The Luminous Blue Variable RMC 127 as Seen with ALMA and ATCA

C. Agliozzo, C. Trigilio, G. Pignata, N. M. Phillips, R. Nikutta, P. Leto, G. Umana, A. Ingallinera, C. Buemi, F. E. Bauer, R. Paladini, A. Noriega-Crespo, J. L. Prieto, M. Massardi, L. Cerrigone

Resultado de la investigación: Article

1 Cita (Scopus)

Resumen

We present ALMA and ATCA observations of the luminous blue variable RMC 127. The radio maps show for the first time the core of the nebula and evidence that the nebula is strongly asymmetric with a Z-pattern shape. Hints of this morphology are also visible in the archival Hubble Space Telescope image, which overall resembles the radio emission. The emission mechanism in the outer nebula is optically thin free-free in the radio. At high frequencies, a component of point-source emission appears at the position of the star, up to the ALMA frequencies. The rising flux density distribution () of this object suggests thermal emission from the ionized stellar wind and indicates a departure from spherical symmetry with. We examine different scenarios to explain this excess of thermal emission from the wind and show that this can arise from a bipolar outflow, supporting the suggestion by other authors that the stellar wind of RMC 127 is aspherical. We fit the data with two collimated ionized wind models, and we find that the mass-loss rate can be a factor of two or more smaller than in the spherical case. We also fit the photometry obtained by IR space telescopes and deduce that the mid-to far-IR emission must arise from extended, cool () dust within the outer ionized nebula. Finally, we discuss two possible scenarios for the nebular morphology: the canonical single-star expanding shell geometry and a precessing jet model assuming the presence of a companion star.

Idioma originalEnglish
Número de artículo130
PublicaciónAstrophysical Journal
Volumen841
N.º2
DOI
EstadoPublished - 1 jun 2017

Huella dactilar

nebulae
stellar winds
thermal emission
shell stars
radio
companion stars
radio emission
Hubble Space Telescope
point sources
suggestion
photometry
density distribution
flux density
dust
telescopes
stars
point source
symmetry
outflow
geometry

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Citar esto

Agliozzo, C., Trigilio, C., Pignata, G., Phillips, N. M., Nikutta, R., Leto, P., ... Cerrigone, L. (2017). The Luminous Blue Variable RMC 127 as Seen with ALMA and ATCA. Astrophysical Journal, 841(2), [130]. https://doi.org/10.3847/1538-4357/aa72a1
Agliozzo, C. ; Trigilio, C. ; Pignata, G. ; Phillips, N. M. ; Nikutta, R. ; Leto, P. ; Umana, G. ; Ingallinera, A. ; Buemi, C. ; Bauer, F. E. ; Paladini, R. ; Noriega-Crespo, A. ; Prieto, J. L. ; Massardi, M. ; Cerrigone, L. / The Luminous Blue Variable RMC 127 as Seen with ALMA and ATCA. En: Astrophysical Journal. 2017 ; Vol. 841, N.º 2.
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abstract = "We present ALMA and ATCA observations of the luminous blue variable RMC 127. The radio maps show for the first time the core of the nebula and evidence that the nebula is strongly asymmetric with a Z-pattern shape. Hints of this morphology are also visible in the archival Hubble Space Telescope image, which overall resembles the radio emission. The emission mechanism in the outer nebula is optically thin free-free in the radio. At high frequencies, a component of point-source emission appears at the position of the star, up to the ALMA frequencies. The rising flux density distribution () of this object suggests thermal emission from the ionized stellar wind and indicates a departure from spherical symmetry with. We examine different scenarios to explain this excess of thermal emission from the wind and show that this can arise from a bipolar outflow, supporting the suggestion by other authors that the stellar wind of RMC 127 is aspherical. We fit the data with two collimated ionized wind models, and we find that the mass-loss rate can be a factor of two or more smaller than in the spherical case. We also fit the photometry obtained by IR space telescopes and deduce that the mid-to far-IR emission must arise from extended, cool () dust within the outer ionized nebula. Finally, we discuss two possible scenarios for the nebular morphology: the canonical single-star expanding shell geometry and a precessing jet model assuming the presence of a companion star.",
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Agliozzo, C, Trigilio, C, Pignata, G, Phillips, NM, Nikutta, R, Leto, P, Umana, G, Ingallinera, A, Buemi, C, Bauer, FE, Paladini, R, Noriega-Crespo, A, Prieto, JL, Massardi, M & Cerrigone, L 2017, 'The Luminous Blue Variable RMC 127 as Seen with ALMA and ATCA', Astrophysical Journal, vol. 841, n.º 2, 130. https://doi.org/10.3847/1538-4357/aa72a1

The Luminous Blue Variable RMC 127 as Seen with ALMA and ATCA. / Agliozzo, C.; Trigilio, C.; Pignata, G.; Phillips, N. M.; Nikutta, R.; Leto, P.; Umana, G.; Ingallinera, A.; Buemi, C.; Bauer, F. E.; Paladini, R.; Noriega-Crespo, A.; Prieto, J. L.; Massardi, M.; Cerrigone, L.

