IoA_Seminar

 

講演リスト

No. 388: 28 July 2022 (Thu) 15:30 - 16:30

Speaker: 細川 隆史(京都大学)

Title: High-mass star formation in the early universe and their analogous observational signatures in the present-day universe

Language: English

Abstract: I present our recent efforts toward understanding the high-mass star formation across cosmic history. The extreme case is the Pop III star formation, for which we have continuously conducted multi-dimensional radiation-hydrodynamic simulations for a decade. Our latest updates allow us to study the evolution in the protostellar accretion stage, where the fragmentation of the star-forming gas and radiative feedback from accreting protostars operate in concert. Whereas simulations reveal the Pop III star formation in great detail, directly detecting it is beyond the abilities of upcoming observational facilities. An alternative way is searching for observational signatures of the nearby analogues in their formation stage. One of such candidates is young massive clusters containing many metal-poor high-mass stars. I also present our ongoing study to extract their possible observational signatures based on numerical simulation results.

No. 387: 21 July 2022 (Thu) 15:30 - 16:30

Speaker: Mason Leist (University of Texas San Antonio)

Title: Resolving Polar Dust in AGN with JWST: Going Beyond the PSF

Language: English

Abstract: The launch of the James Webb Space Telescope (JWST) promises to revolutionize infrared astronomy and our understanding of inflows and outflows in active galactic nuclei (AGN). David Rosario (Newcastle University, U.K.) has been awarded JWST science time to explore and characterize diffuse polar dust emission found in AGN using JWST Mid-infrared Instrument (MIRI) imaging. The Galactic Activity, Torus and Outflow Survey (GATOS2) collaboration will have access to these data, of which I am a member. Thanks to JWST’s exquisite low surface brightness sensitivity in the mid-infrared (MIR; 5-25 μm) observations of the diffuse polar dust emission found in AGN will be enabled unprecedented sensitivity. Relying on JWST’s stable PSF, we plan to use deconvolution to establish the structure of this diffuse emission below the resolution of the telescope. We will explore five different deconvolution techniques and select the best method based on comparisons of the flux conservation, FWHM, and Strehl ratios of the deconvolved images with an input model. To explore each technique, we have used the MIRI simulation software (MIRISim) to simulate JWST’s complex PSF convolved with a toy model of an AGN consisting of a resolved bicone and an unresolved AGN point source. Here I discuss the preliminary results on our assessment of the optimum deconvolution strategy.

No. 386: 12 July 2022 (Tue) 16:15 - 17:15

Speaker: Yutaro Kofuji(Department of Astronomy, The University of Tokyo)

Title: Imaging of the Supermassive Black Hole in Our Galaxy, Sgr A* with the Event Horizon Telescope

Language: English

Abstract: The first event horizon scale image of the supermassive black hole in our Galaxy, Sgr A* was captured by the Event Horizon Telescope(EHT) Collaboration. EHT is the Very Long Baseline Interferometry (VLBI) that links radio dishes around the world to create an Earth-sized telescope virtually. High-resolution observations of EHT enable us to see the vicinity of the black hole. We analyzed the reconstructed images and concluded that it is highly likely that Sgr A* has ~50 uas ring structure and this is consistent with the shadow of the Kerr black hole which weighs ~4 million solar masses. In this seminar, I would like to summarize the major results, then explain the details of our imaging process and briefly introduce the theoretical interpretations of our images.

No. 385: 7 July 2022 (Thu) 15:30 - 16:30

Speaker: Dr. Paul Hertz (NASA Astrophysics Division Director)

Title: NASA Astrophysics: From the past to the future

No. 384: 5 July 2022 (Tue) 16:15 - 17:15

Speaker: 伊藤 慧(東京大学天文学教室)

Title: Environment and AGN activity of distant quiescent galaxies revealed by multi-wavelength surveys in the COSMOS field

No. 383: 21 June 2022 (Tue) 16:15 - 17:15

Speaker: Paul K. H. Yeung(東京大学物理学教室)

Title: Cosmic-ray Acceleration & Escape from Intermediate-Aged Supernova Remnant Kes 79

No. 382: 6 June 2022 (Thu) 15:30 - 16:30

Speaker: 堀内 貴史(東京大学天文学教育研究センター)

Title: Evaluation of magnitudes of the Starlink satellites by simultaneous multicolor observations

Language: English

Abstract: The U.S. company, SpaceX plans to launch 42,000 Starlink satellites by the mid-2020s. However, these satellites orbit at relatively low altitudes (e.g. 550 km), and there are concerns that the light pollution from sunlight reflection likely affects observations. In January 2020, SpaceX launched a test satellite, Darksat with a black coating on its surface to reduce the reflection flux. In order to verify the effect of its black coating, we observed Darksat and unpainted Starlink satellites by simultaneous multicolor observations (g’: green, Rc: red, and Ic: near-infrared) with the 105 cm Murikabushi telescope/MITSuME. While the magnitude of Darksat is about 7, being difficult to see with the naked eyes, this brightness is sufficient to affect any observations. In June 2020, SpaceX launched Visorsat, which is a satellite with a sun visor to reduce the reflected sunlight. At the present stage, there is no sufficient verification on whether the sun visor is effective at various wavelengths. In this study, we are therefore conducting the simultaneous multicolor observations of Visorsat and the ordinary Starlink satellites through the OISTER campaign. The preliminary observations of Visorsat with the Murikabushi telescope have already shown that the apparent magnitude of Visorsat is not fainter than that of Darksat, ranging from 6.5 mag (g' band) to 5.7 mag (Ic band). Since most of the satellites to be launched by SpaceX in the future will be visor satellites, it is very important to investigate the effects of the Starlink satellites as soon as possible to reduce the light pollution in astronomical observations.

No. 381: 10 May 2022 (Tue) 16:15 - 17:15

Speaker: 西村優里(東京大学天文学教室) / Yuri Nishimura (University of Tokyo, Department of Astronomy)

Title: Molecular spectroscopy in local and high-redshift galaxies: What do "dense gas tracers" mean?

Language: Japanese

Abstract: Thanks to the technical advancement of (sub)millimeter observing facilities, a great number of molecular lines are now routinely observed with high sensitivity and high angular resolution. These molecular lines and line ratios are useful tools for studying physical, kinematic, and chemical properties of extragalactic systems. To fully exploit line diagnostics, it is important to relate different size scale observations: detailed understanding of nearby systems by spatially-resolved observations is essential to better interpretation of more distant objects which cannot be observed at the same physical resolution. In this talk, I will present (1) 10 pc-scale multiline mapping toward a Galactic star-forming region W3(OH); (2) spatially- and spectrally-resolved HCN and HCO+ observations of local (ultra)luminous infrared galaxies from the CONquest sample (for more detail on CONquest, see Falstad+2021); and (3) ALMA Band 3 (rest-frame ~350 GHz) line survey toward the Cloverleaf, a gravitationally-lensed quasar at z=2.56. I will first discuss which molecular emission arises from which part of the molecular cloud, and then focus on how galactic-scale dynamics, such as outflows, can alter line ratios.


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