1 / 30

C + As a Primary Coolant and Tracer of Star Formation

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.

mireya
Download Presentation

C + As a Primary Coolant and Tracer of Star Formation

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. C+ As a Primary Coolant and Tracer of Star Formation Dec 21st, 2012

  2. Heating SFR Cooling [CII]

  3. Sargsyan et al. 2012 [CII]/ LIR ~ const + SFR based on LIR SFR([CII]) SFR (24 mm + FUV) ISO [CII] de Looze et al. 2011 KINGFISH Herrera-Camus et al. 2013 ~ 500 pc resolution PACS [CII]

  4. NO Contributions to [CII] Line emission WNM NO Warm H T = 8000 K n = 0.3 cm-3 Warm H+ T = 8000 K Ne = 5 cm-3 WIM r~ 100s pc EUV r ~ 100s pc ? YES! C+/HI r ~ 10s pc CNM OB star Cold H T = 80 K n = 30 cm-3 H+ H+ FUV Cold H2 T = 10 K H+ NO r ~ few pc C+/H2 Classic PDR [CII] a dominant coolant? Maybe

  5. Diffuse Gas Emission Ionization: FUV, X-ray, C.R. Heating: P.E., C.R., X-ray/EUV Cooling: [CII], [OI], Lya, e- recombination WNM stable = nT CNM stable unstable nG = n2L T T = 7860 n = 0.35 cm-3 WNM T = 85 n = 33 cm-3 CNM Wolfireet al. (2003)

  6. Diffuse Gas Emission C II Cooling/H (CNM) > 10 CII Cooling/H (WNM) = nT Pmax Pmin ** Note ** CNM in Thermal Balance: [CII] measures the total energy dumped into the gas. Grain photoelectric 158 mm 63 mm Heating Rate = const n Z T [CII] = const Wolfireet al. (2003)

  7. Fraction of WNM/CNM ? CNM + WNM Emission/L Heiles & Troland 2003: 60% WMN, 40% CNM locally in Galactic disk CNM Absorption/L Assume: 2/3 WNM, 1/3 CNM to outer galaxy [CNM + WNM]/CNM Emission/Absorption Dickey et al. 2009

  8. PAH + hn PAH+ + e- 2eV 6eV PAH- + hn PAH + e- Mathis et al. 1982 In diffuse ISM 10-20% of heating can come from PAH- Weingarter & Draine 2001 and Malloci et al. 2007

  9. PDR Emission [CII] Heating Efficiency Orion PDR FUV FUV Classic PDRs G0/n = const n n Kaufman et al. 1999 Kaufman et al. 1999 Diffuse Gas

  10. PDR Emission [OI]/[CII] Heating Efficiency Orion PDR n[CII] cr FUV FUV Classic PDRs G0/n = const n n Kaufman et al. 1999 Kaufman et al. 1999 Diffuse Gas

  11. Contribution from HII regions Teff= 42000 K Abel et al 2005 Kaufman et al. 2006 Z=3 Stellar association Fraction of [CII] from HII region

  12. Oberst et al. 2011 Carina Nebula ISO [CII] SPIFI [NII] 205 mm Oberst et al. 2006 30% [CII] diffuse ionised 70% [CII] neutral PDR

  13. PACS [CII] [OI] M33 HII Region BCLMP 302 Mookerjea et al. 2011 HerM33es 20-30% [CII] ionised gas 80-70% [CII] neutral PDR

  14. LMC-N 11B Lebouteiller et al. 2012 SHINING 5-15% [CII] diffuse ionised 95-85% [CII] neutral PDR

  15. WIM Emission Diffuse ionized gas Bennett et al 1994, COBE FIRAS 7o beam 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

  16. WIM Emission Diffuse ionized gas Bennett et al 1994, COBE FIRAS 7o beam [CII] [CII] from [NII] Cygnus X [NII] Steiman-Cameron et al. 2010

  17. What is the [CII] Budget ? What dominates the [CII] emission? Beam size? galaxy type ? Metallicity ? Where ? Galactic: WIM – Heiles 1994 CNM – Bennett et al. 1994, Wolfire et al. 1995 GMC – Stacey et al. 1985; Shibai et al. 1991 Cubick et al 2008 Extragalactic: 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 Cormier et al. 2012: Low Z galaxy Haro 11 – 10% PDR, 90% in diffuse ionized

  18. Stacey et al. 2010 [CII] and CO are excited by (nearby?) star formation

  19. On the other hand…… Draine & Li 2007 NGC 6946 PACS 160 resolution ~ 165 pc Aniano et al. 2012

  20. 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? Aniano et al. 2012

  21. 3800 Small Scale Structure Turbulent Dissipation in CNM 1)Warm diffuse cloud chemistry: CH+, HCO+ Godard et al. 2009, Falgarone et al. 2010 2)Tiny-Scale Atomic Structure (TSAS): HI absorption 10s AU e.g. Heiles 1997 (TSIS), (TSMS) 3)Warm diffuse H2 seen in emission Falgarone et al. 2005 Jenkins & Tripp 2011 Log normal fit + 0.05% 3x105 K cm-3

  22. 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 Spitzer H2 observations Model Meudon PDR code L1721 California NGC 7023E Horsehead Rho Oph NGC 2023N FUV field strength FUV field strength Habart et al. 2011

  23. Turbulent Dissipation Region (TDR) MHD shocks: Pineau des Forêts et al 1986 Shears: Joulain et al. 1998 TDRs – 100s AU: Godard et al. 2009 adiabatic cooling

  24. Sargsyan et al. 2012 [CII]/ LIR ~ const + SFR based on LIR SFR([CII]) SFR (24 mm + FUV) ISO [CII] de Looze et al. 2011 KINGFISH Herrera-Camus et al. 2013 ~ 500 pc resolution PACS [CII]

  25. cirrus L(Ha) true + IMF + Starbust99 = SFR extinction opacity Kennicutt et al. 2009

  26. Calzetti et al. 2007 L(Pa) true + IMF + Starbust99 = SFR

  27. Low [CII]/IR seen in AGN, regions of normal galaxies, and ULIRGs. 1)Grain charging 2)Dust optical depth at 158 mm 3)Dusty HII regions 4)High density Low [CII]/24 mm points do not measure SFR Herrera-Camus et al. 2013

  28. Sargsyan et al. 2012 [CII]/ LIR ~ const + SFR based on LIR SFR([CII]) SFR (24 mm + FUV) ISO [CII] de Looze et al. 2011 KINGFISH Herrera-Camus et al. 2013 ~ 500 pc resolution PACS [CII]

  29. 1)[CII] not dominated by high G0- high n PDRs: [OI]/[CII] > 1 and low heating efficiency Heating SFR Cooling 2)WIM/HII contribution is uncertain ~ 30% [CII] 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. 4)Dust fits correct? [CII] comes mainly from low UV fields (everywhere in galaxy). [CII]/CO correlation? [OI] problem? 5)Mechanical heating does not dominate due to correlation with radiative tracers (24 mm)

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

More Related