IAU Central Bureau for Astronomical Telegrams

Central Bureau for Astronomical Telegrams -- Image credits

CBAT Possible-Supernovae Page

Following discussions between the CBAT and the IAU Working Group on Supernovae (WGS) in 2003, it was agreed that a mutual CBAT/WGS mirrored interactive website would be created by WGS members by the end of 2003, in order to address the growing problem of many faint, unconfirmed supernova suspects that have been reported in recent years mostly by the high-z surveys. The interactive webpage, when completed, will permit registered users to post their spectroscopically unconfirmed discovery reports of faint objects (fainter than mag 19 or 20) immediately onto a webpage that will be accessible to all professional astronomers using large telescopes. Because the CBAT/WGS interactive website is not yet working, the CBAT has created this temporary non-interactive website that is being maintained entirely by the CBAT. Pending objects will be posted here until the interactive webpage is up and working.

There is a new provisional designation scheme that will be employed for faint objects that have not been spectroscopically confirmed as supernovae, of the form LYYMM-nnn, where L stands for the century (K = 2000, J = 1900, etc.), YY is for the last two digits of the year, MM is for the month (with leading zeroes through September), and nnn is a consecutive number (with leading zeroes for numbers < 100) for the order in which objects are catalogued in that month. Contributors are requested to adhere strictly to the format listed below, placing all data in the proper columns; for designation, leave the consecutive number after LYYMM as simply "nnn", and the appropriate number will be assigned before posting on this webpage. Reference to the individual objects can then be made as "PSN LYYMM-nnn".


The observations of possible supernovae are listed below in plain ASCII text (with NO tabs!) in a 98-column format. Note the following template to guide you in producing a similar list to send for inclusion.

                                                                                               
         1         2         3         4         5         6         7         8         9          
123456789 123456789 123456789 123456789 123456789 123456789 123456789 123456789 123456789 123456    
PSN        DATE (UT)         R.A. (2000.0) Decl.     Mag.    OFFSET       REPORTER            NOTES 
KYYMM-nnn  YYYY MM DD.DDD  hh mm ss.ss +oo '' ""."  MM.MLx rr.rD rr.rD    Person sending text nnnn  
                                                                                                    

Above, the date (given as year, month, date in Universal Time) should be given to 0.01 or 0.001 day, with leading zeroes if appropriate, in columns 12-25. The right ascension (columns 28-38) and declination (columns 40-50) should be given to full precision (0s.01 in R.A. and 0".1 in Decl.), with leading zeroes if appropriate. The magnitude should be given to tenths in columns 53-56, with column 57 for the bandpass (and column 58 for any additional bandpass character); use usual upper- and lower-letter band letters, and use "U" for unfiltered CCD. The offset (columns 60-64 for right ascension and columns 66-70 for declination) of the new object from the center of the nearest visible host galaxy should be given in arc seconds for both R.A. and Decl., with the values given to 0".1 and the directional letters (E = east = 90 degrees clockwise from north toward south, and W = west for R.A. offsets; N = north and S = south for Decl. offsets) specified. The person(s) who actually send the e-mail with the discovery should be placed (first initial, full last name) in columns 75-93. Columns 95 onwards contain the CBAT published source, if any. Additional information (including the name of the survey, any other contributing astronomers, and important succinct details regarding reference images and their dates and limiting magnitudes, etc.) is given in the notes below.


Below are listed (temporarily) such unconfirmed observations, so that interested observers may attempt confirming observations. Please report any observations (negative or positive) promptly to the CBAT at e-mail address cbat@cfa.harvard.edu.

