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Noriyuki Matsunaga, Michael W. Feast, Takahiro Kawadu, Shogo Nishiyama, Takahiro Nagayama, Tetsuya Nagata, Motohide Tamura, Giuseppe Bono, Naoto Kobayashi, Cepheids and other short-period variables near the Galactic Centre, Monthly Notices of the Royal Astronomical Society, Volume 429, Issue 1, 11 February 2013, Pages 385–397, https://doi.org/10.1093/mnras/sts343
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Abstract
We report the result of our near-infrared survey of short-period variable stars (P < 60 d) in a field of view of 20 arcmin × 30 arcmin towards the Galactic Centre (GC). Forty-five variables are discovered and we classify the variables based on their light-curve shapes and other evidence. In addition to 3 classical Cepheids reported previously, we find 16 type II Cepheids, 24 eclipsing binaries, 1 pulsating star with P = 0.265 d (RR Lyr or δ Sct) and 1 Cepheid-like variable whose nature is uncertain. Eclipsing binaries are separated into the foreground objects and those significantly obscured by interstellar extinction. One of the reddened binaries contains an O-type supergiant and its light curve indicates an eccentric orbit. We discuss the nature and distribution of type II Cepheids as well as the distance to the GC based on these Cepheids and other distance indicators. The estimates of R0(GC) we obtained based on photometric data agree with previous results obtained with kinematics of objects around the GC. Furthermore, our result gives support to the reddening law obtained by Nishiyama and collaborators, AKs/E(H-Ks)=1.44, because a different reddening law would result in a rather different distance estimate.
1 INTRODUCTION
The Galactic Centre (GC) region is an important place for many reasons. A supermassive black hole exists in the direction of Sgr A* within a complex region involving both hot and cold gas (e.g. Morris & Serabyn 1996; Genzel, Eisenhauer & Gillessen 2010). This region hosts the highest density of stars in the Galaxy, and furthermore various stellar populations co-exist with different distribution and characteristics (Launhardt, Zylka & Mezger 2002). First, the extended bulge with a scale of a few kiloparsecs has a triaxial or bar-like shape (Nakada et al. 1991; Whitelock & Catchpole 1992; Stanek et al. 1994) and is populated predominantly by old stars (≥10 Gyr; Zoccali et al. 2003; Clarkson et al. 2011). Secondly, the nuclear bulge shows a disc-like distribution with a radius of ∼200 pc, and a significant population of young stars (a few Myr) are found in this region (Serabyn & Morris 1996; Figer et al. 2004; Yusef-Zadeh et al. 2009). Finally, a dense stellar cluster with numerous massive stars exists within a radius of ∼10 pc (its core radius actually is much smaller, ∼0.3 pc) around the central black hole (Genzel et al. 2003). The GC region provides us with a unique opportunity to study not only stellar evolution but also phenomena in central parts of galaxies at close hand (∼8 kpc). For instance, the most populous group of known young and massive stars, such as O-type stars and Wolf–Rayet stars, within the Galaxy exists there (e.g. Mauerhan et al. 2010).
Pulsating variable stars are useful in studies of stellar populations. In particular, Cepheids play important roles in a wide range of astronomy. There are two groups of Cepheids, i.e. classical Cepheids (hereafter CCEPs) and type II Cepheids (T2Cs). Both of them have period–luminosity relation (PLR), but the luminosities at a given period differ by 1.5–2 mag (Sandage & Tammann 2006; Matsunaga, Feast & Soszyński 2011a). CCEPs are pulsating supergiants with periods typically between 3 and 50 d, evolved from intermediate- to high-mass stars (4–10 M⊙). On the other hand, T2Cs have similar periods to CCEPs, but are old and evolved from low-mass stars, ∼1 M⊙. T2Cs are conventionally subdivided into the BL Her and W Vir stars at periods less than 20 d and the RV Tau stars with greater periods. In addition, Soszyński et al. (2008b) identified peculiar W Vir stars which tend to be brighter than the PLR and to often show light curves with eclipsing or ellipsoidal modulation. There remain uncertainties in the properties and the evolution of T2Cs (see the discussion in Matsunaga et al. 2011a).
A serious difficulty in studying the stars towards the GC lies in observing them beyond the severe interstellar extinction. The foreground extinction is not uniform and strong (around 2–3 mag in the K band, 2.2 μm). Thus, infrared (IR) observations are required in order to study stars in the GC region. In fact, long-term IR observations have made it possible to monitor stellar motions around the central black hole (Ghez et al. 2008; Gillessen et al. 2009, and references therein). These and other data were used to search for variable stars in the few parsec (or smaller) region around Sgr A* (Tamura et al. 1996; Ott, Eckart & Genzel 1999; Peeples, Stanek & DePoy 2007; Rafelski et al. 2007). However, no Cepheids were found in these works.
We carried out near-IR observations to investigate stellar variability in the GC region. Our survey covered a much wider area, |$20\,\text{arcmin} \times 30\,\text{arcmin}$|, than the previous monitoring observations. A large number of long-period variables including Miras were found in the survey region (Matsunaga et al. 2009b, hereafter Paper I), and we discovered three CCEPs, the first of this type in the GC region (Matsunaga et al. 2011b, hereafter Paper II). In this paper we describe our data analysis and a catalogue of the short-period variables in the field, and also discuss their nature as well as the distance to the GC.
2 OBSERVATION AND DATA REDUCTION
Observations were conducted using the IRSF 1.4 m telescope and the SIRIUS camera (Nagashima et al. 1999; Nagayama et al. 2003) which collects images in the J(1.25 μm), H(1.63 μm) and Ks(2.14 μm) bands, simultaneously. The observed field composed of 12 fields of view of IRSF/SIRIUS covered |$20\,\text{arcmin} \times 30\,\text{arcmin}$| around the GC (Table 1). Observations at about 90 epochs were made between 2001 and 2008 of which the majority were obtained in 2005 and 2006. We used this data set in Papers I and II, and further observational details are found there.
Field . | RA (J2000) . | Dec. (J2000.0) . | Nobs . | NShort . |
---|---|---|---|---|
1745−2900A | 17:46:10.5 | −28:53:47.8 | 94 | 3 |
1745−2900B | 17:45:40.0 | −28:53:47.8 | 92 | 6 |
1745−2900C | 17:45:09.5 | −28:53:47.8 | 90 | 3 |
1745−2900D | 17:46:10.5 | −29:00:28.0 | 93 | 3 |
1745−2900E | 17:45:40.0 | −29:00:28.0 | 91 | 6a |
1745−2900F | 17:45:09.5 | −29:00:28.0 | 89 | 5a |
1745−2900G | 17:46:10.5 | −29:07:07.8 | 87 | 4 |
1745−2900H | 17:45:40.0 | −29:07:07.8 | 89 | 3 |
1745−2900I | 17:45:09.5 | −29:07:07.8 | 83 | 4 |
1745−2840G | 17:46:10.5 | −28:47:07.9 | 85 | 6 |
1745−2840H | 17:45:40.0 | −28:47:07.9 | 85 | 1 |
1745−2840I | 17:45:09.5 | −28:47:07.9 | 60 | 2 |
Total | 45b |
Field . | RA (J2000) . | Dec. (J2000.0) . | Nobs . | NShort . |
---|---|---|---|---|
1745−2900A | 17:46:10.5 | −28:53:47.8 | 94 | 3 |
1745−2900B | 17:45:40.0 | −28:53:47.8 | 92 | 6 |
1745−2900C | 17:45:09.5 | −28:53:47.8 | 90 | 3 |
1745−2900D | 17:46:10.5 | −29:00:28.0 | 93 | 3 |
1745−2900E | 17:45:40.0 | −29:00:28.0 | 91 | 6a |
1745−2900F | 17:45:09.5 | −29:00:28.0 | 89 | 5a |
1745−2900G | 17:46:10.5 | −29:07:07.8 | 87 | 4 |
1745−2900H | 17:45:40.0 | −29:07:07.8 | 89 | 3 |
1745−2900I | 17:45:09.5 | −29:07:07.8 | 83 | 4 |
1745−2840G | 17:46:10.5 | −28:47:07.9 | 85 | 6 |
1745−2840H | 17:45:40.0 | −28:47:07.9 | 85 | 1 |
1745−2840I | 17:45:09.5 | −28:47:07.9 | 60 | 2 |
Total | 45b |
aOne object, #15 in Table 2, was detected in the overlapping region of both fields.
bWe do not include the duplicate detection in the neighbouring fields.
Field . | RA (J2000) . | Dec. (J2000.0) . | Nobs . | NShort . |
---|---|---|---|---|
1745−2900A | 17:46:10.5 | −28:53:47.8 | 94 | 3 |
1745−2900B | 17:45:40.0 | −28:53:47.8 | 92 | 6 |
1745−2900C | 17:45:09.5 | −28:53:47.8 | 90 | 3 |
1745−2900D | 17:46:10.5 | −29:00:28.0 | 93 | 3 |
1745−2900E | 17:45:40.0 | −29:00:28.0 | 91 | 6a |
1745−2900F | 17:45:09.5 | −29:00:28.0 | 89 | 5a |
1745−2900G | 17:46:10.5 | −29:07:07.8 | 87 | 4 |
1745−2900H | 17:45:40.0 | −29:07:07.8 | 89 | 3 |
1745−2900I | 17:45:09.5 | −29:07:07.8 | 83 | 4 |
1745−2840G | 17:46:10.5 | −28:47:07.9 | 85 | 6 |
1745−2840H | 17:45:40.0 | −28:47:07.9 | 85 | 1 |
1745−2840I | 17:45:09.5 | −28:47:07.9 | 60 | 2 |
Total | 45b |
Field . | RA (J2000) . | Dec. (J2000.0) . | Nobs . | NShort . |
---|---|---|---|---|
1745−2900A | 17:46:10.5 | −28:53:47.8 | 94 | 3 |
1745−2900B | 17:45:40.0 | −28:53:47.8 | 92 | 6 |
1745−2900C | 17:45:09.5 | −28:53:47.8 | 90 | 3 |
1745−2900D | 17:46:10.5 | −29:00:28.0 | 93 | 3 |
1745−2900E | 17:45:40.0 | −29:00:28.0 | 91 | 6a |
1745−2900F | 17:45:09.5 | −29:00:28.0 | 89 | 5a |
1745−2900G | 17:46:10.5 | −29:07:07.8 | 87 | 4 |
1745−2900H | 17:45:40.0 | −29:07:07.8 | 89 | 3 |
1745−2900I | 17:45:09.5 | −29:07:07.8 | 83 | 4 |
1745−2840G | 17:46:10.5 | −28:47:07.9 | 85 | 6 |
1745−2840H | 17:45:40.0 | −28:47:07.9 | 85 | 1 |
1745−2840I | 17:45:09.5 | −28:47:07.9 | 60 | 2 |
Total | 45b |
aOne object, #15 in Table 2, was detected in the overlapping region of both fields.
bWe do not include the duplicate detection in the neighbouring fields.
The basic data analysis was done in the same manner as in Paper I. In short, point-spread-function (PSF) fitting photometry was performed on every image using the iraf/daophot package, and variable stars were searched for by combining the time series sets of JHKs magnitudes. The standard deviations (SDs) were calculated for repeated measurements of individual stars. We then looked for variable stars with SD more than three times larger than the median value of SDs in the corresponding magnitude range. The variability search was done using the three band data sets independently, so that we could find variables even if they are visible only in one of the JHKs bands.
The saturation limits are 9.5, 9.5 and 9.0 mag, and the detection limits are around 16.4, 14.5 and 13.1 mag in J, H and Ks, respectively. The definition of these values is described in Paper I, but the detection limits vary across the survey region depending on the crowdedness. Especially, the central region around Sgr A* is so crowded that the accuracy of our photometric measurements, with the typical seeing of ∼1 arcsec, is rather limited. The detection limit also changes from frame to frame depending on the weather condition. Therefore, the above limiting magnitudes should be considered only as typical values.
3 RESULTS
3.1 Detection of short-period variables
We detected 45 variable stars with period between 0.14 and 52.1 d. The number of the objects found in each field of view is indicated in Table 1. Table 2 lists their IDs, galactic coordinates, mean magnitudes, amplitudes and periods. The mean magnitudes are intensity-scale means of maximum and minimum, and the amplitudes refer to peak-to-valley variations. The JHKs time series data obtained for all the catalogued variables are compiled in one text file and each line includes the ID number, the modified Julian date (MJD) and the JHKs for each measurement. Table 3 shows the first 10 lines as a sample of the full version to be published online. Fig. 1 plots their folded light curves in the ascending order of period. Because the light curves of eclipsing variables are often nearly symmetrical, a fit of the Fourier series (equation 1) tends to yield half the orbital period and this is listed in Table 2 except in the case of #30 whose light curve is significantly asymmetric. The orbital periods are used in Fig. 1.
