Superluminous supernovae at high redshift
Tim Abbott, Jeff Cooke, Chris Curtin, Shahab Joudaki, Antonios Katsianis, Anton Koekemoer, Jeremy Mould, Edoardo Tescari, Syed Uddin, Lifan Wang
早在再电离时期，就开始在红移处发现超亮超新星。一些候选机制进行审查，连同发现程序。
Superluminous supernovae are beginning to be discovered at redshifts as early as the epoch of reionization. A number of candidate mechanisms is reviewed, together with the discovery programs.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
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Radiative shock waves and their role in solving puzzles of Superluminous Supernovae
本文以教学综述形式介绍超亮超新星的基础物理，重点推导辐射激波相关的重要公式，以帮助理解其背后的物理机制。
Understanding how massive stars die as supernovae is a crucial question in modern astrophysics. Supernovae are powerful stellar explosions and key drivers in the cosmic baryonic cycles by injecting their explosion energy and heavy elements to the interstellar medium that forms new stars. After decades of effort, astrophysicists have built up a stand model for the explosion mechanism of massive stars. However, this model is challenged by new kinds of stellar explosions discovered in the recent transit surveys. In particular, the new population called superluminous supernovae, which are a hundre…
The energy liberated by fallback accretion has been suggested as a possible engine to power hydrogen-poor superluminous supernovae. We systematically investigate this model using the Bayesian light-curve fitting code MOSFiT (Modular Open Source Fitter for Transients), fitting the light curves of 37 hydrogen-poor superluminous supernovae assuming a fallback accretion central engine. We find that this model can yield good fits to their light curves, with a fit quality that rivals the popular magnetar engine models. Examining our derived parameters for the fallback model, we find the total energy…
We analyze recent magnetar light-curve modeling of 38 hydrogen-poor superluminous supernovae (SLSNe), and find that the energies of the explosions themselves, that take place before the magnetar energy is released, are more than what the neutrino-driven explosion mechanism can supply for about half of the systems. These SLSNe must have been exploded by a different process than the delayed neutrino mechanism, most likely the jet feedback mechanism (JFM). The conclusion for magnetar modeling of SLSNe is that jets launched at magnetar birth cannot be ignored, not at the explosion itself and not l…
Properties of magnetars mimicking 56Ni-powered light curves in Type Ic superluminous supernovae
许多Ic型超亮超新星在其光度峰值后的光变曲线衰减率接近于56 Co的核衰变率，这与它们由56 Ni和可能的对不稳定超新星提供动力的解释一致。然而，它们的上升时间通常短于对不稳定超新星的预期，并且Ic型超亮超新星通常被认为是由磁星自旋下降提供动力。如果磁星自旋下降实际上是驱动Ic型超亮超新星的主要机制，那么它应该能够相当容易地产生类似于56 Co衰变率的下降率。在这项研究中，我们调查磁星的条件下，他们的自旋下降的能量输入可以表现得像56 Ni核衰变能量输入。我们发现，在一定范围内的初始磁场强度足以保持磁星的能量沉积在几个因素的56 Co衰变能量为几百天。磁星自旋下降需要通过几乎纯的偶极辐射，制动指数接近3，以在宽的参数范围内模拟56Ni。磁星不仅可以再现56 Co衰变光变曲线，而且可以再现大多数56 Ni动力光变曲线的上升时间和峰值亮度。需要超过700天的辐射热光变曲线来区分这两种能源。我们预计，如果它们主要由磁星自旋下降提供动力，那么应该会发现更多上升时间短的缓慢下降的超亮超新星。
Superluminous supernovae are a new class of supernovae that were recognized about a decade ago. Both observational and theoretical progress has been significant in the last decade. In this review, we first briefly summarize the observational properties of superluminous supernovae. We then introduce the three major suggested luminosity sources to explain the huge luminosities of superluminous supernovae, i.e., the nuclear decay of 56Ni, the interaction between supernova ejecta and dense circumstellar media, and the spin down of magnetars. We compare these models and discuss their strengths and …
We calculate the rate per unit volume of hydrogen-poor superluminous supernovae (SLSNe-I) based on the 17 events discovered with the Pan-STARRS1 Medium Deep Survey (PS1 MDS). Two forms of the luminosity function (LF) are assumed : a log-normal form and a single power-law form, respectively. The rate of SLSNe-I is assumed to be proportional to the cosmic star formation rate with an additional redshift evolution of $(1+z)^α$. Our results show that the single power-low form fits the data better than the log-normal form, and the event rate of SLSNe-I is proportional to the cosmic star formation ra…
I review our current understanding of superluminous supernovae, mysterious events 100 times brighter than conventional stellar explosions.
