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the faint end …. …. in neutral gas

the faint end …. …. in neutral gas. “luminous”. Radio spectroscopy. Upper limits to space density of intergalactic HI Clouds. # Clouds /Mpc 3 /decade. M HI. Volume for each survey that was sensitive to M HI. -. -. -. Volume (Mpc 3 ). -. -.

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the faint end …. …. in neutral gas

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  1. the faint end ….…. in neutral gas

  2. “luminous”

  3. Radio spectroscopy

  4. Upper limits to space density of intergalactic HI Clouds # Clouds /Mpc3 /decade MHI

  5. Volume for each survey that was sensitive to MHI - - - Volume (Mpc3) - - MHI

  6. Upper limits to space density of intergalactic HI Clouds # Clouds /Mpc3 /decade HI in Galaxies MHI

  7. Upper limits to space density of intergalactic HI Clouds # Clouds /Mpc3 /decade MHI

  8. Lo & Sargent (1979) M81, CVn, NGC 1023 Groups MHI /L 18 0.4 15 3 0.4 1.3 Log MHI 6.8 6.6 7.9 7.8 7.7 8.1 Mpg -8.7 -12.3 -11.5 -13.1 -15.2 –15.5

  9. … the writing is on the wall… (… and in the literature…)

  10. more HI in M96 than the Ring (Schneideretal 1989)

  11. Giovanelli, Haynes, Chengalur “Virgo HI Cloud”

  12. HI Mass Function: (dashed curve) Felton 1985, Luminosity Function F-T for MHI/L(L)

  13. HI Content according to galaxy mass

  14. (1990) Parkes HIPASS results (2003): Integral HI mass content: 6.1x107 Mo Mpc-3 ( faint end slope: a = -1.3 ) Integral HI mass content: 7.0x107 Mo Mpc-3 (HIMF faint end slope: a = -1.28 )

  15. … what else in the meanwhile… Relation of Galactic High Velocity Clouds to IGM… … HVCs mostly within 200 kpc (Zwaan 2000, thesis)

  16. HIPark – a parked Parkes survey diffuse clouds in LG & Milky Way halo How sensitive ? … optically thin at the Lyman limit Goals:ultra sensitive to low column densities exercise in observational techniques … rfi, passband calibration, … good match to long maintenance periods

  17. Briggs Barnes de Blok Freeman Gibson Korbalski Reynolds Staveley-Smith Zwaan HI Park proposers… Progess: 25 days observations – John Reynolds extragalactic preview – Jackie Cooper

  18. DLA CIV MgII/ Lyman limit (CII, FeII, SiII, …) MOTIVE ? QSO absorption line interception cross sections Z=3 Ly break galaxy

  19. HI Column density distribution function Number of interceptions in range: N to N+dN f(N) dN /unit Z tLL > 1 Lya forest IGM DLA CIV Petijean etal 1993 -10 -15 Log f(NHI) -20 12 14 18 20 22 Log NHI

  20. M82 M81 NGC 3077 HI Map of M81 Group Yun, Ho & Lo 1994

  21. NGC 3344

  22. HIPARK Goal… Sensitivity: to achieve 6s < 3 x 1017 cm-2 need ~ 6 hours of integration per beam Drift scan: 15’ beam transits in ~ 1 minute a ~360 transits

  23. Multibeam!!! Barnes et al

  24. 1x 4x 3x Feed orientation for drift scans

  25. Path of Survey Strip: Galactic Coords Dcloud >1 kpc at 250 kpc … to fill beam Limits on tiny masses in Sculptor… 3x104 dMpc2 solar masses

  26. 05:56 FORNAX Dec –32d53’ R.A. 03:34 2200 km/s 0

  27. 22:55 Dec –32d53’ R.A. 20:36 2200 km/s 0

  28. Sculptor (Putman et al)

  29. 01:14 SCULPTOR Dec –32d53’ R.A. 22:55 2200 km/s 0

  30. Magellanic Stream (Putman et al)

  31. DEEP Centaurus Survey (Disney et al)

  32. 01:14 Dec –32d53’ R.A. 22:55 2200 km/s 0

  33. Large mass halosStar Formation Galaxies Early Low mass halos Star Formation ISM Lost Late Low mass halos never capture gas, (No Star Formation) No Intergalactic Neutral Hydrogen Clouds at Z=0 Conclusions: (no I.G. HI clouds…) … faint end still not known… ATA… SKA

  34. Velocity Sun up ! 1100 0 -500 RA

  35. Velocity 1100 0 -500 RA

  36. Velocity One Day – One Beam 2800 0 -500 Right Ascension

  37. Galactic Plane crossing: L ~ 250o Velocity 1100 km/s 0 -500 RA

  38. Velocity 1100 0 -500 RA

  39. Velocity 1100 0 -500 RA

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