Astronomy:CE Antliae

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Short description: Young star in the constellation Antlia
CE Antliae
250px
VLT and MIRI observations of the disk and planet candidate around CE Antliae[1]
Observation data
Equinox J2000.0]] (ICRS)
Constellation Antlia
Right ascension  10h 42m 30.10s[2]
Declination −33° 40′ 16.2″[2]
Apparent magnitude (V) 10.91±0.07[3]
Characteristics
Evolutionary stage T Tauri star[4]
Spectral type M1[4]
Variable type rotational variable,[5] flare star[6]
Astrometry
Radial velocity (Rv)10.81±4.41[2] km/s
Proper motion (μ) RA: −118.751(23)[2] mas/yr
Dec.: −19.648(26)[2] mas/yr
Parallax (π)29.3277 ± 0.0273[2] mas
Distance111.2 ± 0.1 ly
(34.10 ± 0.03 pc)
Absolute magnitude (MV)+9.0[7]
Details
Mass0.46±0.09[8] M☉
Radius0.92±0.12[8] R☉
Luminosity0.115±0.019[8] L☉
Surface gravity (log g)4.18±0.17[8] cgs
Temperature3509±116[8] K
Rotation4.92[5] days
Rotational velocity (v sin i)63.2[5] km/s
Age6.4±1.1[9] 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.[10]

TWA 7 was discovered in 1999 with a spectral type of M1 and as a member of the TW Hydrae association.[4] 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.[6]

Planetary system

A light curve for CE Antliae, plotted from TESS data.[12] The star's rotation period is marked in red.
TWA 7 disk with Gemini South telescope

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.[13] 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.[14] An additional observation with Hubble STIS showed three rings, two spirals and a clump.[15] In 2000 dust was detected around TWA 7 due to excess of submillimeter radiation.[16] ALMA observations did however show that most emission come from a background galaxy. The disk was also detected with ALMA.[17] The disk has detected carbon monoxide (CO) gas according to 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.[18]

In 2025 JWST MIRI observations showed a point source that could be a young sub-Jovian planet with a mass of 0.3 |♃|J}}}}}} (about 100 M⊕) and a temperature of around 320 K (47 °C). The candidate can explain the main ring of the debris disk. It also does not fit the spectrum of a background star. It could be consistent with an intermediate-redshift star-forming galaxy, but the probability of such a galaxy appearing that close to TWA 7 is estimated to be 0.34%.[10] If confirmed as a planet, it would be the least massive directly imaged exoplanet.[10] The candidate is located in an underdensity in ring 2 that was noticed before. Opposite to the planet candidate is another underdensity region, which could be created by orbital resonance. The mass of the candidate was previously predicted to be 2 Neptune masses (about 34 M⊕) before it was detected.[15][10]

This candidate planet was independently detected by observations taken with the NIRCam instrument aboard JWST. The observations strongly support a planetary nature for this object, finding a background galaxy to be unlikely. The planet's mass could be similar to Neptune's. A second point-like source was also detected, but it needs follow-up observations to determine its nature.[19]

