SN 2019ehk: A Double-Peaked Ca-rich Transient with Luminous X-ray Emission and Shock-Ionized Spectral Features
We present panchromatic observations and modeling of the Calcium-rich supernova 2019ehk in the star-forming galaxy M100 (d\(\approx\)16.2 Mpc) starting 10 hours after explosion and continuing for ~300 days. SN 2019ehk shows a double-peaked optical light curve peaking at \(t = 3\) and \(15\) days. Th...
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| creator | Jacobson-Galán, Wynn V Margutti, Raffaella Kilpatrick, Charles D Hiramatsu, Daichi Perets, Hagai Khatami, David Foley, Ryan J Raymond, John Sung-Chul Yoon Bobrick, Alexey Zenati, Yossef Galbany, Lluís Andrews, Jennifer Brown, Peter J Cartier, Régis Coppejans, Deanne L Dimitriadis, Georgios Dobson, Matthew Hajela, Aprajita Howell, D Andrew Kuncarayakti, Hanindyo Milisavljevic, Danny Rahman, Mohammed Rojas-Bravo, César Sand, David J Shepherd, Joel Smartt, Stephen J Holland, Stacey Stroh, Michael Swift, Jonathan J Terreran, Giacomo Vinko, Jozsef Wang, Xiaofeng Anderson, Joseph P Baron, Edward A Berger, Edo Blanchard, Peter K Burke, Jamison Coulter, David A DeMarchi, Lindsay DerKacy, James M Fremling, Christoffer Gomez, Sebastian Gromadzki, Mariusz Griffin Hosseinzadeh Kasen, Daniel Kriskovics, Levente McCully, Curtis Müller-Bravo, Tomás E Nicholl, Matt Ordasi, András Pellegrino, Craig Piro, Anthony L Pál, András Ren, Juanjuan Rest, Armin Rich, R Michael Hanna, Sai Sárneczky, Krisztián Shen, Ken J Short, Philip Siebert, Matthew Stauffer, Candice Szakáts, Róbert Zhang, Xinhan Zhang, Jujia Zhang, Kaicheng |
| description | We present panchromatic observations and modeling of the Calcium-rich supernova 2019ehk in the star-forming galaxy M100 (d\(\approx\)16.2 Mpc) starting 10 hours after explosion and continuing for ~300 days. SN 2019ehk shows a double-peaked optical light curve peaking at \(t = 3\) and \(15\) days. The first peak is coincident with luminous, rapidly decaying \(\textit{Swift}\)-XRT discovered X-ray emission (\(L_x\approx10^{41}~\rm{erg~s^{-1}}\) at 3 days; \(L_x \propto t^{-3}\)), and a Shane/Kast spectral detection of narrow H\(\alpha\) and He II emission lines (\(v \approx 500\) km/s) originating from pre-existent circumstellar material. We attribute this phenomenology to radiation from shock interaction with extended, dense material surrounding the progenitor star at \(r |
| doi_str_mv | 10.48550/arxiv.2005.01782 |
| format | Article |
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SN 2019ehk shows a double-peaked optical light curve peaking at \(t = 3\) and \(15\) days. The first peak is coincident with luminous, rapidly decaying \(\textit{Swift}\)-XRT discovered X-ray emission (\(L_x\approx10^{41}~\rm{erg~s^{-1}}\) at 3 days; \(L_x \propto t^{-3}\)), and a Shane/Kast spectral detection of narrow H\(\alpha\) and He II emission lines (\(v \approx 500\) km/s) originating from pre-existent circumstellar material. We attribute this phenomenology to radiation from shock interaction with extended, dense material surrounding the progenitor star at \(r<10^{15}\) cm and the resulting cooling emission. We calculate a total CSM mass of \(\sim\) \(7\times10^{-3}\) \(\rm{M_{\odot}}\) with particle density \(n\approx10^{9}\,\rm{cm^{-3}}\). Radio observations indicate a significantly lower density \(n < 10^{4}\,\rm{cm^{-3}}\) at larger radii. The photometric and spectroscopic properties during the second light curve peak are consistent with those of Ca-rich transients (rise-time of \(t_r =13.4\pm0.210\) days and