Life cycle of Cosmic matter and evolution of

Life cycle of Cosmic matter and evolution of galaxies 宇宙の物質循環と銀河進化 (1) Transmigration in the Galaxy 銀河内物質循環 How Stars are born? Trigger mechanism? 星は何をきっかけに、どのような場所で生まれる？ At what stage, gas outflow happens? 星のガス放出は、どの進化段階で、 どのように起きるのか？ 超新星は塵を作る？壊す？ Interstellar Gas clouds 星間ガス雲(“星の胎盤”) Death of Stars: outflow, supernovae dust formation & destruction 星の終焉：ガス放出／超新星爆発、 塵の生成／破壊 Birth of Stars 星の誕生 p 2

Life cycle of Cosmic matter and evolution of galaxies 宇宙の物質循環と銀河進化 (2) Transmigration of matter in the inter-galaxies 銀河間での物質循環 Outflow due to gravitational interaction 重力相互作用 による物質流出 Galaxy - galaxy interaction 銀河間相互作用 （重力相互作用、衝突） Acetion of Intergalactic gas 銀河間ガスの降着 Intergalactic gas 銀河間ガス Starburst induced by galaxy-galaxy collision 銀河衝突による爆発的星形成 Galaxy Evolution Large-scale material outflow due to Supernovae 大規模な超新星爆発に よる物質流出 Star formation Metal generation Dust Formation Planetary systems formation p 3

Interstellar dust 星間塵 • Solid state Interstellar Matter (1 -2 % in mass) 固体の星間 物質（質量で１～２％） • Dust absorption / emission rate is much stronger than atoms/molecules 星間ガスに比べて光の吸収・放射が非常 に強い Extinction due to dust ＝ absorption ＋ scattering 塵による減光 ＝ 吸収 ＋ 散乱 p 4

Crystalline. Silicate Representative Amorphou dust s Major component of interstellar dust grains, found in meteorites, also rocks on the earth. Forsterite (Mg 2 Si. O 4) Crystalline Enstatite (Mg. Si. O 3) Amorphous ・olivne（カンラン石） (Mg, Fe)2 Si. O 4 ・pyroxene（輝石） (Mg, Fe)Si. O 3

Crystallene silicate 結晶質シリケイト observed with Subaru/COMICS Honda et al. ２００３ p 6

Absorption spectrum due to ice toward a proto-star 原始星周辺の塵に見られる様々な氷の吸収スペクトル Whittet et al. (1996） A&A R 2 -p 8

Comets observed with AKARI/IRC Near-IR image 103 P/Hartley by Epoxi (NASA) C/Lulin H 2 O CO 2 • CO 2/H 2 O=11 -24 % for AKARI comet samples which is lower than those found in low-mass proto-stars, but similar to high mass proto-stars (Ootsubo et al. 2012)

Optical Depth 光学的厚み ds I(s) Area 面積 d. A volume 体積 d. A・ds I(s) + d. I n＝number density of absorbers 吸収体の数密度[m-3] ρ＝mass density 質量密度 [kg/m 3] σ＝absorption cross section 吸収断面積 [m 2] absorption coefficient 吸収係数 [m-1] a = ns a = rk ( κ＝質量吸収係数) Total absorbing area in the volume 領域内の全吸収面積は

Extinction Curves（減光曲線） LMC MW SMC Dot-dashed： graphite Dotted： silicate Dashed： PAH Solid： total extinction Takagi et al. (2003) p 16

UV-optical extinction curve Calzetti et al. 1994

Unidentified Infrared (UIR) Bands • Ubiquitous presence in astrophysical environment – HII region, Reflection Nebulae, Planetary Nebulae, etc. (Tokunaga et al. 1997) – Diffuse ISM (Onaka et al. 1996; Mattila et al. 1996) – External Galaxies (e. g. Helou et al. 2000) even at z~2 (Yan et al. 2004) First detection of 8. 6µm and 11. 2µm features by Gillet et al. (1973) and 3. 3µm, 6. 2µm and 7. 7µm by Russel et al. (1978). Smith+ 2007 Ap. J, 656, 770

Origin of UIR bands : hypothesis Polycyclic Aromatic Hydrocarbons (PAH) 多環芳香族炭化水素 PAH family • PAH hypothesis – Puget & Léger (1984, 1989) – Allamandolla, Tielens & Barker (1989) • - Quenched Carbonaceous Composite – Sakata et al. (1984)

Strength of PAH emission depends strongly on the Charge (Ionization) State • Calculated / measured absorption cross section is remarkably different (CC mode increased relative to C-H mode when ionized) Peeters et al. 2002

Discovery of diffuse UIB emission from the Galaxy. Results from IRTSの成果ー我々の銀河系からの拡散UIB放射の発見 Emission from stars (3 m continuum) 星（波長 3ミクロン連続波）の分布 Emission from 3. 3 m UIB 3. 3ミクロンUIB放射の分布 http: //www. ir. isas. jaxa. jp/irts/nirs/uir_intro. html p 26

Characteristics of Diffuse UIB emission 拡散UIB放射の性質 • G 0： UV radiation strength FIR放射量から見積もった紫外光強度 （Onaka, T. 2003) p 27

SED of interstellar dust in the Galaxy 我々の銀河系の星間塵からの 放射エネルギースペクトル分布（SED） Dot-dashed： graphite Dotted： silicate Dashed： PAH Solid： total (Dwek et al. 1997 & Takagi et al. 2003) p 28