2022A&A...666A..33D


Query : 2022A&A...666A..33D

2022A&A...666A..33D - Astronomy and Astrophysics, volume 666A, 33 (2022/10-1)

The SHARDDS survey: limits on planet occurrence rates based on point sources analysis via the Auto-RSM framework.

DAHLQVIST C.-H., MILLI J., ABSIL O., CANTALLOUBE F., MATRA L., CHOQUET E., DEL BURGO C., MARSHALL J.P., WYATT M. and ERTEL S.

Abstract (from CDS):


Context. In the past decade, high contrast imaging allowed the detection and characterisation of exoplanets, brown dwarfs, and circumstellar disks. Large surveys provided new insights about the frequency and properties of massive sub-stellar companions with separations from 5 to 300 au.
Aims. In this context, our study aims to detect and characterise potential exoplanets and brown dwarfs within debris disks, considering a diverse population of stars with respect to stellar age and spectral type. We present in this paper the analysis of a set of H-band images taken by the VLT/SPHERE instrument in the context of the SHARDDS survey. This survey gathers 55 main-sequence stars within 100 pc, known to host a high-infrared-excess debris disk, allowing us to potentially better understand the complex interactions between substellar companions and disks.
Methods. We rely on the Auto-RSM framework to perform an in-depth analysis of the considered targets, via the computation of detection maps and contrast curves. A clustering approach is used to divide the set of targets into multiple subsets, in order to reduce the computation time by estimating a single optimal parametrisation for each considered subset. Detection maps generated with different approaches are used along with contrast curves to identify potential planetary companions. Planet detection and planet occurrence frequencies are derived from the generated contrast curves, relying on two well-known evolutionary models, namely AMES-DUSTY and AMES-COND. Finally, we study the influence of the observing conditions and observing sequence characteristics on the performance measured in terms of contrast.
Results. The use of Auto-RSM allows us to reach high contrast at short separations, with a median contrast of 105 at 300 mas, for a completeness level of 95%. A new planetary characterisation algorithm, based on the RSM framework, is developed and tested successfully, showing a higher astrometric and photometric precision for faint sources compared to standard approaches. Apart from the already known companion of HD 206893 and two point-like sources around HD 114082 which are most likely background stars, we did not detect any new companion around other stars. A correlation study between achievable contrasts and parameters characterising high contrast imaging sequences highlights the importance of the Strehl ratio, wind speed at a height of 30 meters, and presence of wind-driven halo to define the quality of high contrast images. Finally, planet detection and occurrence rate maps are generated and show, for the SHARDDS survey, a high sensitivity between 10 and 100 au for substellar companions with masses >10 MJ.

Abstract Copyright: © C.-H. Dahlqvist et al. 2022

Journal keyword(s): surveys - planets and satellites: detection - techniques: image processing - techniques: high angular resolution - methods: statistical - methods: data analysis