a peak B-band magnitude of \(M_B =-15.1\pm0.200\) mag). We find that SN 2019ehk synthesized \((3.1\pm0.11)\times10^{-2} ~ \rm{M_{\odot}}\) of \({}^{56}\textrm{Ni}\) and ejected \(M_{\rm ej} = (0.72\pm 0.040)~\rm{M_{\odot}}\) total with a kinetic energy \(E_{\rm k}=(1.8\pm0.10)\times10^{50}~\rm{erg}\). Finally, deep \(\textit{HST}\) pre-explosion imaging at the SN site constrains the parameter space of viable stellar progenitors to massive stars in the lowest mass bin (~10 \(\rm{M_{\odot}}\)) in binaries that lost most of their He envelope or white dwarfs. The explosion and environment properties of SN 2019ehk further restrict the potential WD progenitor systems to low-mass hybrid HeCO WD + CO WD binaries.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.2005.01782</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Astronomical models ; Explosions ; Galaxies ; Hybrid systems ; Kinetic energy ; Light curve ; Massive stars ; Particle density (concentration) ; Phenomenology ; Physics - High Energy Astrophysical Phenomena ; Physics - Solar and Stellar Astrophysics ; Radio astronomy ; Radio observation ; Star formation ; White dwarf stars</subject><ispartof>arXiv.org, 2020-07</ispartof><rights>2020. 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>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,776,780,881,27904</link.rule.ids><backlink>$$Uhttps://doi.org/10.48550/arXiv.2005.01782$$DView paper in arXiv$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.3847/1538-4357/ab9e66$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink></links><search><creatorcontrib>Jacobson-Galán, Wynn V</creatorcontrib><creatorcontrib>Margutti, Raffaella</creatorcontrib><creatorcontrib>Kilpatrick, Charles D</creatorcontrib><creatorcontrib>Hiramatsu, Daichi</creatorcontrib><creatorcontrib>Perets, Hagai</creatorcontrib><creatorcontrib>Khatami, David</creatorcontrib><creatorcontrib>Foley, Ryan J</creatorcontrib><creatorcontrib>Raymond, John</creatorcontrib><creatorcontrib>Sung-Chul Yoon</creatorcontrib><creatorcontrib>Bobrick, Alexey</creatorcontrib><creatorcontrib>Zenati, Yossef</creatorcontrib><creatorcontrib>Galbany, Lluís</creatorcontrib><creatorcontrib>Andrews, Jennifer</creatorcontrib><creatorcontrib>Brown, Peter J</creatorcontrib><creatorcontrib>Cartier, Régis</creatorcontrib><creatorcontrib>Coppejans, Deanne L</creatorcontrib><creatorcontrib>Dimitriadis, Georgios</creatorcontrib><creatorcontrib>Dobson, Matthew</creatorcontrib><creatorcontrib>Hajela, Aprajita</creatorcontrib><creatorcontrib>Howell, D Andrew</creatorcontrib><creatorcontrib>Kuncarayakti, Hanindyo</creatorcontrib><creatorcontrib>Milisavljevic, Danny</creatorcontrib><creatorcontrib>Rahman, Mohammed</creatorcontrib><creatorcontrib>Rojas-Bravo, César</creatorcontrib><creatorcontrib>Sand, David J</creatorcontrib><creatorcontrib>Shepherd, Joel</creatorcontrib><creatorcontrib>Smartt, Stephen J</creatorcontrib><creatorcontrib>Holland, Stacey</creatorcontrib><creatorcontrib>Stroh, Michael</creatorcontrib><creatorcontrib>Swift, Jonathan J</creatorcontrib><creatorcontrib>Terreran, Giacomo</creatorcontrib><creatorcontrib>Vinko, Jozsef</creatorcontrib><creatorcontrib>Wang, Xiaofeng</creatorcontrib><creatorcontrib>Anderson, Joseph P</creatorcontrib><creatorcontrib>Baron, Edward A</creatorcontrib><creatorcontrib>Berger, Edo</creatorcontrib><creatorcontrib>Blanchard, Peter K</creatorcontrib><creatorcontrib>Burke, Jamison</creatorcontrib><creatorcontrib>Coulter, David A</creatorcontrib><creatorcontrib>DeMarchi, Lindsay</creatorcontrib><creatorcontrib>DerKacy, James