                                                                                               
         1         2         3         4         5         6         7         8         9          
123456789 123456789 123456789 123456789 123456789 123456789 123456789 123456789 123456789 123456    
PSN        DATE (UT)         R.A. (2000.0) Decl.     Mag.    OFFSET       REPORTER        PUBLISHED
                                                                                                    
                                                                                                    
PSN        DATE (UT)         R.A. (2000.0) Decl.     Mag.    OFFSET       REPORTER        PUBLISHED
J9711-001  1997 11 28.9    10 27 51.45 -43 54 18.5  12.3K   4  E  3  S    S. Lipari
                                                                                                    
K0210-001  2002 10 16.3    02 34 13.34 +29 18 36.2  14.7K'        5  S    C. C. Dudley    IAUC 8992

K0211-001  2002 11 03      02 16 26.37 -05 04 32.5  26.1i     no host     M. Doi      
K0211-002  2002 11 03      02 17 16.18 -05 06 02.7  26.2i     no host     M. Doi      
K0211-003  2002 11 03      02 18 52.36 -05 01 13.2  24.8i     no host     M. Doi      
K0211-004  2002 11 03      02 20 13.92 -05 07 36.0  25.6i     no host     M. Doi      
                                                                                                    
K0302-001  2003 02 10.12   03 32 37.03 -27 56 53.9  24.4z   0.13E         L. Strolger

K0304-001  2003 04 17.4    15 15 06.97 +42 12 19.3  17.7K' 20  E 17  S    C. C. Dudley    IAUC 8992
                                                                                                    
K0306-001  2003 06 22.5    22 14 24.02 -17 46 36.0  23.5i   0.2W          P. Astier   
K0306-002  2003 06 22.5    22 16 09.91 -18 04 39.1  23.4i   0.2W  0.1S    P. Astier   
K0306-003  2003 06 22.5    22 16 41.55 -17 26 10.6  23.2i   0.2W  0.2S    P. Astier   
K0306-004  2003 06 26.3    14 21 54.20 +52 58 49.7  24.0i   0.1E  0.2S    P. Astier   
K0306-005  2003 06 30.5    22 15 28.14 -17 49 48.6  24.6i   1.0W  0.4S    P. Astier   
                                                                                                    
K0404-001  2004 04 02.08   12 36 20.90 +62 10 19.6  25.4z'  0.5W  0.5S    R. Gibbons  
K0404-002  2004 04 02.08   12 36 25.93 +62 09 37.4  23.7z'  0.0E  0.7S    R. Gibbons  
K0404-003  2004 04 02.08   12 36 29.44 +62 11 41.9  24.4z'  0.0W  0.0N    R. Gibbons  
K0404-004  2004 04 02.74   12 36 19.86 +62 13 48.0  25.1z'  0.1E  0.1S    R. Gibbons  
K0404-005  2004 04 02.74   12 36 27.07 +62 15 09.6  24.4z'  0.2E  0.1S    R. Gibbons  
K0404-006  2004 04 03.40   12 37 06.73 +62 21 17.8  25.4z'  0.0W  0.0S    R. Gibbons  
K0404-007  2004 04 03.40   12 37 09.44 +62 22 15.6  25.1z'  0.3E  0.8N    R. Gibbons  
K0404-008  2004 04 03.34   12 38 03.58 +62 17 11.9  24.7z'  1.0W  0.2N    R. Gibbons  
K0404-009  2004 04 03.54   12 37 21.32 +62 09 35.2  25.7z'  0.1W  0.1N    R. Gibbons  
K0404-010  2004 04 04.71   12 36 46.07 +62 16 25.7  25.8z'  0.1E  0.2S    R. Gibbons  
K0404-011  2004 04 04.71   12 36 49.36 +62 16 04.8  24.9z'  0.0E  0.0S    R. Gibbons  
                                                                                                    
K0405-001  2004 05 21.24   12 35 50.78 +62 10 38.2  24.5z'  0.1E  0.3N    L. Strolger 
K0405-002  2004 05 20.24   12 36 26.66 +62 08 30.2  25.0z'  0.4W  0.0N    L. Strolger 
K0405-003  2004 05 20.13   12 36 34.33 +62 12 13.0  22.5z'  0.8W  0.2S    L. Strolger 
K0405-004  2004 05 21.31   12 36 34.81 +62 15 49.0  23.3z'  0.7W  0.1S    L. Strolger 
K0405-005  2004 05 21.31   12 36 35.96 +62 17 32.3  25.6z'  0.2W  0.4S    L. Strolger 
K0405-006  2004 05 23.67   12 36 54.11 +62 08 22.8  24.8z'  0.1E  0.3N    L. Strolger 
K0405-007  2004 05 21.44   12 36 58.45 +62 16 37.3  23.7z'  0.0E  0.0N    L. Strolger 
K0405-008  2004 05 20.78   12 37 33.86 +62 19 22.3  23.8z'  0.0E  0.0N    L. Strolger 
K0405-009  2004 05 21.18   12 37 52.67 +62 14 08.2  25.6z'  0.1W  0.0N    L. Strolger 
K0405-010  2004 05 21.18   12 37 48.38 +62 13 35.4  23.2z'  0.1W  0.2N    L. Strolger 
                                                                                                    
