A Comprehensive Catalog of Galactic Eclipsing Binary Stars with Eccentric Orbits Based on Eclipse Timing Diagrams

C.-H. Kim; J. M. Kreiner; B. Zakrzewski; W. Ogłoza; H.-W. Kim; M.-J. Jeong

doi:10.3847/1538-4365/aab7ef

1. Introduction

Eclipsing binary (EB) stars with an eccentric orbit are very important stellar systems because they provide the physical and orbital parameters and exhibit some observable phenomena that are fundamental to our understanding of stellar structure, evolution, and tidal phenomena. Accurately determined physical parameters of their constituent stars, such as their mass, radius, temperature, and luminosity, have contributed to testing and improving stellar evolution models (Andersen 1991; Torres et al. 2010). The orbital elements of an eccentric orbit such as the orbital period, eccentricity, and argument of periastron, with the physical parameters, have been successfully used to constrain the timescales of synchronization and circularization predicted by some tidal theories (Zahn 2008). Among the tidally and/or rotationally induced observable effects are ellipsoidal variability, periastron brightening, apsidal motion (AM), and so on. In particular, AMs in eccentric EB (EEB) stars have provided important information on the internal structures of stars, as well as tests of general relativity in some binary stars (Giménez 1985; Claret & Giménez 1993). Moreover, some rare systems exhibiting simultaneously AM and a light-time effects (LITE) due to a third body are very valuable in the sense that they make additional contributions to statistics and the formation of multiple stellar systems and celestial mechanics (Bozkurt & Değirmenci 2007; Tokovinin 2008). Excellent reviews of the various strains of research described above are given by Mazeh (2008) and Torres et al. (2010).

AM is the rotational motion of the line of apsides of an eccentric binary orbit. It is caused by the external gravitational forces due to tidal and rotational distortions of the component stars in the binary star. The AM rate is dependent on the strengths of the forces, which strongly depend on the internal density concentrations of stars. Therefore, the observed AM rate is directly related to the stellar interior density profile in an averaged manner for two component stars, known as the weighted mean AM constant k₂. The observed k₂ constants are compared with the theoretical ones to test and improve the stellar internal structure models. Giménez (2007) gave a detailed review of the AM test, starting from the historical background and including major achievements, present status, and future prospects.

Naturally, many investigators have published catalogs of galactic EEB stars, including AM, which can be used to better understand the stellar internal structure and tidal theories (Sterne 1939; Schwarzschild 1958; Kopal 1959, 1978; Semeniuk 1968; Batten 1973; Petty 1973; Jeffery 1984; Hegedüs 1988, 1989; Claret & Giménez 1993; Giménez 1994; Petrova & Orlov 1999). These catalogs are also very useful for observers who prepare observational programs for chosen targets. The most recent catalog, published by Bulut & Demircan (2007), contains the physical parameters of 124 galactic EEB stars, including AM parameters and 150 candidate systems.

During the last three decades, there have been long-term and large scale photometric surveys with their own missions such as MAssive Compact Halo Objects (MACHO: Faccioli et al. 2007), the Optical Gravitational Lensing Experiment (OGLE: Graczyk et al. 2011; Pawlak et al. 2013, 2016; Soszyński et al. 2016), the All Sky Automated Survey (ASAS: Pojmański 2002), the Super Wide Angle Search for Planets (SWASP: Christian et al. 2006), the Trans-atlantic Exoplanet Survey (TrES: Alonso et al. 2004; Devor et al. 2008), the INTErnational Gamma-Ray Astrophysics Laboratory/Optical Monitoring Camera (INTEGRAL/OMC: Winkler et al. 2003; Sobotka 2007; Alfonso-Garzón et al. 2012), HIgh Precision PARallax COllecting Satellite (HIPPARCOS: Perryman et al. 1997), the Northern Sky Variability Survey (NSVS: Woźniak et al. 2004), the Catalina Sky Survey (CSS: Larson et al. 2003; Drake et al. 2014), the Cluster AgeS Experiment (CASE: Kaluzny et al. 2014, 2015), π of the Sky (PoS: Burd et al. 2004), and the Chandra X-ray Sky Survey (CXSS: Weisskopf et al. 2002; Evans et al. 2010). These surveys, often as a by-product, reported tens of thousands of new EBs not only in our own galaxy but also in other nearby galaxies (e.g., the Large and Small Magellanic Clouds; hereafter LMC, SMC, or MCs), and many of these were EEBs.

In particular, owing to the MACHO and OGLE survey projects, extra-galactic EEB stars showing AM in the SMC and the LMC have been increasingly reported in a series of intensive research efforts (Michalska & Pigulski 2005; Michalska 2007; Zasche & Wolf 2013; Hong et al. 2014; and Zasche et al. 2015 for the LMC, and Graczyk 2003; North et al. 2010; Zasche et al. 2014; and Hong et al. 2015, 2016 for the SMC). It is worth mentioning the very recent work by Hong et al. (2016), presenting the eclipse timing diagrams (hereafter ETDs, commonly referred to as O−C diagrams) for 90 EEB systems with clear AM in the SMC, based on the homogeneous OGLE photometric data, as well as their parameters calculated in a consistent way with the Giménez & Bastero (1995) method.

Despite the flood of new data on EEBs from the abovementioned surveys, no new compilation has appeared after that by Bulut & Demircan (2007). The main aim of this paper is to present an updated catalog of EEB systems, making use of the new observations available since the publication of Bulut & Demircan (2007). Therefore, we compiled a comprehensive catalog consisting of 623 galactic EEB systems, among them, 170 AM systems. The catalog represents the basic parameters of EEB systems, and we also give the parameters for the AM systems computed consistently with the Giménez & Bastero (1995) method.

2. Data Collection and Classification of Eclipsing Binaries with Elliptical Orbits

2.1. Data Collection

An EB star is considered to have an eccentric orbit if it meets one or more observational criteria, such as:

(i)
The ETD of the star shows that the (O−C) values of the primary and secondary minima are 180° out of phase with each other.
(ii)
The photometric light curves have the secondary eclipse displaced from phase 0.5, and/or the durations of primary and secondary eclipses are different from each other.
(iii)
The light curves display some light-brightening near the periastron.
(iv)
The radial velocity curves of the components deviate from a simple sinusoidal curve.

In addition, when one or more of the above criteria clearly vary with time, the EB system is safely classified into an EEB system showing AM.

We made four rules that the EEB stars in our catalog should satisfy:

(a)
They should fulfill observational criteria (i) or (ii). In this sense, our catalog is completely based on ETD.
(b)
We did not consider contact (W Ursae Majoris-type) and semidetached systems even if they fulfill criterion (i). The times of secondary minima for these stars may be displaced from the phase 0.5 due to asymmetry in the light curve caused by some physical processes.
(c)
We did take into account the EEB stars only in our galaxy.
(d)
We excluded new EEB stars discovered by the Kepler mission, which are expected to be more than 200 or 300 in number (see Kirk et al. 2016), but we considered the Kepler stars that have been observed earlier. The Kepler catalog numbers of these stars are presented in the column "remarks" of Tables 1 and 2 (see below). We think the compilation of new EEB stars by the Kepler mission would be another important task.

Under these rules, we compiled the list of EEB stars (Tables 3 and 4) as follows: all O−C diagrams (ETDs) of EB stars have been scrutinized in the timing database TIDAK⁵ managed by the co-authors of this paper (J.M.K., W.O., and B.Z.). If possible, criterion (ii) was checked using the mean light curves taken from the archived data of sky-survey projects such as ASAS, HIPPARCOS, NSVS, SWASP, and others. When there were no consecutive observations near eclipses (most cases) but a mean light curve was well-defined, the eclipse timings were obtained by superposing individual observed points in several consecutive minima onto a mean light curve. Some individual minima for a few stars were determined from the SWASP archived data. The same procedures were applied to the stars reported as new EEB stars from the analysis of the photometric data by some sky-survey projects (e.g., Devor et al. 2008; Shivvers et al. 2014), to the candidate stars in the Bulut & Demircan (2007) catalog and to the stars reported as EEB stars by individual author(s). The work of determining eclipse timings from the abovementioned photometric data archives was mostly carried out by two authors of this paper (B.Z. and C.H.K.).

Table 1. New Times of Minima of EEB Systems with GCVS Names

Star Name	Min. Time^a	Err.	Ty.	Rem.^b	References
OT AND	53969.541	0.010	pri	:	5
OT AND	54397.462	0.025	sec		5
V522 AND	51486.9589	0.0031	sec	n	15
V522 AND	54221.1262	0.0037	sec	n	5
V522 AND	54334.4196	0.0040	sec	n	5
V522 AND	54353.4232	0.0010	pri	n	5
V522 AND	54383.6353	0.0007	pri		5
V522 AND	54436.5038	0.0005	pri		5
V522 AND	55119.9495	0.0054	sec	n	7
BV ANT	52764.7946	0.0013	pri	n	12
BV ANT	52766.8295	0.0021	sec	n	12
BV ANT	53870.2787	0.0005	sec		5
BV ANT	53888.2487	0.0006	sec		5
BV ANT	53906.2213	0.0007	sec		5
BV ANT	54159.3752	0.0003	pri		5

Notes. This table displays only the first 15 lines.

^aHJD2400000+ is suppressed. ^bn = normal minima; := uncertain; ::= very uncertain.References. (1) This paper; (2) Kreiner et al. (2001, TIDAK), (3) Kafka (2017, AAVSO), (4) Burd et al. (2004, PoS), (5) Christian et al. (2006, SWASP), (6) Devor et al. (2008, TrES), (7) Drake et al. (2014, CSS), (8) Evans et al. (2010, CXSS), (9) Høg et al. (2000, TYCHO-2), (10) Perryman et al. (1997, HIPPARCOS), (11) Pojmański (1997, ASAS-2), (12) Pojmański (2002, ASAS-3), (13) Prša et al. (2001, KEPLER), (14) Winkler et al. (2003, INTEGRAL/OMC), (15) Woźniak et al. (2004, NSVS).

Only a portion of this table is shown here to demonstrate its form and content. A machine-readable version of the full table is available.

Download table as: Data Typeset image

Table 2. New Times of Minima of EEB Systems without GCVS Names

Star Name	Min. Time^a	Err.	Ty.	Rem.^b	References
2MASS J00372334+4719206	53271.9587	0.0008	pri	⋯	2
2MASS J00372334+4719206	53274.9945	0.0016	sec	⋯	2
2MASS J00372334+4719206	53277.8186	0.0021	pri	⋯	2
2MASS J00372334+4719206	53280.8770	0.0015	sec	⋯	2
2MASS J00372334+4719206	53283.6864	0.0016	pri	⋯	2
2MASS J00372334+4719206	53286.7316	0.0034	sec	⋯	2
2MASS J00435925+5114000	53250.9123	0.0006	sec	⋯	2
2MASS J00435925+5114000	53256.7689	0.0039	pri	⋯	2
2MASS J00435925+5114000	53262.6987	0.0010	sec	⋯	2
2MASS J00435925+5114000	53263.8253	0.0011	pri	⋯	2
2MASS J00435925+5114000	53270.9079	0.0019	pri	⋯	2
2MASS J00435925+5114000	53276.8600	0.0030	sec	⋯	2
2MASS J00435925+5114000	53282.6968	0.0029	pri	⋯	2
2MASS J00435925+5114000	53283.9434	0.0015	sec	⋯	2
2MASS J00435925+5114000	53303.9250	0.0015	pri	⋯	2

Notes. This table displays only the first 15 lines.

^aHJD2400000+ is suppressed. ^bn = normal minima; := uncertain; ::= very uncertain.References. (1) Christian et al. (2006, SWASP), (2) Devor et al. (2008, TrES), (3) Drake et al. (2014, CSS), (4) Evans et al. (2010, CXSS), (5) Kaluzny et al. (2015, CASE), (6) Perryman et al. (1997, HIPPARCOS), (7) Pojmański (2002, ASAS-3), (8) Woźniak (2004, NSVS), (9) Popov et al. (2015); (10) Davies (2015).

Only a portion of this table is shown here to demonstrate its form and content. A machine-readable version of the full table is available.

Download table as: Data Typeset image

Table 3. GCVS Eclipsing Binaries with Elliptical Orbits Confirmed by the Eclipsing Timing Diagram

