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People > Research Fellow > Curriculum Vita
We (Yu-Hsiu Huang, Hiroyuki Hirashita, et al.) modeled dust evolution in Milky Way-like galaxies by post-processing the IllustrisTNG cosmological hydrodynamical simulations in order to predict dust-to-gas ratios and grain size distributions.
Dust properties predicted in a cosmological simulation
Based on a one-zone evolution model of grain size distribution in a galaxy, we (Hirashita et al. 2020) calculated the evolution of infrared spectral energy distribution (SED), considering silicate, carbonaceous dust, and polycyclic aromatic hydrocarbons (PAHs).
Evolution of grain size distribution in the interstellar medium
We post-processed our cosmological hydrodynamic simulation with a simple dust emission model and calculated the infrared luminosity functions at redshifts z = 1–4 (Aoyama et al. 2019). We compare the calculated infrared (dust-emission) luminosity functions with the data points derived from the JCMT large project in our institute (PI: Wei-Hao Wang; Lim et al., in preparation). We broadly reproduced the observation data. The excess of the observational data points at extremely bright IR luminosity could be reproduced if we include additional heating by active galactic nuclei (AGNs).
Comparison with submillimeter galaxy surveys
Distribution of molecular gas surface density
Simulation of dust and molecules in a disk galaxy
Molecular gas is considered to trace star formation activity in galaxies. We calculated the distribution of hydrogen molecules (H2) in a galactic disk based on our hydrodynamical simulation (Chen, Hirashita, et al. 2018). Since H2 forms on dust grains, it is important to calculate the evolution of dust abundance in the simulation. The figure shows the H2 distribution at various ages (0.3, 1, 5, and 10 giga-year; Gyr). The galaxy is enriched with dust as time passes; that is, an older galaxy is richer in dust content. Accordingly, the system is rich in H2 at old ages. Since H2 traces dense regions where stars form at old (> 1 Gyr) ages, H2 is a good tracer of star formation unless the galaxy is younger than 1 Gyr. In other words, we find that molecular gas is not a good tracer of star formation in young galaxies.
Simulation of molecular gas distribution in a galactic disk
We simulated the evolution of a spiral galaxy with N-body/SPH (Aoyama, Hou, Hirashita, et al. 2017). We implemented the evolution of dust in the simulation. This figure shows the face-on view of the surface densities of small grains (left-hand column) and large grains (right-hand column) at t = 1 and 5 Gyr (top to bottom). We observe that at 1 Gyr, the stellar dust production is still important, which predicts much more large grains than small grains. At 5 Gyr, interstellar processing of dust (especially, dust disruption by shattering and dust growth by accretion) makes the enhancement of small grains. The results are consistent with the observed radial distribution of dust grains.
Dust evolution simulation in a spiral galaxy
The evolution of dust abundance relative to the total gas content calculated by the theoretical models developed by Kuo & Hirashita (2012, MNRAS, 432, 637). The horizontal axis shows the time sequence (precisely, the oxygen abundance 12+log(O/H)). The vertical axis show the dust abundance (dust-to-gas ratio). We examine two cases: without and with small (< 0.1 μm) dust grains. Without small grains (i.e., only with large grains), the rapid increase of dust abundance due to dust growth comes later, failing to explain the observationally acceptable range (blue box) for the distant quasars. With small grains, the rapid increase of the dust abundance by dust growth occurs earlier, and the line successfully pass through the observational range (blue box), which means that we can successfully explain the dust abundance observed in the quasars. The purple and blue curves show the model with and without small grains, respectively.
