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Millimetre Studies of High- z Quasars and Galaxies

Millimetre Studies of High- z Quasars and Galaxies. Pierre Cox IRAM Grenoble, France. The spectrum of a ULIRG: a `field guide’. Non-thermal radio Thermal dust - Dominated luminosity - Hotter in AGN - Mid-IR spectral features (missing in AGN)

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Millimetre Studies of High- z Quasars and Galaxies

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  1. Millimetre Studies of High-z Quasars and Galaxies Pierre Cox IRAM Grenoble, France Venice

  2. The spectrum of a ULIRG: a `field guide’ • Non-thermal radio • Thermal dust • - Dominated luminosity • - Hotter in AGN • - Mid-IR spectral features • (missing in AGN) • Molecular and atomic lines • - mm CO/HCN • - far-IR: C/N/O • - mid-IR: C-C/C=C/H2 • Luminosities involved: 3x1011 <L/Lsun< 1014 From Blain (2003) Venice

  3. Deep Field Sources 15”/10” SCUBA/ MAMBO Source identification critical (usually through RC, Chapman et al. 2004) Pointed Observations - Sources selected from optical (SDSS) and radio (VLA): Quasars (radio-quiet), radio-galaxies - Position well known; redshifts known (1<z<6.4) Venice -> poster

  4. Tdust = 52 K Beta = 1.5 L_FIR = 4x1012 x S250(mJy) L_sun for z=0.5 to 8 SFR = 1400 x S250(mJy)M_sun/yr (very high) M_dust = 1.4x108 x S250(mJy) M_sun Beelen et al. 2005 Venice

  5. Venice

  6. CO Survey of submm Galaxies • 18 radio-detected submm galaxies with known optical/near-IR redshift detected in CO • 1<z<3.5 • Variety of profiles: 780+-230 km/s • Mergers/Rotating Disks • Star Formation Rate: 720 Msun/yr • MH2~ 3x1010 Msun • Mdyn ~ 1011 Msun • The submm-population consists of gas rich and massive, composite starbursts/AGN systems SMM J02396-0134 SMM J02399-0136 SMM J04431+0210 SMM J09431+4700 SMM J13120+4242 SMM J14011+0252 SMM J16368+4057 SMM J16359+6612 SMM J16366+4105 (Greve et al. 2005; Neri et al. 2004; Tacconi et al. 2006) Venice SMM J16371+4053 ERO J16450+4626 SMM J22174+0015

  7. Subarcsecond Imaging Results • < 0.5” (4 kpc)  Compact sources • Scaled-up versions and more gas-rich of the local ULIRG population • Central densities and potential well depths comparable to those of elliptical galaxies or massive bulges • Fulfill the criteria of maximal starbursts: initial gas reservoir 1010-11 Msun is converted to stars on a timescale ~3-10 tdynor a few 108 yr Tacconi, Neri, Chapmanm Genzel et al. (2006) Venice

  8. Gunn Peterson trough J1148+5251 - The Most Distant QSO at z=6.42 Fan et al. 2003; White et al. 2003 z-band (Keck – Djorgovski et al.) • z=6.42; age~870 Myr • one of the first luminous sources • MBH ~ 1-5 x 109 Msun (Willot et al. 2003) • Mdust ~ 108 Msun(Bertoldi et al. 2003) Dust continuum at 1.2 mm Venice

  9. CO(3-2) 46.6149 GHz PdBI continuum VLA Walter et al. 2003 Bertoldi et al. 2003 Venice

  10. Resolving the CO emission in J1148+5251 VLA A+B + C array; res.: 0.15” (~1 kpc) • Two sources separated by 0.3” (1.7 kpc at z=6.4) containing each 5 x 109 Msun • Not likely to be amplified • If gravitationally bound, MDyn=4.5x1010 Msun Walter et al. 2004 Venice

  11. Mass: • MH2 = 2 x 1010 Msun • Mdyn = 3 x 109 sin-2(i) Msun • Mass in C and O: ~3x107 Msun CO excitation in J1148+5251 (filled circles), compared to NGC 253 (dashed) LVG Model: Tkin= 100K, nH2=7x104 cm-3 Bertoldi et al. (2003) Venice

  12. Multiple CO Lines IRAM 30m CO multi-line survey (1, 2, 3mm bands) Weiss et al. (2006) Venice

  13. CO LVG solution: Disk radius: 1 kpc excellent agreement with lens models ! log(n(H2)) = 4.2 cm-3 Tkin = 30 K M(H2) = 8 1010 M L’CO(1-0) = 4.4 1010 K km/s pc2 Xco = 1.8 M/ K km/s pc2 LVG solution Cloverleaf Weiss et al. (2005)

  14. High Density Tracer: HCN J1409+5628 (z=2.56) High density tracer in starbursts: nH2> 10(5) cm(-3) APM08279+5255 APM08279+5255 (z=3.91) Gao & Solomon 2004 Carilli et al. (2004) Wagg et al. 2005 Venice

  15. High Density Tracer: HCO+ APM08279+5255 (z=3.91) L’(HCO+) = 4 x 1010K/(km/s pc2) HCO+(5-4)/HCN(5-4) ~ 1 Burillo et al. 2006 Venice

  16. Search for Neutral Carbon [CI] Cloverleaf (z=2.3) F10214 (z=2.3) SMM 14011 (z=2.5) CI ( 3P2-3P1 ) PdBI CI ( 3P1-3P0 ) 30m CI ( 3P1-3P0 ) 30m CI ( 3P1-3P0 ) 30m 2nd extra galactic CIratio L’CI(21) / L’CI(10)= 0.5, Tex = 30 K [CI]/H2 ~ 3 x 10(-5) PSS2322 (z=4.12) CI ( 3P1-3P0 ) PdBI Barvainis et al. 1997; Weiss et al. 2003, 2004; Pety et al. 2004 Venice

  17. [[CII] 158 microns emission line detected in J1148+5251 at z=6.42Probing the physics of a PDR at the end of the re-ionisation epoch CO(7-6) CII CI(1-0) Venice

  18. [CII] in J1148+5251 • Done at the 30-meter • Massive starburst (2000 Msun/yr) • Significant metal enrichment • The ratio of the [CII] line luminosity to the total far-infrared luminosity is about 0.06%, i.e. an order of magnitude smaller than has been observed locally • One of the 3 key scientific goals of the ALMA project. Maiolino, Cox et al. (2005) Venice

  19. Conclusions • Physics and (chemistry) of the ISM in the early Universe • CO measurements  physical conditions of the dense, warm (40-100 K) gas in star-forming galaxies at high redshifts: massive (1010 M), compact (<4 kpc), dense (104 cm-3) and enriched (abundances ~ solar) • Detection of species other than CO: HCN, HCO+, [CI] and [CII] • Some sources have been resolved with 1 kpc (~0.2”) • Studies in the very early universe (< 1 Gyr): • - Metal enrichment • - Dynamical masses Venice

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