Low-level Carbon Monoxide Line Polarization in Two Protoplanetary Disks: HD 142527 and IM Lup
- Autores
- Stephens, Ian; Fernandez Lopez, Manuel; Li, Zhi-Yun; Looney, Leslie W.; Teague, Richard
- Año de publicación
- 2020
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Magnetic fields are expected to play an important role in accretion processes for circumstellar disks. However, measuring the magnetic field morphology is difficult, especially when given that polarimetric (sub)millimeter continuum observations may not trace the fields in most disks. The Goldreich-Kylafis effect suggests that line polarization is perpendicular or parallel to the magnetic field direction. We attempt to observe CO(2-1), 13CO(2-1), and C18O(2-1) line polarization toward HD 142527 and IM Lup, which are large and bright protoplanetary disks. We use spatial averaging and spectral integration to search for signals in both disks, and we detect a potential CO(2-1) Stokes Q signal toward both disks. The total CO(2-1) polarization fractions are 1.57% ± 0.18% and 1.01% ± 0.10% for HD 142527 and IM Lup, respectively. Our Monte Carlo simulations indicate that these signals are marginal. We also stack Stokes parameters based on the Keplerian rotation, but no signal was found. Across the disk traced by dust of HD 142527, the 3σ upper limits for Pfrac at 0.″5 (∼80 au) resolution are typically less than 3% for CO(2-1) and 13CO(2-1) and 4% for C18O(2-1). For IM Lup the 3σ upper limits for these three lines are typically less than 3%, 4%, and 12%, respectively. Upper limits based on our stacking technique are up to a factor of ∼10 lower, although stacking areas can potentially average out small-scale polarization structure. We also compare our continuum polarization at 1.3 mm to observations at 870 μm from previous studies. The polarization in the northern dust trap of HD 142527 shows a significant change in morphology and an increase in Pfrac as compared to 870 μm. For IM Lup, the 1.3 mm polarization may be more azimuthal and has a higher Pfrac than at 870 μm.
Fil: Stephens, Ian. Worcester State University; Estados Unidos
Fil: Fernandez Lopez, Manuel. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
Fil: Li, Zhi-Yun. University of Virginia; Estados Unidos
Fil: Looney, Leslie W.. University of Illinois. Urbana - Champaign; Estados Unidos
Fil: Teague, Richard. Worcester State University; Estados Unidos - Materia
-
Circumstellar disks
Magnetic fields
Polarimetry
Young stellar objects - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/121348
Ver los metadatos del registro completo
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Low-level Carbon Monoxide Line Polarization in Two Protoplanetary Disks: HD 142527 and IM LupStephens, IanFernandez Lopez, ManuelLi, Zhi-YunLooney, Leslie W.Teague, RichardCircumstellar disksMagnetic fieldsPolarimetryYoung stellar objectshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Magnetic fields are expected to play an important role in accretion processes for circumstellar disks. However, measuring the magnetic field morphology is difficult, especially when given that polarimetric (sub)millimeter continuum observations may not trace the fields in most disks. The Goldreich-Kylafis effect suggests that line polarization is perpendicular or parallel to the magnetic field direction. We attempt to observe CO(2-1), 13CO(2-1), and C18O(2-1) line polarization toward HD 142527 and IM Lup, which are large and bright protoplanetary disks. We use spatial averaging and spectral integration to search for signals in both disks, and we detect a potential CO(2-1) Stokes Q signal toward both disks. The total CO(2-1) polarization fractions are 1.57% ± 0.18% and 1.01% ± 0.10% for HD 142527 and IM Lup, respectively. Our Monte Carlo simulations indicate that these signals are marginal. We also stack Stokes parameters based on the Keplerian rotation, but no signal was found. Across the disk traced by dust of HD 142527, the 3σ upper limits for Pfrac at 0.