High-resolution radio study of SNR IC443 at low radio frequencies
- Autores
- Castelletti, Gabriela Marta; Dubner, Gloria Mabel; Clarke, T.; Kassim, N. E.
- Año de publicación
- 2011
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Aims. We investigate the morphology at low radio frequencies of the supernova remnant (SNR) IC 443 in detail and accurately establish its radio continuum spectral properties. Methods. We used the VLA in multiple configurations to produce high-resolution radio images of IC 443 at 74 and 330 MHz. From these data we produced the first sensitive, spatially resolved spectral analysis of the radio emission at long wavelengths. The changes with position in the radio spectral index were correlated with data in near infrared (NIR) from 2MASS, in gamma-rays from VERITAS, and with the molecular 12CO (J = 1 − 0) line emission. Results. The new image at 74 MHz has HPBW = 35′′ and rms = 30 mJy beam-1 and at 330 MHz HPBW = 17′′ and rms = 1.7 mJy beam-1. The integrated flux densities for the whole SNR are Jy and Jy. Improved estimates of the integrated spectrum were derived taking a turnover into account to fit the lowest frequency measurements in the literature. Combining our measurements with existing data, we derive an integrated spectral index with a free-free continuum optical depth at 330 MHz τ330 ~ 7 × 10-4 (τ10 = 1.07); all measurements above ~ 10 MHz are equally consistent with a power law spectrum. For the pulsar wind nebula associated with the compact source CXOU J061705.3+222127, we calculated Jy, Jy, and . Substantial variations are observed in spectral index between 74 and 330 MHz across IC 443. The flattest spectral components ( − 0.25 ≤ α ≤ − 0.05) coincide with the brightest parts of the SNR along the eastern border, with an impressive agreement with ionic lines as observed in the 2MASS J and H bands. The diffuse interior of IC 443 has a spectrum steeper than found anywhere in the SNR ( − 0.85 ≤ α ≤ − 0.6), while the southern ridge again has a flatter spectrum (α ~ −0.4). With the available statistics the VERITAS γ-ray emission strikingly matches the CO distribution, but no clear evidence is found for a morphological correlation between the TeV distribution and radio emission. Conclusions. The excellent correspondence between the eastern radio flattest spectrum region and NIR ionic lines strongly suggests that the passage of a fast, dissociating J-type shock across the interacting molecular cloud dissociated the molecules and ionized the gas. We therefore conclude that thermal absorption at 74 MHz (τ74 up to ~0.3) is responsible for the localized spectral index flattening observed along the eastern border of IC 443. Towards the interior of IC 443, the spectrum is consistent with those expected from linear diffusive shock acceleration, while the flatter spectrum in the southern ridge is a consequence of the strong shock/molecular cloud interaction.
Fil: Castelletti, Gabriela Marta. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Dubner, Gloria Mabel. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Clarke, T.. Spece Sciences División. Naval Research Laboratory; Estados Unidos
Fil: Kassim, N. E.. Spece Sciences División. Naval Research Laboratory; Estados Unidos - Materia
-
ISM: INDIVIDUAL OBJECTS: IC 443
ISM: SUPERNOVA REMNANTS
RADIO CONTINUUM: ISM
INFRARED: ISM - 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:11336/19818
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oai:ri.conicet.gov.ar:11336/19818 |
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spelling |
High-resolution radio study of SNR IC443 at low radio frequenciesCastelletti, Gabriela MartaDubner, Gloria MabelClarke, T.Kassim, N. E.ISM: INDIVIDUAL OBJECTS: IC 443ISM: SUPERNOVA REMNANTSRADIO CONTINUUM: ISMINFRARED: ISMhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Aims. We investigate the morphology at low radio frequencies of the supernova remnant (SNR) IC 443 in detail and accurately establish its radio continuum spectral properties. Methods. We used the VLA in multiple configurations to produce high-resolution radio images of IC 443 at 74 and 330 MHz. From these data we produced the first sensitive, spatially resolved spectral analysis of the radio emission at long wavelengths. The changes with position in the radio spectral index were correlated with data in near infrared (NIR) from 2MASS, in gamma-rays from VERITAS, and with the molecular 12CO (J = 1 − 0) line emission. Results. The new image at 74 MHz has HPBW = 35′′ and rms = 30 mJy beam-1 and at 330 MHz HPBW = 17′′ and rms = 1.7 mJy beam-1. The integrated flux densities for the whole SNR are Jy and Jy. Improved estimates of the integrated spectrum were derived taking a turnover into account to fit the lowest frequency measurements in the literature. Combining our measurements with existing data, we derive an integrated spectral index with a free-free continuum optical depth at 330 MHz τ330 ~ 7 × 10-4 (τ10 = 1.07); all measurements above ~ 10 MHz are equally consistent with a power law spectrum. For the pulsar wind nebula associated with the compact source CXOU J061705.3+222127, we calculated Jy, Jy, and . Substantial variations are observed in spectral index between 74 and 330 MHz across IC 443. The flattest spectral components ( − 0.25 ≤ α ≤ − 0.05) coincide with