Stripped-envelope core-collapse supernovae can be divided into two broad classes: the common Type Ib/c supernovae (SNe Ib/c), powered by the radioactive decay of $^{56}$Ni, and the rare superluminous supernovae (SLSNe), most likely powered by the spin-down of a magnetar central engine. Up to now, the intermediate regime between these two populations has remained mostly unexplored. Here, we present a comprehensive study of 40 \textit{luminous supernovae} (LSNe), SNe with peak magnitudes of $M_r = -19$ to $-20$ mag, bound by SLSNe on the bright end and by SNe Ib/c on the dim end. Spectroscopical…
Supernovae (SNe) are the most brilliant optical stellar-class explosions. Over the past two decades, several optical transient survey projects discovered more than $\sim 100$ so-called superluminous supernovae (SLSNe) whose peak luminosities and radiated energy are $\gtrsim 7\times 10^{43}$ erg s$^{-1}$ and $\gtrsim 10^{51}$ erg, at least an order of magnitude larger than that of normal SNe. According to their optical spectra features, SLSNe have been split into two broad categories of type I that are hydrogen-deficient and type II that are hydrogen-rich. Investigating and determining the ener…
Superluminous X-rays from a superluminous supernova
超亮超新星（SLSNe）的发现，其峰值亮度比普通超新星亮约100倍（通常SLSNe的M_V <-21），显示了核心坍缩超新星性质的意外多样性。对于这些事件的性质，人们提出了许多模型，包括冲击波与稠密的星周环境的强相互作用、通过中央引擎重新激发外流，或者由于在极其巨大的恒星核心产生对而导致压力损失后恒星灾难性毁灭的起源（所谓的对不稳定超新星）。在这里，我们考虑可以通过XMM-牛顿，钱德拉和斯威夫特的X射线观测对贫氢SLSNe（SLSNe-I）的爆炸机制进行限制，并表明至少有一个SLSNe-I可能是有史以来观测到的最明亮的X射线超新星，L_X ~ 10^45尔格/秒，在最初发现后约150天。这是一个亮度3个数量级高于其他X射线超新星通过拱星相互作用。如此高的X射线亮度足以覆盖喷出物，并显着降低光学深度，使人们有可能看到喷出物的深处以及任何存在于那里的发射源。另一种可能是，一台发动机可能为喷出物外部的适度相对论性喷流提供动力，类似于伽马射线暴中看到的情况。如果X射线的探测确实需要引擎，这意味着这些SNe确实会产生紧凑的物体，并且恒星不会在对不稳定事件中完全摧毁。未来的观测将确定这些机制中的哪些（如果有的话）在超亮超新星中起作用。
The division between stripped-envelope supernovae (SE-SNe) and superluminous supernovae (SLSNe) is not well defined in either photometric or spectroscopic space. While a sharp luminosity threshold has been suggested, there remains an increasing number of transitional objects that reach this threshold without the spectroscopic signatures common to SLSNe. In this work we present data and analysis on four SNe transitional between SE-SNe and SLSNe; the He-poor SNe 2019dwa and 2019cri, and the He-rich SNe 2019hge and 2019unb. Each object displays long-lived and variable photometric evolution with l…
Most neutron stars (NSs) and black holes (BHs) are believed to be the final remnants in the evolution of massive stars. In this study, we propose a new formation channel for the formation of BHs and peculiar NSs (specifically, magnetars and Thorne-$\dot{\rm Z}$ytkow objects [T$\dot{\rm Z}$Os]), which we refer to as the core merger-induced collapse (CMIC) model. This model involves the merger at the end of a common-envelope phase of an oxygen/neon/magnesium composition white dwarf and the core of a hydrogen-rich or helium-rich non-degenerate star, leading to the creation of peculiar new types o…
Are Superluminous Supernovae Powered By Collision Or By Millisecond Magnetars?
使用我们以前推导出的超新星的热光变曲线的简单解析表达式，我们证明了普通超新星爆炸的快速碎片与超新星爆发前相对缓慢移动的外壳的碰撞可以产生所观察到的所有类型的超亮超新星（SLSNe）的热光变曲线。这些包括两种，那些可以解释为由自旋下降的毫秒磁星提供动力的，以及那些不能解释的。这一点以及观测到的SLSNe和普通相互作用SNe的热光度曲线之间的密切相似性表明，SLSNe主要是由超新星爆发前相对缓慢移动的星周壳层碰撞提供动力，而不是由核心坍缩超新星爆炸中诞生的毫秒磁星的自旋下降提供动力。