K0409-001  2004 09 13.1    18 32 41.24 -34 11 26.6  18.7Ks  1.1E  0.8N    S. Matilla     CBET 858
K0409-002  2004 09 23.0    17 16 35.89 -10 20 37.9  18.3J   1.5E  1.1N    S. Matilla  
                                                                                                    
K0504-001  2005 04 02.456  16 02 11.01 +42 55 05.5  17.9Rc  4.6E  6.6S    R. Jansen      IAUC 8512
                                                                                                    
K0508-001  2005 08 08.5    00 09 34.7  +12 45 21.4  19.7U                 G. Aldering    CBET 214
                                                                                                    
K0509-001  2005 09 10      21 26 16.30 -00 33 14.7  20.9r   0.6E  0.6S    J. Frieman         
                                                                                                    
K0810-001  2008 10 30.51   10 05 00.27 +14 22 49.9  18.3U   0.9E  0.1S    A. Drake       CBET 1682

K0811-001  2008 11 18.18   02 53 14.87 +20 06 13.2  18.9U   1.4W  0.3N    A. Drake       CBET 1682
K0811-002  2008 11 19.21   01 30 54.81 -01 42 08.2  19.2U                 A. Drake       CBET 1682
K0811-003  2008 11 19.21   01 59 30.24 -01 26 21.3  18.3U   0.2W  0.7S    A. Drake       CBET 1682
K0811-004  2008 11 30.34   08 28 17.16 +30 24 54.1  19.7U   4.5N  0.1S    A. Drake       CBET 1682

K0812-001  2008 12 01.27   02 37 59.31 +01 30 29.3  18.4U   0.9E          A. Drake       CBET 1682
K0812-002  2008 12 01.52   10 33 53.80 -03 21 25.4  18.3U   0.5W  1.1N    A. Drake       CBET 1682
K0812-003  2008 12 04.52   11 09 32.94 +27 24 40.3  18.1U   0.1N          A. Drake       CBET 1682
K0812-004  2008 12 20.17   02 16 52.47 +13 55 00.7  17.9U   0.3E  0.8S    A. Drake       CBET 1682
K0812-005  2008 12 22.55   12 11 50.13 +15 54 51.3  19.4U   0.7E  0.7N    A. Drake       CBET 1682
K0812-006  2008 12 29.55   13 45 26.56 -10 43 52.8  17.9U                 A. Drake       CBET 1682

K0901-001  2009 01 02.52   13 00 37.49 +17 50 57.0  18.9U                 A. Drake       CBET 1682

K0903-001  2009 03 21.186  11 16 34.27 +03 32 02.8  20.1g   0.2W  2.1N    R. Quimby      CBET 1754
K0903-002  2009 03 26.209  14 30 50.42 +35 37 31.4  18.8g   4.2E  3.3S    R. Quimby      CBET 1754
K0903-003  2009 03 26.230  14 10 18.54 +16 53 38.8  19.0g   4.7E  3.9N    R. Quimby      CBET 1754

