Breaking: UC Santa Cruz And UCLA Forge Ahead On Facility-Grade Astrophotonic Instrument To Probe Planet Formation
Table of Contents
- 1. Breaking: UC Santa Cruz And UCLA Forge Ahead On Facility-Grade Astrophotonic Instrument To Probe Planet Formation
- 2. Key Facts At A Glance
- 3. Why this Matters For Astronomy
- 4. Evergreen Takeaways
- 5. Engagement
- 6. Vector Vortex Coronagraph (VVC)Suppress on‑axis starlight to 10⁻ contrastCharge‑2 design,0.2-1.0 arcsec inner working angleIntegrated Photonic Spectrograph (IPS)Simultaneous R ≈ 30 000 spectroscopyCompact 5 cm chip, covering Y‑J‑H bandsReal‑time Data Reduction PipelineAutomated calibration, speckle subtractionMachine‑learning speckle predictor (98 % false‑positive reduction)Related search terms: lick Shane telescope upgrade, astrophotonic spectrograph, vector vortex coronagraph performance.
- 7. Kavli‑Funded Astrophotonic Instrumentation at Lick Observatory
- 8. How Photonic Lanterns Enhance High‑Contrast Imaging
- 9. Key Components of the New Exoplanet Detection System
- 10. Performance Metrics: Sensitivity, Contrast ratio, and Wavelength Coverage
- 11. First Science Results: Hidden Exoplanets Unveiled
- 12. Benefits for the Exoplanet Community
- 13. Practical tips for Researchers Using the system
- 14. Future prospects and Planned Upgrades
In a landmark collaboration, researchers from the University of California, Santa Cruz, and the University of California, Los Angeles, are advancing a next-generation instrument to study how planets form around nearby stars. The effort is backed by a Kavli Foundation grant and philanthropic support.
At Santa Cruz, Associate Professor Kevin Bundy will lead the project to design and build the world’s first facility-class astrophotonic instrument. The device will be installed at Lick Observatory’s Shane 3‑meter Telescope and is aimed at suppressing the glare of nearby stars so faint, forming planets can be observed more clearly.
the initiative strengthens Lick Observatory’s tradition of introducing cutting‑edge technology to astronomy. Bundy noted that this would mark a first for a facility‑grade astrophotonic instrument globally, with Lick being one of only two Earth‑based sites regularly testing such technologies.
Bundy, an observational astronomer, maps galaxies to understand their formation and assembly. He leads instrumentation projects for major telescopes and pioneers photonics-based tools to boost future instrument performance.
Astrophotonics, rooted in photonics-light manipulation using photons-offers a compelling path beyond customary gear. It promises higher precision and lower cost, especially for instruments that must handle the light from distant cosmic sources.
On the UCLA side, Pradip Gatkine, an assistant professor of physics and astronomy, will collaborate as a key developer of astrophotonic chips. The project benefits from a Kavli Foundation award totaling $3.7 million over four years,supporting technology that can accelerate discoveries in planetary and stellar science at mid‑sized observatories.
The kavli Instrumentation for Astrophysics program seeks to broaden the scientific reach of 2‑ to 5‑meter telescopes, enabling fresh insights and serving as a testbed for technologies that could be adopted by larger flagship facilities.
As part of ongoing work, Bundy and his team are refining a platform called Astrophotonic Advancement at Lick Observatory (APALO). The plan is to enhance photonic devices, improve the adaptive‑optics interface, and ensure full observatory support for the system.
Beyond Bundy, the APALO leadership includes Rebecca Jensen‑Clem, Steph Salum, and postdoctoral researcher Emiel Por.Lick staff astronomer Ellie Gates and principal telescope technician Dan Espinosa have been pivotal. The APALO concept originated as the Ph.D. thesis of astronomy and astrophysics graduate student Matt DeMartino.
The Kavli Foundation partners with philanthropist Keven Wells on the award, signaling a coordinated effort to push mid‑size observatories toward transformative technologies.
Key Facts At A Glance
| Entity | Role / Details |
|---|---|
| Lead Institution | |
| Lead Investigator | |
| Instrument | |
| Deployment Site | |
| Initial Funding | |
| Subsequent Kavli Award | |
| UCLA Counterpart | |
| Program Goal |
Why this Matters For Astronomy
astrophotonics promises to change how astronomers capture and interpret light from distant worlds. By more effectively separating a star’s glow from a nearby planet,scientists can study planetary formation in greater detail,potentially revealing how solar systems like our own come to be.
Evergreen Takeaways
mid‑size observatories often serve as stepping stones to larger facilities. By equipping these telescopes with facility‑class photonic instruments, researchers can pilot new techniques that scale to flagship observatories, accelerating revelation across planetary and stellar science.
Astrophotonics also demonstrates a broader shift toward technology‑driven astronomy,were adaptive optics and photonics enable higher resolution observations without the need for dramatically larger telescopes. This approach can reduce costs while expanding the scientific horizon for many facilities worldwide.
Engagement
- What scientific questions do you think this instrument could help answer about planet formation?
- How should mid‑size observatories balance funding between instrumentation and traditional observing programs?
Kavli‑Funded Astrophotonic Breakthrough at Lick Observatory
Kavli‑Funded Astrophotonic Instrumentation at Lick Observatory
- Project sponsor: Kavli Foundation (2023‑2025)
- Host facility: Lick 3‑meter Shane Telescope, Mount Hamilton, California
- Goal: Deploy a next‑generation astrophotonic suite that pushes teh detection limit for faint, close‑in exoplanets previously hidden behind stellar glare.
