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[vsnet-campaign 1048] VSNET Weekly Campaign Summary
VSNET Weekly Campaign Summary
*** Last week news ***
(new targets)
CI UMa (RA = 10h18m13s.01, Dec = +71d55'42".8)
The SU UMa-type dwarf nova CI UMa experienced an outburst at
13.8mag as reported on July 26 by M. Reszelski. The last
superoutburst occurred in 2000 September (vsnet-campaign 1041).
The outburst was rapidly faded (vsnet-campaign-dn 1039).
SN 2001dh (RA = 20h17m24s.16, Dec = -38d40'37".4)
IAUC 7670 informed that R. Chassagne discovered a new SN 2001dh
on July 22. The brightness of the new object was 15.5 at the
discovery. The position is about 39" east and 11" south of the
nucleus of the edge-on and warped dim galaxy MCG-6-44-26. It was
not detected on June 26.1. The recession velocity of MCG-6-44-26
is around 2600 km/s, which suggests that the typical SN Ia on this
galaxy can reach mag 14 (vsnet-campaign-sn 212).
V503 Cyg (RA = 20h27m15s.61, Dec = +43d41'45".5)
An outburst (13.3mag) was reported by H. McGee on July 23.
The outburst seems to be too early for a superoutburst
(vsnet-campaign-dn 999).
XZ Eri (RA = 04h11m25s.76, Dec = -15d23'24".3)
According to astro-ph/0107505, P. Woudt and B. Warner found
that XZ Eri is an eclipsing dwarf nova with a period of 88.1m.
Outbursts of XZ Eri have been observed roughly once a year
(vsnet-campaign 1045).
HO Del (RA = 20h36m55s.49, Dec = +14d03'09".4)
P. A. Dubovsky reported a possible outburst of HO Del (14.5:mag
on July 28). Confirmations are encouraged (vsnet-campaign-dn 1048).
IP Peg (RA = 23h23m08s.7, Dec = +18d24'59".1)
It is now in outburst. The current magnitude is about 13.3mag
(vsnet-campaign-dn 1050).
(continuous targets)
WZ Sge (RA = 20h07m36s.53, Dec = +17d42'15".3)
The historical outburst of WZ Sge is still ongoing
(vsnet-campaign-dn 996, vsnet-campaign 1024, vsnet-campaign-dn 1000,
1001, 1002, 1008, 1013, 1017, 1038, 1049). The previous outbursts
were observed in 1913, 1946, and 1978 (vsnet-campaign 1015).
On July 23, T. Ohshima discovered the outburst (vsnet-campaign 1016).
Confirmations of the outburst were reported to vsnet-campaign lists
by G. Masi (vsnet-campaign 1014) and P. Schmeer (vsnet-campaign 1015,
vsnet-campaign 1020). K. Ayani promptly performed spectroscopy and
revealed that Balmer lines were in generally absorption
(vsnet-campaign 1022). The light curve obtained by the Kyoto team
shows rapid brightening with a rate of 5 mag/d and birth of short-term
modulations (vsnet-campaign 1025). The light curve provided by
G. Masi after the Kyoto run shows clear humps with a large amplitude,
and furthermore, it had a longer periodicity compared with its orbital
period (vsnet-campaign 1030).
On July 24, A. Good, J. Pietz, G. Masi and the Kyoto team detected
early superhumps with a large amplitude of about 0.5mag
(vsnet-alert 6115, vsnet-campaign 1026, vsnet-campaign 1034).
The period of early superhumps was reported to be 0.05662 day
(vsnet-campaign-dn 1004, vsnet-campaign 1030). The decline rate was
somewhat fast (0.4mag/d) during in the first half of this day
(vsnet-campaign 1026), but then became more gradual (0.23mag/d)
(vsnet-campaign 1030). H. Baba reported that optical spectra taken
by K. Sadakane using 1.88m Okayama telescope show double peak
emission lines of He II and C III/N III which are not seen in
spectra on July 23. Balmer lines had both absorption and emission
components which varied with time (vsnet-campaign 1028, 1031, 1035).
G. Masi noticed the presence of another modulations
(secondary maximum) with an amplitude of 0.15mag
(vsnet-campaign-dn 1005).
