BEYONDPLANCK
We constrained the level of polarized anomalous microwave emission (AME) on large angular scales using Planck Low-Frequency Instrument (LFI) and WMAP polarization data within a Bayesian cosmic microwave background (CMB) analysis framework. We modeled synchrotron emission with a power-law spectral en...
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| Veröffentlicht in: | Astronomy and astrophysics (Berlin) 2023-07, Vol.675 |
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| creator | Herman, D Hensley, B Andersen, K J Aurlien, R Banerji, R Bersanelli, M Bertocco, S Brilenkov, M Carbone, M Colombo, L P L Eriksen, H K Foss, M K Fuskeland, U Galeotta, S Galloway, M Gerakakis, S Gjerløw, E Iacobellis, M Ieronymaki, M Ihle, H T Jewell, J B Karakci, A Keihänen, E Keskitalo, R Maggio, G Maino, D Maris, M Paradiso, S Partridge, B Reinecke, M A.-S. Suur-Uski Svalheim, T L Tavagnacco, D Thommesen, H Wehus, I K Zacchei, A |
| description | We constrained the level of polarized anomalous microwave emission (AME) on large angular scales using Planck Low-Frequency Instrument (LFI) and WMAP polarization data within a Bayesian cosmic microwave background (CMB) analysis framework. We modeled synchrotron emission with a power-law spectral energy distribution, as well as the sum of AME and thermal dust emission through linear regression with the Planck High-Frequency Instrument (HFI) 353 GHz data. This template-based dust emission model allowed us to constrain the level of polarized AME while making minimal assumptions on its frequency dependence. We neglected CMB fluctuations, but show through simulations that these fluctuations have a minor impact on the results. We find that the resulting AME polarization fraction confidence limit is sensitive to the polarized synchrotron spectral index prior. In addition, for prior means βs |
| doi_str_mv | 10.1051/0004-6361/202243081 |
| format | Article |
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Suur-Uski ; Svalheim, T L ; Tavagnacco, D ; Thommesen, H ; Wehus, I K ; Zacchei, A</creator><creatorcontrib>Herman, D ; Hensley, B ; Andersen, K J ; Aurlien, R ; Banerji, R ; Bersanelli, M ; Bertocco, S ; Brilenkov, M ; Carbone, M ; Colombo, L P L ; Eriksen, H K ; Foss, M K ; Fuskeland, U ; Galeotta, S ; Galloway, M ; Gerakakis, S ; Gjerløw, E ; Iacobellis, M ; Ieronymaki, M ; Ihle, H T ; Jewell, J B ; Karakci, A ; Keihänen, E ; Keskitalo, R ; Maggio, G ; Maino, D ; Maris, M ; Paradiso, S ; Partridge, B ; Reinecke, M ; A.-S. Suur-Uski ; Svalheim, T L ; Tavagnacco, D ; Thommesen, H ; Wehus, I K ; Zacchei, A</creatorcontrib><description>We constrained the level of polarized anomalous microwave emission (AME) on large angular scales using Planck Low-Frequency Instrument (LFI) and WMAP polarization data within a Bayesian cosmic microwave background (CMB) analysis framework. We modeled synchrotron emission with a power-law spectral energy distribution, as well as the sum of AME and thermal dust emission through linear regression with the Planck High-Frequency Instrument (HFI) 353 GHz data. This template-based dust emission model allowed us to constrain the level of polarized AME while making minimal assumptions on its frequency dependence. We neglected CMB fluctuations, but show through simulations that these fluctuations have a minor impact on the results. We find that the resulting AME polarization fraction confidence limit is sensitive to the polarized synchrotron spectral index prior. In addition, for prior means βs < −3.1 we find an upper limit of pAMEmax ≲ 0.6% (95% confidence). In contrast, for means βs = −3.0, we find a nominal detection of pAME = 2.5 ± 1.0% (95% confidence). These data are thus not strong enough to simultaneously and robustly constrain both polarized synchrotron emission and AME, and our main result is therefore a constraint on the AME polarization fraction explicitly as a function of βs. Combining the current Planck and WMAP observations with measurements from high-sensitivity low-frequency experiments such as C-BASS and QUIJOTE will be critical to improve these limits further.</description><identifier>ISSN: 0004-6361</identifier><identifier>EISSN: 1432-0746</identifier><identifier>DOI: 10.1051/0004-6361/202243081</identifier><language>eng</language><publisher>Heidelberg: EDP Sciences</publisher><subject>Confidence limits ; Constraints ; Cosmic microwave background ; Dust ; Emission analysis ; Microwave emission ; Polarization ; Spectral energy distribution ; Statistical analysis ; Synchrotrons</subject><ispartof>Astronomy and astrophysics (Berlin), 2023-07, Vol.675</ispartof><rights>2023. 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Notwithstanding the ProQuest Terms and conditions, you may use this content in accordance with the terms of the License.