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The Formation and Evolution of SMGs: A (mostly) Panchromatic View

The Formation and Evolution of SMGs: A (mostly) Panchromatic View. Desika Narayanan Harvard-Smithsonian Center for Astrophysics. The Team:. Chris Hayward. T.J. Cox . Josh Younger. Patrik Jonsson. Lars Hernquist. Discovery History. Barger et al., Hughes et al. .

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The Formation and Evolution of SMGs: A (mostly) Panchromatic View

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  1. The Formation and Evolution of SMGs:A (mostly) Panchromatic View Desika Narayanan Harvard-Smithsonian Center for Astrophysics The Team: Chris Hayward T.J. Cox Josh Younger Patrik Jonsson Lars Hernquist Desika Narayanan EVLA Conference

  2. Discovery History Barger et al., Hughes et al. Desika Narayanan EVLA Conference

  3. The Incredible Fluxes of SMGs: • Median Redshift z~2.4 (Chapman et al 2004) • Selected at S850 > 5 mJy, seen up to S850 ~ 20 mJy z~2.4 ~mJy source Desika Narayanan EVLA Conference (NED; Benford 1999)

  4. Where We’re at with SMGs: • Median Redshift z~2.4 (peak of cosmic BH and SFR activity) Chapman et al 2004 - though see recent z>4 detections by J. Younger et al. • LIR > 1013 L • SFR ~ 1000-3000 M/yr • Huge Masses: • DM: 5x1012 M (Blain et al. 2004) • H2: Gas rich ~1010 M(Greve et al., Tacconi et al.) • Stellar: ~1011 M (Swinbank et al., Lonsdale et al.) Similar to z~2 QSOs Desika Narayanan EVLA Conference

  5. Where We’re at with SMGs: SMGs are the most luminous, heavily star forming galaxies at the epoch of peak galaxy formation • Median Redshift z~2.4 (Chapman et al 2004) • Selected at S850 > 5 mJy, seen up to S850 ~ 20 mJy • Huge Masses: • DM: 5x1012 M (Blain et al. 2004) • H2: Gas rich ~1010 M(Greve et al., Tacconi et al.) • Stellar: ~1011 M (Swinbank et al., Lonsdale et al.) • SFR~ 2000 M/yr Desika Narayanan EVLA Conference

  6. The Theoretical Challenge (how do we catch up to the observers?): • What is a physical model for SMGs (how do we form them)? • How do they fit in an evolutionary scenario for hierarchical galaxy formation? (aka, how do we connect them to quasars?) Desika Narayanan EVLA Conference

  7. Clues for the Modelers: Physical Parameters massive galaxies (~few x 1011 Min stars) Merger? Disks? + Tacconi et al. 2008 Lonsdale et al. 2008 = 5-20 mJy SMGs? Desika Narayanan EVLA Conference

  8. Clues for the Modelers: • Off MBH-M* Relation? (Alexander et al. 2008) (Greve et al. 2004, Carilli & Wang 2006) • Huge CO Line Widths: (800 km/s : (maybe) ~ twice z~2 QSOs) Desika Narayanan EVLA Conference

  9. The Theoretical Challenge (how do we catch up to the observers?): • What is a physical model for SMGs (how do we form them)? • How do they fit in an evolutionary scenario for hierarchical galaxy formation? Desika Narayanan EVLA Conference

  10. The Theoretical Challenge: Forming SMGs Numerical Models: Merger models, diffuse ISM SAMs: Flat IMF: dn/dln(m) ~ m • What is a physical model for SMGs (how do we form them)?  S850---> Time---> S850---> (Baugh et al. 2004, Swinbank et al. 2008) (Chakrabarti et al. 2006) Desika Narayanan EVLA Conference

  11. Physics Included in Hydrodynamics: • -Full numerics: DM, Gas, Stars and BHs • -Multi-phase McKee-Ostriker ISM • Star formation follows KS relations • BH growth and associated AGN feedback • Supernovae pressurization of ISM • -Virial Properties of Galaxy disks scaled to z~3 • -Mergers and Isolated disks simulated • -Halo Masses: 1-5 x 1012 M GADGET (SPH) + SUNRISE (IR)+ Turtlebeach (Molecular Line) Go to http://www.cfa.harvard.edu/~dnarayan/Movies/ for the movies in the presentation Desika Narayanan EVLA Conference

  12. Narayanan et al. 2008 Desika Narayanan EVLA Conference

  13. Diffuse ISM GADGET (SPH) + SUNRISE (IR) + Turtlebeach (Molecular Line) GMC Physics Included in Monte Carlo IR RT: -IR transfer of stellar and AGN spectrum (starburst 99 for stars and Hopkins+ 07 for AGN) -dust radiative equilibrium -Kroupa IMF, MW Dust to Metals (0.4) -Stellar Clusters surrounded by placental GMCs (covering fraction is free parameter; fcover=0.3-1 measured in ULIRGs) Desika Narayanan EVLA Conference