Superluminous supernovae (SLSNe) are at least $\sim$5 times more luminous than common supernovae (SNe). Especially hydrogen-poor SLSN-I are difficult to explain with conventional powering mechanisms. One possible scenario that might explain such luminosities is that SLSNe-I are powered by an internal engine, such as a magnetar or an accreting black hole. Strong magnetic fields or collimated jets can circularly polarize light. In this work, we measured circular polarization of two SLSNe-I with the FOcal Reducer and low dispersion Spectrograph (FORS2) mounted at the ESO's Very Large Telescope (V…
We present results of a search for late-time radio emission and Fast Radio Bursts (FRBs) from a sample of type-I superluminous supernovae (SLSNe-I). We used the Karl G. Jansky Very Large Array to observe ten SLSN-I more than 5 years old at a frequency of 3 GHz. We searched fast-sampled visibilities for FRBs and used the same data to perform a deep imaging search for late-time radio emission expected in models of magnetar-powered supernovae. No FRBs were found. One SLSN-I, PTF10hgi, is detected in deep imaging, corresponding to a luminosity of $1.2\times10^{28}$ erg s$^{-1}$. This luminosity, c…
In this paper, we investigate two hydrogen-poor superluminous supernovae (SLSNe) iPTF15esb and iPTF13dcc whose light curves (LCs) show significant deviation from the smooth rise and fall. The LC of iPTF15esb exhibits two peaks and a post-peak plateau, and furthermore the late-time spectrum of iPTF15esb shows a strong, broad H$α$ emission line. The early-time LC of iPTF13dcc shows a long duration bump followed by the second peak. Here we propose an ejecta-circumstellar medium (CSM) interaction model involving multiple shells/winds and use it to explain the LCs of iPTF15esb and iPTF13dcc. We fin…
Predictions for signatures of the quark-nova in superluminous supernovae
[摘要]超亮超新星（SN 2006 gy，SN 2005 gj，SN 2005 ap，SN 2008 fz，SN 2003 ma）一直是用标准模型解释的一个挑战。我们提出了一个替代方案，涉及夸克新星（QN），爆炸过渡的新出生的中子星的夸克星，其中第二次爆炸（延迟）发生在已经扩大的喷出物的正常SN。与标准SN情况不同，重新加热的SN喷出物可以在更长的时间内以更高的水平辐射，这主要是由于绝热膨胀损失减少。我们的模型被成功地应用到SN 2006 gy，SN 2005 gj，SN 2005 ap，SN 2008 fz，SN 2003 ma与令人鼓舞的光变曲线拟合。在我们的模型中有四个预测：（i）超亮SN的光学光变曲线应该显示一个双峰，SN峰在较弱的震级发生在QN前几天到几周;（ii）两个冲击爆发应该观察到一个相对于一个正常SN。取决于时间延迟，这将表现为两个不同的尖峰在X射线区域或加宽的第一个尖峰极短的延迟;（iii）QN存款的质量数A> 130的重元素在前面的SN喷出物的基础。这些QN r-处理的元素应该是可见的后期光谱（几天几周的情况下，强烈的喷出物混合）的超亮SN;（iv）QN产量也将包含较轻的元素（氢和氦）。我们希望后期光谱包括H_α发射线，这些发射线的速度特征应该与标准H_α发射不同。
We report our first discoveries of high-redshift supernovae from the Subaru HIgh-Z sUpernova CAmpaign (SHIZUCA), the transient survey using Subaru/Hyper Suprime-Cam. We report the discovery of three supernovae at the spectroscopically-confirmed redshifts of 2.399 (HSC16adga), 1.965 (HSC17auzg), and 1.851 (HSC17dbpf), and two supernova candidates with the host-galaxy photometric redshifts of 3.2 (HSC16apuo) and 4.2 (HSC17dsid), respectively. In this paper, we present their photometric properties and the spectroscopic properties of the confirmed high-redshift supernovae are presented in the acco…
Over the past decade wide-field optical time-domain surveys have increased the discovery rate of transients to the point that $\lesssim 10\%$ are being spectroscopically classified. Despite this, these surveys have enabled the discovery of new and rare types of transients, most notably the class of hydrogen-poor superluminous supernovae (SLSN-I), with about 150 events confirmed to date. Here we present a machine-learning classification algorithm targeted at rapid identification of a pure sample of SLSN-I to enable spectroscopic and multi-wavelength follow-up. This algorithm is part of the FLEE…
