ISSN 0917-2211

Variable Star Bulletin
No.30-31

Aug. 1998

Outburst of Possible Eclipsing Symbiotic Variable AS 289
Kesao Takamizawa(65-1 Oohinata, Saku-machi, Nagano 384-0502, Japan)
E-mail: GHA07243@nifty.ne.jp
Minoru Wakuda(345 Kwabukuro, Ryuyo-cho, Iwata-gun, Sizuoka 438-0232 Japan)
E-mail: GZJ02446@nifty.ne.jp
Taichi Kato
(Dept. of Astronomy, Kyoto University, Kyoto 606-8502, Japan)
E-mail: tkato@kusastro.kyoto-u.ac.jp
Received 28 May 1998
1.

Introduction

Takamizawa discovered an unusual variable star TmzV17 in the course of his photographic patrol of variable
stars (Takamizawa 1997). The variable (= GSC 5684.522, J2000.0 coordinates: 18h 12m 22:s 13 -11± 400 07:00 1)
was later found to be identical with an emission line object AS 289 (Merrill and Burwell 1950). AS 289 has
been known as a symbiotic star (Sanduleak and Stephenson 1973; Allen 1978) showing moderately strong
He II line and TiO absorption. The object was also studied spectrophotometrically by Blair et al. (1983).
Despite its relatively abundant history of spectroscopy, neither outbursts nor variablity has been reported.
A typical example of photometry of AS 289 is V=13.62 and B-V=2.10 (Munari et al. 1992b). The He II to
H¯ line ratio suggests a hot (» 1:5 £ 105 K) ionizing source (Kenyon 1986).
2.

Observations and results

The observations by Takamizawa were done at Saku Observatory (Saku-machi, Nagano, Japan), using twin
10-cm patrol cameras (PENTAX 100SDUF, °=400mm) and T-Max400 ¯lms. Wakuda's observations weredone at his home, using a 10-cm camera (°=400mm), T-Max and Tri-X ¯lms. The both observers use
consistently GSC stars for determining the magnitudes. The resultant magnitude estimates are given in
Table 1, the overall light curve in Figure 1. The light curve shows a sharp rise in brightness around JD
2449834 (1985 April 26). The most striking feature is a temporal fading by more than two magnitudes
between 1996 January and May. Assuming the symmetry, the minimum of the fading was determined as
JD 2450176 3 or 1996 April 2. After the recovery from this episode, the system showed a gradual fadetypical for a symbiotic outburst. The system again showed brightening in early 1998 as noticed by Wakuda.
Wakuda's survey on his patrol ¯lms revealed another brightening in 1984, which is also included in Table 1
and Figure 1.
3.

Discussion

The present observation is the ¯rst that revealed the signi¯cant variation of the symbiotic star AS 289.
The variation is globally characterized by episodic outbursts observed in 1984 and 1995. This interval ofoutbursts is typical for those of classical symbiotic variables (the limited observations between these two
outbursts may have missed some other brightenings, though). However, the early 1996 fading episode isunique, and remarkably similar to eclipses seen in FG Ser = AS 296 (Munari et al. 1992) and V1413 Aql =AS 338 (Wakuda 1988; Munari 1992). Figure 2 shows the detailed light curve of the current outburst. We
suspect the eclipse is responsible for the fading episode of AS 289 during outburst. The pro¯le of light curve
suggests the eclipse may be grazing total, while the brightness at minimum is considerably brighter than the1

Figure 1.

Overall light curve of AS 289

pre-outburst level, implying that a certain fraction of the outbursting source remain uneclipsed. It is notstill certain regarding the periodicity, but considering the duration of the fading (» 100 d) comparable tothat of FG Ser (Munari et al. 1992), the orbital period may be an order of » 600-700 d. This period may
imply that the relatively faint level in late 1997 may be somehow related to eclipse, or that the next eclipse
was unfortunately missed during the solar conjunction period.

