Discovery of Carbon Radio Recombination Lines in M82
Carbon radio recombination lines (RRLs) at low frequencies (
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| creator | Morabito, Leah K Oonk, J B R Salgado, Francisco Toribio, M Carmen Rottgering, H J A A G G M Tielens Beck, Rainer Adebahr, Bjorn Best, Philip Beswick, Robert Bonafede, Annalisa Brunetti, Gianfranco Bruggen, Marcus Chyzy, Krzysztof T Conway, J E Wim van Driel Gregson, Jonathan Haverkorn, Marijke Heald, George Horellou, Cathy Horneffer, Andreas Iacobelli, Marco Jarvis, Matt J Marti-Vidal, Ivan Miley, George Mulcahy, D D Orru, Emanuela Pizzo, Roberto Scaife, A M M Varenius, Eskil van Weeren, Reinout J White, Glenn J Wise, Michael W |
| description | Carbon radio recombination lines (RRLs) at low frequencies ( |
| doi_str_mv | 10.48550/arxiv.1410.1544 |
| format | Article |
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We present the detection of carbon RRLs in absorption in M82 with LOFAR in the frequency range of 48-64 MHz. This is the first extragalactic detection of RRLs from a species other than hydrogen, and below 1 GHz. Since the carbon RRLs are not detected individually, we cross-correlated the observed spectrum with a template spectrum of carbon RRLs to determine a radial velocity of 219 +- 9 km/s . Using this radial velocity, we stack 22 carbon-{\alpha} transitions from quantum levels n = 468-508 to achieve an 8.5 sigma detection. The absorption line profile exhibits a narrow feature with peak optical depth of 0.003 and FWHM of 31 km/s. Closer inspection suggests that the narrow feature is superimposed on a broad, shallow component. The total line profile appears to be correlated with the 21 cm H I line profile reconstructed from H I absorption in the direction of supernova remnants in the nucleus. The narrow width and centroid velocity of the feature suggests that it is associated with the nuclear starburst region. It is therefore likely that the carbon RRLs are associated with cold atomic gas in the direction of the nucleus of M82.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.1410.1544</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Absorption ; Carbon ; Frequency ranges ; Inspection ; Interstellar matter ; LOFAR ; Nuclei (nuclear physics) ; Physics - Astrophysics of Galaxies ; Radial velocity ; Supernova remnants</subject><ispartof>arXiv.org, 2014-10</ispartof><rights>2014. This work is published under http://arxiv.org/licenses/nonexclusive-distrib/1.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><rights>http://arxiv.org/licenses/nonexclusive-distrib/1.0</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,776,780,881,27902</link.rule.ids><backlink>$$Uhttps://doi.org/10.48550/arXiv.1410.1544$$DView paper in arXiv$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.1088/2041-8205/795/2/L33$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink></links><search><creatorcontrib>Morabito, Leah K</creatorcontrib><creatorcontrib>Oonk, J B R</creatorcontrib><creatorcontrib>Salgado, Francisco</creatorcontrib><creatorcontrib>Toribio, M Carmen</creatorcontrib><creatorcontrib>Rottgering, H J A</creatorcontrib><creatorcontrib>A G G M Tielens</creatorcontrib><creatorcontrib>Beck, Rainer</creatorcontrib><creatorcontrib>Adebahr, Bjorn</creatorcontrib><creatorcontrib>Best, Philip</creatorcontrib><creatorcontrib>Beswick, Robert</creatorcontrib><creatorcontrib>Bonafede, Annalisa</creatorcontrib><creatorcontrib>Brunetti, Gianfranco</creatorcontrib><creatorcontrib>Bruggen, Marcus</creatorcontrib><creatorcontrib>Chyzy, Krzysztof T</creatorcontrib><creatorcontrib>Conway, J