WISEPA J062309.94-045624.6: Difference between revisions
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{{Short description|Cold brown dwarf with radio emission}} |
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{{Sky|06|23|09.91|-|04|56|24.27|36.9}} |
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{{Starbox begin |
{{Starbox begin |
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|name= |
| name = WISE J0623-0456 |
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}} |
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{{Starbox image |
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| image = [[File:WISE J0623-0456 VLT HAWKI.jpg|250px]] |
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| caption = [[Very Large Telescope]] image of WISE J0623-0456 |
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| credit = <!--credit for image if the image's use requires them (optional)--> |
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}} |
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{{Starbox observe |
{{Starbox observe |
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| epoch = J2000 |
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|epoch=[[Modified Julian date|MJD]] 55468.97<ref name="Kirkpatrick2011v1"/> |
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| equinox = J2000 |
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|equinox=[[J2000]]<ref name="Kirkpatrick2011v1"/> |
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|constell= |
| constell = [[Monoceros]] |
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|ra={{RA|06|23|09. |
| ra = {{RA|06|23|09.68}} |
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| dec = {{Dec|-04|56|23.52}} |
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{{cite journal |
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}} |
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| last=Kirkpatrick |first=J. Davy |
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| coauthors=Cushing, Michael C.; Gelino, Christopher R.; Griffith, Roger L.; Skrutskie, Michael F.; Marsh, Kenneth A.; Wright, Edward L.; Mainzer, A.; Eisenhardt, Peter R.; McLean, Ian S.; Thompson, Maggie A.; Bauer, James M.; Benford, Dominic J.; Bridge, Carrie R.; Lake, Sean E.; Petty, Sara M.; Stanford, S. A.; Tsai, Chao-Wei; Bailey, Vanessa; Beichman, Charles A.; Bloom, Joshua S.; Bochanski, John J.; Burgasser, Adam J.; Capak, Peter L.; Cruz, Kelle L.; Hinz, Philip M.; Kartaltepe, Jeyhan S.; Knox, Russell P.; Manohar, Swarnima; Masters, Daniel; Morales-Calderon, Maria; Prato, Lisa A.; Rodigas, Timothy J.; Salvato, Mara; Schurr, Steven D.; Scoville, Nicholas Z.; Simcoe, Robert A.; Stapelfeldt, Karl R.; Stern, Daniel; Stock, Nathan D.; Vacca, William D. |
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| title=The First Hundred Brown Dwarfs Discovered by the Wide-field Infrared Survey Explorer (WISE) |
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| year=2011 |
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| journal=[[The Astrophysical Journal Supplement]] |
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| volume=197 | issue=2 | pages=19 |
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| arxiv=1108.4677v1 |
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| doi=10.1088/0067-0049/197/2/19 |
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| bibcode=2011ApJS..197...19K}}</ref> |
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|dec={{DEC|-04|56|24.27}}<ref name="Kirkpatrick2011v1"/>}} |
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{{Starbox character |
{{Starbox character |
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| type = brown dwarf |
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|class=T8<ref name="Kirkpatrick2011v1"/><ref name="Kirkpatrick2012"> |
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| class = T8<ref name="Kirkpatrick2011"/> |
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{{cite journal |
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| variable =rotational variable<ref name="Rose2023"/> |
