MOSFiT: Modular Open Source Fitter for Transients

Guillochon, James; Nicholl, M.; Villar, V. Ashley; Mockler, Brenna; Narayan, Gautham; Mandel, Kaisey S.; Berger, E.; Williams, Peter K. G.

doi:10.3847/1538-4365/aab761

Cited by 214 publications

(191 citation statements)

References 42 publications

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“…) for the 42 hosts of our sample SNe and for 23 SN IIn hosts in the SDSS field from the Taddia et al (2015) sample. Figure 17 Percentile contours for the DLPS of CSI-driven SNe as explored by Villar et al (2017) using the MOSFiT code (Guillochon et al 2018). SN-like events are shown in pink (wind-like CSM) and blue (shell-like CSM) whereas shockbreakout (SBO) transients are shown in black.…”

Section: Discussionmentioning

confidence: 99%

Type IIn supernova light-curve properties measured from an untargeted survey sample

Nyholm

Sollerman

Tartaglia

et al. 2020

A&A

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The evolution of a Type IIn supernova (SN IIn) is governed by the interaction between the SN ejecta and a hydrogen-rich circumstellar medium (CSM). SNe IIn thus allow us to probe the late-time mass-loss history of their progenitor stars. We present a sample of SNe IIn from the untargeted, magnitude-limited surveys of the Palomar Transient Factory (PTF) and its successor, the intermediate PTF (iPTF). To date, statistics on SN IIn optical light curve properties have generally been based on small ( 10 SNe) samples from targeted SN surveys. SNe IIn found and followed by the PTF/iPTF were used to select a sample of 42 events with useful constraints on the rise times as well as with available post-peak photometry. The SNe were discovered in 2009-2016 and have at least one low-resolution classification spectrum, as well as photometry from the P48 and P60 telescopes at Palomar Observatory. We study the light-curve properties of these SNe IIn using spline fits (for the peak and the declining portion) and template matching (for the rising portion). We study the peak-magnitude distribution, rise times, decline rates, colour evolution, host galaxies, and K-corrections of the SNe in our sample. We find that the typical rise times are divided into fast and slow risers as 20 ± 8 d and 50 ± 15 d, respectively. The decline rates could possibly be divided into two groups (with slopes 0.013 ± 0.008 mag d −1 and 0.040 ± 0.014 mag d −1 ), but this division has weak statistical significance. We find no significant correlation between the peak luminosity of SNe IIn and their rise times, but the more luminous SNe IIn are generally found to be more durable and the slowly rising SNe IIn are generally found to be slowly declining. The SNe in our sample were hosted by galaxies of absolute magnitude −22 Mg −13 mag. The K-corrections at light-curve peak of the SNe in our sample are found to be within 0.2 mag for the observer's frame r-band, for SNe IIn at redshifts z < 0.25. Applying K-corrections and including also ostensibly "superluminous" SNe IIn, we find that the peak magnitudes are M r peak = −19.18 ± 1.32 mag. We conclude that the occurrence of conspicuous light-curve bumps in SNe IIn, such as in iPTF13z, is limited to 1.4 +14.6 −1.0 % of the SNe IIn. We also investigate a possible subtype of SNe IIn with a fast rise to a 50 d plateau followed by a slow, linear decline. iPTF13agz, iPTF13aki, iPTF13asr, iPTF13cuf, iPTF14bcw, iPTF14bpa, iPTF15aym, iPTF15bky, iPTF15blp, iPTF15eqr, iPTF16fb. ⋆ Based in part on observations made with the Palomar Transient Factory and intermediate Palomar Transient Factory surveys.

