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VSNET Weekly Campaign Summary
*** Last week news ***
(new targets)
SN 2003ik (RA = 08h04m06s.52, Dec = +62d59'19".8)
SN 2003ik is hosted by MCG +11-10-56, an edge-on spiral galaxy
which is a northwestern component of a galaxy triplet CGCG 310-032.
The discovery magnitude (16.6C mag) is consistent with the expected
maximum of typical SN Ia (vsnet-campaign-sn 702). The UCB team
revealed that it was a type Ia SN near maximum on Oct. 2
(vsnet-campaign-sn 704).
AG Dra (RA = 16h01m40s.98, Dec = +66d48'10".3)
An outburst of 9.2mag was reported on September 29 by
E. Muyllaert. The last outburst occurred exactly one year ago
(vsnet-campaign-symbio 82). The outburst continues
(vsnet-campaign-symbio 84).
SV Sge (RA = 19h08m11s.75, Dec = +17d37'41".3)
The object may have started fading in late September
(vsnet-campaign-rcb 164).
V630 Cyg (RA = 21h34m59s.21, Dec = +40d40'18".5)
An outburst was detected on September 24 (vsnet-campaign-dn
3992). A long duration indicates a superoutburst, which is still
ongoing (vsnet-campaign-dn 3999).
Possible Nova in M31 (RA = 00h42m46s.72, Dec = +41d19'46".7)
K. Hornoch reported a discovery of a possible nova in M31 on images
taken on 2003 Sep. 30.835 UT. It was fainter than 18.6mag on
Sep. 26.812 and recorded with 17.0 mag on Sep. 30.835 UT
(vsnet-campaign-nova 1500). K. Hornoch confirmed the object at
17.2mag on October 1/2 (vsnet-campaign-nova 1501). G. Sostero also
reported a confirmation of the object at 16.7mag on Sep. 29.83
(vsnet-campaign-nova 1502).
SN 2003im (RA = 00h44m59s.28, Dec = -08d53'11".5)
SN 2003im is hosted by 2MASX J00445922-0853228 = NPM1G -09.0031, a
small galaxy superimposed on the Abell 85 cluster. The recession
velocity of this galaxy suggests that it would be a foreground
one, and the expected maximum for typical SN Ia is mag about 16.2
(vsnet-campaign-sn 703). The UCB team revealed that it was type Ia
SN about 1 months after maximum (Oct. 2 UT spectrum)
(vsnet-campaign-sn 704).
SN 2003in (RA = 03h35m33s.31, Dec = +05d03'52".7)
SN 2003in is hosted by IC 1956, a barred-spiral galaxy. The
expected maximum for typical SN Ia is mag about 17.0
(vsnet-campaign-sn 703). The UCB team revealed that it was type Ia
SN about 2-3 weeks after maximum (Oct. 2 UT spectrum)
(vsnet-campaign-sn 704).
CH Cyg (RA = 19h24m33s.07, Dec = +50d14'29".5)
The object is now gradually brightening (vsnet-campaign-symbio 83).
V834 Cen (RA = 14h09m07s.4, Dec = -45d17'16")
The object is returning to a bright state (vsnet-campaign-polar 37).
SN 2003io (RA = 02h17m26s.87, Dec = +14d34'36".3)
SN 2003io is hosted by UGC 1761, an irregular galaxy within a
small group of galaxies. The expected maximum for typical SN Ia is
mag about 15.5 (vsnet-campaign-sn 704).
SN 2003ip (RA = 00h33m16s.76, Dec = +07d54'19".5)
SN 2003ip is hosted by UGC 327, a spiral galaxy which makes a pair
with CGCG 409-034. The UCB team took a spectrum of SN 2003ip on
Oct. 2 UT and showed that it was type II SN within a few weeks after
the explosion (vsnet-campaign-sn 704).
(continuous targets)
RU Hor (RA = 02h46m05s.38, Dec = -63d35'04".0)
The best superhump period is reported to be 0.07090(1) d
(vsnet-campaign-dn 3988, 3994). The superoutburst is ongoing
(vsnet-campaign-dn 3990).
SN 2003hf (RA = 16h50m48s.38, Dec = +45d24'01".8)
The UCB team reports that it is indeed a type II SN. It is likely
a type II-L (linearly decliner) (vsnet-campaign-sn 701).
SN 2003hp (RA = 17h40m18s.69, Dec = +51d01'41".3)
The UCB team reports that it is a peculiar type Ic SN (SN
1998bw-like, say, hypernova) (vsnet-campaign-sn 701).
SN 2003ht (RA = 02h59m55s.17, Dec = +24d13'36".8)
It is a type II SN in the nebular (late) phase (vsnet-campaign-sn 701).
SN 2003hw (RA = 03h01m50s.02, Dec = +35d44'36".4)
The UCB team took a spectrum on Sep. 28 and showed that it was a
type Ia SN about 2 months after maximum (vsnet-campaign-sn 701).
SN 2003ig (RA = 04h09m43s.50, Dec = +37d00'45".8)
The UCB team took a spectrum on Sep. 28 and showed that it is a
type Ic SN, within a week after maximum (vsnet-campaign-sn 701).
SN 2003gq (RA = 22h53m20s.68, Dec = +32d07'57".6)
They reobserve it and confirmed the peculiarity. A spectrum
resembles to that of SN 2002cx, which has unusually narrow lines
(vsnet-campaign-sn 701).
SN 2003ij (RA = 05h55m41s.18, Dec = +85d54'21".7)
The UCB team revealed that it was a type Ia SN within a few days
of the maximum light on Oct. 2. It has possibly brightened from the
discovery magnitude (vsnet-campaign-sn 704).
