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[vsnet-campaign 456] VSNET Weekly Campaign Summary
VSNET Weekly Campaign Summary
*** Last week news ***
(new targets)
NSV 14652 (RA = 23h38m49s.1, Dec = +28d19'55")
As reported by T. Vaunmunster on August 22 in [vsnet-alert 5202],
the suspected dwarf nova NSV 14652, the possible identification with
a ROSAT source, experienced the outburst at 15.8mag (vsnet-campaign 439).
P. Schmeer reported another brightening for a few days in 1993 June
(vsnet-campaign 439). T. Vanmunster performed a time-series observation
on August 22/23 which yielded a 0.5 mag modulation in the resulting
light curve (covering a total of 6.1 hours) (vsnet-campaign 443).
The confirmation of modulation and the current state is needed.
V425 Cas (RA = 23h03m38s.60, Dec = +53d17'10".8)
The VY Scl-type novalike system V425 Cas may be in faint state (15.1mag
on August 21 by T. Kinnunen). The object was in "high" state in 1999,
but experienced a low state in 1998 (vsnet-campaign 441).
Both deep nightly observations and time-resolved photometry are
recommended.
V368 Peg (RA = 22h58m43s.5, Dec = +11d09'13")
V368 Peg = Var63 Peg started the outburst, as reported by R. Stubbings
(13.8mag on August 26). The star is an SU UMa-type dwarf nova,
whose nature was revealed by J. Pietz (vsnet-obs 22110, vsnet-alert 3317)
during the last outburst in 1999 August (vsnet-campaign 448).
The E. Muyllaert's observations showed the object was bright on August 26
(12.5mag), which strongly suggested the outburst is a superoutburst
(vsnet-campaign 454).
Time-series photometry is strongly encouraged to study the superhump.
LX And (RA = 02h19m44s.00, Dec = +40d27'23".5)
The outburst of this dwarf nova was detected by M. Simonsen on August 12.
T. Vanmunster performed time-series photometry on August 12/13 and 13/14
and reported that the resulting light curve is more or less flat, with
presumably traces of short term modulations with very low amplitude
(around 0.01 mag) (vsnet-campaign 437).
FX Cep (RA = 21h03m12.5s, Dec = +66d10m51.2s)
T. Kinnunen detected the outburst at 15.0mag on August 23
(vsnet-outburst 415). T. Vanmunster performed a time-series CCD
photometry on August 23/24 and reported the light curve is rather flat.
He suggested that this variable is an UGSS-type dwarf nova
(vsnet-campaign 445).
V1062 Cyg (RA = 21h08m12s.60, Dec = +36d49'16".6)
Recent observations show possible separate outbursts, i.e. 14.6:
on August 21 and 14.6: on August 25 (by M. Simonsen) (vsnet-campaign 450).
Close monitorings and time-series observations are encouraged.
V405 Vul (RA = 19h53m05s.0, Dec = +21d14'50")
T. Vanmunster performed a time-series observations on August 25/26,
and revealed that it clearly shows superhumps with the period of
0.1205 +/- 0.0019 d and a full superhump amplitude of 0.19 mag.
This findings confirmed V405 Vul as an SU UMa dwarf nova with the
second-longest superhump period, and very close to the upper border
of the period gap (vsnet-campaign 452).
This became a high priority target. More observations in early phase of
superoutburst are expected in the next outburst. The confirmation
of the current state is also important.
V1141 Aql (RA = 19h37m10s.01, Dec = +02d35'59".2)
As reported by R. Stubbings, the (still poorly studied) SU UMa-type
dwarf nova V1141 Aql is undergoing an outburst (15.0mag on August 28).
The object was observed in superoutburst in 1999 October, the first
time when superhumps were detected (vsnet-campaign 455).
Time-series observations are strongly encouraged.
(continuous targets)
Rho Cas (RA = 23h54m22s.99, Dec = +57d29'58".7)
T. Kato forwarded the observation by M. Nezel (5.1mag on August 22)
(vsnet-campaign-rhocas 5). The faint state continues. Close
monitorings are encouraged.
V550 Cyg (RA = 20h05m05s.21, Dec = +32d21'21".0)
T. Kato found on August 21 that the real position seems to be slightly
east to the DWS position by comparing the images (in outburst) and available
charts (vsnet-campaign-dn 115). On August 22, Ouda team reported the
revised superhump period of 0.0682 d, or its alias 0.0639 d and that
there is an evidence of super-QPOs around every superhump minimum
(vsnet-campaign 436). J. Pietz provided time-series data which confirms
the presence of superhumps (vsnet-campaign-dn 117). H. Yamaoka
performed astrometry using the images taken at Ouda and reported that
the object observed by O'conner (vsnet-obs 29250) is not the real V550 Cyg,
and the position mentioned on vsnet-campaign 435 (weekly Campaign Summary
by Uemura) is incorrect (the correct coordinate is written above).
