2020- 2021 OSSC Election Results
to the new 2020-2021
OSSC Board of Directors!
President - Kevin Romero
Vice President - Stan Klyza
Secretary - Martin Seilonen
Treasurer - Martin Hagenbuechle
mourns the loss of our good friend and colleague Dr. Antonio Méndez. An innovator, educator and mentor, Antonio served the Southern California optical community throughout his decades-long career. He will be missed.
Private services have been arranged for family. In lieu of flowers, the family suggests donations to a charity of the donor’s choice.
The June 2020 Edition of OSSC's Images eNewsletter is now available.
There was an Information Session - Monday 19 August
OSSC Fellow Donn Silberman was the guest speaker.
Fall 2020 courses begin in Late Sept.:
Go to the links above to learn more about the courses and programs.
15% discount for OSSC Members on courses
Required for a Certificate.
Email: Kadie Heck
with confirmed OSSC
to receive discount code.
Laser Tech Training Program
With the current situation regarding On-Campus Educational instruction, the Laser Tech Training Program is planned to be moved to Pasadena City College this summer with courses beginning this Fall. This, however is subject to change depending of circumstances.
Check back here over the coming months to see updates. The following notes will remain true.
Laser and Photonics Technology instructors lead hands-on, laboratory-driven classes, utilizing state-of-the-art industrial equipment, based on the industry-guided photonics curricula written by industry professionals. In addition to laboratory skills, students are offered one-on-one support and career advice, including résumé and LinkedIn profile building.
For Information Contact:
Prof. Brian Monacelli, Ph.D.
Recent SCAVS Event
Tuesday 21 July
FREE Zoom Webinar:
Thin Film Filters and Coatings for Ultraviolet Astronomy, Astrophysics, and Planetary Science
Dr. April Jewell, JPL Advanced Detectors,
Systems and Nanoscience Group
Abstract: The presentation will discuss JPL’s 2D-doped silicon detectors and advanced coatings technologies, including a discussion of practical materials, design, and deposition techniques for ultraviolet (UV) films. Device response is improved using AR coatings to mitigate reflection losses. JPL uses atomic layer deposition (ALD) to prepare AR coatings, which uses a series of self-limiting chemical reactions to grow thin films on surfaces. Due to its highly controlled growth mechanism, in which a film is deposited a fraction of a monolayer at a time, ALD gives nanometer-scale control over film thickness and composition with well-defined, sharp interfaces. The result is 2D-doped detectors that exhibit record UV performance. The detectors are enabling significant advances in instrument technologies for exciting new science in astrophysics, planetary science, and heliophysics, including on vehicles such as sounding rockets, suborbital balloons, CubeSats, and future Explorer, Probe, and Flagship missions.
Recent VOSA Meeting
Tuesday 12 May
LightSail 2 - Achieving Flight By Light
Justin Mansell, Planetary Society &
Purdue PhD Candidate
Abstract: In July 2019 the LightSail 2 CubeSat unfurled its 32 m2 solar sail in space above the Earth. Then, tacking the sail like the sea-fairing vessels of olde, the spacecraft succeeded in changing its orbit using the pressure of sunlight. The achievement was the culmination of a 10-year crowd funded program sponsored by The Planetary Society to raise the public and technical profiles of solar sailing through a pair of flight experiments. Unencumbered by limited propellant, the technology has the potential to enable entirely new types of space missions, including feasible travel to other stars. But while the concept of solar sailing is centuries old, its realization is new and there is much to learn. This talk will describe the major challenges faced during the LightSail 2 mission, along with the achievements and lessons that resulted. The flight team continues to refine solar sailing and conduct imaging from the spacecraft to engage the public interest and deepen the mission’s technical impact.
Recent OSSC Meetings
Wednesday 24 June
Annual Business Meeting
Online Meeting - Webinar:
Results of 2020-2021 OSSC Board of Directors election were shared with the membership.
The new leadership team was introduced,
The past year reviewed and
The upcoming year previewed.
Wednesday 10 June
Spectrally Controlled Interferometry for the Measurement of Flat and Spherical Optics
Abstract: Conventional interferometry is widely used to measure spherical and flat surfaces with nanometer level precision but it is often plagued by back or multiple surface reflections. At this meeting a new method of isolating the measurement surface by controlling the spectral properties of the source will be described (Spectrally Controlled Interferometry - SCI). Using spectral modulation of the interferometer's source enables formation of localized fringes where the optical path difference is non-zero. As a consequence, it becomes possible to form white-light like fringes in common path interferometers, such as the Fizeau or Twyman-Green. ÄPRE’s SCI technology does not require mechanical phase shifting, resulting in simpler instruments and offers the ability to upgrade existing interferometers. Furthermore, SCI allows absolute measurement of distance, including radius of curvature of lenses, in a single setup with the possibility of improving the throughput and removing some of the pitfalls of inaccurate measurements.
Wednesday 13 May
Multiphoton Imaging of Human Skin
Abstract: Multiphoton imaging of human skin provides access to morphological information with molecular contrast obtained in a noninvasive manner. Our group at Beckman Laser Institute pioneered the clinical skin imaging with multiphoton microscopy. This talk will present the latest developments on the new generation multiphoton microscopy imaging platform for efficient integration into clinical setting.
Wednesday 8 April
Intelligent Positioning in High Throughput Photonics Manufacturing Automation
Abstract: In Silicon Photonics and other precision optical fields, production quantities have exponentiated and competition has intensified over the past few years. In multiple test and packaging steps, submicron-scale alignments are necessary and dominate overall production costs. These commence with optically and electronically probing devices while still on the wafer, and the alignments must be repeated through final packaging and all the intermediate steps in between.
The key is leveraging optical physics to separate dependence on position commandability. A universal implementation is now commercially available and fab-proven. Process cost reductions of 99% are seen. We will discuss this technology and its applications, and a live demonstration of parallel array I/O alignment will be offered.
Wednesday 12 February
The Supernova Acceleration Probe (SNAP)
Studying Dark Energy in the Universe
Abstract: The Supernova Acceleration Probe (SNAP) was a proposed experiment designed to quantify dark energy by measuring the redshift-magnitude diagram of supernovae and to quantify the growth of structure in the universe by measuring weak gravitational lensing over cosmological distances. These techniques, along with baryon acoustic oscillation, are used to constrain dark energy density and matter density in modern cosmological models. The baseline SNAP telescope was an ambient temperature, annular-field, configuration II Korsch, three-mirror anastigmat (TMA), designed to fly at the L2 Earth-Sun Lagrange point. The SNAP project evolved into the Joint Dark Energy Mission (JDEM), and finally the Wide-Field Infrared Survey Telescope (WFIRST). Stray light analyses of the SNAP telescope included both overall systems engineering and budgeting, and detailed non-sequential modeling of the effects of dust, roughness and thermal infrared emission, as well as stop placement and baffle design. The goal of the stray light design was to ensure that stray light in the 0.4 to 1.7 micron wavelength range did not exceed a small fraction of Zodiacal radiation within the mission's target field near the North ecliptic pole. At visible wavelengths, the primary source of stray light was starlight scattered by the telescope mirrors. In the longest wavelength bands, thermal emission from the mirrors and structure dominated the budget. Scattered stray light and thermal emissions were mitigated by baffles, an internal field stop, and a cold (140K) internal aperture stop. Stray light scattered by mirror roughness and particulate contamination, as well as scattering from the telescope baffles, were modeled and shown to be less than 10% of Zodiacal levels in all bands.