S Ori 70: Diferenzas entre revisións

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Liña 11: Liña 11:
| constelación = [[Orión (constelación)|Orión]]
| constelación = [[Orión (constelación)|Orión]]
| ra = {{RA|05|38|10.10}}<ref name=kinematics>{{cita publicación periódica |bibcode=2009AJ....137....1F | título=The Brown Dwarf Kinematics Project I. Proper Motions and Tangential Velocities for a Large Sample of Late-Type M, L, and T Dwarfs | revista=The Astronomical Journal |volume=137 |número=1 |páxinas=1 | autor=Faherty, Jacqueline K.; Burgasser, Adam J.; Cruz, Kelle L.; Shara, Michael M.; Walter, Frederick M.; Gelino, Christopher R. | ano=2009 |doi=10.1088/0004-6256/137/1/1 <!-- |doi-access=free --> }}</ref>
| ra = {{RA|05|38|10.10}}<ref name=kinematics>{{cita publicación periódica |bibcode=2009AJ....137....1F | título=The Brown Dwarf Kinematics Project I. Proper Motions and Tangential Velocities for a Large Sample of Late-Type M, L, and T Dwarfs | revista=The Astronomical Journal |volume=137 |número=1 |páxinas=1 | autor=Faherty, Jacqueline K.; Burgasser, Adam J.; Cruz, Kelle L.; Shara, Michael M.; Walter, Frederick M.; Gelino, Christopher R. | ano=2009 |doi=10.1088/0004-6256/137/1/1 <!-- |doi-access=free --> }}</ref>

| dec = −02° 36′ 00.0″<ref name=kinematics/>
| mag_ap_v = <!--Magnitude aparente (Sistema fotométrico UBV)-->
}}
}}



{{Caixa Características de Estrela
| tipo = <!--Tipo de estrela (por exemplo, estrela na secuencia principal, protoestrela, anana branca, estrela de neutróns etc.)-->
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| clase = T6<ref>{{Cite journal | doi=10.1051/0004-6361:20078600 | arxiv=0710.2776 |bibcode=2008A&A...477..895Z| title=New constraints on the membership of the T dwarf S Ori 70 in theσ Orionis cluster | journal=Astronomy & Astrophysics | volume=477 | issue=3 | pages=895–900 | year=2008 | last1=Zapatero Osorio | first1=M. R. | last2=Béjar | first2=V. J. S. | last3=Bihain | first3=G. | last4=Martín | first4=E. L. | last5=Rebolo | first5=R. | last6=Villó-Pérez | first6=I. | last7=Díaz-Sánchez | first7=A. | last8=Pérez Garrido | first8=A. | last9=Caballero | first9=J. A. | last10=Henning | first10=T. | last11=Mundt | first11=R. | last12=Barrado y Navascués | first12=D. | last13=Bailer-Jones | first13=C. A. L.}}</ref><ref>{{Cite journal |bibcode=2003ApJ...593L.113M |title=Spectroscopic Estimate of Surface Gravity for a Planetary Member in the σ Orionis Cluster |journal=The Astrophysical Journal |volume=593 |issue=2 |pages=L113 |last1=Martín |first1=E. L. |last2=Zapatero Osorio |first2=M. R. |year=2003 |doi=10.1086/378313 |doi-access=free }}</ref>
| mag_ap_1_banda_an = H
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| mag_ap_1 = 20.07<ref name=ramirez/>
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}}



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{{Fin Caixa de Estrela}}




Liña 20: Liña 30:




{{Starbox character
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| class = T6<ref>{{Cite journal | doi=10.1051/0004-6361:20078600 | arxiv=0710.2776 |bibcode=2008A&A...477..895Z| title=New constraints on the membership of the T dwarf S Ori 70 in theσ Orionis cluster | journal=Astronomy & Astrophysics | volume=477 | issue=3 | pages=895–900 | year=2008 | last1=Zapatero Osorio | first1=M. R. | last2=Béjar | first2=V. J. S. | last3=Bihain | first3=G. | last4=Martín | first4=E. L. | last5=Rebolo | first5=R. | last6=Villó-Pérez | first6=I. | last7=Díaz-Sánchez | first7=A. | last8=Pérez Garrido | first8=A. | last9=Caballero | first9=J. A. | last10=Henning | first10=T. | last11=Mundt | first11=R. | last12=Barrado y Navascués | first12=D. | last13=Bailer-Jones | first13=C. A. L.}}</ref><ref>{{Cite journal |bibcode=2003ApJ...593L.113M |title=Spectroscopic Estimate of Surface Gravity for a Planetary Member in the σ Orionis Cluster |journal=The Astrophysical Journal |volume=593 |issue=2 |pages=L113 |last1=Martín |first1=E. L. |last2=Zapatero Osorio |first2=M. R. |year=2003 |doi=10.1086/378313 |doi-access=free }}</ref>
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| appmag_1 = 20.07<ref name=ramirez/>
| appmag_1_passband = H
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}}
{{Starbox astrometry
{{Starbox astrometry
| prop_mo_ra = 10<ref name=kinematics/>
| prop_mo_ra = 10<ref name=kinematics/>
Liña 42: Liña 47:
| Simbad = Mayrit+520267
| Simbad = Mayrit+520267
}}
}}
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{{Fin Caixa de Estrela}}