K0905-001  2009 05 17.229  14 57 03.10 +49 36 40.8  19.4R      --         M. Kasliwal    CBET 1820
K0905-002  2009 05 17.244  17 36 44.27 +53 40 12.0  20.3R   1.4W  3.5S    M. Kasliwal    CBET 1820
K0905-003  2009 05 20.288  14 32 14.64 +54 51 19.5  20.3R   3.5W  2.2N    M. Kasliwal    CBET 1820
K0905-004  2009 04 24.34   12 43 52.36 +24 27 49.2  19.4U  15.3E  7.9S    A. Drake       CBET 1828
K0905-005  2009 04 27.39   14 39 38.53 -07 18 42.6  18.6U   0.3W  0.4N    A. Drake       CBET 1828
K0905-006  2009 05 18.19   12 34 59.13 +24 43 52.1  19.2U   0.2E  1.4N    A. Drake       CBET 1828
K0905-007  2009 05 18.21   12 30 48.77 +28 57 01.4  19.5U  13.9W  4.4N    A. Drake       CBET 1828
K0905-008  2009 05 18.21   12 41 50.08 +30 01 41.8  19.6U   0.2W  0.9N    A. Drake       CBET 1828
K0905-009  2009 05 18.27   12 17 30.34 +41 13 29.1  19.7U   9.4E  9.6S    A. Drake       CBET 1828
K0905-010  2009 05 23.16   14 26 47.44 +12 35 29.1  18.5U   0.4E  0.8N    A. Drake       CBET 1861
K0905-011  2009 05 26.27   13 51 43.30 +09 06 53.2  19.4U   0.2W  0.1N    A. Drake       CBET 1861
K0905-012  2009 05 30.35   14 20 21.31 +29 11 59.4  19.1U   1.1W  0.2N    A. Drake       CBET 1861

K0909-001  2009 09 22.47   22 19 45.87 +00 50 12.6  21.4    0.2E  0.2N    A. Rest        CBET 2012
K0910-001  2009 10 18.78   22 13 13.92 +00 02 57.5  21.2    0.2W  0.3N    A. Rest        CBET 2012
K0910-002  2009 10 18.79   02 22 19.17 -03 46 45.8  21.6    0.8E  0.3S    A. Rest        CBET 2012
K0910-003  2009 10 19.20   03 30 49.84 -28 47 37.6  20.5    0.3W  0.0N    A. Rest        CBET 2012

K0911-001  2009 11 21.478  12 10 05.02 +43 26 42.6  19.5R   3.8W  8.2N    E. Sanders
K0911-001  2009 12 16.481  12 10 05.04 +43 26 42.1  19.7R   4.2W  8.0N    E. Sanders
K0911-001  2009 12 18.393  12 10 05.05 +43 26 42.0  19.8R   3.7W  7.6N    E. Sanders
K0911-001  2009 12 20.369  12 10 05.02 +43 26 42.6  19.7R   4.2W  8.6N    E. Sanders

K1001-001  2010 02 24.6    13 20 35.36 +34 08 22.2  17.7K   0.2E  0.3S    S. Mattila    CBET 2213

---------------                                                                                     
NOTES (listed designation):                                                  

(J9711-001)  S. Lipari and R. Diaz, Cordoba Observatory, report their discovery of a
 possible infrared supernova in NGC 3256 on archival Hubble Space Telescope (HST)  
 NICMOS images, taken at K (2.2-micron) and F237M (2.4-micron) bands as a part of  
 their long-term study of starburst and galactic wind in infrared mergers and QSOs.
 The tabulated offsets above are with respect to the main optical nucleus of the                    
 merger.  The new object appears in the HST images obtained in 1997 Nov. 28.9 UT, but               
 does not appear in 1993 ESO/MPI K-band images (cf. Kotilainen et al. 1996, A.Ap. 305,              
 107, Fig. 1), and also it does not appear in ESO NTT K images from 1999 and 2001                   
 (down to limiting mag K about 18).  This new object was detected only at wavelengths               
 longer that the K band; it is not present in their optical observations at CASLEO                  
 and Bosque Alegre Station, in 1997 and 1998, and it was not detected in the                        
 HST/NICMOS observations of 1997 Nov. 28 in the J (1.1-micron) and H (1.6-micron)                   
 bands.  A similar behavior was found previously for the southern nucleus, which is                 
 located in the region where this object was detected:  it is not observed at                       
 wavelengths shorter than 2.2 microns.                                                              
 The adopted distance of 37 Mpc (H_o = 75) yields an absolute mag of M(K) = -20.6                   
 (without reddening correction).  The HST K-band image from 1997 Nov 28.9, including                
 the new object, was published by Lipari et al. (2000, A.J. 120, 645, Fig. 1g), where               
 J9711-001 is the third-brightest object in the field (dimmer only than the two main                
 nuclei).  J9711-001 is located in the strongly obscured region of this merger (to                  
 the south), in the same extended area where Maiolino et al. (IAUC 7661) detected                   
 another apparent infrared supernova, SN 2001db.  The detection of two obscured                     
 possible supernovae in NGC 3256, in a period of only 3 years, is in agreement with                 
 the very high supernova rate expected in infrared mergers with massive star                        
 formation and galactic wind processes.                                                             
                                                                                                    
