669:
262:
664:{\displaystyle \tan 2\theta _{0}={\frac {K\sum _{k=0}^{K-1}\sin 2\omega t_{k}-2\left(\sum _{k=0}^{K-1}\cos \omega t_{k}\right)\left(\sum _{k=0}^{K-1}\sin \omega t_{k}\right)}{K\sum _{k=0}^{K-1}\cos 2\omega t_{k}-{\big (}\sum _{k=0}^{K-1}\cos \omega t_{k}{\big )}^{2}+{\big (}\sum _{k=0}^{K-1}\sin \omega t_{k}{\big )}^{2}}},}
1442:
2183:
M. Gruberbauer; K. Kolenberg; J. F. Rowe; D. Huber; J. M. Matthews; P. Reegen; R. Kuschnig; C. Cameron; T. Kallinger; W. W. Weiss; D. B. Guenther; A. F. J. Moffat; S. M. Rucinski; D. Sasselov; G. A. H. Walker (2007). "MOST photometry of the RRdLyrae variable AQLeo: two radial modes, 32 combination
904:
1139:
1834:
2247:
M. Gruberbauer; H. Saio; D. Huber; T. Kallinger; W. W. Weiss; D. B. Guenther; R. Kuschnig; J. M. Matthews; A. F. J. Moffat; S. M. Rucinski; D. Sasselov; G. A. H. Walker (2008). "MOST photometry and modeling of the rapidly oscillating (roAp) star γ Equulei".
2669:
K. Zwintz; T. Kallinger; D. B. Guenther; M. Gruberbauer; D. Huber; J. Rowe; R. Kuschnig; W. W. Weiss; J. M. Matthews; A. F. J. Moffat; S. M. Rucinski; D. Sasselov; G. A. H. Walker; M. P. Casey (2009). "MOST photometry of the enigmatic PMS pulsator HD 142666".
2374:
D. Huber; H. Saio; M. Gruberbauer; W. W. Weiss; J. F. Rowe; M. Hareter; T. Kallinger; P. Reegen; J. M. Matthews; R. Kuschnig; D. B. Guenther; A. F. J. Moffat; S. M. Rucinski; D. Sasselov; G. A. H. Walker (2008). "MOST photometry of the roAp star 10 Aquilae".
1297:
1933:
1974:
and to classify stellar pulsation (see references below). The fact that this method incorporates the properties of the time-domain sampling appropriately makes it a valuable tool for typical astronomical measurements containing data gaps.
2422:
T. Kallinger; D. B. Guenther; J. M. Matthews; W. W. Weiss; D. Huber; R. Kuschnig; A. F. J. Moffat; S. M. Rucinski; D. Sasselov (2008). "Nonradial p-modes in the G9.5 giant ε Ophiuchi? Pulsation model fits to MOST photometry".
1308:
2717:
K. Zwintz; M. Hareter; R. Kuschnig; P. J. Amado; N. Nesvacil; E. Rodriguez; D. Diaz-Fraile; W. W. Weiss; T. Pribulla; D. B. Guenther; J. M. Matthews; A. F. J. Moffat; S. M. Rucinski; D. Sasselov; G. A. H. Walker (2009).
677:
912:
73:, appropriately incorporating a time series to be averaged to zero before applying the DFT, which is done in many practical applications. When a zero-mean corrected dataset has to be statistically compared to a
1622:
1732:
1170:
1845:
1658:
157:
254:
200:
2186:
227:
1162:
1692:
1956:
1724:
111:
1437:{\displaystyle \phi (A)={\frac {KA\cdot \operatorname {sock} }{2<x^{2}>}}\exp \left(-{\frac {KA^{2}}{4<x^{2}>}}\cdot \operatorname {sock} \right),}
62:. It represents the answer to the question, βWhat would be the chance to obtain an amplitude like the measured one or higher, if the analysed time series were
2295:
D. B. Guenther; T. Kallinger; P. Reegen; W. W. Weiss; J. M. Matthews; R. Kuschnig; A. F. J. Moffat; S. M. Rucinski; D. Sasselov; G. A. H. Walker (2007).
