CBAT
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.
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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 95-98 contains the number for the note that will contain 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.); the appropriate number will be added by the webmaster.
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.
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PSN DATE (UT) R.A. (2000.0) Decl. Mag. OFFSET REPORTER NOTES
PSN DATE (UT) R.A. (2000.0) Decl. Mag. OFFSET REPORTER NOTES
J9711-001 1997 11 28.9 10 27 51.45 -43 54 18.5 12.3K 4 E 3 S S. Lipari 1997-01
K0211-001 2002 11 03 02 16 26.37 -05 04 32.5 26.1i no host M. Doi 2002-01
K0211-002 2002 11 03 02 17 16.18 -05 06 02.7 26.2i no host M. Doi 2002-01
K0211-003 2002 11 03 02 18 52.36 -05 01 13.2 24.8i no host M. Doi 2002-01
K0211-004 2002 11 03 02 20 13.92 -05 07 36.0 25.6i no host M. Doi 2002-01
K0302-001 2003 02 10.12 03 32 37.03 -27 56 53.9 24.4z 0.13E L. Strolger 2003-01
K0306-001 2003 06 22.5 22 14 24.02 -17 46 36.0 23.5i 0.2W P. Astier 2003-02
K0306-002 2003 06 22.5 22 16 09.91 -18 04 39.1 23.4i 0.2W 0.1S P. Astier 2003-02
K0306-003 2003 06 22.5 22 16 41.55 -17 26 10.6 23.2i 0.2W 0.2S P. Astier 2003-02
K0306-004 2003 06 26.3 14 21 54.20 +52 58 49.7 24.0i 0.1E 0.2S P. Astier 2003-02
K0306-005 2003 06 30.5 22 15 28.14 -17 49 48.6 24.6i 1.0W 0.4S P. Astier 2003-02
K0404-001 2004 04 02.08 12 36 20.90 +62 10 19.6 25.4z' 0.5W 0.5S R. Gibbons 2004-01
K0404-002 2004 04 02.08 12 36 25.93 +62 09 37.4 23.7z' 0.0E 0.7S R. Gibbons 2004-01
K0404-003 2004 04 02.08 12 36 29.44 +62 11 41.9 24.4z' 0.0W 0.0N R. Gibbons 2004-01
K0404-004 2004 04 02.74 12 36 19.86 +62 13 48.0 25.1z' 0.1E 0.1S R. Gibbons 2004-01
K0404-005 2004 04 02.74 12 36 27.07 +62 15 09.6 24.4z' 0.2E 0.1S R. Gibbons 2004-01
K0404-006 2004 04 03.40 12 37 06.73 +62 21 17.8 25.4z' 0.0W 0.0S R. Gibbons 2004-01
K0404-007 2004 04 03.40 12 37 09.44 +62 22 15.6 25.1z' 0.3E 0.8N R. Gibbons 2004-01
K0404-008 2004 04 03.34 12 38 03.58 +62 17 11.9 24.7z' 1.0W 0.2N R. Gibbons 2004-01
K0404-009 2004 04 03.54 12 37 21.32 +62 09 35.2 25.7z' 0.1W 0.1N R. Gibbons 2004-01
K0404-010 2004 04 04.71 12 36 46.07 +62 16 25.7 25.8z' 0.1E 0.2S R. Gibbons 2004-01
K0404-011 2004 04 04.71 12 36 49.36 +62 16 04.8 24.9z' 0.0E 0.0S R. Gibbons 2004-01
K0405-001 2004 05 21.24 12 35 50.78 +62 10 38.2 24.5z' 0.1E 0.3N L. Strolger 2004-02
K0405-002 2004 05 20.24 12 36 26.66 +62 08 30.2 25.0z' 0.4W 0.0N L. Strolger 2004-02
K0405-003 2004 05 20.13 12 36 34.33 +62 12 13.0 22.5z' 0.8W 0.2S L. Strolger 2004-02
K0405-004 2004 05 21.31 12 36 34.81 +62 15 49.0 23.3z' 0.7W 0.1S L. Strolger 2004-02
K0405-005 2004 05 21.31 12 36 35.96 +62 17 32.3 25.6z' 0.2W 0.4S L. Strolger 2004-02
K0405-006 2004 05 23.67 12 36 54.11 +62 08 22.8 24.8z' 0.1E 0.3N L. Strolger 2004-02
K0405-007 2004 05 21.44 12 36 58.45 +62 16 37.3 23.7z' 0.0E 0.0N L. Strolger 2004-02
K0405-008 2004 05 20.78 12 37 33.86 +62 19 22.3 23.8z' 0.0E 0.0N L. Strolger 2004-02
K0405-009 2004 05 21.18 12 37 52.67 +62 14 08.2 25.6z' 0.1W 0.0N L. Strolger 2004-02
K0405-010 2004 05 21.18 12 37 48.38 +62 13 35.4 23.2z' 0.1W 0.2N L. Strolger 2004-02
K0409-001 2004 09 13.1 18 32 41.24 -34 11 26.6 18.7Ks 1.1E 0.8N S. Matilla 2004-03
K0504-001 2005 04 02.456 16 02 11.01 +42 55 05.5 17.9Rc 4.6E 6.6S R. Jansen 2005-01
K0508-001 2005 08 08.5 00 09 34.7 +12 45 21.4 19.7U G. Aldering 2005-02
K0509-001 2005 09 10 21 26 16.30 -00 33 14.7 20.9r 0.6E 0.6S J. Frieman 2005-03
---------------
NOTES (listed by note number, not by designation):
(1997-01) 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.
(2002-01) 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.
(2003-01) 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).
(2003-02) 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.
(2004-01) 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.
(2004-02) 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.
(2004-03) 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.]
(2005-01) Designated as SN 2005bk and published on IAUC 8512.
(2005-02) Designated as SN 2005du and published on CBET 214.
(2005-03) 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.
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