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HTC Vive Flow, EM3 Ether, and Meta's upcoming Project Cambria all share a sleek, thin design and incorporate Pancake lens technology. So, how do Pancake optics differ from the traditional lenses used in current virtual reality headsets, and what does this mean for the future of VR headsets? This shift could signal advancements in the metaverse, virtual worlds, mixed reality, and immersive collaboration tools, such as Microsoft Hololens, Apple Vision, and Microsoft Mesh. With Pancake lenses enhancing optics and form factor, these devices could redefine the user experience in both personal and professional virtual environments.

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FAR INFRARED: In the far-infrared, the stars have all vanished. Instead we now see very cold matter (140 Kelvin or less). Huge, cold clouds of gas and dust in our own galaxy, as well as in nearby galaxies, glow in far-infrared light. In some of these clouds, new stars are just beginning to form. Far-infrared observations can detect these protostars long before they "turn on" visibly by sensing the heat they radiate as they contract." IRAS view of infrared cirrus - dust heated by starlight Michael Hauser (Space Telescope Science Institute), the COBE/DIRBE Science Team, and NASA The center of our galaxy also shines brightly in the far-infrared because of the thick concentration of stars embedded in dense clouds of dust. These stars heat up the dust and cause it to glow brightly in the infrared. The image (at left) of our galaxy taken by the COBE satellite, is a composite of far-infrared wavelengths of 60, 100, and 240 microns. Except for the plane of our own Galaxy, the brightest far-infrared object in the sky is central region of a galaxy called M82. The nucleus of M82 radiates as much energy in the far-infrared as all of the stars in our Galaxy combined. This far-infrared energy comes from dust heated by a source that is hidden from view. The central regions of most galaxies shine very brightly in the far-infrared. Several galaxies have active nuclei hidden in dense regions of dust. Others, called starburst galaxies, have an extremely high number of newly forming stars heating interstellar dust clouds. These galaxies, far outshine all others galaxies in the far-infrared. IRAS infrared view of the Andromeda Galaxy (M31) - notice the bright central region. Discovery of Infrared | What is Infrared? | Infrared Astronomy Overview | Atmospheric Windows | Near, Mid & Far Infrared | The Infrared Universe | Spectroscopy | Timeline | Background | Future Missions | News & Discoveries | Images & Videos | Activities | Infrared Links | Educational Links | Getting into Astronomy HOME INFRARED PROCESSING AND ANALYSIS CENTER INDEX

Augmented reality (AR) is pushing toward affordability and slim designs, largely driven by advancements in waveguide technology. Meanwhile, future virtual reality (VR) headsets will likely evolve around Pancake lens technology.

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In the far-infrared, the stars have all vanished. Instead we now see very cold matter (140 Kelvin or less). Huge, cold clouds of gas and dust in our own galaxy, as well as in nearby galaxies, glow in far-infrared light. In some of these clouds, new stars are just beginning to form. Far-infrared observations can detect these protostars long before they "turn on" visibly by sensing the heat they radiate as they contract."

The Metaverse refers to user-generated online spaces where individuals engage with computer-created environments and digital characters. Virtual reality (VR) fully immerses users in these simulated environments, while augmented reality (AR) integrates digital elements into the physical world.

These Pancake-enabled VR headsets are redefining the perception of VR, shifting from bulky devices to sleek, fashionable wearables. This shift not only makes VR more accessible to the early majority of consumers but also expands the market, driving innovation across the industry. As the industrial metaverse grows, especially with platforms like Microsoft Mesh and devices like Microsoft Hololens, thinner, more powerful headsets will enhance mixed reality experiences for both enterprises and frontline workers worldwide.

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Fresnel lenses, developed by Augustin Fresnel in the early 1800s and known as “the invention that saved a million ships,” work by directing and enhancing light, much like a lighthouse. The lens uses rings of crystalline prisms arranged in a beehive-like structure to reflect and refract light.

When comparing Fresnel lenses to Pancake lenses, several factors come into play: the light source, lens shape, and how the light travels through and exits the lens, as well as the wavelength of the light. Fresnel lenses offer a wider field of view but suffer from chromatic aberrations (ghosting and overlapping colours) and pincushion distortion, which requires real-time software calibration that consumes processing power.

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Though Pancake optics may seem like a new concept, they’ve been used by the military and scientific community long before VR adopted them. The first Pancake VR headset prototype emerged in 2015 from eMargin, followed by Kopin’s "Kopin Elf" in 2017. More recently, companies like Huawei, HTC, Pico, and EM3 have either launched commercial Pancake-enabled headsets or showcased concept designs.

Like augmented reality, virtual reality (VR) is heading toward a slimmer and lighter future. This design evolution is expanding the VR market by attracting casual consumers who may now be more inclined to adopt a VR headset. As a result, the virtual reality market will mature, leading to the growth of ancillary services that further advance the technology.

