Astronomska skupina Fakultete za matematiko in fiziko Univerze v Ljubljani
Teleskop Vega
                                                   Electronic Telegram No. 3792
 Central Bureau for Astronomical Telegrams
 CBAT Director:  Daniel W. E. Green; Hoffman Lab 209; Harvard University;
 20 Oxford St.; Cambridge, MA  02138; U.S.A.
 e-mail: (alternate
 Prepared using the Tamkin Foundation Computer Network

 SUPERNOVA 2014J IN M82 = PSN J09554214+6940260
     Stephen J. Fossey, University of London Observatory (ULO), University
 College, London, reports the discovery of an apparent supernova (magnitude R =
 10.5) in the galaxy NGC 3034 = M82 on CCD images obtained by himself (and
 assisted by students B. Cooke, G. Pollack, M. Wilde, and T. Wright) in poor
 sky conditions with a ULO 35-cm Schmidt-Cassegrain telescope (+ SBIG STL-6303E
 camera) at Mill Hill, London, on Jan. 21.805 UT.  The new object is located at
 R.A. = 9h55m42s.14, Decl. = 69d40'26".0 (equinox 2000.0), which is about 54"
 west and 21" south of the center of the galaxy M82.  The variable was
 designated PSN J09554214+6940260 when it was posted at the Central Bureau's
 TOCP webpage and is here designated SN 2014J based on the spectroscopic
 confirmation reported below.  A pre-discovery image taken by Marco Verstraaten
 (Twisk, The Netherlands; 30-cm reflector) on Jan. 18.977 UT has been posted
 at website URL 
     Additional CCD magnitudes for 2014J:  Jan. 12.09 and 12.13, [16 (Fossey;
 broad-band `Luminance' filter; slightly defocussed images); 13.591 UT, [17.0
 (K. Itagaki, Yamagata, Japan; 0.50-m reflector; host-galaxy light extracted
 using previous images; measured by H. Kaneda, Sapporo, Japan; communicated by
 H. Yamaoka, Kyushu University); 14.559, [17.0 (Itagaki); 15.571, 14.4
 (Itagaki; pre-discovery image); 16.641, 13.9 (Itagaki; pre-discovery image);
 17.612, 13.3 (Itagaki; pre-discovery image); 19.618, 12.2 (Itagaki; pre-
 discovery image); 20.620, 11.9 (Itagaki; pre-discovery image); 21.818, V =
 11.7 (Fossey); 22.150, B = 12.96, V = 11.68, R_c = 11.04, I_c = 10.63 (S.
 Kiyota, Kamagaya, Japan; remotely with an iTelescope 0.43-m astrograph +
 FLI-PL6303E camera near Mayhill, NM, USA; image posted at website URL
); 22.3, R = 11.0
 (Ernesto Guido, Nick Howes, and Martino Nicolini; iTelescope 0.50-m f/6.8
 astrograph near Mayhill; position end figures 42s.17, 25".9; reference stars
 from UCAC-3 catalogue; image posted at URL; animated
 image show a comparison with a red Digitized Sky Survey plate from 1998 is
 posted at URL; 22.396, B = 12.9 (L. Elenin, Lyubertsy,
 Russia, and I. Molotov, Moscow; remotely taken with a 0.4-m f/3 telescope at
 the ISON-NM Observatory near Mayhill; position end figures 42s.15 ± 0".13,
 25".8 ± 0".11; UCAC-4 reference stars; image posted at website URL
); 22.406,
 R = 11.3 (Elenin and Molotov); 22.407, I = 11.3 (Elenin and Molotov); 22.410,
 V = 11.7 (Elenin and Molotov); 22.435, 10.9 (Joseph Brimacombe, Cairns,
 Australia; remotely using a 43-cm CDK telescope + STL-6303 camera + infrared
 filter at the New Mexico Skies observatory near Mayhill; bandpass > 700 nm;
 image posted at URL;
 22.466, 11.6 (Brimacombe; 51-cm telescope + STXL-6303 camera + clear filter;
 image posted at;
 22.490, 11.4 (Toshihide Noguchi, Katori, Chiba-ken, Japan; 0.23-m f/6.3
 Schmidt-Cassegrain reflector + BITRAN BT-11E camera; limiting mag 17.5;
 position end figures 42s.18, 25".8; offset 55" west, 21" south of the galaxy
 center; reference stars from UCAC4 catalogue; image posted at website URL
; communicate by S. Nakano,
 Sumoto, Japan); 22.727, 11.2 (Gianluca Masi, Francesca Nocentini, and Patrick
 Schmeer; remotely with a 43-cm telescope near Ceccano, Italy; position end
 figures 42s.14, 25".9); 22.787, B = 12.83, V = 11.49, R_c = 10.86, I_c = 10.47
 (U. Munari, INAF, Padova; and F. Castellani, R. Belligoli, G. L. Righetti,
 ANS Collaboration; 0.4-m telescope); 22.823, B = 12.8 (A. Oksanen, Muurame,
 Finland; via E. O. Waagen, AAVSO); 22.827, V = 11.5 (Oksanen); 22.830, R =
 10.8 (Oksanen); 22.832, I = 10.2 (Oksanen); 22.915, B = 12.76, V = 11.48,
 R_c = 10.79, I_c = 10.43 (Munari et al.).

     G. Dhungana, Southern Methodist University; J. M. Silverman, University
 of Texas at Austin; J. Vinko, University of Szeged; J. C. Wheeler and G. H.
 Marion University of Texas at Austin; and R. Kehoe and F. V. Ferrante,
 Southern Methodist University, on behalf of the ROTSE collaboration, report
 the pre-discovery detection of PSN J09554214+6940260 = SN 2014J in unfiltered
 images taken with the 0.45-m ROTSE-IIIb telescope located at McDonald
 Observatory.  Available magnitudes:  Jan. 7.340 UT, [14.6; 15.378, 13.5;
 17.300, 12.4.  They add that, given the brightness of the host galaxy (M82)
 and the complexity of the field, there is likely some host-galaxy light
 included in these reported magnitudes due to subtraction artifacts.