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| last=Kirkpatrick |first=J. Davy |
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| coauthors=Gelino, Christopher R.; Cushing, Michael C.; Mace, Gregory N.; Griffith, Roger L.; Skrutskie, Michael F.; Marsh, Kenneth A.; Wright, Edward L.; Eisenhardt, Peter R.; McLean, Ian S.; Mainzer, Amanda K.; Burgasser, Adam J.; Tinney, C. G.; Parker, Stephen; Salter, Graeme |
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| title=Further Defining Spectral Type "Y" and Exploring the Low-mass End of the Field Brown Dwarf Mass Function |
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| year=2012 |
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| journal=[[The Astrophysical Journal]] |
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| volume=753 | issue=2 | pages=156 |
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| arxiv=1205.2122 |
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| doi=10.1088/0004-637X/753/2/156 |
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| bibcode=2012ApJ...753..156K}}</ref> |
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|appmag_1_passband=J <small>([[Two Micron All-Sky Survey|2MASS]] filter system)</small> |
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|appmag_1=17.51 ± 0.10<ref name="Kirkpatrick2011v1"/> |
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|appmag_2_passband=H <small>([[Two Micron All-Sky Survey|2MASS]] filter system)</small> |
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|appmag_2=17.31 ± 0.11<ref name="Kirkpatrick2011v1"/> |
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|appmag_3_passband=K<sub>S</sub> <small>([[Two Micron All-Sky Survey|2MASS]] filter system)</small> |
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|appmag_3=17.80 ± 0.22<ref name="Kirkpatrick2011v1"/> |
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}} |
}} |
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{{Starbox astrometry |
{{Starbox astrometry |
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|prop_mo_ra |
| prop_mo_ra = -906.3 ±1.8 |
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|prop_mo_dec |
| prop_mo_dec = 168.8 ±1.6 |
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| |
| pm_footnote = <ref name="Kirkpatrick2021"/> |
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| parallax = 86.5 |
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|dist_pc=~ 11.5<ref name="Kirkpatrick2012"/>}} |
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| p_error = 1.7 |
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| parallax_footnote = <ref name="Kirkpatrick2021"/> |
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}} |
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{{Starbox detail |
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| mass_mj = {{val|13.18|31.26|9.44}}<ref name="Zhang2023"/> {{jupiter mass}}<br/>12.28 ±13.06<ref name="Sanghi2024"/> |
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| radius_rj = {{val|0.78|0.17|0.13}}<ref name="Zhang2023"/> {{ jupiter radius}}<br/>1.11 ±0.14<ref name="Sanghi2024"/> |
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| luminosity_bolometric = 10<sup>{{val|-5.755|0.060|0.049}}</sup><ref name="Zhang2023"/> |
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| gravity = {{val|4.70|0.47|0.42}}<ref name="Zhang2023"/> |
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| temperature = {{val|743|53|51}}<ref name="Zhang2023"/> K<br/>624 ±40<ref name="Sanghi2024"/> |
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| metal = {{val|-0.32|0.18|0.16}}<ref name="Zhang2023"/> |
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| rotation = 1.912 ± 0.005 hours<ref name="Rose2023"/> |
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| rotational_velocity = {{val|60|70|55}}<ref name="Zhang2023"/> km/s<br/>>63<ref name="Rose2023"/> |
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| age_myr = {{val|738|2701|592}}<ref name="Zhang2023"/> |