Connect global teams. Collaborate with remote experts. Streamline processes and unlock cost savings with industry-ready extended reality technology.

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However, Pancake lenses have lower light efficiency due to internal light bouncing, which can dim the perceived image. This is why high-brightness micro displays, like those mentioned by Fan, are essential for optimal performance. Additionally, Pancake lenses still struggle with ghosting.

When consumers and enterprises not deeply engaged in VR/AR news think of virtual reality headsets, they often picture bulky "shoeboxes" strapped to the head. This perception persists despite design efforts to reduce the bulk since VR’s resurgence in 2012. Even technology enthusiasts and industry experts tend to focus on display specs—pixel density, refresh rates, colour accuracy—while overlooking another key component: the lenses.

Warm interstellar dust also starts to shine as we enter the mid-infrared region. The dust around stars which have ejected material shines most brightly in the mid-infrared. Sometimes this dust is so thick that the star hardly shines through at all and can only be detected in the infrared. Protoplanetary disks, the disks of material which surround newly forming stars, also shines brightly in the mid-infrared. These disks are where new planets are possibly being formed. FAR INFRARED: In the far-infrared, the stars have all vanished. Instead we now see very cold matter (140 Kelvin or less). Huge, cold clouds of gas and dust in our own galaxy, as well as in nearby galaxies, glow in far-infrared light. In some of these clouds, new stars are just beginning to form. Far-infrared observations can detect these protostars long before they "turn on" visibly by sensing the heat they radiate as they contract." IRAS view of infrared cirrus - dust heated by starlight Michael Hauser (Space Telescope Science Institute), the COBE/DIRBE Science Team, and NASA The center of our galaxy also shines brightly in the far-infrared because of the thick concentration of stars embedded in dense clouds of dust. These stars heat up the dust and cause it to glow brightly in the infrared. The image (at left) of our galaxy taken by the COBE satellite, is a composite of far-infrared wavelengths of 60, 100, and 240 microns. Except for the plane of our own Galaxy, the brightest far-infrared object in the sky is central region of a galaxy called M82. The nucleus of M82 radiates as much energy in the far-infrared as all of the stars in our Galaxy combined. This far-infrared energy comes from dust heated by a source that is hidden from view. The central regions of most galaxies shine very brightly in the far-infrared. Several galaxies have active nuclei hidden in dense regions of dust. Others, called starburst galaxies, have an extremely high number of newly forming stars heating interstellar dust clouds. These galaxies, far outshine all others galaxies in the far-infrared. IRAS infrared view of the Andromeda Galaxy (M31) - notice the bright central region. Discovery of Infrared | What is Infrared? | Infrared Astronomy Overview | Atmospheric Windows | Near, Mid & Far Infrared | The Infrared Universe | Spectroscopy | Timeline | Background | Future Missions | News & Discoveries | Images & Videos | Activities | Infrared Links | Educational Links | Getting into Astronomy HOME INFRARED PROCESSING AND ANALYSIS CENTER INDEX

NEAR INFRARED: Between about 0.7 to 1.1 microns we can use the same observing methods as are use for visible light observations, except for observation by eye. The infrared light that we observe in this region is not thermal (not due to heat radiation). Many do not even consider this range as part of infrared astronomy. Beyond about 1.1 microns, infrared emission is primarily heat or thermal radiation. As we move away from visible light towards longer wavelengths of light, we enter the infrared region. As we enter the near-infrared region, the hot blue stars seen clearly in visible light fade out and cooler stars come into view. Large red giant stars and low mass red dwarfs dominate in the near-infrared. The near-infrared is also the region where interstellar dust is the most transparent to infrared light.

Infrared radiation is emitted by any object that has a temperature (ie radiates heat). So, basically all celestial objects emit some infrared. The wavelength at which an object radiates most intensely depends on its temperature. In general, as the temperature of an object cools, it shows up more prominently at farther infrared wavelengths. This means that some infrared wavelengths are better suited for studying certain objects than others.

