The reliability of Type Ia Supernovae (SNe Ia) may be limited by the imprint of their galactic origins. To investigate the connection between supernovae and their host characteristics, we developed ...an improved method to estimate the stellar population age of the host as well as the local environment around the site of the supernova. We use a Bayesian method to estimate the star formation history and mass weighted age of a supernova's environment by matching observed spectral energy distributions to a synthesized stellar population. Applying this age estimator to both the photometrically and spectroscopically classified Sloan Digital Sky Survey II supernovae (N = 103), we find a 0.114 0.039 mag "step" in the average Hubble residual at a stellar age of ∼8 Gyr; it is nearly twice the size of the currently popular mass step. We then apply a principal component analysis on the SALT2 parameters, host stellar mass, and local environment age. We find that a new parameter, PC1, consisting of a linear combination of stretch, host stellar mass, and local age, shows a very significant (4.7 ) correlation with Hubble residuals. There is a much broader range of PC1 values found in the Hubble flow sample when compared with the Cepheid calibration galaxies. These samples have mildly statistically different average PC1 values, at ∼2.5 , resulting in at most a 1.3% reduction in the evaluation of H0. Despite accounting for the highly significant trend in SN Ia Hubble residuals, there remains a 9% discrepancy between the most recent precision estimates of H0 using SN Ia and the CMB.
We present 2603 spectra of 462 nearby Type Ia supernovae (SNe Ia), including 2065 previously unpublished spectra, obtained during 1993-2008 through the Center for Astrophysics Supernova Program. ...Based on nebular spectra of 27 SNe Ia, we find no relation between the FWHM of the iron emission feature at ~4700A and delta msub 15(B) after removing the two low-luminosity SN 1986G and SN 1991bg, suggesting that the peak luminosity is not strongly dependent on the kinetic energy of the explosion for most SNe Ia. Finally, we confirm the correlation of velocity shifts in some nebular lines with the intrinsic B-V color of SNe Ia at maximum light, although several outliers suggest a possible non-monotonic behavior for the largest blue-shifts.
Using the Hubble Space Telescope (HST) and the Large Binocular Telescope, we followed the evolution of the Type Ia supernova (SN Ia) 2011fe for an unprecedented 1840 days past B-band maximum light ...and over a factor of 7 million in flux. At 1840 days, the 4000 - 17000 quasi-bolometric luminosity is just ( 420 20 ) L . By measuring the late-time quasi-bolometric light curve, we present the first confident detection of 57Co decay in a SN Ia light curve and estimate a mass ratio of log ( 57 Co 56 Co ) = − 1.59 − 0.07 + 0.06 . We do not have a clean detection of 55 Fe , but find a limit of 55 Fe 57 Co < 0.22 with 99% confidence. These abundance ratios provide unique constraints on the progenitor system because the central density of the exploding white dwarf(s) dictates these nucleosynthetic yields. The observed ratios strongly prefer the lower central densities of double-degenerate models ( 55 Fe 57 Co = 0.27 ) over the higher central densities of near-Chandrasekhar-mass single-degenerate models ( 55 Fe 57 Co = 0.68 ). However, additional theoretical studies predicting isotopic yields from a broader range of progenitor systems are motivated by these unique observations. We will continue to observe SN 2011fe for another ∼600 days with HST and possibly beyond.
Spectra and light curves of SN 2006gz show the strongest signature of unburned carbon and one of the slowest fading light curves ever seen in a Type Ia event Delta m sub(15)(B) = 0.69 plus or minus ...0.04. The early-time Si II velocity is low, implying it was slowed by an envelope of unburned material. Our best estimate of the luminosity implies M sub(v) = -19.74 and the production of similar to 1.2 M unk of super(56)Ni. This suggests a super-Chandrasekhar mass progenitor. A double degenerate merger is consistent with these observations.
Abstract
Type Ia supernovae (SNe Ia) are standardizable candles, but for over a decade there has been a debate on how to properly account for their correlations with host galaxy properties. Using the ...Bayesian hierarchical model UNITY, we simultaneously fit for the SN Ia light curve and host galaxy standardization parameters on a set of 103 Sloan Digital Sky Survey II SNe Ia. We investigate the influences of host stellar mass, along with both localized (
r
<3 kpc) and host-integrated average stellar ages, derived from stellar population synthesis modeling. We find that the standardization for the light-curve shape (
α
) is correlated with host galaxy standardization terms (
γ
i
) requiring simultaneous fitting. In addition, we find that these correlations themselves are dependent on host galaxy stellar mass that includes a shift in the color term (
β
) of 0.8 mag, only significant at 1.2
σ
due to the small sample. We find a linear host mass standardization term at the 3.7
σ
level, that by itself does not significantly improve the precision of an individual SN Ia distance. However, a standardization that uses both stellar mass and average local stellar age is found to be significant at >3
σ
in the two-dimensional posterior space. In addition, the unexplained scatter of SNe Ia absolute magnitude post standardization, is reduced from
to 0.109 ± 0.017 mag, or ∼10%. We do not see similar improvements when using global ages. This combination is consistent with either metallicity or line-of-sight dust affecting the observed luminosity of SNe Ia.
