2MASS J04442713+2512164
2M0444 is the bright red "star" in the center of this PanSTARRS image. | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Taurus[1] |
| Right ascension | 04h 44m 27.143s |
| Declination | +25° 12′ 16.44″ |
| Apparent magnitude (V) | 17.65±0.38[2] |
| Characteristics | |
| Evolutionary stage | brown dwarf[3] |
| Spectral type | M7.25e±0.25[4] |
| Astrometry | |
| Proper motion (μ) | RA: +5.760±0.067 mas/yr[5] Dec.: −19.848±0.045 mas/yr[5] |
| Parallax (π) | 6.9855±0.0603 mas[5] |
| Distance | 467 ± 4 ly (143 ± 1 pc) |
| Details | |
| Mass | 0.045[6] M☉, 0.043–0.092[3] M☉ |
| Mass | 47[6] MJ, 45–96[3] MJup |
| Luminosity (bolometric) | 0.028[4] L☉ |
| Temperature | 2838[4] K |
| Rotation | 4.4300 days[7] |
| Rotational velocity (v sin i) | 12±2[6] km/s |
| Age | 1[8] Myr |
| Other designations | |
| IRAS 04414+2506, IRAS S04414+2506, 2MASS J04442713+2512164, EPIC 247915927, SSTtau 044427.1+251216, TIC 125977598, UGCS J044427.14+251216.3, WISE J044427.14+251216.3, Gaia DR2 147441558642852736 | |
| Database references | |
| SIMBAD | data |
2MASS J04442713+2512164 (2M0444, IRAS 04414+2506) is a brown dwarf in the Taurus Molecular Cloud. It is surrounded by a protoplanetary disk, which is resolved by multiple observatories. It is one of the brightest brown dwarf disks in millimeter wavelengths.[8][9][3]
IRAS 04414+2506 was first identified as a good pre-main sequence star with IRAS in 1994, resembling a class II disk.[10][11] In 2004 it was identified as the 2MASS source J04442713+2512164 and identified as a brown dwarf as part of the Taurus Cloud for the first time by Kevin Luhman.[4]
The brown dwarf
The brown dwarf was identified as having a spectral type of M7.25 with the MMT Observatory and the spectrum showed emission lines of H-alpha, oxygen and sulfur. The oxygen and sulfur emission lines are associated with class I objects, Herbig-Haro objects and some T Tauri stars.[4] A detailed first study was published in 2008. This work identified additional emission lines with spectra from the Keck Observatory and Calar Alto Observatory. These are emissions by calcium and nitrogen. The H-alpha line has a broad and asymmetric profile, indicating that gas moves with different velocities around the brown dwarf. The emission lines show that the brown dwarf is accreting material intensely, powering an outflow and astrophysical jet. The mass of the brown dwarf was estimated to be 0.045 M☉ (47 MJ) for an age of 5 million years.[6] The mass of the brown dwarf was directly measured using the rotation of the gas disk. A mass of 0.043–0.092 M☉ (45–96 MJ) was measured.[3]
The protoplanetary disk
Spitzer spectroscopy showed silicate dust grains with sizes of less than a few microns. The crystalline minerals forsterite and enstatite were identified from emission. Most of the dust mass of the disk is stored in grains larger than 1 mm.[6] The disk was first resolved with the CARMA array. Published in 2013, 2M0444 was the first brown dwarf disk that was resolved in thermal emission. The disk radius was determined to be at least 15–30 AU. The observation also found evidence for dust grains larger than 1 mm, which is seen as evidence for dust grain growth.[8] The disk was later also resolved with the Very Large Array (VLA). The observations also detected ionized gas emission from the disk at 1.36 cm.[9]
The disk was first observed with ALMA in 2014, which detected rotational carbon monoxide (CO) emission from the disk. This observation determined an outer disk radius of 139+20
−27 AU and a total disk mass of 1.3±0.2 MJ.[12] In 2025 additional high-resolution ALMA observations were published. These have the highest resolution for this disk, with a resolution of 0.046″ (or about 6.4 AU). The CO emission was detected to be rotating around the brown dwarf, a phenomenon also called a Keplerian disk. Researchers tentatively detected a gap at about 13.7 AU, with a width of 2.8 AU. The gap would be adjacent to a ring at around 16.2 AU.[3] The gap was first suspected to exist in 2019 from the spectral energy distribution better fitting a disk with a gap, but this gap was suspected to be between 0.02 and 0.27 AU. This study found a higher disk mass of 2.05 MJ, which is enough to form earth-mass planets.[13]
Possible planet
The detection of the tentative gap could be explained with a planet that is carving the gap at 13.7 AU. This planet would have a mass of 0.3 to 7.7 M🜨 (between sub-earth and super-earth).[3]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (years) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| gap (from SED fitting) | 0.02–0.27 AU | — | — | |||
| gap (from ALMA) | 12.3–15.1 AU | — | — | |||
| b (unconfirmed) | 0.3–7.7 M🜨 | 13.7 | — | — | — | — |
| ring (from ALMA) | 16.2 AU | 49.9±0.5° | — | |||
| outer edge (CO map) | <56 AU | — | — | |||
See also
- List of resolved circumstellar disks
- WISEA J120037.79-784508.3 is the closest brown dwarf surrounded by a disk
- KPNO-Tau 12 is another brown dwarf in Taurus, also surrounded by a disk
References
- ^ Roman, Nancy G. (1987). "Identification of a constellation from a position". Publications of the Astronomical Society of the Pacific. 99 (617): 695. Bibcode:1987PASP...99..695R. doi:10.1086/132034. Constellation record for this object at VizieR.
