CE Antliae

In today's world, CE Antliae has been the subject of increasing interest and debate in various areas. Since its inception, CE Antliae has captured the attention of experts, academics, researchers and the general public, generating a series of discussions and reflections on its impact, relevance and possible implications. The different approaches and perspectives regarding CE Antliae have given rise to an extensive body of knowledge and information that ranges from historical and cultural aspects to scientific and technological issues. In this sense, this article seeks to offer a comprehensive and multidisciplinary vision of CE Antliae, addressing various aspects and approaches that allow us to deepen its understanding and meaning today.

CE Antliae

TWA 7 disk with Gemini South telescope
Observation data
Epoch J2000      Equinox J2000
Constellation Antlia
Right ascension 10h 42m 30.10s[1]
Declination −33° 40′ 16.2″[1]
Apparent magnitude (V) 10.91±0.07[2]
Characteristics
Evolutionary stage T Tauri star[3]
Spectral type M1[3]
Variable type rotational variable,[4] flare star[5]
Astrometry
Radial velocity (Rv)10.81±4.41[1] km/s
Proper motion (μ) RA: −118.751±0.023 mas/yr[1]
Dec.: −19.648±0.026 mas/yr[1]
Parallax (π)29.3277±0.0273 mas[1]
Distance111.2 ± 0.1 ly
(34.10 ± 0.03 pc)
Absolute magnitude (MV)+9.0[6]
Details
Mass0.460±0.086[7] M☉
Radius0.917±0.119[7] R☉
Luminosity0.11490±0.01903[7] L☉
Surface gravity (log g)4.1759±0.1743[7] cgs
Temperature3509.0±115.7[7] K
Rotation4.92[4] days
Rotational velocity (v sin i)63.2[4] km/s
Age6.4±1.1[8] Myr
Other designations
TWA 7, CE Ant, TYC 7190-2111-1, ASAS J104230-3340.3, GSC 07190-02111, 2MASS J10423011-3340162, RX J104230.3-334014, TIC 54147487, WISE J104230.01-334016.4, Gaia DR2 5444751795151480320
Database references
SIMBADdata

CE Antliae (also called TWA 7) is a young low-mass star in the constellation of Antlia. It is surrounded by a debris disk and has one directly imaged planet candidate.[9]

A light curve for CE Antliae, plotted from TESS data.[10] The star's rotation period is marked in red.

TWA 7 was discovered in 1999 with a spectral type of M1 and as a member of the TW Hydrae association.[3] The detection of molecular hydrogen is interpreted as a weak sign of accretion of gas near the star.[11] A giant x-ray flare was detected on 2010-09-07 with MAXI/GSC on the ISS.[5]

Planetary system

The disk was first imaged in scattered light in 1998 with Hubble NICMOS, but it needed a re-processing in 2016 to reveal the disk. The observation showed a pole-on dust ring with a radius of about 35 astronomical units.[12] An outer ring and a spiral arm originating from the main ring was tentatively detected with VLT/SPHERE in 2018. The modelling also showed evidence of an inner ring.[13] An additional observation with Hubble STIS showed three rings, two spirals and a clump.[14] In 2000 dust was detected around TWA 7 due to excess submillimeter radiation.[15] ALMA observations did however show that most emission come from a background galaxy. The disk was also detected with ALMA.[16] The disk has detected carbon monoxide (CO) gas from ALMA observations, which is likely generated by exocomets. It was the first detection of CO gas in a debris disk around an M-dwarf. This kind of detection is more common around more massive stars.[17]

In 2025 JWST MIRI observations showed a point source that could be a young sub-Jovian planet with a mass of 0.3 MJ (about 100 ME) and a temperature of around 320 Kelvin. The candidate can explain the main ring of the debris disk. It also does not fit the spectrum of a background star or galaxy. If confirmed, it would be the least massive directly imaged exoplanet.[9] The candidate is located in an underdensity in ring 2 that was noticed before. Opposite to the planet candidate is another underdensity, which could be created by orbital resonance. The mass of the candidate was previously predicted to be 2 Neptune masses (about 34 ME) before it was detected.[14][9]

