Japanese version Home Page Updated on January 20, 2019
Special Notes on Remarkable StarsHere are the summaries of stars researched and analyzed in the MISAO Project, stars you reported us the information on which, and stars whose interesting features were discovered in the MISAO Project.
EK AndIt is a red variable with a range of 1.1 mag and period of 185 days, however it was not variable in fact (IBVS 5396). FN And
Outburst of a dwarf nova FN And was detected on Dec. 9, 2011, in the
course of Oku Survey by Youichirou Nakashima on the first survey images
of a new 300-mm camera lens.
It was fainter than 16.7 mag on Nov. 16, fainter than 15.8 mag on
Nov. 26, but detected at 14.1 mag on Dec. 9 [vsnet-alert 13946].
Then it was revealed that FN And was already bright as 13.5 mag on our
test images on Dec. 5 through thin clouds [vsnet-alert 13948].
FS AndIt was bright at around 15.5 mag on Oct. 23, 2012, from Youichirou Nakashima's survey images. It tends to be in outburst frequently. The AAVSO database shows it brightened up to 15 mag in September. But nobody reported the outburst in October [vsnet-alert 15230]. V725 AqlOutburst of a dwarf nova V725 Aql was detected from survey images by Youichirou Nakashima, at around 14.0 mag on 2012 Apr. 16.73 (UT). It was not visible in the past images on 2012 Mar. 27.82 (UT) (Image) [vsnet-alert 14450]. The last outburst was recorded in 2011 May by the VSNET and AAVSO database. Taichi Kato reported that the present outburst is superoutburst because 0.2-mag superhumps were observed by Astrokolkhoz team (J. Hambsch and T. Krajci) [vsnet-alert 14460]. V1047 AqlDwarf nova V1047 Aql was detected at around 15.5 mag on May 12.68, 2012 (UT) from survey images by Youichirou Nakashima [vsnet-alert 14579]. Rod Stubbings and Taichi Kato commented that V1047 Aql was revealed to be a SU UMa-type dwarf nova based on the observation by Greg Bolt during 2005 August outburst [vsnet-alert 14584]. HV AurWe detected that a dwarf nova HV Aur in outburst at 16.3 mag on Sept. 25.69, 2012 (UT) from Youichirou Nakashima's survey images. Note that the brightness range of HV Aur is 14.7-<19 mag in the GCVS [vsnet-alert 14956]. V496 AurIt was bright at 16.2 mag on Oct. 18, 2012, from Youichirou Nakashima's survey images [vsnet-alert 15230]. TT Boo
Outburst of this UG-type cataclysmic variable was detected, and its rapid fading was recorded, by chance in the survey in 2007 April by Nobuo Ohkura and Youichirou Nakashima.
It kept bright as 14 mag from Apr. 9 to 12, then became slightly faint as 14.6 mag on Apr. 14.
Then it faded rapidly down to 16.6 mag on Apr. 19.
It became invisible, fainter than 17.5 mag, on Apr. 23.
(Image,
Light Curve).
OV Boo
Masaru Mukai discovered it brightened up to 11.4 mag on Mar. 14, 2017 [vsnet-alert 20778].
Keisuke Isogai suggests this outburst is very likely to be a WZ Sge-like superoutburst [vsnet-alert 20779].
AF Cam
Outburst of this UG-type cataclysmic variable up to 13.7 mag was detected by chance in the survey on 2007 Feb. 12 by Nobuo Ohkura and Youichirou Nakashima.
It had never been brighter than 16.5 mag in the MISAO Project images between 1999 and 2002.
DK Cas
It was bright at 15.3 mag on Oct. 20, 2012, from Youichirou Nakashima's
survey images.
The AAVSO database contains only faint observations around 18 mag in
2012 autumn [vsnet-alert 15230].
V723 CasThe small brightening of this nova was detected in 2001 October, about 6 years after discovery (Brightening of Nova Cas 1995). SV CMiIt was bright at 13.2 mag on Oct. 26, 2012, from Youichirou Nakashima's survey images. It tends to be in outburst frequently. Rod Stubbings reported the outbursts in mid November and mid December. But nobody reported the outburst in late October [vsnet-alert 15230]. GZ CncOutburst of an UG-type cataclysmic variable GZ Cnc was detected at 13.9 mag on 2012 Mar. 24 from survey images by Nobuo Ohkura. It was fainter than 14.6 mag on Mar. 21. Rod Stubbings reported the last outburst on Mar. 17. So GZ Cnc rebrightened within only 1 week [vsnet-alert 14363]. V542 CygWe detected that a dwarf nova V542 Cyg is in outburst at 14.5 mag on July 17.66, 2012(UT) from Youichirou Nakashima's survey images. It was faint at around 17.5 mag on May 27, June 9 and July 7 [vsnet-alert 14773]. V767 Cyg
We detected that a dwarf nova V767 Cyg is in outburst at 15.2 mag on
July 18.53, 2012(UT) from Youichirou Nakashima's survey images.
It was not detected on any past Nakashima's survey images from 2007
Oct. 10 to 2012 June 28 [vsnet-alert 14781].
V792 CygSeveral outbursts of a dwarf nova V792 Cyg up to 14-15 mag were detected from Youichirou Nakashima's survey images, on 2010 Sept. 28, 2012 Mar. 25, May 27 and Aug. 2 [vsnet-alert 14378][vsnet-alert 14823]. V868 CygWe detected that a dwarf nova V868 Cyg is in outburst at 15.2 mag on July 26.68, 2012 (UT) from Youichirou Nakashima's survey images. It brightened up to 14.8 mag on Aug. 2. The outburst of this star is not rare. However, because this outburst has not been reported yet, we reported it to CVnet. V1006 CygWe detected that a dwarf nova V1006 Cyg is in outburst at 15.2-15.5 mag on July 17.66, 2012(UT) from Youichirou Nakashima's survey images. We found another old outburst at 14.5 mag on Nakashima's survey images on Apr. 24, 2008 [vsnet-alert 14774]. V1113 CygWe detected that a dwarf nova V1113 Cyg is in outburst at 14.3 mag on July 30.54, 2012 (UT) from Youichirou Nakashima's survey images. This star seems to brighten in outburst frequently. The last outburst was reported on May 23 at 14.1 mag by Gary Poyner [vsnet-alert 14822]. V1504 CygOutburst of a dwarf nova V1504 Cyg was detected from survey images by Youichirou Nakashima at 13.9-14.2 mag on Mar. 11, 2012. It was fainter than 15.7 mag on Sept. 23 and 15.5 mag on Oct. 18 in 2011 by Youichirou Nakashima [vsnet-alert 14321]. V2289 Cyg
Outburst of a dwarf nova V2289 Cyg was detected from survey images by
Youichirou Nakashima at around 16 mag on Aug. 12, 2013.
