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[vsnet-campaign 1275] VSNET Weekly Campaign Summary
VSNET Weekly Campaign Summary
*** Last week news ***
(new targets)
GSC 4822.39 (RA = 07h04m04s.816, Dec = -03d50'50".94)
T. Iijima relayed the discovery report of a possible nova by
N. J. Brown (vsnet-campaign-nova 713). The presense was confirmed
on January 9 by some observers. The object was still faint until
2001 December 26 as shown by pre-discovery observations by J. Bedient
(vsnet-campaign-nova 672, 681, 690, 691). Its measured precise
position suggests that this object is identical to IRAS 07015-0346,
or 2MASS source (vsnet-campaign-unknown 14, 20, vsnet-campaign-nova
686, 696, 697, 701, 705, 706). According to Iijima's report, the
spectrum is dominated by a very red continuum with a very weak
H-alpha emission having a P Cyg profile (vsnet-campaign 1272,
vsnet-campaign-nova 670, vsnet-campaign-unknown 8). Several weak
metal lines are also seen in emission. Time series observations
show the light curve was flat in minute and hour timescales
(vsnet-campaign-nova 678, 680, 685, 692, vsnet-campaign-unknown 15,
17, 19).
T. Kato commented that the IR color excludes the possibility of a
long-period variable. The IRAS color (of the likely far IR
counterpart) is very unusual for a stellar object (vsnet-campaign
1270, vsnet-campaign-nova 668, vsnet-campaign-unknown 6).
S. Kiyota reported magnitudes of B=12.16, V=10.10, Ic=8.28 on
January 9 (vsnet-campaign-nova 671, vsnet-campaign-unknown 9).
A. Henden reported magnitudes and colors of V=9.975, B-V=1.726,
U-B=1.916, V-R=0.943, R-I=0.931 on January 11. T. Kato mentioned
that the color seems to be on a smooth extension of late-type Barium
stars and the expanded photosphere may somehow mimic a late-type
Barium star both in spectrum and colors (vsnet-campaign-nova 704).
The VLA radio observations were performed on January 11 and 12
as reported by M. Rupen. A possible radio counterpart was found
about 5 arcsec east and 8 arcsec north of the reported optical
position (vsnet-campaign-nova 709, vsnet-campaign-unknown 23).
Although the object seems to be some sort of an eruptive object
or a peculiar nova, the nature of the object is still unknown.
It may be possible the phenomenon is related to a flash in
hydrogen-poor environment. The object is still bright, and
any kind of observations are encouraged
(vsnet-campaign-nova 673, 674, 675, 679, 682, 688, 698, 714, 722,
723, 724, 727, vsnet-campaign-unknown 10, 11, 12, 16, 18, 25, 28, 29).
IM Nor (RA = 15h39m26s.20, Dec = -52d19'21".3)
W. Liller discovered an eruption of the recurrent nova IM Nor
in photographs taken between Jan. 10.3432 and Jan 10.3595. The
object has already been bright as seen in photos taken on Jan.
3.3479 and Jan. 3.3493, and nothing was visible at the position of
the star on Oct. 13 down to magnitude 11.5. IM Nor was originally
discovered by I.E. Woods at 9th magnitude on a blue-sensitive plate
taken on July 7, 1920. No other outbursts were found
(vsnet-campaign-npva 689, 695, 700, vsnet-campaign-news 122).
The proposed identification of IM Nor with 2U 1536-52 (as referred
in IAUC 7789) has proven to be false. 2U 1536-52 is an high-mass
X-ray binary QV Nor (vsnet-campaign-nova 717). A low-dispersion
objective prism spectrum, taken Jan. 12.351 UT by W. Liller, shows
H-alpha to be very strong and relatively narrow with FWHM = 950 km/sec
+/-50 (vsnet-campaign-nova 707, 708). T. Kato suggested its outburst
amplitude of 9mag (vsnet-campaign-nova 716, 718, 719, 720, 721).
The object is still bright (vsnet-campaign-nova 710, 712, 715, 725).
SN 2002A (RA = 07h22m36s.14, Dec = +71d35'41".5)
IAUC 7786 informed that the first SN of this year, SN 2002A was
discovered by Beijing team. SN 2002A was caught on Jan. 1.79 (mag
about 17.4), Jan. 8.61 (mag about 16.8) and Jan. 9.56 (mag about
16.8). The position is about 7" east and 15" south of the nucleus
of a spiral (Scd:) galaxy UGC 3804. UGC 3804 is rather nearby
galaxy (v_r = 2887 km/s). The expected maximum for the typical
SN Ia on this galaxy is mag about 14.7. The reported brightness is
rising (0.6 mag during 8 days)(vsnet-campaign-sn 309). The
spectrum taken on Jan 11.12 by the Asiago team has revealed that
SN 2002A is of type IIn soon after explosion (vsnet-campaign-sn 311).
