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WISE 0535−7500: Difference between revisions

Coordinates: Sky map 05h 35m 16.8s, −75° 00′ 24.9″
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{{Sky|05|35|16.8|-|75|00|24.9|69}}
#REDIRECT [[List of brown dwarfs]]
{{Starbox begin
|name=WISE J053516.80−750024.9}}
{{Starbox observe
|epoch=[[J2000]]{{r|Kirkpatrick2012}}
|equinox=[[J2000]]{{r|Kirkpatrick2012}}
|constell={{Constel|Men}}
|ra={{RA|05|35|16.8}}{{r|Kirkpatrick2012}}
|dec={{DEC|-75|00|24.9}}{{r|Kirkpatrick2012}}}}
{{Starbox character
|class=≥Y1{{r|Kirkpatrick2012}}
|appmag_1_passband=J <small>([[Mauna Kea Observatory|MKO]]-NIR filter system)</small>
|appmag_1=>21.1{{r|Kirkpatrick2012}}
|appmag_3_passband=H <small>([[Mauna Kea Observatory|MKO]]-NIR filter system)</small>
|appmag_3=>21.6{{r|Kirkpatrick2012}}
}}
{{Starbox astrometry
|prop_mo_ra=-310 ± 128{{r|Marsh2013}}
|prop_mo_dec=159 ± 92{{r|Marsh2013}}
|parallax=250
|p_error=79
|parallax_footnote={{r|Marsh2013}}
|dist_ly=13.0{{±|6.0|3.1}}{{r|Paterson2015}}
|dist_pc=4.0{{±|1.9|-0.9}}{{r|Paterson2015}}
}}
{{Starbox catalog
|names=[[Wide-field Infrared Survey Explorer|WISE]] J053516.80−750024.9,{{r|Kirkpatrick2012}}<br>[[Wide-field Infrared Survey Explorer|WISE]] 0535−7500{{r|Kirkpatrick2012}}}}
{{Starbox end}}

[[File:HR-diagram.jpg|thumb|Hertzsprung-Russell diagram of all the nearest stars out to Gliese 1, as well as most brown dwarfs and some planets.,|Hertzsprung-Russell diagram of all the nearest stars out to Gliese 1, as well as most brown dwarfs and some planets. WISE 0535−7500 is at bottom right]]

'''WISE J053516.80−750024.9''' (designation abbreviated to '''WISE 0535−7500''') is either a [[brown dwarf]] or a [[free planet]]. It has [[spectral class]] ≥Y1 and is {{r|Kirkpatrick2012}} located in constellation {{Constel|Men}}. It is estimated to be 13 [[light-year]]s from [[Earth]].{{r|Paterson2015}}. As of October 2015, that makes it the third nearest Y dwarf, after [[WISE 0855−0714]] and [[WISE 0350−5658]]. It is nearer than all but four naked eye stars, and the 31st [[List of nearest stars and brown dwarfs|nearest star system]] to the Solar System. If a [[free planet]], it is the second nearest, the nearest being [[WISE 0855−0714]]. If a brown dwarf, then it is the ninth nearest brown dwarf.

==Discovery==
'''WISE 0535−7500''' was discovered in 2012 by [[J. Davy Kirkpatrick]] et al. from data, collected by [[Wide-field Infrared Survey Explorer|Wide-field Infrared Survey Explorer (WISE)]] [[Earth-orbit]]ing [[satellite]] — [[National Aeronautics and Space Administration|NASA]] [[infrared|infrared-wavelength]] 40 [[centimeter|cm]] (16 [[inch|in]]) [[space observatory|space telescope]], which mission lasted from December 2009 to February 2011. In 2012 Kirkpatrick et al. published a paper in [[The Astrophysical Journal]], where they presented the discovery of seven new found by WISE [[brown dwarf]]s of [[spectral type]] Y, among which also was WISE 0535−7500.{{r|Kirkpatrick2012}}

==Distance==
[[Trigonometric parallax]] of WISE 0535−7500 is 0.250 ± 0.079 [[arcsecond|arcsec]], corresponding to a direct inversion distance{{r|Paterson2015}} of {{nowrap|4.0{{±|1.9|-0.9}} [[parsec|pc]]}} and {{nowrap|13.0{{±|6.1|3.1}} [[light-year|ly]]}}.

