#TITLE_ALTERNATIVE#

• Main Author: TIARA PUTRA (NIM : 103 09 004); Pembimbing : Dr. Rer. Nat. M. Ikbal Arifyanto, ARI
• Format: Final Project
• Language: Indonesia
• Online Access: https://digilib.itb.ac.id/gdl/view/19921
• Institution: Institut Teknologi Bandung

Stellar stream is a group of stars moving with the same velocity and direction (O. <br /> <br /> <br /> J. Eggen, 1996). Helmi & White (1999) states that stellar stream of Galactic halo <br /> <br /> <br /> are the remnants of accreted satellites. It supports hierarchical merging scenario <br /> <br /> <br /> where galaxies are formed of an attracted material surrounding proto system and <br /> <br /> <br /> join up into a larger structure. There are several methods for finding streams of <br /> <br /> <br /> stars in the halo, as an example of a Helmi & White (1999) – Helmi & de Zeeuw <br /> <br /> <br /> (2000) method, Klement et al (2009) method, or Arifyanto & Fuchs (2005) <br /> <br /> <br /> method. The search strategy stellar stream is by looking over densities in phase <br /> <br /> <br /> space. <br /> <br /> <br /> In this final project will be compared the search methods of stream from Helmi & <br /> <br /> <br /> White (1999) – Helmi & de Zeeuw (2000) method and Klement et al (2009). They <br /> <br /> <br /> used a different parameter for Integral of Motion. For Helmi & White (1999) – <br /> <br /> <br /> Helmi & de Zeeuw (2000) uses the energy E, the angular momentum L and the zcomponent <br /> <br /> <br /> Lz for Integral of Motion. As for Klement et al (2009) using the <br /> <br /> <br /> parameters of velocity dispersion and angular orbit (Vaz, V&#916;E, &#965;). By studying <br /> <br /> <br /> about stellar stream, we can learn more about the origins of the formation of <br /> <br /> <br /> galaxies.