Bibcode
Kossakowski, D.; Kürster, M.; Trifonov, T.; Henning, Th.; Kemmer, J.; Caballero, J. A.; Burn, R.; Sabotta, S.; Crouse, J. S.; Fauchez, T. J.; Nagel, E.; Kaminski, A.; Herrero, E.; Rodríguez, E.; González-Álvarez, E.; Quirrenbach, A.; Amado, P. J.; Ribas, I.; Reiners, A.; Aceituno, J.; Béjar, V. J. S.; Baroch, D.; Bastelberger, S. T.; Chaturvedi, P.; Cifuentes, C.; Dreizler, S.; Jeffers, S. V.; Kopparapu, R.; Lafarga, M.; López-González, M. J.; Martín-Ruiz, S.; Montes, D.; Morales, J. C.; Pallé, E.; Pavlov, A.; Pedraz, S.; Perdelwitz, V.; Pérez-Torres, M.; Perger, M.; Reffert, S.; Rodríguez López, C.; Schlecker, M.; Schöfer, P.; Schweitzer, A.; Shan, Y.; Shields, A.; Stock, S.; Wolf, E.; Zapatero Osorio, M. R.; Zechmeister, M.
Bibliographical reference
Astronomy and Astrophysics
Advertised on:
2
2023
Journal
Citations
14
Refereed citations
11
Description
We present the discovery of an Earth-mass planet (Mb sin i = 1.26 ± 0.21 M⊕) on a 15.6 d orbit of a relatively nearby (d ~ 9.6 pc) and low-mass (0.167 ± 0.011 M⊙) M5.0 V star, Wolf 1069. Sitting at a separation of 0.0672 ± 0.0014 au away from the host star puts Wolf 1069 b in the habitable zone (HZ), receiving an incident flux of S = 0.652 ± 0.029 S⊕. The planetary signal was detected using telluric-corrected radial-velocity (RV) data from the CARMENES spectrograph, amounting to a total of 262 spectroscopic observations covering almost four years. There are additional long-period signals in the RVs, one of which we attribute to the stellar rotation period. This is possible thanks to our photometric analysis including new, well-sampled monitoring campaigns undergone with the OSN and TJO facilities that supplement archival photometry (i.e., from MEarth and SuperWASP), and this yielded an updated rotational period range of Prot = 150-170 d, with a likely value at 169.3−3.6+3.7. The stellar activity indicators provided by the CARMENES spectra likewise demonstrate evidence for the slow rotation period, though not as accurately due to possible factors such as signal aliasing or spot evolution. Our detectability limits indicate that additional planets more massive than one Earth mass with orbital periods of less than 10 days can be ruled out, suggesting that perhaps Wolf 1069 b had a violent formation history. This planet is also the sixth closest Earth-mass planet situated in the conservative HZ, after Proxima Centauri b, GJ 1061 d, Teegarden's Star c, and GJ 1002 b and c. Despite not transiting, Wolf 1069 b is nonetheless a very promising target for future three-dimensional climate models to investigate various habitability cases as well as for sub-m s−1 RV campaigns to search for potential inner sub-Earth-mass planets in order to test planet formation theories. Full Table D.2 and additional data (i.e., stellar activity indicators as shown in Fig. 4 and long-term photometry as in Fig. 2) are only available at the CDS via anonymous ftp to cdsarc.cds.unistra.fr (ftp://130.79.128.5) or via https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/670/A84
Related projects
Exoplanets and Astrobiology
The search for life in the universe has been driven by recent discoveries of planets around other stars (known as exoplanets), becoming one of the most active fields in modern astrophysics. The growing number of new exoplanets discovered in recent years and the recent advance on the study of their atmospheres are not only providing new valuable
Enric
Pallé Bago
Very Low Mass Stars, Brown Dwarfs and Planets
Our goal is to study the processes that lead to the formation of low mass stars, brown dwarfs and planets and to characterize the physical properties of these objects in various evolutionary stages. Low mass stars and brown dwarfs are likely the most numerous type of objects in our Galaxy but due to their low intrinsic luminosity they are not so
Rafael
Rebolo López