Name	Max. Mag.(V)	T₀	Period	Type	Number		Phase	Remark	References
	(GCVS)	(HJD2400000+)	(day)		Pri	Sec
OT And	7.32	45711.945	20.852942	D	7	4	0.521		2; 3
V522 And	13.3	53598.068	7.552946	D	4	4	0.484		4
BV Ant	11.5	53447.830	3.594296	D	7	9	0.567		5
PP Aps	9.70	48503.268	4.279837	A	5	3	var		1
PV Aps	7.80	53763.283	28.875231	D	2	2	0.253		6
BW Aqr	10.3	39680.453	6.7196938	A	43	42	var		8
LL Aqr	9.23	48760.602	20.17844	A:	13	6	var		9
V871 Aql	12.5	38637.144	2.9526725	A	14	13	var		10
V889 Aql	8.52	38241.554	11.120756	A+III	39	36	var		11
V1646 Aql	11.9	52137.573	9.278382	D	2	5	0.567		12
V1665 Aql	8.09	52810.680	3.8817673	A	7	5	var		13
CY Ara	12.3	51931.896	3.0148878	D	2	2	0.626:		1
V539 Ara	5.71	45056.742	3.1690852	A+III	26	19	var		14
V883 Ara	8.55	52190.835	61.873150	D	3	2	0.443		5
AF Ari	6.71	48402.090	153.043	D	2	2	0.714:		15
AG Ari	8.14	54033.319	1.9631291	A:	6	14	var		13
AL Ari	9.23	51112.830	3.747455	A+III:	16	7	var		16
CG Aur	11.7	52501.717	1.8048592	A+III	56	35	var		17; 18
V437 Aur	8.42	55984.966	11.793792	D	3	6	0.397	(a)	1
V645 Aur	9.72	52848.592	10.892495	D	5	6	0.788		19
BW Boo	7.13	40362.754	3.3328202	A+III	36	7	var		7; 20
EQ Boo	8.80	47931.524	5.4353569	D	15	11	0.399		21
WW Cam	10.1	39403.554	2.2743627	A	60	41	var	(b)	186
AN Cam	10.4	26006.350	20.99851	D	11	8	0.779		23
AS Cam	8.57	40204.406	3.4309691	A+III:	86	65	var	(a)	24
DT Cam	8.13	48501.635	7.0662668	D	8	2	0.578		1
OO Cam	10.9	56742.289	8.1190451	D	5	5	0.489		19
V347 Cam	11.4	51533.510	9.45932	D	2	2	0.695		19
V361 Cam	11.3	52505.499	8.6386107	D	8	3	0.488:		19
V399 Cam	10.0	51508.615	2.597577	D	3	2	0.430		191
V409 Cam	11.0	51524.67	6.6764669	D	4	2	0.522		19
V422 Cam	11.3	51548.517	17.871	D	2	2	0.490:		19
V469 Cam	12.6	51531.660	11.872601	D	4	3	0.468		25
V498 Cam	11.8	51456.045	12.103206	D	3	3	0.436		19
V534 Cam	13.0	51497.173	3.0142365	A:	6	4	var		26
KX Cnc	7.25	54165.010	31.22009	D	4	8	0.643		27
EN CVn	10.9	51341.868	6.334600	D	7	12	0.513		6
SW CMa	9.12	26705.228	10.091980	A	18	22	var		28
TZ CMa	10.0	55140.754	3.8228660	A:	19	18	var		1
AR CMa	10.9	51869.910	2.332225	A	12	9	var		29
CE CMa	12.8	28098.210	27.072865	D	6	5	0.662		1
CV CMa	13.0	28044.560	3.6282891	A	9	6	var		1
KL CMa	6.73	48170.311	1.7622058	A	16	25	var		30
KV CMa	7.16	48348.430	68.100355	D	3	1	0.338:		31
LT CMa	7.43	48388.536	1.7595257	A:	17	10	var		32
V388 CMa	8.25	53067.815	2.9827176	A:	4	3	var		33
V432 CMa	12.4	54842.771	1.8238629	D	4	4	0.533		34
RW CMi	13.2	25347.152	6.083853	D	14	4	0.796		1
AV CMi	11.4	52500.622	2.277751	A	17	17	var		35
DR CMi	11.1	53841.746	23.76957	D	4	3	0.667		19
EM Car	8.37	46038.813	3.4142750	A	10	12	var	(c)	36
GL Car	9.53	24264.449	2.4222326	A+III	107	92	var	(d)	37
GR Car	13.7	23905.040	17.139505	D	6	4	0.313		38
QX Car	6.62	40701.193	4.477972	A	11	15	var		37
V466 Car	7.27	48036.750	3.455845	A	10	7	var		39
V467 Car	8.02	48692.580	7.0461414	D	4	3	0.639		31
V493 Car	8.84	47945.914	3.2294245	A+III:	14	15	var		7; 39
V529 Car	8.10	48175.415	4.744547	A	11	10	var		39
V606 Car	8.31	53043.210	12.319288	D	4	3	0.588		33
V610 Car	10.2	53383.410	4.844955	D	4	2	0.316		5
V655 Car	6.19	48174.320	16.932884	D	3	2	0.393		6
V661 Car	8.05	53133.420	23.943421	D	2	2	0.652	(e)	40
V674 Car	9.94	52971.790	19.81316	D	2	2	0.307		5
V725 Car	9.96	52978.220	9.410789	D	2	2	0.158	(e)	40
V733 Car	10.8	51920.875	2.956947	D	3	1	0.521:		40
V734 Car	11.2	52662.700	3.107451	D	3	3	0.439	(e)	40
V736 Car	7.91	52702.033	17.799162	D	3	3	0.658		19
AR Cas	4.89	40063.954	6.0663181	A	15	6	var		41
AZ Cas	9.20	32701.0	3372.3	D	5	1	0.559:		42; 43
IT Cas	11.0	28762.522	3.8966495	A:	63	47	var		22
MU Cas	11.2	51877.158	9.652957	A:	26	24	var		44
OX Cas	9.92	46733.770	2.4893461	A+III:	115	95	var	(f)	45
PV Cas	9.73	40227.388	1.7504698	A	190	144	var		45; 46
QX Cas	10.2	36048.858	6.004699	D	38	31	0.370	(g); (h)	47; 48
V381 Cas	10.2	44546.284	1.7459442	A	113	112	var		49
V459 Cas	10.3	25321.581	8.4582605	A:	58	35	var		22; 50
V518 Cas	11.0	51364.712	6.311981	D	4	4	0.504:	(i)	1
V744 Cas	8.44	48277.141	4.7816931	D	8	6	0.540		51
V775 Cas	9.73	48766.437	5.3901648	A	9	7	var	(a)	31
V785 Cas	9.33	48502.375	2.702517	A	23	28	var		52
V799 Cas	8.80	48500.601	7.7029264	A	7	9	var		53
V821 Cas	8.22	51767.352	1.7697435	A	36	34	var		39; 52
V1018 Cas	10.3	51601.455	4.127756	A:	10	3	var		54
V1066 Cas	10.8	51548.918	8.4649094	D	4	4	0.560		19
V1103 Cas	11.4	51556.705	6.1776282	D	4	3	0.531		19
V1110 Cas	10.6	51481.260	24.850	D	2	2	0.711:		19
V1137 Cas	11.8	51473.588	4.1589911	A:	8	9	var		64
V1141 Cas	12.3	51542.502	6.9092343	A	5	4	var		19
V1162 Cas	11.1	51423.730	29.067	D	2	2	0.230:		19
V1176 Cas	11.2	55192.862	6.334432	D	2	3	0.506		56
EL Cen	12.3	54420.142	21.86765	D	3	3	0.317		189
KT Cen	12.1	41696.044	4.130435	A	23	18	var		57
V346 Cen	8.50	21966.827	6.322007	A+III	41	39	var	(j)	58; 179
V383 Cen	13.1	25352.670	6.784384	D	3	3	0.606		59
V384 Cen	11.7	25051.151	12.635271	D	6	4	0.340		60
V636 Cen	8.68	52502.944	4.2839457	A	19	11	var		28
V963 Cen	8.61	51216.195	15.269389	D	5	3	0.290		16
V1000 Cen	8.40	52103.174	16.63481	D	3	2	0.585:		33
V1051 Cen	7.13	47964.540	9.646334	D	3	2	0.413		61; 62
V1071 Cen	9.68	52373.738	2.6953465	D	8	7	0.525		1
V1087 Cen	9.34	50563.588	5.04953	A	14	9	var		63
V1089 Cen	7.88	48503.054	5.48793	D	3	1	0.571:		31
V1118 Cen	9.55	47945.591	11.30489	D	6	4	0.524		54
V1142 Cen	11.7	51257.055	2.5247751	D	2	3	0.552		1
V1166 Cen	8.77	51955.340	13.419817	D	3	3	0.422		31
V1204 Cen	10.9	52652.804	2.3271067	D	3	1	0.479:		5
ψ Cen	4.03	54741.670	38.811612	D	7	4	0.821	(k)	65
CO Cep	12.0	29043.546	4.1375624	D	27	28	0.551		53
CW Cep	7.60	21670.438	2.7291395	A	64	51	var		66; 67
EK Cep	7.99	39002.825	4.4277926	A	136	17	var		68; 177
EY Cep	10.1	52339.190	7.971465	A:	13	21	var	(a)	69
NY Cep	7.40	41902.118	15.27565	D	15	2	0.276		70
V397 Cep	7.39	48501.270	2.086826	A	23	23	var		7
V698 Cep	12.7	50421.200	6.618538	A:	4	4	var		71
V731 Cep	10.5	52591.309	6.0684407	D	13	19	0.509		72
V734 Cep	11.0	51482.697	3.7659743	A:	8	7	var		5
V743 Cep	10.5	51542.754	4.6722928	D	7	4	0.541:		54
V750 Cep	11.4	51465.100	18.8805	D	2	2	0.438:		40
V798 Cep	11.9	51605.485	16.080145	D	7	7	0.232		192
V839 Cep	9.93	51448.701	9.963374	D	5	5	0.510		19
V850 Cep	9.98	51476.360	12.92262	D	2	2	0.601:		19
V880 Cep	10.6	51468.130	27.31397	D	2	2	0.540:		19
V881 Cep	11.6	51466.722	2.3337094	D	6	2	0.234		19
V897 Cep	11.4	51474.615	4.487162	D	3	4	0.516		19
V898 Cep	12.2	51366.390	2.8747772	A:	10	9	var		73; 74
V919 Cep	10.6	51295.784	1.8519818	A	8	8	var		64
V921 Cep	11.6	51311.370	13.70883	D	2	3	0.426:		19
V922 Cep	11.5	51606.755	3.5749710	D	4	5	0.508		19
V944 Cep	10.9	51478.670	6.5600625	D	6	2	0.526		75
V957 Cep	11.5	51504.730	1.988735	A	10	13	var		76
V961 Cep	10.4	51442.653	7.0384546	A:	6	6	var		182
TV Cet	8.60	41275.932	9.1032914	A:	28	21	var		24
DP Cet	6.85	48686.724	2.3681676	D	7	1	0.458:		31
BN Cir	9.20	52644.450	4.4097610	D	7	5	0.774	(a)	77
CL Cir	8.57	48501.960	5.2537967	D	5	6	0.565		78
DK Cir	7.68	52779.150	18.56965	D	3	2	0.758		79
RR Col	10.2	51863.460	12.625105	D	4	4	0.537	(a)	80
AW Col	8.00	52941.185	10.32171	D	3	2	0.780
V454 CrA	10.1	31264.460	2.396844	D	22	5	0.120		1
α CrB	2.21	23165.160	17.359907	A:	10	7	var		81; 82
VV Crv	5.19	56045.713	3.1445102	A:	16	10	var		83
UW Cru	12.3	25362.280	6.354522	D	9	11	0.527:		84
UX Cru	11.7	26044.210	12.29693	D	11	4	0.679		85
DN Cru	8.73	52655.660	9.881198	D	5	5	0.666		86
EP Cru	8.66	52551.881	11.077432	D	6	4	0.615		87
EQ Cru	10.1	52135.205	15.491216	D	2	1	0.460:		33
Y Cyg	7.30	09453.419	2.9963328	A	230	135	var		88
MY Cyg	8.30	41559.599	4.0051877	A	22	30	var		89
V380 Cyg	5.61	41255.983	12.425612	A	13	15	var		90; 178
V453 Cyg	8.29	39340.112	3.8898145	A	46	28	var	(l)	91
V477 Cyg	8.50	19468.300	2.346981	A+III	122	49	var		24
V478 Cyg	8.63	44777486	2.880903	A	35	25	var		66
V490 Cyg	13.1	52841.635	1.1402358	A	22	19	var		92
V541 Cyg	10.2	44881.882	15.337891	A	36	29	var		22; 181
V796 Cyg	10.9	55391.397	1.4808692	A	43	43	var		52
V959 Cyg	11.3	33922.283	1.8398158	D	39	0	⋯	(m)	93
V974 Cyg	11.9	35019.365	3.2044108	A+III	46	47	var		94; 193
V1136 Cyg	12.5	35453.527	3.4627562	A	44	39	var		53; 95
V1143 Cyg	5.85	48410.333	7.6407536	A	53	15	var		22
V1147 Cyg	11.9	50759.573	15.251329	A	33	24	var	(a)	22; 96
V1326 Cyg	11.3	48376.027	16.68178	A	13	16	var		97
V1765 Cyg	6.44	44139.402	13.37370	D	3	2	0.620		98
V2094 Cyg	7.70	48210.561	8.480329	A	37	31	var		99
V2391 Cyg	16.6	51388.271	9.848854	D	11	10	0.634	(a); (n)	1
V2544 Cyg	12.6	55004.489	2.0937745	A	20	13	var		73
V2618 Cyg	10.6	51340.650	47.614432	D	5	1	0.580:		64
V2647 Cyg	11.0	53670.769	5.8553490	A	6	6	var		19
BY Del	11.4	25830.346	10.034213	A:	17	9	var	(a)	1
MP Del	7.62	48246.861	21.338522	D	6	3	0.553		100; 101
NN Del	8.49	20212.002	99.26938	D	2	3	0.188		102
AL Dor	7.80	48665.095	14.905314	D	3	2	0.462		6
BF Dra	10.1	47276.316	11.210998	A:	51	34	var		22; 103
CM Dra	12.9	42893.932	1.2683900	D	107	101	0.499		104
GV Dra	8.59	51741.259	23.854330	D	9	3	0.736		105
HP Dra	8.06	51041.581	10.761534	D	4	2	0.518		106
NS Dra	11.3	51515.750	50.3624	D	7	4	0.630		19
V425 Dra	10.7	51397.888	9.3354096	D	7	5	0.547		107
V432 Dra	12.2	53279.518	11.628189	D	14	10	0.697		108
KY Gem	12.7	27098.309	12.33149	D	18	2	0.510:		1
OW Gem	9.0	48332.580	1258.66	D	37	7	0.233		109
V410 Gem	10.8	51548.811	3.4703382	A	8	7	var		64
DI Her	8.39	42234.767	10.550168	A	73	54	var		110
HS Her	8.50	47382.420	1.6374344	A	89	64	var		24; 111
LV Her	10.9	52070.027	18.435935	D	42	31	0.862	(a)	112
V501 Her	10.5	53550.671	8.5976873	D	23	13	0.479		113
V990 Her	7.72	48048.535	8.193298	D	3	2	0.445		19
V994A Her	6.93	53869.726	2.083265	A+III	43	31	var	(o)	114
V994B Her	6.93	53870.209	1.4200365	A+III	41	29	var	(o)	114
V1146 Her	11.1	51277.788	7.654087	D	2	2	0.485:		64
V1344 Her	11.5	51442.859	7.1461266	D	6	5	0.543		64
AI Hya	9.35	41726.143	8.2896735	A	25	18	var		115
KW Hya	6.11	45021.526	7.750477	D	5	3	0.459	(p)	116
OZ Hya	9.50	51983.944	2.0487656	A:	10	8	var		29
PX Hya	8.47	48457.090	36.15535	D	4	3	0.210		19
V340 Hya	8.24	47948.552	3.647410	D	6	5	0.549	(a)	54
V426 Hya	11.5	51578.820	7.3088523	D	3	3	0.484		5
V434 Hya	12.6	53404.915	5.9198757	D	5	6	0.537		19
RV Hyi	11.8	25477.810	7.1950385	D	5	4	0.617		77
CH Ind	7.50	52854.930	5.952579	A:	9	3	var		1
RW Lac	10.4	52502.488	10.369203	A+III	28	24	var		117
SS Lac	10.1	15908.493	14.41616	D	8	11	0.587	(q); (r)	118; 180
CO Lac	10.3	27534.075	1.5422072	A	99	105	var		45
CY Lac	11.5	54099.083	8.3605554	A:	10	7	var	(a)	119
ES Lac	11.0	34240.529	4.459409	A	31	20	var		95; 120
GX Lac	10.1	46009.306	6.3552425	A:	10	8	var		1
IL Lac	12.5	53226.390	7.395661	D	16	20	0.436		121
MZ Lac	11.2	38264.587	3.1587862	A	78	77	var		95; 122
OT Lac	11.2	56927.832	5.149865	A:	8	4	var		123
V339 Lac	12.9	34006.058	3.4085217	A:	17	10	var		1
V340 Lac	11.8	32806.044	19.943209	D	8	5	0.762		124
V345 Lac	11.1	31343.768	7.491888	A+III:	43	42	var		53
V364 Lac	8.51	44257.385	7.351529	A	56	47	var		53
V398 Lac	8.73	48468.760	5.4060442	A	13	7	var		39; 52
V401 Lac	7.93	48501.882	1.9500920	A	20	19	var		10; 125
V402 Lac	6.70	48501.330	3.782029	A+III	25	15	var		194
AT Lep	11.4	52634.523	10.649468	D	6	3	0.448		5
BC Lep	10.6	53619.883	3.9894146	D	2	2	0.510:		19
GG Lup	5.49	46136.732	1.8496037	A	25	19	var	(a)	14
OR Lup	9.28	48681.678	7.555967	D	3	2	0.505:		5
OU Lup	9.92	52414.109	4.610488	D	8	7	0.290		33
PP Lup	8.67	53167.600	29.69258	D	2	1	0.277:		31
RR Lyn	5.52	33153.613	9.945078	D	27	9	0.450		126
V370 Lyr	14.0	55011.021	7.0028651	D	23	20	0.497	(s)	1
TZ Men	6.19	42403.748	8.568988	A	6	5	var		55
RU Mon	10.3	38409.594	3.5846336	A+III	98	82	var		193
AO Mon	9.6	40588.327	1.8847631	A+III	53	41	var		128
CF Mon	13.6	30049.203	2.6104748	D	45	3	0.522:		185
V498 Mon	10.3	33221.750	2.4727703	A	26	28	var		29
V501 Mon	12.7	34444.200	7.0212085	D	19	20	0.444		129
V521 Mon	10.0	33008.440	2.970671	A+III	21	18	var		29
V536 Mon	9.1	52739.268	6.133969	D	19	15	0.409	(a)	130
V578 Mon	8.54	54469.078	2.4084871	A	26	11	var	(t)	131; 132
V680 Mon	9.6	52992.320	8.537964	D	4	3	0.864	(u)	19
V684 Mon	8.44	54153.537	1.8514195	A	29	31	var	(v)	29
V730 Mon	8.85	48502.744	1.5723188	A	12	12	var		29
V883 Mon	8.71	52529.420	50.36184	D	2	2	0.514:		33
V925 Mon	8.30	52625.888	5.9556834	D	8	3	0.532		64
V935 Mon	9.7	53664.383	5.993953	D	2	2	0.777:		1
AY Mus	10.5	41683.788	3.205549	D	10	6	0.484:	(r)	57; 187
LX Mus	8.85	48770.045	11.75056	D	3	1	0.393:		54
GM Nor	10.6	41696.918	1.884577	A	17	13	var		57
GN Nor	12.6	25720.294	5.703466	A	13	19	var		133
GV Nor	10.9	25560.129	2.971865	A+III:	20	10	var		29
KO Nor	12.0	53486.062	33.56204	D	3	4	0.471		134
NS Nor	10.1	52258.490	3.223601	D	10	8	0.674		29; 86
V373 Nor	8.47	48998.090	4.947891	D	4	2	0.670		61
V396 Nor	8.33	52104.376	5.535534	D	4	3	0.438		31
V405 Nor	8.81	53176.290	15.06126	D	3	2	0.566		135
V451 Nor	9.38	53063.890	3.459123	D	3	2	0.540		135
U Oph	5.84	45892.449	1.6773461	A+III	79	43	var		24
CY Oph	10.8	51930.304	16.35549	D	3	3	0.297	(a)	80
V451 Oph	7.94	44834.361	2.1965971	A	35	28	var		136
V456 Oph	10.2	41897.530	1.0160012	A+III:	65	41	var		193
V577 Oph	11.4	47406.435	6.079082	A+III:	17	13	var		137
V983 Oph	10.5	53851.944	23.01662	D	4	5	0.207	(a)	1; 80
V2368 Oph	6.22	54300.650	38.328573	D	4	3	0.813		138
V2626 Oph	8.26	52787.532	10.874299	A:	5	4	var		100
CW Ori	13.1	56713.242	1.709929	D	14	3	0.489:	(a)	123
EW Ori	9.90	27543.467	6.9368422	A:	45	26	var		22
FT Ori	9.1	41349.057	3.150395	A	102	33	var		139
GG Ori	10.7	35373.482	6.6314930	A	47	44	var		22
V530 Ori	10.6	25558.343	6.1107753	D	35	7	0.466		77; 140
V642 Ori	8.75	27125.980	9.185490	A:	5	11	var	(a)	1
V1027 Ori	10.5	52626.560	10.393775	D	18	20	0.556		80
V2592 Ori	7.80	52912.303	13.54996	D	2	2	0.410		135
V2778 Ori	10.2	53830.516	14.387465	D	4	5	0.435		19
V2783 Ori	10.1	54523.748	4.2161557	A+III	12	9	var		33
V2815 Ori	11.8	53059.622	2.1310132	D	8	5	0.481		1
δ Ori	2.14	43872.581	5.732441	A	10	6	var		141; 142
BO Pav	9.3	51873.391	19.23261	D	10	2	0.533		80
EY Pav	12.5	51871.174	15.32095	D	2	3	0.689		80
QU Pav	12.0	51868.524	9.182556	D	2	2	0.390		80
VW Peg	9.9	50706.165	21.071748	D	16	19	0.271	(a)	143
BK Peg	9.97	41587.726	5.4899085	A:	24	28	var		144
AG Per	6.69	24946.515	2.0287296	A	54	52	var		66
CR Per	12.4	56305.373	8.809700	D	9	8	0.644	(a); (w)	123
IM Per	12.0	33541.370	2.2542275	A	61	41	var		145
IQ Per	7.72	44290.364	1.7435633	A	79	30	var		66
NO Per	11.5	51515.750	5.692295	D	8	6	0.356		146
V436 Per	5.49	43561.733	25.93596	D	12	3	0.413		147
V751 Per	11.5	51508.460	5.961338	D	4	4	0.451		19
V754 Per	12.0	53391.851	5.336624	D	5	4	0.410		4
V871 Per	10.9	51421.540	3.0239166	A	16	16	var		52
V884 Per	10.7	51466.910	12.80698	D	4	2	0.539		64
V966 Per	13.0	54157.901	4.309062	D	3	3	0.325:		148
V982 Per	12.8	54277.205	4.606663	D	4	4	0.365		149
SY Phe	9.75	54163.265	5.2708856	A:	14	12	var	(x)	150
AI Phe	8.58	43410.190	24.59232	D	10	3	0.462		151
ζ Phe	3.91	41643.699	1.6697695	A+III	30	20	var		152
VZ PsA	5.68	48810.941	5.76333	D	1	1	0.573:	(y)	19
KX Pup	12.8	41686.820	2.146795	A:	14	5	var		57
LN Pup	12.5	51873.586	3.951123	A:	12	8	var		86
NO Pup	6.53	41361.815	1.256879	A	20	10	var		37
PV Pup	6.88	43119.710	1.6607283	A+III:	7	9	var		188
V358 Pup	9.30	50818.713	6.7939111	A	14	12	var		153
V365 Pup	7.82	48201.637	30.0338	D	3	1	0.434:		31
V366 Pup	8.07	47860.510	2.483968	A	10	7	var		37
V397 Pup	5.91	48799.940	3.004373	D	5	5	0.680		167
V399 Pup	9.27	47889.838	3.910095	A	15	13	var		154
V438 Pup	5.90	47975.900	4.934993	D	4	3	0.324		61
V596 Pup	6.57	44620.614	4.596174	A:	9	7	var	(z)	155
V611 Pup	8.11	52540.600	6.317750	D	3	3	0.418		31
V642 Pup	10.2	51924.896	5.414142	D	2	1	0.424:		79
TZ Pyx	10.7	52500.360	2.318556	A	38	43	var	(a)	29
AC Pyx	7.80	48502.796	7.667980	D	3	2	0.384		31
DK Pyx	7.85	48112.305	6.178477	D	2	2	0.291		19
VY Ret	7.89	52900.394	14.21605	D	4	2	0.727		79
V370 Sge	11.7	52734.448	8.326220	D	4	3	0.380		19
YY Sgr	10.0	19467.028	2.628475	A+III	52	42	var		156; 157
V523 Sgr	9.57	15971.568	2.3238134	A	29	31	var		156
V526 Sgr	9.78	47739.658	1.9194119	A	56	60	var		14
V1108 Sgr	11.6	26568.560	46.5832	D	2	2	0.518:		158
V1647 Sgr	6.94	41829.304	3.282805	A	13	15	var		156
V2184 Sgr	12.5	53212.280	16.49541	D	4	4	0.234		190
V2283 Sgr	10.2	38948504	3.4714362	A	44	31	var		156
V3895 Sgr	9.0	53578.090	27.11104	D	6	3	0.408		19
V5565 Sgr	10.4	52819.606	4.302860	D	4	3	0.393		79; 86
V5570 Sgr	8.60	52474.238	11.78983	D	3	2	0.432		31
V5643 Sgr	9.53	52562.152	1.9185860	D	4	3	0.452		1
V5695 Sgr	12.8	54350.910	8.31936	D	2	1	0.574:		159
V5697 Sgr	11.9	54652.801	3.682577	D	3	2	0.587		159
V385 Sco	10.9	53268.244	4.6902416	A:	6	7	var	(a); (aa)	29
V629 Sco	11.9	27601.434	3.249126	A	7	7	var		29
V760 Sco	7.04	43250.836	1.7309349	A	59	66	var		156
V881 Sco	8.8	28772.543	2.491561	A	13	13	var		29
V883 Sco	7.39	53685.193	4.3411725	A	22	16	var	(a)	1
V923 Sco	5.86	54269.212	34.83865	D	2	3	0.371:		160
V1046 Sco	9.34	48528.240	11.11645	D	5	2	0.474		61
V1067 Sco	10.4	47925.720	12.05336	D	2	3	0.438:		80
V1082 Sco	10.1	52094.431	23.446225	D	9	10	0.340		29
V1195 Sco	8.86	47963.162	4.003050	D	3	2	0.403		61
V1270 Sco	9.17	52441.559	4.243145	A	5	3	var		1
V1284 Sco	9.54	52722.851	3.729446	D	2	1	0.494:		54
V1296 Sco	12.2	52071.815	5.808091	D	2	1	0.448:		79
V1299 Sco	11.7	52501.714	7.694733	D	2	1	0.558:		79
V1301 Sco	13.0 :	53634.577	1.954066	D	2	2	0.551		19
V1303 Sco	11.7	51977.942	11.09423	D	2	1	0.342:		19
V1306 Sco	11.2	52117.205	5.541743	D	2	1	0.372:		5
V1308 Sco	10.4	52549.397	9.106745	D	2	1	0.471:		5
V1611 Sco	13.1	54570.416	10.70732	D	3	2	0.639		161
AL Scl	6.06	43698.483	2.4450873	D	9	3	0.474		162; 163
CG Scl	8.67	52227.518	11.035697	D	4	3	0.487		1
CI Scl	8.78	52558.840	14.710724	D	5	2	0.379		31
CM Scl	8.81	48077.000	10.288588	D	3	2	0.391		6
CR Sct	11.6	28719.496	4.1923465	A:	14	12	var		10
V490 Sct	13.4	27752.726	12.044118	D	9	7	0.324	(ab)	158
V493 Sct	8.49	52560.294	30.811396	D	3	1	0.749:		79
V335 Ser	7.6	50304.420	3.4498775	A	19	12	var		164; 165
V413 Ser	7.95	49038.828	2.259760	A	24	18	var		166
V1094 Tau	8.95	49702.430	8.9885422	D	22	16	0.652		22; 183
V1154 Tau	6.71	52634.367	1.7679018	A:	11	8	var		184
V1260 Tau	10.2	53347.880	5.4308176	D	8	5	0.555		5
V1287 Tau	8.53	53354.145	13.06200	D	3	3	0.412		1
V1356 Tau	10.9	52645.939	12.80737	D	6	7	0.561		64
LU Tel	12.4	53334.598	1.5717434	D	4	2	0.483:		1
V351 Tel	10.0	52104.646	6.447755	D	5	2	0.511:		31
V356 Tel	9.64	52124.206	23.193696	D	2	1	0.470:		54
V359 Tel	8.54	52109.550	19.24494	D	3	2	0.785		19
SS TrA	10.5	52039.370	8.601227	D	7	4	0.207	(a)	86
MN TrA	8.50	48006.315	2.379818	A:	8	9	var		39
MP TrA	7.76	48077.832	2.069725	D	7	2	0.442:		61
NT TrA	9.20	52062.657	3.229993	D	8	5	0.568:		31
PS UMa	12.5	51628.486	9.271883	D	3	3	0.467		19
YZ Vel	12.2	26363.558	5.488359	D	7	8	0.540		124
AO Vel	9.35	45043.661	1.584612	A+III	50	44	var	(ac)	14; 168
EO Vel	11.4	41713.900	5.329687	D	14	5	0.609		86
ET Vel	11.9	29778.251	3.080878	A	21	10	var		169
GT Vel	9.7	51874.760	4.670074	A:	12	6	var		80; 86
NT Vel	8.33	52710.148	9.255699	D	4	3	0.598		79
PQ Vel	7.66	48257.640	22.26312	D	4	1	0.584:		31
PT Vel	7.05	48293.487	1.8020232	A	11	7	var		170
V403 Vel	9.63	51981.630	7.2025482	D	4	3	0.515		79
V404 Vel	9.37	52714.580	11.423609	D	2	1	0.493:		31
V409 Vel	12.4	52929.545	2.7867265	D	3	1	0.285:		54
δ Vel	1.96	47830.700	45.15005	D	5	5	0.434		171
WZ Vol	8.31	48692.900	226.2416	D	4	2	0.295		5; 172
BP Vul	10.1	46003.229	1.9403458	A	55	35	var		173
DR Vul	8.65	48989.056	2.2508707	A+III	98	92	var	(ac)	24; 127
EQ Vul	11.8	35343.855	9.297184	A	41	50	var		95
FQ Vul	12.3	34238.501	6.262628	A	23	6	var		174
FW Vul	12.7	34706.179	4.5261448	D	9	3	0.496:		1
V399 Vul	7.01	52860.478	4.904902	D	4	2	0.437:		175
V491 Vul	9.94	51510.857	7.6700251	D	5	7	0.337		19
V495 Vul	9.76	54651.500	1.635133	A	16	20	var		176

