A short movie showing how the observed spectrum of star-forming galaxies changes as we observe it at higher and higher redshift. Redshift is denoted here in this movie as "z". Note how the break in the spectrum shifts to redder and redder wavelengths as a result of this redshifting effect. To be able to identify galaxies at the highest redshifts (and thus near the beginning of the universe), it is necessary to be able to measure the fluxes of sources at near-infrared wavelengths (>1000 nm). High-redshift galaxies are frequently found by noting a significant break in the spectrum as seen through a set of discrete filters (shown here in terms of their wavelength sensitivities as a set of colored lines). Download the movie: hst_filters_sed_v2.mp4 (with annotations 13MB) or hst_filters_sed_v1.mp4 (without annotations 4.2MB).
We have submitted to MAST the 1.5 version data release of the Hubble Legacy Fields (HLF) project covering a 25 x 25 arcmin area over the GOODS-S (ECDF-S) region from the HST archival program AR-13252. The release combines exposures from Hubble's two main cameras, the Advanced Camera for Surveys (ACS/WFC) and the Wide Field Camera 3 (WFC3/IR), taken over more than a decade between mid-2002 to the end of 2016. The HLF includes essentially all optical (ACS/WFC F435W, F606W, F775W, F814W and F850LP filters) and infrared (WFC3/ IR F098M, F105W, F125W, F140W and F160W filters) data taken by Hubble over the original CDF-S region including the GOODS-S, ERS, CANDELS and many other programs (31 in total). The data has been released at https://archive.stsci.edu/prepds/hlf/ as images with a common astrometric reference frame, with corresponding inverse variance weight maps. We provide one image per filter of WFC3/IR images at 60 mas per pixel resolution and two ACS/WFC images per filter, at both 30 and 60 mas per pixel. Since this comprehensive dataset combines data from 31 programs on the GOODS-S/CDF-S, the AR proposal identified the MAST products by the global name "Hubble Legacy Field", with this region being identified by "HLF-GOODS-S". This dataset complements that of the Frontier Fields program. The total incorporated in the HLF-GOODS-S is 5.8 Msec in 7211 exposures from 2442 orbits. This is ~70% of a HST full cycle!more
The HDUV is a legacy program using the Hubble Space Telescope to obtain deep UV images of the central parts of the two GOODS fields, which was approved in HST Cycle 22. Our program will build on existing WFC3/UVIS data to obtain deep images at 250-350 nm (in F275W and F336W). These data will provide the first complete census of low-luminosity star-forming galaxies at z~0.5-2 and enable a wealth of research by the community. This includes measuring the physical properties of sub-L* galaxies, and characterizing resolved stellar populations to decipher the build-up of the Hubble sequence from sub-galactic clumps.
To ensure these legacy data are fully exploited, we are releasing high-level science data products to the community. The first epoch v0.5 reduced data are already available on our Data Products page!more
The XDF is the deepest image of the sky taken with Hubble for searching for the earliest galaxies. It includes ALL images taken by Hubble on the small patch of sky first imaged as the Hubble Ultra-Deep Field (HUDF) and subsequently as the HUDF09 and HUDF12. The XDF also adds images that overlapped the HUDF from many other programs including CANDELS, supernova searches and many others (19 in total). These images were taken over a decade from mid-2002 through to early 2013. The XDF is an exposure of 2 million seconds total from Hubble's two premier cameras, the Advanced Camera (ACS) and the Wide Field Camera 3 (WFC3). It consists of 2963 separate images from the ACS and WFC3/IR. ACS flew on the Shuttle to Hubble in 2002 on servicing mission SM3B, while the Wide Field Camera 3 (WFC3) flew to Hubble in 2009 on the final Hubble Shuttle mission (SM4).more
The Hubble Ultra Deep Field 2009 (HUDF09) program observations obtained by HST program 11563 (PI: Garth Illingworth) in Cycle 17 has made publicly available. The program uses WFC3/IR as the prime instrument for 192 orbits to image the deep ACS fields that were obtained in the original HUDF (PI: Steven Beckwith) program and in the HUDF05 (PI: Massimo Stiavelli) program. We have released the data products for this program as an HST High Level Science Product.more
As a part of the HST 10937 (Archival Research) proposal titled Probing the Galaxy Population at z~7-10 Using Archival ACS & NICMOS data PI Rychard Bouwens and colleagues retrieved and process nearly all NICMOS camera 3 F110W and F160W data taken over the GOODS North and South fields.more
HLFRED is a data reduction package for reducing images from Hubble's ACS (WFC) and WFC3 (IR & UVIS) cameras. It is has the capabilities to produce mosaic images from numerous data sets covering a large field. HLFRED was used to create the huge mosaic images for the Hubble Legacy Fields project.more
NICRED is an automatic image processing pipeline for data taken with the Near Infrared Camera and Multi-Object Spectrometer (NICMOS) instrument on the Hubble Space Telescope (HST). The pipeline currently supports imaging data from camera 2 and 3 and is written in Python and C making it portable across many platforms. The automated processing steps include basic calibration (removing the instrumental signature), cosmic-ray removal, treatment for post-SAA cosmic ray persistence and electronic ghosts (a.k.a. the "Mr. Staypuft" effect), sky subtraction, non-linear count-rate correction, artifact masking, robust alignment and registration for large mosaics, weight map generation, and drizzling onto a final image mosaic. NICRED can combined data across different HST observations, visits and proposals with the need for any pre-defined associations. NICRED creates image products with a signal-to-noise ratio that matches the most careful step-by-step manual NICMOS reductions.more
Apsis in an automatic image processing pipeline for the Hubble Space Telescope's Advanced Camera for Surveys (ACS) instrument. The pipeline supports processing of images from the HRC and WFC cameras on the ACS instrument and is written in Python. The processing steps include empirical determination of image offsets and rotation, cosmic ray rejection, image combination using the drizzle routine called via the STScI Pyraf package, object detection and photometry using SExtractor.more