Extrasolar Planet Transits Observed at Kitt Peak National Observatory
ABSTRACT.
We obtained
Received 2011 October 2; accepted 2012 February 7; published 2012 March 15
Keywords:Extrasolar Planets
1. INTRODUCTION
Many exoplanet systems contain Jupiter-mass planets on close-in orbits. These planets are strongly irradiated by their host stars and emit significant radiation in the infrared (Charbonneau et al. 2005, Deming et al. 2005). Characterization of their atmospheres using transit and secondary-eclipse techniques has become a very active field (Seager & Deming 2010). Atmospheric observations using a secondary eclipse are also sensitive to the orbital dynamics: specifically, the eccentricity of the orbit, via the phase of the eclipse (Deming et al. 2007). Consequently, interpreting secondary-eclipse observations requires knowing the ephemeris of the transits to high precision. Continuing explorations of discoveries by transit surveys have given us a sample of more than 70 hot Jupiters transiting systems brighter than
In addition to the preceding motivations, we are interested in transit monitoring at near-IR (
2. OBSERVATIONS AND PHOTOMETRY
2.1. OBSERVATIONS
Our primary observational system is the Kitt Peak National Observatory’s 2.1 m reflector with the FLAMINGOS
Observations at all three telescopes used various degrees of defocus to improve the photometric precision, and all used automatic off-axis or manual guiding to maintain pointing stability: Exposure times varied between 20 s and 120 s, depending on the system used and the stellar magnitude, so that pixel values stayed well within saturation levels. The optical CCD exposures were binned
Flat-field observations were acquired at all three observatories using either twilight sky flats, dome flats, or a series of night-sky exposures that incorporated pointing offsets to allow removal of stars via a median filter. Standard, dark-field corrections were also applied.
2.2. PHOTOMETRY
Subsequent to dark current subtraction and division by a flat-field frame, we performed aperture photometry on the target star and the comparison stars using standard and custom IDL routines. In all cases, except for the McMath-Pierce telescope observations, between two and eight stars of similar magnitude to the target star were used for comparison. This allowed for intercomparison between these stars to make sure no variability was detected in them. Due to the characteristics of the heliostat (image rotation) and the small FOV available at the solar telescope, only the comparison star nearest to the target star was of use. The apertures selected to measure the stars and background varied depending on the degree of defocus and seeing conditions for each observing session. These were chosen such that they minimized the scatter on the final light curve. The defocus on the 2.1 m telescope, in particular, was sensitive to changes throughout the night, due to mechanical flexure and temperature variations. We eventually learned to actively adjust the defocus setting gradually during the observations, so as to maintain image stability. For those data that exhibit variable defocus, we adjusted the numerical apertures accordingly in the data analysis process. Best results were also obtained by averaging the ratios of the target star to each comparison star. This produced similar or smaller scattering than the method of ratioing the target star to the sum of all the comparison stars. In most cases the comparison stars were similar in brightness (
After normalizing the target star to the comparison stars, some gradual variations as a function of time were found in some instances. In the case of the optical observations, the variation was removed by using a linear air-mass-dependent function fit to the baseline before and after the transit. Most transits have at least one hour’s worth of baseline observations before the transit ingress and after the transit egress for this purpose. However, the near-IR observations exhibited a more complex baseline variation that could not be attributed to simple air-mass-dependent comparison star differential extinction. These are most likely due to telluric water vapor absorption variations and/or to other instrumental effects. For these cases, polynomial functions of orders 2–5 were used to fit the baseline photometry. Most of the near-IR light curves included longer preingress and postegress observations, which allowed for improved baseline fits.
Figure 1 shows the near-IR transits observed with the 2.1 m telescope, Figure 2 (left) shows the four transits observed with the McMath-Pierce telescope and the optical transits observed with the Visitor Center telescope. During the observing runs, other transits were recorded as well, but they are either incomplete (show the ingress or egress only) or suffered from clouds and are therefore of limited use and not included in this work.
3. MODELING
In order to fit the observed transit light curves, we first created initial standard model light curves. These were constructed numerically as a tile-the-star procedure using the Binary Maker II software (Bradstreet 2005). The initial system parameters used were obtained from the latest literature available. Linear limb-darkening function coefficients were taken from Claret (2000). For most cases the initial model light curves yielded very good agreement with the observed ones, and only small adjustments to the duration and depth of the model transits were necessary to optimize the fits. This was done by applying small (
Table 1 presents all the observed transits and the principal light-curve parameters (midtransit time, depth, and duration) derived from fitting the models, as explained previously. Because the scatter of the photometry is larger than the formal errors suggest, for each light curve, we used the scatter to estimate the uncertainties.
