|Plot:||Characteristic Strain||Power Spectral Density||Energy Spectrum|
|Sources:||Very low frequency:|
10 March 2016
Custom pulsar timing array. The above plots include the functionality for the user to add their own customised PTA. This is to enable the user to explore the effects of changing the number of pulsars, length and frequency of pulsar observations, and the timing precission of the observations on the sensitivity of the PTA.
To add a custom PTA click on the "New PTA" button on the left hand side of the screen, and a custom PTA detector will appear in the table next to the SKA. Click on the arrow next to the custom PTA label to see a drop down list of options. For details on how the sensitivity is calculated see this paper (or arXiv)
3 March 2016
The ET sensitivity was updated to a more recent design study. The curve identified as ET-D is now plotted, for details see the ET sensitivity page.
11 February 2016
The shaded box labelled GW150914 shows the gravitational-wave strain for a GW150914-like signal; specifically, we plot the strain for an optimally orientated binary black hole system with non-spinning components of 35 and 30 solar masses at a redshift of z = 0.1.
For details of the parameters inferred for GW150914's source, see the parameter estimation paper.
21 January 2016
The sources box for Type IA supernovae was added. These sources are distinct from the higher frequency core collapse supernovae which were already plotted. The amplitude of box plotted here corresponds to an optimally orientated Type IA supernovae at 30 kpc (i.e. in the Milky Way). The event rate for Type IA supernovae in this volume is low; a rate of the order 1 in 100 years.
17 December 2015
The aLIGO sensitivity curve was updated. We now plot two sensitivity curves, one for the sensitivity during the O1 run (commenced September 2015) and one for design sensitivity. Therefore the curves plotted here no longer matches that in the companion paper.
We thank colleagues from the LIGO Scientific Collaboration including Chris Messenger and Rana Adhikari for useful comments and pointers to updated information.
We would also like to thank Ivo Seitenzahl for a useful discussion concerning type IA supernovae as gravitational wave sources.