An extremely metal-poor star complex in the reionization era:Approaching Population III stars with JWST

• DOI: 10.48550/arxiv.2305.14413
• Publication Date: 2023-10-01
• Authors: E. Vanzella; F. Loiacono; P. Bergamini; U. Meštrić; M. Castellano; P. Rosati; M. Meneghetti; C. Grillo; F. Calura; M. Mignoli; M. Bradač; A. Adamo; G. Rihtaršič; M. Dickinson; M. Gronke; A. Zanella; F. Annibali; C. Willott; M. Messa; E. Sani; A. Acebron; A. Bolamperti; A. Comastri; R. Gilli; K. I. Caputi; M. Ricotti; C. Gruppioni; S. Ravindranath; A. Mercurio; V. Strait; N. Martis; R. Pascale; G. B. Caminha; M. Annunziatella; M. Nonino
• Keywords: Galaxies: star formation; Gravitational lensing: strong; Galaxies: high-redshift; Galaxies: star formation; Gravitational lensing: strong; Stars: Population III;; gravitational lensing; Galaxies: high-redshift; FOS: Physical sciences; Astrophysics - Astrophysics of Galaxies; star formation; stars: Population III; galaxies: high-redshift; galaxies: star formation; gravitational lensing: strong; Stars: Population III; 13. Climate action; info:eu-repo/classification/udc/524.8; Astrophysics of Galaxies (astro-ph.GA); Galaxies: high-redshift; Galaxies: star formation; Gravitational lensing: strong; Stars: Population III; high-redshift galaxies

We present JWST/Near Infrared Spectrograph (NIRSpec) integral field spectroscopy (IFS) of a lensed Population III candidate stellar complex (dubbed Lensed And Pristine 1, LAP1), with a lensing-corrected stellar mass of ≲104 M⊙ and an absolute luminosity of MUV > −11.2 (mUV > 35.6), confirmed at redshift 6.639 ± 0.004. The system is strongly amplified (μ ≳ 100) by straddling a critical line of the Hubble Frontier Field galaxy cluster MACS J0416. Although the stellar continuum is currently not detected in the Hubble and JWST/Near Infrared Camera (NIRCam) and Near Infrared Imager and Slitless Spectrograph (NIRISS) imaging, arclet-like shapes of Lyman and Balmer lines, Lyα, Hγ, Hβ and Hα are detected with NIRSpec IFS with signal-to-noise ratios (S/N) of approximately 5 − 13 and large equivalent widths (> 300 − 2000 Å), along with a remarkably weak [O III]λλ4959, 5007 at S/N ≃ 4. LAP1 shows a large ionizing photon production efficiency, log(ξion[erg Hz−1]) > 26. From the metallicity indexes R23 = ([O III] + [O II])/Hβ ≲ 0.74 and R3 = ([O III]/Hβ) = 0.55 ± 0.14, we derive an oxygen abundance of 12 + log(O/H)≲6.3. Intriguingly, the Hα emission is also measured in mirrored subcomponents where no [O III] is detected, providing even more stringent upper limits on the metallicity if in situ star formation is ongoing in this region (12 + log(O/H) < 6). The formal stellar mass limit of the subcomponents would correspond to ∼103 M⊙ or MUV fainter than −10. Alternatively, this metal-free, pure line-emitting region could be the first case of a fluorescing H I gas region induced by transverse escaping ionizing radiation from a nearby star complex. The presence of large equivalent-width hydrogen lines and the deficiency of metal lines in such a small region make LAP1 the most metal-poor star-forming region currently known in the reionization era and a promising site that may host isolated, pristine stars.