2012A&A...537A..67B


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.02CET06:37:35

2012A&A...537A..67B - Astronomy and Astrophysics, volume 537A, 67-67 (2012/1-1)

MESS (multi-purpose exoplanet simulation system). A Monte Carlo tool for the statistical analysis and prediction of exoplanet search results.

BONAVITA M., CHAUVIN G., DESIDERA S., GRATTON R., JANSON M., BEUZIT J.L., KASPER M. and MORDASINI C.

Abstract (from CDS):

The high number of planet discoveries made in the last years provides a good sample for statistical analysis, leading to some clues on the distributions of planet parameters, such as masses and periods, at least in close proximity to the host star. We likely need to wait for the extremely large telescopes (ELTs) to have an overall view of the extrasolar planetary systems. Those facilities will finally ensure an overlap of the discovery space of direct and indirect techniques, which is desirable to completely understand the nature of the discovered objects, obtaining both orbital parameters and physical characterization. In this context it would be useful to have a tool that can be used for the interpretation of the present results that are obtained with various observing techniques, and also to predict what the outcomes would be of the future instruments. For this reason we built MESS: a Monte Carlo simulation code that uses either the results of the statistical analysis of the properties of discovered planets or the results of the planet formation theories to build synthetic planet populations that are fully described in terms of frequency, orbital elements and physical properties. These synthetic planets can then be used to either test the consistency of their properties with the observed ones given different detection techniques (radial velocity, imaging and astrometry) or to predict the expected number of planets for future surveys, as well as to optimize the future multi-technique observations for their characterization down to telluric masses. In addition to the code description, we present here some of its applications to probe the physical and orbital properties of a putative companion within the circumstellar disk of a given star and to test or constrain the orbital distribution properties of a potential planet population around the members of the TW Hydrae association. Finally, we investigated the synergy of future space and ground-based telescopes instrumentation with the predictive mode of the code, to identify the mass-period parameter space that will be probed in future surveys for giant and rocky planets.

Abstract Copyright:

Journal keyword(s): brown dwarfs - methods: statistical - methods: data analysis - planetary systems

VizieR on-line data: <Available at CDS (J/A+A/537/A67): list.dat prog/*>

Simbad objects: 11

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Number of rows : 11

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 * 41 Ari ** 02 49 59.0332406 +27 15 37.826018   3.498 3.594     B8Vn 152 0
2 EM* LkCa 15 Or* 04 39 17.7912813350 +22 21 03.387667491   13.01 12.03 11.61   K5:Ve 580 1
3 TWA 22 LXB 10 17 26.8983656044 -53 54 26.459439803   15.69 13.96 13.72   M5 71 0
4 NAME TW Hya Association As* 11 01.9 -34 42           ~ 839 0
5 V* V1215 Cen TT* 11 13 26.2208332352 -45 23 42.719174706     12.478   10.483 K8IVe 70 0
6 V* V1217 Cen BY* 11 21 05.4812165874 -38 45 16.521880972   14.04 12.58 12.34 10.515 M1Ve 65 0
7 HD 102458 Y*O 11 47 24.5436617458 -49 53 03.018055867   9.70 9.07   8.40 G4V 81 0
8 TWA 23 TT* 12 07 27.3753633293 -32 47 00.253618251   14.157 12.7     M2.5Ve 58 0
9 V* V1249 Cen TT* 12 15 30.7203284919 -39 48 42.605543199   13.09 11.160 10.919 9.50 M0.5 88 0
10 HD 109573 PM* 12 36 01.0317721349 -39 52 10.222698506   5.786 5.774 7.25 5.81 A0V 564 1
11 V* V1267 Cen TT* 13 20 45.3877589173 -46 11 37.712461035   14.0 12.7   10.78 K5IVe 38 0

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2021.03.02-06:37:35

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