VSNET Weekly Campaign Summary *** Last week news *** (new targets) CH Her (RA = 18h34m46s.21, Dec = +24d47'57".0) G. Poyner reported an outburst of CH Her on May 11 and 12. This is one of rare outbursts in the last two years, and would be a target of opportunity (vsnet-campaign-dn 3660). HadV100 (RA = 18h19m05s.76, Dec = -30d19'06".7) It is reported to be a large-amplitude Mira, which is supported in the ASAS-3 data (vsnet-campaign-unknown 200, 201, 202, 203, 204). TmzV772 (RA = 12h45m06s.82, Dec = +21d39'33".4) C. Lloyd and S. Otero call for observations of the new eclipsing variable, TmzV772. The period is proposed to be 1.03, 1.43, and 0.89 d, and C. Lloyd reported that the 0.89-d period is most likely (vsnet-campaign-eclipse 66, 67, 68, 69, 70). AI CMi (RA = 07h35m41s.2, Dec = +00d14'58") S. Otero reported that ASAS-3 data brings a confirmation of his observation of the post-AGB star AI CMi in a very bright maximum: It was at V= 7.86 on May 10 (vsnet-campaign-mira 60). T. Kato commented that AI CMi is suggested to have an evolutionary stage close to proto-planetary nebulae (PPN). If this is the case, the bolometric luminosity of such an object is close to its maximum in its entire lifetime. It is thus noteworthy that if a real "brightening" occurs in addition to its baseline luminosity. It could be one of brightest pulsation maxima, but there may be a possibility that a more dramatic change (such as rho Cas mass-ejection episode) may be taking place (vsnet-campaign-mira 61). SN 2003eg (RA = 12h50m58s.33, Dec = -14d20'01".1) SN 2003eg is hosted by NGC 4727, a spiral galaxy making a close pair with NGC 4724. There are many galaxies having v_r ~ 4000 km/s in 30' of NGC 4727. Though the recession velocity of NGC 4727 itself is tabulated as 7622 km/s, it seems to have a same distance as the surrounding galaxies; it is supported the brightest observed magnitude of SN (type unknown) 1965B also produced by NGC 4727 was B = 16.0. The expected maximum for typical SN Ia in this group is mag about 15.5. The spectral classification of the SN and the determination of the recession velocity is important (vsnet-campaign-sn 622). SN 2003eh (RA = 11h08m24s.34, Dec = +03d29'47".0) SN 2003eh is hosted by MCG +01-29-3, a barred-spiral galaxy. The expected maximum for typical SN Ia is mag about 16.7 (vsnet-campaign-sn 622). (continuous targets) TV Crv (RA = 12h20m23s.56, Dec = -18d27'02".7) The superoutburst is still ongoing (vsnet-campaign-dn 3665, 3670). In the light curve obtained by P. Nelson on May 18, superhumps still persists with a full amplitude of 0.15 mag (vsnet-campaign-dn 3669). RX Vol (RA = 08h39m32s.30, Dec = -66d17'39".2) The data taken by B. Monard clearly indicate that the object was just undergoing a "rebrightening phase" during the terminal portion of a superoutburst plateau on late May 12. This feature is associated with systems with short orbital periods and high outburst amplitudes (the best example being V1028 Cyg) (vsnet-campaign-dn 3661). An analysis of the data until May 12 indicates overall positive period derivative feature (around dot(P)/P = +7*10^(-5)). This is very consistent with the superhump behavior of the SU UMa stars at this superhump period (vsnet-campaign-dn 3662). OU Vir (RA = 14h35m00s.14, Dec = -00d46'07".0) The superhumps have become less prominent. A preliminary analysis of the entire data more strongly suggests the presence of a general period decrease. On May 9-10, post-eclipse "dip"-like phenomenon was observed superimposed on superhump maxima (vsnet-campaign-dn 3663). The object has entered a rapid fading phase