Note. Remarks: (a) new period; (b) old name: DM Cas; (c) star in the region of the open cluster Tr 18; (d) star in the region of the open cluster NGC 3572; (e) star in the η Carinae Nebula; (f) region of the open cluster NGC 381; (g) star in the region of the open cluster NGC 7790; (h) minima disappear?; (i) star in the region of the open cluster Stock ;, (j) star in the field of the open cluster Stock 14; (k) GCVS identifies the star as NSV 20084 rather than ψ Cen; (l) star in open cluster NGC 6871; (m) elliptical orbit not confirmed; (n) star in open cluster NGC 6819; (o) star in quadruple or quintuple system; (p) incorrect name: KM Hya (see: IBVS 2015); (q) probable member of the open cluster NGC 7209; (r) minima disappear; (s) KIC 6766748; (t) in NGC 2244; (u) RR-type in the GCVS; (v) in NGC 2264; (w) star in the region of the open cluster Stock 2; (x) ISB:—type in the GCVS 5.1; (y) uncertain, two minima only; (z) old name: VV Pyx; (aa) star in the region of the open cluster CR 338; (ab) old name: V1049 Sgr; (ac) quadruple system.

References. (1) This paper; (2) Crawford et al. (1984), (3) Husar (2005), (4) Nakajima et al. (2006), (5) Otero & Wils (2005a), (6) Otero & Wils (2005b), (7) Bulut (2009), (8) Volkov & Chochol (2014), (9) Southworth (2013), (10) Wolf et al. (2004), (11) Wolf et al. (2005), (12) Lloyd et al. (2002), (13) İbanoǧlu et al. (2007), (14) Wolf & Zejda (2005), (15) Hauck (2011a), (16) Clausen et al. (2001), (17) Wolf et al. (2011), (18) Sipahi & Dal (2013), (19) Otero et al. (2006), (20) Glazunova (2011), (21) Volkov et al. (2011), (22) Wolf et al. (2010a), (23) Imbert (1987), (24) Bozkurt & Değirmenci (2007), (25) Otero (2008), (26) Khruslov (2010), (27) Sowell et al. (2012), (28) Clausen et al. (2008), (29) Zasche (2012a), (30) Bakış (2015), (31) Otero & Dubovsky (2004), (32) Bakış et al. (2010), (33) Otero (2004), (34) Diethelm (2011), (35) Liška et al. (2013), (36) Andersen & Clausen (1989), (37) Wolf et al. (2008), (38) Woodward & Koch (1993), (39) Bulut & Demircan (2008), (40) Otero (2006), (41) Krylov et al. (2003), (42) Cowley et al. (1977), (43) Walter (2012), (44) Lacy et al. (2004), (45) Švaříček et al. (2008), (46) Yıldız (2005), (47) Kjurkchieva et al. (2007), (48) Guinan et al. (2012), (49) Wolf et al. (2010d), (50) Dariush et al. (2006), (51) Bulut et al. (2006), (52) Wolf et al. (2013), (53) Bulut (2013), (54) Otero et al. (2005), (55) Andersen et al. (1987); (56) Kozyreva et al. (2013), (57) Söderhjelm (1975), (58) Giménez et al. (1986), (59) Uitterdijk (1936), (60) de Kort (1937a), (61) Otero (2003), (62) Mayer et al. (2010a), (63) Khaliullin et al. (2006), (64) Otero et al. (2004), (65) Bruntt et al. (2006), (66) Wolf et al. (2006b), (67) Han et al. (2015), (68) Giménez & Margrave (1985), (69) Lacy et al. (2006), (70) Ahn (1992), (71) Henden et al. (1999), (72) Bakış et al. (2008b), (73) Bulut & Bulut (2015), (74) Kozyreva & Kusakin (2016), (75) Volkov et al. (2015), (76) Kozyreva & Kusakin (2014), (77) Dvorak (2004), (78) Paschke (2006), (79) Otero & Claus (2004), (80) Hoogeveen (2005), (81) Volkov (2005), (82) Schmitt et al. (2016), (83) Fekel et al. (2013), (84) Oosterhoff & van Houten (1949), (85) de Kort (1937b), (86) Shivvers et al. (2014), (87) Clausen et al. (2007), (88) Harmanec et al. (2014), (89) Wolf (2009), (90) Tkachenko et al. (2014), (91) Claret & Giménez (2010), (92) Zasche & Wolf (2011), (93) Diethelm (1993), (94) Kuznetsov et al. (2011), (95) Wolf et al. (1998), (96) Wetterer et al. (2006), (97) Meinunger (1968), (98) Hill & Fisher (1984), (99) Çakırlı (2015), (100) İbanoǧlu et al. (2008), (101) Dumont et al. (2011), (102) Gómez-Forrellad et al. (2003), (103) Lacy et al. (2012b), (104) Morales et al. (2009), (105) Dallaporta et al. (2000), (106) Milone et al. (2010), (107) Volkov & Volkova (2009), (108) Goranskij et al. (2005), (109) Galan C. et al. (2008); (110) Claret et al. (2010), (111) Khaliullin & Khaliullina (2006), (112) Torres et al. (2009), (113) Lacy & Fekel (2014), (114) Zasche & Uhlař (2016), (115) Khaliullin & Kozyreva (1989), (116) Andersen & Vaz (1984), (117) Wolf et al. (2006a), (118) Milone et al. (2000), (119) Zasche (2010), (120) Kozyreva & Khaliullin (2007), (121) Agerer & Berthold (2005), (122) Kozyreva et al. (2005), (123) Kasai & Nagai (2016), (124) Hegedüs (1988), (125) Bulut & Demircan (2006), (126) Khaliullin et al. (2001), (127) Wolf et al. (1999), (128) Wolf et al. (2010c), (129) Torres et al. (2015), (130) Hassforther (2004), (131) Pribulla et al. (2010), (132) Garcia et al. (2011), (133) de Kort (1954), (134) Zasche et al. (2011), (135) Otero (2007), (136) Wolf et al. (2001), (137) Volkov & Volkova (2010), (138) Harmanec et al. (2011), (139) Sabby et al. (2011), (140) Torres et al. (2014), (141) Mayer et al. (2010b), (142) Pablo et al. (2015), (143) Achterberg et al. (2000), (144) Clausen et al. (2010), (145) Lacy et al. (2015), (146) Khruslov (2006), (147) Janík et al. (2003), (148) Siviero et al. (2010), (149) Paschke (2015), (150) Zasche (2012b), (151) Kirkby-Kent et al. (2016), (152) Zasche & Wolf (2007), (153) Zasche et al. (2015), (154) Bulut et al. (2014), (155) Andersen et al. (1984), (156) Wolf (2000), (157) Wolf et al. (2006c), (158) Uitterdijk (1949), (159) Kazarovets & Pastukhova (2013), (160) Fekel et al. (2011), (161) Kazarovets & Pastukhova (2012), (162) Haefner (1981), (163) de Groot (1985), (164) Bozkurt (2011), (165) Lacy et al. (2012a), (166) Çakırlı et al. (2008), (167) Otero (2005), (168) Bulut et al. (2011), (169) Zasche (2009), (170) Bakış et al. (2008a), (171) Pribulla et al. (2011), (172) Hauck (2011b), (173) Csizmadia et al. (2009), (174) Petrova & Orlov (1999), (175) Çakırlı et al. (2012), (176) Soydugan et al. (2015), (177) Claret et al. (1995), (178) Guinan et al. (2000), (179) Mayer et al. (2016), (180) Torres (2001), (181) Torres et al. (2017), (182) Volkov et al. (2010), (183) Maxted et al. (2015), (184) Dallaporta et al. (2003), (185) Ogłoza & Zakrzewski (2004), (186) Wolf et al. (2010b), (187) Söderhjelm (1974), (188) Vaz & Andersen (1984), (189) Khruslov (2012), (190) Khruslov (2011), (191) Khruslov (2007), (192) Volkov et al. (2017), (193) Wolf et al. (2017), (194) Hoyman et al. (2018).

