A massive nebula around the luminous blue variable star RMC 143 revealed by ALMA

C. Agliozzo, A. Mehner, N. M. Phillips, P. Leto, J. H. Groh, A. Noriega-Crespo, C. Buemi, F. Cavallaro, L. Cerrigone, A. Ingallinera, R. Paladini, G. Pignata, C. Trigilio, G. Umana

Resultado de la investigación: Article

Resumen

The luminous blue variable (LBV) RMC 143 is located in the outskirts of the 30 Doradus complex, a region rich with interstellar material and hot luminous stars. We report the 3σ sub-millimetre detection of its circumstellar nebula with ALMA. The observed morphology in the sub-millimetre is different than previously observed with HST and ATCA in the optical and centimetre wavelength regimes. The spectral energy distribution (SED) of RMC 143 suggests that two emission mechanisms contribute to the sub-mm emission: optically thin bremsstrahlung and dust. Both the extinction map and the SED are consistent with a dusty massive nebula with a dust mass of 0.055 ± 0.018â M· (assuming κ850 = 1.7 cm2 g-1). To date, RMC 143 has the most dusty LBV nebula observed in the Magellanic Clouds. We have also re-examined the LBV classification of RMC 143 based on VLT/X-shooter spectra obtained in 2015/16 and a review of the publication record. The radiative transfer code CMFGEN is used to derive its fundamental stellar parameters. We find an effective temperature of ∼8500 K, luminosity of log(L/L·) = 5.32, and a relatively high mass-loss rate of 1.0 × 10-5 M· yr-1. The luminosity is much lower than previously thought, which implies that the current stellar mass of ∼8 M· is comparable to its nebular mass of ∼5.5â M· (from an assumed gas-To-dust ratio of 100), suggesting that the star has lost a large fraction of its initial mass in past LBV eruptions or binary interactions. While the star may have been hotter in the past, it is currently not hot enough to ionize its circumstellar nebula. We propose that the nebula is ionized externally by the hot stars in the 30 Doradus star-forming region.

Idioma originalEnglish
Número de artículoA126
PublicaciónAstronomy and Astrophysics
Volumen626
DOI
EstadoPublished - 1 jun 2019

Huella dactilar

blue stars
variable stars
nebulae
stars
dust
spectral energy distribution
luminosity
hot stars
Magellanic clouds
stellar mass
volcanic eruptions
bremsstrahlung
radiative transfer
energy
extinction
volcanic eruption
wavelength
gases
gas
wavelengths

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Citar esto

Agliozzo, C., Mehner, A., Phillips, N. M., Leto, P., Groh, J. H., Noriega-Crespo, A., ... Umana, G. (2019). A massive nebula around the luminous blue variable star RMC 143 revealed by ALMA. Astronomy and Astrophysics, 626, [A126]. https://doi.org/10.1051/0004-6361/201935239
Agliozzo, C. ; Mehner, A. ; Phillips, N. M. ; Leto, P. ; Groh, J. H. ; Noriega-Crespo, A. ; Buemi, C. ; Cavallaro, F. ; Cerrigone, L. ; Ingallinera, A. ; Paladini, R. ; Pignata, G. ; Trigilio, C. ; Umana, G. / A massive nebula around the luminous blue variable star RMC 143 revealed by ALMA. En: Astronomy and Astrophysics. 2019 ; Vol. 626.
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abstract = "The luminous blue variable (LBV) RMC 143 is located in the outskirts of the 30 Doradus complex, a region rich with interstellar material and hot luminous stars. We report the 3σ sub-millimetre detection of its circumstellar nebula with ALMA. The observed morphology in the sub-millimetre is different than previously observed with HST and ATCA in the optical and centimetre wavelength regimes. The spectral energy distribution (SED) of RMC 143 suggests that two emission mechanisms contribute to the sub-mm emission: optically thin bremsstrahlung and dust. Both the extinction map and the SED are consistent with a dusty massive nebula with a dust mass of 0.055 ± 0.018{\^a} M· (assuming κ850 = 1.7 cm2 g-1). To date, RMC 143 has the most dusty LBV nebula observed in the Magellanic Clouds. We have also re-examined the LBV classification of RMC 143 based on VLT/X-shooter spectra obtained in 2015/16 and a review of the publication record. The radiative transfer code CMFGEN is used to derive its fundamental stellar parameters. We find an effective temperature of ∼8500 K, luminosity of log(L/L·) = 5.32, and a relatively high mass-loss rate of 1.0 × 10-5 M· yr-1. The luminosity is much lower than previously thought, which implies that the current stellar mass of ∼8 M· is comparable to its nebular mass of ∼5.5{\^a} M· (from an assumed gas-To-dust ratio of 100), suggesting that the star has lost a large fraction of its initial mass in past LBV eruptions or binary interactions. While the star may have been hotter in the past, it is currently not hot enough to ionize its circumstellar nebula. We propose that the nebula is ionized externally by the hot stars in the 30 Doradus star-forming region.",
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author = "C. Agliozzo and A. Mehner and Phillips, {N. M.} and P. Leto and Groh, {J. H.} and A. Noriega-Crespo and C. Buemi and F. Cavallaro and L. Cerrigone and A. Ingallinera and R. Paladini and G. Pignata and C. Trigilio and G. Umana",
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Agliozzo, C, Mehner, A, Phillips, NM, Leto, P, Groh, JH, Noriega-Crespo, A, Buemi, C, Cavallaro, F, Cerrigone, L, Ingallinera, A, Paladini, R, Pignata, G, Trigilio, C & Umana, G 2019, 'A massive nebula around the luminous blue variable star RMC 143 revealed by ALMA', Astronomy and Astrophysics, vol. 626, A126. https://doi.org/10.1051/0004-6361/201935239

A massive nebula around the luminous blue variable star RMC 143 revealed by ALMA. / Agliozzo, C.; Mehner, A.; Phillips, N. M.; Leto, P.; Groh, J. H.; Noriega-Crespo, A.; Buemi, C.; Cavallaro, F.; Cerrigone, L.; Ingallinera, A.; Paladini, R.; Pignata, G.; Trigilio, C.; Umana, G.

