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1. Detailed spectrophotometric analysis of the superluminous and fast evolving SN 2019neq

Author

Fiore, Achille, Benetti, Stefano, Tartaglia, Leonardo, Jerkstrand, Anders, Salmaso, Irene, Tomasella, Lina, Morales-Garoffolo, Antonia, Geier, Stefan, Elias-Rosa, Nancy, Cappellaro, Enrico, Wang, Xiaofeng, Mo, Jun, Chen, Zhihao, Yan, Shengyu, Pastorello, Andrea, Mazzali, Paolo A., Ciolfi, Riccardo, Cai, Yongzhi, Fraser, Morgan, Gutiérrez, Claudia P., Karamehmetoglu, Emir, Kuncarayakti, Hanindyo, Moran, Shane, Ochner, Paolo, Reguitti, Andrea, Reynolds, Thomas M., Valerin, Giorgio, Fiore, Achille, Benetti, Stefano, Tartaglia, Leonardo, Jerkstrand, Anders, Salmaso, Irene, Tomasella, Lina, Morales-Garoffolo, Antonia, Geier, Stefan, Elias-Rosa, Nancy, Cappellaro, Enrico, Wang, Xiaofeng, Mo, Jun, Chen, Zhihao, Yan, Shengyu, Pastorello, Andrea, Mazzali, Paolo A., Ciolfi, Riccardo, Cai, Yongzhi, Fraser, Morgan, Gutiérrez, Claudia P., Karamehmetoglu, Emir, Kuncarayakti, Hanindyo, Moran, Shane, Ochner, Paolo, Reguitti, Andrea, Reynolds, Thomas M., and Valerin, Giorgio

Abstract

SN 2019neq was a very fast evolving superluminous supernova. At a redshift z = 0.1059, its peak absolute magnitude was −21.5 ± 0.2 mag in g band. In this work, we present data and analysis from an extensive spectrophotometric follow-up campaign using multiple observational facilities. Thanks to a nebular spectrum of SN 2019neq, we investigated some of the properties of the host galaxy at the location of SN 2019neq and found that its metallicity and specific star formation rate are in a good agreement with those usually measured for SLSNe-I hosts. We then discuss the plausibility of the magnetar and the circumstellar interaction scenarios to explain the observed light curves, and interpret a nebular spectrum of SN 2019neq using published SUMO radiative-transfer models. The results of our analysis suggest that the spin-down radiation of a millisecond magnetar with a magnetic field B ≃ 6×1014 G could boost the luminosity of SN 2019neq.

Published
2024
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2. Detailed spectrophotometric analysis of the superluminous and fast evolving SN 2019neq

Author

National Natural Science Foundation of China, Ministero dell'Istruzione, dell'Università e della Ricerca, European Commission, Junta de Andalucía, Istituto Nazionale di Astrofisica, Agencia Estatal de Investigación (España), Ministerio de Ciencia e Innovación (España), Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, Fiore, Achille, Benetti, Stefano, Tartaglia, Leonardo, Jerkstrand, Anders, Salmaso, Irene, Tomasella, Lina, Morales-Garoffolo, A., Geier, Stefan, Elias-Rosa, Nancy, Cappellaro, Enrico, Wang, Xiaofeng, Mo, Jun, Chen, Zhihao, Mazzali, Paolo A., Ciolfi, Riccardo, Cai, Yongzhi, Fraser, Morgan, Gutiérrez, Claudia P., Karamehmetoglu, Emir, Kuncarayakti, Hanindyo, Moran, Shane, Ochner, Paolo, Reguitti, Andrea, Reynolds, Thomas M., Valerin, Giorgio, National Natural Science Foundation of China, Ministero dell'Istruzione, dell'Università e della Ricerca, European Commission, Junta de Andalucía, Istituto Nazionale di Astrofisica, Agencia Estatal de Investigación (España), Ministerio de Ciencia e Innovación (España), Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, Fiore, Achille, Benetti, Stefano, Tartaglia, Leonardo, Jerkstrand, Anders, Salmaso, Irene, Tomasella, Lina, Morales-Garoffolo, A., Geier, Stefan, Elias-Rosa, Nancy, Cappellaro, Enrico, Wang, Xiaofeng, Mo, Jun, Chen, Zhihao, Mazzali, Paolo A., Ciolfi, Riccardo, Cai, Yongzhi, Fraser, Morgan, Gutiérrez, Claudia P., Karamehmetoglu, Emir, Kuncarayakti, Hanindyo, Moran, Shane, Ochner, Paolo, Reguitti, Andrea, Reynolds, Thomas M., and Valerin, Giorgio

