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	=== Physical parameters ===		=== Physical parameters ===
	The mass and age of WISE 0855−0714 are neither known with certainty, but can be constrained with its known temperature. The age of WISE 0855−0714 depends on its mass; a lower mass would lead to a faster rate of cooling and thus a younger age for WISE 0855−0714, whereas a higher mass would lead to a slower rate of cooling and thus an older age for WISE 0855−0714.<ref name="Luhman2014"/> Assuming an age range of 1–10 billion years, evolutionary models for brown dwarfs predict that WISE 0855−0714 should have a mass between {{Jupiter mass\|3 to 10\|jup=y\|link=yes}}.<ref name="NASA20140425"/><ref name="Luhman2014"/> This mass is in the range of a ] or other ].		The mass and age of WISE 0855−0714 are neither known with certainty, but can be constrained with its known present-day temperature. The age of WISE 0855−0714 depends on its mass; a lower mass would lead to a faster rate of cooling and thus a younger age for WISE 0855−0714, whereas a higher mass would lead to a slower rate of cooling and thus an older age for WISE 0855−0714.<ref name="Luhman2014"/> Assuming an age range of 1–10 billion years, evolutionary models for brown dwarfs predict that WISE 0855−0714 should have a mass between {{Jupiter mass\|3 to 10\|jup=y\|link=yes}}.<ref name="NASA20140425"/><ref name="Luhman2014"/> This mass is in the range of a ] or other ].

	As of 2003, the ] considers an object with a mass above {{Jupiter mass\|13\|jup=y}}, capable of fusing ], to be a brown dwarf. A lighter object and one orbiting another object is considered a planet.<ref name="workinggroup" /> However, if the distinction is based on how the object formed then it might be considered a failed star, a theory advanced for the object ].<ref name="amspace20140428" />		As of 2003, the ] considers an object with a mass above {{Jupiter mass\|13\|jup=y}}, capable of fusing ], to be a brown dwarf. A lighter object and one orbiting another object is considered a planet.<ref name="workinggroup" /> However, if the distinction is based on how the object formed then it might be considered a failed star, a theory advanced for the object ].<ref name="amspace20140428" />

Revision as of 17:36, 7 December 2024

Sub-brown dwarf in the constellation Hydra

WISE J085510.83−071442.5
Observation data Epoch J2000 Equinox J2000
Time-lapsed photo sequence of WISE 0855−0714's movement in the sky using captured images from the JWST
Constellation	Hydra
Right ascension	08 55 10.83168
Declination	−07° 14′ 42.5256″
Characteristics
Evolutionary stage	Sub-brown dwarf
Spectral type	Y4V
Apparent magnitude (J)	25.00±0.53
Apparent magnitude (H)	23.83±0.24
Astrometry

Proper motion (μ)	RA: −8,123.7±1.3 mas/yr Dec.: 673.2±1.3 mas/yr
Parallax (π)	439.0 ± 2.4 mas
Distance	7.43 ± 0.04 ly (2.28 ± 0.01 pc)

Details

Mass	~3–10 M_Jup
Radius	0.89 R_Jup
Radius	63,500 km
Luminosity	4.9545×10 `L`_☉
Surface gravity (log g)	~4 cgs
Temperature	285 K
Metallicity	~0 dex
Age	1–10 Gyr

Other designations
WISEA J085510.74-071442.5, GJ 11286
Database references
SIMBAD	data
WISE 0855−0714Location of WISE 0855−0714 in the constellation Hydra

WISE 0855−0714 (full designation WISE J085510.83−071442.5, or W0855 for short) is a sub-brown dwarf of spectral class Y4, located 7.4 light-years (2.3 parsecs) from Earth in the constellation Hydra. It is the fourth-closest star or (sub-) brown dwarf system to the Sun, and was discovered by Kevin Luhman using data from the Wide-field Infrared Survey Explorer (WISE). As of 2014, WISE 0855−0714 has the third-highest proper motion (8,151.6±1.8 mas/yr) after Barnard's Star (10,300 mas/yr) and Kapteyn's Star (8,600 mas/yr) and the fourth-largest parallax (439.0±2.4 mas) of any known star or brown dwarf. It is also the coldest object of its type found in interstellar space, having a temperature of about 285 K (12 °C; 53 °F).

