Anisotropy in the Microwave Sky: Results from the First Flight of the Balloon-borne Anisotropy Measurement (BAM)

Tucker, Gregory S.; Gush, H. P.; Halpern, M.; Shinkoda, I.; Towlson, W. A.

doi:10.1086/310468

Cited by 33 publications

(10 citation statements)

References 10 publications

(9 reference statements)

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“… (1) Tegmark & Hamilton 1997; (2) Ganga et al 1994; (3) Gutiérrez et al 1997; Hancock et al 1997 (binned); (4) Gundersen et al 1995; (5) Femenia et al 1998; (6) Tucker et al 1997; (7) Platt et al 1997; (8) Piccirillo & Calisse 1993; (9 a ) de Bernardis et al 1994; (9 b ) Masi et al 1996; (10) Tanaka et al 1996 (binned); (11) de Oliveira‐Costa et al 1998; (12) Netterfield et al 1997; (13) Wilson et al 1999; (14 a ) Scott et al 1996; and Hancock & Rocha 1997; (14 b ) Baker et al 1998 (15) Leitch et al 1998. …”

Section: The Observational Datamentioning

confidence: 99%

Cosmic microwave background constraints on the epoch of reionization

Griffiths

Barbosa

Liddle

1999

Monthly Notices of the Royal Astronomical Society

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We use a compilation of cosmic microwave anisotropy data to constrain the epoch of reionization in the Universe, as a function of cosmological parameters. We consider spatially-flat cosmologies, varying the matter density $\Omega_0$ (the flatness being restored by a cosmological constant), the Hubble parameter $h$ and the spectral index $n$ of the primordial power spectrum. Our results are quoted both in terms of the maximum permitted optical depth to the last-scattering surface, and in terms of the highest allowed reionization redshift assuming instantaneous reionization. For critical-density models, significantly-tilted power spectra are excluded as they cannot fit the current data for any amount of reionization, and even scale-invariant models must have an optical depth to last scattering of below 0.3. For the currently-favoured low-density model with $\Omega_0 = 0.3$ and a cosmological constant, the earliest reionization permitted to occur is at around redshift 35, which roughly coincides with the highest estimate in the literature. We provide general fitting functions for the maximum permitted optical depth, as a function of cosmological parameters. We do not consider the inclusion of tensor perturbations, but if present they would strengthen the upper limits we quote.Comment: 9 pages LaTeX file with ten figures incorporated (uses mn.sty and epsf). Corrects some equation typos, superseding published versio

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Section: The Observational Datamentioning

confidence: 99%

Cosmic microwave background constraints on the epoch of reionization

Griffiths

Barbosa

Liddle

1999

Monthly Notices of the Royal Astronomical Society

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“…This analysis used a statistically independent subset of the current data and carried out χ 2 fitting for a range of cosmological models and parameters. The extensions carried out for the present work were (a) the inclusion of the CAT2 point at ℓ = 422; (b) the inclusion of new points from experiments Python (Python III, Platt et al 1997), MSAM (the 2nd and 3rd flights, Cheng et al 1996, Ratra et al 1997, ARGO (Aries+Taurus region, Masi et al 1996), FIRS (Ganga et al 1994) and BAM (Tucker et al 1997), and with the latest calibration correction to the Saskatoon data (i.e. increased by 5%, Leitch, private communication); (c) consideration of a wider class of cosmological models, all treated using exact power spectra rather than the generic forms assumed in Hancock et al (see also Rocha 1997;Rocha et al in preparation).…”

Section: Estimation Of Cosmological Parameters Using New Cat Resultsmentioning

confidence: 99%

Detection of cosmic microwave background structure in a second field with the Cosmic Anisotropy Telescope

Baker¹,

Grainge²,

Hobson³

et al. 1999

Monthly Notices of the Royal Astronomical Society

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We describe observations at frequencies near 15 GHz of the second 2×2 deg2 field imaged with the Cambridge Cosmic Anisotropy Telescope (CAT). After the removal of discrete radio sources, structure is detected in the images on characteristic scales of about half a degree, corresponding to spherical harmonic multipoles in the range ℓ≈330–680. A Bayesian analysis confirms that the signal arises predominantly from the cosmic microwave background (CMB) radiation for multipoles in the lower half of this range; the average broad‐band power in a bin with centroid 𝓁=422 (θ≈51 arcmin) is estimated to be . For multipoles centred on ℓ=615 (θ≈35 arcmin), we find contamination from Galactic emission is significant, and constrain the CMB contribution to the measured power in this bin to be ΔTT<2.0×10−5 (1σ upper limit). These new results are consistent with the first detection made by CAT in a completely different area of sky. Together with data from other experiments, this new CAT detection adds weight to earlier evidence from CAT for a downturn in the CMB power spectrum on scales smaller than 1 deg. Improved limits on the values of H0 and Ω are determined using the new CAT data.

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“…References.-(1) Kuo et al 2004; (2) Alsop et al 1992;Lim et al 1996;Tanaka et al 1996; (3) Gunderson et al 1995; (4) Benoît et al 2003;(5) Ganga et al 1997;Gunderson et al 1995;(6) de Bernardis et al 1993(6) de Bernardis et al , 1994(7) de Bernardis et al 1993Bernardis et al , 1994Masi et al 1995Masi et al , 1996(8) Tucker et al 1997;(9) Mauskopf et al 2000;Piacentini et al 2002;(10) Crill et al 2003;Netterfield et al 2002;Ruhl et al 2003;(11) Scott et al 1996;(12) Baker et al 1999;(13) Padin et al 2001Padin et al , 2002(14) Mason et al 2003;(15) Mason et al 2003;Pearson et al 2003;(16) Kogut et al 1992Kogut et al , 1996Tegmark & Hamilton 1997;(17) Halverson et al 2002;Leitch et al 2002;(18) Page, Cheng, & Meyer 1990;…”

Section: Foregroundsunclassified

Testing the Cosmic Microwave Background Data for Systematic Effects

Griffiths

Lineweaver

2004

ApJ

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Under the assumption that the concordance Ã cold dark matter (CDM) model is the correct model, we test the cosmic microwave background (CMB) anisotropy data for systematic effects by examining the bandpass temperature residuals with respect to this model. Residuals are analyzed as a function of angular scale l, Galactic latitude, frequency, calibration source, instrument type, and several other variables that may be associated with potential systematic effects. Our main result is that we find no significant systematic errors associated with these variables. However, we do find marginal evidence for a trend associated with Galactic latitude indicative of Galactic contamination.

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Anisotropy in the Microwave Sky: Results from the First Flight of the Balloon-borne Anisotropy Measurement (BAM)

Cited by 33 publications

References 10 publications

Cosmic microwave background constraints on the epoch of reionization

Cosmic microwave background constraints on the epoch of reionization

Detection of cosmic microwave background structure in a second field with the Cosmic Anisotropy Telescope

Testing the Cosmic Microwave Background Data for Systematic Effects

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