No. . | ID . | l . | b . | J . | H . | Ks . | ΔJ . | ΔH . | ΔKs . | Mflag . | Period . | Type . |
---|---|---|---|---|---|---|---|---|---|---|---|---|
. | . | (°) . | (°) . | (mag) . | (mag) . | (mag) . | (mag) . | (mag) . | (mag) . | . | (d) . | . |
1 | 17445710−2910057 | −0.2742 | +0.0036 | 15.55 | 14.35 | – | 0.56 | 0.52 | – | 003 | 0.3613 | Ecl |
2 | 17445906−2851235 | −0.0046 | +0.1602 | 15.57 | 14.08 | 12.73 | 1.22 | 1.03 | 0.62 | 777 | 7.46 | Cep(II) |
3 | 17445910−2909440 | −0.2652 | +0.0005 | 13.76 | 12.53 | 11.72 | 0.23 | 0.13 | 0.31 | 000 | 0.265 | RR/DS |
4 | 17450132−2848213 | +0.0428 | +0.1796 | – | 14.46 | 12.87 | – | 0.71 | 0.69 | 300 | 12.544 | Ecl |
5 | 17450204−2857215 | −0.0838 | +0.0990 | 14.58 | 14.06 | – | 0.66 | 0.56 | – | 003 | 0.177 33 | Ecl |
6 | 17450754−2906573 | −0.2097 | −0.0015 | – | 14.13 | 12.51 | – | 0.61 | 0.68 | 300 | 15.097 | Cep(II) |
7 | 17450913−2859417 | −0.1035 | +0.0567 | 16.37 | 13.02 | 11.33 | 0.68 | 0.47 | 0.40 | 000 | 52.224 | Cep(II) |
8 | 17451032−2904526 | −0.1749 | +0.0079 | 14.08 | 13.39 | 12.42 | 0.35 | 0.44 | 0.35 | 077 | 0.219 68 | Ecl |
9 | 17451383−2844443 | +0.1181 | +0.1721 | – | 15.19 | 13.69 | – | 0.53 | 0.50 | 300 | 4.747 | Cep(II) |
10 | 17451719−2857531 | −0.0624 | +0.0474 | – | 14.49 | 12.47 | – | 0.74 | 0.86 | 300 | 24.09 | Cep(II) |
11 | 17451764−2851372 | +0.0275 | +0.1004 | – | 14.91 | 13.30 | – | 0.34 | 0.35 | 300 | 8.2713 | Cep(II) |
12 | 17452092−2858186 | −0.0614 | +0.0321 | 14.30 | 13.53 | – | 0.87 | 0.77 | – | 003 | 0.158 69 | Ecl |
13 | 17452219−2853583 | +0.0027 | +0.0658 | 12.58 | 12.29 | 12.11 | 0.34 | 0.34 | 0.33 | 000 | 1.6094 | Ecl |
14 | 17452573−2909397 | −0.2137 | −0.0815 | – | 14.37 | 12.76 | – | 0.43 | 0.41 | 377 | 1.0984 | Ecl |
15 | 17452600−2900037 | −0.0766 | +0.0010 | 15.69 | 12.93 | 11.36 | 0.90 | 0.92 | 0.96 | 000 | 50.46 | Cep(II) |
16 | 17452837−2858221 | −0.0480 | +0.0084 | 15.02 | 13.94 | – | 0.54 | 0.52 | – | 003 | 1.5838 | Ecl |
17 | 17452987−2854290 | +0.0101 | +0.0375 | 14.97 | 12.18 | 10.67 | 0.29 | 0.26 | 0.27 | 000 | 1.6448 | Ecl |
18 | 17453089−2903105 | −0.1116 | −0.0412 | 16.36 | 12.44 | 10.35 | 0.68 | 0.44 | 0.51 | 000 | 22.76 | Cep(I) |
19 | 17453148−2859531 | −0.0637 | −0.0145 | 10.98 | 10.84 | 10.70 | 0.10 | 0.10 | 0.18 | 000 | 3.6301 | Cep(II) |
20 | 17453227−2902552 | −0.1054 | −0.0433 | 15.42 | 12.00 | 10.17 | 0.60 | 0.46 | 0.57 | 000 | 19.96 | Cep(I) |
21 | 17454075−2852367 | +0.0574 | +0.0198 | – | 14.93 | 13.31 | – | 0.39 | 0.47 | 300 | 0.556 48 | Ecl |
22 | 17454904−2856450 | +0.0142 | −0.0419 | 13.81 | 13.40 | 13.02 | 0.55 | 0.62 | 0.71 | 007 | 0.412 78 | Ecl |
23 | 17455015−2855069 | +0.0396 | −0.0312 | – | 14.25 | 12.53 | – | 0.36 | 0.42 | 377 | 1.628 | Ecl |
24 | 17455150−2903392 | −0.0793 | −0.1094 | 14.18 | 13.72 | 13.58 | 0.40 | 0.42 | 0.54 | 000 | 0.249 46 | Ecl |
25 | 17455257−2900004 | −0.0254 | −0.0811 | 17.05 | 14.03 | 12.19 | 0.89 | 0.57 | 0.58 | 700 | 1.7092 | Ecl |
26 | 17455318−2856206 | +0.0279 | −0.0512 | – | 14.28 | 12.40 | – | 0.84 | 0.85 | 000 | 16.1 | Cep(II) |
27 | 17455325−2904069 | −0.0826 | −0.1189 | – | 14.53 | 12.89 | – | 0.41 | 0.42 | 300 | 1.7316 | Ecl |
28 | 17455413−2845032 | +0.1904 | +0.0437 | – | 14.62 | 12.95 | – | 0.77 | 0.73 | 300 | 15.543 | Cep(II) |
29 | 17455482−2854382 | +0.0553 | −0.0415 | – | 15.29 | 13.58 | – | 0.45 | 0.61 | 377 | 10.26 | Cep(II) |
30 | 17460164−2855155 | +0.0594 | −0.0682 | 13.40 | 10.64 | 9.16 | 0.40 | 0.42 | 0.32 | 000 | 26.792 | Ecl |
31 | 17460200−2852506 | +0.0944 | −0.0484 | – | 12.98 | 11.37 | – | 0.61 | 0.68 | 377 | 40.13 | Cep(II) |
32 | 17460601−2846551 | +0.1864 | −0.0095 | 15.63 | 12.04 | 10.18 | 0.58 | 0.45 | 0.44 | 000 | 23.538 | Cep(I) |
33 | 17460637−2909442 | −0.1377 | −0.2084 | 12.68 | 10.91 | 10.07 | 0.12 | 0.14 | 0.10 | 000 | 18.96 | Cep(II) |
34 | 17461000−2855325 | +0.0712 | −0.0967 | 15.01 | 12.28 | 10.79 | 0.21 | 0.17 | 0.19 | 077 | 2.1932 | Cep(?) |
35 | 17461007−2905173 | −0.0674 | −0.1814 | 16.10 | – | – | 0.73 | – | – | 033 | 0.146 12 | Ecl |
36 | 17461044−2903183 | −0.0385 | −0.1653 | 12.43 | 11.89 | 11.18 | 0.79 | 0.72 | 0.56 | 077 | 0.972 09 | Ecl |
37 | 17461171−2850001 | +0.1533 | −0.0540 | 16.08 | 13.45 | 11.91 | 0.74 | 0.56 | 0.60 | 000 | 0.942 55 | Ecl |
38 | 17461252−2848526 | +0.1709 | −0.0468 | – | 14.24 | 12.24 | – | 0.59 | 0.54 | 300 | 1.6486 | Ecl |
39 | 17461356−2848351 | +0.1770 | −0.0475 | – | – | 12.75 | – | – | 0.86 | 337 | 31.17 | Cep(II) |
40 | 17461357−2859023 | +0.0282 | −0.1381 | – | 14.91 | 13.03 | – | 1.00 | 0.84 | 300 | 19.014 | Cep(II) |
41 | 17461447−2849002 | +0.1728 | −0.0539 | 13.80 | 12.57 | 10.98 | 0.73 | 0.53 | 0.27 | 077 | 0.141 61 | Ecl |
42 | 17461626−2850125 | +0.1590 | −0.0700 | 15.63 | 12.97 | 11.39 | 0.77 | 0.70 | 0.72 | 000 | 1.662 84 | Ecl |
43 | 17462426−2908288 | −0.0860 | −0.2531 | – | 14.06 | 12.49 | – | 0.60 | 0.69 | 300 | 13.52 | Ecl |
44 | 17462642−2857079 | +0.0797 | −0.1616 | 14.33 | 13.53 | 13.23 | 0.30 | 0.35 | 0.37 | 000 | 0.415 46 | Ecl |
45 | 17462846−2908562 | −0.0846 | −0.2702 | 17.17 | 14.03 | 12.46 | 1.34 | 0.99 | 1.10 | 000 | 24.406 | Cep(II) |
No. . | ID . | l . | b . | J . | H . | Ks . | ΔJ . | ΔH . | ΔKs . | Mflag . | Period . | Type . |
---|---|---|---|---|---|---|---|---|---|---|---|---|
. | . | (°) . | (°) . | (mag) . | (mag) . | (mag) . | (mag) . | (mag) . | (mag) . | . | (d) . | . |
1 | 17445710−2910057 | −0.2742 | +0.0036 | 15.55 | 14.35 | – | 0.56 | 0.52 | – | 003 | 0.3613 | Ecl |
2 | 17445906−2851235 | −0.0046 | +0.1602 | 15.57 | 14.08 | 12.73 | 1.22 | 1.03 | 0.62 | 777 | 7.46 | Cep(II) |
3 | 17445910−2909440 | −0.2652 | +0.0005 | 13.76 | 12.53 | 11.72 | 0.23 | 0.13 | 0.31 | 000 | 0.265 | RR/DS |
4 | 17450132−2848213 | +0.0428 | +0.1796 | – | 14.46 | 12.87 | – | 0.71 | 0.69 | 300 | 12.544 | Ecl |
5 | 17450204−2857215 | −0.0838 | +0.0990 | 14.58 | 14.06 | – | 0.66 | 0.56 | – | 003 | 0.177 33 | Ecl |
6 | 17450754−2906573 | −0.2097 | −0.0015 | – | 14.13 | 12.51 | – | 0.61 | 0.68 | 300 | 15.097 | Cep(II) |
7 | 17450913−2859417 | −0.1035 | +0.0567 | 16.37 | 13.02 | 11.33 | 0.68 | 0.47 | 0.40 | 000 | 52.224 | Cep(II) |
8 | 17451032−2904526 | −0.1749 | +0.0079 | 14.08 | 13.39 | 12.42 | 0.35 | 0.44 | 0.35 | 077 | 0.219 68 | Ecl |
9 | 17451383−2844443 | +0.1181 | +0.1721 | – | 15.19 | 13.69 | – | 0.53 | 0.50 | 300 | 4.747 | Cep(II) |
10 | 17451719−2857531 | −0.0624 | +0.0474 | – | 14.49 | 12.47 | – | 0.74 | 0.86 | 300 | 24.09 | Cep(II) |
11 | 17451764−2851372 | +0.0275 | +0.1004 | – | 14.91 | 13.30 | – | 0.34 | 0.35 | 300 | 8.2713 | Cep(II) |
12 | 17452092−2858186 | −0.0614 | +0.0321 | 14.30 | 13.53 | – | 0.87 | 0.77 | – | 003 | 0.158 69 | Ecl |
13 | 17452219−2853583 | +0.0027 | +0.0658 | 12.58 | 12.29 | 12.11 | 0.34 | 0.34 | 0.33 | 000 | 1.6094 | Ecl |
14 | 17452573−2909397 | −0.2137 | −0.0815 | – | 14.37 | 12.76 | – | 0.43 | 0.41 | 377 | 1.0984 | Ecl |
15 | 17452600−2900037 | −0.0766 | +0.0010 | 15.69 | 12.93 | 11.36 | 0.90 | 0.92 | 0.96 | 000 | 50.46 | Cep(II) |
16 | 17452837−2858221 | −0.0480 | +0.0084 | 15.02 | 13.94 | – | 0.54 | 0.52 | – | 003 | 1.5838 | Ecl |
17 | 17452987−2854290 | +0.0101 | +0.0375 | 14.97 | 12.18 | 10.67 | 0.29 | 0.26 | 0.27 | 000 | 1.6448 | Ecl |
18 | 17453089−2903105 | −0.1116 | −0.0412 | 16.36 | 12.44 | 10.35 | 0.68 | 0.44 | 0.51 | 000 | 22.76 | Cep(I) |
19 | 17453148−2859531 | −0.0637 | −0.0145 | 10.98 | 10.84 | 10.70 | 0.10 | 0.10 | 0.18 | 000 | 3.6301 | Cep(II) |
20 | 17453227−2902552 | −0.1054 | −0.0433 | 15.42 | 12.00 | 10.17 | 0.60 | 0.46 | 0.57 | 000 | 19.96 | Cep(I) |
21 | 17454075−2852367 | +0.0574 | +0.0198 | – | 14.93 | 13.31 | – | 0.39 | 0.47 | 300 | 0.556 48 | Ecl |
22 | 17454904−2856450 | +0.0142 | −0.0419 | 13.81 | 13.40 | 13.02 | 0.55 | 0.62 | 0.71 | 007 | 0.412 78 | Ecl |
23 | 17455015−2855069 | +0.0396 | −0.0312 | – | 14.25 | 12.53 | – | 0.36 | 0.42 | 377 | 1.628 | Ecl |
24 | 17455150−2903392 | −0.0793 | −0.1094 | 14.18 | 13.72 | 13.58 | 0.40 | 0.42 | 0.54 | 000 | 0.249 46 | Ecl |
25 | 17455257−2900004 | −0.0254 | −0.0811 | 17.05 | 14.03 | 12.19 | 0.89 | 0.57 | 0.58 | 700 | 1.7092 | Ecl |
26 | 17455318−2856206 | +0.0279 | −0.0512 | – | 14.28 | 12.40 | – | 0.84 | 0.85 | 000 | 16.1 | Cep(II) |
27 | 17455325−2904069 | −0.0826 | −0.1189 | – | 14.53 | 12.89 | – | 0.41 | 0.42 | 300 | 1.7316 | Ecl |
28 | 17455413−2845032 | +0.1904 | +0.0437 | – | 14.62 | 12.95 | – | 0.77 | 0.73 | 300 | 15.543 | Cep(II) |
29 | 17455482−2854382 | +0.0553 | −0.0415 | – | 15.29 | 13.58 | – | 0.45 | 0.61 | 377 | 10.26 | Cep(II) |
30 | 17460164−2855155 | +0.0594 | −0.0682 | 13.40 | 10.64 | 9.16 | 0.40 | 0.42 | 0.32 | 000 | 26.792 | Ecl |
31 | 17460200−2852506 | +0.0944 | −0.0484 | – | 12.98 | 11.37 | – | 0.61 | 0.68 | 377 | 40.13 | Cep(II) |
32 | 17460601−2846551 | +0.1864 | −0.0095 | 15.63 | 12.04 | 10.18 | 0.58 | 0.45 | 0.44 | 000 | 23.538 | Cep(I) |
33 | 17460637−2909442 | −0.1377 | −0.2084 | 12.68 | 10.91 | 10.07 | 0.12 | 0.14 | 0.10 | 000 | 18.96 | Cep(II) |
34 | 17461000−2855325 | +0.0712 | −0.0967 | 15.01 | 12.28 | 10.79 | 0.21 | 0.17 | 0.19 | 077 | 2.1932 | Cep(?) |
35 | 17461007−2905173 | −0.0674 | −0.1814 | 16.10 | – | – | 0.73 | – | – | 033 | 0.146 12 | Ecl |
36 | 17461044−2903183 | −0.0385 | −0.1653 | 12.43 | 11.89 | 11.18 | 0.79 | 0.72 | 0.56 | 077 | 0.972 09 | Ecl |
37 | 17461171−2850001 | +0.1533 | −0.0540 | 16.08 | 13.45 | 11.91 | 0.74 | 0.56 | 0.60 | 000 | 0.942 55 | Ecl |
38 | 17461252−2848526 | +0.1709 | −0.0468 | – | 14.24 | 12.24 | – | 0.59 | 0.54 | 300 | 1.6486 | Ecl |
39 | 17461356−2848351 | +0.1770 | −0.0475 | – | – | 12.75 | – | – | 0.86 | 337 | 31.17 | Cep(II) |
40 | 17461357−2859023 | +0.0282 | −0.1381 | – | 14.91 | 13.03 | – | 1.00 | 0.84 | 300 | 19.014 | Cep(II) |
41 | 17461447−2849002 | +0.1728 | −0.0539 | 13.80 | 12.57 | 10.98 | 0.73 | 0.53 | 0.27 | 077 | 0.141 61 | Ecl |
42 | 17461626−2850125 | +0.1590 | −0.0700 | 15.63 | 12.97 | 11.39 | 0.77 | 0.70 | 0.72 | 000 | 1.662 84 | Ecl |
43 | 17462426−2908288 | −0.0860 | −0.2531 | – | 14.06 | 12.49 | – | 0.60 | 0.69 | 300 | 13.52 | Ecl |
44 | 17462642−2857079 | +0.0797 | −0.1616 | 14.33 | 13.53 | 13.23 | 0.30 | 0.35 | 0.37 | 000 | 0.415 46 | Ecl |
45 | 17462846−2908562 | −0.0846 | −0.2702 | 17.17 | 14.03 | 12.46 | 1.34 | 0.99 | 1.10 | 000 | 24.406 | Cep(II) |
No. . | ID . | l . | b . | J . | H . | Ks . | ΔJ . | ΔH . | ΔKs . | Mflag . | Period . | Type . |
---|---|---|---|---|---|---|---|---|---|---|---|---|
. | . | (°) . | (°) . | (mag) . | (mag) . | (mag) . | (mag) . | (mag) . | (mag) . | . | (d) . | . |
1 | 17445710−2910057 | −0.2742 | +0.0036 | 15.55 | 14.35 | – | 0.56 | 0.52 | – | 003 | 0.3613 | Ecl |
2 | 17445906−2851235 | −0.0046 | +0.1602 | 15.57 | 14.08 | 12.73 | 1.22 | 1.03 | 0.62 | 777 | 7.46 | Cep(II) |
3 | 17445910−2909440 | −0.2652 | +0.0005 | 13.76 | 12.53 | 11.72 | 0.23 | 0.13 | 0.31 | 000 | 0.265 | RR/DS |
4 | 17450132−2848213 | +0.0428 | +0.1796 | – | 14.46 | 12.87 | – | 0.71 | 0.69 | 300 | 12.544 | Ecl |
5 | 17450204−2857215 | −0.0838 | +0.0990 | 14.58 | 14.06 | – | 0.66 | 0.56 | – | 003 | 0.177 33 | Ecl |
6 | 17450754−2906573 | −0.2097 | −0.0015 | – | 14.13 | 12.51 | – | 0.61 | 0.68 | 300 | 15.097 | Cep(II) |
7 | 17450913−2859417 | −0.1035 | +0.0567 | 16.37 | 13.02 | 11.33 | 0.68 | 0.47 | 0.40 | 000 | 52.224 | Cep(II) |
8 | 17451032−2904526 | −0.1749 | +0.0079 | 14.08 | 13.39 | 12.42 | 0.35 | 0.44 | 0.35 | 077 | 0.219 68 | Ecl |
9 | 17451383−2844443 | +0.1181 | +0.1721 | – | 15.19 | 13.69 | – | 0.53 | 0.50 | 300 | 4.747 | Cep(II) |
10 | 17451719−2857531 | −0.0624 | +0.0474 | – | 14.49 | 12.47 | – | 0.74 | 0.86 | 300 | 24.09 | Cep(II) |
11 | 17451764−2851372 | +0.0275 | +0.1004 | – | 14.91 | 13.30 | – | 0.34 | 0.35 | 300 | 8.2713 | Cep(II) |
12 | 17452092−2858186 | −0.0614 | +0.0321 | 14.30 | 13.53 | – | 0.87 | 0.77 | – | 003 | 0.158 69 | Ecl |