(K0211-001, K0211-002, K0211-003, K0211-004)  Further to IAUCs 8119, 8120, and 8121,
 M. Doi, Institute of Astronomy, University of Tokyo, on behalf of the Supernova
 Cosmology Project, reports four additional hostless possible supernovae.  Additional
 magnitudes were obtained on 2002 Nov. 6, 10, 28, 30, Dec. 7, and 8, but Doi requests
 that we only show one additional magnitude (after those tabulated here):  PSN K0211-001,
 Dec. 8, 28.8; PSN K0211-002, Dec. 8, 28.5; PSN K0211-003, Dec. 8, 26.4; PSN K0211-004,
 Dec. 8, 25.9.

(K0210-001)  Notes on IAUC 8992.
                                                                                                    
(K0302-001)  Further to IAUC 8281, 8284, and 8290, L. Strolger and A. Riess, Space     
 Telescope Science Institute (STScI) report the discovery of another apparent supernova
 found within the images of the Ultra Deep Field (UDF) and UDF Parallel fields on                   
 CCD images taken with the Hubble Space Telescope's ACS.  PSN K0302-001 was found in                
 four images taken on Feb. 10, but not detected in images taken on 2003 Sept. 1.89                  
 UT (limiting z mag 28.5).                                                                          
                                                                                                    
(K0306-001, K0306-002, K0306-003, K0306-004, K0306-005)  Further to IAUC 8178, P. Astier
 and C. Pritchet report additional unconfirmed supernovae candidates found via the CFHT
 Legacy Survey Supernova Project.  None of the new objects were visible in images taken
 on 2003 June 5 or 6 (limiting mag about 24.5).  Additional i' magnitudes:  PSN K0306-001, 
 2003 June 26.5 UT, 23.3; 30.5, 23.4; July 4.5, 23.7.  PSN K0306-002, June 26.5, 23.3;
 30.5, 23.4; July 4.5, 23.5.  PSN K0306-003, June 26.5, 22.9; 30.5, 22.6; July 4.5, 22.5.
 PSN K0306-004, June 30.3, 23.7; July 4.3, 23.4.  PSN K0306-005, July 4.5, 24.0.

(K0304-001)  Notes on IAUC 8992.
                                                                                                    
(K0404-001, K0404-002, K0404-003, K0404-004, K0404-005, K0404-006, K0404-007, K0404-008,
 K0404-009, K0404-010, K0404-011)  R. Gibbons, Lawrence Berkeley Laboratory (LBL), on
 behalf of the Supernova Cosmology Project (cf. IAUC 8119, plus N. Kashikawa, M. Kowalski,
 N. Kuznetsova, T. Morokuma); and A. Riess, STScI, on behalf of L. Strolger, H. Ferguson,
 T. Dahlen, and B. Mobasher, STScI; and of P. Challis, CfA, report on new objects found
 with the Advanced Camera for Surveys (ACS) on the Hubble Space Telescope; sums of four
 400-s z' exposures and one 400-s i' exposure (limiting magnitudes z' = 26.2 and i' = 26.5). 
 Subtraction of GOODS HDF-N survey data (obtained 2002 Nov. 21-2003 May 25; limiting
 magnitudes z' = 27.4 and i' = 28.4) from April 2004 F850LP (z') and F775W (i') 2100-s
 images revealed new objects at signal-to-noise ratios > 6 within 0".2 apertures, but
 typically well above 15, and with no evidence of systematic motion indicative of
 solar-system objects.  All reported events appear associated with host galaxies, none of
 which show active galaxy variability at the positions of the candidates over the course
 of the GOODS survey.  More information and discovery images at http://supernova.lbl.gov/.
 Magnitudes of objects in i' band:  K0404-001, 26.3; K0404-003, 24.3; K0404-004, 25.5;
 K0404-005, 25.1; K0404-006, 25.7; K0404-007, 26.5; K0404-008, 25.2; K0404-009, > 26.5;
 K0404-001, 25.7.                                                                
                                                                                                    
