Delorme 1

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Delorme 1 (AB)
Delorme 1 (AB)b HST WFC3.jpg
The binary Delorme 1 (AB) is in the center and the companion is the source on the upper right.
Credit: NASA/ESA Hubble WFC3; Daniel Apai et al.
Observation data
Epoch J2000       Equinox J2000
Constellation Phoenix
Right ascension 01h 03m 35.6551s
Declination −55° 15′ 56.243″
Apparent magnitude  (V)15.40 ±0.05
Characteristics
Evolutionary stage red dwarf
Spectral type M5/6+M5/6+L0(VLG) [1]
Variable type flare star [1]
Astrometry
Radial velocity (Rv)5.2 ±1.6 [2]  km/s
Proper motion (μ)RA: 111.6 ±3.6  mas/yr [2]
Dec.: -43.8 ±8.1  mas/yr [2]
Parallax (π)21.18 ± 1.37  mas [3]
Distance 154 ± 10  ly
(47 ± 3  pc)
Details [4]
Delorme 1A
Mass 0.19 ±0.02  M☉
Delorme 1B
Mass 0.17 ±0.02  M☉
Position (relative to Delorme 1A) [4]
ComponentDelorme 1B
Epoch of observation 2012
Angular distance 0.249 ±0.003″
Projected separation 12 AU
Other designations
SCR J0103-5515, ** DLR 1AB, DENIS  J010335.6-551556, WDS J01036-5516AB, WISE  J010335.75-551556.6, 2MASS  J01033563-5515561
Database references
SIMBAD data
Exoplanet Archive data

Delorme 1 (2MASS J01033563-5515561) is a binary star with a planetary-mass companion (PMC) or protoplanet in a circumbinary orbit. [4] The PMC is notable for showing signs of accretion, despite being 30-45 Myr old, making it similar to Peter Pan disks. [1] [5] [6] These disks show characteristics of a gas-rich disk at unexpected high ages. [7]

Contents

The binary system

The star was resolved in 2013 with the Very Large Telescope NACO instrument by Delorme et al. A spectrum of the binary was taken with GMOS at Gemini South, which showed a spectral type of M5.5/M6 and strong Hydrogen-alpha emission. The astrometry showed that this star belongs to the Tucana-Horologium association. The binary is separated by around 12 astronomical units (AU). [4] In 2014 Riedel et al. found a better match with the Carina association, which has a similar age as Tuc-Hor. They also found the system to be over-luminous, which might either hint at a younger age or further multiplicity. [3] Other searches do, however, find a better match with Tuc-Hor. [2] Because the Washington Double Star Catalog named the binary ** DLR 1 after the first author of the discovery paper in 2013, Eriksson et al. suggested the name Delorme 1 for the binary. [1] The binary is named after Philippe Delorme. [8]

The circumstellar companion

The binary companion was discovered in 2013 as an object with a mass between 12 and 14 MJ and a separation of 84 AU from the central binary. It had a spectrum similar to early L-dwarfs, but redder than field L-dwarfs. [4] In 2020 Eriksson et al. discovered Hydrogen-alpha, -beta and Helium I lines from Delorme 1 (AB)b using MUSE. This is seen as a clear sign of accretion on a planetary-mass object. The spectral type of this object was determined to be L0 with very low gravity due to stronger than expected vanadium oxide absorption. [1] H-alpha can be influenced by chromospheric activity, complicating its interpretation. Betti et al. discovered Paschen and Brackett lines in Delorme 1 (AB)b in the near-infrared, using TripleSpec at SOAR. These observations are in agreement with planetary-shock accretion. [5] In 2023 Ringqvist et al. observed Delorme 1 (AB)b with the VLT UVES, detecting neutral hydrogen in the ultraviolet. [6] Both near-infrared and ultraviolet observations show an accretion rate of about (about 1.2 to 2.3 the mass of 10 Hygiea per year). [5] [6] The circumplanetary disk that fuels this accretion around Delorme 1 (AB)b is not detected (as of August 2024). [6] The planet and the star were observed with MIRI/IFU in August 2023, which should reveal any disk around the planet or star in a future work. [9]

