The MACHO project LMC variable star inventory. VI. The second overtone mode of cepheid pulsation from first/second overtone beat cepheids

C. Alcock; R. A. Allsman; D. Alves; T. S. Axelrod; A. C. Becker; D. P. Bennett; K. H. Cook; K. C. Freeman; K. Griest; M. J. Lehner; S. L. Marshall; D. Minniti; B. A. Peterson; M. R. Pratt; P. J. Quinn; A. W. Rodgers; A. Rorabeck; W. Sutherland; A. Tomaney; T. Vandehei; D. L. Welch

doi:10.1086/306638

The MACHO project LMC variable star inventory. VI. The second overtone mode of cepheid pulsation from first/second overtone beat cepheids

C. Alcock^*, R. A. Allsman, D. Alves, T. S. Axelrod, A. C. Becker, D. P. Bennett, K. H. Cook, K. C. Freeman, K. Griest, M. J. Lehner, S. L. Marshall, D. Minniti, B. A. Peterson, M. R. Pratt, P. J. Quinn, A. W. Rodgers, A. Rorabeck, W. Sutherland, A. Tomaney, T. VandeheiD. L. Welch

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

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Abstract

MACHO Project photometry of 45 LMC first and second overtone (FO and SO, respectively) beat Cepheids that pulsate in the FO and SO has been analyzed to determine the light-curve characteristics for the SO mode of Cepheid pulsation. We predict that singly periodic SO Cepheids will have nearly sinusoidal light curves; that we will only be able to discern SO Cepheids from fundamental (F) and FO Cepheids for P ≲ 1.4 days; and that the SO distribution will overlap the short-period edge of the LMC FO Cepheid period-luminosity relation (when both are plotted as a function of photometric period). We also report the discovery of one SO Cepheid candidate, MACHO*05:03:39.6-70:04:32, with a photometric period of 0.775961 ± 0.000019 days and an instrumental amplitude of 0.047 ± 0.009 mag in V.

Original language	English
Pages (from-to)	185-192
Number of pages	8
Journal	Astrophysical Journal
Volume	511
Issue number	1 PART 1
DOIs	https://doi.org/10.1086/306638
Publication status	Published - 20 Jan 1999

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Alcock, C., Allsman, R. A., Alves, D., Axelrod, T. S., Becker, A. C., Bennett, D. P., Cook, K. H., Freeman, K. C., Griest, K., Lehner, M. J., Marshall, S. L., Minniti, D., Peterson, B. A., Pratt, M. R., Quinn, P. J., Rodgers, A. W., Rorabeck, A., Sutherland, W., Tomaney, A., ... Welch, D. L. (1999). The MACHO project LMC variable star inventory. VI. The second overtone mode of cepheid pulsation from first/second overtone beat cepheids. Astrophysical Journal, 511(1 PART 1), 185-192. https://doi.org/10.1086/306638

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title = "The MACHO project LMC variable star inventory. VI. The second overtone mode of cepheid pulsation from first/second overtone beat cepheids",

abstract = "MACHO Project photometry of 45 LMC first and second overtone (FO and SO, respectively) beat Cepheids that pulsate in the FO and SO has been analyzed to determine the light-curve characteristics for the SO mode of Cepheid pulsation. We predict that singly periodic SO Cepheids will have nearly sinusoidal light curves; that we will only be able to discern SO Cepheids from fundamental (F) and FO Cepheids for P ≲ 1.4 days; and that the SO distribution will overlap the short-period edge of the LMC FO Cepheid period-luminosity relation (when both are plotted as a function of photometric period). We also report the discovery of one SO Cepheid candidate, MACHO*05:03:39.6-70:04:32, with a photometric period of 0.775961 ± 0.000019 days and an instrumental amplitude of 0.047 ± 0.009 mag in V.",

keywords = "Cepheids, Magellanic clouds, Stars: Fundamental parameters, Stars: Oscillations",