Infrared is usually divided into 3 spectral regions: near, mid and far-infrared. The boundaries between the near, mid and far-infrared regions are not agreed upon and can vary. The main factor that determines which wavelengths are included in each of these three infrared regions is the type of detector technology used for gathering infrared light. Near-infrared observations have been made from ground based observatories since the 1960's. They are done in much the same way as visible light observations for wavelengths less than 1 micron, but require special infrared detectors beyond 1 micron. Mid and far-infrared observations can only be made by observatories which can get above our atmosphere. These observations require the use of special cooled detectors containing crystals like germanium whose electrical resistance is very sensitive to heat. Infrared radiation is emitted by any object that has a temperature (ie radiates heat). So, basically all celestial objects emit some infrared. The wavelength at which an object radiates most intensely depends on its temperature. In general, as the temperature of an object cools, it shows up more prominently at farther infrared wavelengths. This means that some infrared wavelengths are better suited for studying certain objects than others. Visible (courtesy of Howard McCallon), near-infrared (2MASS), and mid-infrared (ISO) view of the Horsehead Nebula. Image assembled by Robert Hurt. As we move from the near-infrared into mid and far-infrared regions of the spectrum, some celestial objects will appear while others will disappear from view. For example, in the above image you can see how more stars (generally cooler stars) appear as we go from the visible light image to the near-infrared image. In the near-infrared, the dust also becomes transparent, allowing us to see regions hidden by dust in the visible image. As we go to the mid-infrared image, the cooler dust itself glows. The table below highlights what we see in the different infrared spectral regions. SPECTRAL REGION WAVELENGTH RANGE (microns) TEMPERATURE RANGE (degrees Kelvin) WHAT WE SEE Near-Infrared (0.7-1) to 5 740 to (3,000-5,200) Cooler red stars Red giants Dust is transparent Mid-Infrared 5 to (25-40) (92.5-140) to 740 Planets, comets and asteroidsDust warmed by starlight Protoplanetary disks Far-Infrared (25-40) to (200-350) (10.6-18.5) to (92.5-140) Emission from cold dust Central regions of galaxies Very cold molecular clouds NEAR INFRARED: Between about 0.7 to 1.1 microns we can use the same observing methods as are use for visible light observations, except for observation by eye. The infrared light that we observe in this region is not thermal (not due to heat radiation). Many do not even consider this range as part of infrared astronomy. Beyond about 1.1 microns, infrared emission is primarily heat or thermal radiation. As we move away from visible light towards longer wavelengths of light, we enter the infrared region. As we enter the near-infrared region, the hot blue stars seen clearly in visible light fade out and cooler stars come into view. Large red giant stars and low mass red dwarfs dominate in the near-infrared. The near-infrared is also the region where interstellar dust is the most transparent to infrared light. Visible (left) and Near-Infrared View of the Galactic Center Visible image courtesy of Howard McCallon. The infrared image is from the 2 Micron All Sky Survey (2MASS) Notice in the above images how center of our galaxy, which is hidden by thick dust in visible light (left), becomes transparent in the near-infrared (right). Many of the hotter stars in the visible image have faded in the near-infrared image. The near-infrared image shows cooler, reddish stars which do not appear in the visible light view. These stars are primarily red dwarfs and red giants. Red giants are large reddish or orange stars which are running out of their nuclear fuel. They can swell up to 100 times their original size and have temperatures which range from 2000 to 3500 K. Red giants radiate most intensely in the near-infrared region. Red dwarfs are the most common of all stars. They are much smaller than our Sun and are the coolest of the stars having a temperature of about 3000 K which means that these stars radiate most strongly in the near-infrared. Many of these stars are too faint in visible light to even be detected by optical telescopes, and have been discovered for the first time in the near-infrared. MID INFRARED: As we enter the mid-infrared region of the spectrum, the cool stars begin to fade out and cooler objects such as planets, comets and asteroids come into view. Planets absorb light from the sun and heat up. They then re-radiate this heat as infrared light. This is different from the visible light that we see from the planets which is reflected sunlight. The planets in our solar system have temperatures ranging from about 53 to 573 degrees Kelvin. Objects in this temperature range emit most of their light in the mid-infrared. For example, the Earth itself radiates most strongly at about 10 microns. Asteroids also emit most of their light in the mid-infrared making this wavelength band the most efficient for locating dark asteroids. Infrared data can help to determine the surface composition, and diameter of asteroids. An infrared view of the Earth IRAS mid-infrared view of Comet IRAS-Araki-Alcock Dust warmed by starlight is also very prominent in the mid-infrared. An example is the zodiacal dust which lies in the plane of our solar system. This dust is made up of silicates (like the rocks on Earth) and range in size from a tenth of a micron up to the size of large rocks. Silicates emit most of their radiation at about 10 microns. Mapping the distribution of this dust can provide clues about the formation of our own solar system. The dust from comets also has strong emission in the mid-infrared. Warm interstellar dust also starts to shine as we enter the mid-infrared region. The dust around stars which have ejected material shines most brightly in the mid-infrared. Sometimes this dust is so thick that the star hardly shines through at all and can only be detected in the infrared. Protoplanetary disks, the disks of material which surround newly forming stars, also shines brightly in the mid-infrared. These disks are where new planets are possibly being formed. FAR INFRARED: In the far-infrared, the stars have all vanished. Instead we now see very cold matter (140 Kelvin or less). Huge, cold clouds of gas and dust in our own galaxy, as well as in nearby galaxies, glow in far-infrared light. In some of these clouds, new stars are just beginning to form. Far-infrared observations can detect these protostars long before they "turn on" visibly by sensing the heat they radiate as they contract." IRAS view of infrared cirrus - dust heated by starlight Michael Hauser (Space Telescope Science Institute), the COBE/DIRBE Science Team, and NASA The center of our galaxy also shines brightly in the far-infrared because of the thick concentration of stars embedded in dense clouds of dust. These stars heat up the dust and cause it to glow brightly in the infrared. The image (at left) of our galaxy taken by the COBE satellite, is a composite of far-infrared wavelengths of 60, 100, and 240 microns. Except for the plane of our own Galaxy, the brightest far-infrared object in the sky is central region of a galaxy called M82. The nucleus of M82 radiates as much energy in the far-infrared as all of the stars in our Galaxy combined. This far-infrared energy comes from dust heated by a source that is hidden from view. The central regions of most galaxies shine very brightly in the far-infrared. Several galaxies have active nuclei hidden in dense regions of dust. Others, called starburst galaxies, have an extremely high number of newly forming stars heating interstellar dust clouds. These galaxies, far outshine all others galaxies in the far-infrared. IRAS infrared view of the Andromeda Galaxy (M31) - notice the bright central region. Discovery of Infrared | What is Infrared? | Infrared Astronomy Overview | Atmospheric Windows | Near, Mid & Far Infrared | The Infrared Universe | Spectroscopy | Timeline | Background | Future Missions | News & Discoveries | Images & Videos | Activities | Infrared Links | Educational Links | Getting into Astronomy HOME INFRARED PROCESSING AND ANALYSIS CENTER INDEX

