High Angular Resolution ALMA Images of Dust and Molecules in the SN 1987A Ejecta

We present high angular resolution (∼80 mas) ALMA continuum images of the SN 1987A system, together with CO J = 2 1, J = 6 5, and SiO J = 5 4 to J = 7 6 images, which clearly resolve the ejecta (dust continuum and molecules) and ring (synchrotron continuum) components. Dust in the ejecta is asymmetr...

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Published inThe Astrophysical journal Vol. 886; no. 1; pp. 51 - 77
Main Authors Cigan, Phil, Matsuura, Mikako, Gomez, Haley L., Indebetouw, Remy, Abellán, Fran, Gabler, Michael, Richards, Anita, Alp, Dennis, Davis, Timothy A., Janka, Hans-Thomas, Spyromilio, Jason, Barlow, M. J., Burrows, David, Dwek, Eli, Fransson, Claes, Gaensler, Bryan, Larsson, Josefin, Bouchet, P., Lundqvist, Peter, Marcaide, J. M., Ng, C.-Y., Park, Sangwook, Roche, Pat, van Loon, Jacco Th, Wheeler, J. C., Zanardo, Giovanna
Format Journal Article
LanguageEnglish
Published Goddard Space Flight Center The American Astronomical Society 20.11.2019
IOP Publishing
Subjects
Angular resolution
Astrophysics
Dissociation
Dust
Ejecta
High temperature
Interstellar dust
Interstellar molecules
Radiation
Supernovae
Supernovae
Interstellar Dust
Interstellar Molecules
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Abstract We present high angular resolution (∼80 mas) ALMA continuum images of the SN 1987A system, together with CO J = 2 1, J = 6 5, and SiO J = 5 4 to J = 7 6 images, which clearly resolve the ejecta (dust continuum and molecules) and ring (synchrotron continuum) components. Dust in the ejecta is asymmetric and clumpy, and overall the dust fills the spatial void seen in H images, filling that region with material from heavier elements. The dust clumps generally fill the space where CO J = 6 5 is fainter, tentatively indicating that these dust clumps and CO are locationally and chemically linked. In these regions, carbonaceous dust grains might have formed after dissociation of CO. The dust grains would have cooled by radiation, and subsequent collisions of grains with gas would also cool the gas, suppressing the CO J = 6 5 intensity. The data show a dust peak spatially coincident with the molecular hole seen in previous ALMA CO J = 2 1 and SiO J = 5 4 images. That dust peak, combined with CO and SiO line spectra, suggests that the dust and gas could be at higher temperatures than the surrounding material, though higher density cannot be totally excluded. One of the possibilities is that a compact source provides additional heat at that location. Fits to the far-infrared-millimeter spectral energy distribution give ejecta dust temperatures of 18-23 K. We revise the ejecta dust mass to Mdust = 0.2-0.4 for carbon or silicate grains, or a maximum of <0.7 for a mixture of grain species, using the predicted nucleosynthesis yields as an upper limit.
AbstractList We present high angular resolution (∼80 mas) ALMA continuum images of the SN1987A system, together with CO J = 21, J = 65, and SiO J = 54 to J = 76 images, which clearly resolve the ejecta (dust continuum and molecules) and ring (synchrotron continuum) components. Dust in the ejecta is asymmetric and clumpy, and overall the dust fills the spatial void seen in Hα images, filling that region with material from heavier elements. The dust clumps generally fill the space where CO J = 6 5 is fainter, tentatively indicating that these dust clumps and CO are locationally and chemically linked. In these regions, carbonaceous dust grains might have formed after dissociation of CO. The dust grains would have cooled by radiation, and subsequent collisions of grains with gas would also cool the gas, suppressing the CO J = 6 5 intensity. The data show a dust peak spatially coincident with the molecular hole seen in previous ALMA CO J = 2 1 and SiO J = 5 4 images. That dust peak, combined with CO and SiO line spectra, suggests that the dust and gas could be at higher temperatures than the surrounding material, though higher density cannot be totally excluded. One of the possibilities is that a compact source provides additional heat at that location. Fits to the far-infrared–millimeter spectral energy distribution give ejecta dust temperatures of 18–23 K. We revise the ejecta dust mass to Mdust = 0.2–0.4 Mfor carbon or silicate grains, or a maximum of <0.7 Mfor a mixture of grain species, using the predicted nucleosynthesis yields as an upper limit.
