BEYONDPLANCK: III. Commander3
We describe the computational infrastructure for end-to-end Bayesian cosmic microwave background (CMB) analysis implemented by the BeyondPlanck Collaboration. The code is called Commander3 . It provides a statistically consistent framework for global analysis of CMB and microwave observations and ma...
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| Veröffentlicht in: | Astronomy and astrophysics (Berlin) 2023-06, Vol.675, p.A3 |
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| creator | Galloway, M. Andersen, K. J. Aurlien, R. Banerji, R. Bersanelli, M. Bertocco, S. Brilenkov, M. Carbone, M. Colombo, L. P. L. Eriksen, H. K. Eskilt, J. R. Foss, M. K. Franceschet, C. Fuskeland, U. Galeotta, S. Gerakakis, S. Gjerløw, E. Hensley, B. Herman, D. Iacobellis, M. Ieronymaki, M. Ihle, H. T. Jewell, J. B. Karakci, A. Keihänen, E. Keskitalo, R. Maggio, G. Maino, D. Maris, M. Mennella, A. Paradiso, S. Partridge, B. Reinecke, M. San, M. Suur-Uski, A.-S. Svalheim, T. L. Tavagnacco, D. Thommesen, H. Watts, D. J. Wehus, I. K. Zacchei, A. |
| description | We describe the computational infrastructure for end-to-end Bayesian cosmic microwave background (CMB) analysis implemented by the BeyondPlanck Collaboration. The code is called
Commander3
. It provides a statistically consistent framework for global analysis of CMB and microwave observations and may be useful for a wide range of legacy, current, and future experiments. The paper has three main goals. Firstly, we provide a high-level overview of the existing code base, aiming to guide readers who wish to extend and adapt the code according to their own needs or re-implement it from scratch in a different programming language. Secondly, we discuss some critical computational challenges that arise within any global CMB analysis framework, for instance in-memory compression of time-ordered data, fast Fourier transform optimization, and parallelization and load-balancing. Thirdly, we quantify the CPU and RAM requirements for the current B
EYOND
P
LANCK
analysis, finding that a total of 1.5 TB of RAM is required for efficient analysis and that the total cost of a full Gibbs sample for LFI is 170 CPU-hrs, including both low-level processing and high-level component separation, which is well within the capabilities of current low-cost computing facilities. The existing code base is made publicly available under a GNU General Public Library (GPL) license. |
| doi_str_mv | 10.1051/0004-6361/202243137 |
| format | Article |
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Commander3
. It provides a statistically consistent framework for global analysis of CMB and microwave observations and may be useful for a wide range of legacy, current, and future experiments. The paper has three main goals. Firstly, we provide a high-level overview of the existing code base, aiming to guide readers who wish to extend and adapt the code according to their own needs or re-implement it from scratch in a different programming language. Secondly, we discuss some critical computational challenges that arise within any global CMB analysis framework, for instance in-memory compression of time-ordered data, fast Fourier transform optimization, and parallelization and load-balancing. Thirdly, we quantify the CPU and RAM requirements for the current B
EYOND
P
LANCK
analysis, finding that a total of 1.5 TB of RAM is required for efficient analysis and that the total cost of a full Gibbs sample for LFI is 170 CPU-hrs, including both low-level processing and high-level component separation, which is well within the capabilities of current low-cost computing facilities. The existing code base is made publicly available under a GNU General Public Library (GPL) license.</description><identifier>ISSN: 0004-6361</identifier><identifier>EISSN: 1432-0746</identifier><identifier>DOI: 10.1051/0004-6361/202243137</identifier><language>eng</language><publisher>United States: EDP Sciences</publisher><subject>ASTRONOMY AND ASTROPHYSICS ; cosmic background radiation ; MATHEMATICS AND COMPUTING ; methods: data analysis ; methods: numerical</subject><ispartof>Astronomy and astrophysics (Berlin), 2023-06, Vol.675, p.A3</ispartof><rights>info:eu-repo/semantics/openAccess</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><cites>FETCH-LOGICAL-c181t-e7dd85be77c6f4760b402aeb17a39ee2e5097830a37170c02494c5fbe0117e353</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>230,314,776,780,881,3714,26544,27901,27902</link.rule.ids><backlink>$$Uhttps://www.osti.gov/servlets/purl/2234083$$D View this record in Osti.gov$$Hfree_for_read</backlink></links><search><creatorcontrib>Galloway, M.