SYNAPPS: Data-Driven Analysis for Supernova Spectroscopy

Thomas, R. C.; Nugent, P.; Meza, Juan C.

doi:10.1086/658673

Cited by 178 publications

(211 citation statements)

References 18 publications

(18 reference statements)

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“…Additional study and confirmation was performed by Syn++ (Thomas et al 2011) modeling of a few of the optical spectra as shown in Figure 19. While the synthetic modeling produces most of the ionic signatures, the most obvious Hα profile is not reproduced.…”

Section: Line Identification and Spectrum Modelingmentioning

confidence: 99%

EXTENSIVE SPECTROSCOPY AND PHOTOMETRY OF THE TYPE IIP SUPERNOVA 2013ej

Dhungana

Kehoe

Vinkó

et al. 2016

ApJ

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We present extensive optical (UBV RI, ¢ ¢ ¢ ¢ g r i z , and open CCD) and near-infrared (ZY JH) photometry for the very nearby Type IIP SN 2013ej extending from +1 to +461 days after shock breakout, estimated to be MJD 56496.9±0.3. Substantial time series ultraviolet and optical spectroscopy obtained from +8 to +135 days are also presented. Considering well-observed SNe IIP from the literature, we derive UBV RIJHK bolometric calibrations from UBV RI and unfiltered measurements that potentially reach 2% precision with a B−V colordependent correction. We observe moderately strong Si II l6355 as early as +8 days. The photospheric velocity (v ph ) is determined by modeling the spectra in the vicinity of Fe II l5169 whenever observed, and interpolating at photometric epochs based on a semianalytic method. This gives =  v 4500 500 ph km s −1 at +50 days. We also observe spectral homogeneity of ultraviolet spectra at +10-12 days for SNe IIP, while variations are evident a week after explosion. Using the expanding photosphere method, from combined analysis of SN 2013ej and SN 2002ap, we estimate the distance to the host galaxy to be -+ 9.0 0.6 0.4 Mpc, consistent with distance estimates from other methods. Photometric and spectroscopic analysis during the plateau phase, which we estimated to be 94±7 days long, yields an explosion energy of 0.9 0.3 10 51 erg, a final pre-explosion progenitor mass of 15.2±4.2  M and a radius of 250±70  R . We observe a broken exponential profile beyond +120 days, with a break point at +183±16 days. Measurements beyond this break time yield a 56 Ni mass of 0.013±0.001M  .

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Section: Line Identification and Spectrum Modelingmentioning

confidence: 99%

EXTENSIVE SPECTROSCOPY AND PHOTOMETRY OF THE TYPE IIP SUPERNOVA 2013ej

Dhungana

Kehoe

Vinkó

et al. 2016

ApJ

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“…To estimate line velocities of select atomic species, we utilize the fast and highly parameterized spectrum synthesis code, SYNAPPS (Thomas et al 2011b). The SYNAPPS model, formerly SYNOW (Fisher 2000), assumes spherical symmetry, a sharp photosphere, pure resonance line scattering treated under the Sobolev approximation, and Boltzmann statistics for electron level populations (parameterized by temp in SYNAPPS).…”

Section: The Synapps Modelmentioning

confidence: 99%

“…In SYNAPPS, quadratic warping constants a0, a1, and a2 supplement t phot to form a more flexible continuum reference level; a0, a1, a2, and t phot form the backbone to data-driven minimization. (See Thomas et al 2011b and Fig. 2 of Parrent et al 2012 for an example.…”

Section: The Synapps Modelmentioning

confidence: 99%

Comparative analysis of SN 2012dn optical spectra: days −14 to +114

Parrent¹,

Howell²,

Fesen³

et al. 2016

Mon. Not. R. Astron. Soc.

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SN 2012dn is a super-Chandrasekhar mass candidate in a purportedly normal spiral (SAcd) galaxy, and poses a challenge for theories of type Ia supernova diversity. Here we utilize the fast and highly parameterized spectrum synthesis tool, SYNAPPS, to estimate relative expansion velocities of species inferred from optical spectra obtained with six facilities. As with previous studies of normal SN Ia, we find that both unburned carbon and intermediate mass elements are spatially coincident within the ejecta near and below 14,000 km s −1 . Although the upper limit on SN 2012dn's peak luminosity is comparable to some of the most luminous normal SN Ia, we find a progenitor mass exceeding ∼ 1.6 M is not strongly favored by leading merger models since these models do not accurately predict spectroscopic observations of SN 2012dn and more normal events. In addition, a comparison of light curves and host-galaxy masses for a sample of literature and Palomar Transient Factory SN Ia reveals a diverse distribution of SN Ia subtypes where carbon-rich material remains unburned in some instances. Such events include SN 1991T, 1997br, and 1999aa where trace signatures of C III at optical wavelengths are presumably detected.

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“…We applied the parameterized resonance scattering code SYN++ in combination with SYNAPPS 3 (Thomas, Nugent & Meza 2011) to model the spectroscopic evolution of SN 2013df (hereafter we refer only to SYNAPPS). Detailed spectral modelling based on this code -or on SYNOW, the original version of these kind of codes (see e.g.…”

Section: Spectral Modellingmentioning

confidence: 99%

The continuing story of SN IIb 2013df: new optical and IR observations and analysis

Szalai

Vinkó

Nagy

et al. 2016

Mon. Not. R. Astron. Soc.

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SN 2013df is a nearby Type IIb supernova that seems to be the spectroscopic twin of the well-known SN 1993J. Previous studies revealed many, but not all interesting properties of this event. Our goal was to add new understanding of both the early and late-time phases of SN 2013df. Our spectral analysis is based on 6 optical spectra obtained with the 9.2m Hobby-Eberly Telescope during the first month after explosion, complemented by a near-infrared spectrum. We applied the SYNAPPS spectral synthesis code to constrain the chemical composition and physical properties of the ejecta. A principal result is the identification of "high-velocity" He I lines in the early spectra of SN 2013df, manifest as the blue component of the double-troughed profile at ∼5650Å. This finding, together with the lack of clear separation of H and He lines in velocity space, indicates that both H and He features form at the outer envelope during the early phases. We also obtained ground-based BVRI and g ′ r ′ i ′ z ′ photometric data up to +45 days and unfiltered measurements with the ROTSE-IIIb telescope up to +168 days. From the modelling of the early-time quasi-bolometric light curve, we find M ej ∼ 3.2−4.6 M ⊙ and E kin ∼ 2.6−2.8 × 10 51 erg for the initial ejecta mass and the initial kinetic energy, respectively, which agree well with the values derived from the separate modelling of the light-curve tail. Late-time mid-infrared excess indicates circumstellar interaction starting ∼1 year after explosion, in accordance with previously published optical, X-ray, and radio data.

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SYNAPPS: Data-Driven Analysis for Supernova Spectroscopy

Cited by 178 publications

References 18 publications

EXTENSIVE SPECTROSCOPY AND PHOTOMETRY OF THE TYPE IIP SUPERNOVA 2013ej

EXTENSIVE SPECTROSCOPY AND PHOTOMETRY OF THE TYPE IIP SUPERNOVA 2013ej

Comparative analysis of SN 2012dn optical spectra: days −14 to +114

The continuing story of SN IIb 2013df: new optical and IR observations and analysis

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