Affiliation: NAOJ (M1)
Title: Synthesis of Sc, Ti, and V in core-collapse supernovae
Abstract:
A supernova explosion is an explosive phenomenon that occurs at the end of the life of a massive star. However, the explosion mechanism has not yet been clarified. As a clue to investigate the explosion mechanism, we focused on nucleosynthesis. Metal-poor stars reflect the result of explosive nucleosynthesis in supernova explosions of first stars, and reproducing the chemical abundances of metal-poor stars is one of the important issues in the nucleosynthetic calculation. Recently correlations among Sc, Ti, and V are observationally identified.
Nevertheless, the abundances of Sc, Ti, and V in metal-poor stars have not been reproduced by nucleosynthesis calculations based on the results of hydrodynamical simulation. This is because one of the possible causes is that the explosion mechanism is not yet understood. Then, we attempted to constrain the explosion mechanism by (1) performing nucleosynthesis calculations with setting temperature, density, neutrino flux, etc. as parameters to find physical conditions which reproduce the observed chemical composition of metal-poor stars, and (2) examining the feasibility of these conditions by comparing them with 2D explosion simulations. In this talk, the progress of (1) and (2) will be discussed.

Facilitator
-Name: Masamitsu Mori

Comment: English

=============== February 1 Thu==============

キャンパス:三鷹 野辺山 水沢 岡山 ハワイ
セミナー名:Tea Talk
定例・臨時の別:臨時
日時:2/1(木)14:00~15:00
場所:Zoom
講演者:平松 正顕
所属:天文情報センター周波数資源保護室
タイトル:世界無線通信会議とドバイ4週間の旅
言語:日本語(PPTは英語も併記)

世話人の連絡先:
-名前:藤田登起子

備考:
参加方法:Zoom

2024.1.22-2024.1.28

January 23 Tue 10:00-11:30 太陽系小天体セミナー
Zoom


January 24 Wed 10:30-12:00 SOKENDAI Colloquium
Large Seminar Room in Subaru Building and Zoom (hybrid)


January 24 Wed 13:00-15:00 SOKENDAI Doctoral Thesis Dissertation review
Lecture Room and Zoom (hybrid)


January 24 Wed 13:30-15:00 Solar and Space Plasma Seminar
Insei Seminar Room and Zoom(hybrid)


January 24 Wed 14:30-15:30 ALMA-J seminar
Room 102 in the ALMA Building and Zoom (hybrid)


January 24 Wed 15:30-16:30 NAOJ Science Colloquium
the 3F seminar room in Instrument Development Building No.3 and Zoom (hybrid)


詳細は下記からご覧ください。

=============== January 23 Tue ===============

キャンパス:三鷹
セミナー名:太陽系小天体セミナー
定例・臨時の別:定例
日時:1月23日(火曜日)10時00分~11時30分
場所:zoom
講演者:匠あさみ

世話人の連絡先
 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

=============== January 24 Wed ===============

Campus:Mitaka
Seminar:SOKENDAI Colloquium
Regularly Scheduled/Sporadic:Regular
Date and time:January 24, 2024 10:30-12:00
Place:Large Seminar Room in Subaru Building and Zoom

Speaker: Takumi Kakimoto
Affiliation: SOKENDAI 2nd year (M2) (Supervisor: Masayuki Tanaka, Daisuke Iono, Kiyoto Yabe)
Title: Star formation activity in a massive protocluster at z=4.5

Speaker: Chanoul Seo
Affiliation: SOKENDAI 5th year (D3) (Supervisor: Yuka Fujii, Masahiro Ikoma, Hideko Nomura)
Title: Impact of Magma Redox States on Super-Earth Atmospheres:Unveiling the Connection with Atmospheric Composition

Facilitator
-Name:Matsuda, Graduate Student Affairs Unit

=============== January 24 Wed===============

Campus:Mitaka
Seminar:SOKENDAI Doctoral Thesis Dissertation review
    総研大博士学位論文予備審査会
Regularly Scheduled/Sporadic:Sporadic
Date and time:January 24, 2024 13:00-15:00
Place :Lecture Room and Zoom

Speaker:Takaho Masai
Title:A Study on the Design of Receiver Optics and Waveguide Components Towards High-Performance (Sub)millimeter Wave Multibeam Receivers

