2018A&A...609A...4K


Query : 2018A&A...609A...4K

2018A&A...609A...4K - Astronomy and Astrophysics, volume 609A, 4-4 (2018/1-1)

Simulating the exoplanet yield of a space-based mid-infrared interferometer based on Kepler statistics.

KAMMERER J. and QUANZ S.P.

Abstract (from CDS):

Aims. We predict the exoplanet yield of a space-based mid-infrared nulling interferometer using Monte Carlo simulations. We quantify the number and properties of detectable exoplanets and identify those target stars that have the highest or most complete detection rate. We investigate how changes in the underlying technical assumptions and uncertainties in the underlying planet population impact the scientific return.
Methods. We simulated 2000 exoplanetary systems, based on planet occurrence statistics from Kepler with randomly orientated orbits and uniformly distributed albedos around each of 326 nearby (d<20pc) stars. Assuming thermal equilibrium and blackbody emission, together with the limiting spatial resolution and sensitivity of our simulated instrument in the three specific bands 5.6, 10.0, and 15.0µm, we quantified the number of detectable exoplanets as a function of their radii and equilibrium temperatures.
Results. Approximately 315–77+113 exoplanets, with radii 0.5REarth≤Rp≤6REarth, were detected in at least one band and half were detected in all three bands during ∼0.52 years of mission time assuming throughputs 3.5 times worse than those for the James Webb Space Telescope and ∼40% overheads. Accounting for stellar leakage and (unknown) exozodiacal light, the discovery phase of the mission very likely requires 2-3 years in total. The uncertainties in planet yield are dominated by uncertainties in the underlying planet population, but the distribution of the Bond albedos also has a significant impact. Roughly 50% of the detected planets orbit M stars, which also have the highest planet yield per star; the other 50% orbit FGK stars, which show a higher completeness in the detectability. Roughly 85 planets could be habitable (0.5REarth≤Rp≤1.75REarth and 200K≤Teq≤450K) and are prime targets for spectroscopic observations in a second mission phase. Comparing these results to those of a large optical/near-infrared telescope, we find that a mid-infrared interferometer would detect more planets and the number of planets depends less strongly on the wavelength.
Conclusions. An optimized space-based nulling interferometer operating in the mid-infrared would deliver an unprecedented dataset for the characterization of (small) nearby exoplanets including dozens of potentially habitable worlds.

Abstract Copyright: © ESO, 2017

Journal keyword(s): planets and satellites: detection - planets and satellites: terrestrial planets - instrumentation: high angular resolution - instrumentation: interferometers - methods: numerical

Simbad objects: 20

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Number of rows : 20
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 HD 225213 Er* 00 05 24.4284351777 -37 21 26.507931505 11.074 10.022 8.562 7.589 6.432 M2V 198 0
2 V* GX And Er* 00 18 22.8849799680 +44 01 22.637951588   10.120   7.3   M2V 506 0
3 * zet Tuc PM* 00 20 04.2586334956 -64 52 29.257190108 4.82 4.80 4.23 3.73 3.40 F9.5V 364 0
4 * eta Cas PM* 00 49 06.2945942922 +57 48 54.638239716 4.04 4.02 3.44 2.94 2.58 F9V 621 0
5 * alf CMa SB* 06 45 08.91728 -16 42 58.0171 -1.51 -1.46 -1.46 -1.46 -1.43 A0mA1Va 1484 0
6 * alf CMi SB* 07 39 18.11950 +05 13 29.9552 0.82 0.79 0.37 -0.05 -0.28 F5IV-V+DQZ 1829 0
7 HD 79210 SB* 09 14 22.7748624830 +52 41 11.791503353   9.388   6.8   K7V 288 0
8 HD 95735 Er* 11 03 20.1948195942 +35 58 11.576182057 10.030 8.960 7.520 5.99 4.79 M2+V 679 0
9 HD 119850 Er* 13 45 43.7755597223 +14 53 29.471707437 10.989 9.894 8.50 7.465 6.363 M2V 325 0
10 * alf Cen B PM* 14 39 35.06311 -60 50 15.0992 2.89 2.21 1.33     K1V 976 1
11 * alf Cen A SB* 14 39 36.49400 -60 50 02.3737 0.96 0.72 0.01     G2V 1220 0
12 BD-12 4523 BY* 16 30 18.0583947383 -12 39 45.321217732 12.829 11.638 10.072 8.917 7.421 M3V 291 0
13 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0Va 2615 0
14 HD 173739 PM* 18 42 46.7043860406 +59 37 49.409446059   10.782   8.1   M3V 360 1
15 * alf Aql dS* 19 50 46.99855 +08 52 05.9563 1.07 0.98 0.76 0.62 0.49 A7Vn 856 0
16 * del Pav PM* 20 08 43.6088716052 -66 10 55.442769229 4.78 4.32 3.56 2.95 2.61 G8IV 372 0
17 HD 191849 PM* 20 13 53.3962498530 -45 09 50.470550834 10.627 9.419 7.966 7.053 6.124 M0V 156 0
18 HD 204961 PM* 21 33 33.9751191976 -49 00 32.399427028 11.359 10.176 8.672 7.665 6.479 M2/3V 253 1
19 * alf PsA ** 22 57 39.04625 -29 37 20.0533 1.31 1.25 1.16 1.11 1.09 A4V 1189 3
20 HD 217987 PM* 23 05 52.0357857091 -35 51 11.055185039   8.83 7.39     M2V 250 0

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2022.12.07-04:15:14

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