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By integrating with Windows and other digital tools, HoloLens plays a crucial role in driving digital transformations across industries, reshaping how businesses engage with the metaverse and mixed-reality solutions.

Between about 0.7 to 1.1 microns we can use the same observing methods as are use for visible light observations, except for observation by eye. The infrared light that we observe in this region is not thermal (not due to heat radiation). Many do not even consider this range as part of infrared astronomy. Beyond about 1.1 microns, infrared emission is primarily heat or thermal radiation. As we move away from visible light towards longer wavelengths of light, we enter the infrared region. As we enter the near-infrared region, the hot blue stars seen clearly in visible light fade out and cooler stars come into view. Large red giant stars and low mass red dwarfs dominate in the near-infrared. The near-infrared is also the region where interstellar dust is the most transparent to infrared light.

In technology, there’s a clear trend: devices become more affordable and compact over time. This holds true for smartphones, laptops, chips, and now, VR and AR headsets.

Notice in the above images how center of our galaxy, which is hidden by thick dust in visible light (left), becomes transparent in the near-infrared (right). Many of the hotter stars in the visible image have faded in the near-infrared image. The near-infrared image shows cooler, reddish stars which do not appear in the visible light view. These stars are primarily red dwarfs and red giants. Red giants are large reddish or orange stars which are running out of their nuclear fuel. They can swell up to 100 times their original size and have temperatures which range from 2000 to 3500 K. Red giants radiate most intensely in the near-infrared region. Red dwarfs are the most common of all stars. They are much smaller than our Sun and are the coolest of the stars having a temperature of about 3000 K which means that these stars radiate most strongly in the near-infrared. Many of these stars are too faint in visible light to even be detected by optical telescopes, and have been discovered for the first time in the near-infrared. MID INFRARED: As we enter the mid-infrared region of the spectrum, the cool stars begin to fade out and cooler objects such as planets, comets and asteroids come into view. Planets absorb light from the sun and heat up. They then re-radiate this heat as infrared light. This is different from the visible light that we see from the planets which is reflected sunlight. The planets in our solar system have temperatures ranging from about 53 to 573 degrees Kelvin. Objects in this temperature range emit most of their light in the mid-infrared. For example, the Earth itself radiates most strongly at about 10 microns. Asteroids also emit most of their light in the mid-infrared making this wavelength band the most efficient for locating dark asteroids. Infrared data can help to determine the surface composition, and diameter of asteroids. An infrared view of the Earth IRAS mid-infrared view of Comet IRAS-Araki-Alcock Dust warmed by starlight is also very prominent in the mid-infrared. An example is the zodiacal dust which lies in the plane of our solar system. This dust is made up of silicates (like the rocks on Earth) and range in size from a tenth of a micron up to the size of large rocks. Silicates emit most of their radiation at about 10 microns. Mapping the distribution of this dust can provide clues about the formation of our own solar system. The dust from comets also has strong emission in the mid-infrared. Warm interstellar dust also starts to shine as we enter the mid-infrared region. The dust around stars which have ejected material shines most brightly in the mid-infrared. Sometimes this dust is so thick that the star hardly shines through at all and can only be detected in the infrared. Protoplanetary disks, the disks of material which surround newly forming stars, also shines brightly in the mid-infrared. These disks are where new planets are possibly being formed. FAR INFRARED: In the far-infrared, the stars have all vanished. Instead we now see very cold matter (140 Kelvin or less). Huge, cold clouds of gas and dust in our own galaxy, as well as in nearby galaxies, glow in far-infrared light. In some of these clouds, new stars are just beginning to form. Far-infrared observations can detect these protostars long before they "turn on" visibly by sensing the heat they radiate as they contract." IRAS view of infrared cirrus - dust heated by starlight Michael Hauser (Space Telescope Science Institute), the COBE/DIRBE Science Team, and NASA The center of our galaxy also shines brightly in the far-infrared because of the thick concentration of stars embedded in dense clouds of dust. These stars heat up the dust and cause it to glow brightly in the infrared. The image (at left) of our galaxy taken by the COBE satellite, is a composite of far-infrared wavelengths of 60, 100, and 240 microns. Except for the plane of our own Galaxy, the brightest far-infrared object in the sky is central region of a galaxy called M82. The nucleus of M82 radiates as much energy in the far-infrared as all of the stars in our Galaxy combined. This far-infrared energy comes from dust heated by a source that is hidden from view. The central regions of most galaxies shine very brightly in the far-infrared. Several galaxies have active nuclei hidden in dense regions of dust. Others, called starburst galaxies, have an extremely high number of newly forming stars heating interstellar dust clouds. These galaxies, far outshine all others galaxies in the far-infrared. IRAS infrared view of the Andromeda Galaxy (M31) - notice the bright central region. Discovery of Infrared | What is Infrared? | Infrared Astronomy Overview | Atmospheric Windows | Near, Mid & Far Infrared | The Infrared Universe | Spectroscopy | Timeline | Background | Future Missions | News & Discoveries | Images & Videos | Activities | Infrared Links | Educational Links | Getting into Astronomy HOME INFRARED PROCESSING AND ANALYSIS CENTER INDEX

