alma: resolving (optically) obscured galaxy formation dusty04, c. carilli (nrao)

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ALMA: Resolving (optically) obscured galaxy formation Dusty04, C. Carilli (NRAO). IR. Optical. Franceschini 2000. Cosmic Background Radiation. Obscured galaxy formation: low redshift (Meier & Turner 2004). IC342 distance = 2 Mpc M _gas = 4e7 M _sun SFR = 0.1 M _sun /yr - PowerPoint PPT Presentation


  • ALMA: Resolving (optically) obscured galaxy formationDusty04, C. Carilli (NRAO)Franceschini 2000Cosmic Background RadiationIROptical

  • Obscured galaxy formation: low redshift (Meier & Turner 2004)IC342 distance = 2 Mpc M_gas = 4e7 M_sun SFR = 0.1 M_sun/yr Starburst age = 1e7 yrs30 = 300pc

  • PdBI/VLA position =>K = 23.5 (Dunlop et al.)I K > 5.2 z = 4 +/- 1 (?)S_250 = 2.1 +/- 0.3 mJyS_1.4 = 16 +/- 4 uJyL_FIR=7e12 L_sunGrav. Mag. = 3x (?)Obscured galaxy formation: high redshift (Downes et al 2002; Dunlop et al 2003)Single Scuba galaxy dominates SFR at z>2 in HDF over 10000 optical galaxies!

  • UV selected galaxies large range in bolometric luminosity, but little correlation of L_uv and L_bol Adelberger 2000

  • Magic of (sub)mmL_FIR = 4e12 x S_250(mJy) L_sun for z=0.5 to 8

  • Enabling Technology I: sensitivity Arp 220 vs z (FIR=1.6e12 L_sun)cm: Star formation, AGN(sub)mm Dust, molecular gasNear-IR: Stars, ionized gas, AGN

  • Enabling technology II: Resolution10s mas resolution, T_B = 0.3 K: GMCs at 200MpcPdBI/CARMAALMA

  • Nearby star forming Galaxies Chemistry/Physics: IC342, D=2MpcCO: all gasHC3N: DenseC2H: PDRsALMA: Image with GMC resolution (50pc) to 250 Mpc Rich clusters: Virgo = 16 Mpc, Coma = 100 Mpc ULIRGs: Arp 220 = 75 Mpc, Mrk 273 = 160 Mpc300pcMeier & Turner 2004

  • Nearby Gals II: Dynamics: feeding the nucleus NGC6946, D=5.5Mpc100 pcPdBI 0.5 CO(2-1) - Gas Lanes along Bar Streaming Motions Gas Disk w/ R
  • Probing the epoch of galaxy formation : z = 1.5 3.5 Comparable SFR at high z in dusty starbursts as optical galaxies?IR/(sub)mm galsOptical gals

  • (sub)mm Source counts (Blain 2002) ALMA: 2e6 gals/deg^2 HDF: 4e6 gals/deg^2

    Big Difference: ALMA gals (mostly) at z > 1 HST gals (mostly) at z < 1Current bolometers Lensed fieldsALMA

  • L_FIR vs L(CO) (Beelen + 04)Index=1.7Index=11e11 M_sun1e3 M_sun/yrALMA z>2PdBI/Carma z>2

  • SKA and ALMA: Optimal CO searches ALMA: discovers 10 gals/hr z=0.5 2.5 SKA: discovers 10 gals/hr z=4

  • HCN 1-0 emission: VLA detectionsn(H_2) > 1e5 cm^-3 (vs. CO: n(H_2) > 1e3 cm^-3) z=2.58Solomon et alIndex=170 uJyCurrent z>2ALMA z>2 (if constant T_b)

  • Main ISM cooling line:[CII] 158um (vd Werf 2004)

  • PKS 2322+1944 z=4.12: CO Einstein ringPdBI [CI] (492 GHz rest) => Solar Metallicity (Pety 2004)PdBIVLA CO2-1 0.4 res