JD-2400000
45944.042
47267.272
47274.236
47961.317
47986.271
49485.182
49507.197
49520.219
49531.051
49537.046
49538.192
49546.11949574.143
49575.041
49620.989
49648.892
49756.319
49783.273
49784.261
49788.284
49809.244
49815.243
49831.197
49834.242

mag
12.8
14.5
14.3
14.3
14.4
14.9
14.7
14.3
14.2
14.3
14.2
14.2
14.2
14.7
14.8
14.0
14.8
14.8
14.4
14.9
14.8
14.8
14.7
13.7

Table 1. Observations of AS 289
code¤ JD-2400000 mag code¤ JD-2400000
Wdm
49860.126
13.1 Tmz
50328.928
Wdm
49860.134
12.5 Wdm
50372.899
Wdm
49870.143
12.6 Tmz
50386.889
Wdm
49888.047
12.4 Tmz
50494.342
Wdm
49922.083
12.8 Tmz
50515.313
Tmz
49934.081
12.9 Tmz
50578.190
Tmz
49943.950
12.1 Tmz
50597.097
Wdm
49950.062
11.9 Tmz
50606.201
Wdm
49957.058
12.0 Tmz
50613.155
Tmz
49972.945
12.1 Tmz
50629.128
Wdm
49981.981
11.8 Tmz
50629.153
Tmz
50002.912
12.1 Tmz
50633.144
Wdm
50015.905
12.2 Tmz
50636.110
Tmz
50110.340
13.0 Tmz
50644.178
Tmz
50125.344
12.8 Tmz
50654.019
Tmz
50133.314
12.6 Tmz
50682.985
Tmz
50161.260
14.0 Tmz
50719.933
Tmz
50186.199
13.9 Tmz
50740.914
Wdm
50197.240
13.8 Tmz
50771.888
Tmz
50229.191
12.6 Tmz
50875.299
Tmz
50254.124
12.1 Tmz
50880.289
Tmz
50277.101
11.9 Tmz
50907.283
Tmz
50300.035
11.7 Tmz
50938.231
Tmz
50310.983
11.9 Tmz
¤

mag
11.8
12.0
11.8
12.6
12.7
12.8
12.9
13.0
13.5
13.2
12.6
12.9
13.1
13.1
13.1
13.2
13.1
13.0
13.1
12.7
12.4
12.2
12.3

code¤
Tmz
Tmz
Tmz
Tmz
Tmz
Tmz
Tmz
Tmz
Tmz
Tmz
Wdm
Tmz
Tmz
Tmz
Tmz
Tmz
Tmz
Tmz
Tmz
Tmz
Tmz
Wdm
Wdm

code: Tmz (Takamizawa), Wdm (Wakuda)

References
Allen D. A. 1978, MNRAS 184, 601
Blair W. P., Feibelman W. A., Michalitsianos A. G., Stencel R. E. 1983, ApJ Sup. 53, 573
Kenyon S. J. 1986, The Symbiotic Stars (Cambridge University, Cambridge)
Merrill P. W., Burwell C. G. 1950, ApJ 112, 72
Munari U. 1992, A&A 257, 163
Munari U., Whitelock P. A., Gilmore A. C., Blanco C., Massone G., Schmeer P. 1992a, AJ 104, 262
Munari U., Yudin B. F., Tarnova O. G., Massone G., Marang F., Roberts G., Winkler H., Whitelock P. A., 1992b, A&A Sup.
93, 383
Sanduleak N., Stephenson C. B. 1973, ApJ 185, 899
Takamizawa K. 1997, VSOLJ Variable Star Bulletin 26-27, 1
Wakuda M. 1988, VSOLJ Variable Star Bulletin 5, 17211Photographic Magnitude

AS 289
12

13

14

15

16
46000

47000

48000

49000

JD - 2400000

50000

51000

AS 289 (1995-1998)

Photographic Magnitude

11

12

13

14

15

16
49200

49400

49600

49800

50000

50200

JD - 2400000

50400

50600

50800

51000

22 NEW VARIABLE STARS DISCOVERD FROM PATROL FILMS(NEW VARIABLE STARS SERIES III)
Kesao Takamizawa(65-1 Oohinata, Saku-machi, Nagano, 384-0502 Japan)
E-mail: GHA07243@nifty.ne.jp
Received 1998 Jul. 02
1.