13 | 17452219−2853583 | +0.0027 | +0.0658 | 12.58 | 12.29 | 12.11 | 0.34 | 0.34 | 0.33 | 000 | 1.6094 | Ecl |
14 | 17452573−2909397 | −0.2137 | −0.0815 | – | 14.37 | 12.76 | – | 0.43 | 0.41 | 377 | 1.0984 | Ecl |
15 | 17452600−2900037 | −0.0766 | +0.0010 | 15.69 | 12.93 | 11.36 | 0.90 | 0.92 | 0.96 | 000 | 50.46 | Cep(II) |
16 | 17452837−2858221 | −0.0480 | +0.0084 | 15.02 | 13.94 | – | 0.54 | 0.52 | – | 003 | 1.5838 | Ecl |
17 | 17452987−2854290 | +0.0101 | +0.0375 | 14.97 | 12.18 | 10.67 | 0.29 | 0.26 | 0.27 | 000 | 1.6448 | Ecl |
18 | 17453089−2903105 | −0.1116 | −0.0412 | 16.36 | 12.44 | 10.35 | 0.68 | 0.44 | 0.51 | 000 | 22.76 | Cep(I) |
19 | 17453148−2859531 | −0.0637 | −0.0145 | 10.98 | 10.84 | 10.70 | 0.10 | 0.10 | 0.18 | 000 | 3.6301 | Cep(II) |
20 | 17453227−2902552 | −0.1054 | −0.0433 | 15.42 | 12.00 | 10.17 | 0.60 | 0.46 | 0.57 | 000 | 19.96 | Cep(I) |
21 | 17454075−2852367 | +0.0574 | +0.0198 | – | 14.93 | 13.31 | – | 0.39 | 0.47 | 300 | 0.556 48 | Ecl |
22 | 17454904−2856450 | +0.0142 | −0.0419 | 13.81 | 13.40 | 13.02 | 0.55 | 0.62 | 0.71 | 007 | 0.412 78 | Ecl |
23 | 17455015−2855069 | +0.0396 | −0.0312 | – | 14.25 | 12.53 | – | 0.36 | 0.42 | 377 | 1.628 | Ecl |
24 | 17455150−2903392 | −0.0793 | −0.1094 | 14.18 | 13.72 | 13.58 | 0.40 | 0.42 | 0.54 | 000 | 0.249 46 | Ecl |
25 | 17455257−2900004 | −0.0254 | −0.0811 | 17.05 | 14.03 | 12.19 | 0.89 | 0.57 | 0.58 | 700 | 1.7092 | Ecl |
26 | 17455318−2856206 | +0.0279 | −0.0512 | – | 14.28 | 12.40 | – | 0.84 | 0.85 | 000 | 16.1 | Cep(II) |
27 | 17455325−2904069 | −0.0826 | −0.1189 | – | 14.53 | 12.89 | – | 0.41 | 0.42 | 300 | 1.7316 | Ecl |
28 | 17455413−2845032 | +0.1904 | +0.0437 | – | 14.62 | 12.95 | – | 0.77 | 0.73 | 300 | 15.543 | Cep(II) |
29 | 17455482−2854382 | +0.0553 | −0.0415 | – | 15.29 | 13.58 | – | 0.45 | 0.61 | 377 | 10.26 | Cep(II) |
30 | 17460164−2855155 | +0.0594 | −0.0682 | 13.40 | 10.64 | 9.16 | 0.40 | 0.42 | 0.32 | 000 | 26.792 | Ecl |
31 | 17460200−2852506 | +0.0944 | −0.0484 | – | 12.98 | 11.37 | – | 0.61 | 0.68 | 377 | 40.13 | Cep(II) |
32 | 17460601−2846551 | +0.1864 | −0.0095 | 15.63 | 12.04 | 10.18 | 0.58 | 0.45 | 0.44 | 000 | 23.538 | Cep(I) |
33 | 17460637−2909442 | −0.1377 | −0.2084 | 12.68 | 10.91 | 10.07 | 0.12 | 0.14 | 0.10 | 000 | 18.96 | Cep(II) |
34 | 17461000−2855325 | +0.0712 | −0.0967 | 15.01 | 12.28 | 10.79 | 0.21 | 0.17 | 0.19 | 077 | 2.1932 | Cep(?) |
35 | 17461007−2905173 | −0.0674 | −0.1814 | 16.10 | – | – | 0.73 | – | – | 033 | 0.146 12 | Ecl |
36 | 17461044−2903183 | −0.0385 | −0.1653 | 12.43 | 11.89 | 11.18 | 0.79 | 0.72 | 0.56 | 077 | 0.972 09 | Ecl |
37 | 17461171−2850001 | +0.1533 | −0.0540 | 16.08 | 13.45 | 11.91 | 0.74 | 0.56 | 0.60 | 000 | 0.942 55 | Ecl |
38 | 17461252−2848526 | +0.1709 | −0.0468 | – | 14.24 | 12.24 | – | 0.59 | 0.54 | 300 | 1.6486 | Ecl |
39 | 17461356−2848351 | +0.1770 | −0.0475 | – | – | 12.75 | – | – | 0.86 | 337 | 31.17 | Cep(II) |
40 | 17461357−2859023 | +0.0282 | −0.1381 | – | 14.91 | 13.03 | – | 1.00 | 0.84 | 300 | 19.014 | Cep(II) |
41 | 17461447−2849002 | +0.1728 | −0.0539 | 13.80 | 12.57 | 10.98 | 0.73 | 0.53 | 0.27 | 077 | 0.141 61 | Ecl |
42 | 17461626−2850125 | +0.1590 | −0.0700 | 15.63 | 12.97 | 11.39 | 0.77 | 0.70 | 0.72 | 000 | 1.662 84 | Ecl |
43 | 17462426−2908288 | −0.0860 | −0.2531 | – | 14.06 | 12.49 | – | 0.60 | 0.69 | 300 | 13.52 | Ecl |
44 | 17462642−2857079 | +0.0797 | −0.1616 | 14.33 | 13.53 | 13.23 | 0.30 | 0.35 | 0.37 | 000 | 0.415 46 | Ecl |
45 | 17462846−2908562 | −0.0846 | −0.2702 | 17.17 | 14.03 | 12.46 | 1.34 | 0.99 | 1.10 | 000 | 24.406 | Cep(II) |
No. . | ID . | l . | b . | J . | H . | Ks . | ΔJ . | ΔH . | ΔKs . | Mflag . | Period . | Type . |
---|---|---|---|---|---|---|---|---|---|---|---|---|
. | . | (°) . | (°) . | (mag) . | (mag) . | (mag) . | (mag) . | (mag) . | (mag) . | . | (d) . | . |
1 | 17445710−2910057 | −0.2742 | +0.0036 | 15.55 | 14.35 | – | 0.56 | 0.52 | – | 003 | 0.3613 | Ecl |
2 | 17445906−2851235 | −0.0046 | +0.1602 | 15.57 | 14.08 | 12.73 | 1.22 | 1.03 | 0.62 | 777 | 7.46 | Cep(II) |
3 | 17445910−2909440 | −0.2652 | +0.0005 | 13.76 | 12.53 | 11.72 | 0.23 | 0.13 | 0.31 | 000 | 0.265 | RR/DS |
4 | 17450132−2848213 | +0.0428 | +0.1796 | – | 14.46 | 12.87 | – | 0.71 | 0.69 | 300 | 12.544 | Ecl |
5 | 17450204−2857215 | −0.0838 | +0.0990 | 14.58 | 14.06 | – | 0.66 | 0.56 | – | 003 | 0.177 33 | Ecl |
6 | 17450754−2906573 | −0.2097 | −0.0015 | – | 14.13 | 12.51 | – | 0.61 | 0.68 | 300 | 15.097 | Cep(II) |
7 | 17450913−2859417 | −0.1035 | +0.0567 | 16.37 | 13.02 | 11.33 | 0.68 | 0.47 | 0.40 | 000 | 52.224 | Cep(II) |
8 | 17451032−2904526 | −0.1749 | +0.0079 | 14.08 | 13.39 | 12.42 | 0.35 | 0.44 | 0.35 | 077 | 0.219 68 | Ecl |
9 | 17451383−2844443 | +0.1181 | +0.1721 | – | 15.19 | 13.69 | – | 0.53 | 0.50 | 300 | 4.747 | Cep(II) |
10 | 17451719−2857531 | −0.0624 | +0.0474 | – | 14.49 | 12.47 | – | 0.74 | 0.86 | 300 | 24.09 | Cep(II) |
11 | 17451764−2851372 | +0.0275 | +0.1004 | – | 14.91 | 13.30 | – | 0.34 | 0.35 | 300 | 8.2713 | Cep(II) |
12 | 17452092−2858186 | −0.0614 | +0.0321 | 14.30 | 13.53 | – | 0.87 | 0.77 | – | 003 | 0.158 69 | Ecl |
13 | 17452219−2853583 | +0.0027 | +0.0658 | 12.58 | 12.29 | 12.11 | 0.34 | 0.34 | 0.33 | 000 | 1.6094 | Ecl |
14 | 17452573−2909397 | −0.2137 | −0.0815 | – | 14.37 | 12.76 | – | 0.43 | 0.41 | 377 | 1.0984 | Ecl |
15 | 17452600−2900037 | −0.0766 | +0.0010 | 15.69 | 12.93 | 11.36 | 0.90 | 0.92 | 0.96 | 000 | 50.46 | Cep(II) |
16 | 17452837−2858221 | −0.0480 | +0.0084 | 15.02 | 13.94 | – | 0.54 | 0.52 | – | 003 | 1.5838 | Ecl |
17 | 17452987−2854290 | +0.0101 | +0.0375 | 14.97 | 12.18 | 10.67 | 0.29 | 0.26 | 0.27 | 000 | 1.6448 | Ecl |
18 | 17453089−2903105 | −0.1116 | −0.0412 | 16.36 | 12.44 | 10.35 | 0.68 | 0.44 | 0.51 | 000 | 22.76 | Cep(I) |
19 | 17453148−2859531 | −0.0637 | −0.0145 | 10.98 | 10.84 | 10.70 | 0.10 | 0.10 | 0.18 | 000 | 3.6301 | Cep(II) |
20 | 17453227−2902552 | −0.1054 | −0.0433 | 15.42 | 12.00 | 10.17 | 0.60 | 0.46 | 0.57 | 000 | 19.96 | Cep(I) |
21 | 17454075−2852367 | +0.0574 | +0.0198 | – | 14.93 | 13.31 | – | 0.39 | 0.47 | 300 | 0.556 48 | Ecl |
22 | 17454904−2856450 | +0.0142 | −0.0419 | 13.81 | 13.40 | 13.02 | 0.55 | 0.62 | 0.71 | 007 | 0.412 78 | Ecl |
23 | 17455015−2855069 | +0.0396 | −0.0312 | – | 14.25 | 12.53 | – | 0.36 | 0.42 | 377 | 1.628 | Ecl |
24 | 17455150−2903392 | −0.0793 | −0.1094 | 14.18 | 13.72 | 13.58 | 0.40 | 0.42 | 0.54 | 000 | 0.249 46 | Ecl |
25 | 17455257−2900004 | −0.0254 | −0.0811 | 17.05 | 14.03 | 12.19 | 0.89 | 0.57 | 0.58 | 700 | 1.7092 | Ecl |
26 | 17455318−2856206 | +0.0279 | −0.0512 | – | 14.28 | 12.40 | – | 0.84 | 0.85 | 000 | 16.1 | Cep(II) |
27 | 17455325−2904069 | −0.0826 | −0.1189 | – | 14.53 | 12.89 | – | 0.41 | 0.42 | 300 | 1.7316 | Ecl |
28 | 17455413−2845032 | +0.1904 | +0.0437 | – | 14.62 | 12.95 | – | 0.77 | 0.73 | 300 | 15.543 | Cep(II) |
29 | 17455482−2854382 | +0.0553 | −0.0415 | – | 15.29 | 13.58 | – | 0.45 | 0.61 | 377 | 10.26 | Cep(II) |
30 | 17460164−2855155 | +0.0594 | −0.0682 | 13.40 | 10.64 | 9.16 | 0.40 | 0.42 | 0.32 | 000 | 26.792 | Ecl |
31 | 17460200−2852506 | +0.0944 | −0.0484 | – | 12.98 | 11.37 | – | 0.61 | 0.68 | 377 | 40.13 | Cep(II) |
32 | 17460601−2846551 | +0.1864 | −0.0095 | 15.63 | 12.04 | 10.18 | 0.58 | 0.45 | 0.44 | 000 | 23.538 | Cep(I) |
33 | 17460637−2909442 | −0.1377 | −0.2084 | 12.68 | 10.91 | 10.07 | 0.12 | 0.14 | 0.10 | 000 | 18.96 | Cep(II) |
34 | 17461000−2855325 | +0.0712 | −0.0967 | 15.01 | 12.28 | 10.79 | 0.21 | 0.17 | 0.19 | 077 | 2.1932 | Cep(?) |
35 | 17461007−2905173 | −0.0674 | −0.1814 | 16.10 | – | – | 0.73 | – | – | 033 | 0.146 12 | Ecl |
36 | 17461044−2903183 | −0.0385 | −0.1653 | 12.43 | 11.89 | 11.18 | 0.79 | 0.72 | 0.56 | 077 | 0.972 09 | Ecl |
37 | 17461171−2850001 | +0.1533 | −0.0540 | 16.08 | 13.45 | 11.91 | 0.74 | 0.56 | 0.60 | 000 | 0.942 55 | Ecl |
38 | 17461252−2848526 | +0.1709 | −0.0468 | – | 14.24 | 12.24 | – | 0.59 | 0.54 | 300 | 1.6486 | Ecl |
39 | 17461356−2848351 | +0.1770 | −0.0475 | – | – | 12.75 | – | – | 0.86 | 337 | 31.17 | Cep(II) |
40 | 17461357−2859023 | +0.0282 | −0.1381 | – | 14.91 | 13.03 | – | 1.00 | 0.84 | 300 | 19.014 | Cep(II) |
41 | 17461447−2849002 | +0.1728 | −0.0539 | 13.80 | 12.57 | 10.98 | 0.73 | 0.53 | 0.27 | 077 | 0.141 61 | Ecl |
42 | 17461626−2850125 | +0.1590 | −0.0700 | 15.63 | 12.97 | 11.39 | 0.77 | 0.70 | 0.72 | 000 | 1.662 84 | Ecl |
43 | 17462426−2908288 | −0.0860 | −0.2531 | – | 14.06 | 12.49 | – | 0.60 | 0.69 | 300 | 13.52 | Ecl |
44 | 17462642−2857079 | +0.0797 | −0.1616 | 14.33 | 13.53 | 13.23 | 0.30 | 0.35 | 0.37 | 000 | 0.415 46 | Ecl |
45 | 17462846−2908562 | −0.0846 | −0.2702 | 17.17 | 14.03 | 12.46 | 1.34 | 0.99 | 1.10 | 000 | 24.406 | Cep(II) |
No. . | MJD . | J . | H . | Ks . |
---|---|---|---|---|
1 | 523 43.1514 | 15.60 | 14.49 | 99.99 |
1 | 534 82.0694 | 15.28 | 14.22 | 99.99 |
1 | 535 37.1167 | 15.57 | 99.99 | 99.99 |
1 | 535 40.8287 | 15.69 | 14.56 | 99.99 |
1 | 535 45.8959 | 15.67 | 14.49 | 99.99 |
1 | 535 45.9758 | 15.32 | 14.24 | 99.99 |
1 | 535 48.8325 | 15.48 | 99.99 | 99.99 |
1 | 535 48.9662 | 15.32 | 14.20 | 99.99 |
1 | 535 49.8964 | 15.53 | 14.39 | 99.99 |
1 | 535 50.0148 | 15.32 | 14.17 | 99.99 |
No. . | MJD . | J . | H . | Ks . |
---|---|---|---|---|
1 | 523 43.1514 | 15.60 | 14.49 | 99.99 |
1 | 534 82.0694 | 15.28 | 14.22 | 99.99 |
1 | 535 37.1167 | 15.57 | 99.99 | 99.99 |
1 | 535 40.8287 | 15.69 | 14.56 | 99.99 |
1 | 535 45.8959 | 15.67 | 14.49 | 99.99 |
1 | 535 45.9758 | 15.32 | 14.24 | 99.99 |
1 | 535 48.8325 | 15.48 | 99.99 | 99.99 |
1 | 535 48.9662 | 15.32 | 14.20 | 99.99 |
1 | 535 49.8964 | 15.53 | 14.39 | 99.99 |
1 | 535 50.0148 | 15.32 | 14.17 | 99.99 |
No. . | MJD . | J . | H . | Ks . |
---|---|---|---|---|
1 | 523 43.1514 | 15.60 | 14.49 | 99.99 |
1 | 534 82.0694 | 15.28 | 14.22 | 99.99 |
1 | 535 37.1167 | 15.57 | 99.99 | 99.99 |
1 | 535 40.8287 | 15.69 | 14.56 | 99.99 |
1 | 535 45.8959 | 15.67 | 14.49 | 99.99 |
1 | 535 45.9758 | 15.32 | 14.24 | 99.99 |
1 | 535 48.8325 | 15.48 | 99.99 | 99.99 |
1 | 535 48.9662 | 15.32 | 14.20 | 99.99 |
1 | 535 49.8964 | 15.53 | 14.39 | 99.99 |
1 | 535 50.0148 | 15.32 | 14.17 | 99.99 |
No. . | MJD . | J . | H . | Ks . |
---|---|---|---|---|
1 | 523 43.1514 | 15.60 | 14.49 | 99.99 |
1 | 534 82.0694 | 15.28 | 14.22 | 99.99 |
1 | 535 37.1167 | 15.57 | 99.99 | 99.99 |
1 | 535 40.8287 | 15.69 | 14.56 | 99.99 |
1 | 535 45.8959 | 15.67 | 14.49 | 99.99 |
1 | 535 45.9758 | 15.32 | 14.24 | 99.99 |
1 | 535 48.8325 | 15.48 | 99.99 | 99.99 |
1 | 535 48.9662 | 15.32 | 14.20 | 99.99 |
1 | 535 49.8964 | 15.53 | 14.39 | 99.99 |
1 | 535 50.0148 | 15.32 | 14.17 | 99.99 |
We did not always detect the variables in all of the JHKs bands. Table 2 includes |$\text{M}$|flag which we also used in Paper I to show the reasons of non-detection or the qualities of the listed magnitudes. In this work, only the flag numbers 0, 3 and 7 are relevant. The flags 0 and 3, respectively, indicate that a mean magnitude was obtained properly and that some measurements were affected by the detection limit leading to an uncertain mean magnitude. The flag 7 is newly defined to indicate that the photometry of the object is affected by the crowding. None of our objects was too bright, and none was located too close to the edge of the detector. The light curves in Fig. 1 indicate that the entire variations from minima to maxima were sampled well enough to estimate mean magnitudes except for the faintest cases.
As we see in Fig. 1, our sample includes different types of variables. In order to determine the variable types, shapes of the light curves are discussed in Section 3.2. For CCEPs and T2Cs, as briefly discussed in Paper II, we also consider their absolute magnitudes and the expected distances (Section 3.3). In Section 3.4, we summarize the classification and compare some features among variable types.
