Data

The SPHERE infrared survey for exoplanets (SHINE). First sub-sample analysis

Vigan et al. 2021, A&A, 651, A72
Desidera et al. 2021, A&A, 651, A70
Langlois et al. 2021, A&A, 651, A71
The complete data of the SHINE first sub-sample papers will be availabled on the Direct Imaging Virtual Archive (DIVA) in the HCI-FITS standard as soon as the three papers are accepted.
The mean sensitivity map of the survey as a function of mass and semi-major axis, based on detection limited converted with the BEX-COND-hot, BEX-COND-warm and COND-2003 evolutionary tracks is available below. The data is stored as a FITS table with the mass, semi-major axis and probability stored in colums MASS, SMA and PROB respectively:: shine_bex-cond-hot_detmap.fits - Average detection probability map based on BEX-COND-hot evolutionary models; shine_bex-cond-warm_detmap.fits - Average detection probability map based on BEX-COND-warm evolutionary models; shine_cond-2003_detmap.fits - Average detection probability map based on COND-2003 evolutionary models

Vigan et al. 2017, A&A, 603, A3
Chauvin et al. 2015, A&A, 573, A127
The complete data of the NaCo-LP II and IV papers are available on the Direct Imaging Virtual Archive (DIVA), along with the data of many other published direct imaging surveys. The data includes images, detection maps, detection limits and information about detected candidates. The format of these data follow the HCI-FITS standard defined in collaboration with the STScI (ALICE project) for the distribution of high-level science products in high-contrast imaging.
The complete sample data is available at the CDS:: J/A+A/544/A9 - NaCo-LP sample on VizieR
The mean sensitivity map of the survey as a function of mass and semi-major axis, based on detection limited converted with the COND-2003 evolutionary tracks (Baraffe et al. 2003) is available below. The data is stored as a FITS table with the mass, semi-major axis and probability stored in colums MASS, SMA and PROB respectively:: nacolp_average_detmap.fits - Average detection probability map based on COND-2003 evolutionary models

Vigan et al. 2012, A&A, 544, A9
The complete data of the IDPS I paper is available on the Direct Imaging Virtual Archive (DIVA), along with the data of many other published direct imaging surveys. The data includes images, detection maps, detection limits and information about detected candidates. The format of these data follow the HCI-FITS standard defined in collaboration with the STScI (ALICE project) for the distribution of high-level science products in high-contrast imaging.
The complete sample data is available at the CDS:: J/A+A/544/A9 - IDPS I sample on VizieR
The mean sensitivity map of the survey as a function of mass and semi-major axis, based on detection limited converted with the COND-2003 evolutionary tracks (Baraffe et al. 2003) is available below. The data is stored as a FITS table with the mass, semi-major axis and probability stored in colums MASS, SMA and PROB respectively:: idps_average_detmap.fits - Average detection probability map based on COND-2003 evolutionary models

Vigan et al. 2015, MNRAS, 454, 129
This paper contains the best detection limit ever reported in ground-based high-contrast imaging (~3x10^-7 in the 0.4"-1.0" range). The detection limits reported in the Figure 2 of the paper are available here:: Sirius_irdifs_contrast_ASDI.dat - [49 kB] - ASDI detection limits; Sirius_irdifs_contrast_ADI.dat - [49 kB] - ADI-only detection limits; Sirius_ircs_2011-01_contrast_ADI.dat - [12 kB] - January 2011 IRCS data from Thalmann et al. (2011); Sirius_ircs_2011-03_contrast_ADI.dat - [11 kB] - March 2011 IRCS data from Thalmann et al. (2011)

Vigan et al. 2016, A&A, 587, A55
First light paper of the VLT/SPHERE instrument, dedicated to the characterization of the GJ758 system, including detailed characterization of the known (Thalmann et al. 2009) brown dwarf companion. The raw IRDIS data in the Y23, J23, H23 and K12 DBI filters is publicly available from the ESO archive.: GJ758B_apparent_flux.dat - [1 kB] - Apparent flux of GJ758B (Table 6 from the paper)