The NASA High-Resolution Speckle Interferometric Imaging Program: Validation and Characterization of Exoplanets and Their Stellar Hosts

Draft version January 22, 2021 Typeset using LATEX twocolumn style in AASTeX62

Steve B. Howell,1 Nicholas J. Scott,1 Rachel A. Matson,2 Mark E. Everett,3 Elise Furlan,4 Crystal L. Gnilka,1 David R. Ciardi,4 and Kathryn V. Lester1

1NASA Ames Research Center, Moﬀett Field, CA 94035, USA 2U.S. Naval Observatory, 3450 Massachusetts Avenue NW, Washington, D.C. 20392, USA 3NSF’s National Optical-Infrared Astronomy Research Laboratory, 950 N. Cherry Ave., Tucson, AZ 85719, USA 4NASA Exoplanet Science Institute, Caltech/IPAC, Mail Code 100-22, 1200 E. California Blvd., Pasadena, CA 91125, USA

(Received January 22, 2021; Accepted 19 Jan, 2021) Submitted to Frontiers - Space Science and Astronomy - Exoplanets: The Eﬀect of Stellar Multiplicity on Exoplanetary Systems

ABSTRACT Starting in 2008, NASA has provided the exoplanet community an observational program aimed at obtaining the highest resolution imaging available as part of its mission to validate and characterize exoplanets, as well as their stellar environments, in search of life in the universe. Our current program uses speckle interferometry in the optical (320-1000 nm) with new instruments on the 3.5-m WIYN and both 8-m Gemini telescopes. Starting with Kepler and K2 follow-up, we now support TESS and other space- and ground-based exoplanet related discovery and characterization projects. The im- portance of high-resolution imaging for exoplanet research comes via identification of nearby stellar companions that can dilute the transit signal and confound derived exoplanet and stellar parameters. Our observations therefore provide crucial information allowing accurate planet and stellar properties to be determined. Our community program obtains high-resolution imagery, reduces the data, and provides all final data products, without any exclusive use period, to the community via the Exoplanet Follow-Up Observation Program (ExoFOP) website maintained by the NASA Exoplanet Science Insti- tute. This paper describes the need for high-resolution imaging and gives details of the speckle imaging program, highlighting some of the major scientific discoveries made along the way. 1. INTRODUCTION pixel photometric apertures, it is possible that more The study of exoplanets is one of the most important than one star is measured, and thus the transit mea- topics in astrophysics today. Starting over a decade ago, surement becomes even more uncertain or unreliable. in support of the NASA Kepler mission, a program pro- To support exoplanet discovery, spectroscopic follow- viding follow-up observations began. It became clear up observations consisted of medium- and high-resolution as Kepler was nearing launch, that the 4 arcsec pix- work using reconnaissance spectra at the start and then els (Borucki et al. 2010) as well as the many possible large telescope efforts once specific validation steps were confounding events which could imitate exoplanet tran- passed (Furlan et al. 2018). Likewise, imaging observa- sit events (e.g., Brown et al. 2011; Santerne et al. 2013) tions were performed ranging from standard native see- arXiv:2101.08378v1 [astro-ph.EP] 21 Jan 2021 would require follow-up observations from ground-based ing CCD imaging and lucky imaging to high-resolution telescopes in order to validate and characterize any dis- observations (Furlan et al. 2017). These latter consisted covered transit candidates. In addition, for transit ob- of both Infrared Adaptive Optics (IR/AO) observations servations it is crucial to know the stellar properties well, using Lick, Palomar, and Keck and optical speckle inter- since the planet radius depends directly on the stellar ferometric imaging using WIYN and Gemini telescopes. radius. Also, given the relatively large pixels and multi- As new exoplanet transit missions such as K2 (Howell et al. 2014), and the currently operating missions TESS (Ricker et al. 2015) and CHEOPS (Benz et al. 2020) Corresponding author: Steve B. Howell come along, follow-up high-resolution (sub-arcsecond) [email protected] imaging continues to be needed and in larger amounts than before. While Gaia can resolve companions down 2 Howell et al.

