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Studying the gas, dust, and star formation in the first galaxies at cm and mm wavelengths

Studying the gas, dust, and star formation in the first galaxies at cm and mm wavelengths Chris Carilli, KIAA-PKU reionization workshop, July 2008. QSO host galaxies at z ~ 6: massive galaxy and SMBH hole formation within 1Gyr of the Big Bang Pushing to normal galaxies with ALMA and the EVLA.

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Studying the gas, dust, and star formation in the first galaxies at cm and mm wavelengths

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  1. Studying the gas, dust, and star formation in the first galaxies at cm and mm wavelengths Chris Carilli, KIAA-PKU reionization workshop, July 2008 • QSO host galaxies at z ~ 6: massive galaxy and SMBH hole formation within 1Gyr of the Big Bang • Pushing to normal galaxies with ALMA and the EVLA USA – Carilli, Wang, Wagg, Fan, Strauss Euro – Walter, Bertoldi, Cox, Menten, Omont

  2. Why QSO hosts? • Spectroscopic redshifts • Extreme (massive) systems MB < -26 => Lbol> 1e14 Lo MBH > 1e9 Mo • Rapidly increasing samples: z>4: > 1000 known z>5: 80 z>6: 15 Fan 05

  3. Magorrian, Tremaine, Gebhardt, Merritt… QSO host galaxies – MBH -- Mbulge relation • Most (all?) low z spheroidal galaxies have SMBH: MBH=0.002 Mbulge • ‘Causal connection between SMBH and spheroidal galaxy formation’ • Luminous high z QSOs have massive host galaxies (1e12 Mo)

  4. MAMBO surveys of z>2 QSOs 1e13 Lo 2.4mJy • 1/3 of luminous QSOs have S250 > 2 mJy, independent of redshift from z=1.5 to 6.4 • LFIR ~ 1e13 Lo(HyLIRG) ~ 0.1 x Lbol: Dust heating by starburst or AGN?

  5. Dust => Gas: LFIR vs L’(CO) z ~ 6 QSO hosts Star formation rate 1e3 Mo/yr Index=1.5 1e11 Mo Gas Mass • non-linear => increasing SF eff (SFR/gas mass) with increasing SFR • Massive gas reservoirs > 1010 Mo > 10 x MW

  6. Pushing into reionization: QSO 1148+52 at z=6.4 • Highest redshift SDSS QSO (tuniv = 0.87Gyr) • Lbol = 1e14 Lo • Black hole: ~3 x 109 Mo (Willot etal.) • Gunn Peterson trough (Fan etal.)

  7. 1148+52 z=6.42: Dust detection MAMBO 250 GHz 3’ S250 = 5.0 +/- 0.6 mJy LFIR = 1.2e13 Lo Mdust =7e8 Mo Dust formation? • AGB Winds ≥ 1.4e9yr > tuniv = 0.87e9yr => dust formation associated with high mass star formation:Silicate gains (vs. eg. Graphite) formed in core collapse SNe (Maiolino 07)?

  8. 1148+52 z=6.42: Gas detection VLA CO3-2 VLA IRAM PdBI 1” ~ 5.5kpc + • Size ~ 5.5 kpc • M(H2) ~ 2e10 Mo • ‘Fuel for galaxy formation’ • FWHM = 305 km/s • z = 6.419 +/- 0.001 • Mgas/Mdust ~ 30 (~ starburst galaxies)

  9. 1148+5251 Radio to near-IR SED TD = 50 K Elvis SED Radio-FIR correlation • FIR excess = 50K dust • Radio-FIR SED follows star forming galaxy • SFR ~ 3000 Mo/yr

  10. CO excitation ladder 2 NGC253 Dense, warm gas: CO thermally excited to 6-5, similar to starburst nucleus Tkin > 80 K nH2 ~ 1e5 cm^-3 MW

  11. 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? Riechers +

  12. Atomic fine structure lines: [CII] 158um at z=6.4 • Dominant ISM gas coolant = star formation tracer • z>4 => FS lines observed in (sub)mm bands • [CII] size ~ 6kpc ~ molecular gas => distributed star formation • SFR ~ 6.5e-6 L[CII] ~ 3000 Mo/yr Plateau de Bure IRAM 30m [CII] 1” [NII] [CII] + CO 3-2

  13. [CII] -- the good and the bad • [CII]/FIR decreases rapidly with LFIR (lower heating efficiency due to charged dust grains?) => luminous starbursts are still difficult to detect in C+ • Normal star forming galaxies (eg. LAEs) are not much harder to detect! J1623 z=6.25 Malhotra + 2000

  14. [CII] in J1623+3111 at z = 6.25 FIR-weaker QSO Host S250 < 1mJy => FIR < 3e12 Lo => Dust detection should not be a prerequisite for [CII] search Bertoldi + 2008

  15. Summary of cm/mm detections at z>5.7: 33 quasars J1425+3254 CO at z = 5.9 • Only direct probe of host galaxies • 10 in dust => Mdust > 1e8 Mo • 5 in CO => Mgas > 1e10 Mo • 10 at 1.4 GHz continuum: • -- SFR > 1000 Mo/yr • -- Radio loud AGN fraction ~ 6% • 2 in [CII] => SFR > 1000 Mo/yr Current Plateau de Bure is routinely detecting ~ 1mJy lines, and 0.1 mJy continuum at 90GHz!

