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[vsnet-chat 1793] New variable stars (MisV0001-0004)
- Date: Mon, 19 Apr 1999 09:22:27 +0900
- To: wang@ares.nrl.navy.mil, dab@star.sr.bham.ac.uk, koehn@lowell.Lowell.Edu, dgm@nofs.navy.mil, mperryma@astro.estec.esa.nl, koflaher@astro.estec.esa.nl, mclean@stsci.edu, question@simbad.u-strasbg.fr, pluto@gwi.net, meech@pavo.IFA.Hawaii.Edu, maury@ocar01.obs-azur.fr, obyk@pulvz.spb.su, zj@qso.bao.ac.cn, david@crl.go.jp, ebowell@lowell.edu, awharris@lithos.jpl.nasa.gov, ipatov@spp.keldysh.ru, etedesco@nh.ultranet.com, klet@klet.cz, donald.k.yeomans@jpl.nasa.gov, jscotti@lpl.arizona.edu, szena@ludens.elte.hu, ok2rea@prgate.sci.muni.cz, pfactors@ix.netcom.com, fraserf@dove.net.au, foryta@fisica.ufpr.br, Miquel.Regalado@uv.es, jure.skvarc@ijs.si, mnico@iol.it, vsnet@kusastro.kyoto-u.ac.jp, vsnet-chat@kusastro.kyoto-u.ac.jp, tass@wwa.com, jdsh@mail.nerc-bas.ac.uk, jose.aguiar@mpc.com.br
- From: Seiichi Yoshida <seiichi@muraoka.info.waseda.ac.jp>
- Subject: [vsnet-chat 1793] New variable stars (MisV0001-0004)
- cc: seiichi@mura01.muraoka.info.waseda.ac.jp
- Sender: owner-vsnet-chat@kusastro.kyoto-u.ac.jp
MISAO Project Announce Mail (Apr. 19, 1999)
Hello. I am Seiichi Yoshida working on the MISAO project.
After the announcement on Apr. 3 about our first new variable star
MisV0001, Seiichiro Kiyota sent me his observations of this object in
past. Here I introduce you the whole behavior of the brightness
including the further observations by the Ageo Survey team.
1996 Mar. <16 V Ouda team
1998 Mar. 9 14.94 Rc Seiichiro Kiyota
15 14.62 Rc Seiichiro Kiyota
17 15.08 Rc Seiichiro Kiyota
Apr. 2 <14.74 Rc Seiichiro Kiyota
May 20 <14.74 Rc Seiichiro Kiyota
June 20 14.56: Rc Seiichiro Kiyota (uncertain)
Sept.13 <14.74 Rc Seiichiro Kiyota
1999 Feb. 5 17.56: Rc Seiichiro Kiyota
12 16.9 CCD KenIchi Kadota
Mar. 5 16.47: Rc Seiichiro Kiyota
12 16.19: Rc Seiichiro Kiyota
22 15.0 CCD KenIchi Kadota
31 14.1 CCD KenIchi Kadota
14.0 R60 KenIchi Kadota
Apr. 4 14.1 CCD KenIchi Kadota
7 13.77 Rc Seiichiro Kiyota
In addition, Masayuki Suzuki reported that this object is found on the
Real Sky image taken on May 3, 1987, as a very faint star.
These observations imply that MisV0001 varies between 14 mag and 17.5
mag by CCD with roughly 1-year period. It was discovered just when it
was brightening rapidly in late March, 1999.
After the discovery of MisV0001, three more new variable stars have
been discovered.
Code R.A. (J2000.0) Decl. Max Min ID
------------------------------------------------------------
MisV0001 175226.59 -174000.7 14.1C 16.9C
MisV0002 072403.56 +412602.0 13.3C 14.7C GSC2965.0210 USNO1275.06972791
MisV0003 175244.93 -172401.4 12.5C 13.4C
MisV0004 175313.59 -172844.2 12.1C 13.3C
Two of the three, MisV0003 and MisV0004 are also discovered on the
images of Sakurai's V4334 Sgr and MisV0001. The distance from V4334
Sgr is about 2 arcmin (MisV0001), about 17 arcmin (MisV0003) and about
16 arcmin (MisV0004). It means three new variable stars were
discovered by searching such a small area for only about two months.
Mira type variable stars can be about two or three mag brighter by CCD
than by photo or visually. Therefore, many faint variable stars whose
peak brightness is 14-16 mag visually, which have been unknown, can be
detected bright and discovered by CCD, I guess.
MisV0002 was detected from the 300-mm camera lens or 18-cm reflector
images of Comet 52P/Harrington-Abell taken between Dec. 9 and 20,
1998, by KenIchi Kadota, Ageo City, Saitama, Japan. The magnitude
estimated by the PIXY system show that this object is about one mag
fainter than usual on Dec. 17. Because it is as bright as usual on the
next day, it is probably an ecliptic binary.
Furthermore, another variable star brightening from 10.5 mag to 8.3
mag at R.A. 17h59m48s.2, Decl. -31o16'03" was detected from the Ageo
Survey images.
1999 Jan. 29 10.5 mag
Feb. 20 8.4 mag
Mar. 12 8.3 mag
Here is the search result of known variable stars.
V1725 SGR 93.2"
V1725 SGR R.A.=17 59 41.30 Decl.=-31 16 32.4 13.0 - <15.2 mag (P) type:M Epoch=28415 Period=380 Sp:M7
IRAS 17565-3115 7.9"
IRAS 17565-3115 R.A.=17 59 47.60 Decl.=-31 16 05.0 (41 x 7", p.a.=91) flux(12)=26.49 flux(25)=11.61 flux(60)=2.09 flux(100)=<15.18 93% variable
The position recorded in the GCVS is 1.5 arcmin far away from the
detected position. However, there is no star detected at the position
in the GCVS. So this variable star is V1725 Sgr. This case made it
clear that the position of V1725 Sgr in the GCVS was inaccurate.
P.S.
The past MISAO project announce mails are available at:
http://vsnet.info.waseda.ac.jp/muraoka/members/seiichi/misao/
--
Seiichi Yoshida
seiichi@muraoka.info.waseda.ac.jp
http://vsnet.info.waseda.ac.jp/muraoka/members/seiichi/index.html
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