Star formation in Deep Radio Surveys

1. Star formation in Deep Radio Surveys Nicholas Seymour ARC Future Fellow CSIRO Astronomy and Space Science Bologna 13th September 2011

2. Precision Galactic Evolution Redshift CSIRO. Insert presentation title, do not remove CSIRO from start of footer

3. Precision Galactic Evolution ★ Redshift CSIRO. Insert presentation title, do not remove CSIRO from start of footer

4. Precision Galactic Evolution CSIRO. Insert presentation title, do not remove CSIRO from start of footer

5. What SFG science can we do with deep radio surveys? • Not a discussion on how to identify AGN or SFGs • Example of what we can do once we have a sample of SFGs • Based on Seymour et al. (2008) and unpublished follow-up CSIRO.EMU Bologna Meeting, Nick Seymour, September 13th 2011

6. Radio Luminosity/Redshift Distribution • Not a Seymour et al. (2008) CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th2011

7. Optical Magnitudes Red triangles = SFGs Blue Squares = AGN Seymour et al. (2008) CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 2011

8. Far-Infrared/Radio Correlation for SFGs Condon et al. (1992)

9. Source Counts by type • Not a Seymour et al. (2008) CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 2011

10. Source Counts by type CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 2011

11. Stellar Mass Highest SFRs found at high-z and in the most massive galaxies. 6df SF galaxies CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 2011

12. Stellar Mass Highest SFRs found at high-z and in the most massive galaxies. 6df SF galaxies Seymour et al. (2008) CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 2011

13. Star Formation History • Not a Seymour et al. (2008) CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 2011

14. Contribution by SFR to the >10L* top of the luminosity function • Not a Seymour et al. (2008) CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 2011

15. Characteristic Time (inverse of Specific SFR) • Not a Seymour et al. (2008) CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 2011

16. IR/SFR luminosity density Separated into LIRGs, ULIRGs HyLIRGs CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 2011

17. Radio AGN Luminosity Density Uncorrected CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 2011

18. Radio AGN Luminosity Density Corrected CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 2011

19. Future Meetings • EMU International Meetings: • 5th Meeting: Auckland – February 2012 • 6th Meeting: Sydney - 28-29th May 2012 (provisional) • SPARCS • 2nd Workshop: Sydney - 30th May to 1st June 2012 (provisional) • Southern Cross Astrophysics Conference V – 4th-8th June 2012 (provisional) • This conference on "Large Surveys" is the fifth in the "Southern Cross Astrophysics Conference Series" which are held annually at a suitable venue in Australia. It will be held from June 4 to 8 2012. We hope to hold the conference amongst the vineyards of the Hunter Valley, one of Australia’s premier wine growing regions. • Other face-to-face meetings?? • SPARCS Source-finding sub-group?? CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 2011

20. BETA (Boolardy Engineering Test Array) • First six ASKAP antennae – already in place awaiting first PAFs • Potentially time available for science, after BETA commissioning and before full ASKAP commissioning. • Specs: • Resolution 60-80” • Sensitivity: 450uJy (1hr) 320uJy (2hr) 260uJy (3hr) CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 2011

21. BETA (Boolardy Engineering Test Array) 20 30 40 CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 2011

22. BETA (Boolardy Engineering Test Array) • First six ASKAP antennae – already in place awaiting first PAFs • Potentially time available for science, after BETA commissioning and before full ASKAP commissioning. • Specs: • Resolution 60-80” • Sensitivity: 450uJy (1hr) 320uJy (2hr) 260uJy (3hr) • Maybeconfusion limited after a fewhours • Long exposuresmaybeneededtoobtainuvcoverage CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 2011

23. EMU Value-Added Catalogue (EVACat) • EMU committed to releasing XID catalogue to the community • VO-compatible • 6monthly releases CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 2011

24. Other issues • Use ATLAS as a test for science we can do with EMU • Obtain a better calibration of radio luminosity to SFR conversion • Obtain a better understanding of the detailed physics behind the radio/IR correlation (on which the radio luminosity/SFR conversion is based) • Develop a plan to get the crucial redshifts (combine deep well studied fields with wide area ‘photometric’ redshifts) • Calculate how well we can obtain derived scientific results, like the star formation history, for different surveys (e.g. 8deg2 ATLAS, 30deg2 of EMU with deep ancillary data, 400deg2 of EMU using shallow data,future SKA continuum surveys) CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 2011

25. Mean SED (normalised around 1.6um) Probably should normalise by SFR CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 2011

26. Radio v 24um flux Note 24um excess sources CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 2011

27. SFR v environment Note redshift effects! CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 2011

28. Radio v 24um flux Note 24um excess sources CSIRO.ATLAS Meeting, Nick Seymour, August 9th 2011

29. Flux ratios: Radio/K-band and radio/24um Seymour et al. (2008) CSIRO.ATLAS Meeting, Nick Seymour, August 9th 2011