Table · dataset · 2024
AU Mic radial velocity curves
Listed in IVOA Registry (Virtual Observatory)
Understanding planet formation is important in the context of the origin of planetary systems in general and of the Solar System in particular, as well as to predict the likelihood of finding Jupiter, Neptune, and Earth analogues around other stars.
Description
We aim to precisely determine the radii and dynamical masses of transiting planets orbiting the young M star AUMic using public photometric and spectroscopic datasets. We performed a joint fit analysis of the TESS and CHEOPS light curves and more than 400 high-resolution spectra collected with several telescopes and instruments.
We characterise the stellar activity and physical properties (radius, mass, density) of the transiting planets in the young AUMic system through joint transit and radial velocity fits with Gaussian processes. We determine a radius of R^b^_p_=4.79+/-0.29R_{Earth}_, a mass of M^b^_p_=9.0+/-2.7M_{Earth}_, and a bulk density of {rho}^b^_p_=0.49+/-0.16g/cm^3^ for the innermost transiting planet AUMic b. For the second known transiting planet, AUMic c, we infer a radius of R^c^_p_=2.79+/-0.18R_{Earth}_ , a mass of M^c^_p__=14.5+/-3.4M_{Earth}_ , and a bulk density of {rho}^c^_p_=3.90+/-1.17g/cm^3^.
Read the rest (2 more)
According to theoretical models, AUMic b may harbour an H2 envelope larger than 5% by mass, with a fraction of rock and a fraction of water. AUMic c could be made of rock and/or water and may have an H2 atmosphere comprising at most 5% of its mass. AUMic b has retained most of its atmosphere but might lose it over tens of millions of years due to the strong stellar radiation, while AUMic c likely suers much less photo-evaporation because it lies at a larger separation from its host.
Using all the datasets in hand, we determine a 3 upper mass limit of M^[d]^_p_sini=8.6M_{Earth}_ for the AUMic 'd' TTV-candidate. In addition, we do not confirm the recently proposed existence of the planet candidate AUMic 'e' with an orbital period of 33.4 days.We investigated the level of the radial velocity variations and show that it is lower at longer wavelength with smaller changes from one observational campaign to another.
Links
Where it is published
- Reference page cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/689/A132 ↗
landing page · from IVOA Registry
Documentation and papers
- ADS 2024A&A...689A.132M ui.adsabs.harvard.edu/abs/2024A%26A...689A.132M ↗
publication · from IVOA Registry
Catalogue records · 2
- VOResource record dc.g-vo.org/oai.xml?verb=GetRecord&metadataPrefix=ivo_vor&identifier=ivo%3… ↗
metadata API · from IVOA Registry
- Registry record (GAVO) dc.g-vo.org/I/cds.vizier/j/a%2Ba/689/a132 ↗
catalogue entry · from IVOA Registry
Topics
- From keywords
- Astronomy & Astrophysics
Provenance · 1 source records, 9 field assertions
| Source | Key | Last seen | Raw |
|---|---|---|---|
| IVOA Registry (Virtual Observatory) | ivo://cds.vizier/j/a+a/689/a132 | 12 d ago | JSON v1 |
| Field | Assertion | Extractor | Evidence |
|---|---|---|---|
| access_level | source · IVOA Registry | connector:ivoa_registry@1.0.0 | |
| concepts[field].local:field:astronomy | mapping · IVOA Registry | connector:ivoa_registry@1.0.0 | |
| concepts[modality].ivoa_waveband:infrared | source · IVOA Registry | connector:ivoa_registry@1.0.0 | |
| concepts[modality].ivoa_waveband:optical | source · IVOA Registry | connector:ivoa_registry@1.0.0 | |
| description | source · IVOA Registry | connector:ivoa_registry@1.0.0 | rr.resource.res_description |
| license_text | source · IVOA Registry | connector:ivoa_registry@1.0.0 | |
| publication_date | source · IVOA Registry | connector:ivoa_registry@1.0.0 | |
| title | source · IVOA Registry | connector:ivoa_registry@1.0.0 | rr.resource.res_title |
| updated_date | source · IVOA Registry | connector:ivoa_registry@1.0.0 |