3.2 Shapes of the light curves
No. . | log P . | J band . | H band . | Ks band . | |||||||||
---|---|---|---|---|---|---|---|---|---|---|---|---|---|
. | . | R21 . | ϕ21 . | R31 . | ϕ31 . | R21 . | ϕ21 . | R31 . | ϕ31 . | R21 . | ϕ21 . | R31 . | ϕ31 . |
1 | −0.442a | 0.176 | 1.983 | 0.030 | 1.550 | 0.174 | 2.004 | 0.075 | 0.064 | – | – | – | – |
2 | 0.873 | 0.246 | 2.923 | 0.157 | 0.212 | 0.336 | 2.834 | 0.120 | 0.204 | 0.364 | 2.907 | 0.192 | 0.021 |
3 | −0.577 | 0.312 | 1.181 | 0.181 | 0.690 | 0.309 | 1.304 | 0.242 | 0.862 | 0.526 | 1.484 | 0.144 | 1.518 |
4 | 1.098a | – | – | – | – | 0.301 | 2.055 | 0.072 | 0.739 | 0.268 | 2.067 | 0.074 | 0.728 |
5 | −0.751a | 8.190 | 1.913 | 1.076 | 1.961 | 3.818 | 1.918 | 0.715 | 1.951 | – | – | – | – |
6 | 1.179 | – | – | – | – | 0.038 | 1.403 | 0.051 | 0.774 | 0.044 | 1.002 | 0.113 | 0.812 |
7 | 1.718 | 0.283 | 2.615 | 0.096 | 0.098 | 0.184 | 2.696 | 0.036 | 1.956 | 0.147 | 2.665 | 0.005 | 1.757 |
8 | −0.658a | 0.087 | 2.016 | 0.064 | 0.140 | 0.132 | 1.936 | 0.091 | 0.848 | 0.384 | 1.998 | 0.247 | 1.576 |
9 | 0.676 | – | – | – | – | 0.259 | 1.986 | 0.075 | 0.184 | 0.116 | 2.101 | 0.051 | 0.189 |
10 | 1.382 | – | – | – | – | 0.160 | 1.869 | 0.029 | 0.038 | 0.101 | 1.822 | 0.029 | 1.258 |
11 | 0.918 | – | – | – | – | 0.227 | 2.188 | 0.088 | 0.245 | 0.183 | 2.378 | 0.062 | 0.046 |
12 | −0.799a | 5.306 | 2.023 | 0.526 | 1.955 | 4.916 | 1.983 | 0.615 | 1.894 | – | – | – | – |
13 | 0.207a | 0.683 | 1.912 | 0.568 | 1.877 | 0.733 | 1.923 | 0.585 | 1.888 | 0.689 | 1.949 | 0.621 | 1.932 |
14 | 0.041a | – | – | – | – | 0.493 | 2.043 | 0.308 | 1.833 | 0.702 | 1.908 | 0.237 | 1.707 |
15 | 1.703 | 0.176 | 1.585 | 0.064 | 0.655 | 0.359 | 1.595 | 0.088 | 0.934 | 0.316 | 1.536 | 0.105 | 0.829 |
16 | 0.200a | 0.946 | 2.063 | 0.934 | 0.072 | 0.856 | 2.036 | 0.819 | 0.043 | – | – | – | – |
17 | 0.216a | 0.332 | 2.013 | 0.077 | 1.987 | 0.232 | 1.973 | 0.058 | 1.737 | 0.240 | 2.094 | 0.068 | 0.830 |
18 | 1.357 | 0.236 | 1.729 | 0.240 | 1.059 | 0.189 | 1.896 | 0.138 | 1.740 | 0.239 | 1.922 | 0.182 | 1.710 |
19 | 0.560 | 0.118 | 1.337 | 0.068 | 1.331 | 0.137 | 1.243 | 0.010 | 0.926 | 0.541 | 1.030 | 0.087 | 1.152 |
20 | 1.300 | 0.311 | 1.679 | 0.135 | 1.260 | 0.200 | 1.849 | 0.107 | 1.500 | 0.349 | 1.753 | 0.066 | 1.599 |
21 | −0.255a | – | – | – | – | 0.127 | 2.101 | 0.090 | 0.048 | 0.233 | 1.865 | 0.129 | 1.737 |
22 | −0.384a | 0.692 | 2.030 | 0.423 | 0.069 | 0.696 | 1.979 | 0.430 | 0.006 | 0.497 | 2.117 | 0.854 | 0.329 |
23 | 0.212a | – | – | – | – | 1.853 | 2.542 | 0.189 | 0.838 | 1.713 | 2.694 | 0.114 | 1.046 |
24 | −0.603a | 0.161 | 2.003 | 0.025 | 1.545 | 0.189 | 2.013 | 0.015 | 0.797 | 0.253 | 2.023 | 0.051 | 0.319 |
25 | 0.233a | 0.661 | 2.035 | 0.310 | 0.169 | 0.655 | 2.029 | 0.370 | 0.114 | 0.619 | 2.004 | 0.328 | 0.035 |
26 | 1.207 | – | – | – | – | 0.098 | 1.798 | 0.049 | 0.332 | 0.041 | 1.301 | 0.035 | 0.810 |
27 | 0.238a | – | – | – | – | 0.586 | 2.064 | 0.513 | 0.210 | 0.805 | 2.118 | 0.620 | 0.233 |
28 | 1.192 | – | – | – | – | 0.015 | 1.944 | 0.056 | 0.673 | 0.067 | 1.129 | 0.040 | 0.874 |
29 | 1.011 | – | – | – | – | 0.108 | 2.278 | 0.041 | 0.511 | 0.093 | 1.753 | 0.185 | 0.738 |
30 | 1.428 | 1.969 | 1.022 | 0.856 | 1.179 | 1.818 | 1.016 | 0.734 | 1.160 | 1.656 | 2.980 | 0.566 | 1.157 |
31 | 1.603 | – | – | – | – | 0.151 | 1.749 | 0.049 | 0.952 | 0.118 | 1.719 | 0.084 | 0.843 |
32 | 1.372 | 0.299 | 1.671 | 0.189 | 1.422 | 0.253 | 1.879 | 0.129 | 1.698 | 0.210 | 1.910 | 0.101 | 1.735 |
33 | 1.278 | 0.036 | 2.932 | 0.055 | 1.459 | 0.034 | 1.853 | 0.121 | 1.310 | 0.085 | 1.345 | 0.109 | 1.236 |
34 | 0.341 | 0.124 | 1.771 | 0.180 | 1.735 | 0.086 | 1.757 | 0.029 | 0.409 | 0.049 | 1.722 | 0.068 | 1.395 |
35 | −0.835a | 0.318 | 2.076 | 0.148 | 0.093 | – | – | – | – | – | – | – | – |
36 | −0.012a | 0.458 | 1.978 | 0.265 | 1.985 | 0.461 | 1.985 | 0.252 | 0.003 | 0.414 | 1.935 | 0.234 | 1.949 |
37 | −0.026a | 0.155 | 2.014 | 0.100 | 0.186 | 0.166 | 1.991 | 0.094 | 1.960 | 0.128 | 1.902 | 0.135 | 1.912 |
38 | 0.217a | – | – | – | – | 0.113 | 1.789 | 0.121 | 1.735 | 0.114 | 1.684 | 0.075 | 1.489 |
39 | 1.494 | – | – | – | – | – | – | – | – | 0.099 | 1.414 | 0.194 | 0.897 |
40 | 1.279 | – | – | – | – | 0.142 | 1.902 | 0.064 | 0.275 | 0.087 | 1.662 | 0.051 | 0.793 |
41 | −0.849a | 0.328 | 1.962 | 0.112 | 0.039 | 0.357 | 1.877 | 0.108 | 1.829 | 0.324 | 1.747 | 0.058 | 1.061 |
42 | 0.221a | 0.324 | 1.999 | 0.152 | 1.978 | 0.362 | 1.970 | 0.175 | 0.008 | 0.348 | 1.946 | 0.158 | 0.002 |
43 | 1.131a | – | – | – | – | 0.382 | 1.966 | 0.110 | 1.954 | 0.318 | 1.955 | 0.068 | 1.866 |
44 | −0.381a | 0.585 | 1.922 | 0.255 | 1.888 | 0.779 | 2.031 | 0.327 | 0.072 | 0.548 | 2.022 | 0.340 | 1.827 |
45 | 1.387 | 0.197 | 1.920 | 0.122 | 1.312 | 0.157 | 1.785 | 0.093 | 1.502 | 0.171 | 1.752 | 0.108 | 1.618 |
No. . | log P . | J band . | H band . | Ks band . | |||||||||
---|---|---|---|---|---|---|---|---|---|---|---|---|---|
. | . | R21 . | ϕ21 . | R31 . | ϕ31 . | R21 . | ϕ21 . | R31 . | ϕ31 . | R21 . | ϕ21 . | R31 . | ϕ31 . |
1 | −0.442a | 0.176 | 1.983 | 0.030 | 1.550 | 0.174 | 2.004 | 0.075 | 0.064 | – | – | – | – |
2 | 0.873 | 0.246 | 2.923 | 0.157 | 0.212 | 0.336 | 2.834 | 0.120 | 0.204 | 0.364 | 2.907 | 0.192 | 0.021 |
3 | −0.577 | 0.312 | 1.181 | 0.181 | 0.690 | 0.309 | 1.304 | 0.242 | 0.862 | 0.526 | 1.484 | 0.144 | 1.518 |
4 | 1.098a | – | – | – | – | 0.301 | 2.055 | 0.072 | 0.739 | 0.268 | 2.067 | 0.074 | 0.728 |
5 | −0.751a | 8.190 | 1.913 | 1.076 | 1.961 | 3.818 | 1.918 | 0.715 | 1.951 | – | – | – | – |
6 | 1.179 | – | – | – | – | 0.038 | 1.403 | 0.051 | 0.774 | 0.044 | 1.002 | 0.113 | 0.812 |
7 | 1.718 | 0.283 | 2.615 | 0.096 | 0.098 | 0.184 | 2.696 | 0.036 | 1.956 | 0.147 | 2.665 | 0.005 | 1.757 |
8 | −0.658a | 0.087 | 2.016 | 0.064 | 0.140 | 0.132 | 1.936 | 0.091 | 0.848 | 0.384 | 1.998 | 0.247 | 1.576 |
9 | 0.676 | – | – | – | – | 0.259 | 1.986 | 0.075 | 0.184 | 0.116 | 2.101 | 0.051 | 0.189 |
10 | 1.382 | – | – | – | – | 0.160 | 1.869 | 0.029 | 0.038 | 0.101 | 1.822 | 0.029 | 1.258 |
11 | 0.918 | – | – | – | – | 0.227 | 2.188 | 0.088 | 0.245 | 0.183 | 2.378 | 0.062 | 0.046 |
12 | −0.799a | 5.306 | 2.023 | 0.526 | 1.955 | 4.916 | 1.983 | 0.615 | 1.894 | – | – | – | – |
13 | 0.207a | 0.683 | 1.912 | 0.568 | 1.877 | 0.733 | 1.923 | 0.585 | 1.888 | 0.689 | 1.949 | 0.621 | 1.932 |
14 | 0.041a | – | – | – | – | 0.493 | 2.043 | 0.308 | 1.833 | 0.702 | 1.908 | 0.237 | 1.707 |
15 | 1.703 | 0.176 | 1.585 | 0.064 | 0.655 | 0.359 | 1.595 | 0.088 | 0.934 | 0.316 | 1.536 | 0.105 | 0.829 |
16 | 0.200a | 0.946 | 2.063 | 0.934 | 0.072 | 0.856 | 2.036 | 0.819 | 0.043 | – | – | – | – |
17 | 0.216a | 0.332 | 2.013 | 0.077 | 1.987 | 0.232 | 1.973 | 0.058 | 1.737 | 0.240 | 2.094 | 0.068 | 0.830 |
18 | 1.357 | 0.236 | 1.729 | 0.240 | 1.059 | 0.189 | 1.896 | 0.138 | 1.740 | 0.239 | 1.922 | 0.182 | 1.710 |
19 | 0.560 | 0.118 | 1.337 | 0.068 | 1.331 | 0.137 | 1.243 | 0.010 | 0.926 | 0.541 | 1.030 | 0.087 | 1.152 |
20 | 1.300 | 0.311 | 1.679 | 0.135 | 1.260 | 0.200 | 1.849 | 0.107 | 1.500 | 0.349 | 1.753 | 0.066 | 1.599 |
21 | −0.255a | – | – | – | – | 0.127 | 2.101 | 0.090 | 0.048 | 0.233 | 1.865 | 0.129 | 1.737 |
22 | −0.384a | 0.692 | 2.030 | 0.423 | 0.069 | 0.696 | 1.979 | 0.430 | 0.006 | 0.497 | 2.117 | 0.854 | 0.329 |
23 | 0.212a | – | – | – | – | 1.853 | 2.542 | 0.189 | 0.838 | 1.713 | 2.694 | 0.114 | 1.046 |
24 | −0.603a | 0.161 | 2.003 | 0.025 | 1.545 | 0.189 | 2.013 | 0.015 | 0.797 | 0.253 | 2.023 | 0.051 | 0.319 |
25 | 0.233a | 0.661 | 2.035 | 0.310 | 0.169 | 0.655 | 2.029 | 0.370 | 0.114 | 0.619 | 2.004 | 0.328 | 0.035 |
26 | 1.207 | – | – | – | – | 0.098 | 1.798 | 0.049 | 0.332 | 0.041 | 1.301 | 0.035 | 0.810 |
27 | 0.238a | – | – | – | – | 0.586 | 2.064 | 0.513 | 0.210 | 0.805 | 2.118 | 0.620 | 0.233 |
28 | 1.192 | – | – | – | – | 0.015 | 1.944 | 0.056 | 0.673 | 0.067 | 1.129 | 0.040 | 0.874 |
29 | 1.011 | – | – | – | – | 0.108 | 2.278 | 0.041 | 0.511 | 0.093 | 1.753 | 0.185 | 0.738 |
30 | 1.428 | 1.969 | 1.022 | 0.856 | 1.179 | 1.818 | 1.016 | 0.734 | 1.160 | 1.656 | 2.980 | 0.566 | 1.157 |
31 | 1.603 | – | – | – | – | 0.151 | 1.749 | 0.049 | 0.952 | 0.118 | 1.719 | 0.084 | 0.843 |
32 | 1.372 | 0.299 | 1.671 | 0.189 | 1.422 | 0.253 | 1.879 | 0.129 | 1.698 | 0.210 | 1.910 | 0.101 | 1.735 |
33 | 1.278 | 0.036 | 2.932 | 0.055 | 1.459 | 0.034 | 1.853 | 0.121 | 1.310 | 0.085 | 1.345 | 0.109 | 1.236 |
34 | 0.341 | 0.124 | 1.771 | 0.180 | 1.735 | 0.086 | 1.757 | 0.029 | 0.409 | 0.049 | 1.722 | 0.068 | 1.395 |
35 | −0.835a | 0.318 | 2.076 | 0.148 | 0.093 | – | – | – | – | – | – | – | – |
36 | −0.012a | 0.458 | 1.978 | 0.265 | 1.985 | 0.461 | 1.985 | 0.252 | 0.003 | 0.414 | 1.935 | 0.234 | 1.949 |
37 | −0.026a | 0.155 | 2.014 | 0.100 | 0.186 | 0.166 | 1.991 | 0.094 | 1.960 | 0.128 | 1.902 | 0.135 | 1.912 |
38 | 0.217a | – | – | – | – | 0.113 | 1.789 | 0.121 | 1.735 | 0.114 | 1.684 | 0.075 | 1.489 |
39 | 1.494 | – | – | – | – | – | – | – | – | 0.099 | 1.414 | 0.194 | 0.897 |
40 | 1.279 | – | – | – | – | 0.142 | 1.902 | 0.064 | 0.275 | 0.087 | 1.662 | 0.051 | 0.793 |
41 | −0.849a | 0.328 | 1.962 | 0.112 | 0.039 | 0.357 | 1.877 | 0.108 | 1.829 | 0.324 | 1.747 | 0.058 | 1.061 |
42 | 0.221a | 0.324 | 1.999 | 0.152 | 1.978 | 0.362 | 1.970 | 0.175 | 0.008 | 0.348 | 1.946 | 0.158 | 0.002 |
43 | 1.131a | – | – | – | – | 0.382 | 1.966 | 0.110 | 1.954 | 0.318 | 1.955 | 0.068 | 1.866 |
44 | −0.381a | 0.585 | 1.922 | 0.255 | 1.888 | 0.779 | 2.031 | 0.327 | 0.072 | 0.548 | 2.022 | 0.340 | 1.827 |
45 | 1.387 | 0.197 | 1.920 | 0.122 | 1.312 | 0.157 | 1.785 | 0.093 | 1.502 | 0.171 | 1.752 | 0.108 | 1.618 |
aHalf the orbital periods are given for all the eclipsing binaries except #30.