As we move from the near-infrared into mid and far-infrared regions of the spectrum, some celestial objects will appear while others will disappear from view. For example, in the above image you can see how more stars (generally cooler stars) appear as we go from the visible light image to the near-infrared image. In the near-infrared, the dust also becomes transparent, allowing us to see regions hidden by dust in the visible image. As we go to the mid-infrared image, the cooler dust itself glows. The table below highlights what we see in the different infrared spectral regions. SPECTRAL REGION WAVELENGTH RANGE (microns) TEMPERATURE RANGE (degrees Kelvin) WHAT WE SEE Near-Infrared (0.7-1) to 5 740 to (3,000-5,200) Cooler red stars Red giants Dust is transparent Mid-Infrared 5 to (25-40) (92.5-140) to 740 Planets, comets and asteroidsDust warmed by starlight Protoplanetary disks Far-Infrared (25-40) to (200-350) (10.6-18.5) to (92.5-140) Emission from cold dust Central regions of galaxies Very cold molecular clouds NEAR INFRARED: Between about 0.7 to 1.1 microns we can use the same observing methods as are use for visible light observations, except for observation by eye. The infrared light that we observe in this region is not thermal (not due to heat radiation). Many do not even consider this range as part of infrared astronomy. Beyond about 1.1 microns, infrared emission is primarily heat or thermal radiation. As we move away from visible light towards longer wavelengths of light, we enter the infrared region. As we enter the near-infrared region, the hot blue stars seen clearly in visible light fade out and cooler stars come into view. Large red giant stars and low mass red dwarfs dominate in the near-infrared. The near-infrared is also the region where interstellar dust is the most transparent to infrared light.

Pancake lensVR

In mid-June 2021, Kopin unveiled the P95, an all-plastic Pancake lens design optimised for their 2.6K x 2.6K OLED high-brightness micro displays. Dr. John C.C. Fan, CEO and founder of Kopin Corporation, highlighted that this new technology is "ideal for VR" and marks "a foundational milestone for the emerging VR markets." According to Fan, bulky, heavy headsets have long hindered consumer adoption, and this breakthrough aims to change that.

In virtual reality HMDs, this design creates a "lighthouse-beamed screen" effect, requiring a significant gap between the display and lens, thus adding bulk and weight to the headset. As industries embrace the metaverse, mixed reality, and spatial computing—seen in platforms like Microsoft Mesh and devices like Microsoft Hololens—streamlining this bulky design is crucial for the future of immersive experiences in the industrial metaverse and beyond.

