GW Plotter

The pages are currently maintained by Professor Vuk Mandic (University of Minnesota) and Erik Floden (University of Minnesota). Past contributors to this website include T. Regimbau, C. Lovdal, Chengjian Wu, Kyle Crocker, and Margot Fitz Axen.

If you decide to use a plot generated by this site please consider giving this site, and us, a credit. (You can remove the site address label from the plots with the check box at the bottom of the page.)

Please select each model and the relevent values for the parameters you wish to plot using the form below. When you have finished the selection press "Generate Plot" once and then wait for the new results page to appear. The new page can take some time to appear depending on the server load.
The Plot Specifications must be set to view the plot. Do not be give up if your plot is initially empty or if no plot is generated, instead redetermine the necessary x and y axis bounds. A meaningful plot will appear only if the selected model(s) predict a stochastic gravitational wave background within the selected frequency and amplitude ranges.
Note that the Behroozi et al. star formation rate and the Metallicity Dependent CCBH model are computationally intensive and can thus result in slower plot generation. Decreasing the number of points increases the speed at which plots are generated.

	Min	Max
X Axis ( Frequency):
Y Axis ( Energy Spectrum)
Number of Points	2	As long as you want to wait
Star Formation Rate
Set by	Configure the plot manually?

[Please note there may be up to 30 second wait for plots]
Model Name	Parameters	Plot Specify	Introduction
Astrophysical Models
BBH Range		linewidth
BBN PLI		linewidth
BNS Range		linewidth
Binary Black Holes Model	M(chirp mass) [1MΘ, 2.5MΘ]: λ(mass fraction) [0, 1MΘ-1]： η(mass ratio) [0, 0.25] χ(spin parameter) [-0.85, 0.85]	linewidth	Phys. Rev. D 85, 104024 (2012) arXiv:1112.1898 arxiv 1104.3565 http://iopscience.iop.org/article/10.1088/0004-637X/739/2/86 arxiv 1602.03847 Physics Review Letters 116.131102 (2016)
Binary Neutron Star Model	M(chirp mass) [1MΘ, 2.5MΘ]: λ(mass fraction) [0, 1MΘ-1]：	linewidth	Phys. Rev. D 85, 104024 (2012) arXiv:1112.1898
CMB PLI		linewidth
Core Collapse to Black Hole- Complete	a(model detail 1)[5, 150] b(model detail 2)[40, 400] λ(mass fraction)[0, 1MΘ-1] E_v(energy carried away by neutrinos) <q>(luminosity weighted average neutrino anisotropy)	linewidth
Core Collapse to Black Hole- Ringdown	epsilon (efficiency) alpha (fraction of mass converted to black hole) a (spin factor) Minimum Progenitor Mass (in units of solar mass) Maximum Progenitor Mass (in units of solar mass)	linewidth	arXiv:1506.02631 (see model 1) Phys. Rev. D 92, 063005 (2015)
Magnetar Model	B-Field[7e13G, 1e17G]: ε(ellipticity) [1e-6 - 1e-2]: P0(rot period) [1e-3s,5e-3s]: λ(mass fraction) [1e-4MΘ-1, 1e-2MΘ-1]: Iz(moment of inertia) [in g·cm2]:	linewidth	Phys. Rev. D 87, 042002 (2013)
Metallicity Dependent CCBH (slow)	a (spin factor) epsilon (efficiency)	linewidth	arXiv:1506.02631 (see model 2) Phys. Rev. D 92, 063005 (2015)
NS-BH Model	M(chirp mass) [1MΘ, 2.5MΘ]: λ(mass fraction) [0, 1MΘ-1]：	linewidth	Phys. Rev. D 85, 104024 (2012) arXiv:1112.1898
NSBH Upper Limit		linewidth
Neutron Star Turbulence Model	d0m(Crust core differential shear) [1e-4,1e3]: N(NS Fraction) [1e-6,1]: v(kinematic viscosity) [0.1,10]: M_star(NS mass) [1MΘ,2MΘ]: R_star(NS radius) [7km,20km]:	linewidth	Phys. Rev. D 87, 063004 (2013) arXiv:1302.6033v1
