J/A+A/651/A71 SHINE II (Langlois+, 2021)
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.
<Astron. Astrophys. 651, A71 (2021)>
=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:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 144 2910 Detected point sources parameters
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See also:
J/A+A/651/A70 : SHINE sample definition (Desidera+, 2021)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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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)
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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
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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
(End) Patricia Vannier [CDS] 12-Jul-2021