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Radio Observations of Massive Galaxy and Black Hole Formation in the Early Universe

Explore the formation of massive galaxies and supermassive black holes within a billion years of the Big Bang through radio observations and spectroscopic imaging of molecular gas. Investigate host galaxy properties of high-redshift quasars, pushing the boundaries of cosmic reionization studies.

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Radio Observations of Massive Galaxy and Black Hole Formation in the Early Universe

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  1. Radio observations of massive galaxy and black hole formation in the early Universe Chris Carilli (NRAO) MPIA, Heidelberg, Aug 7, 2009 • Introductory remarks • Massive galaxy and SMBH formation within 1 Gyr of Big Bang: dust, gas, and star formation in quasar host galaxies at z~6 • Future: probing normal galaxy formation with the next generation telescopes • Collaborators: Ran Wang, Walter, Menten, Cox, Bertoldi, Omont, Strauss, Fan, Wagg, Riechers, Wagg, Neri

  2. SDSS J1148+5251 z=6.42 • Why quasar hosts at highest z? • Spectroscopic redshifts • Extreme (massive) systems MB < -26 Lbol ~ 1e14 Lo MBH ~ 1e9 Mo • Rapidly increasing samples: z>5: > 100 z>6: > 20 • Radio only current method for probing host galaxies [Note: MBH derived from Ledd, MgII width, other; eg. Kurk, Fan] Host galaxy CO 3-2 VLA 1”=5.5kpc

  3. 0.9um Gunn-Peterson effect toward z~6 SDSS QSOs • Pushing into the tail-end of cosmic reionization => sets benchmark for first luminous structure formation • GP effect => study of ‘first light’ is restricted to obs> 1um Fan 05

  4. QSO host galaxies – MBH -- Mbulge relation Haaring & Rix 2004 MBH=0.0014 Mbulge • Most (all?) low z spheroidal galaxies have SMBH • ‘Causal connection between SMBH and spheroidal galaxy formation’ • Luminous high z QSOs have massive host galaxies (1e12 Mo)

  5. M82 radio-FIR SED All mechanisms massive star formation rate Thermal dust 20 -- 70K Synchrotron Radio-FIR Free-Free SFR (Mo/yr) = 3e-10 LFIR (Lo/yr) SFR (Mo/yr) = 6e-29 L1.4 (erg/s/Hz)  = 0.8 Mo (K km s-1 pc2)-1

  6. Plateau de Bure Interferometer High res imaging at 90 to 230 GHz rms < 0.1mJy, res < 0.5” MAMBO at 30m 30’ field at 250 GHz, rms < 0.3 mJy Very Large Array 30’ field at 1.4 GHz rms< 10uJy, 1” res High res imaging at 20 to 50 GHz rms < 0.1 mJy, res < 0.2” • Spectroscopic imaging of molecular gas, fuel for star formation in galaxies: gas mass, ISM conditions, dynamics • Fine structure lines: dominant ISM gas coolant • Dust + synchrotron imaging: cm-to-mm SEDs => obscuration-free star formation rates, ISM conditions, AGN

  7. Dust and star formation MAMBO 250GHz surveys 1/3 of z>2 quasars have S250 > 2mJy HyLIRG 1e13 Lo 2.4mJy • Wang sample: 33 z>5.7 quasars (mostly SDSS) • LFIR ~ 0.3 to 1.3 x1013 Lo ~ HyLIRG (47K, β = 1.5) • Mdust ~ 1.5 to 5.5 x108Mo ~ 10x MW (κ125um = 19 cm2 g-1)

  8. Dust formation at tuniv<1Gyr? • AGB Winds ≥ 1.4e9yr > tuniv = 0.87e9yr => dust formation associated with high mass star formation? (Dwek, Shull, Nozawa) • or ‘smoking quasars’: dust formed in BLR winds (Elvis) • Extinction toward z=6.2 QSO and 6.3 GRB => larger, silicate + amorphous carbon dust grains formed in core collapse SNe vs. eg. graphite? SMC, z<4 quasars Galactic z=6.2 quasar, GRB Maiolino, Stratta

  9. Dust heating by starburst or AGN?

  10. Radio to near-IR SED • FIR excess = 47K dust • Radio-FIR SED consistent with star forming galaxy Elvis SED TD ~ 1000K TD = 47 K Radio-FIR correlation

  11. Radio-FIR correlation SFR ~ 400 to 2000 Mo/yr

  12. D Anti-correlation of FIR luminosity and Lya EW D Dust => Log EW < 1.5 No dust => Log EW > 1.5 D D D No D D D D

  13. Molecular gas = fuel for star formation: 8 CO detections at z ~ 6 with PdBI, VLA

  14. High z quasar hosts vs. submm galaxies SMG QSO • Quasars: Mmed = 3e10 Mo, FWHMmed = 413 km s-1 • SMG (z~2.3): Mmed = 2e10 Mo, FWHMmed = 565 km s-1