2622:
M. Zechmeister; M. Kuerster (2009). "The gemeralised Lomb-Scargle periodogram. A new formalism for the floating-mean and
Keplerian periodograms".
899:{\displaystyle \alpha _{0}={\sqrt {{\frac {2}{K^{2}}}\left(K\sum _{k=0}^{K-1}\cos ^{2}\left(\omega t_{k}-\theta _{0}\right)-\left^{2}\right)}},}
2782:
2239:
1134:{\displaystyle \beta _{0}={\sqrt {{\frac {2}{K^{2}}}\left(K\sum _{k=0}^{K-1}\sin ^{2}\left(\omega t_{k}-\theta _{0}\right)-\left^{2}\right)}}.}
2102:
J. D. Scargle (1982). "Studies in astronomical time series analysis. II. Statistical aspects of spectral analysis of unevenly spaced data".
2470:
T. Kallinger; P. Reegen; W. W. Weiss (2008). "A heuristic derivation of the uncertainty for frequency determination in time series data".
2540:
P. Reegen; M. Gruberbauer; L. Schneider; W. W. Weiss (2008). "Cinderella - Comparison of INDEpendent RELative Least-squares
Amplitudes".
1665:
2792:
2530:
78:
1453:
26:) is a statistical technique to provide the reliability of periodicities in a measured (noisy and not necessarily equidistant)
1829:{\displaystyle \Phi _{\operatorname {FA} }(A)=\exp \left(-{\frac {KA^{2}}{4<x^{2}>}}\cdot \operatorname {sock} \right).}
160:
1984:
2006:
35:
2331:
2787:
70:
1292:{\displaystyle \tan \theta ={\frac {\sum _{k=0}^{K-1}\sin \omega t_{k}}{\sum _{k=0}^{K-1}\cos \omega t_{k}}},}
1928:{\displaystyle \operatorname {sig} (A)={\frac {KA^{2}\log e}{4<x^{2}>}}\cdot \operatorname {sock} .}
2233:
1938:
It returns the number of random time series one would have to examine to obtain one amplitude exceeding
2767:
2731:
2689:
2641:
2600:
2559:
2489:
2442:
2394:
2346:
2308:
2267:
2205:
2155:
2111:
2068:
2025:
1630:
116:
2749:
2705:
2679:
2657:
2631:
2575:
2549:
2505:
2479:
2458:
2432:
2410:
2384:
2362:
2283:
2257:
2221:
2195:
2171:
2145:
2084:
2041:
2015:
232:
178:
205:
2526:
2004:
P. Reegen (2007). "SigSpec - I. Frequency- and phase-resolved significance in
Fourier space".
1839:
The sig is defined as the negative logarithm of the false-alarm probability and evaluates to
1147:
2739:
2735:
2697:
2693:
2649:
2645:
2608:
2567:
2563:
2497:
2493:
2450:
2446:
2402:
2398:
2354:
2316:
2275:
2271:
2213:
2163:
2119:
2076:
2072:
2033:
2029:
1967:
31:
1670:
2517:
P. Reegen (2005). ""SigSpec - reliable computation of significance in
Fourier space", in
2604:
2350:
2312:
2209:
2159:
2115:
1941:
1709:
96:
2776:
2753:
2217:
2175:
1971:
172:
164:
74:
2709:
2661:
2579:
2509:
2462:
2366:
2287:
2225:
2045:
2414:
2136:
M. Breger; S. M. Rucinski; P. Reegen (2007). "The
Pulsation of EE Camelopardalis".