Abstract

SN 2019neq was a very fast evolving superluminous supernova. At a redshift z = 0.1059, its peak absolute magnitude was −21.5 ± 0.2 mag in g band. In this work, we present data and analysis from an extensive spectrophotometric follow-up campaign using multiple observational facilities. Thanks to a nebular spectrum of SN 2019neq, we investigated some of the properties of the host galaxy at the location of SN 2019neq and found that its metallicity and specific star formation rate are in a good agreement with those usually measured for SLSNe-I hosts. We then discuss the plausibility of the magnetar and the circumstellar interaction scenarios to explain the observed light curves, and interpret a nebular spectrum of SN 2019neq using published SUMO radiative-transfer models. The results of our analysis suggest that the spin-down radiation of a millisecond magnetar with a magnetic field B 6 × 1014 G could boost the luminosity of SN 2019neq.

Published
2024

3. Supplementary data for Detailed spectrophotometric analysis of the superluminous and fast evolving SN 2019neq

Author

Fiore, Achille, Benetti, Stefano, Tartaglia, Leonardo, Jerkstrand, Anders, Salmaso, Irene, Tomasella, Lina, Morales-Garoffolo, A., Geier, Stefan, Elias-Rosa, Nancy, Cappellaro, Enrico, Wang, Xiaofeng, Mo, Jun, Chen, Zhihao, Mazzali, Paolo A., Ciolfi, Riccardo, Cai, Yongzhi, Fraser, Morgan, Gutiérrez, Claudia P., Karamehmetoglu, Emir, Kuncarayakti, Hanindyo, Moran, Shane, Ochner, Paolo, Reguitti, Andrea, Reynolds, Thomas M., Valerin, Giorgio, Fiore, Achille, Benetti, Stefano, Tartaglia, Leonardo, Jerkstrand, Anders, Salmaso, Irene, Tomasella, Lina, Morales-Garoffolo, A., Geier, Stefan, Elias-Rosa, Nancy, Cappellaro, Enrico, Wang, Xiaofeng, Mo, Jun, Chen, Zhihao, Mazzali, Paolo A., Ciolfi, Riccardo, Cai, Yongzhi, Fraser, Morgan, Gutiérrez, Claudia P., Karamehmetoglu, Emir, Kuncarayakti, Hanindyo, Moran, Shane, Ochner, Paolo, Reguitti, Andrea, Reynolds, Thomas M., and Valerin, Giorgio

