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Molecular Gas in (very) Distant Galaxies

Molecular Gas in (very) Distant Galaxies. Fabian Walter (MPIA) F. Bertoldi, C. Carilli, P. Cox, K. Menten, A. Weiss. History of the Universe. recombination (z~1000). Cosmic ‘Dark Ages’ no stars/quasars. Epoch of Reionization (EoR). mass buildup. galaxies today. High Redshift Galaxies.

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Molecular Gas in (very) Distant Galaxies

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  1. Molecular Gas in (very) Distant Galaxies Fabian Walter (MPIA) F. Bertoldi, C. Carilli, P. Cox, K. Menten, A. Weiss

  2. History of the Universe recombination (z~1000) Cosmic ‘Dark Ages’ no stars/quasars Epoch of Reionization (EoR) mass buildup galaxies today

  3. High Redshift Galaxies • high redshift zoo: • - Lyman Break galaxies • - Lyman a galaxies • - Submm (‘SCUBA’) galaxies • - EROs • - DRG • - BzK galaxies • - faint blue galaxies • - Radio galaxies • - QSO host galaxies • science drivers: • - mass assembly / galaxy formation • - unified picture of galaxy evolution • - history of SFRD (‘Madau plot’) • / stellar mass assembly • - evolution(?) of MBH-s relation mm/submm observations: - detection/imaging of dust emission -> LFIR - detection/imaging of molecular lines -> molecular gas (‘SF reservoir’) -> dynamical masses -> major science drivers for all (sub)mm instruments

  4. Dust Imaging: The Magic of (Sub-)mm ~1mm obs: JCMT - SCUBA Zeus -> poster Hailey-Dunsheath CSO - SHARK-II Bolocam -> talk Glenn -> poster Aguirre 30m - MAMBO SMA PdBI ASTE APEX - LABOCA -> talk Menten 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

  5. Submm (‘SCUBA’) Sources Downes et al. 1999 Hughes et al. 1998 Source identification critical (usually through RC, Chapman ea. 03/04) 15” SCUBA SMA, Iono ea. 05, Peck ea. 05 -> poster

  6. Molecular Gas • first: detection of dust • molecular gas: fuel for SF • cold H2 invisible -> use CO as tracer • -> molecular gas mass, dynamical mass • n[CO(n-(n-1))] = (115GHz x n) / (1+z) z=6 -> CO(1-0): 3mm -> 2cm ! M51 - CO(2-1) SMA M 51 Sakamoto ea. 04 Matsushita ea. 04 • so far 2 major populations: - submm galaxies - QSO host galaxies [but also radio gal, BzK, ...] • problem: accurate z not known - faint in optical (submm gal.) - complex emission lines (QSO hosts)

  7. The Need for Bandwidth CO simulations (from M. Yun) EVLA/ALMA PdBI VLA • fractional BW: VLA: - 0.05 / 40GHz=0.001 [50MHz ~ 300 km s-1] PdBI: - 0.5 / 100GHz=0.005 --> (but upgrade ongoing) GBT: - 1.6 / 22 GHz = 0.08 SMA: - 2 / 230GHz = 0.01 CARMA: - 4 / 100 GHz= 0.04 EVLA: - 8 / 40GHz=0.2 ALMA - 8 / 100GHz=0.08 - 8 / 350GHz=0.02 future