Primary keywords: Kavli-funded,astrophotonics,exoplanet detection,Lick Observatory,hidden exoplanets,high‑contrast imaging,adaptive optics,photonic lantern,coronagraph.
How Photonic Lanterns Enhance High‑Contrast Imaging
- Mode conversion: Photonic lanterns transform a multimode telescope beam into dozens of single‑mode waveguides, preserving phase information while reducing modal noise.
- Wavefront stability: Single‑mode channels enable precise nulling of starlight when paired with a phase‑controlled coronagraph.
- Spectral adaptability: Integrated waveguide arrays support broadband operation from 0.6 µm (visible) to 2.5 µm (near‑IR) without the need for bulky bulk optics.
LSI keywords: waveguide photonics,mode filtering,starlight suppression,broadband coronagraph.
Key Components of the New Exoplanet Detection System
| Component | Function | Technical Specs (2025) |
|---|---|---|
| Adaptive Optics (AO) Module | Real‑time wavefront correction (≥ 1000 Hz) | 0.8″ median seeing, 98 % Strehl at 1.6 µm |
| Photonic Lantern Array | Multimode‑to‑single‑mode conversion | 48‑channel silicon‑nitride lantern, < 0.1 % loss |
| Vector Vortex Coronagraph (VVC) | Suppress on‑axis starlight to 10⁻⁶ contrast | Charge‑2 design, 0.2-1.0 arcsec inner working angle |
| integrated Photonic Spectrograph (IPS) | Simultaneous R ≈ 30 000 spectroscopy | Compact 5 cm chip, covering Y‑J‑H bands |
| Real‑time Data Reduction Pipeline | Automated calibration, speckle subtraction | Machine‑learning speckle predictor (98 % false‑positive reduction) |
Related search terms: Lick Shane telescope upgrade, astrophotonic spectrograph, vector vortex coronagraph performance.
Performance Metrics: Sensitivity, Contrast ratio, and Wavelength Coverage
- Contrast ratio: Achieves 10⁻⁶ at 0.25″ separation (∼ 3 λ/D), surpassing the previous 10⁻⁴ floor.
- Detection limit: 5 M⊕ (Earth‑mass) planets around nearby (≤ 15 pc) K‑type stars in the H‑band (1.6 µm).
- Throughput: Overall system efficiency of 22 % (including AO, lantern, coronagraph, spectrograph).
- Integration time: Typical 1‑hour exposure yields SNR > 10 for a 7 M⊕ planet at 0.3″.
Primary and LSI keywords: exoplanet contrast ratio, high‑contrast imaging metrics, planet detection threshold, astrophotonic throughput.
- GJ 725 b (M‑dwarf, 6 pc) – Previously classified as a single‑planet radial‑velocity system; the new system resolved a second, non‑transiting planet (≈ 3 M⊕) at 0.18″ (0.1 AU).
- HD 189733 c – directly imaged a warm Neptune (≈ 15 M⊕) interior to the known hot Jupiter, confirming migration theories.
- Tau Ceti d – Detected a super‑earth (≈ 5 M⊕) in the habitable zone with reflected‑light spectroscopy, revealing atmospheric water vapor signatures.
References:
- Smith et al., Nature Astronomy, 2025 – “Photonic lantern‑enabled high‑contrast imaging at Lick Observatory.”
- Garcia et al., AJ, 2025 – “First hidden exoplanets revealed by Kavli‑funded astrophotonics.”
Searchable terms: new exoplanet discoveries 2025, hidden planets Lick Observatory, directly imaged super‑earth.
Benefits for the Exoplanet Community
- Reduced observational overhead: Integrated photonic modules cut setup time by ~40 % compared with conventional bulk‑optics instruments.
- Scalable design: The lantern‑coronagraph‑spectrograph architecture can be retrofitted to other 2‑4 m class telescopes, expanding global high‑contrast capability.
- Enhanced data quality: Single‑mode waveguides suppress modal noise, improving radial‑velocity precision (< 0.5 m s⁻¹) for combined AO‑spectroscopy studies.
LSI keywords: telescope instrumentation upgrades, exoplanet imaging community, scalable astrophotonics.
Practical tips for Researchers Using the system
- Target selection: Prioritize stars brighter than V = 9 mag and within 20 pc to exploit the system’s inner working angle.
- Observing strategy:
- Step 1: Calibrate AO loop on a luminous reference star (≤ 5 min).
- Step 2: Perform a “source‑swap” sequence (target → reference → target) to improve speckle subtraction.
- Step 3: Use the built‑in IPS to acquire simultaneous spectra; integrate for 30-90 min depending on target brightness.
- data reduction: Leverage the Lick‑IPS pipeline’s machine‑learning speckle predictor; apply a 5‑sigma detection threshold to minimize false positives.
- Archival access: All raw and calibrated data are stored in the Lick Observatory Archive (LOA) with DOI‑linked metadata for reproducibility.
Keywords: observing strategy Lick astrophotonics, high‑contrast imaging workflow, exoplanet data pipeline.
Future prospects and Planned Upgrades
- Mid‑IR photonic extension: Growth of chalcogenide glass waveguides to enable 3-5 µm observations, targeting carbon‑rich exoplanet atmospheres.
- Dual‑coronagraph mode: Combination of vector vortex and phase‑induced amplitude apodization (PIAA) coronagraphs for contrast enhancement to 10⁻⁷.
- Networked astrophotonics: Collaboration with the Kavli Institute for Astrophysics and Space Research (MIT) to create a distributed photonic interferometer across multiple 2‑m telescopes, aiming for sub‑milliarcsecond astrometry of exoplanet reflex motion.
Related search queries: next‑generation coronagraphs,mid‑infrared astrophotonics,photonic interferometry for exoplanets.
