QUIJOTE scientific results – II. Polarisation measurements of the microwave emission in the Galactic molecular complexes W43 and W47 and supernova remnant W44
We present Q-U-I JOint TEnerife (QUIJOTE) intensity and polarisation maps at 10-20 GHz covering a region along the Galactic plane 24... l ... 45..., |b| ... 8... These maps result from 210 h of data, have a sensitivity in polarisation of ...40 ...K beam super( -1) and an angular resolution of ...1.....
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| Veröffentlicht in: | Monthly notices of the Royal Astronomical Society 2017-02, Vol.464 (4), p.4107-4107 |
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| creator | Genova-Santos, R Rubino-Martin, J A Pelaez-Santos, A Poidevin, F Rebolo, R Vignaga, R Artal, E Harper, S Hoyland, R Lasenby, A Martinez-Gonzalez, E Piccirillo, L Tramonte, D Watson, R A |
| description | We present Q-U-I JOint TEnerife (QUIJOTE) intensity and polarisation maps at 10-20 GHz covering a region along the Galactic plane 24... l ... 45..., |b| ... 8... These maps result from 210 h of data, have a sensitivity in polarisation of ...40 ...K beam super( -1) and an angular resolution of ...1... Our intensity data are crucial to confirm the presence of anomalous microwave emission (AME) towards the two molecular complexes W43 (22...) and W47 (8...). We also detect at high significance (6...) AME associated with W44, the first clear detection of this emission towards a supernova remnant. The new QUIJOTE polarisation data, in combination with Wilkinson Microwave Anisotropy Probe (WMAP), are essential to (i) determine the spectral index of the synchrotron emission in W44, ... = -0.62 plus or minus 0.03, in good agreement with the value inferred from the intensity spectrum once a free-free component is included in the fit; (ii) trace the change in the polarisation angle associated with Faraday rotation in the direction of W44 with rotation measure -404 plus or minus 49 rad m super( -2) and (iii) set upper limits on the polarisation of W43 of ... < 0.39 per cent (95 per cent C.L.) from QUIJOTE 17 GHz, and |
| doi_str_mv | 10.1093/mnras/stw2503 |
| format | Article |
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Polarisation measurements of the microwave emission in the Galactic molecular complexes W43 and W47 and supernova remnant W44</title><source>Oxford Journals Open Access Collection</source><creator>Genova-Santos, R ; Rubino-Martin, J A ; Pelaez-Santos, A ; Poidevin, F ; Rebolo, R ; Vignaga, R ; Artal, E ; Harper, S ; Hoyland, R ; Lasenby, A ; Martinez-Gonzalez, E ; Piccirillo, L ; Tramonte, D ; Watson, R A</creator><creatorcontrib>Genova-Santos, R ; Rubino-Martin, J A ; Pelaez-Santos, A ; Poidevin, F ; Rebolo, R ; Vignaga, R ; Artal, E ; Harper, S ; Hoyland, R ; Lasenby, A ; Martinez-Gonzalez, E ; Piccirillo, L ; Tramonte, D ; Watson, R A</creatorcontrib><description>We present Q-U-I JOint TEnerife (QUIJOTE) intensity and polarisation maps at 10-20 GHz covering a region along the Galactic plane 24... l ... 45..., |b| ... 8... These maps result from 210 h of data, have a sensitivity in polarisation of ...40 ...K beam super( -1) and an angular resolution of ...1... Our intensity data are crucial to confirm the presence of anomalous microwave emission (AME) towards the two molecular complexes W43 (22...) and W47 (8...). We also detect at high significance (6...) AME associated with W44, the first clear detection of this emission towards a supernova remnant. The new QUIJOTE polarisation data, in combination with Wilkinson Microwave Anisotropy Probe (WMAP), are essential to (i) determine the spectral index of the synchrotron emission in W44, ... = -0.62 plus or minus 0.03, in good agreement with the value inferred from the intensity spectrum once a free-free component is included in the fit; (ii) trace the change in the polarisation angle associated with Faraday rotation in the direction of W44 with rotation measure -404 plus or minus 49 rad m super( -2) and (iii) set upper limits on the polarisation of W43 of ... < 0.39 per cent (95 per cent C.L.) from QUIJOTE 17 GHz, and <0.22 per cent from WMAP 41 GHz data, which are the most stringent constraints ever obtained on the polarisation fraction of the AME. For typical physical conditions (grain temperature and magnetic field strengths), and in the case of perfect alignment between the grains and the magnetic field, the models of electric or magnetic dipole emissions predict higher polarisation fractions. 