It was fainter than 17 mag on past survey images in 2012 by Youichirou
Nakashima [vsnet-alert 16188]
(Image).
Then it was detected as bright as about 15-16 mag also on Sept. 18
[vsnet-alert 16437].
V1008 HerMike Simonsen discovered the outburst at 13.3 mag on May 11.2910, 2012. We found that it was already bright at 13.9 mag on May 10.55 from survey images by Youichirou Nakashima [vsnet-alert 14567]. AW GemOutburst was discovered by Gary Poyner on Nov. 18, 2012. Pre-discovery observations was reported by Denis Denisenko by MASTER on Nov. 16. We found that AW Gem was already bright at 13.8 mag on Nov. 14 from Youichirou Nakashima's images [vsnet-alert 15230]. KT GemWe detected that a dwarf nova KT Gem, an UGSS type with a range of 16-20 mag, in outburst at 16.1 mag on Sept. 26.77, 2012 (UT) from Youichirou Nakashima's survey images [vsnet-alert 14980]. PS LacWe detected that a dwarf nova PS Lac, an UGSS type with a range of 15.0-17.6 mag, in outburst at 15.4 mag on Oct. 7.58, 2012 (UT) from Youichirou Nakashima's survey images [vsnet-alert 15004]. V584 Lyr
We detected that a dwarf nova V584 Lyr is in outburst at 15.8 mag on
Aug. 2.49, 2012 (UT) from Youichirou Nakashima's survey images.
Another past outburst was detected on Nov. 24.37, 2011 (UT) at around
15.7 mag from Nakashima's survey images [vsnet-alert 14829].
V426 Oph
The small outburst of this nova-like star was detected in 1999 January
[vsnet-obs 19665].
The VSNET data shows that this outburst was caught only by the MISAO Project.
NS PerWe detected that a dwarf nova NS Per, an UG type with a range of 15-<18 mag(p), in outburst at 16.3 mag on Jan. 15.59(UT) from Youichirou Nakashima's survey images. The AAVSO database contains the bright report at about 16 mag in mid November. So maybe NS Per brightens in outburst frequently in a short time [vsnet-alert 16792]. RY SerOutburst of a dwarf nova RY Ser was detected at 13.6-13.9 mag on 2012 Mar. 31 from survey images by Youichirou Nakashima. It was not visile on Nakashima's survey images on Mar. 21 [vsnet-alert 14410]. V386 Ser
Masaru Mukai discovered it brightened up to 10.7 mag on Jan. 18, 2019 [vsnet-alert 22943].
Hideo Nishimura also discovered it several minutes later (TOCP).
Patrick Schmeer suggests this outburst is very likely to be a WZ Sge-like superoutburst.
V735 SgrThe position of this cataclysmic variable had been ambiguous. Discovery of MisV0041 brought review of past plates and papers, then correct position was revealed. The mistake in the past paper was also revealed (IBVS 5326). V5558 Sgr
We measured the magnitude from the SOHO/LASCO C3 images.
It was constant at about 8.9 mag between 2007 Dec. 18 and Dec. 31.
V354 Vul
The position of V354 Vul = LD 143 is revised in IBVS 4450 based on the
identification with a USNO-A1.0 star. But we only found a faint 16-mag
star at the position on Nobuo Ohkura and Ken-ichi Kadota's unfiltered
CCD images, too faint as a Mira type variable with a V-band range of
13.2 - [15.2 mag.
V405 Vul
Outburst of a dwarf nova V405 Vul was detected on Mar. 13.81, 2012 (UT)
from survey images by Youichirou Nakashima.
V405 Vul is blended with a nearby 15-mag star, but it looks around 15 mag [vsnet-alert 14324].
GCN2056 var
New eclipsing variable near by GRB 030329 (GCN 2056).
Eclipsing variation was confirmed from Ken-ichi Kadota's images of GRB 030329 (light curve).
GRB 030329Our observations measured by Seiichi Yoshida from images taken by Ken-ichi Kadota are utilized in Ken'ichi Torii's paper (Astrophys.J. 597 (2003) L101-L106). GSC 3646-01698
We discovered a star with large proper mition of 0.5415 arcsec/year.
It has been missed because it was blended with another star on Palomar plates around 1950.
NSV 02026
Outburst was detected twice on Feb. 4 (14.8 mag) and Nov. 21 (13.8 mag)
in 2011 from Youichirou Nakashima's survey images. It was faint as
16.8-18.0 mag on other days.
NSV 24062 = V4683 Sgr
Symbiotic star NSV 24062 discovered by Yukio Sakurai in 1994 was recovered.
The star discovered by the MISAO Project as one of the new variable stars was identified with NSV 24062 by Taichi Kato.
The position in IAUC 6051 was inaccurate about 15 arcsec.
Hitoshi Yamaoka reported that a star found on DSS images at the MISAO's position, but none found at the IAUC 6051's position.
OT J063213.1+253623Dwarf nova discovered by Korotkiy Stas at Ka-Dar Observatory from images between 2012 Jan. 24 and 27. It was also visible at 12.4 mag on Oku Survey images on Jan. 26 by Youichirou Nakashima. It was 14.8-15.4 mag from 2011 Jan. 10 to 2011 Dec. 25 on Nakashima's survey images [vsnet-alert 14159]. OT J170609.7+143452
We detected that a dwarf nova OT J170609.7+143452 is bright at around
14-15 mag at July 17.55, 2012(UT) from Nobuo Ohkura's survey images
(Image).
It was not visible on the images on May 23 and June 13 [vsnet-alert 14771].
OT J094854.0+014911New cataclysmic variable OT J094854.0+014911 = CSS120315:094854+014911, discovered by the Catalina Sky Survey on Mar. 15, 2012, was already bright at 14-15 mag on Mar. 11 from survey images by Nobuo Ohkura (Image) [vsnet-alert 14330]. SDSS J032015.296+441059.3We detected that a dwarf nova SDSS J032015.296+441059.3 is in outburst at 16.4 mag on Sept. 11.72, 2012 (UT) from Youichirou Nakashima's survey images. The last outburst was reported on Feb. 29, 2012 up to 15.40: mag from Eddy Muyllaert [vsnet-alert 14943]. TmzV868
Kesao Takamizawa, the discoverer of TmzV868, announced it as a possible Mira type star.
But Nikolai N. Samus pointed out that the type is different.
Photometry from Nobuo Ohkura's images in the course of the MISAO Project supports that TmzV868 is not a Mira type variable.
MisV0001 = V4652 Sgr
Discovered from the observations of V4334 Sgr (Sakurai's object).
