[C II] 158 m Emission from Damped Ly Systems Art Wolfe and Ken Nagamine UCSD UCSD.
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Transcript of [C II] 158 m Emission from Damped Ly Systems Art Wolfe and Ken Nagamine UCSD UCSD.
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[[C IIC II]] 158 158 m Emission from m Emission from Damped LyDamped Ly Systems Systems
Art Wolfe and Ken Nagamine Art Wolfe and Ken Nagamine UCSD UCSD
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DLAS are
•Definition of Damped LySystem (DLA): N(HI) > 2*1020 cm-2
•Distinguishing characteristic of DLAs : Gas is Neutral
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DLAS are
•Definition: N(HI) > 2*1020 cm-2
•Distinguishing characteristic of DLAs : Gas is Neutral
Stars form out of cold gas
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•DLAs Dominate the Neutral Gas Content of the Universe at z=[0,5]
•Gas Content of DLAs at z=[3,4] Accounts for current visible Mass
•DLAs Serve as Important Neutral Gas Reservoirs for Star Formation
Relevance of DLAs for Star FormationRelevance of DLAs for Star Formation
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•DLAs Dominate the Neutral Gas Content of the Universe at z=[0,5]
•Gas Content of DLAs at z=[3,4] Accounts for current visible Mass
•DLAs Serve as Important Neutral Gas Reservoirs for Star Formation
Mass per unitComoving Volume versusredshift
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•DLAs Dominate the Neutral Gas Content of the Universe at z=[0,5]
•Gas Content of DLAs at z=[3,4] Accounts for current visible Mass
•DLAs Serve as Important Neutral Gas Reservoirs for Star Formation
CurrentVisibleMatter
NeutralGas atHigh z
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HIRES Metal-line Velocity Profiles in DLAsHIRES Metal-line Velocity Profiles in DLAsHIRES Metal-line Velocity Profiles in DLAsHIRES Metal-line Velocity Profiles in DLAs
High-resolution spectroscopy on very large telescopes can yield quantitative information about DLAs:
• Cooling Rates
• Star formation rates.
SFRs
ThermalPressure
Chemistry
Kinematics
Nucleosynthesis
Dust & Nucleosynthesis
Nucleosynthesis
Nucleosynthesis
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Obtaining Cooling Rates from CII* AbsorptionObtaining Cooling Rates from CII* Absorption
• [C II] 158 micron transition dominates cooling of neutral gas in Galaxy ISM
• Spontaneous emission rate per atom lc=n[CII] obtained from strength of 1335.7 absorption and Lyman alpha absorption
• Thermal equilibrium condition lc= pe gives heating rate per atom
2121)IH(*)IIC(
][ ~ Ahn NN
IIC ν 2121)IH(*)IIC(
][ ~ Ahn NN
IIC ν
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[C II] 158 micron Emission rates vs N(H I)[C II] 158 micron Emission rates vs N(H I)
• Median lc=10-26.6 ergs s-1 H-1 for positive Detections
• Upper limits tend to have low N(H I)
• DLA lc values about 30 times lower than for Galaxy: explained by lower dust content and similar SFRs per unit area
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Effect of Adding Local FUV HeatingEffect of Adding Local FUV Heating
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An LBG Galaxy Associated with a DLA (Moller etal ‘02)An LBG Galaxy Associated with a DLA (Moller etal ‘02)
8.4 kpc
LyEmission [O III] Emission
CII* Absorption
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[C II] contours superposed on 6.75 [C II] contours superposed on 6.75 m Imagem Image
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[C II] Flux Densities Predicted for DLAs[C II] Flux Densities Predicted for DLAs
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Predicted SPredicted Sνν00 for DLA 2206-19A for DLA 2206-19A
• 33 Alma limit for 20 hr Alma limit for 20 hr integration timeintegration time
• 90 % Mass range 90 % Mass range predicted for CDM predicted for CDM Models of DLAsModels of DLAs
• MMH IH I =m =mDDMM
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Tentative lTentative lcc versus versus v relationv relation
• DLA2206-19ADLA2206-19A
• CDM Models predict CDM Models predict v = 0.6vv = 0.6vcc
• M=vM=vcc33/10GH(z)/10GH(z)
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DLA2206-19ADLA2206-19A
• SSνν00 impliedimplied for Mass for Mass
predicted by lpredicted by lc c versus versus
v relationv relation
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17 kpc17 kpc
608 MHz VLBI Map of PKS 0458-02608 MHz VLBI Map of PKS 0458-02
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Single-Dish versus VLBI 21 cm Absorption profilesSingle-Dish versus VLBI 21 cm Absorption profiles for DLA 0458-02 at z=2.0394for DLA 0458-02 at z=2.0394
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Alma Sensitivity for Detection of C II Alma Sensitivity for Detection of C II EmissionEmission
• Lower Limit for Lower Limit for DLA0458-02 forDLA0458-02 for
MMH IH I=10=101010 M Msunsun
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Predicted SPredicted Sνν0 0 for full Sample for full Sample
• ““Redshift Desert’’Redshift Desert’’
• CNM confirmed by CNM confirmed by absence of absence of Si IISi II* * 1264 1264 absorption absorption