1 / 6

Enhanced Analysis of Dark Energy Survey: Challenges and Improvements for Resolved Stellar Populations

This report discusses the ongoing challenges and improvements needed in the Dark Energy Survey (DES) regarding resolved stellar populations. Key issues include significant proper motions in large right ascension areas, and recovery of magnitude and color distributions. It highlights the potential of adding substructures such as the Galactic Center and LMC spheroid to improve the model. Science priorities are defined considering limited manpower and computational constraints. Finally, contributions from team members in identifying and modeling arcs with N-body simulations are emphasized.

pier
Télécharger la présentation

Enhanced Analysis of Dark Energy Survey: Challenges and Improvements for Resolved Stellar Populations

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Basílio Santiago Jan 2010 Dark Energy Survey in 2010

  2. Resolved Stellar Populations • DC5 pending issues: large RA proper motions; recovering mag and col distributions, comparing to input model. Portal access. • DC6: what can be improved? Perhaps add some substructures: GC + tail, LMC spheroid. • Defining science priorities: limited man-power, computational issues. • 0.1 FTE

  3. SP models Extra remarks: GC tails and the Galaxy cover large solid angles, especially the latter.

  4. Outer LMC: a lot to improve • 1 sq deg • uniform SFH assumed • No depth effects yet 0.1 FTE

  5. Pal 5 and field (SDSS) 0.05 FTE

  6. Strong lensing • Provide a local environment for this new area (locally, I mean...): papers, tutorials, documentation, coding. Supervision: • Cristina: automatically identifying and measuring arcs on space and ground-based images: SOGRAS, DC4, DC5. • Angelo: realistic modelling of arcs using DM halos from N-body simulations. • 0.1 FTE

More Related