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Red giants are large reddish or orange stars which are running out of their nuclear fuel. They can swell up to 100 times their original size and have temperatures which range from 2000 to 3500 K. Red giants radiate most intensely in the near-infrared region. Red dwarfs are the most common of all stars. They are much smaller than our Sun and are the coolest of the stars having a temperature of about 3000 K which means that these stars radiate most strongly in the near-infrared. Many of these stars are too faint in visible light to even be detected by optical telescopes, and have been discovered for the first time in the near-infrared. MID INFRARED: As we enter the mid-infrared region of the spectrum, the cool stars begin to fade out and cooler objects such as planets, comets and asteroids come into view. Planets absorb light from the sun and heat up. They then re-radiate this heat as infrared light. This is different from the visible light that we see from the planets which is reflected sunlight. The planets in our solar system have temperatures ranging from about 53 to 573 degrees Kelvin. Objects in this temperature range emit most of their light in the mid-infrared. For example, the Earth itself radiates most strongly at about 10 microns. Asteroids also emit most of their light in the mid-infrared making this wavelength band the most efficient for locating dark asteroids. Infrared data can help to determine the surface composition, and diameter of asteroids. An infrared view of the Earth IRAS mid-infrared view of Comet IRAS-Araki-Alcock Dust warmed by starlight is also very prominent in the mid-infrared. An example is the zodiacal dust which lies in the plane of our solar system. This dust is made up of silicates (like the rocks on Earth) and range in size from a tenth of a micron up to the size of large rocks. Silicates emit most of their radiation at about 10 microns. Mapping the distribution of this dust can provide clues about the formation of our own solar system. The dust from comets also has strong emission in the mid-infrared. Warm interstellar dust also starts to shine as we enter the mid-infrared region. The dust around stars which have ejected material shines most brightly in the mid-infrared. Sometimes this dust is so thick that the star hardly shines through at all and can only be detected in the infrared. Protoplanetary disks, the disks of material which surround newly forming stars, also shines brightly in the mid-infrared. These disks are where new planets are possibly being formed. FAR INFRARED: In the far-infrared, the stars have all vanished. Instead we now see very cold matter (140 Kelvin or less). Huge, cold clouds of gas and dust in our own galaxy, as well as in nearby galaxies, glow in far-infrared light. In some of these clouds, new stars are just beginning to form. Far-infrared observations can detect these protostars long before they "turn on" visibly by sensing the heat they radiate as they contract." IRAS view of infrared cirrus - dust heated by starlight Michael Hauser (Space Telescope Science Institute), the COBE/DIRBE Science Team, and NASA The center of our galaxy also shines brightly in the far-infrared because of the thick concentration of stars embedded in dense clouds of dust. These stars heat up the dust and cause it to glow brightly in the infrared. The image (at left) of our galaxy taken by the COBE satellite, is a composite of far-infrared wavelengths of 60, 100, and 240 microns. Except for the plane of our own Galaxy, the brightest far-infrared object in the sky is central region of a galaxy called M82. The nucleus of M82 radiates as much energy in the far-infrared as all of the stars in our Galaxy combined. This far-infrared energy comes from dust heated by a source that is hidden from view. The central regions of most galaxies shine very brightly in the far-infrared. Several galaxies have active nuclei hidden in dense regions of dust. Others, called starburst galaxies, have an extremely high number of newly forming stars heating interstellar dust clouds. These galaxies, far outshine all others galaxies in the far-infrared. IRAS infrared view of the Andromeda Galaxy (M31) - notice the bright central region. Discovery of Infrared | What is Infrared? | Infrared Astronomy Overview | Atmospheric Windows | Near, Mid & Far Infrared | The Infrared Universe | Spectroscopy | Timeline | Background | Future Missions | News & Discoveries | Images & Videos | Activities | Infrared Links | Educational Links | Getting into Astronomy HOME INFRARED PROCESSING AND ANALYSIS CENTER INDEX

A key indicator of this trend was the release of the HTC Vive Flow, which emphasised stylish design and targeted a broader customer base, even incorporating non-tech elements like meditation. The driving force behind this shift is the Pancake lens design. While not a new concept, it is revolutionary for VR headsets, enabling sleeker designs that appeal to a wider audience while eventually detaching from the need for external devices like laptops or smartphones.

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Near-infrared observations have been made from ground based observatories since the 1960's. They are done in much the same way as visible light observations for wavelengths less than 1 micron, but require special infrared detectors beyond 1 micron. Mid and far-infrared observations can only be made by observatories which can get above our atmosphere. These observations require the use of special cooled detectors containing crystals like germanium whose electrical resistance is very sensitive to heat. Infrared radiation is emitted by any object that has a temperature (ie radiates heat). So, basically all celestial objects emit some infrared. The wavelength at which an object radiates most intensely depends on its temperature. In general, as the temperature of an object cools, it shows up more prominently at farther infrared wavelengths. This means that some infrared wavelengths are better suited for studying certain objects than others.

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Pancake optics, however, fold multiple lenses together, bouncing light within the glass or plastic. This allows for a slimmer design, reducing the space between the display and the user's eyes and eliminating distortion issues present with Fresnel lenses. Pancake lenses also do not exhibit chromatic aberration, freeing up processing power for other tasks.

