30
rimary Coolant and Tracer of Star F Dec 21 st , 2012

C + As a Primary Coolant and Tracer of Star Formation

  • Upload
    mireya

  • View
    18

  • Download
    0

Embed Size (px)

DESCRIPTION

C + As a Primary Coolant and Tracer of Star Formation. Dec 21 st , 2012. Heating. SFR. Cooling. [CII]. Sargsyan et al. 2012. [CII]/ L IR ~ const + SFR based on L IR SFR([CII]). SFR (24 m m + FUV). ISO [CII]. de Looze et al. 2011. KINGFISH. - PowerPoint PPT Presentation

Citation preview

Page 1: C +  As a Primary Coolant                            and Tracer of  Star Formation

C+ As a Primary Coolant and Tracer of Star Formation

Dec 21st, 2012

Page 2: C +  As a Primary Coolant                            and Tracer of  Star Formation

SFR

[CII]

Hea

ting

Cooling

Page 3: C +  As a Primary Coolant                            and Tracer of  Star Formation

de Looze et al. 2011

SFR

(24

mm +

FU

V)

ISO [CII]Herrera-Camus et al. 2013KINGFISH

PACS [CII]

~ 500 pc resolution

Sargsyan et al. 2012

[CII]/ LIR ~ const + SFR based on LIR SFR([CII])

Page 4: C +  As a Primary Coolant                            and Tracer of  Star Formation

Warm H T = 8000 Kn = 0.3 cm-3

Cold HT = 80 Kn = 30 cm-3Cold H2

T = 10 K

Classic PDR

Contributions to [CII] Line emission

OB star

H+ H+

H+

CNM

WNM

r ~ few pc

r ~ 10s pc

r~ 100s pc

C+/HI

C+/H2

FUV

Warm H+

T = 8000 K Ne = 5 cm-3

WIM

EUVr ~ 100s pc ?

[CII] a dominant coolant? Maybe

NO

NO

NO

YES!

Page 5: C +  As a Primary Coolant                            and Tracer of  Star Formation

Ionization: FUV, X-ray, C.R.Heating: P.E., C.R., X-ray/EUVCooling: [CII], [OI], Lya, e- recombination

nG = n2L

T

= nT

Wolfire et al. (2003)

WNM stable

CNM

stableunstable

T = 7860 n = 0.35 cm-3 WNM

T = 85 n = 33 cm-3 CNM

Diffuse Gas Emission

Page 6: C +  As a Primary Coolant                            and Tracer of  Star Formation

= nT

158 mm

63 mm

Grain photoelectric

C II Cooling/H (CNM) > 10 CII Cooling/H (WNM)

PminPmax

** Note ** CNM in Thermal Balance:[CII] measures the total energy dumped into the gas.

Heating Rate = constn ZT [CII] = const

Wolfire et al. (2003)

Diffuse Gas Emission

Page 7: C +  As a Primary Coolant                            and Tracer of  Star Formation

Fraction of WNM/CNM ?

Dickey et al. 2009

CNM + WNM

CNM

[CNM + WNM]/CNM

Em

issi

on/L

Abs

orpt

ion/

LE

mis

sion

/Abs

orpt

ion

Heiles & Troland 2003: 60% WMN, 40% CNM locally in Galactic disk

Assume: 2/3 WNM, 1/3 CNM to outer galaxy

Page 8: C +  As a Primary Coolant                            and Tracer of  Star Formation

Mathis et al. 1982

Weingarter & Draine 2001 and

6eV

In diffuse ISM 10-20% of heating can come from PAH-

PAH + hn PAH+ + e-

PAH- + hn PAH + e-

2eV

Malloci et al. 2007

Page 9: C +  As a Primary Coolant                            and Tracer of  Star Formation

PDR Emission

Diffuse Gas

Classic PDRs

Orion PDR

[CII]

n

Kaufman et al. 1999 Kaufman et al. 1999

FUV

FUV

Heating Efficiency

G0/n = const

n

Page 10: C +  As a Primary Coolant                            and Tracer of  Star Formation

PDR Emission

Diffuse Gas

Classic PDRs

Orion PDR

n n

Kaufman et al. 1999 Kaufman et al. 1999

FUV

FUV

Heating Efficiency[OI]/[CII]

cr n[CII]

G0/n = const

Page 11: C +  As a Primary Coolant                            and Tracer of  Star Formation

Contribution from HII regionsTeff= 42000 K Abel et al 2005

Fraction of [CII]from HII region

Kaufman et al. 2006

Z=3Stellar association

Page 12: C +  As a Primary Coolant                            and Tracer of  Star Formation

Oberst et al. 2011

Carina Nebula

SPIFI[NII] 205 mm

ISO[CII]

30% [CII] diffuse ionised 70% [CII] neutral PDR

Oberst et al. 2006

Page 13: C +  As a Primary Coolant                            and Tracer of  Star Formation

Mookerjea et al. 2011 HerM33es

PACS [CII] [OI] M33 HII Region BCLMP 302

20-30% [CII] ionised gas80-70% [CII] neutral PDR

Page 14: C +  As a Primary Coolant                            and Tracer of  Star Formation

LMC-N 11B

Lebouteiller et al. 2012SHINING

5-15% [CII] diffuse ionised 95-85% [CII] neutral PDR

Page 15: C +  As a Primary Coolant                            and Tracer of  Star Formation

Bennett et al 1994, COBE FIRAS 7o beam Diffuse ionized gasWIM Emission

Wright et al. 1991 Line log L[C II] 158 mm 7.7[N II] 122 mm 6.9[N II] 205 mm 6.7[C I] 370 mm 5.5[C I] 610 mm 5.3

Page 16: C +  As a Primary Coolant                            and Tracer of  Star Formation

Bennett et al 1994, COBE FIRAS 7o beam

[CII]

[CII] from [NII]

[NII]

Diffuse ionized gas

Steiman-Cameron et al. 2010

Cygnus X

WIM Emission

Page 17: C +  As a Primary Coolant                            and Tracer of  Star Formation

What dominates the [CII] emission?

