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Copious Amounts of Dust and Gas in a z = 7.5 Quasar Host Galaxy

  • Authors: Bram P. Venemans, Fabian Walter, Roberto Decarli, Eduardo Bañados, Chris Carilli, Jan Martin Winters, Karl Schuster, Elisabete da Cunha, Xiaohui Fan, Emanuele Paolo Farina, Chiara Mazzucchelli, Hans-Walter Rix, and Axel Weiss

2017 The Astrophysical Journal Letters 851 L8.

  • Provider: AAS Journals

Caption: Figure 3.

Far-infrared and radio spectral energy distribution of J1342+0928. The data points from left to right represent the NOEMA 1, 2, and 3 mm observations, the tentative VLA 41.0 GHz detection, and the FIRST upper limit. Overplotted are three different dust SEDs scaled to the 1 mm detection and two power laws describing radio synchrotron radiation. The dust model with canonical values (Td = 47 K and ﹩\beta =1.6﹩) agrees well with the upper limits on the continuum emission at 2 and 3 mm, but predicts a much lower continuum flux density at 41.0 GHz. A shallower β (﹩\beta =1.0﹩) or a lower dust temperature (Td = 24 K, slightly above the CMB temperature at z = 7.54), illustrated by the dashed and dotted lines, also predicts a 41.0 GHz flux density below that of the tentative VLA source. The upper limit in FIRST does not provide strong constraints on the slope of the radio emission.

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