The luminous red nova AT 2018bwo in NGC 45 and its binary yellow supergiant progenitor
Luminous Red Novae (LRNe) are astrophysical transients associated with the partial ejection of a binary system's common envelope (CE) shortly before its merger. Here we present the results of our photometric and spectroscopic follow-up campaign of AT2018bwo (DLT18x), a LRN discovered in NGC45,...
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| creator | Blagorodnova, Nadejda Klencki, Jakub Pejcha, Ondrej Vreeswijk, Paul M Bond, Howard E Burdge, Kevin B De, Kishalay Fremling, Christoffer Gehrz, Robert D Jencson, Jacob E Kasliwal, Mansi M Kupfer, Thomas Lau, Ryan M Masci, Frank J Rich, R Michael |
| description | Luminous Red Novae (LRNe) are astrophysical transients associated with the partial ejection of a binary system's common envelope (CE) shortly before its merger. Here we present the results of our photometric and spectroscopic follow-up campaign of AT2018bwo (DLT18x), a LRN discovered in NGC45, and investigate its progenitor system using binary stellar-evolution models. The transient reached a peak magnitude of \(M_r=-10.97\pm0.11\) and maintained this brightness during its optical plateau of \(t_p = 41\pm5\)days. During this phase, it showed a rather stable photospheric temperature of ~3300K and a luminosity of ~\(10^{40}\)erg/s. The photosphere of AT2018bwo at early times appeared larger and cooler than other similar LRNe, likely due to an extended mass-loss episode before the merger. Towards the end of the plateau, optical spectra showed a reddened continuum with strong molecular absorption bands. The reprocessed emission by the cooling dust was also detected in the mid-infrared bands ~1.5 years after the outburst. Archival Spitzer and Hubble Space Telescope data taken 10-14 years before the transient event suggest a progenitor star with \(T_{prog}\sim 6500\)K, \(R_{prog}\sim 100R_{\odot}\) and \(L_{prog}\sim 2\times10^4L_{\odot}\), and an upper limit for optically thin warm (1000 K) dust mass of \(M_d |
| doi_str_mv | 10.48550/arxiv.2102.05662 |
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Here we present the results of our photometric and spectroscopic follow-up campaign of AT2018bwo (DLT18x), a LRN discovered in NGC45, and investigate its progenitor system using binary stellar-evolution models. The transient reached a peak magnitude of \(M_r=-10.97\pm0.11\) and maintained this brightness during its optical plateau of \(t_p = 41\pm5\)days. During this phase, it showed a rather stable photospheric temperature of ~3300K and a luminosity of ~\(10^{40}\)erg/s. The photosphere of AT2018bwo at early times appeared larger and cooler than other similar LRNe, likely due to an extended mass-loss episode before the merger. Towards the end of the plateau, optical spectra showed a reddened continuum with strong molecular absorption bands. The reprocessed emission by the cooling dust was also detected in the mid-infrared bands ~1.5 years after the outburst. Archival Spitzer and Hubble Space Telescope data taken 10-14 years before the transient event suggest a progenitor star with \(T_{prog}\sim 6500\)K, \(R_{prog}\sim 100R_{\odot}\) and \(L_{prog}\sim 2\times10^4L_{\odot}\), and an upper limit for optically thin warm (1000 K) dust mass of \(M_d<10^{-6}M_{\odot}\). Using stellar binary-evolution models, we determined the properties of binary systems consistent with the progenitor parameter space. For AT2018bwo, we infer a primary mass of 12-16 \(M_{\odot}\), which is 9-45% larger than the ~11\(M_{\odot}\) obtained using single-star evolution models. The system, consistent with a yellow-supergiant primary, was likely in a stable mass-transfer regime with -2.4<log (\(\dot{M}/M_{\odot}\)/yr)<-1.2 a decade before the main instability occurred. During the dynamical merger, the system would have ejected 0.15-0.5\(M_{\odot}\) with a velocity of ~500 km/s.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.2102.05662</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Absorption spectra ; Astronomical models ; Binary stars ; Dust ; Dynamic stability ; Hubble Space Telescope ; Luminosity ; Molecular absorption ; Novae ; Photosphere ; Physics - Solar and Stellar Astrophysics ; Space telescopes ; Stellar evolution ; Stellar system evolution ; Transients (astronomy)</subject><ispartof>arXiv.org, 2022-01</ispartof><rights>2022. This work is published under http://creativecommons.org/licenses/by/4.