Download table as: ASCIITypeset images: 1 2 3 4 5 6 7

Table 4. Eclipsing Binaries with Elliptical Orbits without GCVS Names

Name	Max. Mag.(B)	T₀	Period	Type	Number		Phase	Remark^a	References
	(SIMBAD)	(HJD2400000+)	(day)		Pri	Sec
2MASS J00372334+4719206	14.1	53277.868	5.8620643	D	4	4	0.519		14
2MASS J00435925+5114000	13.1	53278.014	2.3588705	D	6	5	0.522		14
2MASS J00470861+5037193	12.2	53277.304	2.2171898	D	17	15	0.640		14
2MASS J00471033+5045123	14.1	53278.518	3.2845636	D	5	5	0.554		14
2MASS J00582982+4925088	15.8	52903.336	18.002176	D	2	3	0.552		14
2MASS J01100914+4818196	15.6	52909.251	11.415996	D	3	2	0.511:		14
2MASS J01173524+4946169	14.2	52905.608	7.8660747	D	5	2	0.504:		14
2MASS J01552928+3750262	10.3	54040.793	15.535326	D	5	1	0.857:	(a)	6
2MASS J02362545−7058141	11.6	54599.349	23.304104	D	2	2	0.212		1
2MASS J03040429−3847265	11.2	53529.425	9.4222528	D	6	4	0.530		1
2MASS J03111389−7402395	11.2	54327.868	28.965206	D	2	2	0.378		1
2MASS J03314391+3631523	12.0	53360.246	3.6474665	D	11	10	0.486		14
2MASS J03341943+3932444	9.85	53353.152	8.4717939	D	2	1	0.462:		14
2MASS J03353366+4000491	14.0	53361.452	4.0698441	D	20	8	0.495		14
2MASS J03404564+3447572	15.8	53358.946	3.9449363	D	4	4	0.479		14
2MASS J03475647+3731318	15.1	53356.360	4.2466720	D	8	8	0.347		14
2MASS J03520066+4003477	14.1	53356.897	4.4568511	D	11	11	0.456		14
2MASS J04223522−4129001	11.1	54040.623	17.554555	D	4	4	0.166		1
2MASS J04233735+2546360	14.7	53735.316	3.2174300	A:+III	8	8	var		14
2MASS J04370204+4205520	11.0	54371.714	1.4547185	A:	12	8	var		12
2MASS J05035114−1541539	10.3	52520.535	7.2792229	D	2	2	0.378:		4
2MASS J05175294−5406053	10.9	52514.755	26.131315	D	2	2	0.698		1
2MASS J05542642+2236022	10.9	53509.897	9.3968497	D	4	3	0.458		1
2MASS J05581929−1446398	12.1	54144.979	6.4048907	D	2	2	0.596		1
2MASS J06071859+1331458	9.52	53172.249	5.0779738	D	2	2	0.364		4
2MASS J06101649−3321209	11.3	54327.82	199.90075	D	5	3	0.428		4
2MASS J06172735+1100176	11.4	53287.061	15.719375	D	2	2	0.667:		4
2MASS J06194134−1107556	11.4	52602.372	2.5891690	D	3	3	0.441		1
2MASS J06200484+0454446	9.32	54520.575	5.9415040	D	2	2	0.615		4
2MASS J06211443−0534451	13.08	54249.729	2.4638010	D	2	2	0.352		4
2MASS J06242824+1217124	8.7	53233.219	5.6351910	D	2	2	0.543		1
2MASS J06275377+0028136	9.9	53059.628	2.9425503	D	2	2	0.482		1
2MASS J06292635−2513294	12.0	54355.995	26.381464	D	3	4	0.365		4
2MASS J06300270−4959171	8.64	52613.483	41.744017	D	2	2	0.686		4
2MASS J06320180−6750381	11.2	52657.284	5.8190621	D	2	2	0.566		4
2MASS J06335056+0501376	11.6	33701.422	25.951174	D	2	2	0.265	(b)	6
2MASS J06405707−2637345	11.0	53862.961	12.445562	D	4	4	0.669		4
2MASS J06430543−0034399	13.3	51618.030	28.917630	D	2	1	0.210:		9
2MASS J06445048−1454157	10.4	52673.582	7.3490852	D	2	2	0.557		1
2MASS J06460938−1923500	8.8	52480.426	2.9039009	D	4	3	0.520		17
2MASS J06475256−1642563	10.6	52785.075	1.8434251	D	3	3	0.423		4
2MASS J06492563−0013367	10.9	52726.890	2.1959315	D	3	3	0.538		1
2MASS J06500763−1351306	10.6	52338.601	1.8238679	D	3	3	0.535		1
2MASS J06531687−1935083	8.9	54339.676	17.777981	D	2	2	0.874		1
2MASS J06574910−0014333	11.2	54278.208	8.2278077	D	2	2	0.847		1
2MASS J07012704−0307032	7.57	52979.874	21.963929	D	2	2	0.296		4
2MASS J07060295−0928283	9.64	54303.477	11.639631	D	2	2	0.508		1
2MASS J07065419−1020296	10.6	52680.242	3.3773007	D	3	3	0.522		1
2MASS J07091421−0707589	11.6	54634.746	5.8660315	D	4	4	0.479		1
2MASS J07151012−2259093	9.0	53414.227	5.5131170	D	2	2	0.775		1
2MASS J07203341−4616474	10.5	54538.652	57.851780	D	2	2	0.528		1
2MASS J07205622+0326048	11.1	54266.832	18.955264	D	2	2	0.407		1
2MASS J07222169−1159457	9.04	52554.315	13.014502	D	2	2	0.682		4
2MASS J07251501−1135496	10.6	53368.994	4.5099820	A	6	6	var		13; 4
2MASS J07255988−1741490	11.0	54302.834	28.879732	D	2	2	0.239		1
2MASS J07290342−1525227	10.8	54305.245	8.8511191	D	2	2	0.374		4
2MASS J07303245−1611383	12.7	54306.718	2.6862032	D	3	3	0.336		4
2MASS J07321787−1436291	11.2	53422.143	8.1779105	D	3	3	0.418		4
2MASS J07330825−0532311	11.1	52896.065	26.916869	D	1	2	0.431:		1
2MASS J07360305−5710149	11.9	52390.174	2.7642236	D	3	3	0.470		1
2MASS J07361070−3123217	11.0	54418.189	8.8552171	D	2	2	0.697		4
2MASS J07412319+0253210	11.7	53275.653	8.5992814	D	3	2	0.564		4
2MASS J07440045−3105246	10.6	54157.714	6.2041862	D	2	2	0.701		4
2MASS J07484467−3801481	10.6	52332.984	3.2050360	D	3	3	0.475		1
2MASS J07493519−2415509	11.0	54443.404	7.2735586	D	2	2	0.198		4
2MASS J07505239+0048040	9.36	54390.442	2.0543260	D	3	4	0.419		4
2MASS J07520655−3032111	10.7	54402.181	10.693038	D	2	2	0.616		4
2MASS J07594157−1411076	12.5	54289.867	4.4057816	D	2	2	0.699		4
2MASS J08065094−4503020	9.8	52620.104	3.6285890	D	2	2	0.599		1
2MASS J08114480−2519465	10.0	54481.332	9.7998670	D	2	2	0.725		4
2MASS J08123735−1356531	12.1	52570.282	9.6467758	D	3	3	0.408		4
2MASS J08163100−3314381	11.4	52586.186	189.30119	D	2	2	0.384		1
2MASS J08173168−6043507	10.5	52657.197	8.3773516	D	2	2	0.639		4
2MASS J08185532−3612483	10.9	54264.455	9.3534665	D	3	3	0.395		4
2MASS J08242802−4525115	11.8	52634.641	3.4510924	D	2	2	0.655		4
2MASS J08314982−1529000	11.5	52523.616	8.7408869	D	3	3	0.367		4
2MASS J08340056−3431241	10.6	54345.918	3.1376346	D	2	3	0.697		4
2MASS J08355532−2755526	9.2	54302.757	16.373716	D	2	2	0.528		1
2MASS J08361133−4547386	10.4	52420.444	6.9555034	D	2	2	0.283		4
2MASS J08404888−4259265	9.5	52657.915	13.797958	D	2	2	0.476		1
2MASS J08442378−3715247	10.6	54372.683	5.7287784	D	2	2	0.619		4
2MASS J08450318−4112597	10.0	52653.335	2.0665963	D	2	2	0.582	(c)	4
2MASS J08453462−2158013	13.0	54402.438	11.042005	D	2	3	0.861		1
2MASS J08515414−4231396	12.0	53409.404	36.783930	D	2	2	0.611		1
2MASS J08542696−4134581	11.0	54381.433	3.4523128	D	2	2	0.401		4
2MASS J09023164−5653225	11.0	53693.985	20.822341	D	2	2	0.507		1
2MASS J09122733−3801412	12.0	54027.800	4.6252704	D	4	3	0.413		4
2MASS J09131290−4744240	10.3	54311.133	2.4159664	D	2	2	0.404		4
2MASS J09170374−5454045	10.8	54220.066	12.354960	D	2	2	0.304:		4
2MASS J09181467−3350293	9.44	54106.214	7.9006282	D	6	2	0.656		11
2MASS J09245390−7128195	11.16	54192.195	6.2940346	D	2	2	0.720		1
2MASS J09262232−5258402	10.0	52760.207	2.3154122	D	2	2	0.491		1
2MASS J09305154−3234215	10.0	54457.346	4.0217218	D	6	7	0.409		4
2MASS J09315590−2656448	10.5	53819.011	17.012082	D	5	3	0.602		1
2MASS J09345147−5424158	11.0	52467.340	2.8424552	D	3	3	0.488:		1
2MASS J09481015−5117218	9.75	53830.355	7.1491716	D	2	2	0.392		4
2MASS J09533771+5245447	16.9	53449.170	9.5528882	D	3	3	0.598		14
2MASS J10010408−5847259	10.1	53477.874	14.320070	D	3	3	0.611		4
2MASS J10024347−5643283	11.9	52806.140	10.940051	D	2	2	0.324		4
2MASS J10042062−3319007	10.1	54145.853	6.7148901	D	9	10	0.583		4; 11
2MASS J10043150−6921202	9.54	53418.870	11.510612	D	3	2	0.220		1
2MASS J10043285−6315432	9.3	54398.316	13.807582	D	2	2	0.778		4
2MASS J10062533−5500446	11.5	54235.230	4.4111902	D	2	2	0.712		4
2MASS J10200389−5737255	11.4	52772.304	13.126427	D	2	2	0.537		1
2MASS J10273191−6400217	10.9	54269.989	5.6468958	D	2	2	0.602		4
2MASS J10344865−6013038	10.0	52945.824	7.5937321	D	2	2	0.393		4
2MASS J10370007−6530057	10.0	53697.532	16.972508	D	2	2	0.777		1
2MASS J10471675−5453183	10.1	54420.492	2.4320280	D	2	2	0.570		1
2MASS J10491406−6744502	11.9	53385.567	13.181955	D	2	2	0.534		1
2MASS J10583499+0329220	12.2	53223.917	24.373083	D	2	2	0.617:		4
2MASS J10591890−5845044	11.8	52449.255	2.8498240	D	3	3	0.455		1
2MASS J10593360−5844304	11.6	54364.334	2.8498169	D	2	2	0.457		1
2MASS J11061317−3158400	12.4	53186.571	7.3017854	D	7	5	0.274		1
2MASS J11081163−3014401	11.3	52686.863	6.2149254	D	6	6	0.329		4
2MASS J11101237−6051471	9.52	54500.061	5.3829054	D	2	2	0.685		4
2MASS J11113415−4956110	8.71	52829.356	7.7357413	D	2	2	0.482		1
2MASS J11150698−4815333	12.1	54369.074	6.7867640	D	2	2	0.580		4
2MASS J11214548−0850136	11.3	54395.241	8.3687688	D	3	3	0.574		4
2MASS J11255084−5922107	10.5	52853.249	4.5563989	D	2	2	0.530		1
2MASS J11292643−6201579	11.5	52497.398	3.2247787	A:	3	3	var		4
2MASS J11351107−5254405	12.0	54556.771	6.7940023	D	2	2	0.411		1
2MASS J11421027−6129302	11.5	52691.987	4.3010512	D	2	2	0.455		1
2MASS J11500699−6425050	11.2	52912.366	6.9052344	D	2	2	0.570:		4
2MASS J12022247−3122251	11.2	53451.984	15.514517	D	4	5	0.314		1
2MASS J12035553−6303028	9.7	53821.882	48.338320	D	2	2	0.504:		1
2MASS J12043357−5241389	10.2	53689.770	7.8944208	D	3	2	0.537		1
2MASS J12053548−6209562	11.2	53871.120	9.9014342	D	2	2	0.437		1
2MASS J12254009−6337334	9.46	52692.641	3.0815849	D	2	2	0.640		4
2MASS J12272884−6412054	12.2	52683.658	15.803677	D	2	2	0.694:		4
2MASS J12274253−6223576	11.4	54252.298	15.550227	D	2	2	0.326		4
2MASS J12482920−6652312	11.3	53577.975	16.504029	D	2	2	0.467		1
2MASS J12515020−4249201	11.4	53943.323	15.723133	D	5	4	0.587		1
2MASS J12542625−5918096	10.3	52521.213	3.0489425	D	3	3	0.472		1
2MASS J13200195−6144515	10.6	52812.115	7.3082481	D	2	2	0.257		4
2MASS J13222883−3925543	11.1	52906.820	5.8121319	D	7	6	0.489		1
2MASS J13353298−5214286	10.7	54229.332	11.440486	D	2	2	0.676	(d)	4
2MASS J13521648−3351386	10.2	54547.058	2.5416458	D	4	1	0.569:		11
2MASS J13581727−3004356	9.06	54224.573	10.286937	D	4	5	0.606		4
2MASS J14055562−6143592	9.84	52413.180	2.1854308	D	3	3	0.460		1
2MASS J14073719−6957341	10.4	54494.875	6.5165640	D	2	2	0.406		4
2MASS J14080858−5906145	11.0	53485.256	8.0909048	D	3	3	0.527		1
2MASS J14163937−4854118	9.8	54253.579	7.6615686	D	2	2	0.559		1
2MASS J14172205−6247429	10.1	52495.357	2.3125837	D	3	3	0.472		1
2MASS J14192329−4642211	11.8	54162.238	7.0807075	D	3	3	0.395		1
2MASS J14230017−4635290	9.91	52174.986	2.2740250	D	10	9	0.461		1
2MASS J14262665−6108242	10.7	54367.615	20.492228	D	2	2	0.257		1
2MASS J14265471−5821490	11.3	52510.141	2.4699821	D	3	3	0.485:		1
2MASS J14265505−6735180	11.2	52489.848	3.8768492	D	3	3	0.573		4
2MASS J14293254−6014360	11.5	54388.346	14.167995	D	2	2	0.778		4
2MASS J14394430−2837082	9.36	46136.620	16.365063	D	4	5	0.442		11
2MASS J14424230−5904033	10.1	54674.766	7.2727806	D	2	2	0.878		4
2MASS J14444107−7721530	12.5	52554.874	10.022060	D	2	2	0.327		4
2MASS J15004561−5014530	8.57	52568.645	9.2879924	D	2	2	0.566		4
2MASS J15053934−6845552	9.35	54383.760	5.4939459	D	2	2	0.492		1
2MASS J15130781−2504191	12.0	54569.958	12.725384	D	4	4	0.696		4
2MASS J15150986−5928476	10.9	52684.398	8.7058893	D	2	2	0.610		4
2MASS J15154331−2035266	10.8	52785.415	17.208106	D	4	4	0.288		4
2MASS J15184839−4942140	11.8	52945.651	21.075039	D	2	2	0.469		1
2MASS J15261758−2459188	9.26	52697.568	7.0694570	D	6	4	0.478		1
2MASS J15291701−7230462	10.3	54480.571	37.715870	D	2	2	0.479		1
2MASS J15325748+7042157	9.41	56423.591	16.25672	D	2	3	0.544		10
2MASS J15391113−6259184	10.5	52744.268	8.0903098	D	2	2	0.534		1
2MASS J15450311−5249284	9.74	52768.813	2.9053469	D	2	2	0.529		1
2MASS J15495183−2323182	11.4	53902.202	8.0185848	D	5	4	0.479		1
2MASS J15502226−5653002	11.0	52986.084	7.8919824	D	2	2	0.472		1
2MASS J16021189−4442468	10.9	52397.375	4.1740043	D	3	3	0.436		1
2MASS J16111795+3307131	13.3	53505.897	8.2836696	A:	3	5	var		7
2MASS J16170981−3840536	11.0	52528.618	3.4875993	D	6	6	0.532		1
2MASS J16475143−4158417	10.0	52444.177	2.0366694	D	3	3	0.476:		1
2MASS J16475313−3239388	12.1	52817.596	3.9442377	D	2	2	0.681		4
2MASS J16533637−4615536	11.6	52705.289	2.3302075	D	2	2	0.577		4
2MASS J16535419−1301575	10.6	54111.192	2.2075680	D	4	3	0.373		4
2MASS J17033584−3638466	11.0	52569.618	7.3946798	D	2	2	0.403		1
2MASS J17114503−2819017	11.4	53367.497	3.1451058	D	2	2	0.655		4
2MASS J17203361−4206111	10.7	54340.654	5.5397338	D	2	2	0.565		4
2MASS J17260899+0659294	10.5	53238.060	3.0409480	D	2	2	0.556		1
2MASS J17331903−4315014	9.83	54431.938	12.776436	D	2	2	0.622		4
2MASS J17533294−2031094	12.2	54126.515	3.3157120	D	3	3	0.317		4
2MASS J17562956−5509415	11.2	54470.025	11.178200	D	2	2	0.564		4
2MASS J18001019−2353463	11.0	52622.813	9.9213567	D	2	2	0.566		1
2MASS J18041338−1557195	11.4	53920.657	49.109261	D	2	1	0.485:		1
2MASS J18074355−2712020	9.98	54259.971	6.9237241	D	2	2	0.349		4
2MASS J18081458−1712030	11.6	54245.281	3.3342176	D	2	2	0.654		4
2MASS J18090792−2128247	11.0	53892.931	2.2703680	D	6	6	0.376		3; 4
2MASS J18142442−3713180	11.4	52842.977	4.4719694	D	2	2	0.548		1
2MASS J18155492−1826008	8.50	52797.310	4.6717110	D	2	2	0.508		1
2MASS J18271844+1908333	12.0	54529.986	7.1461186	D	5	4	0.543		18
2MASS J18302058−0923095	12.0	54229.629	20.122794	D	3	3	0.338		4
2MASS J18311343−4917286	11.4	52491.381	8.6973910	D	2	2	0.254		1
2MASS J18323477−3314408	10.2	52785.544	3.6898498	D	2	2	0.627		4
2MASS J18325868−3125437	10.1	52823.939	6.5302464	D	2	2	0.540		1
2MASS J18335606−2922420	11.0	52814.176	14.897254	D	2	2	0.630		4
2MASS J18370026−4855284	10.4	52610.720	2.3904736	D	3	3	0.472		1
2MASS J18432690+0841321	10.3	53147.312	2.1391991	D	4	3	0.460		17
2MASS J18510539−1818454	11.5	54642.164	4.5623731	D	3	2	0.249		4
2MASS J18524030+0403118	8.14	54204.752	3.6570666	D	3	1	0.538:		2
2MASS J18574027+4840512	14.6	53579.568	8.0495909	D	4	2	0.624	(e)	14
2MASS J18590844+4836000	14.6	35807.296	11.631838	D	6	3	0.360	(f)	14
2MASS J18594647−4740371	11.9	52817.226	4.6946372	D	2	2	0.474		1
2MASS J18595128−4711476	11.8	54207.653	2.8776812	D	2	2	0.600		4
2MASS J19033272+3941003	11.0	55341.769	2.1891140	A:	44	44	var	(g)	5; 16
2MASS J19034114+4736557	14.5	53582.237	40.043374	D	4	2	0.122	(h)	14
2MASS J19042153−3411509	10.6	53903.644	5.0208198	D	4	6	0.552		11
2MASS J19062655+4828470	14.8	53577.881	6.6403103	D	4	7	0.477	(i)	14
2MASS J19105428+4926069	15.7	53576.493	12.318191	D	1	3	0.630:	(j)	14
2MASS J19304303−0615348	11.6	54541.818	7.2765349	D	3	3	0.595		4
2MASS J19372693+0321445	10.8	52881.947	3.2884026	D	3	3	0.527:		1
2MASS J19393409−1739553	11.6	54623.447	10.703580	D	3	3	0.371		4
2MASS J19411609+1301187	9.94	53255.645	1.5609128	D	3	3	0.587		4
2MASS J19534199+0205213	9.58	53563.388	1.6081244	D	3	4	0.476		17
2MASS J19544593+5024053	14.0	53210.725	6.0559005	D	3	3	0.395	(k)	14
2MASS J19554410+5213346	12.2	53210.408	4.4359437	D	9	6	0.497	(l)	14
2MASS J19561308+1630560	9.98	54220.421	3.4445896	D	3	3	0.496		17
2MASS J19585801+4738192	13.7	53211.416	4.9252380	D	11	13	0.505	(m)	14
2MASS J19592592+5223599	11.6	53203.328	11.608127	D	5	6	0.512	(n)	14
2MASS J20020438+4734147	13.7	53212.898	5.5989031	A:	5	4	var	(o)	14
2MASS J20030311+5242041	11.6	53207.175	14.507469	D	1	2	0.506:	(p)	14
2MASS J20072552+5222005	12.9	53215.332	6.5133398	D	8	2	0.495	(q)	14
2MASS J20093821+4905080	11.9	53207.296	12.440529	D	4	2	0.719:	(r)	14
2MASS J20104420+5107517	13.5	53211.541	4.5497242	D	6	3	0.467	(s)	14
2MASS J20104691+4909294	14.1	53208.569	11.619160	D	3	4	0.694	(t)	14
2MASS J20135245+5052231	14.2	53201.858	9.3572418	D	3	1	0.344:	(u)	14
2MASS J20321743+5053479	12.5	56374.966	10.89924	D	3	3	0.409		21
2MASS J20564198+1153023	9.16	54668.305	4.1243839	D	4	3	0.615		4
2MASS J21245175+1916139	11.7	53127.869	3.2130647	D	4	4	0.525		1
2MASS J21264316−0031104	11.7	52910.608	8.3588725	D	4	4	0.574		1
2MASS J21334898−0720407	11.7	51508.478	32.396226	D	2	3	0.653		1
2MASS J21544298+0410320	11.7	54589.468	6.9575534	D	4	4	0.557		1
2MASS J22250315−5348368	8.9	53482.540	8.8834455	D	2	3	0.404		1
2MASS J22335143−2351527	11.6	54540.388	10.351715	D	5	5	0.516		1
2MASS J23303493+6633457	11.8	51478.665	6.5590377	D	2	2	0.528:		15
ASAS J054218+2003.7	11.3(V)	54387.881	5.1158842	D	3	3	0.389		4
ASAS J134702−6237.1	12.1(V)	54389.100	3.8729838	D	2	2	0.695	(v)	4
ASAS J151146−5416.4	12.9(V)	54489.723	2.7021281	D	2	2	0.587		4
ASAS J152227−4718.6	11.7(V)	53024.818	24.215083	D	2	2	0.360		4
ASAS J173941−3002.5	10.3(V)	52407.597	2.9697027	D	3	3	0.436		1
NGC 6362 V40	18.8	53915.586	5.2961754	D	4	8	0.529		19
NGC 6809 V54	18.7	50663.463	9.2691571	D	8	1	0.454:		20
NGC 7142 CT 18	16.1	53637.504	15.650400	D	7	3	0.220	(w)	8