MisV0002 = V523 Aur
Discovered from the observations of Comet 52P/Harrington-Abell. The
comet was at apogee when brightest in 1998 December. Stars near by the
comet were observed in details by chance, and the variation of MisV0002
was discovered.
MisV0005 = V2586 Oph
Taichi Kato identified with V854 Oph.
We thought that V854 Oph was originally identified with the emission-line star Stephenson No.141 by Stephenson, but it is probably erroneous (IBVS 4843).
MisV0015
John Greaves identified with OGLE2-BUL-SC22-V383.
MisV0047 = V4690 SgrJohn Greaves pointed out the possible identification with an X-ray star 1RXS J180000.7-293416. But it is a normal Mira type variable because bright in the 2MASS images. MisV0055 = V5534 Sgr
Taichi Kato identified with CD-27.12786 (9.8 mag).
Kato commented that it may be a recovery of one of the missing CD stars.
Such a bright star is not recorded in the GSC.
Maybe the star was in outburst by chance when the CD catalog was compiled.
However, there are many CD stars whose position is erroneous.
MisV0078Stefan Huemmerich and Klaus Bernhard revealed that it is a Mira type variable with a period of 272.4 days, brightness range of 13.1-16.5 mag(Rc), using the MACHO project data (light curve, phase diagram). MisV0101Tsutomu Fujiwara's observations revealed that MisV0101 is a Mira-type variable with a period of 210 days (light curve). MisV0106 = V2249 CygTaichi Kato identified with NSV 25425. Kato revealed that Margoni and Stagni used blue photographic plate for the finding chart and labelled the wrong star (IBVS 4792). MisV0118Tsutomu Fujiwara's observations revealed that MisV0118 is a Mira-type variable with a period of 290 days (light curve). MisV0126Tsutomu Fujiwara's observations revealed that MisV0126 is a semi regular variable with a period of 430 days (light curve).
MisV0127Tsutomu Fujiwara's observations revealed that MisV0127 is a semi regular variable with a period of 250 days (light curve).
MisV0128 = V1464 CygIdentified with LD 183. And Williams identified LD 183 with V1464 Cyg. MisV0130Identified with HS 1332. Because the policy on new variable stars was not established at the discovery, we assigned the MisV number for this star despite of the identification. MisV0134
Taichi Kato identified with NSV 11661.
We reported MisV0134 as one of the new variable stars because it is 103 arcsec from NSV 11661.
However, Kato revealed that the MisV0134 was marked as NSV 11661 (S9039 in the original paper) on the Hoffmeister's discovery chart.
So the cataloged R.A. and Decl. of NSV 11661 was very erroneous.
MisV0149 = V2225 CygJohn Greaves identified with ISV1956+29 discovered by Iida. MisV0166Tsutomu Fujiwara's observations revealed that MisV0166 is a Mira-type variable with a period of 280 days (light curve).
MisV0170Tsutomu Fujiwara's observations revealed that MisV0170 is a Mira-type variable with a period of 390 days (light curve).
MisV0187
John Greaves pointed out the identification with AC2000 383539.
AC2000 383539 is bright as 11.8 mag (B), but not recorded in any of Hipparcos Input Catalog, Tycho Catalog, GSC.
So MisV0187 may be a cataclysmic variable and was in outburst by chance on the AC2000 plate in 1920.
MisV0200 = V1552 Aql
Photographic observations were reported from Kesao Takamizawa and Katsumi Haseda
[vsnet-newvar 1194],
[vsnet-newvar 1196].
The light curve suggests that MisV0200 is a Mira type variable star with a period of about 350 days.
One of the peak was around 2452205 (JD).
MisV0201Tsutomu Fujiwara's observations revealed that MisV0201 is a Mira-type variable with a period of 190 days (light curve).
MisV0206Tsutomu Fujiwara's observations revealed that MisV0206 is a Mira-type variable with a period of 320 days (light curve).
MisV0218Diego Rodriguez and Adolfo San Segundo's observations between 2009 and 2011, with Ken-ichi Kadota, Nobuo Ohkura and Youichirou Nakashima's observations between 1999 and 2007, suggest that MisV0218 is a Mira type with a period of about 380 days (light curve). MisV0226Tsutomu Fujiwara's observations revealed that MisV0226 is a Mira-type variable with a period of 410 days (light curve).
MisV0297 = V364 SerTaichi Kato pointed out the possible identification with DZ Ser, a nova in 1960. Kato commented that DZ Ser is a 14-mag nova discovered in spectral observations. The position is very different on some papers as follows. Duerbeck 175812.72 -103350.35 (1950.0) Wyckoff and Wehinger 175812.8 -103400.5 (1950.0) However, Seiichi Yoshida revealed that it is found as a faint star on the DSS 1 and DSS 2 images, and it looks brighter on R-band image. So it will be a red variable. MisV0301Diego Rodriguez observed its slow fading in 2010 summer, and pointed out that it is a possible Mira variable. MisV0303Revealed as Mira type by Patrick Wils's research. MisV0306Tsutomu Fujiwara's observations revealed that MisV0306 is a Mira-type variable with a period of 375 days (light curve).
MisV0348Stefan Huemmerich and Klaus Bernhard revealed that it is a Mira type variable with a period of 163.8 days, brightness range of 12.0-15.7 mag(Rc), using the MACHO project data. MisV0357Tsutomu Fujiwara's observations revealed that MisV0357 is a semi regular variable with a period of about 280 days (light curve).
MisV0359Tsutomu Fujiwara's observations revealed that MisV0359 is a Mira-type variable with a period of 295 days (light curve). MisV0367Tsutomu Fujiwara's observations revealed that MisV0367 is a semi regular variable with a period of 305 days (light curve).
MisV0368 = V2271 Cyg
The NSVS data revealed that it is a semi regular variable with a
range of 12.7 - 13.5 mag, and a period of 100 days. The unfiltered
CCD observations from 1999 to 2000 by Ken-ichi Kadota and Nobuo
Ohkura coincided to the magnitude range and the period.
MisV0372 = V5382 SgrTaichi Kato and John Greaves pointed out the possible identification with an X-ray star 1RXP J180245-2942.3. But it is revealed to be a normal Mira type variable based on the OGLE-II data. MisV0374Tsutomu Fujiwara's observations revealed that MisV0374 is a Mira-type variable with a period of 195 days (light curve).
MisV0380
Seiichi Yoshida and John Greaves found that it is not recorded in any of GSC 1.1, USNO-A2.0, IRAS, 2MASS, UCAC1, GSC 2.2.
Greaves investigated the past images at the USNO Flagstaff Station Integrated Image and Catalogue Archive Service, but no star was found within 3 arcsec.
It implies the star may be a cataclysmic variable.