  8. Molecular Gas at High z Object Type Redshift CO Ju TelescopeReference (... et al.) IRAS10214+4724 QSO* 2.28 3 6 12m 30m Brown 1991, Solomon 1992 SMM J16368+4057 SMM 2.385 3 7 PdB Neri 2003 53W002 QSO 2.39 3 OVRO PdB Scoville 1997, Alloin 2000 SMM J04431+0210 SMM 2.509 3 PdB Neri 2003 Cloverleaf QSO* 2.558 3 PdB Barvainis 1994 SMM J14011+0252 SMM* 2.565 3 7 OVRO PdB Frayer 1999, Downes 2003 PSS J1409+5628 QSO 2.56 3 PdB Beelen 2004 MG 0414-0534 QSO* 2.639 3 PdB Barvainis 1998 MS1512-cB58 LBG* 2.72 3 PdB Baker 2003 Q1230+1627B QSO* 2.74 3 PdB Guilloteau 1999 SMM J02399-0136 SMM* 2.808 3 OVRO PdB Frayer 1998, Genzel 2003 B3 J2330+3927 RG 3.094 4 PdB de Breuck 2003 MG 0751+2716 QSO* 3.20 4 PdB Barvainis 2002 SMM J09431+4700 SMM 3.346 4 PdB Neri 2003 TNJ0121+1320 RG 3.520 4 PdB de Breuck 2003 6C1909+722 RG 3.534 4 PdB Papadopoulos 2000 4C60.07 RG * 3.788 4 PdB Papadopoulos 2000 APM 08279+5255 QSO* 3.911 4 9 PdB Downes 1999 PSS J2322+1944 QSO* 4.119 12 45 PdB VLA Eb Cox 2002, Carilli 2002 BRI 0952-0115 QSO* 4.43 5 PdB Guilloteau 1999 BRI 1335-041 QSO 4.407 2 5 PdB VLA Guilloteau 1997, Carilli 2002 BRI 1202-0725 QSO 4.69 12 45 PdB VLA Eb Omont 96a, Ohta 96, Carilli 02 TN J0924-2201 RG 5.2 10 54 ATCA Klamer 05 SDSS J1148+5251 QSO 6.419 3 67 VLA PdB Walter 03/04, Bertoldi 2003 (*) definitely lensed, SMM=submm galaxy, RG=Radio Galaxy 13 QSO +5 SMM+4 RG+ 1 LBG = 23

  9. Submm Galaxies SMM J02396-0134 SMM J02399-0136 SMM J04431+0210 PdBI survey of CO(1-0) of SMM galaxies Greve ea. 2005 Neri ea. 2004 Genzel ea. 2003 SMM J09431+4700 SMM J13120+4242 SMM J14011+0252 SMM J16368+4057 SMM J16359+6612 SMM J16366+4105 MH2 ~ 3x1010 Msun large FWHM: mergers? -> double peak: rotation? Mdyn ~ 1 1011 Msun SMM J16371+4053 ERO J16450+4626 SMM J22174+0015

  10. Submm Galaxies Plateau de Bure survey: most sources unresolved at >0.6” (Tacconi et al. 2005)

  11. ...more Detections J1409: Hainline, Scoville ea. 2004 OVRO w/ COBRA (4GHz!) correlator -> CARMA TN J0924 - radio gal @ z=5.2 ATCA: Klamer ea. 2005 Sheth ea. 2004, Kneib ea. 2004

  12. ...but how about the physical conditions of gas?

  13. CO Line SEDs: gas excitation f(T) f(r) Multiple components 4.2 140 K 3.4 40 K 20 K 3.0 • turnover: measure of the CO excitation • shape is temperature/density dependent • shape: search for extended CO LVG input: n(H2), Tkin, [CO]/[H2]/dv/dr (fixed to 810-5 pc (km/s)-1) Weiss 2005

  14. Multiple CO Lines IRAM 30m CO SED survey (1, 2, 3mm bands) (Weiss, Walter, Downes, Henkel)

  15. CO(1-0) Transition: ‘cm’ Telescopes GBT z=4.7 z=3.9 Walter, Riechers, Knudsen ea. z=4.7 Effelsberg Bertoldi, Menten, Henkel ea.

