The long-lived Type IIn SN 2015da: Infrared echoes and strong interaction within an extended massive shell
L. Tartaglia, A. Pastorello, J. Sollerman, C. Fransson, S. Mattila, M. Fraser, F. Taddia, L. Tomasella, M. Turatto, A. Morales-Garoffolo, N. Elias-Rosa, P. Lund… 展开作者
L. Tartaglia, A. Pastorello, J. Sollerman, C. Fransson, S. Mattila, M. Fraser, F. Taddia, L. Tomasella, M. Turatto, A. Morales-Garoffolo, N. Elias-Rosa, P. Lundqvist, J. Harmanen, T. Reynolds, E. Cappellaro, C. Barbarino, A. Nyholm, E. Kool, E. Ofek, X. Gao, Z. Jin, H. Tan, D. J. Sand, F. Ciabattari, X. Wang, J. Zhang, F. Huang, W. Li, J. Mo, L. Rui, D. Xiang, T. Zhang, G. Hosseinzadeh, D. A. Howell, C. McCully, S. Valenti, S. Benetti, E. Callis, A. S. Carracedo, C. Fremling, T. Kangas, A. Rubin, A. Somero, G. Terreran
备注：
23 pages (19+appendix), 15 figures, 11 tables (Tables A.1-A.4 at CDS only). Accepted for publication on Astronomy and Astrophysics
In this paper we report the results of the first $\sim$four years of spectroscopic and photometric monitoring of the Type IIn supernova SN 2015da (also known as PSN J13522411+3941286, or iPTF16tu). The supernova exploded in the nearby spiral galaxy NGC 5337 in a relatively highly extinguished environment. The transient showed prominent narrow Balmer lines in emission at all times and a slow rise to maximum in all bands. In addition, early observations performed by amateur astronomers give a very well-constrained explosion epoch. The observables are consistent with continuous interaction between the supernova ejecta and a dense and extended H-rich circumstellar medium. The presence of such an extended and dense medium is difficult to reconcile with standard stellar evolution models, since the metallicity at the position of SN 2015da seems to be slightly subsolar. Interaction is likely the mechanism powering the light curve, as confirmed by the analysis of the pseudo bolometric light curve, which gives a total radiated energy $\gtrsim10^{51}\,\rm{erg}$. Modeling the light curve in the context of a supernova shock breakout through a dense circumstellar medium allowed us to infer the mass of the prexisting gas to be $\simeq8\,\rm{M_{\odot}}$, with an extreme mass-loss rate for the progenitor star $\simeq0.6\,\rm{M_{\odot}}\,\rm{yr^{-1}}$, suggesting that most of the circumstellar gas was produced during multiple eruptive events. Near- and mid-infrared observations reveal a flux excess in these domains, similar to those observed in SN 2010jl and other interacting transients, likely due to preexisting radiatively heated dust surrounding the supernova. By modeling the infrared excess, we infer a mass $\gtrsim0.4\times10^{-3}\,\rm{M_{\odot}}$ for the dust.
SN 2024dy: Dust formation in a long-lived Type IIn supernova and constraints on the dust mass
Kagoshima University（鹿儿岛大学）；Hiroshima University（广岛大学）；Tohoku University（东北大学）；Stockholm University（斯德哥尔摩大学）；Indian Institute of Astrophysics（印度天体物理研究所）
Fading Echoes of Interaction: Probing Centuries of Mass-Loss in Four Old Type IIn Supernovae
University of California, San Diego（加利福尼亚大学圣地亚哥分校）；University of Virginia（弗吉尼亚大学）；Indian Institute of Astrophysics（印度天体物理研究所）；University of California, Berkeley（加利福尼亚大学伯克利分校）
Excitation factors for horizonless compact objects: long-lived modes, echoes, and greybody factors
Dipartimento di Fisica, Sapienza Università di Roma（罗马大学物理系）；INFN, Sezione di Roma（意大利国家核物理研究所罗马分部）；Indian Institute of Technology, Gandhinagar（印度理工学院甘地纳加尔分校）；School of Physical Sciences, Indian Association for the Cultivation of Science（印度科学培养协会物理科学学院）
What sort of supernova gave rise to the Crab Nebula? There are several indications that the Crab arose from a sub-energetic explosion of an 8-10 Msun star, this appears to conflict with the high luminosity indicated by historical observations. This paper shows that several properties of the Crab are best suited to Type IIn-P explosions (Type IIn spectra with plateau light curves). These events probably arise from relatively low-energy (1e50 erg) explosions with low 56Ni yield resulting from electron-capture SNe (ecSNe), but their high luminosity and Type IIn spectra are dominated by shock inte…
SN 2019vxm: A luminous and long-lived Type IIn supernova with early flash-ionisation features
Tsinghua University（清华大学）；Yunnan Observatories, Chinese Academy of Sciences (CAS)（中国科学院云南天文台）；INAF - Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；National Astronomical Observatory of Japan, National Institutes of Natural Sciences（日本国立天文台，国立自然科学研究院）；Graduate Institute for Advanced Studies, SOKENDAI（综合研究大学院大学（SOKENDAI））；School of Physics and Astronomy, Monash University（蒙纳士大学物理与天文学院）；Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）；INAF - Osservatorio Astronomico di Brera（意大利国家天体物理研究所布雷拉天文台）；Department of Astronomy, University of California, Berkeley（加州大学伯克利分校天文学系）
SN 2019vxm是一颗峰值亮度高、演化缓慢的IIn型超新星，早期光谱显示闪光电离特征，后期红外超表明新尘埃形成，其光变曲线与SN 2010jl相似。
The bright long-lived Type II SN 2021irp powered by aspherical circumstellar material interaction (I): Revealing the energy source with photometry and spectroscopy
In this study we present the results of a five-year follow-up campaign of the long-lived type IIn supernova SN 2017hcc, found in a spiral dwarf host of near-solar metallicity. The long rise time (57 $\pm$ 2 days, ATLAS $o$ band) and high luminosity (peaking at $-$20.78 $\pm$ 0.01 mag in the ATLAS $o$ band) point towards an interaction of massive ejecta with massive and dense circumstellar material (CSM). The evolution of SN 2017hcc is slow, both spectroscopically and photometrically, reminiscent of the long-lived type IIn, SN 2010jl. An infrared (IR) excess was apparent soon after the peak, an…