Facilitator
-Name:Nozomu Tominaga, Hideyuki Kobayashi, Kaya Kitabayashi (Graduate Student Affairs Unit)

Comment:
https://guas-astronomy.jp/CampusLife/doctor_report.html

=============== January 24 Wed==============

Campus: Mitaka
Seminar: Solar and Space Plasma Seminar
Regularly Scheduled/Sporadic: Sporadic
Date and time:24 January (Wed), 13:30-15:00
Place: hybrid; Insei Seminar Room and Zoom

Speaker:Dr. Yoichiro Hanaoka
Affiliation:NAOJ
Title:Observation of the White-Light Corona at Total Solar Eclipses (Focusing
on Polarization Measurements)
Abstract:Total solar eclipses are good chances to observe the inner white-light corona under a very low background level. Combining the eclipse data and those from spaceborne coronagraphs such as SOHO/LASCO, we can obtain the distribution of the coronal material regardless of the temperature from just above the limb to tens of solar radii.
For this purpose, we carried out eclipse observations several times with amateur observers using polarimetry instruments. Polarimetry is indispensable to separate the K-corona (million-kelvin plasma) from the F-corona (interplanetary dust), and therefore, all the spaceborne coronagraphs have polarimetric capacity.
The results from the eclipses unexpectedly show a systematic difference between the polarimetry results obtained during the eclipses and those by LASCO. The degree of polarization obtained by LASCO is about 30 % less than the eclipse results and it was revealed that combining the eclipse and LASCO data is difficult. This result suggests that the polarimetric calibration of LASCO should be re-examined.
Some future space missions carrying white-light coronagraphs are planned, and they may also have difficulty in polarimetric calibrations. Repeated eclipse observations are expected to provide good calibration data for space coronagraphs. After a consistent calibration becomes possible, the precise distribution of coronal material in the wide range will be obtained.

Facilitator
-Name:Akiko Tei

Comment:English

=============== January 24 Wed==============

Campus: Mitaka
Seminar: ALMA-J seminar
Date and time: January 24 (Wed) 14:30-15:30
Place: hybrid (Room 102 in the ALMA building and Zoom)

Speaker: Kianhong Lee
Affiliation: Tohoku University
Title: ALMA [CII] observations of TN J0924-2201, the radio galaxy at z~5.2

Abstract:
High-redshift radio galaxies are massive star-forming galaxies with powerful radio jets, often located on or below the star-forming main sequence of galaxies, indicating that they are in the process of being quenched. TN J0924-2201 is one of the most distant known radio galaxies, associated with three CO(1-0)-detected companions at z~5.2. In this talk we will present ALMA observations of [CII] 158 um line and the corresponding 1-mm continuum emission of TN J0924-2201. While obtaining the [CII] line and 1mm continuum emission at the host galaxy, our observations revealed no detection at the positions of the three CO(1-0) companions. The derived systematic redshift z_[CII] of the host galaxy from the [CII] is ~5.17, indicating a velocity offset of ~1200 km/s with respect to z_Lya, marking the largest velocity offset between [CII] and Lya recorded at z > 5 to date. Within the host galaxy, we identified an extended [CII] structure with a velocity of ~700 km/s, suggestive of an outflow. This finding aligns with the shell outflow model, providing consistency with the observed large velocity offset of Lya. Assuming three massive CO(1-0) companions are also outflows, their velocities of ~1500 km/s surpass the escape velocity of a 10^13 Msun halo, implying the removal of molecular gas from the system of TN J0924-2201. Our observations and results revealed that we are witnessing a distinctive phase of radio galaxies in their evolution.

=============== January 24 Wed==============

Campus: Mitaka
Seminar: NAOJ Science Colloquium
Date and time: 2023 Jan. 24 (Wed.), 15:30-16:30
Place: the 3F seminar room in Instrument Development Building No.3 / Zoom (hybrid)

