Imagen de Portada

The transitional Type Ibn/IIn SN 2022pda, with pre-explosion outbursts and a double-peaked light curve

Fuente: arXiv

Guardado en:

Detalles Bibliográficos
Autores principales:	Cai, Y. -Z., Pastorello, A., Chiba, R., Moriya, T. J., Reguitti, A., Tartaglia, L., Moran, S., Campana, S., Wang, Z. -Y., Zhao, J. -W., Anderson, J. P., Benetti, S., Brennan, S. J., Cappellaro, E., Chambers, K. C., Chen, T. -W., Chen, Z. -H., de Boer, T., Dong, Y. -Z., Duarte, J., Elias-Rosa, N., Fraser, M., Gan, W. -P., Gao, H., Gromadzki, M., Hosseinzadeh, G., Howell, D. A., Inserra, C., Kangas, T., Kankare, E., Kravtsov, T., Li, L. -P., Lin, C. -C., Lowe, T. B., Lundqvist, P., Magnier, E. A., Matilainen, K., Mazzali, P. A., McCully, C., Minguez, P., Müller-Bravo, T. E., Newsome, M., Gonzalez, E. Padilla, Pellegrino, C., Pessi, P. J., Petrushevska, T., Pignata, G., Santos, R. P., Schulze, S., Smartt, S. J., Smith, I. A., Smith, K. W., Sollerman, J., Srivastav, S., Stritzinger, M. D., Terreran, G., Valerin, G., Wainscoat, R., Wang, S. -Q., Young, D. R., Galbany, L., Li, Z., Salmaso, I., Zha, S., Bai, J. -M., Wang, B., Wang, X. -F., Zhang, J. -J.
Formato:	Preprint
Publicado:	2026
Materias:	High Energy Astrophysical Phenomena Solar and Stellar Astrophysics
Acceso en línea:	Acceder al recurso
Etiquetas:	Agregar Etiqueta Sin Etiquetas, Sea el primero en etiquetar este registro!

