TOI-2266 b: A keystone super-Earth at the edge of the M dwarf radius valley

被引：2

作者：

Parviainen, H. ^{[1
,2
]}

Murgas, F. ^{[1
,2
]}

Esparza-Borges, E. ^{[1
,2
]}

Pelaez-Torres, A. ^{[1
,2
]}

Palle, E. ^{[1
,2
]}

Luque, R. ^{[3
]}

Zapatero-Osorio, M. R. ^{[4
]}

Korth, J. ^{[5
]}

Fukui, A. ^{[2
,6
]}

Narita, N. ^{[2
,6
,7
]}

Collins, K. A. ^{[8
]}

Bejar, V. J. S. ^{[1
,2
]}

Morello, G. ^{[2
,9
]}

Monelli, M. ^{[1
,2
]}

Garcia, N. Abreu ^{[1
,2
]}

Chen, G. ^{[10
]}

Crouzet, N. ^{[11
]}

de Leon, J. P. ^{[12
]}

Isogai, K. ^{[12
,13
]}

Kagetani, T. ^{[12
]}

Kawauchi, K. ^{[14
]}

Klagyivik, P. ^{[15
]}

Kodama, T. ^{[6
]}

Kusakabe, N. ^{[7
,16
]}

Livingston, J. H. ^{[7
,16
,17
]}

Meni, P. ^{[1
,2
]}

Mori, M. ^{[12
]}

Nowak, G. ^{[1
,2
,18
]}

Tamura, M. ^{[7
,16
,19
]}

Terada, Y. ^{[20
,21
]}

Watanabe, N. ^{[12
]}

Ciardi, D. R. ^{[22
]}

Lund, M. B. ^{[22
]}

Christiansen, J. L. ^{[22
]}

Dressing, C. D. ^{[23
]}

Giacalone, S. ^{[23
]}

Savel, A. B. ^{[24
]}

Hirsch, L. ^{[25
]}

Parsons, S. G. ^{[26
]}

Brown, P. ^{[27
]}

Collins, K. I. ^{[28
]}

Barkaoui, K. ^{[1
,29
,30
]}

Timmermans, M. ^{[29
]}

Ghachoui, M. ^{[29
,31
]}

Soubkiou, A. ^{[31
,32
,33
]}

Benkhaldoun, Z. ^{[31
]}

Mcdermott, S. ^{[34
]}

Pritchard, T. ^{[35
]}

Rowden, P. ^{[36
]}

Striegel, S. ^{[37
,38
]}

机构：

[1] Univ La Laguna ULL, Dept Astrofis, San Cristobal la Laguna 38206, Tenerife, Spain

[2] Inst Astrofis Canarias IAC, San Cristobal la Laguna 38200, Tenerife, Spain

[3] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA

[4] CSIC, INTA, Ctr Astrobiol, Carretera Ajalvir km 4, Torrejon De Ardoz 28850, Madrid, Spain

[5] Lund Univ, Dept Phys, Div Astrophys, Lund Observ, Box 43, S-22100 Lund, Sweden

[6] Univ Tokyo, Komaba Inst Sci, 3-8-1 Komaba, Meguro, Tokyo 1538902, Japan

[7] Astrobiol Ctr, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan

[8] Ctr Astrophys Harvard & Smithsonian, 60 Garden St, Cambridge, MA 02138 USA

[9] Chalmers Univ Technol, Dept Space Earth & Environm, S-41296 Gothenburg, Sweden

[10] Chinese Acad Sci, Key Lab Planetary Sci, Purple Mt Observ, Nanjing 210023, Peoples R China

[11] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands

[12] Univ Tokyo, Grad Sch Arts & Sci, Dept Multidisciplinary Sci, 3-8-1 Komaba, Meguro, Tokyo 1538902, Japan

[13] Kyoto Univ, Okayama Observ, 3037-5 Honjo, Asakuchi, Okayama 7190232, Japan

[14] Ritsumeikan Univ, Dept Phys Sci, Kusatsu, Shiga 5258577, Japan

[15] Free Univ Berlin, Inst Geol Sci, Malteserstr 74-100, D-12249 Berlin, Germany

[16] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan

[17] Grad Univ Adv Studies, Dept Astron Sci, SOKENDAI, 2-21-1, Mitaka, Tokyo 1818588, Japan

[18] Nicolaus Copernicus Univ, Inst Astron, Fac Phys Astron & Informat, Grudziaadzka 5, PL-87100 Torun, Poland