Introduction

The author already reported on 21 new variable stars (Takamizawa 1997a, 1998a), and this is the 3rd reportof the new variable stars series. In this report, I report on 22 new variables of 5 di®erent types, with accurate
coordinates, suggested types, elements of variability, individual observations, and identi¯cation charts. The
summary of the 22 new variable stars is given in Table 1.

Desig.
TmzV03TmzV10TmzV13TmzV23TmzV24TmzV27TmzV29TmzV30TmzV31
TmzV32
TmzV33TmzV34
TmzV35
TmzV41
TmzV42TmzV43TmzV44TmzV45
TmzV46
TmzV47
TmzV48TmzV51

R.A.

Table 1. New variable stars
Decl.
max
min
type

(J2000.0)
08 48 12:70 +21± 070 13:00 505 37 29:11 +67± 250 32:00 705 12 54:11 +59± 190 36:00 3
08 24 24:42 +50± 000 50:00 2
07 47 50:05 +58± 590 26:00 0
06 00 31:04 +55± 270 14:00 6
17 43 14:68 -04± 200 56:00 4
18 29 31:47 +22± 340 24:00 3
18 12 44:67 +21± 240 19:00 1
18 28 23:02 +31± 210 33:00 8
18 16 58:18 +15± 590 18:00 409 15 51:69 +09± 000 49:00 909 39 25:57 +34± 140 53:00 0
17 22 45:90 -08± 330 59:00 1
14 13 59:56 +47± 260 42:00 5
15 08 25:79 +09± 360 18:00 9
15 11 58:77 +06± 020 19:00 7
15 18 40:25 +14± 590 02:00 9
15 26 13:99 +08± 180 03:00 8
15 27 23:61 +04± 280 28:00 3
11 45 01:44 +64± 470 37:00 6
17 39 28:09 -07± 580 59:00 9

JD-2400000
49418.007
49477.983
49666.315
49770.937
50074.247

12.1
10.7
12.1
11.6
11.9
11.4
14.6
10.4
11.2
11.3
11.0
13.1
10.3
12.4
12.9
12.0
13.0
11.9
12.8
12.9
12.6
12.8

13.1p
14.8p
(15.3p14.3p
13.1p(14.1p(15.5p
11.6p
12.5p
13.1p
15.0p
15.0p
15.0p
15.0p
15.1p
15.1p
14.4p
14.0p
15.3p
15.0p
15.0p
15.5p

L:
M
M:
EA
SR
M:
M
EA
SR:
EA
M
L
M
M
SR:
M
L
SR
UG:
SR
M:
M

period
530:
180:
310:
310
410:
510
510:
290:
148:
315
280:
170:
230:

Table 2. Observations of TmzV03
mag(p) JD-2400000 mag(p) JD-2400000
12.450095.036
12.850730.282
12.550096.019
12.750758.256
12.750151.964
12.5
50814.196
12.6
50378.319
12.550833.040
12.4

epoch
JD 2400000+
50770:
50800:
50880:
50880
50880
50890:
50900:
50740
50940
50770:
50950:

12.1
12.4
13.1
12.6

The observations were done at Saku Observatory (IAU code 862), using twin 10cm patrol cameras(PENTAX 100SDUF °=400mm) and T-Max400 ¯lms. The magnitudes were determined against neighboring
GSC stars.
32.

TmzV03TmzV03 is identical with GSC1399.1081 = USNO 1050.05960156. No IRAS identi¯cation. The USNO
color(B-R=+0.6)is neutral. The observed range of variability was 12.1 - 13.1p. The type of variability is
L(Takamizawa,1996).
3.

TmzV10TmzV10 is identical with GSC 4093.514 = USNO 1500.04314830 = IRAS 05322 +6723. The observed rangeof variability was 10.7 - 14.8p, the range and USNO color (B-R=+3.8) suggests a Mira-type variable, and a
period of about 530d (Takamizawa,1997b).

JD-2400000
49745.022
49751.967
50050.092
50071.051

4.

