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Ground-based observatories
Input:
Detector:
advanced Virgo (design)
advanced LIGO (design)
advanced LIGO (in O3a)
Einstein Telescope
Cosmic Explorer Stage 1
Cosmic Explorer Stage 2
KAGRA
customised LIGO-type detector
customised ET-type detector
Arm length [m] (LIGO design: 3995 m)):
Laser power [W] (LIGO design: 125 W):
Cavity mirror transmission coefficient (-) (LIGO design: 0.014):
Signal recycling mirror transmission coefficient (-) (LIGO design: 0.2):
Power recycling mirror transmission coefficient (-) (LIGO design: 0.03):
Cavity mirror mass (kg) (LIGO design: 40):
Signal recycling phase offset (deg) (LIGO design: -90):
Power recycling cavity length (m) (LIGO design: 53):
Signal recycling cavity length (m) (LIGO design: 50.525):
Arm length [m] (ET design: 10000 m)):
Laser power [W] (ET design: 500 W):
Cavity mirror transmission coefficient (-) (ET design: 0.014):
Signal recycling mirror transmission coefficient (-) (ET design: 0.2):
Power recycling mirror transmission coefficient (-) (ET design: 0.03):
Cavity mirror mass (kg) (ET design: 200):
Signal recycling phase offset (deg) (ET design: -90):
Power recycling cavity length (m) (ET design: 53):
Signal recycling cavity length (m) (ET design: 50.525):
Event types:
Black Hole Binary Mergers
Double Neutron Star Mergers
NS-BH mergers
individual source
Population model for BHBH
Parameterization I (default param.)
Parameterization I (customised param.)
Parameterization II (default param.)
Parameterization II (customised param.)
[Introduction to models]
Rn (/yr/Gpc3):
(Norm. factor of the merger rate density)
τ (Gyr):
(Delay time from formation to merger)
µ(M☉):
(lower limit of mass)
c:
(related with mass peak)
γ:
(index of mass functoin tail)
mcut(M☉):
(high mass cut)
ql:
(lower cut of mass ratio)
σχ:
(dispersion of effective spin)
[Introduction to models]
Rn (/yr/Gpc3):
(Norm. factor of the merger rate density)
τ (Gyr):
(Delay time from formation to merger)
µ(M☉):
(lower limit of mass)
c:
(related with mass peak)
γ:
(index of mass functoin tail)
mcut(M☉):
(high mass cut)
m_peak(M☉):
(location of Gaussian mass peak)
m_peak_scale:
(relative height of Gaussian mass peak)
m_peak_sig(M☉):
(width of Gaussian mass peak)
ql:
(lower cut of mass ratio)
σχ:
(dispersion of effective spin)
Population model for NSNS
Parameterization I (default param.)
Parameterization I (customised param.)
[Introduction to models]
Rn (/yr/Gpc3):
(Norm. factor of the merger rate density)
tau (Gyr):
(Delay time from formation to merger)
m_peak(M☉):
(Peak of Gaussian mass)
m_scale(M☉):
(Width of Gaussian mass)
m_low(M☉):
(lower limit of mass)
m_high(M☉):
(Upper limit of mass)
σχ:
(dispersion of effective spin)
Population model for BHNS
Parameterization I (default param.)
Parameterization I (customised param.)
Parameterization II (default param.)
Parameterization II (customised param.)
[Introduction to models]
Rn (/yr/Gpc3):
(Norm. factor of the merger rate density)
tau (Gyr):
(Delay time from formation to merger)
m_peak(M☉):
(Peak of neutron star mass distr.)
m_scale(M☉):
(Width of NS mass distr.)
m_low(M☉):
(lower limit of NS mass)
m_high(M☉):
(Upper limit of mass)
µ(M☉):
(lower limit of mass)
c:
(related with mass peak)
γ:
(index of mass functoin tail)
mcut(M☉):
(high mass cut)
σχ:
(dispersion of effective spin)
[Introduction to models]
Rn (/yr/Gpc3):
(Norm. factor of the merger rate density)
tau (Gyr):
(Delay time from formation to merger)
m_peak(M☉):
(Peak of neutron star mass distr.)
m_scale(M☉):
(Width of NS mass distr.)
m_low(M☉):
(lower limit of NS mass)
m_high(M☉):
(Upper limit of mass)
µ(M☉):
(lower limit of mass)
c:
(related with mass peak)
γ:
(index of mass functoin tail)
mcut(M☉):
(high mass cut)
m_peak(M☉):
(location of BH Gaussian mass peak)
m_peak_scale(M☉):
(relative height of BH Gaussian mass peak)
m_peak_sig(M☉):
(width of BH Gaussian mass peak)
σχ:
(dispersion of effective spin)
z:
(cosmological redshift, valid only if D is not provided)
D:
(luminosity distance in Mpc)
m₁:
(mass of the primary star, in unit of solar masses)
m₂:
(mass of the secondary star, in unit of solar masse)
χ:
(effective spin)
Time [days]:
SNR-threshold:
Cosmology:
Flat ΛCDM - WMAP5
Flat ΛCDM - WMAP7
Flat ΛCDM - WMAP9
Flat ΛCDM - Planck13
Flat ΛCDM - Planck15
customised Flat ΛCDM
H0(km/s/Mpc):
Ω0:
Tcmb (K):
Desired outputs:
Number of Detection
Sensitivity Curve
Catalogue
Maximum number of events to generate:
Simulate uncertainties
list detectabilites
Takes a few minutes. Heavy task may cause timeout error. In this case, we recommend to run the python package locally.
Meaning of catalogue columns
m1: mass of the primary star, in unit of solar masses;
m2: mass of the secondary star, in unit of solar masses;
z: cosmological redshift;
D: luminosity distance in Mpc;
χ: effective spin;
d...: uncertainties of corresponding parameters.
Result:
Waiting for your input ...
Sensitivity curve:
File Name:
.json
download curve
Number of events:
Expected number of detection:
____
(The actual number of detection is a Poisson variable round the expectation)
Signal-to-noise ratio:
Expected SNR:
____
Plot:
X-axis:
Y-axis:
(if x-axis=y-axis, return a histogram)
X-error
Y-error
Logarithmic x-axis
Logarithmic y-axis
Table:
File Name:
.json
download catalogue