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

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

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

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

CSIRO. EMU Bologna Meeting, Nick Seymour, September 13 th 2011 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 (2008) and unpublished follow-up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 13 th 2011 Radio Luminosity/Redshift Distribution Not a Seymour et al. (2008)

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

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

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

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

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

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

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

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

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

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

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

CSIRO. EMU Bologna Meeting, Nick Seymour, September 13 th 2011 Future Meetings EMU International Meetings: 5 th Meeting: Auckland – February th Meeting: Sydney th May 2012 (provisional) SPARCS 2 nd Workshop: Sydney - 30 th May to 1 st June 2012 (provisional) Southern Cross Astrophysics Conference V – 4 th -8 th 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 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 13 th 2011 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 13 th 2011 BETA (Boolardy Engineering Test Array)

CSIRO. EMU Bologna Meeting, Nick Seymour, September 13 th 2011 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) Maybe confusion limited after a few hours Long exposures may be needed to obtain uv coverage

CSIRO. EMU Bologna Meeting, Nick Seymour, September 13 th 2011 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 13 th 2011 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. 8deg 2 ATLAS, 30deg 2 of EMU with deep ancillary data, 400deg 2 of EMU using shallow data, future SKA continuum surveys)

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

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

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

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

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