(K0405-001, K0405-002, K0405-003, K0405-004, K0405-005, K0405-006, K0405-007, K0405-008,
K0405-009, K0405-010)  L. Strolger, STScI, and R. Gibbons, LBL, report, on behalf of the
 'Probing Acceleration Now with Supernova' (PANS) Team and the Supernova Cosmology 
 Project, respectively (cf. PSN K0404-001 through K0404-011), new objects found with
 the Advanced Camera for Surveys (ACS) on the Hubble Space Telescope in sums of four
 400-s F850LP (z') exposures and one 400-s F775W (i') exposure (limiting magnitudes 
 z' = 26.2 and i' = 26.5).  Subtraction of the previous campaign of the survey
 (2004 Apr., same limiting magnitudes) and the GOODS HDF-N survey data (obtained during
 2002 Nov. 21-2003 May 25; limiting mags z' = 27.4 and i' = 28.4) from the May 2004
 images revealed new objects at signal-to-noise ratios > 6 within 0".2 apertures.
 There was no evidence of systematic motion indicative of solar-system objects.  
 All reported events appear associated with host galaxies, none of which show active-galaxy 
 variability over the course of the GOODS survey.  Magnitudes of the objects in i' band:
 K0405-001, 25.1; K0405-002, 25.4; K0405-003, 22.7; K0405-004, 23.4; K0405-005, 25.8;
 K0405-006, 26.0; K0405-007, 24.4; K0405-008, 24.3; K0405-009, > 26.5.  SN 2003eq (cf. IAUC
 8140) appeared very close to the position of K045-010, but these appear to be two separate
 events in the same host galaxy.
                                                                                                    
(K0409-001)  S. Mattila, P. Meikle, P. Vaisanen, C. Alard, T. Dahlen, A. Efstathiou,
 D. Farrah, C. Fransson, R. Joseph, P. Lira, P. Lundqvist, G. Ostlin, S. Ryder,
 J. Sollerman report the discovery of an apparent supernova in K_s-band images 
 obtained using the NAOS CONICA Adaptive Optics System on the ESO Very Large   
 Telescope (VLT).  K0409-001, first observed on 2004 Sept. 13.1 UT and again   
 on Sept. 15.0, is located at R.A. = 18h32m41s.24, Decl. = -34o11'26".6 (equinox
 2000.0), which is 1".14 east and 0".78 north of (or 500 pc from) the K_s-band  
 nucleus of the luminous infrared galaxy IRAS 18293-3413.  K0409-001 was detected
 via image-subtraction techniques using a reference K_s-band image obtained under
 similar conditions on May 4.3 with the VLT/NACO as part of the ongoing search   
 campaign for highly obscured supernovae.  A magnitude of K_s = 18.7 ± 0.1 was 
 measured for K0409-001 from the subtracted images.  [This object was designated
 SN 2004ip on CBET 858.]

