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Context. Several dynamically cold streams have been associated with certainglobular clusters (GCs) based on orbital energies and angular momenta. Some ofthese streams are surprisingly far apart from their progenitors and one suchpair is Triangulum and NGC 5824. Triangulum can be considered as a piece of NGC5824 leading tail since the cluster's future orbit matches with the stream'strack well. The existence of the leading tail for NGC 5824 is the motivationbehind the search for its trailing tail. Aims. Our goal is to confirm theconnection between Triangulum and NGC 5824 and seek the trailing tail of thecluster. Methods. The selection of member stars of Triangulum is made throughvarious cuts in metallicity, proper motions (PMs), radial velocity andcolor-magnitude diagram (CMD). The selected members are compared in phase spaceto a mock stream which models the disruption of NGC 5824. We then try to detectthe trailing tail of the cluster based on a modified matched-filter technique.Stars are assigned weights using their color differences from the cluster'slocus in CMD. These weights are further scaled based on stars' departures fromexpected PMs of the model stream. Results. A total of 26 member stars forTriangulum are obtained and 16 of them are newly identified. These members areconsistent with the mock stream in the phase space and their metalicity andposition on the CMD are in good agreements with NGC 5824. By applying thematched-filter, a tenuous trailing tail of the cluster is detected, spanning$\sim$ 50$^\circ$ long on sky. The signature matches with the mock stream'strajectory well. Conclusions. Our results support that Triangulum stream actsas a part of the leading tail for NGC 5824. On the trailing side, we havedetected a 50$^\circ$ tail extended from the cluster. The existence of bothleading and trailing tails for the GC NGC 5824 is verified.

Existence of Tidal Tails for the Globular Cluster NGC 5824