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Polarisation measurements of the microwave emission in the Galactic molecular complexes W43 and W47 and supernova remnant W44</title><title>Monthly notices of the Royal Astronomical Society</title><description>We present Q-U-I JOint TEnerife (QUIJOTE) intensity and polarisation maps at 10-20 GHz covering a region along the Galactic plane 24... l ... 45..., |b| ... 8... These maps result from 210 h of data, have a sensitivity in polarisation of ...40 ...K beam super( -1) and an angular resolution of ...1... Our intensity data are crucial to confirm the presence of anomalous microwave emission (AME) towards the two molecular complexes W43 (22...) and W47 (8...). We also detect at high significance (6...) AME associated with W44, the first clear detection of this emission towards a supernova remnant. The new QUIJOTE polarisation data, in combination with Wilkinson Microwave Anisotropy Probe (WMAP), are essential to (i) determine the spectral index of the synchrotron emission in W44, ... = -0.62 plus or minus 0.03, in good agreement with the value inferred from the intensity spectrum once a free-free component is included in the fit; (ii) trace the change in the polarisation angle associated with Faraday rotation in the direction of W44 with rotation measure -404 plus or minus 49 rad m super( -2) and (iii) set upper limits on the polarisation of W43 of ... < 0.39 per cent (95 per cent C.L.) from QUIJOTE 17 GHz, and <0.22 per cent from WMAP 41 GHz data, which are the most stringent constraints ever obtained on the polarisation fraction of the AME. For typical physical conditions (grain temperature and magnetic field strengths), and in the case of perfect alignment between the grains and the magnetic field, the models of electric or magnetic dipole emissions predict higher polarisation fractions. (ProQuest: ... denotes formulae/symbols omitted.)</description><subject>Astronomy</subject><subject>Emission</subject><subject>Emissions</subject><subject>Grains</subject><subject>Magnetic dipoles</subject><subject>Magnetic fields</subject><subject>Mathematical models</subject><subject>Measurement</subject><subject>Microwave emission</subject><subject>Microwaves</subject><subject>Stars & galaxies</subject><subject>Supernova remnants</subject><subject>Supernovae</subject><subject>Symbols</subject><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2017</creationdate><recordtype>article</recordtype><recordid>eNqNkb1OHDEUha2ISFkIZXpLaWgG7PH8eMoIEViEBEggytFdzx3FaGwvvh5IOt6BF-DZ8iTxLlSpqE5xPh2dew9j36Q4lKJTR85HoCNKT2Ut1Ce2kKqpi7Jrmh22EELVhW6l_MJ2ie6FEJUqmwV7vb5dnl_enHAyFn2yozU8Is1TIv73-YUvl4f8KkwQLUGywXOHQHNEl2HiYeTpF3JnTQxP8IgcnSXaYNZvnVOYwKSc6cKEZs453AS3nvA3Er-rFAc_ZG23SvMaow-PkBs4Dz5lp_rKPo8wEe6_6x67_Xlyc3xWXFyeLo9_XBRGKZmKQRtZlrrtWtVBV8kVjEbjqIQZABrAsZF6BWYQHZQZNLoWpqzbVjbDygwa1R47eMtdx_AwI6U-n2JwmsBjmKmXWgsh61J2H0DrrsrJrczo9__Q-zBHnw_ZULl5LWWVqeKNym8kijj262gdxD-9FP1m2n47bf8-rfoHBAGa2A</recordid><startdate>20170201</startdate><enddate>20170201</enddate><creator>Genova-Santos, R</creator><creator>Rubino-Martin, J A</creator><creator>Pelaez-Santos, A</creator><creator>Poidevin, F</creator><creator>Rebolo, R</creator><creator>Vignaga, R</creator><creator>Artal, E</creator><creator>Harper, S</creator><creator>Hoyland, R</creator><creator>Lasenby, A</creator><creator>Martinez-Gonzalez, E</creator><creator>Piccirillo, L</creator><creator>Tramonte, D</creator><creator>Watson, R A</creator><general>Oxford University Press</general><scope>AAYXX</scope><scope>CITATION</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>7TG</scope><scope>KL.</scope></search><sort><creationdate>20170201</creationdate><title>QUIJOTE scientific results – II. Polarisation measurements of the microwave emission in the Galactic molecular complexes W43 and W47 and supernova remnant W44</title><author>Genova-Santos, R ; Rubino-Martin, J A ; Pelaez-Santos, A ; Poidevin, F ; Rebolo, R ; Vignaga, R ; Artal, E ; Harper, S ; Hoyland, R ; Lasenby, A ; Martinez-Gonzalez, E ; Piccirillo, L ; Tramonte, D ; Watson, R A</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c331t-d8c122879739a941bafc8ef30cdaa6aef618bacd09a2122c850c257716dbcd8e3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2017</creationdate><topic>Astronomy</topic><topic>Emission</topic><topic>Emissions</topic><topic>Grains</topic><topic>Magnetic