This paper analyzes the observational properties of thin-shell gravastars in two astrophysical contexts: surrounded by optically-thin accretion disks and orbited by hot-spots. The gravastar model is defined by two parameters: the radius R and the ratio of mass allocated at the thin-shell, with the interior replaced by a de Sitter condensate. The study uses numerical ray-tracing to simulate the emission profiles and images of these objects. For accretion disks, the results show that smooth gravastars cannot reproduce shadow observations due to the absence of a strong gravitational redshift effect, making them unsuitable for supermassive objects. However, gravastars with a large portion of their mass at the surface can produce such effects and are viable black-hole mimickers. In the case of hot-spots, the astrometric properties of ultra-compact gravastars resemble those of other compact objects like fluid and bosonic stars. However, for low-compactivity configurations, the time-integrated fluxes show additional contributions in the form of a high-intensity plunge-through image. The analysis of the effective potential shows that the number of light rings (LRs) depends on the gravastar radius, with R < 3M leading to two extremum points. The parameter α, which controls the mass distribution, has a subdominant effect on the geodesic structure. The observational properties of gravastars differ from black-hole spacetimes, with distinct features in intensity profiles and shadow images, which could be distinguished by future interferometric experiments. For accretion disk models, the ISCO model assumes the disk does not extend below the innermost stable circular orbit, while the Center model assumes matter accumulates at the center. Observed intensity profiles show that for dilute configurations (R > 4M), the gravastar radius is not a dominant parameter, but for more compact configurations, additional peaks appear. A decrease in α increases the contribution of secondary peaks and moves them closer to the center. Inclined observations show that for values of α far from the minimum, the observational properties remain similar, but near α_min, significant changes occur, including more secondary images and a shadow-like feature. For hot-spot orbits, the time-integrated fluxes show distinct features for ultra-compact configurations, with additional secondary tracks and a plunge-through contribution. The magnitude and centroid of the observed images depend on the orbital radius and α, with changes in α having a subdominant effect. The results highlight the unique observational signatures of gravastars compared to black-hole spacetimes, which could be tested by future gravitational wave and interferometric experiments.This paper analyzes the observational properties of thin-shell gravastars in two astrophysical contexts: surrounded by optically-thin accretion disks and orbited by hot-spots. The gravastar model is defined by two parameters: the radius R and the ratio of mass allocated at the thin-shell, with the interior replaced by a de Sitter condensate. The study uses numerical ray-tracing to simulate the emission profiles and images of these objects. For accretion disks, the results show that smooth gravastars cannot reproduce shadow observations due to the absence of a strong gravitational redshift effect, making them unsuitable for supermassive objects. However, gravastars with a large portion of their mass at the surface can produce such effects and are viable black-hole mimickers. In the case of hot-spots, the astrometric properties of ultra-compact gravastars resemble those of other compact objects like fluid and bosonic stars. However, for low-compactivity configurations, the time-integrated fluxes show additional contributions in the form of a high-intensity plunge-through image. The analysis of the effective potential shows that the number of light rings (LRs) depends on the gravastar radius, with R < 3M leading to two extremum points. The parameter α, which controls the mass distribution, has a subdominant effect on the geodesic structure. The observational properties of gravastars differ from black-hole spacetimes, with distinct features in intensity profiles and shadow images, which could be distinguished by future interferometric experiments. For accretion disk models, the ISCO model assumes the disk does not extend below the innermost stable circular orbit, while the Center model assumes matter accumulates at the center. Observed intensity profiles show that for dilute configurations (R > 4M), the gravastar radius is not a dominant parameter, but for more compact configurations, additional peaks appear. A decrease in α increases the contribution of secondary peaks and moves them closer to the center. Inclined observations show that for values of α far from the minimum, the observational properties remain similar, but near α_min, significant changes occur, including more secondary images and a shadow-like feature. For hot-spot orbits, the time-integrated fluxes show distinct features for ultra-compact configurations, with additional secondary tracks and a plunge-through contribution. The magnitude and centroid of the observed images depend on the orbital radius and α, with changes in α having a subdominant effect. The results highlight the unique observational signatures of gravastars compared to black-hole spacetimes, which could be tested by future gravitational wave and interferometric experiments.