New JWST redshifts for the host galaxies of CDF-S XT1 and XT2: Understanding their nature

¹ Department of Astrophysics/IMAPP, Radboud University, PO Box 9010 6500 GL Nijmegen, The Netherlands
² Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Casilla 306, Santiago 22, Chile
³ Millennium Institute of Astrophysics (MAS), Nuncio Monseñor Sótero Sanz 100, Providencia, Santiago, Chile
⁴ Instituto de Alta Investigación, Universidad de Tarapacá, Casilla 7D, Arica, Chile
⁵ Department of Astronomy & Astrophysics, 525 Davey Laboratory, The Pennsylvania State University, University Park, PA 16802, USA
⁶ Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA 16802, USA
⁷ Department of Physics, 104 Davey Laboratory, The Pennsylvania State University, University Park, PA 16802, USA
⁸ Indian Institute of Astrophysics, Koramangala, Bengaluru, 560034 Karnataka, India
⁹ CAS Key Laboratory for Research in Galaxies and Cosmology, Department of Astronomy, University of Science and Technology of China, Hefei 230026, China
¹⁰ School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
¹¹ Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, PR China

^⋆ Corresponding author; j.quirolavasquez@astro.ru.nl

Received: 7 August 2024
Accepted: 31 January 2025

Abstract

Aims. CDF-S XT1 and XT2 are considered two “canonical” extragalactic fast X-ray transients (FXTs). In this work, we report new constraints on both FXTs, based on recent JWST NIRCam and MIRI photometry, as well as NIRspec spectroscopy for CDF-S XT2 that allow us to improve our understanding of their distances, energetics, and host galaxy properties compared to the pre-JWST era.

Methods. We use the available HST and JWST archival data to determine the host properties and constrain the energetics of each FXT based on spectral energy distribution (SED) photometric fitting.

Results. The host of CDF-S XT1 is now constrained to lie at z_phot = 2.76^+2.21_-0.13, implying a host absolute magnitude M_R = −19.14 mag, stellar mass M_* ≈ 2.8 × 10⁸ M_⊙, and star formation rate SFR ≈ 0.62 M_⊙ yr⁻¹. These properties lie at the upper end of previous estimates, leaving CDF-S XT1 with a peak X-ray luminosity of L_X, peak ≈ 2.8 × 10⁴⁷ erg s⁻¹. We argue that the best progenitor scenario for XT1 is a low-luminosity gamma-ray burst (GRB), although we do not fully rule out a proto-magnetar association or a jetted tidal disruption event involving a white dwarf and an intermediate-massive black hole. In the case of CDF-S XT2, JWST imaging reveals a new highly obscured component of the host galaxy, previously missed in HST images, while NIRspec spectroscopy securely places the host at z_spec = 3.4598 ± 0.0022. The new redshift implies a host with M_R = −21.76 mag, M_* ≈ 5.5 × 10¹⁰ M_⊙, SFR ≈ 160 M_⊙ yr⁻¹, and FXT L_X, peak ≈ 1.4 × 10⁴⁷ erg s⁻¹. The revised energetics, similarity to X-ray flash event light curves, small host offset, and high host SFR favor a low-luminosity collapsar progenitor for CDF-S XT2. Although a magnetar model is not ruled out, it appears improbable.

Conclusions. While these HST and JWST observations shed light on the host galaxies of XT1 and XT2, and by extension, on the nature of FXTs, a unique explanation for both sources remains elusive. Rapid discovery, for instance, with the Einstein Probe satellite, and contemporaneous multiwavelength detections of FXTs remain essential for clarifying the nature of FXTs.