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[vsnet-campaign 1364] VSNET Weekly Campaign Summary
VSNET Weekly Campaign Summary
*** Last week news ***
(new targets)
SN 2003B (RA = 02h46m13s.78, Dec = -30d13'45".1)
SN 2003B was discovered visually by R. Evans. It was revealed to
be a type II SN a few weeks after explosion on Jan 6 UT. The host
galaxy of SN 2003B, NGC 1097 had produced SNe 1992bd and 1999eu.
These two were also SNe II, and the latter is peculiarly dim one
(vsnet-campaign-sn 526, 530).
SN 2003C (RA = 00h41m20s.91, Dec = -01d42'54".1)
A host galaxy of SN 2003C is a ring-shaped barred-spiral galaxy
UGC 439. The UCB team with Keck I revealed that it was a young
type II SN on Jan. 7 (vsnet-campaign-sn 530).
SN 2003D (RA = 09h38m53s.52, Dec = -04d51'05".1)
A host galaxy of SN 2003D is an elliptical galaxy MCG -01-25-9
within a group Arp 321 = HCG (Hickson Compact Groups) 40. The UCB
team revealed that it was subluminous SN Ia, not long after maximum
on Jan 7. The discovery magnitude (17.5mag) is consistent with this
classification (vsnet-campaign-sn 530).
SN 2003E (RA = 04h39m10s.88, Dec = -24d10'36".5)
A host galaxy of SN 2003E is an edge-on spiral galaxy MCG -4-12-4,
which makes a pair with MCG -4-12-3. The SN is superimposed on the
disk, so notable extinction is possible. The expected maximum for
typical unreddened (in the host galaxy) SN Ia is mag about 15.7
(vsnet-campaign-sn 531). A spectrum taken with Baade telescope on
Jan 9.15 showed that it was a young SN II (vsnet-campaign-sn 532).
CP Dra (RA = 10h15m39s.88, Dec = +73d26'05".4)
An outburst (14.5mag) was reported by M. Simonsen on January 8.
D. Nogami commented that during both of its outbursts in 2001
February and 2002 April, prominent, rather coherent oscillations
with periods of ~0.066 d, much shorter than its superhump period
~0.083 d, were found, only in the very early phase of the outburst
(vsnet-campaign-dn 3280, 3284, vsnet-campaign 1362). The Kyoto data
on Jan. 8 clearly showed the presence of fully grown superhumps
(~0.3 mag). The present outburst was thus confirmed to be a
superoutburst (vsnet-campaign-dn 3294, 3297). The superoutburst
continues (vsnet-campaign-dn 3306, 3316).
CY UMa (RA = 10h56m57s.69, Dec = +49d41'09".1)
H. Maehara (VSOLJ) reported the detection of superhumps (0.15
mag). The current outburst of CY UMa was thus confirmed to be a
superoutburst (vsnet-campaign-dn 3282).
HS Vir (RA = 13h43m38s.5, Dec = -08d14'04".1)
An outburst (14.0mag) was reported by M. Simonsen on January 8
(vsnet-campaign-dn 3287). It has quickly faded (vsnet-campaign-dn 3303).
TV Col (RA = 05h29m25s.5, Dec = -32d49'05".2)
According to Kyoto observations, TV Col seems to have undergone an
outburst on Jan. 8. The object was recorded by 0.5-1.0 mag brighter
than on other nights (vsnet-campaign-ip 96).
HH Cnc (RA = 09h16m50s.63, Dec = +28d49'43".3)
An outburst (14.7mag) was detected by M. Simonsen on January 9
(vsnet-campaign-dn 3298). The observations have shown that the
outburst is a "long" outburst, in contrast to the short one recorded
in 1999 November. A partial analysis of the data taken by
R. Ishioka and K. Torii did not reveal clear presence of superhumps.
R. Ishioka reported that the object has started fading on Jan. 12.
Judging from the outburst behavior, T. Kato reported that HH Cnc
seems to be an SS Cyg type dwarf nova possibly with a relatively
short orbital period (vsnet-campaign-dn 3312).
