A revised orbital ephemeris for HAT-P-9b

Jason A. Dittmann; Laird M. Close; Louis J. Scuderi; Jake Turner; Peter C. Stephenson

doi:10.1016/j.newast.2011.10.003

A revised orbital ephemeris for HAT-P-9b

Jason A. Dittmann, Laird M. Close, Louis J. Scuderi, Jake Turner, Peter C. Stephenson

Astronomy

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

12 Scopus citations

Abstract

We present here three transit observations of HAT-P-9b taken on 14 February 2010 and 05 April 2010 UT from the University of Arizona's 1.55 m Kuiper telescope on Mt. Bigelow. Our two light curves were obtained in the Arizona-I filter for all our observations, and underwent the same reduction process. Both transits occurred approximately 24 min earlier than expected from the ephemeris of Shporer et al. (2009). However, due to the large time span between our observed transits and those of Shporer et al. (2009), a 6.5 s shift downwards in orbital period from the value of Shporer et al. (2009) is sufficient to explain all available transit data. We find a new period of 3.922814 ± 0.000002 days for HAT-P-9b, an order of magnitude more precise than previous measurements, with no evidence for significant nonlinearities in the transit period.

Original language	English (US)
Pages (from-to)	438-441
Number of pages	4
Journal	New Astronomy
Volume	17
Issue number	4
DOIs	https://doi.org/10.1016/j.newast.2011.10.003
State	Published - May 2012

Keywords

Planetary systems
Stars: individual: HAT-P-9

ASJC Scopus subject areas

Instrumentation
Astronomy and Astrophysics
Space and Planetary Science

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10.1016/j.newast.2011.10.003

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title = "A revised orbital ephemeris for HAT-P-9b",

abstract = "We present here three transit observations of HAT-P-9b taken on 14 February 2010 and 05 April 2010 UT from the University of Arizona's 1.55 m Kuiper telescope on Mt. Bigelow. Our two light curves were obtained in the Arizona-I filter for all our observations, and underwent the same reduction process. Both transits occurred approximately 24 min earlier than expected from the ephemeris of Shporer et al. (2009). However, due to the large time span between our observed transits and those of Shporer et al. (2009), a 6.5 s shift downwards in orbital period from the value of Shporer et al. (2009) is sufficient to explain all available transit data. We find a new period of 3.922814 ± 0.000002 days for HAT-P-9b, an order of magnitude more precise than previous measurements, with no evidence for significant nonlinearities in the transit period.",

keywords = "Planetary systems, Stars: individual: HAT-P-9",

author = "Dittmann, {Jason A.} and Close, {Laird M.} and Scuderi, {Louis J.} and Jake Turner and Stephenson, {Peter C.}",

note = "Funding Information: We thank the anonymous referees for their insightful comments during the publication process. This manuscript is much improved thanks to their comments. JD and LMC are supported by a NSF Career award and the NASA Origins program. ",

year = "2012",

month = may,

doi = "10.1016/j.newast.2011.10.003",

language = "English (US)",

volume = "17",

pages = "438--441",

journal = "New Astronomy",

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T1 - A revised orbital ephemeris for HAT-P-9b

AU - Dittmann, Jason A.

AU - Close, Laird M.

AU - Scuderi, Louis J.

AU - Turner, Jake

AU - Stephenson, Peter C.

N1 - Funding Information: We thank the anonymous referees for their insightful comments during the publication process. This manuscript is much improved thanks to their comments. JD and LMC are supported by a NSF Career award and the NASA Origins program.

PY - 2012/5

Y1 - 2012/5

N2 - We present here three transit observations of HAT-P-9b taken on 14 February 2010 and 05 April 2010 UT from the University of Arizona's 1.55 m Kuiper telescope on Mt. Bigelow. Our two light curves were obtained in the Arizona-I filter for all our observations, and underwent the same reduction process. Both transits occurred approximately 24 min earlier than expected from the ephemeris of Shporer et al. (2009). However, due to the large time span between our observed transits and those of Shporer et al. (2009), a 6.5 s shift downwards in orbital period from the value of Shporer et al. (2009) is sufficient to explain all available transit data. We find a new period of 3.922814 ± 0.000002 days for HAT-P-9b, an order of magnitude more precise than previous measurements, with no evidence for significant nonlinearities in the transit period.

AB - We present here three transit observations of HAT-P-9b taken on 14 February 2010 and 05 April 2010 UT from the University of Arizona's 1.55 m Kuiper telescope on Mt. Bigelow. Our two light curves were obtained in the Arizona-I filter for all our observations, and underwent the same reduction process. Both transits occurred approximately 24 min earlier than expected from the ephemeris of Shporer et al. (2009). However, due to the large time span between our observed transits and those of Shporer et al. (2009), a 6.5 s shift downwards in orbital period from the value of Shporer et al. (2009) is sufficient to explain all available transit data. We find a new period of 3.922814 ± 0.000002 days for HAT-P-9b, an order of magnitude more precise than previous measurements, with no evidence for significant nonlinearities in the transit period.

KW - Planetary systems

KW - Stars: individual: HAT-P-9

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U2 - 10.1016/j.newast.2011.10.003

DO - 10.1016/j.newast.2011.10.003

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SP - 438

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JO - New Astronomy

JF - New Astronomy

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ER -

A revised orbital ephemeris for HAT-P-9b

Abstract

Keywords

ASJC Scopus subject areas

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