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This infrared image from NASA's Spitzer Space Telescope shows the Helix nebula, a cosmic starlet often photographed by amateur astronomers for its vivid colors and eerie resemblance to a giant eye.
The nebula, located about 700 light-years away in the constellation Aquarius, belongs to a class of objects called planetary nebulae. Discovered in the 18th century, these cosmic butterflies were named for their resemblance to gas-giant planets.
Planetary nebulae are actually the remains of stars that once looked a lot like our sun.
When sun-like stars die, they puff out their outer gaseous layers. These layers are heated by the hot core of the dead star, called a white dwarf, and shine with infrared and visible-light colors. Our own sun will blossom into a planetary nebula when it dies in about five billion years.
In Spitzer's infrared view of the Helix nebula, the eye looks more like that of a green monster's. Infrared light from the outer gaseous layers is represented in blues and greens. The white dwarf is visible as a tiny white dot in the center of the picture. The red color in the middle of the eye denotes the final layers of gas blown out when the star died.
The brighter red circle in the very center is the glow of a dusty disk circling the white dwarf (the disk itself is too small to be resolved). This dust, discovered by Spitzer's infrared heat-seeking vision, was most likely kicked up by comets that survived the death of their star. Before the star died, its comets and possibly planets would have orbited the star in an orderly fashion. But when the star blew off its outer layers, the icy bodies and outer planets would have been tossed about and into each other, resulting in an ongoing cosmic dust storm. Any inner planets in the system would have burned up or been swallowed as their dying star expanded.
The Helix nebula is one of only a few dead-star systems in which evidence for comet survivors has been found.
This image is made up of data from Spitzer's infrared array camera and multiband imaging photometer. Blue shows infrared light of 3.6 to 4.5 microns; green shows infrared light of 5.8 to 8 microns; and red shows infrared light of 24 microns.
Edited Spitzer Space Telescope image of the stars Cepheus C and Cepheus B. Inverted grayscale variant.
Original caption: This image was compiled using data from NASA's Spitzer Space Telescope using the Infrared Array Camera (IRAC) and the Multiband Imaging Photometer (MIPS) during Spitzer's "cold" mission, before the spacecraft's liquid helium coolant ran out in 2009. The colors correspond with IRAC wavelengths of 3.6 microns (blue), 4.5 microns (cyan) and 8 microns (green), and 24 microns (red) from the MIPS instrument.
The green-and-orange delta filling most of this image is a nebula, or a cloud of gas and dust. This region formed from a much larger cloud of gas and dust that has been carved away by radiation from stars.
The bright region at the tip of the nebula is dust that has been heated by the stars' radiation, which creates the surrounding red glow. The white color is the combination of four colors (blue, green, orange and red), each representing a different wavelength of infrared light, which is invisible to human eyes.
The massive stars illuminating this region belong to a star cluster that extends above the white spot.
On the left side of this image, a dark filament runs horizontally through the green cloud. A smattering of baby stars (the red and yellow dots) appear inside it. Known as Cepheus C, the area is a particularly dense concentration of gas and dust where infant stars form. This region is called Cepheus C because it lies in the constellation Cepheus, which can be found near the constellation Cassiopeia. Cepheus-C is about 6 light-years long, and lies about 40 light-years from the bright spot at the tip of the nebula.
The small, red hourglass shape just below Cepheus C is V374 Ceph. Astronomers studying this massive star have speculated that it might be surrounded by a nearly edge-on disk of dark, dusty material. The dark cones extending to the right and left of the star are a shadow of that disk.
The smaller nebula on the right side of the image includes a blue star crowned by a small, red arc of light. This "runaway star" is plowing through the gas and dust at a rapid clip, creating a shock wave or "bow shock" in front of itself.
Some features identified in the annotated image are more visible in the IRAC data alone.
The Jet Propulsion Laboratory in Pasadena, California, manages the Spitzer Space Telescope mission for NASA's Science Mission Directorate in Washington. Science operations are conducted at the Spitzer Science Center at Caltech in Pasadena. Space operations are based at Lockheed Martin Space Systems in Littleton, Colorado. Data are archived at the Infrared Science Archive housed at IPAC at Caltech. Caltech manages JPL for NASA.
The glowing Trifid Nebula is revealed with near- and mid-infrared views from NASA's Spitzer Space Telescope. The Trifid Nebula is a giant star-forming cloud of gas and dust located 5,400 light-years away in the constellation Sagittarius.
The false-color Spitzer image reveals a different side of the Trifid Nebula. Where dark lanes of dust are visible trisecting the nebula in a visible-light picture, bright regions of star-forming activity are seen in the Spitzer picture. All together, Spitzer uncovered 30 massive embryonic stars and 120 smaller newborn stars throughout the Trifid Nebula, in both its dark lanes and luminous clouds. These stars are visible in the Spitzer image, mainly as yellow or red spots. Embryonic stars are developing stars about to burst into existence.
