銀河物理学特論i galactic astrophysics i i-5e i i5: …akiyama/lecture/galaxy/...emission line...
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銀河物理学特論 I銀河物理学特論Galactic Astrophysics I
I 5 E i i li Di tiI-5: Emission-line Diagnostics
2015/05/25
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HII regions in M51M51 の HII 領域の 領域
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HII region NGC604 in M33M33 の HII 領域 NGC604の 領域
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Planetary Nebulae惑星状星雲惑星状星雲
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Narrow-line / Broad-line regions of Active Galactic Nuclei活動銀河中心核の狭/広輝線領域活動銀河中心核の狭/広輝線領域
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Emission line spectrum輝線スペクトル輝線 クトル
• Line ratio vary with ionizing photon spectrum.
Dominated by ions with low ionization degree.
Ionization source~10,000K、density 1000cm 3 Te 7 000density 1000cm-3、Te~7,000-25,000K
Dominated by highly ionized ions
Ionization source~100,000K、density 1000cm 3density~1000cm-3、Te~10,000K
Ions with various ionization states.
Ionization source~power-law continuum density~1000cm-continuum、density~1000cm-3、Te~10,000K
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Photo-ionization Cross-section光電離の断面積光電離の断面積
• Photo ionization cross section peaks at the ionization energy and declines with E^-3. The energy range of photons which can ionize atoms (or ions) is
l ti lrelatively narrow.
“Atomic Astrophysics and Spectroscopy” Pradhan & Nahar 2011
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Source of Ionizing photons電離光子の起源電離光子の起源
• Main sequence massive stars or white dwarfs
Iben 1967, ARAA, 5, 571Shaw & Kaler 1989, ApJS, 69, 495
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Stellar effective temperature and number of ionizing photons星の有効温度と電離光子の数星の有効温度と電離光子の数
Sternberg et al. 2003, ApJ, 599, 1333
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Structure of ionized regions: Hydrogen, Helium電離領域の構造電離領域の構造
Tielens “The Physics and Chemistry of the Interstellar Medium”
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Structure of ionized regions: Oxygen, Nitrogen電離領域の構造電離領域の構造
Tielens “The Physics and Chemistry of the Interstellar Medium”
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Classification of galaxies with emission line properties輝線の性質を用いた銀河の分類輝線の性質を用 た銀河の分類
[OII] Ha,NIIHb [OIII]
Tremonti et al. 2004, ApJ, 613, 898
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Classification of galaxies with emission line properties輝線の性質を用いた銀河の分類輝線の性質を用 た銀河の分類
AGN
LINERLINERHII-region
AGNs tend to have stronger highly ionized emission lines, like [OIII]
Kauffmann et al. 2003, MNRAS, 346, 1055
Solid line :selection line by Kewly et al. (2001) model calculation, Dashed line : empirical line.
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Gas-phase metallicity estimation with emission lines輝線を用いたガス金属量の診断輝線を用 たガ 金属量の診断
• Gas phase metallicity can be evaluated with nebulae emission lines
Maiolino et al. 2008, A&A, 488, 463
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Gas-phase metallicity estimation with emission lines輝線を用いたガス金属量の診断輝線を用 たガ 金属量の診断
• Mass-metallicity relation of nearby galaxies
Tremonti et al., 2004, ApJ, 613, 898
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What does determine the observed relation between SMBH mass and “spheroid” mass ?SMBH mass and spheroid mass ?
Emission-line diagnostics in the nuclear region of galaxiesin the nuclear region of galaxies
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Emission line diagnostics for star-forming galaxies星形成銀河の輝線診断星形成銀河の輝線診断
• Photo-ionization by OB stars.• Effects of metallicity and ionization y
parameter
Kewley et al. 2013, ApJ, 774, 100
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Emission line diagnostics for star-forming galaxies星形成銀河の輝線診断星形成銀河の輝線診断
Kewley et al 2013 ApJ 774 100Kewley et al. 2013, ApJ, 774, 100
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Emission line diagnostics for Active Galactic Nuclei活動銀河中心核の輝線診断活動銀河中心核の輝線診断
• Photo-ionization models of AGN continuum.
Kewley et al. 2013, ApJ, 774, 100y , p , ,
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Emission lines from “shocked” regions衝撃波領域からの輝線放射衝撃波領域からの輝線放射
• Shock: models with collisional excitation of ions.• Precursor: photoionization by UV emission from shocked region.p y g• AGN/LINERs have similar line ratios to shock models.
Allen et al. 2008, ApJS, 178, 20
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Comparison between different emission line models異なる輝線モデルの比較異なる輝線 デルの比較
Sarzi et al. 2010, MNRAS, 402, 2187
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Emission line diagnostics of nuclear regions of nearby galaxies近傍銀河中心各領域の輝線診断近傍銀河中心各領域の輝線診断
• Emission line diagnostics of nuclear regions (~200pc) of galaxies in the nearby universe (<17Mpc).
Ho et al. 2008 ARAA, 46, 475
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Emission line diagnostics of nuclear regions of nearby galaxies近傍銀河中心各領域の輝線診断近傍銀河中心各領域の輝線診断
• Emission line diagnostics of nuclear regions (~200pc) of galaxies in the nearby universe (<17Mpc).
Ho et al. 2008 ARAA, 46, 475
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Emission line diagnostics of nuclear regions of nearby galaxies近傍銀河中心各領域の輝線診断近傍銀河中心各領域の輝線診断
• LINERs are dominant population among nuclear region of early-type galaxies Ho et al. 2008 ARAA, 46, 475Ho et al. 2008 ARAA, 46, 475
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What are LINERs ?LINER とは何かとは何か
• Some LINERs show broad-line component indicating existence of AGN activity.
Ho et al. 2008 ARAA, 46, 475
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What are LINERs ?LINER とは何かとは何か
• Photo-ionization by post-AGB stars can be another ionization mechanism for LINERs.
Sarzi et al. 2010, MNRAS, 402, 2187