The evolution of dust abundance
The evolution of dust abundance relative to the total gas content calculated by the theoretical models developed by Tzu-Ming Kuo and me (Kuo & Hirashita 2012, MNRAS, 432, 637). The horizontal axis shows the time sequence (precisely, the oxygen abundance 12+log(O/H)). The vertical axis show the dust abundance (dust-to-gas ratio). We examine two cases: without and with small (< 0.1 μm) dust grains. Without small grains (i.e., only with large grains), the rapid increase of dust abundance due to dust growth comes later, failing to explain the observationally acceptable range (blue box) for the distant quasars. With small grains, the rapid increase of the dust abundance by dust growth occurs earlier, and the line successfully pass through the observational range (blue box), which means that we can successfully explain the dust abundance observed in the quasars.
Evolution of dust abundance
The figure above demonstrates how the dust-to-gas ratio in a galaxy evolves with increasing metallicity. In the low-metallicity regime, the dust is predominantly supplied by stars, so the dust-to-gas ratio increases in proportion to metallicity. Above a certain metallicity, the dust-to-gas ratio rapidly increases because the dust growth in the interstellar medium becomes more and more important, because interstellar dust growth occurs efficiently in metal-rich interstellar environments. The rapid increase is indeed consistent with the observational data of nearby galaxies.
Effects of grain size distribution on the interstellar dust mass growth
Simulated galaxy distribution. Each point corresponds to an individual galaxy, whose luminosity of dust emission at a submillimeter wavelength of 0.85mm is calculated individually. Therefore, the figure predicts the early Universe (z = 6) that ALMA would see. The larger a point is, the more luminous the galaxy is. The redder a point is, the larger fraction of energy is radiated in submillimeter. We only plot galaxies that are detectable by ALMA. The gray-scale shows the distribution of the dark matter, whose gravity attracts galaxies. From the figure, we see that ALMA can detect huge number of galaxies. We also find that "red" galaxies are the dominant population. Here, "red" means that a galaxy radiates more in the submillimeter than in the optical (so it is different from normal red). The existence of dust makes galaxies "redder", because dust absorbs optical light and emits submillimeter radiation. We emphasize that if the galaxies have "redder" colors, the importance of ALMA is more pronounced. Therefore, a lot of red points in the figure indicate that ALMA is really essential in observing the early Universe.
A simple approach to the high-redshift sub-millimeter galaxies
Hirashita, Hiroyuki
Research Fellow
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Office: ASMAB 1320
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Education and Positions

  • Research Fellow (ASIAA, Taiwan) (2014~present)
  • Associate Research Fellow (ASIAA, Taiwan) (2009~2014)
  • Visiting Assistant Research Fellow (ASIAA, Taiwan) (2008~2009)
