Home > ALMA Jセミナー | 太陽系小天体セミナー | 科学研究部コロキウム > 2021.7.19-2021.7.25


Jul 20 Tue 10:00~11:30  太陽系小天体セミナー / Solar System Minor Body Seminar zoom

Jul 21 Wed 15:00 ~16:00 ALMA-J seminar           zoom

Jul 21 Wed 15:30~17:00  NAOJ Science Colloquium      zoom






Campus: Mitaka
Seminar: ALMA-J seminar
Regularly Scheduled/Sporadic: Every Wednesday Date and Time: 2021 July 21 15:00-16:00
Place: Zoom
Speaker:Jorge Zavala (NAOJ)
Title: The IR luminosity function and dust-obscured star formation up to z~7
Abstract: The majority of the star formation activity in the Universe during the past 10-11Gyr, back to z~2.5, is primarily enshrouded by dust. However, although the history of cosmic star-formation has been thoroughly mapped at UV/optical wavelengths out to z~11, FIR/submm surveys have not kept apace. Consequently, the total amount of star formation that is absorbed and re-emitted by dust at high redshifts remains highly uncertain. During this talk, I will introduce the Mapping Obscuration to Reionization ALMA (MORA) Survey, the first interferometric blind map at 2mm with a total area of ~180 sq. arcmin. By combining our new 2mm number counts with the state-of-the-art galaxy number counts at other wavelengths, we place constraints on the evolution of the IRLF and dust-obscured star formation up to z~7. Does dust-obscured star formation still dominate during the early Universe? Our best answer to this question will be presented.

Facilitator: Yoshito Shimajiri, Shun Ishii


Seminar:NAOJ Science Colloquium
Regularly Scheduled/Sporadic:Every Wednesday
Date and time:2021 July 21, 15:30-17:00
Speaker:Michiko Fujii
Affiliation:The University of Tokyo
Title:Dynamical structures of the Milky-Way disk
Abstract:Gaia, an astrometry satellite, has dramatically updated the dynamical structures of the Milky-Way galaxies. However, the information that we can obtain from observations is limited in terms of both time and space. We can observe only the current positions and velocities of stars within a few kpc from the Sun. On the other hand, simulations provide us the entire time evolution of modeled galaxies.
We performed fully self-consistent N-body simulations of disk galaxies modeling the Milky Way. We model galactic disk, bulge, and dark matter halo as N-body systems with a maximum of 8 billion particles using the same mass resolution to avoid numerical heating. Our high-resolution simulation allows us to follow the individual orbits of stars trapped in the bar’s inner Lindblad resonances. Such resonant orbits explain observed structures in the distribution of stars in the phase space. I will also talk about the transient spiral structures of disk galaxies.
-Name:Akimasa Kataoka

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