SN 2003F (RA = 05h11m33s.03, Dec = +17d03'28".4)
A host galaxy of SN 2003F is a disturbed spiral galaxy UGC 3261.
It is near to the Galactic plain (b = -13o), so there are several
foreground stars superimposed on the host galaxy. A spectrum taken
with the Las Campanas Observatory Baade 6.5-m telescope on Jan 9.11
revealed that it was type Ia SN a few days before maximum. Some
reddening within the host galaxy is suggested, as well as Galactic
one. The reported magnitude (16.1mag on Jan. 9) is thus
considerably brighter than expected maximum for typical SNe Ia (mag
about 16.7) taking account of the redshift and the Galactic
extinction (vsnet-campaign-sn 532).
SN 2003G (RA = 02h08m28s.13, Dec = +06d23'51".9)
A host galaxy of SN 2003G is a face-on spiral galaxy IC 208. A
spectrum taken with Baade telescope on Jan 9.05 revealed that it
was a young SN IIn. The reported magnitudes are consistent with
that of ordinal core-collapsed SNe (vsnet-campaign-sn 532).
SN 2003H (RA = 06h16m25s.68, Dec = -21d22'23".8)
A host galaxy of SN 2003H is an interacting pair NGC 2207 + IC
2163. The classification was not been reported on IAUC 8045. NGC
2207 had produced SN Ia 1975A (B=14.7 at maximum) and SN Ib(?) 1999ec
(discovery mag about 17.9, past maximum)(vsnet-campaign-sn 532).
SN 2003I (RA = 09h27m29s.48, Dec = +03d55'45".6)
A host galaxy of SN 2003I is a small, apparently spiral galaxy IC
2481. The expected maximum for typical SN Ia is mag about 16.0
(vsnet-campaign-sn 533).
SUPERNOVA IN NGC 4157 (RA = 12h10m57s.72, Dec = +50d28'31".8)
K. Ayani et al. performed spectroscopy with the Bisei Astronomical
Observatory 1.01-m telescope on January 12 and reported that this
supernova showed a prominent H-alpha emission with a P-Cyg profile,
which suggests that it is a normal type-II supernova
(vsnet-campaign-sn 534).
SUPERNOVA IN IC 1129 (RA = 15h32m01s.91, Dec = +68d14'35".9)
K. Ayani et al. performed spectroscopy with the Bisei Astronomical
Observatory 1.01-m telescope on January 12 and reported that it was
a type-Ia supernova several days before maximum light. Adopting the
NASA/IPAC Extragalactic Database recession velocity of 6540 km/s,
the expansion velocity deduced from Si II (rest 635.5 nm) is about
12100 km/s (vsnet-campaign-sn 534).
(continuous targets)
NSV 10934 (RA = 18h40m52s.26, Dec = -83d43'10".24)
On January 6, the amplitude of superhumps became slightly
smaller. Based on observations by P. Nelson and C. Stockdale,
T. Kato reported a superhump period of 0.07508(2) d. The initially
reported period (0.0743(8) d) is 1 percent small than this superhump
period. From these analyses, it is evident that the superhump
timings have large O-C's during the earliest stage of the superhump
evolution (vsnet-campaign-dn 3268, 3277). The light curve taken by
T. Richards on January 6 showed fast modulations (QPOs) of ~3min
period and 0.02-0.05 mag amplitude (vsnet-campaign-dn 3271).
