We present the photometric and spectroscopic studies of a Type Ib SN 2015ap and a Type Ic SN 2016P. SN 2015ap is one of the bright (MV =-18.04 mag) Type Ib while SN 2016P lies at an average value among the Type Ic SNe (MV =-17.53 mag). Bolometric light-curve modelling of SNe 2015ap and 2016P indicates that both the SNe are powered by 56Ni + magnetar model with 56Ni masses of 0.01 and 0.002 M⊙, ejecta masses of 3.75 and 4.66 M⊙, spin period P0 of 25.8 and 36.5 ms, and magnetic field Bp of 28.39 × 1014 and 35.3 × 1014 G, respectively. The early spectra of SN 2015ap show prominent lines of He with a 'W' feature due to Fe complexes while other lines of Mg ii, Na i, and Si ii are present in both SNe 2015ap and 2016P. Nebular phase [O i] profile indicates an asymmetric profile in SN 2015ap. The [O i]/[Ca ii] ratio and nebular spectral modelling of SN 2015ap hint towards a progenitor mass between 12 and 20 M⊙. ; BK acknowledges the Science and Engineering Research Board (SERB) under the Department of Science & Technology, Government of India, for financial assistance in the form of National Post-Doctoral Fellowship (Ref. no. PDF/2016/001563). LT is partially supported by the 'PRIN-INAF 2017' with the project 'Towards the SKA and CTA era: discovery, localization, and physics of transient objects'. The work made use of the Swift Optical/Ultraviolet Supernova Archive (SOUSA). SOUSA is supported by NASA's Astrophysics Data Analysis Program through grant NNX13AF35G. SBP and KM acknowledge BRICS grant DST/IMRCD/BRICS/Pilotcall/ProFCheap/2017(G) for this work. NER acknowledges support from the Spanish MICINN grant ESP2017-82674-R and FEDER funds.
We present observations of the unusually luminous Type II supernova (SN) 2016gsd. With a peak absolute magnitude of V = -19.95 +/- 0.08, this object is one of the brightest Type II SNe, and lies in the gap of magnitudes between the majority of Type II SNe and the superluminous SNe. Its light curve shows little evidence of the expected drop from the optically thick phase to the radioactively powered tail. The velocities derived from the absorption in( )H alpha are also unusually high with the blue edge tracing the fastest moving gas initially at 20 000 km s(-1), and then declining approximately linearly to 15000 km s(-1) over similar to 100 d. The dwarf host galaxy of the SN indicates a low-metallicity progenitor which may also contribute to the weakness of the metal lines in its spectra. We examine SN 2016gsd with reference to similarly luminous, linear Type II SNe such as SNe 1979C and 1998S, and discuss the interpretation of its observational characteristics. We compare the observations with a model produced by the JEKYLL code and find that a massive star with a depleted and inflated hydrogen envelope struggles to reproduce the high luminosity and extreme linearity of SN 2016gsd. Instead, we suggest that the influence of interaction between the SN ejecta and circumstellar material can explain the majority of the observed properties of the SN. The high velocities and strong H alpha absorption present throughout the evolution of the SN may imply a circumstellar medium configured in an asymmetric geometry. ; Jenny and AnttiWihuri Foundation Vilho, Yrjo and Kalle Vaisala Fund of the Finnish academy of Science and Letters UCD seed funding scheme SF1518 Science Foundation Ireland Swedish Research Council Villum Fonden 13261 Independent Research Fund Denmark (IRFD) 802100170B Instrument Center for Danish Astronomy (IDA) European Organisation for Astronomical Research in the Southern Hemisphere, Chile as part of PESSTO (the Public ESO Spectroscopic Survey for Transient Objects) ESO program 188.D-3003 191.D-0935 National Aeronautics & Space Administration (NASA) NNX08AR22G National Science Foundation (NSF) AST-1238877 Chinese Academy of Sciences KJCX2-EW-T06 Chinese Astronomical Data Center (CAsDC) National Natural Science Foundation of China 11573003 National Astronomical Observatories of China Chinese Academy of Sciences Special Fund for Astronomy from the Ministry of Finance Science & Technology Facilities Council (STFC) ST/P000312/1 National Aeronautics & Space Administration (NASA) NN12AR55G 80NSSC18K0284 80NSSC18K1575 Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y Turismo de Chile IC120009 CONICYT PAI/INDUSTRIA 79090016 Finnish Cultural Foundation National Science Foundation (NSF) AST-1313484 LSSTC Data Science Fellowship Program - LSSTC NSF Cybertraining Grant 1829740 Brinson Foundation Gordon and Betty Moore Foundation European Union (EU) 839090 European Southern Observatory under ESO programme 0103.D0338(A) EU/FP7-ERC grant 615929
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US under NASA Grant ; National Science Foundation PIRE program grant ; Hubble Fellowship ; KAKENHI of MEXT Japan ; JSPS ; Optical and Near-Infrared Astronomy Inter-University Cooperation Program - MEXT ; UK Science and Technology Facilities Council ; ERC Advanced Investigator Grant ; Lomonosov Moscow State University Development programm ; Moscow Union OPTICA ; Russian Science Foundation ; National Research Foundation of South Africa ; Australian Government Department of Industry and Science and Department of Education (National Collaborative Research Infrastructure Strategy: NCRIS) ; NVIDIA at Harvard University ; University of Hawaii ; National Aeronautics and Space Administration's Planetary Defense Office ; Queen's University Belfast ; National Aeronautics and Space Administration through Planetary Science Division of the NASA Science Mission Directorate ; European Research Council under European Union's Seventh Framework Programme/ERC ; STFC grants ; European Union FP7 programme through ERC ; STFC through an Ernest Rutherford Fellowship ; FONDECYT ; Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) ; NASA in the US ; UK Space Agency in the UK ; Agenzia Spaziale Italiana (ASI) in Italy ; Ministerio de Ciencia y Tecnologia (MinCyT) ; Consejo Nacional de Investigaciones Cientificas y Tecnologicas (CONICET) from Argentina ; USA NSF PHYS ; NSF ; ICREA ; Science and Technology Facilities Council ; UK Space Agency ; National Science Foundation: AST-1138766 ; National Science Foundation: AST-1238877 ; MINECO: AYA2012-39559 ; MINECO: ESP2013-48274 ; MINECO: FPA2013-47986 ; Centro de Excelencia Severo Ochoa: SEV-2012-0234 ; ERC: 240672 ; ERC: 291329 ; ERC: 306478 ; German INTEGRAL through DLR grant: 50 OG 1101 ; US under NASA Grant: NNX15AU74G ; National Science Foundation PIRE program grant: 1545949 ; Hubble Fellowship: HST-HF-51325.01 ; KAKENHI of MEXT Japan: 24103003 ; KAKENHI of MEXT Japan: 15H00774 ; KAKENHI of MEXT Japan: 15H00788 ; JSPS: 15H02069 ; 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UK Space Agency: ST/P002196/1 ; This Supplement provides supporting material for Abbott et al. (2016a). We briefly summarize past electromagnetic (EM) follow-up efforts as well as the organization and policy of the current EM follow-up program. We compare the four probability sky maps produced for the gravitational-wave transient GW150914, and provide additional details of the EM follow-up observations that were performed in the different bands.