SCIENCE

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Deep Sky Hawaiʻi · Observational Astronomy

Science

A planet crosses a distant star. A star begins to pulse.
We turn tiny changes in light into clues about the universe.

Beyond the beautiful image

The universe
leaves a signal.

A telescope can do more than reveal a distant object. It can measure how that object changes. Our mobile observatory is being developed to turn nights under Hawaiʻi’s skies into precise records of starlight.

Science observing program in development
01 / EXOPLANET TRANSITS

NASA Exoplanet Watch methods

A world hidden
in a flicker.

A planet passing in front of its star blocks a little of the light. Measure that tiny dip, exposure after exposure, and a world begins to reveal itself. Repeated observations of known planets can refine when their next transits will happen.

Explore Exoplanet Watch

How a transit worksInteractive model

A planet crosses in front of a starMove the slider to move the dark planet across the bright star. The marker below shows the corresponding dip in observed brightness. Planet crosses the face of the star
A transit light curveRelative brightness drops while the planet is in front of the star and returns to its previous level after the transit. Time runs from left to right. Relative brightness BeforeDuring transitAfter Time →

Planet crossing · light dips

Illustrative model · sizes and transit depth exaggerated.
02 / VARIABLE STARS

AAVSO observing methods

Stars have a rhythm.

Some stars pulse. Others erupt or dim as a companion moves in front of them. Comparing a target with steady stars in the same field lets us trace those changes—and connect one night’s measurements to a much longer story.

Discover variable-star observing

The rhythm of a starInteractive model

A star’s changing glow follows a repeating brightness curveThe star brightens and dims while a moving dot follows the corresponding light curve. Change the pulse speed to change how often the pattern repeats. The glow represents brightness, and time is compressed.BrighteningFollow the light below.Relative brightnessTime →

Illustrative brightness cycle · time compressed.

03 / TESS FOLLOW-UP

A direction for our science program

Follow the next clue.

NASA’s TESS mission finds promising dips in starlight. A closer look from the ground helps establish which star is changing, improve transit timing, and investigate false positives. We are developing the capability to take part in that kind of follow-up.

Explore the TESS follow-up program

From survey to targetIllustration

A candidate star selected from a wide field for closer observation Wide-field surveyGround-based follow-up

How light becomes evidence

From photons
to a light curve.

The science comes from a careful, repeatable process—one exposure at a time.

01

Track.

Equatorial tracking and autoguiding keep the same star field steady through the night.

02

Collect.

Cooled astronomy cameras record a timed sequence of exposures of the target and nearby stars.

03

Calibrate.

Correct camera signatures and compare the target’s brightness with reference stars.

04

Measure.

Plot brightness against time. The pattern reveals what changed—and when.

One observatory. More to discover.

Come for the stars.
Stay for the questions.

On public nights, we reveal nebulae, galaxies, and clusters. Our developing science program takes the same curiosity further: turning the light we collect into measurements that can support research.

Our science program is in development. NASA Exoplanet Watch, AAVSO, and TESS follow-up are referenced as observing frameworks and contribution pathways; these references do not imply sponsorship, partnership, or official affiliation. Graphics are explanatory illustrations.