Star formation in Deep Radio Surveys Nicholas Seymour ARC Future Fellow CSIRO Astronomy and Space...
-
Upload
thomas-holt -
Category
Documents
-
view
220 -
download
1
Transcript of Star formation in Deep Radio Surveys Nicholas Seymour ARC Future Fellow CSIRO Astronomy and Space...
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
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 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 (2008) and unpublished follow-up
CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 2011
Radio Luminosity/Redshift Distribution
• Not a
Seymour et al. (2008)
CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 2011
Optical Magnitudes
Red triangles = SFGsBlue Squares = AGN
Seymour et al. (2008)
Far-Infrared/Radio Correlation for SFGs
Condon et al. (1992)
CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 2011
Source Counts by type
• Not a
Seymour et al. (2008)
CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 2011
Source Counts by type
CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 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 13th 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 13th 2011
Star Formation History
• Not a
Seymour et al. (2008)
CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 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 13th 2011
Characteristic Time (inverse of Specific SFR)
• Not a
Seymour et al. (2008)
CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 2011
IR/SFR luminosity density
Separated into LIRGs, ULIRGsHyLIRGs
CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 2011
Radio AGN Luminosity Density
Uncorrected
CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 2011
Radio AGN Luminosity Density
Corrected
CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 2011
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
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
BETA (Boolardy Engineering Test Array)
203040
CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 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 13th 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 13th 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. 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
Mean SED (normalised around 1.6um)
Probably should normalise by SFR
CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 2011
Radio v 24um flux
Note 24um excess sources
CSIRO. EMU Bologna Meeting, Nick Seymour, September 13th 2011
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
Seymour et al. (2008)