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Thermal dominated X-ray spectra of neutron stars in quiescent transient X-raybinaries and neutron stars that undergo thermonuclear bursts are sensitive tomass and radius. The mass-radius relation of neutron stars depends on theequation of state that governs their interior. Constraining this relationaccurately is thus of fundamental importance to understand the nature of densematter. In this context we introduce a pipeline to calculate realistic modelspectra of rotating neutron stars with hydrogen and helium atmospheres. Anarbitrarily fast rotating neutron star with a given equation of state generatesthe spacetime in which the atmosphere emits radiation. We use theLorene/nrotstar code to compute the spacetime numerically and the ATM24 code tosolve the radiative transfer equations self-consistently. Emerging specificintensity spectra are then ray-traced through the neutron star's spacetime fromthe atmosphere to a distant observer with the Gyoto code. Here, we present andtest our fully relativistic numerical pipeline. To discuss and illustrate theimportance of realistic atmosphere models we compare our model spectra tosimpler models like the commonly used isotropic color-corrected blackbodyemission. We highlight the importance of considering realistic model-atmospherespectra together with relativistic ray tracing to obtain accurate predictions.We also insist on the crucial impact of the star's rotation on the observables.Finally, we close a controversy that has been appearing in the literature inthe recent years regarding the validity of the ATM24 code.

Accurate ray tracing of realistic neutron star atmospheres for constraining their parameters