The impact of correlated noise on SuperWASP detection rates for transiting extrasolar planets

A.~M.~S. Smith; A. Collier Cameron; D.~J. Christian; W.~I. Clarkson; B. Enoch; A. Evans; C.~A. Haswell; C. Hellier; K. Horne; J. Irwin; S.~R. Kane; T.~A. Lister; A.~J. Norton; N. Parley; D.~L. Pollacco; R. Ryans; I. Skillen; R.~A. Street; A.~H.~M.~J. Triaud; R.~G. West; P.~J. Wheatley; D.~M. Wilson

doi:10.1111/j.1365-2966.2006.11095.x

The impact of correlated noise on SuperWASP detection rates for transiting extrasolar planets

A.~M.~S. Smith, A. Collier Cameron, D.~J. Christian, W.~I. Clarkson, B. Enoch, A. Evans, C.~A. Haswell, C. Hellier, K. Horne, J. Irwin, S.~R. Kane, T.~A. Lister, A.~J. Norton, N. Parley, D.~L. Pollacco, R. Ryans, I. Skillen, R.~A. Street, A.~H.~M.~J. Triaud, R.~G. WestP.~J. Wheatley, D.~M. Wilson

Physics and Astronomy

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

30 Citations (Scopus)

Abstract

We present a model of the stellar populations in the fields observed by one of the SuperWASP-N cameras in the 2004 observing season. We use the Besancon Galactic model to define the range of stellar types and metallicities present, and populate these objects with transiting extrasolar planets using the metallicity relation of Fischer amp Valenti. We investigate the ability of SuperWASP to detect these planets in the presence of realistic levels of correlated systematic noise (`red noise'). We find that the number of planets that transit with a signal-to-noise ratio of 10 or more increases linearly with the number of nights of observations. Based on a simulation of detection rates across 20 fields observed by one camera, we predict that a total of 18.6 +/- 8.0 planets should be detectable from the SuperWASP-N 2004 data alone. The best way to limit the impact of covariant noise and increase the number of detectable planets is to boost the signal-to-noise ratio, by increasing the number of observed transits for each candidate transiting planet. This requires the observing baseline to be increased, by spending a second observing season monitoring the same fields.

Original language	English
Pages (from-to)	1151-1158
Number of pages	8
Journal	Royal Astronomical Society. Monthly Notices
Volume	373
DOIs	https://doi.org/10.1111/j.1365-2966.2006.11095.x
Publication status	Published - 1 Dec 2006

Keywords

techniques: photometric, planetary systems

Access to Document

10.1111/j.1365-2966.2006.11095.x

Cite this

Smith, A. M. S., Collier Cameron, A., Christian, D. J., Clarkson, W. I., Enoch, B., Evans, A., Haswell, C. A., Hellier, C., Horne, K., Irwin, J., Kane, S. R., Lister, T. A., Norton, A. J., Parley, N., Pollacco, D. L., Ryans, R., Skillen, I., Street, R. A., Triaud, A. H. M. J., ... Wilson, D. M. (2006). The impact of correlated noise on SuperWASP detection rates for transiting extrasolar planets. Royal Astronomical Society. Monthly Notices, 373, 1151-1158. https://doi.org/10.1111/j.1365-2966.2006.11095.x

@article{610ff927fa264ea8870b1b8cd7cb1ab8,

title = "The impact of correlated noise on SuperWASP detection rates for transiting extrasolar planets",

abstract = "We present a model of the stellar populations in the fields observed by one of the SuperWASP-N cameras in the 2004 observing season. We use the Besancon Galactic model to define the range of stellar types and metallicities present, and populate these objects with transiting extrasolar planets using the metallicity relation of Fischer amp Valenti. We investigate the ability of SuperWASP to detect these planets in the presence of realistic levels of correlated systematic noise (`red noise'). We find that the number of planets that transit with a signal-to-noise ratio of 10 or more increases linearly with the number of nights of observations. Based on a simulation of detection rates across 20 fields observed by one camera, we predict that a total of 18.6 +/- 8.0 planets should be detectable from the SuperWASP-N 2004 data alone. The best way to limit the impact of covariant noise and increase the number of detectable planets is to boost the signal-to-noise ratio, by increasing the number of observed transits for each candidate transiting planet. This requires the observing baseline to be increased, by spending a second observing season monitoring the same fields. ",