Characterization

Observations

WISE 0855−0714 was first imaged by the WISE telescope on 4 May 2010 during its primary mission of surveying the entire sky. It was later discovered by Kevin Luhman in March 2013, who noticed the object's unusually high proper motion while searching for potential binary companions of the Sun in WISE images. In the interest of confirming the object's spectral properties and nearby distance to the Sun, Luhman made follow-up observations with the Spitzer Space Telescope and the Gemini North telescope in 2013–2014. The discovery of the object was announced in a NASA press release in April 2014.

Since WISE 0855−0714 is an isolated object, its luminosity primarily comes from thermal radiation. WISE 0855−0714's temperature is low enough that it roughly matches room temperature, which means WISE 0855−0714's luminosity is very low and primarily emits infrared light as thermal radiation. Hence, it is best observed with infrared telescopes such as WISE and the James Webb Space Telescope (JWST). WISE 0855−0714 has been detected in spectral wavelengths as short as 1.25 μm (J band)—in this near-infrared wavelength, the object appears extremely dim with an apparent magnitude of 26.4. WISE 0855−0714's brightness decreases with decreasing wavelength, so the object is practically invisible in visible light.

Distance and proper motion

Based on direct observations, WISE 0855−0714 has a large parallax, which specifically relates to its distance from the Solar System. This phenomenon results in a distance of around 2.28±0.01 parsecs (7.43±0.04 light-years), with a small margin of error due to the strength of the parallax effect and the clarity of observations. WISE 0855−0714 also has an exceptionally high proper motion.

Spectrometry

Its luminosity in different bands of the thermal infrared in combination with its absolute magnitude—because of its known distance—was used to place it in context of different models; the best characterization of its brightness was in the W2 band of 4.6 μm at an apparent magnitude of 13.89±0.05, though it was brighter into the deeper infrared. Infrared images taken with the Magellan Baade Telescope suggest evidence of sulfide clouds below water ice clouds.

Near- and mid-infrared spectra in the L- and M-band were taken with the GNIRS instrument on the Gemini North Telescope. The M-band (4.5–5.1 μm) spectrum is dominated by water vapour (H₂O) absorption. The L-band (3.4–4.14 μm) spectrum is dominated by methane absorption. Both the M- and L-band surprisingly have no detection of phosphine (PH₃), which appears in the atmosphere of Jupiter. The M-band spectrum shows evidence for water ice clouds and the near-infrared photometry WISE 0855 is faint compared to models, suggesting an additional absorber, probably clouds made of ammonium dihydrogen phosphate (NH₄)(H₂PO₄), which are below the water ice clouds. An approved JWST proposal describes how the team is planning to use a near-infrared time-series to study the hydrological cycle in the atmosphere of WISE 0855 with NIRSpec.

Observations with NIRSpec detected methane (CH₄), water vapor (H₂O), ammonia (NH₃) and carbon monoxide (CO) in the atmosphere, but was not able to confirm any phosphine (PH₃) or carbon dioxide (CO₂) in the atmosphere. Water ice clouds are also not confirmed and the spectrum is well matched with a cloudless model. Observations with MIRI showed a water vapor depletion and a water abundance that is variable with pressure. This is consistent with water condensing out in the upper atmosphere. The observations did however not detect any water ice clouds, which were predicted in previous studies. This discrepancy is explained with the rainout of the water: Water condenses into particles in the upper atmosphere, which quickly sink into the lower atmosphere. Clouds only form if upward mixing is present. A similar process is present for alkali metals in L- and T-dwarfs. A direct rainout would suggest weak mixing, but disequilibrium chemistry suggest rigours mixing. Future variable studies might resolve if upward mixing or settling is the dominant process. Cloud models however potentially detected deep ammonium dihydrogen phosphate (NH₄)(H₂PO₄) clouds. The observations also detected NH₃ for the first time in WISE 0855. The atmosphere has a mass fraction of NH₃/NH₃ = 332+63
−43, meaning it has about 99.7% N and about 0.3% N. Compared to solar values and the ratio of WISE 1828, the atmosphere of WISE 0855 is enriched in N. The nitrogen isotope ratio is closer to today's N-enriched interstellar medium. This could mean that WISE 0855 formed from a younger cloud, but more measurements of N in other brown dwarfs are needed to establish evolutionary trends. In November 2024 a team used archived and new NIRSpec data to detect deuterated methane (CH₃D) and about one part per billion PH₃ in WISE 0855. This detection of deuterium showed that WISE 0855 has a mass below the deuterium-burning-limit. The low amount of PH₃ is on the other hand in disagreement with predictions, showing incomplete knowledge of phosphorus chemistry.

