structure in the sub-mm background towards the hdf
DESCRIPTION
Structure in the sub-mm background towards the HDF. John Peacock & the UK sub-mm survey consortium. Novartis Institute, November 1999. Outline. Motivation for resolving the sub-mm background The SCUBA 850- m m map of the HDF Optical identifications of the S 850 > 2 mJy sources - PowerPoint PPT PresentationTRANSCRIPT
Structure in the sub-mm background towards the HDF
John Peacock
& the UK sub-mm survey consortium
Novartis Institute, November 1999
Outline
Motivation for resolving the sub-mm background
The SCUBA 850-m map of the HDF
Optical identifications of the S850 > 2 mJy sources
Statistical detections of starbursts down to 0.1 mJy
Emission from z > 5 galaxies
Clustering of the 850-m background
Edinburgh: James Dunlop, Dave Hughes, Andy Lawrence, John Peacock
Imperial College: Andreas Efstathiou, Bob Mann, Seb Oliver, Michael Rowan-Robinson, Steve Serjeant
Cambridge: Andrew Blain, Malcolm Longair
UCL: Rob Ivison
JACH: Tim Jenness
The SCUBA 850-m HDF map
50 hours integration
100 arcsec radius
Beam: 14.5’’ FWHM
- 30’’ and 45’’ chop
Noise: 8’’ FWHM
- rms 0.45 mJy
- doubles at 90’’
(divided out)
Number counts
5 sources > 2 mJy
Confusion analysis:
Euclidean counts
to S < 0.3 mJy
7000 deg-2 > 1 mJy
Optical counterparts
50K + =1.5 photometric z’s:
HDF 850.1 must have z > 3
HDF 850.1 continued
IRAM 1.3-mm position coincident with VLA source.
Between z=1 and z=2 galaxies, but inconsistent with either.
Downes et al. astro-ph/9907139
Structure in the background
Subtract 5 brightest point sources:
Residual structure from
source superposition:
correlation with known HDF starbursts?
Predicting sub-mm emission
Photometric redshifts + UV flux
” L1500
Dust-free starburst:
SFR = L1500 / 1021 W Hz-1
S850 / mJy = SFR / 20 h-2 Msun yr-1
Wide z range expected
Predicted sub-mm maps
z z
Significant cross-correlation over 1 < z < 6
Emission at extreme z
NICMOS GTO data found 8 z > 5 candidates (including 4-473.0 at z=5.6):
2 close pairs match well with 1-mJy level peaks
Mean starburst emission
Detect non-zero flux at 0.1 mJy level:
0.14.4SFR visible
SFRhidden
cf. detection limits of 1-2 mJy for single pointings
cf. ratios > 100 for ULIRGs like 850.1
Meaning of hidden SFR
All star formation is ‘hidden’: never expect dust-free burst
‘hidden’ : ‘visible’ ratio depends on lifetime of high-mass stars and dust burnoff time
Jimenez et al. models (astro-ph/9910279) predict 6:1 for Salpeter IMF
Similar boost factor for SFR inferred by Pettini et al. from Balmer lines, but foreground screen is not the right model
Clustering of the background
ln d ) θ ( ) ( ) θ ( 02 Jw
Measure clustering via dimensionless power spectrum
shot noise
true clustering
assume w = ()-0.8 :
find < 2 arcsec
reasonable if sub-mm galaxies have 1 < z < 6: Limber ” factor 3-4 reduction in w wrt Lyman-break galaxies
Summary
HDF starbursts emit at 850-m– statistical detections down to 0.1 mJy
– mean hidden : visible SFR is 4.5 : 1 The 850-m background is clustered
– consistent with shot noise
– limits background clustering to 0 < 2 arcsec
– consistent with very broad redshift range contributing to background
Future issues– what is the upper redshift limit?
– nature of HDF 850.1?
– comparison with NICMOS