SPECTRAL REGION WAVELENGTH RANGE (microns) TEMPERATURE RANGE (degrees Kelvin) WHAT WE SEE Near-Infrared (0.7-1) to 5 740 to (3,000-5,200) Cooler red stars Red giants Dust is transparent Mid-Infrared 5 to (25-40) (92.5-140) to 740 Planets, comets and asteroidsDust warmed by starlight Protoplanetary disks Far-Infrared (25-40) to (200-350) (10.6-18.5) to (92.5-140) Emission from cold dust Central regions of galaxies Very cold molecular clouds NEAR INFRARED: Between about 0.7 to 1.1 microns we can use the same observing methods as are use for visible light observations, except for observation by eye. The infrared light that we observe in this region is not thermal (not due to heat radiation). Many do not even consider this range as part of infrared astronomy. Beyond about 1.1 microns, infrared emission is primarily heat or thermal radiation. As we move away from visible light towards longer wavelengths of light, we enter the infrared region. As we enter the near-infrared region, the hot blue stars seen clearly in visible light fade out and cooler stars come into view. Large red giant stars and low mass red dwarfs dominate in the near-infrared. The near-infrared is also the region where interstellar dust is the most transparent to infrared light.

Microsoft's HoloLens is a mixed-reality device regarded as a key gateway to the metaverse. HoloLens allows users to create and interact with 3D objects and spaces as holograms. The HoloLens 2, in particular, is recognised as industrial metaverse technology, enabling real-time collaboration and immersive experiences for customers.

MID INFRARED: As we enter the mid-infrared region of the spectrum, the cool stars begin to fade out and cooler objects such as planets, comets and asteroids come into view. Planets absorb light from the sun and heat up. They then re-radiate this heat as infrared light. This is different from the visible light that we see from the planets which is reflected sunlight. The planets in our solar system have temperatures ranging from about 53 to 573 degrees Kelvin. Objects in this temperature range emit most of their light in the mid-infrared. For example, the Earth itself radiates most strongly at about 10 microns. Asteroids also emit most of their light in the mid-infrared making this wavelength band the most efficient for locating dark asteroids. Infrared data can help to determine the surface composition, and diameter of asteroids. An infrared view of the Earth IRAS mid-infrared view of Comet IRAS-Araki-Alcock Dust warmed by starlight is also very prominent in the mid-infrared. An example is the zodiacal dust which lies in the plane of our solar system. This dust is made up of silicates (like the rocks on Earth) and range in size from a tenth of a micron up to the size of large rocks. Silicates emit most of their radiation at about 10 microns. Mapping the distribution of this dust can provide clues about the formation of our own solar system. The dust from comets also has strong emission in the mid-infrared. Warm interstellar dust also starts to shine as we enter the mid-infrared region. The dust around stars which have ejected material shines most brightly in the mid-infrared. Sometimes this dust is so thick that the star hardly shines through at all and can only be detected in the infrared. Protoplanetary disks, the disks of material which surround newly forming stars, also shines brightly in the mid-infrared. These disks are where new planets are possibly being formed. FAR INFRARED: In the far-infrared, the stars have all vanished. Instead we now see very cold matter (140 Kelvin or less). Huge, cold clouds of gas and dust in our own galaxy, as well as in nearby galaxies, glow in far-infrared light. In some of these clouds, new stars are just beginning to form. Far-infrared observations can detect these protostars long before they "turn on" visibly by sensing the heat they radiate as they contract." IRAS view of infrared cirrus - dust heated by starlight Michael Hauser (Space Telescope Science Institute), the COBE/DIRBE Science Team, and NASA The center of our galaxy also shines brightly in the far-infrared because of the thick concentration of stars embedded in dense clouds of dust. These stars heat up the dust and cause it to glow brightly in the infrared. The image (at left) of our galaxy taken by the COBE satellite, is a composite of far-infrared wavelengths of 60, 100, and 240 microns. Except for the plane of our own Galaxy, the brightest far-infrared object in the sky is central region of a galaxy called M82. The nucleus of M82 radiates as much energy in the far-infrared as all of the stars in our Galaxy combined. This far-infrared energy comes from dust heated by a source that is hidden from view. The central regions of most galaxies shine very brightly in the far-infrared. Several galaxies have active nuclei hidden in dense regions of dust. Others, called starburst galaxies, have an extremely high number of newly forming stars heating interstellar dust clouds. These galaxies, far outshine all others galaxies in the far-infrared. IRAS infrared view of the Andromeda Galaxy (M31) - notice the bright central region. Discovery of Infrared | What is Infrared? | Infrared Astronomy Overview | Atmospheric Windows | Near, Mid & Far Infrared | The Infrared Universe | Spectroscopy | Timeline | Background | Future Missions | News & Discoveries | Images & Videos | Activities | Infrared Links | Educational Links | Getting into Astronomy HOME INFRARED PROCESSING AND ANALYSIS CENTER INDEX

As we move away from visible light towards longer wavelengths of light, we enter the infrared region. As we enter the near-infrared region, the hot blue stars seen clearly in visible light fade out and cooler stars come into view. Large red giant stars and low mass red dwarfs dominate in the near-infrared. The near-infrared is also the region where interstellar dust is the most transparent to infrared light.

