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Magic of (sub)mm

Magic of (sub)mm. L _FIR = 1.5e12 L _sun. 3mJy. Distance independent probe of universe Biased to > ULIRGs. Submm surveys: Probing the epoch of “galaxy formation” (z=1.5 – 3.5). SCUBA 20mJy. Optical Gal. Submm Gal.

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Magic of (sub)mm

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  1. Magic of (sub)mm L_FIR = 1.5e12 L_sun 3mJy • Distance independent probe of universe • Biased to > ULIRGs

  2. Submm surveys: Probing the epoch of “galaxy formation” (z=1.5 – 3.5) SCUBA 20mJy Optical Gal Submm Gal Comparable SFR at high z in dusty starbursts (“submm gal”) as optically selected galaxies, forming giant elliptical galaxies? SMA/Spitzer

  3. COSMOS/MAMBO 250 GHz survey: dusty galaxy formation Bertoldi, Carilli, Schinnerer, Voss, Smolcic + • MAMBO/30m • 117 pixels • 250 GHz • 10.6” • 0.9 mJy rms • 20’ x 20’ • Goals: • z distribution + contribution SFHU • Environments • AGN fraction • highest z starbursts? • evol radio-FIR

  4. Latest counts including COSBO – scaled to 350 GHz assuming T_D = 40 K PL Index=-2.7 COSMOS: 14 srcs >4s 23 srcs > 3.5s 7mJy 1e13 L_sun

  5. COSMOS: Immediate Gratification

  6. Radio – MAMBO: > 4s = 9/14 (<4”) • Radio – MAMBO: > 3.5s = 2/9 • ‘Optical’ – Radio – MAMBO: [6-9]/23 (<1”) • MAMBO – Xray: 2/23 • Complex morphology: multiple radio = 4/14 • Complex MAMBO: 5/14

  7. Redshift Distribution Opt photo Submm gal Radio photo (limits) Radio photo (det) • Lensing: 1 or 2 • Spurious: 1 or 2

  8. Difficulties with redshifts: templates and ambiguities Optical phot z 20K Z_opt (1,2) Z_rad 60K Radio phot z: (1+z) \propto T_D Z_opt (1) Z_rad, Z_opt(2)

  9. COSBO 7 Z_rad = 3.3 Z_opt = 0.45

  10. Radio and opt faint submm galaxies (10-20%): highest z (> 3) starbursts (4 secure srcs)? COSBO 1: brightest mm source 250 GHz = 6.3+/-0.9 mJy 1.4 GHz = 31 +/- 10 uJy HST I > 27 K_vega > 19.7 Z > 3.3 ? COSBO 9 250 GHz = 4.9 +/-0.9 1.4 GHz < 36 uJy HST I > 27 K_vega > 19.7 Z > 3.7 ?

  11. COSBO • 2005/6: 90hr • Spitzer • Spectroscopy

  12. END

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

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