Variability

Variability of WISE 0855 in the infrared was measured with Spitzer IRAC. A relative small amplitude of 4–5% was measured. Water ice cloud models predicted a large amplitude. This small amplitude might suggest that the hemispheres of WISE 0855 have very small deviation in cloud coverage. The light curve is too irregular to produce a good fit and rotation periods between 9.7 and 14 hours were measured.

Physical parameters

The mass and age of WISE 0855−0714 are neither known with certainty, but can be constrained with its known present-day temperature. The age of WISE 0855−0714 depends on its mass; a lower mass would lead to a faster rate of cooling and thus a younger age for WISE 0855−0714, whereas a higher mass would lead to a slower rate of cooling and thus an older age for WISE 0855−0714. Assuming an age range of 1–10 billion years, evolutionary models for brown dwarfs predict that WISE 0855−0714 should have a mass between 3 to 10 M_Jup. This mass is in the range of a sub-brown dwarf or other planetary-mass object.

As of 2003, the International Astronomical Union considers an object with a mass above 13 M_Jup, capable of fusing deuterium, to be a brown dwarf. A lighter object and one orbiting another object is considered a planet. However, if the distinction is based on how the object formed then it might be considered a failed star, a theory advanced for the object Cha 110913-773444.

Combining its luminosity, distance, and mass it is estimated to be the coldest-known brown dwarf, with a modeled effective temperature of 225 to 260 K (−48 to −13 °C; −55 to 8 °F), depending on the model. Models matching the NIRSpec spectrum are well fitted with a temperature of 285 K (12 °C; 53 °F).

Gallery

Time-lapsed photo sequence of WISE 0855−0714's movement in the sky using captured images from the WISE and the Spitzer telescopes.
JWST NIRCam observation of W0855 (orange "star" at the center) showing the movement over about half a year.
The position of WISE 0855−0714 on a radar map among all stellar objects or stellar systems within 9 light years (ly) from the map's center, the Sun (Sol). The diamond-shapes are their positions entered according to right ascension in hours angle (indicated at the edge of the map's reference disc), and according to their declination. The second mark shows each's distance from Sol, with the concentric circles indicating the distance in steps of one ly.
No water ice clouds are detected in WISE 0855, but maybe deep ammonium dihydrogen phosphate clouds exist. This would make it similar to class III (cloudless) planets on the Sudarsky scale

Notes

Applying the Stefan–Boltzmann law with a nominal solar effective temperature of 5,772 K:
${\sqrt {{\biggl (}{\frac {5,772}{285}}{\biggr )}^{4}\cdot 10^{-7.305}}}=0.091298\ R_{\odot }$ . Using the solar radius value of 695,700 km, the calculated radius of WISE 0855-0714 converts to approximately 63,500 km, or 0.89 R_J when dividing by the nominal Jupiter radius value of 71,492 km.
Derived from a bolometric luminosity logarithm of –7.305 given in Luhman et al. 2024