Note.

^a(a) Member NGC 752; (b) star in cluster NGC 2244; (c) star in open cluster Cr 197; (d) it may be also be identified as 2MASS J13353299−5214287, due to its distance of 0.1 arcsec and the similar magnitude; (e) KIC 11071207; (f) KIC 11071776; (g) KIC 4544587; (h) KIC 10457553; (i) KIC 10965963; (j) KIC 11499757; (k) KIC 12028095; (l) KIC 12903449; (m) KIC 10494460; (n) KIC 12955326; (o) KIC 10431516; (p) KIC 13151640; (q) KIC 12960819; (r) KIC 11324171; (s) KIC 12383145; (t) KIC 11378051; (u) KIC 12236768; (v) very close to V766 Cen; (w) star V2 near NGC 7142.

References. (1) This paper; (2) Maceroni et al. (2009), (3) Rucinski et al. (2007), (4) Shivvers et al. (2014), (5) Gies et al. (2012), (6) Pribulla et al. (2010), (7) Sokolovsky et al. (2011), (8) Sandquist et al. (2013), (9) Maciel et al. (2011), (10) Davies (2015), (11) Smalley et al. (2014), (12) Moschner et al. (2015), (13) Diethelm (2012), (14) Devor et al. (2008), (15) Volkov et al. (2015), (16) Hambleton et al. (2013), (17) Williams et al. (2011), (18) Otero (2004), (19) Kaluzny et al. (2015), (20) Kaluzny et al. (2014), (21) Popov et al. (2015).

Download table as: ASCIITypeset images: 1 2 3 4

Usually, the timings were obtained with the method of Kwee & van Woerden (1956, hereafter KW), but some of them were determined with the graphical method described by Szafraniec (1948). A total of 2830 new times of minima for 571 EEB stars were determined and are listed in Table 1 for the stars with GCVS names and in Table 2 for those without GCVS names, which are given in full in the electronic version of the paper.

2.2. New Observations

New observations of minima of selected systems were made at the Mt. Suhora Observatory, Pedagogical University of Cracow, Poland⁶ and at the Sobaeksan Optical Astronomical Observatory, Republic of Korea.⁷ Three instruments were used at the Mt. Suhora Observatory:

1.
The 0.6 m Zeiss telescope with an Apogee Aspen Camera located at the primary focus.
2.
The 20 cm Ritchey–Chretien telescope with a SBIG-ST10XME.
3.
The portable 3 cm wide-field objective with an Atik 314L. This instrument was also used by one of us (W.O.) at the South African Astronomical Observatory for observations of the southern hemisphere targets.

The times of minima were computed with the KW method and a digital implementation of the graphical method of Szafraniec (1948).

At the Sobaeksan Optical Astronomical Observatory, a 61 cm Boller and Chivens telescope was used. A PIXIS 2K CCD for the observing seasons of 2009−2011 and an FLI 4K CCD for observations between 2015 and 2017 were used, respectively. Times of minima were computed with the KW method. A part of them (a total of 164 minima) were published by Ogłoza et al. (2017) and Kim et al. (2017).

2.3. EBs with Elliptical Orbits and Their Classification

In all, 623 galactic EB systems with an eccentric orbit are finally compiled with more than 13,400 times of minimum lights. The systems are divided into two groups according to whether a system has a GCVS name or not: a total of 384 systems with a GCVS name are presented in Table 3, and 239 systems without a GCVS name are presented in Table 4.

Finally, the systems in each group are further divided into three categories (D, A, and A+III) on the basis of the O−C behaviors of the primary and secondary timings in each of the ETDs: 453 D systems show just constantly displaced secondary minima relative to primary ones, 139 A systems display the AM effect alone, and 31 (A+III) systems exhibit a combined form of AM and a LITE due to a tertiary body gravitationally bound to the system.

The basic data for all the EEB stars are listed together with their representative references in Tables 3 and 4. Usually, the references reported in Tables 3 and 4 include information about the discovery of displaced secondary minimum and/or orbital parameters of an EEB star.

Table 3 contains a list of 384 EBs with GCVS names (GCVS catalog ver 5.1, Samus et al. 2017) having elliptical orbits confirmed by their ETDs, and we present the following data:

(1)
The system name.
(2)
The approximate brightness at the maximum.
(3)
The initial epoch of the minimum used in the construction of the ETD. Note: T₀ is not an observational time of the primary minimum but a mean epoch of primary and secondary minima.
(4)
The period used to construct the ETD was taken from the TIDAK database. Please note that the period P in the table cannot be used for the prediction of future times of the primary or secondary minima.
(5)
Type (see the text for explanation).
(6)
The number of primary minima taken from the TIDAK database (see Section 2.1).
(7)
The number of secondary minima taken from the TIDAK database.
(8)
The phase of the secondary minimum (only for D type stars) expressed as a fraction of the period (a colon implies that the value may be uncertain).
(9)
Remarks. Some EBs (among them, QX Cas, SS Lac, and AY Mus) have no eclipses due to the change in their orbital inclinations (cf. Zasche & Paschke 2012).
(10)
References are listed at the bottom of Table 3.

Table 4 contains 239 stars with temporary names and in the first column we list the provisional names of the systems. The elliptical orbits of these stars were confirmed by their ETDs. The names of systems were mostly taken from the 2MASS (2Micron All-Sky Survey, Cutri et al. 2003) catalog, where the numbers of the stars contain their coordinates (given for the epoch of 2000). Five stars have ASAS names (Pojmański 2002) and three stars have their own numbers in open or globular clusters. The headings of the remaining columns (3−10) have the same meanings as those in Table 3.

3. Calculation of AM and LITE Parameters

For 139 A and 31 (A+III) systems, we calculated their AM parameters and their AM plus LITE parameters, respectively, by using the following formula:

$\begin{eqnarray}&&C={T}_{0}+{P}_{{\rm{s}}}E+{\tau }_{\mathrm{ap}}+{\tau }_{3},\end{eqnarray} \tag{ 1 }$

where T₀, P_s, τ_ap, and τ₃ are the initial epoch, the sidereal period, the AM term, and the LITE term, respectively. For the A systems, only the first three terms (T₀, P_s, and τ_ap) in Equation (1) were used, whereas all terms were computed for the (A+III) systems. The full expression of τ_ap is taken from Equations (15)−(21) in the paper of Giménez & Bastero (1995) and has four unknowns of the anomalistic period (P_a), the rotation rate of the periastron longitude per cycle ( $\dot{\omega }$ , or the AM rate per cycle), the longitude of the periastron point at T₀ (ω₀), and the eccentricity (e). The longitude of periastron (ω) at any cycle E is expressed as follows:

$\begin{eqnarray}&&\omega ={\omega }_{0}+\dot{\omega }E.\end{eqnarray} \tag{ 2 }$

P_s is derived from P_a as follows:

$\begin{eqnarray}&&{P}_{{\rm{s}}}={P}_{{\rm{a}}}\left(1-\displaystyle \frac{\dot{\omega }}{2\pi }\right).\end{eqnarray} \tag{ 3 }$

The standard expression of τ₃ was given by Irwin (1952, 1959) and has five conventional parameters (a₁₂ sin i₃, e₃, ω₁₂, P₃, and T₃). All timings for each of the systems were fitted to Equation (1) to determine the five unknowns for the A systems and the 10 unknowns for the (A+III) systems. The Levenberg−Marquardt iterative least-squares method (Press et al. 1992) was used to solve for the free parameters that are eventually compiled into our catalog. In the calculations, the eccentricities for 37 systems were fixed to those obtained from their light curves and/or radial velocity curves because the time intervals of their timing data are considerably shorter than their apsidal periods and thus the adjusted eccentricities were erroneously different from the published ones.

Table 5 contains the results from computations for the stars exhibiting AM. Columns 2 and 3 denote the numbers of primary and secondary minima used in the calculation. Some minima from TIDAK were not included in the calculations due to their large observational uncertainties. Columns 3 ∼ 10 contain, in turn, reference epoch T₀ in Heliocentric Julian Date, sidereal period P_s in days, anomalistic period P_a in days, rotation rate of the periastron longitude $\dot{\omega }$ in degree/cycle, longitude of the periastron point ω₀ at T₀ in degrees, orbital eccentricity e, and the AM period U in years. In the last column, we listed the semi-amplitude (K_ap) of the theoretical AM curves in days. The numbers in brackets are the uncertainties of the calculated parameters. The "*" symbol in the brackets for the eccentricity means that the eccentricity was, during the calculation, fixed at the value taken from the literature.