No. . | log P . | J band . | H band . | Ks band . | |||||||||
---|---|---|---|---|---|---|---|---|---|---|---|---|---|
. | . | R21 . | ϕ21 . | R31 . | ϕ31 . | R21 . | ϕ21 . | R31 . | ϕ31 . | R21 . | ϕ21 . | R31 . | ϕ31 . |
1 | −0.442a | 0.176 | 1.983 | 0.030 | 1.550 | 0.174 | 2.004 | 0.075 | 0.064 | – | – | – | – |
2 | 0.873 | 0.246 | 2.923 | 0.157 | 0.212 | 0.336 | 2.834 | 0.120 | 0.204 | 0.364 | 2.907 | 0.192 | 0.021 |
3 | −0.577 | 0.312 | 1.181 | 0.181 | 0.690 | 0.309 | 1.304 | 0.242 | 0.862 | 0.526 | 1.484 | 0.144 | 1.518 |
4 | 1.098a | – | – | – | – | 0.301 | 2.055 | 0.072 | 0.739 | 0.268 | 2.067 | 0.074 | 0.728 |
5 | −0.751a | 8.190 | 1.913 | 1.076 | 1.961 | 3.818 | 1.918 | 0.715 | 1.951 | – | – | – | – |
6 | 1.179 | – | – | – | – | 0.038 | 1.403 | 0.051 | 0.774 | 0.044 | 1.002 | 0.113 | 0.812 |
7 | 1.718 | 0.283 | 2.615 | 0.096 | 0.098 | 0.184 | 2.696 | 0.036 | 1.956 | 0.147 | 2.665 | 0.005 | 1.757 |
8 | −0.658a | 0.087 | 2.016 | 0.064 | 0.140 | 0.132 | 1.936 | 0.091 | 0.848 | 0.384 | 1.998 | 0.247 | 1.576 |
9 | 0.676 | – | – | – | – | 0.259 | 1.986 | 0.075 | 0.184 | 0.116 | 2.101 | 0.051 | 0.189 |
10 | 1.382 | – | – | – | – | 0.160 | 1.869 | 0.029 | 0.038 | 0.101 | 1.822 | 0.029 | 1.258 |
11 | 0.918 | – | – | – | – | 0.227 | 2.188 | 0.088 | 0.245 | 0.183 | 2.378 | 0.062 | 0.046 |
12 | −0.799a | 5.306 | 2.023 | 0.526 | 1.955 | 4.916 | 1.983 | 0.615 | 1.894 | – | – | – | – |
13 | 0.207a | 0.683 | 1.912 | 0.568 | 1.877 | 0.733 | 1.923 | 0.585 | 1.888 | 0.689 | 1.949 | 0.621 | 1.932 |
14 | 0.041a | – | – | – | – | 0.493 | 2.043 | 0.308 | 1.833 | 0.702 | 1.908 | 0.237 | 1.707 |
15 | 1.703 | 0.176 | 1.585 | 0.064 | 0.655 | 0.359 | 1.595 | 0.088 | 0.934 | 0.316 | 1.536 | 0.105 | 0.829 |
16 | 0.200a | 0.946 | 2.063 | 0.934 | 0.072 | 0.856 | 2.036 | 0.819 | 0.043 | – | – | – | – |
17 | 0.216a | 0.332 | 2.013 | 0.077 | 1.987 | 0.232 | 1.973 | 0.058 | 1.737 | 0.240 | 2.094 | 0.068 | 0.830 |
18 | 1.357 | 0.236 | 1.729 | 0.240 | 1.059 | 0.189 | 1.896 | 0.138 | 1.740 | 0.239 | 1.922 | 0.182 | 1.710 |
19 | 0.560 | 0.118 | 1.337 | 0.068 | 1.331 | 0.137 | 1.243 | 0.010 | 0.926 | 0.541 | 1.030 | 0.087 | 1.152 |
20 | 1.300 | 0.311 | 1.679 | 0.135 | 1.260 | 0.200 | 1.849 | 0.107 | 1.500 | 0.349 | 1.753 | 0.066 | 1.599 |
21 | −0.255a | – | – | – | – | 0.127 | 2.101 | 0.090 | 0.048 | 0.233 | 1.865 | 0.129 | 1.737 |
22 | −0.384a | 0.692 | 2.030 | 0.423 | 0.069 | 0.696 | 1.979 | 0.430 | 0.006 | 0.497 | 2.117 | 0.854 | 0.329 |
23 | 0.212a | – | – | – | – | 1.853 | 2.542 | 0.189 | 0.838 | 1.713 | 2.694 | 0.114 | 1.046 |
24 | −0.603a | 0.161 | 2.003 | 0.025 | 1.545 | 0.189 | 2.013 | 0.015 | 0.797 | 0.253 | 2.023 | 0.051 | 0.319 |
25 | 0.233a | 0.661 | 2.035 | 0.310 | 0.169 | 0.655 | 2.029 | 0.370 | 0.114 | 0.619 | 2.004 | 0.328 | 0.035 |
26 | 1.207 | – | – | – | – | 0.098 | 1.798 | 0.049 | 0.332 | 0.041 | 1.301 | 0.035 | 0.810 |
27 | 0.238a | – | – | – | – | 0.586 | 2.064 | 0.513 | 0.210 | 0.805 | 2.118 | 0.620 | 0.233 |
28 | 1.192 | – | – | – | – | 0.015 | 1.944 | 0.056 | 0.673 | 0.067 | 1.129 | 0.040 | 0.874 |
29 | 1.011 | – | – | – | – | 0.108 | 2.278 | 0.041 | 0.511 | 0.093 | 1.753 | 0.185 | 0.738 |
30 | 1.428 | 1.969 | 1.022 | 0.856 | 1.179 | 1.818 | 1.016 | 0.734 | 1.160 | 1.656 | 2.980 | 0.566 | 1.157 |
31 | 1.603 | – | – | – | – | 0.151 | 1.749 | 0.049 | 0.952 | 0.118 | 1.719 | 0.084 | 0.843 |
32 | 1.372 | 0.299 | 1.671 | 0.189 | 1.422 | 0.253 | 1.879 | 0.129 | 1.698 | 0.210 | 1.910 | 0.101 | 1.735 |
33 | 1.278 | 0.036 | 2.932 | 0.055 | 1.459 | 0.034 | 1.853 | 0.121 | 1.310 | 0.085 | 1.345 | 0.109 | 1.236 |
34 | 0.341 | 0.124 | 1.771 | 0.180 | 1.735 | 0.086 | 1.757 | 0.029 | 0.409 | 0.049 | 1.722 | 0.068 | 1.395 |
35 | −0.835a | 0.318 | 2.076 | 0.148 | 0.093 | – | – | – | – | – | – | – | – |
36 | −0.012a | 0.458 | 1.978 | 0.265 | 1.985 | 0.461 | 1.985 | 0.252 | 0.003 | 0.414 | 1.935 | 0.234 | 1.949 |
37 | −0.026a | 0.155 | 2.014 | 0.100 | 0.186 | 0.166 | 1.991 | 0.094 | 1.960 | 0.128 | 1.902 | 0.135 | 1.912 |
38 | 0.217a | – | – | – | – | 0.113 | 1.789 | 0.121 | 1.735 | 0.114 | 1.684 | 0.075 | 1.489 |
39 | 1.494 | – | – | – | – | – | – | – | – | 0.099 | 1.414 | 0.194 | 0.897 |
40 | 1.279 | – | – | – | – | 0.142 | 1.902 | 0.064 | 0.275 | 0.087 | 1.662 | 0.051 | 0.793 |
41 | −0.849a | 0.328 | 1.962 | 0.112 | 0.039 | 0.357 | 1.877 | 0.108 | 1.829 | 0.324 | 1.747 | 0.058 | 1.061 |
42 | 0.221a | 0.324 | 1.999 | 0.152 | 1.978 | 0.362 | 1.970 | 0.175 | 0.008 | 0.348 | 1.946 | 0.158 | 0.002 |
43 | 1.131a | – | – | – | – | 0.382 | 1.966 | 0.110 | 1.954 | 0.318 | 1.955 | 0.068 | 1.866 |
44 | −0.381a | 0.585 | 1.922 | 0.255 | 1.888 | 0.779 | 2.031 | 0.327 | 0.072 | 0.548 | 2.022 | 0.340 | 1.827 |
45 | 1.387 | 0.197 | 1.920 | 0.122 | 1.312 | 0.157 | 1.785 | 0.093 | 1.502 | 0.171 | 1.752 | 0.108 | 1.618 |
No. . | log P . | J band . | H band . | Ks band . | |||||||||
---|---|---|---|---|---|---|---|---|---|---|---|---|---|
. | . | R21 . | ϕ21 . | R31 . | ϕ31 . | R21 . | ϕ21 . | R31 . | ϕ31 . | R21 . | ϕ21 . | R31 . | ϕ31 . |
1 | −0.442a | 0.176 | 1.983 | 0.030 | 1.550 | 0.174 | 2.004 | 0.075 | 0.064 | – | – | – | – |
2 | 0.873 | 0.246 | 2.923 | 0.157 | 0.212 | 0.336 | 2.834 | 0.120 | 0.204 | 0.364 | 2.907 | 0.192 | 0.021 |
3 | −0.577 | 0.312 | 1.181 | 0.181 | 0.690 | 0.309 | 1.304 | 0.242 | 0.862 | 0.526 | 1.484 | 0.144 | 1.518 |
4 | 1.098a | – | – | – | – | 0.301 | 2.055 | 0.072 | 0.739 | 0.268 | 2.067 | 0.074 | 0.728 |
5 | −0.751a | 8.190 | 1.913 | 1.076 | 1.961 | 3.818 | 1.918 | 0.715 | 1.951 | – | – | – | – |
6 | 1.179 | – | – | – | – | 0.038 | 1.403 | 0.051 | 0.774 | 0.044 | 1.002 | 0.113 | 0.812 |
7 | 1.718 | 0.283 | 2.615 | 0.096 | 0.098 | 0.184 | 2.696 | 0.036 | 1.956 | 0.147 | 2.665 | 0.005 | 1.757 |
8 | −0.658a | 0.087 | 2.016 | 0.064 | 0.140 | 0.132 | 1.936 | 0.091 | 0.848 | 0.384 | 1.998 | 0.247 | 1.576 |
9 | 0.676 | – | – | – | – | 0.259 | 1.986 | 0.075 | 0.184 | 0.116 | 2.101 | 0.051 | 0.189 |
10 | 1.382 | – | – | – | – | 0.160 | 1.869 | 0.029 | 0.038 | 0.101 | 1.822 | 0.029 | 1.258 |
11 | 0.918 | – | – | – | – | 0.227 | 2.188 | 0.088 | 0.245 | 0.183 | 2.378 | 0.062 | 0.046 |
12 | −0.799a | 5.306 | 2.023 | 0.526 | 1.955 | 4.916 | 1.983 | 0.615 | 1.894 | – | – | – | – |
13 | 0.207a | 0.683 | 1.912 | 0.568 | 1.877 | 0.733 | 1.923 | 0.585 | 1.888 | 0.689 | 1.949 | 0.621 | 1.932 |
14 | 0.041a | – | – | – | – | 0.493 | 2.043 | 0.308 | 1.833 | 0.702 | 1.908 | 0.237 | 1.707 |
15 | 1.703 | 0.176 | 1.585 | 0.064 | 0.655 | 0.359 | 1.595 | 0.088 | 0.934 | 0.316 | 1.536 | 0.105 | 0.829 |
16 | 0.200a | 0.946 | 2.063 | 0.934 | 0.072 | 0.856 | 2.036 | 0.819 | 0.043 | – | – | – | – |
17 | 0.216a | 0.332 | 2.013 | 0.077 | 1.987 | 0.232 | 1.973 | 0.058 | 1.737 | 0.240 | 2.094 | 0.068 | 0.830 |
18 | 1.357 | 0.236 | 1.729 | 0.240 | 1.059 | 0.189 | 1.896 | 0.138 | 1.740 | 0.239 | 1.922 | 0.182 | 1.710 |
19 | 0.560 | 0.118 | 1.337 | 0.068 | 1.331 | 0.137 | 1.243 | 0.010 | 0.926 | 0.541 | 1.030 | 0.087 | 1.152 |
20 | 1.300 | 0.311 | 1.679 | 0.135 | 1.260 | 0.200 | 1.849 | 0.107 | 1.500 | 0.349 | 1.753 | 0.066 | 1.599 |
21 | −0.255a | – | – | – | – | 0.127 | 2.101 | 0.090 | 0.048 | 0.233 | 1.865 | 0.129 | 1.737 |
22 | −0.384a | 0.692 | 2.030 | 0.423 | 0.069 | 0.696 | 1.979 | 0.430 | 0.006 | 0.497 | 2.117 | 0.854 | 0.329 |
23 | 0.212a | – | – | – | – | 1.853 | 2.542 | 0.189 | 0.838 | 1.713 | 2.694 | 0.114 | 1.046 |
24 | −0.603a | 0.161 | 2.003 | 0.025 | 1.545 | 0.189 | 2.013 | 0.015 | 0.797 | 0.253 | 2.023 | 0.051 | 0.319 |
25 | 0.233a | 0.661 | 2.035 | 0.310 | 0.169 | 0.655 | 2.029 | 0.370 | 0.114 | 0.619 | 2.004 | 0.328 | 0.035 |
26 | 1.207 | – | – | – | – | 0.098 | 1.798 | 0.049 | 0.332 | 0.041 | 1.301 | 0.035 | 0.810 |
27 | 0.238a | – | – | – | – | 0.586 | 2.064 | 0.513 | 0.210 | 0.805 | 2.118 | 0.620 | 0.233 |
28 | 1.192 | – | – | – | – | 0.015 | 1.944 | 0.056 | 0.673 | 0.067 | 1.129 | 0.040 | 0.874 |
29 | 1.011 | – | – | – | – | 0.108 | 2.278 | 0.041 | 0.511 | 0.093 | 1.753 | 0.185 | 0.738 |
30 | 1.428 | 1.969 | 1.022 | 0.856 | 1.179 | 1.818 | 1.016 | 0.734 | 1.160 | 1.656 | 2.980 | 0.566 | 1.157 |
31 | 1.603 | – | – | – | – | 0.151 | 1.749 | 0.049 | 0.952 | 0.118 | 1.719 | 0.084 | 0.843 |
32 | 1.372 | 0.299 | 1.671 | 0.189 | 1.422 | 0.253 | 1.879 | 0.129 | 1.698 | 0.210 | 1.910 | 0.101 | 1.735 |
33 | 1.278 | 0.036 | 2.932 | 0.055 | 1.459 | 0.034 | 1.853 | 0.121 | 1.310 | 0.085 | 1.345 | 0.109 | 1.236 |
34 | 0.341 | 0.124 | 1.771 | 0.180 | 1.735 | 0.086 | 1.757 | 0.029 | 0.409 | 0.049 | 1.722 | 0.068 | 1.395 |
35 | −0.835a | 0.318 | 2.076 | 0.148 | 0.093 | – | – | – | – | – | – | – | – |
36 | −0.012a | 0.458 | 1.978 | 0.265 | 1.985 | 0.461 | 1.985 | 0.252 | 0.003 | 0.414 | 1.935 | 0.234 | 1.949 |
37 | −0.026a | 0.155 | 2.014 | 0.100 | 0.186 | 0.166 | 1.991 | 0.094 | 1.960 | 0.128 | 1.902 | 0.135 | 1.912 |
38 | 0.217a | – | – | – | – | 0.113 | 1.789 | 0.121 | 1.735 | 0.114 | 1.684 | 0.075 | 1.489 |
39 | 1.494 | – | – | – | – | – | – | – | – | 0.099 | 1.414 | 0.194 | 0.897 |
40 | 1.279 | – | – | – | – | 0.142 | 1.902 | 0.064 | 0.275 | 0.087 | 1.662 | 0.051 | 0.793 |
41 | −0.849a | 0.328 | 1.962 | 0.112 | 0.039 | 0.357 | 1.877 | 0.108 | 1.829 | 0.324 | 1.747 | 0.058 | 1.061 |
42 | 0.221a | 0.324 | 1.999 | 0.152 | 1.978 | 0.362 | 1.970 | 0.175 | 0.008 | 0.348 | 1.946 | 0.158 | 0.002 |
43 | 1.131a | – | – | – | – | 0.382 | 1.966 | 0.110 | 1.954 | 0.318 | 1.955 | 0.068 | 1.866 |
44 | −0.381a | 0.585 | 1.922 | 0.255 | 1.888 | 0.779 | 2.031 | 0.327 | 0.072 | 0.548 | 2.022 | 0.340 | 1.827 |
45 | 1.387 | 0.197 | 1.920 | 0.122 | 1.312 | 0.157 | 1.785 | 0.093 | 1.502 | 0.171 | 1.752 | 0.108 | 1.618 |
aHalf the orbital periods are given for all the eclipsing binaries except #30.
We also consider the above Fourier parameters for the variables in the Large Magellanic Cloud (LMC), found in the Optical Gravitational Lensing Experiment (OGLE-III), to compare with our objects. In Fig. 2, different types of the LMC variables are plotted in different colours: CCEPs (Soszyński et al. 2008a), T2Cs (Soszyński et al. 2008b), RR Lyr stars (Soszyński et al. 2009) and δ Sct stars (Poleski et al. 2010). Among the δ Sct reported by Poleski et al. (2010), single-mode stars without the uncertainty flag are used. Because they included only R21 and ϕ21, we calculated R31 and ϕ31 using their photometric data.
