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Exploring Changes in Quasar Spectral Energy Distributions across C IV Parameter Space

  • Authors: Angelica B. Rivera, Gordon T. Richards, Sarah C. Gallagher, Trevor V. McCaffrey, Amy L. Rankine, Paul C. Hewett, Ohad Shemmer

Angelica B. Rivera et al 2022 The Astrophysical Journal 931 .

  • Provider: AAS Journals

Caption: Figure 10.

The C IV ∥ distance, log(C IV EQW), and C IV blueshift vs. log(He II EQW) for our sample colored by the C IV ⊥ distance shown in the left, middle, and right panels, respectively. The error bar for the C IV blueshift is the same as that from Figure 2; the error bars for the log(C IV EQW) and log(He II EQW) were carried out in a similar fashion, except in log space. The errors in C IV ∥ distance trace those of the underlying parameters, where the errors will be largest at the extreme where it is more difficult to accurately measure the component with small values. The Pearson r (assuming a linear correlation) values for each relationship are displayed in each panel. The break in the log(He II EQW)−log(C IV EQW) relationship shown in Figure C1 of Timlin et al. (2021b) is shown to be present at different C IV EQWs for different C IV ⊥ distances. Note that the linear trend with log(He II EQW) with the smallest scatter is that with the C IV ∥ distance. The linear best fit to the distribution is shown as the black solid line, with 3σ contours shown in light purple.

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