Subaru Seminars are
usually held in Room 104 of the Hilo Base Facility, adjacent
to the main lobby. Everyone is welcome to attend. If you would like to
give a seminar, please contact Subaru seminar organizers
(Thayne Currie, Tae-Soo Pyo, Nagayoshi Ohashi)
by email : sseminar_at_subaru.naoj.org (please change"_at" to @).
May 1, Monday, 11am in 104B
Metallicity is one of the most fundamental properties of galaxies. It reflects star formation history and gas flows of galaxies. In this seminar, we will talk about our study on chemical evolution of galaxies near and far. We attempt to extract information about star formation and gas flows of dwarf galaxies in the Local Group and distant star-forming galaxies by comparing the observational data with simple chemical evolution models. The results on dwarf galaxies suggest that more massive galaxies may have (i) higher star formation rate and/or (ii) lower outflow rate. On the other hand, our results on more massive distant star-forming galaxies
show that more massive galaxies may have (i) lower star formation rate and/or (ii) higher outflow rate. We will discuss the results and our interpretations.
April 12, Wednesday, 11:30am in 104B
Star-forming activity and ISM conditions of the [OIII]-selected galaxies before the peak epoch "
We focus on the epoch of z=3-3.6, which corresponds to 1-2 Gyr before the highest peak of the galaxy formation and evolution, i.e. z~2. Our final goal is to reveal what physical processes are involved in the increasing star formation rates in the universe towards z~2.
We have constructed samples of star-forming galaxies at z > 3 by the NB imaging surveys, namely Mahalo-Subaru (Kodama et al. 2013) and HiZELS (Best et al. 2013). At z>3, the Halpha emission line is no longer accessible from the ground, and we try to use the [OIII]λ5007 emission line as a tracer of star-forming galaxies at this epoch. We investigate the star-forming activity and the interstellar medium (ISM) conditions of the [OIII]-selected galaxies using the photometric and spectroscopic data and compare these quantities with those of the star-forming galaxies at the peak epoch. Our results suggest that the star-forming activity and the ISM conditions do not strongly evolve since z~3.2 to z~2.2 and that the stellar masses are likely to determine the evolutionary stage of star-forming galaxies between the two epochs.
In this talk, I would like to introduce a series of our studies about the [OIII] emitters at z>3.
Seminars are also held at JAC,