Modeling optical systematics for the Taurus CMB experiment
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2024
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| author | Adler, Alexandre E. Austermann, Jason E. Benton, Steven J. Duff, Shannon M. Filippini, Jeffrey P. Fraisse, Aurelien A. Gascard, Thomas Gibbs, Sho M. Gourapura, Suren Hubmayr, Johannes Gudmundsson, Jon E. Jones, William C. May, Jared L. Nagy, Johanna M. Okun, Kate Padilla, Ivan Rooney, Christopher Tartakovsky, Simon Vissers, Michael R. |
| author_facet | Adler, Alexandre E. Austermann, Jason E. Benton, Steven J. Duff, Shannon M. Filippini, Jeffrey P. Fraisse, Aurelien A. Gascard, Thomas Gibbs, Sho M. Gourapura, Suren Hubmayr, Johannes Gudmundsson, Jon E. Jones, William C. May, Jared L. Nagy, Johanna M. Okun, Kate Padilla, Ivan Rooney, Christopher Tartakovsky, Simon Vissers, Michael R. |
| contents | We simulate a variety of optical systematics for Taurus, a balloon-borne cosmic microwave background (CMB) polarisation experiment, to assess their impact on large-scale E-mode polarisation measurements and constraints of the optical depth to reionisation τ. We model a one-month flight of Taurus from Wanaka, New Zealand aboard a super-pressure balloon (SPB). We simulate night-time scans of both the CMB and dust foregrounds in the 150GHz band, one of Taurus's four observing bands. We consider a variety of possible systematics that may affect Taurus's observations, including non-gaussian beams, pointing reconstruction error, and half-wave plate (HWP) non-idealities. For each of these, we evaluate the residual power in the difference between maps simulated with and without the systematic, and compare this to the expected signal level corresponding to Taurus's science goals. Our results indicate that most of the HWP-related systematics can be mitigated to be smaller than sample variance by calibrating with Planck's TT spectrum and using an achromatic HWP model, with a preference for five layers of sapphire to ensure good systematic control. However, additional beam characterization will be required to mitigate far-sidelobe pickup from dust on larger scales. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2406_11992 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Modeling optical systematics for the Taurus CMB experiment Adler, Alexandre E. Austermann, Jason E. Benton, Steven J. Duff, Shannon M. Filippini, Jeffrey P. Fraisse, Aurelien A. Gascard, Thomas Gibbs, Sho M. Gourapura, Suren Hubmayr, Johannes Gudmundsson, Jon E. Jones, William C. May, Jared L. Nagy, Johanna M. Okun, Kate Padilla, Ivan Rooney, Christopher Tartakovsky, Simon Vissers, Michael R. Cosmology and Nongalactic Astrophysics Instrumentation and Methods for Astrophysics We simulate a variety of optical systematics for Taurus, a balloon-borne cosmic microwave background (CMB) polarisation experiment, to assess their impact on large-scale E-mode polarisation measurements and constraints of the optical depth to reionisation τ. We model a one-month flight of Taurus from Wanaka, New Zealand aboard a super-pressure balloon (SPB). We simulate night-time scans of both the CMB and dust foregrounds in the 150GHz band, one of Taurus's four observing bands. We consider a variety of possible systematics that may affect Taurus's observations, including non-gaussian beams, pointing reconstruction error, and half-wave plate (HWP) non-idealities. For each of these, we evaluate the residual power in the difference between maps simulated with and without the systematic, and compare this to the expected signal level corresponding to Taurus's science goals. Our results indicate that most of the HWP-related systematics can be mitigated to be smaller than sample variance by calibrating with Planck's TT spectrum and using an achromatic HWP model, with a preference for five layers of sapphire to ensure good systematic control. However, additional beam characterization will be required to mitigate far-sidelobe pickup from dust on larger scales. |
| title | Modeling optical systematics for the Taurus CMB experiment |
| topic | Cosmology and Nongalactic Astrophysics Instrumentation and Methods for Astrophysics |
| url | https://arxiv.org/abs/2406.11992 |