Identifying Type IIn supernova progenitors in our Galaxy: the circumstellar environment of the Galactic luminous blue variable candidate Gal 026.47+0.02

Umana, G.; Ingallinera, A.; Trigilio, C.; Buemi, C. S.; Leto, P.; Agliozzo, C.; Noriega-Crespo, A.; Flagey, Nicolas; Paladini, R.; Molinari, S.

doi:10.1111/j.1365-2966.2012.22018.x

Cited by 15 publications

(44 citation statements)

References 41 publications

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“…It is also possible that KISS15s is affected by CSM dust. A promising candidate progenitor of SNe IIn would be the luminous blue variables (LBVs; Gal-Yam & Leonard 2009; Dwarkadas 2011); observationally circumstellar environments of LBVs are preferentially dusty (Umana et al 2012).…”

Section: Host Galaxy Propertiesmentioning

confidence: 99%

A Long-duration Luminous Type IIn Supernova KISS15s: Strong Recombination Lines from the Inhomogeneous Ejecta–CSM Interaction Region and Hot Dust Emission from Newly Formed Dust*

Kokubo

Mitsuda

Morokuma

et al. 2019

ApJ

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We report the discovery of an SN 1988Z-like type IIn supernova KISS15s found in a low-mass star-forming galaxy at redshift z = 0.038 during the course of the Kiso Supernova Survey (KISS). KISS15s shows longduration optical continuum and emission line light curves, indicating that KISS15s is powered by a continuous interaction between the expanding ejecta and dense circumstellar medium (CSM). The Hα emission line profile can be decomposed into four Gaussians of narrow, intermediate, blue-shifted intermediate, and broad velocity width components, with a full width at half maximum of 100, ∼ 2, 000, and ∼ 14, 000 km s −1 for the narrow, intermediate, and broad components, respectively. The presence of the blue-shifted intermediate component, of which the line-of-sight velocity relative to the systemic velocity is about −5, 000 km s −1 , suggests that the ejecta-CSM interaction region has an inhomogeneous morphology and anisotropic expansion velocity. We found that KISS15s shows increasing infrared continuum emission, which can be interpreted as hot dust thermal emission of T ∼ 1, 200 K from newly formed dust in a cool, dense shell in the ejecta-CSM interaction region. The progenitor mass-loss rate, inferred from bolometric luminosity, isṀ ∼ 0.4 M yr −1 (v w /40 km s −1 ), where v w is the progenitor's stellar wind velocity. This implies that the progenitor of KISS15s was a red supergiant star or a luminous blue variable that had experienced a large mass-loss in the centuries before the explosion.

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Section: Host Galaxy Propertiesmentioning

confidence: 99%

A Long-duration Luminous Type IIn Supernova KISS15s: Strong Recombination Lines from the Inhomogeneous Ejecta–CSM Interaction Region and Hot Dust Emission from Newly Formed Dust*

Kokubo

Mitsuda

Morokuma

et al. 2019

ApJ

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“…The emission of the CSE derives from the ionization of the gas ejected by the star in previous moments. The shape of the radio nebula is greatly variable, with example of LBVs showing ring nebulae (Umana et al 2011;Agliozzo et al 2014) or bipolar nebulae (Umana et al 2012). …”

Section: Bubbles With a Central Objectmentioning

confidence: 99%

High-resolution Very Large Array observations of 18 MIPSGAL bubbles

Ingallinera¹,

Trigilio²,

Leto³

et al. 2016

Mon. Not. R. Astron. Soc.

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We present radio observations of 18 MIPSGAL bubbles performed at 5 GHz (6 cm) with the Karl G. Jansky Very Large Array in configuration B and BnA. The observations were aimed at understanding what kind of information high-resolution and high-sensitivity radio maps can supply on the circumstellar envelopes of different kinds of evolved stars and what their comparison with infrared images with similar resolution can tell us. We found that the 18 bubbles can be grouped into five categories according to their radio morphology. The three bubbles presenting a central point source in the radio images all correspond to luminous blue variable star candidates. Eleven bubbles show an elliptical shape and the total lack of a central object in the radio, and are likely associated with planetary nebulae. Under this assumption we derive their distance, their ionized mass and their distribution on the Galactic plane. We discuss the possibility that the MIPSGAL bubbles catalogue (428 objects) may contain a large fraction of all Galactic planetary nebulae located at a distance between 1.4 kpc and 6.9 kpc and lying in the MIPSGAL field of view. Among the remaining bubbles we identify also a H II region and a proto-planetary nebula candidate.

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“…The morphologies of some nebulae are consistent with symmetric mass loss (e.g., Gal 79.29+0.46, LHA 120-S 61, Higgs et al 1994;Weis 2003;Umana et al 2011;Agliozzo et al 2012Agliozzo et al , 2014Agliozzo et al , 2017a. However, the majority of the observed nebulae have a bipolar morphology (e.g., Weis 2011), indicating aspherical mass loss (e.g., Gal 026.47+0.02, Umana et al 2012) or an external shaping mechanism (e.g., IRAS 18576+0341, HR Car, Umana et al 2005;Buemi et al 2010Buemi et al , 2017. Usually, bipolar or equatorial mass losses have been proposed.…”

Section: Introductionmentioning

confidence: 77%

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

Agliozzo

Trigilio

Pignata

et al. 2017

ApJ

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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 Ha 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 (S µ -( ). 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 ( 80 K ) 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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Identifying Type IIn supernova progenitors in our Galaxy: the circumstellar environment of the Galactic luminous blue variable candidate Gal 026.47+0.02

Cited by 15 publications

References 41 publications

A Long-duration Luminous Type IIn Supernova KISS15s: Strong Recombination Lines from the Inhomogeneous Ejecta–CSM Interaction Region and Hot Dust Emission from Newly Formed Dust*

A Long-duration Luminous Type IIn Supernova KISS15s: Strong Recombination Lines from the Inhomogeneous Ejecta–CSM Interaction Region and Hot Dust Emission from Newly Formed Dust*

High-resolution Very Large Array observations of 18 MIPSGAL bubbles

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

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