Figure 1. A schematic timeline of NASA and ESA exoplanet related space missions and the ground-based follow-up telescopes NASA directly participates in. to near 1.0 arcsec and a bit closer using additional observations over time, e.g., EDR3; Fabricius et al. arXiv:2012.06242), it does not reach the spatial resolution of speckle imaging. Additionally, other exoplanet search techniques such as radial velocity (Kane et al. 2019) and ground-based small telescope transit surveys (Bakos et al. 2007) also benefit from speckle imaging of any candidate systems. Finally, the next wave of exoplanet space telescope missions will soon be upon us (Figure 1); missions covering larger and deeper sky areas such as PLATO (transits), and those hoping to obtain detailed exoplanet science such as the James Figure 2. Artist concept of the Ariel space telescope. Webb Space Telescope (JWST; transit spectroscopy, emission spectroscopy, direct imaging of exoplanets) and in order to assess their multiplicity, and secondly, imag- the Nancy Grace Roman Space Telescope (formally the ing of microlens sources to aid in the characterization of Wide Field Infrared Survey Telescope [WFIRST]; direct the source and lens stars. imaging and microlensing planets), as well as complete This paper provides an overview of the NASA high spectroscopic characterization of exoplanet atmospheres resolution speckle imaging program. Exoplanet tran- with Ariel (Figure 2). Anywhere high-resolution imag- sit and radial velocity studies mainly focus on (A)F to ing is needed, including for future missions such as LU- M stars, however, our speckle imaging techniques have VOIR, HabEX, or OST, our speckle program will be been used for research programs related to stars of all valuable. By that time, it is hoped that speckle imag- spectral and luminosity classes, extended objects, and ing will be an integral part of the 30-m ground-based solar system bodies. These applications are not dis- telescope system, providing angular resolutions near 5 cussed further in this report. Section 2 discusses the mas. need for high-resolution imaging, §3 presents the NASA For JWST, our program will provide high resolution mechanism to engage the exoplanet community, §4 and imaging in support of targeted exoplanets and their host §5 give an overview of the instrumentation used, the stars. Roman will make use of speckle imaging to sup- community program, and data produced in this pro- port exoplanet research in two main ways: First, to vet gram, §6 lists some of the major scientific discoveries and fully characterize direct exoplanet imaging targets Speckle Interferometry 3 the speckle program has made in relation to exoplanet is indeed multiple, and we know that about 40-50% of host star multiplicity, and finally we summarize in §7. exoplanet host stars have one or more stellar companions (Horch et al. 2014; Matson et al. 2018), then knowledge 2. THE NEED FOR HIGH-RESOLUTION IMAGING of the brightness and type of any companion stars are crucial in order to properly assess the exoplanet and host Survey telescopes, such as Kepler and TESS, cover star properties. a wide field of view, but have large pixels on the sky. Ciardi et al.(2015); Wang et al.(2015); Furlan and Kepler (and K2) had 4 arcsec/pixel values in their focal Howell(2017); Deacon et al.(2016) and Ziegler et al. plane and TESS has 20 arcsec/pixel. These large pixels (2018), for example, have shown that the presence of gather all the light from any stars present within the third-light will mean that the planet radius determined extracted photometric apertures. If a transit-like event from the transit depth alone is incorrect, the planet is detected, it is not immediately obvious which star in will always be larger than estimated from the transit the pixel (or actually in the pixels) used for light curve depth, at times so large as to lose planet status. Furlan construction is the cause of the event. Thus, the status and Howell(2017) noted that such third-light properties as a real exoplanet transit candidate remains in question will also decrease the mean density of the planet, pos- until some form of validation is carried out. sibly turning a terrestrial exoplanet into an ice giant as Telescopes such as Hubble have great spatial reso- well as causing atmospheric scale height calculations to lution, but they come at the cost of a small field of be flawed. These same two authors (Furlan and How- view and large over-subscription rates for observational ell 2020) also showed how the lack of knowledge of a proposals. While space has the advantage of stable companion star could cause measured stellar properties, observing conditions and no atmospheric effects, high- such as metal content and log g, to be incorrectly de- resolution imaging from the ground must make use of rived from an analysis of the star’s spectrum. Use of clever means to attempt to “remove” the blurring effects the knowledge of a companion (or not) allows a proper of the atmosphere. IR/AO uses (laser) guide stars and characterization of both the exoplanet and stellar prop- deformable mirrors while speckle interferometry freezes erties. High resolution knowledge of the scene around the atmospheric distortions using many short exposures host stars will remain an important diagnostic for fu- and reconstructs these into diffraction limited images ture transit, direct imaging, microlens, and atmospheric using specialized software techniques. spectroscopy exoplanet missions. Figure 3 illustrates these points for the case of KOI- As an aside, ROBO-AO is another high-resolution 1002 imaged from a typical ground-based telescope, Ke- imaging technique used in the optical wavelength range. pler, and TESS. The two bright stars in the top row Ziegler et al.(2017) discuss their results using this of the figure are approximately 25 arcsec apart. The method for exoplanet host stars. Unlike speckle imag- two stars are still separate in the Kepler image but near ing, ROBO-AO uses the mechanical deformable mir- enough to place scattered light or even be both captured ror techniques of IR/AO and applies them to optical in any aperture used to measure the photometry. In the light. To date, this application has suffered from the TESS image, it is difficult to even understand the scene. use of small aperture telescopes (<2-m) at sites provid- A good ground-based image, such as the top left image, ing modest native seeing (∼1 arcsec) and only low-order can be used to help understand the star field imaged by AO corrections due to the very short wavefront coher- TESS, but does not answer the question of which star ence times available in the optical. As such, ROBO-AO had the transit-like event. The bottom row of Figure observations resolve roughly equal mass binaries at sep- 3 shows optical speckle results obtained at Gemini and arations ≥0.8 arcsec with an increasing delta magnitude an IR adaptive optics image obtained at Keck for the contrast from ∼1 at 0.9 arcsec to ∼3 at 1.4 arcsec. star at the center of the top panel. Note the factor of ∼50 scale change in spatial dimension. We see that the speckle and the IR/AO images reveal that the central 3. THE SPECKLE IMAGING PROGRAM star is actually a binary system, thus while the transit- Our speckle imaging program is set up under the aus- like event could be real, the properties of the planet and pices of NASA through the Exoplanet Exploration Of- its host star would need revision due to the third-light fice (ExEP) NN-EXPLORE program located at the Jet of the close, likely bound companion. Propulsion Laboratory (JPL). The ExEP provides ad- These types of follow-up high-resolution images are vocacy for the exoplanet community to NASA in terms key to understanding the light within the scene of an of future mission science directions, needed technol- exoplanet host star candidate. This is an important step ogy, and exoplanet science critical to enable a full un- in exoplanet validation and characterization. If the star derstanding of exoplanets, their environments, and the 4 Howell et al.

