2021A&A...651A..72V

Query : 2021A&A...651A..72V

2021A&A...651A..72V - Astronomy and Astrophysics, volume 651A, 72-72 (2021/7-1)

The SPHERE infrared survey for exoplanets (SHINE). III. The demographics of young giant exoplanets below 300 au with SPHERE.

VIGAN A., FONTANIVE C., MEYER M., BILLER B., BONAVITA M., FELDT M., DESIDERA S., MARLEAU G.-D., EMSENHUBER A., GALICHER R., RICE K., FORGAN D., MORDASINI C., GRATTON R., LE COROLLER H., MAIRE A.-L., CANTALLOUBE F., CHAUVIN G., CHEETHAM A., HAGELBERG J., LAGRANGE A.-M., LANGLOIS M., BONNEFOY M., BEUZIT J.-L., BOCCALETTI A., D'ORAZI V., DELORME P., DOMINIK C., HENNING T., JANSON M., LAGADEC E., LAZZONI C., LIGI R., MENARD F., MESA D., MESSINA S., MOUTOU C., MULLER A., PERROT C., SAMLAND M., SCHMID H.M., SCHMIDT T., SISSA E., TURATTO M., UDRY S., ZURLO A., ABE L., ANTICHI J., ASENSIO-TORRES R., BARUFFOLO A., BAUDOZ P., BAUDRAND J., BAZZON A., BLANCHARD P., BOHN A.J., BROWN SEVILLA S., CARBILLET M., CARLE M., CASCONE E., CHARTON J., CLAUDI R., COSTILLE A., DE CAPRIO V., DELBOULBE A., DOHLEN K., ENGLER N., FANTINEL D., FEAUTRIER P., FUSCO T., GIGAN P., GIRARD J.H., 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., MOLLER-NILSSON O., MOUILLET D., MOULIN T., ORIGNE A., PAVLOV A., PERRET D., PETIT C., PRAGT J., PUGET P., RABOU P., RAMOS J., RICKMAN E.L., RIGAL F., ROCHAT S., ROELFSEMA R., ROUSSET G., ROUX A., SALASNICH B., SAUVAGE J.-F., SEVIN A., SOENKE C., STADLER E., SUAREZ M., WAHHAJ Z., WEBER L. and WILDI F.

Abstract (from CDS):

The SpHere INfrared Exoplanet (SHINE) project is a 500-star survey performed with SPHERE on the Very Large Telescope for the purpose of directly detecting new substellar companions and understanding their formation and early evolution. Here we present an initial statistical analysis for a subsample of 150 stars spanning spectral types from B to M that are representative of the full SHINE sample. Our goal is to constrain the frequency of substellar companions with masses between 1 and 75M_Jup and semimajor axes between 5 and 300au. For this purpose, we adopt detection limits as a function of angular separation from the survey data for all stars converted into mass and projected orbital separation using the BEX-COND-hot evolutionary tracks and known distance to each system. Based on the results obtained for each star and on the 13 detections in the sample, we use a Markov chain Monte Carlo tool to compare our observations to two different types of models. The first is a parametric model based on observational constraints, and the second type are numerical models that combine advanced core accretion and gravitational instability planet population synthesis. Using the parametric model, we show that the frequencies of systems with at least one substellar companion are 23.0_–9.7^+13.5, 5.8_–2.8^+4.7, and 12.6_–7.1^+12.9% for BA, FGK, and M stars, respectively. We also demonstrate that a planet-like formation pathway probably dominates the mass range from 1-75M_Jup for companions around BA stars, while for M dwarfs, brown dwarf binaries dominate detections. In contrast, a combination of binary star-like and planet-like formation is required to best fit the observations for FGK stars. Using our population model and restricting our sample to FGK stars, we derive a frequency of 5.7_–2.8^+3.8%, consistent with predictions from the parametric model. More generally, the frequency values that we derive are in excellent agreement with values obtained in previous studies.