Revealing the binary origin of Type Ic superluminous supernovae through nebular hydrogen emission
我们认为在Ic型超亮超新星iPTF 13 ehe中观测到的星云H-α辐射来自于超新星喷出物与伴星碰撞时从伴星上剥离的物质，辐射的时间演化、谱线展宽和整体蓝移与这一解释是一致的。我们缩放星云的H-α光度预测Ia型超新星在单简并系统中，以获得剥离的质量需要解释的H-α光度的iPTF 13 ehe。我们发现剥离质量为0.1 - 0.9太阳质量，假设超新星光度是由放射性或磁星自旋下降。由于需要一个中央加热源来激发H-α发射，如果H-α发射来自剥离物质，则相互作用动力模型不适合iPTF 13 ehe。我们推导出一个超过20个太阳质量的伴星质量和一个小于20个伴星半径的双星分离的基础上的剥离效率在碰撞过程中，表明超新星的祖先和伴星形成了一个巨大的紧密的双星系统。如果Ic型超亮超新星通常发生在大质量的近距离双星系统中，那么先前在几颗Ic型超亮超新星中观察到的早期增亮也可能是由于与近距离伴星的碰撞。对未来Ic型超亮超新星中星云氢发射的观测将使我们能够检验这一解释。
Magnetar Flare-Driven Bumpy Declining Light Curves in Hydrogen-poor Superluminous Supernovae
本文通过改进含耀发活动的磁星模型，对五个贫氢超亮超新星的起伏光变曲线进行拟合，揭示其耀发可能是伽马射线暴耀发的暗淡长时延伸，为理解二者关联提供依据。
Analytical Expressions For Light-Curves Of Ordinary And Superluminous Supernovae Type Ia
Ia型超新星（SNeIa）可以由缓慢旋转的碳氧白矮星爆炸产生，白矮星的质量通过质量吸积增加到临界值以上。在光球和早期星云阶段与星周物质的碰撞可以增强普通SNeIa的热光度，使其成为超亮的。几个简化的假设导致一个简单的解析主公式，它很好地描述了普通SNeIa和超亮SNeIa的辐射热光变曲线的几个初始物理参数。SNeIa的其他主要性质，包括经验的“更亮-更慢”菲利普斯关系，该关系用于标准化普通SNeIa作为距离指标，并导致宇宙加速膨胀的发现，被再现
Superluminous Supernovae Powered by Magnetars: Late-time Light Curves and Hard Emission Leakage
最近，两个研究小组的研究表明，完全能量捕获的磁星自旋向下能量注入模型可以解释SN 2010 gx，SN 2013 dg，LSQ 12 dlf，SSS 120810和CSS 121015的早期光变曲线，但不能拟合这些超亮超新星（SLSNe）的晚期光变曲线。这些结果意味着，原来的磁星供电模型在解释这些SLSNe的挑战。我们的论文旨在通过考虑硬排放的泄漏来同时解释早期和晚期数据/上限。我们将漏电流效应定量地纳入到原来的磁驱动模型中，并推导出一个新的半解析方程。将修正后的磁星动力模型再现的光变曲线与这5个SLSNe的观测数据和/或上限值进行比较，发现半解析方程再现的晚时光变曲线与SN 2010 gx、CSS 121015、SN 2013 dg和LSQ 12 dlf的晚时观测数据和/或上限值以及SSS 120810的晚时过剩值吻合较好，这表明磁星供电模型可能是造成这些SLSNe的原因，并且当硬光子被下康普顿化为较软光子时，伽马射线和X射线泄漏是不可避免的。为了确定泄漏效应的细节并揭示SLSNe的本质，需要更多高质量的SLSNe的辐射热光变曲线和光谱。
A rapidly spinning magnetar in a young supernova (SN) can produce a superluminous transient by converting a fraction of its rotational energy into radiation. Here, we present the first three-dimensional hydrodynamical simulations ever performed of a magnetar-powered SN in the circumstellar medium formed by the ejection of the outer layers of the star prior to the blast. We find that hydrodynamical instabilities form on two scales in the ejecta, not just one as in ordinary core-collapse SNe: in the hot bubble energized by the magnetar and in the forward shock of the SN as it plows up ambient ga…
GRB 111209A, one of the longest Gamma-Ray Bursts (GRBs) ever observed, is linked to SN 2011kl, the most luminous GRB-Supernova (SN) detected so far, which shows evidence for being powered by a magnetar central engine. We place SN 2011kl into the context of large samples of SNe, addressing in more detail the question of whether it could be radioactively powered, and whether it represents an extreme version of a GRB-SN or an underluminous Superluminous SN (SLSN). We model SN 2011kl using SN 1998bw as a template and derive a bolometric light curve including near-infrared data. We compare the prop…
We present a study of 28 Type I superluminous supernovae (SLSNe) in the context of the ejecta mass and photospheric velocity. We combine photometry and spectroscopy to infer ejecta masses via the formalism of radiation diffusion equations. We show an improved method to determine the photospheric velocity by combining spectrum modeling and cross correlation techniques. We find that Type I SLSNe can be divided into two groups by their pre-maximum spectra. Members of the first group have the W-shaped absorption trough in their pre-maximum spectrum, usually identified as due to O II. This feature …
Exploring GRBs and supernovae connection: does a superluminous hypernova population exist?