(K0409-002)  Discovered by E. Kankare and S. Mattila, Tuorla Observatory; S. Ryder,
 Anglo-Australian Observatory; A. Alonso-Herrero, T. Diaz Santos, and L. Colina
 Instituto de Estructura de la Materia (IEM), Consejo Superior de Investigaciones
 Cientificas (CSIC); J. Kotilainen, Tuorla Observatory; M.-A. Perez-Torres,
 Instituto de Astrofisica de Andalucia (IAA), CSIC; P. Vaisanen, South African 
 Astronomical Observatory; A. Alberdi, IAA/CSIC; and A. Efstathiou, European 
 University, Cyprus, report the discovery of an apparent supernova on near-
 infrared images of the luminous infrared galaxy IRAS 17138-1017 in the course
 of their infrared search program (cf. IAUCs 8473, 8474; CBET 858).  The new
 object, designated here as K0409-002, was detected via comparison of K-band
 images obtained using the Altair/NIRI adaptive optics system with "Laser Guide
 Star" on the Gemini-North Telescope on 2008 Apr. 21.6 UT (when the new 2004
 object was not visible) with F110W (J-band), F160W (H-band), and F187N (K-band)
 NICMOS images obtained with the Hubble Space Telescope on 2004 Sept. 23.0 UT
 (when K0409-002 was detected at J = 18.3, H = 16.9, and K = 16.5, or at
 integrated fluxes of 0.09, 0.18, and 0.20 mJy, respectively.  The offset
 tabulated above is with respect to the galaxy's H-band nucleus.  Nothing is
 visible at the position of K0409-002 in the K-band Altair/NIRI image from
 2008 to a limiting magnitude of approximately 20.0.  Explanations other than
 supernovae for this object are extremely unlikely; also, large numbers of
 supernovae are expected in the nuclear regions of starburst galaxies and
 LIRGs as a result of the large star-formation rates therein (e.g., Mattila
 et al. 2007, ApJ, 659L, 9). 
                                                                                                    
(K0504-001)  Designated as SN 2005bk and published on IAUC 8512.
                                                                                                    
(K0508-001)  Designated as SN 2005du and published on CBET 214. 
                                                                                                    
(K0509-001)  Discovered by Sloan Digital Sky Survey II (reported with supernovae
 announced on CBETs 268 and 272).  Not visible on a reference image taken                           
 approximately two years earlier (limiting magnitudes:  g > 22.5, r > 22, i > 22).                  
 Apparent host galaxy has magnitudes g = 19.4, r = 18.0, i = 17.5.  Eight observing                 
 nights of g, r, and i photometry are available during Sept. 10-Oct. 20; the                        
 estimated peak-brightness date was Sept. 14.  On Oct. 20, it was not detected                      
 in g but appeared at r = 21.8.                                                                     

(K0901-001)  "Confirmed" as a possible-type-Ic supernova and designated SN 2009de
 on CBET 1766.

(K0905-001)  Nothing visible at this position on co-added reference images
 taken during the week before discovery to limiting mag 22.4.  Spectrum shows
 a blue and mostly featureless continuum and requires further spectroscopic 
 follow-up.

(K0905-002)  Nothing visible at this position on co-added reference images
 taken during the week before discovery to limiting mag 22.1.  Spectrum shows
 a blue and mostly featureless continuum and requires further spectroscopic 
 follow-up.

(K0905-003)  Nothing visible at this position on co-added reference images
 taken during the week before discovery to limiting mag 22.0.  Spectrum shows
 a blue and mostly featureless continuum and requires further spectroscopic 
 follow-up.

(K0909-001)  Pan-STARRs survey.  Nothing visible at this position on images taken on
 2009 June 3-July 17 (limiting mag about 22.5).

(K0910-001)  Pan-STARRs survey.  Nothing visible at this position on images taken on
 2009 June 3-Sept. 9 (limiting mag about 22.5).

(K0910-002)  Pan-STARRs survey.  Nothing visible at this position on images taken on
 2009 Aug. 29-Sept. 1 (limiting mag about 22.5).

(K0910-003)  Pan-STARRs survey.  Nothing visible at this position on images taken on
 2009 Aug. 29 (limiting mag about 22.5).

(K0911-001)  The new object -- which appears to be within, or behind, the spiral bar of the host
 galaxy -- is not visible on images taken on 2009 Nov. 23.421 (limiting red mag about 19.9),
 25.414 (limiting red mag about 20.5), and 26.409 (limiting red mag about 20.8).  Nothing is
 visible at the new object's position on a Palomar Sky Survey image (via the Digitized Sky
 Survey) taken on 1996 Mar. 17 (limiting red mag approximately 20.2).

(K1002-001)  Close to center of the galaxy IC 883; infrared observations only.


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