So Greaves called for observations in the MSDG-MISAO Campaign.
MisV0395Taichi Kato revealed that it was observed as NGC 6194 No. 1130 and is a red star. MisV0474 = V4666 SgrStefan Huemmerich and Klaus Bernhard revealed that it is a Mira type variable with a period of 194 days, brightness range of 14.6-18.9 mag(V), using the MACHO project data. MisV0477Stefan Huemmerich and Klaus Bernhard revealed that it is a Mira type variable with a period of 377 days, brightness range of 12.2-16.3: mag(Rc), using the MACHO project data. MisV0490Stefan Huemmerich and Klaus Bernhard revealed that it is a Mira type variable with a period of 342.0 days, brightness range of 11.5-<13.9 mag(Rc), using the MACHO project data. MisV0508 = V949 SgrTaichi Kato identified with V949 Sgr, a nova in 1914. MISAO's observations, followed by Patric Schmeer's observations, revealed that it is not a nova but a red variable (IBVS 4845). MisV0525 = V1694 AqlJohn Greaves pointed out the possible identification with an X-ray star 2RXP J193158.1110964. But it is a normal Mira type variable because bright in the 2MASS images. MisV0531Stefan Huemmerich and Klaus Bernhard revealed that it is a Mira type variable with a period of 356 days, brightness range of 11.8-15.9 mag(Rc), using the MACHO project data. MisV0538Tsutomu Fujiwara's observations revealed that MisV0538 is a Mira-type variable with a period of 240 days (light curve).
MisV0542Stefan Huemmerich and Klaus Bernhard revealed that it is a Mira type variable with a period of 265.3 days, brightness range of 11.8-16.1 mag(Rc), using the MACHO project data (light curve, phase diagram). MisV0547Stefan Huemmerich and Klaus Bernhard revealed that it is a Mira type variable with a period of 291.8 days, brightness range of 11.3-15.8 mag(Rc), using the MACHO project data. MisV0553Stefan Huemmerich and Klaus Bernhard revealed that it is a Mira type variable with a period of 235 days, brightness range of 11.9-[14.2 mag(Rc), using the MACHO project data. MisV0557Stefan Huemmerich and Klaus Bernhard revealed that it is a Mira type variable with a period of 324.9 days, brightness range of 11.2-15.8 mag(Rc), using the MACHO project data (light curve, phase diagram). MisV0562
Mati Morel pointed out the possible identification with Luyten's V915 Sgr.
The range by Luyten (12.3-13.5p) is not too dissimilar to that of MisV0562 (11.8-13.8C).
V915 Sgr is regarded as GSC 6870-00090 in Herbig's paper (PASP 70,605) and classified as RCB type with a period of 285.2 days, which can well refer to the period of MisV0562.
If MisV0562 is V915 Sgr, it turns out to be a SR variable
[vsnet-chat 2797].
MisV0642Tsutomu Fujiwara's observations revealed that MisV0642 is a Mira-type variable with a period of 225 days (light curve).
MisV0645
Taichi Kato pointed out that KY Sgr, a nova in 1926, is close, 126 arcsec from MisV0645.
MisV0665 = V5542 Sgr
Kazuhiro Nakajima's observations revealed it is an Algol-type (EA) eclipsing variable
with unfiltered CCD variations of 13.18 mag at maximum, 13.84 mag at
primary minimum, 13.26 mag at secondary minimum, and period of 1.6351
days (IBVS 5500).
MisV0687Tsutomu Fujiwara's observations revealed that MisV0687 is a Mira-type variable with a period of 167 days (light curve).
MisV0694John Greaves identified with ROTSE1 J185841.70+302042.8. ROTSE's observations revealed that is is a long periodic variable. MisV0701 = V1511 Aql
Taichi Kato pointed out that it is near by a planetary nebula PK 32-3.1 and influenced to the past observations of PK 32-3.1.
MisV0719 = V418 VulThis star is near by M27, so Gianluca Masi had noticed the variability and recorded in his WWW page. MisV0758Tsutomu Fujiwara's observations revealed that MisV0758 is a Mira-type variable with a period of 330 days (light curve).
MisV0762Tsutomu Fujiwara's observations revealed that MisV0762 is a Mira-type variable with a period of 315 days (light curve).
MisV0774 = V559 CygJohn Greaves reported that the position of V559 Cyg was revised in IBVS 4905 and came to coincide with MisV0774. MisV0779 = V1229 CygJohn Greaves reported that the position of V1229 Cyg was revised in IBVS 4799 and came to coincide with MisV0779. MisV0796 = V4694 SgrKlaus Bernhard and Stefan Huemmerich reported the MACHO data revealed it is a Mira type variable with a period of 298 days, brightness range of 12.7-16.4 mag(Rc) (light curve). MisV0797Tsutomu Fujiwara's observations revealed that MisV0797 is a Mira-type variable with a period of 350 days (light curve).
MisV0813Tsutomu Fujiwara's observations revealed that MisV0813 is a Mira-type variable with a period of 283 days (light curve). MisV0814
Identified with 2MASS 0533337+344323.
The 2MASS J-Ks value is 0.384 mag, so it is not a red variable.
MisV0855 = V4656 Sgr
A very faint red variable in very crowded field.
The USNO-A2.0 shows the color as B-R=4.0 mag.
John Greaves commented that the star is only found on red E plate, and not found on blue O plate, though both plates were on the same day, which suggests this star is very red.
MisV0858Stefan Huemmerich and Klaus Bernhard revealed that it is a Mira type variable with a period of 220 days, brightness range of 12.7-16.0 mag(Rc), using the MACHO project data. MisV0871Klaus Bernhard and Stefan Huemmerich reported the MACHO data revealed it is a Mira type variable with a period of 255 days, brightness range of 11.6:-16.5 mag(Rc) (light curve). MisV0880Stefan Huemmerich and Klaus Bernhard revealed that it is a Mira type variable with a period of 222.6 days, brightness range of 11.2:-15.4 mag(Rc), using the MACHO project data. MisV0884
When it was bright as 9.3 mag in the MISAO Project observations, Guy M Hurst and Mike Collins reported that MisV0884 was too faint, fainter than 11 mag.
Hurst's observations are unfiltered CCD, as same as the MISAO observations.
MisV0891In 2010 summer, brightening up to about 11.5 mag was recorded in the survey images by Tadashi Kojima. MisV0898
Identified with 2MASS 1800214-304831, (J=10.764 mag, J-Ks=0.739 mag.
It is probably not a red variable because of the small J-Ks value.
Seiichi Yoshida revealed that it is clearly found on the DSS 2 R-band and Bj-band images, which also implies that it is not a red variable.
