CIB Fluctuations from. l ~ ,000. Marco Viero - Caltech
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1 CIB Fluctuations from l ~ ,000 Marco Viero - Caltech
2 Reichardt et al motivation 2
3 l > 2000 dominated by secondary anisotropies Reichardt et al motivation 2
4 SPT DSFGs Reichardt et al motivation (i) 3
5 SPT DSFGs Reichardt et al motivation (i) 3
6 SPT 2-halo (linear) Reichardt et al motivation (i) 3
7 SPT 1-halo (non-linear) 2-halo (linear) Reichardt et al motivation (i) 3
8 Shape of the Galaxy Spectrum at 3000 < SPT l < 4500 highly dependent on the the way star-forming galaxies occupy massive halos 1-halo (non-linear) 2-halo (linear) Reichardt et al motivation (i) 3
9 ACT 150 GHz motivation (ii) 4
10 ACT 150 GHz motivation (ii) 4
11 ACT 150 GHz motivation (ii) 4
12 Halo Occupation Distribution (HOD): How many satellites per given halo mass? ACT 150 GHz motivation (ii) 4
13 Halo Occupation Distribution (HOD): How many satellites per given halo mass? Luminosity-Mass relation? ACT 150 GHz motivation (ii) 4
14 ACT 150 GHz Halo Occupation Distribution (HOD): How many satellites per given halo mass? Luminosity-Mass relation? This is imprinted on the 1-halo term of the CIB power spectrum! motivation (ii) 4
15 The Team Marco Viero, Plus engineers, instrument builders, software developers etc.
16 1200 GHz 857 GHz 600 GHz data 6
17 XMM-LSS LOCKMAN-SWIRE CDFS-SWIRE ELAIS-S1 SMAP Team Alex Conley Louis Levenson Gaelen Marsden Marco Viero Mike Zemcov BOOTES SPIRE maps at 1200, 857, and 600 GHz Maps made with HeRMES SMAP pipeline 5 fields totaling ~ 70 deg 2 Modes >~ 0.5 deg filtered Sources > 50, 100, 200, 300 mjy masked data 6
18 250 μm (1200 GHz) 350 μm (857 GHz) 500 μm (600 GHz) FWHM = SMAP maps of Neptune calibration 7
19 SPIRE passbands 500 μm 350 μm 250 μm calibration 8
20 SPIRE passbands 500 μm 350 μm 250 μm calibration 9
21 SPIRE passbands 500 μm 350 μm 250 μm calibration 9
22 500 μm 350 μm 250 μm Spectral weight different for Neptune and CIB Beam corrections = 0.99, 0.98, 0.95 at 250, 350, and 500 μm effective beam area 10
23 1200 GHz 857 GHz 600 GHz 857 GHz 1200 GHz Combined 5 fields over 70 deg 2 Preliminary 600 GHz CIB power spectra 11
24 1200 GHz 857 GHz 600 GHz 857 GHz Poisson vs. Masking Level 1200 GHz Combined 5 fields over 70 deg 2 Preliminary 600 GHz CIB power spectra 11
25 Preliminary Poisson Combined 5 fields over 70 deg 2 1-halo 1200 GHz 2-halo 1-halo power vs. masking 12
26 Preliminary Poisson Combined 5 fields over 70 deg 2 1-halo 1200 GHz 2-halo 1-halo power vs. masking 12
27 Preliminary Poisson Combined 5 fields over 70 deg 2 1-halo 1200 GHz 2-halo 1-halo power vs. masking 12
28 Preliminary Poisson Combined 5 fields over 70 deg 2 1-halo 1200 GHz 2-halo 1-halo power vs. masking 12
29 Preliminary Poisson Combined 5 fields over 70 deg 2 1-halo 1200 GHz 2-halo 1-halo power vs. masking 12
30 Preliminary Poisson Combined 5 fields over 70 deg 2 1-halo 1200 GHz 2-halo 1-halo power vs. masking 12
31 1200 GHz 857 GHz 600 GHz 857 GHz Preliminary 1200 GHz Combined 5 fields over 70 deg GHz clustering spectra 13
32 1200 GHz 857 GHz 600 GHz 857 GHz Preliminary 1200 GHz Combined 5 fields over 70 deg GHz clustering spectra 13
33 1200 GHz 857 GHz 600 GHz 857 GHz Preliminary 1200 GHz Combined 5 fields over 70 deg GHz clustering spectra 13
34 ~270 deg 2 MJy/sr Colormap: IRAS 100 μm PI: Viero HerMES Large-Mode Survey (HeLMS) 14
35 ~270 deg 2 MJy/sr Colormap: IRAS 100 μm 15.5 PI: Viero HerMES Large-Mode Survey (HeLMS) 14
36 1200 GHz ~1.2 HeLMS 15
37 1200 GHz 20 ~1.2 HeLMS 15
38 DEC Today SDSS optical ACT (80 deg2 ) CFHT UKIDDS VLA Wiggle-z BOSS Tomorrow Imaging : RA Spectroscopy : Stripe 82 SDSS imaging (ugriz, i<22.75, 270 deg 2 ) CFHT Stripe 82 survey (170 deg 2, i<23.5, seeing<0.8") and VISTA J and K (this proposal) UKIDDS LAS, K vega =18.4 UKIDSS: DXS Field 4 CFHTLS W4 Level 6.5 Radio : BOSS (220 deg 2, 40,000 redshifts) DEEP2 and PRIMUS VVDS Wiggle z VLA ACT ALMA ACTpol Spitzer Warm Planck Visible from most sites HeLMS ancillary data 16
39 conclusions 17
40 Strength of 1-halo clustering term a strong function of the masking level conclusions 17
41 Strength of 1-halo clustering term a strong function of the masking level Fitting an HOD to the CIB spectra should provide insight on how DSFGs occupy dark matter halos conclusions 17
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