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[vsnet-campaign 1368] VSNET Weekly Campaign Summary
VSNET Weekly Campaign Summary
*** Last week news ***
(new targets)
XZ Eri (RA = 04h11m25s.76, Dec = -15d23'24".3)
As reported by R. Stubbings on January 27, the eclipsing dwarf
nova XZ Eri is now undergoing an outburst. The object has an
orbital period of 0.0612 d (Woudt and Warner 2001, MNRAS 328, 158),
it was hence a candidate of a SU UMa-type dwarf nova
(vsnet-campaign-dn 3353). The object was confirmed to be still in
outburst on January 28 (vsnet-campaign-dn 3356). The observations
by G. Bolt detected ~0.4mag superhumps, which established the SU UMa
nature of XZ Eri. The data also showed shallow eclipses, which
resemble the eclipses observed during the first night of a
superoutburst of DV UMa. Among eclipsing SU UMa-type dwarf novae,
XZ Eri has the shortest orbital period (except for the shallow
eclipser WZ Sge) (vsnet-campaign-dn 3358).
The data on January 29 very clearly showed the emergence of narrow
eclipses (depth ~0.4 mag) and superhumps. From two-night
observations, T. Kato reported a superhump period of 0.06289(6) d,
which is 2.7% longer than the orbital period (vsnet-campaign-dn
3362). The profile of the eclipses was highly asymmetric in the
light curve taken by D. Starkey, indicating the non-axisymmetric
brightness distribution of the accretion disk (vsnet-campaign-dn
3366). The best superhump period determined from Jan. 29 and 30 data
is 0.06243(6) d. This period indicates that the superhump period
has shown a dramatic phase/period change between Jan. 28 and 29.
The revised period is 2% longer than the orbital period. This
fractional superhump excess is a very reasonable one for a system
with this orbital period (vsnet-campaign-dn 3377).
T. Kato reported strong beat phenomenon on February 1
(vsnet-campaign-dn 3389). There seems to be no large period change
until January 31 (vsnet-campaign-dn 3390). The eclipses possibly
became broader on February 1 (vsnet-campaign-dn 3398). T. Kato
reported that the available data also suggest a period increase, at
an approximate rate of dot(P)/P = +5x10^(-5) (vsnet-campaign-dn 3405).
The superoutburst continues (vsnet-campaign-dn 3354, 3359, 3361,
3371, 3373, 3383).
BC UMa (RA = 11h52m15s.88, Dec = +49d14'42".0)
P. Schmeer reported an outburst of the rarely outbursting SU UMa-type
dwarf nova BC UMa on February 1 (12.7mag). The last outburst was in
2001 June (vsnet-campaign-dn 3392). An analysis of the combined
data on Feb. 1 is consistent with the presence of low-amplitude
double-wave modulations with a period close to the orbital period
(the best period from the Feb. 1 data is around 0.062 d). This
feature resembles those of "early superhumps" in WZ Sge-type dwarf
novae (vsnet-campaign-dn 3402, 3394, 3397). Observations on
February 2 clearly showed the growth of genuine superhumps (amplitude
growing to 0.1 mag) (vsnet-campaign-dn 3404). The superoutburst
continues (vsnet-campaign-dn 3395, 3403, 3406).
SN 2003S (RA = 13h41m19s.49, Dec = +55d40'36".5)
A host galaxy of SN 2003S is a small galaxy MCG +09-22-94. In its
neighbourhood (within 3'), an interacting galaxy Arp 239 (NGC 5278
+ 5279, a host galaxy of SN Ic 2001ai) and UGC 8671 exist, but
they are not physically related with MCG +09-22-94, which is
further than Arp 239 or UGC 8671. The CfA team revealed that it
was SN Ia near maximum on Jan 27.48. The reported magnitude
(18.0mag) is consistent with the expected maximum (vsnet-campaign-sn 545).
SN 2003T (RA = 09h14m11s.06, Dec = +16d44'48".0)
A host galaxy of SN 2003T is a face-on spiral galaxy UGC 4864.
