Eintrag weiter verarbeiten
Limits on stable iron in Type Ia supernovae from near-infrared spectroscopy
Gespeichert in:
| Zeitschriftentitel: | Astronomy & Astrophysics |
|---|---|
| Personen und Körperschaften: | , , , , , |
| In: | Astronomy & Astrophysics, 620, 2018, S. A200 |
| Format: | E-Article |
| Sprache: | Unbestimmt |
| veröffentlicht: |
EDP Sciences
|
| Schlagwörter: |
| author_facet |
Flörs, A. Spyromilio, J. Maguire, K. Taubenberger, S. Kerzendorf, W. E. Dhawan, S. Flörs, A. Spyromilio, J. Maguire, K. Taubenberger, S. Kerzendorf, W. E. Dhawan, S. |
|---|---|
| author |
Flörs, A. Spyromilio, J. Maguire, K. Taubenberger, S. Kerzendorf, W. E. Dhawan, S. |
| spellingShingle |
Flörs, A. Spyromilio, J. Maguire, K. Taubenberger, S. Kerzendorf, W. E. Dhawan, S. Astronomy & Astrophysics Limits on stable iron in Type Ia supernovae from near-infrared spectroscopy Space and Planetary Science Astronomy and Astrophysics |
| author_sort |
flörs, a. |
| spelling |
Flörs, A. Spyromilio, J. Maguire, K. Taubenberger, S. Kerzendorf, W. E. Dhawan, S. 0004-6361 1432-0746 EDP Sciences Space and Planetary Science Astronomy and Astrophysics http://dx.doi.org/10.1051/0004-6361/201833512 <jats:p>We obtained optical and near infrared spectra of Type Ia supernovae (SNe Ia) at epochs ranging from 224 to 496 days after the explosion. The spectra show emission lines from forbidden transitions of singly ionised iron and cobalt atoms. We used non-local thermodynamic equilibrium (NLTE) modelling of the first and second ionisation stages of iron, nickel, and cobalt to fit the spectra using a sampling algorithm allowing us to probe a broad parameter space. We derive velocity shifts, line widths, and abundance ratios for iron and cobalt. The measured line widths and velocity shifts of the singly ionised ions suggest a shared emitting region. Our data are fully compatible with radioactive <jats:sup>56</jats:sup>Ni decay as the origin for cobalt and iron. We compare the measured abundance ratios of iron and cobalt to theoretical predictions of various SN Ia explosion models. These models include, in addition to <jats:sup>56</jats:sup>Ni, different amounts of <jats:sup>57</jats:sup>Ni and stable <jats:sup>54,56</jats:sup>Fe. We can exclude models that produced only <jats:sup>54,56</jats:sup>Fe or only <jats:sup>57</jats:sup>Ni in addition to <jats:sup>56</jats:sup>Ni. If we consider a model that has <jats:sup>56</jats:sup>Ni, <jats:sup>57</jats:sup>Ni, and <jats:sup>54,56</jats:sup>Fe then our data imply that these ratios are <jats:sup>54,56</jats:sup>Fe / <jats:sup>56</jats:sup>Ni = 0.272 ± 0.086 and <jats:sup>57</jats:sup>Ni / <jats:sup>56</jats:sup>Ni = 0.032 ± 0.011.</jats:p> Limits on stable iron in Type Ia supernovae from near-infrared spectroscopy Astronomy & Astrophysics |
| doi_str_mv |
10.1051/0004-6361/201833512 |
| facet_avail |
Online Free |
| finc_class_facet |
Physik Technik |
| format |
ElectronicArticle |
| fullrecord |
blob:ai-49-aHR0cDovL2R4LmRvaS5vcmcvMTAuMTA1MS8wMDA0LTYzNjEvMjAxODMzNTEy |
| id |
ai-49-aHR0cDovL2R4LmRvaS5vcmcvMTAuMTA1MS8wMDA0LTYzNjEvMjAxODMzNTEy |
| institution |
DE-105 DE-14 DE-Ch1 DE-L229 DE-D275 DE-Bn3 DE-Brt1 DE-Zwi2 DE-D161 DE-Gla1 DE-Zi4 DE-15 DE-Pl11 DE-Rs1 |
| imprint |
EDP Sciences, 2018 |
| imprint_str_mv |
EDP Sciences, 2018 |
| issn |
1432-0746 0004-6361 |
| issn_str_mv |
1432-0746 0004-6361 |
| language |
Undetermined |
| mega_collection |
