The reactivation of water maser emission in the planetary nebula IRAS 18061--2505 through a born-again episode
Water maser emitting planetary nebulae (H$_2$O-PNe) are believed to be among the youngest PNe. We present new optical narrow- and broad-band images, intermediate- and high-resolution long-slit spectra, and archival optical images of the H$_2$O-PN IRAS 18061--2505. It appears a pinched-waist bipolar...
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| creator | Miranda, L. F Suárez, O Olguín, L Vázquez, R Sabin, L Guillén, P. F Gómez, J. F Uscanga, L García-Lario, P de Gregorio-Monsalvo, I Aller, A Manchado, A Boumis, P Riesgo, H Matías, J. M |
| description | Water maser emitting planetary nebulae (H$_2$O-PNe) are believed to be among
the youngest PNe. We present new optical narrow- and broad-band images,
intermediate- and high-resolution long-slit spectra, and archival optical
images of the H$_2$O-PN IRAS 18061--2505. It appears a pinched-waist bipolar PN
consisting of knotty lobes with some point-symmetric regions, a bow-shock near
the tip of each lobe, and a very compact inner nebula where five components are
identified in the spectra by their kinematic and emission properties. The water
masers most probably reside in an oxygen-rich ring tracing the equatorial
region of the bipolar lobes. These two structures probably result from common
envelope evolution plus several bipolar and non-bipolar collimated outflows
that have distorted the lobes. The bow-shocks could be related to a previous
phase to that of common envelope. The inner nebula may be attributed to a late
or very late thermal pulse that occurred before 1951.6 when it was not
detectable in the POSSI-Blue image. Chemical abundances and other properties
favour a 3--4 M$_{\odot}$ progenitor, although if the common envelope phase
accelerated the evolution of the central star, masses |
| doi_str_mv | 10.48550/arxiv.2105.05186 |
| format | Article |
| fullrecord | <record><control><sourceid>arxiv_GOX</sourceid><recordid>TN_cdi_arxiv_primary_2105_05186</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>2105_05186</sourcerecordid><originalsourceid>FETCH-LOGICAL-a676-e54a5e194f1a9ea20e2b77078de18225a502c8af23897e977d4de30f7abc3d9b3</originalsourceid><addsrcrecordid>eNotj81OwzAQhH3pARUegBN-AQf_xLF9rKoClSohQe7RJlm3lhInctICb09auMxIo5nVfoQ8Cp7lVmv-DOk7XDIpuM64Fra4I7E8IU0IzRwuMIch0sHTL5gx0R6mRbEP03TNQ6Tz0h07iDhD-qER63MHdP-x-aTC8kIwJjXXSysN5-OJAq2HFBkcYZniGKahxXuy8tBN-PDva1K-7MrtGzu8v-63mwODwhQMdQ4ahcu9AIcgOcraGG5si8JKqUFz2VjwUlln0BnT5i0q7g3UjWpdrdbk6e_sDbgaU-iXj6sreHUDV7-helKI</addsrcrecordid><sourcetype>Open Access Repository</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype></control><display><type>article</type><title>The reactivation of water maser emission in the planetary nebula IRAS 18061--2505 through a born-again episode</title><source>arXiv.org</source><creator>Miranda, L. F ; Suárez, O ; Olguín, L ; Vázquez, R ; Sabin, L ; Guillén, P. F ; Gómez, J. F ; Uscanga, L ; García-Lario, P ; de Gregorio-Monsalvo, I ; Aller, A ; Manchado, A ; Boumis, P ; Riesgo, H ; Matías, J. M</creator><creatorcontrib>Miranda, L. F ; Suárez, O ; Olguín, L ; Vázquez, R ; Sabin, L ; Guillén, P. F ; Gómez, J. F ; Uscanga, L ; García-Lario, P ; de Gregorio-Monsalvo, I ; Aller, A ; Manchado, A ; Boumis, P ; Riesgo, H ; Matías, J. M</creatorcontrib><description>Water maser emitting planetary nebulae (H$_2$O-PNe) are believed to be among
the youngest PNe. We present new optical narrow- and broad-band images,
intermediate- and high-resolution long-slit spectra, and archival optical
images of the H$_2$O-PN IRAS 18061--2505. It appears a pinched-waist bipolar PN
consisting of knotty lobes with some point-symmetric regions, a bow-shock near
the tip of each lobe, and a very compact inner nebula where five components are
identified in the spectra by their kinematic and emission properties. The water
masers most probably reside in an oxygen-rich ring tracing the equatorial
region of the bipolar lobes. These two structures probably result from common
envelope evolution plus several bipolar and non-bipolar collimated outflows
that have distorted the lobes. The bow-shocks could be related to a previous
phase to that of common envelope. The inner nebula may be attributed to a late
