The slowly declining type Ia supernova 2008fv and the near-infrared second maximum

Biscardi, I.; Brocato, E.; Arkharov, A. A.; Carlo, E. Di; Rico, G. Di; Dolci, M.; Ефимова, Н. В.; Pietrinferni, A.; Valentini, G.

doi:10.1051/0004-6361/201014160

Cited by 18 publications

(25 citation statements)

References 73 publications

(81 reference statements)

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“…The correlation of M2 with ∆m15 is rather weak (Fig. 11) although it appears somewhat stronger than in Biscardi et al (2012) (the Pearson coefficients in our data are 0.5 and 0.63 for J and H compared to 0.12 and 0.08 in Biscardi et al 2012).…”

Section: Discussioncontrasting

confidence: 51%

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Near-infrared light curves of Type Ia supernovae: studying properties of the second maximum

Dhawan

Leibundgut

Spyromilio

et al. 2015

Monthly Notices of the Royal Astronomical Society

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Type Ia supernovae have been proposed to be much better distance indicators at nearinfrared compared to optical wavelengths -the effect of dust extinction is expected to be lower and it has been shown that SNe Ia behave more like 'standard candles' at NIR wavelengths. To better understand the physical processes behind this increased uniformity, we have studied the Y , J and H-filter light curves of 91 SNe Ia from the literature. We show that the phases and luminosities of the first maximum in the NIR light curves are extremely uniform for our sample. The phase of the second maximum, the late-phase NIR luminosity and the optical light curve shape are found to be strongly correlated, in particular more luminous SNe Ia reach the second maximum in the NIR filters at a later phase compared to fainter objects. We also find a strong correlation between the phase of the second maximum and the epoch at which the SN enters the Lira law phase in its optical colour curve (epochs ∼ 15 to 30 days after B band maximum). The decline rate after the second maximum is very uniform in all NIR filters. We suggest that these observational parameters are linked to the nickel and iron mass in the explosion, providing evidence that the amount of nickel synthesised in the explosion is the dominating factor shaping the optical and NIR appearance of SNe Ia.

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Section: Discussioncontrasting

confidence: 51%

“…In parameterising the NIR light curves we follow the nomenclature introduced by Biscardi et al (2012). The first maximum in filter X, M1(X) is reached at a phase, t1(X) relative to the phase of the B maximum (t max B =0 d).…”

Section: Nir Light Curve Morphologymentioning

confidence: 99%

Near-infrared light curves of Type Ia supernovae: studying properties of the second maximum

Dhawan

Leibundgut

Spyromilio

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…15). (Biscardi et al 2012), PS1-10w (Rest et al 2014). For objects with no optical data or bad MLCS fits with reduced χ 2 > 3, t Bmax is estimated from any or all of: the MJD of the brightest point (rounded to the nearest day), optical spectra in listed CBET/IAUC/ATEL notices, and cross checked with fitted phases of NIR LC features, where possible (see F12).…”

Section: Comparing Cfair2 and Csp Lcsmentioning

confidence: 99%

CfAIR2: NEAR-INFRARED LIGHT CURVES OF 94 TYPE Ia SUPERNOVAE

Friedman

Wood‐Vasey

Marion

et al. 2015

ApJS

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CfAIR2 is a large homogeneously reduced set of near-infrared (NIR) light curves for Type Ia supernovae (SN Ia) obtained with the 1.3m Peters Automated InfraRed Imaging TELescope (PAIRITEL). This data set includes 4637 measurements of 94 SN Ia and 4 additional SN Iax observed from 2005-2011 at the Fred Lawrence Whipple Observatory on Mount Hopkins, Arizona. CfAIR2 includes JHK s photometric measurements for 88 normal and 6 spectroscopically peculiar SN Ia in the nearby universe, with a median redshift of z ∼ 0.021 for the normal SN Ia. CfAIR2 data span the range from -13 days to +127 days from B-band maximum. More than half of the light curves begin before the time of maximum and the coverage typically contains ∼ 13-18 epochs of observation, depending on the filter. We present extensive tests that verify the fidelity of the CfAIR2 data pipeline, including comparison to the excellent data of the Carnegie Supernova Project. CfAIR2 contributes to a firm local anchor for supernova cosmology studies in the NIR. Because SN Ia are more nearly standard candles in the NIR and are less vulnerable to the vexing problems of extinction by dust, CfAIR2 will help the supernova cosmology community develop more precise and accurate extragalactic distance probes to improve our knowledge of cosmological parameters, including dark energy and its potential time variation. SN Star α(2000) δ(2000) N J m PTL J σ PTL m J m 2M J σ m 2M J N H m PTL H σ PTL Observed Phase: MJD -(T(Bmax)=53785.9) [days] Apparent Magnitude and Residuals 18 17 16 15 14 13 12 J CfAIR2 CSP H K 0 20 40 60 80 -0.6 -0.4 -0.2 0.0 0.2 0.4 0.6 CSP -CfAIR2 (fit) CSP (fit) -CfAIR2 CSP -CfAIR2 (fit) CSP (fit) -CfAIR2 0.009 +/-0.018 0 20 40 60 80 0.006 +/-0.011 0 20 40 60 80 -0.007 +/-0.010 sn2009dc CfAIR2 & CSP NIR LCs Observed Phase: MJD -(T(Bmax)=54945.5) [days] Apparent Magnitude and Residuals 21 20 19 18 17 16 15 J CfAIR2 CSP H K SN 2005ao Ia PAIRITEL