Figure 3. (Top row) Ground-based seeing-limited image of KOI-1002 (star at center) obtained from the Palomar Observatory Sky Survey (POSS). The image shows the local star field which contains two bright stars. The Kepler image is from the standard 30-minute postage stamp images downloaded from the spacecraft and the TESS “image” was produced (before TESS had observed the Kepler FOV) by convolving the Kepler image with the TESS 20 arcsec pixel size kernel. (Bottom row) Here the much smaller spatial dimension boxes are centered on the bright central star in the top row and it is revealed in the high- resolution images that the star is a binary system with a separation of about 0.5 arcsec. The Keck AO image shows the central 3 arcsec box. The speckle images took a total time of 5 minutes (3 minutes on source) and reached a contrast of 6.5 magnitudes while the IR/AO image required 15 minutes total time (∼1.5 minutes on source) and reached a contrast limit of 9.2 magnitudes. The inner working angle for the speckle and IR/AO observations was ∼20 mas and ∼50 mas respectively. search for life. As an aid to establishing an open fo- stellar parameters and directly assessing the topics rum with the community, the ExEP maintains two “gap of exoplanet formation, migration, dynamics, and lists”, one for technology1 and one for science2. Each evolution. of these documents represent community vetted gaps, Science Gap 10 - Precursor Observations of Direct that is, areas which need additional understanding in • Imaging Targets the pursuit of exoplanet science. The ExEP science gap list contains twelve specific areas that the exoplanet Speckle imaging provides exploratory observations community has agreed are in need of further, detailed of potential targets for future direct imaging and understanding. Our speckle interferometry program di- atmospheric observation missions, assessing their rectly addresses five of these science gaps and enables multiplicity and thus their potential as high-value four additional ones. targets. Science Gap 04 - Planetary System Architectures: Directly Addresses • Occurrence Rates for Exoplanets of all sizes • Science Gap 12 - Measurements of Accurate Tran- Speckle imaging allows the correct exoplanet and siting Planet Radii stellar properties to be determined. This in turn Speckle imaging provides knowledge of compan- is used to derive robust occurrence rates for exo- ions, especially true bound companions and, if de- planets orbiting stars in multiple star systems. tected, the ability to correct the exoplanet radius • Science Gap 05 - Occurrence Rates and Uncertain- and other properties for “third light”. ties for Temperate Rocky Planets (eta-Earth) • Science Gap 07 - Properties of Known Exoplanet Speckle imaging addresses exoplanet occurrence Host Stars rates as described above and allows habitable zone Speckle imaging provides knowledge of the multi- locations in binary host star systems to be deter- plicity of exoplanet host stars providing accurate mined yielding eta-Earth rates for temperate planets.