or very late thermal pulse that occurred before 1951.6 when it was not
detectable in the POSSI-Blue image. Chemical abundances and other properties
favour a 3--4 M$_{\odot}$ progenitor, although if the common envelope phase
accelerated the evolution of the central star, masses <1.5 M$_{\odot}$ cannot
be discarded. The age of the bipolar lobes is incompatible with the existence
of water masers in IRAS 18061--2505, which may have been lately reactivated
through shocks in the oxygen-rich ring, that are generated by the thermal
pulse, implying that this PN is not extremely young. We discuss H$_2$O-PNe and
possibly related objects in the light of our results for IRAS 18061--2505.</description><identifier>DOI: 10.48550/arxiv.2105.05186</identifier><language>eng</language><subject>Physics - Astrophysics of Galaxies</subject><creationdate>2021-05</creationdate><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>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,778,883</link.rule.ids><linktorsrc>$$Uhttps://arxiv.org/abs/2105.05186$$EView_record_in_Cornell_University$$FView_record_in_$$GCornell_University$$Hfree_for_read</linktorsrc><backlink>$$Uhttps://doi.org/10.48550/arXiv.2105.05186$$DView paper in arXiv$$Hfree_for_read</backlink></links><search><creatorcontrib>Miranda, L. F</creatorcontrib><creatorcontrib>Suárez, O</creatorcontrib><creatorcontrib>Olguín, L</creatorcontrib><creatorcontrib>Vázquez, R</creatorcontrib><creatorcontrib>Sabin, L</creatorcontrib><creatorcontrib>Guillén, P. F</creatorcontrib><creatorcontrib>Gómez, J. F</creatorcontrib><creatorcontrib>Uscanga, L</creatorcontrib><creatorcontrib>García-Lario, P</creatorcontrib><creatorcontrib>de Gregorio-Monsalvo, I</creatorcontrib><creatorcontrib>Aller, A</creatorcontrib><creatorcontrib>Manchado, A</creatorcontrib><creatorcontrib>Boumis, P</creatorcontrib><creatorcontrib>Riesgo, H</creatorcontrib><creatorcontrib>Matías, J. M</creatorcontrib><title>The reactivation of water maser emission in the planetary nebula IRAS 18061--2505 through a born-again episode</title><description>Water maser emitting planetary nebulae (H$_2$O-PNe) are believed to be among
the youngest PNe. We present new optical narrow- and broad-band images,
intermediate- and high-resolution long-slit spectra, and archival optical
images of the H$_2$O-PN IRAS 18061--2505. It appears a pinched-waist bipolar PN
consisting of knotty lobes with some point-symmetric regions, a bow-shock near
the tip of each lobe, and a very compact inner nebula where five components are
identified in the spectra by their kinematic and emission properties. The water
masers most probably reside in an oxygen-rich ring tracing the equatorial
region of the bipolar lobes. These two structures probably result from common
envelope evolution plus several bipolar and non-bipolar collimated outflows
that have distorted the lobes. The bow-shocks could be related to a previous
phase to that of common envelope. The inner nebula may be attributed to a late
or very late thermal pulse that occurred before 1951.6 when it was not
detectable in the POSSI-Blue image. Chemical abundances and other properties
favour a 3--4 M$_{\odot}$ progenitor, although if the common envelope phase
accelerated the evolution of the central star, masses <1.5 M$_{\odot}$ cannot
be discarded. The age of the bipolar lobes is incompatible with the existence
of water masers in IRAS 18061--2505, which may have been lately reactivated
through shocks in the oxygen-rich ring, that are generated by the thermal
pulse, implying that this PN is not extremely young. We discuss H$_2$O-PNe and
possibly related objects in the light of our results for IRAS 18061--2505.