MisV0909, MisV0910A pair of double variable stars with 19 arcsec distance. MisV0945Tsutomu Fujiwara's observations revealed that MisV0945 is a Mira-type variable with a period of 190 days (light curve).
MisV0949 = V659 AqlJohn Greaves reported that the position of V659 Aql was revised in the latest online edition of the GCVS and came to coincide with MisV0949. MisV0951Tsutomu Fujiwara's observations revealed that MisV0951 is a Mira-type variable with a period of 235 days (light curve).
MisV0968 = V423 VulJohn Greaves identified with one of the binary WDS 19277+2423 = Pourteau 3835, the pair of 13.6 mag and 13.8 mag stars. The cataloged position of WDS 19277+2423 is 48 arcsec from MisV0968. But the separation and position angle of MisV0968 and a nearby star USNO-A2.0 1125.12713797 is 9.8 arcsec in 111 degree, which correspond to those of WDS 19277+2423, 9.2 arcsec in 115 degree very well. Greaves commented that Pourteau 3835B is probably MisV0968 because the position well coincides with that of IRAS, 2MASS, MSX5C data. MisV0988Tsutomu Fujiwara's observations revealed that MisV0988 is a Mira-type variable with a period of 430 days (light curve).
MisV1005Tsutomu Fujiwara's observations revealed that MisV1005 is a Mira-type variable with a period of 255 days (light curve).
MisV1008Tsutomu Fujiwara's observations revealed that MisV1008 is a Mira-type variable with a period of 207 days (light curve). MisV1010Tsutomu Fujiwara's observations revealed that MisV1010 is a Mira-type variable with a period of 410 days (light curve).
MisV1013Tsutomu Fujiwara's observations revealed that MisV1013 is a semi regular variable with a period of 157 days (light curve).
MisV1015Tsutomu Fujiwara's observations revealed that MisV1015 is a Mira-type variable with a period of 220 days (light curve). MisV1021Tsutomu Fujiwara's observations revealed that MisV1021 is a Mira-type variable with a period of about 430 days (light curve).
MisV1022Tsutomu Fujiwara's observations revealed that MisV1022 is a Mira-type variable with a period of 270 days (light curve). MisV1023 = V1462 Cyg
In 2000, when the position of V1462 Cyg was inaccurate, we the MISAO Project discovered two new variable stars around it.
One of them is identified with NSV 12600.
We thought V1462 Cyg ans NSV 12600 are the same star (IBVS 4814), and announced another star as a new variable star MisV1023.
MisV1024
Because it is identified with IRAS 19596+3350 and an S-type star NSS 49, it is probably a red variable.
But the 2MASS magnitude is J=7.312 mag, J-Ks=0.729 mag, so the J-Ks value is fairly small as a red variable.
MisV1029Tsutomu Fujiwara's observations revealed that MisV1029 is a Mira-type variable with a period of 285 days (light curve). MisV1040Tsutomu Fujiwara's observations revealed that MisV1040 is a Mira-type variable with a period of 500 days (light curve).
MisV1041Tsutomu Fujiwara's observations revealed that MisV1041 is a Mira-type variable with a period of 370 days (light curve).
MisV1042Tsutomu Fujiwara's observations revealed that MisV1042 is a Mira-type variable with a period of 500 days (light curve).
MisV1043Tsutomu Fujiwara's observations revealed that MisV1043 is a Mira-type variable with a period of 335 days (light curve).
MisV1051John Greaves pointed out the possible identification with an X-ray star 1RXS 201351.8+414557. However, Taichi Kato pointed out that a bright star GSC 3159.1639 is closer to the X-ray star and that will be identified with it. So MisV1051 and 1RXS 201351.8+414557 are not the same. MisV1061 = V456 Vul
Kazuhiro Nakajima's observations revealed it is an Algol-type (EA) eclipsing variable
with V-band variations of 12.14 mag at maximum, 12.81 mag at primary
minimum, 12.55 mag at secondary minimum, and period of 3.0421 days
(IBVS 5600).
MisV1062Tsutomu Fujiwara's observations revealed that MisV1062 is a Mira-type variable with a period of 285 days (light curve).
MisV1069Tsutomu Fujiwara's observations revealed that MisV1069 is a Mira-type variable with a period of 175 days (light curve). MisV1073John Greaves pointed out that there is an X-ray star 1RXS 200142.7+465727 about 1 arcmin south of MisV1073. But they are probably not the same because of the large distance. MisV1083Tsutomu Fujiwara's observations revealed that MisV1083 is a Mira-type variable with a period of 530 days (light curve).
MisV1088Tsutomu Fujiwara's observations revealed that MisV1088 is a Mira-type variable with a period of 420 days (light curve).
MisV1095 = V440 And
Kazuhiro Nakajima's observations revealed it is an Algol-type (EA) eclipsing variable
with unfiltered CCD variations of 12.64 mag at maximum, 13.24 mag at
primary minimum, 12.90 mag at secondary minimum, and period of 1.5829
days (IBVS 5600).
MisV1096 = V441 And
Kazuhiro Nakajima's observations revealed that it is a W UMa-type (EW) eclipsing variable with unfiltered CCD variations between 13.48 mag and 14.25 mag, and period of 0.4696 days (IBVS 5600).
The brightness at primary minimum and secondary minimum is almost same.
MisV1097 = V444 And
Ondrej Pejcha revealed it is a W UMa-type (EW) eclipsing variable.
It is probably a blue one (EW/KE type), the minority among them.
MisV1105 = V2421 Cyg
Kazuhiro Nakajima's observations revealed it is a beta Lyr-type (EB) eclipsing
variable with unfiltered CCD variations of 13.79 mag at maximum, 15.03
mag at primary minimum, 14.20 mag at secondary minimum, and period of
0.6331 days (IBVS 5600).
MisV1111Tsutomu Fujiwara's observations revealed that MisV1111 is a Mira-type variable with a period of 345 days (light curve).
MisV1115Tsutomu Fujiwara's observations revealed that MisV1115 is a Mira-type variable with a period of 330 days (light curve).
MisV1136Tsutomu Fujiwara's observations revealed that MisV1136 is a Mira-type variable with a period of 295 days (light curve).
MisV1140 = V450 Lac
It was presumed as an eclipsing variable with large amptitude of almost
2 mag at the discovery.
John Greaves commented that if MisV1140 is an Algol-like eclipsing
variable, the primary may be an A star and the secondary may be a K
star, for the large amplitude.
MisV1141Tsutomu Fujiwara's observations and the MISAO Project surveys revealed that MisV1141 is a Mira-type variable with a period of 318 days (light curve). MisV1147 = V730 Cep
It attracted attention due to the identification with a H-alpha emission star HBHA 65-53.
