1 / 12

PROSPETTIVE SCIENTIFICHE PER LA

UKIRT Infrared Deep Sky Survey :. PROSPETTIVE SCIENTIFICHE PER LA. camera LBC@LBT. The survey is performed with WFCAM. The field of view is 0.77 sq. degs. Commissioning will start by the end of 2003. The survey will commence in early 2004. UKIDSS consists of 5 surveys :.

katina
Download Presentation

PROSPETTIVE SCIENTIFICHE PER LA

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. UKIRT Infrared Deep Sky Survey : PROSPETTIVE SCIENTIFICHE PER LA camera LBC@LBT

  2. The survey is performed with WFCAM The field of view is 0.77 sq. degs Commissioning will start by the end of 2003 The survey will commence in early 2004

  3. UKIDSS consists of 5 surveys: Large Area Survey Galactic Plane Survey Galactic Clusters Survey Deep Extra-galactic Survey Ultra Deep Survey

  4. L A S Y = 20.5, J = 20.0, H = 18.8, K = 18.4 4000 sq. degs Goals: to find out the nearest and faintest cool objects; to break the z = 7 quasar barrier

  5. G P S J=20,H=19.1,K=19.0 1800 sq. degs Goal:build up a 3-D atlas of the Milky Way

  6. G C S J = 19.7 H = 18.8 K = 18.7 1600 sq. degs Goal: the IMF in the sub-stellar regime

  7. D X S J=22.5, H=22.0, K=21.0 35 sq. degs: XMM-LSS, Lockman Hole, Elais-N1, Virmos-4 Goal: abundance of galaxy clusters at 1.0 < z < 1.5

  8. U D S J=25.0,H=24.0,K=23.0 0.77 sq. degrees Goal: understanding massive galaxies formation

  9. UKIDSS vs LBC : two suggestions • Mass Function in the sub-stellar regime • Lyman drop-out at z ~ 3

  10. 1) The IMF in the sub-stellar regime

  11. Take advantage of the efficiency of LBC in I and Z…. (I-J) is the best temperature indicator…. Above +25 deg, no optical or near infrared surveys can be performed by ESO

  12. 2) The formation of massive galaxies Optical coverage of UDS to provide a very powerful baseline for photometric redshifts determination UV continuum measurement to constrain SEDs of z ~ 3 sources U is vital to identify unobscured galaxies at z ~ 3 with th Lyman drop out technique

More Related