TY - JOUR

T1 - Locating the baryon acoustic peak

AU - Simpson, Fergus

AU - Peacock, John A.

AU - Simon, Patrick

PY - 2009/3/1

Y1 - 2009/3/1

N2 - Forthcoming photometric redshift surveys should provide an accurate
probe of the acoustic peak in the two-point galaxy correlation function,
in the form of angular clustering of galaxies within a given shell in
redshift space. We investigate the form of the anticipated signal,
quantifying the distortions that arise due to projection effects, and,
in particular, explore the validity of applying the Limber
approximation. A single-integral prescription is presented, which
provides an alternative to Limber’s equation, and produces a
significantly improved prediction in the regime of interest. The
position of the acoustic peak within the angular correlation function
relates to the angular diameter distance to the far side of the redshift
bin. Thicker redshift bins therefore shift comoving features toward
smaller angular scales. As a result, the value of the photometric
redshift error acquires a greater significance, particularly at lower
redshifts. In order to recover the dark energy equation of state to a
level of 1%, we find the total redshift dispersion must be determined to
within Δσz≲10-3, which may prove
challenging to achieve in practice.

AB - Forthcoming photometric redshift surveys should provide an accurate
probe of the acoustic peak in the two-point galaxy correlation function,
in the form of angular clustering of galaxies within a given shell in
redshift space. We investigate the form of the anticipated signal,
quantifying the distortions that arise due to projection effects, and,
in particular, explore the validity of applying the Limber
approximation. A single-integral prescription is presented, which
provides an alternative to Limber’s equation, and produces a
significantly improved prediction in the regime of interest. The
position of the acoustic peak within the angular correlation function
relates to the angular diameter distance to the far side of the redshift
bin. Thicker redshift bins therefore shift comoving features toward
smaller angular scales. As a result, the value of the photometric
redshift error acquires a greater significance, particularly at lower
redshifts. In order to recover the dark energy equation of state to a
level of 1%, we find the total redshift dispersion must be determined to
within Δσz≲10-3, which may prove
challenging to achieve in practice.

UR - http://www.scopus.com/inward/record.url?scp=63249117617&partnerID=8YFLogxK

U2 - 10.1103/PhysRevD.79.063508

DO - 10.1103/PhysRevD.79.063508

M3 - Article

VL - 79

JO - Physical Review D

JF - Physical Review D

SN - 1550-7998

IS - 6

M1 - 63508

ER -