Published
2024

4. Detailed spectrophotometric analysis of the superluminous and fast evolving SN 2019neq

Author

Fiore, Achille, Benetti, Stefano, Tartaglia, Leonardo, Jerkstrand, Anders, Salmaso, Irene, Tomasella, Lina, Morales-garoffolo, Antonia, Geier, Stefan, Elias-rosa, Nancy, Cappellaro, Enrico, Wang, Xiaofeng, Mo, Jun, Chen, Zhihao, Yan, Shengyu, Pastorello, Andrea, Mazzali, Paolo A, Ciolfi, Riccardo, Cai, Yongzhi, Fraser, Morgan, Gutiérrez, Claudia P, Karamehmetoglu, Emir, Kuncarayakti, Hanindyo, Moran, Shane, Ochner, Paolo, Reguitti, Andrea, Reynolds, Thomas M, Valerin, Giorgio, Fiore, Achille, Benetti, Stefano, Tartaglia, Leonardo, Jerkstrand, Anders, Salmaso, Irene, Tomasella, Lina, Morales-garoffolo, Antonia, Geier, Stefan, Elias-rosa, Nancy, Cappellaro, Enrico, Wang, Xiaofeng, Mo, Jun, Chen, Zhihao, Yan, Shengyu, Pastorello, Andrea, Mazzali, Paolo A, Ciolfi, Riccardo, Cai, Yongzhi, Fraser, Morgan, Gutiérrez, Claudia P, Karamehmetoglu, Emir, Kuncarayakti, Hanindyo, Moran, Shane, Ochner, Paolo, Reguitti, Andrea, Reynolds, Thomas M, and Valerin, Giorgio

Published
2024

5. Detailed spectrophotometric analysis of the superluminous and fast evolving SN 2019neq

Author

Fiore, Achille, Benetti, Stefano, Tartaglia, Leonardo, Jerkstrand, Anders, Salmaso, Irene, Tomasella, Lina, Morales-garoffolo, Antonia, Geier, Stefan, Elias-rosa, Nancy, Cappellaro, Enrico, Wang, Xiaofeng, Mo, Jun, Chen, Zhihao, Yan, Shengyu, Pastorello, Andrea, Mazzali, Paolo A, Ciolfi, Riccardo, Cai, Yongzhi, Fraser, Morgan, Gutiérrez, Claudia P, Karamehmetoglu, Emir, Kuncarayakti, Hanindyo, Moran, Shane, Ochner, Paolo, Reguitti, Andrea, Reynolds, Thomas M, Valerin, Giorgio, Fiore, Achille, Benetti, Stefano, Tartaglia, Leonardo, Jerkstrand, Anders, Salmaso, Irene, Tomasella, Lina, Morales-garoffolo, Antonia, Geier, Stefan, Elias-rosa, Nancy, Cappellaro, Enrico, Wang, Xiaofeng, Mo, Jun, Chen, Zhihao, Yan, Shengyu, Pastorello, Andrea, Mazzali, Paolo A, Ciolfi, Riccardo, Cai, Yongzhi, Fraser, Morgan, Gutiérrez, Claudia P, Karamehmetoglu, Emir, Kuncarayakti, Hanindyo, Moran, Shane, Ochner, Paolo, Reguitti, Andrea, Reynolds, Thomas M, and Valerin, Giorgio

Published
2024

6. Detailed spectrophotometric analysis of the superluminous and fast evolving SN 2019neq

Author

Fiore, Achille, Benetti, Stefano, Tartaglia, Leonardo, Jerkstrand, Anders, Salmaso, Irene, Tomasella, Lina, Morales-Garoffolo, Antonia, Geier, Stefan, Elias-Rosa, Nancy, Cappellaro, Enrico, Wang, Xiaofeng, Mo, Jun, Chen, Zhihao, Yan, Shengyu, Pastorello, Andrea, Mazzali, Paolo A., Ciolfi, Riccardo, Cai, Yongzhi, Fraser, Morgan, Gutiérrez, Claudia P., Karamehmetoglu, Emir, Kuncarayakti, Hanindyo, Moran, Shane, Ochner, Paolo, Reguitti, Andrea, Reynolds, Thomas M., Valerin, Giorgio, Fiore, Achille, Benetti, Stefano, Tartaglia, Leonardo, Jerkstrand, Anders, Salmaso, Irene, Tomasella, Lina, Morales-Garoffolo, Antonia, Geier, Stefan, Elias-Rosa, Nancy, Cappellaro, Enrico, Wang, Xiaofeng, Mo, Jun, Chen, Zhihao, Yan, Shengyu, Pastorello, Andrea, Mazzali, Paolo A., Ciolfi, Riccardo, Cai, Yongzhi, Fraser, Morgan, Gutiérrez, Claudia P., Karamehmetoglu, Emir, Kuncarayakti, Hanindyo, Moran, Shane, Ochner, Paolo, Reguitti, Andrea, Reynolds, Thomas M., and Valerin, Giorgio

