Next-generation planet hunters in the optical and near-infrared Sam Halverson University of Pennsylvania

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1 Next-generation planet hunters in the optical and near-infrared Sam Halverson University of Pennsylvania 1 Image credit: NASA/JPL

2 Next-generation planet hunters in the optical and near-infrared Doppler spectrometers Sam Halverson University of Pennsylvania 2 Image credit: NASA/JPL

3 Next-generation planet hunters in the optical and near-infrared stellar activity measurement machines Sam Halverson University of Pennsylvania 3 Image credit: NASA/JPL

4 Full collaboration snapshot Suvrath Mahadevan (PSU - PI) Larry Ramsey (PSU) Fred Hearty (PSU) Sam Halverson (Penn) Chad Bender (UA) Chris Schwab (Macquarie) Paul Robertson (PSU) Andy Monson (PSU) Jason Wright (PSU) Tyler Anderson (PSU) Scott Diddams (NIST Boulder) Ryan Terrien (NIST Boulder) Cullen Blake (Penn) Mike McElwain (GSFC) Qian Gong (GSFC) Arpita Roy (Caltech) Gudmundur Stefansson (PSU) 4

5 Radial velocity planet discovery space RV signal induced by Earth

6 Current instrumental state of the art in precision Doppler spectroscopy NIR 5 m s -1 Goal VIS 1 m s -1 1 m s -1 Goal 10 cm s -1

7 Sun-like System M-Dwarf System HZ HZ : Center of Mass Halverson JPL AC Colloquium ~10 cm/s ~1 m/s

8 Pushing towards Earth-mass planets will require a shi9 in technologies Earth-size planets in the Habitable-zone Shift focus to Mdwarfs Larger Doppler signals NIR spectrometers Over 50% of stars within 25 pc are M-dwarfs Improve measurement precisions in the optical Improved spectrometer design Optical frequency combs Dedicated telescope time

9 Pushing towards Earth-mass planets will require a shi9 in technologies Earth-size planets in the Habitable-zone Shift focus to Mdwarfs Larger Doppler signals NIR spectrometers Over 50% of stars within 25 pc are M-dwarfs Improve measurement precisions in the optical Improved spectrometer design Optical frequency combs Dedicated telescope time

10 The Habitable-zone Planet Finder (HPF) instrument Near-infrared spectrometer 10 meter telescope h;p://hpf.psu.edu/ NSF MRI funded, Fall 2011

11 The Hobby-Eberly Telescope Located at McDonald Observatory 10 meter effecjve aperture Fixed zenith angle design. University partners: UT AusJn, PSU, Stanford, Munich, GoQngen Queue-based observing 11

12 The Habitable-zone Planet Finder Spectrometer Vacuum chamber Radiation shield Heaters Thermal straps Spectrometer optics Getters LN2 Tank Near-infrared coverage ( nm) Cryogenic operajon (180 K), 0.1 mk thermal stability achieved Fed by custom opjcal fiber delivery system, op4cal frequency comb calibra4on source <1 m/s single measurement precision goal (J<10, 30 min) Q delivery 12

13 HPF opjcal train Asymmetric white-pupil design. R4 echelle grajng for primary dispersion, VPH grism for cross-dispersion R = 50,000, z/y/j band coverage ( nm), 1.5 fiber w/ 0.5 slit 1.7 micron cutoff Hawaii-2RG detector Primary dispersion direction 13

14 Simulated HPF focal plane on H2RG detector Individual diffraction orders Sky fiber Calibration source Starlight λ 14

15 Primary calibrajon source is broadband laser frequency comb Picket fence of lines Jed to atomic standard. Stable at the <1 cm s -1 level. HPF will use broadband electroopcc comb for primary calibracon 1064 nm CW laser Optical amplifier Pulse shaper Optical amplifier 30 GHz RF signal Block diagram of HPF EOM laser comb ide credit: AJ Metcalf, NIST Boulder 15

16 Illumination stability is critical Spectrometer focal plane Telescope focus d Flux Fiber output 6 km/s Wavelength Fundamentally, spectrometer records monochromacc images of fiber face Guiding errors and telescope pupil changes manifest as spectral line changes* Not traced with calibrajon source 16

