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Observing Molecules in the EoR

This presentation discusses the observation of molecular and atomic emissions from ultra-luminous infrared galaxies (ULIRGs) during the Epoch of Reionization (EoR), using data from the SKA Workshop. Key findings include the characterization of CO and HCN emissions, the analysis of thermal and non-thermal radio emissions, and their implications for star formation in high-redshift galaxies. The study also highlights the importance of using both SKA and ALMA instruments to enhance our understanding of galaxy formation in the early universe by probing physical conditions of galactic environments at various redshifts.

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Observing Molecules in the EoR

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  1. Observing Molecules in the EoR Pierre Cox IRAM Grenoble, France SKA Workshop, Paris

  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) SKA Workshop, Paris

  3. SKA Workshop, Paris

  4. 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)

  5. 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) SKA Workshop, Paris

  6. J1148+5251 - The Most Distant QSO at z=6.42 Observing First Light at Radio Wavelengths Gunn Peterson trough 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 SKA Workshop, Paris

  7. CO(3-2) 46.6149 GHz PdBI continuum VLA Walter et al. 2003 Bertoldi et al. 2003 SKA Workshop, Paris

  8. 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) SKA Workshop, Paris

  9. 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 CO 3-2 at 45GHz 1” • Early enrichment of heavy elements (z_sf > 8) • Integration times: hours to days on HLIRGs Walter et al. 2004 SKA Workshop, Paris

  10. [[CII] 158 microns and [CI] emission lines 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) SKA Workshop, Paris

  11. Other High Density Tracer: HCN, HNC and HCO+ APM08279+5255 (z=3.91) HCO+(5-4) HNC(5-4) HNC(5-4) & CN(5-4) L’(HCO+) = 4 x 1010K/(km/s pc2) HCO+(5-4)/HCN(5-4) ~ 1 HNC(5-4)/HCN(5-4) ~ 0.9 Wagg et al. 2005; Burillo et al. 2006; Guelin, Salome et al. 2006 SKA Workshop, Paris

  12. ALMA/EVLA/GBT Redshift coverage for CO Epoch of Reionization VLA CO(3-2), PdBI CO 6-5, 7-6 in J1148+5251 @ z=6.42 Other lines: HCN, HCO+, CI, CII, H2O SKA Workshop, Paris

  13. SKA and CO M 82 SKA Workshop, Paris

  14. SKA and ALMA: Optimal CO searches • SKA/ALMA – comparable speed at 22 GHz, SKA clearly faster at 43 GHz (FoV, fractional bandwidth, sensitivity) • SKA/ALMA – complementary: high vs. low order transitions SKA Workshop, Paris

  15. Complementarity: Line sensitivity z=5 SFR=10M_sun/yr High order, C+… Low order transitions SKA Workshop, Paris

  16. Radio studies of the first luminous objects RadioContinuum studies of star forming galaxies 1e13 L_sun 1e12 L_sun 1e11 L_sun CO (+other molecules) at z>4 VLA:3s in 3 hrs for L_FIR = 1e13 M_sun (‘HLIRG’) SKA (20 – 40 GHz): 3s in 3hrs for L_FIR =1e11 M_sun (‘LIRG’) SKA Workshop, Paris

  17. Complementarity: continuum sensitivity AGN, star formation dust Stars, ionized gas SKA Workshop, Paris

  18. SKA into the EoR: Low Order Molecular Lines, Star Formation 1148+5651: Hyperluminous IR galaxies • Detect low order CO emission in seconds, including imaging on subkpc scales. • Detect high dipole moment molecules (HCO+, HCN…) in minutes (critical densities > 1e5 cm^-3). • Image non-thermal emission associated with star formation and/or AGN at mas resolution. Studying 1st galaxies • Detect ‘normal’ (eg. Ly a), star forming galaxies, like M51, at z>6, in few hours • Determine redshifts directly from molecular lines z=6.55 SFR>10 M_sun/yr SKA Workshop, Paris

  19. The Future (is now): Probing the EoR! • Study physics of the first luminous sources • This can only be done at near-IR to radio wavelengths • Currently limited to ‘pathological’ systems (HLIRGs) • SKA and ALMA 10-100 more sensitive which is critical for the study of ‘normal’ galaxies z=6.4 SKA Workshop, Paris

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