Table 5. Parameters of Apsidal Motion Obtained from Eclipse Timing Diagram

Name	Number		T₀	P_s	P_a	$\dot{\omega }$	ω₀	e^a	U	K_ap
	Pri	Sec	(HJD2400000+)	(day)	(day)	(deg/cycle)	(deg)		(year)	(day)
PP APS	5	3	48503.2737 (3)	4.279823 (41)	4.280082 (29)	0.0218 (24)	98.5 (8)	0.0624 (56)	194 (22)	0.0851 (77)
BW AQR	39	39	39680.4601 (1)	6.71969637 (23)	6.71971686 (18)	0.001098 (8)	100.60 (1)	0.17 (*)	6033 (44)	0.364988 (18)
LL AQR	13	5	48760.9070 (14)	20.1782936 (96)	20.1783048 (92)	0.000199 (48)	155.46 (8)	0.31654 (*)	100000 (24000)	2.057830 (29)
V871 AQL	14	13	38637.1658 (8)	2.9526665 (31)	2.9527721 (22)	0.01287 (27)	168.4 (1.9)	0.1247 (15)	226.1 (4.7)	0.1175 (15)
V1665 AQL	7	4	52810.7272 (5)	3.8817457 (49)	3.8819249 (36)	0.01662 (31)	124.4 (1)	0.2418 (*)	230.3 (4.3)	0.305147 (93)
AG ARI	6	14	54033.3259 (1)	1.9631279 (12)	1.96319198 (88)	0.01173 (14)	110.3 (1)	0.0907 (*)	164.9 (2.0)	0.057766 (20)
WW CAM	25	13	39403.5546 (2)	2.2743627 (86)	2.2744028 (61)	0.00634 (96)	119.9 (6.0)	0.0094 (*)	354 (54)	0.00680837 (36)
V534 CAM	6	4	51497.1695 (2)	3.014237 (14)	3.0145467 (99)	0.0370 (12)	18.9 (1.8)	0.07330 (86)	80.3 (2.6)	0.07038 (83)
SW CMA	17	21	26705.2803 (4)	10.0919732 (32)	10.0921624 (21)	0.006747 (87)	167.5 (1)	0.30519 (5)	1474 (19)	0.99142 (17)
TZ CMA	14	8	55140.7559 (35)	3.822868 (45)	3.822882 (44)	0.00133 (42)	289 (56)	0.062 (18)	2830 (890)	0.076 (21)
AR CMA	11	9	51869.9099 (2)	2.332225 (34)	2.332346 (24)	0.0186 (38)	110.7 (2.0)	0.0149 (15)	124 (25)	0.0110 (11)
CV CMA	8	6	28044.5594 (11)	3.6282856 (28)	3.6283987 (19)	0.01122 (21)	174.2 (1.4)	0.22570 (51)	318.9 (5.9)	0.26223 (60)
KL CMA	14	22	48170.3045 (1)	1.76221426 (31)	1.76233061 (21)	0.023767 (45)	59.1 (1)	0.20035 (19)	73.08 (14)	0.11394 (11)
LT CMA	17	10	48388.5412 (2)	1.75952345 (99)	1.75968043 (71)	0.03212 (14)	78.9 (4)	0.04539 (17)	53.90 (24)	0.02645 (10)
V388 CMA	3	3	53067.7537 (32)	2.982741 (36)	2.982814 (32)	0.0088 (19)	72 (12)	0.49 (14)	334 (74)	0.48 (14)
AV CMI	11	15	52500.6147 (4)	2.2777520 (64)	2.2778108 (44)	0.00929 (73)	193.3 (2.2)	0.1092 (11)	242 (19)	0.07973 (81)
EM CAR	9	10	45038.8131 (1)	3.414275 (15)	3.414759 (10)	0.0511 (11)	24.3 (1.5)	0.01411 (19)	65.9 (1.4)	0.01551 (21)
QX CAR	11	15	40701.2258 (1)	4.47797312 (93)	4.47814181 (63)	0.013561 (55)	117.10 (4)	0.26645 (39)	325.5 (1.3)	0.38413 (57)
V466 CAR	10	7	48036.7444 (3)	3.4558337 (18)	3.4560317 (12)	0.02062 (13)	194.8 (4)	0.19585 (50)	165.2 (1.1)	0.21906 (57)
V529 CAR	11	10	48157.3801 (12)	4.7445731 (61)	4.7448226 (42)	0.01893 (33)	31.2 (5)	0.133 (*)	247.1 (4.4)	0.204532 (65)
AR CAS	15	6	40063.9101 (3)	6.0663123 (15)	6.0664011 (10)	0.005271 (67)	35.1 (3)	0.21636 (74)	1134 (14)	0.4208 (15)
IT CAS	62	44	28762.5245 (3)	3.8966488 (10)	3.89666729 (72)	0.001710 (67)	328.9 (4)	0.085 (*)	2246 (88)	0.1055197 (13)
MU CAS	24	24	51877.1784 (11)	9.6529390 (67)	9.6531007 (46)	0.00603 (18)	345.4 (7)	0.19288 (58)	1578 (48)	0.5960 (18)
PV CAS	162	120	40227.3870 (1)	1.75046985 (66)	1.75056472 (46)	0.019509 (96)	177.4 (5)	0.03199 (8)	88.44 (44)	0.017888 (45)
V381 CAS	49	48	44546.2827 (2)	1.7459434 (15)	1.7463658 (11)	0.08707 (22)	269.7 (1.3)	0.02578 (10)	19.764 (49)	0.014333 (56)
V459 CAS	58	34	25321.5738 (8)	8.4582629 (79)	8.4583337 (56)	0.00302 (24)	230.0 (8)	0.0244 (*)	2760 (220)	0.0657012 (11)
V775 CAS	9	5	48766.4536 (10)	5.390159 (21)	5.390236 (14)	0.0051 (10)	353.9 (1.2)	0.24746 (7)	1040 (210)	0.42767 (12)
V785 CAS	23	28	48502.3735 (1)	2.70251432 (76)	2.70275432 (54)	0.031969 (72)	115.4 (1)	0.09111 (9)	83.32 (19)	0.078461 (78)
V799 CAS	7	9	48500.3927 (3)	7.70293311 (91)	7.70306184 (76)	0.006016 (23)	230.89 (2)	0.4345 (*)	1261.0 (4.8)	1.091990 (81)
V821 CAS	35	31	51767.3480 (1)	1.76973848 (41)	1.76980937 (29)	0.014421 (60)	146.9 (1)	0.13952 (12)	120.96 (50)	0.079603 (72)
V1018 CAS	10	3	51601.488 (11)	4.127759 (46)	4.127826 (31)	0.0058 (29)	125 (13)	0.227 (68)	700 (360)	0.300 (90)
V1137 CAS	7	6	54763.3492 (1)	4.158989 (89)	4.159442 (63)	0.0393 (55)	57.8 (3.8)	0.0166 (17)	104 (15)	0.0220 (22)
V1141 CAS	5	4	51542.5194 (2)	6.9092748 (41)	6.9122578 (29)	0.15536 (15)	129.30 (7)	0.14748 (19)	43.834 (43)	0.32532 (42)
KT CEN	23	18	41696.0724 (6)	4.1304376 (18)	4.1305591 (13)	0.01059 (11)	214.0 (4)	0.2068 (10)	384.2 (4.0)	0.2735 (14)
V636 CEN	15	10	34540.3604 (3)	4.28394652 (37)	4.28395795 (29)	0.000961 (20)	278.91 (8)	0.1348 (*)	4393 (91)	0.1842066 (20)
V1087 CEN	11	8	50563.5959 (3)	5.0496454 (18)	5.0502159 (15)	0.040667 (68)	275.24 (2)	0.365 (*)	122.40 (21)	0.597314 (60)
CW CEP	60	43	41669.5724 (1)	2.72913959 (68)	2.72957960 (48)	0.058033 (63)	201.8 (2)	0.02910 (6)	46.351 (50)	0.025507 (53)
EK CEP	77	16	39002.8143 (29)	4.427794 (25)	4.427802 (25)	0.00065 (11)	59.2 (8.2)	0.139 (33)	6700 (1100)	0.197 (47)
EY CEP	7	14	52339.3254 (2)	7.9714716 (10)	7.97148733 (91)	0.000712 (20)	109.75 (1)	0.4415 (*)	11030(310)	1.1482917 (42)
V397 CEP	23	23	48501.2685 (2)	2.0868237 (12)	2.08688277 (86)	0.01019 (15)	20.5 (8)	0.14342 (96)	201.7 (3.0)	0.09649 (65)
V698 CEP	4	4	50421.1608 (58)	6.618513 (68)	6.618668 (47)	0.0084 (27)	204.9 (9.6)	0.141 (11)	780 (250)	0.297 (24)
V734 CEP	8	6	51482.7078 (33)	3.76596 (12)	3.76599 (12)	0.0033 (12)	72 (17)	0.186 (95)	1110 (390)	0.22 (11)
V898 CEP	10	9	51366.3811 (3)	2.8747637 (42)	2.8748413 (28)	0.00971 (39)	166.3 (3)	0.27352 (18)	292 (12)	0.25381 (18)
V919 CEP	8	8	51295.7813 (3)	1.8519816 (28)	1.8521142 (19)	0.02576 (39)	181.0 (1.2)	0.09515 (45)	70.9 (1.1)	0.05616 (27)
V957 CEP	10	13	51504.7302 (2)	1.9887340 (48)	1.9888017 (33)	0.01225 (62)	315.4 (7)	0.1289 (15)	160. (8.)	0.08174 (94)
V961 CEP	6	6	51442.6550 (2)	7.03847 (17)	7.03868 (16)	0.0107 (24)	180.9 (6.4)	0.0288 (*)	650 (150)	0.0646001 (60)
TV CET	22	17	41275.9334 (2)	9.1032902 (49)	9.1032978 (35)	0.00030 (14)	244.9 (2)	0.0247 (*)	30000 (13000)	0.0715853 (19)
alpha CRB	9	6	23165.4584 (21)	17.3599095 (49)	17.3599499 (41)	0.000837 (56)	309.84 (8)	0.374 (*)	20400 (1400)	2.10357 (12)
VV CRV	15	9	56045.7141 (1)	3.1445164 (25)	3.1446797 (18)	0.01869 (19)	256.10 (7)	0.0852 (*)	165.8 (1.7)	0.0853855 (40)
Y CYG	111	90	46308.3107 (1)	2.99633138 (13)	2.99684513 (9)	0.061714 (11)	132.50 (2)	0.14595 (6)	47.854 (9)	0.139835 (60)
MY CYG	22	29	41559.5996 (1)	4.0051878 (34)	4.0052115 (24)	0.00213 (21)	110.7 (5)	0.01 (*)	1850 (190)	0.01275305 (55)
V380 CYG	13	13	41256.0394 (47)	12.425608 (31)	12.425942 (21)	0.00968 (66)	134.0 (2.1)	0.2029 (67)	1265 (87)	0.817 (27)
V453 CYG	22	14	39340.1154 (1)	3.8898190 (16)	3.8902876 (11)	0.04336 (10)	301.2 (3)	0.02288 (20)	88.42 (21)	0.02834 (25)
V478 CYG	35	23	44777.4851 (1)	2.8809008 (21)	2.8817297 (15)	0.10355 (18)	46.7 (5)	0.01499 (9)	27.422 (48)	0.014059 (85)
V490 CYG	20	18	51491.5924 (1)	1.1402372 (11)	1.14042844 (82)	0.06036 (25)	344.3 (8)	0.04418 (25)	18.618 (78)	0.016043 (91)
V541 CYG	16	17	44881.7603 (2)	15.33790145 (72)	15.33791835 (45)	0.000397 (13)	262.76 (1)	0.479 (*)	38100 (1300)	2.409127 (11)
V796 CYG	38	36	37997.0990 (5)	1.48086983 (77)	1.48105480 (53)	0.04496 (13)	281.7 (1.5)	0.07224 (21)	32.463 (96)	0.034077 (99)
V1136 CYG	44	39	35453.4840 (19)	3.4627576 (17)	3.4628132 (11)	0.00579 (14)	32.7 (1.2)	0.3198 (50)	580 (14)	0.3569 (57)
V1143 CYG	53	15	48410.0562 (1)	7.64074057 (28)	7.64075715 (11)	0.000781 (12)	48.76 (0)	0.538 (*)	9640 (150)	1.36244 (13)
V1147 CYG	33	24	34120.2429 (4)	15.2513209 (11)	15.25132728 (84)	0.000150 (17)	51.34 (2)	0.275 (*)	100000 (11000)	1.347092 (13)
V1326 CYG	13	16	28391.269 (43)	16.68178 (79)	16.68191 (55)	0.003 (12)	122 (96)	0.079 (21)	6000 (23000)	0.42 (11)
V2094 CYG	37	31	54969.469(11)	8.480341 (72)	8.480389 (67)	0.0021 (11)	319 (45)	0.27 (17)	4000 (2100)	0.72 (47)
V2544 CYG	20	12	55004.4892 (1)	2.0937660 (13)	2.09403539 (90)	0.04631 (16)	342.9 (2)	0.07978 (12)	44.56 (15)	0.053556 (81)
V2647 CYG	6	6	53670.7767 (3)	5.855308 (11)	5.8555732 (73)	0.01631 (49)	176.6 (2)	0.26630 (9)	354 (11)	0.50055 (17)
BY DEL	17	9	25830.3751 (31)	10.03420 (13)	10.034928 (94)	0.0261 (34)	101.7 (7.2)	0.00827 (10)	379 (49)	0.02641 (32)
BF DRA	50	33	47276.3401 (2)	11.21099183 (67)	11.21100657 (42)	0.000473 (17)	93.27 (1)	0.3865 (*)	23350 (840)	1.405494 (72)
V410 GEM	8	7	51548.8122 (19)	3.470335 (34)	3.470469 (23)	0.0139 (25)	68.8 (3.9)	0.185 (31)	246 (45)	0.205 (35)
DI HER	73	54	42234.892 (94)	10.550167 (22)	10.550189 (13)	0.00077 (61)	344 (11)	0.450 (20)	14000 (11000)	1.551 (71)
HS HER	88	55	47382.4226 (1)	1.6374342 (18)	1.6375329 (13)	0.02169 (28)	233.6 (8)	0.02029 (23)	74.39 (97)	0.01058 (12)
AI HYA	25	17	41726.0880 (3)	8.28967011 (92)	8.28971167 (70)	0.001805 (26)	245.91 (3)	0.23 (*)	4528 (65)	0.6106838 (19)
OZ HYA	9	7	51983.9427 (2)	2.0487659 (11)	2.04880419 (77)	0.00673 (13)	232.8 (3)	0.071 (*)	300.0 (5.9)	0.047102 (15)
CH IND	9	3	52854.935 (14)	5.95258 (14)	5.95260 (14)	0.00138 (83)	301 (81)	0.084 (39)	4300 (2600)	0.159 (75)
CO LAC	75	79	27534.0756 (2)	1.54220722 (29)	1.54235781 (21)	0.035149 (48)	165.9 (8)	0.02900 (10)	43.246 (59)	0.014285 (49)
CY LAC	10	7	54098.8707 (2)	8.3605382 (34)	8.3606619 (24)	0.00533 (10)	31.83 (3)	0.2565 (*)	1547 (30)	0.69256 (14)
ES LAC	31	20	34240.5644 (4)	4.4594000 (14)	4.45957249 (92)	0.013922 (79)	306.4 (3)	0.19200 (6)	315.7 (1.8)	0.275138 (90)
GX LAC	10	8	46009.3070 (1)	6.355241 (71)	6.355923 (50)	0.0387 (28)	153.0 (2.7)	0.00311 (11)	162 (12)	0.00630 (22)
MZ LAC	78	77	38264.5464 (25)	3.1587897 (12)	3.15883224 (63)	0.00485 (12)	57.7 (8)	0.5122 (88)	642 (15)	0.5338 (99)
OT LAC	7	4	56927.8591 (3)	5.1498634 (19)	5.1505782 (14)	0.049962 (95)	180.6 (3)	0.08545 (18)	101.61 (19)	0.14022 (30)
V339 LAC	15	10	34006.0536 (12)	3.408522 (14)	3.408989 (10)	0.0493 (11)	247.6 (6.7)	0.01640 (12)	68.1 (1.5)	0.01779 (13)
V364 LAC	46	41	44257.3666 (1)	7.35153706 (36)	7.35157681 (28)	0.001947 (11)	83.60 (1)	0.2873 (*)	3722 (21)	0.679021 (17)
V398 LAC	13	7	48501.1735 (3)	5.4060405 (37)	5.4064895 (25)	0.02989 (18)	183.0 (2)	0.20381 (13)	178.2 (1.1)	0.35745 (25)
V401 LAC	20	19	48501.8792 (2)	1.9500921 (14)	1.95017805 (95)	0.01586 (19)	38.5 (6)	0.1978 (19)	121.2 (1.4)	0.1249 (12)
GG LUP	25	19	46136.7444 (1)	1.84959990 (46)	1.84969065 (32)	0.017663 (63)	85.95 (8)	0.15654 (19)	103.21 (37)	0.09258 (11)
TZ MEN	6	5	42403.7495 (3)	8.568991 (54)	8.569228 (37)	0.0099 (16)	294.9 (2)	0.035 (*)	850 (140)	0.0955053 (38)
V498 MON	26	28	33221.7470 (6)	2.4727700 (35)	2.4730321 (25)	0.03815 (36)	156.9 (2.9)	0.04342 (28)	63.88 (61)	0.03473 (22)
V578 MON	26	11	54469.0793 (1)	2.40848583 (41)	2.40898092 (28)	0.073988 (44)	127.8 (1)	0.07808 (21)	32.085 (19)	0.06305 (17)
V684 MON	29	31	54153.5377 (1)	1.8514207 (16)	1.8515194 (11)	0.01918 (21)	171.9 (6)	0.02603 (10)	95.2 (1.1)	0.015340 (59)
V730 MON	11	12	48502.7455 (2)	1.57231877 (70)	1.57243100 (51)	0.02569 (11)	241.6 (3)	0.08244 (21)	60.31 (26)	0.04335 (11)
GM NOR	17	13	41696.9087 (4)	1.8845768 (24)	1.8847167 (17)	0.02673 (33)	164.0 (2.2)	0.04415 (27)	69.50 (85)	0.02666 (16)
GN NOR	13	15	25720.3299 (12)	5.7034540 (61)	5.7036379 (42)	0.01160 (28)	135.7 (3)	0.19386 (90)	484 (12)	0.3536 (17)
V451 OPH	33	27	44834.3611 (1)	2.1965971 (41)	2.1966759 (29)	0.01292 (47)	246.5 (9)	0.01169 (29)	167.6 (6.1)	0.00819 (20)
V2626 OPH	5	4	52787.4983 (2)	10.8743102 (76)	10.8745973 (46)	0.00951 (20)	244.43 (3)	0.191 (*)	1127 (24)	0.665067 (68)
EW ORI	45	26	27543.4613 (4)	6.9368445 (12)	6.93685316 (79)	0.000451 (44)	307.5 (2)	0.0758 (*)	15200 (1500)	0.16748264 (72)
FT ORI	102	32	41349.0192 (5)	3.15039304 (34)	3.15044416 (20)	0.005841 (31)	21.5 (2)	0.41055 (53)	531.6 (2.8)	0.42048 (57)
GG ORI	47	44	35373.5094 (51)	6.631492 (45)	6.631509 (45)	0.00094 (26)	137 (71)	0.161 (18)	6900 (1900)	0.342 (39)
V642 ORI	5	11	27126.003 (13)	9.185527 (92)	9.185593 (89)	0.00258 (73)	103 (21)	0.40 (14)	3510 (990)	1.20 (43)
δ ORI	10	6	43872.5941 (3)	5.7324322 (81)	5.7326979 (57)	0.01669 (36)	105.3 (3)	0.1120 (18)	338.5 (7.4)	0.2110 (33)
BK PEG	12	15	41587.7276 (3)	5.489908 (18)	5.490122 (13)	0.01403 (85)	92.3 (2.1)	0.0053 (*)	386 (23)	0.00926797 (58)
AG PER	54	51	24946.5140 (1)	2.02872978 (11)	2.02887602 (8)	0.025949 (14)	64.1 (2)	0.07091 (10)	77.057 (42)	0.046343 (67)
IM PER	61	41	33541.3792 (6)	2.2542265 (72)	2.2543156 (51)	0.01424 (82)	317.6 (7.6)	0.0503 (28)	156.1 (9.0)	0.0363 (20)
IQ PER	73	26	44290.3640 (1)	1.74356232 (48)	1.74364137 (34)	0.016321 (71)	57.3 (2)	0.06644 (16)	105.30 (46)	0.036905 (89)
V871 PER	16	16	51421.5601 (1)	3.02388343 (97)	3.02422984 (67)	0.041236 (83)	144.79 (9)	0.23375 (15)	72.28 (15)	0.22647 (15)
SY PHE	14	12	54163.2641 (1)	5.270884 (56)	5.272218 (39)	0.0911 (27)	208.6 (2.2)	0.00639 (13)	57.1 (1.7)	0.01074 (22)
KX PUP	14	5	41686.8054 (14)	2.1467975 (11)	2.14685561 (77)	0.00974 (13)	302.5 (8)	0.17309 (38)	217.3 (2.9)	0.11960 (27)
LN PUP	9	8	27803.3012 (25)	3.9511289 (32)	3.9513742 (22)	0.02234 (20)	60.9 (1.5)	0.12183 (72)	174.3 (1.6)	0.15350 (91)
NO PUP	19	10	41361.8145 (1)	1.25688036 (22)	1.25699509 (15)	0.032859 (46)	3.4 (4)	0.12398 (24)	37.700 (53)	0.05086 (10)
V358 PUP	14	12	52503.6027 (3)	6.79391 (97)	6.79400 (97)	0.0048 (21)	114 (55)	0.0034 (20)	1390(620)	0.0074 (44)
V366 PUP	10	7	47860.4656 (6)	2.48398097 (74)	2.48405727 (42)	0.011058 (88)	61.9 (2)	0.3994 (24)	221.4 (1.8)	0.3227 (20)
V399 PUP	15	13	47889.8276 (2)	3.91012557 (84)	3.91055796 (59)	0.039804 (55)	56.94 (7)	0.148 (*)	96.84 (13)	0.190317 (85)
V596 PUP	9	7	44620.6173 (0)	4.5961749 (16)	4.5961985 (12)	0.001845 (86)	108.65 (2)	0.0956 (*)	2460 (114)	0.1400299 (40)
TZ PYX	9	11	52226.7765 (1)	2.318552 (12)	2.3191955 (85)	0.0998 (13)	297.6 (1.1)	0.01072 (19)	22.89 (30)	0.00791 (14)
V523 SGR	29	31	15971.5678 (6)	2.32381294 (49)	2.32388440 (34)	0.011071 (55)	274.3 (9)	0.16479 (66)	206.9 (1.0)	0.12319 (50)
V526 SGR	56	60	47739.6528 (1)	1.91941209 (15)	1.91947734 (10)	0.012238 (21)	254.90 (5)	0.21813 (26)	154.59 (27)	0.13403 (16)
V1647 SGR	13	15	41829.2399 (7)	3.28280023 (40)	3.28284030 (24)	0.004394 (35)	211.3 (3)	0.4331 (10)	736.4 (5.9)	0.4634 (12)
V2283 SGR	44	31	38948.4924 (8)	3.47142163 (69)	3.47148345 (42)	0.006411 (57)	2.5 (2)	0.48764 (50)	533.7 (4.7)	0.55591 (61)
V385 SCO	6	7	53268.2494 (2)	4.690243 (25)	4.690308 (18)	0.0049 (13)	147.8 (7)	0.018 (*)	930 (250)	0.0269197 (27)
V629 SCO	7	7	53626.9294 (1)	3.2491189 (83)	3.2502574 (57)	0.12610 (67)	320.7 (3)	0.06163 (19)	25.41 (14)	0.06455 (20)
V760 SCO	16	13	43250.8363 (1)	1.7309336 (12)	1.73115416 (82)	0.04586 (17)	311.2 (6)	0.02641 (25)	37.21 (14)	0.01469 (14)
V881 SCO	10	11	52128.4205 (3)	2.4915579 (82)	2.4916499 (57)	0.01329 (85)	186.0 (1.9)	0.11007 (59)	185 (12)	0.08802 (47)
V883 SCO	22	16	53685.1893 (1)	4.3411773 (57)	4.3415019 (41)	0.02692 (34)	338.8 (3)	0.07841 (13)	158. (2.)	0.10843 (18)
V1270 SCO	5	3	52441.5905 (47)	4.24316 (12)	4.24325 (12)	0.00713 (69)	102 (21)	0.363 (64)	586 (57)	0.498 (91)
CR SCT	12	11	28719.4993 (16)	4.1923458 (19)	4.1923529 (16)	0.000605 (78)	70.6 (8)	0.089 (*)	6830 (880)	0.11887583 (9)
V335 SER	19	11	50304.4201 (2)	3.4498757 (11)	3.44989807 (84)	0.002333 (78)	61.4 (1)	0.14 (*)	1457 (49)	0.154275 (13)
V413 SER	22	18	49038.8373 (2)	2.25975738 (90)	2.26001340 (63)	0.04078 (10)	81.9 (3)	0.06416 (11)	54.62 (14)	0.046909 (82)
V1154 TAU	10	7	53064.1259 (1)	1.7679033 (18)	1.7680738 (13)	0.03472 (26)	208.4 (6)	0.02609 (31)	50.18 (38)	0.01468 (17)
MN TRA	8	9	48006.3050 (3)	2.3798199 (50)	2.3799037 (35)	0.01268 (54)	203.3 (2.1)	0.0891 (16)	185.0 (7.9)	0.0676 (12)
ET VEL	21	10	29778.2106 (15)	3.0808828 (20)	3.0810589 (15)	0.02058 (16)	260.8 (1.2)	0.06984 (51)	147.6 (1.1)	0.06853 (50)
GT VEL	12	6	41689.3159 (6)	4.6700757 (69)	4.6701727 (49)	0.00748 (38)	18.4 (2.1)	0.1557 (24)	615 (31)	0.2321 (36)
PT VEL	8	6	48293.4700 (3)	1.8020239 (45)	1.8020689 (31)	0.00901 (64)	260.9 (7)	0.1390 (85)	197 (14)	0.0799 (49)
BP VUL	51	33	46003.2323 (1)	1.9403457 (13)	1.94038100 (91)	0.00656(17)	145.4 (8)	0.03192 (12)	291.7 (7.6)	0.019750 (74)
EQ VUL	41	50	35343.8116 (33)	9.2971468 (60)	9.2973245 (39)	0.00688 (18)	198.9 (8)	0.3216 (16)	1331 (34)	0.9639 (49)
FQ VUL	20	6	34238.4546 (18)	6.2626912 (46)	6.2628263 (25)	0.00777 (22)	268.43 (9)	0.527 (10)	795 (23)	1.092 (23)
V495 VUL	15	19	54651.5002 (1)	1.6351323 (23)	1.6352195 (12)	0.01918 (26)	2.0 (3)	0.07679 (18)	84.0 (0.7)	0.04042 (10)
2MASS J04370204+4205520	12	8	52500.9459 (2)	1.4547187 (56)	1.4548116 (39)	0.02299 (99)	301.7 (1.2)	0.03010 (62)	62.4 (2.7)	0.01394 (29)
2MASS J07251501-1135496	6	6	53368.881 (16)	4.509982 (73)	4.510048 (66)	0.0053 (25)	222 (42)	0.46 (14)	840 (390)	0.68 (21)
2MASS J11292643-6201579	3	3	52500.6313 (3)	3.224771 (16)	3.225391 (11)	0.0692 (12)	127.8 (2)	0.13804 (47)	45.95 (82)	0.14203 (49)
2MASS J16111795+3307131	3	5	52503.5747 (47)	8.2837 (12)	8.2844 (12)	0.0325 (58)	297 (32)	0.060 (17)	251 (45)	0.158 (45)
2MASS J19033272+3941003	44	44	52500.3152 (2)	2.1891046 (21)	2.1892176 (14)	0.01858 (25)	328.2 (2)	0.23843 (26)	116.1 (1.6)	0.16727 (18)
2MASS J20020438+4734147	5	4	52501.9431 (32)	5.59890 (25)	5.60151 (15)	0.168 (13)	274.3 (7)	0.3475 (98)	32.9 (2.5)	0.629 (18)