M</creatorcontrib><creatorcontrib>Fremling, Christoffer</creatorcontrib><creatorcontrib>Gomez, Sebastian</creatorcontrib><creatorcontrib>Gromadzki, Mariusz</creatorcontrib><creatorcontrib>Griffin Hosseinzadeh</creatorcontrib><creatorcontrib>Kasen, Daniel</creatorcontrib><creatorcontrib>Kriskovics, Levente</creatorcontrib><creatorcontrib>McCully, Curtis</creatorcontrib><creatorcontrib>Müller-Bravo, Tomás E</creatorcontrib><creatorcontrib>Nicholl, Matt</creatorcontrib><creatorcontrib>Ordasi, András</creatorcontrib><creatorcontrib>Pellegrino, Craig</creatorcontrib><creatorcontrib>Piro, Anthony L</creatorcontrib><creatorcontrib>Pál, András</creatorcontrib><creatorcontrib>Ren, Juanjuan</creatorcontrib><creatorcontrib>Rest, Armin</creatorcontrib><creatorcontrib>Rich, R Michael</creatorcontrib><creatorcontrib>Hanna, Sai</creatorcontrib><creatorcontrib>Sárneczky, Krisztián</creatorcontrib><creatorcontrib>Shen, Ken J</creatorcontrib><creatorcontrib>Short, Philip</creatorcontrib><creatorcontrib>Siebert, Matthew</creatorcontrib><creatorcontrib>Stauffer, Candice</creatorcontrib><creatorcontrib>Szakáts, Róbert</creatorcontrib><creatorcontrib>Zhang, Xinhan</creatorcontrib><creatorcontrib>Zhang, Jujia</creatorcontrib><creatorcontrib>Zhang, Kaicheng</creatorcontrib><title>SN 2019ehk: A Double-Peaked Ca-rich Transient with Luminous X-ray Emission and Shock-Ionized Spectral Features</title><title>arXiv.org</title><description>We present panchromatic observations and modeling of the Calcium-rich supernova 2019ehk in the star-forming galaxy M100 (d\(\approx\)16.2 Mpc) starting 10 hours after explosion and continuing for ~300 days. SN 2019ehk shows a double-peaked optical light curve peaking at \(t = 3\) and \(15\) days. The first peak is coincident with luminous, rapidly decaying \(\textit{Swift}\)-XRT discovered X-ray emission (\(L_x\approx10^{41}~\rm{erg~s^{-1}}\) at 3 days; \(L_x \propto t^{-3}\)), and a Shane/Kast spectral detection of narrow H\(\alpha\) and He II emission lines (\(v \approx 500\) km/s) originating from pre-existent circumstellar material. We attribute this phenomenology to radiation from shock interaction with extended, dense material surrounding the progenitor star at \(r<10^{15}\) cm and the resulting cooling emission. We calculate a total CSM mass of \(\sim\) \(7\times10^{-3}\) \(\rm{M_{\odot}}\) with particle density \(n\approx10^{9}\,\rm{cm^{-3}}\). Radio observations indicate a significantly lower density \(n < 10^{4}\,\rm{cm^{-3}}\) at larger radii. The photometric and spectroscopic properties during the second light curve peak are consistent with those of Ca-rich transients (rise-time of \(t_r =13.4\pm0.210\) days and a peak B-band magnitude of \(M_B =-15.1\pm0.200\) mag). We find that SN 2019ehk synthesized \((3.1\pm0.11)\times10^{-2} ~ \rm{M_{\odot}}\) of \({}^{56}\textrm{Ni}\) and ejected \(M_{\rm ej} = (0.72\pm 0.040)~\rm{M_{\odot}}\) total with a kinetic energy \(E_{\rm k}=(1.8\pm0.10)\times10^{50}~\rm{erg}\). Finally, deep \(\textit{HST}\) pre-explosion imaging at the SN site constrains the parameter space of viable stellar progenitors to massive stars in the lowest mass bin (~10 \(\rm{M_{\odot}}\)) in binaries that lost most of their He envelope or white dwarfs. The explosion and environment properties of SN 2019ehk further restrict the potential WD progenitor systems to low-mass hybrid HeCO WD + CO WD binaries.