Optical and IR observations of SN 2013L, a Type IIn Supernova surrounded by asymmetric CSM

Andrews, Jennifer E.; Smith, Nathan; McCully, C.; Fox, O.; Valenti, S.; Howell, D. A.

doi:10.1093/mnras/stx1844

Cited by 37 publications

(31 citation statements)

References 98 publications

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“…Indicated next to each spectrum is the phase, i.e., days from discovery. The spectra that were already published in Andrews et al (2017) and publicly available are marked by a star next to their phases, the four late-time spectra from A17 are marked by two stars. Each spectrum was normalized by its median and shifted by a constant for better visualization.…”

Section: Resultsmentioning

confidence: 99%

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The Carnegie Supernova Project II

Taddia

Stritzinger

Fransson

et al. 2020

A&A

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We present ultra-violet (UV) to mid-infrared (MIR) observations of the long-lasting Type IIn supernova (SN) 2013L obtained by the Carnegie Supernova Project II (CSP-II) beginning two days after discovery and extending until +887 days (d). The SN reached a peak r-band absolute magnitude of ≈ −19 mag and an even brighter UV peak, and its light curve evolution resembles that of SN 1988Z. The spectra of SN 2013L are dominated by hydrogen emission features, characterized by three components attributed to different emission regions. A unique feature of this Type IIn SN is that, apart from the first epochs, the blue shifted line profile is dominated by the macroscopic velocity of the expanding shock wave of the SN. We are therefore able to trace the evolution of the shock velocity in the dense and partially opaque circumstellar medium (CSM), from ∼ 4800 km s −1 at +48 d, decreasing as t −0.23 to ∼ 2700 km s −1 after a year. We performed spectral modeling of both the broad-and intermediate-velocity components of the Hα line profile. The high-velocity component is consistent with emission from a radially thin, spherical shell located behind the expanding shock with emission wings broadened by electron scattering. We propose that the intermediate component originates from preionized gas from the unshocked dense CSM with the same velocity as the narrow component, ∼ 100 km s −1 , but also that it is broadened by electron scattering. These features provide direct information about the shock structure, which is consistent with model calculations. The spectra exhibit broad O i and [O i] lines that emerge at +144 d and broad Ca ii features. The spectral continua and the spectral energy distributions (SEDs) of SN 2013L after +132 d are well reproduced by a two-component black-body (BB) model; one component represents emitting material with a temperature between 5×10 3 to 1.5×10 4 K (hot component) and the second component is characterized by a temperature around 1-1.5×10 3 K (warm component). The warm component dominates the emission at very late epochs ( +400 d), as is evident from both the last near infrared (NIR) spectrum and MIR observations obtained with the Spitzer Space Telescope. Using the BB fit to the SEDs, we constructed a bolometric light curve that was modeled together with the unshocked CSM velocity and the shock velocity derived from the Hα line modeling. The circumstellar-interaction model of the bolometric light curve reveals a mass-loss rate history with large values ( 1.7 × 10 −2 − 0.15 M yr −1 ) over the ∼25 -40 years before explosion, depending on the radiative efficiency and anisotropies in the CSM. The drop in the light curve at ∼ 350 days and the presence of electron scattering wings at late epochs indicate an anisotropic CSM. The mass-loss rate values and the unshocked-CSM velocity are consistent with the characteristics of a massive star, such as a luminous blue variable (LBV) undergoing strong eruptions, similar to η Carina. Our analysis also suggests a scenario where pre-existing dust grains have a dis...

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Section: Resultsmentioning

confidence: 99%

“…The phase of each spectrum relative to discovery is indicated next to each spectrum. The spectra that were already published in Andrews et al (2017) are marked by a star next to their phases. Each spectrum was normalized by its median and shifted by a constant for a better visualization.…”