We present high angular resolution (similar to 80 mas) ALMA continuum images of the SN.1987A system, together with CO J = 2 -&gt; 1, J = 6 -&gt; 5, and SiO J = 5 -&gt; 4 to J = 7 -&gt; 6 images, which clearly resolve the ejecta (dust continuum and molecules) and ring (synchrotron continuum) components. Dust in the ejecta is asymmetric and clumpy, and overall the dust fills the spatial void seen in H alpha images, filling that region with material from heavier elements. The dust clumps generally fill the space where CO J = 6 -&gt; 5 is fainter, tentatively indicating that these dust clumps and CO are locationally and chemically linked. In these regions, carbonaceous dust grains might have formed after dissociation of CO. The dust grains would have cooled by radiation, and subsequent collisions of grains with gas would also cool the gas, suppressing the CO J = 6 -&gt; 5 intensity. The data show a dust peak spatially coincident with the molecular hole seen in previous ALMA CO J = 2 -&gt; 1 and SiO J = 5 -&gt; 4 images. That dust peak, combined with CO and SiO line spectra, suggests that the dust and gas could be at higher temperatures than the surrounding material, though higher density cannot be totally excluded. One of the possibilities is that a compact source provides additional heat at that location. Fits to the far-infrared-millimeter spectral energy distribution give ejecta dust temperatures of 18-23 K. We revise the ejecta dust mass to M-dust = 0.2-0.4 M-circle dot for carbon or silicate grains, or a maximum of &lt;0.7 M-circle dot for a mixture of grain species, using the predicted nucleosynthesis yields as an upper limit.
We present high angular resolution (∼80 mas) ALMA continuum images of the SN 1987A system, together with CO J = 2 1, J = 6 5, and SiO J = 5 4 to J = 7 6 images, which clearly resolve the ejecta (dust continuum and molecules) and ring (synchrotron continuum) components. Dust in the ejecta is asymmetric and clumpy, and overall the dust fills the spatial void seen in H images, filling that region with material from heavier elements. The dust clumps generally fill the space where CO J = 6 5 is fainter, tentatively indicating that these dust clumps and CO are locationally and chemically linked. In these regions, carbonaceous dust grains might have formed after dissociation of CO. The dust grains would have cooled by radiation, and subsequent collisions of grains with gas would also cool the gas, suppressing the CO J = 6 5 intensity. The data show a dust peak spatially coincident with the molecular hole seen in previous ALMA CO J = 2 1 and SiO J = 5 4 images. That dust peak, combined with CO and SiO line spectra, suggests that the dust and gas could be at higher temperatures than the surrounding material, though higher density cannot be totally excluded. One of the possibilities is that a compact source provides additional heat at that location. Fits to the far-infrared-millimeter spectral energy distribution give ejecta dust temperatures of 18-23 K. We revise the ejecta dust mass to Mdust = 0.2-0.4 for carbon or silicate grains, or a maximum of <0.7 for a mixture of grain species, using the predicted nucleosynthesis yields as an upper limit.
We present high angular resolution (∼80 mas) ALMA continuum images of the SN 1987A system, together with CO J = 2 \(\to \) 1, J = 6 \(\to \) 5, and SiO J = 5 \(\to \) 4 to J = 7 \(\to \) 6 images, which clearly resolve the ejecta (dust continuum and molecules) and ring (synchrotron continuum) components. Dust in the ejecta is asymmetric and clumpy, and overall the dust fills the spatial void seen in Hα images, filling that region with material from heavier elements. The dust clumps generally fill the space where CO J = 6 \(\to \) 5 is fainter, tentatively indicating that these dust clumps and CO are locationally and chemically linked. In these regions, carbonaceous dust grains might have formed after dissociation of CO. The dust grains would have cooled by radiation, and subsequent collisions of grains with gas would also cool the gas, suppressing the CO J = 6 \(\to \) 5 intensity. The data show a dust peak spatially coincident with the molecular hole seen in previous ALMA CO J = 2 \(\to \) 1 and SiO J = 5 \(\to \) 4 images. That dust peak, combined with CO and SiO line spectra, suggests that the dust and gas could be at higher temperatures than the surrounding material, though higher density cannot be totally excluded. One of the possibilities is that a compact source provides additional heat at that location. Fits to the far-infrared–millimeter spectral energy distribution give ejecta dust temperatures of 18–23 K. We revise the ejecta dust mass to M dust = 0.2–0.4 \({M}_{\odot }\) for carbon or silicate grains, or a maximum of <0.7 \({M}_{\odot }\) for a mixture of grain species, using the predicted nucleosynthesis yields as an upper limit.
