Response to the reviewer 1 of the manuscript: &amp;amp;#8220;Comparison of different droplet measurement techniques in the Braunschweig Icing Wind Tunnel&amp;amp;#8221; by Inken Knop et al.

Knop, Inken

doi:10.5194/amt-2019-494-ac2

Cited by 2 publications

(3 citation statements)

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“…This leaves us with the smallest group of SLSNe, which Gal-Yam (2012) defined as SLSN-R, for radioactive. This group includes only a small number of SNe, notably SN 2007bi, SN 1999as, the first SLSN observed (Knop et al 1999), PTF12dam (Nicholl et al 2013), SN 2015bn (Jerkstrand et al 2016;Nicholl et al 2015), and PS1-14bj (Lunnan et al 2016). While also showing SN Ic spectra, these SNe decline slowly in luminosity, following the 56 Co decline rate, and are not known to show O II lines early on (but early observations are scarce and the rise time is highly uncertain).…”

Section: Introductionmentioning

confidence: 99%

The nature of PISN candidates: clues from nebular spectra

Mazzali

Moriya

Tanaka

et al. 2019

Monthly Notices of the Royal Astronomical Society

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A group of super-luminous supernovae (SL-SNe) characterised by broad light curves have been suggested to be Pair Instability SNe (PISNe). Nebular spectra computed using PISN models have failed to reproduce the broad emission lines observed in these SNe, casting doubts on their true nature. Here, models of both PISNe and the explosion following the collapse of the core of a very massive star (100 M ⊙ ) are used to compute nebular spectra, which are compared to the spectrum of the prototypical PISN candidate, SN 2007bi. PISN models are confirmed to produce synthetic spectra showing narrow emission lines, resulting from the confinement of 56 Ni to the lowest velocities ( ∼ < 2000 km s −1 ) and in clear disagreement with the spectrum of SN 2007bi. Spectra more closely resembling SN 2007bi are obtained if the PISN models are fully mixed in abundance. Massive core-collapse models produce enough 56 Ni to power the light curve of PISN candidates, but their spectra are also not adequate. The nebular spectrum of SN 2007bi can be successfully reproduced if the inner region is artificially filled with oxygen-rich, low-velocity ejecta. This most likely requires a grossly aspherical explosion. A major difference between PISN and massive collapse models is that the former emit much more strongly in the NIR. It is concluded that: a) current PISN candidates, in particular SN 2007bi, are more likely the result of the collapse and explosion of massive stars below the PI limit; b) significant asymmetry is required to reproduce the late-time spectrum of SN 2007bi.

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Section: Introductionmentioning

confidence: 99%

The nature of PISN candidates: clues from nebular spectra

Mazzali

Moriya

Tanaka

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…Remarkably, CATS results include observations of SN 2002ic, the first SN Ia showing interaction with a dense circumstellar medium (Hamuy et al 2003), and SN 2003bg the first Type IIb hypernova (Hamuy et al 2009). Here we add to these notable achievements, the observations of SN 2002gh, the second SLSN discovered after SN 1999as (Knop et al 1999), for which its superluminous nature remained unnoticed for nearly two decades until now. In Section 2, we describe the data reduction and present the observations.…”

Section: Introductionmentioning

confidence: 87%

“…Objects such as SN 1999as (Knop et al 1999), SN 2005ap (Quimby et al 2007), SCP 06F6 (Barbary et al 2009), and SN 2007bi (Gal-Yam et al 2009 were the first SLSN-I reported, several years before they were distinguished as a separate SN class. Their bright peak luminosities together with the identification of a common set of spectral features made it possible to distinguish them as members of a completely new SN class (Quimby et al 2011).…”

Section: Introductionmentioning

confidence: 99%

A puzzle solved after two decades: SN 2002gh among the brightest of superluminous supernovae

Cartier,

Hamuy,

Contreras

et al. 2021

Preprint

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We present optical photometry and spectroscopy of the superluminous SN 2002gh from maximum light to +202 days, obtained as part of the Carnegie Type II Supernova (CATS) project. SN 2002gh is among the most luminous discovered supernovae ever, yet it remained unnoticed for nearly two decades. Using Dark Energy Camera archival images we identify the potential SN host galaxy as a faint dwarf galaxy, presumably having low metallicity, and in an apparent merging process with other nearby dwarf galaxies. We show that SN 2002gh is among the brightest hydrogen-poor SLSNe with 𝑀 𝑉 = −22.40 ± 0.02, with an estimated peak bolometric luminosity of 2.6 ± 0.2 × 10 44 erg s −1 . We discount the decay of radioactive nickel as the main SN power mechanism, and assuming that the SN is powered by the spin down of a magnetar we obtain two alternative solutions. The first case, is characterized by significant magnetar power leakage, and 𝑀 ej between 0.8 and 1.6 𝑀 , 𝑃 spin = 3.4 ms, and 𝐵 = 5 × 10 13 G. The second case does not require power leakage, resulting in a huge ejecta mass of about 30 𝑀 , a fast spin period of 𝑃 spin ∼ 1 ms, and 𝐵 ∼ 1.6 × 10 14 G. We estimate a zero-age main-sequence mass between 16 and 19 𝑀 for the first case and of about 135 𝑀 for the second case. The latter case would place the SN progenitor among the most massive stars observed to explode as a SN.

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Response to the reviewer 1 of the manuscript: &#8220;Comparison of different droplet measurement techniques in the Braunschweig Icing Wind Tunnel&#8221; by Inken Knop et al.

Abstract: Interactive comment on "Comparison of different droplet measurement techniques in the Braunschweig Icing Wind Tunnel" by Inken Knop et al. Inken Knop et al.

Cited by 2 publications

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The nature of PISN candidates: clues from nebular spectra

The nature of PISN candidates: clues from nebular spectra

A puzzle solved after two decades: SN 2002gh among the brightest of superluminous supernovae

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