  16. F10214 MG 0751 Cloverleaf PSS 1409 PSS 2322 APM 0827 Tkin~80 K, n(H2)~10 4.6 cm-3 SMM 16359 SMM 14011 Tkin~30–70 K, n(H2) ~ 10 3.3-4.2 cm-3 CO Line SEDs (I) • single gas component • QSO turnover: >6-5 • SMM turnover: 5-4 • compact (<1.5kpc) • no indication for extended comp. (Weiss, Walter, Downes, Henkel)

  17. Antennae M51 Arp220 Mrk 231 rCO ~200 pc rCO ~ 4kpc rCO ~ 500 pc rCO ~ 1.5kpc CO Line SEDs (II) Local starbursts: Tkin ~ 50 K, n(H2) ~ 10 4.0cm-3 merger of two spirals (r~ 4 kpc) -> if central gas concentration as in ULIRGs (200 pc), -> average molecular density rises by >2 orders of magnitudes

  18. Neutral Carbon (CI) Cloverleaf F10214 SMM 14011 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 Weiss, Downes, Walter, Henkel. 03, 04 BR1202: CII line Iono et al. 2005 (SMA) PSS2322: CI ( 1-0) IRAM PdBI Pety ea. 2004 -> poster

  19. High Density Tracer: HCN J1409+5628 L(FIR) F10214 - GBT(!) Solomon ea 2004 Gao & Solomon 2004 L(HCN) Carilli, Vanden Bout, Solomon, Walter ea. 2004 HCN(5-4) in APM08279: poster Wagg

  20. Resolution is Key ...so far - galaxy-integrated properties • ultimate goal: resolve CO emission spatially/kinematically • compare to optical/NIR imaging • dynamical masses! 1” ~ 7.5kpc [8.5 kpc @ z=2, 5.8 kpc @ z=6] -> need ~0.15” resolution to get 1 kpc resolution z=6.5 CO(7-6): 100 GHz (band 3): 4 km baselines z=2.5 CO(3-2): 100 GHz (band 3): 4 km baselines CO(6-5): 230 GHz (band 6): 1.8 km baselines -> high-res (0.15”) CO studies at high z need long baselines currently only doable with VLA!

  21. VLA imaging at 0.2” resolution BRI 1335-041 (z=4.407) - CO(2-1) observed at 7mm (Q band) 10 kpc VLA B array - 0.2” res. channel width: ~15 MHz (100 kms-1) Riechers, Walter, Carilli et al.

  22. ...out to the Epoch of Reionization...

  23. Gunn Peterson trough J1148+5251 - The Most Distant QSO J1148+5251 at z=6.4 (@ end of EoR) Fan et al. 2003, White et al. 2003 • 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)

  24. Molecular Gas @ End of EoR • molecular gas mass: • MH2 = 2 x 1010 Msun • mass in C and O: ~3x107 Msun • -> Pop III stars? CO(3-2) 46.6149 GHz continuum VLA z=6.419 Tkin=60K, nH2=104.5 cm-3 PdBI Walter et al. 2003 Bertoldi et al. 2003

  25. Resolved CO @ z=6.4 VLA B + C array; res.: 0.3” (~2 kpc) • assuming disk geometry: bmaj=3.6 kpc, vrot=280 kms-1 Mdyn~ 6 x 1010 Msun MBH=3 109 Msun -> Mbulge = few 1012 Msun? MBH-s breakdown? [Willot ea 2005: no companions -> low MDM, but M-s=f(z) ?] channel maps (width: 60 km s-1): Walter et al. 2004

  26. Other Tracers in 1148+5251 Carilli, Vanden Bout, Solomon, Walter ea. 2004 L(FIR) HCN(4-3) VLA Q-band (nondetection) Gao & Solomon 2004 L(HCN) L(HCN) CI (809 GHz) - observed at 109 GHz with PdBI: CII: (157 microns) - nondetection - JCMT (Bolatto ea. 2004) - detection (30m) (Maiolino et al. 2005) -> poster Bertoldi et al. 2005

  27. Summary • from ‘blobology’ -> real physics • molecular gas all the way back to the EoR! • CO SEDs: submm<->QSOs single T, no extended comp. high densities (not nec. high T) • CI, HCN detectable at high z • resolve high-z @ 1 kpc res. (~0.2”) • studies in very early universe (< 1Gyr): - metal enrichment, Mdyn - M-s(z) relation • so far: tip of the iceberg

  28. The End

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