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[vsnet-campaign 711] VSNET Weekly Campaign Summary
VSNET Weekly Campaign Summary
*** Last week news ***
(new targets)
IP Peg (RA = 23h23m08s.7, Dec = +18d24'59".1)
The eclipsing dwarf nova IP Peg experienced an outburst at
13.6mag on January 17 (vsnet-campaign-dn 401). The outburst
amplitude is rather small (vsnet-campaign-dn 405). The fading from
the outburst was observed on January 20 (vsnet-campaign-dn 408).
RX J1155.4-5641 (RA = 11h55m27s.03, Dec = -56d41'53".3)
R. Stubbings and A. Pearce reported an outburst of RX J1155.4-5641
on January 15. The last outburst was observed on 2000 December 9
(vsnet-campaign-dn 403). The object further brightened to 11.8mag
on January 21 as reported by R. Stubbings (vsnet-campaign-dn 409).
SN 2001L (RA = 11h36m48s.83, Dec = -08d35'07".0)
IAUC 7566 informed that KAIT discovered an bright SN Ia.
The discovery made by the image taken on January 18 when the new
object was mag about 15.4. The location is about 4" north of
the nucleus of nearly edge-on spiral (SAb: sp) galaxy MCG-01-30-11.
The spectrum taken by CfA team on January 19 reveals that SN 2001L
is SN Ia about 1 week after maximum. The recession velocity of
the host galaxy (4567 km/s) suggest that the typical SN Ia would
have the maximum brightness of mag 15.7. Reported magnitude is
somewhat brighter, and the peak of the light curve seems to be broader
than the typical one. So, it can be an overluminous SN Ia like SN
1991T.
AG Hya (RA = 09h50m30s.94, Dec = -23d45'03".7)
R. Stubbings reported that the dwarf nova AG Hya has been in
a long outburst since January 14. This star was formerly suspected
as an SU UMa-type dwarf nova, mainly based on its high frequency
of short outbursts. On one previous night, T. Kato performed
a CCD run, which showed a flat light curve, which more favors
an SS Cyg-type classification. However, the observation covered
a only tiny part of a (unknown type) outburst, independent check
for superhumps is encouraged (vsnet-campaign 709).
(continuous targets)
SN 2001G (RA = 09h09m33s.18, Dec = +50d16'51".3)
It has been brightening since its discovery. O. Trondal and
M. Fiaschi reported the magnitude of 15.3C on January 15 and
14.4R on January 16, respectively (vsnet-campaign-sn 135, 137).
V344 Ori (RA = 06h15m18.94, Dec = +15d30'59".9)
The present outburst outshined the GCVS maximum (14.2p)
(vsnet-campaign 692). On the basis of the light curve taken
at Kyoto on January 16, M. Uemura, the Kyoto team, reported
the detection of modulations which they considered to be
attributed to superhumps (vsnet-campaign-dn 397, vsnet-campaign-696).
These modulations however turned out to be more irregular
rather than typical superhumps. T. Vanmunster performed
7.7 hours time-series photometry on January 16/17, and reported
that there's indeed a 0.1 mag modulation, but it definitely
doesn't look like a common superhump, being very irregular in
shape and pattern (vsnet-campaign 698). H. Yamaoka performed
astrometry using CCD images taken at Kyoto, and suggests the
quiescent identification in USNO A2.0 1050-03226705 r=17.8 b=18.4
(vsnet-campaign 699, 701). M. Moilanen also reported the results of
astrometry which is consistent with the above one (vsnet-campaign 707).
S. Kiyota reported a short run on January 17 (13.30-13.48 mag)
(vsnet-campaign 700). T. Kato noted that there is a neighbor
known variable star V645 Ori, which needs to be avoided as a
companion star (vsnet-campaign 703). From the data by VSNET
collaboration team on January 16 - 19 (the Kyoto team, B. Martin,
the Nyrola team, H. Boffin, J. Pietz, T. Vanmunster), M. Uemura
reported that the object gradually faded with a rate of 0.08mag/d,
and the modulations show a weak periodicity of 0.066 and 0.039,
however their amplitudes is very variable between 0.02 - 0.1mag
(vsnet-campaign 704, 705, 706). T. Vanmunster commented the
similarity of the activity of V344 Ori to that of V405 Vul
(vsnet-campaign 708). Following this, T. Kato also commented that
EP Car also showed similar activity on 2000 February (vsnet-campaign 710).
The outburst is now ongoing (vsnet-campaign-dn 396, 399, 402, 404,
406, 407, 410).