  15. CO excitation: Dense, warm gas -- thermally excited to 6-5 Tk = 50 K nH2 = 104.2 cm-3 J1148 J1048 GMC (50pc) ~ 100 to 2000 cm-3 GMC cores (<1pc) > 104 cm-3

  16. LFIR vs L’(CO): ‘integrated Kennicutt-Schmidt law’ • Star formation efficiency(SFR/Mgas) increases with increasing SFR • Gas depletion timescale(Mgas/SFR) decreases with SFR • Need imaging! • Gas resupply is required to form GE ~ 1012 M* SFR 1e3 Mo/yr Index=1.5 1e11 Mo Mgas FIR ~ 1e10 Lo/yr => tdep~ 3e8yr FIR ~ 1e13 Lo/yr => tdep ~ 1e7yr

  17. 1148+52 z=6.42: VLA imaging at 0.15” resolution CO3-2 VLA IRAM 0.3” 1” ~ 5.5kpc + • Size ~ 6 kpc • Double peaked 2kpc separation, each ~ 1kpc, M(H2)~ 5 x109 Mo • TB ~ 35 K ~ starburst nuclei

  18. Gas surface density GMC core ~ 1pc GMC ~ 50pc

  19. CO rotation curves: QSO host galaxy dynamics at high z CO 2-1 2322+1944, z=4.2 Molecular Einstein ring Riechers et al. 2008 50 km/s channels

  20. 2322+1944 CO rotation curve: lens inversion and QSO host galaxy dynamics Riechers + 08 • Galaxy dynamical mass (r<3kpc) ~ 4.4e10 Mo • M(H2) ~ 1.7e10 Mo

  21. Break-down of MBH -- Mbulge relation at very high z Use CO rotation curves to get host galaxy dynamical mass High z QSO hosts Low z QSO hosts Other low z galaxies Perhaps black holes form first? but Lauer Bias for optically selected quasars Riechers +

  22. Mbh/Mdyn vs. inclination for z=6 QSOs Low z relation All must be face-on: i < 20o Need imaging!

  23. [CII] 158um • Dominant ISM gas cooling line (Spitzer 1976) • Traces CNM and PDRs • z>4 => FS lines observed in (sub)mm bands; z>6 => Bure! COBE => [CII] 10 to 100x more luminous than any other mm to FIR line in Galaxy (Bennett et al.)

  24. [CII] 158um search in z > 6.2 quasars IRAM 30m [CII] 1” [NII] • J1148+5251 z=6.42 • S[CII] = 10mJy • L[CII] = 4x109 Lo(L[NII] < 0.1L[CII] ) • J1623+3112 z=6.25 • S[CII] = 3mJy • S250GHz < 1mJy Kundsen, Bertoldi, Walter, Maiolino +

  25. ‘Maximal star forming disk’ (Walter + 2009) 1” PdBI, 0.25”res • [CII] size ~ 1.5 kpc => SFR/area ~ 1000 Mo yr-1 kpc-2 (vs. SMGs ~ 50) • Maximal starburst: (Thompson, Quataert, Murray 2005) • Self-gravitating gas disk • Vertical disk support by radiation pressure on dust grains • ‘Eddington limited’ SFR/area ~ 1000 Mo yr-1 kpc-2 • eg. Arp 220 on 100pc scale, Orion on 0.1pc scale

  26. [CII] z >4 • [CII]/FIR decreases with LFIR = lower gas heating efficiency due to charged dust grains => luminous starbursts are still hard to detect in C+ • Normal star forming galaxies are not much harder to detect • HyLIRG at z> 4: no worse than ULIRG at low z => lower metalicity? • Don’t pre-select on dust Maiolino, Bertoldi, Knudsen, Iono, Wagg…

  27. Summary of cm/mm detections at z>5.7: 33 quasars J1425+3254 CO at z = 5.9 J1048 z=6.23 PdBI, VLA • Only direct probe of host galaxies of most distant quasars • 11 in dust => Mdust > 1e8 Mo: Dust formation in SNe? • 8 in CO => Mgas > 1e10 Mo: Fuel for star formation in galaxies • 10 at 1.4 GHz continuum: radio loud AGN fraction ~ 8% • Radio – FIR SED => SFR ~ 1000 Mo/yr • 2 in [CII] => maximal star forming disk: 1000 Mo yr-1 kpc-2