  16. Building a giant elliptical galaxy + SMBH at tuniv < 1Gyr 10 10.5 • Multi-scale simulation isolating most massive halo in 3Gpc^3 (co-mov) • Stellar mass ~ 1e12 Mo forms in series (7) of major, gas rich mergers from z~14, with SFR ~ 1e3 - 1e4 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 • Generally consistent with ‘downsizing’ Li, Hernquist, Roberston.. 8.1 6.5 • 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

  17. Pushing to ‘normal galaxies’ during reionization, eg. z=5.7 Ly galaxies in COSMOS NB850nm Murayama et al. 07 • SUBARU: Ly ~ 10 Mo/yr • 100 deg^-2 in z ~ 5.7 +/- 0.05

  18. Pushing to ‘normal galaxies’ during reionization, eg. z=5.7 Ly galaxies in COSMOS • Stacking analysis (100 LAEs) • MAMBO: <S250> < 2mJy => SFR<300 • VLA: <S1.4> < 2.5uJy => SFR<125 • Still factor 10 away from SFR(Lya) VLA Stacking analysis Need order magnitude improvement in sensitivity at radio through submm wavelengths in order to study earliest generation of normal galaxies.

  19. What is EVLA? First steps to the SKA 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) Status • Antenna retrofits now 50% completed. • Early science in 2010, using new correlator. • Full receiver complement completed 2012.

  20. 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

  21. ALMA into reionization • Spectral simulation of J1148+5251 • Detect dust emission in 1sec (5) at 250 GHz • Detect [CII] in minutes • Detect multiple lines, molecules per band => detailed astrochemistry • Image dust and gas at sub-kpc resolution – gas dynamics CO HCO+ HCN CCH LAE, LBGs: ALMA will detect dust, molecular, and FS lines in 1 to 3 hours in normal galaxies at z ~ 6

  22. Pushing to normal galaxies: spectral lines 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

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

  24. Array operations center at 5000m AOS Technical Building Japanese antennas at 3000m

  25. ALMA Status • Antennas, receivers, correlator fully prototyped, now in production: best (sub)mm receivers and antennas ever! • Site construction well under way: Observation Support Facility and Array Operations Site • North American ALMA Science Center (C’Ville): gearing up for science commissioning and early operations • Timeline Q1 2007: First fringes at ATF (Socorro) Q1 2009: Three antenna array at AOS Q2 2010: First call for (early science) proposals Q4 2010: Start early science (16 antennas) Q4 2012: Full operations ESO

  26. END ESO

  27. Pushing uJy radio studies to z>2: Cosmos LBG, BzK, and LAE samples • 8500 LBGs (U,B,V) identified, z~ 3, 4, 5 • 100 LAE in NB850 filter z = 5.7 • 30,000 BzK star forming galaxies z ~ 1.5 to 2 • ‘normal’ galaxy population at high redshift?

  28. J1000+0234 -- V-drop+radio ID: most distant submm galaxy Ha + IR: high extinction • V-drop, z>4.5 • S1.4 = 45 uJy • S230 = 5 ± 1.4 mJy • Keck spectrum => starburst galaxy at z = 4.52 • Most distant, spectroscopically confirmed submm galaxy (the next most distant at z=3.6) • Complex optical/IR morphology: varying extinction 1” UV knot+ Lya Capak + Figure 5 - A color image of J1000+0234 with radio contours

  29. J1000+0234 -- V-drop+radio ID: most distant submm galaxy VLA CO 2-1 VLA 1.4 GHz ACS • CO/radio continuum coincident with a dust-lane seen rest frame UV image • Gass mass ~ 2e10 Mo= fuel for galaxy formation • Massive galaxy forming from a merging system, SFR ~ 3000 Mo/yr • Comparison to uv-derived SFR => uv extinction factor ~100

  30. LBG Stacking (SKA Science without the SKA) • Find the average properties of our “non-detections” using stacking: reduces noise by ~ √N. • Mean stacking: exclude 3, 4 sources: significantly affects results • Median stacking does not require source exclusion, and is more robust calculation (see FIRST analysis by White et. al, 2006)

  31. U-Dropouts (2.5 < z < 3.5) • <SFRuv> ~ 17 Mo/yr • <SFRrad> ~ 31 Mo/yr • UV either extinction ~ factor 2 (vs. standard LBG factor 5) • or Radio-FIR correlation fails at high z? Median Flux Density = 0.90+/-0.21 Jy

  32. BzK galaxies: Star forming galaxies at z~ 1.5 to 2 (Pannella et al) Star forming galaxies with stellar masses ~ 1e10 to 1e11 Mo SFR ~ 30 -- 50 Moyr

  33. 1.4 GHz vs. Stellar Mass Stacking detections ~ 2 to 9 +/- 0.2 uJy

  34. 1.4 GHz vs. B-z

  35. Specific star formation rate (= SFR/M*) vs. stellar mass: radio vs. UV data • Radio: no dust-bias => SSFR ~ constant w. M* • UV not corrected for dust: more massive SF galaxies with higher SFR are also more extincted Radio SFR UV SFR

  36. 1.4GHz vs. BAB

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