Speaker: Ryota Ichimura
Affiliation: NAOJ (D1)
Title: Carbon Isotope Fractionation of Complex Organic Molecules in Star-Forming Cores
Abstract:
Recent high-resolution and sensitivity ALMA observations have unveiled the carbon isotope ratios (12C/13C) of Complex Organic Molecules (COMs) in a low-mass protostellar source. To understand the 12C/13C ratios of COMs, we investigated the carbon isotopic fractionation of COMs from prestellar cores to protostellar cores with a gas-grain chemical network model. We confirmed that in the prestellar phase, the 12C/13C ratios of small molecules are bimodal: CO and species formed from CO (e.g.,CH3OH) are slightly enriched in 13C compared to the local ISM (by ∼ 10 %), while those from C and C+ are depleted in 13C owing to isotope exchange reactions. COMs are formed from the simple species on grain surface, and thus basically inherit the bimodality of 12C/13C. In the protostellar phase, COMs are formed on the grain surface and in the hot gas (> 100 K) and have different 12C/13C from those in the prestellar phase. We additionally incorporate reactions between gaseous atomic C and H2O ice or CO ice on the grain surface to form H2CO ice or C2O ice suggested by recent laboratory studies. The direct C-atom addition reactions open pathways to form 13C-enriched COMs from atomic C and CO ice. We find that these direct C-atom addition reactions mitigate isotope fractionation, and the model with the direct C-atom addition reactions better reproduces the observations than our base model. Our calculations also show that cosmic-ray ionization rates affect the 12C/13C ratios of COMs.

Speaker: Akifumi Matsumura
Affiliation: The University of Tokyo (M1)
Title: Estimating the characteristics of ejecta from magma ocean for water production on the protoplanet
Abstract:
How water is delivered to rocky planets during the planet-forming stage is a major issue in planetary science. While many previous studies considered water delivery by icy planetesimals, we consider water production by chemical interaction between the primordial atmosphere and the surface of the magma ocean of a rocky planet growing through planetesimal accretion. Previous studies based on this idea assumed that iron oxides in the magma ocean and atmospheric hydrogen are always in constant contact, which must be examined; namely, we need to consider properly how to bring the magma into contact with the atmosphere. In this study, we focus on the reaction between the atmospheric gas and the materials ejected from the magma ocean when planetesimals collide with the magma ocean surface during the growth phase of a planet. I am currently studying the scatter of magma upon the impact of planetesimals on the planet’s surface and its influence on the atmospheric composition. In this talk, I will describe our progress in the research to date and future research plans.

Facilitator
-Name: Kanji Mori

Comment: English

2024.1.15-2024.1.21

January 16 Tue 10:00-11:30 太陽系小天体セミナー
Zoom


January 17 Wed 10:30-12:00 SOKENDAI Colloquium
Large Seminar Room in Subaru Building and Zoom (hybrid)


January 17 Wed 14:30-15:30 ALMA-J seminar
Room 102 in the ALMA Building and Zoom (hybrid)


January 17 Wed 15:30-16:30 NAOJ Science Colloquium
Zoom


January 18 Thu 10:00-12:00 SOKENDAI Doctoral Thesis Dissertation review
Lecture Room and Zoom (hybrid)


January 18 Thu 15:30-17:30 SOKENDAI Doctoral Thesis Dissertation review
Lecture Room and Zoom (hybrid)


January 19 Fri 10:30-12:00 Solar and Space Plasma Seminar
Central Building (North) / 310 and Zoom (hybrid)


詳細は下記からご覧ください。

=============== January 16 Tue ===============

キャンパス:三鷹
セミナー名:太陽系小天体セミナー
定例・臨時の別:定例
日時:1月16日(火曜日)10時00分~11時30分
場所:zoom
講演者:宇田豊和
所属:Aiharasoft
タイトル:ハワイ・マウナケア星空ライブからの流星自動検出システム概要
Abstract:ハワイ・マウナケア星空ライブからの流れ星自動検出システムを構築しました。
2022年1月より、大きな流れ星を検出すると、Xでポストする運用を行っています。
今回の発表では、このシステムの概要、流れ星の検出アルゴリズム概要、
ふたご座流星群などの検出状況、現状の問題点、課題についてご説明します。

世話人の連絡先
 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

=============== January 17 Wed ===============

Campus:Mitaka
Seminar:SOKENDAI Colloquium
Regularly Scheduled/Sporadic:Regular
Date and time:January 17, 2024 10:30-12:00
Place:Large Seminar Room in Subaru Building and Zoom

Speaker: Kazuki Watanabe
Affiliation: SOKENDAI 1st year (M1) (Supervisor: Yoshinori Uzawa, Takafumi Kojima, Tai Oshima)
Title: Development of a sub-THz MKID Camera for Deep Space Observation