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}} |
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{{Starbox catalog |
{{Starbox catalog |
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| names =CNS5 1581, WISEA J062309.92-045624.5, WISEP J062309.94-045624.6, EQ J0623-0456 |
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|names=WISEPA J062309.94-045624.6,<ref name="Kirkpatrick2011v1"/> WISE J0623-0456,<ref name="Kirkpatrick2011v1"/> WISE 0623-0456<ref name="Kirkpatrick2011v1"/>}} |
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}} |
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{{Starbox end}} |
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{{Starbox reference |
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| Simbad =WISE+J062309.94-045624.6 |
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}} |
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{{starbox end}} |
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'''WISEPA J062309.94-045624.6''' (also called '''WISE J0623-0456''') is a [[brown dwarf]] of [[T dwarf|spectral type T8]]. It is the coldest brown dwarf with a [[Radio astronomy|radio emission]] (as of October 2024).<ref name="Rose2023"/> |
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WISE J0623-0456 was discovered in 2011 with the [[Wide-field Infrared Survey Explorer]] and a spectrum with the [[NASA Infrared Telescope Facility]] confirmed it as a T8-dwarf.<ref name="Kirkpatrick2011"/> WISE J0623-0456 was identified as a radio source with the [[Australian Square Kilometre Array Pathfinder|Australian SKA Pathfinder]]. Follow-up observations were carried out with the [[Australia Telescope Compact Array|Australian Telescope Compact Array]] (ATCA) and [[MeerKAT]]. The source showed a double-peaked pulsed emission, with a period of 1.889 ± 0.018 hours in ATCA and 1.912 ± 0.005 hours in MeerKAT. The source has a radio luminousity of 10<sup>14.8</sup> [[erg]] s<sup>−1</sup> [[Hertz|Hz]]<sup>−1</sup> and is comparable to other radio bright [[ultracool dwarf|ultracool dwarfs]] with a similar spectral type. The radio emission of WISE J0623-0456 is s strongly circularly polarized and periodic. The researchers therefore think that the radio emission comes from electron cyclotron maser instability (ECMI), which is connected to [[aurora]] in ultracool dwarfs. The researchers find that the magnetic field has a strength of at least B > 0.71 [[Gauss (unit)|kG]].<ref name="Rose2023"/> Another work finds that the shape of the lightcurve can be reproduced by active field lines (AFLs). This work also found that the brown dwarf is likely seen pole-on. The rotation and magnetic axes are misaligned significantly (similar to [[Uranus]] and [[Neptune]]) and the magnetic cycle is likely longer than 6 months. [[Red dwarf|M-]] and [[L dwarf|L-dwarfs]] can produce the observed radio luminosities on their own, but cooler T- and [[Y dwarf|Y-dwarfs]] don't have the necessary [[Stellar corona|corona]] to produce the radio emission. The alternative is that the plasma is fed to the magnetosphere from a companion, similar to the role of [[Io (moon)|Io]] for the aurora on [[Jupiter]].<ref name="Kavanagh2024"/> |
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'''WISEPA J062309.94-045624.6''' (designation abbreviated to '''WISE 0623-0456''', or '''WISE J0623-0456''') is [[brown dwarf]] of [[spectral class]] T8,<ref name="Kirkpatrick2011v1"/><ref name="Kirkpatrick2012"/> located in constellation {{Constel|Mon}} at approximately 38 [[light-year]]s from [[Earth]].<ref name="Kirkpatrick2012"/> |
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== |
== See also == |
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Other T-dwarfs with detected radio emission<ref name="Rose2023"/> |
