Star formation in Deep Radio Surveys

Star formation in Deep Radio Surveys

Nicholas Seymour

ARC Future Fellow

CSIRO Astronomy and Space Science

Bologna 13th September 2011

Precision Galactic Evolution

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

Redshift



Redshift

★

CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 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 (2008) and unpublished follow-up


Radio Luminosity/Redshift Distribution

• Not a

Seymour et al. (2008)


Optical Magnitudes

Red triangles = SFGsBlue Squares = AGN


Far-Infrared/Radio Correlation for SFGs

Condon et al. (1992)


Source Counts by type

• Not a



Source Counts by type


Stellar Mass

Highest SFRs found at high-z and in the most massive galaxies.

6df SF galaxies


Star Formation History

• Not a



Contribution by SFR to the >10L* top of the luminosity function

• Not a



Characteristic Time (inverse of Specific SFR)

• Not a



IR/SFR luminosity density

Separated into LIRGs, ULIRGsHyLIRGs


Radio AGN Luminosity Density

Uncorrected


Radio AGN Luminosity Density

Corrected


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??


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)



203040



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


EMU Value-Added Catalogue (EVACat)

• EMU committed to releasing XID catalogue to the community• VO-compatible• 6monthly releases


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)


Mean SED (normalised around 1.6um)

Probably should normalise by SFR


Radio v 24um flux

Note 24um excess sources


SFR v environment

Note redshift effects!

CSIRO. ATLAS Meeting, Nick Seymour, August 9th 2011

Radio v 24um flux

Note 24um excess sources

CSIRO. ATLAS Meeting, Nick Seymour, August 9th 2011

Flux ratios:

Radio/K-band and radio/24um


Star formation in Deep Radio Surveys

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