Speaker: Miho Tan
Affiliation: SOKENDAI 1st year (M1) (Supervisor: Mami Machida, Tomoya Takiwaki, Kazunari Iwasaki)
Title: Effect of an optical star wind on SS433’s jet propagation

Facilitator
-Name:Matsuda, Graduate Student Affairs Unit

=============== January 17 Wed===============

Campus: Mitaka
Seminar: ALMA-J seminar
Date and time: January 17 (Wed) 14:30-15:30
Place: hybrid (Room 102 in the ALMA building and Zoom)

1st speaker: Yuzuki Nagashima
Affiliation: Fukushima university / NAOJ
Title: High-precision SFR mapping of the nearby galaxy NGC 1068 using ALMA 100 GHz continuum and HST Paα line and the effect of DIG contamination.

Abstract:
The star formation rate (SFR) is an important indicator in the context of galaxy evolution. However, it is not easy to accurately measure the SFR in external galaxies. For example, the most common method is to use radiation from the HII region, but the to assume temperature of the HII region and the contribution of other radiation sources make it difficult to accurately estimate the SFR. Furthermore, in the infrared and optical wavelength bands, the effect of dust extinction is significant and needs to be corrected. Therefore, it is important to observe in the millimeter and sub-millimeter wavelength bands with ALMA, which are not affected to dust extinction, especially, which has high sensitivity and high resolution. In recent years, with the improvement of data accuracy, a method to isolate, identify, and extract whether the source of ionized gas is from star formation or not is being established. By identifying and subtracting stronger ionization sources (e.g., AGN origin) and weaker (Diffuse Ionized Gas; DIG origin) than star formation sources, SFRs that are less contradiction with SFRs derived from multiple tracers have been reported (e.g., Michiyama et al. 2020). Michiyama et al. 2020).
We produced a precise SFR map for the nearby galaxy NGC 1068 by comparing the two different ionized gas tracers, free-free emission and hydrogen recombination line the Paα, and by considering the effect of DIG.
In this talk, I will introduce how to make an accurate SFR map and the result.
In addition, I will focus on the DIG correction.

2nd speaker: Mahoshi Sawamura
Affiliation: University of Tokyo / NAOJ
Title: No galaxy-scale [CII] outflow detected in a z=6.72 red quasar with ALMA

Abstruct:
It has been claimed that active galactic nucleus (AGN)-driven massive outflows, which would happen during a transition phase from an obscured dusty quasar to a normal blue quasar, are the key physical process in driving the co-evolution of galaxies and supermassive black holes (SMBHs). Partially dust-obscured red quasars are thought to be the immediate phase of this transition. However, while many blue quasars at z = 6~7 have been found in recent years, it is still hard to identify red quasars at that epoch due to their apparent faintness. Deep, wide-area surveys and subsequent multi-wavelength follow-up observations are thus required to identify such red objects and test the above evolutionary scenario. Here we report our ALMA cycle 7 observations of the z = 6.72 red quasar HSC 120505.09−000027.9 (J1205−0000). This is one of the highest redshift (z > 6) red quasars originally identified by our deep Subaru Hyper Suprime-Cam (HSC) survey. It is apparently faint, but is intrinsically as luminous as −24.4 mag at rest-UV and hosts a massive BH of 2.2 × 10^9 Msun. It is also known to be N V and C IV BAL object, indicating the existence of nuclear outflows. We successfully detected both the [CII] 158 μm line and the underlying rest-FIR continuum emission (resolution ~0.6″, 1σ ~ 0.1 mJy/beam at dV = 75 km/s). The continuum is very bright, with the estimated luminosity of 2.3 × 10^12 Lsun (or equivalently SFR ~ 485 Msun/yr), which indicates that the host galaxy of this red quasar is indeed a starburst system. However, the detailed analysis of the visibility data suggests that the bulk of this IR emission originates from a spatially unresolved compact component, likely the AGN itself. Hence the actual SFR could be much smaller. Regarding the AGN feedback, our observations do not conclusively assert the presence of [CⅡ] outflows. One possible interpretation of this is that the spatial scale of the outflow is not large enough to reach the host galaxy. However, we propose that this red quasar is indeed in a key evolutionary phase of AGN feedback. We will also discuss possible future observations to explore the existence of this wing component.

