JWST spectroscopic confirmation of the Cosmic Gems arc at <i>z</i> = 9.625

We present JWST/NIRSpec integral field spectroscopy of the Cosmic Gems arc, strongly magnified by the galaxy cluster SPT-CL J0615−5746. Six-hour integration using NIRSpec prism spectroscopy (resolution R ≃ 30 − 300), covering the spectral range 0.8 − 5.3 μm, reveals a pronounced Ly α -continuum break at λ ≃ 1.3 μm, as well as weak optical H β and [O III ] λ 4959 emission lines at z = 9.625 ± 0.002, located in the reddest part of the spectrum ( λ > 5.1 μm). No additional ultraviolet or optical emission lines are reliably detected. A weak Balmer break is measured alongside a very blue ultraviolet slope ( β ≤ −2.5, F λ ∼ λ β ). Spectral fitting with Bagpipes suggests that the Cosmic Gems galaxy is in a post-starburst phase, making it the highest-redshift system currently observed in a mini-quenched state. Spatially resolved spectroscopy at tens of parsecs shows relatively uniform features across subcomponents of the arc. These findings align well with the physical properties previously derived from JWST/NIRCam photometry of the stellar clusters, now corroborated by spectroscopic evidence. In particular, five observed star clusters exhibit ages of 7 − 30 Myr. An updated lens model constrains the intrinsic sizes and masses of these clusters, confirming they are extremely compact and denser than typical star clusters in local star-forming galaxies (Σ M ★ = 10 5 − 10 6 M ⊙ ). Additionally, four compact stellar systems consistent with star clusters (≲10 pc) are identified along the extended tail of the arc. A sub-parsec line-emitting H II 1.2ex region straddling the critical line, lacking a NIRCam counterpart, is also serendipitously detected. The Cosmic Gems arc thus offers a rare opportunity to investigate, at parsec scales, the aftermath of a star formation burst in the early Universe.