And, the real V550 Cyg is about 3" east or east-southeast from the DWS
position and the position of the candidate of V550 Cyg at quiescent (Skiff,
1999, IBVS 4675). Further, on the DSS2 Bj images, the faint object
(19.5-20.0) lies on the neighbour of the position. The amplitude of
this CV is therefore quite large, likely more than 5 magnitude
(vsnet-campaign-dn 120, vsnet-campaign 447).
The final phase of this superoutburst will come within this few days.
Observations are encouraged.
V1504 Cyg (RA = 19h28m55s.87, Dec = +43d05'39".9)
Relatively bright outburst (14.2mag) was detected by L. Cook on
August 26 (vsnet-campaign 449).
Delta Sco (RA = 16h00m19s.9, Dec = -22d37'17")
The object is still brighter than the normal state.
Close monitorings are encouraged.
SN 2000cx (RA = 01h24m46s.15, Dec = +09o30'30".9)
The object showed a relatively rapid fading in the last week
(vsnet-campaign-sn 54).
XTE J1118+480 (RA = 11h18m10s.9, Dec = +48d02'12".9)
M. Uemura reported a possible rebrightening from the rapid decline
on August 22 from the recent Kyoto observations (vsnet-campaign-xray 41),
however, no prominent rebrightening is confirmed from the data on August 23.
The decline trend has become more gradual (vsnet-campaign-xray 42).
Nyrola team performed a time-series photometry on August 24 and reported
that the data shows 0.5 magnitude variability that is about twice the
measurement error and the average magnitude to be 17.03mag
(vsnet-campaign-xray 43).
The object is now faint, but still brighter than the quiescent state.
Observations are encouraged.
V803 Cen (RA = 13h23m44.5s, Dec = -41d44'30".1)
The brightness of this object again showed an oscillation from 14.2mag
on August 17.419 to 13.4mag on August 20.456 reported by R. Stubbings
(vsnet-campaign-dn 114). The fading from this outburst was observed
on August 22 by R. Stubbings (vsnet-campaign-dn 119), and then,
again enter the fainter state on August 26 (14.6mag by R. Stubbings).
NSV 26158 (RA = 23h53m51.02s and Dec = +23d09'19.5")
The unclassified brightening continues during the last week
(vsnet-campaign 442). T. Kinnunen reported the fading from this
brightening on August 23 (15.2mag) - 25 (15.5mag) (vsnet-campaign 451).
Multicolor photometry and spectroscopy are encouraged to monitor
the change in the object's status.
V446 Her (RA = 18h57m21s.51, Dec = +13d14'27".3)
D. Nogami reported a preliminary results of V446 Her campaign scheduled
throughout this summer. The light curve is peculiar for a dwarf nova.
See below for more detail information (vsnet-campaign 446).
*** Future schedule ***
V446 Her campaign (throughout this summer)
Boris T. Gaensicke organize a campaign on the post nova V446 Her (V~18).
Their aim is to obtain a *good* contiguous light curve of V446 Her that
covers 2-3 dwarf nova-like outbursts of the system, in order to compare
its outburst characteristics to those of ``normal'' dwarf novae.
They invite those of you equipped with a CCD camera to obtain a couple
of images of V446 Her per night throughout the next three months, say,
until the end of September.
For more information, please see [vsnet-campaign 325] or contact
with Boris T. Gaensicke (boris@uni-sw.gwdg.de).
In [vsnet-campaign 446].....
"Now, one and a half month later, we present a preliminary lightcurve
which you can find at
"http://alpha.uni-sw.gwdg.de/~mschrei/v446her/light.gif".
The light curve is very interesting, ......
Hence we again invite those of you equipped with a CCD camera to
obtain a couple of images of V446Her per night at least until the
end of September. Together we can rewrite the post nova scenario !!!"
*** General information ***
P Cyg
E. Pollmann presents the development of the Halpha-emission of P Cyg
after the minimum at JD 2451770, see [vsnet-campaign-image 3] or
[vsnet-campaign 444].
V446 Her
Preliminary light curve from V446 Her campaign team:
http://alpha.uni-sw.gwdg.de/~mschrei/v446her/light.gif
[vsnet-campaign 446]
(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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