TY - JOUR

T1 - SN 2024ggi in NGC 3621

T2 - Rising Ionization in a Nearby, Circumstellar-material-interacting Type II Supernova

AU - Jacobson-Galán, W. V.

AU - Davis, K. W.

AU - Kilpatrick, C. D.

AU - Dessart, L.

AU - Margutti, R.

AU - Chornock, R.

AU - Foley, R. J.

AU - Arunachalam, P.

AU - Auchettl, K.

AU - Bom, C. R.

AU - Cartier, R.

AU - Coulter, D. A.

AU - Dimitriadis, G.

AU - Dickinson, D.

AU - Drout, M. R.

AU - Gagliano, A. T.

AU - Gall, C.

AU - Garretson, B.

AU - Izzo, L.

AU - LeBaron, N.

AU - Miao, H. Y.

AU - Milisavljevic, D.

AU - Rest, A.

AU - Rojas-Bravo, C.

AU - Santos, A.

AU - Sears, H.

AU - Subrayan, B. M.

AU - Taggart, K.

AU - Tinyanont, S.

PY - 2024/9/5

Y1 - 2024/9/5

N2 - We present UV-optical-near-infrared observations and modeling of supernova (SN) 2024ggi, a type II supernova (SN II) located in NGC 3621 at 7.2 Mpc. Early-time (“flash”) spectroscopy of SN 2024ggi within +0.8 days of discovery shows emission lines of H i, He i, C iii, and N iii with a narrow core and broad, symmetric wings (i.e., “IIn-like”) arising from the photoionized, optically thick, unshocked circumstellar material (CSM) that surrounded the progenitor star at shock breakout (SBO). By the next spectral epoch at +1.5 days, SN 2024ggi showed a rise in ionization as emission lines of He ii, C iv, N iv/v, and O v became visible. This phenomenon is temporally consistent with a blueward shift in the UV-optical colors, both likely the result of SBO in an extended, dense CSM. The IIn-like features in SN 2024ggi persist on a timescale of t IIn = 3.8 ± 1.6 days, at which time a reduction in CSM density allows the detection of Doppler-broadened features from the fastest SN material. SN 2024ggi has peak UV-optical absolute magnitudes of M w2 = −18.7 mag and M g = −18.1 mag, respectively, that are consistent with the known population of CSM-interacting SNe II. Comparison of SN 2024ggi with a grid of radiation hydrodynamics and non-local thermodynamic equilibrium radiative-transfer simulations suggests a progenitor mass-loss rate of M ̇ = 10 − 2 M ⊙ yr−1 (v w = 50 km s−1), confined to a distance of r < 5 × 1014 cm. Assuming a wind velocity of v w = 50 km s−1, the progenitor star underwent an enhanced mass-loss episode in the last ∼3 yr before explosion.

AB - We present UV-optical-near-infrared observations and modeling of supernova (SN) 2024ggi, a type II supernova (SN II) located in NGC 3621 at 7.2 Mpc. Early-time (“flash”) spectroscopy of SN 2024ggi within +0.8 days of discovery shows emission lines of H i, He i, C iii, and N iii with a narrow core and broad, symmetric wings (i.e., “IIn-like”) arising from the photoionized, optically thick, unshocked circumstellar material (CSM) that surrounded the progenitor star at shock breakout (SBO). By the next spectral epoch at +1.5 days, SN 2024ggi showed a rise in ionization as emission lines of He ii, C iv, N iv/v, and O v became visible. This phenomenon is temporally consistent with a blueward shift in the UV-optical colors, both likely the result of SBO in an extended, dense CSM. The IIn-like features in SN 2024ggi persist on a timescale of t IIn = 3.8 ± 1.6 days, at which time a reduction in CSM density allows the detection of Doppler-broadened features from the fastest SN material. SN 2024ggi has peak UV-optical absolute magnitudes of M w2 = −18.7 mag and M g = −18.1 mag, respectively, that are consistent with the known population of CSM-interacting SNe II. Comparison of SN 2024ggi with a grid of radiation hydrodynamics and non-local thermodynamic equilibrium radiative-transfer simulations suggests a progenitor mass-loss rate of M ̇ = 10 − 2 M ⊙ yr−1 (v w = 50 km s−1), confined to a distance of r < 5 × 1014 cm. Assuming a wind velocity of v w = 50 km s−1, the progenitor star underwent an enhanced mass-loss episode in the last ∼3 yr before explosion.

U2 - 10.3847/1538-4357/ad5c64

DO - 10.3847/1538-4357/ad5c64

M3 - Journal article

AN - SCOPUS:85203287247

VL - 972

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2

M1 - 177

ER -