2088:
59:
2744:
2719:
2701:
2653:
1702:
Integration of the pdf yields the false-alarm probability that white noise in the
2571:
2501:
2454:
2406:
2279:
2037:
2297:"Searching for p-modes in η Bootis & Procyon using MOST satellite data"
2059:
N. R. Lomb (1976). "Least-squares frequency analysis of unequally spaced data".
1703:
55:
27:
168:
51:
47:
54:
measure of the probability that the given amplitude level would be seen in
1661:
2330:
D. B. Guenther; T. Kallinger; K. Zwintz; W. W. Weiss; J. Tanner (2007).
2020:
2080:
2613:
2588:
2321:
2296:
63:
2358:
2167:
2123:
2684:
2636:
2554:
2484:
2437:
2389:
2262:
2200:
2150:
89:
Probability density function (pdf) of white noise in
Fourier space
82:
2525:. Cambridge, UK: Cambridge University Press. pp. 791β798.
2768:
Website with further information on SigSpec calculation, etc.
1617:{\displaystyle \operatorname {sock} (\omega ,\theta )=\left}
2521:, eds. J. Zverko, J. Ziznovsky, S.J. Adelman, W.W. Weiss".
93:
Considering a time series to be represented by a set of
2720:"MOST observations of the young open cluster NGC 2264"
1944:
1848:
1735:
1712:
1673:
1633:
1456:
1311:
1173:
1150:
915:
680:
265:
235:
208:
181:
175:
angle may be described in terms of three parameters,
119:
99:
69:
SigSpec may be considered a formal extension to the
2523:
The A-Star Puzzle, Proceedings of IAU Symposium 224
2332:"Seismology of Pre-Main-Sequence Stars in NGC 6530"
1950:
1927:
1828:
1718:
1686:
1652:
1616:
1436:
1302:the probability density of amplitudes is given by
1291:
1156:
1133:
898:
663:
248:
221:
194:
151:
105:
2589:"A new slowly pulsating subdwarf-B star: HD 4539"
2187:Monthly Notices of the Royal Astronomical Society
1698:False-alarm probability and spectral significance
256:, defining the βsampling profileβ, according to
1144:In terms of the phase angle in Fourier space,
644:
590:
574:
520:
8:
2519:The A-Star Puzzle, Proceedings IAU Symp. 224
2743:
2683:
2635:
2612:
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2019:
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1601:
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1517:
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1310:
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1241:
1229:
1204:
1193:
1186:
1172:
1149:
1115:
1099:
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1056:
1045:
1021:
1008:
987:
971:
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931:
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914:
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851:
821:
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213:
207:
186:
180:
140:
127:
118:
98:
2587:C. Schoenaers; A. E. Lynas-Gray (2007).
38:(DFT) and assigns a quantity called the
1996:
2231:
1447:where the sock function is defined by
7:
2593:Communications in Asteroseismology
2301:Communications in Asteroseismology
2238:: CS1 maint: unflagged free DOI (
1958:at the given frequency and phase.
1737:
1706:produces an amplitude of at least
14:
2218:10.1111/j.1365-2966.2007.12042.x
2061:Astrophysics and Space Science
1861:
1855:
1752:
1746:
1475:
1463:
1321:
1315:
146:
120:
1:
2783:Statistical signal processing
1966:SigSpec is primarily used in
1653:{\displaystyle <x^{2}>}
152:{\displaystyle (t_{k},x_{k})}
30:. It relies on the amplitude
42:(frequently abbreviated by β
2745:10.1051/0004-6361/200911863
2702:10.1051/0004-6361:200811116
2654:10.1051/0004-6361:200811296
1985:Spectral density estimation
249:{\displaystyle \theta _{0}}
195:{\displaystyle \alpha _{0}}
2809:
2724:Astronomy and Astrophysics
2672:Astronomy and Astrophysics
2624:Astronomy and Astrophysics
2572:10.1051/0004-6361:20078855
2542:Astronomy and Astrophysics
2502:10.1051/0004-6361:20077559
2472:Astronomy and Astrophysics
2455:10.1051/0004-6361:20078171
2425:Astronomy and Astrophysics
2407:10.1051/0004-6361:20079220
2377:Astronomy and Astrophysics
2280:10.1051/0004-6361:20078830
2250:Astronomy and Astrophysics
2038:10.1051/0004-6361:20066597
2007:Astronomy and Astrophysics
222:{\displaystyle \beta _{0}}
36:Discrete Fourier transform
2793:Digital signal processing
2339:The Astrophysical Journal
2184:frequencies and beyond".
