2020A&A...641A.131L


C.D.S. - SIMBAD4 rel 1.7 - 2020.11.28CET20:25:01

2020A&A...641A.131L - Astronomy and Astrophysics, volume 641A, 131-131 (2020/9-1)

The search for disks or planetary objects around directly imaged companions: a candidate around DH Tauri B.

LAZZONI C., ZURLO A., DESIDERA S., MESA D., FONTANIVE C., BONAVITA M., ERTEL S., RICE K., VIGAN A., BOCCALETTI A., BONNEFOY M., CHAUVIN G., DELORME P., GRATTON R., HOULLE M., MAIRE A.L., MEYER M., RICKMAN E., SPALDING E.A., ASENSIO-TORRES R., LANGLOIS M., MULLER A., BAUDINO J.-L., BEUZIT J.-L., BILLER B., BRANDNER W., BUENZLI E., CANTALLOUBE F., CHEETHAM A., CUDEL M., FELDT M., GALICHER R., JANSON M., HAGELBERG J., HENNING T., KASPER M., KEPPLER M., LAGRANGE A.-M., LANNIER J., LECOROLLER H., MOUILLET D., PERETTI S., PERROT C., SALTER G., SAMLAND M., SCHMIDT T., SISSA E. and WILDI F.

Abstract (from CDS):


Context. In recent decades, thousands of substellar companions have been discovered with both indirect and direct methods of detection. While the majority of the sample is populated by objects discovered using radial velocity and transit techniques, an increasing number have been directly imaged. These planets and brown dwarfs are extraordinary sources of information that help in rounding out our understanding of planetary systems.
Aims. In this paper, we focus our attention on substellar companions detected with the latter technique, with the primary goal of investigating their close surroundings and looking for additional companions and satellites, as well as disks and rings. Any such discovery would shed light on many unresolved questions, particularly with regard to their possible formation mechanisms.
Methods. To reveal bound features of directly imaged companions, whether for point-like or extended sources, we need to suppress the contribution from the source itself. Therefore, we developed a method based on the negative fake companion technique that first estimates the position in the field of view (FoV) and the flux of the imaged companion with high precision, then subtracts a rescaled model point spread function (PSF) from the imaged companion, using either an image of the central star or another PSF in the FoV. Next it performs techniques, such as angular differential imaging, to further remove quasi-static patterns of the star (i.e., speckle contaminants) that affect the residuals of close-in companions.
Results. After testing our tools on simulated companions and disks and on systems that were chosen ad hoc, we applied the method to the sample of substellar objects observed with SPHERE during the SHINE GTO survey. Among the 27 planets and brown dwarfs we analyzed, most objects did not show remarkable features, which was as expected, with the possible exception of a point source close to DH Tau B. This candidate companion was detected in four different SPHERE observations, with an estimated mass of ∼1MJup, and a mass ratio with respect to the brown dwarf of 1/10. This binary system, if confirmed, would be the first of its kind, opening up interesting questions for the formation mechanism, evolution, and frequency of such pairs. In order to address the latter, the residuals and contrasts reached for 25 companions in the sample of substellar objects observed with SPHERE were derived. If the DH Tau Bb companion is real, the binary fraction obtained is ∼7%, which is in good agreement with the results obtained for field brown dwarfs .
Conclusions. While there may currently be many limitations affecting the exploration of bound features to directly imaged exoplanets and brown dwarfs, next-generation instruments from the ground and space (i.e., JWST, ELT, and LUVOIR) will be able to image fainter objects and, thus, drive the application of this technique in upcoming searches for exo-moons and circumplanetary disks.

