A Near-IR Search for Helium in the Superluminous Supernova SN 2024ahr
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| Autores principales: | , , , , , , , , , , , , , , , |
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2025
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| author | Kumar, Harsh Berger, Edo Blanchard, Peter K. Gomez, Sebastian Hiramatsu, Daichi Andrews, Moira Bostroem, K. Azalee Dong, Yize Farah, Joseph Gonzalez, Estefania Padilla Howell, D. Andrew McCully, Curtis Mehta, Darshana Newsome, Megan Ravi, Aravind P. Terreran, Giacomo |
| author_facet | Kumar, Harsh Berger, Edo Blanchard, Peter K. Gomez, Sebastian Hiramatsu, Daichi Andrews, Moira Bostroem, K. Azalee Dong, Yize Farah, Joseph Gonzalez, Estefania Padilla Howell, D. Andrew McCully, Curtis Mehta, Darshana Newsome, Megan Ravi, Aravind P. Terreran, Giacomo |
| contents | We present a detailed study of SN 2024ahr, a hydrogen-poor superluminous supernova (SLSN-I), for which we determine a redshift of $z=0.0861$. SN 2024ahr has a peak absolute magnitude of $M_g\approx M_r\approx -21$ mag, rest-frame rise and decline times (50$\%$ of peak) of about 40 and 80 days, respectively, and typical spectroscopic evolution in the optical band. Similarly, modeling of the UV/optical light curves with a magnetar spin-down engine leads to typical parameters: an initial spin period of $\approx 3.3$ ms, a magnetic field strength of $\approx 6\times 10^{13}$ G, and an ejecta mass of $\approx 9.5$ M$_\odot$. Due to its relatively low redshift we obtained a high signal-to-noise ratio near-IR spectrum about 43 rest-frame days post-peak to search for the presence of helium. We do not detect any significant feature at the location of the He I $\,λ2.058$ $μ$m feature, and place a conservative upper limit of $\sim 0.05$ M$_\odot$ on the mass of helium in the outer ejecta. We detect broad features of Mg I $\,λ1.575$ $μ$m and a blend of Co II $\,λ2.126$ $μ$m and Mg II, $λ2.136$ $μ$m, which are typical of Type Ic SNe, but with higher velocities. Examining the sample of SLSNe-I with NIR spectroscopy, we find that, unlike SN 2024ahr, these events are generally peculiar. This highlights the need for a large sample of prototypical SLSNe-I with NIR spectroscopy to constrain the fraction of progenitors with helium (Ib-like) and without helium (Ic-like) at the time of the explosion, and hence the evolutionary path(s) leading to the rare outcome of SLSNe-I. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2501_01485 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | A Near-IR Search for Helium in the Superluminous Supernova SN 2024ahr Kumar, Harsh Berger, Edo Blanchard, Peter K. Gomez, Sebastian Hiramatsu, Daichi Andrews, Moira Bostroem, K. Azalee Dong, Yize Farah, Joseph Gonzalez, Estefania Padilla Howell, D. Andrew McCully, Curtis Mehta, Darshana Newsome, Megan Ravi, Aravind P. Terreran, Giacomo High Energy Astrophysical Phenomena Astrophysics of Galaxies Solar and Stellar Astrophysics We present a detailed study of SN 2024ahr, a hydrogen-poor superluminous supernova (SLSN-I), for which we determine a redshift of $z=0.0861$. SN 2024ahr has a peak absolute magnitude of $M_g\approx M_r\approx -21$ mag, rest-frame rise and decline times (50$\%$ of peak) of about 40 and 80 days, respectively, and typical spectroscopic evolution in the optical band. Similarly, modeling of the UV/optical light curves with a magnetar spin-down engine leads to typical parameters: an initial spin period of $\approx 3.3$ ms, a magnetic field strength of $\approx 6\times 10^{13}$ G, and an ejecta mass of $\approx 9.5$ M$_\odot$. Due to its relatively low redshift we obtained a high signal-to-noise ratio near-IR spectrum about 43 rest-frame days post-peak to search for the presence of helium. We do not detect any significant feature at the location of the He I $\,λ2.058$ $μ$m feature, and place a conservative upper limit of $\sim 0.05$ M$_\odot$ on the mass of helium in the outer ejecta. We detect broad features of Mg I $\,λ1.575$ $μ$m and a blend of Co II $\,λ2.126$ $μ$m and Mg II, $λ2.136$ $μ$m, which are typical of Type Ic SNe, but with higher velocities. Examining the sample of SLSNe-I with NIR spectroscopy, we find that, unlike SN 2024ahr, these events are generally peculiar. This highlights the need for a large sample of prototypical SLSNe-I with NIR spectroscopy to constrain the fraction of progenitors with helium (Ib-like) and without helium (Ic-like) at the time of the explosion, and hence the evolutionary path(s) leading to the rare outcome of SLSNe-I. |
| title | A Near-IR Search for Helium in the Superluminous Supernova SN 2024ahr |
| topic | High Energy Astrophysical Phenomena Astrophysics of Galaxies Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2501.01485 |