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    <lastmod>2022-12-21</lastmod>
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      <image:title>Research - Make it stand out</image:title>
      <image:caption>HEAD Meeting Poster, March 2022</image:caption>
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      <image:caption>The image to the left is a typical XLF (from Ueda et. al. 2014) and the image to the right is a typical X-ray AGN spectra, and multiplying the number density with intensity of spectra at observed frame energy E, and integrating over all redshift, luminosities and obscuration levels produces the cosmic X-ray background.</image:caption>
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      <image:caption>Allowed regions of the spectral parameter space, for unconstrained XLF. Contours for 1σ, 2σ and 3σ are shown in yellow, green, and blue, respectively. The black triangular data points indicate results of the Bayesian analysis using the XLF from Paper I. To create this figure, the same spectral set was assumed for all absorption bins. The values of σE and σR were kept constant at 36 keV and 0.14, respectively. The entire probability space can be explored quantitatively using the interactive tool described in Section 4.2, which allows users to specify a different spectral set for each absorption bin and explore other values of σE and σR as well as the variables shown in this plot.</image:caption>
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      <image:caption>Figure 3. From left to right: field of Stripe 82X XMM-Newton source ID 2794 (solid black circle with radius 7'') at the optical SDSS r band, near-infrared IRAC Ch1 (3.6 μm), and AllWISE W1 (3.4 μm). The positional errors for SDSS, VHS, and IRAC are only a few milliarcseconds; for clarity, we use bigger circles to indicate the location of the source in each band: a dashed green circle with radius 1'' around the SDSS r band, a solid yellow circle with radius 12 for the VHS K band, and a solid red circle with radius 1'' for the IRAC CH1 source positions. In this example, the most likely optical counterpart from the MLE analysis (left) is the bright source at the top (solid green circle), but the infrared images suggest a more reliable counterpart below and to the left. The dashed green circles indicate other nearby optical sources that have a lower reliability match. We identify the source circled in yellow as the correct counterpart, which is the most likely counterpart according to VHS and IRAC but more accurately pinpointed by VHS.</image:caption>
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      <image:title>Research</image:title>
      <image:caption>Figure 6. Flow chart showing how we assign counterpart(s) to each X-ray source and how the QF is defined (see Section 2.5). QF values 1, 1.5, and 2 are secure; 3 and 4 are problematic; and −1 refers to the discarded, second-best candidate.</image:caption>
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      <image:caption>Figure 11. Spectroscopic vs. photometric redshift for point-like (left) and extended (right) sources in the uniform XMM-Newton fields. The results in the other fields are very similar, as can be seen in Table 7. Black crosses indicate cases where the primary redshift is incorrect and the secondary redshift is correct (i.e., it lies within the dashed black lines). The quantity "zphotN/A" reports the percentage of sources for which we are unable to calculate photometric redshifts altogether due to data in very few bands or not having an appropriate SED template in our template library.</image:caption>
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    <lastmod>2021-10-24</lastmod>
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      <image:caption>Whatever it is, the way you tell your story online can make all the difference.</image:caption>
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