Company
Portfolio Data
Back to Company SearchNEW INTEGRATION PHOTONICS
Address
5301 DORSET AVECHEVY CHASE, MD, 20815-6629
USA
UEI: V53MN9576TE6
Number of Employees: 2
HUBZone Owned: No
Woman Owned: No
Socially and Economically Disadvantaged: No
SBIR/STTR Involvement
Year of first award: 2020
3
Phase I Awards
1
Phase II Awards
33.33%
Conversion Rate
$423,157
Phase I Dollars
$849,408
Phase II Dollars
$1,272,565
Total Awarded
Awards
Ultra-high resolution integrated arrayed waveguide spectrometer with reusable delay lines for exoplanet detection
Amount: $849,408 Topic: S12
New Integration Photonics, Inc. is proposing to developnbsp;an ultra-high resolving power (R gt; 150,000), high throughput (gt;70%)nbsp;spectrometer leveraging arrayed waveguide gratings (AWGs) on a Si3N4/SiO2 photonic integrated chip (PIC). Our groundbreaking approach introduces a reusable delay line (RDL) as a transformative alternative to the traditional multitude of waveguides. This innovation not only drastically reduces the device#39;s footprint, potentially by a factor of 1000, but also enhances chip stability and reduces the weight, power, and cost (Swap-C) . The spectrometer PIC will feature an inventive integration with a linear InGaAs detector array at the output and will incorporate fiber coupling at the input. This strategic design is meticulously crafted to yield a highly functional device housed within a butterfly package. The result is a substantial reduction in form factor (lt; 20 cmsup3;) when compared to prevailing competitors (~ 200 cmsup3;). This cutting-edge, high-resolution, and high-throughput integrated spectrometer are poised to make significant contributions, not only in applications such as the detection of exoplanets using the Precision Radial Velocity (PRV) method, but also in commercial marketsnbsp;where bulk spectrometer are currently used. The potential impact of this technology is underscored by its innovative design and promising advancements in performance, reliability and cost.
Tagged as:
SBIR
Phase II
2024
NASA
High resolution and high dynamic range integrated spectrometers based on arrayed waveguide gratings with reusable delay lines for fire detection
Amount: $149,576 Topic: T8
We are proposing to develop a photonic integrated circuit for implementing a reusable delay line arrayed waveguide gratings (RDL-AWG) on a Si3N4/SiO2 platform for use as miniature spectrometers with high resolution (resolving power R gt; 10,000) and high dynamic range (gt; 4 orders of magnitude) in the 1.6 to 2.0 um band for fire detection. In Phase I of this proposal, an integrated high spectral resolving power (R gt; 10,000), lownbsp;cross-talk level (lt;nbsp;40 dB) RDL-AWG miniature spectrometer on a Si3N4/SiO2 platform will be designed, optimized, fabricated and characterized. It will be followed by a Phase II proposal for designing a wide operational bandwidth (1.6 to 2.0 um wavelength) RDL-AWG miniature spectrometer, with excellent performance across the desired bandwidth. Integration on a chip reduces the size, weight, power (SWaP) and cost, and increases the stability and reliability of astronomical spectrographs. The future chip size reduction by reusing delay line addresses several issues related to integrated photonic sensors, in particular, better phase control which leads to high resolving power and high dynamic range spectrographs.
Tagged as:
STTR
Phase I
2023
NASA
Ultra-high resolution integrated arrayed waveguide spectrometer with reusable delay lines for exoplanet detection
Amount: $148,913 Topic: S12
New Integration Photonics, Inc., is proposing to develop an ultra-high resolving power (Rgt;150,000) spectrometer based on arrayed waveguide gratings (AWGs) on a Si3N4/SiO2 photonic integrated chip (PIC). The spectrometer implements a reusable delay line (RDL), replacing the large number of waveguides in the traditional AWG, which significantly reduces the size and increases the stability of the chip. This high-resolution integrated spectrometer can be used in the detection of exoplanets based on the Precision Radial Velocity (PRV) method. The proposed photonic chip has three unique advantages to significantly improve the performance of the traditional spectrometer and increases the feasibility of chip fabrication. 1.By reducing the number of waveguides to just one, and coupling the power from single waveguide to achieve the correct power and phase distributions, the new technique eliminates the need for making large AWGs and the associated step of actively compensating the phase error.nbsp;The footprint of the spectrometer can be potentially reduced by a factor of more than 100. 2. A parabolic taper will be implemented instead of a linear taper before the free propagation region (FPR) to reducing the cross-coupling, and thus the phase distribution error. 3.nbsp;The photonic chip will be directly coupled to a 1-D CCD array in Phase II. To achieve this, a three-stigmatic-points compensation approach is proposed for the RDL-AWG design to realize a flat focal-plane at the output of the free propagating region. It also improves the accuracy and the uniformity of the RDL-AWG and compensates for the aberration.
Tagged as:
SBIR
Phase I
2023
NASA
Cascaded Arrayed Waveguide Gratings for High Resolution Integrated Photonic Spectrographs
Amount: $124,668 Topic: S2
We arenbsp;proposing to develop an integrated photonic chip for implementing a cascadednbsp;arrayed waveguide gratings (AWG) spectrometers on a Si3N4/SiO2 platform for use in the detection of exoplanets based on Precision Radial Velocity (PRV) method.nbsp;In Phase I of this proposal, an integrated high spectral resolving power (R~150,000), high throughput (~25%) AWG spectrometer with multiple fiber inputs for simultaneous calibration on a Si3N4/SiO2 platform is proposed, which will be followed by a Phase II proposal for designing a flat focal field AWG spectrometer, with the focal signals of all wavelengths of operation focusing along a straight line, and for designing a polarization insensitive AWG for measuring the optical spectra of the star and the planet.nbsp;Integration on a chip reduces the size, the weight, the cost, and increases the stability of astronomical spectrographs.nbsp;An external calibration sources, like Optical Frequency Combs (OFCs), can be coupled to the AWG spectrometers through the additional fiber inputs to provide the broad spectral coverage and long-term (years) stability needed for extreme PRV detection of exoplanets.
Tagged as:
SBIR
Phase I
2020
NASA