</description><subject>Astronomical models</subject><subject>Explosions</subject><subject>Galaxies</subject><subject>Hybrid systems</subject><subject>Kinetic energy</subject><subject>Light curve</subject><subject>Massive stars</subject><subject>Particle density (concentration)</subject><subject>Phenomenology</subject><subject>Physics - High Energy Astrophysical Phenomena</subject><subject>Physics - Solar and Stellar Astrophysics</subject><subject>Radio astronomy</subject><subject>Radio observation</subject><subject>Star formation</subject><subject>White dwarf 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Alexey ; Zenati, Yossef ; Galbany, Lluís ; Andrews, Jennifer ; Brown, Peter J ; Cartier, Régis ; Coppejans, Deanne L ; Dimitriadis, Georgios ; Dobson, Matthew ; Hajela, Aprajita ; Howell, D Andrew ; Kuncarayakti, Hanindyo ; Milisavljevic, Danny ; Rahman, Mohammed ; Rojas-Bravo, César ; Sand, David J ; Shepherd, Joel ; Smartt, Stephen J ; Holland, Stacey ; Stroh, Michael ; Swift, Jonathan J ; Terreran, Giacomo ; Vinko, Jozsef ; Wang, Xiaofeng ; Anderson, Joseph P ; Baron, Edward A ; Berger, Edo ; Blanchard, Peter K ; Burke, Jamison ; Coulter, David A ; DeMarchi, Lindsay ; DerKacy, James M ; Fremling, Christoffer ; Gomez, Sebastian ; Gromadzki, Mariusz ; Griffin Hosseinzadeh ; Kasen, Daniel ; Kriskovics, Levente ; McCully, Curtis ; Müller-Bravo, Tomás E ; Nicholl, Matt ; Ordasi, András ; Pellegrino, Craig ; Piro, Anthony L ; Pál, András ; Ren, Juanjuan ; Rest, Armin ; Rich, R Michael ; Hanna, Sai ; Sárneczky, Krisztián ; Shen, Ken J ; Short, Philip ; Siebert, Matthew ; Stauffer, Candice 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Matthew</creatorcontrib><creatorcontrib>Stauffer, Candice</creatorcontrib><creatorcontrib>Szakáts, Róbert</creatorcontrib><creatorcontrib>Zhang, Xinhan</creatorcontrib><creatorcontrib>Zhang, Jujia</creatorcontrib><creatorcontrib>Zhang, Kaicheng</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>Jacobson-Galán, Wynn V</au><au>Margutti, Raffaella</au><au>Kilpatrick, Charles D</au><au>Hiramatsu, Daichi</au><au>Perets, Hagai</au><au>Khatami, David</au><au>Foley, Ryan J</au><au>Raymond, John</au><au>Sung-Chul Yoon</au><au>Bobrick, Alexey</au><au>Zenati, Yossef</au><au>Galbany, Lluís</au><au>Andrews, Jennifer</au><au>Brown, Peter J</au><au>Cartier, Régis</au><au>Coppejans, Deanne L</au><au>Dimitriadis, Georgios</au><au>Dobson, Matthew</au><au>Hajela, Aprajita</au><au>Howell, D Andrew</au><au>Kuncarayakti, Hanindyo</au><au>Milisavljevic, Danny</au><au>Rahman, Mohammed</au><au>Rojas-Bravo, César</au><au>Sand, David J</au><au>Shepherd, Joel</au><au>Smartt, Stephen J</au><au>Holland, Stacey</au><au>Stroh, Michael</au><au>Swift, Jonathan J</au><au>Terreran, Giacomo</au><au>Vinko, Jozsef</au><au>Wang, Xiaofeng</au><au>Anderson, Joseph P</au><au>Baron, Edward A</au><au>Berger, Edo</au><au>Blanchard, Peter K</au><au>Burke, Jamison</au><au>Coulter, David A</au><au>DeMarchi, Lindsay</au><au>DerKacy, James M</au><au>Fremling, Christoffer</au><au>Gomez, Sebastian</au><au>Gromadzki, Mariusz</au><au>Griffin Hosseinzadeh</au><au>Kasen, Daniel</au><au>Kriskovics, Levente</au><au>McCully, Curtis</au><au>Müller-Bravo, Tomás E</au><au>Nicholl, Matt</au><au>Ordasi, András</au><au>Pellegrino, Craig</au><au>Piro, Anthony L</au><au>Pál, András</au><au>Ren, Juanjuan</au><au>Rest, Armin</au><au>Rich, R Michael</au><au>Hanna, Sai</au><au>Sárneczky, Krisztián</au><au>Shen, Ken J</au><au>Short, Philip</au><au>Siebert, Matthew</au><au>Stauffer, Candice</au><au>Szakáts, Róbert</au><au>Zhang, Xinhan</au><au>Zhang, Jujia</au><au>Zhang, Kaicheng</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>SN 2019ehk: A