QUIJOTE scientific results - VII. Galactic AME sources in the QUIJOTE-MFI northern hemisphere wide survey
The QUIJOTE-MFI Northern Hemisphere Wide Survey has provided maps of the sky above declinations −30◦ at 11, 13, 17, and 19 GHz. These data are combined with ancillary data to produce Spectral Energy Distributions in intensity in the frequency range 0.4–3 000 GHz on a sample of 52 candidate compact s...
| Autores: | , , , , , , , , , , , , , , , , , , , |
|---|---|
| Tipo de recurso: | artículo |
| Fecha de publicación: | 2023 |
| País: | España |
| Institución: | Universidad de Cantabria (UC) |
| Repositorio: | UCrea Repositorio Abierto de la Universidad de Cantabria |
| Idioma: | inglés |
| OAI Identifier: | oai:repositorio.unican.es:10902/31814 |
| Acceso en línea: | https://hdl.handle.net/10902/31814 |
| Access Level: | acceso abierto |
| Palabra clave: | ISM: clouds Photodissociation region (PDR) Radiation mechanisms: general Radiation mechanisms: non-thermal Radiation mechanisms: thermal Radio continuum: ISM |
| id |
ES_facf4476fe69cfa87af669faf5f708ec |
|---|---|
| oai_identifier_str |
oai:repositorio.unican.es:10902/31814 |
| network_acronym_str |
ES |
| network_name_str |
España |
| repository_id_str |
|
| dc.title.none.fl_str_mv |
QUIJOTE scientific results - VII. Galactic AME sources in the QUIJOTE-MFI northern hemisphere wide survey |
| title |
QUIJOTE scientific results - VII. Galactic AME sources in the QUIJOTE-MFI northern hemisphere wide survey |
| spellingShingle |
QUIJOTE scientific results - VII. Galactic AME sources in the QUIJOTE-MFI northern hemisphere wide survey Poidevin, F. ISM: clouds Photodissociation region (PDR) Radiation mechanisms: general Radiation mechanisms: non-thermal Radiation mechanisms: thermal Radio continuum: ISM |
| title_short |
QUIJOTE scientific results - VII. Galactic AME sources in the QUIJOTE-MFI northern hemisphere wide survey |
| title_full |
QUIJOTE scientific results - VII. Galactic AME sources in the QUIJOTE-MFI northern hemisphere wide survey |
| title_fullStr |
QUIJOTE scientific results - VII. Galactic AME sources in the QUIJOTE-MFI northern hemisphere wide survey |
| title_full_unstemmed |
QUIJOTE scientific results - VII. Galactic AME sources in the QUIJOTE-MFI northern hemisphere wide survey |
| title_sort |
QUIJOTE scientific results - VII. Galactic AME sources in the QUIJOTE-MFI northern hemisphere wide survey |
| dc.creator.none.fl_str_mv |
Poidevin, F. Génova-Santos, R.T. Rubiño-Martín, J.A. López-Caraballo, C.H. Watson, R.A. Artal Latorre, Eduardo|||0000-0002-2569-1894 Ashdown, M. Barreiro Vilas, Rita Belén|||0000-0002-6139-4272 Casas Reinares, Francisco Javier|||0000-0002-2217-5843 Hoz López-Collado, Elena de la Fernández-Torreiro, M. Guidi, F. Herranz Muñoz, Diego|||0000-0003-4540-1417 Hoyland, R.J. Lasenby, A.N. Martínez González, Enrique Peel, M.W. Piccirillo, L. Rebolo López, Rafael Vielva Martínez, Patricio|||0000-0003-0051-272X |
| author |
Poidevin, F. |
| author_facet |
Poidevin, F. Génova-Santos, R.T. Rubiño-Martín, J.A. López-Caraballo, C.H. Watson, R.A. Artal Latorre, Eduardo|||0000-0002-2569-1894 Ashdown, M. Barreiro Vilas, Rita Belén|||0000-0002-6139-4272 Casas Reinares, Francisco Javier|||0000-0002-2217-5843 Hoz López-Collado, Elena de la Fernández-Torreiro, M. Guidi, F. Herranz Muñoz, Diego|||0000-0003-4540-1417 Hoyland, R.J. Lasenby, A.N. Martínez González, Enrique Peel, M.W. Piccirillo, L. Rebolo López, Rafael Vielva Martínez, Patricio|||0000-0003-0051-272X |
| author_role |
author |
| author2 |
Génova-Santos, R.T. Rubiño-Martín, J.A. López-Caraballo, C.H. Watson, R.A. Artal Latorre, Eduardo|||0000-0002-2569-1894 Ashdown, M. Barreiro Vilas, Rita Belén|||0000-0002-6139-4272 Casas Reinares, Francisco Javier|||0000-0002-2217-5843 Hoz López-Collado, Elena de la Fernández-Torreiro, M. Guidi, F. Herranz Muñoz, Diego|||0000-0003-4540-1417 Hoyland, R.J. Lasenby, A.N. Martínez González, Enrique Peel, M.W. Piccirillo, L. Rebolo López, Rafael Vielva Martínez, Patricio|||0000-0003-0051-272X |
| author2_role |
author author author author author author author author author author author author author author author author author author author |
| dc.contributor.none.fl_str_mv |
