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This page developed under the auspices of the U.S. LISA Mission Science Office at JPL.


Enter Your Observatory Parameters

In the generator fields listed below, default values for the Observatory Parameters will generate a standard LISA sensitivity curve (equal arms, all-sky + polarization average, SNR = 1) for the root spectral density of gravitational wave strain vs. gravitational wave frequency.

Sensitivity curve SNR -- LISA = 1.0

Armlength -- LISA = 5.0E9 meters

Telescope Diameter -- LISA = 0.3 meters

Laser wavelength -- LISA = 1064 nanometers

Laser Power [Watts] -- LISA = 1.0 Watt

Optical train efficiency -- LISA = 0.3

Root spectral density accleration noise [m/(s^2 root Hz)] -- LISA = 3.0E-15

Root spectral density position noise budget (1-way) [m/(root Hz)] -- LISA = 2.0E-11

sets value of sensitivity floor -- default = Position Noise Budget

Type of curve to return -- default = Root Spectral Density

Astrophysical noise -- default = No White Dwarf Noise

spacer Hils-Bender Estimate
spacer Analytic fit to Hils-Bender

If You Use This Page

We would like to provide updates and information to the community of people who use this generator. If you would like to join our automated listserv to receive periodic news about this service, please visit the "lisacurve" listserv webpage and subscribe: http://www.srl.caltech.edu/mailman/listinfo/lisacurve

If you would rather not join the listserv, we would still like to know that you are using the generator, and welcome suggestions you have. Please drop an email to: shane@srl.caltech.edu

How It Works

A white paper describing the standard LISA sensitivity curve adopted by the project is available: LISA Sensitivity White Paper.

The method used to generate a sensitivity curve here follows Larson, Hiscock and Hellings (PRD, 62, 062001 [2000]). This sensitivity curve is equivalent to the equal arm limit sensitivity of the X(t) variable of Armstrong, Estabrook and Tinto (ApJ, 527, 814 [1999]).

This generator, in its current form, works only in the equal arm limit, and cannot compute any additional time-delay interferometry variables. For details regarding sensitivities and computational issues related to these variables, see (e.g.) Armstrong, Estabrook and Tinto (ApJ, 527, 814 [1999]).

White Dwarf Background (Astrophysical Noise)

The current version of the curve generator has been extended to include simple estimates of the confusion-limited white dwarf background from the galaxy. The estimates are due to Hils and Bender (CQG, 14, 1439 [1997]), and an analytic fit to the Hils-Bender spectrum by Hiscock, Larson, Routzahn and Kulick ( ApJ, 540, L5 [2000]).

As they can be adapted, other schemes for estimating the white dwarf background will be provided as options in the curve generator. If you have suggestions for realizations of the background to use, please contact me (shane@srl.caltech.edu).

If you have Problems with the Generator

This page is currently a beta test! Please email suggestions and bug reports about this page to shane@srl.caltech.edu. Be sure it include a complete list of parameters for the observatory you were designing -- it will greatly aid me in debugging your problem on this end.

Clear skies!
-- Shane

  Footer Map Page Maintained by: Shane L. Larson
Email: shane@srl.caltech.edu
Last Updated: 29 April 2003