dipoles</topic><topic>Magnetic fields</topic><topic>Mathematical models</topic><topic>Measurement</topic><topic>Microwave emission</topic><topic>Microwaves</topic><topic>Stars & galaxies</topic><topic>Supernova remnants</topic><topic>Supernovae</topic><topic>Symbols</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Genova-Santos, R</creatorcontrib><creatorcontrib>Rubino-Martin, J A</creatorcontrib><creatorcontrib>Pelaez-Santos, A</creatorcontrib><creatorcontrib>Poidevin, F</creatorcontrib><creatorcontrib>Rebolo, R</creatorcontrib><creatorcontrib>Vignaga, R</creatorcontrib><creatorcontrib>Artal, E</creatorcontrib><creatorcontrib>Harper, S</creatorcontrib><creatorcontrib>Hoyland, R</creatorcontrib><creatorcontrib>Lasenby, A</creatorcontrib><creatorcontrib>Martinez-Gonzalez, E</creatorcontrib><creatorcontrib>Piccirillo, L</creatorcontrib><creatorcontrib>Tramonte, D</creatorcontrib><creatorcontrib>Watson, R A</creatorcontrib><collection>CrossRef</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><jtitle>Monthly notices of the Royal Astronomical Society</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Genova-Santos, R</au><au>Rubino-Martin, J A</au><au>Pelaez-Santos, A</au><au>Poidevin, F</au><au>Rebolo, R</au><au>Vignaga, R</au><au>Artal, E</au><au>Harper, S</au><au>Hoyland, R</au><au>Lasenby, A</au><au>Martinez-Gonzalez, E</au><au>Piccirillo, L</au><au>Tramonte, D</au><au>Watson, R A</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>QUIJOTE scientific results – II. Polarisation measurements of the microwave emission in the Galactic molecular complexes W43 and W47 and supernova remnant W44</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><date>2017-02-01</date><risdate>2017</risdate><volume>464</volume><issue>4</issue><spage>4107</spage><epage>4107</epage><pages>4107-4107</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><abstract>We present Q-U-I JOint TEnerife (QUIJOTE) intensity and polarisation maps at 10-20 GHz covering a region along the Galactic plane 24... l ... 45..., |b| ... 8... These maps result from 210 h of data, have a sensitivity in polarisation of ...40 ...K beam super( -1) and an angular resolution of ...1... Our intensity data are crucial to confirm the presence of anomalous microwave emission (AME) towards the two molecular complexes W43 (22...) and W47 (8...). We also detect at high significance (6...) AME associated with W44, the first clear detection of this emission towards a supernova remnant. The new QUIJOTE polarisation data, in combination with Wilkinson Microwave Anisotropy Probe (WMAP), are essential to (i) determine the spectral index of the synchrotron emission in W44, ... = -0.62 plus or minus 0.03, in good agreement with the value inferred from the intensity spectrum once a free-free component is included in the fit; (ii) trace the change in the polarisation angle associated with Faraday rotation in the direction of W44 with rotation measure -404 plus or minus 49 rad m super( -2) and (iii) set upper limits on the polarisation of W43 of ... < 0.39 per cent (95 per cent C.L.) from QUIJOTE 17 GHz, and <0.22 per cent from WMAP 41 GHz data, which are the most stringent constraints ever obtained on the polarisation fraction of the AME. For typical physical conditions (grain temperature and magnetic field strengths), and in the case of perfect alignment between the grains and the magnetic field, the models of electric or magnetic dipole emissions predict higher polarisation fractions. (ProQuest: ... denotes formulae/symbols omitted.)</abstract><cop>London</cop><pub>Oxford University Press</pub><doi>10.1093/mnras/stw2503</doi><tpages>1</tpages></addata></record> |
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| identifier | ISSN: 0035-8711 |
| ispartof | Monthly notices of the Royal Astronomical Society, 2017-02, Vol.464 (4), p.4107-4107 |
| issn | 0035-8711 1365-2966 |
| language | eng |
| recordid | cdi_proquest_miscellaneous_1880015219 |
| source | Oxford Journals Open Access Collection |
| subjects | Astronomy Emission Emissions Grains Magnetic dipoles Magnetic fields Mathematical models Measurement Microwave emission Microwaves Stars & galaxies Supernova remnants Supernovae Symbols |
| title | QUIJOTE scientific results – II. Polarisation measurements of the microwave emission in the Galactic molecular complexes W43 and W47 and supernova remnant W44 |
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