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“…Recent studies (e.g. Biscardi et al 2012;Dhawan et al 2015) found that more luminous SNe Ia reach the second maximum in NIR filters at a later phase. This was predicted by Kasen (2006), who also indicated that the phase of the second maximum (designated in the following as t 2 and measured relative to the B-band light curve maximum) should be a function of the 56 Ni mass in the explosion.…”

Section: Introductionmentioning

confidence: 99%

A reddening-free method to estimate the⁵⁶Ni mass of Type Ia supernovae

Dhawan

Leibundgut

Spyromilio

et al. 2016

A&A

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The increase in the number of Type Ia supernovae (SNe Ia) has demonstrated that the population shows greater diversity than has been assumed in the past. The reasons (e.g. parent population, explosion mechanism) for this diversity remain largely unknown. We investigated a sample of SNe Ia near-infrared light curves and correlated the phase of the second maximum with the bolometric peak luminosity. The peak bolometric luminosity is related to the time of the second maximum (relative to the B light curve maximum) as follows: L max (10 43 erg s −1 ) = (0.039 ± 0.004) × t 2 (J)(days) + (0.013 ± 0.106). 56 Ni masses can be derived from the peak luminosity based on Arnett's rule, which states that the luminosity at maximum is equal to the instantaneous energy generated by the nickel decay. We checked this assumption against recent radiative-transfer calculations of Chandrasekhar-mass delayed detonation models and find this assumption is valid to within 10% in recent radiative-transfer calculations of Chandrasekhar-mass delayed detonation models. The L max vs. t 2 relation is applied to a sample of 40 additional SNe Ia with significant reddening (E(B − V) > 0.1 mag), and a reddening-free bolometric luminosity function of SNe Ia is established. The method is tested with the 56 Ni mass measurement from the direct observation of γ-rays in the heavily absorbed SN 2014J and found to be fully consistent. Super-Chandrasekhar-mass explosions, in particular SN 2007if, do not follow the relations between peak luminosity and second IR maximum. This may point to an additional energy source contributing at maximum light. The luminosity function of SNe Ia is constructed and is shown to be asymmetric with a tail of low-luminosity objects and a rather sharp high-luminosity cutoff, although it might be influenced by selection effects.

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The slowly declining type Ia supernova 2008fv and the near-infrared second maximum

Cited by 18 publications

References 73 publications

Near-infrared light curves of Type Ia supernovae: studying properties of the second maximum

Near-infrared light curves of Type Ia supernovae: studying properties of the second maximum

CfAIR2: NEAR-INFRARED LIGHT CURVES OF 94 TYPE Ia SUPERNOVAE

A reddening-free method to estimate the⁵⁶Ni mass of Type Ia supernovae

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The slowly declining type Ia supernova 2008fv and the near-infrared second maximum

Cited by 18 publications

References 73 publications

Near-infrared light curves of Type Ia supernovae: studying properties of the second maximum

Near-infrared light curves of Type Ia supernovae: studying properties of the second maximum

CfAIR2: NEAR-INFRARED LIGHT CURVES OF 94 TYPE Ia SUPERNOVAE

A reddening-free method to estimate the56Ni mass of Type Ia supernovae

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A reddening-free method to estimate the⁵⁶Ni mass of Type Ia supernovae