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HerCULES

HerCULES. Lorentz Centre February 28, 2012. Introducing HerCULES. Herschel Comprehensive (U)LIRG Emission Survey Open Time Key Program on the Herschel satellite. Who is HerCULES ?. Jesus Mart ín-Pintado (Madrid) Joe Mazzarella (IPAC) Rowin Meijerink (Leiden)

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HerCULES

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  1. HerCULES Lorentz Centre February 28, 2012

  2. Introducing HerCULES Herschel Comprehensive (U)LIRG Emission Survey Open Time Key Program on the Herschel satellite HerCULES

  3. Who is HerCULES? Jesus Martín-Pintado (Madrid) Joe Mazzarella (IPAC) RowinMeijerink (Leiden) David Naylor (Lethbridge) Padelis Papadopoulos (Bonn) Dave Sanders (U Hawaii) Giorgio Savini (Cardiff/UCL) Howard Smith (CfA) Marco Spaans (Groningen) Luigi Spinoglio (Rome) Gordon Stacey (Cornell) Sylvain Veilleux (U Maryland) Cat Vlahakis (Leiden/Santiago) Fabian Walter (MPIA) Axel Weiß (MPIfR) Martina Wiedner (Paris) ManolisXilouris (Athens) Paul van derWerf (Leiden; PI) Susanne Aalto (Onsala) Lee Armus (Spitzer SC) VassilisCharmandaris (Crete) KalliopiDasyra (CEA) Aaron Evans (Charlottesville) Jackie Fischer (NRL) Yu Gao (Purple Mountain) Eduardo González-Alfonso (Henares) Thomas Greve (Copenhagen) Rolf Güsten (MPIfR) Andy Harris (U Maryland) Chris Henkel (MPIfR) Kate Isaak (ESA) Frank Israel (Leiden) Carsten Kramer (IRAM) Edo Loenen (Leiden) Steve Lord (NASA Herschel SC) HerCULES

  4. LIR/LCO  SFR/MH2  SFE (Gao & Solomon 2001) LIR SFR Conditions in ULIRGs • Starbursts cannot • be simply scaled up. • More intense starbursts are also more efficient with their fuel. HerCULES

  5. (U)LIRGs (LIR>10(11)12L) (Evans et al.) HerCULES

  6. (U)LIRGs from low to high z • LIRGs dominate cosmic star formation at high redshift (Magnelliet al. 2011) HerCULES

  7. ISM in luminous high-z galaxies (Danielson et al. 2010) (Weiß et al. 2007) • Even in ALMA era, limited spatial resolution on high-z galaxies. • For unresolved galaxies, multi-line spectroscopy will be a key diagnostic HerCULES

  8. HerCULES in a nutshell • HerCULES will uniformly and statistically measure the neutral gas cooling lines in a flux-limited sample of 29 (U)LIRGs. • Sample: • all IRAS RBGS ULIRGs with S60 > 12.19 Jy (6 sources) • all IRAS RBGS LIRGs with S60 > 16.8 Jy (23 sources) • Observations: • SPIRE/FTS full high-resolution scans: 200 to 670 m at R ≈ 600, covering CO 4—3 to 13—12 and [CI] + any other bright lines • PACS line scans of [CII] and both [OI] lines • All targets observed to same (expected) S/N • Extended sources observed at several positions HerCULES

  9. HerCULES sample HerCULES

  10. Mrk231 • At z=0.042, one of the closest QSOs (DL=192 Mpc) • With LIR = 41012 L , the most luminous ULIRG in the IRAS Revised bright Galaxy Sample • “Warm” infrared colours • Star-forming disk (~500 pc radius) + absorbed X-ray nucleus • Face-on molecular disk, MH2 ~ 5109 M HST/ACS (Evans et al., 2008) HerCULES

  11. Warning: may contain... • quiescent molecular (and atomic) gas • star-forming molecular gas (PDRs) • AGN (X-ray) excited gas (XDRs) • cosmic ray heated gas • shocks • mechanically (dissipation of turbulence) heated gas • warm very obcured gas (hot cores) HerCULES