- ^ Lasker, Barry M.; Lattanzi, Mario G.; McLean, Brian J.; Bucciarelli, Beatrice; Drimmel, Ronald; Garcia, Jorge; Greene, Gretchen; Guglielmetti, Fabrizia; Hanley, Christopher; Hawkins, George; Laidler, Victoria G.; Loomis, Charles; Meakes, Michael; Mignani, Roberto; Morbidelli, Roberto (2008-07-11). "The Second-Generation Guide Star Catalog: Description and Properties". The Astronomical Journal. 136 (2): 735–766. arXiv:0807.2522. Bibcode:2008AJ....136..735L. doi:10.1088/0004-6256/136/2/735. ISSN 0004-6256.
- ^ a b c d e f g h Alejandro Santamaría Miranda; Curone, Pietro; Pérez, Laura; Kurtovic, Nicolás T.; Agurto-Gangas, Carolina; Sierra, Anibal; Itziar De Gregorio-Monsalvo; Huélamo, Nuria; Miley, James M.; Palau, Aína; Pinilla, Paola; Rebollido, Isabel; Ribas, Álvaro; Rivière-Marichalar, Pablo; Schreiber, Matthias R.; Sai, Jinshi; Carrera, Benjamín (2025). "Hints of Disk Substructure in the First Brown Dwarf with a Dynamical Mass Constraint". arXiv:2505.08107 [astro-ph.SR].
- ^ a b c d e Luhman, K. L. (2004-12-20). "New Brown Dwarfs and an Updated Initial Mass Function in Taurus*". The Astrophysical Journal. 617 (2): 1216–1232. arXiv:astro-ph/0411447. Bibcode:2004ApJ...617.1216L. doi:10.1086/425647. ISSN 0004-637X.
- ^ a b 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.
- ^ a b c d e Bouy, H.; Huélamo, N.; Pinte, C.; Olofsson, J.; Navascués, D. Barrado y; Martín, E. L.; Pantin, E.; Monin, J.-L.; Basri, G.; Augereau, J.-C.; Ménard, F.; Duvert, G.; Duchêne, G.; Marchis, F.; Bayo, A. (2008-08-01). "Structural and compositional properties of brown dwarf disks: the case of 2MASS J04442713+2512164". Astronomy & Astrophysics. 486 (3): 877–890. arXiv:0803.2051. Bibcode:2008A&A...486..877B. doi:10.1051/0004-6361:20078866. ISSN 0004-6361.
- ^ Rebull, L. M.; Stauffer, J. R.; Cody, A. M.; Hillenbrand, L. A.; Bouvier, J.; Roggero, N.; David, T. J. (2020-05-26). "Rotation of Low-mass Stars in Taurus with K2". The Astronomical Journal. 159 (6): 273. arXiv:2004.04236. Bibcode:2020AJ....159..273R. doi:10.3847/1538-3881/ab893c. ISSN 0004-6256.
- ^ a b c Ricci, L.; Isella, A.; Carpenter, J. M.; Testi, L. (February 2013). "CARMA Interferometric Observations of 2MASS J044427+2512: The First Spatially Resolved Observations of Thermal Emission of a Brown Dwarf Disk". The Astrophysical Journal. 764 (2): L27. arXiv:1301.2624. Bibcode:2013ApJ...764L..27R. doi:10.1088/2041-8205/764/2/L27. ISSN 0004-637X.
- ^ a b Ricci, L.; Rome, H.; Pinilla, P.; Facchini, S.; Birnstiel, T.; Testi, L. (September 2017). "VLA Observations of the Disk around the Young Brown Dwarf 2MASS J044427+2512". The Astrophysical Journal. 846 (1): 19. arXiv:1707.07197. Bibcode:2017ApJ...846...19R. doi:10.3847/1538-4357/aa81bf. ISSN 0004-637X.
- ^ Gomez, Mercedes; Kenyon, Scott J.; Hartmann, Lee (May 1994). "A near-infrared survey for pre-main sequence stars in Taurus". The Astronomical Journal. 107: 1850. Bibcode:1994AJ....107.1850G. doi:10.1086/116994. ISSN 0004-6256.
- ^ Kenyon, Scott J.; Gomez, Mercedes; Marzke, Ronald O.; Hartmann, Lee (July 1994). "New Pre-Main-Sequence Stars in the Taurus-Auriga Molecular Cloud". The Astronomical Journal. 108: 251. Bibcode:1994AJ....108..251K. doi:10.1086/117064. ISSN 0004-6256.
- ^ Ricci, L.; Testi, L.; Natta, A.; Scholz, A.; de Gregorio-Monsalvo, I.; Isella, A. (2014-07-22). "Brown Dwarf Disks with Alma". The Astrophysical Journal. 791 (1): 20. arXiv:1406.0635. Bibcode:2014ApJ...791...20R. doi:10.1088/0004-637x/791/1/20. hdl:10023/8607. ISSN 0004-637X.
- ^ a b Rilinger, Anneliese M.; Espaillat, Catherine C.; Macías, Enrique (2019-06-19). "Modeling the Protoplanetary Disks of Two Brown Dwarfs in the Taurus Molecular Cloud". The Astrophysical Journal. 878 (2): 103. arXiv:1905.05829. Bibcode:2019ApJ...878..103R. doi:10.3847/1538-4357/ab211d. ISSN 0004-637X.