2023A&A...671A.114J


Query : 2023A&A...671A.114J

2023A&A...671A.114J - Astronomy and Astrophysics, volume 671A, 114 (2023/3-1)

Imaging of exocomets with infrared interferometry.

JANSON M., PATEL J., RINGQVIST S.C., LU C., REBOLLIDO I., LICHTENBERG T., BRANDEKER A., ANGERHAUSEN D. and NOACK L.

Abstract (from CDS):

Active comets have been detected in several exoplanetary systems, although so far only indirectly, when the dust or gas in the extended coma has transited in front of the stellar disk. The large optical surface and relatively high temperature of an active cometary coma also makes it suitable to study with direct imaging, but the angular separation is generally too small to be reachable with present-day facilities. However, future imaging facilities with the ability to detect terrestrial planets in the habitable zones of nearby systems will also be sensitive to exocomets in such systems. Here we examine several aspects of exocomet imaging, particularly in the context of the Large Interferometer for Exoplanets (LIFE), which is a proposed space mission for infrared imaging and spectroscopy through nulling interferometry. We study what capabilities LIFE would have for acquiring imaging and spectroscopy of exocomets, based on simulations of the LIFE performance as well as statistical properties of exocomets that have recently been deduced from transit surveys. We find that for systems with extreme cometary activities such as β Pictoris, sufficiently bright comets may be so abundant that they overcrowd the LIFE inner field of view. More nearby and moderately active systems such as є Eridani or Fomalhaut may turn out to be optimal targets. If the exocomets have strong silicate emission features, such as in comet Hale-Bopp, it may become possible to study the mineralogy of individual exocometary bodies. We also discuss the possibility of exocomets as false positives for planets, with recent deep imaging of α Centauri as one hypothetical example. Such contaminants could be common, primarily among young debris disk stars, but should be rare among the main sequence population. We discuss strategies to mitigate the risk of any such false positives.

Abstract Copyright: © The Authors 2023

Journal keyword(s): infrared: planetary systems - comets: general - planets and satellites: detection

Simbad objects: 21

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Number of rows : 21
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 * 49 Cet PM* 01 34 37.7786780856 -15 40 34.898673000   5.667 5.607   5.54 A1V 303 0
2 * eps Eri b Pl 03 32 55.8444911587 -09 27 29.739493865           ~ 146 1
3 * eps Eri BY* 03 32 55.8444911587 -09 27 29.739493865 5.19 4.61 3.73 3.00 2.54 K2V 1934 1
4 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1908 1
5 * bet Pic b Pl 05 47 17.0876901 -51 03 59.441135           ~ 511 1
6 * bet Pic c Pl 05 47 17.0876901 -51 03 59.441135           ~ 62 0
7 * eta Crv PM* 12 32 04.2264018482 -16 11 45.618615379   4.658 4.294     F2V 318 0
8 NAME Proxima Centauri Er* 14 29 42.9461331854 -62 40 46.164680672 14.21 12.95 11.13 9.45 7.41 M5.5Ve 1303 0
9 NAME beta Pic Moving Group MGr 14 30 -42.0           ~ 777 0
10 * alf Cen B PM* 14 39 35.06311 -60 50 15.0992 2.89 2.21 1.33     K1V 1025 2
11 * alf Cen A SB* 14 39 36.49400 -60 50 02.3737 0.96 0.72 0.01     G2V 1280 1
12 * alf Cen ** 14 39 40.4 -60 50 20   0.4 -0.1     G2V+K1V 954 0
13 BD-07 4003 BY* 15 19 26.8269387505 -07 43 20.189497466 13.403 11.76 10.560 9.461 8.911 M3V 645 2
14 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0Va 2687 1
15 HD 172555 PM* 18 45 26.9009806435 -64 52 16.534807985   4.967 4.767     A7V 278 0
16 TYC 3134-1024-1 V* 19 22 52.9408736880 +38 41 41.489123208   10.41 9.98     ~ 17 0
17 HD 197481b Pl? 20 45 09.5324974119 -31 20 27.237889841           ~ 107 0
18 HD 197481 BY* 20 45 09.5324974119 -31 20 27.237889841   10.05 8.627 9.078 6.593 M1VeBa1 1160 0
19 HD 197481c Pl? 20 45 09.5324974119 -31 20 27.237889841           ~ 51 0
20 * alf PsA b Pl 22 57 39.04625 -29 37 20.0533           ~ 201 1
21 * alf PsA PM* 22 57 39.04625 -29 37 20.0533 1.31 1.25 1.16 1.11 1.09 A4V 1236 3

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