The expected maximum for typical SN Ia is mag about 17.0
(vsnet-campaign-sn 545). The UCB team revealed that it was quite
young type II SN soon (a week) after the explosion on Jan. 28
(vsnet-campaign-sn 547).
SN 2003U (RA = 17h22m45s.66, Dec = +62d09'50".4)
A host galaxy of SN 2003U is a face-on barred-spiral galaxy NGC
6365A, which is making a probably interacting pair NGC 6365 = Arp
30 with a northern egde-on Sdm galaxy NGC 6365B. The expected
maximum for typical SN Ia is mag about 17.0 (vsnet-campaign-sn 546).
The CfA team revealed that it was a type-Ia SN a few days before
maximum light on Jan 29.53 (vsnet-campaign-sn 549).
V504 Cen (RA = 14h12m49s.36, Dec = -40d21'02".2)
The onset of rising from a deep fading was detected by
R. Stubbings on January 27 (13.4mag; vsnet-campaign-nl 103).
SN 2003V (RA = 03h05m43s.05, Dec = -01d24'12".8)
A host galaxy of SN 2003V is a small and dim (mag about 18.5)
galaxy APMUKS(BJ) B030310.79-013550.9 (vsnet-campaign-sn 547).
SN 2003W (RA = 09h46m49s.48, Dec = +16d02'37".6)
A host galaxy of SN 2003W is a spiral galaxy UGC 5234. There is a
very bright (mag about 11) foreground star about 20" due east of the
nucleus of UGC 5234. The CfA team took a spectrum on Jan. 29.34,
which revealed that it was type Ia supernova well (about 12 days)
before maximum. The expected maximum for typical SN Ia is mag about
16.3, if an extinction within the host galaxy is small
(vsnet-campaign-sn 549).
TU Crt (RA = 11h03m36s.50, Dec = -21d37'45".6)
B. Monard detected an outburst (13.2mag) of TU Crt on January 29
(vsnet-campaign-dn 3367). The last reported outburst was in 2002
July (vsnet-campaign-dn 3369). On January 30, the light curve looks
rather flat and slowly fading, and no great superhumps have been
detected (vsnet-campaign-dn 3382).
DV UMa (RA = 09h46m36s.67, Dec = +44d46'45".1)
According to Kyoto observation on January 29, DV UMa experienced
an outburst (vsnet-campaign-dn 3368). On January 30, the light
curve on outside the eclipses looks rather flat, bur neither shows a
rapid fading trend (vsnet-campaign-dn 3381).
SN 2003X (RA = 18h12m05s.67, Dec = +29d09'17".3)
A host galaxy of SN 2003X is a tilted spiral galaxy UGC 11151. It
is elongated in north-south direction, and SN is located at the edge
of bright bulge region. The expected maximum for typical SN Ia is
mag about 16.7 (vsnet-campaign-sn 550).
SN 2003Y (RA = 08h54m34s.60, Dec = +57d10'19".8)
A host galaxy of SN 2003Y is a lenticular galaxy IC 522, which is
thought to produce SN Ia only. The expected maximum for typical SN
Ia is mag about 16.0 (vsnet-campaign-sn 550). The CfA team has
revealed that it was type Ia SN near maximum on Jan. 31.34. They
comment that it may be a subluminous event (vsnet-campaign-sn 551).
SN 2003Z (RA = 09h07m32s.46, Dec = +60d29'17".5)
A host galaxy of SN 2003Z is a nearby open-spiral galaxy NGC 2742.
The SN is superimposed on the outermost northern arm. The expected
maximum for typical SN Ia without extinction in NGC 2742 is 13.2,
but it seems not the case (vsnet-campaign-sn 550). The CfA team
reported that it is type II SN (vsnet-campaign-sn 551).
PV Per (RA = 02h42m43s.50, Dec = +38d07'44".4)
M. Simonsen reported on January 31 that PV Per is undergoing an
outburst (14.7-14.9mag). PV Per is an SU UMa-type dwarf nova
(superhump period about 0.0805 d, T. Vanmunster (1997)), but still
needs to be refined. The brightness seems to suggest a
superoutburst (vsnet-campaign-dn 3378, 3380, 3407).