  • Assistant Professor (Center for Computational Sciences, University of Tsukuba, Japan) (2005~2008)
  • Postdoctoral Fellow (SISSA, Italy) (2004~2005)
  • Postdoctoral Fellow of the Japan Society for the Promotion of Science for Young Scientists (Nagoya University, Japan) (2003~2005)
  • Postdoctoral Fellow of the Japan Society for the Promotion of Science for Research Abroad (Arcetri Observatory, Italy) (2001~2003)
  • Research Fellow of the Japan Society of the Promotion of Science for Young Scientists (1998~2001)
  • Department of Astronomy, Kyoto University, Japan (PhD) (1998~2001)
  • Department of Astronomy, Kyoto University, Japan (master's degree) (1996~1998)
  • Faculty of Science, Kyoto University, Japan (bachelor's degree) (1992~1996)

Research Interests

(1) Galaxy evolution and metal enrichment; (2) Far-infrared dust emission from galaxies; (3) Physics of dust

Journal Papers affiliated with ASIAA

  1. Otsuki M; Hirashita H, "Dust enrichment in the circum-galactic medium" , MNRAS: 528(3), 5008-5018, Mar, 2024 [SCI] ( ADS | Fulltext )
  2. Chiang ID; Hirashita H; Chastenet J; Koch EW; Leroy AK; Rosolowsky E; Sandstrom KM; Sardone A; Sun J; Williams TG, "Kpc-scale properties of dust temperature in terms of dust mass and star formation activity" , MNRAS: 520, 5506-5520, April, 2023 [SCI] ( ADS | Fulltext )
  3. Hirashita H, "Evolution of grain size distribution with enhanced abundance of small carbonaceous grains in galactic environments" , MNRAS: 518(3), 3827-3837, Jan, 2023 [SCI] ( ADS | Fulltext )
  4. Hirashita H, "Effects of dust grain size distribution on the abundances of CO and H2 in galaxy evolution" , MNRAS: 522(3), 4612-4625, July, 2023 [SCI] ( ADS | Fulltext )
  5. Hirashita H; Chen C-C, "Submillimetre galaxies as laboratories for dust grain coagulation" , MNRAS: 526(3), 4710-4717, Dec, 2023 [SCI] ( ADS | Fulltext )
  6. Hsu Y-M; Hirashita H; Lin Y-H; Camps P; Baes M, "Effects of dust sources on dust attenuation properties in IllustrisTNG galaxies at z 7" , MNRAS: 519(2), 2475-2485, Feb, 2023 [SCI] ( ADS | Fulltext )
  7. Abdurro'uf; Lin Y-T; Hirashita H; Morishita T; Tacchella S; Akiyama M; Takeuchi TT; Wu P-F, "Dissecting Nearby Galaxies with piXedfit. I. Spatially Resolved Properties of Stars, Dust, and Gas as Revealed by Panchromatic SED Fitting" , ApJ: 926(1), id.81 (27pp), Feb, 2022 [SCI] ( ADS | Fulltext )
  8. Abdurro'uf; Lin Y-T; Hirashita H; Morishita T; Tacchella S; Wu P-F; Akiyama M; Takeuchi TT, "Dissecting Nearby Galaxies with piXedfit. II. Spatially Resolved Scaling Relations among Stars, Dust, and Gas" , ApJ: 935(2), id.98 (21pp), Aug, 2022 [SCI] ( ADS | Fulltext )
  9. Chang C-Y; Huang Y-H; Hirashita H; Cooper Andrew P., "Dust spectral energy distributions in Milky Way-like galaxies in the IllustrisTNG simulations based on the evolution of grain size distribution" , MNRAS: 513(2), 2158–2167, June, 2022 [SCI] ( ADS | Fulltext )
  10. Chen YY; Hirashita H; Wang W-H; Nakai N, "A simple numerical experiment on the dust temperature bias for Lyman break galaxies at z≳5" , MNRAS: 509(2), 2258–2268, Jan, 2022 [SCI] ( ADS | Fulltext )
