2MASS J04442713+2512164
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| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Taurus[1] |
| Right ascension | 04h 44m 27.143s[2] |
| Declination | +25° 12′ 16.44″[2] |
| Apparent magnitude (V) | 17.65±0.38[3] |
| Characteristics | |
| Evolutionary stage | brown dwarf[4] |
| Spectral type | M7.25e±0.25[5] |
| Astrometry | |
| Proper motion (μ) | RA: +5.760±0.067 mas/yr[2] Dec.: −19.848±0.045 mas/yr[2] |
| Parallax (π) | 6.9855±0.0603 mas[2] |
| Distance | 467 ± 4 ly (143 ± 1 pc) |
| Details | |
| Mass | 0.045[6] M☉, 0.043–0.092[4] M☉ |
| Mass | 47[6] MJ, 45–96[4] MJup |
| Luminosity (bolometric) | 0.028[5] L☉ |
| Temperature | 2838[5] 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][4]
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.[5]
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.[5] 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.[4]
