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HI at moderate redshifts Philip Lah Science with MIRA workshop

Research School of Astronomy & Astrophysics. Mount Stromlo Observatory. HI at moderate redshifts Philip Lah Science with MIRA workshop. What do I mean by “HI at moderate redshifts” ??. HI 21cm emission from galaxies with z > 0.08 look-backtime > 1 Gyr

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HI at moderate redshifts Philip Lah Science with MIRA workshop

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  1. Research School of Astronomy & Astrophysics Mount Stromlo Observatory HI at moderate redshiftsPhilip LahScience with MIRA workshop

  2. What do I mean by “HI at moderate redshifts” ?? HI 21cm emission from galaxies with z > 0.08 look-backtime > 1 Gyr Enough time for significant cosmological evolution in galaxies

  3. Talk Outline The Past • why HI emission detection is hard at moderate redshifts • older HI emission galaxy detections The Present • recent WSRT HI detections of galaxies in clusters at z0.2 • my result for HI in star-forming galaxies at z=0.24 The Future • what MIRA can do

  4. The Past

  5. Why HI detection is hard z=0.05

  6. Older HI emission at moderate redshifts

  7. HI emission detections • Zwaan et al. 2001 z = 0.176 • galaxy in the outskirts ofgalaxy cluster Abell 2218 WSRT 200 hours • Verheijen 2004 z = 0.1887 • galaxy in the outskirts of galaxy cluster Abell 2192  VLA ~80 hours

  8. The Present

  9. WSRT Cluster Survey Verheijen et al. January 2007 – results from a completed pilot study of two galaxy clusters • Abell 2192 z=0.188 (1196 MHz) • Abell 963 z=0.206 (1178 MHz)

  10. Observations Details HI masses detected range between 5109 M and 41010 M (0.8 M* to 6.3 M*)

  11. An example galaxy in Abell 2192 z=0.1888

  12. HI Coadded Signal no HI detection For both clusters, galaxies in surrounding field with optical redshifts MHI= 2109 M

  13. HI in star-forming galaxies at z=0.24

  14. Collaborators:Frank Briggs (ANU) Jayaram Chengalur (NCRA) Matthew Colless (AAO)Roberto De Propris (CTIO)Michael Pracy (ANU)Erwin de Blok (ANU)

  15. Giant Metrewave Radio Telescope

  16. Giant Metrewave Radio Telescope

  17. Giant Metrewave Radio Telescope

  18. Giant Metrewave Radio Telescope

  19. Giant Metrewave Radio Telescope

  20. Giant Metrewave Radio Telescope

  21. Giant Metrewave Radio Telescope

  22. Giant Metrewave Radio Telescope

  23. The Suprime-Cam Field 24’ × 30’ Fujita et al. 2003 narrow band imaging - H emission at z=0.24 348 galaxies SFRDz=0.24 ~ 3 SFRDz=0 RA DEC

  24. Fujita galaxies - B filter thumbnails 10 arcsec  10 arcsec ordered by increasing H luminosity

  25. Fujita galaxies – 2dF redshifts thumbnails 10 arcsec  10 arcsec ordered by increasing H luminosity

  26. GMRT data for the field

  27. Coadded HI Spectrum

  28. neutral hydrogen gas measurement using 121 redshifts MHI = (2.26 ± 0.90) ×109 M 0.36 ± 0.14 M* HI spectrum all

  29. The Cosmic Neutral Gas Density

  30. Cosmic Neutral Gas Density vs. Redshift Rao et al. 2006 DLAs from MgII absorption Prochaska et al. 2005 DLAs Zwaan et al. 2005 HIPASS HI 21cm

  31. Cosmic Neutral Gas Density vs. Redshift my new point

  32. Cosmic Neutral Gas Density vs. Time my new point

  33. The Future

  34. MIRA: Frequency Parameters • frequency coverage from 700 - 1700 MHz  HI from z=0 to 1 • instantaneous bandwidth is 300 MHz

  35. MIRA HI Coadding

  36. MIRA: coadding HI signal observational constraint is the number of optical redshifts available redshift bins Δz =0.025

  37. MIRA: coadding HI signal observational constraint is the number of optical redshifts available redshift bins Δz =0.025

  38. MIRA: coadding HI signal observational constraint is the number of optical redshifts available redshift bins Δz =0.025

  39. Future Optical Data AAOmega on AAT - ~3 sq degrees Wigglez Survey - due to be complete by 2009 • equation of state for dark energy from baryonic acoustic oscillations in galaxy clustering • redshift survey of 400,000 galaxies with active star formation z =0.5 to 1 over 1000 sq degrees • 10+ fields  each ~81 sq degrees  400 targets/sq degree ANU SkyMapper1.3m telescope  8sq degreefield of view- operational sometime later this year

  40. The End

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