1 https://exoplanets.nasa.gov/exep/technology/gap-lists/ 2 https://exoplanets.nasa.gov/internal resources/1547/ Enables Speckle Interferometry 5

• Science Gap 01 - Spectral characterization of at- time during the year. ‘Alopeke and Zorro are able to mospheres of small exoplanets be operated remotely from the Gemini control room or anywhere internet is available via a secure connection to • Science Gap 02 - Modeling exoplanet atmospheres the observatory. • Science Gap 03 - Spectral signature retrieval

• Science Gap 06 - Yield estimation for exoplanet direct imaging missions

4. THE SPECKLE INSTRUMENTS Just before the Kepler mission was launched, we began our speckle imaging work to support the NASA community. At that time, we used the Differential Speckle Survey Instrument (DSSI; Horch et al. 2009) on the 3.5- m WIYN telescope located on Kitt Peak in southern Arizona, USA. This instrument was a workhorse during the Kepler mission, providing high-resolution images of ∼1000 Kepler Objects of Interest (KOIs). Since Figure 4. Schematic CAD drawing of ’Alopeke or Zorro that time, three new instruments of similar overall de- (they are identical), the speckle instruments residing at the sign but with increased functionality, larger and faster twin Gemini 8-m telescopes. The compact design is illus- EMCCD imagers, and modernization in terms of au- trated along with the primary parts labeled. ’Alopeke and tomation, user interface, filter wheels, and remote op- Zorro both mean fox in the indigenous language of the local eration have been built and deployed. The three new people. instruments are the NN-EXPLORE Exoplanet Star and 3 Survey Imager (NESSI ; Scott et al. 2018) at the 3.5- 5. THE COMMUNITY OBSERVING PROGRAM m WIYN telescope, and ’Alopeke and Zorro4, (Scott et al. 2021, in prep.) duplicate instruments at the twin The NASA speckle imaging program is openly avail- Gemini 8-m telescopes in Hawaii and Chile. able to the world-wide exoplanet community. While we Each of the new instruments provide simultaneous ob- have built and deployed the speckle instruments, our servations in two optical bands, determined by filters observing protocol is a community-based program with placed in each of two beams, split at 700 nm. Fig- targets and observing priorities set by the missions and ure 4 presents a schematic of the Gemini instruments the community. with the major parts labeled and Figure 5 shows one Below, we discuss the observational program, the tar- of the instruments being constructed in our optics lab get selection methodology, the data reduction processes, at NASA Ames (left) and the completed instrument and the archives which house the raw and reduced data mounted on the Gemini telescope (middle and right). products. Table 1 presents the general parameters of these new in- 5.1. Observations struments with ’Alopeke and Zorro being identical there- Proposals to use the speckle instruments, including fore having identical parameters. The instruments have proposals submitted by our team, are peer reviewed for two field of view options user selectable in real-time; a each telescope by the relevant telescope allocation com- narrow speckle imaging field and a wider more tradi- mittee (TAC). Once the approved programs are known tional imaging field of view. The angular resolution of for a semester, we work with each observatory to set these instruments provide inner working angle spatial up block scheduled observation runs, once or twice each resolutions for nearby exoplanet host stars (e.g., TESS) semester on each telescope. Each run consists of 6-10 of <10 au (Matson et al. 2019). nights depending on time demand. These instruments are fully integrated into the tele- All speckle targets are placed in a queue to be ob- scope control systems where they reside and the Gemini served by our team during the observing block. Most instruments are permanently mounted for use at any targets are observed in the usual manner (Howell et al. 2011) that is, thousands of 40 to 60 msec images are 3 https://www.wiyn.org/Instruments/wiynnessi.html simultaneously collected in two narrow band filters, one 4 https://www.gemini.edu/instrumentation/current- each in the blue and red regions of the optical band- instruments/alopeke-zorro pass. Here blue and red are defined by the dichroic 6 Howell et al.

