Mikako Matsuura (University College London) · Matsuura et al. (2009, MNRAS 396, 918) SAGE 0.5x10-8...
Transcript of Mikako Matsuura (University College London) · Matsuura et al. (2009, MNRAS 396, 918) SAGE 0.5x10-8...
![Page 1: Mikako Matsuura (University College London) · Matsuura et al. (2009, MNRAS 396, 918) SAGE 0.5x10-8 - 1.5x10-8 M yr-1 1.5x10-8 - 5x10-8 M yr-1 5x10-8 - 50x10-8 M yr-1 Dust ejection](https://reader034.fdocuments.in/reader034/viewer/2022050413/5f898141662c5059fe2ecdf8/html5/thumbnails/1.jpg)
Mikako Matsuura (University College London)
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Dust is found in the interstellar media (ISM) of many galaxies
Cosmic dust
Infrared image of the Milky Way (90 micron)
Submm-galaxies (z~6.4)
M33 Spitzer 3.6, 4.5 and 8.0 micron
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>8(10?) M
1- 8(10?) M
Concept of cycle of matter Past: Theory/models
(population synthesis/chemical evolution models of galaxies)
Mikako Matsuura (Origins Institute, UCL) Can stellar sources form enough dust in galaxies?
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The origins of dust : evolved stars ◦ Low-and intermediate-mass (1-8 M) stars Asymptotic Giant Branch (AGB) stars
◦ High mass (>8 M) stars Luminous blue variables (LBVs) Wolf Rayet (WR) stars Red supergiants Supernovae? ◦ Novae?
To understand the origin of dust and its evolution in galaxies ◦ Stellar population/stellar evolution + dust formation in stars
Mikako Matsuura (Origins Institute, UCL) Can stellar sources form enough dust in galaxies?
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Can stellar sources form enough dust to account the mass present in galaxies? ◦ Dispute Observations
Milky Way: yes (Gehrz 1989); no (Tielens 2001) Large Magellanic Cloud: no (Matsuura et al. 2009)
Models Yes…. (default answer?) Milky Way: yes (Dwek 1998); no (Zhukovska et al. 2008) SDSS J1148+5251 (quasar at z = 6.4):yes (Valiante et al. 2009)
◦ ELT will be able to make a significant step to resolve this situation Observational constrains on metallicity age dependence of dust production
Mikako Matsuura (Origins Institute, UCL) Can stellar sources form enough dust in galaxies?
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Following chemical evolution of galaxies
Dus
t m
ass
(M
)
Stellar mass
AGB stars SNe
Carbon
Silicate Others (Fe, etc)
Valiante et al. (2009)
Inputs
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Oxides ◦ Olivines : Mg2xFe(2-2x)SiO4
◦ Pyroxenes : MgxFe1-xSiO3
Carbonaceous dust ◦ Graphite : C ◦ Amorphous : C ◦ Polycyclic aromatic hydrocarbons
(PAHs)
Dust mass : as a function of metallicity of the interstellar medium of galaxies. … but … elements synthesized in stars themselves affect the dust mass/compositions (at least for carbon-rich AGB; Sloan, Matsuura et al. 2009, Science 323, 353)
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Following chemical evolution of galaxies
Valiante et al. (2009)
Inputs
Star
form
atio
n ra
te
Time since the formation of galaxies
SDSS J1148+5251 (quasar at z = 6.4)
![Page 9: Mikako Matsuura (University College London) · Matsuura et al. (2009, MNRAS 396, 918) SAGE 0.5x10-8 - 1.5x10-8 M yr-1 1.5x10-8 - 5x10-8 M yr-1 5x10-8 - 50x10-8 M yr-1 Dust ejection](https://reader034.fdocuments.in/reader034/viewer/2022050413/5f898141662c5059fe2ecdf8/html5/thumbnails/9.jpg)
Following chemical evolution of galaxies
Dus
t m
ass
(M
)
Carbon
Silicate Others (Fe, etc)
Valiante et al. (2009) Time since the formation of galaxies
Evolution of dust mass Evolution of the metallicity and the (Si+O)/C elemental ratio
Mass of stars
Total mass of dust
SDSS J1148+5251 (quasar at z = 6.4)
![Page 10: Mikako Matsuura (University College London) · Matsuura et al. (2009, MNRAS 396, 918) SAGE 0.5x10-8 - 1.5x10-8 M yr-1 1.5x10-8 - 5x10-8 M yr-1 5x10-8 - 50x10-8 M yr-1 Dust ejection](https://reader034.fdocuments.in/reader034/viewer/2022050413/5f898141662c5059fe2ecdf8/html5/thumbnails/10.jpg)
Following chemical evolution of galaxies
No observational constrains given D
ust
mas
s (M
)
Stellar mass
AGB stars SNe
Carbon
Silicate Others (Fe, etc)
Valiante et al. (2009)
Inputs
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Matsuura et al. (2009, MNRAS 396, 918)
SAGE
0.5x10-8 - 1.5x10-8 M yr-1
1.5x10-8 - 5x10-8 M yr-1
5x10-8 - 50x10-8 M yr-1
Dust ejection rate
(from stars into the interstellar medium)
Field stars in the Large Magellanic Cloud (LMC)
Total dust input from evolved stars into the interstellar medium ◦ AGB: (4-9)x10-5 M yr-1
◦ SNe: (0.1-10)x10-5 M yr-1
(up to 100x10-5M yr-1 ?)
◦ Total dust input: 104 -105 M Over 1 Gyrs (=life time of dust), if SFR
is constant
◦ ISM dust: 106 M
No info about age, metallicity (elemental abundances) and main sequence mass of individual stars
Mikako Matsuura (Origins Institute, UCL) Can stellar sources form enough dust in galaxies?
![Page 12: Mikako Matsuura (University College London) · Matsuura et al. (2009, MNRAS 396, 918) SAGE 0.5x10-8 - 1.5x10-8 M yr-1 1.5x10-8 - 5x10-8 M yr-1 5x10-8 - 50x10-8 M yr-1 Dust ejection](https://reader034.fdocuments.in/reader034/viewer/2022050413/5f898141662c5059fe2ecdf8/html5/thumbnails/12.jpg)
Following chemical evolution of galaxies
No observational constrains given D
ust
mas
s (M
)
Stellar mass
AGB stars SNe
Carbon
Silicate Others (Fe, etc)
Valiante et al. (2009)
Inputs
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Dust formation in AGB stars in clusters ◦ Field stars in galaxies -> Clusters (LMC and beyond) Age, mass, and metallicity Elemental abundances (of planetary nebulae)
Carbon abundance in AGB stars UV (HST) or deep optical spectra with ELT
Dust measured from near/ mid-infrared emissions (ELT+JWST)
Dust formation in SNe?
Mikako Matsuura (Origins Institute, UCL) Can stellar sources form enough dust in galaxies?
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Stellar evolution along the AGB stars
Maraston (2005) Mikako Matsuura (Origins Institute, UCL) Can stellar sources form enough dust in galaxies?
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Mikako Matsuura (Origins Institute, UCL) Can stellar sources form enough dust in galaxies?
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ELT: bridging observational and theoretical works Parameters poorly constrained by observations Population synthesis + dust evolution ◦ Evolution of elemental abundances in the gas and dust phases
Dust production along with stellar evolution ◦ Dust condensation rate / Dust ejection rate in a star Dust production over stellar evolution
◦ Stellar population Metallicity / elemental abundance/ Stellar yields Star formation history Initial mass function
Mikako Matsuura (Origins Institute, UCL) Can stellar sources form enough dust in galaxies?