SIMBAD references

Further to CBET 2012, S. Valenti, M. Fraser, D. Young, K. Smith, and M. T. Botticella, Queen's University, Belfast (QUB); R. Chornock, R. Foley, A. Rest, and G. Narayan, Harvard-Smithsonian Center for Astrophysics (CfA); M. Huber, Johns Hopkins University (JHU); S. Smartt, QUB; J. Tonry and P. A. Price, Institute for Astronomy, University of Hawaii; C. Stubbs, CfA; A. Riess, JHU; and W. M. Wood-Vasey, University of Pittsburgh, report the discovery of three additional spectroscopically-confirmed supernovae in the Pan-STARRs Medium Deep Survey. Spectra were obtained at the William Herschel Telescope (+ ISIS; range 320-1000 nm) on Feb. 22.12 UT for SN 2010ar (= PS1-1000022), on Feb. 23.06 for SN 2010aq (= PS1-1000026), and on Feb. 23.16 for SN 2010ap

---------------------------------------------------------------------------— SN 2010 UT R.A. (2000.0) Decl. Mag. Type z ---------------------------------------------------------------------------— 2010ap Feb. 12.4 8 36 12.606 +44 00 25.51 20.4 Ia 0.14 2010aq Feb. 15.4 10 02 09.744 + 1 14 00.92 21.0 IIP 0.088 2010ar Feb. 15.4 10 03 26.060 + 1 01 46.20 19.2 Ia 0.09 ---------------------------------------------------------------------------—

SN 2010ar is located 3".58 east and 2".79 north of the center of its host galaxy; SN 2010aq is located < 0".1 east and 0".3 north of the center of its host galaxy. The spectra were compared with a library of supernova spectra using the "GELATO" code (Harutyunyan et al. 2008, A.Ap. 488, 383). For SN 2010ar, the spectrum closely matches that of the type-Ia supernova 2007ap (cf. CBETs 883, 887) around maximum light at redshift z = 0.09. For SN 2010aq, the best match is found with the type-IIP supernova 2004et at three days before maximum light; the redshift of SN 2010aq, measured from the narrow Balmer emission lines of the host galaxy (SDSS J100209.73+011400.5), is z = 0.088. For SN 2010ap, the spectrum is similar to that of the type-Ia supernova 1989B (Barbon et al. 1990, A.Ap. 237, 79) at a redshift of z = 0.14, two weeks after maximum light.

These discoveries were enabled using the PS1 System operated by the PS1 Astronomy at the University of Hawaii; The Pan-STARRS Project Office; the Max-Planck Society and its participating institutes (the Max Planck Institute for Astronomy, Heidelberg, and the Max Planck Institute for Extraterrestial Physics, Garching); The Johns Hopkins University; the University of Durham; the University of Edinburgh; the Queen's University of Belfast; the Harvard-Smithsonian Center for Astrophysics; the Las Cumbres Observatory Global Network; and the National Central University of Taiwan. The staffs at the PS1 and Nordic Optical Telescope are thanked for their assistance in obtaining these observations.