2MASS J03480772−6022270

2MASS near-infrared image of 2MASS J0348−6022 (center)
Observation data
Epoch J2000      Equinox J2000
Constellation Reticulum
Right ascension 03h 48m 07.721s[1]
Declination –60° 22′ 27.062″[1]
Characteristics
Spectral type T7[2]
Apparent magnitude (J) 15.318 ± 0.050[1]
Apparent magnitude (H) 15.559 ± 0.143[1]
Apparent magnitude (K) 15.602 ± 0.230[1]
Astrometry
Radial velocity (Rv)−14.1 ± 3.7[2] km/s
Proper motion (μ) RA: –279.7 ± 0.6[3] mas/yr
Dec.: –768.5 ± 0.7[3] mas/yr
Parallax (π)120.1 ± 1.8 mas[3]
Distance27.2 ± 0.4 ly
(8.3 ± 0.1 pc)
Details[2]
Mass0.041+0.021
−0.017 M☉
Radius0.093+0.016
−0.010 R☉
Surface gravity (log g)5.1 ± 0.3 cgs
Temperature880 ± 110 K
Rotation1.080+0.004
−0.005 h
Rotational velocity (v sin i)103.5 ± 7.4 km/s
Age3.5+11.5
−2.9 Gyr
Other designations
WISE J034807.33-602234.9, WISEA J034807.33-602235.2, WISEP J034807.34-602234.9, UGCS J121951.36+312849.4, TIC 237922091[1]
Database references
SIMBADdata

2MASS J03480772−6022270 (abbreviated to 2MASS J0348−6022) is a brown dwarf of spectral class T7, located in the constellation Reticulum approximately 27.2 light-years from the Sun. It was discovered by astronomer Adam Burgasser and collaborators of the 2MASS Wide-Field T Dwarf Search in 2002. With a rotation period of 1.08 hours, it is the fastest-rotating brown dwarf confirmed as of 2022.[4] The rotational velocity at its equator is over 100 km/s (62 mi/s), approaching the predicted rotational speed limit beyond which it would break apart due to centripetal forces.[5] As a consequence of its rapid rotation, the brown dwarf is slightly flattened at its poles to a similar degree as Saturn, the most oblate planet in the Solar System. Its rapid rotation may enable strong auroral radio emissions via charged particle interactions in its magnetic field, as observed in other known rapidly-rotating brown dwarfs.[2]

Discovery

2MASS J0348−6022 was first catalogued as a point source in June 2003 by the Two Micron All-Sky Survey (2MASS) organized by the University of Massachusetts Amherst and the Infrared Processing and Analysis Center under the California Institute of Technology.[6] It was discovered to be a brown dwarf of the spectral class T7 by Adam Burgasser and collaborators of the 2MASS Wide-Field T Dwarf Search, based on spectra in the near-infrared region of the electromagnetic spectrum obtained in September 2002 with the Víctor M. Blanco Telescope at the Cerro Tololo Inter-American Observatory, Chile. Their discovery and characterization of 2MASS J0348−6022 along with two other T dwarfs located in the southern celestial hemisphere was published in The Astronomical Journal in November 2003.[7]

Location and proper motion

2MASS J0348−6022 is located in the southern celestial hemisphere in the constellation Reticulum.[7] Its equatorial coordinates based on the J2000 epoch are: RA 03h 48m 07.72s and Dec –60° 22′ 27.0″.[1] These coordinates in sexagesimal notation are displayed in its identifier 2MASS J03480772−6022270.[6] The trigonometric parallax of 2MASS J0348−6022 has been measured to be 120.1±1.8 milliarcseconds, from 16 observations by the New Technology Telescope (NTT) collected over 6.4 years.[3] This corresponds to a distance of 8.3 ± 0.1 parsecs (27.2 ± 0.4 ly). A previous estimate by Burgasser and collaborators from the spectrophotometric relation of spectral type and near-infrared absolute magnitude resulted in a value of 9 ± 4 parsecs (29 ± 13 ly), based on 2MASS JHK-band photometry.[7]

The NTT has also measured the proper motion of 2MASS J0348−6022 in two directions: RA −279.7±0.6 mas/yr and Dec −768.5±0.7 mas/yr, which indicate motion in south-west direction on the sky.[3] Given the distance estimate from trigonometric parallax, the corresponding tangential velocity is 32.3±0.5 km/s, consistent with the kinematics of the stars of the Galactic disk.[3][7]