ABSTRACT
We report XMM–Newton and TESS observations of V496 UMa, an AM Herculis-type cataclysmic variable. The XMM–Newton observation reveals that at times, two poles on the white dwarf accrete ...simultaneously, but accretion on to the secondary magnetic pole is erratic and can nearly cease in less than one binary orbit (1.5 h). Modelling of the X-ray spectrum during the primary maximum reveals no change in the accretion structures on to the primary pole when accretion on to the secondary pole is disrupted, suggesting that the disruption of accretion on to the secondary pole may be caused by mass-transfer variations from the donor star. The TESS observation, which spanned eight weeks at a 2-min cadence, shows a stable, double-humped orbital modulation due to cyclotron emission from the post-shock region, while the observed times of maximum light show a slow systematic drift that does not correlate with the system’s overall brightness.
A series of optical and one near-infrared nebular spectra covering the first year of the Type Ia supernova SN 2011fe are presented and modelled. The density profile that proved best for the early ...optical/ultraviolet spectra, '...-11fe', was extended to lower velocities to include the regions that emit at nebular epochs. Model ...-11fe is intermediate between the fast deflagration model W7 and a low-energy delayed-detonation. Good fits to the nebular spectra are obtained if the innermost ejecta are dominated by neutron-rich, stable Fe-group species, which contribute to cooling but not to heating. The correct thermal balance can thus be reached for the strongest FeII and FeIII lines to be reproduced with the observed ratio. The ... mass thus obtained is ~0.47 plus or minus 0.05 M... The bulk of 56Ni has an outermost velocity of ~8500 km s... The mass of stable iron is ~0.23 plus or minus 0.03 M... Stable Ni has low abundance, ... This is sufficient to reproduce an observed emission line near 7400 A. A sub-Chandrasekhar explosion model with mass ... and no central stable Fe does not reproduce the observed line ratios. A mock model where neutron-rich Fe-group species are located above 56Ni following recent suggestions is also shown to yield spectra that are less compatible with the observations. The densities and abundances in the inner layers obtained from the nebular analysis, combined with those of the outer layers previously obtained, are used to compute a synthetic bolometric light curve, which compares favourably with the light curve of SN 2011fe. (ProQuest: ... denotes formulae/symbols omitted.)
ABSTRACT We discovered two transient events in the Kepler field with light curves that strongly suggest they are type II-P supernovae (SNe II-P). Using the fast cadence of the Kepler observations we ...precisely estimate the rise time to maximum for KSN2011a and KSN2011d as 10.5 0.4 and 13.3 0.4 rest-frame days, respectively. Based on fits to idealized analytic models, we find the progenitor radius of KSN2011a (280 20 R ) to be significantly smaller than that for KSN2011d (490 20 R ), but both have similar explosion energies of 2.0 0.3 × 1051 erg. The rising light curve of KSN2011d is an excellent match to that predicted by simple models of exploding red supergiants (RSG). However, the early rise of KSN2011a is faster than the models predict, possibly due to the supernova shock wave moving into pre-existing wind or mass-loss from the RSG. A mass-loss rate of 10−4M yr−1 from the RSG can explain the fast rise without impacting the optical flux at maximum light or the shape of the post-maximum light curve. No shock breakout emission is seen in KSN2011a, but this is likely due to the circumstellar interaction suspected in the fast rising light curve. The early light curve of KSN2011d does show excess emission consistent with model predictions of a shock breakout. This is the first optical detection of a shock breakout from a SNe II-P.
ABSTRACT Due to its proximity, SN 1987A offers a unique opportunity to directly observe the geometry of a stellar explosion as it unfolds. Here we present spectral and imaging observations of SN ...1987A obtained ∼10,000 days after the explosion with HST/STIS and VLT/SINFONI at optical and near-infrared wavelengths. These observations allow us to produce the most detailed 3D map of H to date, the first 3D maps for Ca ii , O i , and Mg ii , as well as new maps for Si i+Fe ii and He i 2.058 m. A comparison with previous observations shows that the Si i+Fe ii flux and morphology have not changed significantly during the past ten years, providing evidence that this line is powered by 44Ti. The time evolution of H shows that it is predominantly powered by X-rays from the ring, in agreement with previous findings. All lines that have sufficient signal show a similar large-scale 3D structure, with a north-south asymmetry that resembles a broken dipole. This structure correlates with early observations of asymmetries, showing that there is a global asymmetry that extends from the inner core to the outer envelope. On smaller scales, the two brightest lines, H and Si i+Fe ii 1.644 m, show substructures at the level of ∼200-1000 km s-1and clear differences in their 3D geometries. We discuss these results in the context of explosion models and the properties of dust in the ejecta.
We present 645 optical spectra of 73 supernovae (SNe) of Types IIb, Ib, Ic, and broad-lined Ic. All of these types are attributed to the core collapse of massive stars, with varying degrees of intact ...H and He envelopes before explosion. The SNe in our sample have a mean redshift left angle bracketczright angle bracket = 4200 km s super(-1). Most of these spectra were gathered at the Harvard-Smithsonian Center for Astrophysics (CfA) between 2004 and 2009. For 53 SNe, these are the first published spectra. The data coverage ranges from mere identification (1-3 spectra) for a few SNe to extensive series of observations (10-30 spectra) that trace the spectral evolution for others, with an average of 9 spectra per SN. For 44 SNe of the 73 SNe presented here, we have well-determined dates of maximum light to determine the phase of each spectrum. Our sample constitutes the most extensive spectral library of stripped-envelope SNe to date. We provide very early coverage (as early as 30 days before V-band max) for photospheric spectra, as well as late-time nebular coverage when the innermost regions of the SN are visible (as late as 2 yr after explosion, while for SN 1993J, we have data as late as 11.6 yr). This data set has homogeneous observations and reductions that allow us to study the spectroscopic diversity of these classes of stripped SNe and to compare these to SNe-gamma-ray bursts. We undertake these matters in follow-up papers.
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