=============== January 17 Wed==============

Campus: Mitaka
Seminar: NAOJ Science Colloquium
Date and time: 2023 Jan. 17 (Wed.), 15:30-16:30
Place: Zoom

Speaker: Bruce Gendre
Affiliation: Australian National University
Title: Progenitors of ultra-long gamma-ray bursts: an ultra-long and ultra-slow developing story
Abstract:
Gamma-ray bursts are fantastic explosions seen at cosmological distances, and one of the most extreme high energy events of the Universe. Because of their distance, understanding the phenomenon at play is challenging. In this seminar, I will review the GRB phenomenon, what we already know about the progenitor of those events, focusing on the most unknown kind of event, the ultra-long ones, and how we use the current technology for improving our knowledge.

Facilitator
-Name: Maria Giovanna Dainotti
Comment: English

=============== January 18 Thu==============

Campus:Mitaka
Seminar:SOKENDAI Doctoral Thesis Dissertation review
     総研大博士学位論文予備審査会
Regularly Scheduled/Sporadic:Sporadic
Date and time:January 18, 2024 10:00-12:00
Place :Lecture Room and Zoom

Speaker:Raiga Kashiwagi
Title:Instability and Evolution of Shocked Clouds Formed by Collisions between Filamentary Molecular Clouds

Facilitator
-Name:Nozomu Tominaga, Hideyuki Kobayashi, Kaya Kitabayashi (Graduate Student Affairs Unit)

Comment:
https://guas-astronomy.jp/CampusLife/doctor_report.html

=============== January 18 Thu==============

Campus:Mitaka
Seminar:SOKENDAI Doctoral Thesis Dissertation review
     総研大博士学位論文予備審査会
Regularly Scheduled/Sporadic:Sporadic
Date and time:January 18, 2024 15:30-17:30
Place :Lecture Room and Zoom

Speaker:Rikuto Omae
Title:Probing the Magnetic Fields of Distant Galaxies to Unravel the Evolution of Galactic Magnetic Fields

Facilitator
-Name:Nozomu Tominaga, Hideyuki Kobayashi, Kaya Kitabayashi (Graduate Student Affairs Unit)

Comment:
https://guas-astronomy.jp/CampusLife/doctor_report.html

=============== January 19 Fri==============

Campus: Mitaka
Seminar: Solar and Space Plasma Seminar
Regularly Scheduled/Sporadic: Sporadic
Date and time:19th January (Fri), 10:30-12:00
Place: hybrid; Central Building (North) / 310 and Zoom

Speaker:Dr. Ryoko Ishikawa
Affiliation:NAOJ
Title:3D mapping of the magnetic field in the whole atmosphere of an active region plage with the CLASP2.1 sounding rocket experiment
Abstract:Probing the magnetic field throughout the solar atmosphere is critically important for understanding the energy transfer from the photosphere to the corona. However, there is an overwhelming lack of empirical information on the magnetic field in the upper chromosphere and the layers above, where the magnetic pressure dominates the gas pressure (β < 1). To this end, a novel approach is to measure and model the polarization of magnetically-sensitive ultraviolet (UV) spectral lines. The series of sounding rocket experiments CLASP (2015), CLASP2 (2019) and CLASP2.1 (2021) have demonstrated that UV spectro-polarimetry is indeed a suitable diagnostic tool for investigating the magnetic fields in the whole solar chromosphere. On October 8, 2021, CLASP2.1 measured the Stokes profiles of the 280 nm spectral region at 16 consecutive slit positions covering a two-dimensional field of view in an active region plage. This near-UV spectral region contains the resonance lines of Mn I (which provide information on the lower chromosphere) and the Mg II h & k lines (which provide information on the middle and upper chromosphere). Combined with coordinated observations with the Solar Optical Telescope (SOT) aboard the Hinode satellite, we obtained a line-of-sight magnetogram covering a sunspot penumbra and a plage (moss) region at multiple heights from the photosphere to the top chromosphere. The 3D mapping enables how the magnetic patches expand with height and how much magnetic flux reaches higher in the chromosphere. The obtained magnetogram is compared with the high-resolution images recorded by IRIS and SDO/AIA, revealing the connectivity between the magnetic structure in the chromosphere and the coronal loops.

Facilitator
-Name:Akiko Tei

Comment:English

2024.1.8-2024.1.14

January 9 Tue 14:00-15:00 NAOJ Seminar
Face to face/ hybrid; Large Seminar Room in Subaru Building

If this NAOJ seminar is held also by hybrid form,
we will announce the Zoom URL with another email.