Spectral class

2MASS J0348−6022 is classified as a late T-type brown dwarf with the spectral class T7, distinguished by the presence of strong methane (CH4) and water (H2O) absorption bands in its near-infrared spectrum between wavelengths 1.2 and 2.35 μm.[7] The near-infrared spectrum of 2MASS J0348−6022 also displays a pair of narrow absorption lines at 1.243 and 1.252 μm, which are attributed to the presence of neutral potassium (K I) in the brown dwarf's atmosphere. Compared to other T dwarfs, the K I doublet lines in 2MASS J0348−6022's spectrum appear relatively faded due to its late spectral type; K I doublet lines are typically more prominent in the spectra of early- and mid-type T dwarfs as well as late-type L and M dwarfs.[7] Absorption bands of iron(I) hydride (FeH) have also been found in 2MASS J0348−6022's spectrum between 1.72–1.78 μm.[2]

Like most T dwarfs, the optical and near-infrared color of 2MASS J0348−6022 is very red. The near-infrared 2MASS color indices are J–H = −0.24±0.16 and H–K = −0.04±0.28, indicating that the brown dwarf appears brighter in longer (thus redder) wavelengths of light.[7]

Physical properties

In this artist's impression, the brown dwarf is depicted resembling the planet Jupiter with narrow, red atmospheric bands. The object's shape is slightly flattened at its poles due to its rapid rotation.
Artist's impression of an oblate brown dwarf with narrow atmospheric bands

The near-infrared spectrum of a brown dwarf can be modelled by a photosphere primarily defined by two fixed intrinsic properties: effective temperature (Teff) and surface gravity (log g).[2] In a 2021 study, Megan Tannock and collaborators compared the near-infrared spectrum of 2MASS J0348−6022 to various published photospheric models and derived multiple best-fit solutions for its effective temperature and surface gravity. They took a weighted mean of these best-fit solutions and adopted the following values for these two fundamental properties: Teff = 880±110 K and log g = 5.1±0.3 dex (105.1 times Earth's gravity in centimetre-gram-second units). From photospheric modeling they were also able to determine 2MASS J0348−6022's radial velocity and projected rotational velocity, which facilitated the confirmation of the brown dwarf's rapid rotation.[2]

The mass, radius, and age of 2MASS J0348−6022 are estimated by interpolation of brown dwarf evolutionary models based on effective temperature and surface gravity. From their adopted effective temperature and surface gravity values from photospheric modelling, Tannock and collaborators derive a mass of 0.041+0.021
−0.017 M☉ (~43 MJup), a Jupiter-like equatorial radius of 0.093+0.016
−0.010 R☉ (69,700 km), and an age of 3.5+11.5
−2.9 billion years.[2] The high estimated age of 2MASS J0348−6022 is due to its late T-type spectral class, which is generally expected to describe the later evolutionary stages of brown dwarfs as they cool.[8]

Rotation

Photometric variability and periodicity

2MASS J0348−6022 is the fastest-rotating brown dwarf confirmed as of 2022, with a photometric periodicity of 1.080+0.004
−0.005 hours.[lower-alpha 1] It along with L dwarfs 2MASS J1219+3128 and 2MASS J0407+1546 have had their short rotation periods measured and studied in detail in 2021 by Megan Tannock and collaborators using data from the Spitzer Space Telescope.[5] The double-peaked light curve of 2MASS J0348−6022 may indicate the presence of two dominant photospheric spots configured on opposite hemispheres of the brown dwarf.[2]

Photometric variability in 2MASS J0348−6022 was first reported in 2008 by Fraser Clarke and collaborators using the New Technology Telescope's (NTT) near-infrared spectrograph. They reported an upper limit J-band amplitude of <1% in a six hour observation period.[10] Likewise, astrophysicist Jacqueline Radigan estimated a J-band amplitude of <1.1%±0.4% in an independent analysis of 2011–2012 NTT observations published by Paul Wilson and collaborators in 2014, who initially derived a spuriously high amplitude of 2.4%±0.5% due to systematic errors in their measurement.[11][8] Low-amplitude (<2%) variability is common among brown dwarfs of all spectral types, and is presumed to be the result of patchy photospheres with subtle heterogeneities.[11]

Infrared observations by the Spitzer Space Telescope show that 2MASS J0348−6022's brightness appears flat in the Infrared Array Camera's 3.6 μm band and only exhibits discernible variability in the 4.5 μm band, a behavior typical of previously observed T dwarfs. This can be explained by the presence of CH4 in its atmosphere, which is opaque to wavelengths around 3.3 μm.[2]

Physical effects

2MASS J0348-6022 has an oblateness comparable to those of Solar System planets Jupiter and Saturn, which spin 10 times slower than the brown dwarf.
Oblateness and size comparison of 2MASS J0348−6022 to Solar System planets Jupiter and Saturn
2MASS J0348−6022 is expected to exhibit radio aurorae, similar those depicted in this artist's impression of the radio-emitting T dwarf SIMP J013656.5+093347

