This paper investigates the observational properties of thin-shell gravastars in two astrophysical frameworks: optically-thin accretion disks and hot-spots. The authors analyze the geodesic structure and effective potential of the gravastar model, which is described by two free parameters: the radius \( R \) and the constant \( \alpha \). They use numerical ray-tracing codes to produce observables, such as intensity profiles and images, for different configurations. For accretion disks, the authors consider two models: the ISCO model and the Center model. The ISCO model assumes that the accretion disk truncates at the innermost stable circular orbit (ISCO), while the Center model assumes central matter accumulation. The results show that for dilute configurations, the gravastar radius is not a significant parameter, but for more compact configurations, additional peaks in the intensity profiles appear due to light rings and secondary contributions. The presence of a central shadow-like feature is observed for configurations with \( \alpha = \alpha_{\text{min}} \), where the entire mass of the gravastar is distributed at the thin-shell. For inclined observations, the authors find that for \( \alpha \) close to \( \alpha_{\text{min}} \), the gravitational redshift effects induce significant changes in the observed images, including the appearance of a shadow-like feature. For hot spots orbiting the central gravastar, the authors analyze the time-integrated fluxes, temporal fluxes, and temporal centroids. They observe qualitative differences in the integrated fluxes compared to black-hole scenarios, particularly in the ultra-compact regime. The effects of the orbital radius and the parameter \( \alpha \) are also studied, showing that they have minor impacts on the astrometric observables. In conclusion, the study highlights that smooth gravastar models are inadequate for reproducing astrophysical observations of shadows, and that a thin-shell with a significant portion of the total mass at the surface is necessary. The observational properties of gravastars differ from those of other exotic compact objects, such as fluid stars and bosonic stars, due to the repulsive de-Sitter core in gravastar spacetimes.This paper investigates the observational properties of thin-shell gravastars in two astrophysical frameworks: optically-thin accretion disks and hot-spots. The authors analyze the geodesic structure and effective potential of the gravastar model, which is described by two free parameters: the radius \( R \) and the constant \( \alpha \). They use numerical ray-tracing codes to produce observables, such as intensity profiles and images, for different configurations. For accretion disks, the authors consider two models: the ISCO model and the Center model. The ISCO model assumes that the accretion disk truncates at the innermost stable circular orbit (ISCO), while the Center model assumes central matter accumulation. The results show that for dilute configurations, the gravastar radius is not a significant parameter, but for more compact configurations, additional peaks in the intensity profiles appear due to light rings and secondary contributions. The presence of a central shadow-like feature is observed for configurations with \( \alpha = \alpha_{\text{min}} \), where the entire mass of the gravastar is distributed at the thin-shell. For inclined observations, the authors find that for \( \alpha \) close to \( \alpha_{\text{min}} \), the gravitational redshift effects induce significant changes in the observed images, including the appearance of a shadow-like feature. For hot spots orbiting the central gravastar, the authors analyze the time-integrated fluxes, temporal fluxes, and temporal centroids. They observe qualitative differences in the integrated fluxes compared to black-hole scenarios, particularly in the ultra-compact regime. The effects of the orbital radius and the parameter \( \alpha \) are also studied, showing that they have minor impacts on the astrometric observables. In conclusion, the study highlights that smooth gravastar models are inadequate for reproducing astrophysical observations of shadows, and that a thin-shell with a significant portion of the total mass at the surface is necessary. The observational properties of gravastars differ from those of other exotic compact objects, such as fluid stars and bosonic stars, due to the repulsive de-Sitter core in gravastar spacetimes.