  11. Hirashita H; Chiang ID, "Analytic models of dust temperature in high-redshift galaxies" , MNRAS: 516(2), 1612-1623, Oct, 2022 [SCI] ( ADS | Fulltext )
  12. Hirashita H; Il'in VB, "Evolution of dust grain size distribution and grain porosity in galaxies" , MNRAS: 509(4), 5771-5789, Feb, 2022 [SCI] ( ADS | Fulltext )
  13. Makiya R; Hirashita H, "Cosmic evolution of grain size distribution in galaxies using the ν2GC semi-analytic model" , MNRAS: 517(2), pp.2076-2087, Dec, 2022 [SCI] ( ADS | Fulltext )
  14. Morishita T; Abdurro'uf; Hirashita H; Newman AB; Stiavelli M; Chiaberge M, "Compact Dust Emission in a Gravitationally Lensed Massive Quiescent Galaxy at z = 2.15 Revealed in 130 pc Resolution Observations by the Atacama Large Millimeter/submillimeter Array" , ApJ: 938(2), id.144 (10pp), Oct, 2022 [SCI] ( ADS | Fulltext )
  15. Relaño M; De Looze I; Saintonge A; K C; Hou; Romano LEC; Nagamine K; Hirashita H; Aoyama S; Lamperti I; Lisenfeld U; Smith MWL; Chastenet J; Xiao T; Gao Y; Sargent M; Van Der Giessen SA, "Dust grain size evolution in local galaxies: a comparison between observations and simulations" , MNRAS: 515(4), 5306-5334, Oct, 2022 [SCI] ( ADS | Fulltext )
  16. Romano LEC; Nagamine K; Hirashita H, "Dust diffusion in SPH simulations of an isolated galaxy" , MNRAS: 514(1), 1441-1460, July, 2022 [SCI] ( ADS | Fulltext )
  17. Romano LEC; Nagamine K; Hirashita H, "The co-evolution of molecular hydrogen and the grain size distribution in an isolated galaxy" , MNRAS: 514(1), 1461-1476, July, 2022 [SCI] ( ADS | Fulltext )
  18. Hirashita H; Il'in VB; Pagani L; Lefèvre C, "Evolution of dust porosity through coagulation and shattering in the interstellar medium" , MNRAS: 502(1), 15-31, Mar, 2021 [SCI] ( ADS | Fulltext )
  19. Hirashita H; Lan T-W, "Shattering as a source of small grains in the circum-galactic medium" , MNRAS: 505(2), 1794–1805, Aug, 2021 [SCI] ( ADS | Fulltext )
  20. Huang Y-H; Hirashita H; Hsu Y-H; Lin Y-T; Nelson D; Cooper AP, "Evolution of the grain size distribution in Milky Way-like galaxies in post-processed IllustrisTNG simulations" , MNRAS: 501(1), 1336-1351, Feb, 2021 [SCI] ( ADS | Fulltext )
  21. Lin Y-H; Hirashita H; Camps P; Baes M, "Geometry effects on dust attenuation curves with different grain sources at high redshift" , MNRAS: 507(2), 2755-2765, Oct, 2021 [SCI] ( ADS | Fulltext )
  22. Aoyama S; Hirashita H; Nagamine K, "Galaxy simulation with the evolution of grain size distribution" , MNRAS: 491(3), 3844-3859, Jan, 2020 [SCI] ( ADS | Fulltext )
  23. Burgarella D; Nanni A; Hirashita H; et al., "Observational and theoretical constraints on the formation and early evolution of the first dust grains in galaxies at 5 < z < 10" , A&A: 637, id.A32 (16pp.), May, 2020 [SCI] ( ADS | Fulltext )
  24. Hirashita H; Deng W; Murga MS, "Spectral energy distributions of dust and PAHs based on the evolution of grain size distribution in galaxies" , MNRAS: 499(2), 3046-3060, Oct, 2020 [SCI] ( ADS | Fulltext )
  25. Hirashita H; Hoang T, "Effects of rotational disruption on the evolution of grain size distribution in galaxies" , MNRAS: 494(1), 1058-1070, Apr, 2020 [SCI] ( ADS | Fulltext )
