An early-time infrared and optical study of the Type Ia Supernova 1998bu in M96

Hernández, Miguel; Meikle, W. P. S.; Aparicio, A.; Benn, Chris; Burleigh, M. R.; Chrysostomou, A.; Fernandes, Amadeu J. L.; Geballe, T. R.; Hammersley, P. L.; Iglésias-Páramo, J.; James, D. J.; James, P. A.; Kemp, S. N.; Lister, Tim; Martínez–Delgado, David; Oscoz, A.; Pollacco, D.; Rozas, M.; Smartt, S. J.; Sorensen, P.; Swaters, Robert A.; Telting, J. H.; Vacca, William D.; Walton, N. A.; Osorio, M. R. Zapatero

doi:10.1046/j.1365-8711.2000.03841.x

Cited by 69 publications

(20 citation statements)

References 40 publications

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“…1. K+ is the miscellaneous early sample (Jha et al 1999;Hernandez et al 2000;Krisciunas et al 2000Krisciunas et al , 2003Krisciunas et al , 2004aKrisciunas et al , 2004bKrisciunas et al , 2007Valentini et al 2003;Phillips et al 2006;Pastorello et al 2007aPastorello et al , 2007bStanishev et al 2007;Pignata et al 2008) et al 2008) to F15 owing to the 74 additional SNe Ia from the final data release (Friedman et al 2015). We do not use any of the peculiar Type Iax SNe (Foley et al 2013) from Friedman et al (2015).…”

Section: Sne Iamentioning

confidence: 99%

Are Type Ia Supernovae in Rest-frame H Brighter in More Massive Galaxies?

Ponder

Wood‐Vasey

Weyant

et al. 2021

ApJ

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We analyze 143 Type Ia supernovae (SNe Ia) observed in H band (1.6–1.8 μm) and find that SNe Ia are intrinsically brighter in H band with increasing host galaxy stellar mass. We find that SNe Ia in galaxies more massive than 1010.43 M ⊙ are 0.13 ± 0.04 mag brighter in H than SNe Ia in less massive galaxies. The same set of SNe Ia observed at optical wavelengths, after width–color–luminosity corrections, exhibit a 0.10 ± 0.03 mag offset in the Hubble residuals. We observe an outlier population ( ∣ Δ H max ∣ > 0.5 mag) in the H band and show that removing the outlier population moves the mass threshold to 1010.65 M ⊙ and reduces the step in H band to 0.08 ± 0.04 mag, but the equivalent optical mass step is increased to 0.13 ± 0.04 mag. We conclude that the outliers do not drive the brightness–host-mass correlation. Less massive galaxies preferentially host more higher-stretch SNe Ia, which are intrinsically brighter and bluer. It is only after correction for width–luminosity and color–luminosity relationships that SNe Ia have brighter optical Hubble residuals in more massive galaxies. Thus, finding that SNe Ia are intrinsically brighter in H in more massive galaxies is an opposite correlation to the intrinsic (pre-width–luminosity correction) optical brightness. If dust and the treatment of intrinsic color variation were the main driver of the host galaxy mass correlation, we would not expect a correlation of brighter H-band SNe Ia in more massive galaxies.

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Section: Sne Iamentioning

confidence: 99%

Are Type Ia Supernovae in Rest-frame H Brighter in More Massive Galaxies?

Ponder

Wood‐Vasey

Weyant

et al. 2021

ApJ

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“…Recently, Tammann & Reindl (2013) derived M V ,max = −19.45 ± 0.15 for SN 1989B and M V ,max = −19.38 ± 0.16 for SN 1998bu from the photometry in the literature Jha et al 1999;Hernandez et al 2000;Wells et al 1994), adopting a mean TRGB distance of the Leo I Group, (m − M) 0 = 30.39 ± 0.10. These values were obtained after correcting for the Galactic extinction, host galaxy extinction, and decline rates (Δm 15 ).…”

Section: The Calibration Of the Absolute Magnitudes Of Sne Ia And Thementioning

confidence: 99%

“…M66 (NGC 3627, SAB(s)b) and M96 (NGC 3368, SAB(rs)ab) are nearby bright spiral galaxies hosting SNe Ia: SN 1989B in M66 (Evans & McNaught 1989;Wells et al 1994) and SN 1998bu in M96 (Villi et al 1998;Suntzeff et al 1999;Jha et al 1999;Hernandez et al 2000;Spyromilio et al 2004). M66 has been host to other three SNe as well: SN II 1973R (Ciatti & Rosino 1977), SN imposter SN 1997bs (Van Dyk et al 2000, and SN II-L 2009hd (Elias-Rosa et al 2011).…”