author = "C. Alcock and Allsman, {R. A.} and D. Alves and Axelrod, {T. S.} and Becker, {A. C.} and Bennett, {D. P.} and Cook, {K. H.} and Freeman, {K. C.} and K. Griest and Lehner, {M. J.} and Marshall, {S. L.} and D. Minniti and Peterson, {B. A.} and Pratt, {M. R.} and Quinn, {P. J.} and Rodgers, {A. W.} and A. Rorabeck and W. Sutherland and A. Tomaney and T. Vandehei and Welch, {D. L.}",

year = "1999",

month = jan,

day = "20",

doi = "10.1086/306638",

language = "English",

volume = "511",

pages = "185--192",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

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Alcock, C, Allsman, RA, Alves, D, Axelrod, TS, Becker, AC, Bennett, DP, Cook, KH, Freeman, KC, Griest, K, Lehner, MJ, Marshall, SL, Minniti, D, Peterson, BA, Pratt, MR, Quinn, PJ, Rodgers, AW, Rorabeck, A, Sutherland, W, Tomaney, A, Vandehei, T & Welch, DL 1999, 'The MACHO project LMC variable star inventory. VI. The second overtone mode of cepheid pulsation from first/second overtone beat cepheids', Astrophysical Journal, vol. 511, no. 1 PART 1, pp. 185-192. https://doi.org/10.1086/306638

TY - JOUR

T1 - The MACHO project LMC variable star inventory. VI. The second overtone mode of cepheid pulsation from first/second overtone beat cepheids

AU - Alcock, C.

AU - Allsman, R. A.

AU - Alves, D.

AU - Axelrod, T. S.

AU - Becker, A. C.

AU - Bennett, D. P.

AU - Cook, K. H.

AU - Freeman, K. C.

AU - Griest, K.

AU - Lehner, M. J.

AU - Marshall, S. L.

AU - Minniti, D.

AU - Peterson, B. A.

AU - Pratt, M. R.

AU - Quinn, P. J.

AU - Rodgers, A. W.

AU - Rorabeck, A.

AU - Sutherland, W.

AU - Tomaney, A.

AU - Vandehei, T.

AU - Welch, D. L.

PY - 1999/1/20

Y1 - 1999/1/20

N2 - MACHO Project photometry of 45 LMC first and second overtone (FO and SO, respectively) beat Cepheids that pulsate in the FO and SO has been analyzed to determine the light-curve characteristics for the SO mode of Cepheid pulsation. We predict that singly periodic SO Cepheids will have nearly sinusoidal light curves; that we will only be able to discern SO Cepheids from fundamental (F) and FO Cepheids for P ≲ 1.4 days; and that the SO distribution will overlap the short-period edge of the LMC FO Cepheid period-luminosity relation (when both are plotted as a function of photometric period). We also report the discovery of one SO Cepheid candidate, MACHO*05:03:39.6-70:04:32, with a photometric period of 0.775961 ± 0.000019 days and an instrumental amplitude of 0.047 ± 0.009 mag in V.

AB - MACHO Project photometry of 45 LMC first and second overtone (FO and SO, respectively) beat Cepheids that pulsate in the FO and SO has been analyzed to determine the light-curve characteristics for the SO mode of Cepheid pulsation. We predict that singly periodic SO Cepheids will have nearly sinusoidal light curves; that we will only be able to discern SO Cepheids from fundamental (F) and FO Cepheids for P ≲ 1.4 days; and that the SO distribution will overlap the short-period edge of the LMC FO Cepheid period-luminosity relation (when both are plotted as a function of photometric period). We also report the discovery of one SO Cepheid candidate, MACHO*05:03:39.6-70:04:32, with a photometric period of 0.775961 ± 0.000019 days and an instrumental amplitude of 0.047 ± 0.009 mag in V.

KW - Cepheids

KW - Magellanic clouds

KW - Stars: Fundamental parameters

KW - Stars: Oscillations

UR - http://www.scopus.com/inward/record.url?scp=0033585316&partnerID=8YFLogxK

U2 - 10.1086/306638

DO - 10.1086/306638

M3 - Article

SN - 0004-637X

VL - 511

SP - 185

EP - 192

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1 PART 1

ER -

The MACHO project LMC variable star inventory. VI. The second overtone mode of cepheid pulsation from first/second overtone beat cepheids

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