Quantifying the dust in SN 2012aw and iPTF14hls with ORBYTS

Abstract

Core-collapse supernovae (CCSNe) are potentially capable of producing large quantities of dust, with strong evidence that ejecta dust masses can grow significantly over extended periods of time. Red-blue asymmetries in the broad emission lines of CCSNe can be modelled using the Monte Carlo radiative transfer code DAMOCLES, to determine ejecta dust masses. To facilitate easier use of DAMOCLES, we present a Tkinter graphical user interface (GUI) running DAMOCLES. The GUI was tested by high school students as part of the Original Research By Young Twinkle Students (ORBYTS) programme, who used it to measure the dust masses formed at two epochs in two Type IIP CCSNe: SN 2012aw and iPTF14hls, demonstrating that a wide range of people can contribute significantly to scientific advancement. Bayesian methods were used to quantify uncertainties on our model parameters. From the presence of a red scattering wing in the day 1863 H$\alpha$ profile of SN 2012aw, we were able to constrain the dust composition to large (radius $>0.1\mu$m) silicate grains, with a dust mass of $6.0_{-3.6}^{+21.9}\times 10^{-4}{M}_{\odot }$. From the day 1158 H$\alpha$ profile of SN 2012aw, we found a dust mass of $3.0_{-2.5}^{+14}\times 10^{-4}$ M${}_{\odot }$. For iPTF14hls, we found a day 1170 dust mass of 8.1 ${}_{-7.6}^{+81}\times 10^{-5}$ M${}_{\odot }$ for a dust composition consisting of 50% amorphous carbon and 50% astronomical silicate. At 1000 days post explosion, SN 2012aw and iPTF14hls have formed less dust than SN 1987A, suggesting that SN 1987A could form larger dust masses than other Type IIP's.

Accepted by MNRAS on 28/11/2022, 10 pages, 6 figures. Author accepted manuscript

References in corpus (26)

• A dusty, normal galaxy in the epoch of reionization
• Dust in the reionization era: ALMA observations of a $z$=8.38 Galaxy
• The Evolution of Dust in the Early Universe with Applications to the Galaxy SDSS J1148+5251
• Rapid formation of large dust grains in the luminous supernova SN 2010jl
• Dust and the type II-plateau supernova 2004et
• A stubbornly large mass of cold dust in the ejecta of Supernova 1987A
• Condensation of dust in the ejecta of type II-P supernovae
• The dust mass in Cassiopeia A from a spatially resolved Herschel analysis
• Energetic eruptions leading to a peculiar hydrogen-rich explosion of a massive star
• The timing and location of dust formation in the remnant of SN 1987A
• The dust and gas content of the Crab Nebula
• Explaining iPTF14hls as a common envelope jets supernova
• A Massive Shell of Supernova-formed Dust in SNR G54.1+0.3
• Marvel analysis of the measured high-resolution rovibrational spectra of H2S
• Dust masses for SN 1980K, SN1993J and Cassiopeia A from red-blue emission line asymmetries
• MARVEL analysis of the measured high-resolution rovibronic spectra of ${}^{48}$Ti${}^{16}$O
• The dust content of the Crab Nebula
• The mass, location and heating of the dust in the Cassiopeia A supernova remnant
• Original Research By Young Twinkle Students (ORBYTS): Ephemeris Refinement of Transiting Exoplanets
• Revisiting the dust destruction efficiency of supernovae
• Dust masses for a large sample of core-collapse supernovae from optical emission line asymmetries: dust formation on 30-year timescales
• MARVEL analysis of the measured high-resolution spectra of ${}^{14}$NH
• Dust masses and grain size distributions of a sample of Galactic pulsar wind nebulae
• Original Research By Young Twinkle Students (ORBYTS): Ephemeris Refinement of Transiting Exoplanets II
• Detection of Late-Time Optical Emission from SN 1941C in NGC 4136
• A Study of the Soft X-ray Emission Lines in NGC 4151 I. Kinematic Properties of the Plasma Wind