E</creatorcontrib><creatorcontrib>Wim van Driel</creatorcontrib><creatorcontrib>Gregson, Jonathan</creatorcontrib><creatorcontrib>Haverkorn, Marijke</creatorcontrib><creatorcontrib>Heald, George</creatorcontrib><creatorcontrib>Horellou, Cathy</creatorcontrib><creatorcontrib>Horneffer, Andreas</creatorcontrib><creatorcontrib>Iacobelli, Marco</creatorcontrib><creatorcontrib>Jarvis, Matt J</creatorcontrib><creatorcontrib>Marti-Vidal, Ivan</creatorcontrib><creatorcontrib>Miley, George</creatorcontrib><creatorcontrib>Mulcahy, D D</creatorcontrib><creatorcontrib>Orru, Emanuela</creatorcontrib><creatorcontrib>Pizzo, Roberto</creatorcontrib><creatorcontrib>Scaife, A M M</creatorcontrib><creatorcontrib>Varenius, Eskil</creatorcontrib><creatorcontrib>van Weeren, Reinout J</creatorcontrib><creatorcontrib>White, Glenn J</creatorcontrib><creatorcontrib>Wise, Michael W</creatorcontrib><title>Discovery of Carbon Radio Recombination Lines in M82</title><title>arXiv.org</title><description>Carbon radio recombination lines (RRLs) at low frequencies (<=500 MHz) trace the cold, diffuse phase of the interstellar medium, which is otherwise difficult to observe. We present the detection of carbon RRLs in absorption in M82 with LOFAR in the frequency range of 48-64 MHz. This is the first extragalactic detection of RRLs from a species other than hydrogen, and below 1 GHz. Since the carbon RRLs are not detected individually, we cross-correlated the observed spectrum with a template spectrum of carbon RRLs to determine a radial velocity of 219 +- 9 km/s . Using this radial velocity, we stack 22 carbon-{\alpha} transitions from quantum levels n = 468-508 to achieve an 8.5 sigma detection. The absorption line profile exhibits a narrow feature with peak optical depth of 0.003 and FWHM of 31 km/s. Closer inspection suggests that the narrow feature is superimposed on a broad, shallow component. The total line profile appears to be correlated with the 21 cm H I line profile reconstructed from H I absorption in the direction of supernova remnants in the nucleus. The narrow width and centroid velocity of the feature suggests that it is associated with the nuclear starburst region. It is therefore likely that the carbon RRLs are associated with cold atomic gas in the direction of the nucleus of M82.</description><subject>Absorption</subject><subject>Carbon</subject><subject>Frequency ranges</subject><subject>Inspection</subject><subject>Interstellar matter</subject><subject>LOFAR</subject><subject>Nuclei (nuclear physics)</subject><subject>Physics - Astrophysics of Galaxies</subject><subject>Radial velocity</subject><subject>Supernova remnants</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2014</creationdate><recordtype>article</recordtype><sourceid>BENPR</sourceid><sourceid>GOX</sourceid><recordid>eNotj0tLAzEUhYMgWGr3riTgeuqdvCZZSn1UGBFK90MmuYEUO6lJW-y_d2pdHTgcPs5HyF0Nc6GlhEebf-JxXouxqKUQV2TCOK8rLRi7IbNSNgDAVMOk5BMinmNx6Yj5RFOgC5v7NNCV9THRFbq07eNg93Hs2jhgoXGgH5rdkutgvwrO_nNK1q8v68Wyaj_f3hdPbWVlbSqrUIZGKtVwBKcRvRbBGPQcDHjNTY8Gg1NSGgeWefAuCBEaJbTyjjs-JfcX7J9Rt8txa_OpO5t1Z7Nx8HAZ7HL6PmDZd5t0yMN4qWOgxQg23PBfPYhPcg</recordid><startdate>20141029</startdate><enddate>20141029</enddate><creator>Morabito, Leah K</creator><creator>Oonk, J B R</creator><creator>Salgado, Francisco</creator><creator>Toribio, M Carmen</creator><creator>Rottgering, H J A</creator><creator>A G G M Tielens</creator><creator>Beck, Rainer</creator><creator>Adebahr, Bjorn</creator><creator>Best, Philip</creator><creator>Beswick, Robert</creator><creator>Bonafede, Annalisa</creator><creator>Brunetti, Gianfranco</creator><creator>Bruggen, Marcus</creator><creator>Chyzy, Krzysztof