Supermassive Binary Black Holes		linewidth	arXiv:1211.5375
White Dwarf Binary		linewidth	D. Hils and P. L. Bender, Ap. J., 360, 75-94 (1990)
bar-mode Model	P0(period) [0.5ms, 10ms]: λ(mass fraction) [0, 1e-2MΘ-1]:	linewidth	doi:10.1088/1674-4527/11/4/001 arXiv:1101.2762v3
r-mode Model	P0(period) [0.5ms, 10ms]: λ(mass fraction) [0, 1e-2MΘ-1]:	linewidth	doi:10.1088/1674-4527/11/4/001 arXiv:1101.2762v3
Cosmological Models
Axion Inflation Model	p(potential form) 1 or 2: ξcmb; (ξ at Φcmb)[1.2 2.7]: Ncmb(Number of e-foldings)[45 65]:	linewidth	Phys. Rev. D 85, 023525 (2012) arXiv:1110.3327v1
Cosmic String Model	P(probability)[1e-3, 1]: ε(size)[1e-13, 1]: Gμ[1e-12,1e-6]:	linewidth	Phys. Rev. Lett. 98, 111101 (2007) arXiv:astro-ph/0610920v2
Inflation Model	r (Tensor-to-Scalar Ratio)	linewidth	Phys. Rev. D 55, R435(R) (1997)
Phase Transition	T(critical temperature) , GeV g(relativistic d.o.f) v(bubble wall velocity)[0,1] Beta/H(energy density parameter)[10, 1000]	linewidth	arXiv:1602.04203
Phase Transition (2018)	Case # (1: non-runaway bubbles 2: runaway bubbles in a plasma 3: runaway bubbles in vacuum): α: β/H: T:	linewidth	Chiara Caprini et al JCAP04(2016)001
Pre-Big-Bang Model	μ(0, 2]: F1[1e8, 1e11]: Fs[1, 1e11]:	linewidth	Phys. Rev. D 73, 063008 (2006) arXiv:astro-ph/0510341v2
Stiff Equation of State	r (Tensor-to-Scalar Ratio) w (Effective Equation of State Parameter) n (Effective Tensor Index)	linewidth	Phys. Rev. D 78, 043531 (2008) arXiv:0708.2279
Experimental Limits
BBN		linewidth	10.1016/j.bbr.2011.03.031 arXiv:gr-qc/9909001v4
CMB+LSS		linewidth	arXiv:astro-ph/0603144v1
COBE		linewidth	arXiv:gr-qc/9604033v3
LIGO S6 1000-1726 Hz		linewidth	arXiv:1406.4556
LIGO S6 600-1000 Hz		linewidth	arXiv:1406.4556
Pulsar Timing 2015		linewidth	arXiv:1508.03024 http://iopscience.iop.org/article/10.3847/0004-637X/821/1/13
Projected sensitivities
Cosmic Explorer		linewidth	Phys. Review D. 91 082001 (2015)
Cosmic Explorer PLI		linewidth
Design A+		linewidth
Design HLV		linewidth
Einstein Telescope		linewidth	http://www.et-gw.eu/etdsdocument
Voyager		linewidth	LIGO Document Control Center Portal
eLisa		linewidth	https://www.elisascience.org/whitepaper/
Old Results
Hanford Detectors (LIGO S5)		linewidth	arXiv:1410.6211 Phys. Rev. D 91, 022003 (2015)
LIGO O1+O2		linewidth
LIGO S3		linewidth	Phys. Rev. Lett. 95, 221101 (2005) arXiv:astro-ph/0507254v1
LIGO S4		linewidth	doi:10.1086/511329 arXiv:astro-ph/0608606v2
LIGO S6 170-600 Hz		linewidth	arXiv:1406.4556
Pulsar Timing (2006)		linewidth	doi:10.1086/508702 arXiv:astro-ph/0609013v1
Pulsar Timing 2013		linewidth	10.1126/science.1238012 arXiv:1310.4569
Up to Date Results
LIGO O1+O2+O3		linewidth
LIGO S5		linewidth	doi:10.1038/nature08278 arXiv:0910.5772v1
LIGO S6 41.5-169.25 Hz		linewidth	arXiv:1406.4556
Check here to remove site information from main plot.
Check here to remove our names from main plot.
[Please note there may be up to 30 second wait for plots]

Welcome to GW Plotter
An Interactive Plotter for Energy Spectrum of Stochastic Gravitational Wave Backgrounds from Various Theoretical Models

PLOT SPECIFICATIONS

Welcome to GW Plotter An Interactive Plotter for Energy Spectrum of Stochastic Gravitational Wave Backgrounds from Various Theoretical Models

PLOT SPECIFICATIONS

Welcome to GW Plotter
An Interactive Plotter for Energy Spectrum of Stochastic Gravitational Wave Backgrounds from Various Theoretical Models