″5 (∼80 au) resolution are typically less than 3% for CO(2-1) and 13CO(2-1) and 4% for C18O(2-1). For IM Lup the 3σ upper limits for these three lines are typically less than 3%, 4%, and 12%, respectively. Upper limits based on our stacking technique are up to a factor of ∼10 lower, although stacking areas can potentially average out small-scale polarization structure. We also compare our continuum polarization at 1.3 mm to observations at 870 μm from previous studies. The polarization in the northern dust trap of HD 142527 shows a significant change in morphology and an increase in Pfrac as compared to 870 μm. For IM Lup, the 1.3 mm polarization may be more azimuthal and has a higher Pfrac than at 870 μm.Fil: Stephens, Ian. Worcester State University; Estados UnidosFil: Fernandez Lopez, Manuel. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; ArgentinaFil: Li, Zhi-Yun. University of Virginia; Estados UnidosFil: Looney, Leslie W.. University of Illinois. Urbana - Champaign; Estados UnidosFil: Teague, Richard. Worcester State University; Estados UnidosIOP Publishing2020-09info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/121348Stephens, Ian; Fernandez Lopez, Manuel; Li, Zhi-Yun; Looney, Leslie W.; Teague, Richard; Low-level Carbon Monoxide Line Polarization in Two Protoplanetary Disks: HD 142527 and IM Lup; IOP Publishing; Astrophysical Journal; 901; 1; 9-2020; 1-240004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/abaef7info:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/abaef7info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:41:44Zoai:ri.conicet.gov.ar:11336/121348instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-29 09:41:45.231CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
Low-level Carbon Monoxide Line Polarization in Two Protoplanetary Disks: HD 142527 and IM Lup |
title |
Low-level Carbon Monoxide Line Polarization in Two Protoplanetary Disks: HD 142527 and IM Lup |
spellingShingle |
Low-level Carbon Monoxide Line Polarization in Two Protoplanetary Disks: HD 142527 and IM Lup Stephens, Ian Circumstellar disks Magnetic fields Polarimetry Young stellar objects |
title_short |
Low-level Carbon Monoxide Line Polarization in Two Protoplanetary Disks: HD 142527 and IM Lup |
title_full |
Low-level Carbon Monoxide Line Polarization in Two Protoplanetary Disks: HD 142527 and IM Lup |
title_fullStr |
Low-level Carbon Monoxide Line Polarization in Two Protoplanetary Disks: HD 142527 and IM Lup |
title_full_unstemmed |
Low-level Carbon Monoxide Line Polarization in Two Protoplanetary Disks: HD 142527 and IM Lup |
title_sort |
Low-level Carbon Monoxide Line Polarization in Two Protoplanetary Disks: HD 142527 and IM Lup |
dc.creator.none.fl_str_mv |
Stephens, Ian Fernandez Lopez, Manuel Li, Zhi-Yun Looney, Leslie W. Teague, Richard |
author |
Stephens, Ian |
author_facet |
Stephens, Ian Fernandez Lopez, Manuel Li, Zhi-Yun Looney, Leslie W. Teague, Richard |
author_role |
author |
author2 |
Fernandez Lopez, Manuel Li, Zhi-Yun Looney, Leslie W. Teague, Richard |
author2_role |
author author author author |
dc.subject.none.fl_str_mv |
Circumstellar disks Magnetic fields Polarimetry Young stellar objects |
topic |
Circumstellar disks Magnetic fields Polarimetry Young stellar objects |
purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
dc.description.none.fl_txt_mv |
Magnetic fields are expected to play an important role in accretion processes for circumstellar disks. However, measuring the magnetic field morphology is difficult, especially when given that polarimetric (sub)millimeter continuum observations may not trace the fields in most disks. The Goldreich-Kylafis effect suggests that line polarization is perpendicular or parallel to the magnetic field direction. We attempt to observe CO(2-1), 13CO(2-1), and C18O(2-1) line polarization toward HD 142527 and IM Lup, which are large and bright protoplanetary disks. We use spatial averaging and spectral integration to search for signals in both disks, and we detect a potential CO(2-1) Stokes Q signal toward both disks. The total CO(2-1) polarization fractions are 1.57% ± 0.18% and 1.01% ± 0.10% for HD 142527 and IM Lup, respectively. Our Monte Carlo simulations indicate that these signals are marginal. We also stack Stokes parameters based on the Keplerian rotation, but no signal was found. Across the disk traced by dust of HD 142527, the 3σ upper limits for Pfrac at 0.