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We have analyzed XMM-Newton, Chandra, and Suzaku observations of Kepler'ssupernova remnant (SNR) to investigate the properties of both the SN ejecta andthe circumstellar medium (CSM). For comparison, we have also analyzed twosimilarly-aged, ejecta-dominated SNRs: Tycho's SNR, thought to be the remnantof a typical Type Ia SN, and SNR 0509-67.5 in the Large Magellanic Cloud,thought to be the remnant of an overluminous Type Ia SN. By simply comparingthe X-ray spectra, we find that line intensity ratios of iron-group elements(IGE) to intermediate-mass elements (IME) for Kepler's SNR and SNR 0509-67.5are much higher than those for Tycho's SNR. We therefore argue that Kepler isthe product of an overluminous Type Ia SN. This inference is supported by ourspectral modeling, which reveals the IGE and IME masses respectively to be~0.95 M_sun and ~0.12 M_sun (Kepler's SNR), ~0.75 M_sun and ~0.34 M_sun (SNR0509-67.5), and ~0.35 M_sun and ~0.70 M_sun (Tycho's SNR). We find that the CSMcomponent in Kepler's SNR consists of tenuous diffuse gas (~0.3 M_sun) presentthroughout the entire remnant, plus dense knots (~0.035 M_sun). Both of thesecomponents have an elevated N abundance (N/H ~ 4 times the solar value),suggesting that they originate from CNO-processed material from the progenitorsystem. The mass of the diffuse CSM allows us to infer the pre-SN mass-lossrate to be ~1.5e-5 (V_w/10 km/s) M_sun/yr, in general agreement with resultsfrom recent hydrodynamical simulations. Since the dense knots have slow propermotions and relatively small ionization timescales, they were likely located afew pc away from the progenitor system. Therefore, we argue that Kepler's SNwas an overluminous event that started to interact with massive CSM a fewhundred years after the explosion. This supports the possible link betweenoverluminous SNe and the so-called "Ia-CSM" SNe.

Kepler's Supernova: An Overluminous Type Ia Event Interacting with a Massive Circumstellar Medium at a Very Late Phase