  26. Hirashita H; Lin C-Y, "Dust abundance and grain size in galaxy halos" , Planet Space Sci: 183, id.104504 (11pp.), Apr, 2020 [SCI] ( ADS | Fulltext )
  27. Hirashita H; Murga MS, "Self-consistent modelling of aromatic dust species and extinction curves in galaxy evolution" , MNRAS: 492(3), 3779-3793, Mar, 2020 [SCI] ( ADS | Fulltext )
  28. Nanni A; Burgarella D; Theulé P; Côté B; Hirashita H, "The gas, metal, and dust evolution in low-metallicity local and high-redshift galaxies" , A&A: 641, id.A168 (26pp), Sep, 2020 [SCI] ( ADS | Fulltext )
  29. Aoyama S; Hirashita H; Lim C-F; Chang YY; Wang W-H; et al., "Comparison of cosmological simulations and deep submillimetre galaxy surveys" , MNRAS: 484(2), 1852-1864, Apr, 2019 [SCI] ( ADS | Fulltext )
  30. Hirashita H; Aoyama S, "Remodelling the evolution of grain size distribution in galaxies" , MNRAS: 482(2), 2555-2572, Jan, 2019 [SCI] ( ADS | Fulltext )
  31. Hirashita H; Inoue AK, "Radiation-pressure-driven dust transport to galaxy haloes at z ∼ 10" , MNRAS: 487(1), 961-974, July, 2019 [SCI] ( ADS | Fulltext )
  32. Hou K-C; Aoyama S; Hirashita H; et al., "Dust scaling relations in a cosmological simulation" , MNRAS: 485(2), 1727-1744, May, 2019 [SCI] ( ADS | Fulltext )
  33. Liu H-M; Hirashita H, "Expected dust grain-size distributions in galaxies detected by ALMA at z > 7" , MNRAS: 490(1), 540-549, Nov, 2019 [SCI] ( ADS | Fulltext )
  34. Michałowski MJ; Hjorth J; Gall C; ...; Hirashita H; et al., "The fate of the interstellar medium in early-type galaxies. I. First direct measurement of the timescale of dust removal" , A&A: 632, id.A43 (11 pp.), Dec, 2019 [SCI] ( ADS | Fulltext )
  35. Rau S-J; Hirashita H;Murga M, "Modelling the evolution of PAH abundance in galaxies" , MNRAS: 489(4), 5218-5224, Nov, 2019 [SCI] ( ADS | Fulltext )
  36. Aoyama S; Hou K-C; Hirashita H; et al., "Cosmological simulation with dust formation and destruction" , MNRAS: 478(4), 4905-4921, Aug, 2018 [SCI] ( ADS | Fulltext )
  37. Chen L-H; Hirashita H; Hou K-C; et al., "Populating H2 and CO in galaxy simulation with dust evolution" , MNRAS: 474(2), 1545-1563, Feb, 2018 [SCI] ( ADS | Fulltext )
  38. Aoyama S; Hou K-C; Shimizu I; Hirashita H; et al., "Galaxy Simulation with Dust Formation and Destruction" , MNRAS: 466(1), 105-121, April, 2017 [SCI] ( ADS | Fulltext )
  39. Ferrara A; Hirashita H; Ouchi M; Fujimoto S, "The infrared-dark dust content of high redshift galaxies" , MNRAS: 471(4), 5018-5024, Nov, 2017 [SCI] ( ADS | Fulltext )
  40. Harada N*; Hasegawa Y; Aikawa Y; Hirashita H; Liu HB; Hirano N, "Effects of grain growth on molecular abundances in young stellar objects" , ApJ: 837(1), 78, March, 2017 [SCI] ( ADS | Fulltext )
  41. Hirashita H; Burgarella D; Bouwens RJ, "Dust masses of z > 5 galaxies from SED fitting and ALMA upper limits" , MNRAS: 472(4), 4587-4597, Dec 21, 2017 [SCI] ( ADS | Fulltext )
  42. Hirashita H; Harada N, "Effects of dust evolution on the abundances of CO and H2" , MNRAS: 467(1), 699-714, May, 2017 [SCI] ( ADS | Fulltext )
