Electronic Telegram No. 2214
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
CBAT Director:  Daniel W. E. Green; Room 209; Dept. of Earth and Planetary
 Sciences; Harvard University; 20 Oxford St.; Cambridge, MA  02138; U.S.A.
e-mail:  cbat@iau.org; cbatiau@eps.harvard.edu
URL http://www.cfa.harvard.edu/iau/cbat.html


SUPERNOVAE 2010ap, 2010aq, 2010ar
     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 (= PS1-1000031).

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 Science Consortium (PS1SC) and its member institutions.  The PS1
Surveys have been made possible through the combination of the Institute
for 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.


NOTE: These 'Central Bureau Electronic Telegrams' are sometimes
      superseded by text appearing later in the printed IAU Circulars.

                         (C) Copyright 2010 CBAT
2010 March 20                    (CBET 2214)              Daniel W. E. Green