Galactic:WIM – Heiles 1994CNM – Bennett et al. 1994, Wolfire et al. 1995 GMC – Stacey et al. 1985; Shibai et al. 1991 Cubick et al 2008

What is the [CII] Budget ?

Beam size? galaxy type ? Metallicity ? Where ?

Extragalactic:

Cormier et al. 2012: Low Z galaxy Haro 11 – 10% PDR, 90% in diffuse ionized

Madden et al. 1997: Low Z galaxy IC 10 – 10% WIM, 10% CNM, 80% PDR with C+/H2

Malhotra et al. 2001: Normal Galaxies - 50% WIM, PDRs G0 = 102 - 104.5, n = 102 - 104.5

Page 18: C +  As a Primary Coolant                            and Tracer of  Star Formation

Stacey et al. 2010

[CII] and CO are excited by (nearby?) star formation

Page 19: C +  As a Primary Coolant                            and Tracer of  Star Formation

Aniano et al. 2012

Draine & Li 2007

NGC 6946 PACS 160 resolution

On the other hand……

~ 165 pc

Page 20: C +  As a Primary Coolant                            and Tracer of  Star Formation

Aniano et al. 2012

Low average U ~ 5, low fPDR < 20%

Wolfire, Hollenbach in prep: average U on GMCs ~10-30

Also Cubick et al. 2008, Pineda et al. 2010 found U < 100

Mechanical Heating?

Page 21: C +  As a Primary Coolant                            and Tracer of  Star Formation

Jenkins & Tripp 2011

Small Scale StructureTurbulent Dissipation in CNM

3800

Log normal fit + 0.05% 3x105 K cm-3

1)Warm diffuse cloud chemistry: CH+, HCO+

Godard et al. 2009, Falgarone et al. 2010

2)Tiny-Scale Atomic Structure (TSAS): HI absorption 10s AUe.g. Heiles 1997 (TSIS), (TSMS)

3)Warm diffuse H2 seen in emission Falgarone et al. 2005

Page 22: C +  As a Primary Coolant                            and Tracer of  Star Formation

Small Scale Structure (Continued)Turbulent Dissipation in CNM

4) High H2/PAH ratios seen in high latitude clouds. Ingalls et al. 2011

5)Warm H2 in MC surfaces (low UV field). Goldsmith et al. 2010, Habart et al. 2011

Habart et al. 2011

Spitzer H2 observationsModel Meudon PDR code

FUV field strength FUV field strength

L1721CaliforniaNGC 7023EHorseheadRho OphNGC 2023N

Page 23: C +  As a Primary Coolant                            and Tracer of  Star Formation

MHD shocks: Pineau des Forêts et al 1986

Shears: Joulain et al. 1998

TDRs – 100s AU:Godard et al. 2009

Turbulent Dissipation Region (TDR)

adiabatic cooling

Page 24: C +  As a Primary Coolant                            and Tracer of  Star Formation

de Looze et al. 2011

SFR

(24

mm +

FU

V)

ISO [CII]Herrera-Camus et al. 2013KINGFISH

PACS [CII]

~ 500 pc resolution

[CII]/ LIR ~ const + SFR based on LIR SFR([CII])

Sargsyan et al. 2012

Page 25: C +  As a Primary Coolant                            and Tracer of  Star Formation

extinction

opacity

cirrusL(Ha) true +IMF +Starbust99 =SFR

Kennicutt et al. 2009

Page 26: C +  As a Primary Coolant                            and Tracer of  Star Formation

L(Pa) true +IMF +Starbust99 =SFR

Calzetti et al. 2007

Page 27: C +  As a Primary Coolant                            and Tracer of  Star Formation

Herrera-Camus et al. 2013

Low [CII]/IR seen in AGN, regions of normal galaxies, and ULIRGs.

1)Grain charging2)Dust optical depth at 158 mm3)Dusty HII regions4)High density

Low [CII]/24 mm points do not measure SFR

Page 28: C +  As a Primary Coolant                            and Tracer of  Star Formation

de Looze et al. 2011

SFR

(24

mm +

FU

V)

ISO [CII]Herrera-Camus et al. 2013KINGFISH

PACS [CII]

~ 500 pc resolution

[CII]/ LIR ~ const + SFR based on LIR SFR([CII])

Sargsyan et al. 2012

Page 29: C +  As a Primary Coolant                            and Tracer of  Star Formation

SFR

[CII]

Hea

ting

Cooling

1)[CII] not dominated by high G0 - high n PDRs:[OI]/[CII] > 1 and lowheating efficiency

2)WIM/HII contribution is uncertain ~ 30%

3)[CII] mainly comes from low to moderate G0 and moderate n PDRs plus some neutral diffuse gas (mainly in outer galaxy).Keeps CII/CO relation and [CII] as a dominant coolant.

5)Mechanical heating does not dominate due to correlation with radiative tracers (24 mm)

4)Dust fits correct? [CII] comes mainly from low UV fields (everywhere in galaxy). [CII]/CO correlation? [OI] problem?

Page 30: C +  As a Primary Coolant                            and Tracer of  Star Formation

6)[CII] as SFR breaks down (or another calibration is needed – Sargsyan et al. 2012) for AGN and ULIRGs due to low [CII]/LIR