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An IRAM PdBI CO Survey of Luminous Submm Galaxies A spearhead project for ALMA

An IRAM PdBI CO Survey of Luminous Submm Galaxies A spearhead project for ALMA. Thomas R. Greve (Caltech). R. Genzel (MPE), R. J. Ivison (ROE), R. Neri (IRAM), I. Smail (Durham), S. Chapman (Caltech), A. W. Blain (Caltech), F. Bertoldi (MPIfR), L. Tacconi (MPE), P. Cox (Orsay),

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An IRAM PdBI CO Survey of Luminous Submm Galaxies A spearhead project for ALMA

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  1. An IRAM PdBI CO Survey of Luminous SubmmGalaxiesA spearhead project for ALMA Thomas R. Greve (Caltech) R. Genzel (MPE), R. J. Ivison (ROE), R. Neri (IRAM), I. Smail (Durham), S. Chapman (Caltech), A. W. Blain (Caltech), F. Bertoldi (MPIfR), L. Tacconi (MPE), P. Cox (Orsay), A. Omont (AIP) IDA Meeting, Copenhagen 20-21 Dec. 2004

  2. Outline • A Brief History of CO at high z • Why CO? • High-z CO detections to date • An interferometric CO survey of (sub)mm galaxies (SMGs) • Duty cycle and current status • Bulk gas properties of SMGs • Comparison with ULIRGs • Implications for galaxy formation models • Conclusions and future directions IDA Meeting, Copenhagen 20-21 Dec. 2004

  3. High-z CO detections to date • 13 QSOs, including IRAS F10214+4714 the first ever high-z CO detection (Brown & Vanden Bout 1991) • 6 High-z Radio Galaxies (HzRGs) • 1 Lyman Break Galaxy (LBGs) IDA Meeting, Copenhagen 20-21 Dec. 2004

  4. High-z CO detections to date Omont et al. (1996) z=4.69 • 13 QSOs, including IRAS F10214+4714 the first ever high-z CO detection (Brown & Vanden Bout 1991) • 6 High-z Radio Galaxies (HzRGs) • 1 Lyman Break Galaxy (LBGs) IDA Meeting, Copenhagen 20-21 Dec. 2004

  5. High-z CO detections to date Omont et al. (1996) z=4.69 • 13 QSOs, including IRAS F10214+4714 the first ever high-z CO detection (Brown & Vanden Bout 1991) • 6 High-z Radio Galaxies (HzRGs) • 1 Lyman Break Galaxy (LBGs) De Breuck et al. (2003) z=3.52 IDA Meeting, Copenhagen 20-21 Dec. 2004

  6. High-z CO detections to date Omont et al. (1996) z=4.69 • 13 QSOs, including IRAS F10214+4714 the first ever high-z CO detection (Brown & Vanden Bout 1991) • 6 High-z Radio Galaxies (HzRGs) • 1 Lyman Break Galaxy (LBGs) De Breuck et al. (2003) z=3.52 Baker et al. (2003) z=2.73 IDA Meeting, Copenhagen 20-21 Dec. 2004

  7. High-z CO detections to date Omont et al. (1996) • 13 QSOs, including IRAS F10214+4714 the first ever high-z CO detection (Brown & Vanden Bout 1991) • 6 High-z Radio Galaxies (HzRGs) • 1 Lyman Break Galaxy • QSOs+HzRGs show strong CO emission from extended (~10kpc) starburst regions • Typical gas and dynamical masses of ~1x1011Mo • Co-eval growth of stellar bulges and massive black holes • Rapid enrichment before z~7 De Breuck et al. (2003) Baker et al. (2003) IDA Meeting, Copenhagen 20-21 Dec. 2004

  8. High-z CO detections to date Omont et al. (1996) • 13 QSOs, including IRAS F10214+4714 the first ever high-z CO detection (Brown & Vanden Bout 1991) • 6 High-z Radio Galaxies (HzRGs) • 1 Lyman Break Galaxy • QSOs+HzRGs show strong CO emission from extended (~10kpc) starburst regions • Typical gas and dynamical masses of ~1x1011Mo • Co-eval growth of stellar bulges and massive black holes • Rapid enrichment before z~7 However, most high-z CO detections are a mixed bag of non-uniformly selected (and often strongly lensed) QSOs and HzRGs De Breuck et al. (2003) Baker et al. (2003) IDA Meeting, Copenhagen 20-21 Dec. 2004