  43. Hirashita H; Nozawa T, "Dust evolution with active galactic nucleus feedback in elliptical galaxies" , Planet Space Sci: 149, 45-55, Dec, 2017 [SCI] ( ADS | Fulltext )
  44. Hou K-C; Hirashita H; Nagamine K; et al., "Evolution of dust extinction curves in galaxy simulation" , MNRAS: 469(1), 870-885, July, 2017 [SCI] ( ADS | Fulltext )
  45. Wang W-C*; Hirashita H; Hou K-C, "Dust evolution processes in normal galaxies at z > 6 detected by ALMA" , MNRAS: 465(3), 3475-3482, March, 2017 [SCI] ( ADS | Fulltext )
  46. Hirashita H; Koch PM; Matsushita S; Takakuwa S; Nakamura M; Asada K; Liu HB; Urata U; Wang M-J; Wang W-H; Takahashi S; Tang Y-W; Chang H-H; Huang K; Morata O; Otsuka M; Lin K-Y; Tsai A-L; Lin Y-T; Srinivasan S; Martin-Cocher P; Pu J-Y; Kemper F; Patel N; Grimes P; Huang Y-D; Han C-C; Huang Y-R; Nishioka H; Lin C-CL; Zhang Q; Keto E; Burgos R; Chen M-T; Inoue M; Ho PTP, "First-generation Science Cases for Ground-based Terahertz Telescopes" , PASJ: 68(1), R1, Feb, 2016 [SCI] ( ADS | Fulltext )
  47. Hirashita H; Nozawa T; Asano RS; Lee T, "Revisiting the lifetime estimate of large presolar grains in the interstellar medium" , Planet Space Sci: 133, 17-22, Nov, 2016 [SCI] ( ADS | Fulltext )
  48. Hou K-C*; Hirashita H; Michałowski MJ, "Dust evolution processes constrained by extinction curves in nearby galaxies" , PASJ: 68(6), 94, Dec, 2016 [SCI] ( ADS | Fulltext )
  49. Wong YHV; Hirashita H; Li Z-Y, "Millimeter-sized grains in the protostellar envelopes: where do they come from?" , PASJ: 68(4), 67, Aug, 2016 [SCI] ( ADS | Fulltext )
  50. Bekki K; Hirashita H; Tsujimoto T, "The Origin of Dust Extinction Curves with or without the 2175 Å Bump in Galaxies: the Case of the Magellanic Clouds" , ApJ: 810(1), 39, Sept 1, 2015 [SCI] ( ADS | Fulltext )
  51. Hirashita H, "Two-size approximation: a simple way of treating the evolution of grain size distribution in galaxies" , MNRAS: 447(3), 2937-2950, March 1, 2015 [SCI] ( ADS | Fulltext )
  52. Hirashita H*; Nozawa T; Villaume A; Srinivasan S, "Dust processing in elliptical galaxies" , MNRAS: 454, 1620-1633, Dec, 2015 [SCI] ( ADS | Fulltext )
  53. Naslim N; Kemper F; Madden SC; ....; Chu Y-H; ...; Yang Y; Seok J; ....; Otsuka M; Hirashita H; Morata O; ...; Srinivasan S; et al., "Molecular hydrogen emission in the interstellar medium of the Large Magellanic Cloud" , MNRAS: 446(3), 2490-2504, Jan, 2015 [SCI] ( ADS | Fulltext )
  54. Nozawa T; Asano RS; Hirashita H; Takeuchi TT, "Evolution of grain size distribution in high-redshift dusty quasars: integrating large amounts of dust and unusual extinction curves" , MNRAS: 447(1), L16-L20, Feb, 2015 [SCI] ( ADS | Fulltext )
  55. Seok JY*; Koo B-C; Hirashita H, "Dust cooling in supernova remnants in the Large Magellanic Cloud" , ApJ: 807(1), 100, July 1, 2015 [SCI] ( ADS | Fulltext )
  56. Urata Y; Huang K; Asada K; Hirashita H; Inoue M; Ho PTP, "A New Era of Submillimeter GRB Afterglow Follow-Ups with the Greenland Telescope" , Advances in Astronomy, Article ID 165030, 2015 [SCI] ( ADS | Fulltext )
  57. Asano RS; Takeuchi TT; Hirashita H; Nozawa T, "Evolution of extinction curves in galaxies" , MNRAS: 440(1), 134-142, May 1, 2014 [SCI] ( ADS | Fulltext )
