Making sky maps from Planck data

Creators: Ashdown, M. A. J.; Baccigalupi, C.; Balbi, A.; Bartlett, J. G.; Borrill, J.; Cantalupo, C.; De Gasperis, G.; Górski, K. M.; Hivon, E.; Keihanen, E.; Kurki-Suonio, H.; Lawrence, C. R.; Natoli, P.; Poutanen, T.; Prunet, S.; Reinecke, M.; Stompor, R.; Wandelt, B.; Planck CTP Working Group

Abstract

Aims. We compare the performance of multiple codes written by different groups for making polarized maps from Planck-sized, all-sky cosmic microwave background (CMB) data. Three of the codes are based on a destriping algorithm; the other three are implementations of an optimal maximum-likelihood algorithm. Methods. Time-ordered data (TOD) were simulated using the Planck Level-S simulation pipeline. Several cases of temperature-only data were run to test that the codes could handle large datasets, and to explore effects such as the precision of the pointing data. Based on these preliminary results, TOD were generated for a set of four 217 GHz detectors (the minimum number required to produce I, Q, and U maps) under two different scanning strategies, with and without noise. Results. Following correction of various problems revealed by the early simulation, all codes were able to handle the large data volume that Planck will produce. Differences in maps produced are small but noticeable; differences in computing resources are large.

Additional Information

© ESO 2007 Received 14 June 2006 / Accepted 9 February 2007 Acknowledgements. The authors would like to thank the University of Helsinki for its hospitality in June 2004 when the CTP Working Group met to undertake this work. MAJA is a member of the Cambridge Planck Analysis Centre, supported by PPARC grant PPA/G/R/1997/00837. Part of this work was supported by NASA. CB was partly supported by the NASA LTSA Grant NNG04CG90G. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC03- 76SF00098. We acknowledge the use of version 0.1 of the Planck reference sky model, prepared by the members of Planck Working Group 2 and available at http://www.planck.fr/heading79.html/. EK and TP were supported by the Academy of Finland grants no. 75065, 205800, 213984, and 214598. TP wishes to thank the Väisälä Foundation for financial support. Some of the results in this paper have been derived using the HEALPix (Górski et al. 2005) package.

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