TY - JOUR
T1 - The rates and time-delay distribution of multiply imaged supernovae behind lensing clusters
AU - Li, Xue
AU - Hjorth, Jens
AU - Richard, Johan
PY - 2012/11/4
Y1 - 2012/11/4
N2 - Time delays of gravitationally lensed sources can be used to constrain the mass model of a deflector and determine cosmological parameters. We here present an analysis of the time-delay distribution of multiply imaged sources behind 17 strong lensing galaxy clusters with well-calibrated mass models. We find that for time delays less than 1000 days, at z = 3.0, their logarithmic probability distribution functions are well represented by P(log Δt) = 5.3 × 10 -4Δt M 250 2, with = 0.77, where M 250 is the projected cluster mass inside 250 kpc (in 10 14 M), and is the power-law slope of the distribution. The resultant probability distribution function enables us to estimate the time-delay distribution in a lensing cluster of known mass. For a cluster with M 250 = 2 × 10 14 M, the fraction of time delays less than 1000 days is approximately 3%. Taking Abell 1689 as an example, its dark halo and brightest galaxies, with central velocity dispersions σ500kms -1, mainly produce large time delays, while galaxy-scale mass clumps are responsible for generating smaller time delays. We estimate the probability of observing multiple images of a supernova in the known images of Abell 1689. A two-component model of estimating the supernova rate is applied in this work. For a magnitude threshold of m AB = 26.5, the yearly rate of Type Ia (core-collapse) supernovae with time delays less than 1000 days is 0.004±0.002 (0.029±0.001). If the magnitude threshold is lowered to m AB ∼ 27.0, the rate of core-collapse supernovae suitable for time delay observation is 0.044±0.015 per year.
AB - Time delays of gravitationally lensed sources can be used to constrain the mass model of a deflector and determine cosmological parameters. We here present an analysis of the time-delay distribution of multiply imaged sources behind 17 strong lensing galaxy clusters with well-calibrated mass models. We find that for time delays less than 1000 days, at z = 3.0, their logarithmic probability distribution functions are well represented by P(log Δt) = 5.3 × 10 -4Δt M 250 2, with = 0.77, where M 250 is the projected cluster mass inside 250 kpc (in 10 14 M), and is the power-law slope of the distribution. The resultant probability distribution function enables us to estimate the time-delay distribution in a lensing cluster of known mass. For a cluster with M 250 = 2 × 10 14 M, the fraction of time delays less than 1000 days is approximately 3%. Taking Abell 1689 as an example, its dark halo and brightest galaxies, with central velocity dispersions σ500kms -1, mainly produce large time delays, while galaxy-scale mass clumps are responsible for generating smaller time delays. We estimate the probability of observing multiple images of a supernova in the known images of Abell 1689. A two-component model of estimating the supernova rate is applied in this work. For a magnitude threshold of m AB = 26.5, the yearly rate of Type Ia (core-collapse) supernovae with time delays less than 1000 days is 0.004±0.002 (0.029±0.001). If the magnitude threshold is lowered to m AB ∼ 27.0, the rate of core-collapse supernovae suitable for time delay observation is 0.044±0.015 per year.
U2 - 10.1088/1475-7516/2012/11/015
DO - 10.1088/1475-7516/2012/11/015
M3 - Journal article
SN - 1475-7516
VL - 2012
SP - 015
JO - Journal of Cosmology and Astroparticle Physics
JF - Journal of Cosmology and Astroparticle Physics
IS - 11
ER -