Table 3. Observations of TmzV10mag(p) JD-2400000 mag(p) JD-2400000
14.3
50672.219
13.650804.001
14.850762.182
10.750814.097
14.4
50776.046
10.750874.931
13.650786.216
10.850890.937

mag(p)
10.9
11.4
13.6
14.6

TmzV13The star is identical with GSC 3747.1489 = USNO 1425.05952289 = IRAS 05084 +5916. The star is a
Mira-type variable star with a range 12.1-(15.3p, and a period of about 180d. The USNO color(B-R=+4.0),
and the IRAS variability °ag support this (Takamizawa 1997c).

JD-2400000
49665.085
49710.969
49745.012
50050.090

5.

Table 4. Observations of Tmz13
mag(p) JD-2400000 mag(p) JD-2400000(15.050672.218(15.1
50814.080(15.150776.078
12.850874.931(15.3
50786.215
12.1
50890.957(15.150804.036
12.1

mag(p)
12.1
15.0
(14.5

TmzV23TmzV23 is identical with GSC 3421.2216 = USNO 1350.07535203. No IRAS identi¯cation; the USNO color
neutral. This star seems to be an eclipsing binary. The observed range of variability was 11.6-14.3. I havejudged the type of variability as EA (Takamizawa 1998b).

JD-2400000
49668.186
49770.922
50734.240

6.

Table 5. Observations of TmzV23
mag(p) JD-2400000 mag(p) JD-2400000
11.750758.239
11.650874.956
12.2
50814.128
11.750901.972
14.3
50833.023
12.0

mag(p)
13.8
11.8

TmzV24TmzV24 is identical with GSC 3795.1847 = USNO 1425.07109987 = IRAS FSC 07435 +5906. The observed range of variability was 11.9-13.1p. Although the range is rather small due to the limited number ofobservations, I have judged the type of variability as SR(Takamizawa 1998c).

4

JD-2400000
49668.181
49769.015
50734.232
50758.224

7.

Table 6. Observations of TmzV24
mag(p) JD-2400000 mag(p) JD-2400000
12.650762.226
12.950874.956
12.650814.119
12.1
50890.953
13.1
50816.065
11.950901.969
13.0

mag(p)
12.4
11.9
12.3

TmzV27This star is identical with USNO 1425.06458060 = IRAS 05563 +5527. The observed range of variability was
11.5-14.1p. Although the range is rather small due to the limited number of observations,the range suggests
the Mira-type (Takamizawa 1998d).

JD-2400000
49745.030
49751.968
50071.064
50372.249
50672.228

8.

Table 7. Observations of TmzV27
mag(p) JD-2400000 mag(p) JD-2400000
13.550762.175
13.050814.097
13.7
50776.087
12.650832.962
14.1
50777.046
12.850874.940(14.150804.008
12.250890.943(14.1

mag(p)
12.0
11.5
11.4
11.4

TmzV29TmzV20 is identical with USNO 0825.11076786 = IRAS 17405 -0419. The star is Mira-type variable star witha range of 14.6-(15.5p, and period of about 310d. The USNO color(B-R=+4.8) support this (Takamizawa
1998e).

JD-2400000
49457.172
49507.149
49518.100
49620.965
49647.916
49749.323
49756.309

9.

Table 8. Observations of TmzV29
mag(p) JD-2400000 mag(p) JD-2400000(15.549775.281(15.2
50578.174(15.549860.152(15.550606.176(15.050003.944(15.050631.053
14.650109.347(15.2
50644.169(15.050254.112
14.550746.915(14.750494.314(15.250880.253(15.2
50517.279
15.3
50906.239

mag(p)
15.0
15.1
(15.0
(15.2
(15.0
14.7
14.9

TmzV30The star is identical with GSC 2106.2463 = USNO 1125.09746325 = 1RXS 18291.3 +223426. In the 1st reportof discovery of this star, the author suspected TmzV30 to be an eclipsing binary. The type of variability is EA.
The period and the epoch were not determined from the available data(Takamizawa 1998f). Japanese novae
discoverer M.Wakuda(Shizuoka), checked his patrol ¯lms of this area. His observation on JD 2449520.099(2days after from my second observation) indicated 11.6mpv(personal communication). Also,T.Kato suspected,
the star is detected by ROSAT(Kato 1998a). A search for the period is encouraged.
10.