On July 25, the spectra taken by K. Ayani also show He II and
C III/N III emissions (vsnet-campaign 1033). The Kyoto team reported
that the early superhumps were similar to those on July 24 during
the early July 25 (vsnet-campaign-dn 1007), however their profiles
changed from "V"-shaped to "U"-shaped one (vsnet-campaign-dn 1009).
The hump period was calculated to be 0.05664 d (vsnet-campaign 1037).
G. Masi reported that amplitudes of humps became smaller and the
profiles were changing (vsnet-campaign-dn 1006, 1010, 1012,
vsnet-campaign 1032). M. Richmond reported that they performed
time-series photometry on July 25 (vsnet-campaign 1038).
On July 26, G. Masi and F. Mallia reported that the profile of
humps, particularly secondary maximum, varies with time as observed
on July 25 (vsnet-campaign 1042). The decrease of hump amplitudes
was confirmed in the light curve presented by the Nyrola team.
Their data also show possible feature like QPOs (vsnet-campaign 1043).
K. Ayani and M. Ioroi (Bisei Observatory) performed spectroscopy
covering two entire orbital cycles (vsnet-campaign 1044). M. Richmond
performed 7.5 hours run (vsnet-campaign-dn 1021).
On July 27, G. Masi reported that the hump profile became complex.
He also reported that the short-term fluctuations became dominant
(vsnet-campaign-dn 1019, 1024, 1029). T. Kato also reported similar
characteristics from the Kyoto observation (vsnet-campaign-dn 1025).
R. Novak and L. Cook informed us that they performed time-series
photometry (vsnet-campaign-dn 1020, 1031).
On July 28, contrary to the last tendency, G. Masi reported that
the profile became more regular and the period seems to be longer,
which may imply that normal superhumps appeared (vsnet-campaign-dn
1030, 1032). T. Kato confirmed this longer periodicity, but noticed
that such phenomenon was observed in the first night of the current
outburst (vsnet-campaign-dn 1035). R. Novak also performed
time-series photometry (vsnet-campaign-dn 1036).
On July 29, T. Kato performed period analysis using the data set
taken by G. Masi, R. Novak, J. Pietz, L. Cook, and Kyoto team during
July 28.8 to 29.7. It yielded a period of 0.05669 d, which is in
agreement not with superhump period, but with the orbital period
(vsnet-campaign-dn 1043). Time-series observations by S. Kiyota
are available in [vsnet-campaign-data 67]. The hump profile is
now more irregular (vsnet-campaign-dn 1052).
G. Masi reported a revised coordinate as shown above
(vsnet-campaign 1014). The outburst cycle of the current outburst
is quite shorter than that previously reported (vsnet-campaign 1023).
M. Watanabe reported a new prediscovery observation by T. Inoue
(mag. 10.5p on July 23.525) (vsnet-campaign 1036). T. Kato wondered
about the reality of the 7.0 mag maximum documented in the literature
since the maxima of the past two outbursts of WZ Sge have been around
8.0 or even fainter (vsnet-campaign-dn 1026). E. Kuulkers reported
that it may be because of the photographic observations taken during
the 1913 outburst which was brighter than the 1946/1978 outbursts
(vsnet-campaign-dn 1041).
Nova Cyg 2001 (RA = 20h07m17s.94, Dec = +36d04'37".2)
(= V2274 Cyg)
Some multi-color observations taken by L. Brat and P. Hajek
are available in [vsnet-campaign-nova 415, 416, 417, 419].
They reported that this nova is very rapidly fading since around
July 28 (vsnet-campaign-nova 419, 420).
V803 Cen (RA = 13h23m44.5s, Dec = -41d44'30".1)
Observations show oscillations of the magnitude of this object
(vsnet-campaign-dn 997).
V818 Sco (RA = 16h19m55s.07, Dec = -15d38'24".5)
This X-ray binary again shows strong activity (vsnet-campaign-xray 77).
V1504 Cyg (RA = 19h28m55.87s, Dec = +43d05'39".9)
The superoutburst is still ongoing (vsnet-campaign-dn 998, 1040).
V1141 Aql (RA = 19h37m10s.01, Dec = +02d35'59".2)
The superoutburst still continues (vsnet-campaign-dn 1014).