Section: Introductionmentioning

confidence: 99%

THE TIP OF THE RED GIANT BRANCH DISTANCES TO TYPE Ia SUPERNOVA HOST GALAXIES. II. M66 AND M96 IN THE LEO I GROUP

Lee

Jang

2013

ApJ

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M66 and M96 in the Leo I Group are nearby spiral galaxies hosting Type Ia supernovae (SNe Ia). We estimate the distances to these galaxies from the luminosity of the tip of the red giant branch (TRGB). We obtain VI photometry of resolved stars in these galaxies from F555W and F814W images in the Hubble Space Telescope archive. From the luminosity function of these red giants, we find the TRGB I-band magnitude to be I TRGB = 26.20 ± 0.03 for M66 and 26.21 ± 0.03 for M96. These values yield distance modulus (m − M) 0 = 30.12 ± 0.03(random) ± 0.12(systematic) for M66 and (m − M) 0 = 30.15 ± 0.03(random) ± 0.12(systematic) for M96. These results show that they are indeed the members of the same group. With these results we derive absolute maximum magnitudes of two SNe (SN 1989B in M66 and SN 1998bu in M96). V-band magnitudes of these SNe Ia are ∼0.2 mag fainter than SN 2011fe in M101, one of the nearest recent SNe Ia. We also derive near-infrared magnitudes for SN 1998bu. Optical magnitudes of three SNe Ia (SN 1989B, SN 1998bu, and SN 2011fe)

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“…Recently, Ponder et al (2020) used separate SN P (Burns et al 2011) fits to optical and -band light curves of SNe Ia to explore how correlations with host mass change between the optical and NIR. They analysed the -band (optical) light curves of 99 (71) supernovae from the CfA/CfAIR2 (Wood-Vasey et al 2008;Friedman et al 2015), CSP, SweetSpot (Weyant et al 2018), and elsewhere in the literature (Jha et al 1999;Hernandez et al 2000;Krisciunas et al 2000Krisciunas et al , 2003Krisciunas et al , 2004aKrisciunas et al ,b, 2007Valentini et al 2003;Phillips et al 2006;Pastorello et al 2007a,b;Stanishev et al 2007;Pignata et al 2008), finding an -band mass step of 0.18 ± 0.05 mag (0.10 ± 0.04 mag after an outlier cut) at a best fit location of 10 10.44 M , with a comparably sized 0.17 ± 0.05 mag step in the optical. Contemporary work by Uddin et al (2020) recovered a similar result in an analysis of the CSP-I sample.…”

Section: Introductionmentioning

confidence: 99%

Testing the consistency of dust laws in SN Ia host galaxies: A BayeSN Examination of Foundation DR1

Thorp

Mandel

Jones

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We apply BayeSN, our new hierarchical Bayesian model for the SEDs of Type Ia supernovae (SNe Ia), to analyse the griz light curves of 157 nearby SNe Ia (0.015 < z < 0.08) from the public Foundation DR1 dataset. We train a new version of BayeSN, continuous from 0.35–0.95 μm, which we use to model the properties of SNe Ia in the rest-frame z-band, study the properties of dust in their host galaxies, and construct a Hubble diagram of SN Ia distances determined from full griz light curves. Our griz Hubble diagram has a low total RMS of 0.13 mag using BayeSN, compared to 0.16 mag using SALT2. Additionally, we test the consistency of the dust law RV between low- and high-mass host galaxies by using our model to fit the full time- and wavelength-dependent SEDs of SNe Ia up to moderate reddening (peak apparent B − V ≲ 0.3). Splitting the population at the median host mass, we find RV = 2.84 ± 0.31 in low-mass hosts, and RV = 2.58 ± 0.23 in high-mass hosts, both consistent with the global value of RV = 2.61 ± 0.21 that we estimate for the full sample. For all choices of mass split we consider, RV is consistent across the step within ≲ 1.2σ. Modelling population distributions of dust laws in low- and high-mass hosts, we find that both subsamples are highly consistent with the full sample’s population mean μ(RV) = 2.70 ± 0.25 with a 95 per cent upper bound on the population σ(RV) < 0.61. The RV population means are consistent within ≲ 1.2σ. We find that simultaneous fitting of host-mass-dependent dust properties within our hierarchical model does not account for the conventional mass step.

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An early-time infrared and optical study of the Type Ia Supernova 1998bu in M96

Cited by 69 publications

References 40 publications

Are Type Ia Supernovae in Rest-frame H Brighter in More Massive Galaxies?

Are Type Ia Supernovae in Rest-frame H Brighter in More Massive Galaxies?

THE TIP OF THE RED GIANT BRANCH DISTANCES TO TYPE Ia SUPERNOVA HOST GALAXIES. II. M66 AND M96 IN THE LEO I GROUP

Testing the consistency of dust laws in SN Ia host galaxies: A BayeSN Examination of Foundation DR1

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