A5103257298- Astrophysics and Star Formation Studies
- Galaxies: Formation, Evolution, Phenomena
- Stellar, planetary, and galactic studies
- Astronomy and Astrophysical Research
- Astrophysical Phenomena and Observations
- Impact of Light on Environment and Health
- Astro and Planetary Science
- Cosmology and Gravitation Theories
- Gamma-ray bursts and supernovae
Nagoya University
2013-2022
Kavli Institute for the Physics and Mathematics of the Universe
2014
The University of Tokyo
2014
Institute of Astronomy and Astrophysics, Academia Sinica
2014
This paper analyses the behaviour of gas-to-dust mass ratio (G/D) local Universe galaxies over a large metallicity range. We combine three samples: Dwarf Galaxy Survey, KINGFISH survey and subsample from Galametz et al. (2011) totalling 126 galaxies, covering 2 dex range, with 30% sample 12+log(O/H) < 8.0. The dust masses are homogeneously determined semi-empirical model, including submm constraints. atomic molecular gas compiled literature. Two XCO used to estimate masses: Galactic XCO,...
This paper investigate what is the main driver of dust mass growth in interstellar medium (ISM) by using a chemical evolution model galaxy with metals (elements heavier than helium) phase addition to total amount metals. We consider asymptotic giant branch (AGB) stars, type II supernovae (SNe II) and ISM as sources dust, SN shocks destruction mechanism dust. Further, describe precisely, our takes into account age metallicity (the ratio metal mass) dependence particularly focused on growth,...
We construct a dust evolution model taking into account the grain size distribution, and investigate what kind of processes determine distribution at each stage galaxy evolution. In addition to production by type II supernovae (SNeII) asymptotic giant branch (AGB) stars, we consider three in ISM: (i) destruction SN shocks, (ii) metal accretion onto surface preexisting grains cold neutral medium (CNM) (called growth), (iii) grain-grain collisions (shattering coagulation) warm (WNM) CNM. found...
Abstract We present the Atacama Large Millimeter/submillimeter Array detection of [O iii ] 88 μ m line and rest-frame 90 dust continuum emission in a Y -dropout Lyman break galaxy (LBG), MACS0416_Y1 lying behind Frontier Field cluster MACS J0416.1−2403. This confirms LBG with spectroscopic redshift z = 8.3118 ± 0.0003, making this object one farthest galaxies ever identified spectroscopically. The observed 850 flux density 137 26 Jy corresponds to de-lensed total infrared (IR) luminosity...
Polycyclic aromatic hydrocarbons (PAHs) are some of the major dust components in interstellar medium (ISM). We present our evolution models for abundance PAHs ISM on a galaxy-evolution timescale. consider shattering carbonaceous grains turbulence as formation mechanism while PAH can be reduced by coagulation onto grains, destruction supernova shocks, and incorporation into stars. implement these processes one-zone chemical model to obtain galaxy. find that becomes accelerated above certain...
We investigate the evolution of extinction curves in galaxies based on our model grain-size distribution. In this model, we considered various processes: dust formation by Type II supernovae and asymptotic giant branch stars, destruction supernova shocks interstellar medium, metal accretion onto surface grains (referred to as grain growth), shattering coagulation. find that curve is flat earliest stage galaxy evolution. As enriched with dust, becomes effective, producing a large abundance...
Abstract The discoveries of huge amounts dust and unusual extinction curves in high-redshift quasars (z ≳ 4) cast challenging issues on the origin properties early Universe. In this Letter, we investigate evolutions content curve a high-z quasar, based evolution model taking account grain size distribution. First, show that Milky Way is reproduced by introducing moderate fraction (≃0.2) dense molecular-cloud phases interstellar medium for graphite–silicate model. Then peculiar can be...
The spectral energy distribution (SED) of galaxies provides fundamental information on the related physical processes. However, SED is significantly affected by dust in its interstellar medium. Dust mainly produced asymptotic giant branch stars and Type II supernovae. In addition, mass increases through metal accretion, grain size changes collisions between grains. contribution each process extinction depend distribution. Therefore, model should treat evolution spite importance evolution,...
Polycyclic aromatic hydrocarbons (PAHs) are one of the major dust components in interstellar medium (ISM).We present our model calculations for PAH abundance ISM on a galaxy-evolution timescale.We consider shattering carbonaceous grains as formation mechanism PAHs while is reduced by coagulation onto grains, destruction supernova shocks, and injection into star formation.We implement these processes an one-zone chemical evolution to obtain galaxy.We find that becomes accelerated at certain...
Abstract Recently huge amount of dust M ≃ 10 6−7 ⊙ in galaxies at z = 7–8 has been discovered by ALMA observations. The suggested timescale the production was a few–several×10 8 yr, while stellar mass several × 9 . This cannot be easily explained only supply from supernovae if we consider destruction reverse shocks. We propose that these values can consistently take into account grain growth interstellar medium (ISM). scenario successfully reproduces evolution mass, as well SFR, and...
Abstract We present ALMA detection of the [O iii ] 88 μ m line and 850 dust continuum emission in a Y -dropout Lyman break galaxy, MACS0416_Y1. The confirms object with spectroscopic redshift to be z = 8.3118±0.0003. intensity (0.14 mJy) implies large mass on order 4×10 6 M ⊙ . ultraviolet-to-far infrared spectral energy distribution modeling, where emissivity model is incorporated, suggests presence young (τ age ≍ 4 Myr), star-forming (SFR 60 yr −1 ), moderately metal-polluted ( Z 0.2 )...
Abstract The spectral energy distribution (SED) model should treat the evolution of a galaxy from its birth. Dust in galaxies affects formation and various ways. For example, dust grains scatter absorb stellar emitted ultraviolet (UV) photons re-emit radiation at infrared (IR) wavelengths. In this work, we construct SED based on our (Asano et al. 2013a,b, 2014) with rigorous treatment chemical evolution. To reduce computational cost, adopt mega-grain approximation (MGA; Inoue, 2005). MGA...