Abstract

SN 2019neq was a very fast evolving superluminous supernova. At a redshift z=0.1059, its peak absolute magnitude was -21.5+/-0.2 mag in g band. In this work, we present data and analysis from an extensive spectrophotometric follow-up campaign using multiple observational facilities. Thanks to a nebular spectrum of SN 2019neq, we investigated some of the properties of the host galaxy at the location of SN 2019neq and found that its metallicity and specific star formation rate are in a good agreement with those usually measured for SLSNe-I hosts. We then discuss the plausibility of the magnetar and the circumstellar interaction scenarios to explain the observed light curves, and interpret a nebular spectrum of SN 2019neq using published SUMO radiative-transfer models. The results of our analysis suggest that the spindown radiation of a millisecond magnetar with a magnetic field B~6e14 G could boost the luminosity of SN 2019neq., Comment: 32 pages, 23 figures. Accepted by MNRAS

Published
2023

7. Close, bright, and boxy: the superluminous SN 2018hti

Author

European Commission, University of Hawaii, Ministero dell'Istruzione, dell'Università e della Ricerca, Comisión Nacional de Investigación Científica y Tecnológica (Chile), Fondo Nacional de Desarrollo Científico y Tecnológico (Chile), European Research Council, Agencia Nacional de Investigación y Desarrollo (Chile), National Science Foundation (US), Fiore, Achille, Benetti, Stefano, Nicholl, Matt, Reguitti, Andrea, Cappellaro, Enrico, Campana, Sergio, Bose, S., Paraskeva, E., Berger, E., Müller-Bravo, Tomás E., Burke, Jamison, Cai, Y-Z, Chen, T. W., Ciolfi, Riccardo, Dong, Subo, Gómez, Sergio, Gromadzki, Mariusz, Gutiérrez, Claudia P., Hiramatsu, Daichi, Hosseinzadeh, Griffin, Howell, D. A., Jerkstrand, Anders, Kankare, E., Kozyreva, A., Maguire, Kate, McCully, Curtis, Ochner, Paolo, Pellegrino, Conte, Pignata, Giuliano, Post, R. S., Elias-Rosa, Nancy, Shahbandeh, Melissa, Schuldt, S., Thomas, B. P., Tomasella, Lina, Vinkó, Jozsef, Vogl, Christian, Wheeler, J. Craig, Young, D. R., European Commission, University of Hawaii, Ministero dell'Istruzione, dell'Università e della Ricerca, Comisión Nacional de Investigación Científica y Tecnológica (Chile), Fondo Nacional de Desarrollo Científico y Tecnológico (Chile), European Research Council, Agencia Nacional de Investigación y Desarrollo (Chile), National Science Foundation (US), Fiore, Achille, Benetti, Stefano, Nicholl, Matt, Reguitti, Andrea, Cappellaro, Enrico, Campana, Sergio, Bose, S., Paraskeva, E., Berger, E., Müller-Bravo, Tomás E., Burke, Jamison, Cai, Y-Z, Chen, T. W., Ciolfi, Riccardo, Dong, Subo, Gómez, Sergio, Gromadzki, Mariusz, Gutiérrez, Claudia P., Hiramatsu, Daichi, Hosseinzadeh, Griffin, Howell, D. A., Jerkstrand, Anders, Kankare, E., Kozyreva, A., Maguire, Kate, McCully, Curtis, Ochner, Paolo, Pellegrino, Conte, Pignata, Giuliano, Post, R. S., Elias-Rosa, Nancy, Shahbandeh, Melissa, Schuldt, S., Thomas, B. P., Tomasella, Lina, Vinkó, Jozsef, Vogl, Christian, Wheeler, J. Craig, and Young, D. R.