While interaction with circumstellar material is known to play an important role in Type IIn supernovae (SNe), analyses of the more common SNe IIP and IIL have not traditionally included interaction as a significant power source. However, recent campaigns to observe SNe within days of explosion have revealed narrow emission lines of high-ionization species in the earliest spectra of luminous SNe II of all subclasses. These "flash ionization" features indicate the presence of a confined shell of material around the progenitor star. Here we present the first low-luminosity (LL) SN to show flash …
Two years of shock interaction tracing three phases of evolution: the explosion of a Type IIn supernova, SN 2019vxm
Indian Institute of Astrophysics（印度天体物理研究所）；Academy of Scientific and Innovative Research (AcSIR)（科学创新研究学院）；Tsung-Dao Lee Institute, Shanghai Jiao Tong University（上海交通大学李政道研究所）；Amanogawa Galaxy Astronomy Research Center (AGARC), Graduate School of Science and Engineering, Kagoshima University（鹿儿岛大学理工学研究系银河天文研究中心）；Department of Astronomy, Kyoto University（京都大学天文学系）；Hiroshima Astrophysical Science Centre, Hiroshima University（广岛大学广岛天体物理科学中心）；Graduate School of Science and Engineering, Kagoshima University（鹿儿岛大学理工学研究科）
We report on small-amplitude optical variability and recent dissipation of the unusually persistent broad emission lines in the blue compact dwarf galaxy PHL 293B. The galaxy's unusual spectral features (P Cygni-like profiles with $\sim$800 km s$^{-1}$ blueshifted absorption lines) have resulted in conflicting interpretations of the nature of this source in the literature. However, analysis of new Gemini spectroscopy reveals the broad emission has begun to fade after being persistent for over a decade prior. Precise difference imaging light curves constructed with the Sloan Digital Sky Survey …
The Type IIn supernova (SN) 2005ip is one of the most well-studied and long-lasting examples of a SN interacting with its circumstellar environment. The optical light curve plateaued at a nearly constant level for more than five years, suggesting ongoing shock interaction with an extended and clumpy circumstellar medium (CSM). Here we present continued observations of the SN from $\sim 1000-5000$ days post-explosion at all wavelengths, including X-ray, ultraviolet, near-infrared, and mid-infrared. The UV spectra probe the pre-explosion mass loss and show evidence for CNO processing. From the b…
Hydrogen-rich, core-collapse supernovae are typically divided into four classes: IIP, IIL, IIn, and IIb. In general, interaction with circumstellar material is only considered for Type IIn supernovae. However, recent hydrodynamic modeling of IIP and IIL supernovae requires circumstellar material to reproduce their early light curves. In this scenario, IIL supernovae experience large amounts of mass loss before exploding. We test this hypothesis on ASASSN-15oz, a Type IIL supernova. With extensive follow-up in the X- ray, UV, optical, IR, and radio we present our search for signs of interaction…
We present low-resolution near-IR 0.8-2.5 um spectra of SN2009ip, taken immediately before, during, and just after its rapid brightening in late Sep/Oct 2012. The first epoch shows the same general spectral characteristics as the later epochs (smooth continuum, narrow H and HeI emission lines), but the IR continuum shape is substantially redder than the later epochs. The epoch 1 continuum can be approximated by reddening the peak-luminosity (epoch 3) spectrum by E(B-V)=1.0 mag, but the blue color seen in visual-wavelength spectra at the same time indicates that strong wavelength-dependent exti…
The dominant mechanism and time scales over which stripped-envelope supernovae (SNe) progenitor stars shed their hydrogen envelopes are uncertain. Observations of Type Ib and Ic SNe at late phases could reveal the optical signatures of interaction with distant circumstellar material (CSM) providing important clues on the origin of the necessary pre-SN mass loss. We report deep late-time optical spectroscopy of the Type Ib explosion SN 2004dk 4684 days (13 years) after discovery. Prominent intermediate-width H-alpha emission is detected, signaling that the SN blast wave has caught up with the h…
We present photometry and spectroscopy of SN2013fs and SN2013fr in the first 100 days post-explosion. Both objects showed transient, relatively narrow H$α$ emission lines characteristic of SNeIIn, but later resembled normal SNeII-P or SNeII-L, indicative of fleeting interaction with circumstellar material (CSM). SN2013fs was discovered within 8hr of explosion. Its light curve exhibits a plateau, with spectra revealing strong CSM interaction at early times. It is a less luminous version of the transitional SNIIn PTF11iqb, further demonstrating a continuum of CSM interaction intensity between SN…
Nearby Supernova Science in the Era of High Cadence, Deep Time Domain Surveys
University of Arizona（亚利桑那大学）；University of California, San Diego（加州大学圣地亚哥分校）；Caltech（加州理工学院）；Gemini Observatory/NSF’s NOIRLab（吉米尼天文台/美国国家光学红外天文实验室）；Center for Astrophysics | Harvard & Smithsonian（哈佛-史密森天体物理中心）