En: Astrophysical Journal, Vol. 841, N.º 2, 130, 01.06.2017.

Resultado de la investigación: Article

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T1 - The Luminous Blue Variable RMC 127 as Seen with ALMA and ATCA

AU - Agliozzo, C.

AU - Trigilio, C.

AU - Pignata, G.

AU - Phillips, N. M.

AU - Nikutta, R.

AU - Leto, P.

AU - Umana, G.

AU - Ingallinera, A.

AU - Buemi, C.

AU - Bauer, F. E.

AU - Paladini, R.

AU - Noriega-Crespo, A.

AU - Prieto, J. L.

AU - Massardi, M.

AU - Cerrigone, L.

PY - 2017/6/1

Y1 - 2017/6/1

N2 - We present ALMA and ATCA observations of the luminous blue variable RMC 127. The radio maps show for the first time the core of the nebula and evidence that the nebula is strongly asymmetric with a Z-pattern shape. Hints of this morphology are also visible in the archival Hubble Space Telescope image, which overall resembles the radio emission. The emission mechanism in the outer nebula is optically thin free-free in the radio. At high frequencies, a component of point-source emission appears at the position of the star, up to the ALMA frequencies. The rising flux density distribution () of this object suggests thermal emission from the ionized stellar wind and indicates a departure from spherical symmetry with. We examine different scenarios to explain this excess of thermal emission from the wind and show that this can arise from a bipolar outflow, supporting the suggestion by other authors that the stellar wind of RMC 127 is aspherical. We fit the data with two collimated ionized wind models, and we find that the mass-loss rate can be a factor of two or more smaller than in the spherical case. We also fit the photometry obtained by IR space telescopes and deduce that the mid-to far-IR emission must arise from extended, cool () dust within the outer ionized nebula. Finally, we discuss two possible scenarios for the nebular morphology: the canonical single-star expanding shell geometry and a precessing jet model assuming the presence of a companion star.

AB - We present ALMA and ATCA observations of the luminous blue variable RMC 127. The radio maps show for the first time the core of the nebula and evidence that the nebula is strongly asymmetric with a Z-pattern shape. Hints of this morphology are also visible in the archival Hubble Space Telescope image, which overall resembles the radio emission. The emission mechanism in the outer nebula is optically thin free-free in the radio. At high frequencies, a component of point-source emission appears at the position of the star, up to the ALMA frequencies. The rising flux density distribution () of this object suggests thermal emission from the ionized stellar wind and indicates a departure from spherical symmetry with. We examine different scenarios to explain this excess of thermal emission from the wind and show that this can arise from a bipolar outflow, supporting the suggestion by other authors that the stellar wind of RMC 127 is aspherical. We fit the data with two collimated ionized wind models, and we find that the mass-loss rate can be a factor of two or more smaller than in the spherical case. We also fit the photometry obtained by IR space telescopes and deduce that the mid-to far-IR emission must arise from extended, cool () dust within the outer ionized nebula. Finally, we discuss two possible scenarios for the nebular morphology: the canonical single-star expanding shell geometry and a precessing jet model assuming the presence of a companion star.

KW - stars: individual (RMC 127)

KW - stars: mass-loss

KW - stars: massive

KW - stars: rotation

KW - stars: winds outflows

KW - submillimeter: stars

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U2 - 10.3847/1538-4357/aa72a1

DO - 10.3847/1538-4357/aa72a1

M3 - Article

AN - SCOPUS:85020739282

VL - 841

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

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Agliozzo C, Trigilio C, Pignata G, Phillips NM, Nikutta R, Leto P y otros. The Luminous Blue Variable RMC 127 as Seen with ALMA and ATCA. Astrophysical Journal. 2017 jun 1;841(2). 130. https://doi.org/10.3847/1538-4357/aa72a1