[19] Univ Tokyo, Dept Astron, 7-3-1 Hongo,Bunkyo Ku, Tokyo 1130033, Japan

[20] Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan

[21] Natl Taiwan Univ, Dept Astrophys, Taipei 10617, Taiwan

[22] Caltech, IPAC, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA

[23] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA

[24] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

[25] Stanford Univ, Kavli Ctr Particle Astrophys & Cosmol, Stanford, CA 94305 USA

[26] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, England

[27] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA

[28] George Mason Univ, 4400 Univ Dr, Fairfax, VA 22030 USA

[29] Univ Liege, Astrobiol Res Unit, Allee 6 Aout 19C, B-4000 Liege, Belgium

[30] MIT, Dept Earth Atmospher & Planetary Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA

[31] Cadi Ayyad Univ, Fac Sci Semlalia, High Energy Phys & Astrophys Lab, Oukaimeden Observ, Marrakech, Morocco

[32] Univ Porto, Fac Ciencias, Dept Fis & Astron, Rua Campo Alegre, P-4169007 Porto, Portugal

[33] Univ Porto, Inst Astrofis & Ciencias Espaco, CAUP, Rua Estrelas, P-150762 Porto, Portugal

[34] Proto Log LLC, 1718 Euclid St NW, Washington, DC 20009 USA

[35] NASA Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA

[36] Royal Astron Soc, Burlington House, London W1J 0BQ, England

[37] SETI Inst, Mountain View, CA 94043 USA

[38] NASA Ames Res Ctr, Moffett Field, CA 94035 USA

[39] Tsinghua Univ, Dept Astron, Beijing 100084, Peoples R China

[40] Tsinghua Univ, Tsinghua Ctr Astrophys, Beijing 100084, Peoples R China

[41] Univ St Andrews, SUPA Phys & Astron, St Andrews KY16 9SS, Fife, Scotland

[42] Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA

[43] MIT, Dept Phys, Cambridge, MA 02139 USA

[44] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA

[45] Kotizarovci Observ, Sarsoni 90, Viskovo 51216, Croatia

[46] MIT, Dept Aeronaut & Astronaut, Cambridge, MA 02139 USA

[47] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA

[48] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA

[49] Univ New Mexico, Dept Phys & Astron, 1919 Lomas Blvd NE, Albuquerque, NM 87131 USA

来源：

ASTRONOMY & ASTROPHYSICS | 2024年 / 683卷

基金：

瑞典研究理事会;

关键词：

methods: statistical; techniques: photometric; planets and satellites: general; planets and satellites: terrestrial planets; stars: individual: TIC 8348911; ERROR-CORRECTION; ADAPTIVE OPTICS; I-ARCHITECTURE; PLANET RADII; LIGHT CURVES; KEPLER; STARS; VALIDATION; DEPENDENCE; ROCKY;

D O I：

10.1051/0004-6361/202347431

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We validate the Transiting Exoplanet Survey Satellite (TESS) object of interest TOI-2266.01 (TIC 8348911) as a small transiting planet (most likely a super-Earth) orbiting a faint M5 dwarf (V = 16.54) on a 2.33 d orbit. The validation is based on an approach where multicolour transit light curves are used to robustly estimate the upper limit of the transiting object's radius. Our analysis uses SPOC-pipeline TESS light curves from Sectors 24, 25, 51, and 52, simultaneous multicolour transit photometry observed with MuSCAT2, MuSCAT3' and HiPERCAM, and additional transit photometry observed with the LCOGT telescopes. TOI-2266 b is found to be a planet with a radius of 1.54 +/- 0.09 R-circle plus, which locates it at the edge of the transition zone between rocky planets, water-rich planets, and sub-Neptunes (the so-called M dwarf radius valley). The planet is amenable to ground-based radial velocity mass measurement with red-sensitive spectrographs installed in large telescopes, such as MAROON-X and Keck Planet Finder (KPF), which makes it a valuable addition to a relatively small population of planets that can be used to probe the physics of the transition zone. Further, the planet's orbital period of 2.33 days places it inside a 'keystone planet' wedge in the period-radius plane where competing planet formation scenarios make conflicting predictions on how the radius valley depends on the orbital period. This makes the planet also a welcome addition to the small population of planets that can be used to test small-planet formation scenarios around M dwarfs.

引用

页数：13

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