An optical and near-infrared study of the Type Ia/IIn Supernova PS15si

Kilpatrick, C. D.; Andrews, Jennifer E.; Smith, Nathan; Milne, Peter; Rieke, G. H.; Zheng, W.; Filippenko, A. V.

doi:10.1093/mnras/stw2061

Cited by 6 publications

(5 citation statements)

References 73 publications

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“…When Las Cumbres Observatory began observing again on MJD 58748 the BgV i data all show a slightly slower decline rate of ∼ 0.009 mag day −1 , while the Las Cumbres Observatory r is similar to that of DLT40 at ∼ 0.010 mag day −1 . This value is almost identical to that of the interacting SN 2005gj (Prieto et al 2007), and similar to other values measured in other interacting SNe (Kiewe et al 2012;Kilpatrick et al 2016), although we expect a wide range of decline rates as the CSM around interacting SNe will have different densities and geometries.…”

Section: Light Curve Evolutionsupporting

confidence: 88%

High Cadence TESS and ground-based data of SN 2019esa, the less energetic sibling of SN 2006gy

Andrews,

Pearson,

Lundquist

et al. 2022

Preprint

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We present photometric and spectroscopic observations of the nearby (D ≈ 28 Mpc) interacting supernova (SN) 2019esa, discovered within hours of explosion and serendipitously observed by the Transiting Exoplanet Survey Satellite (TESS ). Early, high cadence light curves from both TESS and the DLT40 survey tightly constrain the time of explosion, and show a 30 day rise to maximum light followed by a near constant linear decline in luminosity. Optical spectroscopy over the first 40 days revealed a highly reddened object with narrow Balmer emission lines seen in Type IIn supernovae. The slow rise to maximum in the optical lightcurve combined with the lack of broad Hα emission suggest the presence of very optically thick and close circumstellar material (CSM) that quickly decelerated the supernova ejecta. This CSM was likely created from a massive star progenitor with an Ṁ ∼ 0.3 M yr −1 lost in a previous eruptive episode 3-4 years before eruption, similar to giant eruptions of luminous blue variable stars. At late times, strong intermediate-width Ca II, Fe I, and Fe II lines are seen in the optical spectra, identical to those seen in the superluminous interacting SN 2006gy. The strong CSM interaction masks the underlying explosion mechanism in SN 2019esa, but the combination of the luminosity, strength of the Hα lines, and mass loss rate of the progenitor all point to a core collapse origin.

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Section: Light Curve Evolutionsupporting

confidence: 88%

High Cadence TESS and ground-based data of SN 2019esa, the less energetic sibling of SN 2006gy

Andrews,

Pearson,

Lundquist

et al. 2022

Preprint

Self Cite

View full text Add to dashboard Cite

show abstract

“…When Las Cumbres Observatory began observing again on MJD 58748, the BgVi data all show a slightly slower decline rate of ∼0.009 mag day −1 , while the Las Cumbres Observatory r is similar to that of DLT40 at ∼0.010 mag day −1 . This value is almost identical to that of the interacting (and possible Ia-CSM) SN 2005gj (Prieto et al 2007), and similar to other values measured in other interacting SNe (Kiewe et al 2012;Kilpatrick et al 2016, for example), although we expect a wide range of decline rates as the CSM around interacting SNe will have different densities and geometries.…”

Section: Light-curve Evolutionsupporting

confidence: 87%

High-Cadence TESS and Ground-based Data of SN 2019esa, the Less Energetic Sibling of SN 2006gy ^∗