'''WISE 0535−7500 distance estimates'''
{| class="wikitable"
|-
! Source !! Parallax, [[milliarcsecond|mas]] !! Distance, [[parsec|pc]] !! Distance, [[light-year|ly]] !! Ref.
|-
| Marsh et al. (2013)<br><small>(according Kirkpatrick et al. (2012))</small> || 170 ± 44 || 5.9{{±|2.1|1.2}} || 19.2{{±|6.7|3.9}} || {{r|Kirkpatrick2012}}
|-
| Marsh et al. (2013) || 250 ± 79 || 21{{±|13|11}} || 68.5{{±|42.4|35.9}} || {{r|Marsh2013}}
|-
| Paterson (2015) || '''250 ± 79''' || '''4.0{{±|1.9|-0.9}}''' || '''13.0{{±|6.1|3.1}}''' || {{r|Paterson2015}}
|}
<small>Non-trigonometric distance estimates are marked in ''italic''. The best estimate is marked in '''bold'''.</small>

==Y dwarf==
Brown dwarfs are defined as substellar objects that have at some time in their lives burnt deuterium in their interior. The borderline between a brown dwarf and a planet is conventionally taken to be 13 times the mass of Jupiter. All brown dwarfs are either L dwarfs, T dwarfs or Y dwarfs, in order of decreasing temperature. An increasing number after the letter in the spectral type also means decreasing temperature, a Y2 dwarf is cooler than a Y1 dwarf is cooler than a Y0 dwarf. Planets can also be L dwarfs, T dwarfs or Y dwarfs{{r|Reid2008}}.

If planets are L dwarfs or T dwarfs then they must be both young (younger than 350 million years) and heavy{{r|Reid2008}}. The cooler a Y dwarf, the higher the likelihood that it’s a planet. WISE 0535-7500 is the second nearest Y dwarf that could be of a type cooler than Y1, so could easily be the second nearest [[free planet]] to Earth. Of the two nearer Y dwarfs, [[WISE 0855−0714]] has an effective temperature below the freezing point of water, and [[WISE 0350−5658]] has an effective temperature above the boiling point of water. WISE 0535−7500 is of a spectral type between that of [[WISE 0855−0714]] and [[WISE 0350−5658]] so the possibility exists that it may in the correct temperature range for liquid water to exist on its surface.

==References==
{{reflist|colwidth=30em|refs=
<ref name="Kirkpatrick2012">{{cite doi|10.1088/0004-637X/753/2/156}}</ref>
<ref name="Marsh2013">{{cite doi|10.1088/0004-637X/762/2/119}}</ref>
<ref name="Paterson2015"> Paterson, David.A. [http://www.keepandshare.com/doc15/6950/topicsinastronomytopic8 "Topics in Astronomy: Topic 8. Inappropriateness of the Lutz-Kelker equation for brown dwarfs"]. Retrieved on 24 September 2015.</ref>
<ref name="Reid2008"> I. Neill Reid and Stanimir A. Metchev, Chapter 5: The Brown Dwarf – Exoplanet Connection, in John W. Mason (ed.) Exoplanets: Detection, Formation, Properties, Habitability; Springer, Berlin, 2008.</ref>
}}

{{Nearest star systems|14}}

{{Stars of Mensa}}

{{DEFAULTSORT:WISE 0535-7500}}
[[Category:Brown dwarfs]]
[[Category:Y-type stars]]
[[Category:Mensa (constellation)]]
[[Category:Astronomical objects discovered in 2012|20120515]]
[[Category:WISE objects]]
[[Category:Objects within 100 ly of Earth|68.5]]


{{star-stub}}

Revision as of 08:09, 3 October 2015

WISE J053516.80−750024.9
Observation data
Epoch J2000[1]      Equinox J2000[1]
Constellation Template:Constel
Right ascension 05h 35m 16.8s[1]
Declination −75° 00′ 24.9″[1]
Characteristics
Spectral type ≥Y1[1]
Apparent magnitude (J (MKO-NIR filter system)) >21.1[1]
Apparent magnitude (H (MKO-NIR filter system)) >21.6[1]
Astrometry
Proper motion (μ) RA: -310 ± 128[2] mas/yr
Dec.: 159 ± 92[2] mas/yr
Parallax (π)250 ± 79 mas[2]
Distance13.0+6.0
−3.1[3] ly
(4.0+1.9
−-0.9[3] pc)
Other designations
WISE J053516.80−750024.9,[1]
WISE 0535−7500[1]
Hertzsprung-Russell diagram of all the nearest stars out to Gliese 1, as well as most brown dwarfs and some planets. WISE 0535−7500 is at bottom right