Revisión como estaba o 14 de xullo de 2021 ás 18:30


S Ori J053810.1-023626

{{Caixa Observación de Estrela

época = 2.000[[ano xuliano|X] equinoccio = 2.000[[ano xuliano|X] constelación = Orión ra = 05h 38m 10.10s[1]

}}


Características
Tipo espectral T6[2][3]
Magnitude aparente (H) 20.07[4]



Modelo:Starbox astrometry Modelo:Starbox detail Modelo:Starbox catalog Modelo:Starbox reference


S Ori 70 or S Ori J053810.1-023626 is a mid-T type astronomical object in the foreground of the σ Orionis cluster, which is approximately 1,150 light-years from Earth. It was discovered on November 24, 2002 by M. R. Zapatero Osorio and E. L. Martin's team at the Roque de los Muchachos Observatory. It has yet to be determined if it is a field brown dwarf or a 3-million-year-old planet that is part of a cluster. Near-infrared spectroscopy images taken 3 years after its discovery led to the first motion measurements for the object. Its behavior is significantly different from what may be expected; it was further described as either a low-gravity atmosphere or an atmosphere with metallicity. The object's small proper motion suggests that it is farther away than expected if it were a single field T dwarf.

Descubrimento

The σ Orionis open cluster has been the focus of Osorio's team observations due to the age of the cluster (approximately 3 to 8 million years). The cluster also has low extinction, its distance is convenient, and it is observed to be rich and dense. Using the 4,2-meter (170-inch) William Herschel Telescope in a pencil-beam deep mini-survey measuring 55 square minutes of arc at a sensitivity of 21 magnitudes in the J and H Bands[5] allowed the team to find S Ori 70. The raw data collected was reduced to IRAF (an acronym for Image Reduction and Analysis Facility), a standard technique used with near-infrared images; after subtracting the sky background and dark current, an extracted object spectrum was derived. It was the faintest and coolest member found in the cluster and was named S Ori 70.

Argument of the initial study

Adam J. Burgasser[6][7] examined the claims of Osorio's T-type brown dwarf discovery and its spectroscopically verified low-mass. A comparison of the J band spectrum between S Ori 70 and other field objects was done. The J band spectrum revealed a distinct triangular-shaped spectral morphology which was previously explained by Osorio and Martin was due to the surface's low gravity. In order to see if similar discrepancies occurred in the T dwarf's behavior, Burgasser's team compared data from the claims of Osorio to that of standard COND models. Identical wavelength scales interpolated through both empirical and model spectra were Gaussian smoothed; this showed that best-fit spectral models can yield skewed gravities for late-type field T dwarfs which resulted in the underestimation of age and mass. Burgasser concluded that S Ori 70 is not a member of the Sigma Ori cluster but is rather a foreground field brown dwarf. Further study of the object suggest that the low gravity was not from the field T dwarf but rather a nearby background star.[6] As of 2009 no direct scientific data have dispelled nor confirmed either conclusion.

It could be the first "free floating" non-stellar planet discovered[8] with a mass of 3 MJ, but needs confirmation.

References

  1. ↑ Faherty, Jacqueline K.; Burgasser, Adam J.; Cruz, Kelle L.; Shara, Michael M.; Walter, Frederick M.; Gelino, Christopher R. (2009). "The Brown Dwarf Kinematics Project I. Proper Motions and Tangential Velocities for a Large Sample of Late-Type M, L, and T Dwarfs". The Astronomical Journal 137 (1): 1. Bibcode:2009AJ....137....1F. doi:10.1088/0004-6256/137/1/1. 
  2. ↑ Zapatero Osorio, M. R.; Béjar, V. J. S.; Bihain, G.; Martín, E. L.; Rebolo, R.; Villó-Pérez, I.; Díaz-Sánchez, A.; Pérez Garrido, A.; Caballero, J. A.; Henning, T.; Mundt, R.; Barrado y Navascués, D.; Bailer-Jones, C. A. L. (2008). "New constraints on the membership of the T dwarf S Ori 70 in theσ Orionis cluster". Astronomy & Astrophysics 477 (3): 895–900. Bibcode:2008A&A...477..895Z. arXiv:0710.2776. doi:10.1051/0004-6361:20078600. 
  3. ↑ Martín, E. L.; Zapatero Osorio, M. R. (2003). "Spectroscopic Estimate of Surface Gravity for a Planetary Member in the σ Orionis Cluster". The Astrophysical Journal 593 (2): L113. Bibcode:2003ApJ...593L.113M. doi:10.1086/378313.  Parámetro descoñecido |doi-access= ignorado (Axuda)
  4. ↑ Erro no código da cita: Etiqueta <ref> non válida; non se forneceu texto para as referencias de nome ramirez
  5. ↑ Modelo:Cite arxiv
  6. ↑ 6,0 6,1 Burgasser, Adam J.; Kirkpatrick, J. Davy; McGovern, Mark R.; McLean, Ian S.; Prato, L.; Reid, I. Neill (2004). "S Orionis 70: Just a Foreground Field Brown Dwarf?". The Astrophysical Journal 604 (2): 827. Bibcode:2004ApJ...604..827B. doi:10.1086/382129. 
  7. ↑ "T dwarfs". MIT.edu. Consultado o 2010-02-08. 
  8. ↑ Erro no código da cita: Etiqueta <ref> non válida; non se forneceu texto para as referencias de nome silverstar
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