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A scale dependent bias on linear scales: the case for HI intensity mapping at z=1

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A scale dependent bias on linear scales : the case for HI intensity mapping at z=1. / Pénin, Aurélie; Umeh, Obinna; Santos, Mario.

In: Monthly Notices of the Royal Astronomical Society, Vol. 473, No. 1, 01.02.2018, p. 4297–4305.

Research output: Contribution to journalArticlepeer-review

Harvard

Pénin, A, Umeh, O & Santos, M 2018, 'A scale dependent bias on linear scales: the case for HI intensity mapping at z=1', Monthly Notices of the Royal Astronomical Society, vol. 473, no. 1, pp. 4297–4305. https://doi.org/10.1093/mnras/stx2635

APA

Pénin, A., Umeh, O., & Santos, M. (2018). A scale dependent bias on linear scales: the case for HI intensity mapping at z=1. Monthly Notices of the Royal Astronomical Society, 473(1), 4297–4305. https://doi.org/10.1093/mnras/stx2635

Vancouver

Pénin A, Umeh O, Santos M. A scale dependent bias on linear scales: the case for HI intensity mapping at z=1. Monthly Notices of the Royal Astronomical Society. 2018 Feb 1;473(1):4297–4305. https://doi.org/10.1093/mnras/stx2635

Author

Pénin, Aurélie ; Umeh, Obinna ; Santos, Mario. / A scale dependent bias on linear scales : the case for HI intensity mapping at z=1. In: Monthly Notices of the Royal Astronomical Society. 2018 ; Vol. 473, No. 1. pp. 4297–4305.

Bibtex

@article{112b0d9480934e7da2297018fd944b5b,
title = "A scale dependent bias on linear scales: the case for HI intensity mapping at z=1",
abstract = "Neutral hydrogen (HI) will soon be the dark matter tracer observed over the largest volumes of Universe thanks to the 21 cm intensity mapping technique. To unveil cosmological information it is indispensable to understand the HI distribution with respect to dark matter. Using a full one-loop derivation of the power spectrum of HI, we show that higher order corrections change the amplitude and shape of the power spectrum on typical cosmological (linear) scales. These effects go beyond the expected dark matter non-linear corrections and include non-linearities in the way the HI signal traces dark matter. We show that, on linear scales at z = 1, the HI bias drops by up to 15% in both real and redshift space, which results in underpredicting the mass of the halos in which HI lies. Non-linear corrections give rise to a significant scale dependence when redshift space distortions arise, in particular on the scale range of the baryonic acoustic oscillations (BAO). There is a factor of 5 difference between the linear and full HI power spectra over the full BAO scale range, which will modify the ratios between the peaks. This effect will also be seen in other types of survey and it will be essential to take it into account in future experiments in order to match the expectations of precision cosmology. ",
keywords = "astro-ph.CO",
author = "Aur{\'e}lie P{\'e}nin and Obinna Umeh and Mario Santos",
note = "10 pages, 7 figures, Accepted by MNRAS",
year = "2018",
month = feb,
day = "1",
doi = "10.1093/mnras/stx2635",
language = "English",
volume = "473",
pages = "4297–4305",
journal = "MNRAS",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "1",

}

RIS

TY - JOUR

T1 - A scale dependent bias on linear scales

T2 - the case for HI intensity mapping at z=1

AU - Pénin, Aurélie

AU - Umeh, Obinna

AU - Santos, Mario

N1 - 10 pages, 7 figures, Accepted by MNRAS

PY - 2018/2/1

Y1 - 2018/2/1

N2 - Neutral hydrogen (HI) will soon be the dark matter tracer observed over the largest volumes of Universe thanks to the 21 cm intensity mapping technique. To unveil cosmological information it is indispensable to understand the HI distribution with respect to dark matter. Using a full one-loop derivation of the power spectrum of HI, we show that higher order corrections change the amplitude and shape of the power spectrum on typical cosmological (linear) scales. These effects go beyond the expected dark matter non-linear corrections and include non-linearities in the way the HI signal traces dark matter. We show that, on linear scales at z = 1, the HI bias drops by up to 15% in both real and redshift space, which results in underpredicting the mass of the halos in which HI lies. Non-linear corrections give rise to a significant scale dependence when redshift space distortions arise, in particular on the scale range of the baryonic acoustic oscillations (BAO). There is a factor of 5 difference between the linear and full HI power spectra over the full BAO scale range, which will modify the ratios between the peaks. This effect will also be seen in other types of survey and it will be essential to take it into account in future experiments in order to match the expectations of precision cosmology.

AB - Neutral hydrogen (HI) will soon be the dark matter tracer observed over the largest volumes of Universe thanks to the 21 cm intensity mapping technique. To unveil cosmological information it is indispensable to understand the HI distribution with respect to dark matter. Using a full one-loop derivation of the power spectrum of HI, we show that higher order corrections change the amplitude and shape of the power spectrum on typical cosmological (linear) scales. These effects go beyond the expected dark matter non-linear corrections and include non-linearities in the way the HI signal traces dark matter. We show that, on linear scales at z = 1, the HI bias drops by up to 15% in both real and redshift space, which results in underpredicting the mass of the halos in which HI lies. Non-linear corrections give rise to a significant scale dependence when redshift space distortions arise, in particular on the scale range of the baryonic acoustic oscillations (BAO). There is a factor of 5 difference between the linear and full HI power spectra over the full BAO scale range, which will modify the ratios between the peaks. This effect will also be seen in other types of survey and it will be essential to take it into account in future experiments in order to match the expectations of precision cosmology.

KW - astro-ph.CO

U2 - 10.1093/mnras/stx2635

DO - 10.1093/mnras/stx2635

M3 - Article

VL - 473

SP - 4297

EP - 4305

JO - MNRAS

JF - MNRAS

SN - 0035-8711

IS - 1

ER -

ID: 11020976