SN 2024ggi in NGC 3621: Rising Ionization in a Nearby, CSM-Interacting Type II Supernova
arxiv(2024)
摘要
We present UV/optical/NIR 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. 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 shock
breakout 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 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 (nLTE)
radiative-transfer simulations suggests a progenitor mass-loss rate of Ṁ
= 10^-2M_⊙ yr^-1 (v_w = 50 km/s), confined to a distance of r
< 5× 10^14 cm. Assuming a wind velocity of v_w = 50 km/s, the
progenitor star underwent an enhanced mass-loss episode in the last 3 years
before explosion.
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