Reference s

^ "WISEA J085510.74-071442.5". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 15 May 2017.
^ Kirkpatrick, J. Davy; Gelino, Christopher R.; Faherty, Jacqueline K.; Meisner, Aaron M.; Caselden, Dan; Schneider, Adam C.; et al. (March 2021). "The Field Substellar Mass Function Based on the Full-sky 20 pc Census of 525 L, T, and Y Dwarfs". The Astrophysical Journal Supplement Series. 253 (1): 85. arXiv:2011.11616. Bibcode:2021ApJS..253....7K. doi:10.3847/1538-4365/abd107. S2CID 227126954. 7.
Mamajek, Eric. "A Modern Mean Dwarf Stellar Color and Effective Temperature Sequence". Retrieved 7 February 2021.
^ Luhman, K. L.; Tremblin, P.; Alves de Oliveira, C.; Birkmann, S. M.; Baraffe, I.; Chabrier, G.; et al. (January 2024). "JWST/NIRSpec Observations of the Coldest Known Brown Dwarf". The Astronomical Journal. 167 (1): 5. arXiv:2311.17316. Bibcode:2024AJ....167....5L. doi:10.3847/1538-3881/ad0b72. S2CID 265498620.
Golovin, Alex; Reffert, Sabine; Just, Andreas; Jordan, Stefan; Vani, Akash; Jahreiß, Hartmut (November 2022). "The Fifth Catalogue of Nearby Stars (CNS5)". Astronomy & Astrophysics. 670: A19. arXiv:2211.01449. Bibcode:2023A&A...670A..19G. doi:10.1051/0004-6361/202244250. S2CID 253264922. Catalogue can be accessed here.
^ Luhman, Kevin L. (May 2014). "Discovery of a ~250 K Brown Dwarf at 2 pc from the Sun". The Astrophysical Journal Letters. 786 (2): 6. arXiv:1404.6501. Bibcode:2014ApJ...786L..18L. doi:10.1088/2041-8205/786/2/L18. S2CID 119102654. L18.
^ Clavin, Whitney; Harrington, J. D. (25 April 2014). "NASA's Spitzer and WISE Telescopes Find Close, Cold Neighbor of Sun". NASA.gov. Archived from the original on 26 April 2014.
Luhman, Kevin L. (January 2014). "A Search for a Distant Companion to the Sun with the Wide-field Infrared Survey Explorer". The Astrophysical Journal. 781 (1): 7. Bibcode:2014ApJ...781....4L. doi:10.1088/0004-637X/781/1/4. S2CID 122930471. 4.
Schneider, Adam C.; Cushing, Michael C.; Kirkpatrick, J. Davy; Gelino, Christopher R. (June 2016). "The Collapse of the Wien Tail in the Coldest Brown Dwarf? Hubble Space Telescope Near-infrared Photometry of WISE J085510.83-071442.5". The Astrophysical Journal Letters. 823 (2): 6. arXiv:1605.05618. Bibcode:2016ApJ...823L..35S. doi:10.3847/2041-8205/823/2/L35. S2CID 13222844. L35.
Faherty, Jacqueline K.; Tinney, C. G.; Skemer, Andrew; Monson, Andrew J. (September 2016). "Indications of Water Clouds in the Coldest Known Brown Dwarf". The Astrophysical Journal Letters. 793 (1): 5. arXiv:1408.4671. Bibcode:2014ApJ...793L..16F. doi:10.1088/2041-8205/793/1/L16. S2CID 119246100. L16.
Skemer, Andrew J.; Morley, Caroline V.; Allers, Katelyn N.; Geballe, Thomas R.; Marley, Mark S.; Fortney, Jonathan J.; et al. (August 2016). "The First Spectrum of the Coldest Brown Dwarf". The Astrophysical Journal. 826 (2): 5. arXiv:1605.04902. Bibcode:2016ApJ...826L..17S. doi:10.3847/2041-8205/826/2/L17. S2CID 59393726. L17.
Morley, Caroline V.; Skemer, Andrew J.; Allers, Katelyn N.; Marley, Mark. S.; Faherty, Jacqueline K.; Visscher, Channon; et al. (May 2018). "An L Band Spectrum of the Coldest Brown Dwarf". The Astrophysical Journal. 858 (2): 17. arXiv:1804.07771. Bibcode:2018ApJ...858...97M. doi:10.3847/1538-4357/aabe8b. S2CID 118954481. 97.
Skemer, Andrew; Miles, Brittany E.; Morley, Caroline; Allers, Katelyn; Bjoraker, Gordon; Carter, Aarynn; Cushing, Michael C.; Faherty, Jacqueline Kelly; Fortney, Jonathan; Freedman, Richard; Geballe, Thomas R.; Line, Michael; Lupu, Roxana; Marley, Mark S.; Martin, Emily (1 March 2021). "Water Ice Clouds and Weather on the Coldest Brown Dwarf". JWST Proposal. Cycle 1: 2327. Bibcode:2021jwst.prop.2327S.
Kühnle, H.; Patapis, P.; Mollière, P.; Tremblin, P.; Matthews, E.; Glauser, A. M.; Whiteford, N.; Vasist, M.; Absil, O. (14 October 2024). "Water depletion and 15NH3 in the atmosphere of the coldest brown dwarf observed with JWST/MIRI". arXiv:2410.10933 .
Rowland, Melanie J.; Morley, Caroline V.; Miles, Brittany E.; Suárez, Genaro; Faherty, Jacqueline K.; Skemer, Andrew J.; Beiler, Samuel A.; Line, Michael R.; Bjoraker, Gordon L. (21 November 2024). "Protosolar D-to-H abundance and one part-per-billion PH₃ in the coldest brown dwarf". arXiv:2411.14541 .
Esplin, T. L.; Luhman, K. L.; Cushing, M. C.; Hardegree-Ullman, K. K.; Trucks, J. L.; Burgasser, A. J.; et al. (November 2016). "Photometric Monitoring of the Coldest Known Brown Dwarf with the Spitzer Space Telescope". The Astrophysical Journal. 832 (1): 5. arXiv:1609.05850. Bibcode:2016ApJ...832...58E. doi:10.3847/0004-637X/832/1/58. S2CID 118611233. 58.
"Working Group on Extrasolar Planets: Definition of a "Planet"". Working Group on Extrasolar Planets of the International Astronomical Union. 28 February 2003. Archived from the original on 16 December 2014. Retrieved 28 April 2014.
Papadopoulos, Leonidas (28 April 2014). "Between the Planet and the Star: A New Ultra-Cold, Sub-Stellar Object Discovered Close to Sun". AmericaSpace.com. Retrieved 28 April 2014.