T</creator><creator>Conway, J E</creator><creator>Wim van Driel</creator><creator>Gregson, Jonathan</creator><creator>Haverkorn, Marijke</creator><creator>Heald, George</creator><creator>Horellou, Cathy</creator><creator>Horneffer, Andreas</creator><creator>Iacobelli, Marco</creator><creator>Jarvis, Matt J</creator><creator>Marti-Vidal, Ivan</creator><creator>Miley, George</creator><creator>Mulcahy, D D</creator><creator>Orru, Emanuela</creator><creator>Pizzo, Roberto</creator><creator>Scaife, A M M</creator><creator>Varenius, Eskil</creator><creator>van Weeren, Reinout J</creator><creator>White, Glenn J</creator><creator>Wise, Michael W</creator><general>Cornell University Library, arXiv.org</general><scope>8FE</scope><scope>8FG</scope><scope>ABJCF</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>HCIFZ</scope><scope>L6V</scope><scope>M7S</scope><scope>PIMPY</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PRINS</scope><scope>PTHSS</scope><scope>GOX</scope></search><sort><creationdate>20141029</creationdate><title>Discovery of Carbon Radio Recombination Lines in M82</title><author>Morabito, Leah K ; Oonk, J B R ; Salgado, Francisco ; Toribio, M Carmen ; Rottgering, H J A ; A G G M Tielens ; Beck, Rainer ; Adebahr, Bjorn ; Best, Philip ; Beswick, Robert ; Bonafede, Annalisa ; Brunetti, Gianfranco ; Bruggen, Marcus ; Chyzy, Krzysztof T ; Conway, J E ; Wim van Driel ; Gregson, Jonathan ; Haverkorn, Marijke ; Heald, George ; Horellou, Cathy ; Horneffer, Andreas ; Iacobelli, Marco ; Jarvis, Matt J ; Marti-Vidal, Ivan ; Miley, George ; Mulcahy, D D ; Orru, Emanuela ; Pizzo, Roberto ; Scaife, A M M ; Varenius, Eskil ; van Weeren, Reinout J ; White, Glenn J ; Wise, Michael W</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a519-a6e5f756673e0c8eed84f99ed3090d839be9efc6559c0a2d0dcf44f76486dc3c3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2014</creationdate><topic>Absorption</topic><topic>Carbon</topic><topic>Frequency ranges</topic><topic>Inspection</topic><topic>Interstellar matter</topic><topic>LOFAR</topic><topic>Nuclei (nuclear physics)</topic><topic>Physics - Astrophysics of Galaxies</topic><topic>Radial velocity</topic><topic>Supernova remnants</topic><toplevel>online_resources</toplevel><creatorcontrib>Morabito, Leah K</creatorcontrib><creatorcontrib>Oonk, J B R</creatorcontrib><creatorcontrib>Salgado, Francisco</creatorcontrib><creatorcontrib>Toribio, M Carmen</creatorcontrib><creatorcontrib>Rottgering, H J A</creatorcontrib><creatorcontrib>A G G M Tielens</creatorcontrib><creatorcontrib>Beck, Rainer</creatorcontrib><creatorcontrib>Adebahr, Bjorn</creatorcontrib><creatorcontrib>Best, Philip</creatorcontrib><creatorcontrib>Beswick, Robert</creatorcontrib><creatorcontrib>Bonafede, Annalisa</creatorcontrib><creatorcontrib>Brunetti, Gianfranco</creatorcontrib><creatorcontrib>Bruggen, Marcus</creatorcontrib><creatorcontrib>Chyzy, Krzysztof T</creatorcontrib><creatorcontrib>Conway, J E</creatorcontrib><creatorcontrib>Wim van Driel</creatorcontrib><creatorcontrib>Gregson, Jonathan</creatorcontrib><creatorcontrib>Haverkorn, Marijke</creatorcontrib><creatorcontrib>Heald, George</creatorcontrib><creatorcontrib>Horellou, Cathy</creatorcontrib><creatorcontrib>Horneffer, Andreas</creatorcontrib><creatorcontrib>Iacobelli, Marco</creatorcontrib><creatorcontrib>Jarvis, Matt J</creatorcontrib><creatorcontrib>Marti-Vidal, Ivan</creatorcontrib><creatorcontrib>Miley, George</creatorcontrib><creatorcontrib>Mulcahy, D D</creatorcontrib><creatorcontrib>Orru, Emanuela</creatorcontrib><creatorcontrib>Pizzo, Roberto</creatorcontrib><creatorcontrib>Scaife, A M