2104:The Astrophysical Journal
2138:The Astronomical Journal
71:Lomb-Scargle periodogram
2736:2009A&A...502..239Z
2694:2009A&A...494.1031Z
2646:2009A&A...496..577Z
2564:2008A&A...484..601R
2494:2008A&A...481..571K
2447:2008A&A...478..497K
2399:2008A&A...483..239H
2272:2008A&A...480..223G
2073:1976Ap&SS..39..447L
2030:2007A&A...467.1353R
1157:{\displaystyle \theta }
1952:
1929:
1830:
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85:only) has to be zero.
1953:
1930:
1831:
1721:
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1687:{\displaystyle x_{k}}
1655:
1619:
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806:
721:
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251:
224:
197:
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108:
50:. This quantity is a
40:spectral significance
24:SIGnificance SPECtrum
16:Statistical technique
1942:
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1631:
1454:
1309:
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263:
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117:
97:
58:, in the sense of a
2605:2007CoAst.151...67S
2351:2007ApJ...671..581G
2313:2007CoAst.151....5G
2210:2007MNRAS.379.1498G
2160:2007AJ....134.1994B
2116:1982ApJ...263..835S
1606:
1543:
2081:10.1007/BF00648343
1948:
1925:
1826:
1716:
1684:
1666:dependent variable
1650:
1614:
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1289:
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1131:
896:
661:
246:
219:
192:
163:of white noise in
149:
103:
2614:10.1553/cia151s67
1951:{\displaystyle A}
1914:
1810:
1719:{\displaystyle A}
1607:
1544:
1418:
1364:
1284:
1126:
946:
891:
711:
656:
106:{\displaystyle K}
81:(rather than the
2800:
2788:Fourier analysis
2757:
2747:
2713:
2687:
2678:(3): 1031β1040.
2665:
2639:
2618:
2616:
2583:
2557:
2536:
2513:
2487:
2466:
2440:
2418:
2392:
2370:
2336:
2326:
2324:
2322:10.1553/cia151s5
2291:
2265:
2243:
2237:
2229:
2203:
2194:(4): 1498β1506.
2179:
2153:
2144:(5): 1994β1998.
2128:
2127:
2099:
2093:
2092:
2056:
2050:
2049:
2023:
2014:(3): 1353β1371.
2001:
1968:asteroseismology
1957:
1955:
1954:
1949:
1934:
1932:
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1615:
1613:
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1608:
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1600:
1591:
1590:
1586:
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1561:
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1523:
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1234:
1233:
1214:
1203:
1187:
1163:
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1119:
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159:, the amplitude
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112:
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34:obtained by the
2808:
2807:
2803:
2802:
2801:
2799:
2798:
2797:
2773:
2772:
2764:
2730:(1): 1239β252.
2716:
2668:
2621:
2586:
2539:
2533:
2516:
2469:
2421:
2373:
2334:
2329:
2294:
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2021:physics/0703160
2003:
2002:
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983:
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839:
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769:
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167:, depending on
136:
123:
115:
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95:
94:
91:
83:population mean
17:
12:
11:
5:
2806:
2804:
2796:
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2785:
2775:
2774:
2771:
2770:
2763:
2762:External links
2760:
2759:
2758:
2714:
2666:
2630:(2): 577β584.
2619:
2584:
2548:(2): 601β608.
2537:
2531:
2514:
2478:(2): 571β574.
2467:
2431:(2): 497β505.
2419:
2383:(1): 239β248.
2371:
2359:10.1086/522880
2345:(1): 581β591.
2327:
2292:
2256:(1): 223β232.