KR Aur (RA = 06h15m45s.05, Dec = +28d34'16".0)
A possible fading of the VY Scl-type star KR Aur was reported on
February 2, but it was confirmed to be at normal brightness
(vsnet-campaign-nl 104, 105, 106).
SN 2003aa (RA = 10h46m36s.82, Dec = +13d45'32".2)
A host galaxy of SN 2003aa is a face-on barred-spiral galaxy NGC
3367. This galaxy has also produced SN Ia 1986A (maximum mag
14.4) and SN II-p 1992C (discovered at mag 16.5 after maximum)
(vsnet-campaign-sn 551).
IGR J16318-4848 (RA = 16h31m52s, Dec = -48d48'.5)
According to IAUC No. 8063, INTEGRAL satellite detected a new
X-ray transient. The intensity source was reported to be 50-100
mCrab (15-50 keV) (vsnet-campaign-xray 186).
(continuous targets)
EP Car (RA = 10h28m23s.21, Dec = -58d57'58".6)
The light curve taken by P. Nelson on January 23 showed no
apparent superhumps. The object more looks like to be an SS
Cyg-type dwarf nova (vsnet-campaign-dn 3401).
OY Car (RA = 10h06m22s.46, Dec = -70d14'04".4)
Since the rebrightening, the object entered a superoutburst
(vsnet-campaign-dn 3352, 3355, 3372, 3400).
SN 2003P (RA = 08h01m15s.63, Dec = +55d44'34".8)
The UCB team revealed that this was type-Ia SN about a month past
maximum on Jan. 28 (vsnet-campaign-sn 547).
IP Peg (RA = 23h23m08s.7, Dec = +18d24'59".1)
An outburst was reported on February 1 (vsnet-campaign-dn 3399).
GZ Cnc (RA = 09h15m51s.70, Dec = +09d00'50".2)
A new bright outburst (~13.6mag) was reported by M. Uemura on
January 28. The last outburst was reported on January 15
(vsnet-campaign-dn 3357). It was still in outburst on January 29
(vsnet-campaign-dn 3363). In the light curve on January 29 taken by
A. Oksanen, there were at least three variation components. 1) slow
fading, 2) slow modulations (full amplitude 0.07 mag) with a period
near the orbital period, and 3) spiky, coherent-looking short-period
oscillations (vsnet-campaign-dn 3364). These variations were
already appeared late in January 28. The best determined period
is 0.0903(2) d, which is about 2.8% longer than the orbital period
(0.0878 d). These modulations thus can be interpreted as superhumps
during the growing stage (vsnet-campaign-dn 3365).
On January 30, the most prominent feature was the presence of
large-amplitude humps, but the dominant period was drastically
different from the night before. The main period on January 30 was
around 0.075 d, and whose profile even looks like superhumps. These
modulations may be so-called negative superhumps, but the period
seems to be slightly too short (vsnet-campaign-dn 3376, 3379, 3385).
Later on January 30, there appeared what strongly looked like
superhumps. However, the humps do not seem to be as periodic as in
usual SU UMa-type dwarf novae (vsnet-campaign-dn 3384).
The observation by A. Oksanen on January 31 also showed a 0.3 mag
hump and short period spike-like variation (vsnet-campaign-dn 3386).
In the light curve obtained by G. Bolt on January 31, superimposed
on a general fading, there exist almost coherent, large-amplitude
(0.3-0.4 mag) oscillations. The period is around 0.031 d, which is
different from any other previously detected periods during the
present outburst (vsnet-campaign-dn 3387). T. Vanmunster also
reported complicated profile of the light curve, that is, a 0.35mag
dip and 0.1-0.2mag short period oscillations (vsnet-campaign-dn
3391). Rapid flares of 0.5mag within 30 min were reported by
A. Oksanen on February 1, and the object started fading
(vsnet-campaign-dn 3338, 3393, 3360, 3370, 3373, 3374, 3375).