Abstract Copyright: © ESO 2020

Journal keyword(s): instrumentation: adaptive optics - methods: data analysis - methods: observational - techniques: image processing - planets and satellites: detection - planets and satellites: formation

Simbad objects: 72

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Number of rows : 72

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 HD 1160C LM* 00 15 57.2389782387 +04 15 09.090222186           M3.5 12 0
2 HD 1160B LM* 00 15 57.26 +04 15 03.7           ~ 26 0
3 HD 1160 * 00 15 57.3020078544 +04 15 04.004951787   7.159 7.119     A0V 78 1
4 HD 4747 SB* 00 49 26.7612113944 -23 12 44.865754071 8.244 7.927 7.155 6.732 6.344 G8/K0V 135 0
5 HD 4747b Pl? 00 49 26.7612113944 -23 12 44.865754071           ~ 18 0
6 CD-52 381 PM* 01 52 14.6258722411 -52 19 33.185337378   11.836 10.953 10.42 9.825 K2V(e) 48 0
7 HD 19467B BD* 03 07 18.48 -13 45 43.3           T5.5+1 20 0
8 HD 19467 PM* 03 07 18.5750358835 -13 45 42.419198459   7.65 7.00 7.79 8.82 G3V 127 0
9 HD 284149b * 04 06 38.8 +20 18 11           ~ 11 0
10 V* DH Tau Or* 04 29 41.5520056304 +26 32 58.123761109 15.14 14.62 13.10 13.01   M1Ve 269 0
11 V* DH Tau B LM* 04 29 41.66 +26 32 56.5           M9.25 60 1
12 V* DI Tau Or* 04 29 42.4736177473 +26 32 49.119618729 16.39 15.20 13.60     M0Ve 197 0
13 * 51 Eri PM* 04 37 36.1323118067 -02 28 24.778826936   5.486 5.209     F0IV 175 0
14 * 51 Eri b Pl 04 37 36.1323118067 -02 28 24.778826936           ~ 104 0
15 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3575 0
16 V* AB Dor C LM* 05 28 44.83 -65 26 54.9           M8: 61 0
17 V* AB Dor TT* 05 28 44.8916324761 -65 26 55.289846904 8.259 7.856 6.999 6.496 5.993 K0V 939 0
18 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1678 1
19 * bet Pic b Pl 05 47 17.0876901 -51 03 59.441135           ~ 358 1
20 CD-35 2722 ** 06 09 19.2082646634 -35 49 31.062882043   12.61 11.083 10.682 9.337 M1Ve 62 0
21 NAME Columba Association As* 06 14.0 -40 03           ~ 211 0
22 HD 44627 Ro* 06 19 12.9129838711 -58 03 15.524890610   10.01 9.205   8.185 K1V(e) 141 1
23 HD 44627B BD* 06 19 12.94 -58 03 20.9           L1 112 1
24 HD 50571B BD* 06 50 00.93 -60 14 56.7           L4-10 10 0
25 HD 50571 PM* 06 50 01.0154778405 -60 14 56.919001147   6.548 6.098 7.26   F5VFe+0.4 58 0
26 HD 76346 ** 08 53 03.7788614388 -56 38 58.137676320   5.982 5.998     A0V 46 0
27 HD 95086 * 10 57 03.0216129217 -68 40 02.446874288   7.60 7.36     A8III 130 1
28 HD 95086b Pl 10 57 03.0216129217 -68 40 02.446874288           ~ 74 1
29 V* CT Cha B LM* 11 04 08.44 -76 27 18.0           M8 40 0
30 V* CT Cha Or* 11 04 09.0989057683 -76 27 19.326914289   13.44 13.00   10.89 K7Ve 111 0
31 HD 97334B BD* 11 12 25.6347484565 +35 48 12.777435627           L4.5+L6 67 0
32 CD-33 7795B LM* 11 31 55.2500 -34 36 25.200     20.40   15.8 M8.5/9e 119 0
33 * e Vir PM* 13 16 46.5161591991 +09 25 26.967205938   5.81   4.8   G0V 507 1
34 * e Vir b Pl 13 16 46.5161591991 +09 25 26.967205938           ~ 83 1
35 HD 115470 * 13 18 05.1042056946 -44 03 19.376995020   6.77 6.79     B9.5V 24 0
