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

C. Gall, M. D. Stritzinger, C. Ashall, E. Baron, C. R. Burns, P. Hoeflich, E. Y. Hsiao, P. A. Mazzali, M. M. Phillips, A. V. Filippenko, J. P. Anderson, S. Benetti, P. J. Brown, A. Campillay, P. Challis, C. Contreras, N. Elias De La Rosa, G. Folatelli, R. J. Foley, M. FraserS. Holmbo, G. H. Marion, N. Morrell, Y. C. Pan, G. Pignata, N. B. Suntzeff, F. Taddia, S. Torres Robledo, S. Valenti

Resultado de la investigación: Article

15 Citas (Scopus)

Resumen

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 Δm15 (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, 56Ni 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 colour evolution along the Lira regime suggest that the progenitor of SN 2011iv had a higher central density than SN 2007on.

Idioma originalEnglish
Número de artículoA58
PublicaciónAstronomy and Astrophysics
Volumen611
DOI
EstadoPublished - 1 mar 2018

Huella dactilar

supernovae
luminosity
color
light curve
detonation
explosions
explosion
near infrared
rate
parameter

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Citar esto

Gall, C., Stritzinger, M. D., Ashall, C., Baron, E., Burns, C. R., Hoeflich, P., ... Valenti, S. (2018). Two transitional type Ia supernovae located in the Fornax cluster member NGC 1404: SN 2007on and SN 2011iv. Astronomy and Astrophysics, 611, [A58]. https://doi.org/10.1051/0004-6361/201730886
Gall, C. ; Stritzinger, M. D. ; Ashall, C. ; Baron, E. ; Burns, C. R. ; Hoeflich, P. ; Hsiao, E. Y. ; Mazzali, P. A. ; Phillips, M. M. ; Filippenko, A. V. ; Anderson, J. P. ; Benetti, S. ; Brown, P. J. ; Campillay, A. ; Challis, P. ; Contreras, C. ; Elias De La Rosa, N. ; Folatelli, G. ; Foley, R. J. ; Fraser, M. ; Holmbo, S. ; Marion, G. H. ; Morrell, N. ; Pan, Y. C. ; Pignata, G. ; Suntzeff, N. B. ; Taddia, F. ; Robledo, S. Torres ; Valenti, S. / Two transitional type Ia supernovae located in the Fornax cluster member NGC 1404 : SN 2007on and SN 2011iv. En: Astronomy and Astrophysics. 2018 ; Vol. 611.
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title = "Two transitional type Ia supernovae located in the Fornax cluster member NGC 1404: SN 2007on and SN 2011iv",
abstract = "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 Δm15 (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, 56Ni 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 colour evolution along the Lira regime suggest that the progenitor of SN 2011iv had a higher central density than SN 2007on.",
keywords = "Dust, extinction, Supernovae: general, Supernovae: individual: SN 2007on, Supernovae: individual: SN 2011iv",
author = "C. Gall and Stritzinger, {M. D.} and C. Ashall and E. Baron and Burns, {C. R.} and P. Hoeflich and Hsiao, {E. Y.} and Mazzali, {P. A.} and Phillips, {M. M.} and Filippenko, {A. V.} and Anderson, {J. P.} and S. Benetti and Brown, {P. J.} and A. Campillay and P. Challis and C. Contreras and {Elias De La Rosa}, N. and G. Folatelli and Foley, {R. J.} and M. Fraser and S. Holmbo and Marion, {G. H.} and N. Morrell and Pan, {Y. C.} and G. Pignata and Suntzeff, {N. B.} and F. Taddia and Robledo, {S. Torres} and S. Valenti",
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Gall, C, Stritzinger, MD, Ashall, C, Baron, E, Burns, CR, Hoeflich, P, Hsiao, EY, Mazzali, PA, Phillips, MM, Filippenko, AV, Anderson, JP, Benetti, S, Brown, PJ, Campillay, A, Challis, P, Contreras, C, Elias De La Rosa, N, Folatelli, G, Foley, RJ, Fraser, M, Holmbo, S, Marion, GH, Morrell, N, Pan, YC, Pignata, G, Suntzeff, NB, Taddia, F, Robledo, ST & Valenti, S 2018, 'Two transitional type Ia supernovae located in the Fornax cluster member NGC 1404: SN 2007on and SN 2011iv', Astronomy and Astrophysics, vol. 611, A58. https://doi.org/10.1051/0004-6361/201730886

Two transitional type Ia supernovae located in the Fornax cluster member NGC 1404 : SN 2007on and SN 2011iv. / Gall, C.; Stritzinger, M. D.; Ashall, C.; Baron, E.; Burns, C. R.; Hoeflich, P.; Hsiao, E. Y.; Mazzali, P. A.; Phillips, M. M.; Filippenko, A. V.; Anderson, J. P.; Benetti, S.; Brown, P. J.; Campillay, A.; Challis, P.; Contreras, C.; Elias De La Rosa, N.; Folatelli, G.; Foley, R. J.; Fraser, M.; Holmbo, S.; Marion, G. H.; Morrell, N.; Pan, Y. C.; Pignata, G.; Suntzeff, N. B.; Taddia, F.; Robledo, S. Torres; Valenti, S.

En: Astronomy and Astrophysics, Vol. 611, A58, 01.03.2018.

Resultado de la investigación: Article

TY - JOUR

T1 - Two transitional type Ia supernovae located in the Fornax cluster member NGC 1404

T2 - SN 2007on and SN 2011iv

AU - Gall, C.

AU - Stritzinger, M. D.

AU - Ashall, C.

AU - Baron, E.

AU - Burns, C. R.

AU - Hoeflich, P.

AU - Hsiao, E. Y.

AU - Mazzali, P. A.

AU - Phillips, M. M.

AU - Filippenko, A. V.

AU - Anderson, J. P.

AU - Benetti, S.

AU - Brown, P. J.

AU - Campillay, A.

AU - Challis, P.

AU - Contreras, C.

AU - Elias De La Rosa, N.

AU - Folatelli, G.

AU - Foley, R. J.

AU - Fraser, M.

AU - Holmbo, S.

AU - Marion, G. H.

AU - Morrell, N.

AU - Pan, Y. C.

AU - Pignata, G.

AU - Suntzeff, N. B.

AU - Taddia, F.

AU - Robledo, S. Torres

AU - Valenti, S.

PY - 2018/3/1

Y1 - 2018/3/1

N2 - 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 Δm15 (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, 56Ni 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 colour evolution along the Lira regime suggest that the progenitor of SN 2011iv had a higher central density than SN 2007on.

AB - 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 Δm15 (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, 56Ni 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 colour evolution along the Lira regime suggest that the progenitor of SN 2011iv had a higher central density than SN 2007on.

KW - Dust, extinction

KW - Supernovae: general

KW - Supernovae: individual: SN 2007on

KW - Supernovae: individual: SN 2011iv

UR - http://www.scopus.com/inward/record.url?scp=85044825882&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/201730886

DO - 10.1051/0004-6361/201730886

M3 - Article

AN - SCOPUS:85044825882

VL - 611

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

SN - 0004-6361

M1 - A58

ER -