Delorme 1 (AB)b has been called a protoplanet candidate and a super-Jupiter. [5] [6] The researchers found that the high accretion is in better agreement with a formation via disk fragmentation, hinting that it might have formed from a circumstellar disk. [5] Giant planets and brown dwarfs are thought to form via disk fragmentation in rare cases in the outer regions of a disk (r>50 AU). [10] Teasdale et al. modelled three formation scenarios in which the planet could have formed. In the first two scenarios the planet forms in a massive disk via gravitational instability. The first two scenarios produce planets that have accretion and separation comparable to the observed ones, but the resulting planets are more massive than Delorme 1 (AB)b. In a third scenario the planet forms via core accretion in a less massive disk much closer to the binary. In this third scenario the mass and accretion are similar to the observed ones, but the separation is smaller. [11]

The Delorme 1 (AB) planetary system [4] [12]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(years)		 Eccentricity Inclination Radius
b12 to 14  MJ 102+47
−27		1682+1308
−628		0.32+0.27
−0.23		127+17
−8 ° 		1.5764 [5]   RJ

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References

  1. 1 2 3 4 5 Eriksson, Simon C.; Asensio Torres, Rubén; Janson, Markus; Aoyama, Yuhiko; Marleau, Gabriel-Dominique; Bonnefoy, Mickael; Petrus, Simon (2020-06-01). "Strong Halpha emission and signs of accretion in a circumbinary planetary mass companion from MUSE". Astronomy and Astrophysics. 638: L6. arXiv: 2005.11725 . Bibcode:2020A&A...638L...6E. doi:10.1051/0004-6361/202038131. ISSN   0004-6361. S2CID   218870278.
  2. 1 2 3 4 Gagné, Jonathan; Lafrenière, David; Doyon, René; Malo, Lison; Artigau, Étienne (2015-01-01). "BANYAN. V. A Systematic All-sky Survey for New Very Late-type Low-mass Stars and Brown Dwarfs in Nearby Young Moving Groups". The Astrophysical Journal. 798 (2): 73. arXiv: 1410.4864 . Bibcode:2015ApJ...798...73G. doi:10.1088/0004-637X/798/2/73. ISSN   0004-637X.
  3. 1 2 Riedel, Adric R.; Finch, Charlie T.; Henry, Todd J.; Subasavage, John P.; Jao, Wei-Chun; Malo, Lison; Rodriguez, David R.; White, Russel J.; Gies, Douglas R.; Dieterich, Sergio B.; Winters, Jennifer G.; Davison, Cassy L.; Nelan, Edmund P.; Blunt, Sarah C.; Cruz, Kelle L. (2014-04-01). "The Solar Neighborhood. XXXIII. Parallax Results from the CTIOPI 0.9 m Program: Trigonometric Parallaxes of Nearby Low-mass Active and Young Systems". The Astronomical Journal. 147 (4): 85. arXiv: 1401.0722 . Bibcode:2014AJ....147...85R. doi:10.1088/0004-6256/147/4/85. ISSN   0004-6256.
  4. 1 2 3 4 5 6 Delorme, P.; Gagné, J.; Girard, J. H.; Lagrange, A. M.; Chauvin, G.; Naud, M. -E.; Lafrenière, D.; Doyon, R.; Riedel, A.; Bonnefoy, M.; Malo, L. (2013-05-01). "Direct-imaging discovery of a 12-14 Jupiter-mass object orbiting a young binary system of very low-mass stars". Astronomy and Astrophysics. 553: L5. arXiv: 1303.4525 . Bibcode:2013A&A...553L...5D. doi: 10.1051/0004-6361/201321169 . ISSN   0004-6361.
