Capabilities and performance of the Automated Planet Finder telescope with the implementation of a dynamic scheduler

Burt, Jennifer; Holden, B.; Hanson, R. P. C.; Laughlin, G.; Vogt, S. S.; Butler, R. Paul; Keiser, Sandra A.; Deich, William T. S.

doi:10.1117/1.jatis.1.4.044003

Cited by 15 publications

(10 citation statements)

References 26 publications

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“…To span the transit with at least 10 observations, we set the length of each exposure to 20 mins. This provides us with 11 and 12 radial velocities during the Kepler-9 b and c transits, respectively, with uncertainties of 5 m s −1 (Burt et al 2015), which is consistent with the radial velocity precision achieved by Holman et al (2010) with Keck/HIRESr. The R-M effect induced velocity anomaly is modeled using the analytical approach of Hirano et al (2010) and is discussed in detail in Addison et al (2013).…”

Section: Inclinationsupporting

confidence: 89%

Transiting Exoplanet Monitoring Project (TEMP). III. On the Relocation of the Kepler-9 b Transit

Wang

Addison

et al. 2018

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The Kepler-9 system harbors three known transiting planets. The system holds significant interest for several reasons. First, the outer two planets exhibit a period ratio that is close to a 2:1 orbital commensurability, with attendant dynamical consequences. Second, both planets lie in the planetary mass "desert" that is generally associated with the rapid gas agglomeration phase of the core accretion process. Third, there exist attractive prospects for accurately measuring both the sky-projected stellar spin-orbit angles as well as the mutual orbital inclination between the planets in the system. Following the original Kepler detection announcement in 2010, the initially reported orbital ephemerides for Kepler-9 b and c have degraded significantly, due to the limited time base-line of observations on which the discovery of the system rested. Here, we report new ground-based photometric observations and extensive dynamical modeling of the system. These efforts allow us to photometrically recover the transit of Kepler-9 b, and thereby greatly improve the predictions for upcoming transit midtimes. Accurate ephemerides of this system are important in order to confidently schedule follow-up observations of this system, for both in-transit Doppler measurements as well as for atmospheric transmission spectra taken during transit.

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Section: Inclinationsupporting

confidence: 89%

Transiting Exoplanet Monitoring Project (TEMP). III. On the Relocation of the Kepler-9 b Transit

Wang

Addison

et al. 2018

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“…For M dwarf stars down to at least V=10, the APF facility achieves very comparable speed-on-sky as Keck, due largely to the higher spectral resolution of its spectrometer. We are currently using APF to follow up on many promising targets from our 20-year HIRES exoplanet survey with much higher cadence (Burt et al 2014(Burt et al , 2015. In particular, combining the higher cadence available from APF with the long time baseline of the HIRES program is proving to be very effective for characterizing complex multi-planet systems such as HD 141399 and HD 219134 (Vogt et al 2014b.…”

Section: Discussionmentioning

confidence: 99%

The LCES HIRES/Keck Precision Radial Velocity Exoplanet Survey

Butler

Vogt

Laughlin

et al. 2017

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368

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We describe a 20-year survey carried out by the Lick-Carnegie Exoplanet Survey Team (LCES), using precision radial velocities from HIRES on the Keck-I telescope to find and characterize extrasolar planetary systems orbiting nearby F, G, K, and M dwarf stars. We provide here 60,949 precision radial velocities for 1,624 stars contained in that survey. We tabulate a list of 357 significant periodic signals that are of constant period and phase, and not coincident in period and/or phase with stellar activity indices. These signals are thus strongly suggestive of barycentric reflex motion of the star induced by one or more candidate exoplanets in Keplerian motion about the host star. Of these signals, 225 have already been published as planet claims, 60 are classified as significant unpublished planet candidates that await photometric follow-up to rule out activity-related causes, and 54 are also unpublished, but are classified as "significant" signals that require confirmation by additional data before rising to classification as planet candidates. Of particular interest is our detection of a candidate planet with M sin(i) = 3.8 M ⊕ , and P = 9.9 days orbiting Lalande 21185, the fourthclosest main sequence star to the Sun. For each of our exoplanetary candidate signals, we provide the period and semi-amplitude of the Keplerian orbital fit, and a likelihood ratio estimate of its statistical significance. We also tabulate 18 Keplerian-like signals that we classify as likely arising from stellar activity.

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“…In the future, the APF will provide support for the NASA TESS mission. A big advantage of the APF is that it is a robotic instrument and the observing scripts can be launched from remote sites (Burt et al 2015). The unique combination of large telescope time allocation and small user group allows the facility to obtain very high cadence measurements.…”

Section: 7mentioning

confidence: 99%

State of the Field: Extreme Precision Radial Velocities

Fischer

Anglada‐Escudé

Arriagada³

et al. 2016

PASP

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254

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The Second Workshop on Extreme Precision Radial Velocities defined circa 2015 the state of the art Doppler precision and identified the critical path challenges for reaching 10 cm s −1 measurement precision. The presentations and discussion of key issues for instrumentation and data analysis and the workshop recommendations for achieving this bold precision are summarized here.Beginning with the HARPS spectrograph, technological advances for precision radial velocity measurements have focused on building extremely stable instruments. To reach still higher precision, future spectrometers will need to improve upon the state of the art, producing even higher fidelity spectra. This should be possible with improved environmental control, greater stability in the illumination of the spectrometer optics, better detectors, more precise wavelength calibration, and broader bandwidth spectra. Key data analysis challenges for the precision radial velocity community include distinguishing center of mass Keplerian motion from photospheric velocities (time correlated noise) and the proper treatment of telluric contamination. Success here is coupled to the instrument design, but also requires the implementation of robust statistical and modeling techniques. Center of mass velocities produce Doppler shifts that affect every line identically, while photospheric velocities produce line profile asymmetries with wavelength and temporal dependencies that are different from Keplerian signals.Exoplanets are an important subfield of astronomy and there has been an impressive rate of discovery over the past two decades. However, higher precision radial velocity measurements are required to serve as a discovery technique for potentially habitable worlds, to confirm and characterize detections from transit missions, and to provide mass measurements for other space-based missions. The future of exoplanet science has very different trajectories depending on the precision that can ultimately be achieved with Doppler measurements.

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Capabilities and performance of the Automated Planet Finder telescope with the implementation of a dynamic scheduler

Cited by 15 publications

References 26 publications

Transiting Exoplanet Monitoring Project (TEMP). III. On the Relocation of the Kepler-9 b Transit

Transiting Exoplanet Monitoring Project (TEMP). III. On the Relocation of the Kepler-9 b Transit

The LCES HIRES/Keck Precision Radial Velocity Exoplanet Survey

State of the Field: Extreme Precision Radial Velocities

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