The spectral lines in 2MASS J0348−6022's spectrum are Doppler-broadened due to the brown dwarf's rapid rotation, consistent with its short photometric periodicity. This rotational broadening can be modelled as a function of the brown dwarf's projected rotational velocity (v sin i), which is estimated at 103.5 ± 7.4 km/s (64.3 ± 4.6 mi/s).[2]

The rotational velocity at 2MASS J0348−6022's equator (v) is separately calculated from its radius and rotation period, giving 105+18
−12 km/s. While it has the highest reported v sin i value of all known ultra-cool dwarfs, its equatorial rotational velocity only comes second after the slightly larger L8 dwarf 2MASS J1219+3128. The high equatorial rotational velocity of 2MASS J0348−6022 decreases the surface gravity at its equator due to centrifugal acceleration, though this has a negligible effect on the validity of the nominal surface gravity log g = 5.1±0.3 dex inferred from photospheric modelling.[2]

The centrifugal forces exerted by its rapid rotation also cause the brown dwarf to become oblate, being slightly flattened at its poles. Tannock and collaborators calculate an oblateness of 0.08; the difference between the brown dwarf's polar and equatorial radii is 8%. For comparison, the Solar System's most oblate planet Saturn has an oblateness of 0.10.[2] 2MASS J0348−6022 is expected to exhibit significant linear polarization in its optical and infrared thermal emission due to its oblate, dusty atmosphere induced by its rapid rotation and lower surface gravity.[2][12]

Extrapolations for the breakup periods of typical brown dwarfs older than 1 billion years range tens of minutes depending on mass and radius. The high spin rate and oblateness of 2MASS J0348−6022 places it at about 45% of its rotational stability limit, assuming a smoothly varying fluid interior. Taking into account of magnetic dynamos generated by the brown dwarf's metallic hydrogen interior, the rotational velocity threshold may be even lower and implies that 2MASS J0348−6022 may be closer to breakup than predicted.[2] As brown dwarfs cool and age, they contract in size and spin faster so as to conserve angular momentum; theoretically rapid rotators like 2MASS J0348−6022 should eventually approach their rotational stability limit and break apart, but no such phenomena have been observed as of 2021.[2] It is possible that some unknown rotational braking mechanism may be preventing brown dwarfs from breaking up as they age.[5]

The rapid rotation of 2MASS J0348−6022 may enhance its magnetic field through a dynamo process involving convection induced by differential rotation in its interior. This in turn enables strong aurorae in the form of circularly polarized radio wave emissions via charged particle interactions in its magnetic field, which are driven by the so-called electron cyclotron maser instability that has been observed in other known rapidly-rotating and radio-emitting brown dwarfs.[13] The inclination of 2MASS J0348−6022's spin axis to Earth is 81°+9°
−27°, derived from its v sin i value. This places it in a nearly equator-on configuration viewed from Earth, which makes it a favorable target for observing these hypothesized auroral radio emissions.[2]

See also

The other two discoveries of rapidly-rotating brown dwarfs, presented in Tannock et al. (2021):[2]

Notes

  1. ↑ The T dwarfs 2MASS J0718−6415 (1.080+0.004
    −0.003     h    ) and WISEPC J1122+2550 (~0.288 h) may have comparable—if not faster—rotation periods than 2MASS J0348−6022, but both of their measurements are tentative due to possible aliasing[9] or distance uncertainties.[4]