En: Astronomy and Astrophysics, Vol. 626, A126, 01.06.2019.

Resultado de la investigación: Article

TY - JOUR

T1 - A massive nebula around the luminous blue variable star RMC 143 revealed by ALMA

AU - Agliozzo, C.

AU - Mehner, A.

AU - Phillips, N. M.

AU - Leto, P.

AU - Groh, J. H.

AU - Noriega-Crespo, A.

AU - Buemi, C.

AU - Cavallaro, F.

AU - Cerrigone, L.

AU - Ingallinera, A.

AU - Paladini, R.

AU - Pignata, G.

AU - Trigilio, C.

AU - Umana, G.

PY - 2019/6/1

Y1 - 2019/6/1

N2 - The luminous blue variable (LBV) RMC 143 is located in the outskirts of the 30 Doradus complex, a region rich with interstellar material and hot luminous stars. We report the 3σ sub-millimetre detection of its circumstellar nebula with ALMA. The observed morphology in the sub-millimetre is different than previously observed with HST and ATCA in the optical and centimetre wavelength regimes. The spectral energy distribution (SED) of RMC 143 suggests that two emission mechanisms contribute to the sub-mm emission: optically thin bremsstrahlung and dust. Both the extinction map and the SED are consistent with a dusty massive nebula with a dust mass of 0.055 ± 0.018â M· (assuming κ850 = 1.7 cm2 g-1). To date, RMC 143 has the most dusty LBV nebula observed in the Magellanic Clouds. We have also re-examined the LBV classification of RMC 143 based on VLT/X-shooter spectra obtained in 2015/16 and a review of the publication record. The radiative transfer code CMFGEN is used to derive its fundamental stellar parameters. We find an effective temperature of ∼8500 K, luminosity of log(L/L·) = 5.32, and a relatively high mass-loss rate of 1.0 × 10-5 M· yr-1. The luminosity is much lower than previously thought, which implies that the current stellar mass of ∼8 M· is comparable to its nebular mass of ∼5.5â M· (from an assumed gas-To-dust ratio of 100), suggesting that the star has lost a large fraction of its initial mass in past LBV eruptions or binary interactions. While the star may have been hotter in the past, it is currently not hot enough to ionize its circumstellar nebula. We propose that the nebula is ionized externally by the hot stars in the 30 Doradus star-forming region.

AB - The luminous blue variable (LBV) RMC 143 is located in the outskirts of the 30 Doradus complex, a region rich with interstellar material and hot luminous stars. We report the 3σ sub-millimetre detection of its circumstellar nebula with ALMA. The observed morphology in the sub-millimetre is different than previously observed with HST and ATCA in the optical and centimetre wavelength regimes. The spectral energy distribution (SED) of RMC 143 suggests that two emission mechanisms contribute to the sub-mm emission: optically thin bremsstrahlung and dust. Both the extinction map and the SED are consistent with a dusty massive nebula with a dust mass of 0.055 ± 0.018â M· (assuming κ850 = 1.7 cm2 g-1). To date, RMC 143 has the most dusty LBV nebula observed in the Magellanic Clouds. We have also re-examined the LBV classification of RMC 143 based on VLT/X-shooter spectra obtained in 2015/16 and a review of the publication record. The radiative transfer code CMFGEN is used to derive its fundamental stellar parameters. We find an effective temperature of ∼8500 K, luminosity of log(L/L·) = 5.32, and a relatively high mass-loss rate of 1.0 × 10-5 M· yr-1. The luminosity is much lower than previously thought, which implies that the current stellar mass of ∼8 M· is comparable to its nebular mass of ∼5.5â M· (from an assumed gas-To-dust ratio of 100), suggesting that the star has lost a large fraction of its initial mass in past LBV eruptions or binary interactions. While the star may have been hotter in the past, it is currently not hot enough to ionize its circumstellar nebula. We propose that the nebula is ionized externally by the hot stars in the 30 Doradus star-forming region.

KW - Dust

KW - Extinction

KW - Stars: evolution

KW - Stars: individual: RMC143

KW - Stars: mass-loss

KW - Stars: massive

KW - Stars: variables: S Doradus

UR - http://www.scopus.com/inward/record.url?scp=85068330381&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/201935239

DO - 10.1051/0004-6361/201935239

M3 - Article

VL - 626

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

SN - 0004-6361

M1 - A126

ER -

Agliozzo C, Mehner A, Phillips NM, Leto P, Groh JH, Noriega-Crespo A y otros. A massive nebula around the luminous blue variable star RMC 143 revealed by ALMA. Astronomy and Astrophysics. 2019 jun 1;626. A126. https://doi.org/10.1051/0004-6361/201935239