Quantitative comparison between type Ia supernova spectra   at low and high redshifts: a case study

Garavini, G.; Folatelli, G.; Nobili, S.; Aldering, G.; Amanullah, R.; Antilogus, P.; Astier, P.; Blanc, G.; Bronder, T. J.; Burns, M. S.; Conley, A.; Deustua, Susana E.; Doi, Mamoru; Fabbro, S.; Fadeyev, V.; Gibbons, R.; Goldhaber, G.; Goobar, A.; Groom, D. E.; Hook, I. M.; Howell, D. A.; Kashikawa, Nobunari; Kim, A. G.; Kowalski, M.; Кузнецова, Н.; Lee, B. C.; Lidman, C.; Méndez, J.; Morokuma, Tomoki; Motohara, Kentaro; Nugent, P.; Pain, R.; Perlmutter, S.; Quimby, R.; Raux, J.; Regnault, Nicolas; Ruiz‐Lapuente, P.; Sainton, G.; Schahmanèche, K.; Smith, E.; Spadafora, A. L.; Stanishev, V.; Thomas, R. C.; Walton, N. A.; Wang, L.; Wood‐Vasey, W. M.; Yasuda, Naoki

doi:10.1051/0004-6361:20065400

Cited by 52 publications

(58 citation statements)

References 56 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…3 (left panel), measurements are made of their pseudo-equivalent width (pEW), which is a common method to quantify spectral properties of SNe Ia at optical wavelengths (e.g., Folatelli 2004;Garavini et al 2007;Folatelli et al 2013). Parameters that define the two UV pEW indicators considered here were obtained following the prescription of Garavini et al (2007) and are summarised in Table 9. In short, the two pEW indicators are defined from the blue to the red maximum of an absorption trough.…”

Section: Uv Pseudo-equivalent Widthmentioning

confidence: 99%

Two transitional type Ia supernovae located in the Fornax cluster member NGC 1404: SN 2007on and SN 2011iv

Gall

Stritzinger

Ashall

et al. 2018

A&A

Self Cite

View full text Add to dashboard Cite

We present an analysis of ultraviolet (UV) to near-infrared observations of the fast-declining Type Ia supernovae (SNe Ia) 2007on and 2011iv, hosted by the Fornax cluster member NGC 1404. The B-band light curves of SN 2007on and SN 2011iv are characterised by ∆m 15 (B) decline-rate values of 1.96 mag and 1.77 mag, respectively. Although they have similar decline rates, their peak B-and H-band magnitudes differ by ∼ 0.60 mag and ∼ 0.35 mag, respectively. After correcting for the luminosity vs. decline rate and the luminosity vs. colour relations, the peak B-band and H-band light curves provide distances that differ by ∼ 14% and ∼ 9%, respectively. These findings serve as a cautionary tale for the use of transitional SNe Ia located in early-type hosts in the quest to measure cosmological parameters. Interestingly, even though SN 2011iv is brighter and bluer at early times, by three weeks past maximum and extending over several months, its B − V colour is 0.12 mag redder than that of SN 2007on. To reconcile this unusual behaviour, we turn to guidance from a suite of spherical one-dimensional Chandrasekhar-mass delayed-detonation explosion models. In this context, 56 Ni production depends on both the so-called transition density and the central density of the progenitor white dwarf. To first order, the transition density drives the luminosity-width relation, while the central density is an important second-order parameter. Within this context, the differences in the B − V color evolution along the Lira regime suggests the progenitor of SN 2011iv had a higher central density than SN 2007on.

show abstract

Section: Uv Pseudo-equivalent Widthmentioning

confidence: 99%

Two transitional type Ia supernovae located in the Fornax cluster member NGC 1404: SN 2007on and SN 2011iv

Gall

Stritzinger

Ashall

et al. 2018

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…Although the minima of the spectral features is not going to be strongly affected (thus the v), both the slope of the pseudo-continuum and its deepness would be affected. Nordin et al (2011) and Garavini et al (2007) studied the effect of reddening in the uncertainties of pW measurement and concluded that for values of E(B − V ) lower than 0.3 the difference is lower than 5%, but for more extinguished SN it could be important, which is the case of SN 2014J. Observed unredshifted pre-maximum, maximum-light, and post-maximum spectra taken at ORM (La Palma).…”

Section: Measurement Of the Spectral Parametersmentioning

confidence: 99%

SN 2014J at M82 – I. A middle-class Type Ia supernova by all spectroscopic metrics

Galbany

Moreno-Raya

Ruiz‐Lapuente

et al. 2016

Mon. Not. R. Astron. Soc.

Self Cite

View full text Add to dashboard Cite

We present the intensive spectroscopic follow up of the type Ia supernova (SN Ia) 2014J in the starburst galaxy M82. Twenty-seven optical spectra have been acquired from January 22 nd to September 1 st 2014 with the Isaac Newton (INT) and William Herschel (WHT) Telescopes. After correcting the observations for the recession velocity of M82 and for Milky Way and host galaxy extinction, we measured expansion velocities from spectral line blueshifts and pseudo-equivalent width of the strongest features in the spectra, which gives an idea on how elements are distributed within the ejecta. We position SN 2014J in the Benetti (2005)

show abstract

“…Observational trends appear to emerge in the way the velocities within the supernova ejecta evolve , but the interpretation of these correlations are not clear yet. It is noteworthy that the distant objects appear to follow the general spectral evolution of their nearby counterparts and there is no obvious sign of differences in the spectral appearance of SNe Ia (Blondin et al 2006, Garavini et al 2007b. The interpretation of the spectra has now also been expanded to reconstruct the element distribution in the ejecta through the spectral evolution (Fisher et al 1999, Stehle et al 2005, which gives a direct input to the explosion models.…”

Section: Type Ia Supernovaementioning

confidence: 99%

Supernovae and cosmology

Leibundgut

2007

Gen Relativ Gravit

View full text Add to dashboard Cite

The extreme luminosity and their fairly unique temporal behaviour have made supernovae a superb tool to measure distances in the universe. As complex astrophysical events they provide interesting insights into explosion physics, explosive nucleosynthesis, hydrodynamics of the explosion and radiation transport. They are an end product of stellar evolution and provide clues to the stellar composition. Since they can be observed at large distances they have become critical probes to further explore astrophysical effects, like dust properties in external galaxies and the star formation history of galaxies. Some of the astrophysics interferes with the cosmological applications of supernovae. The local velocity field, distorted by the gravitational attraction of the local large scale structure, and the reddening law appear at the moment the major limitations in the accuracy with which cosmological parameters can be determined. These absorption effects can introduce a secondary bias into the observations of the distant supernovae, which needs to be carefully evaluated. Supernovae have been used for the measurement of the Hubble constant, i.e. the current expansion rate of the universe, and the accelerated cosmic expansion directly inferred from the apparent faintness of the distant supernovae.

show abstract

Quantitative comparison between type Ia supernova spectra at low and high redshifts: a case study

Cited by 52 publications

References 56 publications

Two transitional type Ia supernovae located in the Fornax cluster member NGC 1404: SN 2007on and SN 2011iv

Two transitional type Ia supernovae located in the Fornax cluster member NGC 1404: SN 2007on and SN 2011iv

SN 2014J at M82 – I. A middle-class Type Ia supernova by all spectroscopic metrics

Supernovae and cosmology

Contact Info

Product

Resources

About