  9. High-z CO detections to date Omont et al. (1996) • 13 QSOs, including IRAS F10214+4714 the first ever high-z CO detection (Brown & Vanden Bout 1991) • 6 High-z Radio Galaxies (HzRGs) • 1 Lyman Break Galaxy • QSOs+HzRGs show strong CO emission from extended (~10kpc) starburst regions • Typical gas and dynamical masses of ~1x1011Mo • Co-eval growth of stellar bulges and massive black holes • Rapid enrichment before z~7 However, most high-z CO detections are a mixed bag of non-uniformly selected (and often strongly lensed) QSOs and HzRGs. SMGs: 2+1 sources detected in CO prior to our survey. De Breuck et al. (2003) Baker et al. (2003) IDA Meeting, Copenhagen 20-21 Dec. 2004

  10. L2 L1 Dec. (2000) R.A. (2000) 1s SMMJ02399-0136 (z=2.81) Ivison et al. 1998, MNRAS 298, 583 Frayer et al. 1998, ApJ, 506, L7 Genzel et al. 2003, ApJ, 584, 633 Mdyn(R<8kpc) ~ 2-3x1011 MO Most of which is baryonic IDA Meeting, Copenhagen 20-21 Dec. 2004

  11. SMMJ14011+0252 (z=2.51) Ivison et al. 2001 ApJ 561, L45 Frayer et al. 1999, ApJ, 514, L13 Downes & Solomon 2003 ApJ 582, 37 IDA Meeting, Copenhagen 20-21 Dec. 2004

  12. An IRAM PdBI CO Survey of SMGs(Genzel, Ivison, Neri, Bertoldi, Blain, Chapman, Cox, Greve, Neri, Omont, Smail, Tacconi) We are undertaking a first systematic CO survey of dust-enshrouded starburst galaxies at high redshifts Bright (S850>5mJy) submm-selected galaxies detected in the radio. This population is responsible for ~25% of the submm background. IDA Meeting, Copenhagen 20-21 Dec. 2004

  13. An IRAM PdBI CO Survey of SMGs(Genzel, Ivison, Neri, Bertoldi, Blain, Chapman, Cox, Greve, Neri, Omont, Smail, Tacconi) Duty-cycle and current status: We are undertaking a first systematic CO survey of dust-enshrouded starburst galaxies at high redshifts • SCUBA/MAMBO sources with VLA 1.4GHz counterparts (Lockman E, ELAIS N2, SSA 22, SSA13, HDF-N etc). • Keck follow-up spectroscopy with LRIS-B: ~70 redshifts, <z>=2.4 IDA Meeting, Copenhagen 20-21 Dec. 2004

  14. Keck (LRIS-B + NIRSPEC) spectroscopy Chapman et al. (2003) Ivison et al. (2002) IDA Meeting, Copenhagen 20-21 Dec. 2004

  15. An IRAM PdBI CO Survey of SMGs Duty-cycle and current status: • SCUBA/MAMBO sources with VLA 1.4GHz counterparts (Lockman E, ELAIS N2, SSA 22, SSA13, HDF-N etc). • Keck follow-up spectroscopy with LRIS-B: ~70 redshifts, <z>=2.4 • PdBI follow-up for redshift confirmation (2-3 tracks each) • High-resolution PdBI follow-up for spatially resolved CO dynamics IDA Meeting, Copenhagen 20-21 Dec. 2004

  16. An IRAM PdBI CO Survey of SMGs Duty-cycle and current status: • SCUBA/MAMBO sources with VLA 1.4GHz counterparts (Lockman E, ELAIS N2, SSA 22, SSA13, HDF-N etc). • Keck follow-up spectroscopy with LRIS-B: ~70 redshifts, <z>=2.4 • PdBI follow-up for redshift confirmation (2-3 tracks each) • High-resolution PdBI follow-up for spatially resolved CO dynamics • Status winter 2004: 7 (+1) new CO detections, 6 non-detections - the number of SMGs detected in CO almost tripled! IDA Meeting, Copenhagen 20-21 Dec. 2004

  17. An IRAM PdBI CO Survey of SMGs First resultsNeri et al. (2003) z=2.380 z=2.509 z=3.349 IDA Meeting, Copenhagen 20-21 Dec. 2004