EDP Sciences (CrossRef) |
| match_str |
flors2018limitsonstableironintypeiasupernovaefromnearinfraredspectroscopy |
| publishDateSort |
2018 |
| publisher |
EDP Sciences |
| recordtype |
ai |
| record_format |
ai |
| series |
Astronomy & Astrophysics |
| source_id |
49 |
| title |
Limits on stable iron in Type Ia supernovae from near-infrared spectroscopy |
| title_unstemmed |
Limits on stable iron in Type Ia supernovae from near-infrared spectroscopy |
| title_full |
Limits on stable iron in Type Ia supernovae from near-infrared spectroscopy |
| title_fullStr |
Limits on stable iron in Type Ia supernovae from near-infrared spectroscopy |
| title_full_unstemmed |
Limits on stable iron in Type Ia supernovae from near-infrared spectroscopy |
| title_short |
Limits on stable iron in Type Ia supernovae from near-infrared spectroscopy |
| title_sort |
limits on stable iron in type ia supernovae from near-infrared spectroscopy |
| topic |
Space and Planetary Science Astronomy and Astrophysics |
| url |
http://dx.doi.org/10.1051/0004-6361/201833512 |
| publishDate |
2018 |
| physical |
A200 |
| description |
<jats:p>We obtained optical and near infrared spectra of Type Ia supernovae (SNe Ia) at epochs ranging from 224 to 496 days after the explosion. The spectra show emission lines from forbidden transitions of singly ionised iron and cobalt atoms. We used non-local thermodynamic equilibrium (NLTE) modelling of the first and second ionisation stages of iron, nickel, and cobalt to fit the spectra using a sampling algorithm allowing us to probe a broad parameter space. We derive velocity shifts, line widths, and abundance ratios for iron and cobalt. The measured line widths and velocity shifts of the singly ionised ions suggest a shared emitting region. Our data are fully compatible with radioactive <jats:sup>56</jats:sup>Ni decay as the origin for cobalt and iron. We compare the measured abundance ratios of iron and cobalt to theoretical predictions of various SN Ia explosion models. These models include, in addition to <jats:sup>56</jats:sup>Ni, different amounts of <jats:sup>57</jats:sup>Ni and stable <jats:sup>54,56</jats:sup>Fe. We can exclude models that produced only <jats:sup>54,56</jats:sup>Fe or only <jats:sup>57</jats:sup>Ni in addition to <jats:sup>56</jats:sup>Ni. If we consider a model that has <jats:sup>56</jats:sup>Ni, <jats:sup>57</jats:sup>Ni, and <jats:sup>54,56</jats:sup>Fe then our data imply that these ratios are <jats:sup>54,56</jats:sup>Fe / <jats:sup>56</jats:sup>Ni = 0.272 ± 0.086 and <jats:sup>57</jats:sup>Ni / <jats:sup>56</jats:sup>Ni = 0.032 ± 0.011.</jats:p> |
| container_start_page |
0 |
| container_title |
Astronomy & Astrophysics |
| container_volume |
620 |
| format_de105 |
Article, E-Article |
| format_de14 |
Article, E-Article |
| format_de15 |
Article, E-Article |
| format_de520 |
Article, E-Article |
| format_de540 |
Article, E-Article |
| format_dech1 |
Article, E-Article |
| format_ded117 |
Article, E-Article |
| format_degla1 |
E-Article |
| format_del152 |
Buch |
| format_del189 |
Article, E-Article |
| format_dezi4 |
Article |
| format_dezwi2 |
Article, E-Article |
| format_finc |
Article, E-Article |
| format_nrw |
Article, E-Article |
| _version_ |
1792343407536898060 |
| geogr_code |
not assigned |
| last_indexed |
2024-03-01T16:51:13.04Z |
| geogr_code_person |
not assigned |
| openURL |
