Few published ultraviolet (UV) spectra exist for stripped-envelope supernovae and none to date for broad-lined Type Ic supernovae (SNe Ic-bl). These objects have extremely high ejecta velocities and are the only supernova type directly linked to gamma-ray bursts (GRBs). Here we present two epochs of HST/STIS spectra of the SN Ic-bl 2014ad, the first UV spectra for this class. We supplement this with 26 new epochs of ground-based optical spectra, augmenting a rich spectral time series. The UV spectra do not show strong features and are consistent with broadened versions of other SN Ic spectra observed in the UV. We measure Fe
- Home
- Search Results
- Page 1 of 1
Search for: All records
-
Total Resources2
- Resource Type
-
20
- Availability
-
11
- Author / Contributor
- Filter by Author / Creator
-
-
Jha, Saurabh W. (2)
-
Kwok, Lindsey A. (2)
-
McCully, Curtis (2)
-
Andrews, Jennifer E. (1)
-
Bostroem, K. Azalee (1)
-
Burke, Jamison (1)
-
Camacho-Neves, Yssavo (1)
-
Dai, Mi (1)
-
Dong, Yize (1)
-
Foley, Ryan J. (1)
-
Garnavich, Peter (1)
-
Gonzalez, Estefania Padilla (1)
-
Haislip, Joshua (1)
-
Hosseinzadeh, Griffin (1)
-
Howell, D. Andrew (1)
-
Janzen, Daryl (1)
-
Jencson, Jacob E. (1)
-
Kouprianov, Vladimir (1)
-
Kundu, Esha (1)
-
Lundquist, Michael (1)
-
- Filter by Editor
-
-
& Spizer, S. M. (0)
-
& . Spizer, S. (0)
-
& Ahn, J. (0)
-
& Bateiha, S. (0)
-
& Bosch, N. (0)
-
& Chen, B. (0)
-
& Chen, Bodong (0)
-
& Drown, S. (0)
-
& Higgins, A. (0)
-
& Kali, Y. (0)
-
& Ruiz-Arias, P.M. (0)
-
& S. Spitzer (0)
-
& Spitzer, S. (0)
-
& Spitzer, S.M. (0)
-
:Chaosong Huang, Gang Lu (0)
-
A. Beygelzimer (0)
-
A. E. Lischka, E.B. Dyer (0)
-
A. Ghate, K. Krishnaiyer (0)
-
A. Higgins (0)
-
A. I. Sacristán, J. C. (0)
-
-
Have feedback or suggestions for a way to improve these results?
!
Note: When clicking on a Digital Object Identifier (DOI) number, you will be taken to an external site maintained by the publisher.
Some full text articles may not yet be available without a charge during the embargo (administrative interval).
What is a DOI Number?
Some links on this page may take you to non-federal websites. Their policies may differ from this site.
-
Abstract ii 5169 Å velocities and show that SN 2014ad has even higher ejecta velocities than most SNe Ic both with and without observed GRBs. We construct models of the SN 2014ad UV+optical spectra usingtardis , a 1D Monte Carlo radiative-transfer spectral synthesis code. The models fit the data well at multiple epochs in the optical but underestimate the flux in the UV, likely due to simplifying assumptions. We find that high densities at high velocities are needed to reproduce the spectra, with ∼3M ⊙of material atv > 22,000 km s−1, assuming spherical symmetry. Our nebular line fits suggest a steep density profilemore » -
Hosseinzadeh, Griffin ; Sand, David J. ; Lundqvist, Peter ; Andrews, Jennifer E. ; Bostroem, K. Azalee ; Dong, Yize ; Janzen, Daryl ; Jencson, Jacob E. ; Lundquist, Michael ; Meza Retamal, Nicolas E. ; et al ( , The Astrophysical Journal Letters)Abstract We present high-cadence optical and ultraviolet light curves of the normal Type Ia supernova (SN) 2021aefx, which shows an early bump during the first two days of observation. This bump may be a signature of interaction between the exploding white dwarf and a nondegenerate binary companion, or it may be intrinsic to the white dwarf explosion mechanism. In the case of the former, the short duration of the bump implies a relatively compact main-sequence companion star, although this conclusion is viewing-angle dependent. Our best-fit companion-shocking and double-detonation models both overpredict the UV luminosity during the bump, and existing nickel-shell models do not match the strength and timescale of the bump. We also present nebular spectra of SN 2021aefx, which do not show the hydrogen or helium emission expected from a nondegenerate companion, as well as a radio nondetection that rules out all symbiotic progenitor systems and most accretion disk winds. Our analysis places strong but conflicting constraints on the progenitor of SN 2021aefx; no current model can explain all of our observations.Free, publicly-accessible full text available July 1, 2023