SIMP J013656.5+093347 (abbreviated SIMP0136) is a planetary mass object[4] at 19.9 light-years from Earth in the constellation Pisces. It belongs to the spectral class T2.5[1] and its position shifts due to its proper motion annually by about 1.24 arcsec in the right ascension.[3]
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Pisces |
| Right ascension | 01h 36m 57s |
| Declination | +09° 33′ 47.3″ |
| Characteristics | |
| Spectral type | T2.5[1] |
| Apparent magnitude (i) | 20.42 ± 0.06 |
| Apparent magnitude (z) | 16.01 ± 0.02 |
| Apparent magnitude (J) | 13.455 ± 0.030 |
| Apparent magnitude (H) | 12.771 ± 0.032 |
| Apparent magnitude (K) | 12.562 ± 0.024 |
| Astrometry | |
| Radial velocity (Rv) | 12.3 ± 0.8[2] km/s |
| Proper motion (μ) | RA: 1238.244 ± 0.554[3] mas/yr Dec.: -16.156 ± 0.328[3] mas/yr |
| Parallax (π) | 163.4478 ± 0.4629 mas[3] |
| Distance | 19.95 ± 0.06 ly (6.12 ± 0.02 pc) |
| Details | |
| Mass | 12.7 ± 1.0[4] MJup |
| Radius | 1.22 ± 0.01[4] RJup |
| Surface gravity (log g) | 4.31 ± 0.03[4] cgs |
| Temperature | 1098 ± 6[4] K |
| Rotation | 2.406 ± 0.008[5] hours |
| Rotational velocity (v sin i) | 52.8+1.1 −1.0[2] km/s |
| Age | 200 ± 50[4] Myr |
| Other designations | |
2MASS J01365662+0933473; IPMS J013656.57+093347.3; IBIS J013656.57+093347.3 | |
| Database references | |
| SIMBAD | data |
  SIMP0136 Location of SIMP0136 in the constellation Pisces | |
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Physical properties
editIn 2017, it was announced that the object's mass may be as low as 12.7 Jupiter masses and might be considered a rogue planet rather than a brown dwarf as it seems to be a member of the relatively young, 200 million-year-old Carina-Near stellar moving group.[4][6][7]
In 2018, astronomers noted, "Detecting SIMP J01365663+0933473 with the VLA through its auroral radio emission, also means that we may have a new way of detecting exoplanets, including the elusive rogue ones not orbiting a parent star ... This particular object is exciting because studying its magnetic dynamo mechanisms can give us new insights on how the same type of mechanisms can operate in extrasolar planets - planets beyond our Solar System ... We think these mechanisms can work not only in brown dwarfs, but also in both gas giant and terrestrial planets."[7] During the observation with the VLA only one pulse was detected for SIMP0136. The magnetic flux of SIMP0136 was estimated to be 3.2 kG.[8]
In 2017 the rotational velocity and radial velocity was measured. It was found that we see SIMP0136 almost equator-on with an inclination of 80 ±12°.[2]
Weather and clouds
editThis brown dwarf provided the first evidence for periodic variability flux variations among T dwarfs. A team observed this object with the 1.8-m Perkins Telescope Observatory near Flagstaff, Arizona in 2015. SIMP0136 was observed in 15 nights, spread out over 90 days. The variation has been interpreted as a signature of weather patterns coming in and out of view over the object's 2.4h rotation period. The shape of this lightcurve evolves over timescales of days, which has been interpreted as a sign of evolution of the cloud patterns in its atmosphere.[5] In 2016 a phase shift between Spitzer and Hubble observations was noticed, which was measured to be 33.4 ±3.9°.[9] In 2023 a team found that SIMP0136 has patchy forsterite (Mg2SiO4) clouds above an iron cloud deck. This patchy cloud layer covers between 69% and 72% of the surface of the object.[10] In 2024 a team re-analysed the 2015 data and detected a phase shift between the J-band and Ks-band of 39.9+3.6
−1.1°. The team concluded that the phase shift can be explained with at least two different patchy cloud layers. The J- and Ks-bands both probe different layers of the atmosphere.[11]
See also
editOther planetary-mass objects:
Other T-dwarfs with detected radio emission:
References
edit- ^ a b Artigau; et al. (2009). "Photometric Variability of the T2.5 Brown Dwarf SIMP J013656.5+093347: Evidence for Evolving Weather Patterns". The Astrophysical Journal. 701 (2): 1534–1539. arXiv:0906.3514. Bibcode:2009ApJ...701.1534A. doi:10.1088/0004-637X/701/2/1534. S2CID 3123957.