url_ver=Z39.88-2004&ctx_ver=Z39.88-2004&ctx_enc=info%3Aofi%2Fenc%3AUTF-8&rfr_id=info%3Asid%2Fvufind.svn.sourceforge.net%3Agenerator&rft.title=Limits+on+stable+iron+in+Type+Ia+supernovae+from+near-infrared+spectroscopy&rft.date=2018-12-01&genre=article&issn=1432-0746&volume=620&pages=A200&jtitle=Astronomy+%26+Astrophysics&atitle=Limits+on+stable+iron+in+Type+Ia+supernovae+from+near-infrared+spectroscopy&aulast=Dhawan&aufirst=S.&rft_id=info%3Adoi%2F10.1051%2F0004-6361%2F201833512&rft.language%5B0%5D=und |
| SOLR | |
| _version_ | 1792343407536898060 |
| author | Flörs, A., Spyromilio, J., Maguire, K., Taubenberger, S., Kerzendorf, W. E., Dhawan, S. |
| author_facet | Flörs, A., Spyromilio, J., Maguire, K., Taubenberger, S., Kerzendorf, W. E., Dhawan, S., Flörs, A., Spyromilio, J., Maguire, K., Taubenberger, S., Kerzendorf, W. E., Dhawan, S. |
| author_sort | flörs, a. |
| container_start_page | 0 |
| container_title | Astronomy & Astrophysics |
| container_volume | 620 |
| description | <jats:p>We obtained optical and near infrared spectra of Type Ia supernovae (SNe Ia) at epochs ranging from 224 to 496 days after the explosion. The spectra show emission lines from forbidden transitions of singly ionised iron and cobalt atoms. We used non-local thermodynamic equilibrium (NLTE) modelling of the first and second ionisation stages of iron, nickel, and cobalt to fit the spectra using a sampling algorithm allowing us to probe a broad parameter space. We derive velocity shifts, line widths, and abundance ratios for iron and cobalt. The measured line widths and velocity shifts of the singly ionised ions suggest a shared emitting region. Our data are fully compatible with radioactive <jats:sup>56</jats:sup>Ni decay as the origin for cobalt and iron. We compare the measured abundance ratios of iron and cobalt to theoretical predictions of various SN Ia explosion models. These models include, in addition to <jats:sup>56</jats:sup>Ni, different amounts of <jats:sup>57</jats:sup>Ni and stable <jats:sup>54,56</jats:sup>Fe. We can exclude models that produced only <jats:sup>54,56</jats:sup>Fe or only <jats:sup>57</jats:sup>Ni in addition to <jats:sup>56</jats:sup>Ni. If we consider a model that has <jats:sup>56</jats:sup>Ni, <jats:sup>57</jats:sup>Ni, and <jats:sup>54,56</jats:sup>Fe then our data imply that these ratios are <jats:sup>54,56</jats:sup>Fe / <jats:sup>56</jats:sup>Ni = 0.272 ± 0.086 and <jats:sup>57</jats:sup>Ni / <jats:sup>56</jats:sup>Ni = 0.032 ± 0.011.</jats:p> |
| doi_str_mv | 10.1051/0004-6361/201833512 |
| facet_avail | Online, Free |
| finc_class_facet | Physik, Technik |
| format | ElectronicArticle |
| format_de105 | Article, E-Article |
| format_de14 | Article, E-Article |
| format_de15 | Article, E-Article |
| format_de520 | Article, E-Article |
| format_de540 | Article, E-Article |
| format_dech1 | Article, E-Article |
| format_ded117 | Article, E-Article |
| format_degla1 | E-Article |
| format_del152 | Buch |
| format_del189 | Article, E-Article |
| format_dezi4 | Article |
| format_dezwi2 | Article, E-Article |
| format_finc | Article, E-Article |
| format_nrw | Article, E-Article |
| geogr_code | not assigned |
| geogr_code_person | not assigned |
| id | ai-49-aHR0cDovL2R4LmRvaS5vcmcvMTAuMTA1MS8wMDA0LTYzNjEvMjAxODMzNTEy |
| imprint | EDP Sciences, 2018 |
| imprint_str_mv | EDP Sciences, 2018 |
| institution | DE-105, DE-14, DE-Ch1, DE-L229, DE-D275, DE-Bn3, DE-Brt1, DE-Zwi2, DE-D161, DE-Gla1, DE-Zi4, DE-15, DE-Pl11, DE-Rs1 |