  14. co co co GADGET (SPH) + SUNRISE (IR)+ Turtlebeach (Molecular Line) co co co co Narayanan et al. (2008) co Physics Included in Monte Carlo CO RT -Mass spectrum of GMCs included as SISs -Molecular statistical equilibrium (collisions and radiation) -Pressure-driven H2 formation/destruction (Blitz & Rosolowsky 2006) -Milky Way Abundances for CO Desika Narayanan EVLA Conference

  15. Opacity dominated by birth clouds during starburst Opacity dominated by diffuse dust during inspiral SMGs are Major Mergers at z~2 Desika Narayanan EVLA Conference Narayanan, Hayward, Cox et al. in prep. Narayanan, Hayward, Cox, Younger et al. submitted

  16. Low luminosity (~5 mJy) SMGs are smaller scale (~100-200 M/yr) starbursts. The most luminous (~20 mJy) SMGs are “maximal” high mass starbursts during final coalesence. Individual Spirals will have trouble reproducing anything except very low luminosity SMGs. Opacity dominated by birth clouds during starburst SMGs are Major Mergers at z~2 Opacity dominated by diffuse dust during inspiral Desika Narayanan EVLA Conference Narayanan, Hayward, Cox et al. in prep. Narayanan, Hayward, Cox, Younger et al. submitted.

  17. Pope et al. (2006) Kovacs et al. (2006) Model SED at z=2: Matching Observations Narayanan, Hayward, Cox, Younger et al. submitted Desika Narayanan EVLA Conference

  18. The Theoretical Challenge: • What is a physical model for SMGs (how do we form them)? • How do they fit in an evolutionary scenario for hierarchical galaxy formation? Are SMGs and quasars related? Desika Narayanan EVLA Conference

  19. √2 Narayanan, Cox, Hayward, Younger et al. in prep. The life of an SMG: Sub-mm, CO and B-band evolution Sub-mm Flux B-band Flux Coppin et al. 2008 virial = 225 km/s * 2.354 = 530 km/s FWHM escape ~ 225 km/s * 2.354 * √2 = 750 km/s FWHM Narayanan, Hayward, Cox et al. in prep. Desika Narayanan EVLA Conference

  20. Sub-mm Flux The Connection between SMGs and QSOs B-band Flux Time Scale between peak SMG phase and peak QSO phase: ~50 Myr - though note tons of overlap Narayanan, Hayward, Cox et al. in prep. Desika Narayanan EVLA Conference

  21. The MBH-M* Relation in SMGs and Quasars: Observed Quasars Shileds et al. SMGs Alexander et al. Desika Narayanan EVLA Conference

  22. The MBH-M* Relation in SMGs and Quasars: Modeled Time Desika Narayanan EVLA Conference

  23. The Trip Toward the Magorrian Relation: SMGs Models (DN, Hayward, Cox, Younger et al.) Observations (Alexander et al.) Desika Narayanan EVLA Conference

  24. Are High-z QSOs on the MBH-M* relation ? Quasars at z~6 Walter, Carilli et al. ~120 km/s  Quasars at z~2 Shields et al. 2006 Desika Narayanan EVLA Conference

  25. CO FWHM-QSO Luminosity Relation Optically Luminous LOSs have small CO FWHMs because of molecular disk formation Narayanan, Li et al. (2008) Desika Narayanan EVLA Conference

  26. Line widths of lower luminosity z~6 quasars Are observed to be broader (~600 km/s), consistent with large halo mases Carilli et al. (2007) Maiolino et al. (2007) Desika Narayanan EVLA Conference

  27. Potential Contribution from the eVLA: Morphologies of SMGs(does our merger-driven scenario work in real life?) Sub-mm flux Desika Narayanan EVLA Conference

  28. Contribution from the EVLA: True Line Width Distribution of QSOs Sub-mm flux Desika Narayanan EVLA Conference

  29. Conclusions • Merger-driven model can reproduce S850 5-20 mJy using only observationally motivated physical parameters • Sub-mm duty cycles, SEDs, CO fluxes and line widths naturally reproduced in a merger-driven model • SMGs evolve naturally into QSOs and then onto Magorrian Relation • Quasars may be selected to have face-on molecular disks Desika Narayanan EVLA Conference

  30. Coppin et al. 2008 QSOs QSOs may have preferentially face-on disks Sub-mm Flux SMGs Narayanan, Hayward, Cox et al. in prep. Narayanan et al. 2008 Desika Narayanan EVLA Conference

  31. Physics Included in Monte Carlo IR RT: -IR transfer of stellar and AGN spectrum (starburst 99 for stars and Hopkins+ 07 for AGN) -dust radiative equilibrium -Kroupa iMF, MW Dust to Gas -Stellar Clusters surrounded by placental GMCs (covering fraction is free parameter) Diffuse ISM GADGET (SPH) + SUNRISE (IR) + Turtlebeach (Molecular Line) GMC z = 2.5 SED input Desika Narayanan EVLA Conference

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