In this section you will find more information about the scientific goals of the project and regular updates on the most recent results. A variety of statistical indicators will be used to explore the properties of high-redshift galaxies and AGNs based on the scientific analysis of the unique data set produced by the Astrodeep project.
ASTRODEEP is a coordinated and comprehensive program of i) algorithm/software development and testing; ii) data reduction/release, and iii) scientific data validation/analysis aimed at making Europe the world leader in the exploitation of the deepest multi-frequency astronomical survey data.Accessing the faint luminosity regime (L < 0.2 L*) at z > 6 is crucial in the context of cosmic reionization: faint galaxies dominate the global ultraviolet luminosity density and possibly have an escape fraction of ionizing radiation larger than the brighter counterparts. Here we report on the LBT/MODS1 spectroscopic confirmation of two faint z = 6.4 sources, which are significantly magnified by the FF galaxy cluster MACSJ0717.5+3745, study their physical properties, and discuss the contributions of such objects to the reionization of the IGM.
In this section you can find information about the data sets that have been used by the Astrodeep project, as well as links to all Astrodeep data products.
The Hawk‐I UDS and GOODS Survey (HUGS) represents the deepest wide-area survey ever completed in the K band. Exploiting the excellent performances of the VLT near IR imager HawkI, it delivers deep (K=27), high‐ quality (0.4 arcsec seeing) imaging at 2.2 microns over GOODS-South (including the HUDF13 area) and UDS-CANDELS, and at 1micron over UDS-CANDELS. HUGS fills a crucial gap in spectral coverage between the HST and Spitzer data in two of the CANDELS survey fields. All images and catalogs are made public. Click here for full description and download.
One of the main Astrodeep goals is to update existing algorithms and if necessary develop new software to create high quality multi-wavelength catalogs extracted from both space and ground-based datasets. In this section you will be able to download all new software developed by Astrodeep members.
CONVPHOT (De Santis et al. 2006) is a C code developed at INAF‐OAR that can compute background for each source and subtract it on-the-fly. The convolution is performed via straight pixel-‐by-‐pixel summation. Cutouts, templates, and also segmentations for each object can be stored as FITS files (requiring a large amount of memory), but the code may be run without storing images. Its only pre‐ requirement is the CFTISIO library.TFIT (Laidler et al. 2007) was initially conceived and written by C. Papovich in 1999 as a C++ code.In its latest version, TFIT consists of a Python envelop performing the entirety of tasks, except for the fitting core routine, which is based on the original C++ routines. It requires the pre‐ installation of the following software: Python (and some of its standard modules/interfaces, such as numpy, scipy, matplotlib, anfft, pyraf); CFITSIO libraries; STSCI; IRAF; STSDAS; FFTW3.