| issn | 1432-0746, 0004-6361 |
| issn_str_mv | 1432-0746, 0004-6361 |
| language | Undetermined |
| last_indexed | 2024-03-01T16:51:13.04Z |
| match_str | flors2018limitsonstableironintypeiasupernovaefromnearinfraredspectroscopy |
| mega_collection | EDP Sciences (CrossRef) |
| physical | A200 |
| publishDate | 2018 |
| publishDateSort | 2018 |
| publisher | EDP Sciences |
| record_format | ai |
| recordtype | ai |
| series | Astronomy & Astrophysics |
| source_id | 49 |
| spelling | Flörs, A. Spyromilio, J. Maguire, K. Taubenberger, S. Kerzendorf, W. E. Dhawan, S. 0004-6361 1432-0746 EDP Sciences Space and Planetary Science Astronomy and Astrophysics http://dx.doi.org/10.1051/0004-6361/201833512 <jats:p>We obtained optical and near infrared spectra of Type Ia supernovae (SNe Ia) at epochs ranging from 224 to 496 days after the explosion. The spectra show emission lines from forbidden transitions of singly ionised iron and cobalt atoms. We used non-local thermodynamic equilibrium (NLTE) modelling of the first and second ionisation stages of iron, nickel, and cobalt to fit the spectra using a sampling algorithm allowing us to probe a broad parameter space. We derive velocity shifts, line widths, and abundance ratios for iron and cobalt. The measured line widths and velocity shifts of the singly ionised ions suggest a shared emitting region. Our data are fully compatible with radioactive <jats:sup>56</jats:sup>Ni decay as the origin for cobalt and iron. We compare the measured abundance ratios of iron and cobalt to theoretical predictions of various SN Ia explosion models. These models include, in addition to <jats:sup>56</jats:sup>Ni, different amounts of <jats:sup>57</jats:sup>Ni and stable <jats:sup>54,56</jats:sup>Fe. We can exclude models that produced only <jats:sup>54,56</jats:sup>Fe or only <jats:sup>57</jats:sup>Ni in addition to <jats:sup>56</jats:sup>Ni. If we consider a model that has <jats:sup>56</jats:sup>Ni, <jats:sup>57</jats:sup>Ni, and <jats:sup>54,56</jats:sup>Fe then our data imply that these ratios are <jats:sup>54,56</jats:sup>Fe / <jats:sup>56</jats:sup>Ni = 0.272 ± 0.086 and <jats:sup>57</jats:sup>Ni / <jats:sup>56</jats:sup>Ni = 0.032 ± 0.011.</jats:p> Limits on stable iron in Type Ia supernovae from near-infrared spectroscopy Astronomy & Astrophysics |
| spellingShingle | Flörs, A., Spyromilio, J., Maguire, K., Taubenberger, S., Kerzendorf, W. E., Dhawan, S., Astronomy & Astrophysics, Limits on stable iron in Type Ia supernovae from near-infrared spectroscopy, Space and Planetary Science, Astronomy and Astrophysics |
| title | Limits on stable iron in Type Ia supernovae from near-infrared spectroscopy |
| title_full | Limits on stable iron in Type Ia supernovae from near-infrared spectroscopy |
| title_fullStr | Limits on stable iron in Type Ia supernovae from near-infrared spectroscopy |
| title_full_unstemmed | Limits on stable iron in Type Ia supernovae from near-infrared spectroscopy |
| title_short | Limits on stable iron in Type Ia supernovae from near-infrared spectroscopy |
| title_sort | limits on stable iron in type ia supernovae from near-infrared spectroscopy |
| title_unstemmed | Limits on stable iron in Type Ia supernovae from near-infrared spectroscopy |
| topic | Space and Planetary Science, Astronomy and Astrophysics |
| url | http://dx.doi.org/10.1051/0004-6361/201833512 |