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The "cosmic Seagull": A Highly Magnified Disk-like Galaxy at z ≃ 2.8 behind the Bullet Cluster

Research output: Contribution to journalArticle

  • V. Motta
  • E. Ibar
  • T. Verdugo
  • J. Molina
  • T. M. Hughes
  • M. Birkinshaw
  • O. López-Cruz
  • J. H. Black
  • D. Gunawan
  • C. Horellou
  • J. Magana
Original languageEnglish
Article numberL16
Number of pages5
JournalAstrophysical Journal Letters
Volume863
Issue number2
Early online date13 Aug 2018
DOIs
DateAccepted/In press - 28 Jul 2018
DateE-pub ahead of print - 13 Aug 2018
DatePublished (current) - 20 Aug 2018

Abstract

We present Atacama Large Millimeter/submillimeter Array measurements of the "Cosmic Seagull," a strongly magnified galaxy at z = 2.7779 behind the Bullet Cluster. We report CO(3-2) and continuum 344 μm (rest-frame) data at one of the highest differential magnifications ever recorded at submillimeter wavelengths (μ up to ∼50), facilitating a characterization of the kinematics of a rotational curve in great detail (at ∼620 pc resolution in the source plane). We find no evidence for a decreasing rotation curve, from which we derive a dynamical mass of (6.3 ± 0.7) × 1010 M o within r = 2.6 ± 0.1 kpc. The discovery of a third, unpredicted, image provides key information for a future improvement of the lensing modeling of the Bullet Cluster and allows a measure of the stellar mass, , unaffected by strong differential magnification. The baryonic mass is expected to be dominated by the molecular gas content (f gas ≤ 80 ± 20%) based on an mass estimated from the difference between dynamical and stellar masses. The star formation rate (SFR) is estimated via the spectral energy distribution (SFR = 190 ± 10 M o yr-1), implying a molecular gas depletion time of 0.25 ± 0.08 Gyr.

    Research areas

  • galaxies: clusters: individual (1ES0657-558), galaxies: evolution, galaxies: ISM, gravitational lensing: strong, submillimeter: galaxies

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    Rights statement: This is the final published version of the article (version of record). It first appeared online via IOP at http://iopscience.iop.org/article/10.3847/2041-8213/aad6de#artAbst. Please refer to any applicable terms of use of the publisher.

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