DOI: 10.7910/dvn/djaaig
title: Dust Spectral Energy Distribution Data from Zelko & Finkbeiner 2020a and 2020b

description: Data set containing the dust spectral energy distribution data from Zelko & Finkbeiner 2020a[1] and 2020b[2].
&lt;br /&gt;
&lt;br /&gt;
Interstellar dust emission is modeled with Draine-like models with grain-size distributions constrained by optical/UV extinction, far IR emission, and interstellar abundances (Zelko & Finkbeiner 2020a), for a fixed and variable radiation field.
&lt;br /&gt; 
&lt;br /&gt;
The frequency for the interstellar dust emission follows the proposed frequency spectrum of the proposed Primordial Inflation Explorer (PIXIE, Kogut et al. 2016). There are 416 frequency bins, each spaced 14.4GHz apart, spanning a frequency range from 14.4GHz to 5994.1GHz.
&lt;br /&gt; 
&lt;br /&gt;
Nashimoto et al. (2020) discussed the effect of interstellar dust absorption of the cosmic microwave background. The data presented here has two dataset, one which includes the effect of the absorption of the CMB (marked as "shadow"), and one which does not (marked as "no_shadow").
&lt;br /&gt; 
&lt;br /&gt;
We consider the case of a fixed interstellar radiation field, with datasets marked "fixed_chi", as well as the case of variable radiation field with the coefficient χISRF taking values between 0.5 and 2. The latter datasets are labeled with "variable_chi". 
&lt;br /&gt; 
&lt;br /&gt;
For the case where ISRF varies, χISRF takes the 10 values: [0.5, 0.58326452, 0.680395, 0.79370053, 0.92587471, 1.08005974, 1.25992105, 1.46973449, 1.71448797, 2.].
&lt;br /&gt; 
&lt;br /&gt;
The dust emission collections are also separated based on their Rv' (defined in Schlafly et al. 2016, together with its corresponding x parameter) since the size distributions of the dust grains that give rise to the SEDs were constrained to have reddening laws corresponding to 15 different Rv' (see Zelko & Finkbeiner 2020a).
&lt;br /&gt; 
&lt;br /&gt;
The 15 values of Rv' are: [2.936, 2.988, 3.04, 3.092, 3.144, 3.196, 3.248, 3.3, 3.352, 3.404, 3.456, 3.508, 3.56, 3.612, 3.664].
&lt;br /&gt; 
&lt;br /&gt;
The corresponding 15 values of the x parameter: [-0.04, -0.03428571, -0.02857143, -0.02285714, -0.01714286, -0.01142857, -0.00571429, 0., 0.00571429, 0.01142857, 0.01714286, 0.02285714, 0.02857143, 0.03428571, 0.04].
&lt;br /&gt; 
&lt;br /&gt;
For each χISRF and Rv' case, 300 sample end of chains positions were stored from the MCMC processes run.
&lt;br /&gt; 
&lt;br /&gt;
The values for the frequencies, Rv', x are stored as attributes of the master dataset.
&lt;br /&gt; 
&lt;br /&gt;
Thus, the dimmensions of the dataset are:
&lt;br /&gt;
- for the no-shadow, fixed_chi case: (Rv, samples, frequency), corresponding to (15, 300, 416)
&lt;br /&gt;
- for the no-shadow, variable_chi case: (χISRF, Rv, samples, frequency), corresponding to (10, 15, 300, 416)
&lt;br /&gt;
- for the shadow, fixed_chi case: (Rv, samples, frequency), corresponding to (15, 300, 416)
&lt;br /&gt;
- for the shadow, variable_chi case: (χISRF, Rv, samples, frequency), corresponding to (10, 15, 300, 416)
&lt;br /&gt;
&lt;br /&gt;
For more details about the creation process of the data set, see &lt;a href="https://arxiv.org/abs/2009.11869 "&gt; Zelko & Finkbeiner 2020a&lt;/a&gt;, and &lt;a href="https://arxiv.org/abs/2010.06589"&gt; Zelko & Finkbeiner 2020b&lt;/a&gt;.
description: Python, null