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'''WISE 0623-0456''' was discovered in 2011 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 2011 Kirkpatrick et al. published a paper in [[The Astrophysical Journal Supplement]], where they presented discovery of 98 new found by WISE [[brown dwarf]] systems with components of [[spectral type]]s M, L, T and Y, among which also was WISE 0623-0456.<ref name="Kirkpatrick2011v1"/><ref name="note 1" group="note">This 98 brown dwarf systems are only among first, not all brown dwarf systems, discovered from data, collected by WISE: six discoveries was published earlier (however, also listed in Kirkpatrick et al. (2011)) in Mainzer et al. (2011) and Burgasser et al. (2011), and the other discoveries was published later.</ref> |
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* [[SIMP J013656.5+093347.3]] T2.5, planetary-mass object |
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* [[2MASS J10475385+2124234]] T6.5 |
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* [[WISEPC J112254.73+255021.5]] T6 |
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* [[WISEPA J101905.63+652954.2]] T5.5+T7.0 |
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== |
== References == |
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{{reflist|refs= |
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[[Trigonometric parallax]] of WISE 0623-0456 is not yet measured. Therefore, there are only distance estimates of this object, obtained by indirect — spectrofotometric — means (see table). |
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<ref name="Kavanagh2024">{{Cite arxiv | eprint=2410.18073 |class=astro-ph |last=Kavanagh |first=Robert D. |title=Unravelling sub-stellar magnetospheres |date=2024-10-23 |last2=Vedantham |first2=Harish K. |last3=Rose |first3=Kovi |last4=Bloot |first4=Sanne}}</ref> |
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'''WISE 0623-0456 distance estimates''' |
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{| class="wikitable" |
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|- |
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! Source !! Parallax, [[milliarcsecond|mas]] !! Distance, [[parsec|pc]] !! Distance, [[light-year|ly]] !! Ref. |
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|- |
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| Kirkpatrick et al. (2011) || || ''~11.3'' || ''~36.9'' || <ref name="Kirkpatrick2011v1"/> |
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|- |
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| Kirkpatrick et al. (2012) || || ''~11.5'' || ''~37.5'' || <ref name="Kirkpatrick2012"/> |
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|} |
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<ref name="Kirkpatrick2011">{{Cite journal |last1=Kirkpatrick |first1=J. Davy |last2=Cushing |first2=Michael C. |last3=Gelino |first3=Christopher R. |last4=Griffith |first4=Roger L. |last5=Skrutskie |first5=Michael F. |last6=Marsh |first6=Kenneth A. |last7=Wright |first7=Edward L. |last8=Mainzer |first8=A. |last9=Eisenhardt |first9=Peter R. |last10=McLean |first10=Ian S. |last11=Thompson |first11=Maggie A. |last12=Bauer |first12=James M. |last13=Benford |first13=Dominic J. |last14=Bridge |first14=Carrie R. |last15=Lake |first15=Sean E. |date=2011-12-01 |title=The First Hundred Brown Dwarfs Discovered by the Wide-field Infrared Survey Explorer (WISE) |url=https://ui.adsabs.harvard.edu/abs/2011ApJS..197...19K/abstract |journal=The Astrophysical Journal Supplement Series |volume=197 |issue=2 |pages=19 |arxiv=1108.4677 |bibcode=2011ApJS..197...19K |doi=10.1088/0067-0049/197/2/19 |issn=0067-0049}}</ref> |
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<small>Non-trigonometric distance estimates are marked in ''italic''.</small> |
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<ref name="Rose2023">{{Cite journal |last1=Rose |first1=Kovi |last2=Pritchard |first2=Joshua |last3=Murphy |first3=Tara |last4=Caleb |first4=Manisha |last5=Dobie |first5=Dougal |last6=Driessen |first6=Laura |last7=Duchesne |first7=Stefan W. |last8=Kaplan |first8=David L. |last9=Lenc |first9=Emil |last10=Wang |first10=Ziteng |date=2023-07-01 |title=Periodic Radio Emission from the T8 Dwarf WISE J062309.94-045624.6 |journal=The Astrophysical Journal |volume=951 |issue=2 |pages=L43 |arxiv=2306.15219 |bibcode=2023ApJ...951L..43R |doi=10.3847/2041-8213/ace188 |doi-access=free |issn=0004-637X}}</ref> |
