Supernovae at Distances < 40 Mpc: II. Supernova Rate in the Local Universe
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2025
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| author | Ma, Xiaoran Wang, Xiaofeng Mo, Jun Howell, D. Andrew Pellegrino, Craig Zhang, Jujia Wu, Chengyuan Yan, Shengyu Liu, Dongdong Arcavi, Iair Chen, Zhihao Farah, Joseph Gonzalez, Estefania Padilla Guo, Fangzhou Hiramatsu, Daichi Li, Gaici Lin, Han Liu, Jialian McCully, Curtis Newsome, Megan Sai, Hanna Terreran, Giacomo Xiang, Danfeng Zhang, Xinhan |
| author_facet | Ma, Xiaoran Wang, Xiaofeng Mo, Jun Howell, D. Andrew Pellegrino, Craig Zhang, Jujia Wu, Chengyuan Yan, Shengyu Liu, Dongdong Arcavi, Iair Chen, Zhihao Farah, Joseph Gonzalez, Estefania Padilla Guo, Fangzhou Hiramatsu, Daichi Li, Gaici Lin, Han Liu, Jialian McCully, Curtis Newsome, Megan Sai, Hanna Terreran, Giacomo Xiang, Danfeng Zhang, Xinhan |
| contents | Context.This is the second paper of a series aiming to determine the birth rates of supernovae in the local Universe. Aims. In this paper, we aim to estimate the SN rates in the local universe and fit the delay-time distribution of SNe Ia to put constraints on their progenitor scenarios. Methods.We performed a Monte-Carlo simulation to estimate the volumetric rates with the nearby SN sample introduced in Paper I of the series. The rate evolution of core-collapse SNe well traces the evolution of cosmic star formation history; while that of SNe Ia involves the convolution of cosmic star-formation history and a two-component delay-time distribution including a power law and a Gaussian component. Results.The volumetric rates of type Ia, Ibc and II SNe are derived as $0.325\pm0.040^{+0.016}_{-0.010}$, $0.160\pm0.028^{+0.044}_{-0.014}$, and $0.528\pm0.051^{+0.162}_{-0.013}$ (in unit of $10^{-4} yr^{-1} Mpc^{-3} h^3_{70}$), respectively. The rate of CCSNe is consistent with previous estimates. The newly derived local SN Ia rate is larger than existing results given at redshifts 0.01 < z < 0.1, favoring an increased rate from the universe at z ~ 0.1 to the local universe. A two-component model can well fit the rate variation, with the power law component accounting for the rate evolution at larger redshifts and the Gaussian component with a delay time of 12.63$\pm$0.38 Gyr accounting for the local rate evolution. This delayed component with such a longer delay time suggests that the progenitors of these SNe Ia were formed at around 1 Gyr after the birth of the universe, which could only be explained by a double-degenerate progenitor scenario. This is evidenced by the comparison with the PTF sample of SNe Ia at z = 0.073, which reveals that the increase in SN Ia rate at z < 0.01 is primarily due to the SNe Ia of massive E and S0 galaxies with old stellar populations. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2504_04507 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Supernovae at Distances < 40 Mpc: II. Supernova Rate in the Local Universe Ma, Xiaoran Wang, Xiaofeng Mo, Jun Howell, D. Andrew Pellegrino, Craig Zhang, Jujia Wu, Chengyuan Yan, Shengyu Liu, Dongdong Arcavi, Iair Chen, Zhihao Farah, Joseph Gonzalez, Estefania Padilla Guo, Fangzhou Hiramatsu, Daichi Li, Gaici Lin, Han Liu, Jialian McCully, Curtis Newsome, Megan Sai, Hanna Terreran, Giacomo Xiang, Danfeng Zhang, Xinhan High Energy Astrophysical Phenomena Astrophysics of Galaxies Context.This is the second paper of a series aiming to determine the birth rates of supernovae in the local Universe. Aims. In this paper, we aim to estimate the SN rates in the local universe and fit the delay-time distribution of SNe Ia to put constraints on their progenitor scenarios. Methods.We performed a Monte-Carlo simulation to estimate the volumetric rates with the nearby SN sample introduced in Paper I of the series. The rate evolution of core-collapse SNe well traces the evolution of cosmic star formation history; while that of SNe Ia involves the convolution of cosmic star-formation history and a two-component delay-time distribution including a power law and a Gaussian component. Results.The volumetric rates of type Ia, Ibc and II SNe are derived as $0.325\pm0.040^{+0.016}_{-0.010}$, $0.160\pm0.028^{+0.044}_{-0.014}$, and $0.528\pm0.051^{+0.162}_{-0.013}$ (in unit of $10^{-4} yr^{-1} Mpc^{-3} h^3_{70}$), respectively. The rate of CCSNe is consistent with previous estimates. The newly derived local SN Ia rate is larger than existing results given at redshifts 0.01 < z < 0.1, favoring an increased rate from the universe at z ~ 0.1 to the local universe. A two-component model can well fit the rate variation, with the power law component accounting for the rate evolution at larger redshifts and the Gaussian component with a delay time of 12.63$\pm$0.38 Gyr accounting for the local rate evolution. This delayed component with such a longer delay time suggests that the progenitors of these SNe Ia were formed at around 1 Gyr after the birth of the universe, which could only be explained by a double-degenerate progenitor scenario. This is evidenced by the comparison with the PTF sample of SNe Ia at z = 0.073, which reveals that the increase in SN Ia rate at z < 0.01 is primarily due to the SNe Ia of massive E and S0 galaxies with old stellar populations. |
| title | Supernovae at Distances < 40 Mpc: II. Supernova Rate in the Local Universe |
| topic | High Energy Astrophysical Phenomena Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2504.04507 |