Predictions for the 21 cm-galaxy cross-power spectrum observable with LOFAR and Subaru

Vrbanec, Dijana; Ciardi, B.; Jelić, Vibor; Jensen, Hannes; Zaroubi, Saleem; Fernandez, Elizabeth R.; Ghosh, A.; Iliev, Ilian T.; Kakiichi, Koki; Koopmans, L. V. E.; Mellema, Garrelt

doi:10.1093/mnras/stv2993

Cited by 35 publications

(33 citation statements)

References 96 publications

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“…Imaging involves many difficulties (e.g., efficient gridding and mapmaking, foreground modeling), but if systematics can be overcome, it has the potential to compete with other more targeted experiments and analysis styles. More broadly, imaging analyses will be necessary to perform cross-correlation studies with complimentary probes such as galaxy surveys or other intensity mapping experiments (e.g., Lidz et al 2009;Doré et al 2014;Beardsley et al 2015;Silva et al 2015;DeBoer et al 2016;Vrbanec et al 2016), which will ultimately unlock the full potential of 21 cm observations. Here, we have identified a crucial region of power spectrum space that is currently contaminated, with suggestions for improvement in future analysis.…”

Section: Summary Of Planned Analysis Improvementsmentioning

confidence: 99%

First Season Mwa Eor Power Spectrum Results at Redshift 7

Beardsley

Hazelton

Sullivan

et al. 2016

ApJ

193

207

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The Murchison Widefield Array (MWA) has collected hundreds of hours of Epoch of Reionization (EoR) data and now faces the challenge of overcoming foreground and systematic contamination to reduce the data to a cosmological measurement. We introduce several novel analysis techniques, such as cable reflection calibration, hyper-resolution gridding kernels, diffuse foreground model subtraction, and quality control methods. Each change to the analysis pipeline is tested against a two-dimensional power spectrum figure of merit to demonstrate improvement. We incorporate the new techniques into a deep integration of 32 hoursof MWA data. This data set is used to place a systematic-limited upper limit on the cosmological power spectrum of  D2.7 10 2 4 mK 2 at k = 0.27 h Mpc −1 and z = 7.1, consistent with other published limits, and a modest improvement (factor of 1.4) over previous MWA results. From this deep analysis, we have identified a list of improvements to be made to our EoR data analysis strategies. These improvements will be implemented in the future and detailed in upcoming publications.

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Section: Summary Of Planned Analysis Improvementsmentioning

confidence: 99%

First Season Mwa Eor Power Spectrum Results at Redshift 7

Beardsley

Hazelton

Sullivan

et al. 2016

ApJ

193

207

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“…Lidz et al 2009;Park et al 2014;Vrbanec et al 2016). The turnover in the RSCFs shifts to larger scales if the EoR morphology is characterized by larger HII structures (c.f.…”

Section: Building Physical Intuition: Halo-21 CM Cross Correlationmentioning

confidence: 99%

Cross-correlation of the cosmic 21-cm signal and Lyman α emitters during reionization

Sobacchi

Mesinger

Greig

2016

Mon. Not. R. Astron. Soc.

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Interferometry of the cosmic 21-cm signal is set to revolutionize our understanding of the Epoch of Reionization (EoR), eventually providing 3D maps of the early Universe. Initial detections however will be low signal-to-noise, limited by systematics. To confirm a putative 21-cm detection, and check the accuracy of 21-cm data analysis pipelines, it would be very useful to cross-correlate against a genuine cosmological signal. The most promising cosmological signals are wide-field maps of Lyman alpha emitting galaxies (LAEs), expected from the Subaru Hyper-Suprime Cam (HSC) Ultra-Deep field. Here we present estimates of the correlation between LAE maps at z ∼ 7 and the 21-cm signal observed by both the Low Frequency Array (LOFAR) and the planned Square Kilometer Array Phase 1 (SKA1). We adopt a systematic approach, varying both: (i) the prescription of assigning LAEs to host halos; and (ii) the large-scale structure of neutral and ionized regions (i.e. EoR morphology). We find that the LAE-21cm cross-correlation is insensitive to (i), thus making it a robust probe of the EoR. A 1000 h observation with LOFAR would be sufficient to discriminate at ∼ > 1σ a fully ionized Universe from one with a mean neutral fraction ofx HI ≈ 0.50, using the LAE-21cm cross-correlation function on scales of R ≈3-10 Mpc. Unlike LOFAR, whose detection of the LAE-21cm cross-correlation is limited by noise, SKA1 is mostly limited by ignorance of the EoR morphology. However, the planned 100 h wide-field SKA1-Low survey will be sufficient to discriminate an ionized Universe from one withx HI = 0.25, even with maximally pessimistic assumptions.

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“…In Vrbanec et al (2016 we had investigated the feasibility of cross-correlations at z = 6.6 and 7.3 with LOFAR and HSC, as an agreement was in place among the two teams to observe the common field ELAIS-N1. As the LOFAR peak performance turned out to be at redshifts higher than initially envisioned (i.e.…”

Section: Introductionmentioning

confidence: 99%

Predictions for the 21cm-galaxy cross-power spectrum observable with SKA and future galaxy surveys

Vrbanec

Ciardi

Jelić

et al. 2020

Monthly Notices of the Royal Astronomical Society

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In this paper we use radiative transfer + N-body simulations to explore the feasibility of measurements of cross-correlations between the 21 cm field observed by the Square Kilometer Array (SKA) and high-z Lyman Alpha Emitters (LAEs) detected in galaxy surveys with the Subaru Hyper Supreme Cam (HSC), Subaru Prime Focus Spectrograph (PFS) and Wide Field Infrared Survey Telescope (WFIRST). 21cm-LAE cross-correlations are in fact a powerful probe of the epoch of reionization as they are expected to provide precious information on the progress of reionization and the typical scale of ionized regions at different redshifts. The next generation observations with SKA will have a noise level much lower than those with its precursor radio facilities, introducing a significant improvement in the measurement of the cross-correlations. We find that an SKA-HSC/PFS observation will allow to investigate scales below ∼ 10 h −1 Mpc and ∼ 60 h −1 Mpc at z = 7.3 and 6.6, respectively. WFIRST will allow to access also higher redshifts, as it is expected to observe spectroscopically ∼900 LAEs per square degree and unit redshift in the range 7.5 z 8.5. Because of the reduction of the shot noise compared to HSC and PFS, observations with WFIRST will result in more precise cross-correlations and increased observable scales.

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Predictions for the 21 cm-galaxy cross-power spectrum observable with LOFAR and Subaru

Cited by 35 publications

References 96 publications

First Season Mwa Eor Power Spectrum Results at Redshift 7

First Season Mwa Eor Power Spectrum Results at Redshift 7

Cross-correlation of the cosmic 21-cm signal and Lyman α emitters during reionization

Predictions for the 21cm-galaxy cross-power spectrum observable with SKA and future galaxy surveys

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