</creatorcontrib><creatorcontrib>Andersen, K. J.</creatorcontrib><creatorcontrib>Aurlien, R.</creatorcontrib><creatorcontrib>Banerji, R.</creatorcontrib><creatorcontrib>Bersanelli, M.</creatorcontrib><creatorcontrib>Bertocco, S.</creatorcontrib><creatorcontrib>Brilenkov, M.</creatorcontrib><creatorcontrib>Carbone, M.</creatorcontrib><creatorcontrib>Colombo, L. P. L.</creatorcontrib><creatorcontrib>Eriksen, H. K.</creatorcontrib><creatorcontrib>Eskilt, J. R.</creatorcontrib><creatorcontrib>Foss, M. K.</creatorcontrib><creatorcontrib>Franceschet, C.</creatorcontrib><creatorcontrib>Fuskeland, U.</creatorcontrib><creatorcontrib>Galeotta, S.</creatorcontrib><creatorcontrib>Gerakakis, S.</creatorcontrib><creatorcontrib>Gjerløw, E.</creatorcontrib><creatorcontrib>Hensley, B.</creatorcontrib><creatorcontrib>Herman, D.</creatorcontrib><creatorcontrib>Iacobellis, M.</creatorcontrib><creatorcontrib>Ieronymaki, M.</creatorcontrib><creatorcontrib>Ihle, H. T.</creatorcontrib><creatorcontrib>Jewell, J. B.</creatorcontrib><creatorcontrib>Karakci, A.</creatorcontrib><creatorcontrib>Keihänen, E.</creatorcontrib><creatorcontrib>Keskitalo, R.</creatorcontrib><creatorcontrib>Maggio, G.</creatorcontrib><creatorcontrib>Maino, D.</creatorcontrib><creatorcontrib>Maris, M.</creatorcontrib><creatorcontrib>Mennella, A.</creatorcontrib><creatorcontrib>Paradiso, S.</creatorcontrib><creatorcontrib>Partridge, B.</creatorcontrib><creatorcontrib>Reinecke, M.</creatorcontrib><creatorcontrib>San, M.</creatorcontrib><creatorcontrib>Suur-Uski, A.-S.</creatorcontrib><creatorcontrib>Svalheim, T. L.</creatorcontrib><creatorcontrib>Tavagnacco, D.</creatorcontrib><creatorcontrib>Thommesen, H.</creatorcontrib><creatorcontrib>Watts, D. J.</creatorcontrib><creatorcontrib>Wehus, I. K.</creatorcontrib><creatorcontrib>Zacchei, A.</creatorcontrib><creatorcontrib>Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States)</creatorcontrib><title>BEYONDPLANCK: III. Commander3</title><title>Astronomy and astrophysics (Berlin)</title><description>We describe the computational infrastructure for end-to-end Bayesian cosmic microwave background (CMB) analysis implemented by the BeyondPlanck Collaboration. The code is called
Commander3
. It provides a statistically consistent framework for global analysis of CMB and microwave observations and may be useful for a wide range of legacy, current, and future experiments. The paper has three main goals. Firstly, we provide a high-level overview of the existing code base, aiming to guide readers who wish to extend and adapt the code according to their own needs or re-implement it from scratch in a different programming language. Secondly, we discuss some critical computational challenges that arise within any global CMB analysis framework, for instance in-memory compression of time-ordered data, fast Fourier transform optimization, and parallelization and load-balancing. Thirdly, we quantify the CPU and RAM requirements for the current B
EYOND
P
LANCK
analysis, finding that a total of 1.5 TB of RAM is required for efficient analysis and that the total cost of a full Gibbs sample for LFI is 170 CPU-hrs, including both low-level processing and high-level component separation, which is well within the capabilities of current low-cost computing facilities. The existing code base is made publicly available under a GNU General Public Library (GPL) license.</description><subject>ASTRONOMY AND ASTROPHYSICS</subject><subject>cosmic background radiation</subject><subject>MATHEMATICS AND COMPUTING</subject><subject>methods: data analysis</subject><subject>methods: numerical</subject><issn>0004-6361</issn><issn>1432-0746</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2023</creationdate><recordtype>article</recordtype><sourceid>3HK</sourceid><recordid>eNo90E1PwzAMBuAIgUTZ-AVcEPcyO07q9DjG-BDVxgEOnKI0S0URtKjphX9PqsEutiw9eqXXQlwgXCNoXACAygsqcCFBSkVIfCQyVCRzYFUci-wgTsVZjB_plGgoE_Ob9dt2c_tcLTerp7k4adxnDOd_eyZe79Yvq4e82t4_rpZV7tHgmAfe7YyuA7MvGsUF1AqkCzWyozIEGTSUbAgcMTJ4kKpUXjd1AEQOpGkmrva5fRxbG307Bv_u-64LfrRSkgJDCV3ukR_axDrb9YOzCEbLNDUoToT-SR_jEBr7PbRfbvhJYDJop9p2qm0Pj6FfepxPWQ</recordid><startdate>20230628</startdate><enddate>20230628</enddate><creator>Galloway, M.