The determination of the focal length distance depends on how strongly the lens converges the light to focus the subject being imaged. This, in turn, affects ...

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Red dwarfs are the most common of all stars. They are much smaller than our Sun and are the coolest of the stars having a temperature of about 3000 K which means that these stars radiate most strongly in the near-infrared. Many of these stars are too faint in visible light to even be detected by optical telescopes, and have been discovered for the first time in the near-infrared. MID INFRARED: As we enter the mid-infrared region of the spectrum, the cool stars begin to fade out and cooler objects such as planets, comets and asteroids come into view. Planets absorb light from the sun and heat up. They then re-radiate this heat as infrared light. This is different from the visible light that we see from the planets which is reflected sunlight. The planets in our solar system have temperatures ranging from about 53 to 573 degrees Kelvin. Objects in this temperature range emit most of their light in the mid-infrared. For example, the Earth itself radiates most strongly at about 10 microns. Asteroids also emit most of their light in the mid-infrared making this wavelength band the most efficient for locating dark asteroids. Infrared data can help to determine the surface composition, and diameter of asteroids. An infrared view of the Earth IRAS mid-infrared view of Comet IRAS-Araki-Alcock Dust warmed by starlight is also very prominent in the mid-infrared. An example is the zodiacal dust which lies in the plane of our solar system. This dust is made up of silicates (like the rocks on Earth) and range in size from a tenth of a micron up to the size of large rocks. Silicates emit most of their radiation at about 10 microns. Mapping the distribution of this dust can provide clues about the formation of our own solar system. The dust from comets also has strong emission in the mid-infrared. Warm interstellar dust also starts to shine as we enter the mid-infrared region. The dust around stars which have ejected material shines most brightly in the mid-infrared. Sometimes this dust is so thick that the star hardly shines through at all and can only be detected in the infrared. Protoplanetary disks, the disks of material which surround newly forming stars, also shines brightly in the mid-infrared. These disks are where new planets are possibly being formed. FAR INFRARED: In the far-infrared, the stars have all vanished. Instead we now see very cold matter (140 Kelvin or less). Huge, cold clouds of gas and dust in our own galaxy, as well as in nearby galaxies, glow in far-infrared light. In some of these clouds, new stars are just beginning to form. Far-infrared observations can detect these protostars long before they "turn on" visibly by sensing the heat they radiate as they contract." IRAS view of infrared cirrus - dust heated by starlight Michael Hauser (Space Telescope Science Institute), the COBE/DIRBE Science Team, and NASA The center of our galaxy also shines brightly in the far-infrared because of the thick concentration of stars embedded in dense clouds of dust. These stars heat up the dust and cause it to glow brightly in the infrared. The image (at left) of our galaxy taken by the COBE satellite, is a composite of far-infrared wavelengths of 60, 100, and 240 microns. Except for the plane of our own Galaxy, the brightest far-infrared object in the sky is central region of a galaxy called M82. The nucleus of M82 radiates as much energy in the far-infrared as all of the stars in our Galaxy combined. This far-infrared energy comes from dust heated by a source that is hidden from view. The central regions of most galaxies shine very brightly in the far-infrared. Several galaxies have active nuclei hidden in dense regions of dust. Others, called starburst galaxies, have an extremely high number of newly forming stars heating interstellar dust clouds. These galaxies, far outshine all others galaxies in the far-infrared. IRAS infrared view of the Andromeda Galaxy (M31) - notice the bright central region. Discovery of Infrared | What is Infrared? | Infrared Astronomy Overview | Atmospheric Windows | Near, Mid & Far Infrared | The Infrared Universe | Spectroscopy | Timeline | Background | Future Missions | News & Discoveries | Images & Videos | Activities | Infrared Links | Educational Links | Getting into Astronomy HOME INFRARED PROCESSING AND ANALYSIS CENTER INDEX

From 2024 and beyond, virtual reality is poised to mature both in hardware and use cases, particularly within the metaverse and industrial metaverse. This often-overlooked Pancake optics design will be the catalyst for these advancements, enhancing mixed reality experiences for employees and enabling the development of industrial metaverse solutions through platforms like Microsoft Hololens and the wider metaverse world.

4 — MAGNIFYING definition: 1. present participle of magnify 2. to make something look larger than it is, especially by looking…. Learn more.

Overall, Pancake lenses offer more advantages over Fresnel lenses, especially in terms of image quality and enabling thinner, lighter VR headsets. This innovation is critical as the VR market expands into the industrial metaverse, mixed reality, and collaborative platforms like Microsoft Mesh and Microsoft Teams. These advancements are poised to transform VR/AR solutions for the enterprise, frontline workers, and the broader metaverse world.

In the context of the metaverse, platforms like Microsoft Hololens are shaping the future of mixed reality, allowing employees and colleagues to interact seamlessly with digital and real-world elements. These mixed reality offerings are transforming how we collaborate and engage in virtual worlds.