The SPHERE infrared survey for exoplanets (SHINE). II. Observations, data reduction and analysis, detection performances, and initial results. Langlois M., Gratton R., Lagrange A.-M., Delorme P., Boccaletti A., Bonnefoy M., Maire A.-L., Mesa D., Chauvin G., Desidera S., Vigan A., Cheetham A., Hagelberg J., Feldt M., Meyer M., Rubini P., Le Coroller H., Cantalloube F., Biller B., Bonavita M., Bhowmik T., Brandner W., Daemgen S., D'Orazi V., Flasseur O., Fontanive C., Galicher R., Girard J., Janin-Potiron P., Janson M., Keppler M., Kopytova T., Lagadec E., Lannier J., Lazzoni C., Ligi R., Meunier N., Perreti A., Perrot C., Rodet L., Romero C., Rouan D., Samland M., Salter G., Sissa E., Schmidt T., Zurlo A., Mouillet D., Denis L., Thiebaut E., Milli J., Wahhaj Z., Beuzit J.-L., Dominik C., Henning Th., Menard F., Mueller A., Schmid H.M., Turatto M., Udry S., Abe L., Antichi J., Allard A.Baruolo F., Baudoz P., Baudrand J., Bazzon A., Blanchard P., Carbillet M., Carle M., Cascone E., Charton J., Claudi R., Costille A., De Caprio V., Delboulbe A., Dohlen K., Fantinel D., Feautrier P., Fusco T., Gigan P., Giro E., Gisler D., Gluck L., Gry C., Hubin N., Hugot E., Jaquet M., Kasper M., Le Mignant D., Llored M., Madec F., Magnard Y., Martinez P., Maurel D., Messina S., Moeller-Nilsson O., Mugnier L., Moulin T., Origne A., Pavlov A., Perret D., Petit C., Pragt J., Puget P., Rabou P., Ramos J., Rigal F., Rochat S., Roelfsema R., Rousset G., Roux A., Salasnich B., Sauvage J.-F., Sevin A., Soenke C., Stadler E., Suarez M., Weber L., Wildi F., Rickman E. =2021A&A...651A..71L 2021A&A...651A..71L (SIMBAD/NED BibCode) ADC_Keywords: Stars, double and multiple ; Exoplanets ; Photometry Keywords: methods: observational - planets and satellites: detection - techniques: image processing - methods: statistical - instrumentation: high angular resolution - planets and satellites: formation Abstract: In recent decades, direct imaging has confirmed the existence of substellar companions (exoplanets or brown dwarfs) on wide orbits (>10 au) around their host stars. In striving to understand their formation and evolution mechanisms, in 2015 we initiated the SPHERE infrared survey for exoplanets (SHINE), a systematic direct imaging survey of young, nearby stars that is targeted at exploring their demographics. We aim to detect and characterize the population of giant planets and brown dwarfs beyond the snow line around young, nearby stars. Combined with the survey completeness, our observations offer the opportunity to constrain the statistical properties (occurrence, mass and orbital distributions, dependency on the stellar mass) of these young giant planets. In this study, we present the observing and data analysis strategy, the ranking process of the detected candidates, and the survey performances for a subsample of 150 stars that are representative of the full SHINE sample. Observations were conducted in a homogeneous way between February 2015 and February 2017 with the dedicated ground-based VLT/SPHERE instrument equipped with the IFS integral field spectrograph and the IRDIS dual-band imager, covering a spectral range between 0.9 and 2.3m. We used coronographic, angular, and spectral differential imaging techniques to achieve the best detection performances for this study, down to the planetary mass regime. We processed, in a uniform manner, more than 300 SHINE observations and datasets to assess the survey typical sensitivity as a function of the host star and of the observing conditions. The median detection performance reached 5-contrasts of 13mag at 200mas and 14.2mag at 800mas with the IFS (YJ and YJH bands), and of 11.8mag at 200mas, 13.1mag at 800mas, and 15.8mag at 3as with IRDIS in H band, delivering one of the deepest sensitivity surveys thus far for young, nearby stars. A total of sixteen substellar companions were imaged in this first part of SHINE: seven brown dwarf companions and ten planetary-mass companions. These include two new discoveries, HIP 65426 b and HIP 64892 B, but not the planets around PDS70 that had not been originally selected for the SHINE core sample. A total of 1483 candidates were detected, mainly in the large field of view that characterizes IRDIS. The color-magnitude diagrams, low-resolution spectrum (when available with IFS), and follow-up observations enabled us to identify the nature (background contaminant or comoving companion) of about 86% of our subsample. The remaining cases are often connected to crowded-field follow-up observations that were missing. Finally, even though SHINE was not initially designed for disk searches, we imaged twelve circumstellar disks, including three new detections around the HIP 73145, HIP 86598, and HD106906 systems. Nowadays, direct imaging provides a unique opportunity to probe the outer part of exoplanetary systems beyond 10au to explore planetary architectures, as highlighted by the discoveries of: one new exoplanet, one new brown dwarf companion, and three new debris disks during this early phase of SHINE. It also offers the opportunity to explore and revisit the physical and orbital properties of these young, giant planets and brown dwarf companions (relative position, photometry, and low-resolution spectrum in near-infrared, predicted masses, and contrast in order to search for additional companions). Finally, these results highlight the importance of finalizing the SHINE systematic observation of about 500 young, nearby stars for a full exploration of their outer part to explore the demographics of young giant planets beyond 10au and to identify the most interesting systems for the next generation of high-contrast imagers on very large and extremely large telescopes. Description: We process, in a uniform manner, more than 300 datasets from the SPHERE/SHINE Survey obtained at the VLT/ESO in visitor mode and assess the SHINE survey's typical sensitivity as a function of the host star and observing conditions. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file tablea1.dat 144 2910 Detected point sources parameters -------------------------------------------------------------------------------- See also: J/A+A/651/A70 : SHINE sample definition (Desidera+, 2021) Byte-by-byte Description of file: tablea1.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 15 A15 --- Name Host star ID 17- 26 A10 "date" Obs.date Observation date 28- 30 A3 --- Filt Filter pair (Filter0Filter1) used for the observations (1) 32- 34 I3 --- NNCID1 Unique candidate companion ID (NNCID1 NNCID2) 36- 38 I3 --- NNCID2 Unique candidate companion ID (NNCID1 NNCID2) 42- 49 F8.2 mas Sep Candidate companion separation from host star 51- 55 F5.2 mas e_Sep ? rms uncertainty on Sep 57- 62 F6.2 deg PA Candidate companion position angle from host star 64- 69 F6.2 deg e_PA ? rms uncertainty on PA 71- 75 F5.2 mag dm0 Candidate companion relative magnitude from host star (filter 0) 77- 80 F4.2 mag e_dm0 ? rms uncertainty on dm0 82- 86 F5.2 mag dm1 Candidate companion relative magnitude from host star (filter 1) 88- 91 F4.2 mag e_dm1 ? rms uncertainty on dm1 93- 97 F5.2 mag absm0 Candidate companion absolute magnitude (filter 0) 99-102 F4.2 mag e_absm0 ? rms uncertainty on absm0 104-108 F5.2 mag absm1 Candidate companion absolute magnitude (filter 1) 110-113 F4.2 mag e_absm1 ? rms uncertainty on absm1 115-120 F6.2 --- snr0 Candidate companion signal to noise ratio (filter 0) 122-127 F6.2 --- snr1 Candidate companion signal to noise ratio (filter 1) 129-134 F6.2 --- Prob ? Standard ranking probability 136-141 F6.2 --- ProbColor Ranking probability based on color-magnitude diagram 143-144 A2 --- Status Final status (2) -------------------------------------------------------------------------------- Note (1): Filter pair as follows: BBH = broad-band BB-H H23 = dual-band DB-H23 J23 = dual-band DB-J23 K12 = dual-band DB-K12 Note (2): Final status of the candidates as follows: C = companion with a confirmed common-proper motion B = contaminants either discriminated using the CMD or the common-proper motion test A = Ambiguous cases U = non-straightforward, non-clear detections, which correspond to the identification of candidates with unreliable astrometry or photometry and for which our standard classification scheme could not be applied FP = non-straightforward, non-clear detections, which correspond to the identification of candidates with unreliable astrometry or photometry and for which our standard classification scheme could not be applied -------------------------------------------------------------------------------- Acknowledgements: Maud Langlois, maud.langlois(at)univ-lyon1.fr References: Desidera et al., Paper I 2021A&A...651A..70D 2021A&A...651A..70D, Cat. J/A+A/651/A70