Accueil > Sites heberges > CFHTLS-Deep > Overview

 

Overview

Par Genevieve Soucail - 25/10/2005

 

Observing Strategy

The detection of distant supernovae being the main scientific dirver of the Deep survey, observations are scheduled with specific time constraints : one observation every 2 or 3 nights for 5 months/year over 5 years. 4 fields are selected which cover the RA distribution over the year. At the end of the survey, the total expected integration time will as high as 33h in u* and g’, 66h in r’ and z’ and 132h in i’. Limiting magnitudes should nearly reach 28, an unprecedented level ever attained on ground-based observations and over a 1 degree scale.

In more details, the observing strategy is fixed by constraints in the detection of supernovae : each "block" of observation has been fixed as follows :

  • 1h integration time in i’ is the first priority. One exposure is taken every 2-3 nights
  • 30mn in r’, 15mn in g’ and 30mn in z’ are obtained the same night or the following one.
  • u* observations do not follow these time constraints, but are supposed to be acquired at the same "speed", equivalent to 15mn per "block".
The average rate of "blocks" acquisition, estimated from general statistics of observations in queue mode at CFHT and including weather statistics, is 5.25 "blocks" per dark run. Note that a dark run is considered as long as 18 days of dark and grey time.

Expected performances

For each filter, the expected limiting magnitudes in the AB system (S/N=5 in a 1.16" diam. aperture) and total integration times are estimated throuhg the last evaluations of MegaPrime performances by using the MegaPrime exposure time calculator DIET :

Filter Expected integration time after 1 year Limiting magnitude (AB) Total integration time at the end of the survey Limititing magnitude (AB)
u* 6.5 h 27.3 33h 28.2
g’ 6.5 h 27.9 33h 28.8
r’ 13h 27.7 66h 28.6
i’ 26.5h 27.4 132h 28.3
z’ 13h 26.1 66h 27.0

Fields selection


Alpha (2000) Dec (2000) Comments
D1
02h 26m 00s -04d 30m 00s Embedded in the CFHTLS-W1 field.
- Centered in the Deep area of the VLT-VIRMOS Deep Survey field, in which spectroscopic optical follow-up is taking place at the VLT with VIMOS, up to I_AB=24 at more than 80% completeness.
- Located within the area covered by the XMM-LSS survey : 20 ksec XMM pointings per field.
- Also a GALEX and SIRTF target
D2
10h 00m 29s 02d 12m 21s Field selected within the area of the Cosmos/ACS project. HST data will be publicly available very rapidly.
- Several multi-wavelength follow-ups on-going or planned (XMM, GALEX, SIRTF, ESO/VIMOS ...). Quick release of the data.
- low extinction field
D3
14h 19m 28s +52d 40m 41s Embedded in the CFHTLS-W3 field.
- Located within the ’’Groth Strip’’ area, with low extinction.
- Redshifts available from the Deep II collaboration (I_AB<23.5), obtained with the Keck telescope.
- Also a GALEX target
D4
22h 15m 31s -17d 44m 00s Field selected for its lowest extinction field around RA=22h.
- Centered around the quasar LBQS2212-17 in the anti-Leonids area. A deep XMM-Newton exposure (250ksec) publicly available. Source positions and catalogues developped by the XMM SSC are expected to be released soon.

 

 

[Page Précédente] [Dans la même rubrique] [Sommaire]

 

 

Site du CNRS Logo OMP
Logo UPS
Logo INSU-CNRS

Annuaire

Rechercher

Sur ce site



Bibliotheque

Laboratoire Astrophysique de Toulouse - Tarbes (UMR5572)

CNRS (Midi-Pyrénées)

Univ. Paul Sabatier

Liens utiles

Accueil Imprimer Contact mail Plan du site Crédits