NGC 6093 / C1614-228 / Messier 80
RA: 16:17:02.41 DEC: -22:58:33.9 (J2000)
(Most recent updates:
Membership probability flag - 2024; Remaining data - July 2017)
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Bytes Format Explanation
1-8 A8 Star ID
10-32 A11,1x,A11 Position
34-35 A2 Membership probability flag based on data published
by Prudil & Arellano Ferro (2024)
m1: prob >=0.85; m2: prob >=0.7 and <0.85;
m3: prob >= 0.5 and <0.7; f: prob <0.5
u: no data available
37-44 F8.4 Period (days)
46-51 F6.3 Mean magnitude (or maximum magnitude if "max"
is indicated in the remarks column)
53-57 F5.3 Light amplitude (range of variability)
59 A1 Colour for mean magnitude and amplitude
e.g. B, V, R, I, J, K
or P (for photographic).
61-65 A5 Type of variable (draft 2006 GCVS classifications)
CST denotes non variable stars previously designated
as variables
67-80 A19 Notes and Remarks (f denotes field star)
"--" or "----" indicates no data available
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ID Position Mem Period <mag> ampl C Type Notes/
RA Dec Flag Remarks
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1 16:16:52.62 -22:57:16.1 m1 16.3042 13.365 -- V CW Note
2 16:17:04.22 -22:58:53.8 m1 ---- 13.31 -- V SR? Note
3 16:17:10.23 -22:57:38.0 m1 0.3457 16.144 0.418 V RR1
4 16:16:56.48 -22:57:34.2 m1 0.3864 16.164 0.430 V RR1
5 16:17:03.59 -22:59:40.4 m1 0.6642 16.180 0.931 V RR0
6 16:17:40.21 -22:53:35.8 u 178.2010 10.46 3.75 V M f;max;Note
7 16:17:39.07 -22:56:40.4 u 225.1432 9.94 5.2 V M f;max;Note
8 16:17:00.76 -22:58:17.1 m1 0.6618 16.070 1.097 V RR0
9 16:17:03.66 -22:57:58.7 f 0.6641 16.833 0.927 V RR0
10 16:17:01.17 -22:58:34.6 m1 0.6140 -- -- RR0 Note
11 16:17:02.2 -22:58:37.9 f ---- 19.3 2.3 U UG? max;Note
12 16:16:59.8 -22:58:18.0 f ---- 19.0 3.3 U UG? max;Note
13 16:17:12.94 -22:58:49.3 m1 0.4974 -- -- V RR1
14 16:16:55.32 -22:57:30.9 m1 0.3164 16.180 0.134 V RR1
15 16:17:04.04 -22:58:40.2 u 0.3479 -- -- RR1
16 16:17:04.61 -22:56:40.0 m1 0.3532 16.126 0.181 V RR1 multi P
17 16:17:02.88 -22:58:32.6 u 0.4154 -- -- RR1 Note
18 16:16:58.60 -22:58:35.3 m1 0.4282 16.260 0.089 V RR1
19 16:17:02.11 -22:58:29.5 f 0.5956 -- -- RR0 Note
20 16:17:03.26 -22:58:37.5 f 0.7448 -- -- RR0
21 16:17:02.60 -22:58:06.9 m1 0.8143 15.967 0.494 V RR0
22 16:17:06.76 -22:58:29.4 f 0.0458 18.170 0.298 V SXP
23 16:16:58.11 -22:57:44.1 m1 0.0459 18.838 0.112 V SXP
24 16:17:02.99 -22:59:21.1 f 0.0494 18.259 0.099 V SXP Note
25 16:17:00.33 -22:56:20.9 m1 0.1394 21.821 0.340 V SXP? f?;Note
26 16:17:04.49 -22:59:17.9 u 0.3190 19.280 0.147 V EW
27 16:17:04.02 -22:58:26.5 f 0.4117 -- -- EW
28 16:17:01.89 -23:00:47.7 m1 2.14 19.306 0.166 V ? f?
