Terms and Conditions for the usage of HTTP data:
When using data from HTTP, please cite the following papers:    Sabbi et al. 2013,    Sabbi et al. 2016,    and include the following acknowledgment:
“This work is based on observations taken by the Hubble Tarantula Treasury Project with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555."



HTTP was awarded 60 orbits of HST time in Cycle 20 to survey the entire Tarantula Nebula, using both the UVIS and the IR channels of the Wide Field Camera 3 (WFC3), and, in parallel, the Wide Filed Channel (WFC) of the Advanced Camera for Surveys (ACS). Each of the UVIS orbits consists of one short (14 s) and two long (697 s each) exposures in the filter F336W followed by two long exposures (697 and 467 s respectively) in the F275W filter. Each couple of UVIS long exposures were obtained using a two point dither pattern to enable the rejection of cosmic-rays (CRs) and cover the chip gap. While WFC3 was acquiring the UVIS images, ACS was used to collect one short (13  s), and four long (3x640+1x337 s) exposures in the filter F555W. For the deep F555W exposures we used a four point dither pattern, improving the sampling of the PSF. 

The IR orbits consist of two long (2x799 s) exposures in the F160W filter followed by two long (799 and 499 s respectively) exposures in the F110W filter. At the same time, ACS was used to obtain four long (3x640+1x399s) exposures in the F658N filter. Archival observations in the ACS+WFC3 F775W filters were used to complete the wavelengths coverage. 

WFC3/UVIS and ACS/WFC images were corrected for the degrading charge transfer efficiency using the pixel-based solution described in Anderson & Bedin (2010). 

Photometric Catalog

The HTTP Photometric Catalog was obtained from the analysis of all the images used in the HTTP program (HST 12939, PI Elena Sabbi + HST 12499, PI Danny Lennon), as defined by Sabbi et al. 2016. The measurements were made using the KS2 (Anderson et al. in prep) PSF astro-photometric package. The photometry was carried out directly on the CTE corrected FLT images. Zero points were adopted from the STScI Web site. 

The HTTP photometric catalog can be dowloaded here. When using the HTTP catalog please refer to Sabbi et al. 2016.

Catalog Download (zip)


Interactive Display

These mosaics of 30 Doradus were constructed from all the WFC3/IR observations on this fields from the program 12939 (PI: E. Sabbi), consisting of 72 exposures in F110W and another 72 exposures in F160W. You can download the mosaics in FITS format by clicking on the previews above, or by visiting the Interactive Display page using the button. Note: Currently, only the last two filters in the above row of mosaics are available for download, the others will be available soon.
The exposures were all aligned astrometrically to the master reference catalog (Sabbi et al. 2016) using algorithms that make use of the latest drizzlepac/tweakreg scripts, and were combined using astrodrizzle onto an output reference mosaic with the following World Coordinate System (WCS) specifications:
            NAXIS1 =  32000
            NAXIS2 =  29000
            CRPIX1 =  17388.023478781
            CRPIX2 =  13865.850155511
            CRVAL1 =  84.5426015
            CRVAL2 = -69.1394085
            CD1_1   = -9.010672487E-06
            CD1_2   = -6.309340800E-06
            CD2_1   = -6.309340800E-06
            CD2_2   =  9.010672487E-06
The drizzled science mosaics (drz) are all in units of electrons/s, and are accompanied by weight files (wht) that are based on the exposure times of all the input exposures. For further details about the observations, please refer to Sabbi et al. (2016).