M</creatorcontrib><creatorcontrib>Varenius, Eskil</creatorcontrib><creatorcontrib>van Weeren, Reinout J</creatorcontrib><creatorcontrib>White, Glenn J</creatorcontrib><creatorcontrib>Wise, Michael W</creatorcontrib><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>Materials Science & Engineering Collection</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest Central UK/Ireland</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>SciTech Premium Collection</collection><collection>ProQuest Engineering Collection</collection><collection>Engineering Database</collection><collection>Publicly Available Content Database</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central China</collection><collection>Engineering Collection</collection><collection>arXiv.org</collection><jtitle>arXiv.org</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Morabito, Leah K</au><au>Oonk, J B R</au><au>Salgado, Francisco</au><au>Toribio, M Carmen</au><au>Rottgering, H J A</au><au>A G G M Tielens</au><au>Beck, Rainer</au><au>Adebahr, Bjorn</au><au>Best, Philip</au><au>Beswick, Robert</au><au>Bonafede, Annalisa</au><au>Brunetti, Gianfranco</au><au>Bruggen, Marcus</au><au>Chyzy, Krzysztof T</au><au>Conway, J E</au><au>Wim van Driel</au><au>Gregson, Jonathan</au><au>Haverkorn, Marijke</au><au>Heald, George</au><au>Horellou, Cathy</au><au>Horneffer, Andreas</au><au>Iacobelli, Marco</au><au>Jarvis, Matt J</au><au>Marti-Vidal, Ivan</au><au>Miley, George</au><au>Mulcahy, D D</au><au>Orru, Emanuela</au><au>Pizzo, Roberto</au><au>Scaife, A M M</au><au>Varenius, Eskil</au><au>van Weeren, Reinout J</au><au>White, Glenn J</au><au>Wise, Michael W</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Discovery of Carbon Radio Recombination Lines in M82</atitle><jtitle>arXiv.org</jtitle><date>2014-10-29</date><risdate>2014</risdate><eissn>2331-8422</eissn><abstract>Carbon radio recombination lines (RRLs) at low frequencies (<=500 MHz) trace the cold, diffuse phase of the interstellar medium, which is otherwise difficult to observe. We present the detection of carbon RRLs in absorption in M82 with LOFAR in the frequency range of 48-64 MHz. This is the first extragalactic detection of RRLs from a species other than hydrogen, and below 1 GHz. Since the carbon RRLs are not detected individually, we cross-correlated the observed spectrum with a template spectrum of carbon RRLs to determine a radial velocity of 219 +- 9 km/s . Using this radial velocity, we stack 22 carbon-{\alpha} transitions from quantum levels n = 468-508 to achieve an 8.5 sigma detection. The absorption line profile exhibits a narrow feature with peak optical depth of 0.003 and FWHM of 31 km/s. Closer inspection suggests that the narrow feature is superimposed on a broad, shallow component. The total line profile appears to be correlated with the 21 cm H I line profile reconstructed from H I absorption in the direction of supernova remnants in the nucleus. The narrow width and centroid velocity of the feature suggests that it is associated with the nuclear starburst region. It is therefore likely that the carbon RRLs are associated with cold atomic gas in the direction of the nucleus of M82.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.1410.1544</doi><oa>free_for_read</oa></addata></record> |
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| subjects | Absorption Carbon Frequency ranges Inspection Interstellar matter LOFAR Nuclei (nuclear physics) Physics - Astrophysics of Galaxies Radial velocity Supernova remnants |
| title | Discovery of Carbon Radio Recombination Lines in M82 |
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