@article{10902/36394,
year = {2025},
month = {3},
url = {https://hdl.handle.net/10902/36394},
abstract = {This work focuses on the study of the anomalous microwave emission (AME), an important emission mechanism between 10 and 60 GHz whose polarisation properties are not yet fully understood and is therefore a potential contaminant for future cosmic microwave background (CMB) polarisation observations. We used new QUIJOTE-MFI maps at 11, 13, 17, and 19 GHz obtained from the combination of the public wide survey data and additional 1800 h of dedicated raster scan observations together with other public ancillary data, including WMAP and Planck, to study the polarisation properties of the AME in three Galactic regions: ρ Ophiuchi, Perseus, and W43. We obtained the spectral energy distributions (SEDs) of the three regions over the frequency range 0:4-3000 GHz in intensity and polarisation. The intensity SEDs are well described by a combination of free-free emission, thermal dust, AME, and CMB anisotropies. In polarisation, we extracted the flux densities using all available data between 11 and 353 GHz. We implemented an improved intensity-to-polarisation leakage correction that allowed reliable polarisation constraints well below the 1% level from Planck-LFI data to be derived for the first time. A frequency stacking of maps in the range 10-60 GHz allowed us to reduce the statistical noise and to push the upper limits on the AME polarisation level. We obtained upper limits on the AME polarisation fraction of the order .1% (95% confidence level) for the three regions. In particular, we obtained ΠAME < 1:0% (at 28.4 GHz), ΠAME < 0:9% (at 28.4 GHz), and ΠAME < 0:28% (at 33 GHz) in ρ Ophiuchi, Perseus, and W43, respectively. At the QUIJOTE 17 GHz frequency band, we found ΠAME < 5:0% for ρ Ophiuchi, ΠAME < 3:4% for Perseus, and ΠAME < 0:85% for W43. We note that for the ρ Ophiuchi molecular cloud, the new QUIJOTE-MFI data allowed us to set the first constraints on the AME polarisation in the range 10-20 GHz. Our final upper limits derived using the stacking procedure are ΠAME < 0:58% for ρ Ophiuchi, ΠAME < 0:67% for Perseus, and ΠAME < 0:31% for W43. Altogether, these are the most stringent constraints to date on the AME polarisation fraction of these three star-forming regions. © The Authors 2025.},
organization = {We thank the staff of the Teide Observatory for invaluable assistance in the commissioning and operation of QUIJOTE. The QUIJOTE experiment is being developed by the Instituto de Astrofisica de Canarias (IAC), the Instituto de Fisica de Cantabria (IFCA), and the Universities of Cantabria, Manchester and Cambridge. Partial financial support was provided by the Spanish Ministry of Science and Innovation under the projects AYA2007-68058-C03-01, AYA2007-68058-C03-02, AYA2010-21766-C03-01, AYA2010-21766-C03-02, AYA2014-60438-P, ESP2015-70646-C2-1-R, AYA2017-84185-P, ESP2017-83921-C2-1-R, PGC2018-101814-B-I00, PID2019-110610RB-C21, PID2020-120514GB-I00, IACA13-3E-2336, IACA15-BE-3707, EQC2018-004918-P, PID2023-150398NB-I00 and PID2023-151567NB-I00, the Severo Ochoa Programs SEV-2015-0548 and CEX2019-000920-S, the Maria de Maeztu Program MDM-2017-0765, and by the Consolider-Ingenio project CSD2010-00064 (EPI: Exploring the Physics of Inflation). We acknowledge support from the ACIISI, Consejeria de Economia, Conocimiento y Empleo del Gobierno de Canarias and the European Regional Development Fund (ERDF) under grant with reference ProID2020010108, and Red de Investigación RED2022-134715-T funded by MCIN/AEI/10.13039/501100011033. This project has received funding from the European Union’s Horizon 2020 research and innovation program under grant agreement number 687312 (RADIOFOREGROUNDS), and the Horizon Europe research and innovation program under GA 101135036 (RadioForegroundsPlus).
This research made use of computing time available on the high-performance computing systems at the IAC. We thankfully acknowledge the technical expertise and assistance provided by the Spanish Supercomputing Network (Red Española de Supercomputación), as well as the computer resources used: the Deimos/Diva Supercomputer, located at the IAC. This research used resources of the National Energy Research Scientific Computing Center, that is supported by the O_ce of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. RGG acknowledges support from Italian Ministry of education, university and research. MFT acknowledges support from from the Agencia Estatal de Investigación (AEI) of the Ministerio de Ciencia, Innovación y Universidades (MCIU), from the European Social Fund (ESF) under grant with reference PRE-C-2018-0067 and from the French Programme d’investissements d’avenir through the Enigmass Labex. FP acknowledges support from the Spanish Ministerio de Ciencia, Innovación y Universidades (MICINN) under grant numbers PID2022-141915NB-C21. DT acknowledges financial support from the XJTLU Research Development Fund (RDF) grant with number RDF-22-02-068. CHM acknowledges financial support from the Spanish Ministry of Science and Innovation under project PID2021-126616NB-I00. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France (Wenger et al. 2000). Some of the presented results are based on observations obtained with Planck (http://www.esa.int/Planck), an ESA science mission with instruments and contributions directly funded by ESA Member States, NASA, and Canada. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by the NASA O_ce of Space Science. Some of the results in this paper have been derived using the healpy and HEALPix packages (Górski et al. 2005; Zonca et al. 2019).We have also used scipy (Virtanen et al. 2020), emcee (Foreman-Mackey et al. 2013), numpy (Harris et al. 2020), matplotlib (Hunter 2007), corner (Foreman-Mackey 2016) and astropy (Astropy Collaboration 2013, 2018) python packages.},
publisher = {EDP Sciences},
publisher = {Astronomy and Astrophysics, 2025, 695, A245},
title = {QUIJOTE scientific results: XVIII. New constraints on the polarisation of the anomalous microwave emission in bright Galactic regions: p Ophiuchi, Perseus, and W43},
author = {González González.Raúl and Génova Santos, Ricardo Tanasu and Rubiño Martín, José Alberto and Peel, Mike W. and Guidi, Frederica and López Caraballo, Carlos H. and Fernandez Torreiro, Mateo and Rebolo López, Rafael and Hernández Monteagudo, Carlos and Adak, Debabrata and Artal Latorre, Eduardo and Ashdown, Mark A.J. and Barreiro Vilas, Rita Belén and Casas Reinares, Francisco Javier and Cepeda-Arroita, Roke and Hoz López-Collado, Elena de la and Herranz Muñoz, Diego and Martínez González, Enrique and Pascual Cisneros, Guillermo and Vielva Martínez, Patricio},
}