DIVA currently contains high-level science products (HLSP) for the surveys listed in the following table. If you wish your survey to be available in DIVA, please contact the scientific team.
|High-Level Science Products|
|Survey author||Year||Survey name||Reference paper||Note||PSF image||Reduced image||Detection limit||Sensitivity map||Candidates||Download|
|Masciadri||2005||Masciadri-05||2005ApJ...625.1004M||No||No||Yes||No||No||Archive (46 KB)|
|Song||2005||Song-HST||GO10176, unpublished||(a)||No||Yes||No||Yes||No||Archive (48 MB)|
|Biller||2007||Biller-07||2007ApJS..173..143B||No||Yes||Yes||No||No||Archive (9.7 MB)|
|Kasper||2007||Kasper-07||2007A&A...472..321K||No||Yes||Yes||No||No||Archive (2.7 MB)|
|Lafrenière||2007||GDPS||2007ApJ...670.1367L||No||No||Yes||No||Yes||Archive (1.1 MB)|
|Chauvin||2010||DISYNAS||2010A&A...509A..52C||Yes||Yes||Yes||No||Yes||Archive (422 MB)|
|Heinze||2010||Heinze-10||2010ApJ...714.1551H||(b)||No||Yes||Yes||No||Yes||Archive (33 MB)|
|Vigan||2012||IDPS-I||2012A&A...544A...9V||Yes||Yes||Yes||Yes||Yes||Archive (731 MB)|
|Rameau||2013||YoungDusty||2013A&A...553A..60R||Yes||Yes||Yes||Yes||Yes||Archive (125 MB)|
|Chauvin||2015||NaCo-LP||2015A&A...573A.127C||Yes||Yes||Yes||Yes||Yes||Archive (1.6 GB)|
|Meshkat||2015||Meshkat-15a||2015ApJ...800....5M||(c)||No||Yes||Yes||No||Yes||Archive (9.5 KB)|
|Meshkat||2015||Meshkat-15b||2015MNRAS.453.2533M||(c)||No||Yes||Yes||No||Yes||Archive (19 kB)|
|Durkan||2016||Durkan-Spitzer||2016ApJ...824...58D||(d)||Yes||Yes||Yes||No||No, but see (d)||Archive (636 MB)|
Song-HST: the results of this HST/NICMOS survey (GO10176) were never published, but the follow-up of most candidates was done in the DISYNAS survey (Chauvin et al. 2010). For a more complete analysis of this survey including the position and contrast of detected candidates, please see the re-analysis of the HST/NICMOS coronagraphic archive by the ALICE project
Heinze-10: The detection limits of this survey are directly provided in apparent magnitude in L- or M-band.
Meshkat-15a, Meshkat-15b: The observations of these two surveys were performed with the NaCo apodizing phase plate (APP), which provides diffraction suppression only on one side of the PSF. The targets were observed at two different dates to cover properly the complete field-of-view. For this reason, no date of observation is reported in the database for all targets except the ones where a candidate companion was detected. For the latter, the date at which the astrometry of the candidates are reported have been used in DIVA for the corresponding observations.
Durkan-Spitzer: The detection limits of this survey are directly provided in apparent Vega magnitude (see Durkan et al. 2016 and Marengo et al. 2009). All candidates with 2 arcseconds have been determined to be either background objects or bad pixels (Durkan et al. 2016)
For the observations contained in DIVA, the following information can be available. If the information is unknown, the field is empty in the database.
For the detected candidates, the following information is provided when available: