| 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±0.067mas/yr[2] Dec.: −19.848±0.045mas/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 abrown dwarf in theTaurus Molecular Cloud. It is surrounded by aprotoplanetary disk, which is resolved by multiple observatories. It is one of the brightest brown dwarf disks in millimeterwavelengths.[8][9][4]
IRAS 04414+2506 was first identified as a goodpre-main sequence star withIRAS in 1994, resembling a class II disk.[10][11] In 2004 it was identified as the2MASS source J04442713+2512164 and identified as a brown dwarf as part of the Taurus Cloud for the first time byKevin Luhman.[5]
The brown dwarf was identified as having a spectral type of M7.25 with theMMT Observatory and the spectrum showedemission lines ofH-alpha,oxygen andsulfur. The oxygen and sulfur emission lines are associated with class I objects,Herbig-Haro objects and someT Tauri stars.[5] A detailed first study was published in 2008. This work identified additional emission lines with spectra from theKeck Observatory andCalar Alto Observatory. These are emissions bycalcium andnitrogen. 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 isaccreting material intensely, powering an outflow andastrophysical 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 therotation of the gas disk. A mass of 0.043–0.092 M☉ (45–96 MJ) was measured.[4]
Spitzer spectroscopy showedsilicate dust grains with sizes of less than a fewmicrons. The crystalline mineralsforsterite andenstatite were identified from emission. Most of the dust mass of the disk is stored in grains larger than 1mm.[6] The disk was first resolved with theCARMA 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 least15–30 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 theVery Large Array (VLA). The observations also detected ionized gas emission from the disk at 1.36 cm.[9]
The disk was first observed withALMA in 2014, which detected rotationalcarbon monoxide (CO) emission from the disk. This observation determined an outer disk radius of139+20
−27 AU and a total disk mass of1.3±0.2 MJ.[12] In 2025 additional high-resolution ALMA observations were published. These have the highest resolution for this disk, with a resolution of0.046″ (or about6.4 AU). The CO emission was detected to be rotating around the brown dwarf, a phenomenon also called aKeplerian 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.[4] The gap was first suspected to exist in 2019 from thespectral energy distribution better fitting a disk with a gap, but this gap was suspected to be between 0.02 and0.27 AU. This study found a higher disk mass of2.05 MJ, which is enough to formearth-mass planets.[13]
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 of0.3 to 7.7 M🜨 (betweensub-earth andsuper-earth).[4]
| Companion (in order from star) | Mass | Semimajor axis (AU) | Orbital period (years) | Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| gap (from SED fitting) | 0.02–0.27AU | — | — | |||
| gap (from ALMA) | 12.3–15.1AU | — | — | |||
| b(unconfirmed) | 0.3–7.7M🜨 | 13.7 | — | — | — | — |
| ring (from ALMA) | 16.2AU | 49.9±0.5° | — | |||
| outer edge (CO map) | <56AU | — | — | |||