IP Peg (RA = 23h23m08s.7, Dec = +18d24'59".1)
A new outburst was reported by J. Pietz on January 13 at 13.0mag
(vsnet-campaign-dn 2044).
CR Boo (RA = 13h48m55s.42, Dec = +07d57'30".3)
A bright outburst of CR Boo was reported at 13.2mag on January
11 by H. Itoh (vsnet-campaign-dn 2041). The outburst was confirmed
at 13.6mag on January 12 by M. Simonsen (vsnet-campaign-dn 2043).
Variable object by the Deep Lens Survey
(RA = 10h49m32s.82, Dec = -04d31'45".4)
The Deep Lens Survey team reported a new variable object
which was present in images taken on 2002 January 11 at V=22.0
(vsnet-campaign-unknown 22).
KS UMa (RA = 10h20m26s.54, Dec = +53d04'33".5)
As reported by M. Simonsen on January 12, the SU UMa-type
dwarf nova KS UMa experienced an outburst at 13.7mag
(vsnet-campaign-dn 2042).
W Com (RA = 12h21m31.5s, Dec = +28d13m57.6s)
M. Simonsen reported a brightening to 14.1mag on January 10
and confirmed on January 12 (vsnet-campaign-blazar 242).
UX Ori (RA = 05h04m30s.39, Dec = -03d47'18".3)
A fading to 10.2mag was reported on January 11 by E. Muyllaert
(vsnet-campaign-orion 5).
V378 Peg (RA = 23h40m04s.33, Dec = +30d17'47".7)
This novalike variable has been reported to be slightly brighter
(about 13.5mag) (vsnet-campaign-nl 58).
(continuous targets)
HV Vir (RA = 13h21m03s.0, Dec = +01d53'28")
T. Kato reported on January 8 that their reduced data show
clear superhumps with the amplitude of 0.2mag. The analysis
of earlier data has also confirmed that the final transition
to early superhumps to genuine superhumps took less than 5
hours, quite comparable to a sudden change observed in WZ Sge
(vsnet-campaign-dn 2037, 2040, vsnet-campaign-hvvir 38, 41,
42, 45). The period of superhumps were reported to be
0.058330(19) d (vsnet-campaign-hvvir 39, 43). The light curve
observed on January 6 show super-QPOs with a period of 8-10 m
and the maximum amplitude of 0.1 mag (vsnet-campaign-hvvir 40).
Morikawa-san's observation on Jan. 7 revealed the transient
presence of QPOs with a period of 5-6 min (vsnet-campaign-hvvir 44).
On January 9, a possible bump-like structure appeared on the
superhumps (vsnet-campaign-hvvir 47). Clear superhumps were
observed also on January 10 and 11 (vsnet-campaign-hvvir 49, 51).
The clear secondary superhumps appeared on January 11 and 12
(vsnet-campaign-hvvir 53, 55, 58). The data show that superhumps
became less conspicuous on Jan. 13 (vsnet-campaign-hvvir 60).
T. Kato reported a negative superhump period change (around
-2x10^-5), significant at 4 sigma. This negative value makes a
clear contrast to the positive value (Kato et al. 2001, PASJ 53,
1191) observed during the 1992 superoutburst (vsnet-campaign-hvvir
52). Subsequent superhumps however show that the superhump period
has started to lengthen. Such O-C behavior (variable period changes)
was seen in AL Com (vsnet-campaign-hvvir 56).
The superoutburst is still ongoing (vsnet-campaign-hvvir 46, 48,
50, 54, 59).
MisV1147 (RA = 22h54m03s.78, Dec = +58d54'02".1)
S. Yoshida reported the MISAO observations and that it is not
a red variable in conjunction with the DSS images
(vsnet-campaign-unknown 5, 27). Reported observations show the object
may be bright now (visually 13.0-13.2mag) (vsnet-campaign-unknown 26).
HL CMa (RA = 06h45m17s.0, Dec = -16d51'35")
The object further faded until January 8 when a possible
brightening was reported (vsnet-campaign-dn 2038, 2039).
Reported observations then show that the object varies with a
very short time scale (vsnet-campaign 1273). A active state is
still ongoing at about 12.6--12.8mag (vsnet-campaign-dn 2047,
vsnet-campaign 1274).
eta Car (RA = 10h45m03s.65, Dec = -59d41'03".7)
S. Otero reported that observations by J. Garcia show the
reported brightening lasted just a few days (vsnet-campaign-sdor
6, 7). Its activity seems not to increase (vsnet-campaign-sdor 8).
BL Lac (RA = 22h02m42.86s, Dec = +42d16'37.6")
The object is reported to be slightly brighter
(vsnet-campaign-blazar 243).
V854 Cen (RA = 14h34m49s.8, Dec = -39d33'18")
The object began brightening from the faint state
(vsnet-campaign-rcb 10).
