Orateur
Description
Accurately modelling pulsar noise is one of the main challenges for current radio PTA experiments. For many pulsars, the data are not informative enough to efficiently solve the covariance between chromatic and achromatic processes. In gamma-ray PTA (GPTA) experiments instead, the sensitivity to stochastic processes is limited by the low photon flux of gamma-ray pulsar observations; thus, the radio folding procedures becomes inapplicable for most pulsars. However, because of the high frequency of the gamma rays, there is no interaction with the interstellar medium. This results in much simpler noise models, which include only the pulsar’s spin noise and Poisson statistics noise.
In this talk, I will discuss the new data analysis pipeline that the GPTA group has been developing for GW searches from gamma-ray data and present a method to consistently combine radio and gamma-ray pulsar observations. Being able to break the degeneracy between chromatic and achromatic signals would not only provide valuable information on the interstellar medium distribution, but would also improve our sensitivity to a GWB signal.