″5 (∼80 au) resolution are typically less than 3% for CO(2-1) and 13CO(2-1) and 4% for C18O(2-1). For IM Lup the 3σ upper limits for these three lines are typically less than 3%, 4%, and 12%, respectively. Upper limits based on our stacking technique are up to a factor of ∼10 lower, although stacking areas can potentially average out small-scale polarization structure. We also compare our continuum polarization at 1.3 mm to observations at 870 μm from previous studies. The polarization in the northern dust trap of HD 142527 shows a significant change in morphology and an increase in Pfrac as compared to 870 μm. For IM Lup, the 1.3 mm polarization may be more azimuthal and has a higher Pfrac than at 870 μm. Fil: Stephens, Ian. Worcester State University; Estados Unidos Fil: Fernandez Lopez, Manuel. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina Fil: Li, Zhi-Yun. University of Virginia; Estados Unidos Fil: Looney, Leslie W.. University of Illinois. Urbana - Champaign; Estados Unidos Fil: Teague, Richard. Worcester State University; Estados Unidos |
description |
Magnetic fields are expected to play an important role in accretion processes for circumstellar disks. However, measuring the magnetic field morphology is difficult, especially when given that polarimetric (sub)millimeter continuum observations may not trace the fields in most disks. The Goldreich-Kylafis effect suggests that line polarization is perpendicular or parallel to the magnetic field direction. We attempt to observe CO(2-1), 13CO(2-1), and C18O(2-1) line polarization toward HD 142527 and IM Lup, which are large and bright protoplanetary disks. We use spatial averaging and spectral integration to search for signals in both disks, and we detect a potential CO(2-1) Stokes Q signal toward both disks. The total CO(2-1) polarization fractions are 1.57% ± 0.18% and 1.01% ± 0.10% for HD 142527 and IM Lup, respectively. Our Monte Carlo simulations indicate that these signals are marginal. We also stack Stokes parameters based on the Keplerian rotation, but no signal was found. Across the disk traced by dust of HD 142527, the 3σ upper limits for Pfrac at 0.″5 (∼80 au) resolution are typically less than 3% for CO(2-1) and 13CO(2-1) and 4% for C18O(2-1). For IM Lup the 3σ upper limits for these three lines are typically less than 3%, 4%, and 12%, respectively. Upper limits based on our stacking technique are up to a factor of ∼10 lower, although stacking areas can potentially average out small-scale polarization structure. We also compare our continuum polarization at 1.3 mm to observations at 870 μm from previous studies. The polarization in the northern dust trap of HD 142527 shows a significant change in morphology and an increase in Pfrac as compared to 870 μm. For IM Lup, the 1.3 mm polarization may be more azimuthal and has a higher Pfrac than at 870 μm. |
publishDate |
2020 |
dc.date.none.fl_str_mv |
2020-09 |
dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
format |
article |
status_str |
publishedVersion |
dc.identifier.none.fl_str_mv |
http://hdl.handle.net/11336/121348 Stephens, Ian; Fernandez Lopez, Manuel; Li, Zhi-Yun; Looney, Leslie W.; Teague, Richard; Low-level Carbon Monoxide Line Polarization in Two Protoplanetary Disks: HD 142527 and IM Lup; IOP Publishing; Astrophysical Journal; 901; 1; 9-2020; 1-24 0004-637X CONICET Digital CONICET |
url |
http://hdl.handle.net/11336/121348 |
identifier_str_mv |
Stephens, Ian; Fernandez Lopez, Manuel; Li, Zhi-Yun; Looney, Leslie W.; Teague, Richard; Low-level Carbon Monoxide Line Polarization in Two Protoplanetary Disks: HD 142527 and IM Lup; IOP Publishing; Astrophysical Journal; 901; 1; 9-2020; 1-24 0004-637X CONICET Digital CONICET |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/abaef7 info:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/abaef7 |
dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
eu_rights_str_mv |
openAccess |
rights_invalid_str_mv |
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
dc.format.none.fl_str_mv |
application/pdf application/pdf |
dc.publisher.none.fl_str_mv |
IOP Publishing |
publisher.none.fl_str_mv |
IOP Publishing |
dc.source.none.fl_str_mv |
reponame:CONICET Digital (CONICET) instname:Consejo Nacional de Investigaciones Científicas y Técnicas |
reponame_str |
CONICET Digital (CONICET) |
collection |
CONICET Digital (CONICET) |
instname_str |
Consejo Nacional de Investigaciones Científicas y Técnicas |
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CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas |
repository.mail.fl_str_mv |
dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
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13.070432 |