January 10 Wed 10:30-12:00 SOKENDAI Colloquium
Large Seminar Room in Subaru Building and Zoom (hybrid)


January 10 Wed 15:30-16:30 NAOJ Science Colloquium
Large Seminar Room in Subaru Building and Zoom (hybrid)


詳細は下記からご覧ください。

=============== January 9 Tue ===============

Campus:Mitaka
Seminar:NAOJ Seminar
Regularly Scheduled/Sporadic:Sporadic
Date and time:January 9, 2024 14:00-15:00
Place:Large Seminar Room
*If this NAOJ seminar is held also by hybrid form, we will announce the Zoom URL with another email.

Speaker:Prof. Fabio Favata
Affiliation:Italian National Astronomy Institute (INAF) & Thalatta Consulting Ltd.
Title:Space astronomy, past and future: a personal (Western) perspective

Abstract:
Space astronomy is a fairly recent discipline, with the first successful space telescope (OAO-2, a 30 cm UV telescope) launched by NASA in 1968. While the first space telescopes were hardly larger than today’s amateur instruments, we have gone a long way to reach the Webb observatory, the largest space telescope ever launched. We have surely lived, in the past few decades, through a “golden age” of space astronomy, that has enabled discoveries that have changed our understanding of physics and of the Universe (e.g., the existence of dark energy, or the accurate cosmological models enabled by the CMB maps).

This unprecedented success story has been made possible by a number of circumstances which may not extend into the future, at least in the US and in Europe. While many astronomers take further significant progress in the development of space facilities for granted, in fact reality is likely to be more complex. The development of new large facilities by both NASA and ESA has met a number of challenges, both politically and technically. In addition, the time elapsed from the initial scientific idea to its fruition through the results of an actual space mission has become rather long. It is not obvious that the same approach and vision that has served space astronomy so well in the past will be successful in the future, and the golden age risks to be followed by an era in which the pace of progress slows significantly.

In my talk I discuss how and why have we come to this point, what are the risks for the future, in particular for the younger generation of scientists, and I will discuss new opportunities and possible solutions. Key elements include the importance of a diverse ecosystem of scientific ideas and facilities, of the new space ecosystem, as well as the growing, critical role in this field played by space actors in Asia.

Facilitator
-Name: Hori Yasunori

=============== January 10 wed===============

Campus:Mitaka
Seminar:SOKENDAI Colloquium
Regularly Scheduled/Sporadic:Regular
Date and time:January 10, 2024 10:30-12:00
Place:Large Seminar Room in Subaru Building and Zoom

Speaker: Kiyoaki Doi
Affiliation: SOKENDAI 4th year (D2) (Supervisor: Akimasa Kataoka, Hideko Nomura, Misato Fukagawa)
Title: Multi-wavelength ALMA observations of the PDS 70 disk with planets

Speaker: Suzuka Nakano
Affiliation: SOKENDAI 55h year (D3) (Supervisor: Koichiro Nakanishi, Takashi Sekii, Takuma Izumi)
Title: TBA

Facilitator
-Name:Matsuda, Graduate Student Affairs Unit

=============== January 10 wed==============

Campus: Mitaka
Seminar: NAOJ Science Colloquium
Date and time: 2023 Jan. 10 (Wed.), 15:30-16:30
Place: the large seminar room / Zoom (hybrid)

Speaker: Go Murakami
Affiliation: JAXA
Title: Ultraviolet Spectroscopy and Imaging in Solar System Science and Beyond
Abstract:
Ultraviolet spectroscopy technique is one of the most powerful tools for solar-terrestrial plasma physics, planetary science, and astronomy.
For example, JAXA’s UV space telescope Hisaki performed long-term and continuous monitoring of Io plasma torus and revealed dynamic relations between Io’s volcanic activity and Jupiter’s magnetosphere. We also developed a UV spectrograph for planetary exploration probes such as BepiColombo, ESA-JAXA joint Mercury exploration mission. Now we are studying a concept and preliminary design of future UV spectroscopy mission LAPYUTA. Here I present overviews of our past UV observation heritages such as Kaguya, BepiColombo, and Hisaki, brief instrumentations, current developments, and future plans.

Facilitator
-Name: Yuka Fujii
Comment: English