J/ApJS/170/288 WMAP 3 Year Temperature Analysis (Hinshaw+, 2007)
Three-year Wilkinson microwave anisotropy probe (WMAP) observations:
temperature analysis.
Hinshaw G., Nolta M.R., Bennett C.L., Bean R., Dore O., Greason M.R.,
Halpern M., Hill R.S., Jarosik N., Kogut A., Komatsu E., Limon M.,
Odegard N., Meyer S.S., Page L., Peiris H.V., Spergel D.N., Tucker G.S.,
Verde L., Weiland J.L., Wollack E., Wright E.L.
<Astrophys. J. Suppl. Ser., 170, 288-334 (2007)>
=2007ApJS..170..288H 2007ApJS..170..288H
ADC_Keywords: Effective temperatures ; Radio sources ; Spectroscopy
Mission_Name: WMAP
Keywords: cosmic microwave background - cosmology: observations - dark matter -
early universe instrumentation: detectors -
space vehicles: instruments - telescopes
Abstract:
We present new full-sky temperature maps in five frequency bands from
23 to 94GHz, based on data from the first 3 years of the WMAP sky
survey. The new maps are consistent with the first-year maps and are
more sensitive. We employ two forms of multifrequency analysis to
separate astrophysical foreground signals from the CMB, each of which
improves on our first-year analyses. First, we form an improved
"Internal Linear Combination" (ILC) map, based solely on WMAP data,
by adding a bias-correction step and by quantifying residual
uncertainties in the resulting map. Second, we fit and subtract new
spatial templates that trace Galactic emission; in particular, we now
use low-frequency WMAP data to trace synchrotron emission instead of
the 408MHz sky survey. The WMAP point source catalog is updated to
include 115 new sources whose detection is made possible by the
improved sky map sensitivity. We derive the angular power spectrum
of the temperature anisotropy using a hybrid approach that combines
a maximum likelihood estimate at low l (large angular scales) with a
quadratic cross-power estimate for l>30. The resulting multifrequency
spectra are analyzed for residual point source contamination.
At 94GHz the unmasked sources contribute 128±27{micron}K2 to
l(l+1)Cl/2π at l=1000. After subtracting this contribution, our
best estimate of the CMB power spectrum is derived by averaging
cross-power spectra from 153 statistically independent channel pairs.
A simple six-parameter {LAMBDA}CDM model continues to fit CMB data and
other measures of large-scale structure remarkably well. The new
polarization data produce a better measurement of the optical depth to
reionization, τ=0.089±0.03. This new and tighter constraint on
τ help break a degeneracy with the scalar spectral index, which is
now found to be ns=0.960±0.016.
Description:
The Wilkinson Microwave Anisotropy Probe (WMAP) is a Medium-class
Explorer (MIDEX) mission designed to elucidate cosmology by producing
full-sky maps of the cosmic microwave background (CMB) anisotropy. The
3 year WMAP data encompass the period from 00:00:00 UT, 2001 August 10
(day 222) to 00:00:00 UT, 2004 August 9 (day 222).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table6.dat 95 323 Three-Year Wilkinson Microwave Anisotropy Probe
(WMAP) Observations: Temperature Analysis
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See also:
VIII/40 : GB6 catalog of radio sources (Gregory+ 1996)
VIII/38 : The Parkes-MIT-NRAO 4.85GHz (PMN) Surveys (Griffith+ 1993-96)
J/AZh/85/483 : Sources from the WMAP catalog (Vol'vach+, 2008)
J/ApJS/170/108 : NEWPS5σ Source Catalogue (Lopez-Caniego+, 2007)
J/ApJS/148/97 : The WMAP First Year Source Catalog (WMAP1) (Bennett+, 2003)
Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 2 I2 h RAh Hour of Right Ascension (J2000)
4- 5 I2 min RAm Minute of Right Ascension (J2000)
7- 8 I2 s RAs Second of Right Ascension (J2000)
10 A1 --- DE- Sign of the Declination (J2000)
11- 12 I2 deg DEd Degree of Declination (J2000)
14- 15 I2 arcmin DEm Arcminute of Declination (J2000)
17- 19 I3 --- WMAP ? Source identification number (1)
21- 24 F4.1 Jy S(K) ? The K band (22.5GHz) flux density
26- 29 F4.2 Jy e_S(K) ? Uncertainty in KFlux
31- 34 F4.1 Jy S(Ka) ? The Ka band (32.8GHz) flux density
36- 39 F4.2 Jy e_S(Ka) ? Uncertainty in KaFlux
41- 44 F4.1 Jy S(Q) ? The Q band (40.4GHz) flux density
46- 49 F4.2 Jy e_S(Q) ? Uncertainty in QFlux
51- 54 F4.1 Jy S(V) ? The V band (60.2GHz) flux density
56- 58 F3.1 Jy e_S(V) ? Uncertainty in VFlux
60- 63 F4.1 Jy S(W) ? The W band (93.0GHz) flux density
65- 67 F3.1 Jy e_S(W) ? Uncertainty in WFlux
69- 72 F4.1 --- alf Spectral index in the WMAP bands
74- 77 F4.2 --- e_alf Uncertainty in spectral index alf
79- 93 A15 --- 5GHzID The 5GHz identification
95 A1 --- Note Source note (2)
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Note (1): From the first-year catalog, Bennett et al. 2003, Cat. J/ApJS/148/97
Note (2): Note as follows:
a = Indicates the source has multiple possible identifications.
b = Source J0322-3711 (Fornax A) is extended, and the fluxes listed were
obtained by aperture photometry.
c = Source J0519-0540 is a blend of the Lynds Bright Nebulae
LBN 207.65-23.11 and LBN 207.29-22.66.
d = Source J1357+7644 is outside of the declination range of the GB6 and
PMN catalogs. Identified as QSO NVSSJ135755+764320 by Trushkin (2006,
private communication).
e = Source J1633+8227 is outside of the declination range of the GB6 and
PMN catalogs. It was identified as NGC 6251 by
Trushkin (2003BSAO...55...90T 2003BSAO...55...90T).
f = Source J1657+4749 is identified as QSO GB6J1658+4737 by
Trushkin (2006, private communication). Offset from the WMAP position
is 11.6 arcminutes.
g = Source J2356+4952 is identified as GB6 J2355+4950 by
Trushkin (2003BSAO...55...90T 2003BSAO...55...90T).
Offset from the WMAP position is 11.9 arcminutes.
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 09-Apr-2009