Note.

^aEccentricity with "*" is fixed during the calculation. See the text for details.

Download table as: ASCIITypeset images: 1 2 3

Table 6 contains the results of computations for 31 EEBs exhibiting a combined form of both AM and LITE. The heading of Table 6 has two rows. The upper part represents the parameters of the AM of EEBs (the same as those in Table 5) and the lower part represents the LITE parameters of the eclipsing pair with respect to the mass center of the triple system. Columns 4 ∼ 8 are self-explanatory. The last column denotes the semi-amplitude (K₁₂, in days) of the LITE orbit.

Table 6. Parameters of Apsidal Motion and LITE Obtained from the Eclipse Timing Diagram

Name	Number		T₀(HJD)	P_s(day)	P_a(day)	$\dot{\omega }$ (deg/cycle)	ω₀ (deg)	e^a	U (year)	K_ap (day)
	Pri	Sec	a₁₂ sin i₃(au)	ω₁₂ (deg)	e₃	P₃ (year)	T_peri (HJD)	K₁₂ (day)
V889 Aql	39	36	2438241.7646 (23)	11.1207549 (19)	11.1207648 (19)	0.000323 (13)	125.48 (2)	0.3745 (*)	33900 (1400)	1.349198 (65)
			9.19 (35)	91.3 (4.2)	0.486 (38)	68.10 (85)	2447740 (210)	0.0531 (23)
V539 Ara	19	17	2439314.3645 (3)	3.1690847 (13)	3.16926083 (88)	0.02001 (10)	84.2 (1)	0.05376 (17)	156.10 (79)	0.05445 (17)
			3.64 (11)	74.2 (4.1)	0.456 (28)	53 (1)	2444610 (180)	0.0209 (47)
AL Ari	13	5	2451112.83 (15)	3.747462 (53)	3.747468 (53)	0.00059 (10)	72.2 (3)	0.06 (*)	6200 (1100)	0.0716010 (20)
			1.71 (20)	124 (52)	0.86 (26)	92 (18)	2452170 (120)	0.0086 (38)
CG Aur	91	50	2427148.8680 (23)	1.8048587 (59)	1.8049108 (42)	0.01038 (85)	169 (10)	0.0527 (17)	171 (14)	0.03028 (90)
			0.706 (19)	184.7 (9.6)	0.257 (44)	1.896 (4)	2449999 (24)	0.0039 (3)
BW Boo	36	7	2440362.752 (13)	3.3328179 (96)	3.3328298 (93)	0.00129 (26)	190 (29)	0.14 (2)	2540 (511)	0.151 (18)
			1.127 (62)	189 (8)	0.469 (57)	7.812 (52)	2444410 (150)	0.0058 (20)
AS Cam	83	67	2440204.4043 (3)	3.4309673 (23)	3.4309993 (16)	0.00336 (17)	205.3 (1.8)	0.1079 (16)	1008 (51)	0.1180 (18)
			0.427 (24)	78.1 (6.1)	0.585 (70)	2.216 (1)	2409154 (26)	0.0024 (10)
GL Car	106	90	2424264.4510 (10)	2.42223150 (20)	2.42287242 (15)	0.095230 (20)	85.8 (2)	0.14459 (16)	25.077 (5)	0.11194 (12)
			1.016 (63)	161 (40)	0.019 (14)	123 (14)	2491110 (460)	0.0059 (5)
V493 Car	14	15	2447945.828 (9)	3.229516 (47)	3.229658 (47)	0.01579 (21)	16.1 (6)	0.21166 (76)	201.5 (2.7)	0.22207 (81)
			15.5 (1.7)	73 (46)	0.69 (23)	34.8 (7.7)	2447680 (110)	0.088 (14)
OX Cas	36	35	2446733.7639 (83)	2.489349 (14)	2.489804 (14)	0.06580 (26)	203.9 (9)	0.04222 (12)	37.29 (15)	0.033650 (96)
			1.48 (64)	87 (16)	0.48 (18)	63 (17)	2440400 (180)	0.0086 (37)
V346 Cen	33	34	2421966.9330 (44)	6.3219876 (34)	6.3223450 (34)	0.020354 (40)	273.24 (9)	0.28663 (15)	306.16 (60)	0.58593 (33)
			36.34 (97)	90.9 (7.7)	0.171 (40)	150.3 (6.7)	2438910 (940)	0.2099 (57)
V477 Cyg	122	48	2450988.259 (14)	2.34697860 (52)	2.34701539 (51)	0.005643 (17)	168.3 (1)	0.32238 (11)	409.9 (1.2)	0.244615 (92)
			3.48 (16)	317 (31)	0.41 (14)	161 (44)	2415230 (320)	0.0192 (15)
V974 Cyg	46	47	2435019.3607 (4)	3.2044133 (59)	3.2044405 (42)	0.00306 (48)	202 (6)	0.0579 (25)	1030 (160)	0.0591 (25)
			1.163 (45)	275 (4)	0.528 (47)	23.85 (15)	2450356 (65)	0.0067 (7)
V994A Her	41	26	2448501.1424 (3)	2.0832650 (67)	2.0833678 (47)	0.01775 (82)	308.6 (2.9)	0.02752 (11)	115.7 (5.4)	0.018357 (73)
			2.025 (26)	229.4 (5.4)	0.854 (45)	2.962 (3)	2452787.3 (9.3)	0.0097 (5)
V994B Her	38	29	2455375.4586 (1)	1.4200396 (15)	1.4200838 (11)	0.01120 (27)	309.1 (9)	0.1368 (23)	124. (3.)	0.0621 (11)
			2.432 (31)	65.5 (1.4)	0.494 (22)	2.875 (2)	2452882.8 (3.2)	0.0138 (19)
RW Lac	26	24	2418657.4008 (23)	10.36921 (68)	10.36924 (68)	0.00114 (24)	235 (51)	0.0215 (33)	9000 (1900)	0.071 (11)
			3.41 (11)	334.5 (1.5)	0.762 (17)	28.56 (52)	2401490 (950)	0.0141 (6)
V345 Lac	42	41	2431343.539 (25)	7.491915 (16)	7.491934 (16)	0.00089 (13)	245 (32)	0.54 (17)	8300 (1200)	1.35 (46)
			5.7 (1.1)	5.3 (5.3)	0.53 (14)	56.0 (1.1)	2571200 (1200)	0.028 (8)
V402 Lac	25	15	2448501.3221 (33)	3.7820021 (27)	3.7821371 (22)	0.01285 (16)	16.6 (5)	0.32415 (84)	290.2 (3.5)	0.4027 (11)
			4.45 (19)	211 (13)	0.216 (31)	28.4 (1.7)	2439530 (480)	0.0252 (73)
RU Mon	98	81	2438409.5755 (3)	3.58464746 (33)	3.58474834 (21)	0.010131 (26)	71.08 (6)	0.39758 (71)	348.78 (90)	0.46271 (86)
			5.160 (56)	288.3 (9)	0.540 (10)	61.92 (12)	2443100 (47)	0.0294 (25)
AO Mon	45	35	2440588.3305 (4)	1.8847625 (32)	1.8850334 (23)	0.05172 (44)	260.4 (3.0)	0.01657 (21)	35.92 (30)	0.00996 (13)
			0.927 (40)	310 (39)	0.087 (39)	3.568 (5)	2440690 (140)	0.0053 (8)
V521 Mon	20	16	2433008.4033 (10)	2.97067068 (75)	2.97079373 (53)	0.014911 (63)	270.2 (5)	0.1899 (2)	196.37 (83)	0.18192 (20)
			1.763 (89)	239.8 (6.5)	0.420 (37)	8.433 (35)	2437013 (89)	0.0100 (52)
GV Nor	20	10	2425560.1402 (30)	2.971864 (18)	2.972000 (13)	0.0165 (16)	0 (13)	0.0968 (13)	178 (17)	0.0920 (12)
			1.01 (32)	124 (15)	0.69 (21)	8.347 (84)	2428490 (240)	0.005 (21)
U Oph	63	32	2445892.4499 (1)	1.6773457 (41)	1.6777097 (29)	0.07810 (62)	230.9 (2.9)	0.00347 (13)	21.17 (17)	0.001857 (69)
			1.748 (33)	134.3 (6.7)	0.147 (17)	37.40 (12)	2449820 (290)	0.0100 (8)
V456 Oph	56	31	2453923.9350 (1)	1.01600123 (86)	1.01612327 (61)	0.04324 (22)	359.9 (8)	0.01889 (27)	23.16 (12)	0.006113 (87)
			0.243 (64)	244 (21)	0.49 (15)	5.930 (33)	2452080 (150)	0.0014 (28)
V577 Oph	17	13	2447406.372 (29)	6.0790922 (51)	6.0791119 (49)	0.001172 (70)	51.67 (4)	0.2 (*)	5110 (310)	0.388955 (18)
			7.57 (76)	331 (15)	0.48 (14)	85.7 (7.3)	2437950 (780)	0.0397 948)
V2783 Ori	12	9	2452946.8915 (65)	4.216169 (54)	4.216299 (51)	0.0111 (15)	49 (13)	0.166 (43)	375 (52)	0.223 (58)
			1.853 (96)	56.7 (4.2)	0.541 (68)	9.09 (14)	2454032 (23)	0.0102 (63)
ζ Phe	29	20	2441643.7084 (55)	1.6697697 (29)	1.6698738 (28)	0.02246 (18)	43.5 (9)	0.01310 (25)	73.31 (59)	0.00697 (13)
			2.56 (19)	295 (22)	0.56 (15)	162 (12)	2445010 (730)	0.0144 (13)
PV Pup	6	9	2443119.7156 (5)	1.6607268 (43)	1.6607581 (31)	0.00678 (66)	147.4 (2.6)	0.0519 (13)	241 (24)	0.02767 (68)
			0.96 (11)	243 (15)	0.038 (14)	0.637 (1)	2442173 (99)	0.0055 (8)
YY Sgr	50	40	2419467.0395 (8)	2.62847397 (35)	2.62853757 (25)	0.008710 (34)	119.8 (4)	0.15728 (30)	297.4 (1.2)	0.13190 (25)
			1.544 (98)	135.3 (4.6)	0.531 (63)	18.509 (78)	2418760 (150)	0.0083 (6)
AO Vel	50	44	2445043.6715 (1)	1.58461532 (10)	1.58473986 (7)	0.028292 (16)	96.69 (7)	0.07429 (9)	55.211 (31)	0.037509 (46)
			11.357 (9)	10.3 (4)	0.2925 (16)	40.886 929)	2445770 (10)	0.0628 (4)
DR Vul	96	86	2448989.1040 (1)	2.25087313 (18)	2.25125756 (14)	0.061475 (19)	146.51 (5)	0.09416 (8)	36.095 (11)	0.067572 (58)
			11.660 (34)	99.5 (2)	0.6718 (23)	65.465 (83)	2430355 (32)	0.0669 (11)
2MASS J04233735+2546360	8	8	2453735.288 (16)	3.21749 (11)	3.21769 (10)	0.0226 (52)	45 (17)	0.090 (27)	140 (32)	0.103 (28)
			4.79 (34)	269 (87)	0.89 (17)	1.665 (53)	2455750 (51)	0.0277 (20)

Note.

