Resumen
SN 2013dy is a Type Ia supernova (SN Ia) for which we have compiled an extraordinary data set spanning from 0.1 to ~ 500 d after explosion. We present 10 epochs of ultraviolet (UV) through near-infrared (NIR) spectra with Hubble Space Telescope/Space Telescope Imaging Spectrograph, 47 epochs of optical spectra (15 of them having high resolution), and more than 500 photometric observations in the BVrRiIZYJH bands. SN 2013dy has a broad and slowly declining light curve (Δm15(B)=0.92 mag), shallow Si II λ6355 absorption, and a low velocity gradient. We detect strong C II in our earliest spectra, probing unburned progenitor material in the outermost layers of the SN ejecta, but this feature fades within a few days. The UV continuum of SN 2013dy, which is strongly affected by the metal abundance of the progenitor star, suggests that SN 2013dy had a relatively high-metallicity progenitor. Examining one of the largest single set of high-resolution spectra for an SN Ia, we find no evidence of variable absorption from circumstellar material. Combining our UV spectra, NIR photometry, and high-cadence optical photometry, we construct a bolometric light curve, showing that SN 2013dy had a maximum luminosity of 10.0+4.8 -3.8 × 1042 erg s-1. We compare the synthetic light curves and spectra of several models to SN 2013dy, finding that SN 2013dy is in good agreement with a solar-metallicity W7 model.
| Idioma original | English |
|---|---|
| Páginas (desde-hasta) | 4307-4325 |
| Número de páginas | 19 |
| Publicación | Monthly Notices of the Royal Astronomical Society |
| Volumen | 452 |
| N.º | 4 |
| DOI | |
| Estado | Published - 1 ene 2015 |
Huella dactilar
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science
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500 days of SN 2013dy : Spectra and photometry from the ultraviolet to the infrared. / Pan, Y. C.; Foley, R. J.; Kromer, M.; Fox, O. D.; Zheng, W.; Challis, P.; Clubb, K. I.; Filippenko, A. V.; Folatelli, G.; Graham, M. L.; Hillebrandt, W.; Kirshner, R. P.; Lee, W. H.; Pakmor, R.; Patat, F.; Phillips, M. M.; Pignata, G.; Röpke, F.; Seitenzahl, I.; Silverman, J. M.; Simon, J. D.; Sternberg, A.; Stritzinger, M. D.; Taubenberger, S.; Vinko, J.; Wheeler, J. C.
En: Monthly Notices of the Royal Astronomical Society, Vol. 452, N.º 4, 01.01.2015, p. 4307-4325.Resultado de la investigación: Article
TY - JOUR
T1 - 500 days of SN 2013dy
T2 - Spectra and photometry from the ultraviolet to the infrared
AU - Pan, Y. C.
AU - Foley, R. J.
AU - Kromer, M.
AU - Fox, O. D.
AU - Zheng, W.
AU - Challis, P.
AU - Clubb, K. I.
AU - Filippenko, A. V.
AU - Folatelli, G.
AU - Graham, M. L.
AU - Hillebrandt, W.
AU - Kirshner, R. P.
AU - Lee, W. H.
AU - Pakmor, R.
AU - Patat, F.
AU - Phillips, M. M.
AU - Pignata, G.
AU - Röpke, F.
AU - Seitenzahl, I.
AU - Silverman, J. M.
AU - Simon, J. D.
AU - Sternberg, A.
AU - Stritzinger, M. D.
AU - Taubenberger, S.
AU - Vinko, J.
AU - Wheeler, J. C.
PY - 2015/1/1
Y1 - 2015/1/1
N2 - SN 2013dy is a Type Ia supernova (SN Ia) for which we have compiled an extraordinary data set spanning from 0.1 to ~ 500 d after explosion. We present 10 epochs of ultraviolet (UV) through near-infrared (NIR) spectra with Hubble Space Telescope/Space Telescope Imaging Spectrograph, 47 epochs of optical spectra (15 of them having high resolution), and more than 500 photometric observations in the BVrRiIZYJH bands. SN 2013dy has a broad and slowly declining light curve (Δm15(B)=0.92 mag), shallow Si II λ6355 absorption, and a low velocity gradient. We detect strong C II in our earliest spectra, probing unburned progenitor material in the outermost layers of the SN ejecta, but this feature fades within a few days. The UV continuum of SN 2013dy, which is strongly affected by the metal abundance of the progenitor star, suggests that SN 2013dy had a relatively high-metallicity progenitor. Examining one of the largest single set of high-resolution spectra for an SN Ia, we find no evidence of variable absorption from circumstellar material. Combining our UV spectra, NIR photometry, and high-cadence optical photometry, we construct a bolometric light curve, showing that SN 2013dy had a maximum luminosity of 10.0+4.8 -3.8 × 1042 erg s-1. We compare the synthetic light curves and spectra of several models to SN 2013dy, finding that SN 2013dy is in good agreement with a solar-metallicity W7 model.
AB - SN 2013dy is a Type Ia supernova (SN Ia) for which we have compiled an extraordinary data set spanning from 0.1 to ~ 500 d after explosion. We present 10 epochs of ultraviolet (UV) through near-infrared (NIR) spectra with Hubble Space Telescope/Space Telescope Imaging Spectrograph, 47 epochs of optical spectra (15 of them having high resolution), and more than 500 photometric observations in the BVrRiIZYJH bands. SN 2013dy has a broad and slowly declining light curve (Δm15(B)=0.92 mag), shallow Si II λ6355 absorption, and a low velocity gradient. We detect strong C II in our earliest spectra, probing unburned progenitor material in the outermost layers of the SN ejecta, but this feature fades within a few days. The UV continuum of SN 2013dy, which is strongly affected by the metal abundance of the progenitor star, suggests that SN 2013dy had a relatively high-metallicity progenitor. Examining one of the largest single set of high-resolution spectra for an SN Ia, we find no evidence of variable absorption from circumstellar material. Combining our UV spectra, NIR photometry, and high-cadence optical photometry, we construct a bolometric light curve, showing that SN 2013dy had a maximum luminosity of 10.0+4.8 -3.8 × 1042 erg s-1. We compare the synthetic light curves and spectra of several models to SN 2013dy, finding that SN 2013dy is in good agreement with a solar-metallicity W7 model.
KW - Supernovae: general
KW - Supernovae: individual: SN 2013dy
UR - http://www.scopus.com/inward/record.url?scp=84940118255&partnerID=8YFLogxK
U2 - 10.1093/mnras/stv1605
DO - 10.1093/mnras/stv1605
M3 - Article
AN - SCOPUS:84940118255
VL - 452
SP - 4307
EP - 4325
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
SN - 0035-8711
IS - 4
ER -