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><rights>http://creativecommons.org/licenses/by/4.0</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.2102.05662$$DView paper in arXiv$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.1051/0004-6361/202140525$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink></links><search><creatorcontrib>Blagorodnova, Nadejda</creatorcontrib><creatorcontrib>Klencki, Jakub</creatorcontrib><creatorcontrib>Pejcha, Ondrej</creatorcontrib><creatorcontrib>Vreeswijk, Paul M</creatorcontrib><creatorcontrib>Bond, Howard E</creatorcontrib><creatorcontrib>Burdge, Kevin B</creatorcontrib><creatorcontrib>De, Kishalay</creatorcontrib><creatorcontrib>Fremling, Christoffer</creatorcontrib><creatorcontrib>Gehrz, Robert D</creatorcontrib><creatorcontrib>Jencson, Jacob E</creatorcontrib><creatorcontrib>Kasliwal, Mansi M</creatorcontrib><creatorcontrib>Kupfer, Thomas</creatorcontrib><creatorcontrib>Lau, Ryan M</creatorcontrib><creatorcontrib>Masci, Frank J</creatorcontrib><creatorcontrib>Rich, R Michael</creatorcontrib><title>The luminous red nova AT 2018bwo in NGC 45 and its binary yellow supergiant progenitor</title><title>arXiv.org</title><description>Luminous Red Novae (LRNe) are astrophysical transients associated with the partial ejection of a binary system's common envelope (CE) shortly before its merger. Here we present the results of our photometric and spectroscopic follow-up campaign of AT2018bwo (DLT18x), a LRN discovered in NGC45, and investigate its progenitor system using binary stellar-evolution models. The transient reached a peak magnitude of \(M_r=-10.97\pm0.11\) and maintained this brightness during its optical plateau of \(t_p = 41\pm5\)days. During this phase, it showed a rather stable photospheric temperature of ~3300K and a luminosity of ~\(10^{40}\)erg/s. The photosphere of AT2018bwo at early times appeared larger and cooler than other similar LRNe, likely due to an extended mass-loss episode before the merger. Towards the end of the plateau, optical spectra showed a reddened continuum with strong molecular absorption bands. The reprocessed emission by the cooling dust was also detected in the mid-infrared bands ~1.5 years after the outburst. Archival Spitzer and Hubble Space Telescope data taken 10-14 years before the transient event suggest a progenitor star with \(T_{prog}\sim 6500\)K, \(R_{prog}\sim 100R_{\odot}\) and \(L_{prog}\sim 2\times10^4L_{\odot}\), and an upper limit for optically thin warm (1000 K) dust mass of \(M_d<10^{-6}M_{\odot}\). Using stellar binary-evolution models, we determined the properties of binary systems consistent with the progenitor parameter space. For AT2018bwo, we infer a primary mass of 12-16 \(M_{\odot}\), which is 9-45% larger than the ~11\(M_{\odot}\) obtained using single-star evolution models. The system, consistent with a yellow-supergiant primary, was likely in a stable mass-transfer regime with -2.4<log (\(\dot{M}/M_{\odot}\)/yr)<-1.2 a decade before the main instability occurred. During the dynamical merger, the system would have ejected 0.15-0.5\(M_{\odot}\) with a velocity of ~500 km/s.</description><subject>Absorption spectra</subject><subject>Astronomical models</subject><subject>Binary stars</subject><subject>Dust</subject><subject>Dynamic stability</subject><subject>Hubble Space Telescope</subject><subject>Luminosity</subject><subject>Molecular absorption</subject><subject>Novae</subject><subject>Photosphere</subject><subject>Physics - Solar and Stellar Astrophysics</subject><subject>Space telescopes</subject><subject>Stellar evolution</subject><subject>Stellar system evolution</subject><subject>Transients (astronomy)</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2022</creationdate><recordtype>article</recordtype><sourceid>BENPR</sourceid><sourceid>GOX</sourceid><recordid>eNotj81OwzAQBi0kJKrSB-DESpxTnPVvjlUFBamCS8Q1clKnuErtYictfXtC4bSX0X4zhNzldM61EPTRxG93nGNOcU6FlHhFJshYnmmOeENmKe0opSgVCsEm5KP8tNANe-fDkCDaDfhwNLAoAWmu61MA5-FttQQuwPgNuD5B7byJZzjbrgsnSMPBxq0zvodDDFvrXR_iLbluTZfs7P9OSfn8VC5fsvX76nW5WGdGoMyYEI3EotEapVHKspZyo7jWoqBNwdBYUTMt21rmomGcM1RIRxBbYfmmsGxK7v_eXqKrQ3T70az6ja8u8SPx8EeMbl-DTX21C0P0o1OF45BSjHHJfgCobVnu</recordid><startdate>20220127</startdate><enddate>20220127</enddate><creator>Blagorodnova, Nadejda</creator><creator>Klencki, Jakub</creator><creator>Pejcha, Ondrej</creator><creator>Vreeswijk, Paul M</creator><creator>Bond, Howard E</creator><creator>Burdge, Kevin B</creator><creator>De, Kishalay</creator><creator>Fremling, Christoffer</creator><creator>Gehrz, Robert D</creator><creator>Jencson, Jacob E</creator><creator>Kasliwal, Mansi M</creator><creator>Kupfer, Thomas</creator><creator>Lau, Ryan M</creator><creator>Masci, Frank J</creator><creator>Rich, R Michael</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>20220127</creationdate><title>The luminous red nova AT 2018bwo in NGC 45 and its binary yellow supergiant progenitor</title><author>Blagorodnova, Nadejda ; Klencki, Jakub ; Pejcha, Ondrej ; Vreeswijk, Paul M ; Bond, Howard E ; Burdge, Kevin B ; De, Kishalay ; Fremling, Christoffer ; Gehrz, Robert D ; Jencson, Jacob E ; Kasliwal, Mansi M ; Kupfer, Thomas ; Lau, Ryan M ; Masci, Frank J ; Rich, R Michael</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a526-355c629c8826a77e3f04a7488590c932ae5b386fb615c34432720a772f5e4d9e3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2022</creationdate><topic>Absorption spectra</topic><topic>Astronomical models</topic><topic>Binary stars</topic><topic>Dust</topic><topic>Dynamic stability</topic><topic>Hubble Space Telescope</topic><topic>Luminosity</topic><topic>Molecular absorption</topic><topic>Novae</topic><topic>Photosphere</topic><topic>Physics - Solar and Stellar Astrophysics</topic><topic>Space telescopes</topic><topic>Stellar evolution</topic><topic>Stellar system evolution</topic><topic>Transients (astronomy)</topic><toplevel>online_resources</toplevel><creatorcontrib>Blagorodnova, Nadejda</creatorcontrib><creatorcontrib>Klencki, Jakub</creatorcontrib><creatorcontrib>Pejcha, Ondrej</creatorcontrib><creatorcontrib>Vreeswijk, Paul M</creatorcontrib><creatorcontrib>Bond, Howard E</creatorcontrib><creatorcontrib>Burdge, Kevin B</creatorcontrib><creatorcontrib>De, Kishalay</creatorcontrib><creatorcontrib>Fremling, Christoffer</creatorcontrib><creatorcontrib>Gehrz, Robert D</creatorcontrib><creatorcontrib>Jencson, Jacob E</creatorcontrib><creatorcontrib>Kasliwal, Mansi M</creatorcontrib><creatorcontrib>Kupfer, Thomas</creatorcontrib><creatorcontrib>Lau, Ryan M</creatorcontrib><creatorcontrib>Masci, Frank J</creatorcontrib><creatorcontrib>Rich, R Michael</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>Blagorodnova, Nadejda</au><au>Klencki, Jakub</au><au>Pejcha, Ondrej</au><au>Vreeswijk, Paul M</au><au>Bond, Howard E</au><au>Burdge, Kevin B</au><au>De, Kishalay</au><au>Fremling, Christoffer</au><au>Gehrz, Robert D</au><au>Jencson, Jacob E</au><au>Kasliwal, Mansi M</au><au>Kupfer, Thomas</au><au>Lau, Ryan M</au><au>Masci, Frank J</au><au>Rich, R Michael</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The luminous red nova AT 2018bwo in NGC 45 and its binary yellow supergiant progenitor</atitle><jtitle>arXiv.org</jtitle><date>2022-01-27</date><risdate>2022</risdate><eissn>2331-8422</eissn><abstract>Luminous Red Novae (LRNe) are astrophysical transients associated with the partial ejection of a binary system's common envelope (CE) shortly before its merger. Here we present the results of our photometric and spectroscopic follow-up campaign of AT2018bwo (DLT18x), a LRN discovered in NGC45, and investigate its progenitor system using binary stellar-evolution models. The transient reached a peak magnitude of \(M_r=-10.97\pm0.11\) and maintained this brightness during its optical plateau of \(t_p = 41\pm5\)days. During this phase, it showed a rather stable photospheric temperature of ~3300K and a luminosity of ~\(10^{40}\)erg/s. The photosphere of AT2018bwo at early times appeared larger and cooler than other similar LRNe, likely due to an extended mass-loss episode before the merger. Towards the end of the plateau, optical spectra showed a reddened continuum with strong molecular absorption bands. The reprocessed emission by the cooling dust was also detected in the mid-infrared bands ~1.5 years after the outburst. Archival Spitzer and Hubble Space Telescope data taken 10-14 years before the transient event suggest a progenitor star with \(T_{prog}\sim 6500\)K, \(R_{prog}\sim 100R_{\odot}\) and \(L_{prog}\sim 2\times10^4L_{\odot}\), and an upper limit for optically thin warm (1000 K) dust mass of \(M_d<10^{-6}M_{\odot}\). Using stellar binary-evolution models, we determined the properties of binary systems consistent with the progenitor parameter space. For AT2018bwo, we infer a primary mass of 12-16 \(M_{\odot}\), which is 9-45% larger than the ~11\(M_{\odot}\) obtained using single-star evolution models. The system, consistent with a yellow-supergiant primary, was likely in a stable mass-transfer regime with -2.4<log (\(\dot{M}/M_{\odot}\)/yr)<-1.2 a decade before the main instability occurred. During the dynamical merger, the system would have ejected 0.15-0.5\(M_{\odot}\) with a velocity of ~500 km/s.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.2102.05662</doi><oa>free_for_read</oa></addata></record> |
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| subjects | Absorption spectra Astronomical models Binary stars Dust Dynamic stability Hubble Space Telescope Luminosity Molecular absorption Novae Photosphere Physics - Solar and Stellar Astrophysics Space telescopes Stellar evolution Stellar system evolution Transients (astronomy) |
| title | The luminous red nova AT 2018bwo in NGC 45 and its binary yellow supergiant progenitor |
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