  58. Hasegawa Y; Hirashita H, "Planet Traps and First Planets: the Critical Metallicity for Gas Giant Formation" , ApJ: 788(1), 62, June 10, 2014 [SCI] ( ADS | Fulltext )
  59. Hirashita H; Asano RS; Nozawa T; Li Z-Y; Liu M-C, "Dense molecular cloud cores as a source of micrometer-sized grains in galaxies" , Planet Space Sci: 100, 40-45, Oct 1, 2014 [SCI] ( ADS | Fulltext )
  60. Hirashita H; Ferrara A; Dayal F; Ouchi M, "Constraining dust formation in high-redshift young galaxies" , MNRAS: 443(1), 1704-1712, Sept, 2014 [SCI] ( ADS | Fulltext )
  61. Hirashita H; Voshchinnikov NV, "Effects of grain growth mechanisms on the extinction curve and the metal depletion in the interstellar medium" , MNRAS: 437(2), 1636-1645, Jan, 2014 [SCI] ( ADS | Fulltext )
  62. Inoue M; Algaba-Marcos JC; Asada K; Chang C-C; Chen M-T; Han J; Hirashita H; Ho PTP; Hsieh S-N; Huang T; Jiang H; Koch PM; Kubo DY; Kuo C-Y; Liu B; Martin-Cocher P; Matsushita S; Meyer-Zhao Z; Nakamura M; Nishioka H; Nystrom G; Pradel N; Pu H-Y; Raffin PA; Shen H-Y; Snow W; Srinivasan R; Wei T-S; Blundell R; Burgos R; Grimes P; Keto E; Paine S; Patel N; Sridharan TK; Doeleman SS; Fish V; Brisken W; Napier P, "Greenland telescope project: Direct confirmation of black hole with sub-millimeter VLBI" , Radio Science: 49(7), 564-571, July, 2014 [SCI] ( ADS | Fulltext )
  63. Schneider R*; Valiante R; Ventura P; ...; Hirashita H; Kemper F, "The dust production rate of asymptotic giant branch stars in the Magellanic Clouds" , MNRAS: 442(2), 1440-1450, Aug 1, 2014 [SCI] ( ADS | Fulltext )
  64. Seok JY; Hirashita H; Asano RS, "Formation History of Polycyclic Aromatic Hydrocarbons in Galaxies" , MNRAS: 439(2), 2186-2196, Feb, 2014 [SCI] ( ADS | Fulltext )
  65. Voshchinnikov NV; Hirashita H, "Effects of grain growth on the interstellar polarization curve" , MNRAS: 445(1), 301-308, Nov 21, 2014 [SCI] ( ADS | Fulltext )
  66. Asano R; Takeuchi TT; Hirashita H; Inoue AK, "Dust formation history of galaxies: a critical role of metallicity for the dust mass growth by accreting materials in the interstellar medium" , Earth Planets and Space: 65(3), 213-222, Mar, 2013 [SCI] ( ADS | Fulltext )
  67. Asano RS; Takeuchi TT; Hirashita H; Nozawa T, "What determines the grain size distribution in galaxies?" , MNRAS: 432(1), 637-652, June, 2013 [SCI] ( ADS | Fulltext )
  68. Fujita Y; Okabe N; ...; Matsushita S; Hirashita H; Nakamura M; et al, "Discovery of an Outstanding Disk in the cD Galaxy of the Hydra A Cluster" , PASJ: 65(6), 15, Dec 25, 2013 [SCI] ( ADS | Fulltext )
  69. Hirashita H, "Properties of free-free, dust, and CO emissions in the starbursts of blue compact dwarf galaxies" , MNRAS: 429(4), 3390-3401, Mar 11, 2013 [SCI] ( ADS | Fulltext )
  70. Hirashita H; Kobayashi H, "Evolution of dust grain size distribution by shattering in the interstellar medium: robustness and uncertainty" , Earth Planets and Space: 65(10), 1083-1094, Oct, 2013 [SCI] ( ADS | Fulltext )
  71. Hirashita H; Li Z-Y, "Condition for the formation of micron-sized dust grains in dense molecular cloud cores" , MNRAS: 434(1), L70-L74, July, 2013 [SCI] ( ADS | Fulltext )
