The Astrophysical Journal Letters (Jan 2024)

Ionized Gas Kinematics with FRESCO: An Extended, Massive, Rapidly Rotating Galaxy at z = 5.4

  • Erica Nelson,
  • Gabriel Brammer,
  • Clara Giménez-Arteaga,
  • Pascal A. Oesch,
  • Rohan P. Naidu,
  • Hannah Übler,
  • Jasleen Matharu,
  • Alice E. Shapley,
  • Katherine E. Whitaker,
  • Emily Wisnioski,
  • Natascha M. Förster Schreiber,
  • Renske Smit,
  • Pieter van Dokkum,
  • John Chisholm,
  • Ryan Endsley,
  • Abigail I. Hartley,
  • Justus Gibson,
  • Emma Giovinazzo,
  • Garth Illingworth,
  • Ivo Labbe,
  • Michael V. Maseda,
  • Jorryt Matthee,
  • Alba Covelo Paz,
  • Sedona H. Price,
  • Naveen A. Reddy,
  • Irene Shivaei,
  • Andrea Weibel,
  • Stijn Wuyts,
  • Mengyuan Xiao,
  • Stacey Alberts,
  • William M. Baker,
  • Andrew J. Bunker,
  • Alex J. Cameron,
  • Stephane Charlot,
  • Daniel J. Eisenstein,
  • Anna de Graaff,
  • Zhiyuan Ji,
  • Benjamin D. Johnson,
  • Gareth C. Jones,
  • Roberto Maiolino,
  • Brant Robertson,
  • Lester Sandles,
  • Katherine A. Suess,
  • Sandro Tacchella,
  • Christina C. Williams,
  • Joris Witstok

DOI
https://doi.org/10.3847/2041-8213/ad7b17
Journal volume & issue
Vol. 976, no. 2
p. L27

Abstract

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With the remarkable sensitivity and resolution of JWST in the infrared, measuring rest-optical kinematics of galaxies at z > 5 has become possible for the first time. This study pilots a new method for measuring galaxy dynamics for highly multiplexed, unbiased samples by combining FRESCO NIRCam grism spectroscopy and JADES medium-band imaging. Here we present one of the first JWST kinematic measurements for a galaxy at z > 5. We find a significant velocity gradient, which, if interpreted as rotation, yields V _rot = 305 ± 70 km s ^−1 , and we hence refer to this galaxy as Twister-z5. With a rest-frame optical effective radius of r _e = 2.25 kpc, the high rotation velocity in this galaxy is not due to a compact size, as may be expected in the early Universe, but rather to a high total mass, $\mathrm{log}({M}_{\mathrm{dyn}}/{M}_{\odot })=11.2\pm 0.2$ . This is a factor of roughly 10× higher than the stellar mass within r _e . We also observe that the radial H α equivalent width profile and the specific star formation rate map from resolved stellar population modeling are centrally depressed by a factor of ∼1.5 from the center to r _e . Combined with the morphology of the line-emitting gas in comparison to the continuum, this centrally suppressed star formation is consistent with a star-forming disk surrounding a bulge growing inside out. While large, rapidly rotating disks are common to z ∼ 2, the existence of one after only 1 Gyr of cosmic time, shown for the first time in ionized gas, adds to the growing evidence that some galaxies matured earlier than expected in the history of the Universe.

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