The campaign in "vsnet-campaign-unknown" and the MSDG observing campaign were launched, and many visual observers have been monitoring it.
It did not show any evident variation in the first half of 2002, however, it showed frequent deep eclipse-like fadings in the latter half of the year.
Based on the spectrums taken by Kenzo Kinugasa and Mitsugu Fujii, Taichi Kato revealed MisV1147 is a young stellar object, a Herbig Ae/Be type star.
MisV1181 = V709 Cep
We discovered a nova, which had been missed in 2001, in 2002.
It was 12.7 mag in 2001 September, 14.3 mag in November, but faded to 20 mag in 2002 October.
It was not found in any past Palomar plates nor DSS images.
MisV1202 = V728 CepJohn Greaves pointed out that MisV1202 lies within/behind bright emission nebula Sharpless 134. MisV1220 = V452 AndKazuhiro Nakajima's observations revealed it is a beta Lyr-type (EB) eclipsing variable with unfiltered CCD variations of 13.80 mag at maximum, 15.14 mag at primary minimum, 14.04 mag at secondary minimum, and period of 0.9784 days (IBVS 5600). MisV1222 = V1001 Cas
Kazuhiro Nakajima's observations revealed it is a beta Lyr-type (EB) eclipsing
variable with unfiltered CCD variations of 13.61 mag at maximum, 14.71
mag at primary minimum, 14.06 mag at secondary minimum, and period of
0.4288 days (IBVS 5600).
MisV1223 = MN Cam
Patrick Wils and John Greaves revealed that it is a Cepheid variable
with a period of 8.2 days from the NSVS data (IBVS 5512).
MisV1224 = MQ Cam
Patrick Wils and John Greaves revealed that it is a Cepheid variable
with a period of 6.60 days from the NSVS data (IBVS 5512).
MisV1225 = MP CamKazuhiro Nakajima's observations revealed it is a beta Lyr-type (EB) eclipsing variable with unfiltered CCD variations of 12.68 mag at maximum, 14.04 mag at primary minimum, 13.19 mag at secondary minimum, and period of 2.6092 days (IBVS 5600). MisV1226 = MT CamKazuhiro Nakajima's observations revealed it is a W UMa-type (EW) eclipsing variable with unfiltered CCD variations of 12.94 mag at maximum, 13.54 mag at primary minimum, 13.50 mag at secondary minimum, and period of 0.3662 days (IBVS 5600). MisV1227 = V962 CasKazuhiro Nakajima's observations revealed it is an Algol-type (EA) eclipsing variable with unfiltered CCD variations of 12.93 mag at maximum, 13.51 mag at primary minimum, 13.41 mag at secondary minimum, and period of 2.7129 days (IBVS 5600). MisV1228 = V727 CepKazuhiro Nakajima's observations revealed it is an Algol-type (EA) eclipsing variable with unfiltered CCD variations of 14.15 mag at maximum, 14.53 mag at primary minimum, 14.48 mag at secondary minimum, and period of 6.6490 days (IBVS 5700). MisV1237 = V522 And
Kazuhiro Nakajima's observations revealed it is an Algol-type (EA) eclipsing
variable with unfiltered CCD variations of 13.34 mag at maximum, 13.94
mag at primary minimum, 13.90 mag at secondary minimum, and period of
7.5530 days (IBVS 5700).
MisV1239 = V959 Cas
Kazuhiro Nakajima's observations revealed it is a W UMa-type eclipsing variable with
unfiltered CCD variations of 11.97 mag at maximum, 12.61 mag at primary
minimum, 12.47 mag at secondary minimum, and period of 1.0650 days
(IBVS 5600).
MisV1253It was mis-classified as SR type at the discovery. But Tsutomu Fujiwara revealed that it is not reddish as V-Rc = 0.0 mag. It seems to be an Algol-type eclipsing variable. MisV1258Tsutomu Fujiwara's observations revealed that MisV1258 is a Mira-type variable with a period of 320 days (light curve).
MisV1262
It was announced as a possible semi-regular variable with a small
amplitude at the discovery. But further observations revealed it is a
Mira type variable with large amplitude.
MisV1267
MisV1267 is recorded in the Hamburg-Bergedorf H-alpha Stars in Northern
Milky Way as HBHA 18-40.
MisV1268John Greaves researched the NSVS data and confirmed the RR type variation between 13.5 - 14.3 mag with a period of 0.564 days. MisV1269John Greaves found it may be variable while researching the NSVS data. Seiichi Yoshida confirmed this is indeed variable, and a new variable star, from images taken by Nobuo Ohkura, and announced it as one of the MISAO Project new variable stars. MisV1273Tsutomu Fujiwara's observations revealed that MisV1273 is a semi regular variable with a range of 1.9 mag (light curve). The period may be about 140 days. MisV1275 = V756 PerKazuhiro Nakajima's observations revealed it is an Algol-type (EA) eclipsing variable with unfiltered CCD variations of 12.25 mag at maximum, 12.97 mag at primary minimum, 12.87 mag at secondary minimum, and period of 4.6050 days (IBVS 5700). MisV1276 = QY CamPatrick Wils researched the NSVS data and found that it is an EA type star with a period of 1.2727 days (or double). MisV1277 = V892 PerPatrick Wils researched the NSVS data and found that it is a Cepheid type variable with a period of 4.24(7) days. MisV1278
Patrick Wils researched the NSVS data and commented that MisV1278 has a
small range 12.6-12.8, and a possible frequency of 2.787 cycles/day, or
an alias thereof, but because of the small range, it is doubtful.
MisV1279The eclipse events were detected only twice, 2003 Oct. 19 and 2008 Nov. 18, during our survey from 2000 to 2011 by Nobuo Ohkura and Youichirou Nakashima. It seems to be an Algol-type eclipsing variable with a very long period. MisV1282John Greaves researched the NSVS data and found that it is a Mira type variable with a period of 170 days. MisV1286
It may be identified with NSV 11227 whose position is uncertain.