The CE Antlae planetary system[14][9]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(years) 		Eccentricity Inclination Radius
Ring 1 24.49±0.04 AU — —
CC#1 (candidate) 0.3 MJ 52 550 — — —
Ring 2 52.38±0.12 AU — —
Ring 3 101+2
−3 AU 		— —

See also

Other M dwarfs with debris disks

References

  1. ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  2. ^ Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355. Bibcode:2000A&A...355L..27H.
  3. ^ a b c Webb, R. A.; Zuckerman, B.; Platais, I.; Patience, J.; White, R. J.; Schwartz, M. J.; McCarthy, C. (1999-02-01). "Discovery of Seven T Tauri Stars and a Brown Dwarf Candidatein the Nearby TW Hydrae Association". The Astrophysical Journal. 512 (1): L63 – L67. arXiv:astro-ph/9812189. Bibcode:1999ApJ...512L..63W. doi:10.1086/311856. ISSN 0004-637X.
  4. ^ a b c Yamashita, Mai; Itoh, Yoichi; Takagi, Yuhei (November 2024). "Chromospheric Mg I emission lines of pre-main-sequence stars". Astronomy & Astrophysics. 691: A304. arXiv:2410.03087. Bibcode:2024A&A...691A.304Y. doi:10.1051/0004-6361/202452025. ISSN 0004-6361.
  5. ^ a b Uzawa, Akiko; Tsuboi, Yohko; Morii, Mikio; Yamazaki, Kyohei; Kawai, Nobuyuki; Matsuoka, Masaru; Nakahira, Satoshi; Serino, Motoko; Matsumura, Takanori; Mihara, Tatehiro; Tomida, Hiroshi; Ueda, Yoshihiro; Sugizaki, Mutsumi; Ueno, Shiro; Daikyuji, Arata (2011-11-25). "A Large X-Ray Flare from a Single Weak-Lined T Tauri Star TWA-7 Detected with MAXI GSC". Publications of the Astronomical Society of Japan. 63 (sp3): S713 – S716. arXiv:1108.5897. Bibcode:2011PASJ...63S.713U. doi:10.1093/pasj/63.sp3.S713. ISSN 0004-6264.
  6. ^ Bell, Cameron P. M.; Mamajek, Eric E.; Naylor, Tim (2015). "A self-consistent, absolute isochronal age scale for young moving groups in the solar neighbourhood". Monthly Notices of the Royal Astronomical Society. 454 (1): 593. arXiv:1508.05955. Bibcode:2015MNRAS.454..593B. doi:10.1093/mnras/stv1981.
  7. ^ a b c d e Stassun, Keivan G.; Oelkers, Ryan J.; Paegert, Martin; Torres, Guillermo; Pepper, Joshua; Lee, Nathan De; Collins, Kevin; Latham, David W.; Muirhead, Philip S.; Chittidi, Jay; Rojas-Ayala, Bárbara; Fleming, Scott W.; Rose, Mark E.; Tenenbaum, Peter; Ting, Eric B. (2019-09-09). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal. 158 (4): 138. arXiv:1905.10694. Bibcode:2019AJ....158..138S. doi:10.3847/1538-3881/ab3467. ISSN 0004-6256.
  8. ^ Binks, A. S.; Jeffries, R. D.; Wright, N. J. (2020). "A kinematically hot population of young stars in the solar neighbourhood". Monthly Notices of the Royal Astronomical Society. 494 (2): 2429. arXiv:2003.13369. Bibcode:2020MNRAS.494.2429B. doi:10.1093/mnras/staa909.
  9. ^ a b c d Lagrange, A.-M.; Wilkinson, C.; Mâlin, M.; Boccaletti, A.; Perrot, C.; Matrà, L.; Combes, F.; Rouan, D.; Beust, H. (2025-02-20). "Evidence for a sub-jovian planet in the young TWA7 disk". arXiv:2502.15081 .
