Matsuura, M. ; Dwek, E. ; Barlow, M. J. ; Babler, B. ; Baes, M. ; Meixner, M. ; Cernicharo, J. ; Clayton, G. C. ; Dunne, L. ; Fransson, C. ; Fritz, J. ; Gear, W. ; Gomez, H. L. ; Groenewegen, M. A. T. ; Indebetouw, R. ; Ivison, R. J. ; Jerkstrand, A. ; Lebouteiller, V. ; Lim, T. L. ; Lundqvist, P. ; Pearson, C. P. ; Roman-Duval, J. ; Royer, P. ; Staveley-Smith, L. ; Swinyard, B. M. ; van Hoof, P. A. M. ; van Loon, J. T. ; Verstappen, J. ; Wesson, R. ; Zanardo, G. ; Blommaert, J. A. D. L. ; Decin, L. ; Reach, W. T. ; Sonneborn, G. ; Van de Steene, G. C. ; Yates, J. A.

published in The Astrophysical Journal, 800, pp. 50 (2015)

Abstract: We present new Herschel photometric and spectroscopic observations of Supernova 1987A, carried out in 2012. Our dedicated photometric measurements provide new 70 µm data and improved imaging quality at 100 and 160 µm compared to previous observations in 2010. Our Herschel spectra show only weak CO line emission, and provide an upper limit for the 63 µm [O I] line flux, eliminating the possibility that line contaminations distort the previously estimated dust mass. The far-infrared spectral energy distribution (SED) is well fitted by thermal emission from cold dust. The newly measured 70 µm flux constrains the dust temperature, limiting it to nearly a single temperature. The far-infrared emission can be fitted by 0.5 ± 0.1 M ? of amorphous carbon, about a factor of two larger than the current nucleosynthetic mass prediction for carbon. The observation of SiO molecules at early and late phases suggests that silicates may also have formed and we could fit the SED with a combination of 0.3 M ? of amorphous carbon and 0.5 M ? of silicates, totalling 0.8 M ? of dust. Our analysis thus supports the presence of a large dust reservoir in the ejecta of SN 1987A. The inferred dust mass suggests that supernovae can be an important source of dust in the interstellar medium, from local to high-redshift galaxies. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC and UKSA (UK); and NASA (USA).

DOI: 10.1088/0004-637X/800/1/50
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