TmzV31

TmzV31 is identical with GSC 1579.1739 = USNO 1050.10094312. The star color (B-R=+1.3) is notextermely red as judged from the USNO identi¯cation. The observed range of variability was 11.2-12.5p,anda period of about 410d. The type of variabi-lity is SR(Takamizawa 1998g).
5

11.

JD-2400000
49457.205
49518.126
49531.019
49680.880

Table 9. Observations of TmzV30
mag(p) JD-2400000 mag(p) JD-2400000
10.549749.331
10.4
50004.912
10.449756.294
10.4
50688.012
10.749888.032
11.650880.245
10.5

mag(p)
10.5
10.4
10.4

JD-2400000
49457.205
49518.126
49531.019
49680.880

Table 10. Observations of TmzV31
mag(p) JD-2400000 mag(p) JD-2400000
11.549749.331
11.4
50004.912
12.1
49756.294
11.2
50688.012
12.2
49888.032
11.750880.245
12.3

mag(p)
12.3
11.3
12.5

TmzV32This star is identical with GSC 2624.209 = USNO 1200.09424157 = IRAS FSC 18264 +3119. The observed
range of variability was 10.4-11.6, and only one timing of minima were observed. The type of variability is
EA. A search for the period is encouraged(Takamizawa 1998h).

JD-2400000
49457.201
49518.131
49531.024
49537.029

12.

Table 11. Observations of TmzV32
mag(p) JD-2400000 mag(p) JD-2400000
11.4
49749.331
11.3
50688.011
11.4
49888.024
11.450880.237
11.4
50004.921
11.450880.242
11.3
50631.064
11.5

mag(p)
11.4
13.1
13.1

TmzV33The star is identical with GSC 1568.727 = USNO 1050.10257492 = IRAS 18147 +1558. The star is a Miratype variable with a range of 11.0-15.0p, and a period of about 510d. The USNO color(B-R=+4.0) support
this(Takamizawa 1998h).
13.

TmzV34

TmzV34 is identical with GSC 819.892 = USNO 0975.06284313 = 1RXS 091552.3 +090056. On JD244968.215 and JD-2449687.218, only one timing of maximum were observed. The star is visible at mag
15 on Real-Sky CD (Takamizawa 1998i). T.Kato suggested irregular-looking light variation and the likely
ROSAT identi¯cation(Kato 1998b).
14.

TmzV35The star is identicial with USNO 1200.06413746 = IRAS 09364 +3424. The star is a Mira-type variablewith a range of 10.3-(15.0p, and a period of about 510d(Takamizawa 1998i).
15.

TmzV41

TmzV41 is identicial with USNO 0750.10964275 = IRAS 17200 -0831. This star is a Mira-type variable
star with a range of 12.4-(15.0p,and a period of about 290d. The star is visible at mag. 17 on Real-Sky
CD(Takamizawa 1998j).

6

JD-2400000
49457.209
49518.122
49546.135
49680.880

Table 12. Observations of TmzV33
mag(p) JD-2400000 mag(p) JD-2400000
15.049749.339
12.0
50004.912
15.2
49756.294
12.1
50688.002
15.049888.032(15.050880.245
13.0

mag(p)
14.8
(15.0
11.0

JD-2400000
49418.031
49471.024
49485.030
49660.228
49687.215

Table 13. Observations of TmzV34
mag(p) JD-2400000 mag(p) JD-2400000
14.949687.218
13.1
50721.308
14.8
49770.995
14.650734.276(14.550096.071
14.750816.128(15.050151.985
14.550891.069
13.1

mag(p)
(14.5
14.4
14.6
14.6

JD-2400000
49418.019
49471.036
49485.060
49659.218
49686.309

Table 14. Observations of TmzV35
mag(p) JD-2400000 mag(p) JD-2400000
12.049687.232
12.950721.294
13.2
49770.980
12.650751.251
13.750011.247
11.2
50816.110(14.050096.050
13.750891.060
13.050151.972(15.0

mag(p)
14.5
14.6
(15.0
10.3

JD-2400000
49401.336
49454.302
49479.190
49507.140
49620.959
49647.892
49745.337
49759.294

Table 15. Observations of TmzV41
mag(p) JD-2400000 mag(p) JD-2400000
15.249775.267
12.950513.291
12.7
49834.176
15.050606.151
12.450109.329
15.050631.031
13.050135.297(15.050746.889(15.050213.092(15.050839.340(15.050254.067
15.2
50875.260
12.850492.319(15.050898.240
12.8mag(p)
(15.0
13.0
13.4
(15.0
14.8
13.0
12.8

7

16.

