galaxies and galaxy clusters at mm wavelengths: the view from the south pole telescope
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Galaxies and galaxy clusters at mm wavelengths:
the view from the South Pole Telescope
Gil Holder
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On one side: CMB/SZ, “fundamental physics”
on the other side: BLAST, “astrophysics”
Outline• Small scale CMB anisotropy
– Detection of secondary anisotropies– Limits on thermal SZ, kinetic SZ
Lueker et al, Hall et al (both submitted)
• Galaxies– “point sources” in SPT maps– Dusty and/or synchroton-dominated galaxies– a new class of dusty galaxies?
Vieira et al (submitted)
Zoom in on 2 mm map~ 4 deg2 of actual data
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Detecting the SZ Power Spectrum
SPT Measured Points(model + Gaussian scatter)
• after removing bright sources, there is still small-scale contamination from residual sources
•Primary CMB looks right
• Poisson Point-sources as expected
10 K-arcmin point sources
guess at SZ power spectrum (8=0.8)
primary C
MB
150GHz
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Detecting the SZ Power Spectrum
SPT Measured Points(model + Gaussian scatter)
10 K-arcmin point sources
Hall et al. (2009, arxiv:0912.4315): we report tSZ + kSZ + clustered point-source power of 10K2 at=150GHz and l=3000
primary C
MB
150GHz
What happened to all the thermal SZ power?
Clustering of Point Sources
• Radio and IR/submm sources presumably trace the large scale matter fluctuations
• Back of the envelope:– Power spectrum
contribution: mean T2 x projected clustering amplitude
– Arcminute scales: few Mpc has clustering ~1 in 3D, divide by number of independent cells along line of sight => 1e-3
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The importance of multiple frequencies
Frequency scaling of Dusty Galaxy Background
9Scaling of Poisson power with frequency
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Hall et al 2010
10
First detection of clustered point source power from CIB sources in the mm bands
Hall et al 2010
Frequency scaling of Dusty Galaxy Backgrounds
Single-SED model assumes all galaxies have same rest-frame properties (T=34 K, =2) spread over a broad range in redshift (peaking at z=2)
Removing dusty galaxies
• Models suggest that nearly all of the residual power (both Poisson and clustered) is from high-z dusty galaxies
• To remove these, SPT constructed a map that is T150-xT220– Subtraction factor is tuned to minimize small scale power [no
noise bias in power spectrum]
– New map has all of tSZ, but has subtracted some fraction of CMB+kSZ
– Subtraction is imperfect: unknown and non-unique spectral behaviour of dusty sources
Temperature scaling
• Radio sources look a lot like CMB
• Dusty galaxies are much brighter at higher frequencies Frequency
(GHz)
Dusty galaxies (z=0,2,5)
Radio galaxies
dTcmb
Power Spectrum: Dusty Galaxy Contributions Largely Subtracted
Direct subtraction of (220 GHz map)/3 from 150 GHz map to
remove dusty galaxies
Power Spectrum: Dusty Galaxy Contributions Subtracted
Best fit 150 GHz power:
tSZ+0.46*kSZ=4.2 1.5 uK2
tSZ
kSZ
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What does the low SZ power mean?
• If we assume the fiducial tSZ model is correct (and some fiducial kSZ template), we find 8 = 0.746 ± 0.017
Compare to 8 = 0.794 ± 0.027 for WMAP5 + ACBAR + QUaD
• Allowing the best estimate (from theory considerations) 50% uncertainty on tSZ model amplitude gives 8 = 0.779 ± 0.025
Not Much Room for kSZ• Thermal SZ alone is
already a bit low• Using X-ray-based
profiles and WMAP chains, cl 8
16
• covariances between parameters conspire, in particular , h
• SPT analysis (Lueker et al.) used semi-analytic gas model, with cl 8
11 in CMB
chains
Best fit 150 GHz power:
tSZ+0.46*kSZ=4.2 ±1.5 uK2
Where does SZ Power Come From?
• Broad range in z
• Extends to low mass (relative to SPT SZ-detected clusters)
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From Shaw et al 09
Rough SPT mass limit for detection
Non-Gaussianity of statistics
d2cl /(dlnM dz) at ell~2500
SPT Galaxies at 150 & 220 GHz
Distribution of Spectral Indices
sources cleanly separate into two populations
synchrotron
dust
AGN counts
AGN counts as predicted
at high flux
source counts
dominated by
synchrotron-
dominated
sources
at the low flux end of the 1.4 mm band where dusty
sources become
dominant
150 GHz
220 GHz
dust source counts
red = Lagacheblue = Pearson
BCS image of a dusty SPT source with an IRAS counterpart
r band 5σ = 24.65 AB mag
i band 5σ = 24.35 AB mag
S1.4 = 14 mJyS2.0 = 8 mJy
BCS image of a dusty SPT source without any counterpart
r band 5σ = 24.65 AB mag
i band 5σ = 24.35 AB mag
S1.4 = 17 mJyS2.0 = 5 mJy
dust source countsWITH IRAS SOURCES REMOVED
red = Lagacheblue = Pearson
Comparison to Negrello et al. 2007
Current Followup Campaign
• ATCA: 3 mm 4 detections after two weeks of observing
• SMA: 1.4 mm detections for ~ 10 or our most northern sources
• Spitzer: 3.6 + 4.5 um observations down to 1 uJy (data taken, fully reduced)
• NOAO SOAR 4m: R,I,J,K observations done, data being reduced
• Gemini-S: spectroscopy for z>4 candidates in queue
• BCS griz ~ 60 square degrees in the can
Interferometric Follow-up
• ATCA at 90 GHz– Hard frequency
– Good location (Australia)
• SMA at 220 GHz– Easy frequency– Terrible location (Mauna Kea)
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SMG 10S1.4mm=21 mJy
SPT,SMA,IRAC,Gemini
SMG 03S1.4mm=37 mJy
BCS
Summary• SPT has measured the small-scale CMB
power spectrum, detecting secondaries– SZ power may be a bit low (or matter power spectrum is a
bit low)Hall et al, Lueker et al (submitted)
• interesting population of galaxies at mm wavelengths– Either nearby galaxies with very cold dust or extremely
bright high-z galaxies– Lensed?– Discovered because of large area (~100 deg^2) searched
compared to existing catalogsVieira et al (submitted)
IR/Submm Source Clustering
• Mean Tcmb~104 uK at 500 um (FIRAS)
• Clustering amplitude 10-3
• => few 105 uK2
• BLAST: 106 uK2
• Mean Tcmb~50 uK at 150 GHz (FIRAS, number counts)
• => few uK2
• We do actually have a clustering model
BLAST: Viero et al 2009
• Extrapolate ARCADE results to 150 GHz: 5uK
• Extrapolate source models: less than 1 uK
– => << 1uK2 clustering power at 150 GHz
• Aside: ARCADE extrapolation to 30 GHz: T~200 uK
• 30 GHz clustering power could be >50 uK2
• However: widely agree that ARCADE results are hard to reconcile with known populations
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Radio Source Clustering
Fixsen et al 2009
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