This page provides an Event Browser, that can be used to display any event in the data release. Events can be selected by providing their id or by selecting the value of some of their main properties. Some example events can also be selected from the menu below.
Once an event is selected its components can be browsed in different tabs.
Can't display event id , no event found with this id.
Different views of the event are available by selecting the corresponding tabs.
In this tab the full extention of the ground array is displayed, with each dot being a surface detector (in light gray detectors not yet installed at the moment of the event). The Malargüe city where the Observatory headquarters are located is indicated (MGUE) and the other 4 squares are the 4 Fluorescence buildings (LL: Los Leones, CO: Coihueco, LA: Loma Amarilla, LM: Los Morados). They appear in color if they were triggered by the event. The main roads of the area are also displayed. Empty dots are stations determined to be random coincidences. Stations part of the event are displayed with a circle of area corresponding to the logarithm of their integrated signal and color corresponding to the station timing. The cosmic ray incoming direction and core impact are displayed with an arrow.
In this tab the FADC traces of the 3 PMTs of all triggered stations are displayed. Inactive PMTs are displayed with a signal of 0. Stations determined to be random coincidences and not being part of the event are dimmed and listed at the end.
This tab shows the SD LDF reconstruction: the total signal in the different stations versus the distance of the station to the event core. The signal at 1000m from the core is used as an energy estimate. More details on the SD reconstruction can be found here.
The FD camera view of the event is displayed below. The color code corresponds to the time at which the light reaches each pixel. Dark pixels are random coincidences and not used in the reconstruction.
This tab shows the FD reconstructed profile, the energy deposited in the atmosphere as a function of the slant depth crossed by the cosmic ray. The integral of this curve gives a direct measurement of the calorimetric energy, while the depth at which the maximum of the energy deposition occurs is used to infer the primary particle properties. See here for more details on the FD reconstruction.
This tab shows a 3D animation of the cosmic ray that generated the selected event. Different visualization options are available in the menu on the left. The menu on the right contains many details about the shower, both for SD and Hybrid events.