TmzV42The star is identical with GSC 3465.188 = USNO 1350.08565342. The observed range of variability was
12.9-15.1p. The USNO color(B-R=+0.4) suggests a non-red variable star(Takamizawa 1998k). C.Lloyd(United Kingdom) suspected that, despite the apparent lack of redness this star is still probably one formof late-type variable, and a period of 148d(Lloyd 1998).

JD-2400000
49538.044
49809.109
50213.042

17.

Table 16. Observations of TmzV42mag(p) JD-2400000 mag(p) JD-2400000
13.550438.266
13.950902.189
12.950513.274
14.5
50921.058
14.4
50816.281
13.8

mag(p)
15.1
14.4

TmzV43TmzV43 is identcial with GSC 919.29 = USNO 0975.07831129 = IRAS 15060 +0947. The star has a range of
12.0-15.1p, and a period of 315d. The range suggests Mira-type classi¯cation, but the possibility of SR-type
is not excluded (Takamizawa 1998l).

JD-2400000
49427.186
49539.090
49620.926
49716.312
49815.191

18.

Table 17. Observations of TmzV43
mag(p) JD-2400000 mag(p) JD-2400000
13.550054.349
12.950741.892
13.050082.310
12.3
50819.325
14.2
50254.009
14.2
50906.221
14.2
50684.021
12.850923.133
12.3

mag(p)
12.0
13.5
14.2
15.1

TmzV44TmzV44 is identical with GSC 347.695 = USNO 0900.07988745. No IRAS identi¯cation. The star color(BR=+0.3) is not exteremely red as judged from the USNO identi¯cation. The observed range of variability
was 13.0-14.4p, without detectable regularity. I have judged the type of variability as L (Takamiza 1998l).

JD-2400000
49427.193
49454.231
49539.086
49620.931
49716.332
49745.289

19.

Table 18. Observations of TmzV44mag(p) JD-2400000 mag(p) JD-2400000
13.549815.196
12.850254.009
14.4
49870.015
13.250606.112
13.650054.349
13.1
50684.977
13.550082.318
13.2
50819.325
13.450187.197
13.050906.221
14.0

mag(p)
13.7
13.5
13,0
13.2
12.3

TmzV45

TmzV45 is identical with GSC 926.303 = USNO 0975.07890045. No IRAS identi¯cation, but the USNO
color(B-R=+4.4) suggests a red variable. This star is an SR-type variable star with a range of 11.9-14.0p,
and a period of 280d(Takamiza 1998m).
20.

TmzV46

TmzV46 is identical with USNO 0975.07935332. No IRAS identi¯cation. In the 1st report of discovery of thisstar, the author suspected the possible a Mira-type classi¯cation.The star is visible at mag 18 on Real-Sky
8

JD-2400000
49427.183
49478.126
49539.078
49620.923

Table 19. Observations of TmzV45
mag(p) JD-2400000 mag(p) JD-2400000
13.6
49701.341
13.850684.021
13.2
49716.312
13.350741.892
11.9
49815.203
12.050819.317
13.050082.310
12.850906.214

mag(p)
12.4
12.8
14.0
12.8

CD(Takamizawa 1998n). T.Kato suggested the USNO color is more neutral(rather than red); variable ofother type (e.g.UG-type) can not be excluded(Kato 1998c).

JD-2400000
49427.186
49539.090
49620.926
49716.312
49815.203

21.