Short-term modulations were also detected in the light curve taken
by T. Richards on January 11 (vsnet-campaign-dn 3317). In the
data by P. Nelson on January 8, the superhumps has become slightly
more rounded. There was a hint of short-period oscillations (a few
to 5 min)(vsnet-campaign-dn 3299). On January 10, The amplitudes of
the superhumps have decreased to ~0.2 mag. the profile has become
rather complex with secondary and sometimes tertiary hump features
on the declining branch from superhump maxima. The mean superhump
period between Jan. 4 and 12 is 0.07485 d. There is an undisputed
presence of period shortening (about -1.5*10^-5)(vsnet-campaign-dn
3300, 3310). The superoutburst continues (vsnet-campaign-dn 3273,
3290, 3295, 3304, 3315).
V485 Cen (RA = 12h57m23s.30, Dec = -33d12'06".8)
The superoutburst continues (vsnet-campaign-dn 3275).
MKN 421 (RA = 11h04m27s, Dec = +38d12'32")
It has been reported to further brighten (vsnet-campaign-blazar 295).
UV Gem (RA = 06h38m44s.16, Dec = +18d16'11".5)
T. Vanmunster commented that the object showed no superhumps
during a long outburst in December 2000 (vsnet-campaign-dn 3264).
T. Kato also commented that no definite superhump was detected
also during a long outburst in February 2001 (vsnet-campaign-dn 3266).
A. Oksanen and M. Aho reported that the light curve on January 6
showed 0.1mag superhumps, which indicates that the current outburst
is a superoutburst (vsnet-campaign-dn 3267, 3269). T. Kato reported
that, up to Jan. 7, the superhumps were well expressed by a single
period of 0.0966 d. After that, The period suddenly switched to
0.0932 d. The difference between these periods are comparable to
the differences between superhump periods and orbital periods. Such
a dramatic change (and a large change) in the superhump period is
quite unexpected and unprecedented in SU UMa-type superhumps
(vsnet-campaign-dn 3302, 3278, 3279, 3281, 3283, 3293). The rate of
decrease in superhump period is around -3*10^(-4), which is
comparable to what we saw in KK Tel (vsnet-campaign-dn 3307, 3311).
T. Vanmunster confirmed this trend in his observations
(vsnet-campaign-dn 3308, 3309). The superoutburst is now ongoing
(vsnet-campaign-dn 3274, 3289, 3296, 3305, 3314).
V1208 Tau (RA = 04h59m44s.00, Dec = +19d26'23".7)
A. Oksanen reported that the object started rapid fading on
January 6 (vsnet-campaign-dn 3265).
GZ Cnc (RA = 09h15m51s.70, Dec = +09d00'50".2)
The outburst still continues (vsnet-campaign-dn 3276).
DI UMa (RA = 09h12m22s.16, Dec = +50d49'39".1)
The Jan. 7 data by K. Tanabe indicated the start of a new
outburst. The object was weakly humping (superhumps?) and rising.
28 days had past since the start of the last superoutburst in
December (vsnet-campaign-dn 3286). It faded on January 8, which
indicates that it was a normal outburst (vsnet-campaign-dn 3288).
BU Tau (RA = 03h49m11s.19, Dec = +24d08'12".4)
D. West performed photoelectric photometry and reported that the
nearby star HD 23873 had not faded noticeably, at least on January
13 (vsnet-campaign-be 209, vsnet-campaign 1363).
V803 Cen (RA = 13h23m44s.5, Dec = -41d44'30".1)
It was reported to brightened again on January 5
(vsnet-campaign-dn 3291). The object is now in an oscillating
bright state (vsnet-campaign-dn 3313).
V838 Mon (RA = 07h04m04s.816, Dec = -03d50'50".94)
The object was reported to be possibly in 13.8mag in March 27,
1998 (vsnet-campaign-v838mon 409), but it seems to be a nearby star
(vsnet-campaign-v838mon 410, 411, 412, 413).