V1294 Aql (RA = 19h33m36s.9, Dec = +03d45'41")
S. Otero reports that the object finally reached V=7.55 -according
to ASAS-3 data (by G. Pojmanski)- breaking its previous record of V=
7.51 (vsnet-campaign-be 272).
V551 Sgr (RA = 18h00m56s.46, Dec = -34d35'45".6)
T. Kato reports that timing analysis of the superhumps has yielded
a slightly positive period derivative. This Pdot is seemingly
unusual for this superhump period (vsnet-campaign-dn 3989). The
superoutburst is ongoing (vsnet-campaign-dn 3991).
V2573 Oph (RA = 17h19m14s.086, Dec = -27d22'35".21)
The object rapidly faded in September (vsnet-campaign-nova 1499, 1504).
V585 Lyr (RA = 19h13m58s.5, Dec = +40d44'09")
The object entered a rapid fading phase. The object remained
bright until Sep. 29 (vsnet-campaign-dn 3993). A rebrightening was
detected by E. Pavlenko at Oct. 3.8UT. It was R=16.4 on Oct. 3 and
fainter than 18.5mag on Oct. 2 (vsnet-campaign-dn 3996). The
rebrightening was also observed by the Kyoto team. The resultant
light curve did not show a rapid fading trend, indicating that the
rebrightening was caught during its premaximum stage. There were
also superimposed hump-like features (about 0.1 mag), which may be
persistent (late)superhumps (vsnet-campaign-dn 3998). D. Rodriguez
reported that it was fainter than 17.1mag on Oct. 4
(vsnet-campaign-dn 3997).
V475 Sct (RA = 18h49m37s.60, Dec = -09d33'50".85)
The object remained calm at ~10 mag (vsnet-campaign-nova 1503),
and then, started rebrightening in early October
(vsnet-campaign-nova 1506).
Z Cam (RA = 08h25m13s.2, Dec = +73d06'39")
The standstill has been confirmed. The last standstill was in
2001 April-July (vsnet-campaign-dn 3995).
*** Future schedule ***
Call for Proposals
for Cycle 1 of the Swift Guest Investigator Program
Notices of Intent due: October 6, 2003
Proposal due date: December 1, 2003
[vsnet-campaign-grb 39]
Stellar-Mass, Intermediate-Mass, and Supermassive Black Holes
Kyoto International Community House, Kyoto, Japan
October 28 - 31, 2003
http://vsnet.astro.isas.ac.jp/conference/bh2003/
[vsnet-campaign-agn 6]
[vsnet-campaign-xray 260]
ASTRONOMICAL POLARIMETRY
CURRENT STATUS AND FUTURE DIRECTIONS
15-19 March 2004, Waikoloa Beach Marriott, Waikoloa, Hawaii
http://vsnet.jach.hawaii.edu/JACpublic/JAC/pol2004
[vsnet-campaign-polar 35]
IAU Symposium No. 222 - BHSIGN Conference
The Interplay among Black Holes, Stars and ISM in Galactic Nuclei
March 1-5, 2004, Gramado, Brasil
http://bhsign.if.ufrgs.br/
[vsnet-campaign-agn 5]
WEBT campaign on AO 0235+16
Campaign with VLBA conducted by Claudia M. Raiteri
from September 2003
see [vsnet-campaign-blazar 305]
X-RAY AND RADIO CONNECTIONS
Santa Fe, New Mexico, USA
3 - 6 February 2004
http://vsnet.aoc.nrao.edu/events/xraydio/
[vsnet-campaign-xray 258]
X-Ray Timing 2003: Rossi and Beyond
November 3-5, 2003
Harvard-Smithsonian Center for Astrophysics
http://hea-www.harvard.edu/xrt2003/
[vsnet-campaign-xray 242]
AR UMa and AM Her campaign with the HST
TOO program conducted by S. Saar and F. Ringwald
see [vsnet-campaign-polar 24]
QS Tel: Call for observations
TOO program with the Chandra conducted by C. Mauche
until the end of 2004
see [vsnet-campaign-polar 28]
WEBT Campaign for AO 0235+16 with XMM-Newton
January-February 2004
please contact to Claudia M. Raiteri,
see [vsnet-campaign-blazar 301]
Multiwavelength AGN Surveys
a "Guillermo Haro" Astrophysics Conference
organized by INAOE
December 8-12, 2003
Cozumel, Mexico
http://vsnet.inaoep.mx/~agn2003/
[vsnet-campaign-agn 4]
Conference: THE INTERPLAY AMONG BLACK HOLES, STARS AND ISM IN
GALACTIC NUCLEI
in Gramado, south of Brasil, March 1-5, 2004
for more information, please contact to BHSIGN@if.ufrgs.br
[vsnet-campaign-agn 3]
eta Car: The next "shell event"/X-ray eclipse
M. Corcoran reported the event will occur this summer.
Coordinated ground-based observations of eta car along with the
X-ray observations would be really important.
For more information:
Latest X-ray light curve:
http://lheawww.gsfc.nasa.gov/users/corcoran/eta_car/etacar_rxte_lightcurve/
[vsnet-campaign-sdor 23, 24,
25, 26, 28, 29, 46]
[vsnet-campaign-xray 172]
Light curve provided by S. Otero:
http://ar.geocities.com/varsao/Curva_Eta_Carinae.htm
[vsnet-campaign-sdor 22, 32, 33]
*** General information ***
RU Hor
VSNET page:
http://vsnet.kusastro.kyoto-u.ac.jp/vsnet/DNe/ruhor.html
[vsnet-campaign-dn 3988]
NMO digest, see [vsnet-campaign-mira 78]
(This summary can be cited.)
Regards,
Makoto Uemura
Return to the Powerful Daisaku
vsnet-adm@kusastro.kyoto-u.ac.jp
