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%%%%%%%%%%%%  Probing the mass and star formation of high-redshift lensed galaxies %%%%%%%%%%%%
%%%%%%%%%%%%                  with SPIFFI 3D spectroscopy                          %%%%%%%%%%%%					   
Team responsible: Marie Lemoine-Busserolle (Institute of stronomy, Cambridge, UK)

Team members: M. Kissler-Patig (ESO, Garching), T. Contini, R. Pello, J-F Leborgne, 
J-P Kneib (Laboratoire D'Astrophysique, Toulouse), I. Parry (Institute of Astronomy,
 Cambridge)

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ABSTRACT :
	 We propose to use SPIFFI to make a spatially-resolved study of about 2 images
 of spectroscopicaly confirmed high redshift galaxies behind the cores of galaxy lensing
 clusters .The main goal of this programme is to obtain 2D velocity maps from Halpha and
 [OIII] emission line for 2 star-forming lensed galaxies in the two clusters lenses AC114
 (RA=22:58:47.7, DEC=-34:48:14) and A370 (RA=02:37:00, DEC=-01:48:00).

The two target are the2 lensed Arc A370-A5 et AC114-V4 (see fig. finding chart).

 -- For A5-370 (z=1.341, RA=02:39:52.860, DEC=-01:35:40.320) the Halpha emission falls in 
the SPIFFI H band and the Hbeta and [OIII] emission in SPIFFI J band. 

-- In the case of AC114-V4 (z = 2.274, RA=22:58: 44.528, DEC=-34:48:06.730) the Halpha
emission is redshifted in SPIFFI K band and the H? and [OIII] emission in SPIFFI H band. We
estimate our exposure time (on source) based on our ISAAC longslit observations of the
arcs. 

The SPIFFI sensitivity suggest that we will detect with a S/N of ~5 in a 0.25 arcsec
diameter lenslet, the Halpha emission in 2H00 for A370-A5 and in 4H00 for AC 114-V4. To
reach the same S/N for the [OIII] emission we need 3H30 for A370-A5 and 4H00 for AC114-V4.

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OBSERVATIONS :
`````````````
2 lensed Arc A370-A5 et AC114-V4 (see fig. finding chart).

Strategy : 

on V4: O-S-O with FoV=8x8 arcsec, DIT 900s and NDIT 1. We request a seeing < 0.8" if possible
on A5: noding 4 arcsec N-S in the 8x8" FoV DIT 900s and NDIT 1. We request a seeing <0.8" 
if possible

Calibration: For telluric standars please select stars that are hotter than B4. 

Finding charts: A370-A5.jpg and AC114-V4.jpg

OBs: 178711 to 178722  (only Halpha, i.e. K band and H band observations fo V4 and A5
respectively)

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The acquisitions are done on a bright star followed by a blind offset.
The object is observed (for 3 or 4 times 900s) and we finally take
an exposure of another bright star to verify the centering/offsets.

The stars/offsets are given below (cf also the finding charts)

convention: positif in North and East direction

1/ A370-A5 (A370-A5.jpg)
```````````````
--- A5 coords (J2000):
ra : 02 39 52.860 ;   dec: -01 35 40.320 

--- star #1:
ra :  02 39 49.395   dec:  -01 35 12.30

Direction from star #1 to  A5 : WEST-EST 
Acquisition on star #1 and offset to A5:
RA_offset : 51.96
DEC_offset: -28.02

--- star #2:
ra :  02 39 59.025   dec: -01 34 00.91
Acquisition on A5 and offset to star #2
Direction from star #2 to A5 : NORTH-WEST
RA_offset :- 92.44 
DEC_offset: +99.41


2/ AC114-V4 (AC114-V4.jpg)
`````````````````
--- V4 coords (J2000):
ra : 22 58 44.528 ;   dec: -34 48 06.730

--- star #2:
ra : 22 58 41.719   dec: -34 48 30.71

Direction from star #2 to V4 : NORTH-EST 
Acquisition on star #2 and offset to V4:
RA_offset : + 34.60 
DEC_offset: +23.98 

---star #5:
ra : 22 58 41.266  dec: -34 47 26.000

Direction from star #5 to V4 : NORTH-WEST
Acquisition on V4 and offset to A5:
RA_offset : - 40.17 
DEC_offset: + 40.73