2cm Far-infrared Emission Lines in Galaxies: 0.1cm The ... · 5 high-z star forming galaxies (MIPS...

Far-infrared Emission Lines in Galaxies |

Far-infrared Emission Lines in Galaxies:

The SHINING Contribution to the Understanding of General Trends

Javier Graciá-Carpio (MPE)

on behalf of the SHINING team:

E. Sturm (PI), S. Hailey-Dunsheath, J. Fischer, A. Contursi, A. Poglitsch,E. González-Alfonso, A. Sternberg, A. Verma, N. Christopher, R. Genzel, R. Davies,

H. Feuchtgruber, J. A. de Jong, D. Lutz and L. Tacconi

Stormy Cosmos | Pasadena | 04 / 11 / 2010 1 / 12

Far-infrared Emission Lines in Galaxies | Introduction

SHINING


« We aim to obtain a comprehensive view of the physical processes atwork in the interstellar medium of local galaxies... »


SHINING


« We aim to obtain a comprehensive view of the physical processes atwork in the interstellar medium of local galaxies ranging from objectswith moderately enhanced star formation to the most dense, energetic,and obscured environments in ultraluminous infrared galaxies... »


SHINING


« We aim to obtain a comprehensive view of the physical processes atwork in the interstellar medium of local galaxies ranging from objectswith moderately enhanced star formation to the most dense, energetic,and obscured environments in ultraluminous infrared galaxies andaround AGN »


SHINING


« We aim to obtain a comprehensive view of the physical processes atwork in the interstellar medium of local galaxies ranging from objectswith moderately enhanced star formation to the most dense, energetic,and obscured environments in ultraluminous infrared galaxies andaround AGN »

Eckhard Sturm et al.


SHINING


• Fine structure lines

• Molecular lines

• High-J CO lines

• Full PACS SEDs

• Resolved spatial information


SHINING


Far-infrared fine structure lines:

• PDR lines: [C II] 158µm, [O I] 145µm, [O I] 63µm

• HII lines: [N II] 122µm, [O III] 88µm, [N III] 57µm, [O III] 52µm

Sample:

• 9 local starbursts (M 82, NGC 253, M 83, ...)

• 18 Seyfert galaxies (NGC 1068, Cen A, Circinus, ...)

• 28 LIRGs and ULIRGs (NGC 4418, Arp 220, Mrk 231, ...)

• 5 high-z star forming galaxies (MIPS J142824.0, ...)

• 4 high-z AGNs (IRAS F10214, Cloverleaf, ...)

Far-infrared Emission Lines in Galaxies | First results

The [CII] line deficit


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NGC 4418

LFIR [ LSun ]

[C II

] (15

7.7µµ

m)

/ FIR ●

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HII galaxyLINERSeyfert & QSOBlue Compact DwarfUnclassified

[ Graciá-Carpio et al. 2010, submitted ]

[ Brauher et al. 2008, ApJS 178: 280 ]

[ Luhman et al. 2003, ApJ 594: 758 ]




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NGC 4418

LFIR [ LSun ]

[C II

] (15

7.7µµ

m)

/ FIR ●

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HII galaxyLINERSeyfert & QSOBlue Compact DwarfUnclassifiedHigh−z galaxy



[ Luhman et al. 2003, ApJ 594: 758 ]

[ Stacey et al. 2010, arXiv:1009.4216 ]




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LFIR [ LSun ]

[C II

] (15

7.7µµ

m)

/ FIR

LFIR / MH2 [ LSun / MSun ]

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[ Luhman et al. 2003, ApJ 594: 758 ]

[ Stacey et al. 2010, arXiv:1009.4216 ]


A general far-infrared line deficit


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[C II] 158µµm

FIR

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[O I] 145µµm

FIR

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[N II] 122µµm

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[O III] 88µµm

FIR

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NGC 4418

Arp 220

IRAS 17208−0014

[O I] 63µµm

FIR

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FIR

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[O III] 52µµm

FIR


Line

flux

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IR

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Two modes of star formation


[ Genzel et al. 2010, MNRAS 407: 2091 ]

[ Daddi et al. 2010, ApJ 714: L118 ]


Line emission vs. LFIR/MH2


LFIR/MH2' 1–100 L� M�

−1


Line emission vs. LFIR/MH2


LFIR/MH2' 1–100 L� M�

−1 LFIR/MH2' 100–1000 L� M�

−1


A general far-infrared line deficit


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[C II] 158µµm

FIR

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[O I] 145µµm

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[N II] 122µµm

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[O III] 88µµm

FIR

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Arp 220

IRAS 17208−0014

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FIR

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[O III] 52µµm

FIR


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Cloudy models


T∗ = 36000 K, AV = 100 mag

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[C II] 158µµm

FIR[O I] 145µµm

FIR

[N II] 122µµm

FIR[O III] 88µµm

FIR

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[O I] 63µµm

FIR

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[N III] 57µµm

FIR

1.0 1.5 2.0 2.5 3.0 3.5 4.0

[O III] 52µµm

FIR

log nH [ cm−3 ]

log

(ioni

zatio

n pa

ram

eter

)


Cloudy models


T∗ = 36000 K, AV = 100 mag

−3.5

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−0.5

[C II] 158µµm

FIR[O I] 145µµm

FIR

[N II] 122µµm

FIR[O III] 88µµm

FIR

1.0 1.5 2.0 2.5 3.0 3.5 4.0

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[O I] 63µµm

FIR

1.0 1.5 2.0 2.5 3.0 3.5 4.0

[N III] 57µµm

FIR

1.0 1.5 2.0 2.5 3.0 3.5 4.0

[O III] 52µµm

FIR

log nH [ cm−3 ]

log

(ioni

zatio

n pa

ram

eter

)

Low LFIR / MH2 range


Cloudy models


T∗ = 36000 K, AV = 100 mag

−3.5

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−0.5

[C II] 158µµm

FIR[O I] 145µµm

FIR

[N II] 122µµm

FIR[O III] 88µµm

FIR

1.0 1.5 2.0 2.5 3.0 3.5 4.0

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[O I] 63µµm

FIR

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[N III] 57µµm

FIR

1.0 1.5 2.0 2.5 3.0 3.5 4.0

[O III] 52µµm

FIR

log nH [ cm−3 ]

log

(ioni

zatio

n pa

ram

eter

)

Low LFIR / MH2 range

High LFIR / MH2 range


Spatially resolved information


M 82 [C II] 158µm

[ Contursi et al. 2010, in preparation ]




M 82 [C II] 158µm

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[C II

] (15

7.7µµ

m)

/ FIR





M 82 [C II] 158µm

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/ FIR ●

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Far-infrared Emission Lines in Galaxies | Conclusions

Conclusions

• LFIR/MH2is a good proxy for the relative brightness of the far-infrared fine

structure lines.

• We find line deficits in all the fine structure lines, regardless of their origin in theionized or neutral phase of the ISM.

• The LFIR/MH2threshold is similar to the limit that separates between the two

modes of star formation recently found in galaxies.

• High ionization parameters can explain the line deficits in the [C II], [O I] and[N II] lines. Further modeling is needed to explain the [N III] and [O III] lines.

• More to come!


2cm Far-infrared Emission Lines in Galaxies: 0.1cm The ... · 5 high-z star forming galaxies (MIPS...

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Transcript of 2cm Far-infrared Emission Lines in Galaxies: 0.1cm The ... · 5 high-z star forming galaxies (MIPS...