_version_	1866917531633057792
author	Cai, Y. -Z. Pastorello, A. Chiba, R. Moriya, T. J. Reguitti, A. Tartaglia, L. Moran, S. Campana, S. Wang, Z. -Y. Zhao, J. -W. Anderson, J. P. Benetti, S. Brennan, S. J. Cappellaro, E. Chambers, K. C. Chen, T. -W. Chen, Z. -H. de Boer, T. Dong, Y. -Z. Duarte, J. Elias-Rosa, N. Fraser, M. Gan, W. -P. Gao, H. Gromadzki, M. Hosseinzadeh, G. Howell, D. A. Inserra, C. Kangas, T. Kankare, E. Kravtsov, T. Li, L. -P. Lin, C. -C. Lowe, T. B. Lundqvist, P. Magnier, E. A. Matilainen, K. Mazzali, P. A. McCully, C. Minguez, P. Müller-Bravo, T. E. Newsome, M. Gonzalez, E. Padilla Pellegrino, C. Pessi, P. J. Petrushevska, T. Pignata, G. Santos, R. P. Schulze, S. Smartt, S. J. Smith, I. A. Smith, K. W. Sollerman, J. Srivastav, S. Stritzinger, M. D. Terreran, G. Valerin, G. Wainscoat, R. Wang, S. -Q. Young, D. R. Galbany, L. Li, Z. Salmaso, I. Zha, S. Bai, J. -M. Wang, B. Wang, X. -F. Zhang, J. -J.
author_facet	Cai, Y. -Z. Pastorello, A. Chiba, R. Moriya, T. J. Reguitti, A. Tartaglia, L. Moran, S. Campana, S. Wang, Z. -Y. Zhao, J. -W. Anderson, J. P. Benetti, S. Brennan, S. J. Cappellaro, E. Chambers, K. C. Chen, T. -W. Chen, Z. -H. de Boer, T. Dong, Y. -Z. Duarte, J. Elias-Rosa, N. Fraser, M. Gan, W. -P. Gao, H. Gromadzki, M. Hosseinzadeh, G. Howell, D. A. Inserra, C. Kangas, T. Kankare, E. Kravtsov, T. Li, L. -P. Lin, C. -C. Lowe, T. B. Lundqvist, P. Magnier, E. A. Matilainen, K. Mazzali, P. A. McCully, C. Minguez, P. Müller-Bravo, T. E. Newsome, M. Gonzalez, E. Padilla Pellegrino, C. Pessi, P. J. Petrushevska, T. Pignata, G. Santos, R. P. Schulze, S. Smartt, S. J. Smith, I. A. Smith, K. W. Sollerman, J. Srivastav, S. Stritzinger, M. D. Terreran, G. Valerin, G. Wainscoat, R. Wang, S. -Q. Young, D. R. Galbany, L. Li, Z. Salmaso, I. Zha, S. Bai, J. -M. Wang, B. Wang, X. -F. Zhang, J. -J.
contents	We report the results of a photometric and spectroscopic follow-up campaign of the unusual interacting supernova (SN) 2022pda. Precursor variability lasting $\sim 100$ days is observed before the explosion. The SN light curve has a double peak shape. It reached a first maximum of $M_{\rm{r}} = -19.6 \pm 0.2$\,mag, followed by an initial two-month decline and a second, broad peak lasting about six months. The early spectra show a blue continuum with dominant H and He emission lines. A high-resolution pre-maximum spectrum shows that the profile of the \Hei~$λ$5876 line consists of a moderately narrow ($\sim 1900$ \kms) P~Cygni absorption superposed on a broader ($\sim 3300$ \kms) component. In the blue region, several spectral features are identified, including C {\sc iii}/N {\sc iii}/O {\sc ii} blends. Two broad bumps at 4600--5200 Å, 6400--6800~Å regions reveal a complex profile, which are likely due to blends of H, He, and other emission lines. Late-time spectra are still dominated by prominent and broad H and He lines in emission. Shock-driven model fits to the bolometric light curve suggest that the SN is powered by interaction with a massive CSM with enhanced mass loss rates $\sim 5$ \msun yr$^{-1}$, expelled during two events occurred $\sim 1$ and $\sim 0.2$ years before the explosion. The overall SN evolution indicates that SN\,2022pda is a transitional event between a H-rich SN IIn (SN\,2009ip-like) and a He-rich SN Ibn. Our findings suggest that the progenitor was likely a Luminous Blue Variable transitioning towards a Wolf--Rayet stage.
format	Preprint
id	arxiv_https___arxiv_org_abs_2605_25823
institution	arXiv
publishDate	2026
record_format	arxiv
spellingShingle	The transitional Type Ibn/IIn SN 2022pda, with pre-explosion outbursts and a double-peaked light curve Cai, Y. -Z. Pastorello, A. Chiba, R. Moriya, T. J. Reguitti, A. Tartaglia, L. Moran, S. Campana, S. Wang, Z. -Y. Zhao, J. -W. Anderson, J. P. Benetti, S. Brennan, S. J. Cappellaro, E. Chambers, K. C. Chen, T. -W. Chen, Z. -H. de Boer, T. Dong, Y. -Z. Duarte, J. Elias-Rosa, N. Fraser, M. Gan, W. -P. Gao, H. Gromadzki, M. Hosseinzadeh, G. Howell, D. A. Inserra, C. Kangas, T. Kankare, E. Kravtsov, T. Li, L. -P. Lin, C. -C. Lowe, T. B. Lundqvist, P. Magnier, E. A. Matilainen, K. Mazzali, P. A. McCully, C. Minguez, P. Müller-Bravo, T. E. Newsome, M. Gonzalez, E. Padilla Pellegrino, C. Pessi, P. J. Petrushevska, T. Pignata, G. Santos, R. P. Schulze, S. Smartt, S. J. Smith, I. A. Smith, K. W. Sollerman, J. Srivastav, S. Stritzinger, M. D. Terreran, G. Valerin, G. Wainscoat, R. Wang, S. -Q. Young, D. R. Galbany, L. Li, Z. Salmaso, I. Zha, S. Bai, J. -M. Wang, B. Wang, X. -F. Zhang, J. -J. High Energy Astrophysical Phenomena Solar and Stellar Astrophysics We report the results of a photometric and spectroscopic follow-up campaign of the unusual interacting supernova (SN) 2022pda. Precursor variability lasting $\sim 100$ days is observed before the explosion. The SN light curve has a double peak shape. It reached a first maximum of $M_{\rm{r}} = -19.6 \pm 0.2$\,mag, followed by an initial two-month decline and a second, broad peak lasting about six months. The early spectra show a blue continuum with dominant H and He emission lines. A high-resolution pre-maximum spectrum shows that the profile of the \Hei~$λ$5876 line consists of a moderately narrow ($\sim 1900$ \kms) P~Cygni absorption superposed on a broader ($\sim 3300$ \kms) component. In the blue region, several spectral features are identified, including C {\sc iii}/N {\sc iii}/O {\sc ii} blends. Two broad bumps at 4600--5200 Å, 6400--6800~Å regions reveal a complex profile, which are likely due to blends of H, He, and other emission lines. Late-time spectra are still dominated by prominent and broad H and He lines in emission. Shock-driven model fits to the bolometric light curve suggest that the SN is powered by interaction with a massive CSM with enhanced mass loss rates $\sim 5$ \msun yr$^{-1}$, expelled during two events occurred $\sim 1$ and $\sim 0.2$ years before the explosion. The overall SN evolution indicates that SN\,2022pda is a transitional event between a H-rich SN IIn (SN\,2009ip-like) and a He-rich SN Ibn. Our findings suggest that the progenitor was likely a Luminous Blue Variable transitioning towards a Wolf--Rayet stage.
title	The transitional Type Ibn/IIn SN 2022pda, with pre-explosion outbursts and a double-peaked light curve
topic	High Energy Astrophysical Phenomena Solar and Stellar Astrophysics
url	https://arxiv.org/abs/2605.25823