Issue |
A&A
Volume 677, September 2023
|
|
---|---|---|
Article Number | A182 | |
Number of page(s) | 28 | |
Section | Planets and planetary systems | |
DOI | https://doi.org/10.1051/0004-6361/202346692 | |
Published online | 27 September 2023 |
Two super-Earths at the edge of the habitable zone of the nearby M dwarf TOI-2095★
1
Instituto de Astrofisica de Canarias (IAC),
38205
La Laguna, Tenerife, Spain
e-mail: fmurgas@iac.es
2
Departamento de Astrofisica, Universidad de La Laguna (ULL),
38206
La Laguna, Tenerife, Spain
3
Centro de Astrobiologia (CSIC-INTA),
ESAC campus,
28692
Villanueva de la Canada (Madrid), Spain
4
NASA Exoplanet Science Institute-Caltech/IPAC,
Pasadena, CA
91125, USA
5
University of California Santa Cruz,
Santa Cruz, CA
95065, USA
6
Sternberg Astronomical Institute, M.V. Lomonosov Moscow State University,
13, Universitetskij pr.,
119234
Moscow, Russia
7
Center for Astrophysics | Harvard & Smithsonian,
60 Garden Street,
Cambridge, MA
02138, USA
8
Department of Astronomy and Tsinghua Centre for Astrophysics, Tsinghua University,
Beijing
100084, PR China
9
Campo Catino Astronomical Observatory,
Regione Lazio, Guarcino (FR)
03010, Italy
10
Lund Observatory, Division of Astrophysics, Department of Physics, Lund University,
PO Box 43,
22100
Lund, Sweden
11
Komaba Institute for Science, The University of Tokyo,
3-8-1 Komaba, Meguro,
Tokyo
153-8902, Japan
12
Astrobiology Center,
2-21-1 Osawa, Mitaka,
Tokyo
181-8588, Japan
13
Department of Multi-Disciplinary Sciences, Graduate School of Arts and Sciences, The University of Tokyo,
3-8-1 Komaba, Meguro,
Tokyo
153-8902, Japan
14
Instituto de Astrofisica de Andalucia (IAA-CSIC),
Glorieta de la Astronomia s/n,
18008
Granada, Spain
15
Max-Planck-Institut für Astronomie,
Königstuhl 17,
69117
Heidelberg, Germany
16
Department of Astronomy and Astrophysics, University of Chicago,
Chicago, IL
60637, USA
17
Landessternwarte, Zentrum für Astronomie der Universität Heidelberg,
Königstuhl 12,
69117
Heidelberg, Germany
18
Institut für Astrophysik und Geophysik, Georg-August-Universität,
Friedrich-Hund-Platz 1,
37077
Göttingen, Germany
19
Institut de Ciències de l’Espai (CSIC),
Campus UAB, c/ de Can Magrans s/n,
08193
Bellaterra, Barcelona, Spain
20
Institut d’Estudis Espacials de Catalunya,
08034
Barcelona, Spain
21
Hamburger Sternwarte, Universität Hamburg,
Gojenbergsweg 112,
21029
Hamburg, Germany
22
Department of Physics and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology,
Cambridge, MA
02139, USA
23
Steward Observatory and Department of Astronomy, The University of Arizona,
Tucson, AZ
85721, USA
24
Vereniging Voor Sterrenkunde (VVS),
Oostmeers 122 C,
8000
Brugge, Belgium
25
Centre for Mathematical Plasma-Astrophysics, Department of Mathematics, KU Leuven,
Celestijnenlaan 200B,
3001
Heverlee, Belgium
26
Public Observatory ASTROLAB IRIS, Provinciaal Domein “De Palingbeek”,
Verbrandemolenstraat 5,
8902
Zillebeke, Ieper, Belgium
27
Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology,
Cambridge, MA
02139, USA
28
Department of Aeronautics and Astronautics, Massachusetts Institute of Technology,
Cambridge, MA
02139, USA
29
NASA Ames Research Center,
Moffett Field, CA
94035, USA
30
Department of Astrophysical Sciences, Princeton University,
Princeton, NJ
08544, USA
31
Department of Space, Earth and Environment, Chalmers University of Technology,
412 96
Gothenburg, Sweden
Received:
18
April
2023
Accepted:
26
July
2023
The main scientific goal of TESS is to find planets smaller than Neptune around stars that are bright enough to allow for further characterization studies. Given our current instrumentation and detection biases, M dwarfs are prime targets in the search for small planets that are in (or near) the habitable zone of their host star. In this work, we use photometric observations and CARMENES radial velocity (RV) measurements to validate a pair of transiting planet candidates found by TESS. The data were fitted simultaneously, using a Bayesian Markov chain Monte Carlo (MCMC) procedure and taking into account the stellar variability present in the photometric and spectroscopic time series. We confirm the planetary origin of the two transiting candidates orbiting around TOI-2095 (LSPM J1902+7525). The star is a nearby M dwarf (d = 41.90 ± 0.03 pc, Teff = 3759 ± 87 K, V = 12.6 mag), with a stellar mass and radius of M* = 0.44 ± 0.02 M⊙ and R* = 0.44 ± 0.02 R⊙, respectively. The planetary system is composed of two transiting planets: TOI-2095b, with an orbital period of Pb = 17.66484 ± (7 × 10−5) days, and TOI-2095c, with Pc = 28.17232 ± (14 × 10−5) days. Both planets have similar sizes with Rb = 1.25 ± 0.07 R⊕ and Rc = 1.33 ± 0.08 R⊕ for planet b and planet c, respectively. Although we did not detect the induced RV variations of any planet with significance, our CARMENES data allow us to set stringent upper limits on the masses of these objects. We find Mb < 4.1 M⊕ for the inner and Mc < 7.4 M⊕ for the outer planet (95% confidence level). These two planets present equilibrium temperatures in the range of 300–350 K and are close to the inner edge of the habitable zone of their star.
Key words: planets and satellites: detection / techniques: photometric / techniques: radial velocities
Radial velocity measurement table is available at the CDS via anonymous ftp to cdsarc.cds.unistra.fr (130.79.128.5) or via https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/677/A182
© The Authors 2023
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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