Table 1. Speckle Interferometers

Instrument Telescope Detectorsa FOV(”)b ”/pixelb Filtersc Resolution (mas) Limiting Mag (R) NESSI WIYN EMCCD 19/83 0.02/0.08 SDSS ugriz + 4 narrow band 39 @550nm/ 64 @880nm ∼13.2 ’Alopeke Gemini-North EMCCD 6.7/60 0.01/0.1 SDSS ugriz + 4 narrow band 17 @562nm/ 28 @832nm ∼18 Zorro Gemini-South EMCCD 6.7/60 0.01/0.1 SDSS ugriz + 4 narrow band 17 @562nm/ 28 @832nm ∼18 aEach instrument uses two Andor iXon Ultra 888 back-illuminated Electron Multiplying (1024X1024, 13 micron) pixel CCDs (EMCCDs). b Values given are for the “speckle” / “wide-ﬁeld” of view modes. c Narrow band ﬁlters are centered at 466nm, 562nm, 716nm, and 832nm.

Figure 5. (Left) One of the two identical speckle imagers under construction at the NASA Ames Research Center. The two grey boxes extending out of the black box are the two Andor EMCCD cameras. (Middle) A close-up view of the instrument mounted on Gemini at the GCAL port and (Right) a view of the instrument (black box) with the associated power supply, electronics, and computer unit (white box). See yellow arrows.

in our instruments, splitting the optical light at 700 nm and selection. The priority order reflects target bright- (See Table 1). Some observations may come with special ness, number, location or type of exoplanet candidates, requirements such as the use of specific filters, extended or stellar properties. The list contains 100-200 targets integration times, or specific time constraints. at a time and gets updated throughout each observing season. 5.2. Target Selection The second main way is direct communication with Targets to observe are selected in three main ways. our group. If an exoplanet host star is in need of high- First, each space mission or ground-based exoplanet pro- resolution imaging, regardless of what space mission or gram has a team of scientists and staff designated to ground-based telescope discovered it or who is currently produce a priority list of targets to be observed. These studying the target, we will add it into our priority list targets, usually called “objects of interest” (e.g., Ke- and observe the target for the PI. This method usu- pler objects of interest, KOIs or TESS objects of in- ally involves 1 to a few targets of immediate interest to terest, TOIs) are listed in priority order and provided someone in the exoplanet community. to our observing team ahead of each observation run. Finally, PIs can propose for telescope time themselves For example, the TESS Follow-up Observing Program as each of our instruments at their associated telescopes Working Group as well as the TESS sub-group for high- have “open sky” policies, that is, proposals are accepted resolution imaging (SG3) play roles in target ranking from anyone. Speckle Interferometry 7

5.3. Data Reduction Speckle interferometry produces diffraction-limited images over a small field of view (∼1 arcsec) by using very short exposure times to ”freeze” the atmosphere. Fourier or other techniques are then used to reconstruct these images and search for interference fringes that exist if two or more stars are within the narrow field of view (See Figure 6).