- ^ a b c Vos, Johanna M.; Allers, Katelyn N.; Biller, Beth A. (2017-06-01). "The Viewing Geometry of Brown Dwarfs Influences Their Observed Colors and Variability Amplitudes". The Astrophysical Journal. 842 (2): 78. arXiv:1705.06045. Bibcode:2017ApJ...842...78V. doi:10.3847/1538-4357/aa73cf. ISSN 0004-637X.
- ^ a b c d Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ a b c d e f g Gagné, Jonathan; Faherty, Jacqueline K.; Burgasser, Adam J.; Artigau, Étienne; Bouchard, Sandie; Albert, Loïc; Lafrenière, David; Doyon, René; Bardalez-Gagliuffi, Daniella C. (2017-05-15). "SIMP J013656.5+093347 is Likely a Planetary-Mass Object in the Carina-Near Moving Group". The Astrophysical Journal. 841 (1): L1. arXiv:1705.01625. Bibcode:2017ApJ...841L...1G. doi:10.3847/2041-8213/aa70e2. ISSN 2041-8213. S2CID 119024210.
- ^ a b Croll, Bryce; Muirhead, Philip S.; Lichtman, Jack; Han, Eunkyu; Dalba, Paul A.; Radigan, Jacqueline (12 Sep 2016). "Long-term, Multiwavelength Light Curves of Ultra-Cool Dwarfs: II. The evolving Light Curves of the T2.5 SIMP 0136 & the Uncorrelated Light Curves of the M9 TVLM 513". arXiv:1609.03587 [astro-ph.SR].
- ^ "Presto change-o! Brown dwarf star is now a planet". newatlas.com. 2017-05-11. Retrieved 2018-08-07.
- ^ a b Starr, Michelle (3 August 2018). "There Is an Absolutely Gigantic Rogue Planet Wandering Our Galactic Neighbourhood". ScienceAlert.com. Retrieved 3 August 2018.
- ^ Kao, Melodie M.; Hallinan, Gregg; Pineda, J. Sebastian; Stevenson, David; Burgasser, Adam (August 2018). "The Strongest Magnetic Fields on the Coolest Brown Dwarfs". Astrophysical Journal Supplement Series. 237 (2): 25. arXiv:1808.02485. Bibcode:2018ApJS..237...25K. doi:10.3847/1538-4365/aac2d5. ISSN 0067-0049.
- ^ Yang, Hao; Apai, Dániel; Marley, Mark S.; Karalidi, Theodora; Flateau, Davin; Showman, Adam P.; Metchev, Stanimir; Buenzli, Esther; Radigan, Jacqueline; Artigau, Étienne; Lowrance, Patrick J.; Burgasser, Adam J. (2016-07-01). "Extrasolar Storms: Pressure-dependent Changes in Light-curve Phase in Brown Dwarfs from Simultaneous HST and Spitzer Observations". The Astrophysical Journal. 826 (1): 8. arXiv:1605.02708. Bibcode:2016ApJ...826....8Y. doi:10.3847/0004-637X/826/1/8. ISSN 0004-637X.
- ^ Vos, Johanna M.; Burningham, Ben; Faherty, Jacqueline K.; Alejandro, Sherelyn; Gonzales, Eileen; Calamari, Emily; Bardalez Gagliuffi, Daniella; Visscher, Channon; Tan, Xianyu; Morley, Caroline V.; Marley, Mark; Gemma, Marina E.; Whiteford, Niall; Gaarn, Josefine; Park, Grace (2023-02-01). "Patchy Forsterite Clouds in the Atmospheres of Two Highly Variable Exoplanet Analogs". The Astrophysical Journal. 944 (2): 138. arXiv:2212.07399. Bibcode:2023ApJ...944..138V. doi:10.3847/1538-4357/acab58. ISSN 0004-637X.
- ^ McCarthy, Allison M.; Muirhead, Philip S.; Tamburo, Patrick; Vos, Johanna M.; Morley, Caroline V.; Faherty, Jacqueline; Bardalez Gagliuffi, Daniella C.; Agol, Eric; Theissen, Christopher (2024). "Multiple Patchy Cloud Layers in the Planetary Mass Object SIMP0136+0933". The Astrophysical Journal. 965 (1): 83. arXiv:2402.15001. Bibcode:2024ApJ...965...83M. doi:10.3847/1538-4357/ad2c76.