Final SINFONI data cube of ESO program 283.A-5058(A), PI Lehnert
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Target: UDFy-38135539
wavelength of the detected emission line: 11615.6 AA
total on-source exposure time: 53400 s
Reference: Lehnert et al. (2010), Nature, in press

The cube shows the inner regions of the combined data cube
corresponding to the region of the sky which was covered by all
individual observations. It was constructed by averaging 89 individual
frames with individual exposure times of 600s. To ease comparison with
Bouwens et al. (2010), we shifted the cube to the same reference frame,
taking into account imperfections of the relative offsets between
acquisition star and target (see the supplementary material for
details). The position targeted by Bouwens et al. corresponds to the
spatial pixel x/y = 25/25, the source is centered on pixel x/y =
27/23.

We masked slitlets (pixel rows) which were affected by strong
vignetting in the raw frames. SINFONI's image slicer projects pixel
rows, that are relatively near the center of the field of view on the
sky and in the data cube onto the periphery of the detector in the raw
frames. We also masked a set of 4 pixels that were affected by strong
non-Gaussian noise (a stronly deviant "bad" pixel).

Noise near the left and right edges of this cube is enhanced due to
imperfections in the wavelength calibration near the edges of slitlets
in the individual cubes, and accordingly, bad subtraction of the night
sky. The region around the galaxy is not affected by this effect. 

We give 3 x 3 versions of the same cube: 

yUDF38135539_cube_smooth111.fits (at full spatial resolution)
yUDF38135539_cube_smooth331.fits (smoothed with a 3pix x 3pix Gaussian spatially)
yUDF38135539_cube_smooth551.fits (smoothed with a 5pix x 5pix Gaussian spatially)

These are the full cubes including regions with strong night sky lines. 

yUDF38135539_cube_smooth111_nsk.fits (at full spatial resolution)
yUDF38135539_cube_smooth331_nsk.fits (smoothed with a 3pix x 3pix Gaussian spatially)
yUDF38135539_cube_smooth551_nsk.fits (smoothed with a 5pix x 5pix Gaussian spatially)

These are the cubes where we clipped parts of the spectrum with noise
greater by a factor 2 than at the wavelength of the line.


yUDF38135539_cube_smooth111_nsk_1.fits (at full spatial resolution)
yUDF38135539_cube_smooth331_nsk_1.fits (smoothed with a 3pix x 3pix Gaussian spatially)
yUDF38135539_cube_smooth551_nsk_1.fits (smoothed with a 5pix x 5pix Gaussian spatially)

These are the cubes where we clipped parts of the spectrum with noise
greater than at the wavelength of the line.

We did not smooth the cube along the spectral axis. 

To view the cubes ...
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... we recommend to start with the cube smoothed by 5x5 pixels. We
recommend to use QFitsView, http://www.mpe.mpg.de/~ott/QFitsView,
which has been written by Thomas Ott at MPE in Garching. Any other
3D viewer should work as well, but has not been tested.

We recommend you mark the spectral region around 11615.1 AA to
visualize the source (move the cursor over the region of interest in
the spectrum, while pushing Ctrl+C on your keyboard). The screenshots
give examples for the source in all three data cubes, along with the
settings with which these line images and spectra were produced.

To compare if some other feature appears like noise, please compare
data cubes at all 3 spatial resolutions provided, and ensure that the
feature does not fall in a region of enhanced sky noise, masked in
some of the cubes.