SN 2001B (RA = 04h57m19s.24, Dec = +78d11'16".5)
The object seems to reach the maximum in the last week at the
magnitude of around 14.4C (vsnet-campaign-sn 134, 136).
V445 Pup (RA = 07h37m56s.88, Dec = -25d56'59".1)
W. Liller reported no short-term variations are seen in 6.5 hours
light curve taken on January 14, and following to T. Kato's remark
about CK Vul, commented that V445 Pup is perhaps similar to the
hydrogen deficient cataclysmic variables CR Boo, CP Eri and V803 Cen,
the main difference being temperature (vsnet-campaign-nova 163).
The fading trend continued until January 17 at about 9.5-9.6mag
(vsnet-campaign-nova 164, 165, 170), however, observations on
January 17 also show it was temporary very faint 9.8-9.9mag
(vsnet-campaign-nova 177). The object again entered gradual
fading phase (vsnet-campaign-nova 181, 182). B. Monard and J. Bedient
reported a brightening to 9.3mag on January 20 and 19, respectively
(vsnet-campaign-nova 183, 184, 185). M. Fujii performed spectroscopic
observation on January 13 and 21, and reported that little change
between them and the line at 659 nm remains the strongest one on
January 21 (vsnet-campaign-nova 186). The nature of the object is
still puzzled.Discussions about similarities of V445 Pup to known
variables are seen in [vsnet-campaign-nova 163, 166, 167, 168, 169,
171, 172, 173, 174, 175, 176, 179, 180].
RZ Leo (RA = 11h37m22s.27, Dec = +01d48'58".9)
The Kyoto observation on January 15 (Ishioka and Uemura) confirms
that RZ Leo remained approximately at the same level as on January 14.
Modulations close to the orbital/superhump period have became more
evident. Very preliminary period analysis favors the superhump
period, which may suggest that the tidally distorted disk remains.
The situation looks very similar to that of EG Cnc (vsnet-campaign 694).
The similar features were also observed on January 16 at Kyoto
(vsnet-campaign 697).
UV Per (RA = 02h10m13s.58, Dec = +57d11'26".8)
The Kyoto observation on January 15 (Uemura and Ishioka) shows
that UV Per continued to fade slowly (vsnet-campaign 695).
BL Lac (RA = 22h02m42.86s, Dec = +42d16'37.6")
Observations on January 16 and 17 shows BL Lac is slightly brighter
(vsnet-campaign-blazar 126).
TV Col (RA = 05h29m25s.5, Dec = -32d49'05".2)
The relatively calm state was interrupted on January 20 when
it again experienced a 1-day outburst at 12.7mag (vsnet-campaign-ip 34,
35, 36).
3C 66A (RA = 02h22m39s.6, Dec = +43d02'08")
The blazar 3C66A is rapidly fading as seen in observations reported
during the last week (vsnet-campaign-blazar 127).
Delta Sco (RA = 16h00m19s.9, Dec = -22d37'17")
It remained at 1.9-2.1mag until January 21 when S. Otero reported
a brightening to 1.81mag and it is now probably in the third maximum
(vsnet-campaign-be 78, 79, 80).
V803 Cen (RA = 13h23m44.5s, Dec = -41d44'30".1)
The observations on January 15 reported by R. Stubbings and
A. Pearce show possible presence of short-term variation between
<13.9 and 13.5 (vsnet-campaign-dn 398). As reported by A. Pearce,
P. Williams, and R. Stubbings, an outburst was reported
on January 19 -- 20 and it remained bright on January 21
(vsnet-campaign-dn 411).
*** General information ***
V344 Ori
CCD image taken at Kyoto:
http://ftp.kusastro.kyoto-u.ac.jp/pub/vsnet/DNe/V344_Ori/v344.gif
[vsnet-campaign 693]
CCD image provided by M. Moilanen:
http://ftp.kusastro.kyoto-u.ac.jp/pub/vsnet/DNe/V344_Ori/v344orir.jpg
[vsnet-campaign 702]
IP Peg
eclipse ephemeris, see [vsnet-campaign-dn 400]
V445 Pup
spectrum taken by M. Fujii on January 13:
http://vsnet1.harenet.ne.jp/~aikow/0113pnp.gif
[vsnet-campaign-nova 186]
(This summary is reproduction free.)
Regards,
Makoto Uemura
vsnet-adm@kusastro.kyoto-u.ac.jp
Return to Daisaku Nogami
vsnet-adm@kusastro.kyoto-u.ac.jp
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