1 / 33

Neutral Hydrogen Gas in Star Forming Galaxies at z=0.24

Neutral Hydrogen Gas in Star Forming Galaxies at z=0.24. Philip Lah Frank Briggs (ANU) Jayaram Chengalur (NCRA) Matthew Colless (AAO) Roberto De Propris (CTIO) Michael Pracy (ANU) Erwin de Blok (ANU). Background.  H α Spectroscopy  H α Narrow Band Imaging

peony
Télécharger la présentation

Neutral Hydrogen Gas in Star Forming Galaxies at z=0.24

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Neutral Hydrogen Gas in Star Forming Galaxies at z=0.24 Philip Lah Frank Briggs (ANU) Jayaram Chengalur (NCRA) Matthew Colless (AAO) Roberto De Propris (CTIO) Michael Pracy (ANU) Erwin de Blok (ANU)

  2. Background

  3.  Hα Spectroscopy  Hα Narrow Band Imaging  UV (with no dust correction) Subaru Field Star Formation Rate

  4. Rao et al. 2006 Prochaska et al. 2005 Zwaan et al. 2005 HIPASS HI 21cm HI redshift

  5. HI look back

  6. HI 21cm Emission at High Redshift

  7. Previous highest redshift HI Westerbork Synthesis Radio Telescope (WSRT) Netherlands Abell 2218 z = 0.18 integration time 36 days, Zwaan et al. 2001 Very Large Array (VLA) Abell 2192 z = 0.1887 integration time ~80 hours, Veheijen et al. 2004

  8. Giant Metrewave Radio Telescope

  9. GMRT Antenna Positions

  10. GMRT Collecting Area 30 dishes of 45 m diameter GMRT Collecting Area  21 × ATCA  15 × Parkes  6.9 × WSRT  3.6 × VLA

  11. Frequency HI Redshift DEC RA Method of HI Detection Radio Data Cube • pick out HI signal using optical redshifts • coadd faint signals to make measurement

  12. The Subaru Field - H emission galaxies

  13. Subaru Field 24’ × 30’ Fujita et al. 2003 narrow band imaging - H emission flux RA used 2dF to get optical redshifts DEC

  14. Subaru Field Data

  15. Subaru Galaxies - B magnitude Thumbnails 10’’ sq Ordered by H luminosity

  16. Subaru Galaxies - redshifts Thumbnails 10’’ sq Ordered by H luminosity

  17. 2dF (& AAOmega) redshifts Redshift histogram GMRT HI freq range Subaru Narrow Band Filter FWHM (120 Å)

  18. HI spectrum all 121 redshifts Neutral Hydrogen measurement MHI = (1.47 ± 0.89) ×109 M

  19. used the Fujita et al. 2003H Luminosity function for volume calculation • comparable error to low z DLA measurements but required less observing effort (no need lots of HST time) HI redshift mine all

  20. Radio Continuum in the Subaru Field

  21. Deepest GMRT Image RMS ~ 16 Jy Sub field 12’ × 12’ several hundred continuum sources some with optical counterparts

  22. Sullivan et al. 2001 H Luminosity vs. 1.4 GHz Luminosity & UV Luminosity vs. 1.4 GHz Luminosity Sullivan et al. 2003

  23. 10’ × 10’ Halpha vs. RC line from Sullivan et al. 2001

  24. Conclusions • measured the neutral gas density at z=0.24 with similar accuracy to the DLA method – with plenty of room for improvement • made the current deepest GMRT continuum image • the H emission - radio continuum correlation for star forming galaxies seems to hold true at z=0.24

  25. The End

  26. Additional Slides

  27. HI redshift mine all taking into account narrow band (H) filter shape – brighter galaxies will be seen over a larger volume

  28. Model no error

  29. model

  30. UV Plane

  31. Fuzzy RC Integrated Flux = 17.035  0.077 mJy

  32. Fuzzy B galaxy UGC 05849 at redshift z=0.026045

More Related