from the superoutburst on May 18 (vsnet-campaign-dn 3665, 3666). During this phase, the eclipses observed by T. Krajci are sharp and deep (1.5 mag). Outside the eclipses, the light curve looks like undulations. It may have been possible that the superhumps are beginning to lose its coherence (vsnet-campaign-dn 3667). SN 2003dh (RA = 10h44m50s.030, Dec = +21d31'18".15) The Subaru team observed SN 2003dh, a supernova component of GRB030329 spectropolarimetrically and spectroscopically (May 8.3 and 9.3 UT). It closely resembles that of SN 1997ef (type-Ic hypernova) about 40 days after explosion, which is comparable to the rest-frame age of SN 2003dh (34-35 days). (IAUC 8133)(vsnet-campaign-sn 621). V445 Pup (RA = 07h37m56s.88, Dec = -25d56'59".1) S. Otero reported that ASAS-3 data provide pre-discovery observations of V445 Pup. It reveals that V445 Pup had already been bright on 2000 November 20, and experienced a maximum at V=8.46 on November 30 (vsnet-campaign-nova 1253, 1254). V4745 Sgr (RA = 18h40m02s.54, Dec = -33d26'55".1) The rebrightening was terminated, and then the object started rapid fading again (vsnet-campaign-nova 1249, 1250, 1255, 1256). V4743 Sgr (RA = 19h01m09s.38, Dec = -22d00'06".2) Reported observations show possible oscillations having a 30-d periodicity. The nova may be experiencing some sort of "transition phase" activity. If it is the case, the analogy with V1494 Aql may be more strengthened. However, the ASAS-3 data show a smoother decline with little fluctuation (vsnet-campaign-nova 1252). AH Her (RA = 16h44m09s.99, Dec = +25d15'02".1) A possible fading from a standstill was reported (vsnet-campaign-dn 3659). MV Lyr (RA = 19h07m15s.93, Dec = +44d01'10".7) Some observations show that it is now very bright at 12.1-12.3mag. The current brightness surpasses the recorded magnitudes at least since 1994 (vsnet-campaign-nl 117). GY Cnc (RA = 09h09m50s.5, Dec = +18d49'47") The eclipsing dwarf nova, GY Cnc experienced an outburst on May 13 and 14, as reported by E. Muyllaert and M. Simonsen (vsnet-campaign-dn 3364). *** Future schedule *** IM Nor Campaign by I. Hachisu (University of Tokyo) and the VSNET team For more information, see [vsnet-campaign-nova 1241] GRB Mini-Symposium in JENAM2003 For more information, http://vsnet.konkoly.hu/jenam03/ [vsnet-campaign-grb 31] IAU JD17 "ATOMIC DATA FOR X-RAY ASTRONOMY" ON JULY 22-23, 2003 at the XXVth IAU GENERAL ASSEMBLY SYDNEY, AUSTRALIA, JULY 13-26, 2003 for more information: http://vsnet.astronomy.ohio-state.edu/~pradhan/Iau/iau.html [vsnet-campaign-xray 227] "X-ray and Radio Emission of Young Stars" July 28 - 29, 2003, Rikkyo University, Tokyo, Japan for more information , please contact to kitamoto@rikkyo.ne.jp [vsnet-campaign-xray 218] 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] [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] The 2003 Gamma Ray Burst conference Hosted by Los Alamos, in Santa Fe, New Mexico (USA), between September 8 and 12, 2003 http://grb2003.lanl.gov/ [vsnet-campaign-grb 13] *** General information *** OU Vir Eclipse ephemeris, see [vsnet-campaign-dn 3658, 3668] TmzV772 CCDV chart and phase plots at: http://members.aol.com/dwest61506/page39.html Visual chart: http://members.aol.com/dwest61506/page40.html Reversed Visual Chart: http://members.aol.com/dwest61506/page65.html Eclipse ephemeris, see [vsnet-campaign-ecl 66, 69] AI CMi Light curve provided by S. Otero: http://ar.geocities.com/varsao/Curva_AI_CMi.htm [vsnet-campaign-mira 60] (This summary can be cited.) Regards, Makoto Uemura
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