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In order to protect your home and maintain its beauty and value, it is essential for you as a homeowner to take proactive measures against UV radiation – a process which starts with your home's windows.

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.

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

Low-E coatings are microscopically thin, virtually invisible layers that are applied to the glass surface of windows. These coatings work by reflecting a large portion of the UV rays, helping to protect your home's interior from fading and damage.

In addition to Low-E coatings, there are many other types of modern window technologies that can enhance the UV protection of your home. For example, some windows are designed with multiple layers of glass, filled with insulating gases, and equipped with spectrally selective coatings. These technologies not only reduce the UV radiation entering your home, but also enhance your home's energy efficiency, making them a valuable investment for any homeowner.

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In addition to selecting the right windows and doors, consider other UV protection strategies for your home. Utilize window treatments like blinds, shades, or curtains with UV-blocking properties, as these can further reduce the amount of UV radiation that enters your home and protect your furnishings from fading.

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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.

Additionally, you can use window treatments such as blinds, shades, or curtains with UV-blocking properties to further reduce the amount of UV radiation that enters your home.

UV rays can cause significant damage to your property, leading to fading of furniture, carpets, and the visible structural elements of your home. They can also pose potential health risks for you and your family as well.

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

One of the most effective ways to minimize the impact of UV rays on your home is by installing the right windows. Modern window technologies, such as Low-E (low emissivity) coatings, can significantly reduce the amount of UV radiation that enters your home while still allowing natural light to brighten your living space.

OBJECTIVE LENS meaning: a lens or system of lenses in a microscope, telescope, etc., that forms an image of an object.

There are many strategies you can rely on to block UV rays on your home windows, and one of the most effective of these methods is to install windows with Low-E coatings, as these coatings reflect a significant portion of UV radiation while still allowing natural light into your home.

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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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Older windows are often less effective at blocking UV rays, and can allow a significant amount of radiation to enter your home. By replacing them with modern, energy-efficient windows, you can enhance both the UV protection and energy efficiency of your home.

At Canadian Choice Windows and Doors, our team is here for you to help you find the perfect windows for your home. Reach out to us today to schedule a consultation with ease!

Certain materials are more effective at blocking UV rays than others, and when it comes to windows, glass with Low-E coatings is highly effective at minimizing the amount of UV radiation that enters your home.

When we think of protecting ourselves from harmful UV rays, we often focus on sunscreen, hats, and sunglasses. However, many homeowners overlook the importance of safeguarding their homes from the damaging effects of ultraviolet radiation, which can lead to the need for costly and avoidable renovations down the line.

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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.

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.

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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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

When choosing replacement windows and doors, look for products that are specifically designed to provide superior UV protection. Make sure to also consult with a reputable window and door replacement company to explore your options, as they can guide you through the selection process and help you choose the best windows and doors that suit your needs, budget, and style preferences.

It's definitely possible for you to add UV protection to your windows, especially if you have existing windows that do not have UV-blocking properties.

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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3MUVWindow Film

At the end of the day, for the most effective and long-lasting UV protection for your home, it's always recommended to consult with professionals from a reputable window and door replacement company who can provide you with expert guidance and offer solutions tailored to your specific needs, ensuring optimal UV protection and energy efficiency for your home. By implementing the right strategies and investing in UV-protective materials, you can effectively shield your home from the damaging effects of UV rays

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 founder and President at Canadian Choice Windows and Doors, I've turned my passion for home improvement into a national brand. From our humble beginnings as a single store, we've expanded to six locations across Canada, specializing in windows, doors, and energy-efficient home solutions.

ClearUVBlocking Window Film

The right windows can minimize UV impact in your home, which is why replacing older windows to maximize UV protection is paramount. UV rays can cause the fading of furniture, carpets, and artwork, as well as pose potential health risks to you and your family. By taking proactive measures to protect your home from UV rays, you can maintain its beauty, prolong its lifespan, and create a safe and comfortable living environment

If your home currently has older windows and doors, it may be time to consider replacing them to maximize your UV protection.

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.

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Our homes are not only a sanctuary for us and our families, but also a valuable investment that requires proper care and maintenance, and while we often focus on protecting ourselves from the harmful effects of UV rays, it's equally important to shield our homes from the damaging impact of ultraviolet radiation.

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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."

Other materials that can block UV rays include acrylic, polycarbonate, and specialized films designed for UV protection.

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The right windows, equipped with technologies like Low-E coatings, can significantly minimize the impact of UV radiation on your home's interior, and replacing older windows and doors with modern, UV-protective ones can further enhance your home's level of protection. By taking these proactive steps and consulting with a reputable window and door replacement company like Canadian Choice Windows and Doors, you can safeguard your home, enjoy more natural light, and ensure a comfortable living environment for years to come.

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.

Consider applying UV-blocking films or tints to the glass surface of your windows - these films can be professionally installed, and will provide an additional layer of UV protection. However, it's important to ensure that these films are specifically designed for your windows, and that they won't interfere with the functionality or appearance of the windows in your home. When in doubt, it's always a good idea to consult with window professionals to explore the best options for adding UV protection to your windows.