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VSNET campaign target list (2003 June 20)
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VSNET Collaboration Paper on GRB 030329 published in Nature
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We are happy to announce that a VSNET Collaboration paper on the
gamma-ray burst (GRB) on 2003 March 29 is now published in the June 19
issue of Nature (volume 423, page 843).
The authors of the papers are:
* Makoto Uemura (Department of Astronomy, Kyoto University)
* Taichi Kato (Department of Astronomy, Kyoto University)
* Ryoko Ishioka (Department of Astronomy, Kyoto University)
* Hitoshi Yamaoka (Faculty of Science, Kyushu University)
* Berto Monard (Bronberg Observatory, South Africa)
* Daisaku Nogami (Hida Observatory, Kyoto University)
* Hiroyuki Maehara (Variable Star Observers League in Japan)
* Atsushi Sugie (Dynic Astronomical Observatory)
* Susumu Takahashi (Dynic Astronomical Observatory)
Congratulations to all the collaborators! And this publication
illustrates the ability of the VSNET Collaboration, the global newtork
of amateur/professional astronomers dedicated to transient phenomena
and variability, in the field of GRBs, needless to say in cataclysmic
variables and black hole accretion disks.
We hope we can make a fruitful collaboration on a next suitable burst!
<< For more details, please read the following message from Uemura-san >>
We are pleased to notify everyone that the following paper has been
published in Nature June 19 issue.
"Structure in the early afterglow lightcurve of the gamma-ray burst of
29 March 2003"
Makoto Uemura, Taichi Kato, Ryoko Ishioka, Hitoshi Yamaoka, Berto Monard,
Daisaku Nogami, Hiroyuki Maehara, Atsushi Sugie, and Susumu Takahashi
As you know, on 29 March 2003, one of the most closest and brightest
GRB appeared. We obtained the optical light curve of the early afterglow
of the GRB. In the above paper, we report on our results.
Our observation revealed that, even early phase (<1d) of the afterglow,
the light curve shows unexpectedly complicated structures on the fading
trend. This result showed that continuous observations with a short
exposure-time will be important and useful to study the new feature of
GRB afterglows, rather than a snap-shot observation. Regarding this,
it should be emphasized that this work was supported by the collaboration
of researchers and amateur astronomers. We hope this work encourages
observers all over the world.
Our paper has been published in Nature vol.423, 843.
We put the preprint version of this paper in the astro-ph preprint server,
which will be available in astro-ph/0306396.
If you want to get our data in the paper, please see the comments of
our preprint article.
For general information on GRB030329, see:
http://vsnet.kusastro.kyoto-u.ac.jp/vsnet/GRB/grb030329.html
The special web page for our paper is now under construction.
Regards,
Makoto Uemura
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*** VSNET campaign selected current target list 2003 June 20 ***
Object Class Position Type State Data Remark
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V803 Cen 1 southern HeDN superoutburst! 1 (1)
now oscillating!
GO Com 2 northern UGSU rare superoutburst 1 (2)
evening to post-superoutburst
midnight (rebrightening expected?)
V504 Cen 2 southern NL(VY) new target, mag 13 1 (3)
MV Lyr 2 northern NL(VY) extremely bright 1 (4)
QPOs present
VY Scl 3 southern, NL(VY) rare fading? 1 (5)
morning
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* Class: 1 = primary target, 2 = secondary target, 3 = optional target
* Data: data request, 1 = VSNET core team, data will be received by
campaign report list. 2 = as above, in collaboration with
Hachisu-san.
(1) V803 Cen: definite superoutburst, now entered a new stage of
damping oscillation to a more stable(?) plateau phase.
The present variation very much resembles that of "oscillatory"
rebrightening stage of the 2001 superoutburst of WZ Sge (see abobe URL).
http://vsnet.kusastro.kyoto-u.ac.jp/vsnet/DNe/v803cen0306.html
(2) GO Com: rare superoutburst of the large-amplitude SU UMa-type.
Now in post-superoutburst stage (mag about 16-17) linearly fading
at a rate of 0.1 mag/d. Rebrightening(s) are expected, unless the
system fails to trigger a disk-instability. Observations at this
stage are important in constraining the physics of dwarf novae.
Please continue monitoring, and turn to the priority 1 if it erupts
again.
[VSNET web page]
http://vsnet.kusastro.kyoto-u.ac.jp/vsnet/DNe/gocom0306.html
Possibly related WZ Sge page:
http://vsnet.kusastro.kyoto-u.ac.jp/vsnet/DNe/wzsge01.html
(3) V504 Cen: bright overlooked VY Scl star, now at maximum (mag about 13).
Position: 14:12:49.11, -40:21:37.1 (J2000.0).
(4) MV Lyr: short-term variations with time scales of 10-30 min are
dominant. QPOs with P about 10-11 min sometimes become prominent
Excellent coverage from different observers. No clear superhump
signal is recorded up to now. We may also receive V449 Lyr observations
in the same field (19 07 35.68 +43 59 53.0, J2000.0; the GCVS position
is incorrect). Although V449 Lyr is not particularly a campaign target,
the reported data will be forwarded to vsnet-ecl members for further
analysis.
(5) VY Scl: rare faint state. Visible in the morning only.
Objects recently dropped from the list: PU CMa (faded), CR Boo (now
treated as a continous target), IM Nor (moonlight)
Please closely watch vsnet-alert and vsnet-outburst for other new
outbursts.
Web resource:
http://vsnet.kusastro.kyoto-u.ac.jp/vsnet/DNe/gocom0306.html
http://vsnet.kusastro.kyoto-u.ac.jp/vsnet/DNe/gocom.html [background info]
http://vsnet.kusastro.kyoto-u.ac.jp/vsnet/DNe/v803cen0306.html
*** Notice ***
This list is "read-only", i.e. it is used only for announcement of
the target lists. Other information, as well as reports and discussions
on particular targets, should be directed to the appropriate VSNET campaign
sub-lists (e.g. vsnet-campaign-dn for dwarf novae).
Nightly time-series observations should be now directed to (rather than
private e-mails):
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vsnet-campaign-report@ooruri.kusastro.kyoto-u.ac.jp
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Reports sent to this address will be delivered to the VSNET campaign
local staffs, including Ishioka-san, Uemura-san and me, and are expected
to be more convenient than personal e-mails to separate addresses.
Regards,
Taichi Kato
VSNET admin
Return to the Daisaku Nogami
vsnet-adm@kusastro.kyoto-u.ac.jp