  28. Building a giant elliptical galaxy + SMBH at tuniv< 1Gyr 10 • Multi-scale simulation isolating most massive halo in 3Gpc^3 • Stellar mass ~ 1e12 Mo forms in series (7) of major, gas rich mergers from z~14, with SFR 1e3 Mo/yr • SMBH of ~ 2e9 Mo forms via Eddington-limited accretion + mergers • Evolves into giant elliptical galaxy in massive cluster (3e15 Mo) by z=0 6.5 Li, Hernquist et al. • Rapid enrichment of metals, dust in ISM (z > 8) • Rare, extreme mass objects: ~ 100 SDSS z~6 QSOs on entire sky • Integration times of hours to days to detect HyLIGRs

  29. Pushing to ‘normal galaxies’ during reionization, eg. z=5.7 Ly galaxies in COSMOS Murayama et al. 07 NB850nm • SUBARU: LySFR ~ 10 Mo/yr • 100 sources in 2 deg-2 in z ~ 5.7 +/- 0.05 • Stacking analysis (100 LAEs) • MAMBO: S250 < 2mJy => SFR<300 • VLA: S1.4 < 2.5uJy => SFR<125 => Need order magnitude improvement in sensitivity at radio through submm wavelengths in order to study earliest generation of normal galaxies.

  30. What is EVLA? First steps to the SKA-high • By building on the existing infrastructure, multiply ten-fold the VLA’s observational capabilities, including: • 10x continuum sensitivity (<1uJy) • full frequency coverage (1 to 50 GHz) • 80x BW (8GHz)

  31. What is ALMA? North American, European, Japanese, and Chilean collaboration to build & operate a large millimeter/submm array at high altitude site (5000m) in northern Chile -> order of magnitude, or more, improvement in all areas of (sub)mm astronomy, including resolution, sensitivity, and frequency coverage. 50 x 12m array Atacama Compact Array 12x7m + 4x12m TP

  32. J1148 in 24hrs with ALMA • Detect multiple lines, molecules per band => detailed astrochemistry • Image dust and gas at sub-kpc resolution – gas dynamics, K-S • LAE, LBGs: detect dust, molecular, and FS lines in 1 to 3 hrs

  33. Key role for EVLA: total gas masses from low order CO z=6 [CII] Not excited? 6-5 3-2 Dannerbauer et al. 2009 reionization Normal galaxies may not have high order lines excited, in particular for dense gas tracers like HCN, HCO+ (critical densities > 106 cm-3). EVLA crucial for low order transitions => total gas mass

  34. Pushing to normal galaxies: spectral lines Arp220 z=5 cm telescopes: low order molecular transitions -- total gas mass, dense gas tracers (sub)mm: high order molecular lines. fine structure lines -- ISM physics, dynamics • FS lines will be workhorse lines in the study of the first galaxies with ALMA. • Study of molecular gas in first galaxies will be done primarily with cm telescopes

  35. Pushing to normal galaxies: continuum A Panchromatic view of 1st galaxy formation Arp 220 vs z cm: Star formation, AGN (sub)mm Dust, FSL, mol. gas Near-IR: Stars, ionized gas, AGN

  36. EVLA Status • Antenna retrofits now > 50% completed. • Early science start in Q1 2010, using new correlator • proposal deadline Oct 1, 2009 for shared-risk obs • 2GHz BW • 20 to 50 GHz complete • 8 GHz correlator ready in late 2010 • Full receiver complement completed 2012.

  37. Antennas, receivers, correlator in production: best submm receivers and antennas ever! • Site construction well under way: Observation Support Facility, Array Operations Site, antenna pads AOS Technical Building Array operations center Antenna commissioning in progress • North American ALMA Science Center (C’Ville): support early science Q4 2010, full ops Q4 2012

  38. END ESO

  39. Break-down of radio-FIR correlation: inverse Compton losses off CMB? IC losses off CMB dominate synchrotron in nuclear starbursts at z>4 IC losses dominate in normal galaxies at z>0.5 dEe/dt  UB, U

  40. [CII] 158um • Dominant ISM gas cooling line (Spitzer 1976) • Traces CNM and PDRs • z>4 => FS lines observed in (sub)mm bands

  41. Comparison to low z quasar hosts z=6 quasars IRAS selected Stacked mm non-detections PG quasars Hao et al. 2005

  42. Massive galaxies form most of their stars quickly, at high z ‘specific star formation rates’ = SFR/M* ‘active star formation’ tH-1 ‘red and dead’ ‘Downsizing’ Zheng+

  43. GBT limits on CO in z>6 LAE Wagg + 2009 Even with strong lensing (4.5x) and optimistic α (0.8): M(H2) < 5x109 Mo => still 2x MW gas masses

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