Figure 7. One of our standard pipeline reduced data products. The plot shows our 5σ contrast curves in both filters Figure 6. Power spectrum of TOI-1356, an exoplanet host- as a function of the angular separation out to 1.2 arcsec, the ing star, produced by our reduction pipeline using 2000 end of speckle coherence. In addition, the inset shows the speckle images and obtained at the WIYN telescope. Note reconstructed 832 nm image with a 1 arcsec scale bar. This the interference fringes whose spacing, intensity, and orien- star, TOI 141, was found to have two close companions, one tation allow a reconstructed image (right) to be produced. at 0.5 arcsec (PA=240 degrees, Delta magnitude = 4.6) and From this image and the Fourier analysis, we can determine one at 1.3 arcsec (PA=307 degrees, Delta magnitude = 6.2). the separation, position angle, and magnitude difference of The yellow arrows mark the companions in the reconstructed the two stars. In this case, the host star is a member of image and the black stars mark the locations of the stars on a close binary having a separation near 0.16 arcsec. The the main plot, the 1.3 arcsec companion placed at 1.2” to fit reconstructed image is 2 arcsec on a side. within the plot.

FOP) archive6. They are accessible to the public once Speckle imaging has been used since the early 1970’s the proprietary period has ended. All of our community but has been greatly upgraded since then, now using dig- observations, that is those observed within the NASA ital detectors, large telescopes, and advanced software proposed program time, are available to the public with techniques. For example, EMCCDs provide for electron no proprietary period. Other PIs observing exoplanet multiplication in the output gain register, increasing the targets can specify a proprietary period of up to 12 input signal by up to 1000 times. Stars as faint as 19th months, however, most PIs choose no proprietary pe- magnitude can now be observed using our instruments riod as well. at Gemini coupled with their EMCCD detectors. All observed targets are listed on the Exoplanet Our standard data reduction pipeline and the data Follow-Up Observation Program website7 within days of products available are described in Howell et al.(2011) an observing run; in this way the community is informed with some additional reduced data products now pro- about which exoplanet host stars have been imaged with vided (e.g., Figure 7). The following reduced data prod- our speckle instruments. Final data products from the ucts are delivered to each PI: sensitivity curves, recon- reductions are also posted on ExoFOP; tags link them structed images, and any binary ﬁt parameters if a com- to the corresponding entries in the imaging observations panion is detected. tables. For targets observed as part of our community program, the reduced data products are posted on Exo- 5.4. Data Archives FOP soon after an observing run ends and the reduction Our raw data and reduced data products are archived has been completed, typically within a few weeks. To at both the Gemini data archive5 and the NASA Ex- date, we have observed over 1,000 exoplanet host stars oplanet Archive, Exoplanet Follow-up Program (Exo-