RR Tau (RA = 05h39m30s.53, Dec = +26d22'26".3)
The object brightened again. It was reported to be 12.1mag
on January 12 (vsnet-campaign-orion 6).
OW Gem (RA = 06h31m41s.78, Dec = +17d04'56".0)
The object has recovered from the bottom of the eclipse.
The center of eclipse occurred in the early January
(vsnet-campaign-ecl 22, 23, 24, 25, 26, 27, 28, 29, 30, 31,
32, 33, 34, 35, 36).
DY Per (RA = 02h35m17s.12, Dec = +56d08'44".7)
The object faded very slowly (vsnet-campaign-rcb 11).
delta Sco (RA = 16h00m19s.9, Dec = -22d37'17")
The object is now bright at about 1.7mag as reported by
T. Kato and S. Otero (vsnet-campaign-be 154).
V445 Pup (RA = 07h37m56s.88, Dec = -25d56'59".1)
Lynch et al. (2001, AJ, 122, 3313) treats V445 Pup as a
hydrogen-deficient nova, written in a context of the received
diversity of nova phenomenon (vsnet-campaign-nova 703).
SN 2001is (RA = 05h42m09s.07, Dec = +69d21'54".8)
IAUC 7787 reported that SN 2001is is of type Ib, 2-3 weeks after
maximum on Jan. 8.86 (vsnet-campaign-sn 310).
SN 2001it (RA = 15h06m09s.40, Dec = +53d24'41".6)
IAUC 7787 reported that this SN turned out to be of type II SN
around maximum on Jan. 8 (vsnet-campaign-sn 310).
*** Future schedule ***
International Conference on Classical Nova Explosions
Sitges (Barcelona), Spain: 20-24 May 2002
For more detailed information, see http://vsnet.ieec.fcr.es/novaconf
[vsnet-campaign-nova 643]
[vsnet-campaign-nova 666]
Blazar meeting at Tuorla: June 17-21, 2002
for more information, see http://vsnet.astro.utu.fi/blazar02
[vsnet-campaign-blazar 232]
International workshop
"XEUS - studying the evolution of the hot universe"
March 11-13, 2002 ; MPE Garching, Germany
for more information, see
http://wave.xray.mpe.mpg.de/conferences/xeus-workshop
[vsnet-campaign-xray 98]
[vsnet-campaign-xray 104]
*** General information ***
HV Vir
Superhump profile:
http://ftp.kusastro.kyoto-u.ac.jp/pub/vsnet/DNe/HV_Vir/hv2.gif
[vsnet-campaign-hvvir 39]
http://ftp.kusastro.kyoto-u.ac.jp/pub/vsnet/DNe/HV_Vir/hv12.gif
[vsnet-campaign-hvvir 57]
GSC 4822.39
Multi-band CCD images:
http://ftp.kusastro.kyoto-u.ac.jp/pub/vsnet/Novae/gsc4822.39/
[vsnet-campaign 1271]
[vsnet-campaign-nova 669]
[vsnet-campaign-unknown 7]
Spectrum taken by M. Fujii:
http://vsnet1.harenet.ne.jp/~aikow/gsc4822_39.gif
[vsnet-campaign-nova 676]
[vsnet-campaign-unknown 13]
http://vsnet1.harenet.ne.jp/~aikow/gsc4822_39_0111.gif
[vsnet-campaign-nova 711]
[vsnet-campaign-unknown 24]
Charts provided by A. Price:
http://vsnet.aavso.org/charts/standard/MON/VAR_MON_02/
[vsnet-campaign-nova 684]
Charts provided by R. Bouma and E. van Dijk:
http://vsnet.shopplaza.nl/astro/vs-charts/pnovamon.htm
[vsnet-campaign-nova 683]
http://charts.aavso.org/MON/VAR_MON_02/
[vsnet-campaign-nova 693]
UBVRI field photometry presented by A. Henden:
http://ftp.nofs.navy.mil/pub/outgoing/aah/sequence/nmon02.dat
[vsnet-campaign-nova 687]
Color CCD image provided by T. Scarmato:
http://digilander.iol.it/infosis/homepage/suspectnova.html
[vsnet-campaign-nova 692]
IM Nor
Some useful comparison stars, see [vsnet-campaign-nova 699]
Sequence, see [vsnet-campaign-nova 702, 726]
MisV1147
Charts provided by M. Simonsen:
http://joevp.20m.com/cgi-bin/i/charts/sxncharts/MisV1141_sxn.gif
http://joevp.20m.com/cgi-bin/i/charts/sxncharts/MisV1141_Rsxn.gif
[vsnet-campaign-unknown 21]
IP Peg
Eclipse ephemeris, see [vsnet-campaign-dn 2045]
Light curve provided by J. Pietz, see [vsnet-campaign-dn 2046]
Spectra of omega CMi and omega CMa taken by E. Pollmann,
see [vsnet-campaign-be 152, 153]
(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
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