Abstract

SN 2018hti was a very nearby (z = 0.0614) superluminous supernova with an exceedingly bright absolute magnitude of −21.7 mag in r band at maximum. The densely sampled pre-maximum light curves of SN 2018hti show a slow luminosity evolution and constrain the rise time to ∼50 rest-frame d. We fitted synthetic light curves to the photometry to infer the physical parameters of the explosion of SN 2018hti for both the magnetar and the CSM-interaction scenarios. We conclude that one of two mechanisms could be powering the luminosity of SN 2018hti; interaction with ∼10 M⊙ of circumstellar material or a magnetar with a magnetic field of Bp∼ 1.3 × 1013 G, and initial period of Pspin∼ 1.8 ms. From the nebular spectrum modelling we infer that SN 2018hti likely results from the explosion of a ∼40M⊙ progenitor star.

Published
2022

8. SN 2020wnt: a slow-evolving carbon-rich superluminous supernova with no O II lines and a bumpy light curve

Author

Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), European Commission, National Aeronautics and Space Administration (US), Gutiérrez, Claudia P., Pastorello, Andrea, Bersten, M. C., Benetti, Stefano, Orellana, M., Fiore, Achille, Karamehmetoglu, Emir, Kravtsov, T., Reguitti, Andrea, Reynolds, Thomas M., Valerin, Giorgio, Mazzali, Paolo A., Sullivan, Mark, Cai, Y-Z, Elias-Rosa, Nancy, Fraser, Morgan, Hsiao, E. Y., Kankare, E., Kotak, R., Kuncarayakti, Hanindyo, Li, Z., Mattila, Seppo, Mo, Jianhong, Morán, Sebastián, Ochner, Paolo, Shahbandeh, Melissa, Tomasella, Lina, Wang, X., Yan, S., Zhang, J., Zhang, T., Stritzinger, Maximilian, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), European Commission, National Aeronautics and Space Administration (US), Gutiérrez, Claudia P., Pastorello, Andrea, Bersten, M. C., Benetti, Stefano, Orellana, M., Fiore, Achille, Karamehmetoglu, Emir, Kravtsov, T., Reguitti, Andrea, Reynolds, Thomas M., Valerin, Giorgio, Mazzali, Paolo A., Sullivan, Mark, Cai, Y-Z, Elias-Rosa, Nancy, Fraser, Morgan, Hsiao, E. Y., Kankare, E., Kotak, R., Kuncarayakti, Hanindyo, Li, Z., Mattila, Seppo, Mo, Jianhong, Morán, Sebastián, Ochner, Paolo, Shahbandeh, Melissa, Tomasella, Lina, Wang, X., Yan, S., Zhang, J., Zhang, T., and Stritzinger, Maximilian

Abstract

We present the analysis of SN 2020wnt, an unusual hydrogen-poor superluminous supernova (SLSN-I), at a redshift of 0.032. The light curves of SN 2020wnt are characterized by an early bump lasting ∼5 d, followed by a bright main peak. The SN reaches a peak absolute magnitude of Mmaxr=−20.52±0.03 mag at ∼77.5 d from explosion. This magnitude is at the lower end of the luminosity distribution of SLSNe-I, but the rise-time is one of the longest reported to date. Unlike other SLSNe-I, the spectra of SN 2020wnt do not show O II, but strong lines of C II and Si II are detected. Spectroscopically, SN 2020wnt resembles the Type Ic SN 2007gr, but its evolution is significantly slower. Comparing the bolometric light curve to hydrodynamical models, we find that SN 2020wnt luminosity can be explained by radioactive powering. The progenitor of SN 2020wnt is likely a massive and extended star with a pre-SN mass of 80 M⊙ and a pre-SN radius of 15 R⊙ that experiences a very energetic explosion of 45 × 1051 erg, producing 4 M⊙ of 56Ni. In this framework, the first peak results from a post-shock cooling phase for an extended progenitor, and the luminous main peak is due to a large nickel production. These characteristics are compatible with the pair-instability SN scenario. We note, however, that a significant contribution of interaction with circumstellar material cannot be ruled out.

