Explosion Diagnostics of Type Ia Supernovae from Early Infrared Spectra

Wheeler, J. C.; Höflich, Peter; Harkness, Robert; Spyromilio, J.

doi:10.1086/305427

Cited by 116 publications

(183 citation statements)

References 23 publications

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“…Similar trends appear in the J, H, and K-band LC (Krisciunas et al 2004b), although interesting exceptions have been sought out (e.g., SN 2000cx Candia et al 2003). Despite the theoretical insights (e.g., Hoflich et al 1995;Wheeler et al 1998;Pinto & Eastman 2000a,b;Kasen 2006), the origin of the NIR secondary maximum and its dependence on the SN ejecta properties remain unclear. These NIR LCs therefore provide promising means of investigating a possible empirical secondary parameter, which may explain the deviations from the standard width-luminosity relation (Kasen 2006), and thus help us to understand the intrinsic differences among SNe Ia.…”

Section: Introductionmentioning

confidence: 80%

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

Biscardi

Brocato

Arkharov

et al. 2012

A&A

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Aims. We present optical and near-infrared (NIR) photometry of supernova (SN) 2008fv and a brief investigation of SN type Ia to search for possible correlations between the properties of NIR light curves and the optical decline rate. Methods. We analyse our BVRI and JHK observations to derive light curves (LCs), colour curves, and the bolometric behaviour of SN 2008fv. Data range from about five days before to two months after maximum. We also collect a database of the main characteristics of NIR LCs of SNe Ia available in literature. Results. We find close similarities between the observed LCs of the SN event studied here and SN 2000E. SN 2008fv is a slow-declining SNe Ia with a post-maximum decline of Δm 15,B = 0.96 ± 0.08 mag and a B-band maximum luminosity of M B,0 = −19.40 ± 0.1 mag, close to the value of normal SNe Ia. The optical and NIR data allow us to constrain the host galaxy reddening of NGC 3147, E(B−V) = 0.22 ± 0.05 mag and its distance μ = 33.2 ± 0.1 mag. Furthermore, we derive a synthesized 56 Ni mass of about 0.7 M , by using the well-known relation between the maximum luminosity of the uvoir bolometric light curve and the initial content of 56 Ni. We investigate the correlation between the NIR characteristics of LCs and optical properties by collecting data of a sample of 40 SNe. We derive quantitative relationships involving the epoch of the secondary maximum in the JHK bands and the decline rate Δm 15 (B). Further, we find no correlations between Δm 15 measured in the JHK bands and the optical Δm 15 (B). In contrast, quite evident correlations with the Δm 15 (B) and Δm 40 (J)/Δm 15 (H).

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Section: Introductionmentioning

confidence: 80%

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

Biscardi

Brocato

Arkharov

et al. 2012

A&A

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“…The separation of the features depends on the differential expansion rate of the Fe-group element region combined with the wavelength separation of the multiplets. In normal SNe Ia where the differential expansion rate is high, these features are blended leading to the characteristic features observed (Wheeler et al 1998). However, at longer wavelength (∼2 μm) the Fe-group element multiplets are only partially blended allowing the individual multiplets to be identified.…”

Section: Discussionmentioning

confidence: 96%

Optical and near-IR observations of the faint and fast 2008ha-like supernova 2010ae

Stritzinger

Hsiao

Valenti

et al. 2014

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A comprehensive set of optical and near-infrared (NIR) photometry and spectroscopy is presented for the faint and fast 2008ha-like supernova (SN) 2010ae. Contingent on the adopted value of host extinction, SN 2010ae reached a peak brightness of −13.8 > M V > −15.3 mag, while modeling of the UVOIR light curve suggests it produced 0.003-0.007 M of 56 Ni, ejected 0.30−0.60 M of material, and had an explosion energy of 0.04-0.30 × 10 51 erg. The values of these explosion parameters are similar to the peculiar SN 2008ha -for which we also present previously unpublished early phase optical and NIR light curves -and places these two transients at the faint end of the 2002cx-like SN population. Detailed inspection of the post-maximum NIR spectroscopic sequence indicates the presence of a multitude of spectral features, which are identified through SYNAPPS modeling to be mainly attributed to Co ii. Comparison with a collection of published and unpublished NIR spectra of other 2002cx-like SNe, reveals that a Co ii footprint is ubiquitous to this subclass of transients, providing a link to Type Ia SNe. A visual-wavelength spectrum of SN 2010ae obtained at +252 days past maximum shows a striking resemblance to a similar epoch spectrum of SN 2002cx. However, subtle differences in the strength and ratio of calcium emission features, as well as diversity among similar epoch spectra of other 2002cx-like SNe indicates a range of physical conditions of the ejecta, highlighting the heterogeneous nature of this peculiar class of transients.

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“…The origin of this feature has been discussed widely by several authors, especially in the context of type Ia SNe, with Wheeler et al (1998) favouring Mg II and Meikle et al (1996) suggesting a blend of Mg II and He I 1.083 μm; the latter is a line that is easily excited in a variety of astrophysical contexts. In fact, other elements such as C, O, Si, and Fe may also contribute to features in this region.…”

Section: Near-infrared Spectramentioning

confidence: 96%

Extensive optical and near-infrared observations of the nearby, narrow-lined type Ic SN 2007gr: days 5 to 415

Hunter

Valenti

Kotak

et al. 2009

A&A

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We present photometric and spectroscopic observations at optical and near-infrared wavelengths of the nearby type Ic supernova 2007gr. These represent the most extensive data-set to date of any supernova of this sub-type, with frequent coverage from shortly after discovery to more than one year post-explosion. We deduce a rise time to B-band maximum of 11.5 ± 2.7 d. We find a peak B-band magnitude of M B = −16.8, and light curves which are remarkably similar to the so-called "hypernova" SN 2002ap. In contrast, the spectra of SNe 2007gr and 2002ap show marked differences, not least in their respective expansion velocities. We attribute these differences primarily to the density profiles of their progenitor stars at the time of explosion i.e. a more compact star for SN 2007gr compared to SN 2002ap. From the quasi-bolometric light curve of SN 2007gr, we estimate that 0.076 ± 0.010 M of 56 Ni was produced in the explosion. Our near-infrared (IR) spectra clearly show the onset and disappearance of the first overtone of carbon monoxide (CO) between ∼70 to 175 d relative to B-band maximum. The detection of the CO molecule implies that ionised He was not microscopically mixed within the carbon/oxygen layers. From the optical spectra, near-IR light curves, and colour evolution, we find no evidence for dust condensation in the ejecta out to about +400 d. Given the combination of unprecedented temporal coverage, and high signal-to-noise data, we suggest that SN 2007gr could be used as a template object for supernovae of this sub-class.

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Explosion Diagnostics of Type Ia Supernovae from Early Infrared Spectra

Cited by 116 publications

References 23 publications

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

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

Optical and near-IR observations of the faint and fast 2008ha-like supernova 2010ae

Extensive optical and near-infrared observations of the nearby, narrow-lined type Ic SN 2007gr: days 5 to 415

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