Abstract Copyright: © A. Vigan et al. 2021

Journal keyword(s): techniques: high angular resolution - methods: statistical - infrared: planetary systems - planetary systems - planets and satellites: formation

Simbad objects: 29

Full paper

View the references in ADS

Number of rows : 29

N	Identifier	Otype	ICRS (J2000) RA	ICRS (J2000) DEC	Mag U	Mag B	Mag V	Mag R	Mag I	Sp type	#ref 1850 - 2023	#notes
1	CD-52 381B	LM*	01 52 14.63	-52 19 30.0						M9.5	23	0
2	* 51 Eri b	Pl	04 37 36.1323118067	-02 28 24.778826936						~	159	0
3	* 51 Eri	PM*	04 37 36.1326090888	-02 28 24.775726260		5.486	5.209			F0IV	229	0
4	* bet Pic	PM*	05 47 17.0876901	-51 03 59.441135	4.13	4.03	3.86	3.74	3.58	A6V	1836	1
5	* bet Pic b	Pl	05 47 17.0876901	-51 03 59.441135						~	463	1
6	CD-35 2722	**	06 09 19.2081174720	-35 49 31.065774636		12.61	11.083	10.682	9.337	M1Ve	78	0
7	CD-35 2722B	BD*	06 09 19.2082646634	-35 49 31.062882043						L0-1	61	0
8	HD 44627	Er*	06 19 12.9130449912	-58 03 15.527294208		10.01	9.205		8.185	K1V(e)	168	1
9	HD 44627B	BD*	06 19 12.9988086984	-58 03 20.198341332						L1	124	1
10	HD 95086	*	10 57 03.0215719872	-68 40 02.449216128		7.60	7.36			A8III	165	1
11	HD 95086b	Pl	10 57 03.0216129217	-68 40 02.446874288						~	93	1
12	HD 113457	*	13 05 02.0410828608	-64 26 29.702042952		6.632	6.628			A0V	51	0
13	HD 115470	*	13 18 05.1042607440	-44 03 19.380018204		6.77	6.79			B9.5V	35	0
14	HD 116434	**	13 24 36.0977360304	-51 30 16.044711840		7.08	6.98		6.87	A2V	63	0
15	HD 116434C	BD*	13 24 36.13	-51 30 16.7						L5-7	63	1
16	CD-40 8434b	Pl	14 08 10.1545137760	-41 23 52.576649494						~	154	0
17	HD 143567	*	16 01 55.4547295632	-21 58 49.398900888		7.27	7.19	7.87		B9V	125	0
18	HD 143567B	LM*	16 01 55.65696	-21 58 53.0076						M8	34	0
19	NAME Upper Sco-Cen	As*	16 15	-24.2						~	1281	1
20	HD 326277	Ro*	16 49 13.3066092624	-43 55 27.923505996		11.02	10.168		9.232	K0IV	17	0
21	V* PZ Tel	BY*	18 53 05.8735056984	-50 10 49.897437168		9.22	8.342		7.464	G9IV	321	0
22	* eta Tel	PM*	19 22 51.2060774616	-54 25 26.145617376		5.035	5.020		4.99	A0V	211	0
23	* eta Tel B	LM*	19 22 51.3580284238	-54 25 31.569876496						M7.5V	70	0
24	HD 206893	PM*	21 45 21.9052532928	-12 47 00.060804636		7.11	6.67			F5V	97	0
25	HD 218396e	Pl	23 07 28.7156905667	+21 08 03.302133882						~	189	1
26	HD 218396d	Pl	23 07 28.7156905667	+21 08 03.302133882						~	225	1
27	HD 218396c	Pl	23 07 28.7156905667	+21 08 03.302133882						~	245	1
28	HD 218396b	Pl	23 07 28.7156905667	+21 08 03.302133882						~	261	1
29	HD 218396	El*	23 07 28.7157209544	+21 08 03.310767492		6.21	5.953			F0+VkA5mA5	1082	0

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