AM Her (RA = 18h16m13s.4, Dec = +49d52'03".1)
The object is now very bright at about 12.9mag (vsnet-campaign 1047).
BL Lac (RA = 22h02m42.86s, Dec = +42d16'37.6")
The object is now fading. The current magnitude is about 14.7mag
(vsnet-campaign-blazar 218).
V1548 Aql (RA = 19h07m28s.42, Dec = +11d44'45".8)
This nova brightened to 13.0mag on July 25 as reported b y H. McGee
(vsnet-campaign-nova 418).
*** Future schedule ***
WZ Sge campaign
D. Steeghs wrote:
"Several of us are organizing a campaign on the current outburst
of WZ Sge, using a large variety of ground based facilities as well as
space observatories. A web-page has been setup listing the scheduled
observations so far which we intend to keep up to date at:
http://vsnet.astro.soton.ac.uk/~ds/wzsge.html
"
For more information, see [vsnet-campaign 1039]
EM Cyg campaign with HST on 23 - 29 July
(most likely 12:22-13:10 UT on July 29)
conducted by T. Marsh
For more detailed information, see [vsnet-campaign 999]
V446 Her campaign until September
conducted by Matthias Schreiber, Boris Gaensicke, and Daisaku Nogami
For more detailed information, see [vsnet-campaign-dn 918],
[vsnet-campaign-nova 349], or [vsnet-campaign 983]
CV conference at Goettingen, 5-10 August 2001
[vsnet-announce 15, 20]
Two Years of Science with Chandra *
* This meeting will also be the 12th Annual Maryland Astrophysics
Conference
September 5-7, 2001
For more information, see [vsnet-campaign-xray 66]
*** General information ***
WZ Sge
For observations,
Please make sure that WZ Sge (and comparison) do not saturate
on your images (vsnet-campaign 1017).
Eclipse ephemeris, see [vsnet-campaign 1018]
CCD image during the outburst presented by G. Masi:
http://ftp.kusastro.kyoto-u.ac.jp/pub/vsnet/DNe/WZ_Sge/masi0723.jpg
[vsnet-campaign 1019]
Spectrum presented by K. Ayani:
http://ftp.kusastro.kyoto-u.ac.jp/pub/vsnet/DNe/WZ_Sge/bisei0723.jpg
Comparison of light curves of all previous outbursts:
http://saturn.sron.nl/~erikk/wzsge/wzsge_2001.gif
http://saturn.sron.nl/~erikk/wzsge/wzsge_1913_1946_1978.gif
[vsnet-campaign-dn 1003]
VSNET web pare:
http://vsnet.kusastro.kyoto-u.ac.jp/vsnet/DNe/wzsge01.html
[vsnet-campaign 1027, 1029,
vsnet-campaign-dn 1011, 1040, 1015, 1023,
1027, 1028, 1033, 1034, 1037, 1044, 1045,
1046]
WZ Sge page by G. Masi:
http://vsnet.eurolink.it/comets/wzsge.htm
[vsnet-campaign-dn 1005]
Photometry by M. Richmond:
http://spiff.rit.edu/richmond/ritobs/jul25_2001/jul25_2001.html
http://spiff.rit.edu/richmond/ritobs/jul25_2001/wzsge_jul25ut.dat
[vsnet-campaign 1038]
http://spiff.rit.edu/richmond/ritobs/jul27_2001/jul27_2001.html
[vsnet-campaign-dn 1021]
Photometry by L. Cook
http://vsnet.geocities.com/lcoo/wzsge.htm
[vsnet-campaign-dn 1031, 1042]
WZ Sge light curves presented by R. Novak
http://ada.astronomy.cz
[vsnet-campaign-dn 1054]
V893 Sco
eclipse ephemeris, see [vsnet-campaign-dn 1016]
IP Peg
eclipse ephemeris, see [vsnet-campaign-dn 1047]
(This summary can be cited.)
Regards,
Makoto Uemura
vsnet-adm@kusastro.kyoto-u.ac.jp
Return to Daisaku Nogami
vsnet-adm@kusastro.kyoto-u.ac.jp
VSNET Home Page