New ATCA, ALMA and VISIR observations of the candidate LBV SK-67 266 (S61): The nebular mass from modelling 3D density distributions

C. Agliozzo, R. Nikutta, G. Pignata, N. M. Phillips, A. Ingallinera, C. Buemi, G. Umana, P. Leto, C. Trigilio, A. Noriega-Crespo, R. Paladini, F. Bufano, F. Cavallaro

Resultado de la investigación: Article

4 Citas (Scopus)

Resumen

We present new observations of the nebula around the Magellanic candidate Luminous Blue Variable S61. These comprise high-resolution data acquired with the Australia Telescope Compact Array (ATCA), the Atacama Large Millimetre/Submillimetre Array (ALMA), and the VLT Imager and Spectrometer for mid Infrared (VISIR) at the Very Large Telescope. The nebula was detected only in the radio, up to 17 GHz. The 17 GHz ATCA map, with 0.8 arcsec resolution, allowed a morphological comparison with the Ha Hubble Space Telescope image. The radio nebula resembles a spherical shell, as in the optical. The spectral index map indicates that the radio emission is due to free-free transitions in the ionized, optically thin gas, but there are hints of inhomogeneities. We present our new public code RHOCUBE to model 3D density distributions and determine via Bayesian inference the nebula's geometric parameters. We applied the code to model the electron density distribution in the S61 nebula. We found that different distributions fit the data, but all of them converge to the same ionized mass, ~0.1M, which is an order of magnitude smaller than previous estimates. We show how the nebula models can be used to derive the mass-loss history with high-temporal resolution. The nebula was probably formed through stellar winds, rather than eruptions. From the ALMA and VISIR non-detections, plus the derived extinction map, we deduce that the infrared emission observed by space telescopes must arise from extended, diffuse dust within the ionized region.

Idioma originalEnglish
Páginas (desde-hasta)213-227
Número de páginas15
PublicaciónMonthly Notices of the Royal Astronomical Society
Volumen466
N.º1
DOI
EstadoPublished - 2017

Huella dactilar

nebulae
density distribution
spectrometer
telescopes
spectrometers
radio
modeling
inhomogeneity
electron density
volcanic eruption
extinction
shell
dust
high resolution
spherical shells
stellar winds
radio emission
distribution
temporal resolution
inference

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Citar esto

Agliozzo, C. ; Nikutta, R. ; Pignata, G. ; Phillips, N. M. ; Ingallinera, A. ; Buemi, C. ; Umana, G. ; Leto, P. ; Trigilio, C. ; Noriega-Crespo, A. ; Paladini, R. ; Bufano, F. ; Cavallaro, F. / New ATCA, ALMA and VISIR observations of the candidate LBV SK-67 266 (S61) : The nebular mass from modelling 3D density distributions. En: Monthly Notices of the Royal Astronomical Society. 2017 ; Vol. 466, N.º 1. pp. 213-227.
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title = "New ATCA, ALMA and VISIR observations of the candidate LBV SK-67 266 (S61): The nebular mass from modelling 3D density distributions",
abstract = "We present new observations of the nebula around the Magellanic candidate Luminous Blue Variable S61. These comprise high-resolution data acquired with the Australia Telescope Compact Array (ATCA), the Atacama Large Millimetre/Submillimetre Array (ALMA), and the VLT Imager and Spectrometer for mid Infrared (VISIR) at the Very Large Telescope. The nebula was detected only in the radio, up to 17 GHz. The 17 GHz ATCA map, with 0.8 arcsec resolution, allowed a morphological comparison with the Ha Hubble Space Telescope image. The radio nebula resembles a spherical shell, as in the optical. The spectral index map indicates that the radio emission is due to free-free transitions in the ionized, optically thin gas, but there are hints of inhomogeneities. We present our new public code RHOCUBE to model 3D density distributions and determine via Bayesian inference the nebula's geometric parameters. We applied the code to model the electron density distribution in the S61 nebula. We found that different distributions fit the data, but all of them converge to the same ionized mass, ~0.1M⊙, which is an order of magnitude smaller than previous estimates. We show how the nebula models can be used to derive the mass-loss history with high-temporal resolution. The nebula was probably formed through stellar winds, rather than eruptions. From the ALMA and VISIR non-detections, plus the derived extinction map, we deduce that the infrared emission observed by space telescopes must arise from extended, diffuse dust within the ionized region.",
keywords = "Circumstellar matter, Methods: statistical, Radio continuum: stars, Stars: individual: (SK -67 266), Stars: mass-loss, Stars: massive",
author = "C. Agliozzo and R. Nikutta and G. Pignata and Phillips, {N. M.} and A. Ingallinera and C. Buemi and G. Umana and P. Leto and C. Trigilio and A. Noriega-Crespo and R. Paladini and F. Bufano and F. Cavallaro",
year = "2017",
doi = "10.1093/mnras/stw2986",
language = "English",
volume = "466",
pages = "213--227",
journal = "Monthly Notices of the Royal Astronomical Society",
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Agliozzo, C, Nikutta, R, Pignata, G, Phillips, NM, Ingallinera, A, Buemi, C, Umana, G, Leto, P, Trigilio, C, Noriega-Crespo, A, Paladini, R, Bufano, F & Cavallaro, F 2017, 'New ATCA, ALMA and VISIR observations of the candidate LBV SK-67 266 (S61): The nebular mass from modelling 3D density distributions', Monthly Notices of the Royal Astronomical Society, vol. 466, n.º 1, pp. 213-227. https://doi.org/10.1093/mnras/stw2986

