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The rates and time-delay distribution of multiply imaged supernovae behind lensing clusters
Cosmology and Nongalactic Astrophysics · Submitted 29 Oct 2012
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim 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 \Delta t)=5.3 x 10^-4 \Delta t^\beta M_250^-2\beta, with \beta=0.77, where M_250 is the projected cluster mass inside 250 kpc (in 10^14 M_sun), and \beta is the power-law slope of the distribution.
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The abstract, sentence by sentence
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 \Delta t)=5.3 x 10^-4 \Delta t^\beta M_250^-2\beta, with \beta=0.77, where M_250 is the projected cluster mass inside 250 kpc (in 10^14 M_sun), and \beta 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 x 10^14 M_sun, 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 larger than 500 km/s, 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.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Time delays of gravitationally lensed sources can be used to constrain the mass model of a deflector and determine cosmological parameters. | background 1.00 | 0.04 | 0.04 | asserted 0.63 |
| s1 | 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. | contribution 0.99 | 0.94 | 0.06 | asserted 0.91 |
| s2 | 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 \Delta t)=5.3 x 10^-4 \Delta t^\beta M_250^-2\beta, with \beta=0.77, where M_250 is the projected cluster mass inside 250 kpc (in 10^14 M_sun), and \beta is the power-law slope of the distribution. | result 1.00 | 0.96 | 0.53 | asserted 1.00 |
| s3 | The resultant probability distribution function enables us to estimate the time-delay distribution in a lensing cluster of known mass. | interpretation 0.68 | 0.73 | 0.13 | asserted 0.82 |
| s4 | For a cluster with M_250=2 x 10^14 M_sun, the fraction of time delays less than 1000 days is approximately 3%. | result 1.00 | 0.89 | 0.09 | asserted 0.91 |
| s5 | Taking Abell 1689 as an example, its dark halo and brightest galaxies, with central velocity dispersions larger than 500 km/s, mainly produce large time delays, while galaxy-scale mass clumps are responsible for generating smaller time delays. | interpretation 0.70 | 0.79 | 0.08 | asserted 0.99 |
| s6 | We estimate the probability of observing multiple images of a supernova in the known images of Abell 1689. | contribution 0.86 | 0.92 | 0.04 | asserted 0.89 |
| s7 | A two-component model of estimating the supernova rate is applied in this work. | method 0.98 | 0.82 | 0.03 | asserted 0.98 |
| s8 | 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). | result 1.00 | 0.92 | 0.16 | asserted 1.00 |
| s9 | 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. | result 1.00 | 0.89 | 0.12 | asserted 0.97 |
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The paper
Original abstract
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 \Delta t)=5.3 x 10^-4 \Delta t^\beta M_250^-2\beta, with \beta=0.77, where M_250 is the projected cluster mass inside 250 kpc (in 10^14 M_sun), and \beta 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 x 10^14 M_sun, 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 larger than 500 km/s, 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.
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How the literature uses it
1 arXiv paper cite this in 1 sentence
What it cites · 12 sentences without a confident label
Uses the method or tool of 2 papers
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With the help of Lenstool [ref] , we can obtain a list of all images of every source in the source plane.
A Bayesian approach to strong lensing modelling of galaxy clusters · Modeling clusters of galaxies · 1.00
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In group one, with data of photometry from HST/ACS in bands B, V, I, Z, ground-based near-infrared imaging and Spitzer/IRAC photometry [ref] , we derive their stellar mass from SED fitting [ref] .
Fitting the integrated Spectral Energy Distributions of Galaxies · The rate of lensed supernovae in Abell 1689 · 0.80
Uses data or values from 3 papers
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The cluster masses [ref] [ref] and the fitting values of $β$ are shown in table [ref].
LoCuSS: First Results from Strong-lensing Analysis of 20 Massive Galaxy Clusters at z~0.2 · Estimating $β$ · 0.96
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We base our work on the mass model consisting of 35 plausible lensed sources and 116 multiple images [ref] [ref] [ref] .
Cosmological Constraints from Strong Gravitational Lensing in Galaxy Clusters · An example: Abell 1689 · 0.95
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For parameters $Â$ and $α$, we choose $Â = 1.05 ±0.16$ and $α= 0.68 ±0.01$ [ref] .
The SDSS-II Supernova Survey: Parameterizing the Type Ia Supernova Rate as a Function of Host Galaxy Properties · The rate of lensed supernovae in Abell 1689 · 1.00
Compares with 1 paper
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We compared the results in this work to [ref] as shown in figure <ref>, and discussed the possible reasons which may cause the differences.
Near-IR search for lensed supernovae behind galaxy clusters: III. Implications for cluster modeling and cosmology · Summary and discussion · 1.00
Cites as background 11 papers
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There are several theoretical profiles established to describe the mass distribution of a cluster: the SIS profile, the dPIE profile (dual pseudo isothermal elliptical profile) [ref] , and the NFW profile (Navarro-Frenk-White profile) [ref] , etc.
Where is the matter in the Merging Cluster Abell 2218? · Time delay theory · 0.97
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So far, time delays have been studied and applied in many ways: to constrain the Hubble parameter $H_0$ [ref] [ref] [ref] ; to study the galaxy mass profile with Monte Carlo simulations [ref] ; to measure the cosmological parameter $w$ [ref] [ref] [ref] [ref] [ref] ; to improve the mass models of galaxies with the time delays of quasars [ref] .
Two accurate time-delay distances from strong lensing: Implications for cosmology · Introduction · 0.82
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So far, time delays have been studied and applied in many ways: to constrain the Hubble parameter $H_0$ [ref] [ref] [ref] ; to study the galaxy mass profile with Monte Carlo simulations [ref] ; to measure the cosmological parameter $w$ [ref] [ref] [ref] [ref] [ref] ; to improve the mass models of galaxies with the time delays of quasars [ref] .
Cosmological Constraints from Gravitational Lens Time Delays · Introduction · 0.82
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