the brightest parts of the SNR along the eastern border, with an impressive agreement with ionic lines as observed in the 2MASS J and H bands. The diffuse interior of IC 443 has a spectrum steeper than found anywhere in the SNR ( − 0.85 ≤ α ≤ − 0.6), while the southern ridge again has a flatter spectrum (α ~ −0.4). With the available statistics the VERITAS γ-ray emission strikingly matches the CO distribution, but no clear evidence is found for a morphological correlation between the TeV distribution and radio emission. Conclusions. The excellent correspondence between the eastern radio flattest spectrum region and NIR ionic lines strongly suggests that the passage of a fast, dissociating J-type shock across the interacting molecular cloud dissociated the molecules and ionized the gas. We therefore conclude that thermal absorption at 74 MHz (τ74 up to ~0.3) is responsible for the localized spectral index flattening observed along the eastern border of IC 443. Towards the interior of IC 443, the spectrum is consistent with those expected from linear diffusive shock acceleration, while the flatter spectrum in the southern ridge is a consequence of the strong shock/molecular cloud interaction.Fil: Castelletti, Gabriela Marta. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Dubner, Gloria Mabel. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Clarke, T.. Spece Sciences División. Naval Research Laboratory; Estados UnidosFil: Kassim, N. E.. Spece Sciences División. Naval Research Laboratory; Estados UnidosEDP Sciences2011-04info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/19818Castelletti, Gabriela Marta; Dubner, Gloria Mabel; Clarke, T.; Kassim, N. E.; High-resolution radio study of SNR IC443 at low radio frequencies; EDP Sciences; Astronomy and Astrophysics; 534; A21; 4-2011; 1-140004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201016081info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1104.0205info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2011/10/aa16081-10/aa16081-10.htmlinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:39:38Zoai:ri.conicet.gov.ar:11336/19818instacron: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:34982025-10-22 11:39:38.797CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
High-resolution radio study of SNR IC443 at low radio frequencies |
title |
High-resolution radio study of SNR IC443 at low radio frequencies |
spellingShingle |
High-resolution radio study of SNR IC443 at low radio frequencies Castelletti, Gabriela Marta ISM: INDIVIDUAL OBJECTS: IC 443 ISM: SUPERNOVA REMNANTS RADIO CONTINUUM: ISM INFRARED: ISM |
title_short |
High-resolution radio study of SNR IC443 at low radio frequencies |
title_full |
High-resolution radio study of SNR IC443 at low radio frequencies |
title_fullStr |
High-resolution radio study of SNR IC443 at low radio frequencies |
title_full_unstemmed |
High-resolution radio study of SNR IC443 at low radio frequencies |
title_sort |
High-resolution radio study of SNR IC443 at low radio frequencies |
dc.creator.none.fl_str_mv |
Castelletti, Gabriela Marta Dubner, Gloria Mabel Clarke, T. Kassim, N. E. |
author |
Castelletti, Gabriela Marta |
author_facet |
Castelletti, Gabriela Marta Dubner, Gloria Mabel Clarke, T. Kassim, N. E. |
author_role |
author |
author2 |
Dubner, Gloria Mabel Clarke, T. Kassim, N. E. |
author2_role |
author author author |
dc.subject.none.fl_str_mv |
ISM: INDIVIDUAL OBJECTS: IC 443 ISM: SUPERNOVA REMNANTS RADIO CONTINUUM: ISM INFRARED: ISM |
topic |
ISM: INDIVIDUAL OBJECTS: IC 443 ISM: SUPERNOVA REMNANTS RADIO CONTINUUM: ISM INFRARED: ISM |
purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
dc.description.none.fl_txt_mv |
Aims. We investigate the morphology at low radio frequencies of the supernova remnant (SNR) IC 443 in detail and accurately establish its radio continuum spectral properties. Methods. We used the VLA in multiple configurations to produce high-resolution radio images of IC 443 at 74 and 330 MHz. From these data we produced the first sensitive, spatially resolved spectral analysis of the radio emission at long wavelengths. The changes with position in the radio spectral index were correlated with data in near infrared (NIR) from 2MASS, in gamma-rays from VERITAS, and with the molecular 12CO (J = 1 − 0) line emission. Results. The new image at 74 MHz has HPBW = 35′′ and rms = 30 mJy beam-1 and at 330 MHz HPBW = 17′′ and rms = 1.7 mJy beam-1. The integrated flux densities for the whole SNR are Jy and Jy. Improved estimates of the integrated spectrum were derived taking a turnover into account to fit the lowest frequency measurements in the literature. Combining our measurements with existing data, we derive an integrated spectral index with a free-free continuum optical depth at 330 MHz τ330 ~ 7 × 10-4 (τ10 = 1.07); all measurements above ~ 10 MHz are equally consistent with a power law spectrum. For the pulsar wind nebula associated with the compact source CXOU J061705.3+222127, we calculated Jy, Jy, and . Substantial variations are observed in spectral index between 74 and 330 MHz across IC 443. The flattest spectral components ( − 0.25 ≤ α ≤ − 0.05) coincide with the brightest parts of the SNR along the eastern border, with an impressive agreement with ionic lines as observed in the 2MASS J and H