  18. An IRAM PdBI CO Survey of SMGs Greve et al. (2005) IDA Meeting, Copenhagen 20-21 Dec. 2004

  19. An IRAM PdBI CO Survey of SMGs ID Transition zspec zCO FWHM ICOOur Detections km/s Jy km/sSMMJ02396-0134 (2-1) 1.062+-0.001 1.062+-0.002 780+-60 3.4+- 0.3SMMJ13120+4242 (4-3) 3.405+-0.001 3.408+-0.002 530+-50 1.7+- 0.3 SMMJ16366+4105 (3-2) 2.454+-0.001 2.450+-0.002 870+-80 1.8+- 0.3SMMJ16371+4053 (3-2) 2.374+-0.001 2.380+-0.004 830+-130 1.0+- 0.2 SMMJ22174+0015 (3-2) 3.098+-0.002 3.099+-0.004 780+-100 0.8+- 0.2 SMMJ04431+0210 (3-2) 2.5092+-0.0008 2.5094+-0.0002 350+-60 1.4+-0.2SMMJ09431+4700 (4-3) 3.349+-0.001 3.3460+-0.0001 420+-50 1.1+-0.1 SMMJ16368+4057 (3-2) 2.380+-0.002 2.3853+-0.0014 840+-110 2.3+-0.2 (7-6) . . . 2.383+-0.002 . . . 1.1+- 0.2Non-detectionsSMMJ10523+5722 (3-2) 2.611+-0.001 2.5901 - 2.6119 . . . < 0.5SMMJ10524+5724 (3-2) 3.036+-0.001 3.0593 - 3.0318 . . . < 0.8SMMJ12360+6210 (3-2) 1.994+-0.001 1.9865 - 2.0015 . . . < 0.9SMMJ13123+4239 (3-2) 2.320+-0.001 2.3115 - 2.3300 . . . < 1.0SMMJ16363+4055 (3-2) 2.283+-0.001 2.2676 - 2.2919 . . . < 0.4SMMJ16363+4056 (2-1) 1.495+-0.001 1.4802 - 1.5001 . . . < 0.8Literature sourcesSMMJ02399-0136 (3-2) 2.803+-0.003 2.808+-0.002 710+-80 3.0+- 0.4 (3-2) . . . 2.8076+-0.0002 >1100 3.1+-0.4SMMJ14011+0252 (3-2) 2.562+-0.002 2.5653+-0.0003 200+-40 2.4+-0.3 (3-2) . . . 2.5652+-0.0001 190+-11 2.8+-0.3 (7-6) . . . 2.5651+-0.0002 170+-30 3.2+-0.5SMMJ16359+6612 (3-2) 2.5165+-0.0015 2.5168+-0.0003 500+-100 3.5+-0.1 (3-2) . . . 2.5174+-0.0002 500+-100 2.50+-0.12EROJ16450+4626 (2-1) 1.443+-0.001 1.439+-0.001 400+-20 1.40+-0.10 (5-4) . . . 1.440+-0.001 380+-20 1.35+-0.10 (1-0) . . . . . . . . . 0.6+-0.1

  20. An IRAM PdBI CO Survey of SMGs z=1.062 z=2.803 z=2.509 Genzel et al. (2003) Greve et al. (2005) Neri et al. (2003) z=3.349 z=3.405 z=2.562 Neri et al. (2003) Greve et al. (2005) Downes & Solomon (2003) Greve et al. (2005) IDA Meeting, Copenhagen 20-21 Dec. 2004

  21. An IRAM PdBI CO Survey of SMGs z=2.380 z=2.517 z=2.454 Neri et al. (2003) Kneib et al. (2004) Greve et al. (2005) z=3.098 z=1.439 z=3.098 Greve et al. (2005) Andreani et al. (2000) Greve et al. (2005) Greve et al. (2005) IDA Meeting, Copenhagen 20-21 Dec. 2004

  22. An IRAM PdBI CO Survey of SMGs • 7 (+1) out of 13 (+1): detection rate of 54-57%. Remarkably good - comparable to the radio-ID fraction. • This confirms the <z>=2.4 redshift distribution of the bright, radio-detected SMG population (Chapman et al. 2003). IDA Meeting, Copenhagen 20-21 Dec. 2004

  23. An IRAM PdBI CO Survey of SMGs • 7 (+1) out of 13 (+1): detection rate of 53-57%. Remarkably good - comparable to the radio-ID fraction. • This confirms the <z>=2.3 redshift distribution of the bright, radio-detected SMG population (Chapman et al. 2003). Greve et al. (2005) IDA Meeting, Copenhagen 20-21 Dec. 2004

