[Message Prev][Message Next][Thread Prev][Thread Next][Message Index][Thread Index]
[vsnet-campaign 620] VSNET Weekly Campaign Summary
VSNET Weekly Campaign Summary
*** Last week news ***
(new targets)
RZ Leo (RA = 11h37m22s.27, Dec = +01d48'58".9)
As reported by Rod Stubbings in [vsnet-alert 5437], the possible WZ Sge
type dwarf nova RZ Leo is undergoing an extremely rare outburst (12.1mag on
December 20.662). The magnitude (12.1v) is probably the brightest one
except for the original discovery at mpg=11.5 (vsnet-campaign 584, 589).
[vsnet-obs 31246] tells that the rare outburst of RZ Leo has been
confirmed by T. Kinnunen, at mv=12.2 on December 21.21 UT
(vsnet-campaign 591, vsnet-campaign-dn 327).
T. Vanmunster detected periodic modulations in a light curve on
December 20/21 (vsnet-alert 5446). The Kyoto team (R. Ishioka et al.)
performed CCD time-series observations on December 21, 22, 23, 24
(vsnet-campaign 594, vsnet-campaign-dn 338,349). Gary W. Billings
presented a light curve and its data on December 20/21 at his web site
(see below,"General Information")(vsnet-campaign 611). Combined with
G. W. Billings's data, the early Kyoto data shows periodicity of
0.07631 d which is extraordinally close to the photometric period
(0.0756 +/- 0.0012 d, Mennieckent et al., 1999, Astron. Astrophys.
352, 239). The observed early hump profile is also peculiar in contrast
to "usual" superhumps in SU UMa stars. The humps show a complex structure,
similar to "early superhumps" observed in other WZ Sge-type stars
(vsnet-campaign 598, 599, 600, 617). T. Vanmunster analyzed his 3 nights
data and reported 0.0755 d period which is consistent with the results
by the Kyoto team (vsnet-campaign 602).
The light curve obtained by the Kyoto team on December 23 revealed
"true" superhumps was evolving with an amplitude of ~0.3mag
(vsnet-campaign 603). G. Masi showed a light curve and a CCD image on
December 23 at his web site (see below, "General Information")
(vsnet-campaign 604, vsnet-campaign-dn 341), which shows superhumps with
some secondary features whose period is about 0.08d and amplitude is
about 0.2mag (vsnet-campaign-dn 341). S. Kiyota performed CCD
time-series observation on December 21, 23, 24 (vsnet-campaign 600, 603).
Combined with S. Kiyota, G. Masi, and the Kyoto data, the data on
December 23 showed a 0.0813 d period (vsnet-campaign 606).
A preliminary period analysis of the combined data by the Kyoto and
S. Kiyota on December 24 yields the the decrease of the superhump period
to 0.079 d (vsnet-campaign 612). B. Warner and P. Woudt have observed
RZ Leo for three nights at the South African Astronomical Observatory.
They report that they saw low amplitude humps on the first two nights,
but that last night there was a full superhump with an amplitude of about
0.35 mag (vsnet-campaign 609, vsnet-campaign 610).
WY Tri (RA = 02h25m12s.08, Dec = +33d00'31".5)
T. Vanmunster performed time-series photometry on December 20/21 at
CBA Belgium Observatory, and reported that the light curve clearly shows
the presence of a 0.38 mag modulation, to be attributed to superhumps.
The superhump period is calculated to be 0.0786 d, and he thus concluded
WY Tri is a new member of SU UMa-type dwarf novae (vsnet-campaign 588,
vsnet-campaign-dn 326). J. Pietz performed 3h45m run on December 20
(vsnet-campaign 595). The Kyoto team (R. Ishioka et al.) also
calculated a superhump period of 0.0784 d with a 4.1-hour observation on
December 22 (vsnet-campaign 601). T. Kato reported a light curve
presented by R. Novak (at Brno) also clearly shows superhumps
(vsnet-campaign 605). Based on Kyoto data and Brno data the superhump
period was calculated to be 0.07889 d (vsnet-campaign 608).
The Kyoto team obtained another series of WY Tri on December 24. The best
superhump period from all observations (Kyoto data and Brno data) is
0.07863 d, which is slightly shorter than the previous result.
T. Kato commented this may have been a result of shortening of the
superhump period (vsnet-campaign 616). The superoutburst is still
ongoing, and the current magnitude is around 16.1mag (vsnet-campaign-dn 343).
UV Per (RA = 02h10m13s.58, Dec = +57d11'26".8)
As reported by M. Simonsen on December 25 in [vsnet-outburst 1233],
the SU UMa-type dwarf nova UV Per is undergoing one of its relatively
rare outbursts at 12.0mag. The most recent outbursts were in 1999 June
(mv=12.8, Poyner, normal outburst) and 1998 July superoutburst.
The outburst interval suggest that the present outburst is a superoutburst
(vsnet-campaign 613, 614). The Kyoto team performed four hours
time-series photometry on December 25, and confirmed the outburst
at about 12.2mag (vsnet-campaign 615).
CH UMa (RA = 10h07m00s.90, Dec = +67d32'45".0)
As reported by J. Gunther, the long-period dwarf nova CH UMa is
in outburst. The last major outburst was observed in 2000 April
(vsnet-campaign-dn 318).