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Section: Discussionmentioning

confidence: 99%

Type IIn supernova light-curve properties measured from an untargeted survey sample

Nyholm

Sollerman

Tartaglia

et al. 2020

A&A

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“…A number of photometric modelling codes using semianalytic models to provide fits to the observed light curves of SNe and other transients have become available in recent years, such as MOSFiT (Guillochon et al 2018) and TigerFit (Chatzopoulos 2018). In this section we discuss the use of MOSFiT 6 to produce model fits to the light curve of LSQ13ddu.…”

Section: Photometric Modellingmentioning

confidence: 99%

LSQ13ddu: a rapidly evolving stripped-envelope supernova with early circumstellar interaction signatures

Clark

Maguire

Inserra

et al. 2020

Monthly Notices of the Royal Astronomical Society

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This paper describes the rapidly evolving and unusual supernova LSQ13ddu, discovered by the La Silla-QUEST survey. LSQ13ddu displayed a rapid rise of just 4.8±0.9 d to reach a peak brightness of −19.70±0.02 mag in the LSQgr band. Early spectra of LSQ13ddu showed the presence of weak and narrow He i features arising from interaction with circumstellar material (CSM). These interaction signatures weakened quickly, with broad features consistent with those seen in stripped-envelope SNe becoming dominant around two weeks after maximum. The narrow He i velocities are consistent with the wind velocities of luminous blue variables but its spectra lack the typically seen hydrogen features. The fast and bright early light curve is inconsistent with radioactive 56 Ni powering but can be explained through a combination of CSM interaction and an underlying 56 Ni decay component that dominates the later time behaviour of LSQ13ddu. Based on the strength of the underlying broad features, LSQ13ddu appears deficient in He compared to standard SNe Ib.

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“…We use the Modular Open Source Fitter for Transients (MOSFiT; Guillochon et al 2018), an open source modular transient Markov Chain Monte Carlo (MCMC) code, to fit the multi-band observed light curves of SN 2017dwh. We fit the SN with two models, one where the energy input is solely provided by a magnetar central engine and another in which energy from the radioactive decay of 56 Ni is also included.…”

Section: Light Curve Modelingmentioning

confidence: 99%

A Hydrogen-poor Superluminous Supernova with Enhanced Iron-group Absorption: A New Link between SLSNe and Broad-lined Type Ic SNe

Blanchard

Nicholl

Berger

et al. 2019

ApJ

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We present optical observations of the Type I superluminous supernova (SLSN-I) SN 2017dwh at z ≈ 0.13, which reached M i ≈ −21 mag at peak. Spectra taken a few days after peak show an unusual and strong absorption line centered near 3200Å that we identify with Co II, suggesting a high fraction of synthesized 56 Ni in the ejecta. By ∼ 1 month after peak, SN 2017dwh became much redder than other SLSNe-I, instead strongly resembling broad-lined Type Ic supernovae (Ic-BL SNe) with clear suppression of the flux redward of ∼ 5000Å, providing further evidence for a large mass of Fe-group elements. Late-time upper limits indicate a 56 Ni mass of 0.6 M , leaving open the possibility that SN 2017dwh produced a 56 Ni mass comparable to SN 1998bw (≈ 0.4 M ). Fitting the light curve with a combined magnetar and 56 Ni model using MOSFiT, we find that the light curve can easily accommodate such masses without affecting the inferred magnetar parameters. We also find that SN 2017dwh occurred in the least-luminous detected host galaxy to date for a SLSN-I, with M B = −13.5 mag and an implied metallicity of Z ∼ 0.08 Z . The spectral properties of SN 2017dwh provide new evidence linking SLSNe-I with Type Ic-BL SNe, and in particular the high Fe-group abundance may be due to enhanced 56 Ni production or mixing due to asphericity. Finally, we find that SN 2017dwh represents the most extreme end of a correlation between continuum shape and Co II absorption strength in the near-peak spectra of SLSNe-I, indicating that Fe-group abundance likely accounts for some of the variation in their spectral shapes.

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MOSFiT: Modular Open Source Fitter for Transients

Cited by 214 publications

References 42 publications

Type IIn supernova light-curve properties measured from an untargeted survey sample

Type IIn supernova light-curve properties measured from an untargeted survey sample

LSQ13ddu: a rapidly evolving stripped-envelope supernova with early circumstellar interaction signatures

A Hydrogen-poor Superluminous Supernova with Enhanced Iron-group Absorption: A New Link between SLSNe and Broad-lined Type Ic SNe

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