  24. An IRAM PdBI CO Survey of SMGs • 7 (+1) out of 13 (+1): detection rate of 54-57%. Remarkably good - comparable to the radio-ID fraction. • This confirms the <z>=2.4 redshift distribution of the bright, radio-detected SMG population (Chapman et al. 2003). • H provides much more reliable estimate of the systemic (CO) redshift: V(CO-Ly) V(CO-H) blueshifted: 5 0 redshifted : 2 0 zero offset : 1 4 IDA Meeting, Copenhagen 20-21 Dec. 2004

  25. An IRAM PdBI CO Survey of SMGs Bulk gas properties: CO luminosity: <LCO>=(3.8+-2.0)x1010K km/s 4x ULIRGs Gas masses (including HI+He): <Mgas>=(3.0+-1.6)x1010MO 4x ULIRGs So SMGs contains 3-4x more gas than local ULIRGs. Depletion of Gas as the merger progresses (Gao et al. 1999)? Detection rate: z>2.4 : 5/7 (71%) z<2.4 : 2/6 (33%) Is this evidence for evolution in gas mass content? Greve et al. (2005) IDA Meeting, Copenhagen 20-21 Dec. 2004

  26. An IRAM PdBI CO Survey of SMGs Starformation efficiency: • SMGs extend the (non-linear) FIR-CO correlation to higher z and luminosities SMGs: <LFIR/LCO>=(450+-170) LO MO-1 ULIRGs: <LFIR/LCO>=(180+-130) LO MO-1 • Starformation efficiency might be higher in SMGs than in ULIRGs • Tentative evidence of a FIR-CO correlation within the SMG sample itself log(LCO) = 0.6 log(LFIR) + 2.4 Greve et al. (2005) IDA Meeting, Copenhagen 20-21 Dec. 2004

  27. An IRAM PdBI CO Survey of SMGs Starformation efficiency: • SMGs extend the (non-linear) FIR-CO correlation to higher z and luminosities SMGs: <LFIR/LCO>=(450+-170) LO MO-1 ULIRGs: <LFIR/LCO>=(180+-130) LO MO-1 • Starformation efficiency might be higher in SMGs than in ULIRGs • Tentative evidence of a FIR-CO correlation within the SMG sample itself Greve et al. (2005) IDA Meeting, Copenhagen 20-21 Dec. 2004

  28. An IRAM PdBI CO Survey of SMGs Dynamical masses: • The double horn profiles are indicative of ordered orbital motion: either circum-nuclear disk or a merger. • Assuming: 1) a conservative source size of D=0.5” (~3.7kpc at z=2.3) 2) random orbital inclinations (factor of /4) 3) Merger model* <Mdyn>SMG = (1.2+-1.5) x 1011MO * Toomre stability criterion: Q = vsG 1 for a gaseous disk to be stable. We find Q << 1 for Mgas=3x1010MO and R~4kpc. IDA Meeting, Copenhagen 20-21 Dec. 2004

  29. An IRAM PdBI CO Survey of SMGs Dynamical masses: • Velocity dispersion of SMGs is comparable to that of HzRGs and 3-4x that of ULIRGs. • Assuming Mdyn ~ R2, and ULIRGs: Mdyn(R<0.6kpc) ~ 6x109MO, we find SMGs: Mdyn(R<0.6kpc) ~ 4x1010MO • The large line widths of SMGs strongly suggest that they are massive systems - with Mdyn comparable to HzRGs. Greve e al. (2005) IDA Meeting, Copenhagen 20-21 Dec. 2004

  30. An IRAM PdBI CO Survey of SMGs Gas mass fractions: • Gas fraction: SMGs : Mgas/Mdyn ~ 0.3 ULIRGs: ~ 0.16 (Downes & Solomon 1998) • So SMGs appear to be more gas-rich than local ULIRGs, although this is subject to uncertainties in the CO-H2 conversion factor and dynamical mass estimates. But overall there is mounting evidence that SMGs are neither high-z replicas of local ULIRGs, nor simply scaled up versions. Rather SMGs are more gas-rich and seem to form stars more efficiently (caveat: CO doesn’t trace the dense starforming gas, HCN does!) IDA Meeting, Copenhagen 20-21 Dec. 2004