Published
2022

9. Observations of the Very Young Type Ia Supernova 2019np with Early-excess Emission

Author

Sai, Hanna, Wang, Xiaofeng, Elias-Rosa, Nancy, Yang, Yi, Zhang, Jujia, Lin, Weili, Mo, Jun, Piro, Anthony L., Zeng, Xiangyun, Andrea, Reguitti, Brown, Peter, Burns, Christopher R., Cai, Yongzhi, Fiore, Achille, Hsiao, Eric Y., Isern, Jordi, Itagaki, K., Li, Wenxiong, Li, Zhitong, Pessi, Priscila J., Phillips, M. M., Schuldt, Stefan, Shahbandeh, Melissa, Stritzinger, Maximilian D., Tomasella, Lina, Vogl, Christian, Wang, Bo, Wang, Lingzhi, Wu, Chengyuan, Yang, Sheng, Zhang, Jicheng, Zhang, Tianmeng, Zhang, Xinghan, Sai, Hanna, Wang, Xiaofeng, Elias-Rosa, Nancy, Yang, Yi, Zhang, Jujia, Lin, Weili, Mo, Jun, Piro, Anthony L., Zeng, Xiangyun, Andrea, Reguitti, Brown, Peter, Burns, Christopher R., Cai, Yongzhi, Fiore, Achille, Hsiao, Eric Y., Isern, Jordi, Itagaki, K., Li, Wenxiong, Li, Zhitong, Pessi, Priscila J., Phillips, M. M., Schuldt, Stefan, Shahbandeh, Melissa, Stritzinger, Maximilian D., Tomasella, Lina, Vogl, Christian, Wang, Bo, Wang, Lingzhi, Wu, Chengyuan, Yang, Sheng, Zhang, Jicheng, Zhang, Tianmeng, and Zhang, Xinghan

Abstract

Early-time radiative signals from type Ia supernovae (SNe Ia) can provide important constraints on the explosion mechanism and the progenitor system. We present observations and analysis of SN 2019np, a nearby SN Ia discovered within 1-2 days after the explosion. Follow-up observations were conducted in optical, ultraviolet, and near-infrared bands, covering the phases from $\sim-$16.7 days to $\sim$+367.8 days relative to its $B-$band peak luminosity. The photometric and spectral evolutions of SN 2019np resembles the average behavior of normal SNe Ia. The absolute B-band peak magnitude and the post-peak decline rate are $M_{\rm max}(B)=-19.52 \pm 0.47$mag and $\Delta m_{\rm15}(B) =1.04 \pm 0.04$mag, respectively. No Hydrogen line has been detected in the near-infrared and nebular-phase spectra of SN 2019np. Assuming that the $^{56}$Ni powering the light curve is centrally located, we find that the bolometric light curve of SN 2019np shows a flux excess up to 5.0% in the early phase compared to the radiative diffusion model. Such an extra radiation perhaps suggests the presence of an additional energy source beyond the radioactive decay of central nickel. Comparing the observed color evolution with that predicted by different models such as interactions of SN ejecta with circumstellar matter (CSM)/companion star, a double-detonation explosion from a sub-Chandrasekhar mass white dwarf (WD), and surface $^{56}$Ni mixing, the latter one is favored., Comment: 23 pages, 16 figures, accepted for publication in MNRAS

Published
2022
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10. SN 2017gci: a nearby Type I Superluminous Supernova with a bumpy tail