^aEccentricity with "*" is fixed during the calculation. See the text for details.

Download table as: ASCIITypeset images: 1 2

Figures 1 and 2 show the ETDs of sample EEBs corresponding to the A and A+III systems, respectively. In the figures, assorted symbols were used according to the eclipse type and observational methods. Small plus signs (+), filled circles (•), and filled squares (■) were used to represent the photographic plate,⁸ visual or photographic, and the photoelectric or CCD times of minimum lights for the primary eclipse, respectively; and small cross signs (×), open circles (◦), and open squares (□) for the secondary eclipse. In the upper panel of each of the ETDs in Figure 1, the theoretical AM curves for the primary and secondary eclipses were drawn with the solid curves. In the lower panel, residuals from the curves were plotted. In Figure 2 for the A+III systems, each star has four ETDs as displayed from left to right. The ETD in the first panel shows both AM and LITE, while the second panel shows only AM. The third panel presents only the LITE effect, and the last panel shows the residuals from the AM and LITE ephemerides. The full version (16 images) of the ETDs of the A and A+III systems are presented online.

**Figure 1.** Eclipse timing diagrams (ETDs) of 16 systems showing only AM. According to eclipse type and observational methods, assorted symbols were used: small plus signs (+), filled circles (•), and filled squares (■) were used to represent the photographic plate, visual or photographic, and photoelectric or CCD times of minimum lights for primary eclipse, respectively. On the other hand, small cross signs (×), open circles (◦), and open squares (□) were used for secondary eclipse. Each star has two ETDs from top to bottom. In the upper panel the theoretical AM curves for primary and secondary eclipses were drawn as the solid curves. In the lower panel we plot residuals from the ephemeris curves. All the other systems are shown in the extended figure.
(An extended version of this figure is available.)
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**Figure 2.** Eclipse timing diagrams (ETDs) of 5 systems showing both AM and LITE. The symbols used are the same as those in Figure 1. Each star has four ETDs from left to right. The first panel contains the ETD showing both AM and LITE. The second panel contains the ETD showing only AM. The third panel shows only LITE and the last panel shows the residuals from the AM and LITE ephemeris. All the other systems are shown in the extended figure.
(An extended version of this figure is available.)
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4. Statistics and Discussion

In recent years, Michalska & Pigulski (2005), Michalska (2007), Zasche & Wolf (2013), Hong et al. (2014), and Zasche et al. (2015) presented the AM parameters of the 14, 11, 5, 3, and 13 AM systems in the LMC, respectively. On the other hand, Zasche et al. (2014) and Hong et al. (2015, 2016) gave the AM parameters of 18, 27, and 90 AM systems in the SMC, respectively. Their studies were based primarily on the photometric products of the EROS, MACHO, and OGLE surveys. On the basis of the abovementioned results and including our own, derived in this work, AM parameters are available for 170, 46, and 135 AM systems in our galaxy, the LMC, and the SMC, respectively. In this section, we investigate the statistics, distributions, and relations among the AM parameters of the three different groups defined in this paper.

A summary of the statistics is shown in Table 7, which contains the minimum, maximum, mean, and median values for anomalistic period (P_a), eccentricity (e), AM period (U), and semi-amplitude of a theoretical AM curve (K_ap). The stars with the minimum or maximum values of the parameters are identified in the row following the values. As listed in Table 5, the range between minimum and maximum values for each of the parameters in our galaxy is significantly wider than those in the LMC and the SMC, indicating that an observational selection effect exists in the SMC and the LMC. The observational selection effect is also seen in the histogram of the AM periods in Figure 3, as already noticed by Hong et al. (2016). The entire range of the distribution is divided into five intervals: log U < 1, 1 ≤ log U < 2, 2 ≤ log U < 3, 3 ≤ log U < 4, and log U ≥ 4.

**Figure 3.** Distribution of AM periods in our galaxy, the LMC, and the SMC. The LMC and the SMC are differentiated as indicated in the legend.
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Table 7. Statistics of Some Apsidal Parameters of Apsidal Motion Systems in Our Galaxy, the LMC, and the SMC

	P_a	e	U	K_ap
	(day)		(year)	(day)
Our galaxy
Minimum	1.0161	0.0031	18.6	0.0019
Star^a	(1)	(2)	(3)	(4)
Maximum	20.1783	0.5421	>100,000	2.4091
Star^a	(5)	(6)	(5), (7)	(8)
Mean	4.5294	0.1582	3171.1	0.2876
Median	3.4405	0.1244	235.8	0.1182
LMC
Minimum	1.4423	0.011	19.9	0.0059
Star^a	(9)	(10), (11)	(9)	(11)
Maximum	6.5362	0.3990	1800	0.8467
Star^a	(12)	(12)	(12)	(12)
Mean	3.2633	0.1329	157.7	0.1691
Median	2.9898	0.105	85.8	0.0861
SMC
Minimum	1.0889	0.021	7.1	0.0101
Star^a	(13)	(14)	(15)	(13)
Maximum	6.8339	0.502	897.0	0.6939
Star^a	(16)	(17)	(18)	(19)
Mean	2.7424	0.171	112.8	0.1638
Median	2.4378	0.153	69.0	0.1168

Note.

^a(1) V456 Oph; (2) GX Lac; (3) V490 Cyg; (4) U Oph; (5) LL Aqr; (6) V345 Lac; (7) V1147 Cyg; (8) V541 Cyg; (9) OGLE LMC-ECL-12908; (10) OGLE LMC-ECL-10279; (11) OGLE LMC-ECL-7902; (12) OGLE LMC-ECL-15856; (13) OGLE SMC-ECL-6029; (14) OGLE SMC-ECL-4927; (15) OGLE SMC-ECL-2194; (16) OGLE SMC-ECL-2290; (17) OGLE SMC-ECL-3200; (18) OGLE SMC-ECL-4718; (19) OGLE SMC-ECL-4711.

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Figure 4 shows a diagram of log P versus log U, where filled circles and upright and inverted triangles represent the AM systems in our galaxy, the LMC, and the SMC, respectively. The same symbols have the same meaning in the subsequent figures. For a global comparison between the observations and the AM theory, assuming that the components in an EB system have the same mass (M₁ = M₂), theoretical AM periods (U) as a function of orbital period (P) were calculated for two sets of masses (M₁ = 1 M_⊙ and 20 M_⊙), varying the orbital eccentricity as 0.001, 0.3, and 0.5. In the calculation, we used the relationship $U=360^\circ P/\dot{\omega }$ , where $\dot{\omega }(={\dot{\omega }}_{{\rm{N}}}+{\dot{\omega }}_{{\rm{R}}})$ is the sum of the Newtonian term ( ${\dot{\omega }}_{{\rm{N}}}$ ) and the general relativistic term ( ${\dot{\omega }}_{{\rm{R}}}$ ). The complete forms of ${\dot{\omega }}_{{\rm{N}}}$ and ${\dot{\omega }}_{{\rm{R}}}$ were taken from Giménez (1985; e.g., his Equations (3), (11), (13), and (14)). In Figure 4, the upper three (solid, dashed, and dotted) lines designated as (a, b, c) correspond to the theoretical lines with different eccentricities (0.001, 0.3, 0.5), respectively, for M₁ = M₂ = 1 M_⊙. The lower three lines (d, e, f) are for the higher-mass value of M₁ = M₂ = 20 M_⊙. As can be seen in Figure 4, it is interesting to see that almost all, except for four, data points reside between the lines (a) and (f). For the LMC binaries, Mazeh (2008) discussed the possibility that a linear dependence of the AM period on the binary orbital period exists for the binaries with P ≤ 3^d, while U ∼ P^11/3 for the binaries with P > 3^d. Following the suggestion of Mazeh (2008), Hong et al. (2016) supposed that the distribution of log P versus log U in the SMC is slightly different from that in our galaxy, as a result of their different ages and metallicities. However, a careful examination of Figure 4 and the other subsequent distributions shows that the apparent difference between the EBs of the SMC, plus the LMC and those of our galaxy, may also be due to an observational selection effect, rather than due to a real difference in their physical properties. Nevertheless, the EBs in the SMC and the LMC provide rich data between 15 < P ≤ 65 and 15^y < U ≤ 350^y in the log P versus log U distribution.

The distribution of eccentricities relative to the orbital period is shown in Figure 5, where the symbols are the same as those in Figure 4, and the upper and lower curves given by Mazeh (2008) are drawn as solid and dashed curves, respectively. The two curves have the same parametric form as $f=E-A\,\times \exp (-{(B\times P)}^{C})$ . For the upper curve, E = 0.98, A = 3.25, B = 6.3, and C = 0.23; for the lower curve, A = 3.5 and B = 3. Mazeh derived these curves from the 2,751 spectroscopic binary (SB) orbits in the SB9 catalog (Pourbaix et al. 2005). Similar to the SBs, all the EBs, except one, lie below the upper curve, and there is a relatively sparse region between the upper and the lower curves, as also discussed with the SBs by Mazeh. The exceptional binary star is the OGLEIII-SMC-ECL-3200 (see Hong et al. 2016 for the physical parameters). In addition, we note that there are no AM EBs with an eccentricity larger than e = 0.55, whereas the eccentricity distribution of the SB systems (see Figure 1 of Mazeh 2008), on the other hand, shows that many systems have eccentricities higher than e = 0.55. Therefore, the absence of the high eccentric AM systems must be due to an observational selection effect rather than a real evolutionary effect such as a fast damping of the eccentricity induced by the strong tidal interaction between the components with high eccentricity (Zahn 2008). Along these lines, the presence of AM EBs with eccentricity larger than 0.55 at the orbital periods longer than about 34 is very valuable.

**Figure 5.** Diagram of orbital period vs. eccentricity. The symbols are the same as those in Figure 4. Two curves derived from the SB9 spectroscopic catalog by Mazeh (2008) are overplotted as solid (upper) and dashed (lower) curves. They both are of the form $f=E-A\times \exp -{(P\times B)}^{C}$ . For the upper curve, E = 0.98, A = 3.25, B = 6.3 and C = 0.23. Almost all binaries are below the upper curve. For the lower curve, A = 3.5 and B = 3.
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Next, we investigated the distribution of e cos ω versus e sin ω. The distribution provides valuable information on the size and the direction of an eccentricity vector of an eccentric binary star (well-known as a Laplace−Runge−Lenz vector; refer to Goldstein 1980 and Eggleton 2006 for details). For this purpose, we calculated the longitude of periastron (ω) at the epoch of J2000.0 for all EBs using Equation (2). Figure 6 shows the distribution. The symbols are the same as those in Figure 4. Three eccentricity circles with e = 0.05, 0.3, and 0.6 were overplotted as the solid, dashed, and dotted circles, respectively. In addition, as a supplement to Figure 6, two histograms of longitudes of periastron and eccentricities are presented in Figure 7. Figure 7(a) shows a histogram of longitudes of periastron belonging to each of the four quadrants. On the other hand, Figure 7(b) shows a histogram of eccentricities belonging to each of three eccentricity circles. Careful investigation of the three figures shows that (1) the eccentricity vectors of the AM EBs in our galaxy and the LMC have no preferred directions, while about half the EBs in the SMC are populated in the first quadrant, and (2) about 80% or more of the EBs in all stellar groups are within the eccentricity circle of 0.3.

**Figure 6.** Diagram of e cos ω vs. e sin ω. The symbols are the same as those in Figure 4. Three solid, dashed, and dotted circles represent the eccentricity circles with e = 0.05, 0.3, and 0.6, respectively. The longitudes of periastron (ω) of all EBs are the values at the epoch of J2000.0.
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**Figure 7.** (a) Distribution of longitude of periastron (ω) in each quadrant. (b) Distribution of eccentricities belonging to each of three eccentricity circles. The LMC and the SMC are differentiated using the same pattern used in Figure 3.
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Finally, we plotted a distribution of K_ap (a semi-amplitude of an AM curve) as a function of the orbital period in Figure 8. From the figure, we found that K_ap may have a maximum limit for a given orbital period. Using the maximum values of the K_ap data between P = 25 and P = 77, we derived a linear equation describing the maximized limit value that K_ap at a given period can have, as follows:

$\begin{eqnarray}&&{K}_{\mathrm{ap}}^{\max }=0.190\,P-0\buildrel{\rm{d}}\over{.} 0665.\end{eqnarray} \tag{ 4 }$

Equation (4) was drawn as the dotted line in Figure 8 where all data are below the line. If the existence of the maximum limit of K_ap is possibly real, it is certain to have a complicated relationship with the eccentricity, inclination, longitude of periastron, and orbital period (see Equations (15) ∼ (21) in the paper of Giménez & Bastero (1995)).

5. Final Remarks

Our catalog contains basic stellar parameters of 623 galactic EEBs as well as AM parameters of 170 systems, including the AM plus LITE parameters of 31 systems computed in a consistent way. At the moment, it is the most up-to-date and largest catalog of galactic EEB stars ever compiled. Such a comprehensive catalog, containing data spanning a decade since the previous one was published (Bulut & Demircan 2007), can be used for studying various astrophysical subjects, such as the stellar interior structure, synchronization, circularization, statistics, and celestial mechanics occurring in binary and multiple stellar systems, and it also could be useful for researchers planning their observational programs.

We thank the operating staff of the SOAO 61 cm telescope of KASI. Our warm thanks also go to thank Dr. S. Zola for some helpful suggestions and comments on the draft version of the manuscript, and the anonymous referee for the positive suggestions. This research has been conducted using the SIMBAD and VizieR databases operated by the Centre de Donnees Astronomiques (Strasbourg). We acknowledge the WASP consortium, which comprises the University of Cambridge, Keele University, University of Leicester, The Open University, The Queen's University Belfast, St. Andrews University, and the Isaac Newton Group. Funding for WASP comes from the consortium universities and from the UK's Science and Technology Facilities Council. The CSS survey "CATALINA" is funded by the National Aeronautics and Space Administration under grant No. NNG05GF22G issued through the Science Mission Directorate Near-Earth Objects Observations Program. The CRTS survey is supported by the US National Science Foundation under grants AST-0909182 and AST-1313422. Observations at Mt. Suhora were supported by Polish NCN grant No. 2011/03/D/ST9/01808 and by a grant of the Polish Ministry of Science and Higher Education, No. 204255/E-347/SPUB/2016/1-1. C.-H.K. was supported by the Basic Science Research Program through the National Research Foundation of Korea (NRF) grant funded by the Ministry of Education (NRF-2015R1D1A1A01058924) and the Korea government (MEST) (No. 2017R1A4A1015178).

A Comprehensive Catalog of Galactic Eclipsing Binary Stars with Eccentric Orbits Based on Eclipse Timing Diagrams

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Abstract

1. Introduction

2. Data Collection and Classification of Eclipsing Binaries with Elliptical Orbits

2.1. Data Collection

2.2. New Observations

2.3. EBs with Elliptical Orbits and Their Classification

3. Calculation of AM and LITE Parameters

4. Statistics and Discussion

5. Final Remarks

Footnotes

A Comprehensive Catalog of Galactic Eclipsing Binary Stars with Eccentric Orbits Based on Eclipse Timing Diagrams

Article metrics

Permissions

Share this article

Author e-mails

Author affiliations

ORCID iDs

Dates

Abstract

1. Introduction

2. Data Collection and Classification of Eclipsing Binaries with Elliptical Orbits

2.1. Data Collection

2.2. New Observations

2.3. EBs with Elliptical Orbits and Their Classification

3. Calculation of AM and LITE Parameters

4. Statistics and Discussion

5. Final Remarks

Footnotes