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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 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 • 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
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
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
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)
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
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
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
Submm Galaxies Plateau de Bure survey: most sources unresolved at >0.6” (Tacconi et al. 2005)
...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
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
Multiple CO Lines IRAM 30m CO SED survey (1, 2, 3mm bands) (Weiss, Walter, Downes, Henkel)
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.
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)
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
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
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
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!
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.
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)
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
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
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
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