MisV1287Kazuhiro Nakajima's observations revealed it is a beta Lyr-type eclipsing variable with unfiltered CCD variations between 12.25 and 12.78 magnitude, and period of 0.7655 days (IBVS 5700). MisV1288Kazuhiro Nakajima's observations revealed it is a W UMa-type eclipsing variable with unfiltered CCD variations between 12.52 and 13.25 magnitude, and period of 0.3280 days (IBVS 5700). MisV1289Kazuhiro Nakajima's observations revealed it is a W UMa-type eclipsing variable with unfiltered CCD variations between 15.59 and 16.37 magnitude, and period of 0.7053 days (IBVS 5700). MisV1290 = V639 AurKazuhiro Nakajima's observations revealed it is a W UMa-type eclipsing variable with unfiltered CCD variations between 14.01 and 14.85 magnitude, and period of 0.3571 days (IBVS 5700). MisV1291 = V1025 CasKazuhiro Nakajima's observations revealed it is a beta Lyr-type eclipsing variable with unfiltered CCD variations between 12.68 and 13.15 magnitude, and period of 1.0996 days (IBVS 5700). MisV1292 = V1043 CasKazuhiro Nakajima's observations revealed it is a beta Lyr-type eclipsing variable with unfiltered CCD variations between 13.29 and 14.18 magnitude, and period of 0.6616 days (IBVS 5700). MisV1293 = V877 PerKazuhiro Nakajima's observations revealed it is an Algol-type eclipsing variable with unfiltered CCD variations between 13.91 and 15.27 magnitude, and period of 1.1110 days (IBVS 5700). MisV1294 = V1068 CasKazuhiro Nakajima's observations revealed it is an Algol-type eclipsing variable with unfiltered CCD variations between 14.58 and 16.20 magnitude, and period of 1.8060 days (IBVS 5700). MisV1295 = V753 PerKazuhiro Nakajima's observations revealed it is an Algol-type eclipsing variable with unfiltered CCD variations between 12.98 and 13.73 magnitude, and period of 2.2002 days (IBVS 5700). MisV1296 = V343 CamKazuhiro Nakajima's observations revealed it is an Algol-type eclipsing variable with unfiltered CCD variations between 13.61 and 14.89 magnitude, and period of 5.2633 days (IBVS 5700). MisV1306 = V754 Per
Kazuhiro Nakajima's observations revealed it is an Algol-type eclipsing variable with
unfiltered CCD variations between 11.97 and 12.50 magnitude, and
period of 5.3364 days
(IBVS 5700).
MisV1311Tsutomu Fujiwara's observations revealed that MisV1311 is a semi regular variable with a period of 220 days (light curve).
MisV1313Kazuhiro Nakajima's observations revealed it is an Algol-type eclipsing variable with unfiltered CCD variations between 14.65 and 16.18 magnitude, and period of 4.5899 days (IBVS 5700). MisV1317 = V882 Per
Kazuhiro Nakajima's observations revealed it is a beta Lyr-type (EB) eclipsing
variable with unfiltered CCD variations of 11.90 mag at maximum, 12.70
mag at primary minimum, 12.12 mag at secondary minimum, and period of
1.28482 days (IBVS 5700).
MisV1325
Observations by Kazuhiro Nakajima, and the NSVS data suggest that
MisV1325 is almost constant at about 14.2 mag. Observations by Nobuo
Ohkura and Youichirou Nakashima also suggest that it keeps almost
constant at 13.5-13.8 mag from 2001 to 2007, however, it faded only in
2000 and became fainter than 14 mag. So MisV1325 may be a RCB type
variable, which rarely fades out.
MisV1327 = V377 CamKazuhiro Nakajima's observations revealed it is a RRAB type variable with unfiltered CCD variations between 13.85 and 14.80 magnitude, and period of 0.53201 days (IBVS 5700). MisV1329Kazuhiro Nakajima's observations revealed it is an Algol-type eclipsing variable with unfiltered CCD variations between 13.82 and 14.80 magnitude, and period of 4.9478 days (IBVS 5700). MisV1330Kazuhiro Nakajima's observations revealed it is an Algol-type eclipsing variable with unfiltered CCD variations between 14.22 and 14.71 magnitude, and period of 2.8610 days (IBVS 5700). MisV1331Kazuhiro Nakajima's observations revealed it is a beta Lyr-type (EB) eclipsing variable with unfiltered CCD variations of 14.40 mag at maximum, 15.10 mag at primary minimum, 14.80 mag at secondary minimum, and period of 2.8271 days (IBVS 5700). MisV1332Kazuhiro Nakajima's observations revealed it is an Algol-type eclipsing variable with unfiltered CCD variations between 13.74 and 15.14 magnitude, and period of 2.6525 days (IBVS 5700). MisV1333
The variation of this star was discovered in 1999 September in the
course of the MISAO Project. But we regarded it as DV Oph because it
was only 2.1 arcmin from the catalogued position of DV Oph [vsnet-id 111].
MisV1334Taichi Kato analyzed the Catalina Sky Survey data and revealed it is an RR Lyr-type (RRAB type) variable with a period of 0.5772 days. MisV1335Taichi Kato analyzed the Catalina Sky Survey data and revealed it is an RR Lyr-type (RRAB type) variable with a period of 0.6338 days. MisV1336
Discovered during time series photometry of MisV1275.
MisV1337 = PS CamKazuhiro Nakajima's observations revealed it is a beta Lyr-type (EB) eclipsing variable with unfiltered CCD variations of 12.58 mag at maximum, 13.55 mag at primary minimum, 13.01 mag at secondary minimum, and period of 0.9202 days (IBVS 5700). MisV1339
Discovered during time series photometry of MisV1317.
MisV1340
New Mira type variable adjoining to a Mira type variable V2010 Cyg =
LD 162. MisV1340 is a northern component of double stars with similar
brightness lying north-south direction with a separation of 20 arcsec,
and the southern component is V2010 Cyg.
MisV1341Tsutomu Fujiwara's observations detected the rapid brightening up to 11.5 mag in 2014 February, although it kept almost constant at 12.3 mag for over one year from 2012 Novembet to 2014 January [vsnet-alert 16920]. MisV1344The NSVS data suggests it is a Mira type variable with a period of about 300 days and the epoch of JD = 2451370. MisV1347The NSVS data suggests it is a Mira type variable, although the period is not determined. MisV1351
An Algol-type eclipsing variable. However, only two eclipsing events
were detected on 164 nights during three years by Kazuhiro
Nakajima. So the eclipse of MisV1351 must be very rare.
MisV1354 = V1141 CasIt was already found by Patrick Wils and solved by Sebastian Otero to be an EA eclipser with a period of 6.9092 days using the NSVS data, and published in IBVS 5681. Actually, it is not a new variable star of the MISAO Project. MisV1355
Although it had been almost constant during two months in 2001, the
light curve during two months between 2006 and 2007 looks like a
long term variation.
MisV1357Tsutomu Fujiwara's observations revealed that MisV1357 is a Mira-type variable with a range of 4.2 mag (light curve). MisV1358Tsutomu Fujiwara's observations revealed that MisV1358 is a Mira-type variable with a period of 320 days (light curve). MisV1360Hidehiko Akazawa and Nobuo Ohkura revealed that MisV1360 is a W UMa-type eclipsing variable with a period of 0.398132 days based on their observations and the ASASSN data (light curve). MisV1364Tsutomu Fujiwara's observations revealed that MisV1364 is a semi regular variable with a period of 300 days (light curve). MisV1370
Hidehiko Akazawa and Nobuo Ohkura revealed that MisV1370 is a W UMa-type eclipsing variable with a period of 0.246804 days based on their observations and the ASASSN data (light curve).