External links

[http://byw.tools/wiseview#ra=133.786245&dec=-7.244372&size=250&band=3&speed=150.34&minbright=-50.0000&maxbright=500.0000&window=0.5&diff_window=1&linear=1&color=&zoom=7.5&border=0&gaia=0&invert=0&maxdyr=0&scandir=0&neowise=0&diff=0&outer_epochs=0&unique_window=1&smooth_scan=0&shift=0&pmra=0&pmdec=0&synth_a=0&synth_a_sub=0&synth_a_ra=&synth_a_dec=&synth_a_w1=&synth_a_w2=&synth_a_pmra=0&synth_a_pmdec=0&synth_a_mjd=&synth_b=0&synth_b_sub=0&synth_b_ra=&synth_b_dec=&synth_b_w1=&synth_b_w2=&synth_b_pmra=0&synth_b_pmdec=0&synth_b_mjd=

WISE 0855−0714 on WiseView], a tool created by volunteers of the Backyard Worlds citizen science project

Celestial objects within 10 light-years →

Primary member type

Celestial objects by systems.

Main-sequence
stars

A-type	Sirius (Alpha Canis Majoris) (8.7094±0.0054 ly) white dwarf B
G-type	Sun (0 ly) rest of Solar System Alpha Centauri α Cen (Rigil Kentaurus) (4.3441±0.0022 ly) K-type main-sequence star B (Toliman) red dwarf C (Proxima Centauri) (4.2465 ± 0.0003 ly) 2 (5?) planets: Ab?; Bc?; Cb, Cc?, Cd
M-type (red dwarfs)	Barnard's Star (5.9629±0.0004 ly) Wolf 359 (7.8558±0.0013 ly) 1? planets: b? Lalande 21185 (8.3044±0.0007 ly) 2 (3?) planets: b, d?, c Gliese 65 A (BL Ceti) (8.724±0.012 ly) red dwarf B (UV Ceti) Ross 154 (9.7063±0.0009 ly)

Brown dwarfs

L-type	Luhman 16 (6.5029±0.0011 ly) T-type brown dwarf B

Sub-brown dwarfs
and rogue planets

Y-type	WISE 0855−0714 (7.430±0.041 ly)