29 16:17:06.22 -22:58:36.9 f 2.421 17.870 0.115 V ? f
30 16:17:05.54 -22:57:42.6 m1 ---- 13.864 0.027 V SR?
31 16:17:05.24 -22:57:55.3 m1 ---- 13.520 0.037 V SR?
32 16:17:05.33 -22:58:41.5 m1 ---- 13.871 0.029 V SR?
33 16:17:02.16 -22:58:33.2 f 0.0385 -- -- SXP Note
34 16:17:02.82 -22:58:33.8 u ---- 16.44 0.36 I ? Note
35 16:17:03.31 -22:58:33.2 m1 ---- 11.40 0.09 I L
36 16:17:03.15 -22:58:41.9 m1 ---- 11.50 0.12 I L
37 16:17:02.32 -22:58:30.5 f ---- 11.51 0.09 I L
38 16:17:03.26 -22:58:35.0 f ---- 11.70 0.04 I L
39 16:17:02.20 -22:58:34.5 f ---- 11.75 0.07 I L
40 16:17:03.04 -22:58:25.7 f ---- 12.36 0.13 I L
Nova 16:17:02.82 -22:58:33.9 u ---- 6.8 -- V N max;TSco
PSR -- -- -- -- -- -- u ---- -- -- 1 msP
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Supplementary Notes
The data for V1-33 are from Kopacki (2013) unless indicated otherwise in
the notes on individual stars (e.g. V6, V7, V11, V12)
The data for V34-40 are from Figuera Jaimes et al. (2016).
For the Nova, the RA and dec are from Dieball et al. (2010). It is their
X-ray source CX01. The maximum visual apparent magnitude was derived by
Sawyer (1938 - see page 75), based on the estimates of 7.0 and 6.5 by
Auwers and Luther respectively, on May 21, 1860.
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Notes on Individual Stars
V1: Wehlau et al. (1984) pointed out that the y value that Sawyer Hogg
listed for for V1 in her 2nd and 3rd catalogues (Sawyer 1955, 1973)
was incorrect. It should be y = +79 arcsec (instead of +49).
The period listed above is from Wehlau et al. (1990) and the mean V
magnitude is from Kopacki (2013).
Matsunaga et al. (2006) observed V1 in the JHK bands and confirmed
Wehlau's period. In their paper, Matsunaga et al. listed incorrect
values of RA and dec for V1. The values they listed were the RA
and dec for V2.
K magnitude observations of V1 were obtained with the Kepler space
telescope. The results were reported by Plachy et al. (2016) who
detected clear cycle-to-cycle variations in the light curve and
period doubling in the pulsation.
V2: The V magnitude listed for V2 in the above table is from the CM
diagram (Fig 10) published by Kopacki (2013) which shows that the
star is located at the RG tip. He derived the V magnitude by
adding 0.61 to the value published by Alcaino et al. (1998) to
match the photometric system of Stetson (2000). Kopacki did not
detect any variability in V2 but pointed out this might have been
due to the short length of his observing run.
Wehlau et al. (1990) commented that V2 showed very little amplitude
in either B or V and pointed out that the tentative period
(24.9 days) published by Sawyer Hogg (1973) in her 3rd catalog was
not confirmed in subsequent data.
V6, V7:
These two stars are S Sco and R Sco respectively. The RA and dec
listed above are from Samus et al. (2009) and the remaining data are
from the ASAS survey (Pojmanski 2002). The listed magnitudes are
maximum V magnitudes. Both stars are considered to be field stars.
V10:
Figuera Jaimes et al. (2016) derived mean I = 14.25 mag for V10,
which is a magnitude brighter than the values they derived for the
three other RR Lyrae variables in their field: V17 (I=15.31), V19
(I=15.28), V20 (I=15.31). Since these stars are all located in the
crowded central region of the cluster, it is assumed that they are
all cluster members and that the anomalously bright magnitude for
V10 is caused by an unresolved companion. Kopacki (2013) published
V-filter light curves, expressed in flux units, for these four
variables, but did not derive mean magnitudes.
