Testing the Cosmic Microwave Background Data for Systematic Effects

Griffiths, Louise M.; Lineweaver, Charles H.

doi:10.1086/381493

Cited by 3 publications

(4 citation statements)

References 88 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The different instruments have different potential systematic problems and they cover a wide range of frequencies. The agreement therefore indicates that none of the experiments is seriously contaminated by foreground emission or other systematic effects (see also Griffiths & Lineweaver 2004). From the analysis of the peak structure (Section 5.3), there is extremely good agreement on the peak structure between experiments, except for a slight discrepancy in the amplitude of the third peak, which may have important consequences for the cosmological models.…”

Section: O N C L U S I O N Smentioning

confidence: 74%

High-sensitivity measurements of the cosmic microwave background power spectrum with the extended Very Small Array

Dickinson

Battye

Carreira

et al. 2004

Monthly Notices of the Royal Astronomical Society

188

View full text Add to dashboard Cite

We present deep Ka‐band (ν≈ 33 GHz) observations of the cosmic microwave background (CMB) made with the extended Very Small Array (VSA). This configuration produces a naturally weighted synthesized FWHM beamwidth of ∼11 arcmin, which covers an ℓ range of 300 to 1500. On these scales, foreground extragalactic sources can be a major source of contamination to the CMB anisotropy. This problem has been alleviated by identifying sources at 15 GHz with the Ryle Telescope and then monitoring these sources at 33 GHz using a single‐baseline interferometer collocated with the VSA. Sources with flux densities ≳20 mJy at 33 GHz are subtracted from the data. In addition, we calculate a statistical correction for the small residual contribution from weaker sources that are below the detection limit of the survey. The CMB power spectrum corrected for Galactic foregrounds and extragalactic point sources is presented. A total ℓ range of 150–1500 is achieved by combining the complete extended array data with earlier VSA data in a compact configuration. Our resolution of Δℓ≈ 60 allows the first three acoustic peaks to be clearly delineated. This is achieved by using mosaiced observations in seven regions covering a total area of 82 deg2. There is good agreement with the Wilkinson Microwave Anisotropy Probe (WMAP) data up to ℓ= 700 where WMAP data run out of resolution. For higher ℓ values out to ℓ= 1500, the agreement in power spectrum amplitudes with other experiments is also very good despite differences in frequency and observing technique.

show abstract

Section: O N C L U S I O N Smentioning

confidence: 74%

High-sensitivity measurements of the cosmic microwave background power spectrum with the extended Very Small Array

Dickinson

Battye

Carreira

et al. 2004

Monthly Notices of the Royal Astronomical Society

188

View full text Add to dashboard Cite

show abstract

“…It is therefore critical to ensure that these contaminants can be controlled to a level that does not jeopardize the science goals of the mission. The impact of systematic effects plays a central role in the analysis of modern CMB experiments [2-4, 27, 44, 47] and is the main subject of several papers as well (e.g., [16,20,32,45]), many of them focusing specifically on polarization specific systematics and their treatment [19,33,36,54]. The definition of a systematic effect is somewhat dependent on the context.…”

Section: Jcap04(2018)022mentioning

confidence: 99%

“…The impact of systematic effects plays a central role in the analysis of modern CMB experiments (Baxter et al 2015;Bennett et al 2013;BICEP2 Collaboration et al 2016;Louis et al 2016;Planck Collaboration et al 2016c,f) and is the main subject of several papers as well (e.g., Griffiths and Lineweaver (2004); Karakci et al (2013); Miller et al (2009a); Planck Collaboration et al (2016d)), many of them focusing specifically on polarization specific systematics and their treatment (Kaplan and Delabrouille 2002;Miller et al 2009b;Pagano et al 2009;Shimon et al 2008). The definition of a systematic effect is somewhat dependent on the context.…”

Section: Introductionmentioning

confidence: 99%

Exploring cosmic origins with CORE: Mitigation of systematic effects

Natoli

Ashdown

Banerji

et al. 2018

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

We present an analysis of the main systematic effects that could impact the measurement of CMB polarization with the proposed CORE space mission. We employ timeline-to-map simulations to verify that the CORE instrumental setup and scanning strategy allow us to measure sky polarization to a level of accuracy adequate to the mission science goals. We also show how the CORE observations can be processed to mitigate the level of contamination by potentially worrying systematics, including intensity-to-polarization leakage due to bandpass mismatch, asymmetric main beams, pointing errors and correlated noise. We use analysis techniques that are well validated on data from current missions such as Planck to demonstrate how the residual contamination of the measurements by these effects can be brought to a level low enough not to hamper the scientific capability of the mission, nor significantly increase the overall error budget. We also present a prototype of the CORE photometric calibration pipeline, based on that used for Planck, and discuss its robustness to systematics, showing how CORE can achieve its calibration requirements. While a fine-grained assessment of the impact of systematics requires a level of knowledge of the system that can only be achieved in a future study phase, the analysis presented here strongly suggests that the main areas of concern for the CORE mission can be addressed using existing knowledge, techniques and algorithms.

show abstract

Section: Introductionmentioning

confidence: 99%

Exploring cosmic origins with CORE: mitigation of systematic effects

Natoli,

Ashdown,

Banerji

et al. 2017

Preprint

View full text Add to dashboard Cite

We present an analysis of the main systematic effects that could impact the measurement of CMB polarization with the proposed CORE space mission. We employ timeline-to-map simulations to verify that the CORE instrumental set-up and scanning strategy allow us to measure sky polarization to a level of accuracy adequate to the mission science goals. We also show how the CORE observations can be processed to mitigate the level of contamination by potentially worrying systematics, including intensity-to-polarization leakage due to bandpass mismatch, asymmetric main beams, pointing errors and correlated noise. We use analysis techniques that are well validated on data from current missions such as Planck to demonstrate how the residual contamination of the measurements by these effects can be brought to a level low enough not to hamper the scientific capability of the mission, nor significantly increase the overall error budget. We also present a prototype of the CORE photometric calibration pipeline, based on that used for Planck, and discuss its robustness to systematics, showing how CORE can achieve its calibration requirements. While a fine-grained assessment of the impact of systematics requires a level of knowledge of the system that can only be achieved in a future study phase, the analysis presented here strongly suggests that the main areas of concern for the CORE mission can be addressed using existing knowledge, techniques and algorithms.

show abstract

Testing the Cosmic Microwave Background Data for Systematic Effects

Cited by 3 publications

References 88 publications

High-sensitivity measurements of the cosmic microwave background power spectrum with the extended Very Small Array

High-sensitivity measurements of the cosmic microwave background power spectrum with the extended Very Small Array

Exploring cosmic origins with CORE: Mitigation of systematic effects

Exploring cosmic origins with CORE: mitigation of systematic effects

Contact Info

Product

Resources

About