Ten of the 30 massive embryos discovered by Spitzer were found in four dark cores, or stellar "incubators," where stars are born. Astronomers using data from the Institute of Radioastronomy millimeter telescope in Spain had previously identified these cores but thought they were not quite ripe for stars. Spitzer's highly sensitive infrared eyes were able to penetrate all four cores to reveal rapidly growing embryos.
Astronomers can actually count the individual embryos tucked inside the cores by looking closely at the Spitzer image taken by its infrared array camera (IRAC). This instrument has the highest spatial resolution of Spitzer's imaging cameras. The Spitzer image from the multiband imaging photometer (MIPS), on the other hand, specializes in detecting cooler materials. Its view highlights the relatively cool core material falling onto the Trifid's growing embryos. This image is a combination of Spitzer data from both of these instruments.
The embryos are thought to have been triggered by a massive "type O" star, which can be seen as a white spot at the center of the nebula. Type O stars are the most massive stars, ending their brief lives in explosive supernovas. The small newborn stars probably arose at the same time as the O star, and from the same original cloud of gas and dust.
This Spitzer mosaic image combines data from IRAC and MIPS, showing light of 4.5 microns (blue), 8.0 microns (green) and 24 microns (red).
C/2025 A6 (Comet Lemmon): A Visitor Beyond the Frost Line
Captured on the evening of October 24, 2025, from Desert Bloom Observatory in St. David, Arizona, this image reveals the subtle beauty of Comet C/2025 A6 (Lemmon)—a celestial wanderer tracing its path through the outer reaches of our Solar System. Using a Celestron Nexstar Evolution 9.25” Schmidt-Cassegrain telescope paired with a ZWO ASI2600MC Pro camera, the comet’s delicate coma and faint green hue emerge through the Optolong L-Pro multiband pass filter, hinting at ionized gases released as sunlight warms its icy core. Guided by precision optics and the quiet hum of equatorial tracking, this frozen relic from the early Solar System whispers stories from the age of planetary creation—its journey, timeless and luminous, across the star-filled silence.
Sgt. Raymond Walters, 1437thEngineer company, Sault Saint Marie, Mich., Michigan Army National Guard, demonstrates to AN/PRC-152 Multiband Handheld Radio to members of the Latvian Engineer Battalion ( ZS 54 ITBN), in Orge, Latvia, Sept. 28, 2014. The Michigan Army National Guard is training the Latvian Engineers on their equipment, while, in turn the Latvians train the Michigan soldiers on theirs. The Michigan and Latvian Engineers are training together in support of Operation Silver Arrow, in conjunction with United States Army Europe and Operation Northern Resolve. (U.S. Army photo by Sgt. 1st Class Helen Miller, Michigan National Guard/released)
Soldiers with the 5th Security Force Assistance Brigade trained virtually on new equipment in April 2020 to ensure their readiness using multiband radios for current and future missions. (U.S. Army photo by 5th Security Force Assistance Brigade public affairs).
I've got a rather large old radio that can tune into AM, FM, CB, PB, AIR, TV1, TV2, SW1 and SW2 frequencies, it's quite fun to listen to. Heard broadcasts on it as far as Vietnam in the east to Czech Republic in the west. ^_^
A while back I assisted some other Hams take down an antenna and tower. Thats me at the top 80ft level. Roger, N5RCS is below me lowering the multiband beam.
Born of Darkness: Orion’s Fire in a Sky That Still Knows Night
Captured beneath the stillness of the Desert Bloom Observatory, where the sky rests at Bortle 2 and deepens toward near-Bortle 1 after midnight, this portrait of the Orion Nebula (M42) reveals what the universe shares only when darkness is allowed to remain unbroken. Across 161 exposures of 600 seconds, taken over 14 sleepless nights, 110 hours of ancient photons gathered here — each one a fragment of a star’s beginning.
Through a carefully tuned imaging system — the Celestron NexStar Evolution 9.25” Schmidt-Cassegrain with HyperStar, the ZWO ASI2600MC Pro, ZWO guiding optics, and the Sky-Watcher EQ-6R — every photon was captured with precision. In processing, the stars were shaped with restraint, preventing bloat and preserving their natural presence in the field. The nebula itself was handled with gentle care, allowing its filaments, dust lanes, and ionized fronts to unfold exactly as the light intended.