Author

Fiore, Achille, Chen, Ting-Wan, Jerkstrand, Anders, Benetti, Stefano, Ciolfi, Riccardo, Inserra, Cosimo, Cappellaro, Enrico, Pastorello, Andrea, Leloudas, Giorgos, Schulze, Steve, Berton, Marco, Gutiérrez, Claudia Patricia, Burke, Jamison, Gromadzki, Mariusz, Nicholl, Matt, Rau, Arne, Sollerman, Jesper, McCully, Curtis, Fong, Wen-fai, Galbany, Lluís, Hiramatsu, Daichi, Howell, D. Andrew, Kankare, Erkki, Lunnan, Ragnhlid, Müller-Bravo, Tomás E., Neill, David O, Young, David R., Terreran, Giacomo, Valenti, Stefano, Fiore, Achille, Chen, Ting-Wan, Jerkstrand, Anders, Benetti, Stefano, Ciolfi, Riccardo, Inserra, Cosimo, Cappellaro, Enrico, Pastorello, Andrea, Leloudas, Giorgos, Schulze, Steve, Berton, Marco, Gutiérrez, Claudia Patricia, Burke, Jamison, Gromadzki, Mariusz, Nicholl, Matt, Rau, Arne, Sollerman, Jesper, McCully, Curtis, Fong, Wen-fai, Galbany, Lluís, Hiramatsu, Daichi, Howell, D. Andrew, Kankare, Erkki, Lunnan, Ragnhlid, Müller-Bravo, Tomás E., Neill, David O, Young, David R., Terreran, Giacomo, and Valenti, Stefano

Abstract

We present and discuss the optical spectro-photometric observations of the nearby (z=0.087) Type I superluminous supernova (SLSN I) SN 2017gci, whose peak K-corrected absolute magnitude reaches Mg=-21.5 mag. Its photometric and spectroscopic evolution includes features of both slow and of fast evolving SLSN I, thus favoring a continuum distribution between the two SLSN-I subclasses. In particular, similarly to other SLSNe I, the multi-band light curves of SN 2017gci show two rebrightenings at about 103 and 142 days after the maximum light. Interestingly, this broadly agrees with a broad emission feature emerging around 6520 A after 51 days from the maximum light, which is followed by a sharp knee in the light curve. If we interpret this feature as Halpha, this could support the fact that the bumps are the signature of late interactions of the ejecta with a (hydrogen rich) circumstellar material. Then we fitted magnetar and CSM-interaction powered synthetic light curves onto the bolometric one of SN 2017gci. In the magnetar case, the fit suggests a polar magnetic field Bp = 6 x 1e14 G, an initial period of the magnetar Pinitial=2.8 ms, an ejecta mass Mejecta=9 Msun and an ejecta opacity k = 0.08 cm g^{-1} . A CSM interaction scenario would imply a CSM mass of 5 Msun and an ejecta mass of 12 Msun. Finally, the nebular spectrum of phase 187 days was modeled, deriving a mass of 10 Msun for the ejecta. Our models suggest that either a magnetar or CSM interaction might be the power sources for SN 2017gci and that its progenitor was a massive (40 Msun) star., Comment: 25 pages, 16 Figures, 15 Tables, accepted for publication in MNRAS

Published
2020
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11. Photometric and spectroscopic evolution of the peculiar Type IIn SN 2012ab

Author

Gangopadhyay, Anjasha, Turatto, Massimo, Benetti, Stefano, Misra, Kuntal, Kumar, Brajesh, Cappellaro, Enrico, Pastorello, Andrea, Tomasella, Lina, Vanni, Sabrina, Fiore, Achille, Morales-Garoffolo, A., Elias-Rosa, Nancy, Singh, Mridweeka, Dastidar, Raya, Ochner, Paolo, Tartaglia, Leonardo, Kumar, Brijesh, Pandey, Shashi Bhushan, Gangopadhyay, Anjasha, Turatto, Massimo, Benetti, Stefano, Misra, Kuntal, Kumar, Brajesh, Cappellaro, Enrico, Pastorello, Andrea, Tomasella, Lina, Vanni, Sabrina, Fiore, Achille, Morales-Garoffolo, A., Elias-Rosa, Nancy, Singh, Mridweeka, Dastidar, Raya, Ochner, Paolo, Tartaglia, Leonardo, Kumar, Brijesh, and Pandey, Shashi Bhushan