本文回顾了超长伽马射线暴与超亮超新星之间可能存在的联系，重点分析了GRB 111209A/SN 2011kl等关键事件、前身星与宿主星系的作用以及磁星中心引擎等模型，指出需进一步观测和理论研究以确定是否存在超亮超新星族群。
Rapidly spinning, strongly magnetized proto-neutron stars ("millisecond proto-magnetars") are candidate central engines of long-duration gamma-ray bursts (GRB), superluminous supernovae (SLSNe), and binary neutron star mergers. Magnetar birth may be accompanied by the fall-back of stellar debris, lasting for seconds or longer following the explosion. Accretion alters the magnetar evolution by (1) providing an additional source of rotational energy (or a potential sink, if the propeller mechanism operates); (2) enhancing the spin-down luminosity above the dipole rate by compressing the magnetos…
The discovery of early bumps in some type-I superluminous supernovae (SLSNe-I) before the main peaks offers an important clue to their energy source mechanisms. In this paper, we updated an analytic magnetar-powered model for fitting the multi-band light curves of double-peaked SLSNe-I: the early bump is powered by magnetar-driven shock breakout thermal emission, and the main peak is powered by a radiative diffusion through the SN ejecta as in the standard magnetar-powered model. Generally, the diffusive luminosity is greater than the shock breakout luminosity at the early time, which makes th…
Superluminous supernovae (SLSNe) are a rare class of stellar explosions with luminosities ~10-100 times greater than ordinary core-collapse supernovae. One popular model to explain the enhanced optical output of hydrogen-poor (Type I) SLSNe invokes energy injection from a rapidly spinning magnetar. A prediction in this case is that high-energy gamma rays, generated in the wind nebula of the magnetar, could escape through the expanding supernova ejecta at late times (months or more after optical peak). This paper presents a search for gamma-ray emission in the broad energy band from 100 MeV to …
We model the late evolution and mass loss history of rapidly rotating Wolf-Rayet stars in the mass range $5\,\rm{M}_{\odot}\dots 100\,\rm{M}_{\odot}$. We find that quasi-chemically homogeneously evolving single stars computed with enhanced mixing retain very little or no helium and are compatible with Type\,Ic supernovae. The more efficient removal of core angular momentum and the expected smaller compact object mass in our lower mass models lead to core spins in the range suggested for magnetar driven superluminous supernovae. Our more massive models retain larger specific core angular moment…
New optical photometric, spectrocopic and imaging polarimetry data are combined with publicly available data to study some of the physical properties of the two H-poor superluminous supernovae (SLSN) SN 2021bnw and SN 2021fpl. For each SLSN, the best-fit parameters obtained from the magnetar model with \texttt{MOSFiT} do not depart from the range of parameter obtained on other SLSNe discussed in the literature. A spectral analysis with \texttt{SYN++} shows that SN 2021bnw is a W Type, Fast evolver, while SN 2021fpl is a 15bn Type, Slow evolver. The analysis of the polarimetry data obtained on …
Hydrogen-poor Superluminous Supernovae with Bumpy Light Curves Powered by Precessing Magnetars
本研究将磁星进动效应纳入磁星供能模型，成功再现了6个具有峰后隆起的氢贫超亮超新星的多波段光变曲线，为峰后隆起起源和新生磁星早期进动提供了证据。
We present light curves and classification spectra of 17 hydrogen-poor superluminous supernovae (SLSNe) from the Pan-STARRS1 Medium Deep Survey (PS1 MDS). Our sample contains all objects from the PS1 MDS sample with spectroscopic classification that are similar to either of the prototypes SN2005ap or SN2007bi, without an explicit limit on luminosity. With a redshift range $0.3 < z < 1.6$, PS1MDS is the first SLSN sample primarily probing the high-redshift population; our multi-filter PS1 light curves probe the rest-frame UV emission, and hence the peak of the spectral energy distribution. We m…
