Normal or transitional? The evolution and properties of two type Ia supernovae in the Virgo cluster

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Abstract
Type Ia supernovae (SNe Ia) are among the most precise cosmological distance indicators used to study the expansion history of the Universe. The vast increase in SN Ia data due to large-scale astrophysical surveys has led to the discovery of a wide variety of SN Ia sub-classes, such as transitional and fast-declining SNe Ia. However, their distinct photometric and spectroscopic properties differentiate them from the population of normal SNe Ia such that their use as cosmological tools remains challenged. Here, we present a high-cadenced photometric and spectroscopic dataset of two SNe Ia, SNe 2020ue and 2020nlb, which were discovered in the nearby Virgo cluster of galaxies. Our study shows that SN 2020nlb is a normal SN Ia whose unusually red colour is intrinsic, arising from a lower photospheric temperature rather than interstellar reddening, providing clear evidence that colour diversity among normal SNe Ia can have a physical origin. In contrast, SN 2020ue has photometric properties, such as colour evolution and light curve decay rate, similar to those of transitional SNe. It is hence more spectroscopically aligned with normal SNe Ia. This is evident from spectroscopic indicators such as the pseudo-equivalent width of Si II lines. Thus, such SNe Ia, which lie photometrically at the edge of the standard normal SNe Ia range, may be missed in cosmological SNe Ia samples. Our results highlight that a spectroscopic analysis of SNe Ia around peak brightness is crucial for identifying intrinsic colour variations and constructing a more complete and physically homogeneous SN Ia sample for precision cosmology.
Funding Information
  • NASA (80NSSC23K0301)
  • NASA (80NSSC24K1411)
  • NSF (AST--1815935)
  • NSF (AST--1720756)
  • Marie Skłodowska-Curie Grant Agreemen (873089)
  • Villum Fonden (VIL69896)
  • Villum Fonden (VIL16599)
  • Villum Fonden (VIL54489)
  • National Science Foundation (1842402)
  • National Science Foundation (2236415)
  • INAF (1.05.23.05.15)
  • European Research Council (101002652)
  • UK Research and Innovation (EP/Z000475/1)
  • NSF (AST--2407632)
  • NSF (AST--2429450)
  • NASA (80NSSC24M0023)
  • HST (HST-GO-17128.028)
  • HST (HST-GO-16269.012)
  • JWST (JWST-GO-05324.031)
  • NSF (AST--2432037)
  • HST (HST-SNAP-17070)
  • HST (HST-GO-17706)
  • JWST (JWST-AR-6241)
  • JWST (JWST-AR-5441)
  • NSF CAREER (AST--2239364)
  • NSF (AST--2206195)
  • NSF (OAC--2311355)
  • NSF (AST--2432428)
  • NSF (AST--2421845)
  • HST (HST-GO-16764)
  • STFC (ST/Y001605/1)
  • Heising-Simons Foundation (2018-0913)
  • Heising-Simons Foundation (2018-0911)
  • NASA (NNG17PX03C)
  • NSF (AST--1909796)
  • NSF (AST--1944985)
  • NASA SSO Near Earth Observation Program (80NSSC18K0971)
  • NASA SSO Near Earth Observation Program (NNX14AM74G)
  • NASA SSO Near Earth Observation Program (NNX12AR65G)
  • NASA SSO Near Earth Observation Program (NNX13AQ47G)
  • NASA SSO Near Earth Observation Program (NNX08AR22G)
  • NASA SSO Near Earth Observation Program (80NSSC21K1572)
  • NSF (DGE-1339067)

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