Table 20. Observations of TmzV46
mag(p) JD-2400000 mag(p) JD-2400000(15.350054.349(14.050741.892(15.1
50082.310(15.1
50819.325
12.850254.009(15.3
50906.221
14.850684.021(14.050923.133(15.3

mag(p)
(12.9
(14.8
12.8
(15.3

TmzV47TmzV21 is identical with GSC 345.1078 = USNO 0900.08115606 = IRAS FSC 15248 +0438. This staris an SR-type variable with a range of 12.9-15.0p. The USNO color and IRAS °ux suggest a normal red
variable(Takamizawa 1998o).

JD-2400000
49427.193
49454.231
49539.086
49620.931
49716.332
49745.289

22.

Table 21. Observations of TmzV47
mag(p) JD-2400000 mag(p) JD-2400000
13.649815.196
13.050254.009
12.9
49870.015
13.550606.112
13.150054.349(13.050684.977
13.450082.318
13.1
50819.325
13.550187.197
14.050906.221
13.2

mag(p)
(14.5
14.6
13.8
14.8
15.0

TmzV48TmzV48 is identical with GSC 4156.392 = USNO 1500.05514302 = IRAS 11422 +6504. The star has a rangeof 12.6-(15.0p, and a period about 170d. The range suggests a Mira-type classi¯cation, but the possibilityof SR-type is not excluded (Takamizawa 1998p).
23.

TmzV51The star is identical with GSC 5660.180 = USNO 0750.11669838.= IRAS 17367 -07 57. The star is a Miratype variable with a range of 12.8-15.5p, and a period of about 230d. The USNO color(B-R=+4.0) support
this (Takamizawa 1998q).

9JD-2400000
50192.008
50548.974
50564.992
50748.219

Table 22. Observations of TmzV48
mag(p) JD-2400000 mag(p) JD-2400000(15.050750.288
13.350808.219(15.050754.267
12.8
50839.203(15.050762.275
12.650920.995
13.5

mag(p)
12.7
13.6
(15.0

JD-2400000
49401.342
49457.168
49507.152
49537.094
49620.969
49647.910
49749.323
49756.309
49775.279
49860.152
49860.152

Table 23. Observations of TmzV51
mag(p) JD-2400000 mag(p) JD-2400000(15.450109.347(15.250606.176
13.3
50135.305(15.250644.169
13.650254.112
15.3
50654.001(15.4
50328.951
15.4
50682.962(15.4
50372.911(14.2
50710.933(15.050494.322(14.2
50746.915
13.5
50515.287(15.4
50875.306
13.650549.262
15.5
50898.275
14.1
50570.163(14.5
50906.239(15.2
50578.167(15.4
50924.159
14.2

mag(p)
(15.4
(15.4
15.2
13.7
13.6
(14.2
15.2
14.2
13.3
12.8

Acknowledgments
I wish to express my sincere gratitude to Dr.Taichi Kato, Kyoto University, who kindly read themanuscript and suggested many improvements. Many thanks are also due to Mr.Seiichro Kiyota and
Mr.Minoru Wakuda.
References
Kato,T., 1998a. Vsnet-obs circular No.10232||- 1998b. ditto, No.10504||- 1998c. ditto No.11015
Lloyd,C.,1998. Vsnet-obs circular No.10772
Takamizawa,K.,1996. NIFTY-Serve FSPACE cir.3 No.2631|||| 1997a. Variable star bulletin.No.26-27|||| 1997b. VSOLJ-obs circular No.46|||| 1997c. ditto No.106|||| 1998a. Variable star bulletin. No.28-29|||| 1998b. VSOLJ-obs circular. No.162|||| 1998c. ditto, No.170|||| 1998d. ditto, No.231|||| 1998e. ditto, No.265|||| 1998f. ditto, No.266|||| 1998g. ditto, No.268|||| 1998h. ditto, No.288|||| 1998i. ditto, No.296|||| 1998j. ditto, No.313|||| 1998k. ditto, No.320|||| 1998l. ditto, No.334|||| 1998m. ditto, No.342|||| 1998n. ditto, No.345|||| 1998o. ditto, No.346|||| 1998p. ditto, No.361|||| 1998q. ditto, No.370

10Figure 1. Finding charts of 22 new variable stars

EditorAssistant-editor
Sta®

Keiichi
Seiichi
MakotoMasahiko
Seiichiro

11

Saijo
SakumaWatanabe
MomoseKiyota