</description><subject>Physics - Astrophysics of Galaxies</subject><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2021</creationdate><recordtype>article</recordtype><sourceid>GOX</sourceid><recordid>eNotj81OwzAQhH3pARUegBN-AQf_xLF9rKoClSohQe7RJlm3lhInctICb09auMxIo5nVfoQ8Cp7lVmv-DOk7XDIpuM64Fra4I7E8IU0IzRwuMIch0sHTL5gx0R6mRbEP03TNQ6Tz0h07iDhD-qER63MHdP-x-aTC8kIwJjXXSysN5-OJAq2HFBkcYZniGKahxXuy8tBN-PDva1K-7MrtGzu8v-63mwODwhQMdQ4ahcu9AIcgOcraGG5si8JKqUFz2VjwUlln0BnT5i0q7g3UjWpdrdbk6e_sDbgaU-iXj6sreHUDV7-helKI</recordid><startdate>20210511</startdate><enddate>20210511</enddate><creator>Miranda, L. F</creator><creator>Suárez, O</creator><creator>Olguín, L</creator><creator>Vázquez, R</creator><creator>Sabin, L</creator><creator>Guillén, P. F</creator><creator>Gómez, J. F</creator><creator>Uscanga, L</creator><creator>García-Lario, P</creator><creator>de Gregorio-Monsalvo, I</creator><creator>Aller, A</creator><creator>Manchado, A</creator><creator>Boumis, P</creator><creator>Riesgo, H</creator><creator>Matías, J. M</creator><scope>GOX</scope></search><sort><creationdate>20210511</creationdate><title>The reactivation of water maser emission in the planetary nebula IRAS 18061--2505 through a born-again episode</title><author>Miranda, L. F ; Suárez, O ; Olguín, L ; Vázquez, R ; Sabin, L ; Guillén, P. F ; Gómez, J. F ; Uscanga, L ; García-Lario, P ; de Gregorio-Monsalvo, I ; Aller, A ; Manchado, A ; Boumis, P ; Riesgo, H ; Matías, J. M</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a676-e54a5e194f1a9ea20e2b77078de18225a502c8af23897e977d4de30f7abc3d9b3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2021</creationdate><topic>Physics - Astrophysics of Galaxies</topic><toplevel>online_resources</toplevel><creatorcontrib>Miranda, L. F</creatorcontrib><creatorcontrib>Suárez, O</creatorcontrib><creatorcontrib>Olguín, L</creatorcontrib><creatorcontrib>Vázquez, R</creatorcontrib><creatorcontrib>Sabin, L</creatorcontrib><creatorcontrib>Guillén, P. F</creatorcontrib><creatorcontrib>Gómez, J. F</creatorcontrib><creatorcontrib>Uscanga, L</creatorcontrib><creatorcontrib>García-Lario, P</creatorcontrib><creatorcontrib>de Gregorio-Monsalvo, I</creatorcontrib><creatorcontrib>Aller, A</creatorcontrib><creatorcontrib>Manchado, A</creatorcontrib><creatorcontrib>Boumis, P</creatorcontrib><creatorcontrib>Riesgo, H</creatorcontrib><creatorcontrib>Matías, J. M</creatorcontrib><collection>arXiv.org</collection></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Miranda, L. F</au><au>Suárez, O</au><au>Olguín, L</au><au>Vázquez, R</au><au>Sabin, L</au><au>Guillén, P. F</au><au>Gómez, J. F</au><au>Uscanga, L</au><au>García-Lario, P</au><au>de Gregorio-Monsalvo, I</au><au>Aller, A</au><au>Manchado, A</au><au>Boumis, P</au><au>Riesgo, H</au><au>Matías, J. M</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The reactivation of water maser emission in the planetary nebula IRAS 18061--2505 through a born-again episode</atitle><date>2021-05-11</date><risdate>2021</risdate><abstract>Water maser emitting planetary nebulae (H$_2$O-PNe) are believed to be among
the youngest PNe. We present new optical narrow- and broad-band images,
intermediate- and high-resolution long-slit spectra, and archival optical
images of the H$_2$O-PN IRAS 18061--2505. It appears a pinched-waist bipolar PN
consisting of knotty lobes with some point-symmetric regions, a bow-shock near
the tip of each lobe, and a very compact inner nebula where five components are
identified in the spectra by their kinematic and emission properties. The water
masers most probably reside in an oxygen-rich ring tracing the equatorial
region of the bipolar lobes. These two structures probably result from common
envelope evolution plus several bipolar and non-bipolar collimated outflows
that have distorted the lobes. The bow-shocks could be related to a previous
phase to that of common envelope. The inner nebula may be attributed to a late
or very late thermal pulse that occurred before 1951.6 when it was not
detectable in the POSSI-Blue image. Chemical abundances and other properties
favour a 3--4 M$_{\odot}$ progenitor, although if the common envelope phase
accelerated the evolution of the central star, masses <1.5 M$_{\odot}$ cannot
be discarded. The age of the bipolar lobes is incompatible with the existence
of water masers in IRAS 18061--2505, which may have been lately reactivated
through shocks in the oxygen-rich ring, that are generated by the thermal
pulse, implying that this PN is not extremely young. We discuss H$_2$O-PNe and
possibly related objects in the light of our results for IRAS 18061--2505.</abstract><doi>10.48550/arxiv.2105.05186</doi><oa>free_for_read</oa></addata></record> |
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| title | The reactivation of water maser emission in the planetary nebula IRAS 18061--2505 through a born-again episode |
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