Section: Resultsmentioning

confidence: 99%

The Carnegie Supernova Project II

Taddia

Stritzinger

Fransson

et al. 2020

A&A

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“…The red peak of λ6300 would fall at ∼6335 Å, while the blue peak of λ6364 would fall at ∼6330 Å, making the red peak of λ6300 seem as bright as the blue peak, and swamping the emission at the center of the line. Double-peaked emission lines in SN spectra are often interpreted as ejecta interacting with asymmetric CSM, most commonly in a disk or torus (Hoffman et al 2008;Mauerhan et al 2014;Smith et al 2015;Andrews et al 2017). In this scenario, the underlying broad component traces emission from the free expansion of the SN ejecta, while the intermediate components are formed in the post-shock region between the forward and reverse shocks created as the ejecta crashes into Vinkó et al (2006;2004dj).…”

Section: Circumstellar Interaction or Asymmetric Explosion?mentioning

confidence: 99%

SN 2017gmr: An Energetic Type II-P Supernova with Asymmetries

2019

The Astrophysical Journal

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We present high-cadence UV, optical, and near-infrared data on the luminous Type II-P supernova SN2017gmr from hours after discovery through the first 180 days. SN2017gmr does not show signs of narrow, high-ionization emission lines in the early optical spectra, yet the optical light-curve evolution suggests that an extra energy source from circumstellar medium (CSM) interaction must be present for at least 2 days after explosion. Modeling of the early light curve indicates a ∼500 R e progenitor radius, consistent with a rather compact red supergiant, and latetime luminosities indicate that up to 0.130±0.026 M e of 56 Ni are present, if the light curve is solely powered by radioactive decay, although the 56 Ni mass may be lower if CSM interaction contributes to the post-plateau luminosity. Prominent multipeaked emission lines of Hα and [O I] emerge after day 154, as a result of either an asymmetric explosion or asymmetries in the CSM. The lack of narrow lines within the first 2 days of explosion in the likely presence of CSM interaction may be an example of close, dense, asymmetric CSM that is quickly enveloped by the spherical supernova ejecta.

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“…This presents an interesting mystery, because equatorial mass loss from rotating stars or from close mass-transferring binaries should be azimuthally symmetric like the ring around SN 1987A. Some examples with such azimuthal asymmetry are SN 1998S (Leonard et al 2000;Mauerhan & Smith 2012;Shivvers et al 2015), SN 2010jl (Fransson et al 2014), PTF11iqb (Smith et al 2015), SN 2012ab (Bilinski et al 2017), SN2013L (Andrews et al 2017), and others. Episodic mass ejection and eccentric binaries have been invoked as possible explanations for some of these events.…”

Section: One-sided Equatorial Mass Ejectionmentioning

confidence: 99%

A disrupted molecular torus around Eta Carinae as seen in 12CO with ALMA

Smith

Ginsburg

Bally

2017

Monthly Notices of the Royal Astronomical Society

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We present Atacama Large Millimeter Array (ALMA) observations of 12 CO 2−1 emission from circumstellar material around the massive star η Carinae. These observations reveal new structural details about the cool equatorial torus located ∼4000 au from the star. The CO torus is not a complete azimuthal loop, but rather, is missing its near side, which appears to have been cleared away. The missing material matches the direction of apastron in the eccentric binary system, making it likely that η Car's companion played an important role in disrupting portions of the torus soon after ejection. Molecular gas seen in ALMA data aligns well with the cool dust around η Car previously observed in mid-infrared (IR) maps, whereas hot dust resides at the inner surface of the molecular torus. The CO also coincides with the spatial and velocity structure of near-IR H 2 emission. Together, these suggest that the CO torus seen by ALMA is actually the pinched waist of the Homunculus polar lobes, which glows brightly because it is close to the star and warmer than the poles. The near side of the torus appears to be a blowout, associated with fragmented equatorial ejecta. We discuss implications for the origin of various features northwest of the star. CO emission from the main torus implies a total gas mass in the range of 0.2 -1 M ⊙ (possibly up to 5 M ⊙ or more, although with questionable assumptions). Deeper observations are needed to constrain CO emission from the cool polar lobes.

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Optical and IR observations of SN 2013L, a Type IIn Supernova surrounded by asymmetric CSM

Cited by 37 publications

References 98 publications

The Carnegie Supernova Project II

The Carnegie Supernova Project II

SN 2017gmr: An Energetic Type II-P Supernova with Asymmetries

A disrupted molecular torus around Eta Carinae as seen in 12CO with ALMA

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