  31. An IRAM PdBI CO Survey of SMGs Gas consumption time-scale and baryonic masses: • The median starformation rate is <SFR>=720 MO yr-1, hence the duration of the ‘SCUBA/MAMBO’-phase is:  = M(H2)/SFR ~ 40Myr • This is a lower limit since it assumes continuous starformation and ignores negative feedback and the possibility of HI falling in from outer regions. IDA Meeting, Copenhagen 20-21 Dec. 2004

  32. An IRAM PdBI CO Survey of SMGs Gas consumption time-scale and baryonic masses: • The median starformation rate is <SFR>=720 MO yr-1, hence the duration of the ‘SCUBA/MAMBO’-phase is:  = M(H2)/SFR ~ 40Myr • This is a lower limit since it assumes continuous starformation and ignores negative feedback and the possibility of HI falling in from outer regions. • The median V-band restframe luminosity is 2 x 1011LO, which implies median stellar mass of M* ~ 3 x 1010 MO (Smail et al. 2004). So the typical baryonic mass is Mbar ~ 6 x 1010 MO - comparable to the masses of local L* galaxies. And SMGs are baryon-dominated in their inner regions: Mbar/Mdyn ~ 0.5. Assembling that much baryonic matter so early is a severe challenge for models! IDA Meeting, Copenhagen 20-21 Dec. 2004

  33. Implications for Models of Galaxy Formation A fundamental test-bed for galaxy formation models is the assembly of massive baryonic galaxies. Co-moving number density of Mbar = 6 x 1010MO is n(M>Mbar) ~ 5 x 10-6 Mpc-3 Corrected for our CO detection Fraction (0.53) and finite survey volume. Greve et al. (2005) IDA Meeting, Copenhagen 20-21 Dec. 2004

  34. Implications for Models of Galaxy Formation A fundamental test-bed for galaxy formation models is the assembly of massive baryonic galaxies. Co-moving number density of Mbar = 6 x 1010MO is n(M>Mbar) ~ 5 x 10-6 Mpc-3 Corrected for our CO detection Fraction (0.53) and finite survey volume. This is a lower limit since we must correct for the finite life time of SMGs: (2.0-3.5)/SMG = 1.5Gyr/(40-200)Myr = 8-38 5x1010Mo 1011Mo 7x1010Mo Greve et al. (2005) IDA Meeting, Copenhagen 20-21 Dec. 2004

  35. High-resolution PdBI observations of SMGs- a taste of ALMA SMMJ09431+4700: H6 + H7 (both radio sources) are part of the same physical structure - separation 22kpc 1.3mm continuum, beam 0.7”x0.6” Tacconi et al. in prep. IDA Meeting, Copenhagen 20-21 Dec. 2004

  36. High-resolution PdBI observations of SMGs- a taste of ALMA SMMJ09431+4700: CO(4-3) is detected in H7 (but not H6). Tentative evidence for a blueshifted filament of gas between H7+H6. Tacconi et al. in prep. IDA Meeting, Copenhagen 20-21 Dec. 2004

  37. High-resolution PdBI observations of SMGs- a taste of ALMA SMMJ09431+4700: CO(4-3) is detected in H7 (but not H6). Tentative evidence for a blueshifted filament of gas between H7+H6. We have ‘tasted’ what we might expect to achieve with ALMA! Tacconi et al. in prep. IDA Meeting, Copenhagen 20-21 Dec. 2004

  38. High-resolution PdBI observations of SMGs- a taste of ALMA SMMJ163681+4057: Tacconi et al. in prep. IDA Meeting, Copenhagen 20-21 Dec. 2004

  39. The Future… …is here and it’s interferometrical! • CO is great! But… • It doesn’t trace the dense starforming gas • Need high-density tracers such as HCN • Other molecular/atomic lines, e.g. CI • Ultimate goal: detail ISM studies at high-z as well as ‘blind’ CO surveys. IDA Meeting, Copenhagen 20-21 Dec. 2004

  40. The Future… …is here and it’s interferometrical! • CO is great! But… • It doesn’t trace the dense starforming gas • Need high-density tracers such as HCN • Other molecular/atomic lines, e.g. CI • Ultimate goal: detail ISM studies at high-z as well as ‘blind’ CO surveys IDA Meeting, Copenhagen 20-21 Dec. 2004

  41. The Future… IDA Meeting, Copenhagen 20-21 Dec. 2004

  42. The Future… Courtesy Jesper Sommer Larsen IDA Meeting, Copenhagen 20-21 Dec. 2004

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