Universidad de Cantabria |
| dc.subject.none.fl_str_mv |
ISM: clouds Photodissociation region (PDR) Radiation mechanisms: general Radiation mechanisms: non-thermal Radiation mechanisms: thermal Radio continuum: ISM |
| topic |
ISM: clouds Photodissociation region (PDR) Radiation mechanisms: general Radiation mechanisms: non-thermal Radiation mechanisms: thermal Radio continuum: ISM |
| description |
The QUIJOTE-MFI Northern Hemisphere Wide Survey has provided maps of the sky above declinations −30◦ at 11, 13, 17, and 19 GHz. These data are combined with ancillary data to produce Spectral Energy Distributions in intensity in the frequency range 0.4–3 000 GHz on a sample of 52 candidate compact sources harbouring anomalous microwave emission (AME). We apply a component separation analysis at 1◦ scale on the full sample from which we identify 44 sources with high AME significance. We explore correlations between different fitted parameters on this last sample. QUIJOTE-MFI data contribute to notably improve the characterization of the AME spectrum, and its separation from the other components. In particular, ignoring the 10–20 GHz data produces on average an underestimation of the AME amplitude, and an overestimation of the free–free component. We find an average AME peak frequency of 23.6 ± 3.6 GHz, about 4 GHz lower than the value reported in previous studies. The strongest correlation is found between the peak flux density of the thermal dust and of the AME component. A mild correlation is found between the AME emissivity (AAME/τ250) and the interstellar radiation field. On the other hand no correlation is found between the AME emissivity and the free–free radiation Emission Measure. Our statistical results suggest that the interstellar radiation field could still be the main driver of the intensity of the AME as regards spinning dust excitation mechanisms. On the other hand, it is not clear whether spinning dust would be most likely associated with cold phases of the interstellar medium rather than with hot phases dominated by free–free radiation. |
| publishDate |
2023 |
| dc.date.none.fl_str_mv |
2023 2023-01-09 |
| dc.type.none.fl_str_mv |
journal article http://purl.org/coar/resource_type/c_6501 NA http://purl.org/coar/version/c_be7fb7dd8ff6fe43 |
| dc.type.openaire.fl_str_mv |
info:eu-repo/semantics/article |
| format |
article |
| dc.identifier.none.fl_str_mv |
https://hdl.handle.net/10902/31814 |
| url |
https://hdl.handle.net/10902/31814 |
| dc.language.none.fl_str_mv |
Inglés eng |
| language_invalid_str_mv |
Inglés |
| language |
eng |
| dc.relation.none.fl_str_mv |
European Commission http://dx.doi.org/10.13039/501100000780 Horizon 2020 Framework Programme 687312 |
| dc.rights.none.fl_str_mv |
open access http://purl.org/coar/access_right/c_abf2 |
| dc.rights.openaire.fl_str_mv |
info:eu-repo/semantics/openAccess |
| rights_invalid_str_mv |
open access http://purl.org/coar/access_right/c_abf2 |
| eu_rights_str_mv |
openAccess |
| dc.publisher.none.fl_str_mv |
Oxford University Press |
| publisher.none.fl_str_mv |
Oxford University Press |
| dc.source.none.fl_str_mv |
Monthly Notices of the Royal Astronomical Society, 2023, 519(3), 3481-3503 reponame:UCrea Repositorio Abierto de la Universidad de Cantabria instname:Universidad de Cantabria (UC) |
| instname_str |
Universidad de Cantabria (UC) |
| reponame_str |
UCrea Repositorio Abierto de la Universidad de Cantabria |
| collection |
UCrea Repositorio Abierto de la Universidad de Cantabria |
| repository.name.fl_str_mv |
|
| repository.mail.fl_str_mv |
|
| _version_ |
1869425271832051712 |
| spelling |