keywords = "techniques: photometric, planetary systems",

author = "A.~M.~S. Smith and {Collier Cameron}, A. and D.~J. Christian and W.~I. Clarkson and B. Enoch and A. Evans and C.~A. Haswell and C. Hellier and K. Horne and J. Irwin and S.~R. Kane and T.~A. Lister and A.~J. Norton and N. Parley and D.~L. Pollacco and R. Ryans and I. Skillen and R.~A. Street and A.~H.~M.~J. Triaud and R.~G. West and P.~J. Wheatley and D.~M. Wilson",

year = "2006",

month = dec,

day = "1",

doi = "10.1111/j.1365-2966.2006.11095.x",

language = "English",

volume = "373",

pages = "1151--1158",

journal = "Royal Astronomical Society. Monthly Notices",

issn = "0035-8711",

publisher = "SIPRI/Oxford University Press",

}

Smith, AMS, Collier Cameron, A, Christian, DJ, Clarkson, WI, Enoch, B, Evans, A, Haswell, CA, Hellier, C, Horne, K, Irwin, J, Kane, SR, Lister, TA, Norton, AJ, Parley, N, Pollacco, DL, Ryans, R, Skillen, I, Street, RA, Triaud, AHMJ, West, RG, Wheatley, PJ & Wilson, DM 2006, 'The impact of correlated noise on SuperWASP detection rates for transiting extrasolar planets', Royal Astronomical Society. Monthly Notices, vol. 373, pp. 1151-1158. https://doi.org/10.1111/j.1365-2966.2006.11095.x

TY - JOUR

T1 - The impact of correlated noise on SuperWASP detection rates for transiting extrasolar planets

AU - Smith, A.~M.~S.

AU - Collier Cameron, A.

AU - Christian, D.~J.

AU - Clarkson, W.~I.

AU - Enoch, B.

AU - Evans, A.

AU - Haswell, C.~A.

AU - Hellier, C.

AU - Horne, K.

AU - Irwin, J.

AU - Kane, S.~R.

AU - Lister, T.~A.

AU - Norton, A.~J.

AU - Parley, N.

AU - Pollacco, D.~L.

AU - Ryans, R.

AU - Skillen, I.

AU - Street, R.~A.

AU - Triaud, A.~H.~M.~J.

AU - West, R.~G.

AU - Wheatley, P.~J.

AU - Wilson, D.~M.

PY - 2006/12/1

Y1 - 2006/12/1

N2 - We present a model of the stellar populations in the fields observed by one of the SuperWASP-N cameras in the 2004 observing season. We use the Besancon Galactic model to define the range of stellar types and metallicities present, and populate these objects with transiting extrasolar planets using the metallicity relation of Fischer amp Valenti. We investigate the ability of SuperWASP to detect these planets in the presence of realistic levels of correlated systematic noise (`red noise'). We find that the number of planets that transit with a signal-to-noise ratio of 10 or more increases linearly with the number of nights of observations. Based on a simulation of detection rates across 20 fields observed by one camera, we predict that a total of 18.6 +/- 8.0 planets should be detectable from the SuperWASP-N 2004 data alone. The best way to limit the impact of covariant noise and increase the number of detectable planets is to boost the signal-to-noise ratio, by increasing the number of observed transits for each candidate transiting planet. This requires the observing baseline to be increased, by spending a second observing season monitoring the same fields.

AB - We present a model of the stellar populations in the fields observed by one of the SuperWASP-N cameras in the 2004 observing season. We use the Besancon Galactic model to define the range of stellar types and metallicities present, and populate these objects with transiting extrasolar planets using the metallicity relation of Fischer amp Valenti. We investigate the ability of SuperWASP to detect these planets in the presence of realistic levels of correlated systematic noise (`red noise'). We find that the number of planets that transit with a signal-to-noise ratio of 10 or more increases linearly with the number of nights of observations. Based on a simulation of detection rates across 20 fields observed by one camera, we predict that a total of 18.6 +/- 8.0 planets should be detectable from the SuperWASP-N 2004 data alone. The best way to limit the impact of covariant noise and increase the number of detectable planets is to boost the signal-to-noise ratio, by increasing the number of observed transits for each candidate transiting planet. This requires the observing baseline to be increased, by spending a second observing season monitoring the same fields.

KW - techniques: photometric, planetary systems

U2 - 10.1111/j.1365-2966.2006.11095.x

DO - 10.1111/j.1365-2966.2006.11095.x

M3 - Article

SN - 0035-8711

VL - 373

SP - 1151

EP - 1158

JO - Royal Astronomical Society. Monthly Notices

JF - Royal Astronomical Society. Monthly Notices

ER -

The impact of correlated noise on SuperWASP detection rates for transiting extrasolar planets

Abstract

Keywords

Access to Document

Fingerprint

Cite this