The Planck thermal dust model (Planck Collaboration et. al. 2014) at resolution 5' was used to find the zero level adjustments for the four Herschel intensity maps for each field. A table of these adjustments is available in PDF format for preview and download, and in CSV format for download.
The SED fit using χ2 minimization requires accurate uncertainties for weighting. We investigated and quantified multiple sources of uncertainty in the observed intensity maps. The uncertainties assessed fall into four main categories:
Detailed explanations of each of the sources have been presented in Singh & Martin (2022).
There are various ways to convert τ maps to column density. One commonly used method to obtain the column density of H2 requires the dust opacity κ. In various analyses using HOTT maps, the following values have been adopted:
As emphasized in Singh & Martin (2022), the value of κ is quite uncertain, and could vary from region to region and even within an individual field.
During the course of the analysis in Singh & Martin (2022), we have generated HOTT maps for various fields not in the Gould Belt, including low intensity fields at intermediate Galactic latitude (Draco and Spider) and GMCs that are forming massive stars (California and W3). These HOTT maps will be added to this archive. Additionally, we anticipate adding additional fields from HOBYS.
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