Constellation of Hydra

Stars

Bayer	α (Alphard) β γ δ ε (Ashlesha) ζ η θ ι (Ukdah) κ λ μ ν ξ ο π ρ σ (Minchir) τ τ υ (Zhang) υ φ φ φ χ χ ψ ω
Flamsteed	1 2 3 6 (a) 9 10 12 (D) 14 15 17 19 20 21 23 24 25 26 27 (P) 28 29 33 (A) 34 37 44 47 48 50 51 (k) 52 (l) 54 (m) 55 56 57 58 (E) 59 60 3 Crt (b) 5 Crt (b) 6 Crt (b) 10 Crt 17 Crt (N) 20 Crt 14 Lib 30 Mon (C) 31 Mon (F) 2 Sex
Variable	R U V W TW EX HS KU LQ V419 V421 V434 V478
HR	3378 3538 3749 (G) 3750 3858 (I) 3862 3919 3923 (Felis) 4162 4328 4339 4445 5265
HD	72659 74156 82943 86226 86264 90156
Gliese	328 357 433 453 3517 3634
Other	HE 1256-2738 HE 1327-2326 LHS 2065 LHS 3003 LTT 3780 2MASS 1114−2618 WASP-25 WASP-36 WASP-84 WISE 0855−0714

Star clusters

Open	Messier 48
Globular	Messier 68 NGC 5694

Nebulae

Planetary	Abell 33 Abell 35 NGC 3242

Galaxies

Messier	83
NGC	2617 2835 2865 2890 2936 2937 2992 3054 3081 3109 3285 3305 3307 3308 3309 3311 3312 3313 3314 3315 3316 3336 3369 3393 3402 3464 3585 3621 3717 3923 4980 4993 5078 5101 5135 5260 5264 5495
Other	3C 196.1 AM 1316-241 Arp 7 ESO 510-G13 GAMA202627 IC 535 MRC 1138-262 Peekaboo Galaxy TN J0924-2201 Tololo 1247-232

Galaxy clusters

Abell	754 3411 3412
Other	Hickson 40

Astronomical events

GW170817

Portals:

Categories:

Revision as of 17:34, 7 December 2024 editNrco0e (talk \| contribs)Extended confirmed users18,650 edits age-mass relationship← Previous edit		Revision as of 17:36, 7 December 2024 edit undoNrco0e (talk \| contribs)Extended confirmed users18,650 edits →Physical parameters Next edit →
Line 87:		Line 87:

	=== Physical parameters ===		=== Physical parameters ===
	The mass and age of WISE 0855−0714 are neither known with certainty, but can be constrained with its known temperature. The age of WISE 0855−0714 depends on its mass; a lower mass would lead to a faster rate of cooling and thus a younger age for WISE 0855−0714, whereas a higher mass would lead to a slower rate of cooling and thus an older age for WISE 0855−0714.<ref name="Luhman2014"/> Assuming an age range of 1–10 billion years, evolutionary models for brown dwarfs predict that WISE 0855−0714 should have a mass between {{Jupiter mass\|3 to 10\|jup=y\|link=yes}}.<ref name="NASA20140425"/><ref name="Luhman2014"/> This mass is in the range of a ] or other ].		The mass and age of WISE 0855−0714 are neither known with certainty, but can be constrained with its known present-day temperature. The age of WISE 0855−0714 depends on its mass; a lower mass would lead to a faster rate of cooling and thus a younger age for WISE 0855−0714, whereas a higher mass would lead to a slower rate of cooling and thus an older age for WISE 0855−0714.<ref name="Luhman2014"/> Assuming an age range of 1–10 billion years, evolutionary models for brown dwarfs predict that WISE 0855−0714 should have a mass between {{Jupiter mass\|3 to 10\|jup=y\|link=yes}}.<ref name="NASA20140425"/><ref name="Luhman2014"/> This mass is in the range of a ] or other ].

	As of 2003, the ] considers an object with a mass above {{Jupiter mass\|13\|jup=y}}, capable of fusing ], to be a brown dwarf. A lighter object and one orbiting another object is considered a planet.<ref name="workinggroup" /> However, if the distinction is based on how the object formed then it might be considered a failed star, a theory advanced for the object ].<ref name="amspace20140428" />		As of 2003, the ] considers an object with a mass above {{Jupiter mass\|13\|jup=y}}, capable of fusing ], to be a brown dwarf. A lighter object and one orbiting another object is considered a planet.<ref name="workinggroup" /> However, if the distinction is based on how the object formed then it might be considered a failed star, a theory advanced for the object ].<ref name="amspace20140428" />

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