  10. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 24 February 2025.
  11. ^ Flagg, Laura; Johns-Krull, Christopher M.; France, Kevin; Herczeg, Gregory; Najita, Joan; Carpenter, John M.; Kenyon, Scott J. (2021-11-01). "Detection of H2 in the TWA 7 System: A Probable Circumstellar Origin". The Astrophysical Journal. 921 (1): 86. arXiv:2108.08327. Bibcode:2021ApJ...921...86F. doi:10.3847/1538-4357/ac1d4c. ISSN 0004-637X.
  12. ^ Choquet, Élodie; Perrin, Marshall D.; Chen, Christine H.; Soummer, Rémi; Pueyo, Laurent; Hagan, James B.; Gofas-Salas, Elena; Rajan, Abhijith; Golimowski, David A.; Hines, Dean C.; Schneider, Glenn; Mazoyer, Johan; Augereau, Jean-Charles; Debes, John; Stark, Christopher C.; Wolff, Schuyler; n'Diaye, Mamadou; Hsiao, Kevin (2016). "First Images of Debris Disks around TWA 7, TWA 25, HD 35650, and HD 377". The Astrophysical Journal. 817 (1): L2. arXiv:1512.02220. Bibcode:2016ApJ...817L...2C. doi:10.3847/2041-8205/817/1/L2.`
  13. ^ Olofsson, J.; van Holstein, R. G.; Boccaletti, A.; Janson, M.; Thébault, P.; Gratton, R.; Lazzoni, C.; Kral, Q.; Bayo, A.; Canovas, H.; Caceres, C.; Ginski, C.; Pinte, C.; Asensio-Torres, R.; Chauvin, G. (September 2018). "Resolving faint structures in the debris disk around TWA 7". Astronomy & Astrophysics. 617: A109. arXiv:1804.01929. Bibcode:2018A&A...617A.109O. doi:10.1051/0004-6361/201832583. ISSN 0004-6361.
  14. ^ a b c Ren 任, Bin 彬; Choquet, Élodie; Perrin, Marshall D.; Mawet, Dimitri; Chen, Christine H.; Milli, Julien; Debes, John H.; Rebollido, Isabel; Stark, Christopher C.; Hagan, J. Brendan; Hines, Dean C.; Millar-Blanchaer, Maxwell A.; Pueyo, Laurent; Roberge, Aki; Schneider, Glenn (2021-06-01). "A Layered Debris Disk around M Star TWA 7 in Scattered Light". The Astrophysical Journal. 914 (2): 95. arXiv:2105.09949. Bibcode:2021ApJ...914...95R. doi:10.3847/1538-4357/ac03b9. ISSN 0004-637X.
  15. ^ Webb, R. A.; Zuckerman, B.; Greaves, J. S.; Holland, W. S. (December 2000). "Large, cold dust grains orbiting stars in the TW Hydrae Association". American Astronomical Society, 197th AAS Meeting, Id.08.27. 32: 1410. Bibcode:2000AAS...197.0827W.
  16. ^ Bayo, A; Olofsson, J; Matrà, L; Beamín, J C; Gallardo, J; de Gregorio-Monsalvo, I; Booth, M; Zamora, C; Iglesias, D; Henning, Th; Schreiber, M R; Cáceres, C (July 2019). "Sub-millimetre non-contaminated detection of the disc around TWA 7 by ALMA". Monthly Notices of the Royal Astronomical Society. 486 (4): 5552–5557. arXiv:1806.09252. Bibcode:2019MNRAS.486.5552B. doi:10.1093/mnras/stz1133. ISSN 0035-8711.
  17. ^ Matrà, L.; Öberg, K. I.; Wilner, D. J.; Olofsson, J.; Bayo, A. (2019-02-14). "On the Ubiquity and Stellar Luminosity Dependence of Exocometary CO Gas: Detection around M Dwarf TWA 7". The Astronomical Journal. 157 (3): 117. arXiv:1901.05004. Bibcode:2019AJ....157..117M. doi:10.3847/1538-3881/aaff5b. ISSN 0004-6256.