We present high angular resolution (∼80 mas) ALMA continuum images of the SN 1987A system, together with CO J  = 2 1, J  = 6  5, and SiO J  = 5 4 to J  = 7  6 images, which clearly resolve the ejecta (dust continuum and molecules) and ring (synchrotron continuum) components. Dust in the ejecta is asymmetric and clumpy, and overall the dust fills the spatial void seen in H α images, filling that region with material from heavier elements. The dust clumps generally fill the space where CO J  = 6 5 is fainter, tentatively indicating that these dust clumps and CO are locationally and chemically linked. In these regions, carbonaceous dust grains might have formed after dissociation of CO. The dust grains would have cooled by radiation, and subsequent collisions of grains with gas would also cool the gas, suppressing the CO J  = 6 5 intensity. The data show a dust peak spatially coincident with the molecular hole seen in previous ALMA CO J  = 2 1 and SiO J  = 5 4 images. That dust peak, combined with CO and SiO line spectra, suggests that the dust and gas could be at higher temperatures than the surrounding material, though higher density cannot be totally excluded. One of the possibilities is that a compact source provides additional heat at that location. Fits to the far-infrared–millimeter spectral energy distribution give ejecta dust temperatures of 18–23 K. We revise the ejecta dust mass to M dust  = 0.2–0.4 for carbon or silicate grains, or a maximum of <0.7 for a mixture of grain species, using the predicted nucleosynthesis yields as an upper limit.
Audience PUBLIC
Author Alp, Dennis
Burrows, David
Indebetouw, Remy
Barlow, M. J.
Bouchet, P.
van Loon, Jacco Th
Abellán, Fran
Gaensler, Bryan
Dwek, Eli
Zanardo, Giovanna
Gabler, Michael
Roche, Pat
Wheeler, J. C.
Davis, Timothy A.
Fransson, Claes
Ng, C.-Y.
Richards, Anita
Spyromilio, Jason
Janka, Hans-Thomas
Park, Sangwook
Marcaide, J. M.
Gomez, Haley L.
Lundqvist, Peter
Cigan, Phil
Matsuura, Mikako
Larsson, Josefin
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  orcidid: 0000-0002-8736-2463
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  fullname: Cigan, Phil
  email: ciganp@cardiff.ac.uk
  organization: Cardiff University School of Physics and Astronomy, Cardiff CF24 3AA, UK
– sequence: 2
  givenname: Mikako
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  surname: Matsuura
  fullname: Matsuura, Mikako
  organization: Cardiff University School of Physics and Astronomy, Cardiff CF24 3AA, UK
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  organization: Universidad de Valencia Departamento de Astronomía y Astrofísica, C/Dr. Moliner 50, E-46100 Burjassot, Spain
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  givenname: Anita
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  givenname: Timothy A.
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https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-177486$$DView record from Swedish Publication Index
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Snippet We present high angular resolution (∼80 mas) ALMA continuum images of the SN 1987A system, together with CO J = 2 1, J = 6 5, and SiO J = 5 4 to J = 7 6...
We present high angular resolution (∼80 mas) ALMA continuum images of the SN1987A system, together with CO J = 21, J = 65, and SiO J = 54 to J = 76 images,...
We present high angular resolution (∼80 mas) ALMA continuum images of the SN 1987A system, together with CO J  = 2 1, J  = 6  5, and SiO J  = 5 4 to J  = 7  6...
We present high angular resolution (∼80 mas) ALMA continuum images of the SN 1987A system, together with CO J = 2 \(\to \) 1, J = 6 \(\to \) 5, and SiO J = 5...
We present high angular resolution (similar to 80 mas) ALMA continuum images of the SN.1987A system, together with CO J = 2 -&gt; 1, J = 6 -&gt; 5, and SiO J =...
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SubjectTerms Angular resolution
Astrophysics
Dissociation
Dust
Ejecta
High temperature
Interstellar dust
Interstellar molecules
Radiation
Supernovae
Title High Angular Resolution ALMA Images of Dust and Molecules in the SN 1987A Ejecta
URI https://iopscience.iop.org/article/10.3847/1538-4357/ab4b46
https://ntrs.nasa.gov/citations/20210013376
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