36 HD 115470b Pl? 13 18 05.1042056946 -44 03 19.376995020           ~ 6 0
37 HD 116434 ** 13 24 36.0982987288 -51 30 16.046513257   7.08 6.98   6.87 A2V 40 0
38 HD 116434C BD* 13 24 36.13 -51 30 16.7           L5-7 34 1
39 ASAS J140748-3945.7 pr* 14 07 47.9296051120 -39 45 42.766332988   13.56 12.31 11.91 10.92 K5IVe 52 0
40 CD-40 8434c Pl 14 08 10.1545137760 -41 23 52.576649494           ~ 27 0
41 CD-40 8434b Pl 14 08 10.1545137760 -41 23 52.576649494           ~ 60 0
42 CD-40 8434 TT* 14 08 10.1545137760 -41 23 52.576649494   13.42 12.18 11.71 10.506 K7IVe 130 0
43 NAME beta Pic Moving Group MGr 14 30 -42.0           ~ 582 0
44 NAME HD 130948BC BD* 14 50 16.00 +23 54 41.8           L4+L4 55 0
45 BD+16 2708B SB* 14 54 29.4185719182 +16 06 08.616294953           M8.5 131 0
46 CD-35 10525B LM* 15 49 12.04 -35 39 05.1           M9-L4 6 0
47 CD-35 10525 Or* 15 49 12.1055573607 -35 39 05.053991067 12.19 12.76 11.66 11.15   K7Ve 245 0
48 CD-35 10525C LM* 15 49 13.3081131346 -35 39 11.790418380           ~ 101 0
49 HD 143567 * 16 01 55.4546289923 -21 58 49.397570493   7.27 7.19 7.87   B9V 107 0
50 HD 143567B LM* 16 01 55.65696 -21 58 53.0076           M8 28 0
51 [PGZ2001] J161031.9-191305 pr* 16 10 31.9521727854 -19 13 06.081499389   15.14 13.56 13.31   K7e 31 0
52 NAME ASSOC II SCO As* 16 15 -24.2           ~ 1149 1
53 NAME GSC 6214-210 b Pl? 16 21 54.6675132629 -20 43 09.138884434           ~ 2 0
54 NAME SR 12C LM* 16 27 19.66704 -24 41 48.8292           M9.0 31 0
55 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3086 0
56 ROXs 42B TT* 16 31 15.0191785687 -24 32 43.717222006     14.27 13.03 11.72 ~ 45 0
57 HD 163318 * 17 56 41.8404746450 -28 03 55.421464577   5.964 5.763     A7III/IV 31 0
58 V* PZ Tel BY* 18 53 05.8733807460 -50 10 49.901380086   9.22 8.342   7.464 G9IV 291 0
59 * eta Tel PM* 19 22 51.2064652963 -54 25 26.152538950   5.035 5.020   4.99 A0V+M7/8V 192 0
60 * eta Tel B LM* 19 22 51.26 -54 25 30.7           M7.5V 66 0
61 Kepler-1625b Pl 19 41 43.0401596937 +39 53 11.498985535           ~ 43 1
62 HD 206893 PM* 21 45 21.9056012837 -12 47 00.068065895   7.11 6.67     F5V 66 0
63 HD 206893b Pl? 21 45 21.9056012837 -12 47 00.068065895           ~ 15 0
64 * eps Ind B BD* 22 04 10.52064 -56 46 57.7452     24.12 20.8 15.60 T1V+T6V 134 2
65 * alf PsA b Pl 22 57 39.04625 -29 37 20.0533           ~ 187 1
66 HD 218396b Pl 23 07 28.7156905667 +21 08 03.302133882           ~ 209 1
67 HD 218396e Pl 23 07 28.7156905667 +21 08 03.302133882           ~ 136 1
68 HD 218396 El* 23 07 28.7156905667 +21 08 03.302133882   6.21 5.953     F0+VkA5mA5 916 0
69 HD 218396d Pl 23 07 28.7156905667 +21 08 03.302133882           ~ 181 1
70 HD 218396c Pl 23 07 28.7156905667 +21 08 03.302133882           ~ 199 1
71 NAME AB Dor Moving Group MGr ~ ~           ~ 373 0
72 NAME Carina Moving Group MGr ~ ~           ~ 38 0

    Equat.    Gal    SGal    Ecl

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2020.11.28-20:25:01

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