A Magnetar Engine and Circumstellar Medium Interaction: Synergistic Effects in Producing Superluminous Supernovae
研究磁星引擎与星际介质相互作用对超亮超新星的影响，开发半解析混合模型跟踪系统耦合动力学等，该模型能产生多样光变曲线形态，为降低相关解释中的能量要求提供合理方法。
We present the results of 3 GHz radio continuum observations of 23 superluminous supernovae (SLSNe) and their host galaxies by using the Karl G. Jansky Very Large Array conducted 5-21 years after the explosions. The sample consists of 15 Type I and 8 Type II SLSNe at z < 0.3, providing one of the largest sample of SLSNe with late-time radio data. We detected radio emission from one SLSN (PTF10hgi) and 5 hosts with a significance of >5$σ$. No time variability is found in late-time radio light curves of the radio-detected sources in a timescale of years except for PTF10hgi, whose variability is …
We present the largest and deepest late-time radio and millimeter survey to date of superluminous supernovae (SLSNe) and long duration gamma-ray bursts (LGRBs) to search for associated non-thermal synchrotron emission. Using the Karl G. Jansky Very Large Array (VLA) and the Atacama Large Millimeter/submillimeter Array (ALMA), we observed 43 sources at 6 and 100 GHz on a timescale of $\sim 1 - 19$ yr post-explosion. We do not detect radio/mm emission from any of the sources, with the exception of a 6 GHz detection of PTF10hgi (Eftekhari et al. 2019), as well as the detection of 6 GHz emission n…
A Monte Carlo Approach to Magnetar-powered Transients: I. Hydrogen-deficient Superluminous Supernovae
本文收集了19颗贫氢超亮超新星（SLSNe），基于磁星动力模型拟合了它们的光变曲线、温度演化和速度演化。为了获得最佳拟合参数，我们采用马尔可夫链蒙特卡罗方法。其中7个事件的拟合效果较好（$χ^2$ /d.o.f = $0.24-0.96$），另外7个事件的拟合效果较好（$χ^2$ /d.o.f = $1.37-3.13$）。我们发现，初始周期（$P_{0}$）和磁场强度（$B_{p}$）的磁星应该为这些SLSNe供电的范围内的$\sim 1.2-8.3$ ms和$\sim (0.2-8.8)\times 10^{14}\,$ G，分别;这些SLSNe的喷出物的推断质量在1和27.6 $M_{\odot }$之间，和伽马射线不透明度值$κ_{γ}$在0.01和0.82厘米$^2$ ~g $^{-1}$之间。我们还计算了在这些SLSNe的残余物的中心窝藏的磁星的初始旋转能量被转换为喷出物的动能的分数，并发现该分数是$\sim 19-97$为不同的值的$P_{0}$和$B_{p}$，表明加速效应不能忽略。此外，我们发现，大多数这些SLSNe的初始动能是如此之小（$\lesssim 2\times 10^{51}$ erg），它们可以很容易地解释中微子驱动的机制。这些结果有助于澄清与SLSNe的能源机制和爆炸机制相关的一些重要问题，并揭示SLSNe的本质。
Spectrum formation in Superluminous Supernovae (Type I)
大多数不受富氢CSM（SLSN-I）相互作用支配的超亮超新星的近最大光谱的特征是蓝色光谱峰和一系列被确定为OII的吸收线。与超长伽马射线暴GRB 111209 A相关的SN 2011 kl也有一个蓝色峰值，但没有特征的光学/紫外光谱。辐射输运方法被用来表明，光谱（不包括SN 2007 bi，它有一个红色的光谱在峰值，像普通的SNe Ic）可以解释为一个相当陡峭的密度分布的喷出物，其组成似乎是典型的碳氧核心的大质量恒星，可以有低的金属含量。如果光球的速度是10000-15000 km/s，那么在紫外线中会形成几条线。然而，OII线是从非常高激发的低能级产生的，这需要显著偏离局部热力学平衡来填充。这些SLSNe并不被认为主要由56 Ni衰变提供动力。一个吸引人的设想是，它们是由磁星风驱动的冲击波产生的X射线激发的。明显缺乏随时间的演变的线速度的特点SLSNe高达约最大值是另一个论点，有利于磁星的情况。SN 2011 kl平滑的紫外线连续谱需要更高的喷出物速度（约20000 km/s）：谱线覆盖导致几乎没有特征的光谱。在最大值之后，在一些SLSNe中观察到氦。接近最大值的高电离意味着He和H都可能存在，但在早期没有观察到。SLSNe的光谱分类可能反映SNe Ib/c的光谱分类。准确的分类需要广泛的时间覆盖。
SN 2012au: A Golden Link Between Superluminous Supernovae and Their Lower-Luminosity Counterparts
我们提出了SN 2012 au的光学和近红外观测，SN 2012 au是一种缓慢演化的超新星（SN），其性质表明高能和H-贫SNe和超亮SNe的子集之间存在联系。SN 2012 au在其早期光谱中表现出明显的类似SN Ib的He I线和其他吸收特征，速度达到2 x 10^4 km/s，并且具有宽的光变曲线，峰值为M_B = -18.1 mag.这些数据的模型表明，大爆炸动能为10^{52} erg，56 Ni质量喷射为0.3兆太阳能，与SN 1998 bw相当。SN 2012 au的光谱在爆炸后近一年显示出持续的Fe II P-Cyg散射和来自两个不同速度区域的星云发射的混合物。这些晚期的排放包括速度> 4500 km/s的强[Fe II]、[Ca II]、[O I]、Mg I]和Na I线，以及速度明显较小的2000 km/s的O I和Mg I线。SN 2012 au的许多晚期性质类似于演化缓慢的超新星SN 1997 dq和SN 1997 ef，以及超亮的SN 2007 bi。我们的观测结果表明，一个单一的爆炸机制可能统一了所有这些跨越-21 < M_B < -17 mag.非球面和可能喷流爆炸最有可能是由一个大质量祖星的核心坍缩，并创造了大量的高密度，低速富镍的材料。
Superluminous supernovae (SLSNe) are massive star explosions too luminous to be powered by traditional energy sources, such as radioactive 56Ni. These transients may instead be powered by a central engine, such as a millisecond pulsar or magnetar, whose relativistic wind inflates a nebula of high energy particles and radiation behind the expanding ejecta. We present 3D Monte Carlo radiative transfer calculations which follow the production and thermalization of high energy radiation from the nebula into optical radiation and, conversely, determine the gamma-ray emission that escapes the ejecta…