V11, V12:
The data for V11-12 are from the discovery paper by Shara et al. (2005)
V17, V19:
These two stars were independently detected as variables by
Thomson et al. (2010) who designated them as TDK1 (V19) and TDK3 (V17).
Dieball et al (2010) designated them as #2324 and #2817. They were
also observed by Figuera Jaimes et al. (2016) who derived mean I
magnitudes of 15.31 and 15.28 respectively.
V24: Kopacki (2013) found 2 periods for this star with period ratio
f1/f2=0.98. He concluded that one of the modes is nonradial.
Salinas et al. (2016) derived a mean r magnitude and amplitude
18.67 and 0.13 mag.
V25: Kopacki (2013) tentatively classified this star as SX Phe, but
pointed out that it could also be a W UMa or ellipsoidal binary
system. If V25 in an SX Phe variable, it is probably not a cluster
member since it is about 3 magnitudes fainter than the SX Phe
variables, V22, V23 and V24.
V33: The period and classification for V33 are from Thomson et al.
(2010). It was their variable TDK#2.
V34: Figuera Jaimes et al. (2016) detected a brightening in this star
which is located at the position that Dieball et al. (2010)
published for the Nova. It has not been determined whether or
not this is associated with the Nova.
=======================================================
Discovery of the variable stars in M80:
V1-2
Bailey (1902) with x,y position and ID chart
(see Appendix page 237 for x,y tables and page 246 for
description of plates).
V3-6
Sawyer (1942) with x,y positions and an ID chart.
V6-7 = S Sco, R Sco
These are both Mira variables in the field and were discovered in
1853. The number V6 was assigned by Sawyer (1942) and V7 by Sawyer
(1955) in the 2nd edition of her catalogue.
V8-10
Wehlau et al. (1984) with x,y coordinates
ID charts for V1-10 were later published by Wehlau et al. (1990).
V11-V12 = DN1&DN2
Shara et al. (2005 ) with RA, dec and ID chart
The numbers V11&V12 are assigned here.
V13-V32
Kopacki (2013) with RA and dec
In a preliminary report, Kopacki (2009) announced his new variables,
but used a different numbering system. In the above table, we use
the numbers he assigned in his 2013 paper.
V33 = Dieball et al. (2010) #2238 = TDK #2 of Thomson et al. (2010)
The number V33 was assigned by Kopacki (2013)
Dieball et al. (2010) and Thomson et al. (2010) identified this
star as a blue straggler and derived a period of approximately
55 minutes. They classified it as an SX Phe variable.
V34-40
Figuera Jaimes et al. (2016) with RA, dec and ID chart
Nova = T Sco
The nova was discovered in 1860. An account of its discovery
was given by Sawyer (1938) and also by Wehlau et al. (1990).
The RA and dec listed above are from Dieball et al. (2010)
PSR: According to Paulo Freire's website at the Max Planck
Institute in Bonn (July 2024 version), there is
1 millisecond pulsar in NGC 6093 (M80).
----------------------------------------------------
Additional candidate variables
Heinke et al. (2003) identified 19 Chandra X-ray sources: CX1-CX19
in M80.
They classified CX2 and CX6 as quiescent LMXBs
and CX3, CX4, CX5 and CX15 as candidate cataclysmic variables.
They also suggested that CX1 might be the X-ray counterpart of
Nova 1860 and Dieball et al. (2010) concur.
Moni Bidin et al. (2009) identified a candidate
EHB close binary in M80 (their star #16389).
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References
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N., Smirnov, O. 1998, AJ, 116, 2415
Bailey, S. I. 1902, Harv. Ann., 38
Dieball, A., Long, K. S., Knigge, C., Thomson, G. S., Zurek, D. R.
2010, ApJ, 710, 332
Figuera Jaimes, R., Bramich, D. M., Skottfelt, J., Kains, N.,
Jorgensen, U. G., Horne, K., Dominik, M. and 26 coauthors, 2016,
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Heinke, C. O., Grindlay, J. E., Edmonds, P. D., Lloyd, D. A., Murray, S.
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