  12. Mrk231SPIREFTS (Van der Werf et al., 2010) HerCULES

  13. Mrk231SPIREFTS HerCULES

  14. Mrk231SPIREFTS HerCULES

  15. Mrk231SPIREFTS HerCULES

  16. Mrk231SPIREFTS HerCULES

  17. Mrk231SPIREFTS HerCULES

  18. Mrk231SPIREFTS HerCULES

  19. CO excitation 2 PDRs + XDR 6.4:1:4.0 n=104.2, FX=28* n=103.5, G0=102.0 n=105.0, G0=103.5 * 28 erg cm-2 s-1 G0=104.2 HerCULES

  20. CO excitation 3 PDRs6.4:1:0.03 n=106.5, G0=105.0 n=103.5, G0=102.0 n=105.0, G0=103.5 HerCULES

  21. High-J lines: PDR or XDR? • High-J CO lines can also be produced by PDR with n=106.5 cm—3 and G0=105, containinghalf the molecular gas mass. • Does this work? • G0=105 only out to 0.3 pc from O5 star; then we must havehalf of the molecular gas and dust in 0.7% of volume. • With G0=105,50% of the dust mass would be at 170K, which is ruled out by the Spectral Energy Distribution • [OH+] and [H2O+] > 10—9 in dense gas requires efficient and penetrative source of ionization;PDR abundances factor 100—1000 lower Only XDR model works! HerCULES

  22. Analysis of analysis • Model not unique • At least 9 free parameters, not really a proper fit • Reasonable, based on prior knowledge • External constraints available for all 3 components ... but what if we did not have this prior knowledge? • role of H2O • role of shocks • role of OH+ HerCULES

  23. Modeling-free result Highly excited CO ladders are found in all high luminosity/compact sources with an energetically dominant AGN (and only in those sources). HerCULES

  24. Water in molecular clouds • H2O ice abundant in molecular clouds • Can be released into the gas phase by UV photons, X-rays, cosmic rays, shocks,... • Can be formed directly in the gas phase in warm molecular gas • Abundant, many strong transitions  expected to be major coolant of warm, dense molecular gas Herschel image of (part of) the Rosetta Molecular Cloud HerCULES

  25. H2O in HerCULES red = wet HerCULES

  26. H2O lines in Mrk231 • Low lines: pumping by cool component + some collisional excitation • High lines: pumping by warm component • Radiative pumping dominates and reveals an infrared-opaque (100m ~ 1) disk. (González-Alfonso et al., 2010) HerCULES

  27. Lessons from H2O (1 + 2 + 3 + 4) 2) Radiatively H2O lines reveal extended infrared-opaque circumnuclear gas disks. 3) Extinction and radiative pumping of highest CO lines. 1) In spite of high luminosities, H2O lines are unimportant for cooling the warm molecular gas. 4) Detection of H2O lines implies high FIR radiation field, but not the presence of an AGN. HerCULES

  28. Lessons from H2O (5) Radiation pressure from the strong IR radiation field: Since both 100 and Td are high,radiation pressure dominates the gas dynamics in the circumnuclear disk. 5) Conditions in the circumnuclear molecular disk are Eddington-limited. HerCULES

  29. Mechanical feedback • Radiation pressure can drive the observed molecular outflows (e.g., Murray et al., 2005) • Aalto et al., 2012: flow prominent in HCN  dense gas • Key process in linking ULIRGs and QSOs? • Shocks probably of minor importance in Mrk231 (Fischer et al., 2010) HerCULES (Feruglioet al., 2010)

  30. NGC6240: CO lines as tracers of what? • X-ray nuclei  AGNs? • PAH emission  PDRs? • H2 lines  shocks! • NB: FTS shows 12CO/13CO > 50 ! Optically thin CO lines HerCULES

  31. NGC253: shocks or PDRs? • chemistry  shocks? • H2 lines  PDRs! SINFONI H2v=10 S(1), Rosenberg et al., in prep. HerCULES

  32. NGC7469SPIREFTS:CO ladder suggests PDR? HerCULES

  33. NGC7469SPIREFTS:OH+ suggests XDR? HerCULES

  34. NGC7469SPIREFTS:OH+ suggests XDR?But no H2O+... HerCULES

  35. High-z connection (1): H2O at z=3.9 Van der Werf et al., 2011 • Line ratios similar to Mrk231 • FIR pumping dominates, implies 100 m-opaque disk • Radiation pressure dominates, Eddington-limited HerCULES

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