Superluminous supernovae
本文综述了超亮超新星的观测特性与四种主要光度来源模型，指出未来高红移巡天发现将有助于揭示其本质。
Superluminous supernovae (SLSNe) and long gamma ray bursts (LGRBs) have been proposed as progenitors of repeating Fast Radio Bursts (FRBs). In this scenario, bursts originate from the interaction between a young magnetar and its surrounding supernova remnant (SNR). Such a model could explain the repeating, apparently non-Poissonian nature of FRB121102, which appears to display quiescent and active phases. This bursting behaviour is better explained with a Weibull distribution, which includes parametrisation for clustering. We observed 10 SLSNe/LGRBs for 63 hours, looking for repeating FRBs wit…
Some Hydrogen-poor superluminous supernovae are likely powered by a magnetar central engine, making their luminosity larger than common supernovae. Although a significant amount of X-ray flux is expected from the spin down of the magnetar, direct observational evidence is still to be found, giving rise to the "missing energy" problem. Here we present NuSTAR observations of nearby SN 2018hti 2.4y (rest frame) after its optical peak. We expect that, by this time, the ejecta have become optically thin for photons more energetic than about 15keV. No flux is detected at the position of the supernov…
The First Two Years of FLEET: an Active Search for Superluminous Supernovae
本研究介绍了用于识别I型超亮超新星的机器学习算法FLEET前两年的运行成果，验证了其高纯度与完备率，推出训练样本量提升的FLEET 2.0并分析了系统误差，同时开源了该算法。
Magnetar-Powered Supernovae in Two Dimensions. I. Superluminous Supernovae
以前的研究表明，嵌入年轻超新星中的快速旋转磁星发出的辐射可以大大放大其亮度。这些一维的研究还揭示了超新星内部深处的薄而致密的壳层中存在着由辐射加速物质堆积而产生的不稳定性。在这里，我们在两个维度上研究这个问题，并发现，虽然不稳定性导致混合和破裂，这个壳成非线性结构，减少密度对比，在一个空心壳的物质浓度持续存在。混合的程度取决于磁星输入的相对能量和内部喷出物的动能。由此产生的超新星的光变曲线和光谱将发生明显的变化，超新星遗迹的外观也会发生明显的变化，它将是无细胞的和无细胞的。类似的堆积和混合可能是其他事件的特征，其中能量是由中心集中源在一段时间内输入的，例如脉冲星，放射性衰变，中微子风或碰撞壳。我们的模型的相关性，最近的发光瞬态ASASSN-15 lh进行了简要讨论。
We present synthetic light curves of fallback-powered supernovae based on a neutrino-driven explosion of a 40 Msun zero-metallicity star with significant fallback accretion onto a black hole that was previously simulated by Chan et al. (2018) until shock breakout. Here, we investigate the light curve properties of the explosion after shock breakout for various fallback models. Without extra power from fallback accretion, the light curve is that of a Type IIP supernova with a plateau magnitude of around -14 mag and a plateau duration of 40 days. With extra power for the light curve from fallbac…
Forecast of cosmological constraints with superluminous supernovae from the Chinese Space Station Telescope
本研究探讨了中国空间站望远镜（CSST）超亮超新星（SLSNe）的宇宙学应用，预测其在2.5年内可观测约360颗SLSNe，并利用峰值-颜色关系严格约束宇宙学参数，揭示高红移暗能量本质。
We analyze the properties of 42 rapidly rotating, low metallicity, quasi-chemically homogeneously evolving stellar models in the mass range between 4 and 45 $\,\mathrm{M}_\odot$ at the time of core collapse. Such models were proposed as progenitors for both superluminous supernovae (SLSNe) and long duration gamma-ray bursts (lGRBs), and the Type Ic-BL supernovae (SNe) that are associated with them. Our findings suggest that whether these models produce a magnetar driven SLSN explosion or a near-critically rotating black hole (BH) is not a monotonic function of the initial mass. Rather, their e…
The central engines of some superluminous supernovae (SLSNe) are generally suggested to be newly born fast rotating magnetars, which spin down mainly through magnetic dipole radiation and gravitational wave emission. We calculate the magnetar-powered SLSNe light curves (LCs) with the tilt angle evolution of newly born magnetars involved. We show that, depending on the internal toroidal magnetic fields ${\bar B}_{\rm t}$, the initial spin periods $P_{\rm i}$, and the radii $R_{\rm DU}$ of direct Urca (DU) cores of newly born magnetars, as well as the critical temperature $T_{\rm c}$ for $^3P_2$…