17 Specialty fibers essential for stabilizing spectrometer PSF Single fiber: Fibers + double scrambler: Telescope focal plane Fiber output Instrument profile (spectral line) Flux Flux λ λ 17

18 Optic integration complete Echelle grating VPH grism Camera assembly

19 Robertson Thermal control stability within cryostat

20 Environmental control precision

21 First light laboratory image 1280 nm 810 nm

22 Pushing towards Earth-mass planets will require a shi9 in technologies Earth-size planets in the Habitable-zone Shift focus to Mdwarfs Larger Doppler signals NIR spectrometers Improve measurement precisions in the optical Improved spectrometer design Optical frequency combs Dedicated telescope time

23 h;p://neid.psu.edu/

24 NASA Exoplanet roadmap TESS launch

25 WIYN telescope Ki; Peak in southern Arizona 3.5 meter primary mirror Partners: Wisconsin, Indiana, NOAO, NSF NN-Explore program announced in 2015 for dedicated exoplanet research 140 nights / year allocated to exoplanet studies Queue-based observing implemented for NEID GTO program (30 queue nights per year, 5 years) h;p:// 25

26 NEID: the next technological step in Doppler measurement machines Vacuum chamber Radiation shield Heaters Spectrometer optics Getters LN2 Tank Covers full opjcal range ( nm) Precision goal is 10 cm s-1 (not including star) Broadband commercial op4cal frequency comb calibra4on source Q delivery 26

27 NEID optical layout Fiber-fed, symmetric white-pupil design. R4 disperser, large prism cross-disperser R = 100,000, nm coverage 9k x 9k e2v CCD, 10 micron pixel pitch (90 x 90 mm) 27 Primary dispersion direction

28 Wide spectral grasp is essential HARPS NEID Wide bandwidth essenjal for acjvity indicators Enables study of wide range of spectral types

29 What does 10 cm s-1 look like? Ki Bun Kin, SPIE 2012 TEM image of silicon wafer lattice

30 What does 10 cm s-1 look like? Ki Bun Kin, SPIE 2012 TEM image of silicon wafer lattice

31 Major component fabrication well underway Echelle grating complete Vacuum chamber, radiation shield, optical bench complete HPF Prism being fabricated NEID

32 New technologies to tackle old problems Beyond the era where single instrumental error source dominates measurement precision NEID will require suite of cuqng edge technologies to reach precision goal: Broadband commercial laser frequency comb calibra4on source Stabilized broadband fabry-perot etalon source (Halverson+ 2012, Halverson+ 2013, Halverson+ 2014a) Extremely stable instrument illumina4on. (Halverson & Roy+ 2015, Halverson+ 2016a) New fiber modal noise mi4ga4on techniques (Halverson+ 2014b, Mahadevan & Halverson+ 2014) Improved CCD characteriza4on and calibra4on (Blake & Halverson+ 2017, Halverson in prep) Solar contamina4on mi4ga4on techniques (Roy & Halverson+ 2017, in prep.) Novel barycentric correc4on techniques n -> Halverson JPL Colloquium 32

33 Performance budgeting is key for estimating measurement precision at these levels Halverson JPL Colloquium 33 Halverson+ 2016

34 New era of high precision Doppler spectroscopy HPF will be first NIR RV planet hunter on 10 m telescope (Q3 2017) Large aperture gives unparalleled access to wide array of nearby M-dwarfs Valuable instrument for following up TESS M-dwarf targets, down selecjon for JWST Will ujlize a suite of new technologies to probe the M-dwarf planet discovery space: Highly stabilized opjcal train OpJcal frequency comb calibrajon source Unique opjcal fiber delivery system NEID aims to be next technological step in Doppler spectroscopy for finding Earth-twins Gives US community unprecedented capability for planet detecjon, follow-up of interesjng targets discovered by TESS / K2, direcjon for JWST / WFIRST-AFTA Queue-based observing, combined with extremely stable spectrometer. Builds off technologies developed for HPF Modeling of instrumental errors at the cm/s level is key for understanding systemajcs, charjng path towards 10 cm s -1 34