Survey
* Your assessment is very important for improving the workof artificial intelligence, which forms the content of this project
* Your assessment is very important for improving the workof artificial intelligence, which forms the content of this project
Observing Molecules in the EoR October 27, 2006 SKA Workshop, Paris Pierre Cox IRAM Grenoble, France 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 From Blain (2003) October 27, 2006 Luminosities involved: 3x1011 <L/Lsun< 1014 SKA Workshop, Paris October 27, 2006 SKA Workshop, Paris LVG solution Cloverleaf 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 Weiss et al. (2005) Subarcsecond Imaging Results < 0.5” (4 kpc) Tacconi, Neri, Chapmanm Genzel et al. (2006) October 27, 2006 SKA Workshop, Paris 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 tdyn or a few 108 yr 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) October 27, 2006 SKA Workshop, Paris Dust continuum at 1.2 mm CO(3-2) 46.6149 GHz PdBI continuum VLA October 27, 2006 SKA Workshop, Paris CO excitation in J1148+5251 (filled circles), compared to NGC 253 (dashed) Mass: LVG Model: MH2 = 2 x 1010 Msun Tkin= 100K, nH2=7x104 cm-3 Mdyn = 3 x 109 sin-2(i) Msun Mass in C and O: ~3x107 Msun Bertoldi et al. (2003) October 27, 2006 SKA Workshop, Paris Resolving the CO emission in J1148+5251 VLA A+B + C array; res.: 0.15” (~1 kpc) CO 3-2 at 45GHz 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 1” Integration times: hours to days on HLIRGs Walter et al. 2004 October 27, 2006 Early enrichment of heavy elements (z_sf > 8) SKA Workshop, Paris [[CII] 158 microns and [CI] emission lines in J1148+5251 at z=6.42 Probing the physics of a PDR at the end of the reionisation epoch CO(7-6) CII CI(1-0) October 27, 2006 SKA Workshop, Paris 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) Wagg et al. 2005; Burillo et al. 2006; Guelin, Salome et al. 2006 October 27, 2006 L’(HCO+) = 4 x 1010 K/(km/s pc2) HCO+(5-4)/HCN(5-4) ~ 1 HNC(5-4)/HCN(5-4) ~ 0.9 SKA Workshop, Paris 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 October 27, 2006 SKA Workshop, Paris SKA and CO M 82 October 27, 2006 SKA Workshop, Paris 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 October 27, 2006 SKA Workshop, Paris Complementarity: Line sensitivity z=5 SFR=10M_sun/yr High order, C+… Low order transitions October 27, 2006 SKA Workshop, Paris Radio studies of the first luminous objects Radio Continuum 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’) October 27, 2006 SKA Workshop, Paris Complementarity: continuum sensitivity AGN, star formation dust Stars, ionized gas October 27, 2006 SKA Workshop, Paris 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 October 27, 2006 SKA Workshop, Paris z=6.55 SFR>10 M_sun/yr The Future (is now): Probing the EoR! • Study physics of the first luminous sources z=6.4 • This can only be done at near-IR to radio wavelengths • Currently limited to ‘pathological’ systems (HLIRGs) • SKA and ALMA 10100 more sensitive which is critical for the study of ‘normal’ galaxies October 27, 2006 SKA Workshop, Paris