1 / 19

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)

eddy
Download Presentation

Millimetre Studies of High- z Quasars and Galaxies

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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

More Related