WISE J053516.80−750024.9 (designation abbreviated to WISE 0535−7500) is either a brown dwarf or a free planet. It has spectral class ≥Y1 and is [1] located in constellation Template:Constel. It is estimated to be 13 light-years from Earth.[3]. As of October 2015, that makes it the third nearest Y dwarf, after WISE 0855−0714 and WISE 0350−5658. It is nearer than all but four naked eye stars, and the 31st nearest star system to the Solar System. If a free planet, it is the second nearest, the nearest being WISE 0855−0714. If a brown dwarf, then it is the ninth nearest brown dwarf.

Discovery

WISE 0535−7500 was discovered in 2012 by J. Davy Kirkpatrick et al. from data, collected by Wide-field Infrared Survey Explorer (WISE) Earth-orbiting satellite — NASA infrared-wavelength 40 cm (16 in) space telescope, which mission lasted from December 2009 to February 2011. In 2012 Kirkpatrick et al. published a paper in The Astrophysical Journal, where they presented the discovery of seven new found by WISE brown dwarfs of spectral type Y, among which also was WISE 0535−7500.[1]

Distance

Trigonometric parallax of WISE 0535−7500 is 0.250 ± 0.079 arcsec, corresponding to a direct inversion distance[3] of 4.0+1.9
−-0.9 pc and 13.0+6.1
−3.1 ly.

WISE 0535−7500 distance estimates

Source Parallax, mas Distance, pc Distance, ly Ref.
Marsh et al. (2013)
(according Kirkpatrick et al. (2012))		 170 ± 44 5.9+2.1
−1.2		 19.2+6.7
−3.9		 [1]
Marsh et al. (2013) 250 ± 79 21+13
−11		 68.5+42.4
−35.9		 [2]
Paterson (2015) 250 ± 79 4.0+1.9
−-0.9		 13.0+6.1
−3.1		 [3]

Non-trigonometric distance estimates are marked in italic. The best estimate is marked in bold.

Y dwarf

Brown dwarfs are defined as substellar objects that have at some time in their lives burnt deuterium in their interior. The borderline between a brown dwarf and a planet is conventionally taken to be 13 times the mass of Jupiter. All brown dwarfs are either L dwarfs, T dwarfs or Y dwarfs, in order of decreasing temperature. An increasing number after the letter in the spectral type also means decreasing temperature, a Y2 dwarf is cooler than a Y1 dwarf is cooler than a Y0 dwarf. Planets can also be L dwarfs, T dwarfs or Y dwarfs[4].

If planets are L dwarfs or T dwarfs then they must be both young (younger than 350 million years) and heavy[4]. The cooler a Y dwarf, the higher the likelihood that it’s a planet. WISE 0535-7500 is the second nearest Y dwarf that could be of a type cooler than Y1, so could easily be the second nearest free planet to Earth. Of the two nearer Y dwarfs, WISE 0855−0714 has an effective temperature below the freezing point of water, and WISE 0350−5658 has an effective temperature above the boiling point of water. WISE 0535−7500 is of a spectral type between that of WISE 0855−0714 and WISE 0350−5658 so the possibility exists that it may in the correct temperature range for liquid water to exist on its surface.

References

  1. ^ a b c d e f g h i j k l Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1088/0004-637X/753/2/156, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1088/0004-637X/753/2/156 instead.
  2. ^ a b c d Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1088/0004-637X/762/2/119, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1088/0004-637X/762/2/119 instead.
  3. ^ a b c d e Paterson, David.A. "Topics in Astronomy: Topic 8. Inappropriateness of the Lutz-Kelker equation for brown dwarfs". Retrieved on 24 September 2015.
  4. ^ a b I. Neill Reid and Stanimir A. Metchev, Chapter 5: The Brown Dwarf – Exoplanet Connection, in John W. Mason (ed.) Exoplanets: Detection, Formation, Properties, Habitability; Springer, Berlin, 2008.


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