SN 2003L (RA = 11h03m12s.33, Dec = +11d04'38".3)
GCN No. 1834 reported the radio observation of SN Ic 2003L
(vsnet-campaign-sn 535, 538, 544), which was detected as a quite
bright transient in 8.5 GHz band. The reporter says it is
comparable to the radio luminosity of type-Ic hypernova SN 1998bw,
so it possibly is a very energetic event (vsnet-campaign-sn 548).
SN 2003M (RA = 12h13m21s.00, Dec = +21d38'48".4)
The CfA team took a spectrum of SN 2003M on Jan. 26.38. They
reported that it was an unusual type-Ia SN, resembling a dim SN Ia
1991bg 3 weeks after maximum light (vsnet-campaign-sn 546).
MisV1147 (RA = 22h54m03s.78, Dec = +58d54'02".1)
The object had recovered from the last fading
(vsnet-campaign-unknown 180). And then, it again experienced fading
on January 1 (vsnet-campaign-unknown 181).
SN 2002gz (RA = 02h34m10s.36, Dec = -00d53'18".2)
The Las Campanas Observatory spectra of this object taken between
2002 Oct. 29 and 2003 Jan. 10 suggest that it has evolved into
normal type Ic supernova, though it showed some difference in the
earlier dates. It did not show evidence for strong He I lines, so
type IIb classification is unlikely. The reporters (M. Hamuy,
M. Phillips and J. Maza) proposed that, if the undulation near
H-alpha is indeed due to the hydrogen, this object should be called
as "type IIc" (vsnet-campaign-sn 546).
V4744 Sgr (RA = 17h47m21s.724, Dec = -23d28'22".79)
S. Kiyota reported on January 30 that V4744 Sgr (the fourth nova
in Sgr last year) has experienced a dramatic fading (Ic=13.55). The
nova has been proposed to be an Fe II-class nova caught during the
early stage of an outburst (cf. vsnet-alert 7566, 7576). Together
with the slow fading and the narrowness of the emission lines
observed in November (before the solar conjunction), the nova may
have experienced a dust fading as observed in the slow nova V705 Cas
(vsnet-campaign-nova 1150).
*** Future schedule ***
eta Car: The next "shell event"/X-ray eclipse
M. Corcoran reported the event will occur this summer.
Coordinated ground-based observations of eta car along with the
X-ray observations would be really important.
For more information:
Latest X-ray light curve:
http://lheawww.gsfc.nasa.gov/users/corcoran/eta_car/etacar_rxte_lightcurve/
[vsnet-campaign-sdor 23, 24]
[vsnet-campaign-xray 172]
Light curve provided by S. Otero:
http://ar.geocities.com/varsao/Curva_Eta_Carinae.htm
[vsnet-campaign-sdor 22]
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 ***
XZ Eri
Eclipse ephemeris, see [vsnet-campaign-dn 3362, 3408]
DV UMa
Eclipse ephemeris, see [vsnet-campaign-dn 3368]
GZ Cnc
Light curve by T. Vanmunster:
http://vsnet.cbabelgium.com
[vsnet-campaign-dn 3385]
UX UMa
Time-series observation by H. Maehara, see [vsnet-campaign-data
107]
BC UMa
Data observed by T. Hynek:
http://ostrava.astronomy.cz/czdetails.php?id=153
[vsnet-campaign 1367]
[vsnet-campaign-dn 3396]
SN 2003M
Spectrum taken by the CfA team:
http://cfa-www.harvard.edu/cfa/oir/Research/supernova/spectra/sn2003m-20030126.flm.gif
[vsnet-campaign-sn 546]
Discussion about "Multi-letter codes: CR, CV, CI, CB"
[vsnet-campaign-ccd-discussion 13, 14, 15, 16, 17, 18, 19, 20, 21]
(This summary can be cited.)
Regards,
Makoto Uemura
Return to Daisaku Nogami
vsnet-adm@kusastro.kyoto-u.ac.jp
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