Simbad objects: 58

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Number of rows : 58
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 HD 105 PM* 00 05 52.5447817152 -41 45 11.044988352   8.13 7.53     G0V 179 0
2 HD 203 PM* 00 06 50.0863238088 -23 06 27.145662264   6.547 6.173   5.74 F3V 129 0
3 HD 377 PM* 00 08 25.7454555168 +06 37 00.489407808   8.22 7.59   6.90 G2V 148 0
4 * bet03 Tuc ** 00 32 43.9053745704 -63 01 53.402028960 5.15 5.13 5.09     A0V 126 0
5 HD 3670 PM* 00 38 56.7030427128 -52 32 03.387011784   8.68 8.21     F5V 27 0
6 * 49 Cet PM* 01 34 37.7786780856 -15 40 34.898673000   5.667 5.607   5.54 A1V 303 0
7 HD 10472 PM* 01 40 24.0655876848 -60 59 56.626037484   8.01 7.61   7.13 F2IV/V 63 0
8 HD 10638 PM* 01 44 22.8101731920 +32 30 57.159014724   6.96 6.73   6.45 A3 37 0
9 HD 13246 PM* 02 07 26.1250439520 -59 40 45.941799000   8.02 7.50     F7V 87 1
10 HD 14082B BY* 02 17 24.7369490496 +28 44 30.411007188   8.33 7.74     G2V 111 0
11 BD+30 397 PM* 02 27 29.2543096632 +30 58 24.596323968   11.3 10.12 9.32 8.78 K7V 107 1
12 * 12 Tri PM* 02 28 09.9798701064 +29 40 09.585503796 5.680 5.580 5.290     F0III 72 0
13 HD 16743 PM* 02 39 07.5626487408 -52 56 05.304122592   7.13 6.77   6.33 F0/2III/IV 56 0
14 HD 17390 PM* 02 46 45.1042039656 -21 38 22.278982308   6.850 6.469     F3IV/V 57 0
15 HD 21997 PM* 03 31 53.6470102728 -25 36 50.940001116   6.501 6.372   6.25 A3IV/V 155 0
16 HD 22179 TT* 03 35 29.9010684744 +31 13 37.444642500   9.536 8.932 8.59   G5IV 41 0
17 HD 24636 PM* 03 48 11.4715618344 -74 41 38.819425776   7.513 7.127     F3IV/V 63 0
18 HD 25457 TT* 04 02 36.7442719512 -00 16 08.119921152   5.88 5.38     F7V 265 0
19 HD 31392 PM* 04 54 04.2085021752 -35 24 16.263520632   8.40 7.61     G9V 85 0
20 HD 35650 Ro* 05 24 30.1695408744 -38 58 10.747077852 11.54 10.365 9.054 8.293 7.577 K6V 94 0
21 V* VZ Col BY? 05 30 14.0042313744 -42 41 50.379896724 12.333 11.096 9.706 8.851 8.078 M0V 30 0
22 HD 37484 * 05 37 39.6269435064 -28 37 34.655407824   7.66 7.25   6.79 F4V 96 0
23 HD 38207 * 05 43 20.9563546392 -20 11 21.441628716   8.83 8.47     F2V 34 0
24 HD 38206 * 05 43 21.6709239120 -18 33 26.911637928   5.711 5.727   5.72 A0V 109 0
25 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1908 1
26 HD 40540 * 05 57 52.5987257424 -34 28 34.006454004   7.82 7.54   7.23 A8IV(m) 24 0
27 HD 53842 PM* 06 46 13.5367594104 -83 59 29.517958896   8.880 8.622     F5V 72 0
28 HD 60491 BY* 07 34 26.1676173360 -06 53 48.036803172 9.554 9.027 8.144 7.654 7.214 K1V 82 0
29 HD 69830 PM* 08 18 23.9469682407 -12 37 55.817187530   6.74 5.95     G8:V 527 1
30 HD 71722 * 08 26 25.2055695408 -52 48 26.990371908   6.097 6.041     A0V 49 0
31 V* V401 Hya BY* 08 37 50.2937396460 -06 48 24.779911420 7.577 7.394 6.725 6.365 6.029 G8/K0(IV) 175 0
32 * omi02 Cnc PM* 08 57 35.1996769392 +15 34 52.625733024   5.892 5.677     F0IV 64 0
33 HD 80950 * 09 17 27.5695868640 -74 44 04.524994932   5.844 5.857     A0V 51 0
34 HD 82943 PM* 09 34 50.7353072232 -12 07 46.369202196   7.17 6.53     F9VFe+0.5 470 2
35 HD 84075 TT* 09 36 17.8234661352 -78 20 41.588588076   9.18 8.59     G2V 57 0
36 HD 107649 * 12 22 24.8547408624 -51 01 34.361873436   9.26 8.78     F5V 38 0
37 BD+21 2486 ** 13 06 15.39818 +20 43 45.2749 11.909 10.715 9.398 8.575 7.823 K4V 75 0
38 HD 114082 * 13 09 16.1926316904 -60 18 30.055543200   8.64 8.21     F3V 80 1
39 HD 120534 SB* 13 50 40.2155260752 -31 12 23.072500224   7.29 7.02     A5V+(F) 17 0
40 HD 122652 PM* 14 02 31.6383121656 +31 39 39.089147004   7.69 7.15     F8 87 0
41 HD 133803 gD* 15 07 14.9365580040 -29 30 16.132469112   8.47 8.12     F2IVm-2 55 0
42 HD 135599 BY* 15 15 59.1668432664 +00 47 46.900249728 8.215 7.748 6.905 6.438 6.028 K0V 119 0
43 HD 138965 PM* 15 40 11.5557598920 -70 13 40.379510928   6.499 6.424     A1V 49 0
44 HD 145229 PM* 16 09 26.6275032840 +11 34 28.047914868   8.03 7.44     G0 77 0
45 * 73 Her PM* 17 24 06.5870998728 +22 57 37.016126892 5.980 5.930 5.720     A7V 74 0
46 HD 164249 PM* 18 03 03.4097283792 -51 38 56.432149872   7.438 7.007 7.90   F6V 120 0
47 HD 172555 PM* 18 45 26.9009806435 -64 52 16.534807985   4.967 4.767     A7V 278 0
48 * eta Tel PM* 19 22 51.2060774616 -54 25 26.145617376   5.035 5.020   4.99 A0V 216 0
49 HD 182681 PM* 19 26 56.4829971576 -29 44 35.617721496   5.635 5.644     B8.5V 71 0
50 HD 192758 PM* 20 18 15.7880861160 -42 51 36.297564804   7.34 7.03     F0V 42 0
51 HD 201219 PM* 21 07 56.5197854640 +07 25 58.594324908       7.6   G5 75 0
52 HD 205674 PM* 21 37 21.1116403080 -18 26 28.243601556   7.57 7.17   6.73 F3/5IV 44 0
53 HD 206893b Pl 21 45 21.9052532928 -12 47 00.060804636           ~ 40 0
54 HD 206893 PM* 21 45 21.9052532928 -12 47 00.060804636   7.11 6.67     F5V 114 0
55 * alf PsA C ** 22 48 04.4928501697 -24 22 07.717793375   14.301 12.624 12.216 9.674 M4.0Ve 78 0
56 HD 218396 El* 23 07 28.7157209544 +21 08 03.310767492   6.21 5.953     F0+VkA5mA5 1141 0
57 HD 218340 PM* 23 08 12.3705531504 -63 37 41.372351436   9.07 8.44     G3V 50 0
58 HD 221853 PM* 23 35 36.1523996880 +08 22 57.426983076   7.75 7.34   6.88 F0 51 0

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