here - Institute for Astronomy Umleitung

Title: Science preparation and key personnel
Reference: MUSE-MEM-SCI-053
Issue: 1.0
Date: 02/02/04
Page: 10/25
Fig 6. (left) Observational estimates of the cumulative luminosity function of candidate Ly α emitters
(LAE) at z ~ 5.8. The three continuous functions are from (l-r) the LALA survey [19], the Subara
Deep Survey [1] and the CADIS survey [18]. LALA only picks up LAE of very high equivalent width
but has a high confirmation rate so far [19], so it is likely a lower limit. CADIS has a lower
confirmation rate and may be regarded as an upper limit. The three points separated by a dotted
line is the sample of 15 objects from Hu et al (2003). The right-angled limits represents the lack of
detection by Martin & Sawicki using a similar but less sensitive technique to that used by us. The
hatched area is a reasonable representation of these observations with reality likely lying in the
middle. (right) As at left, except at z = 6.5. The hatched region is simply translated from the z = 5.8
diagram assuming no evolution. The upper and far-left axes show observational quantities. Only
three galaxies are known at this redshift, those from Hu et al (H02) and Kodaira et al (K03) The
former is shown both as observed and also demagnified by the A370 lens. The variable sensitivity of
the proposed survey arising from sky lines and spatial effects due to the VPH grating gives the
curved sensitivity-area relation shown as the heavy line. We expect to detect 20 LAE down to a
sensitivity limit substantially below that explored by the previous narrow-band surveys. Adapting
the number density from Hu et al would boost this by an order of magnitude.
4.2.3. Future plans
We plan to continue and extend these
observations in the context of MUSE science
preparation. For example, a third SAURON
deep field has recently been obtained on another
region of the SSA cluster. The 20 hours of
integration on this field would allow us to get
deeper and to improve our experience in datareduction
of IFUs in this context. Along the
same line, we plan to use the PMAS IFU (Roth
et al, 2000) in operation at Calar Alto 3.5m
telescope. The recently commissioned new
PPAK fiber bundle gives a large field of view
(70x70 arcsec²) at the cost of low spatial
sampling (2.7 arcsec). An example of PMAS
capabilities is shown in Figure 7.
Fig.7. Ly α contours of the DLA galaxy on the lineof-sight
to Q2233+131 as observed with PMAS at
the Calar Alto 3.5m Telescope, superimposed on
an 8” × 8” WFPC2 image. The total Ly α flux
measured from the 2 hours PMAS exposure is
2.4×10 -16 erg/cm 2 /sec with a 3σ detection limit of
1×10 -17 erg/cm 2 /sec. The inferred velocity field is
inconsistent with rotation of the DLA galaxy and
interpreted as an outflow. From Christensen et
al.2004, A&A in press.