  72. Hirashita H; Nozawa T, "Synthesized grain size distribution in the interstellar medium" , Earth Planets and Space: 65(3), 183-192, Mar, 2013 [SCI] ( ADS | Fulltext )
  73. Kuo T-M; Hirashita H; Zafar T, "Evolution of dust content in galaxies probed by gamma-ray burst afterglows" , MNRAS: 436(2), 1238-1244, Dec, 2013 [SCI] ( ADS | Fulltext )
  74. Hirashita H, "Dust growth in the interstellar medium: How do accretion and coagulation interplay?" , MNRAS: 422, 1263-1271, May, 2012 [SCI] ( ADS | Fulltext )
  75. Kuo T-M; Hirashita H, "Impact of grain size distributions on the dust enrichment in high-redshift quasars" , MNRAS: 424(1), L34-L38, July, 2012 [SCI] ( ADS | Fulltext )
  76. Hirashita H, "Central free-free dominated 880-μm emission in II Zw 40" , MNRAS: 418(2), 828-837, Dec, 2011 [SCI] ( ADS | Fulltext )
  77. Hirashita H; Kuo T-M, "Effects of grain size distribution on the interstellar dust mass growth" , MNRAS: 416(2), 1340-1353, Sept, 2011 [SCI] ( ADS | Fulltext )
  78. Jang MS; ...; Urata Y; Huang KY; Hirashita H; et al., "Dust Properties in the Afterglow of GRB 071025 at z ~ 5" , ApJ: 741(1), L20, Nov 1, 2011 [SCI] ( ADS | Fulltext )
  79. Kawara K*; Hirashita H; et al., "Supernova dust for the extinction law in a young infrared galaxy at z∼ 1" , MNRAS: 412(2), 1070-1080, April, 2011 [SCI] ( ADS | Fulltext )
  80. Sun A-L; Hirashita H, "Importance of far-infrared mapping in a spiral galaxy: AKARI observation of M81" , MNRAS: 411(3), 1707-1715, Mar, 2011 [SCI] ( ADS | Fulltext )
  81. Yamasawa D*; Habe A; ...; Hirashita H; et al., "The Role of Dust in the Early Universe. I. Protogalaxy Evolution" , ApJ: 735(1), 44, July 1, 2011 [SCI] ( ADS | Fulltext )
  82. Dayal P; Hirashita H; Ferrara A, "Detecting Lyman alpha emitters in the submillimetre" , MNRAS: 403(2), 620-624, April, 2010 [SCI] ( ADS | Fulltext )
  83. Hirashita H, "Shattering by turbulence as a production source of very small grains" , MNRAS: 407(1), L49-L53, Sept, 2010 [SCI] ( ADS | Fulltext )
  84. Hirashita H; Nozawa T; Yan H; Kozasa T, "Effects of grain shattering by turbulence on extinction curves in starburst galaxies" , MNRAS: 404(3), 1437-1448, May, 2010 [SCI] ( ADS | Fulltext )
  85. Suwa T; Hirashita H; Tamura Y, "A simple approach to the high-redshift sub-millimeter galaxies" , Ap&SS: 330(2), 219-226, Dec, 2010 [SCI] ( ADS | Fulltext )
  86. Hirashita H; Ichikawa TT, "Effects of dust abundance on the far-infrared colours of blue compact dwarf galaxies" , MNRAS: 396(1), 500-510, Jun 11, 2009 [SCI] ( ADS | Fulltext )
  87. Hirashita H; Omukai K, "Dust coagulation in star formation with different metallicities" , MNRAS: 399 (4), 1975-1801, November, 2009 [SCI] ( ADS | Fulltext )
  88. Hirashita H; Yan H, "Shattering and coagulation of dust grains in interstellar turbulence" , MNRAS: 394(2), 1061-1074, April, 2009 [SCI] ( ADS | Fulltext )
  89. Hunt LK; Hirashita H, "The size-density relation of extragalactic HII regions" , A&A: 507(3), 1327-1343, Dec, 2009 [SCI] ( ADS | Fulltext )
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