Search

Image Details

View Article Bookmark & Share

Choose export citation format:

Export Citation
Large resolution
Hi-Resolution Export to PDF

Nāpōwawā‘enakaulua: A Close Quasar Pair at Cosmic Dawn in the Aether Survey

  • Authors: Silvia Onorato, Emanuele Paolo Farina, Roberto Decarli, Klaudia Protušová, Elia Pizzati, Debora Pelliccia, Devin S. Chu, Larry Lindsey Kimura, Leinani Lozi, Emily Peavy, Fabrizio Arrigoni–Battaia, Eduardo Bañados, Aaron J. Barth, Silvia Belladitta, Manuela Bischetti, Sarah E. I. Bosman, Hyunseop Choi, Tiago Costa, Anna-Christina Eilers, Xiaohui Fan, Simona Gallerani, Thomas R. Geballe, Anniek J. Gloudemans, Eunchong Kim, Brian C. Lemaux, Weizhe Liu, 伟哲 刘, Yoshiki Matsuoka, Chiara Mazzucchelli, Atsuko Nitta, Jan-Torge Schindler, Andrew W. Stephens, Hyewon Suh, Fabian Walter, Feige Wang, Jinyi Yang

Silvia Onorato et al 2026 The Astrophysical Journal Letters 1011 .

  • Provider: AAS Journals

Caption: Figure 3.

Comparison of the Hβ, [O III], and Hα emission line profiles of Nāpōwawā‘enakaulua, after subtracting the best-fit continuum (power law + Fe II template) from both the data and the model, with the shaded regions showing the 1σ uncertainty. (a) Hβ profile, obtained by additionally subtracting all [O III] (and He I, for “A”) model components. (b) [O III]λλ4959, 5007 Å doublet, obtained by additionally subtracting all Hβ model components. (c) Hα + [N II] blend. In each panel, data and best-fit model of “B” are rescaled by a multiplicative factor (quoted in the legend), so that the peak of its best-fit model matches the peak of “A” within the line of interest, allowing a direct comparison of the line profiles, despite “B” being much fainter than “A”. Vertical dotted lines mark the rest-frame wavelengths of the relevant transitions.

Other Images in This Article
Image in this article
Image in this article
Image in this article
Copyright and Terms & Conditions

Additional terms of reuse