</creator><creator>Andersen, K. 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K.</creatorcontrib><creatorcontrib>Zacchei, A.</creatorcontrib><creatorcontrib>Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States)</creatorcontrib><collection>CrossRef</collection><collection>NORA - Norwegian Open Research Archives</collection><collection>OSTI.GOV - Hybrid</collection><collection>OSTI.GOV</collection><jtitle>Astronomy and astrophysics (Berlin)</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Galloway, M.</au><au>Andersen, K. J.</au><au>Aurlien, R.</au><au>Banerji, R.</au><au>Bersanelli, M.</au><au>Bertocco, S.</au><au>Brilenkov, M.</au><au>Carbone, M.</au><au>Colombo, L. P. L.</au><au>Eriksen, H. K.</au><au>Eskilt, J. R.</au><au>Foss, M. K.</au><au>Franceschet, C.</au><au>Fuskeland, U.</au><au>Galeotta, S.</au><au>Gerakakis, S.</au><au>Gjerløw, E.</au><au>Hensley, B.</au><au>Herman, D.</au><au>Iacobellis, M.</au><au>Ieronymaki, M.</au><au>Ihle, H. T.</au><au>Jewell, J. B.</au><au>Karakci, A.</au><au>Keihänen, E.</au><au>Keskitalo, R.</au><au>Maggio, G.</au><au>Maino, D.</au><au>Maris, M.</au><au>Mennella, A.</au><au>Paradiso, S.</au><au>Partridge, B.</au><au>Reinecke, M.</au><au>San, M.</au><au>Suur-Uski, A.-S.</au><au>Svalheim, T. L.</au><au>Tavagnacco, D.</au><au>Thommesen, H.</au><au>Watts, D. J.</au><au>Wehus, I. K.</au><au>Zacchei, A.</au><aucorp>Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States)</aucorp><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>BEYONDPLANCK: III. Commander3</atitle><jtitle>Astronomy and astrophysics (Berlin)</jtitle><date>2023-06-28</date><risdate>2023</risdate><volume>675</volume><spage>A3</spage><pages>A3-</pages><issn>0004-6361</issn><eissn>1432-0746</eissn><abstract>We describe the computational infrastructure for end-to-end Bayesian cosmic microwave background (CMB) analysis implemented by the BeyondPlanck Collaboration. The code is called
Commander3
. It provides a statistically consistent framework for global analysis of CMB and microwave observations and may be useful for a wide range of legacy, current, and future experiments. The paper has three main goals. Firstly, we provide a high-level overview of the existing code base, aiming to guide readers who wish to extend and adapt the code according to their own needs or re-implement it from scratch in a different programming language. Secondly, we discuss some critical computational challenges that arise within any global CMB analysis framework, for instance in-memory compression of time-ordered data, fast Fourier transform optimization, and parallelization and load-balancing. Thirdly, we quantify the CPU and RAM requirements for the current B
EYOND
P
LANCK
analysis, finding that a total of 1.5 TB of RAM is required for efficient analysis and that the total cost of a full Gibbs sample for LFI is 170 CPU-hrs, including both low-level processing and high-level component separation, which is well within the capabilities of current low-cost computing facilities. The existing code base is made publicly available under a GNU General Public Library (GPL) license.</abstract><cop>United States</cop><pub>EDP Sciences</pub><doi>10.1051/0004-6361/202243137</doi><oa>free_for_read</oa></addata></record> |
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| ispartof | Astronomy and astrophysics (Berlin), 2023-06, Vol.675, p.A3 |
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| language | eng |
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| source | Bacon EDP Sciences France Licence nationale-ISTEX-PS-Journals-PFISTEX; EDP Sciences; NORA - Norwegian Open Research Archives; Elektronische Zeitschriftenbibliothek - Frei zugängliche E-Journals |
| subjects | ASTRONOMY AND ASTROPHYSICS cosmic background radiation MATHEMATICS AND COMPUTING methods: data analysis methods: numerical |
| title | BEYONDPLANCK: III. Commander3 |
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