The habitable-zone planet finder: engineering and commissioning on the Hobby Eberly telescope (Conference Presentation)

Mahadevan, Suvrath; Anderson, Tyler; Balderrama, Edmundo; Bender, Chad F.; Bevins, Emily; Blakeslee, Scott; Cole, Amanda; Conran, David; Diddams, Scott A.; Dykhouse, Adam; Darling, John; Fredrick, Connor; Halverson, Samuel; Hearty, Fred; Jennings, Jeff; Kaplan, Kyle; Kanodia, Shubham; Levi, Eric; Lubar, Emily; Metcalf, Andrew J.; Monson, Andrew; Ninan, Joe P.; Nitroy, Colin; Ramsey, Lawrence W.; Robertson, Paul; Roy, Arpita; Schwab, Christian; Shetrone, M.; Spencer, Renny; Stefánsson, Guðmundur; Terrien, Ryan C.; Wright, Jason T.

doi:10.1117/12.2313835

Cited by 8 publications

(4 citation statements)

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“…The Habitable Zone Planet Finder (HPF; Mahadevan et al 2012) will specifically target mid-to late-type M dwarfs at near-infrared wavelengths, with a goal of 1 m s −1 precision. Recent commissioning observations with HPF have already achieved 1.3 m s −1 precision on Barnard's Star (Mahadevan et al 2018).…”

Section: Discussionmentioning

confidence: 99%

Kepler Planet Occurrence Rates for Mid-type M Dwarfs as a Function of Spectral Type

et al. 2019

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Previous studies of planet occurrence rates largely relied on photometric stellar characterizations. In this paper, we present planet occurrence rates for mid-type M dwarfs using spectroscopy, parallaxes, and photometry to determine stellar characteristics. Our spectroscopic observations have allowed us to constrain spectral type, temperatures, and in some cases metallicities for 337 out of 561 probable mid-type M dwarfs in the primary Kepler field. We use a random forest classifier to assign a spectral type to the remaining 224 stars. Combining our data with Gaia parallaxes, we compute precise (∼3%) stellar radii and masses, which we use to update planet parameters and planet occurrence rates for Kepler mid-type M dwarfs. Within the Kepler field, there are seven M3 V to M5 V stars which host 13 confirmed planets between 0.5 and 2.5 Earth radii and at orbital periods between 0.5 and 10 days. For this population, we compute a planet occurrence rate of 1.19 +0.70 −0.49 planets per star. For M3 V, M4 V, and M5 V, we compute planet occurrence rates of 0.86 +1.32 −0.68 , 1.36 +2.30 −1.02 , and 3.07 +5.49 −2.49 planets per star, respectively. 2. TARGET SELECTION, OBSERVATIONS, AND DATA REDUCTION Using revised KIC temperature estimates, DC13 identified 202 stars with T eff 3, 300 K. Muirhead et al. (2015) identified 509 probable mid-type M dwarfs from KIC photometry using the following color selection criteria: r − J > 3.2 to identify red objects, and J − K < 0.0555×(r−J)+0.7622 to remove giant stars. The union between these samples produces 561 probable mid-type M dwarfs which we targeted in this study. In total, we observed 337 of the 561 targets (60%), obtaining optical spectra of 327 stars and near-infrared spectra of 82 stars. We have both optical and infrared spectra for 72 targets. Magnitude distributions of our targets in rband and K s -band are shown in Figure 1, including the distributions of targets we observed.