     R. Itoh, K. Takaki, T. Ui, and K. S. Kawabata, Hiroshima University; and
 M. Yamanaka, Kyoto University, obtained a low-resolution optical spectrogram
 (range 480-900 nm) of PSN J09554214+6940260 = SN 2014J on Jan. 22.4 UT with
 the 1.5-m Kanata telescope (+ HOWPol) at the Higashi-Hiroshima Observatory.  A
 comparison with a library of supernova spectra using GELATO (Harutyunyan et
 al. 2008, A.Ap. 488, 383) suggests that the spectrum is consistent with that
 of a high-velocity type-Ia supernova a week before maximum.  The best match is
 with SN 2002dj at eight days before B-band maximum.  After correction of the
 recession velocity of the host galaxy, it exhibits an absorption line of Si II
 635.5-nm at 604 nm, which corresponds to a line velocity of -15000 km/s. 

     K. Ayani, Bisei Astronomical Observatory (BAO), Ibara, Okayama, Japan,
 obtained a low-resolution spectrogram (range 400-800 nm; resolution 0.6 nm at
 H-alpha) of PSN J09554214+6940260 = SN 2014J with the BAO 1.01-m telescope on
 Jan. 22.5 UT.  The spectrum is that of a type-Ia supernova around or several
 days before maximum, using SNID (Blondin and Tonry 2007, Ap.J. 666, 1024).
 Assuming that a heliocentric velocity for M82 of 203 km/s (de Vaucouleurs et
 al. 1991, RC3.9; via NED), the blueshift of the Si II 635.5-nm absorption
 minimum is about 14000 km/s.  The spectrum has deep Na D absorption. 

     Y. Cao, California Institute of Technology; M. M. Kasliwal, Carnegie
 Institution and Princeton University; A. McKay, University of Texas at
 Austin; and A. Bradley, Apache Point Observatory, on behalf of the
 "intermediate Palomar Transient Factory" (iPTF) Collaboration, report that a
 spectrogram of PSN J09554214+6940260 = SN 2014J, obtained on Jan. 22.305 UT
 with the Dual Imaging Spectrograph on the ARC 3.5-m telescope, indicates that
 the variable is a type-Ia supernova with a Si II velocity of 20000 km/s.  The
 best superfit match (cf. website URL
 is to SN 2002bo at -14 days.  SN 2014J has a red continuum and deep Na D
 absorption.  SN 2014J is not visible in an iPTF image of M82 taken on Jan.
 12 (limiting red mag 20.4).

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

                         (C) Copyright 2014 CBAT
 2014 January 23                  (CBET 3792)              Daniel W. E. Green

                                                 Electronic Telegram No. 3807
 Central Bureau for Astronomical Telegrams
 CBAT Director:  Daniel W. E. Green; Hoffman Lab 209; Harvard University;
 20 Oxford St.; Cambridge, MA  02138; U.S.A.
 e-mail: (alternate
 Prepared using the Tamkin Foundation Computer Network

     D. Li, C. Telesco, and C. Packham, University of Florida, on behalf of
 the CanariCam Science Team, report the first detection at 10 micrometers of
 the type-Ia supernova 2014J in M82 (cf. CBET 3792).  Four 200-s (on-source,
 excluding overhead) exposures -- two at 10.3 micrometers and two at 11.75
 micrometers, were acquired with CanariCam on the 10.4-m Gran Telescopio
 Canarias (GTC) starting at Feb. 10.12 UT.  The supernova is visible at both
 wavelengths and is the only source detected in the imager field-of-view.
 The source location in the field-of-view was 3" from the imager center (i.e.,
 the nominal location of the supernova), which is within the absolute
 pointing accuracy of the telescope that night.  The flux densities of the
 supernova are 7.2 (+/- 2.9) mJy at 10.3 micrometers and 12.4 (+/- 3.0) mJy at
 11.75 micrometers.  The combined value is 9.8 (+/- 2.1) mJy at a nominal
 wavelength of 11.0 micrometers.  These data were obtained using the CanariCam
 Guaranteed Time; the GTC is a joint initiative of Spain, the University of
 Florida, and Mexico.

     Arto Oksanen, Muurame, Finland, reports the following pre-discovery
 magnitudes measured by himself for 2014J from CCD images taken by A.
 Murtovaara (Kiiminki, Finland; 0.25-m f/4 reflector):  Jan. 11.670 UT, [16.0
 (unfiltered); 17.699, R = 13.0; 17.749, G = 13.6; 17.798, B = 15.03; 18.779,
 R = 13.3; 18.741, G = 13.1; 18.681, B = 14.44.  The supernova is saturated in
 the R- and G-band images.
      S. Nakano, Sumoto, Japan, reports the following CCD magnitudes measured
 by Katsumi Yoshimoto (Yamaguchi; 0.16-m f/6.3 reflector + Johnson-Cousins
 filters + STXEi camera) for 2014J:  Jan. 26.754 UT, V = 10.88; 26.756, R_c
 = 10.24; 26.758, I_c = 9.85; 26.761, B = 12.11.
     Visual magnitude estimates:  Jan. 25.875 UT, 11.1 (M. Lehky, Hradec
 Kralove, Czech Republic); 28.817, 10.9 (Patrick Schmeer, Bischmisheim,

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

                         (C) Copyright 2014 CBAT
 2014 February 17                 (CBET 3807)              Daniel W. E. Green
Zadnja sprememba 07.04.2014 20:00 CEST
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