The OGLE-III light curves were taken in the I band. The available light curves are rather limited in JHKs, but the result in Laney & Stobie (1993) suggests that, at least, J-band light curves are similar to the I-band ones for CCEPs. We plot the parameters for J-band light curves whenever possible for our objects. Those for the H band are used in other cases, but for the object with neither of J and H light curves the Ks-band parameters are considered. The second column of Table 5 indicates the variability types judged by the light-curve shapes.
No. . | LC . | |$A_{K_{\mathrm{s}}}$| . | D . | Type . |
---|---|---|---|---|
. | shape . | (mag) . | (kpc) . | . |
1 | Ecl | – | – | Ecl |
2 | I/II: | 1.3 | 23.9 (I), 9.0 (II) | Cep(II) |
3 | RR/DS | – | – | RR/DSa |
4 | Ecl | – | – | Ecl |
5 | Ecl | – | – | Ecl |
6 | I/II: | 2.1 | 22.2 (I), 6.9 (II) | Cep(II) |
7 | II | 2.2 | 26.3 (I), 6.7 (II) | Cep(II) |
8 | Ecl | – | – | Ecl |
9 | II | 1.9 | 19.1 (I), 7.7 (II) | Cep(II) |
10 | II | 2.6 | 23.2 (I), 6.5 (II) | Cep(II) |
11 | II | 2.1 | 21.6 (I), 7.7 (II) | Cep(II) |
12 | Ecl | – | – | Ecl |
13 | Ecl | – | – | Ecl |
14 | Ecl | – | – | Ecl |
15 | II | 1.9 | 31.3 (I), 8.0 (II) | Cep(II) |
16 | Ecl | – | – | Ecl |
17 | Ecl | – | – | Ecl |
18 | I | 2.7 | 7.7 (I), 2.3 (II) | Cep(I) |
19 | II: | 0.0 | 9.9 (I), 4.3 (II) | Cep(II) |
20 | I | 2.3 | 7.8 (I), 2.4 (II) | Cep(I) |
21 | Ecl | – | – | Ecl |
22 | Ecl | – | – | Ecl |
23 | Ecl | – | – | Ecl |
24 | Ecl: | – | – | Ecl |
25 | Ecl | – | – | Ecl |
26 | I/II: | 2.4 | 18.7 (I), 5.7 (II) | Cep(II) |
27 | Ecl | – | – | Ecl |
28 | II | 2.2 | 26.9 (I), 8.3 (II) | Cep(II) |
29 | I/II: | 2.3 | 26.6 (I), 9.0 (II) | Cep(II) |
30 | Ecl | – | – | Ecl |
31 | II | 2.1 | 25.4 (I), 6.4 (II) | Cep(II) |
32 | I | 2.4 | 8.3 (I), 2.5 (II) | Cep(I) |
33 | II | 1.1 | 13.0 (I), 4.1 (II) | Cep(II) |
34 | Cep: | 1.9 | 3.0 (I), 1.4 (II) | Cep(?)a |
35 | Ecl | – | – | Ecl |
36 | Ecl | – | – | Ecl |
37 | Ecl | – | – | Ecl |
38 | Ecl | – | – | Ecl |
39 | II | – | – | Cep(II) |
40 | II | 2.4 | 28.0 (I), 8.3 (II) | Cep(II) |
41 | Ecl | – | – | Ecl |
42 | Ecl | – | – | Ecl |
43 | Ecl | – | – | Ecl |
44 | Ecl | – | – | Ecl |
45 | II | 2.1 | 28.6 (I), 8.5 (II) | Cep(II) |
No. . | LC . | |$A_{K_{\mathrm{s}}}$| . | D . | Type . |
---|---|---|---|---|
. | shape . | (mag) . | (kpc) . | . |
1 | Ecl | – | – | Ecl |
2 | I/II: | 1.3 | 23.9 (I), 9.0 (II) | Cep(II) |
3 | RR/DS | – | – | RR/DSa |
4 | Ecl | – | – | Ecl |
5 | Ecl | – | – | Ecl |
6 | I/II: | 2.1 | 22.2 (I), 6.9 (II) | Cep(II) |
7 | II | 2.2 | 26.3 (I), 6.7 (II) | Cep(II) |
8 | Ecl | – | – | Ecl |
9 | II | 1.9 | 19.1 (I), 7.7 (II) | Cep(II) |
10 | II | 2.6 | 23.2 (I), 6.5 (II) | Cep(II) |
11 | II | 2.1 | 21.6 (I), 7.7 (II) | Cep(II) |
12 | Ecl | – | – | Ecl |
13 | Ecl | – | – | Ecl |
14 | Ecl | – | – | Ecl |
15 | II | 1.9 | 31.3 (I), 8.0 (II) | Cep(II) |
16 | Ecl | – | – | Ecl |
17 | Ecl | – | – | Ecl |
18 | I | 2.7 | 7.7 (I), 2.3 (II) | Cep(I) |
19 | II: | 0.0 | 9.9 (I), 4.3 (II) | Cep(II) |
20 | I | 2.3 | 7.8 (I), 2.4 (II) | Cep(I) |
21 | Ecl | – | – | Ecl |
22 | Ecl | – | – | Ecl |
23 | Ecl | – | – | Ecl |
24 | Ecl: | – | – | Ecl |
25 | Ecl | – | – | Ecl |
26 | I/II: | 2.4 | 18.7 (I), 5.7 (II) | Cep(II) |
27 | Ecl | – | – | Ecl |
28 | II | 2.2 | 26.9 (I), 8.3 (II) | Cep(II) |
29 | I/II: | 2.3 | 26.6 (I), 9.0 (II) | Cep(II) |
30 | Ecl | – | – | Ecl |
31 | II | 2.1 | 25.4 (I), 6.4 (II) | Cep(II) |
32 | I | 2.4 | 8.3 (I), 2.5 (II) | Cep(I) |
33 | II | 1.1 | 13.0 (I), 4.1 (II) | Cep(II) |
34 | Cep: | 1.9 | 3.0 (I), 1.4 (II) | Cep(?)a |
35 | Ecl | – | – | Ecl |
36 | Ecl | – | – | Ecl |
37 | Ecl | – | – | Ecl |
38 | Ecl | – | – | Ecl |
39 | II | – | – | Cep(II) |
40 | II | 2.4 | 28.0 (I), 8.3 (II) | Cep(II) |
41 | Ecl | – | – | Ecl |
42 | Ecl | – | – | Ecl |
43 | Ecl | – | – | Ecl |
44 | Ecl | – | – | Ecl |
45 | II | 2.1 | 28.6 (I), 8.5 (II) | Cep(II) |
aThe classification of #3 and #34 is unclear (see the text).
No. . | LC . | |$A_{K_{\mathrm{s}}}$| . | D . | Type . |
---|---|---|---|---|
. | shape . | (mag) . | (kpc) . | . |
1 | Ecl | – | – | Ecl |
2 | I/II: | 1.3 | 23.9 (I), 9.0 (II) | Cep(II) |
3 | RR/DS | – | – | RR/DSa |
4 | Ecl | – | – | Ecl |
5 | Ecl | – | – | Ecl |
6 | I/II: | 2.1 | 22.2 (I), 6.9 (II) | Cep(II) |
7 | II | 2.2 | 26.3 (I), 6.7 (II) | Cep(II) |
8 | Ecl | – | – | Ecl |
9 | II | 1.9 | 19.1 (I), 7.7 (II) | Cep(II) |
10 | II | 2.6 | 23.2 (I), 6.5 (II) | Cep(II) |
11 | II | 2.1 | 21.6 (I), 7.7 (II) | Cep(II) |
12 | Ecl | – | – | Ecl |
13 | Ecl | – | – | Ecl |
14 | Ecl | – | – | Ecl |
15 | II | 1.9 | 31.3 (I), 8.0 (II) | Cep(II) |
16 | Ecl | – | – | Ecl |
17 | Ecl | – | – | Ecl |
18 | I | 2.7 | 7.7 (I), 2.3 (II) | Cep(I) |
19 | II: | 0.0 | 9.9 (I), 4.3 (II) | Cep(II) |
20 | I | 2.3 | 7.8 (I), 2.4 (II) | Cep(I) |
21 | Ecl | – | – | Ecl |
22 | Ecl | – | – | Ecl |
23 | Ecl | – | – | Ecl |
24 | Ecl: | – | – | Ecl |
25 | Ecl | – | – | Ecl |
26 | I/II: | 2.4 | 18.7 (I), 5.7 (II) | Cep(II) |
27 | Ecl | – | – | Ecl |
28 | II | 2.2 | 26.9 (I), 8.3 (II) | Cep(II) |
29 | I/II: | 2.3 | 26.6 (I), 9.0 (II) | Cep(II) |
30 | Ecl | – | – | Ecl |
31 | II | 2.1 | 25.4 (I), 6.4 (II) | Cep(II) |
32 | I | 2.4 | 8.3 (I), 2.5 (II) | Cep(I) |
33 | II | 1.1 | 13.0 (I), 4.1 (II) | Cep(II) |
34 | Cep: | 1.9 | 3.0 (I), 1.4 (II) | Cep(?)a |
35 | Ecl | – | – | Ecl |
36 | Ecl | – | – | Ecl |
37 | Ecl | – | – | Ecl |
38 | Ecl | – | – | Ecl |
39 | II | – | – | Cep(II) |
40 | II | 2.4 | 28.0 (I), 8.3 (II) | Cep(II) |
41 | Ecl | – | – | Ecl |
42 | Ecl | – | – | Ecl |
43 | Ecl | – | – | Ecl |
44 | Ecl | – | – | Ecl |
45 | II | 2.1 | 28.6 (I), 8.5 (II) | Cep(II) |
No. . | LC . | |$A_{K_{\mathrm{s}}}$| . | D . | Type . |
---|---|---|---|---|
. | shape . | (mag) . | (kpc) . | . |
1 | Ecl | – | – | Ecl |
2 | I/II: | 1.3 | 23.9 (I), 9.0 (II) | Cep(II) |
3 | RR/DS | – | – | RR/DSa |
4 | Ecl | – | – | Ecl |
5 | Ecl | – | – | Ecl |
6 | I/II: | 2.1 | 22.2 (I), 6.9 (II) | Cep(II) |
7 | II | 2.2 | 26.3 (I), 6.7 (II) | Cep(II) |
8 | Ecl | – | – | Ecl |
9 | II | 1.9 | 19.1 (I), 7.7 (II) | Cep(II) |
10 | II | 2.6 | 23.2 (I), 6.5 (II) | Cep(II) |
11 | II | 2.1 | 21.6 (I), 7.7 (II) | Cep(II) |
12 | Ecl | – | – | Ecl |
13 | Ecl | – | – | Ecl |
14 | Ecl | – | – | Ecl |
15 | II | 1.9 | 31.3 (I), 8.0 (II) | Cep(II) |
16 | Ecl | – | – | Ecl |
17 | Ecl | – | – | Ecl |
18 | I | 2.7 | 7.7 (I), 2.3 (II) | Cep(I) |
19 | II: | 0.0 | 9.9 (I), 4.3 (II) | Cep(II) |
20 | I | 2.3 | 7.8 (I), 2.4 (II) | Cep(I) |
21 | Ecl | – | – | Ecl |
22 | Ecl | – | – | Ecl |
23 | Ecl | – | – | Ecl |
24 | Ecl: | – | – | Ecl |
25 | Ecl | – | – | Ecl |
26 | I/II: | 2.4 | 18.7 (I), 5.7 (II) | Cep(II) |
27 | Ecl | – | – | Ecl |
28 | II | 2.2 | 26.9 (I), 8.3 (II) | Cep(II) |
29 | I/II: | 2.3 | 26.6 (I), 9.0 (II) | Cep(II) |
30 | Ecl | – | – | Ecl |
31 | II | 2.1 | 25.4 (I), 6.4 (II) | Cep(II) |
32 | I | 2.4 | 8.3 (I), 2.5 (II) | Cep(I) |
33 | II | 1.1 | 13.0 (I), 4.1 (II) | Cep(II) |
34 | Cep: | 1.9 | 3.0 (I), 1.4 (II) | Cep(?)a |
35 | Ecl | – | – | Ecl |
36 | Ecl | – | – | Ecl |
37 | Ecl | – | – | Ecl |
38 | Ecl | – | – | Ecl |
39 | II | – | – | Cep(II) |
40 | II | 2.4 | 28.0 (I), 8.3 (II) | Cep(II) |
41 | Ecl | – | – | Ecl |
42 | Ecl | – | – | Ecl |
43 | Ecl | – | – | Ecl |
44 | Ecl | – | – | Ecl |
45 | II | 2.1 | 28.6 (I), 8.5 (II) | Cep(II) |
aThe classification of #3 and #34 is unclear (see the text).
In Fig. 2 filled circles in black indicate CCEPs and open circles indicate T2Cs. The two types of Cepheids in the LMC have reasonably different trends of the Fourier parameters against period. Thus, they are useful for the classification, although there is a considerable scatter blurring the separation. The discrimination between the two types can be more robustly done with estimating their distances than solely based on the light-curve shape (Section 3.3).
The plus symbols in Fig. 2 indicate eclipsing binaries. Their ϕ21 and ϕ31 values are mostly around 2π (or equivalently 0) indicating their symmetric variations. Three objects (#1, #4 and #24) have ϕ31 values different from 2π, but the amplitudes of the third harmonics are too low. #23 (P = 3.26 d) also has the Fourier parameters unexpected for an eclipsing binary. This comes from the apparent difference of the levels outside the eclipsing phases, which however is caused by the photometric uncertainty due to the crowding effect. An eye inspection of its light curve suggests that this star is an eclipsing binary. Light curves of some binaries such as #1 and #21 look similar to those of overtone RR Lyr stars (RRc). However, their amplitudes are larger than the typical amplitudes of RRc, and furthermore do not show a decreasing trend with increasing wavelengths which is a common characteristic of pulsating variables.
Two other objects are indicated by triangles in Fig. 2. #3 (P = 0.265 d) shows an asymmetric variation typical of pulsating stars. Also, its amplitude decreases with increasing wavelength, which is expected for a pulsating star. Its period is at the boundary between δ Sct stars and RR Lyrs in the overtone mode, and we cannot decide to which group the object belongs (also see Section 3.4). We consider that #34 is a Cepheid but it is unclear to which Cepheid type the object belongs. The ϕ31 of #34 (P = 2.19 d) seems to favour the classification as a CCEP in the overtone mode, rather than T2Cs, but the R31 is much larger than expected. There is an object classified as an LMC anomalous Cepheid, OGLE-LMC-ACEP-047, which has the similar Fourier parameters (see fig. 9 in Soszyński et al. 2008b), although that star itself shows a slightly different light curve from the majority of anomalous Cepheids.
3.3 Reddenings and distances to Cepheids
We can also make use of the difference between the absolute magnitudes of CCEPs and those of T2Cs for the classification. The estimated distances from the PLRs are very different depending on the assumed Cepheid population. Note that the period–colour relations are almost the same for both types so that a rough estimate of the reddening does not depend on the classification.
For each Cepheid candidate, the distance and extinction are tentatively derived using the PLRs of both types of Cepheid (Table 5). As we discussed in Paper I, an estimate of |$(\mu _0, A_{K_{\mathrm{s}}})$| is possible with a pair of two-band photometry, and three estimates can be obtained with JHKs magnitudes. The reddening law in JHKs is taken from Nishiyama et al. (2006a). The panel (a) of Fig. 3 compares the distances from the Sun assuming that the variables are CCEPs, D(I), with those assuming that they are T2Cs, D(II). For example, the objects with D(II) ∼ 8 kpc would be further than 20 kpc if assumed to be CCEPs. It is almost certain that such stars are T2Cs in the Galactic bulge rather than CCEPs far behind the GC, especially when their extinctions are not larger than the values expected at the distance of the GC.
In addition, there is a constraint on the distribution of T2Cs; they are concentrated to the Galactic bulge. Paper I showed that short-period Miras (P ≤ 350 d) found in the same survey are strongly concentrated to the distance of the GC (∼8.24 kpc) and also that they suffer from interstellar extinctions larger than ∼2 mag in Ks. One can assume as a first approximation that T2Cs are distributed in the same manner because such short-period Miras are considered to be as old as T2Cs. Panel (b) of Fig. 3 compares the Galactocentric distances under the two assumptions, RGC(I) and RGC(II) (here we assumed that the GC distance is 8.24 kpc; Paper I). The bulk of the open circles are concentrated towards small RGC(II), but they would be significantly further than the GC if assumed to be CCEPs. The extinction |$A_{K_{\mathrm{s}}}$| are estimated to be 2–2.5 mag for these objects, regardless of the Cepheid type. This is the approximate range of values expected for objects at the GC distance. Thus, they are considered to be T2Cs in the Galactic bulge. Two objects with RGC(II) ∼ 4 kpc fall at the intermediate range in Fig. 3 (#19 and #33). However, their small extinctions strongly suggest that they are relatively close T2Cs rather than CCEPs further than the GC. In contrast, three objects are found to be CCEPs as we reported in Paper II.
The periods of six T2Cs are longer than 20 d. From the work on the T2Cs in the Magellanic Clouds, it is known that such long-period T2Cs show a large scatter in the period–magnitude diagrams and may be systematically brighter than the PLR obtained for the shorter period T2Cs, BL Her and W Vir types (Matsunaga et al. 2009a). The scatter, however, is not so large as to change the classification.