  • Very wide field surveys: role of bolometer cameras Bolometers (+ EVLA, Spizter): survey large areas to sub-mJy sensitivity ALMA: detailed SED and CO follow-up ALMA: uJy, narrow field surveys

  • Enabling technology III: Wideband spectroscopy Redshifts for obscured/faint sources: 8 - 32 GHz spectrometers on ALMA, LMT, GBT (Min Yun 04, Harris 04)L_FIR = 1e13 L_sunALMA

  • History of IGM bench-mark in cosmic structure formation indicating the first luminous structuresEpoch of Reionization (EoR)ionizedNeutral F(HI)=1Ionized F(HI)=1e-5CoIs: Walter, Bertoldi, Cox, Omont, Beelen, Fan, Strauss...

  • The Gunn-Peterson EffectFan et al 2003Fast reionization at z=6.3 => opaque at l_obs
  • Thompson scattering at EoR t_e = 0.17 => F(HI) < 0.5 at z=17Complex reionization from z=6 to 15?WMAP Large scale polarization of CMB (Kogut et al.) 20deg

  • highest redshift quasar knownL_bol = 1e14 L_suncentral black hole: 1-5 x 109 Msun => M_bulge = 1.5e12 M_sun (Willot etal.)

    clear Gunn Peterson trough (Fan etal.)Objects within EoR QSO 1148+52 at z=6.4

  • Pre-ALMA Science 1148+52 Dust + CO detection z=6.42 S_250 = 5.0 mJy => L_FIR = 1.2e13 L_sun, M_dust=7e8 M_sun S Dv = 0.2 Jy km/s => M(H_2) = 2e10 M_sun3MAMBOVLA CO 3-246.6149 GHz Off channelsrms = 60 uJyProdigious dust and molecular gas formation within 0.9 Gyr of big bangeg. Dust formation in SNR/massive stars?

  • IRAM Plateau de Bure FWHM = 305 km/s z = 6.419 +/- 0.001n2(3-2)(7-6)(6-5) Tkin=100K, nH2=105cm-3 Typical of starburst nucleus

  • VLA imaging of CO3-2 at 0.4 and 0.15 resolution Separation = 0.3 = 1.7 kpc T_B = 20K = T_B (starburst) Merging galaxies? Or Dissociation by QSO?rms=50uJy at 47GHz CO extended to NW by 1 (=5.5 kpc) tidal(?) feature M_dyn (r break-down of M-s relation => SMBH form first?

  • 1148+5251: radio-FIR SED Star forming galaxy characteristics: radio-FIR SED, L_CO/FIR, CO excitation and T_B => Coeval starburst/AGN: SFR = 1000 M_sun/yr Stellar spheroid formation in few e7 yrs = e-folding time for SMBH => Coeval formation of galaxy/SMBH at z = 6.4 ? S_1.4= 55 +/- 12 uJy1048+46Beelen et al. T_D = 50 K

  • Objects within the EoR nearIR detection of normal star forming galaxy at z=6.56 (Hu et al)L_uv = 2e10 L_sun + LBG dust correction (5x) => L_FIR=1e11 L_sunS_250 = 0.03 mJy => 4s ALMA detection in 3 hrs Expect 1 2 normal galaxies ALMA FoV at z>6

  • ALMA de-obscuring galaxy formationI. Seeing through the dust: Physics, chemistry, dynamics of star formation at GMC scale to 250MpcUnveiling the submm galaxy population at z=1 to 3 => SFHU

    II. First light: Seeing through neutral IGM (GP=> limited to NIR to radio)Study dust, gas, star formation in the first luminous sources Currently limited to pathological systems (HLIRGs)ALMA, EVLA 10-100x sensitivity is critical to study normal galaxiesz=6.4

  • mm VLBI10s mas resolutionPdBI/CARMAALMAmmVLBI

  • Millimeter VLBI Imaging the Galactic center black hole (Falcke 2000)KerrSchwarzschildModel: opt. thin synch0.6 mm VLBI 16uas res1.3 mm VLBI 33 uas resR_g = 3 uas

  • mm-vlbi of the Galactic center (Krichbaum 1998)


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