Abstract

We present an extensive ($\sim$ 1200 d) photometric and spectroscopic monitoring of the Type IIn supernova (SN) 2012ab. After a rapid initial rise leading to a bright maximum (M$_{R}$ = $-$19.39 mag), the light curves show a plateau lasting about 2 months followed by a steep decline up to about 100 d. Only in the $U$ band the decline is constant in the same interval. At later phases, the light curves remain flatter than the $^{56}$Co decline suggesting the increasing contribution of the interaction between SN ejecta with circumstellar material (CSM). Although heavily contaminated by emission lines of the host galaxy, the early spectral sequence (until 32 d) shows persistent narrow emissions, indicative of slow unshocked CSM, and the emergence of broad Balmer lines of hydrogen with P-Cygni profiles over a blue continuum, arising from a fast expanding SN ejecta. From about 2 months to $\sim$1200 d, the P-Cygni profiles are overcome by intermediate width emissions (FWHM $\sim 6000$ \kms), produced in the shocked region due to interaction. On the red wing a red bump appears after 76 d, likely a signature of the onset of interaction of the receding ejecta with the CSM. The presence of fast material both approaching and then receding is suggestive that we are observing the SN along the axis of a jet-like ejection in a cavity devoid of or uninterrupted by CSM in the innermost regions., Comment: 8 Tables, 17 Figures. Accepted for publication in MNRAS

Published
2020
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12. Photometric and spectroscopic evolution of the peculiar Type IIn SN 2012ab

Author

Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), European Commission, Istituto Nazionale di Fisica Nucleare, Gangopadhyay, Anjansha, Turatto, Massimo, Benetti, Stefano, Misra, Kuntal, Kumar, Brajesh, Cappellaro, Enrico, Pastorello, Andrea, Tomasella, Lina, Vanni, Sabrina, Fiore, Achille, Morales-Garoffolo, A., Elias-Rosa, Nancy, Singh, Mridweeka, Dastidar, Raya, Ochner, Paolo, Tartaglia, Leonardo, Kumar, Brijesh, Pandey, Shashi Bhushan, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), European Commission, Istituto Nazionale di Fisica Nucleare, Gangopadhyay, Anjansha, Turatto, Massimo, Benetti, Stefano, Misra, Kuntal, Kumar, Brajesh, Cappellaro, Enrico, Pastorello, Andrea, Tomasella, Lina, Vanni, Sabrina, Fiore, Achille, Morales-Garoffolo, A., Elias-Rosa, Nancy, Singh, Mridweeka, Dastidar, Raya, Ochner, Paolo, Tartaglia, Leonardo, Kumar, Brijesh, and Pandey, Shashi Bhushan

Abstract

We present an extensive (∼1200 d) photometric and spectroscopic monitoring of the Type IIn supernova (SN) 2012ab. After a rapid initial rise leading to a bright maximum (MR = −19.39 mag), the light curves show a plateau lasting about 2 months followed by a steep decline up to about 100 d. Only in the U band, the decline is constant in the same interval. At later phases, the light curves remain flatter than the 56Co decline, suggesting the increasing contribution of the interaction between SN ejecta with circumstellar material (CSM). Although heavily contaminated by emission lines of the host galaxy, the early spectral sequence (until 32 d) shows persistent narrow emissions, indicative of slow unshocked CSM, and the emergence of broad Balmer lines of hydrogen with P-Cygni profiles over a blue continuum, arising from a fast expanding SN ejecta. From about 2 months to ∼1200 d, the P-Cygni profiles are overcome by intermediate width emissions [full width at half-maximum (FWHM) ∼6000 km s−1], produced in the shocked region due to interaction. On the red wing, a red bump appears after 76 d, likely a signature of the onset of interaction of the receding ejecta with the CSM. The presence of fast material both approaching and then receding is suggestive that we are observing the SN along the axis of a jet-like ejection in a cavity devoid of or uninterrupted by CSM in the innermost regions.

Published
2020

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