2244:
2180:
2168:10.1086/522795
2130:
2129:
2124:10.1086/160554
2094:
2067:(2): 447β462.
2051:
1995:
1994:
1992:
1989:
1988:
1987:
1980:
1977:
1972:variable stars
1963:
1960:
1947:
1936:
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1199:
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389:
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90:
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15:
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10:
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2:
2805:
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2017:
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2009:
2008:
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1990:
1986:
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1982:
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1973:
1969:
1961:
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1945:
1922:
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1183:
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1128:
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1005:
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165:Fourier space
162:
141:
137:
133:
128:
124:
100:
88:
86:
84:
80:
76:
75:random sample
72:
67:
65:
61:
57:
53:
49:
45:
41:
37:
33:
29:
25:
21:
2727:
2723:
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2234:cite journal
2191:
2185:
2141:
2137:
2107:
2103:
2097:
2064:
2060:
2054:
2011:
2005:
1999:
1970:to identify
1965:
1962:Applications
1937:
1838:
1701:
1660:denotes the
1626:
1446:
1301:
1143:
92:
68:
60:type I error
43:
39:
23:
22:(acronym of
19:
18:
2110:: 835β853.
1704:time domain
79:sample mean
56:white noise
52:logarithmic
46:β) to each
28:time series
2777:Categories
1991:References
2754:123505620
2685:0812.1960
2637:0901.2573
2599:: 67β76.
2555:0710.2963
2485:0801.0683
2438:0711.0837
2390:0803.1721
2263:0801.0863
2201:0705.4603
2176:120843648
2151:0709.3393
1917:⋅
1887:
1853:
1813:⋅
1770:−
1762:
1738:Φ
1594:β
1578:θ
1574:−
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1563:
1531:α
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1508:θ
1500:
1473:θ
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1421:⋅
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1257:−
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1178:
1152:θ
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1080:ω
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1061:−
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1019:θ
1015:−
1002:ω
994:
976:−
958:∑
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862:θ
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826:−
808:∑
798:−
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780:−
767:ω
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545:−
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412:∑
388:ω
385:
374:−
356:∑
344:−
331:ω
325:
314:−
296:∑
277:θ
270:
238:θ
211:β
184:α
169:frequency
48:amplitude
2710:54503935
2662:10408194
2580:11390524
2510:18481860
2463:18201762
2367:54866017
2307:: 5β25.
2288:54726017
2226:55678660
2046:15076973
1979:See also
1662:variance
32:spectrum
2732:Bibcode
2690:Bibcode
2642:Bibcode
2601:Bibcode
2560:Bibcode
2490:Bibcode
2443:Bibcode
2415:3032930
2395:Bibcode
2347:Bibcode
2309:Bibcode
2268:Bibcode
2206:Bibcode
2156:Bibcode
2112:Bibcode
2089:2671466
2069:Bibcode
2026:Bibcode
1664:of the
1164:, with
20:SigSpec
2752:
2708:
2660:
2578:
2529:
2508:
2461:
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2286:
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2174:
2087:
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113:pairs
77:, the
64:random
2750:S2CID
2706:S2CID
2680:arXiv
2658:S2CID
2632:arXiv
2576:S2CID
2550:arXiv
2506:S2CID
2480:arXiv
2459:S2CID
2433:arXiv
2411:S2CID
2385:arXiv
2363:S2CID
2335:(PDF)
2284:S2CID
2258:arXiv
2222:S2CID
2196:arXiv
2172:S2CID
2146:arXiv
2085:S2CID
2042:S2CID
2016:arXiv
173:phase
2527:ISBN
2240:link
1920:sock
1911:>
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2108:263
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2034:doi
2012:467
1884:log
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1759:exp
1554:sin
1491:cos
1367:exp
1265:cos
1217:sin
1175:tan
1069:sin
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834:cos
750:cos
623:sin
553:cos
494:cos
438:sin
382:cos
322:sin
267:tan
161:pdf
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