Z Cha (RA = 08h07m16s.29, Dec = -76d32'20".9)
As reported by R. Stubbings on December 20, the eclipsing SU UMa-type
dwarf nova Z Cha was in outburst at 12.3mag (vsnet-outburst 1187,
vsnet-campaign-dn 325). The outburst continued (vsnet-campaign-dn 328)
until R. Stubbings and A. Pearce observed its fading to about 15mag
on December 23(vsnet-campaign-dn 348).
KV And (RA = 02h17m13s.85, Dec = +40d41'30".6)
P. A. Dubovsky reports an outburst (13.6mag) of the SU UMa star KV And
on December 20. In spite of past superhump detections, the last reported
likely superoutburst occurred in 1998 January (vsnet-campaign 590).
The outburst continues, and the current magnitude is around 14.6
(vsnet-campaign-dn 344).
BR Lup (RA = 15h35m51s.61, Dec = -40d34'25".4)
As reported by A. Pearce on December 22, the SU UMa-type dwarf nova
BR Lup is in outburst at 14.0mag (vsnet-campaign-dn 345).
(continuous targets)
V383 Vel (RA = 10h21m41s.7, Dec = -49d49'24".33")
The outburst since December 13 was terminated as reported by
R. Stubbings on December 17 (15.2mag; vsnet-campaign-dn 320).
CY UMa (RA = 10h56m57s.69, Dec = +49d41'09".1)
J. Pietz reported his 3-hour observation on December 17 shows
clear humps with an amplitude of 0.3mag (vsnet-campaign-dn 317).
The superoutburst continues, and the current magnitude is around 13.7mag
(vsnet-campaign-dn 347).
VZ Pyx (RA = 08h59m20s.0, Dec = -24d28'56".1)
The superoutburst was terminated around December 18
(vsnet-campaign-dn 321). The time-series observation by S. Kiyota
can be available in [vsnet-campaign-data 53 (December 9), 54 (December 11),
55 (December 16)].
TY PsA (RA = 22h49m40s.31, Dec = -27d06'54".3)
Time-series observations by S. Kiyota can be available in
[vsnet-campaign-data 56 (December 5)].
V803 Cen (RA = 13h23m44.5s, Dec = -41d44'30".1)
On December 17, a bright outburst of V803 Cen again occurred as
indicated by R. Monard's observation of 14.2mag (vsnet-campaign-dn 322).
The outburst continues (vsnet-campaign-dn 346).
OY Car (RA = 10h06m22s.46, Dec = -70d14'04".4)
The fading part from the superoutburst was observed during the last week
(vsnet-campaign-dn 323).
BL Lac (RA = 22h02m42.86s, Dec = +42d16'37.6")
The activity can still be seen. M. Verdenet's observation of
13.5mag on December 17 indicates a brightenings of BL Lac
(vsnet-campaign-blazar 113,114).
Delta Vel (RA = 08h44m42s.1, Dec = -54d42'30")
The eclipse observations by S. Otero on December 17 were seen in
[vsnet-campaign-deltavel 33]. S. Otero posted a light curve of
eclipses to [vsnet-image 29] (vsnet-campaign-deltavel 34).
TV Col (RA = 05h29m25s.5, Dec = -32d49'05".2)
The Kyoto team (M. Uemura et al.) reported a brightenings of TV Col
on December 24 (vsnet-campaign-ip 17). S. Kerr reported the other
outburst on December 21 (vsnet-campaign-ip 19, vsnet-campaign-ip 20).
OJ 287 (RA = 08h51m57s, Dec = 20d17'59")
The bright state continues. H. Itoh reported 14.5mag on December 23
(vsnet-campaign-blazar 115).
*** Future schedule ***
TV Col campaign conducted by A. Retter (2001 January 2 - 15):
"Recently using previously published data, we discovered evidence for
another periodicity in the light curve of TV Col. The 6.4-h period would
be the longest recorded positive superhump. To confirm this period, I'll
carry out continuous photometry on TV Col during two weeks in January
(2-15) using the 0.75-m reflector with the UCT CCD in Sutherland, South
Africa.
I am calling for a campaign on TV Col during these nights. As the
candidate periodicity is relatively long, multi-longitude continuous
monitoring of the object is extremely important to reduce the aliasing
problem. So, if you can observe the object for at least ~4 h (preferably
more than one 6.4-h cycle), please let me know."
for more information, see [vsnet-campaign 579],[vsnet-campaign-ip 15]
*** General information ***
Z Cha
eclipse ephemeris, see [vsnet-campaign-dn 324]
RZ Leo
BV sequence:
http://ftp.nofs.navy.mil/pub/outgoing/aah/sequence/sumner/rzleo.seq
[vsnet-campaign 587]
Historical outburst record, see [vsnet-campaign 593]
VSNET RZ Leo page:
http://vsnet.kusastro.kyoto-u.ac.jp/vsnet/DNe/rzleo.html
[vsnet-campaign 597]
Light curve on December 23 presented by J. Pietz:
http://vsnet.eurolink.it/comets/rzleo.gif
CCD image on December 23 presented by J. Pietz:
http://vsnet.eurolink.it/comets/rzleo.jpg
[vsnet-campaign-dn 341]
Light curve on December 20/21 presented by Gary W. Billings:
http://vsnet.telusplanet.net/public/obs681/RZLo1220.gif
and its data:
http://vsnet.telusplanet.net/public/obs681/RZLo1220.txt
[vsnet-campaign 611]
TV Col
eclipse ephemeris, see [vsnet-campaign-ip 18]
UV Per
VSNET UV Per 1996 page:
http://vsnet.kusastro.kyoto-u.ac.jp/vsnet/DNe/uvper96.html
(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
VSNET Home Page