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==Notes== |
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<references group="note"/> |
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<ref name="Kirkpatrick2021">{{Cite journal |last1=Kirkpatrick |first1=J. Davy |last2=Gelino |first2=Christopher R. |last3=Faherty |first3=Jacqueline K. |last4=Meisner |first4=Aaron M. |last5=Caselden |first5=Dan |last6=Schneider |first6=Adam C. |last7=Marocco |first7=Federico |last8=Cayago |first8=Alfred J. |last9=Smart |first9=R. L. |last10=Eisenhardt |first10=Peter R. |last11=Kuchner |first11=Marc J. |last12=Wright |first12=Edward L. |last13=Cushing |first13=Michael C. |last14=Allers |first14=Katelyn N. |last15=Bardalez Gagliuffi |first15=Daniella C. |date=2021-03-01 |title=The Field Substellar Mass Function Based on the Full-sky 20 pc Census of 525 L, T, and Y Dwarfs |journal=The Astrophysical Journal Supplement Series |volume=253 |issue=1 |pages=7 |arxiv=2011.11616 |bibcode=2021ApJS..253....7K |doi=10.3847/1538-4365/abd107 |doi-access=free |issn=0067-0049}}</ref> |
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==References== |
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{{reflist|colwidth=30em}} |
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<ref name="Zhang2023">{{Cite journal |last1=Zhang |first1=Zhoujian |last2=Liu |first2=Michael C. |last3=Marley |first3=Mark S. |last4=Line |first4=Michael R. |last5=Best |first5=William M. J. |date=2021-11-01 |title=Uniform Forward-modeling Analysis of Ultracool Dwarfs. II. Atmospheric Properties of 55 Late-T Dwarfs |journal=The Astrophysical Journal |volume=921 |issue=1 |pages=95 |arxiv=2105.05256 |bibcode=2021ApJ...921...95Z |doi=10.3847/1538-4357/ac0af7 |doi-access=free |issn=0004-637X}}</ref> |
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{{Nearest star systems|8}} |
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<ref name="Sanghi2024">{{Cite web |last=Sanghi |first=Aniket |date=November 8, 2023 |title=Table of Ultracool Fundamental Properties |url=https://zenodo.org/records/10086810 |access-date=2024-10-05 |website=zenodo|doi=10.5281/zenodo.10086810 }}</ref> |
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[[Category:Brown dwarfs]] |
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[[Category:T-type stars]] |
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[[Category:Monoceros (constellation)]] |
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[[Category:WISE objects]] |
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}} |
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[[Category:T-type brown dwarfs]] |
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{{star-stub}} |
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[[Category:Monoceros]] |
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[[Category:Astronomical radio sources]] |
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Latest revision as of 13:39, 26 October 2024
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Monoceros |
| Right ascension | 06h 23m 09.68s |
| Declination | −04° 56′ 23.52″ |
| Characteristics | |
| Evolutionary stage | brown dwarf |
| Spectral type | T8[1] |
| Variable type | rotational variable[2] |
| Astrometry | |
| Proper motion (μ) | RA: -906.3 ±1.8 mas/yr[3] Dec.: 168.8 ±1.6 mas/yr[3] |
| Parallax (π) | 86.5 ± 1.7 mas[3] |
| Distance | 37.7 ± 0.7 ly (11.6 ± 0.2 pc) |
| Details | |
| Mass | 13.18+31.26 −9.44[4] MJ 12.28 ±13.06[5] MJup |
| Radius | 0.78+0.17 −0.13[4] RJ 1.11 ±0.14[5] RJup |
| Luminosity (bolometric) | 10−5.755+0.060 −0.049[4] L☉ |
| Surface gravity (log g) | 4.70+0.47 −0.42[4] cgs |
| Temperature | 743+53 −51[4] K 624 ±40[5] K |
| Metallicity | −0.32+0.18 −0.16[4] |
| Rotation | 1.912 ± 0.005 hours[2] |
| Rotational velocity (v sin i) | 60+70 −55[4] km/s >63[2] km/s |
| Age | 738+2701 −592[4] Myr |
| Other designations | |
CNS5 1581, WISEA J062309.92-045624.5, WISEP J062309.94-045624.6, EQ J0623-0456 | |
| Database references | |