References

  1. 1 2 3 4 5 6 7 "2MASS J03480772-6022270 – Brown Dwarf (M<0.08solMass)". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 4 March 2021.
  2. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 Tannock, Megan E.; Metchev, Stanimir; Heinze, Aren; Miles-Páez, Paulo A.; Gagné, Jonathan; Burgasser, Adam; et al. (May 2021). "Weather on Other Worlds. V. The Three Most Rapidly Rotating Ultra-Cool Dwarfs". The Astronomical Journal. 161 (5): 21. arXiv:2103.01990. Bibcode:2021AJ....161..224T. doi:10.3847/1538-3881/abeb67. S2CID 232105126. 224.
  3. 1 2 3 4 5 6 Kirkpatrick, J. Davy; Martin, Emily C.; Smart, Richard L.; Cayago, Alfred J.; Beichman, Charles A.; Marocco, Federico; et al. (February 2019). "Preliminary Trigonometric Parallaxes of 184 Late-T and Y Dwarfs and an Analysis of the Field Substellar Mass Function into the "Planetary" Mass Regime". The Astrophysical Journal Supplement Series. 240 (2): 69. arXiv:1812.01208. Bibcode:2019ApJS..240...19K. doi:10.3847/1538-4365/aaf6af. 19.
  4. 1 2 Vos, Johanna M.; Faherty, Jacqueline K.; Gagné, Jonathan; Marley, Mark; Metchev, Stanimir; Gizis, John; et al. (January 2022). "Let the Great World Spin: Revealing the Stormy, Turbulent Nature of Young Giant Exoplanet Analogs with the Spitzer Space Telescope". The Astrophysical Journal. 924 (2): 24. arXiv:2201.04711. Bibcode:2022ApJ...924...68V. doi:10.3847/1538-4357/ac4502. S2CID 245904001. 68.
  5. 1 2 3 Cofield, Calla (7 April 2021). "Trio of Fast-Spinning Brown Dwarfs May Reveal a Rotational Speed Limit". Jet Propulsion Laboratory. NASA. Retrieved 7 April 2021.
  6. 1 2 Cutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E.; Fowler, John W.; Gizis, John E.; Howard, Elizabeth V.; Huchra, John P.; Jarrett, Thomas H.; Kopan, Eugene L.; Kirkpatrick, J. Davy; Light, Robert M.; Marsh, Kenneth A.; McCallon, Howard L.; Schneider, Stephen E.; Stiening, Rae; Sykes, Matthew J.; Weinberg, Martin D.; Wheaton, William A.; Wheelock, Sherry L.; Zacarias, N. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues. 2246: II/246. Bibcode:2003yCat.2246....0C.
  7. 1 2 3 4 5 6 7 Burgasser, Adam J.; McElwain, Michael W.; Kirkpatrick, J. Davy (November 2003). "The 2MASS Wide-Field T Dwarf Search. II. Discovery of Three T Dwarfs in the Southern Hemisphere". The Astronomical Journal. 126 (5): 2487–2494. arXiv:astro-ph/0307374. Bibcode:2003AJ....126.2487B. doi:10.1086/378608. S2CID 14734365.
  8. 1 2 Wilson, P. A.; Rajan, A.; Patience, J. (June 2014). "The brown dwarf atmosphere monitoring (BAM) project I. The largest near-IR monitoring survey of L and T dwarfs". Astronomy & Astrophysics. 566 (A111): 16. arXiv:1404.4633. Bibcode:2014A&A...566A.111W. doi:10.1051/0004-6361/201322995. S2CID 118656241.
  9. ↑ Route, Matthew; Wolszczan, Alexander (April 2016). "Radio Flaring from the T6 Dwarf WISEPC J112254.73+255021.5 with a Possible Ultra-short Periodicity". The Astrophysical Journal. 821 (2): 5. arXiv:1604.04543. Bibcode:2016ApJ...821L..21R. doi:10.3847/2041-8205/821/2/L21. S2CID 118478221. L21.
  10. ↑ Clarke, F. J.; Hodgkin, S. T.; Oppenheimer, B. R.; Robertson, J.; Haubois, X. (July 2008). "A search for J-band variability from late-L and T brown dwarfs". Monthly Notices of the Royal Astronomical Society. 386 (4): 2009–2014. Bibcode:2008MNRAS.386.2009C. doi:10.1111/j.1365-2966.2008.13135.x.
  11. 1 2 Jacqueline, Radigan (December 2014). "An Independent Analysis of the Brown Dwarf Atmosphere Monitoring (BAM) Data: Large-amplitude Variability is Rare Outside the L/T Transition". The Astrophysical Journal. 797 (2): 12. arXiv:1408.5919. Bibcode:2014ApJ...797..120R. doi:10.1088/0004-637X/797/2/120. OSTI 22364797. 120.
  12. ↑ Miles-Páez, P. A.; Zapatero Osorio, M. R.; Pallé, E.; Peña Ramírez, K. (August 2013). "Linear polarization of rapidly rotating ultracool dwarfs". Astronomy & Astrophysics. 566 (A125): 11. arXiv:1306.6314. Bibcode:2013A&A...556A.125M. doi:10.1051/0004-6361/201321851. S2CID 54966404.
  13. ↑ Kao, Melodie M.; Hallinan, Gregg; Pineda, J. Sebastian; Stevenson, David; Burgasser, Adam (August 2018). "The Strongest Magnetic Fields on the Coolest Brown Dwarfs". The Astrophysical Journal Supplement Series. 237 (2): 25. arXiv:1808.02485. Bibcode:2018ApJS..237...25K. doi:10.3847/1538-4365/aac2d5. 25.
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