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

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

4. L _FIR = 4x10 12 x S 250 (mJy) L _sun for z=0.5 to 8 SFR = 1400 x S 250 (mJy)M _sun /yr (very high) M _dust = 1.4x10 8 x S 250 (mJy) M _sun 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

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

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

7. CO simulations (from M. Yun) The Need for Bandwidth   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 PdBI VLA EVLA/ALMA

8. Object TypeRedshiftCO J u Telescope Reference (... 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*2.723PdBBaker 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* 4.11912 45 PdB VLA Eb Cox 2002, Carilli 2002 BRI 0952-0115 QSO* 4.435 PdB Guilloteau 1999 BRI 1335-041 QSO 4.407 2 5 PdB VLAGuilloteau 1997, Carilli 2002 BRI 1202-0725 QSO 4.69 12 45 PdB VLA Eb Omont 96a, Ohta 96, Carilli 02 TN J0924-2201 RG5.210 54ATCAKlamer 05 SDSS J1148+5251 QSO 6.419 3 67 VLA PdBWalter 03/04, Bertoldi 2003 (*) definitely lensed, SMM=submm galaxy, RG=Radio Galaxy 13 QSO + 5 SMM + 4 RG + 1 LBG = 23 Molecular Gas at High z

9. PdBI survey of CO(1-0) of SMM galaxies Greve ea. 2005 Neri ea. 2004 Genzel ea. 2003 M H2 ~ 3x10 10 M sun large FWHM: mergers? -> double peak: rotation? M dyn ~ 1 10 11 M sun SMM J02396-0134SMM J02399-0136SMM J04431+0210 SMM J09431+4700SMM J13120+4242SMM J14011+0252 SMM J16368+4057SMM J16359+6612SMM J16366+4105 SMM J16371+4053ERO J16450+4626SMM J22174+0015 Submm Galaxies

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

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

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

13. CO Line SEDs: gas excitation turnover: measure of the CO excitation shape is temperature/density dependent shape: search for extended CO f(T) f(  ) LVG input: n(H 2 ), T kin, [CO]/[H 2 ]/dv/dr (fixed to 810 -5 pc (km/s) -1 ) Multiple components Weiss 2005 20 K 40 K 140 K 3.0 3.4 4.2

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

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

16. single gas component QSO turnover: >6-5 SMM turnover: 5-4 compact (<1.5kpc) no indication for extended comp. Cloverleaf F10214MG 0751 PSS 1409PSS 2322APM 0827 SMM 14011 SMM 16359 CO Line SEDs (I) T kin ~80 K, n(H 2 )~10 4.6 cm -3 T kin ~30–70 K, n(H 2 ) ~ 10 3.3-4.2 cm -3 (Weiss, Walter, Downes, Henkel)

17. Local starbursts: T kin ~ 50 K, n(H 2 ) ~ 10 4.0 cm -3 CO Line SEDs (II) M51 Antennae Arp220 Mrk 231 r CO ~ 4kpc r CO ~ 1.5kpc r CO ~ 500 pc r CO ~200 pc 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. 2 nd extra galactic CI ratio L’ CI(21) / L’ CI(10) = 0.5, T ex = 30 K CI ( 3 P 2 - 3 P 1 ) PdBI CI ( 3 P 1 - 3 P 0 ) 30m CI ( 3 P 1 - 3 P 0 ) 30m CI ( 3 P 1 - 3 P 0 ) 30m F10214CloverleafSMM 14011 Neutral Carbon (CI) BR1202: CII line Iono et al. 2005 (SMA) PSS2322: CI ( 1-0 ) IRAM PdBI Pety ea. 2004 Weiss, Downes, Walter, Henkel. 03, 04 -> poster

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

20. 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 Resolution is Key...so far - galaxy-integrated properties currently only doable with VLA! ultimate goal: resolve CO emission spatially/kinematically - - compare to optical/NIR imaging - - dynamical masses!

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

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

23. J1148+5251 - The Most Distant QSO J1148+5251 at z=6.4 (@ end of EoR) Gunn Peterson trough Fan et al. 2003, White et al. 2003   z=6.42; age~870 Myr   one of the first luminous sources   M BH ~ 1-5 x 10 9 M sun (Willot et al. 2003)   M dust ~ 10 8 M sun (Bertoldi et al. 2003)

24. Molecular Gas @ End of EoR Walter et al. 2003 Bertoldi et al. 2003 CO(3-2) 46.6149 GHz continuum  molecular gas mass: M H2 = 2 x 10 10 M sun M H2 = 2 x 10 10 M sun  mass in C O: ~3x10 7 M sun  mass in C and O: ~3x10 7 M sun -> Pop III stars? -> Pop III stars? VLA PdBI z=6.419 T kin =60K, n H2 =10 4.5 cm -3

25. VLA B + C array; res.: 0.3” (~2 kpc) Resolved CO @ z=6.4  assuming disk geometry: b maj =3.6 kpc, v rot =280 kms -1 b maj =3.6 kpc, v rot =280 kms -1 M dyn ~ 6 x 10 10 M sun M dyn ~ 6 x 10 10 M sun M BH =3 10 9 M sun -> M bulge = few 10 12 M sun ? M BH -  breakdown? [Willot ea 2005: no companions -> low M DM, but M-  =f(z) ?] channel maps (width: 60 km s -1 ): Walter et al. 2004

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

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, M dyn - M-  (z) relation so far: tip of the iceberg

28. The End