| SIMBAD | data |
WISEPA J062309.94-045624.6 (also called WISE J0623-0456) is a brown dwarf of spectral type T8. It is the coldest brown dwarf with a radio emission (as of October 2024).[2]
WISE J0623-0456 was discovered in 2011 with the Wide-field Infrared Survey Explorer and a spectrum with the NASA Infrared Telescope Facility confirmed it as a T8-dwarf.[1] WISE J0623-0456 was identified as a radio source with the Australian SKA Pathfinder. Follow-up observations were carried out with the Australian Telescope Compact Array (ATCA) and MeerKAT. The source showed a double-peaked pulsed emission, with a period of 1.889 ± 0.018 hours in ATCA and 1.912 ± 0.005 hours in MeerKAT. The source has a radio luminousity of 1014.8 erg s−1 Hz−1 and is comparable to other radio bright ultracool dwarfs with a similar spectral type. The radio emission of WISE J0623-0456 is s strongly circularly polarized and periodic. The researchers therefore think that the radio emission comes from electron cyclotron maser instability (ECMI), which is connected to aurora in ultracool dwarfs. The researchers find that the magnetic field has a strength of at least B > 0.71 kG.[2] Another work finds that the shape of the lightcurve can be reproduced by active field lines (AFLs). This work also found that the brown dwarf is likely seen pole-on. The rotation and magnetic axes are misaligned significantly (similar to Uranus and Neptune) and the magnetic cycle is likely longer than 6 months. M- and L-dwarfs can produce the observed radio luminosities on their own, but cooler T- and Y-dwarfs don't have the necessary corona to produce the radio emission. The alternative is that the plasma is fed to the magnetosphere from a companion, similar to the role of Io for the aurora on Jupiter.[6]
See also
[edit]Other T-dwarfs with detected radio emission[2]
- SIMP J013656.5+093347.3 T2.5, planetary-mass object
- 2MASS J10475385+2124234 T6.5
- WISEPC J112254.73+255021.5 T6
- WISEPA J101905.63+652954.2 T5.5+T7.0
References
[edit]- ^ a b Kirkpatrick, J. Davy; Cushing, Michael C.; Gelino, Christopher R.; Griffith, Roger L.; Skrutskie, Michael F.; Marsh, Kenneth A.; Wright, Edward L.; Mainzer, A.; Eisenhardt, Peter R.; McLean, Ian S.; Thompson, Maggie A.; Bauer, James M.; Benford, Dominic J.; Bridge, Carrie R.; Lake, Sean E. (2011-12-01). "The First Hundred Brown Dwarfs Discovered by the Wide-field Infrared Survey Explorer (WISE)". The Astrophysical Journal Supplement Series. 197 (2): 19. arXiv:1108.4677. Bibcode:2011ApJS..197...19K. doi:10.1088/0067-0049/197/2/19. ISSN 0067-0049.
- ^ a b c d e f Rose, Kovi; Pritchard, Joshua; Murphy, Tara; Caleb, Manisha; Dobie, Dougal; Driessen, Laura; Duchesne, Stefan W.; Kaplan, David L.; Lenc, Emil; Wang, Ziteng (2023-07-01). "Periodic Radio Emission from the T8 Dwarf WISE J062309.94-045624.6". The Astrophysical Journal. 951 (2): L43. arXiv:2306.15219. Bibcode:2023ApJ...951L..43R. doi:10.3847/2041-8213/ace188. ISSN 0004-637X.
- ^ a b Kirkpatrick, J. Davy; Gelino, Christopher R.; Faherty, Jacqueline K.; Meisner, Aaron M.; Caselden, Dan; Schneider, Adam C.; Marocco, Federico; Cayago, Alfred J.; Smart, R. L.; Eisenhardt, Peter R.; Kuchner, Marc J.; Wright, Edward L.; Cushing, Michael C.; Allers, Katelyn N.; Bardalez Gagliuffi, Daniella C. (2021-03-01). "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): 7. arXiv:2011.11616. Bibcode:2021ApJS..253....7K. doi:10.3847/1538-4365/abd107. ISSN 0067-0049.
- ^ a b c d e f g h Zhang, Zhoujian; Liu, Michael C.; Marley, Mark S.; Line, Michael R.; Best, William M. J. (2021-11-01). "Uniform Forward-modeling Analysis of Ultracool Dwarfs. II. Atmospheric Properties of 55 Late-T Dwarfs". The Astrophysical Journal. 921 (1): 95. arXiv:2105.05256. Bibcode:2021ApJ...921...95Z. doi:10.3847/1538-4357/ac0af7. ISSN 0004-637X.
- ^ a b c Sanghi, Aniket (November 8, 2023). "Table of Ultracool Fundamental Properties". zenodo. doi:10.5281/zenodo.10086810. Retrieved 2024-10-05.
- ^ Kavanagh, Robert D.; Vedantham, Harish K.; Rose, Kovi; Bloot, Sanne (2024-10-23). "Unravelling sub-stellar magnetospheres". arXiv:2410.18073 [astro-ph].