What question did this study set out to answer?

This research aims to compare dust-obscured and unobscured star formation in distant galaxies using new observational techniques.

April 8, 2026

A first look at a complete view of spatially resolved star formation at 1 <

Puntos clave

This research aims to compare dust-obscured and unobscured star formation in distant galaxies using new observational techniques.
Utilized JWST NIRCam and NIRISS for slitless spectroscopy of 31 galaxies at redshifts 1 < z < 1.8.
Stacked Paα and Hα emission-line maps along with stellar continuum images.
Measured surface brightness and computed equivalent width profiles across stellar mass bins.
Found evidence for inside-out galaxy growth through both dust-obscured and unobscured star formation.
Identified a weakly positive Paα/Hα gradient in central stellar mass bins and a negative gradient in the highest mass range.
Detected that low-mass galaxies also exhibit negative gradients, indicating variations in star formation rates across different masses.

Resumen

The previously inaccessible star formation tracer Paschen-Alpha (Paα) can now be spatially resolved by JWST NIRCam slitless spectroscopy in distant galaxies up to cosmic noon. In the first study of its kind, we combine JWST NGDEEP NIRISS and FRESCO NIRCam slitless spectroscopy to provide the first direct comparison of spatially resolved dust-obscured (traced by Paα) versus unobscured (traced by Hα) star formation across the main sequence. We stacked Paα and Hα emission-line maps, along with stellar continuum images at both wavelengths of 31 galaxies at 1 < z < 1.8 in three bins of stellar mass spanning 7.7 ≤ log(M*/M⊙) < 11. Surface brightness profiles were measured and equivalent width (EW) profiles computed. Increasing Paα and Hα EW profiles with galactocentric radius across all stellar masses probed provides direct evidence for the inside-out growth of galaxies both via dust-obscured and unobscured star formation for the first time. For galaxies predominantly on the main sequence (log(M*/M⊙)≥8.8), a weakly positive (0.1 ± 0.1) Paα/Hα line profile gradient as a function of radius is found at 8.8 ≤ log(M*/M⊙) < 9.9, with a negative (−0.4 ± 0.1) Paα/Hα line profile gradient as a function of radius found at the highest stellar masses of 9.9 ≤ log(M*/M⊙) < 11.0. Low-mass galaxies (7.7 ≤ log(M*/M⊙) < 8.8) with predominantly high specific star formation rates relative to the main sequence are also found to have a negative (−0.5 ± 0.1) Paα/Hα line profile gradient as a function of radius. Our results demonstrate that while inside-out growth via star formation is ubiquitous across the main sequence just after cosmic noon, centrally concentrated dust attenuation is not. Along with other recent work in the literature, our findings now motivate future studies of resolved SFR and dust attenuation profiles in large samples of individual cosmic noon galaxies across the main sequence, aimed at understanding the intrinsic scatter in spatially resolved star formation.

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