In order to derive improved orbital periods for the transiting systems, we utilized the transit timings reported in the published literature, including the observations from this article, and we implemented a least-squares linear fit to the data, weighting the individual transit times by their uncertainties. When relevant, we have converted reported Heliocentric Julian Dates (HJDs) to Barycentric Julian Dates (BJDs) (Eastman et al. 2010) and have used the Dynamical Time-based system (BJD_TDB) instead of the Coordinated Universal Time-based system (BJD_UTC). The difference between heliocentric and barycentric times can be up to about 4 s, but most often it is less than this value and well within the individual timing uncertainties reported, so it has limited effect on the derived periods. However, the difference between UTC-based and TDB-based timings is a systematic offset that depends on recent additions of leap seconds to UTC. To convert BJD_TDB to BJD_UTC, subtract 0.000766 days for transits observed after 2009 January 1 (JD 2,454,832.5), 0.000754 days from transits between 2006 January 1 (JD 2,453,736.5) and 2009 January 1, and 0.000743 days from transits between 1999 January 1 (JD 2,451,179.5), and 2006 January 1. The resulting system periods are presented in Table 2, along with the number of midtransit timings used and the time span between the first and last observations reported. The reference epoch presented (JD0) is the result from the fit and generally corresponds with the first reported transit found in the literature.
For some of the best light curves obtained with the KPNO 2.1 m telescope (
4. RESULTS AND DISCUSSION
We now discuss the results of modeling our 2.1 m
4.1. COMPARISON WITH OPTICAL PLANETARY RADII
Stellar limb-darkening is much less prominent in the near-infrared, as compared with optical wavelengths, so the depth of an infrared transit is closely proportional to
The large stellar photon flux available to optical observers usually produces significantly smaller random errors than for our
4.2. DISCUSSION OF INDIVIDUAL SYSTEMS
4.2.1. COROT-1
The brightness of the COROT-1 (
4.2.2. COROT-2
COROT-2 is a transiting system that exhibits clear evidence of starspots that have been used to estimate the rotation period of the star (Lanza et al. 2009). Alonso et al. (2008), in their discovery article, present an ephemeris that summarizes the 78 transits observed by the COROT mission. We combined this ephemeris with prediscovery transits reported by Rauer et al. (2010), one ephemeris reported by Vereš et al. (2009), and our current measurement (Fig. 2) to calculate the period of the system. Our result of
4.2.3. GJ 1214
The first two of the observations presented here have already been analyzed and discussed in Sada et al. (2010). See this reference for a more thorough modeling analysis of this system. However, since then, other transits have been reported. Here, we assemble the original midtransit observations of Charbonneau et al. (2009), as reevaluated in Berta et al. (2011); other observations also reported in Berta et al. (2011), including two high-precision VLT transits; and those of Sada et al. (2010). In the period solution we also include 12 new full transits (ingress and egress recorded) presented by Carter et al. (2011), three transits reported by Kundurthy et al. (2011) (their best result: chain003a), four near-infrared transits observed from Hawaii (Croll et al. 2011), plus two recent unreported transit we observed simultaneously at KPNO using the 2.1 m telescope (
4.2.4. HAT-P-1
Two HAT-P-1 transits were observed with the NAC through an
4.2.5. HAT-P-3
We observed two transits of HAT-P-3 on 2009 May 15 and 2010 May 27. Each transit was observed with the KPNO 2.1 m telescope with a
4.2.6. HAT-P-4
We observed one transit for HAT-P-4 on 2011 May 22 with the KPNO 2.1 m telescope using a
4.2.7. HAT-P-6
We observed one transit of HAT-P-6 on 2009 November 25 with the KPNO 2.1 m telescope through a
4.2.8. HAT-P-11
We observed one transit of HAT-P-11 with both the KPNO 2.1 m telescope (
4.2.9. HAT-P-12
The only other midtransit ephemeris for HAT-P-12 available in the literature corresponds to the discovery article by Hartman et al. (2009). Combined with our 2.1 m telescope
4.2.10. HAT-P-27 / WASP-40
We combined our single recent observation of this transiting system (KPNO 2.1 m telescope,
4.2.11. HAT-P-32
One ephemeris for this system is reported in the literature resulting from the observation of several transits in the discovery article (Hartman et al. 2011). We combined our three KPNO 2011 observations (two 2.1 m telescope
Our simultaneous observations of 2011 October 11 through
4.2.12. HD 17156
HD 17156 is a system with a relatively long orbital period (
4.2.13. HD 189733
This is a well-observed transiting system with ample reported transits. We observed HD 189733 with the 2.1 m telescope (
For this system, we obtained all ground-based (Bouchy et al. 2005; Bakos et al. 2006; Winn et al. 2007b; Hrudková et al. 2010) and spacecraft (Pont et al. 2007; Knutson et al. 2007, 2009; Miller-Ricci et al. 2008; Agol et al. 2010) midtransit times reported in the literature to derive a period of
This is an often-studied bright system that has been observed from space, and its light-curve parameters are well constrained. Our single light-curve observation cannot improve on those results, but it was of particular help in refining the data analysis and modeling techniques used throughout this work. Within our much larger uncertainties, our light-curve model parameters correspond with those of the literature.
