The data published below is a sample of the observations delivered by Mauve and was collected during early calibration observations carried out in the commissioning phase. Further details about the data and its scientific interpretation are available in a paper.
We welcome you to download and use the data, provided that you include the following acknowledgement:
“This publication has used Mauve data provided by Blue Skies Space, originally presented in Saba et al. [INSERT NATURE PAPER URL].”
Data Analysis
Mauve’s data can be analysed with a variety of packages; however, Blue Skies Space suggests using Xspec as it is specifically designed to handle very low-resolution data. We have provided a tutorial video and links to help users install and utilise the software.
Why Xspec?
- The resolution of Mauve spectra is comparable to the resolution of spectra obtained with X-ray telescopes, which operate at very low resolution.
- To address the data analysis and to be able to perform science in this regime, the community has been using specialised software.
How does Xspec work?
- Xspec takes in the instrument line function and the telescope effective area.
- It then convolves the chosen stellar model with the detector response and compares the model to the data.
- If necessary, the model parameters can be adjusted by the user until the best fit is reached.
- Users can compute the flux (in physical units) from the best-fit model spectrum, not on the observed data.
Useful Links:
- Download and installation instructions
- Adding your own models to XSPEC
- XSPEC user manual [in PDF]
- XSPEC release notes
- Getting help with XSPEC
- Local models to load into XSPEC, including many from the community
- XSPEC internal functions guide [in PDF]
- XSPEC Facebook group
- External guides, tutorials, and examples from the community
- Historical XSPEC information
- Python version of XSPEC
- Commands quick reference
- Full Commands