Suchergebnisse

We thank the anonymous referee for their comments. W.B.H. acknowledges support from the Research Experience for Undergraduates program at the Institute for Astronomy, University of Hawaii-Manoa, funded through NSF grant #2050710. L.G. acknowledges financial support from the Spanish Ministry of Science, Innovation and Universities (MCIN) under the 2019 Ramon y Cajal program RYC2019-027683 and from the Spanish MCIN project HOSTFLOWS PID2020-115253GA-I00. M.G.M., R.G.D., and S.M.T. were funded by the European Union's Horizon 2020 research and innovation program under the Marie Skodowska-Curie grant agreement No. 839090. Based on observations collected at the European Southern Observatory under ESO program 106.2104. The work of the CSP-II has been generously supported by the National Science Foundation under grant Nos. AST-1008343, AST-1613426, AST-1613455, and AST-1613472. The CSP-II was also supported in part by the Danish Agency for Science and Technology and Innovation through a Sapere Aude Level 2 grant. E.B. was partially supported by NASA grant No. 80NSSC20K0538 J.D.L. acknowledges support from a UK Research and Innovation Fellowship (MR/T020784/1). C.R.B. acknowledges support from NSF grant Nos. AST-1008384, AST-1613426, AST-1613455, and AST-1613472. M.S and S.H. are supported by grants from the VILLUM FONDEN (grant No. 28021) and the Independent Research Fund Denmark (IRFD; 8021-00170B). ; We present optical and near-infrared photometric and spectroscopic observations of the fast-declining Type Ia supernova (SN) 2015bo. SN 2015bo is underluminous (MB=−17.50 ± 0.15 mag) and has a fast-evolving light curve (Δm15(B)=1.91 ± 0.01 mag and sBV=0.48 ± 0.01). It has a unique morphology in the observed V −r color curve, where it is bluer than all other supernovae (SNe) in the comparison sample. A 56Ni mass of 0.17±0.03Me was derived from the peak bolometric luminosity, which is consistent with its location on the luminosity–width relation. Spectroscopically, SN 2015bo is a cool SN in the Branch classification scheme. The velocity evolution measured from spectral features is consistent with 1991bg-like SNe. SN 2015bo has a SN twin (similar spectra) and sibling (same host galaxy), SN 1997cn. Distance moduli of μ=34.33±0.01 (stat)± 0.11 (sys) mag and μ=34.34±0.04 (stat)±0.12 (sys) mag are derived for SN 2015bo and SN 1997cn, respectively. These distances are consistent at the 0.06σ level with each other, and they are also consistent with distances derived using surface-brightness fluctuations and redshift-corrected cosmology. This suggests that fast-declining SNe could be accurate distance indicators, which should not be excluded from future cosmological analyses. ; Research Experience for Undergraduates program at the Institute for Astronomy, University of Hawaii-Manoa ; National Science Foundation (NSF) AST-1008384 AST-1613426 AST-1613455 AST-1613472 ; Spanish Ministry of Science, Innovation and Universities (MCIN) RYC2019-027683 ; Spanish MCIN project HOSTFLOWS PID2020-115253GA-I00 ; European Union's Horizon 2020 research and innovation program under the Marie Skodowska-Curie 839090 106.2104 ; National Science Foundation (NSF) AST-1613426 AST-1613455 AST-1613472 AST-1008343 ; Danish Agency for Science and Technology and Innovation through a Sapere Aude Level 2 grant ; National Aeronautics & Space Administration (NASA) 80NSSC20K0538 ; UK Research and Innovation Fellowship MR/T020784/1 ; Villum Fonden 28021 ; Independent Research Fund Denmark 8021-00170B