According to the variable type determined here, the distance moduli and extinctions are derived and listed in Table 6. Mean estimates of the (|$\mu _0, A_{K_{\mathrm{s}}}$|), whenever available, are also listed in Table 6 and they are used in the following discussions. The estimates from the different pairs of filters agree reasonably well with each other, except for the case of #2 (P = 7.46 d) whose photometry is uncertain due to the effect of crowding. Inconsistent |$A_{K_{\mathrm{s}}}$| estimates from the JH and HKs pairs occur if the measured colours are not in accordance with the sum of the intrinsic colours and the reddening vector. Such inconsistency can happen when blue and red stars are merged in the line of sight (see the discussion in section 4.2 of Paper I).
No. . | Type . | log P . | μHK0 . | |$A_{K_{\mathrm{s}}}^{HK}$| . | μJK0 . | |$A_{K_{\mathrm{s}}}^{JK}$| . | μJH0 . | |$A_{K_{\mathrm{s}}}^{JH}$| . | μMean0 . | |$A_{K_{\mathrm{s}}}^{\rm Mean}$| . |
---|---|---|---|---|---|---|---|---|---|---|
2 | II | 0.873 | 14.17: | 1.72: | 14.66: | 1.23: | 15.49: | 0.96: | 14.77: | 1.30: |
6 | II | 1.179 | 14.23 | 2.09 | – | – | – | – | 14.23 | 2.09 |
7 | II | 1.718 | 14.12 | 2.24 | 14.12 | 2.24 | 14.12 | 2.24 | 14.12 | 2.24 |
9 | II | 0.676 | 14.47 | 1.87 | – | – | – | – | 14.47 | 1.87 |
10 | II | 1.382 | 14.11 | 2.62 | – | – | – | – | 14.11 | 2.62 |
11 | II | 0.918 | 14.41 | 2.09 | – | – | – | – | 14.41 | 2.09 |
15 | II | 1.703 | 14.18 | 2.06 | 14.32 | 1.92 | 14.56 | 1.84 | 14.35 | 1.94 |
18 | I | 1.357 | 14.50 | 2.68 | 14.43 | 2.75 | 14.32 | 2.79 | 14.42 | 2.74 |
19 | II | 0.560 | 13.07 | 0.04 | 13.18 | −0.07 | 13.36 | −0.13 | 13.20 | −0.05 |
20 | I | 1.300 | 14.53 | 2.32 | 14.50 | 2.35 | 14.45 | 2.37 | 14.49 | 2.35 |
26 | II | 1.207 | 13.93 | 2.38 | – | – | – | – | 13.93 | 2.38 |
28 | II | 1.192 | 14.60 | 2.18 | – | – | – | – | 14.60 | 2.18 |
29 | II | 1.011 | 14.60 | 2.31 | – | – | – | – | 14.60 | 2.31 |
31 | II | 1.603 | 13.97 | 2.13 | – | – | – | – | 13.97 | 2.13 |
32 | I | 1.372 | 14.69 | 2.36 | 14.57 | 2.48 | 14.38 | 2.54 | 14.55 | 2.46 |
33 | II | 1.278 | 13.05 | 1.04 | 13.04 | 1.05 | 13.02 | 1.06 | 13.04 | 1.05 |
40 | II | 1.279 | 14.63 | 2.44 | – | – | – | – | 14.63 | 2.44 |
45 | II | 1.387 | 14.51 | 2.10 | 14.55 | 2.06 | 14.62 | 2.04 | 14.56 | 2.07 |
No. . | Type . | log P . | μHK0 . | |$A_{K_{\mathrm{s}}}^{HK}$| . | μJK0 . | |$A_{K_{\mathrm{s}}}^{JK}$| . | μJH0 . | |$A_{K_{\mathrm{s}}}^{JH}$| . | μMean0 . | |$A_{K_{\mathrm{s}}}^{\rm Mean}$| . |
---|---|---|---|---|---|---|---|---|---|---|
2 | II | 0.873 | 14.17: | 1.72: | 14.66: | 1.23: | 15.49: | 0.96: | 14.77: | 1.30: |
6 | II | 1.179 | 14.23 | 2.09 | – | – | – | – | 14.23 | 2.09 |
7 | II | 1.718 | 14.12 | 2.24 | 14.12 | 2.24 | 14.12 | 2.24 | 14.12 | 2.24 |
9 | II | 0.676 | 14.47 | 1.87 | – | – | – | – | 14.47 | 1.87 |
10 | II | 1.382 | 14.11 | 2.62 | – | – | – | – | 14.11 | 2.62 |
11 | II | 0.918 | 14.41 | 2.09 | – | – | – | – | 14.41 | 2.09 |
15 | II | 1.703 | 14.18 | 2.06 | 14.32 | 1.92 | 14.56 | 1.84 | 14.35 | 1.94 |
18 | I | 1.357 | 14.50 | 2.68 | 14.43 | 2.75 | 14.32 | 2.79 | 14.42 | 2.74 |
19 | II | 0.560 | 13.07 | 0.04 | 13.18 | −0.07 | 13.36 | −0.13 | 13.20 | −0.05 |
20 | I | 1.300 | 14.53 | 2.32 | 14.50 | 2.35 | 14.45 | 2.37 | 14.49 | 2.35 |
26 | II | 1.207 | 13.93 | 2.38 | – | – | – | – | 13.93 | 2.38 |
28 | II | 1.192 | 14.60 | 2.18 | – | – | – | – | 14.60 | 2.18 |
29 | II | 1.011 | 14.60 | 2.31 | – | – | – | – | 14.60 | 2.31 |
31 | II | 1.603 | 13.97 | 2.13 | – | – | – | – | 13.97 | 2.13 |
32 | I | 1.372 | 14.69 | 2.36 | 14.57 | 2.48 | 14.38 | 2.54 | 14.55 | 2.46 |
33 | II | 1.278 | 13.05 | 1.04 | 13.04 | 1.05 | 13.02 | 1.06 | 13.04 | 1.05 |
40 | II | 1.279 | 14.63 | 2.44 | – | – | – | – | 14.63 | 2.44 |
45 | II | 1.387 | 14.51 | 2.10 | 14.55 | 2.06 | 14.62 | 2.04 | 14.56 | 2.07 |
No. . | Type . | log P . | μHK0 . | |$A_{K_{\mathrm{s}}}^{HK}$| . | μJK0 . | |$A_{K_{\mathrm{s}}}^{JK}$| . | μJH0 . | |$A_{K_{\mathrm{s}}}^{JH}$| . | μMean0 . | |$A_{K_{\mathrm{s}}}^{\rm Mean}$| . |
---|---|---|---|---|---|---|---|---|---|---|
2 | II | 0.873 | 14.17: | 1.72: | 14.66: | 1.23: | 15.49: | 0.96: | 14.77: | 1.30: |
6 | II | 1.179 | 14.23 | 2.09 | – | – | – | – | 14.23 | 2.09 |
7 | II | 1.718 | 14.12 | 2.24 | 14.12 | 2.24 | 14.12 | 2.24 | 14.12 | 2.24 |
9 | II | 0.676 | 14.47 | 1.87 | – | – | – | – | 14.47 | 1.87 |
10 | II | 1.382 | 14.11 | 2.62 | – | – | – | – | 14.11 | 2.62 |
11 | II | 0.918 | 14.41 | 2.09 | – | – | – | – | 14.41 | 2.09 |
15 | II | 1.703 | 14.18 | 2.06 | 14.32 | 1.92 | 14.56 | 1.84 | 14.35 | 1.94 |
18 | I | 1.357 | 14.50 | 2.68 | 14.43 | 2.75 | 14.32 | 2.79 | 14.42 | 2.74 |
19 | II | 0.560 | 13.07 | 0.04 | 13.18 | −0.07 | 13.36 | −0.13 | 13.20 | −0.05 |
20 | I | 1.300 | 14.53 | 2.32 | 14.50 | 2.35 | 14.45 | 2.37 | 14.49 | 2.35 |
26 | II | 1.207 | 13.93 | 2.38 | – | – | – | – | 13.93 | 2.38 |
28 | II | 1.192 | 14.60 | 2.18 | – | – | – | – | 14.60 | 2.18 |
29 | II | 1.011 | 14.60 | 2.31 | – | – | – | – | 14.60 | 2.31 |
31 | II | 1.603 | 13.97 | 2.13 | – | – | – | – | 13.97 | 2.13 |
32 | I | 1.372 | 14.69 | 2.36 | 14.57 | 2.48 | 14.38 | 2.54 | 14.55 | 2.46 |
33 | II | 1.278 | 13.05 | 1.04 | 13.04 | 1.05 | 13.02 | 1.06 | 13.04 | 1.05 |
40 | II | 1.279 | 14.63 | 2.44 | – | – | – | – | 14.63 | 2.44 |
45 | II | 1.387 | 14.51 | 2.10 | 14.55 | 2.06 | 14.62 | 2.04 | 14.56 | 2.07 |
No. . | Type . | log P . | μHK0 . | |$A_{K_{\mathrm{s}}}^{HK}$| . | μJK0 . | |$A_{K_{\mathrm{s}}}^{JK}$| . | μJH0 . | |$A_{K_{\mathrm{s}}}^{JH}$| . | μMean0 . | |$A_{K_{\mathrm{s}}}^{\rm Mean}$| . |
---|---|---|---|---|---|---|---|---|---|---|
2 | II | 0.873 | 14.17: | 1.72: | 14.66: | 1.23: | 15.49: | 0.96: | 14.77: | 1.30: |
6 | II | 1.179 | 14.23 | 2.09 | – | – | – | – | 14.23 | 2.09 |
7 | II | 1.718 | 14.12 | 2.24 | 14.12 | 2.24 | 14.12 | 2.24 | 14.12 | 2.24 |
9 | II | 0.676 | 14.47 | 1.87 | – | – | – | – | 14.47 | 1.87 |
10 | II | 1.382 | 14.11 | 2.62 | – | – | – | – | 14.11 | 2.62 |
11 | II | 0.918 | 14.41 | 2.09 | – | – | – | – | 14.41 | 2.09 |
15 | II | 1.703 | 14.18 | 2.06 | 14.32 | 1.92 | 14.56 | 1.84 | 14.35 | 1.94 |
18 | I | 1.357 | 14.50 | 2.68 | 14.43 | 2.75 | 14.32 | 2.79 | 14.42 | 2.74 |
19 | II | 0.560 | 13.07 | 0.04 | 13.18 | −0.07 | 13.36 | −0.13 | 13.20 | −0.05 |
20 | I | 1.300 | 14.53 | 2.32 | 14.50 | 2.35 | 14.45 | 2.37 | 14.49 | 2.35 |
26 | II | 1.207 | 13.93 | 2.38 | – | – | – | – | 13.93 | 2.38 |
28 | II | 1.192 | 14.60 | 2.18 | – | – | – | – | 14.60 | 2.18 |
29 | II | 1.011 | 14.60 | 2.31 | – | – | – | – | 14.60 | 2.31 |
31 | II | 1.603 | 13.97 | 2.13 | – | – | – | – | 13.97 | 2.13 |
32 | I | 1.372 | 14.69 | 2.36 | 14.57 | 2.48 | 14.38 | 2.54 | 14.55 | 2.46 |
33 | II | 1.278 | 13.05 | 1.04 | 13.04 | 1.05 | 13.02 | 1.06 | 13.04 | 1.05 |
40 | II | 1.279 | 14.63 | 2.44 | – | – | – | – | 14.63 | 2.44 |
45 | II | 1.387 | 14.51 | 2.10 | 14.55 | 2.06 | 14.62 | 2.04 | 14.56 | 2.07 |
The object #39 (P = 30.9 d) was detected only in the Ks band, so that the distance and extinction cannot be obtained. This star is much fainter than the three CCEPs in spite of the fact that its period is longer than theirs. If this star is a CCEP at the distance of the GC, the extinction |$A_{K_{\mathrm{s}}}$| should be as large as 5.5 mag. In contrast, a T2C with |$A_{K_{\mathrm{s}}}\sim 2.8$| would be consistent with the observed Ks magnitude and the faintness in J and H. We conclude that this star is a T2C in the Galactic bulge.
3.4 Summary of the classification
The previous subsections show that most of the variables can be reasonably classified. The adopted types are indicated in the last columns of Tables 2 and 5. About half, 24, of the objects are classified as eclipsing binaries. Three are CCEPs and 16 are T2Cs. #3 is a pulsating star with a short period, 0.265 d, and falls in the period range between RR Lyr and δ Sct stars. The classification of #34 is uncertain.
Fig. 4 shows colour–magnitude diagrams for our catalogued variables and the other sources we detected in the survey. The open circles indicate T2Cs. The foreground T2Cs, #19 and #33, are relatively blue and bright. The (J − H) colour of a faint T2C, #2, is blue but its photometry was affected by the crowding. The other T2Cs are reddened and lie on the broadened giant branch of the Galactic bulge. Three CCEPs indicated by filled circles are located close to each other on the colour–magnitude diagrams; they are significantly reddened but relatively bright.
Eclipsing binaries, plus symbols in Fig. 4, are separated roughly into two groups, around the foreground main sequence or on the giant branch of the bulge. A few points exist in the intermediate colour range, #8, #36 and #41, but their colours are affected by the crowding (see their |$\text{M}$|flag in Table 2). The colours of the redder group suggest that they have large interstellar extinction and are thus distant and likely in the GC region. Excluding those affected by the crowding, this group includes #17, #21, #25, #27, #30, #37, #38, #42 and #43. They tend to have longer orbital periods than the bluer binaries. The brightest of the reddened binaries, #30 (P = 26.8 d), is of particular interest. It was reported as an O-type supergiant located near the GC (Mauerhan et al. 2010), but we find that it is a binary system. Furthermore, its asymmetric light curve suggests that the system has an eccentric orbit. Since the other reddened binaries may well be at the distance of the GC, they are also interesting objects for further study.
The triangle for #3 falls near the diagonal sequence of the red clump giants in the disc (Lucas et al. 2008), where the RR Lyr and δ Sct stars in the foreground are roughly expected. On the other hand, #34 is highly reddened and relatively bright, although the images in the H and Ks bands indicate that the photometry may be affected by crowding. Its distance would be 3.6 kpc if it were an overtone CCEP, and the distance would be smaller otherwise. Therefore, it is much closer than the GC, and yet the extinction is quite high, |$A_{K_{\mathrm{s}}}\sim 2$| mag. These values may be subject to the uncertainty due to the crowding, but it would not change the conclusion that this object is in the foreground of the GC. The nature of the star remains to be investigated.
4 DISCUSSION
4.1 Samples of type II Cepheids
Our catalogue includes 16 T2Cs; 14 are located in the bulge and 2 in the foreground (#19 and #33). In the following discussion, we consider 14 objects as our sample of T2Cs in the bulge unless otherwise mentioned. We found a few T2Cs with short period (P < 5 d). In fact, our survey was not deep enough to detect such objects. The PLR enables us to tell whether the detection limit is deep enough to detect a Cepheid with a given period, foreground extinction and distance. Fig. 5 illustrates the range in the parameter plane of |$(\log P, A_{K_{\mathrm{s}}})$| where we should be able to detect T2Cs at the distance of the GC. For example, a T2C with log P = 1 could not be detected if the foreground extinction is larger than |$A_{K_{\mathrm{s}}}=2$| mag. Considering that the majority of the objects near the GC are reddened more strongly, our survey is far from complete. In Fig. 5, several of the detected T2Cs seem to be beyond the detection limit in the H band or even in the Ks band. This happens because the limiting magnitude depends on the crowdedness which varies within our survey region. Our survey region includes the extremely crowded region near Sgr A* and also sparse regions towards dark cloud lanes.
Recently, Soszyński et al. (2011) found a rich population of T2Cs in the outer bulge towards low-extinction regions away from the Galactic plane. We combined their catalogue with the Two Micron All Sky Survey (2MASS) near-IR catalogue (Skrutskie et al. 2006) with the tolerance radius of 1 arcsec. There are 156 BL Her, 128 W Vir and 51 RV Tau objects in the OGLE-III catalogue, and we found 97, 117 and 49 counterparts for the three types of T2Cs, respectively (263 in total; Table 7). Because of their faintness, a significant fraction of the BL Her stars were not detected in 2MASS. In addition, the 2MASS catalogue indicates that photometric accuracies for quite a few objects are limited because of confusion or other reasons. Considering the quality flag, the blend flag and the confusion flag (Qflag, Bflag and Cflag in Table 7), there remain 166, 138 and 138 measurements in the JHKs bands with good photometric quality. We discriminate these ‘good’ magnitudes from the others below. In addition, we use the I-band light curves obtained by the OGLE-III survey to make phase corrections to convert the single-epoch 2MASS magnitudes into mean magnitudes. The same method was described and used in Matsunaga et al. (2009a, 2011a). Table 7 lists the size of the correction, Δϕ, which is to be added to the 2MASS magnitudes for each object. Some I-band light curves show a large scatter, and we do not apply the phase correction for those T2Cs (mainly RV Tau stars, with Δϕ = 99.999 in Table 7).