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Section: Discussionmentioning

confidence: 99%

Kepler Planet Occurrence Rates for Mid-type M Dwarfs as a Function of Spectral Type

et al. 2019

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“…Using the Habitable-zone Planet Finder Spectrograph (HPF) (13)(14)(15) on the Hobby-Eberly Telescope (HET) (16)(17)(18), we observed HAT-P-32 b with time-series high-resolution (R ≈ 55,000) spectra to detect a helium outflow and investigate atmospheric escape. HAT-P-32 b is a hot Jupiter transiting a late-F star, HAT-P-32 A, on a 2.15-day orbit with an in-transit duration of 3.12 hours (19,20).…”

Section: Introductionmentioning

confidence: 99%

Giant tidal tails of helium escaping the hot Jupiter HAT-P-32 b

et al. 2023

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Capturing planets in the act of losing their atmospheres provides rare opportunities to probe their evolution history. This analysis has been enabled by observations of the helium triplet at 10,833 angstrom, but past studies have focused on the narrow time window right around the planet’s optical transit. We monitored the hot Jupiter HAT-P-32 b using high-resolution spectroscopy from the Hobby-Eberly Telescope covering the planet’s full orbit. We detected helium escaping HAT-P-32 b at a 14σ significance,with extended leading and trailing tails spanning a projected length over 53 times the planet’s radius. These tails are among the largest known structures associated with an exoplanet. We interpret our observations using three-dimensional hydrodynamic simulations, which predict Roche Lobe overflow with extended tails along the planet’s orbital path.

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“…This scrambling is particularly important for a telescope with a variable pupil illumination (such as the HET). There are two low-resolution fiber integral field spectrographs: VIRUS, and the second-generation Low Resolution Spectrograph (LRS2, Chonis et al 2016;Hill et al 2021), and two fiber-fed high-resolution spectrographs: the Habitable-zone Planet Finder (HPF, Mahadevan et al 2018) and a forthcoming upgrade of the HET High Resolution Spectrograph (HRS, Tull 1998); the latter two instruments reside in temperaturecontrolled enclosures located in the basement inside the telescope pier. LRS2 is based on two VIRUS spectrograph units with the gratings replaced by higher dispersion grisms that span 3700 -10500 Å in four spectrograph channels.…”

Section: Introductionmentioning

confidence: 99%

The HETDEX Instrumentation: Hobby-Eberly Telescope Wide Field Upgrade and VIRUS

Hill,

Lee,

MacQueen

et al. 2021

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Hill et al.The Hobby-Eberly Telescope (HET) Dark Energy Experiment (HETDEX) is undertaking a blind wide-field low-resolution spectroscopic survey of 540 deg 2 of sky to identify and derive redshifts for a million Lyman-α emitting galaxies (LAEs) in the redshift range 1.9 < z < 3.5. The ultimate goal is to measure the expansion rate of the Universe at this epoch, to sharply constrain cosmological parameters and thus the nature of dark energy. A major multi-year wide field upgrade (WFU) of the HET was completed in 2016 that substantially increased the field of view to 22 arcminutes diameter and the pupil to 10 meters, by replacing the optical corrector, tracker, and prime focus instrument package and by developing a new telescope control system. The new, widefield HET now feeds the Visible Integral-field Replicable Unit Spectrograph (VIRUS), a new low-resolution integral field spectrograph (LRS2), and the Habitable Zone Planet Finder (HPF), a precision near-infrared radial velocity spectrograph. VIRUS consists of 156 identical spectrographs fed by almost 35,000 fibers in 78 integral field units arrayed at the focus of the upgraded HET. VIRUS operates in a bandpass of 3500−5500 Å with resolving power R 800. VIRUS is the first example of large-scale replication applied to instrumentation in optical astronomy to achieve spectroscopic surveys of very large areas of sky. This paper presents technical details of the HET WFU and VIRUS, as flowed-down from the HETDEX science requirements, along with experience from commissioning this major telescope upgrade and the innovative instrumentation suite for HETDEX.

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The habitable-zone planet finder: engineering and commissioning on the Hobby Eberly telescope (Conference Presentation)

Cited by 8 publications

References 0 publications

Kepler Planet Occurrence Rates for Mid-type M Dwarfs as a Function of Spectral Type

Kepler Planet Occurrence Rates for Mid-type M Dwarfs as a Function of Spectral Type

Giant tidal tails of helium escaping the hot Jupiter HAT-P-32 b

The HETDEX Instrumentation: Hobby-Eberly Telescope Wide Field Upgrade and VIRUS

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