MisV1371Hidehiko Akazawa and Nobuo Ohkura revealed that MisV1371 is a W UMa-type eclipsing variable with a period of 0.421379 days based on their observations and the ASASSN data (light curve). MisV1372
Tsutomu Fujiwara revealed the color is Rc-V=0.5 mag. USNO-A2.0 color is R-B=2.0 mag. So it is not a red variable.
MisV1376
Ken-ichi Kadota investigated the DSS images, and found that the DSS
images revealed that two faint stars are blending on the Nobuo Ohkura
and Youichirou Nakashima's images. The northern counterpart is clearly
visible on the DSS Bj-band image in 1989, however, not visible on the
B-band images in 1952 and 1954. It looks bright on the DSS R-band and
I-band images.
MisV1384Patrick Wils analyzed the NSVS data and revealed that MisV1384 seems to be an EA type variable with a period of 1.1609 days. MisV1385Patrick Wils commented that it has been found before by Wils P., Lloyd C., Bernhard K. (MNRAS 368, 1757), RRAB type variable with a period of 0.47414 days (not 0.902 days). MisV1386Patrick Wils analyzed the NSVS data and revealed that MisV1386 is an EW type star with a period of 0.3406 days. Kazuhiro Nakajima revised the accuracy of the period as 0.340533 days. MisV1387Patrick Wils analyzed the NSVS data and revealed that MisV1387 is an EW type star with a period of 0.2628 days. Kazuhiro Nakajima revised the accuracy of the period as 0.263002 days. MisV1396
The USNO-A2.0 color is B-R = -0.4 mag.
The RGB composite image from DSS I, R and Bj images also suggests that MisV1396 is remarkably blue.
MisV1424Phase diagram is revised based on the observations by Hidehiko Akazawa and Nobuo Ohkura with the ASASSN data (light curve). MisV1426Stefan Huemmerich reported the Catalina Sky Survey data revealed it is an Algol-type (EA) eclipsing variable with a period of 0.57889 days, brightness range of 15.20-15.90 mag(CV). MisV1427
Stefan Huemmerich, Klaus Bernhard and Sebastian Otero reported the
Catalina Sky Survey data revealed it is an Algol-type (EA) eclipsing
variable with a period of 0.393231 days, brightness range of 15.45-16.20
mag(V)
(light curve,
phase diagram).
MisV1428Hidehiko Akazawa and Nobuo Ohkura revealed that MisV1428 is a W UMa-type eclipsing variable with a period of 0.772402 days, brightness range of 12.12-12.55 mag(V) based on their observations and the ASASSN data (light curve). MisV1429Stefan Huemmerich and Klaus Bernhard reported the LINEAR and Catalina Sky Survey data revealed it is an Algol-type eclipsing variable with a chromospheric activity (EA/RS type), with a period of 0.4629 days, brightness range of 14.35-14.90 mag(CV). It exhibits a long term mean magnitude change, probably caused by a long period spot cycle (light curve, phase diagram). MisV1435Stefan Huemmerich reported the Catalina Sky Survey data revealed it is a W UMa-type (EW) eclipsing variable with a period of 0.32119 days, brightness range of 14.7-15.6 mag(V) (light curve). MisV1436 = QSO B0133+47
We discovered a quasar QSO B0133+47 brightened up to 14 mag in 2007 November.
It is recorded as 18-19 mag in the catalogs, so it is revealed to be an optically violently variable QSO.
Taichi Kato commented that a quasar with such a large amplitude is rare.
Well researched in the radio observations, however, little observed optically.
Nobody has noticed that this quasar becomes so bright.
It is about 7 billion light years from our planet, and the apparent brightness of 14 mag is extraordinary at this distance.
MisV1439 = OT 081
Another optically violently variable quasar observed by the MISAO Project.
But this is a well known quasar.
We assigned the MisV number, but this is not our new discovery.
MisV1441
Seiichi Yoshida, Patrick Wils and Taichi Kato identified it with an
H-alpha emission source HBHA 50-20 = IPHAS J205050.39+445011.7.
MisV1442New eclipsing variable. Seiichi Yoshida found it is recorded in the LONEOS Photometry File "loneos.phot" as follows: 12.95(Ic) 13.57(Rc) 14.22(V) 15.28(B) Four eclipse events of MisV1442 were detected on Oct. 6, Oct. 16, Nov. 4 and Dec. 18 in 2010 by Diego Rodriguez, Esteban Reina Lorenz, Miguel Rodriguez Marco, Faustino Garcia, Adolfo San Segundo, and it is revealed to be an eclipsing variable with a short period. MisV1443
New bright dwarf nova discovered at 14 mag from 2011 Jan. 8 images.
It was bright as 12.8 mag already on Jan. 2 in the Stanislav Korotkiy and Kirill Sokolovsky's images.
It revealed that the MISAO Project discovered this object about one week after the explosion, and the object has already faded by about 2 mag.
MisV1444
On the DSS images, it looks brighter on the blue plate than infrared plate.
But Akira Arai obtained optical spectra and revealed it to be a Mira type.
Probably the POSS2 Blue plate was taken around the maximum, and the POSS2 Infrared plate was taken around the minimum.
MisV1445
Youichirou Nakashima's survey images on 2011 Dec. 17 detected that it brightened rapidly by 2 mag or more, from fainter than 16.8 mag up to 14.7 mag, withiin only 4 minutes.
It is possible real-time flare detection of a new flare star.
MisV1446 = 1RXS J074112.2-094529
Bright new object of 14.1 mag discovered from Youichirou Nakashima's survey images on 2012 Jan. 5.
It will be an outburst of an X-ray source 1RXS J074112.2-094529.
MisV1447
First new object discovered by Masaru Mukai, Kagoshima, Japan.
The variation was confirmed by Youichirou Nakashima's Oku Survey and Akira Takao.
MisV1448New bright dwarf nova discovered at 13.4 mag from 2012 May 27 images. Seiichi Yoshida discovered this object on June 8, about 2 weeks have already passed. However, Denis Denisenko found the pre-discovery data by the MASTER robotic telescopes at 12 mag on May 13, and confirmed the outburst of this star. MisV1449
Possible new cataclysmic variable discovered at 15 mag from 2014 April 23 images [vsnet-alert 17303].
Seiichi Yoshida discovered this object on May 18, about 1 month has already passed.
So we could not confirm it
(Image by Kazuyuki Takeshita on May 18,
Image by Toshikazu Muramatsu on June 1).
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