OGLE ID . | P . | 2MASS ID . | J . | H . | Ks . | Qflag . | Bflag . | Cflag . | Δϕ . |
---|---|---|---|---|---|---|---|---|---|
. | (d) . | . | (mag) . | (mag) . | (mag) . | . | . | . | (mag) . |
OGLE-BLG-T2CEP-001 | 3.998 3508 | 17052035−3228176 | 12.904 | 12.412 | 12.273 | AAA | 111 | 000 | 0.160 |
OGLE-BLG-T2CEP-002 | 2.268 4194 | 17061499−3301275 | 13.130 | 12.713 | 12.587 | AAA | 111 | 000 | −0.050 |
OGLE-BLG-T2CEP-003 | 1.484 4493 | 17084014−3254104 | 13.826 | 13.457 | 13.276 | AAA | 111 | 00c | 0.295 |
OGLE-BLG-T2CEP-004 | 1.211 8999 | 17131083−2905453 | 13.817 | 13.355 | 13.248 | AAA | 111 | 000 | 0.052 |
OGLE-BLG-T2CEP-006 | 7.637 9292 | 17142541−2846465 | 12.213 | 11.863 | 11.682 | AAA | 111 | 000 | 0.266 |
OGLE-BLG-T2CEP-007 | 1.817 3297 | 17235478−2902378 | 14.293 | 13.607 | 13.426 | AAA | 111 | 000 | −0.200 |
OGLE-BLG-T2CEP-008 | 1.182 9551 | 17242093−2755493 | 14.573 | 99.999 | 99.999 | AUU | 200 | c00 | 0.091 |
OGLE-BLG-T2CEP-009 | 1.896 0106 | 17242227−2927352 | 14.218 | 13.539 | 13.245 | AAA | 112 | 0dc | −0.159 |
OGLE-BLG-T2CEP-010 | 1.914 6495 | 17270554−2536015 | 13.671 | 13.143 | 12.989 | AAA | 111 | 000 | 0.138 |
OGLE-BLG-T2CEP-011 | 15.388 6022 | 17271765−2538234 | 12.006 | 11.208 | 10.995 | AAA | 111 | 000 | −0.300 |
OGLE ID . | P . | 2MASS ID . | J . | H . | Ks . | Qflag . | Bflag . | Cflag . | Δϕ . |
---|---|---|---|---|---|---|---|---|---|
. | (d) . | . | (mag) . | (mag) . | (mag) . | . | . | . | (mag) . |
OGLE-BLG-T2CEP-001 | 3.998 3508 | 17052035−3228176 | 12.904 | 12.412 | 12.273 | AAA | 111 | 000 | 0.160 |
OGLE-BLG-T2CEP-002 | 2.268 4194 | 17061499−3301275 | 13.130 | 12.713 | 12.587 | AAA | 111 | 000 | −0.050 |
OGLE-BLG-T2CEP-003 | 1.484 4493 | 17084014−3254104 | 13.826 | 13.457 | 13.276 | AAA | 111 | 00c | 0.295 |
OGLE-BLG-T2CEP-004 | 1.211 8999 | 17131083−2905453 | 13.817 | 13.355 | 13.248 | AAA | 111 | 000 | 0.052 |
OGLE-BLG-T2CEP-006 | 7.637 9292 | 17142541−2846465 | 12.213 | 11.863 | 11.682 | AAA | 111 | 000 | 0.266 |
OGLE-BLG-T2CEP-007 | 1.817 3297 | 17235478−2902378 | 14.293 | 13.607 | 13.426 | AAA | 111 | 000 | −0.200 |
OGLE-BLG-T2CEP-008 | 1.182 9551 | 17242093−2755493 | 14.573 | 99.999 | 99.999 | AUU | 200 | c00 | 0.091 |
OGLE-BLG-T2CEP-009 | 1.896 0106 | 17242227−2927352 | 14.218 | 13.539 | 13.245 | AAA | 112 | 0dc | −0.159 |
OGLE-BLG-T2CEP-010 | 1.914 6495 | 17270554−2536015 | 13.671 | 13.143 | 12.989 | AAA | 111 | 000 | 0.138 |
OGLE-BLG-T2CEP-011 | 15.388 6022 | 17271765−2538234 | 12.006 | 11.208 | 10.995 | AAA | 111 | 000 | −0.300 |
OGLE ID . | P . | 2MASS ID . | J . | H . | Ks . | Qflag . | Bflag . | Cflag . | Δϕ . |
---|---|---|---|---|---|---|---|---|---|
. | (d) . | . | (mag) . | (mag) . | (mag) . | . | . | . | (mag) . |
OGLE-BLG-T2CEP-001 | 3.998 3508 | 17052035−3228176 | 12.904 | 12.412 | 12.273 | AAA | 111 | 000 | 0.160 |
OGLE-BLG-T2CEP-002 | 2.268 4194 | 17061499−3301275 | 13.130 | 12.713 | 12.587 | AAA | 111 | 000 | −0.050 |
OGLE-BLG-T2CEP-003 | 1.484 4493 | 17084014−3254104 | 13.826 | 13.457 | 13.276 | AAA | 111 | 00c | 0.295 |
OGLE-BLG-T2CEP-004 | 1.211 8999 | 17131083−2905453 | 13.817 | 13.355 | 13.248 | AAA | 111 | 000 | 0.052 |
OGLE-BLG-T2CEP-006 | 7.637 9292 | 17142541−2846465 | 12.213 | 11.863 | 11.682 | AAA | 111 | 000 | 0.266 |
OGLE-BLG-T2CEP-007 | 1.817 3297 | 17235478−2902378 | 14.293 | 13.607 | 13.426 | AAA | 111 | 000 | −0.200 |
OGLE-BLG-T2CEP-008 | 1.182 9551 | 17242093−2755493 | 14.573 | 99.999 | 99.999 | AUU | 200 | c00 | 0.091 |
OGLE-BLG-T2CEP-009 | 1.896 0106 | 17242227−2927352 | 14.218 | 13.539 | 13.245 | AAA | 112 | 0dc | −0.159 |
OGLE-BLG-T2CEP-010 | 1.914 6495 | 17270554−2536015 | 13.671 | 13.143 | 12.989 | AAA | 111 | 000 | 0.138 |
OGLE-BLG-T2CEP-011 | 15.388 6022 | 17271765−2538234 | 12.006 | 11.208 | 10.995 | AAA | 111 | 000 | −0.300 |
OGLE ID . | P . | 2MASS ID . | J . | H . | Ks . | Qflag . | Bflag . | Cflag . | Δϕ . |
---|---|---|---|---|---|---|---|---|---|
. | (d) . | . | (mag) . | (mag) . | (mag) . | . | . | . | (mag) . |
OGLE-BLG-T2CEP-001 | 3.998 3508 | 17052035−3228176 | 12.904 | 12.412 | 12.273 | AAA | 111 | 000 | 0.160 |
OGLE-BLG-T2CEP-002 | 2.268 4194 | 17061499−3301275 | 13.130 | 12.713 | 12.587 | AAA | 111 | 000 | −0.050 |
OGLE-BLG-T2CEP-003 | 1.484 4493 | 17084014−3254104 | 13.826 | 13.457 | 13.276 | AAA | 111 | 00c | 0.295 |
OGLE-BLG-T2CEP-004 | 1.211 8999 | 17131083−2905453 | 13.817 | 13.355 | 13.248 | AAA | 111 | 000 | 0.052 |
OGLE-BLG-T2CEP-006 | 7.637 9292 | 17142541−2846465 | 12.213 | 11.863 | 11.682 | AAA | 111 | 000 | 0.266 |
OGLE-BLG-T2CEP-007 | 1.817 3297 | 17235478−2902378 | 14.293 | 13.607 | 13.426 | AAA | 111 | 000 | −0.200 |
OGLE-BLG-T2CEP-008 | 1.182 9551 | 17242093−2755493 | 14.573 | 99.999 | 99.999 | AUU | 200 | c00 | 0.091 |
OGLE-BLG-T2CEP-009 | 1.896 0106 | 17242227−2927352 | 14.218 | 13.539 | 13.245 | AAA | 112 | 0dc | −0.159 |
OGLE-BLG-T2CEP-010 | 1.914 6495 | 17270554−2536015 | 13.671 | 13.143 | 12.989 | AAA | 111 | 000 | 0.138 |
OGLE-BLG-T2CEP-011 | 15.388 6022 | 17271765−2538234 | 12.006 | 11.208 | 10.995 | AAA | 111 | 000 | −0.300 |
4.2 Period distribution and surface density
The period distributions of our T2Cs and the OGLE-III sample are shown in Fig. 6. Most of our sample have long periods (P > 10 d). This bias is caused by the detection limit of our survey as mentioned above. In contrast, with more than 300 T2Cs, the OGLE-III sample clearly shows the distinct groups of BL Her, W Vir and RV Tau stars. Such a feature is well seen in the T2C samples of the Magellanic Clouds but not in those of globular clusters (see fig. 5 in Matsunaga et al. 2011a).
In addition, there are significantly more W Vir stars than RV Tau stars and the periods of W Vir stars show a broad, or even two distinct, peak(s), both of which are similar to the case of the LMC T2Cs. The number of BL Her stars is even larger than W Vir stars, i.e. NWV/NBL = 0.82 ± 0.14 (error from the Poisson noise). This ratio falls between the cases of the LMC (1.25) and the SMC (0.6) given in Matsunaga et al. (2011a). The reason for these variations in the T2C populations is presumably related to age and/or metallicity, but the lack of theoretical models for T2Cs prevents us from further discussion.
It is of interest to examine the surface density of T2Cs in the bulge. We detected 11 T2Cs with P > 15 d, which leads to the density of 66 deg−2 considering the area of our survey towards the GC (1/6 deg−2). However, our survey was not complete even for the relatively long-period T2Cs because of thick dark nebulae (Fig. 5), and the above density is an underestimate thus indicated by the arrow in Fig. 7. For the outer bulge region, we obtained the surface density of T2Cs for each OGLE-III region. Fig. 7 plots the surface densities of the OGLE-III T2Cs with P > 15 d (filled circles) and all T2Cs (crosses) in each field against the angular distance from the GC. We consider only the fields with |l| < 2° and |b| < 4° where the density is high enough. The profile in Fig. 7 shows, in effect, the variation along the minor axis. In addition, Fig. 8 shows a similar plot of the density profile for Miras. In Paper I, we found 547 Miras with period determined in the same IRSF survey field, among which 251 objects have periods less than 350 d. Whilst the Miras have a broad range of age (from ∼10 to 1 Gyr or even younger), such short-period Miras are found in globular clusters (Frogel & Whitelock 1998) and considered to belong to the old stellar population. The number of the short-period Miras towards the GC field corresponds to a surface density of 2200 deg−2. The surface densities for the outer region were obtained using the catalogue of the OGLE-II Miras compiled by Matsunaga, Fukushi & Nakada (2005). In Fig. 8, the density profile for the OGLE-II Miras is well represented by the exponential law, N ∼ exp (−0.24r). This exponential fits the OGLE-II points better than a de Voucouleurs law or a Sérsic law, N ∼ exp (r1/n), with n = 2. Note that the exponential and the de Voucouleurs law correspond to the Sérsic law with n = 1 and 4, respectively. In contrast, the lower limit inferred by our sample is higher than the exponential law predicted by the OGLE-II Miras. This excess agrees with the idea that an additional population of Miras exist in the nuclear bulge, the disc-like system within ∼200 pc. Although the density profile for T2Cs is uncertain due to the small number, our result on the T2C distribution also suggests that the nuclear bulge holds an additional group of T2Cs in the central region.
4.3 The distance to the GC
There have been a considerable number of estimates of the distance to the GC based on stellar distance indicators. Many of these rely on data from the general region of the Galactic bulge and may, to a greater or lesser degree, be affected by the bar-like and other structure of the bulge. In this section, we concentrate on data obtained in the areas close to the Centre which should be free from any such effects.
We now concentrate on our T2Cs, which are in the vicinity of the GC, and whose periods fall within the range of W Vir stars. Previous work found that the PLRs of BL Her/RV Tau stars may be different between different galaxies (Matsunaga et al. 2009a, 2011a; Soszyński et al. 2011), although we did not confirm significant deviation of our T2C samples from the PLR of those in globular clusters (Fig. 9). We obtained the average modulus of μ0 = 14.38 ± 0.13 mag, based on five W Vir stars (5 ≥ P ≥ 20 d) excluding #26, under the assumption of μ0(LMC) = 18.50 mag. The errors in the above estimates account just for statistical errors, and we need to consider systematic uncertainties. Our estimates are affected by errors in the extinction law and the LMC distance as well as the possible population effect on the PLR. We adopt an uncertainty of 0.05 mag for the LMC modulus and 0.07 mag for the adopted reddening law as we did in Paper I for the GC Miras. The results of Matsunaga et al. (2006, 2011a) suggest that any population effect on the PLR of T2Cs (W Vir stars) is small. Nevertheless, to be conservative we adopt an uncertainty of 0.07 mag for this. Considering these errors and the above estimates, the current sample of T2Cs results in an estimate of the GC distance modulus to be 14.38 ± 0.17 mag. There is a further uncertainty due, as discussed above, to our detection limit. This might result in the modulus being slightly underestimated.1 With the same survey data, we obtained the distances to Miras (Paper I) and CCEPs (Paper II). Adopting μ0(LMC) = 18.50 mag, the average of the distances to Miras gives μ0(GC) = 14.63 ± 0.11 mag. On the other hand, the calibration of CCEPs is based on the nearby calibrators and the average of the three distances leads to μ0(GC) = 14.49 ± 0.12 mag. The error budgets for these estimates are discussed in Papers I and II.
JHKs observations of red clump stars in the region around the GC were obtained by Nishiyama et al. (2006b) using the IRSF/SIRIUS. Recently, Laney, Joner & Pietrzyński (2012) obtained new high-precision JHKs magnitudes of red clump giants with the Hipparcos parallaxes, which give a new calibration of the red clump. Nishiyama et al. (2006b) adopted (H − Ks)0 = 0.07 and Ks = −1.59 from theoretical isochrones by Bonatto, Bica & Girardi (2004), whereas Laney et al. (2012) obtained (H − Ks)0 = 0.123 and Ks = −1.613. Using this new calibration leads to μ0(GC) = 14.53 ± 0.10 mag, that is 8.05 ± 0.37 kpc, without any population effect taken into account. There is a large scatter in metallicities of red clump giants in the bulge, and the median metallicity seems slightly higher than the solar abundance (Hill et al. 2011). The error, adopted from Nishiyama et al. (2006b), includes and is affected by the uncertainty of a possible population effect.
These estimates based on near-IR data of stellar distance indicators in areas close to the Centre are compared with the results from kinematic methods in Fig. 10. These latter methods are the Kepler rotation of the star S2 around Sgr A* (Gillessen et al. 2009), the statistical parallax method applied to the central stellar cluster (Trippe et al. 2008) and the parallax of Sgr B (Reid et al. 2009). The photometric and kinematic determinations are in satisfactory agreement and indicate a value of R0, close to 8.0 kpc. The uncertainty in the reddening law is the dominant remaining error for the photometric distances discussed here. Thus, the agreement of the photometric and kinematic results lends support to the reddening law of Nishiyama et al. (2006a). For a typical value of |$E_{H-K_{\mathrm{s}}}=1.8$|, for instance, the Nishiyama value of |$A_{K_{\mathrm{s}}}$| is 2.5 mag whereas the Rieke & Lebofsky (1985) law gives 3.2 mag and would lead to an unacceptably small value of R0(GC).
5 SUMMARY
Through our near-IR survey of stellar variability towards the GC, 45 short-period variables have been discovered. Their light curves are investigated to determine the variable types, and for the Cepheid candidates their distances and foreground extinctions are also considered based on the PLRs. Most of the objects are reasonably classified: 3 CCEPs, 16 T2Cs, 24 eclipsing binaries, and 2 others. The numbers of T2Cs and short-period Miras in our survey region are higher than the surface density following the exponential law which fits the distribution of T2Cs and Miras in the outer bulge. This strongly suggests that the nuclear bulge hosts a significant population of old stars (≥10 Gyr). We also discuss the distance to the GC based on stellar distance indicators in the central region. These are insensitive to problems associated with the three-dimensional structure of the bulge which may affect other determinations. Our main result is close to 8 kpc and agrees well with kinematic estimates. Since the photometric results are rather sensitive to the IR reddening law, the results give support to the reddening law of Nishiyama et al. (2006a) which we adopted.
We thank the IRSF/SIRIUS team and the staff of South African Astronomical Observatory (SAAO) for their support during our near-IR observations. The IRSF/SIRIUS project was initiated and supported by Nagoya University, National Astronomical Observatory of Japan and University of Tokyo in collaboration with South African Astronomical Observatory under financial support of Grant-in-Aid for Scientific Research on Priority Area (A) Nos 10147207 and 10147214 of the Ministry of Education, Culture, Sports, Science and Technology of Japan. This work was supported by Grant-in-Aid for Scientific Research (Nos 15071204, 15340061, 19204018, 21540240 and 07J05097). In addition, NM acknowledges the support by Grant-in-Aid for Research Activity Start-up (No. 22840008) and Grant-in-Aid for Young Scientists (No. 23684005) from the Japan Society for the Promotion of Science (JSPS). MWF gratefully acknowledges the receipt of a research grant from the National Research Council of South Africa (NRF). This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.
47 OGLE-III T2Cs in the same period range give a modulus of 14.40 ± 0.05 (internal error).
REFERENCES
SUPPORTING INFORMATION
Additional Supporting Information may be found in the online version of this article:
Table 3. The released table of light variation for the catalogued variables.
Table 7. 2MASS counterparts for the OGLE-III T2Cs in the bulge (Supplementary Data).
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