We explore and demonstrate the capabilities of LSST to study Type I superluminous supernovae (SLSNe). We first fit the light curves of 58 known SLSNe at z~0.1-1.6, using an analytical magnetar spin-down model implemented in MOSFiT. We then use the posterior distributions of the magnetar and ejecta parameters to generate thousands of synthetic SLSN light curves, and we inject those into the OpSim to generate realistic ugrizy light curves. We define simple, measurable metrics to quantify the detectability and utility of the light curve, and to measure the efficiency of LSST in returning SLSN lig…
Results from a systematic survey of X-ray emission from Hydrogen-poor Superluminous Supernovae
利用Swift、Chandra和XMM对26颗邻近的贫氢超亮超新星（SLSNe-I）进行了灵敏的X射线测量。这个数据集限制了SLSN从爆发后几天到2000天的演化，达到亮度L_x~10^40 erg/s，并揭示了在PTF 12 dam位置存在显著的X射线发射。在L_x~10^41 erg/s以上没有检测到SLSN-I，这表明与SCP 60 F6相关的发光X射线发射L_x~10^45 erg/s在SLSNe-I中并不常见。我们通过逆康普顿辐射来限制离轴伽玛暴喷流、磁星中心发动机的电离爆发和SLSNe-I亚pc环境中的密度。最深的极限排除了最弱的未准直伽玛暴外流，这表明如果SLSNe-I与伽玛暴/超新星的相似性延伸到它们最快的喷出物，那么SLSNe-I要么是由指向远离我们视线θ>30度的高能喷流提供动力，要么是没有成功突破恒星包层的失败喷流。此外，如果磁星中心引擎是造成SLSNe-I异常亮度的原因，我们的X射线分析支持大磁场B> 2 × 10 ^（14）G和喷出物质量M_ej>3 Msun，这与光学/紫外研究结果一致。最后，我们限制了SLSNe-I的恒星祖先爆炸前的质量损失率。对于PTF 12 dam，我们推断Mdot<2x 10 ^（-5）Msun/yr，这表明SN激波与CSM的相互作用不太可能提供光学瞬变的主要能量来源，并且一些SLSN-I的祖先在生命结束时是被低密度介质包围的致密…
A possible relation between flare activity in superluminous supernovae and gamma-ray bursts
最近发现的超亮超新星（SLSN）SN 2015bn在第一个峰值之后的光变曲线中出现了显著的波动，而光变曲线的基本轮廓可以很好地解释为来自中央引擎的持续能量供应，可能是毫秒磁星的自旋下降。我们认为这些波动是由间歇性脉冲能量供应引起的，表明SLSN中心引擎的高能耀斑活动。在对伽马射线暴（GRB）的X射线余辉观测中发现了许多暴后耀斑。我们发现，这里描述的SLSN耀斑近似服从GRB耀斑的光度和时间尺度之间的经验相关性，外推到SLSN耀斑的相关更长的时间尺度。这证实了先前提出的这两种不同现象之间的可能联系。
Constraining the ellipticity of strongly magnetized neutron stars powering superluminous supernovae
超亮超新星（SLSNe）被认为是由强烈磁化的快速旋转的中子星提供动力的，中子星通常被称为磁星。在这个过程中，磁星的旋转能量通过磁偶极辐射辐射，并加热超新星喷出物。然而，如果磁星的几何形状高度扭曲，旋转能量主要作为引力波辐射损失，因此这样的磁星不能为SLSNe提供动力。通过简单地比较电磁波和引力波的发射时间尺度，我们约束上限的磁星的椭圆率，假设他们的权力所观察到的SLSNe。我们发现，它们的椭圆率通常需要小于约几个1 e-3。这表明，在这些磁星的环形磁场强度通常小于几个1 e 16 G，使其失真保持小。由于SLSNe的光变曲线模型表明，它们的偶极磁场强度为1 e14 G的量级，极向与环向磁场强度的比值被发现在为SLSNe供电的磁星中大于~ 0.01。
Type W and Type 15bn subgroups of hydrogen-poor superluminous supernovae: pre-maximum diversity, post-maximum homogeneity?
本文通过分析27颗I型超亮超新星极大后光谱，发现W型与15bn型在极大后温度和速度趋于一致、伪星云光谱均匀，主要差异源于极大前演化。
Photometrically-Classified Superluminous Supernovae from the Pan-STARRS1 Medium Deep Survey: A Case Study for Science with Machine Learning-Based Classification
本文利用 SuperRAENN 与 Superphot 对 PS1-MDS 超亮超新星进行测光分类，并用 MOSFiT 磁陀星模型验证其参数与光谱样本一致，为 LSST 时代扩大稀有瞬变样本提供方法。
Quark-Novae occurring in massive binaries : A universal energy source in superluminous Supernovae with double-peaked light curves
夸克新星（QN，从中子星到夸克星的突然转变）发生在大质量双星的第二公共包络（CE）阶段（Ouyed等人，2015a&b），非常适合超高亮度、贫氢、超新星（SLSNe），具有双峰光变曲线，包括DES13S2cmm、SN 2006oz和LSQ14bdq（http：//www.quarknova.ca/LCGallery.html）。在我们的模型中，质量较小的伴星的H包层在第一个CE阶段被喷射出来，而QN则发生在第二个CE阶段的深处，在CE的大小扩展到几十到几千个太阳半径的半径之后，这产生了我们模型中的第一个峰值。夸克星与CO核的合并导致了黑洞的形成和吸积，这解释了第二个持久的峰值。我们研究了具有双峰光变曲线的8个SLSNe Ic样品。我们的模型对所有这些都有很好的拟合，第一个峰的通用爆炸能量为2 × 10^52尔格（这是QN喷出物的动能）。在iPTF13ehe和LSQ14bdq中看到的后期发射与即将离开的富He（即第二个）CE和先前喷射的富H（即第一个）CE之间的激波相互作用相吻合。
The observed sub-class of "superluminous" Type Ia supernovae lacks a convincing theoretical explanation. If the emission of such objects were powered exclusively by radioactive decay of 56Ni formed in the explosion, a progenitor mass close to or even above the Chandrasekhar limit for a non-rotating white dwarf star would be required. Masses significantly exceeding this limit can be supported by differential rotation. We, therefore, explore explosions and predict observables for various scenarios resulting from differentially rotating carbon-oxygen white dwarfs close to their respective limit o…
A Swift Fix II: Physical Parameters of Type I Superluminous Supernovae
本研究利用Swift UVOT重新校准数据，对2014-2021年间发现的I型超亮超新星进行测光和建模，提取物理参数，发现磁星模型下自转周期与光度、辐射能量等存在强相关性。
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