Double-Peaked Ca-rich Transient with Luminous X-ray Emission and Shock-Ionized Spectral Features</atitle><jtitle>arXiv.org</jtitle><date>2020-07-01</date><risdate>2020</risdate><eissn>2331-8422</eissn><abstract>We present panchromatic observations and modeling of the Calcium-rich supernova 2019ehk in the star-forming galaxy M100 (d\(\approx\)16.2 Mpc) starting 10 hours after explosion and continuing for ~300 days. SN 2019ehk shows a double-peaked optical light curve peaking at \(t = 3\) and \(15\) days. The first peak is coincident with luminous, rapidly decaying \(\textit{Swift}\)-XRT discovered X-ray emission (\(L_x\approx10^{41}~\rm{erg~s^{-1}}\) at 3 days; \(L_x \propto t^{-3}\)), and a Shane/Kast spectral detection of narrow H\(\alpha\) and He II emission lines (\(v \approx 500\) km/s) originating from pre-existent circumstellar material. We attribute this phenomenology to radiation from shock interaction with extended, dense material surrounding the progenitor star at \(r<10^{15}\) cm and the resulting cooling emission. We calculate a total CSM mass of \(\sim\) \(7\times10^{-3}\) \(\rm{M_{\odot}}\) with particle density \(n\approx10^{9}\,\rm{cm^{-3}}\). Radio observations indicate a significantly lower density \(n < 10^{4}\,\rm{cm^{-3}}\) at larger radii. The photometric and spectroscopic properties during the second light curve peak are consistent with those of Ca-rich transients (rise-time of \(t_r =13.4\pm0.210\) days and a peak B-band magnitude of \(M_B =-15.1\pm0.200\) mag). We find that SN 2019ehk synthesized \((3.1\pm0.11)\times10^{-2} ~ \rm{M_{\odot}}\) of \({}^{56}\textrm{Ni}\) and ejected \(M_{\rm ej} = (0.72\pm 0.040)~\rm{M_{\odot}}\) total with a kinetic energy \(E_{\rm k}=(1.8\pm0.10)\times10^{50}~\rm{erg}\). Finally, deep \(\textit{HST}\) pre-explosion imaging at the SN site constrains the parameter space of viable stellar progenitors to massive stars in the lowest mass bin (~10 \(\rm{M_{\odot}}\)) in binaries that lost most of their He envelope or white dwarfs. The explosion and environment properties of SN 2019ehk further restrict the potential WD progenitor systems to low-mass hybrid HeCO WD + CO WD binaries.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.2005.01782</doi><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | EISSN: 2331-8422 |
| ispartof | arXiv.org, 2020-07 |
| issn | 2331-8422 |
| language | eng |
| recordid | cdi_arxiv_primary_2005_01782 |
| source | arXiv.org; Free E- Journals |
| subjects | Astronomical models Explosions Galaxies Hybrid systems Kinetic energy Light curve Massive stars Particle density (concentration) Phenomenology Physics - High Energy Astrophysical Phenomena Physics - Solar and Stellar Astrophysics Radio astronomy Radio observation Star formation White dwarf stars |
| title | SN 2019ehk: A Double-Peaked Ca-rich Transient with Luminous X-ray Emission and Shock-Ionized Spectral Features |
| url | https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-01-25T19%3A51%3A53IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest_arxiv&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=SN%202019ehk:%20A%20Double-Peaked%20Ca-rich%20Transient%20with%20Luminous%20X-ray%20Emission%20and%20Shock-Ionized%20Spectral%20Features&rft.jtitle=arXiv.org&rft.au=Jacobson-Gal%C3%A1n,%20Wynn%20V&rft.date=2020-07-01&rft.eissn=2331-8422&rft_id=info:doi/10.48550/arxiv.2005.01782&rft_dat=%3Cproquest_arxiv%3E2399015881%3C/proquest_arxiv%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_pqid=2399015881&rft_id=info:pmid/&rfr_iscdi=true |