</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c1231-2a9c53d7a6688fd6058b64686fd5c1ad475f6fcb736f0b2d507f885bdf01fb0c3</citedby></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,780,784,27924,27925</link.rule.ids></links><search><creatorcontrib>Herman, D</creatorcontrib><creatorcontrib>Hensley, B</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>Foss, M K</creatorcontrib><creatorcontrib>Fuskeland, U</creatorcontrib><creatorcontrib>Galeotta, S</creatorcontrib><creatorcontrib>Galloway, M</creatorcontrib><creatorcontrib>Gerakakis, S</creatorcontrib><creatorcontrib>Gjerløw, E</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>Paradiso, S</creatorcontrib><creatorcontrib>Partridge, B</creatorcontrib><creatorcontrib>Reinecke, M</creatorcontrib><creatorcontrib>A.-S. Suur-Uski</creatorcontrib><creatorcontrib>Svalheim, T L</creatorcontrib><creatorcontrib>Tavagnacco, D</creatorcontrib><creatorcontrib>Thommesen, H</creatorcontrib><creatorcontrib>Wehus, I K</creatorcontrib><creatorcontrib>Zacchei, A</creatorcontrib><title>BEYONDPLANCK</title><title>Astronomy and astrophysics (Berlin)</title><description>We constrained the level of polarized anomalous microwave emission (AME) on large angular scales using Planck Low-Frequency Instrument (LFI) and WMAP polarization data within a Bayesian cosmic microwave background (CMB) analysis framework. We modeled synchrotron emission with a power-law spectral energy distribution, as well as the sum of AME and thermal dust emission through linear regression with the Planck High-Frequency Instrument (HFI) 353 GHz data. This template-based dust emission model allowed us to constrain the level of polarized AME while making minimal assumptions on its frequency dependence. We neglected CMB fluctuations, but show through simulations that these fluctuations have a minor impact on the results. We find that the resulting AME polarization fraction confidence limit is sensitive to the polarized synchrotron spectral index prior. In addition, for prior means βs < −3.1 we find an upper limit of pAMEmax ≲ 0.6% (95% confidence). In contrast, for means βs = −3.0, we find a nominal detection of pAME = 2.5 ± 1.0% (95% confidence). These data are thus not strong enough to simultaneously and robustly constrain both polarized synchrotron emission and AME, and our main result is therefore a constraint on the AME polarization fraction explicitly as a function of βs. 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Suur-Uski</creatorcontrib><creatorcontrib>Svalheim, T L</creatorcontrib><creatorcontrib>Tavagnacco, D</creatorcontrib><creatorcontrib>Thommesen, H</creatorcontrib><creatorcontrib>Wehus, I K</creatorcontrib><creatorcontrib>Zacchei, A</creatorcontrib><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>Astronomy and astrophysics (Berlin)</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Herman, D</au><au>Hensley, B</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>Foss, M K</au><au>Fuskeland, U</au><au>Galeotta, S</au><au>Galloway, M</au><au>Gerakakis, S</au><au>Gjerløw, E</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>Paradiso, S</au><au>Partridge, B</au><au>Reinecke, M</au><au>A.-S. Suur-Uski</au><au>Svalheim, T L</au><au>Tavagnacco, D</au><au>Thommesen, H</au><au>Wehus, I K</au><au>Zacchei, A</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>BEYONDPLANCK</atitle><jtitle>Astronomy and astrophysics (Berlin)</jtitle><date>2023-07-01</date><risdate>2023</risdate><volume>675</volume><issn>0004-6361</issn><eissn>1432-0746</eissn><abstract>We constrained the level of polarized anomalous microwave emission (AME) on large angular scales using Planck Low-Frequency Instrument (LFI) and WMAP polarization data within a Bayesian cosmic microwave background (CMB) analysis framework. We modeled synchrotron emission with a power-law spectral energy distribution, as well as the sum of AME and thermal dust emission through linear regression with the Planck High-Frequency Instrument (HFI) 353 GHz data. This template-based dust emission model allowed us to constrain the level of polarized AME while making minimal assumptions on its frequency dependence. We neglected CMB fluctuations, but show through simulations that these fluctuations have a minor impact on the results. We find that the resulting AME polarization fraction confidence limit is sensitive to the polarized synchrotron spectral index prior. In addition, for prior means βs < −3.1 we find an upper limit of pAMEmax ≲ 0.6% (95% confidence). In contrast, for means βs = −3.0, we find a nominal detection of pAME = 2.5 ± 1.0% (95% confidence). These data are thus not strong enough to simultaneously and robustly constrain both polarized synchrotron emission and AME, and our main result is therefore a constraint on the AME polarization fraction explicitly as a function of βs. Combining the current Planck and WMAP observations with measurements from high-sensitivity low-frequency experiments such as C-BASS and QUIJOTE will be critical to improve these limits further.</abstract><cop>Heidelberg</cop><pub>EDP Sciences</pub><doi>10.1051/0004-6361/202243081</doi><oa>free_for_read</oa></addata></record> |
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| subjects | Confidence limits Constraints Cosmic microwave background Dust Emission analysis Microwave emission Polarization Spectral energy distribution Statistical analysis Synchrotrons |
| title | BEYONDPLANCK |
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