QUIJOTE scientific results - VII. Galactic AME sources in the QUIJOTE-MFI northern hemisphere wide surveyPoidevin, F.Génova-Santos, R.T.Rubiño-Martín, J.A.López-Caraballo, C.H.Watson, R.A.Artal Latorre, Eduardo|||0000-0002-2569-1894Ashdown, M.Barreiro Vilas, Rita Belén|||0000-0002-6139-4272Casas Reinares, Francisco Javier|||0000-0002-2217-5843Hoz López-Collado, Elena de laFernández-Torreiro, M.Guidi, F.Herranz Muñoz, Diego|||0000-0003-4540-1417Hoyland, R.J.Lasenby, A.N.Martínez González, EnriquePeel, M.W.Piccirillo, L.Rebolo López, RafaelVielva Martínez, Patricio|||0000-0003-0051-272XISM: cloudsPhotodissociation region (PDR)Radiation mechanisms: generalRadiation mechanisms: non-thermalRadiation mechanisms: thermalRadio continuum: ISMThe QUIJOTE-MFI Northern Hemisphere Wide Survey has provided maps of the sky above declinations −30◦ at 11, 13, 17, and 19 GHz. These data are combined with ancillary data to produce Spectral Energy Distributions in intensity in the frequency range 0.4–3 000 GHz on a sample of 52 candidate compact sources harbouring anomalous microwave emission (AME). We apply a component separation analysis at 1◦ scale on the full sample from which we identify 44 sources with high AME significance. We explore correlations between different fitted parameters on this last sample. QUIJOTE-MFI data contribute to notably improve the characterization of the AME spectrum, and its separation from the other components. In particular, ignoring the 10–20 GHz data produces on average an underestimation of the AME amplitude, and an overestimation of the free–free component. We find an average AME peak frequency of 23.6 ± 3.6 GHz, about 4 GHz lower than the value reported in previous studies. The strongest correlation is found between the peak flux density of the thermal dust and of the AME component. A mild correlation is found between the AME emissivity (AAME/τ250) and the interstellar radiation field. On the other hand no correlation is found between the AME emissivity and the free–free radiation Emission Measure. Our statistical results suggest that the interstellar radiation field could still be the main driver of the intensity of the AME as regards spinning dust excitation mechanisms. On the other hand, it is not clear whether spinning dust would be most likely associated with cold phases of the interstellar medium rather than with hot phases dominated by free–free radiation.We thank the referee of this article, Simon Casassus, for his comments that help to improve the communication of some of the concepts presented in this work. 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, AYA2017-90675-REDC (co-funded with EU FEDER - Fondo Europeo de Desarrollo Regional funds), PGC2018-101814-B-I00, PID2019-110610RB-C21, PID2020-120514GB-I00, IACA13-3E-2336, IACA15-BE-3707, EQC2018-004918-P, 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 ProID 2020010108. This project has received funding from the European Union's Horizon 2020 research and innovation program under grant agreement number 687312 (RADIOFOREGROUNDS).FP acknowledges the European Commission under the Marie Sklodowska-Curie Actions within the European Union's Horizon 2020 research and innovation programme under Grant Agreement number 658499 (PolAME). FP acknowledges support from the Spanish State Research Agency (AEI) under grant numbers PID2019-105552RB-C43. FG acknowledges funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement No 101001897). EdlH acknowledge partial financial support from the Concepcion Arenal Programme of the Universidad de Cantabria. BR -G acknowledges the Agenzia Spaziale Italiana - Istituto Nazionale di Fisica Nucleare (ASI-INFN) Agreement 2014-037-R.0. DT acknowledges the support from the Chinese Academy of Sciences President's International Fellowship Initiative, Grant No. 2020PM0042. We acknowledge the use of data from the Planck/ESA mission, downloaded from the Planck Legacy Archive, and of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by the NASA Office of Space Science. Some of the results in this paper have been derived using the HEALPIX (Gorski et al. 2005 ) package.Oxford University PressUniversidad de Cantabria20232023-01-09journal articlehttp://purl.org/coar/resource_type/c_6501NAhttp://purl.org/coar/version/c_be7fb7dd8ff6fe43info:eu-repo/semantics/articlehttps://hdl.handle.net/10902/31814Monthly Notices of the Royal Astronomical Society, 2023, 519(3), 3481-3503reponame:UCrea Repositorio Abierto de la Universidad de Cantabriainstname:Universidad de Cantabria (UC)InglésengEuropean Commission http://dx.doi.org/10.13039/501100000780 Horizon 2020 Framework Programme 687312open accesshttp://purl.org/coar/access_right/c_abf2info:eu-repo/semantics/openAccessoai:repositorio.unican.es:10902/318142026-06-02T12:39:31Z |
| score |
15,298079 |