6 https://exoplanetarchive.ipac.caltech.edu 7 5 https://archive.gemini.edu/searchform https://exofop.ipac.caltech.edu/tess/ 8 Howell et al. from Kepler and K2 and more than 500 TESS mission Everett et al.(2015) and Hirsch et al.(2017) also used TOIs, so far, for the community. These observations model isochrones to provide evidence that companion have been used to validate and characterize exoplanets stars around KOIs are bound or not. Finally, Colton in over 65 published papers in the past 1.5 years. et al.(2020) has begun to measure space and orbital mo- tions for exoplanet host stars with stellar companions, 6. DISCOVERIES IN STELLAR MULTIPLICITY a process that takes decades for the far away Kepler stars, but will only take a few years for some very close In addition to validating and characterizing numerous K2 and TESS binary host stars with separations of ≤10 exoplanet discoveries as contributions to the exoplanet au. These astrometric measurements have already be- community research, we have used the large samples of gun to provide information on the formation, dynamics, exoplanet host stars observed at high resolution to en- and evolution of exoplanet systems. able a number of overarching findings. 4) Which star in a binary hosts the exoplanet: Tran- 1) Percentage of binary exoplanet host stars: For both sit discoveries in binary host stars often leave open the the Kepler and K2 exoplanet host stars, and it seems question of which of the stars the exoplanet(s) actually true also for TESS, we have shown that for those stars orbit. If the planet orbits the primary, the transit depth hosting at least one exoplanet, 40-50% of them reside in may require only a modest correction due to a fainter binary or multiple star systems; See (Horch et al. 2014; secondary star. However, if the transit is due to some- Matson et al. 2018) and the upcoming papers by Howell thing orbiting the secondary star or the two stars are et al. (2021) and Lester et al. (2021). nearly equal in brightness, it can be very unclear what 2) Binary host star properties: Recent work (Howell the measured transit depth is really telling us. One way et al. 2021) has shown that the mass ratio of exoplanet to solve this dilemma was employed by Howell et al. host star binaries follows that of field binaries, that is (2019) for the binary A star exoplanet host Kepler-13. an excess of nearly equal mass systems. The orbital Using simultaneous time-series speckle observations of period distribution however does not. These authors both stars in the pair, it was shown that the transit find that exoplanet hosting binary stars show generally occurs on Kepler-13A. larger mean separations having a peak in their orbital separation near 100 au, not 40 au as for the field sample (Raghavan et al. 2010). Furlan and Howell(2017, 2020) have shown that it 7. SUMMARY is critical to fully understand the “scene” of light near We have summarized our continuing decade long an exoplanet host star. If a close companion is present, NASA high resolution imaging work for exoplanet re- both the exoplanet and the stellar properties determined search. Using speckle interferometry, we carry out a may be in error. community led observational program that supports 3) Bound vs. line of sight companions: Using statis- space- and ground-based exoplanet efforts. Observa- tical modeling, Horch et al.(2014) and Matson et al. tions are obtained at the WIYN 3.5-m telescope in (2018) have shown that most stellar companions that Arizona, and at both the Gemini-North and Gemini- reside within 0.4 arcsec (at Gemini) and 0.8 arcsec (at South 8-m telescopes located in Chile and Hawaii. We WIYN) of the primary star are true bound companions have designed and built new instruments for these tele- (at ≥90% probability). These limits are important to scopes that are available to the community through peer note as stellar companions found to lie farther from the review proposals under the NN-EXPLORE/NOIRLabs host star are most likely, but not exclusively, line of open-sky policies. All our observations and their fully sigh companions, therefore not part of the formation, reduced data products are made available via public dynamical, and evolutionary processes of the exoplan- data archives. etary system. However, they nonetheless cause transit Sub-arcsec imaging, especially inside of 0.4 arcsec, is dilution, and so their flux has to be taken into account critical for our detailed understanding of exoplanets, when the transit depth and exoplanet properties are de- their host stars, and the search for other life in the rived. Observational techniques such as lucky imaging Universe. Exoplanet radii and mean densities, plus the or ROBO-AO tend to only detect companion stars which stellar properties of their hosts, can be incorrectly de- are 0.75 arcsec or farther away. Even Gaia cuts off at termined without proper knowledge of the close-in light direct companion detection near 1.0 arcsec. At such sub- scene. arcsecond angular resolutions, speckle imaging provides Our imaging program has supported many exoplanet inner working angles for many of the target stars of 1 to validation and characterization studies for space mis- a few au. sions and ground-based surveys, and radial velocity Speckle Interferometry 9 studies as well as made scientific findings itself along We thank Elliott Horch and William Sherry for their the way. previous team work. Additionally, we thank the gener- We plan to continue our community service program ous support and collaboration of the staff at the WIYN throughout the TESS extended mission and into the and Gemini Telescopes, they are indeed part of the JWST and Roman missions and beyond. Team. We appreciate the reviews by the referees which led to a better paper. Finally, we’d like to thank NASA CONFLICT OF INTEREST headquarters and the Exoplanet Program Office at JPL, The authors declare that the discussion and research in particular, Doug Hudgins, Gary Blackwood, and John was conducted in the absence of any commercial or fi- Callas, for their substantial support of the speckle imag- nancial relationships that could be construed as a po- ing program over these many years. tential conflict of interest. Facilities: WIYN:3.5m (NESSI), Gemini-North:8-m (’Alopeke), Gemini-South:8-m (Zorro) ACKNOWLEDGMENTS

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