bands. The diffuse interior of IC 443 has a spectrum steeper than found anywhere in the SNR ( − 0.85 ≤ α ≤ − 0.6), while the southern ridge again has a flatter spectrum (α ~ −0.4). With the available statistics the VERITAS γ-ray emission strikingly matches the CO distribution, but no clear evidence is found for a morphological correlation between the TeV distribution and radio emission. Conclusions. The excellent correspondence between the eastern radio flattest spectrum region and NIR ionic lines strongly suggests that the passage of a fast, dissociating J-type shock across the interacting molecular cloud dissociated the molecules and ionized the gas. We therefore conclude that thermal absorption at 74 MHz (τ74 up to ~0.3) is responsible for the localized spectral index flattening observed along the eastern border of IC 443. Towards the interior of IC 443, the spectrum is consistent with those expected from linear diffusive shock acceleration, while the flatter spectrum in the southern ridge is a consequence of the strong shock/molecular cloud interaction. Fil: Castelletti, Gabriela Marta. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina Fil: Dubner, Gloria Mabel. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina Fil: Clarke, T.. Spece Sciences División. Naval Research Laboratory; Estados Unidos Fil: Kassim, N. E.. Spece Sciences División. Naval Research Laboratory; Estados Unidos |
description |
Aims. We investigate the morphology at low radio frequencies of the supernova remnant (SNR) IC 443 in detail and accurately establish its radio continuum spectral properties. Methods. We used the VLA in multiple configurations to produce high-resolution radio images of IC 443 at 74 and 330 MHz. From these data we produced the first sensitive, spatially resolved spectral analysis of the radio emission at long wavelengths. The changes with position in the radio spectral index were correlated with data in near infrared (NIR) from 2MASS, in gamma-rays from VERITAS, and with the molecular 12CO (J = 1 − 0) line emission. Results. The new image at 74 MHz has HPBW = 35′′ and rms = 30 mJy beam-1 and at 330 MHz HPBW = 17′′ and rms = 1.7 mJy beam-1. The integrated flux densities for the whole SNR are Jy and Jy. Improved estimates of the integrated spectrum were derived taking a turnover into account to fit the lowest frequency measurements in the literature. Combining our measurements with existing data, we derive an integrated spectral index with a free-free continuum optical depth at 330 MHz τ330 ~ 7 × 10-4 (τ10 = 1.07); all measurements above ~ 10 MHz are equally consistent with a power law spectrum. For the pulsar wind nebula associated with the compact source CXOU J061705.3+222127, we calculated Jy, Jy, and . Substantial variations are observed in spectral index between 74 and 330 MHz across IC 443. The flattest spectral components ( − 0.25 ≤ α ≤ − 0.05) coincide with the brightest parts of the SNR along the eastern border, with an impressive agreement with ionic lines as observed in the 2MASS J and H bands. The diffuse interior of IC 443 has a spectrum steeper than found anywhere in the SNR ( − 0.85 ≤ α ≤ − 0.6), while the southern ridge again has a flatter spectrum (α ~ −0.4). With the available statistics the VERITAS γ-ray emission strikingly matches the CO distribution, but no clear evidence is found for a morphological correlation between the TeV distribution and radio emission. Conclusions. The excellent correspondence between the eastern radio flattest spectrum region and NIR ionic lines strongly suggests that the passage of a fast, dissociating J-type shock across the interacting molecular cloud dissociated the molecules and ionized the gas. We therefore conclude that thermal absorption at 74 MHz (τ74 up to ~0.3) is responsible for the localized spectral index flattening observed along the eastern border of IC 443. Towards the interior of IC 443, the spectrum is consistent with those expected from linear diffusive shock acceleration, while the flatter spectrum in the southern ridge is a consequence of the strong shock/molecular cloud interaction. |
publishDate |
2011 |
dc.date.none.fl_str_mv |
2011-04 |
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/11336/19818 Castelletti, Gabriela Marta; Dubner, Gloria Mabel; Clarke, T.; Kassim, N. E.; High-resolution radio study of SNR IC443 at low radio frequencies; EDP Sciences; Astronomy and Astrophysics; 534; A21; 4-2011; 1-14 0004-6361 CONICET Digital CONICET |
url |
http://hdl.handle.net/11336/19818 |
identifier_str_mv |
Castelletti, Gabriela Marta; Dubner, Gloria Mabel; Clarke, T.; Kassim, N. E.; High-resolution radio study of SNR IC443 at low radio frequencies; EDP Sciences; Astronomy and Astrophysics; 534; A21; 4-2011; 1-14 0004-6361 CONICET Digital CONICET |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201016081 info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1104.0205 info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2011/10/aa16081-10/aa16081-10.html |
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 |
EDP Sciences |
publisher.none.fl_str_mv |
EDP Sciences |
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 |
repository.name.fl_str_mv |
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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12.8982525 |