New ATCA, ALMA and VISIR observations of the candidate LBV SK-67 266 (S61) : The nebular mass from modelling 3D density distributions. / Agliozzo, C.; Nikutta, R.; Pignata, G.; Phillips, N. M.; Ingallinera, A.; Buemi, C.; Umana, G.; Leto, P.; Trigilio, C.; Noriega-Crespo, A.; Paladini, R.; Bufano, F.; Cavallaro, F.

En: Monthly Notices of the Royal Astronomical Society, Vol. 466, N.º 1, 2017, p. 213-227.

Resultado de la investigación: Article

TY - JOUR

T1 - New ATCA, ALMA and VISIR observations of the candidate LBV SK-67 266 (S61)

T2 - The nebular mass from modelling 3D density distributions

AU - Agliozzo, C.

AU - Nikutta, R.

AU - Pignata, G.

AU - Phillips, N. M.

AU - Ingallinera, A.

AU - Buemi, C.

AU - Umana, G.

AU - Leto, P.

AU - Trigilio, C.

AU - Noriega-Crespo, A.

AU - Paladini, R.

AU - Bufano, F.

AU - Cavallaro, F.

PY - 2017

Y1 - 2017

N2 - We present new observations of the nebula around the Magellanic candidate Luminous Blue Variable S61. These comprise high-resolution data acquired with the Australia Telescope Compact Array (ATCA), the Atacama Large Millimetre/Submillimetre Array (ALMA), and the VLT Imager and Spectrometer for mid Infrared (VISIR) at the Very Large Telescope. The nebula was detected only in the radio, up to 17 GHz. The 17 GHz ATCA map, with 0.8 arcsec resolution, allowed a morphological comparison with the Ha Hubble Space Telescope image. The radio nebula resembles a spherical shell, as in the optical. The spectral index map indicates that the radio emission is due to free-free transitions in the ionized, optically thin gas, but there are hints of inhomogeneities. We present our new public code RHOCUBE to model 3D density distributions and determine via Bayesian inference the nebula's geometric parameters. We applied the code to model the electron density distribution in the S61 nebula. We found that different distributions fit the data, but all of them converge to the same ionized mass, ~0.1M⊙, which is an order of magnitude smaller than previous estimates. We show how the nebula models can be used to derive the mass-loss history with high-temporal resolution. The nebula was probably formed through stellar winds, rather than eruptions. From the ALMA and VISIR non-detections, plus the derived extinction map, we deduce that the infrared emission observed by space telescopes must arise from extended, diffuse dust within the ionized region.

AB - We present new observations of the nebula around the Magellanic candidate Luminous Blue Variable S61. These comprise high-resolution data acquired with the Australia Telescope Compact Array (ATCA), the Atacama Large Millimetre/Submillimetre Array (ALMA), and the VLT Imager and Spectrometer for mid Infrared (VISIR) at the Very Large Telescope. The nebula was detected only in the radio, up to 17 GHz. The 17 GHz ATCA map, with 0.8 arcsec resolution, allowed a morphological comparison with the Ha Hubble Space Telescope image. The radio nebula resembles a spherical shell, as in the optical. The spectral index map indicates that the radio emission is due to free-free transitions in the ionized, optically thin gas, but there are hints of inhomogeneities. We present our new public code RHOCUBE to model 3D density distributions and determine via Bayesian inference the nebula's geometric parameters. We applied the code to model the electron density distribution in the S61 nebula. We found that different distributions fit the data, but all of them converge to the same ionized mass, ~0.1M⊙, which is an order of magnitude smaller than previous estimates. We show how the nebula models can be used to derive the mass-loss history with high-temporal resolution. The nebula was probably formed through stellar winds, rather than eruptions. From the ALMA and VISIR non-detections, plus the derived extinction map, we deduce that the infrared emission observed by space telescopes must arise from extended, diffuse dust within the ionized region.

KW - Circumstellar matter

KW - Methods: statistical

KW - Radio continuum: stars

KW - Stars: individual: (SK -67 266)

KW - Stars: mass-loss

KW - Stars: massive

UR - http://www.scopus.com/inward/record.url?scp=85018318150&partnerID=8YFLogxK

U2 - 10.1093/mnras/stw2986

DO - 10.1093/mnras/stw2986

M3 - Article

AN - SCOPUS:85018318150

VL - 466

SP - 213

EP - 227

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 1

ER -