Andrews

Lundquist

Sand

et al. 2022

ApJ

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We present photometric and spectroscopic observations of the nearby (D ≈ 28 Mpc) interacting supernova (SN) 2019esa, discovered within hours of explosion and serendipitously observed by the Transiting Exoplanet Survey Satellite (TESS). Early, high-cadence light curves from both TESS and the DLT40 survey tightly constrain the time of explosion, and show a 30 day rise to maximum light followed by a near-constant linear decline in luminosity. Optical spectroscopy over the first 40 days revealed a reddened object with narrow Balmer emission lines seen in Type IIn SNe. The slow rise to maximum in the optical light curve combined with the lack of broad Hα emission suggest the presence of very optically thick and close circumstellar material (CSM) that quickly decelerated the SN ejecta. This CSM was likely created from a massive star progenitor with an M ̇ ∼ 0.2 M ☉ yr−1 lost in a previous eruptive episode 3–4 yr before eruption, similar to giant eruptions of luminous blue variable stars. At late times, strong intermediate-width Ca ii, Fe i, and Fe ii lines are seen in the optical spectra, identical to those seen in the superluminous interacting SN 2006gy. The strong CSM interaction masks the underlying explosion mechanism in SN 2019esa, but the combination of the luminosity, strength of the Hα lines, and mass-loss rate of the progenitor seem to be inconsistent with a Type Ia CSM model and instead point to a core-collapse origin.

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“…However, within 6 days of core collapse, the SN 2013cu spectrum evolved into a relatively featureless, but still extremely blue, continuum. Even if high-ionisation species were present at a relatively low level in Gaia16cfr, strong continuum emission might decrease the S/N of a detection, as has been noted in SN IIn and SN Ia/IIn spectra (Smith & McCray 2007;Fox et al 2015;Kilpatrick et al 2016).…”

Section: Thermal Continuum Emissionmentioning

confidence: 92%

Connecting the progenitors, pre-explosion variability and giant outbursts of luminous blue variables with Gaia16cfr

Kilpatrick

Foley

Drout

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present multi-epoch, multi-colour pre-outburst photometry and post-outburst light curves and spectra of the luminous blue variable (LBV) outburst Gaia16cfr discovered by the Gaia satellite on 1 December 2016 UT. We detect Gaia16cfr in 13 epochs of Hubble Space Telescope imaging spanning phases of 10 yr to 8 months before the outburst and in Spitzer Space Telescope imaging 13 yr before outburst. Pre-outburst optical photometry is consistent with an 18 M F8 I star, although the star was likely reddened and closer to 30 M . The preoutburst source exhibited a significant near-infrared excess consistent with a 120 AU shell with 4 × 10 −6 M of dust. We infer that the source was enshrouded by an optically-thick and compact shell of circumstellar material from an LBV wind, which formed a pseudophotosphere consistent with S Dor-like variables in their "maximum" phase. Within a year of outburst, the source was highly variable on 10-30 day timescales. The outburst light curve closely matches that of the 2012 outburst of SN 2009ip, although the observed velocities are significantly slower than in that event. In Hα, the outburst had an excess of blueshifted emission at late times centred around −1500 km s −1 , similar to that of double-peaked Type IIn supernovae and the LBV outburst SN 2015bh. From the pre-outburst and post-outburst photometry, we infer that the outburst ejecta are evolving into a dense, highly structured circumstellar environment from precursor outbursts within years of the December 2016 event.1 Although "SN impostor" implies that these objects are not genuine corecollapse SNe and thus confuses a physical mechanism with an observational class of transients, we use this label for consistency with the existing literature. This does not imply that we think a single physical mechanism powers these objects or that none of these objects is a core-collapse SN.

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An optical and near-infrared study of the Type Ia/IIn Supernova PS15si

Cited by 6 publications

References 73 publications

High Cadence TESS and ground-based data of SN 2019esa, the less energetic sibling of SN 2006gy

High Cadence TESS and ground-based data of SN 2019esa, the less energetic sibling of SN 2006gy

High-Cadence TESS and Ground-based Data of SN 2019esa, the Less Energetic Sibling of SN 2006gy ^∗

Connecting the progenitors, pre-explosion variability and giant outbursts of luminous blue variables with Gaia16cfr

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An optical and near-infrared study of the Type Ia/IIn Supernova PS15si

Cited by 6 publications

References 73 publications

High Cadence TESS and ground-based data of SN 2019esa, the less energetic sibling of SN 2006gy

High Cadence TESS and ground-based data of SN 2019esa, the less energetic sibling of SN 2006gy

High-Cadence TESS and Ground-based Data of SN 2019esa, the Less Energetic Sibling of SN 2006gy ∗

Connecting the progenitors, pre-explosion variability and giant outbursts of luminous blue variables with Gaia16cfr

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Product

Resources

About

High-Cadence TESS and Ground-based Data of SN 2019esa, the Less Energetic Sibling of SN 2006gy ^∗