  5. 1 2 3 4 5 6 Betti, S. K.; Follette, K. B.; Ward-Duong, K.; Aoyama, Y.; Marleau, G. -D.; Bary, J.; Robinson, C.; Janson, M.; Balmer, W.; Chauvin, G.; Palma-Bifani, P. (2022-08-01). "Near-infrared Accretion Signatures from the Circumbinary Planetary-mass Companion Delorme 1 (AB)b". The Astrophysical Journal. 935 (1): L18. arXiv: 2208.05016 . Bibcode:2022ApJ...935L..18B. doi: 10.3847/2041-8213/ac85ef . ISSN   0004-637X.
  6. 1 2 3 4 5 Ringqvist, Simon C.; Viswanath, Gayathri; Aoyama, Yuhiko; Janson, Markus; Marleau, Gabriel-Dominique; Brandeker, Alexis (2023-01-01). "Resolved near-UV hydrogen emission lines at 40-Myr super-Jovian protoplanet Delorme 1 (AB)b. Indications of magnetospheric accretion". Astronomy and Astrophysics. 669: L12. arXiv: 2212.03207 . Bibcode:2023A&A...669L..12R. doi:10.1051/0004-6361/202245424. ISSN   0004-6361.
  7. ↑ Silverberg, Steven M.; Wisniewski, John P.; Kuchner, Marc J.; Lawson, Kellen D.; Bans, Alissa S.; Debes, John H.; Biggs, Joseph R.; Bosch, Milton K. D.; Doll, Katharina; Luca, Hugo A. Durantini; Enachioaie, Alexandru; Hamilton, Joshua; Holden, Jonathan; Hyogo, Michiharu; the Disk Detective Collaboration (2020-01-14). "Peter Pan Disks: Long-lived Accretion Disks Around Young M Stars". The Astrophysical Journal. 890 (2): 106. arXiv: 2001.05030 . Bibcode:2020ApJ...890..106S. doi: 10.3847/1538-4357/ab68e6 . S2CID   210718358.
  8. ↑ "Members of the Exoplanets team". IPAG - Institut de Planétologie et d’Astrophysique de Grenoble. Retrieved 2024-08-27.
  9. ↑ Perrin, Marshall; Balmer, William; Chen, Christine; Girard, Julien; Hoch, Kielan K. W.; Kammerer, Jens; Konopacky, Quinn; Lu, Cicero; Mountain, Matt; Pueyo, Laurent; Rebollido, Isabel; Rickman, Emily; Ruffio, Jean-Baptiste; Ward-Duong, Kimberly; Worthen, Kadin (2022-09-01). "Imaging Spectroscopy of the Coldest Imaged Exoplanet and a Low-Mass Accreting Protoplanet". JWST Proposal. Cycle 2: 2778. Bibcode:2022jwst.prop.2778P.
  10. ↑ Rice, Ken; Lopez, Eric; Forgan, Duncan; Biller, Beth (2015-12-01). "Disc fragmentation rarely forms planetary-mass objects". Monthly Notices of the Royal Astronomical Society. 454 (2): 1940–1947. arXiv: 1508.06528 . Bibcode:2015MNRAS.454.1940R. doi: 10.1093/mnras/stv1997 . ISSN   0035-8711.
  11. ↑ Teasdale, Matthew; Stamatellos, Dimitris (2024-08-01). "On the potential origin of the circumbinary planet Delorme 1 (AB)b". Monthly Notices of the Royal Astronomical Society. 533 (2): 2294–2302. arXiv: 2408.06231 . Bibcode:2024MNRAS.533.2294T. doi: 10.1093/mnras/stae1964 . ISSN   0035-8711.
  12. ↑ Blunt, Sarah; Nielsen, Eric L.; De Rosa, Robert J.; Konopacky, Quinn M.; Ryan, Dominic; Wang, Jason J.; Pueyo, Laurent; Rameau, Julien; Marois, Christian; Marchis, Franck; Macintosh, Bruce; Graham, James R.; Duchêne, Gaspard; Schneider, Adam C. (2017-05-01). "Orbits for the Impatient: A Bayesian Rejection-sampling Method for Quickly Fitting the Orbits of Long-period Exoplanets". The Astronomical Journal. 153 (5): 229. arXiv: 1703.10653 . Bibcode:2017AJ....153..229B. doi: 10.3847/1538-3881/aa6930 . ISSN   0004-6256. 68 % confidence range
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