MisV1147 (RA = 22h54m03s.78, Dec = +58d54'02".1)
A new fading started on January 4. The fading has been confirmed
by Kyoto observations, too. This fading seems to have been a
shallower than those in the past. The object was caught in rise on
Jan. 8. There seems to be a quasi-period of 30+ d
(vsnet-campaign-unknown 171, 174). D. West reported JHK magnitudes of
MisV1147 from the 2MASS catalogue, and that the J-K color of
MisV1147 fits nicely into the range of known YSO's while none of the
observations have been de-reddened (vsnet-campaign-unknown 172, 173).
V1159 Ori (RA = 05h28m59s.52, Dec = -03d33'52".8)
The Jan. 7 data by K. Torii showed a definite brightening and
growth of superhumps. The object entered its superoutbursting state
again (vsnet-campaign-dn 3285, 3292).
SN 2003A (RA = 10h48m33s.86, Dec = +66d22'29".4)
The UCB group has revealed that it was of type Ib/c, a few weeks
after maximum on Jan. 6 (vsnet-campaign-sn 527, 528).
eta Gem (RA = 06h14m52s.87, Dec = +22d30'24".5)
Recently reported observations are shown in [vsnet-campaign-ecl 56].
*** Future schedule ***
The 2003 Gamma Ray Burst conference
Hosted by Los Alamos,
in Santa Fe, New Mexico (USA), between September 8 and 12, 2003
http://grb2003.lanl.gov/
[vsnet-campaign-grb 13]
WEBT campaign on Mkn 421
M. Villata announced possible WEBT campaign on Mkn 421, in
December 2002 and February-March 2003, to be carried out during
multifrequency campaigns.
The relevant information on the MW campaign of December 2-16 is at
the VERITAS site <http://veritas.sao.arizona.edu> .
[vsnet-campaign-blazar 287]
[vsnet-campaign-blazar 288]
SUPERNOVAE (10 YEARS OF SN1993J)
22-26 April 2003, Valencia, Spain
Web site: http://vsnet.uv.es/2003supernovae/
[vsnet-campaign-sn 342]
[vsnet-campaign-sn 452]
[vsnet-campaign-sn 512]
*** General information ***
Supernovas and the NASA CHIPS mission
http://science.nasa.gov/headlines/y2003/06jan_bubble.htm?list813119
[vsnet-campaign-dn 3270]
[vsnet-campaign-sn 529]
UV Gem
Image by Nyrola team
http://vsnet.kusastro.kyoto-u.ac.jp/pub/vsnet/DNe/UV_Gem/UVGem20030106.jpg
[vsnet-campaign-dn 3272]
Time-series observations by H. Maehara, see [vsnet-campaign-data 105]
Light curves by T. Vanmunster:
http://vsnet.cbabelgium.com
[vsnet-campaign-dn 3308]
GZ Cnc
Image by Nyrola team
http://vsnet.kusastro.kyoto-u.ac.jp/pub/vsnet/DNe/GZ_Cnc/GZCnc20030106.jpg
[vsnet-campaign-dn 3272]
CY UMa
Time-series data by H. Maehara, see [vsnet-campaign-data 103, 104].
NSV 10934
CCD image and NSV 10934 page:
http://vsnet.kusastro.kyoto-u.ac.jp/vsnet/DNe/nsv10934.html
[vsnet-campaign-dn 3301]
U Sco
Preprint by K. Matsumoto et al.
http://vsnet.kusastro.kyoto-u.ac.jp/pub/vsnet/preprints/U_Sco/usco1999.pdf
http://vsnet.kusastro.kyoto-u.ac.jp/pub/vsnet/preprints/U_Sco/usco1999.ps.gz
or
http://ftp.kusastro.kyoto-u.ac.jp/pub/vsnet/preprints/U_Sco/usco1999.pdf
http://ftp.kusastro.kyoto-u.ac.jp/pub/vsnet/preprints/U_Sco/usco1999.ps.gz
[vsnet-campaign-nova 1148]
(This summary can be cited.)
Regards,
Makoto Uemura
Return to Daisaku Nogami
vsnet-adm@kusastro.kyoto-u.ac.jp
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