4.2.14. Qatar-1
Our single KPNO 2.1 m
4.2.15. TrES-1
There are few midtransit times reported in the professional literature for this system, despite this being one of the earliest exoplanet systems to be discovered and announced. We managed to observe two consecutive transits in 2007 using the NAC array at the KPNO NSO McMath-Pierce Solar Telescope (
4.2.16. TrES-2
We obtained two transits of this well-observed and characterized exoplanet system in 2011 with both KPNO telescopes on May 20 (VC telescope
4.2.17. TrES-3
We observed one transit of TrES-3, with the KPNO VC telescope (
4.2.18. TrES-4
We observed one transit of TrES-4 with both the KPNO 2.1 m telescope (
4.2.19. WASP-1
We observed WASP-1 on one occasion with the KPNO 2.1 m telescope (
4.2.20. WASP-2
We observed WASP-2 on one occasion with the KPNO 2.1 m telescope (
4.2.21. WASP-3
WASP-3 is a well-observed system with ample midtransit timings found in the literature. Here, we gathered the earlier observations from Pollacco et al. (2008), Gibson et al. (2008), a low-precision measurement by Damasso et al. (2010), well-observed events by Tripathi et al. (2010), Maciejewski et al. (2010), Littlefield (2011), and space-based observations by Christiansen et al. (2011), and we combine them with our four observations (three from the VC telescope and one from the 2.1 m telescope [Figs. 1 and 2]) to derive an improved period of
4.2.22. WASP-6
We have combined our 2011 October 12
4.2.23. WASP-10
WASP-10 was the first system that we observed transiting at both the KPNO 2.1 m telescope (
Maciejewski et al. (2011a) report midtransit timing variations that can be explained by the presence of an additional planet about one-tenth of the mass of Jupiter orbiting close to the outer
There has been some discussion in the literature concerning the radius of WASP-10b (Johnson et al. 2009; Dittman et al. 2010). Our
4.2.24. WASP-11/HAT-P-10
We observed four transits of this system on 2009 November 26 with the KPNO 2.1 m telescope, on 2010 November 7 with the KPNO VC telescope, and on 2011 October 8 with both telescopes (see Figs. 1 and 2). We combined our midtransit timings with those reported on both discovery articles (West et al. 2009; Bakos et al. 2010a) to derive an improved period of
Our higher-quality
4.2.25. WASP-12
We observed one transit of WASP-12 with the KPNO VC telescope (Fig. 2,
4.2.26. WASP-24
We observed one transit of WASP-24 with the KPNO 2.1 m telescope (
4.2.27. WASP-32
We observed one transit of WASP-32 through a
4.2.28. WASP-33
WASP-33 is the hottest known hot Jupiter (Smith et al. 2011) closely orbiting a bright δ Scuti variable host star (Herrero et al. 2011). Only two epochs are reported in the literature: in the discovery article (Collier Cameron et al. 2010) and by Smith et al. (2011). We combine these midtransit times with our observations: a
Both observations obtained on 2011 October 13 clearly show short-period variability that interferes with a clean determination of the light-curve parameters in Table 1 and the near-IR model parameters of Table 3. This is evidenced as an offset of the baseline before ingress compared with the egress baseline, and there is also an increase in brightness affecting the first half of the transit depth. These effects are enhanced on the shorter-wavelength and narrower-bandpass Hα light curve that shows the transit of the planet against the chromosphere of the star compared with the
4.2.29. WASP-48
There is only one discovery epoch reported for this system (Enoch et al. 2011). We combine this midtransit time with our KPNO 2.1 m
4.2.30. WASP-50
We combined our two consecutive 2011 observations of this system from KPNO (
4.2.31. XO-1
We observed one transit of this system with the KPNO VC telescope (
4.2.32. XO-5
We observed one transit of XO-5 with the KPNO 2.1 m telescope (
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1 Universidad de Monterrey, Departamento de Física y Matemáticas, Avenida I. Morones Prieto 4500 Poniente, San Pedro Garza García, Nuevo León, 66238, México; pedro.valdes@udem.edu.mx.
2 Visiting Astronomer, Kitt Peak National Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy under cooperative agreement with the National Science Foundation.
3 Department of Astronomy, University of Maryland, College Park, MD 20742; ddeming@astro.umd.edu, jfraine@astro.umd.edu.
4 Planetary Systems Laboratory, Goddard Space Flight Center, Mail Code 693, Greenbelt, MD 20771; donald.e.jennings@nasa.gov, brian.k.jackson@nasa.gov.
5 Dickinson College, Carlisle, PA 17013; hamiltoc@dickinson.edu.
6 Kitt Peak National Observatory, National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719; speterson@noao.edu, fhaase@noao.edu, kbays@noao.edu.
7 The Catholic University of America, Washington, DC 20064; allen.w.lunsford@nasa.gov.
8 Trinity College, Dublin, Dublin 2, Ireland; eogorma@tdc.ie.