The CE Antliae planetary system[15][10]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(years) 		Eccentricity Inclination Radius
Ring 1 24.49±0.04 AU — —
b (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. ↑ "Webb captures evidence of a lightweight planet around TWA 7". 25 June 2025. https://esawebb.org/news/weic2512/. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  3. ↑ Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P. et al. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics 355. Bibcode: 2000A&A...355L..27H. 
  4. ↑ 4.0 4.1 4.2 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. doi:10.1086/311856. ISSN 0004-637X. Bibcode: 1999ApJ...512L..63W. 
  5. ↑ 5.0 5.1 5.2 Yamashita, Mai; Itoh, Yoichi; Takagi, Yuhei (November 2024). "Chromospheric Mg I emission lines of pre-main-sequence stars" (in en). Astronomy & Astrophysics 691: A304. doi:10.1051/0004-6361/202452025. ISSN 0004-6361. Bibcode: 2024A&A...691A.304Y. 
  6. ↑ 6.0 6.1 Uzawa, Akiko; Tsuboi, Yohko; Morii, Mikio; Yamazaki, Kyohei; Kawai, Nobuyuki; Matsuoka, Masaru; Nakahira, Satoshi; Serino, Motoko et al. (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. doi:10.1093/pasj/63.sp3.S713. ISSN 0004-6264. Bibcode: 2011PASJ...63S.713U. 
  7. ↑ 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. doi:10.1093/mnras/stv1981. Bibcode: 2015MNRAS.454..593B. 
  8. ↑ 8.0 8.1 8.2 8.3 8.4 Stassun, Keivan G.; Oelkers, Ryan J.; Paegert, Martin; Torres, Guillermo; Pepper, Joshua; Lee, Nathan De; Collins, Kevin; Latham, David W. et al. (2019-09-09). "The Revised TESS Input Catalog and Candidate Target List" (in en). The Astronomical Journal 158 (4): 138. doi:10.3847/1538-3881/ab3467. ISSN 0004-6256. Bibcode: 2019AJ....158..138S. 
  9. ↑ 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. doi:10.1093/mnras/staa909. Bibcode: 2020MNRAS.494.2429B. 
  10. ↑ 10.0 10.1 10.2 10.3 10.4 Lagrange, A.-M.; Wilkinson, C.; Mâlin, M.; Boccaletti, A.; Perrot, C.; Matrà, L.; Combes, F.; Rouan, D. et al. (25 June 2025). "Evidence for a sub-Jovian planet in the young TWA 7 disk". Nature 642 (8069): 905–908. doi:10.1038/s41586-025-09150-4. PMID 40562924. Bibcode: 2025Natur.642..905L. 
  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" (in en). The Astrophysical Journal 921 (1): 86. doi:10.3847/1538-4357/ac1d4c. ISSN 0004-637X. Bibcode: 2021ApJ...921...86F. 
  12. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html. 
  13. ↑ Choquet, Élodie; Perrin, Marshall D.; Chen, Christine H.; Soummer, Rémi; Pueyo, Laurent; Hagan, James B.; Gofas-Salas, Elena; Rajan, Abhijith et al. (2016). "First Images of Debris Disks around TWA 7, TWA 25, HD 35650, and HD 377". The Astrophysical Journal 817 (1): L2. doi:10.3847/2041-8205/817/1/L2. Bibcode: 2016ApJ...817L...2C. `
  14. ↑ Olofsson, J.; van Holstein, R. G.; Boccaletti, A.; Janson, M.; Thébault, P.; Gratton, R.; Lazzoni, C.; Kral, Q. et al. (September 2018). "Resolving faint structures in the debris disk around TWA 7" (in en). Astronomy & Astrophysics 617: A109. doi:10.1051/0004-6361/201832583. ISSN 0004-6361. Bibcode: 2018A&A...617A.109O. 
  15. ↑ 15.0 15.1 15.2 Ren 任, Bin 彬; Choquet, Élodie; Perrin, Marshall D.; Mawet, Dimitri; Chen, Christine H.; Milli, Julien; Debes, John H.; Rebollido, Isabel et al. (2021-06-01). "A Layered Debris Disk around M Star TWA 7 in Scattered Light" (in en). The Astrophysical Journal 914 (2): 95. doi:10.3847/1538-4357/ac03b9. ISSN 0004-637X. Bibcode: 2021ApJ...914...95R. 
  16. ↑ 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. 
  17. ↑ Bayo, A; Olofsson, J; Matrà, L; Beamín, J C; Gallardo, J; de Gregorio-Monsalvo, I; Booth, M; Zamora, C et al. (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. doi:10.1093/mnras/stz1133. ISSN 0035-8711. Bibcode: 2019MNRAS.486.5552B. 
  18. ↑ 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" (in en). The Astronomical Journal 157 (3): 117. doi:10.3847/1538-3881/aaff5b. ISSN 0004-6256. Bibcode: 2019AJ....157..117M. 
  19. ↑ Crotts, Katie A. et al. (2025). "Follow-Up Exploration of the TWA 7 Planet-Disk System with JWST NIRCam". The Astrophysical Journal Letters 987 (2): L41. doi:10.3847/2041-8213/ade798. Bibcode: 2025ApJ...987L..41C. 



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