From this treatment, M42 emerges in a gentle pink-rose hue, the natural expression of hydrogen emission through a broadband L-Pro filter. Soft teal accents from oxygen slip between the clouds, revealing the dynamic physics at work: gravitational collapse forming new suns, ultraviolet radiation carving glowing hollows in the dust, and stellar winds sculpting shapes that will one day cradle forming worlds.
More than an image, this is a reminder of the fragile gift of darkness. Only under protected night skies can the universe reveal its deepest truths. When we defend the night from artificial light, we preserve not just beauty — but humanity’s ability to wonder, to learn, and to trace our origins to the stars themselves.
Technical Summary
Object: M42 — The Orion Nebula
Constellation: Orion
Distance: ~1,344 light-years
Total Integration: 110 hours (161 × 600s)
Processing Pipeline: DeepSkyStacker → PixInsight → Photoshop
Location: Desert Bloom Observatory — Bortle 2 sky, approaching near-Bortle 1 after midnight
Equipment Used:
• Celestron NexStar Evolution 9.25" SCT (235mm f/10)
• Starizona HyperStar 4
• ZWO ASI2600MC Pro
• Sky-Watcher EQ-6R Pro Mount
• ZWO 30F4 MiniScope (Guide Scope)
• ZWO ASI462MC (Guide Camera)
• Optolong L-Pro 2" Multiband Filter
• ZWO Electronic Automatic Focuser (EAF)
• ZWO ASIAir Plus Controller
• Starizona Telrad Reflex Sight
• Astrozap Dew Heater
• Celestron Dew Shield
• Samsung Phone
• Memory Card
A Soldier assigned to the 3rd Infantry Brigade Combat Team, 25th Infantry Division checks a Manpack radio for an exercise on Aug. 22. The TSM waveform enables multiband and multimode operations. (Photo by Kathryn Bailey, PEO C3T)
Where Darkness Breathes Light — The California Nebula Under a Pristine Sky
Stretching across the constellation Perseus, the California Nebula (NGC 1499) glows like a slow-burning ember suspended in interstellar night. This vast emission nebula spans nearly 100 light-years and shines primarily through hydrogen-alpha emission, energized by the intense ultraviolet radiation of the hot, nearby star Xi Persei. What appears as a soft crimson mist is, in truth, a dynamic region where hydrogen atoms recombine and release light after being stripped by stellar photons.
This image is the result of 111 individual exposures, each 300 seconds long, carefully stacked and processed to reveal faint structures otherwise invisible to the human eye. Captured under a Bortle 2 sky, the darkness itself became a collaborator—allowing delicate filaments and subtle gradients to emerge without the veil of artificial light pollution.
Dark skies are not empty; they are alive with ancient photons traveling for thousands of years before reaching our sensors. Protecting them preserves not only scientific discovery, but our shared cosmic heritage. When we defend the night, we allow the universe to speak in its own quiet, luminous language.
Captured with the Following Equiptments:
>Telescope: Celestron Nexstar Evo 9.25 235mm f/10 Schmidt Cassegrain
>Camera: ZWO-ASI2600MCPRO
>Mount: Sky-Watcher EQ-6R Pro Computerized Equatorial Mount S303000
>Guide Scope: ZWO 30F4Miniscope
>Guide Camera: ZWO ASI462 MC Planetary Camera
>Starizona Hyperstar 4HS4-C9.25 white 10014
>ZWO standard Electronic Automatic Focuser EAF-5V
>ZWO ASIAir Plus Wifi Camera Controller
>Optolong- L-Pro 2” multiband Pass Filter
>Samsung Cellular Phone
>Memory Card
Flames Under a Borrowed Moon
Description
NGC 2024, the Flaming Nebula, burns quietly along the eastern edge of Orion’s Belt, embedded within the vast Orion Molecular Cloud Complex some 1,400 light-years from Earth. This emission nebula is powered by massive, newly formed stars whose intense ultraviolet radiation ionizes surrounding hydrogen gas, causing it to glow predominantly in deep red H-alpha light. Dark lanes of cold dust slice through the nebula, shaping its flame-like appearance and partially obscuring its stellar nursery within.
This image was intentionally captured under the presence of a waxing Moon to explore how natural sky brightness influences nebular color and contrast. Moonlight, rich in scattered blue wavelengths due to Rayleigh scattering in Earth’s atmosphere, subtly alters the color balance of deep-sky objects. As a result, the Flaming Nebula’s typical crimson tones shift toward a softer pink, while surrounding stars exhibit a cooler blue cast. This interaction demonstrates a real-world example of natural light pollution and its effect on broadband astrophotography, even when using a multiband filter.
Captured using a Hyperstar system at a fast focal ratio, this image emphasizes how optical speed, modern CMOS sensitivity, and careful calibration can still reveal faint cosmic structures under less-than-ideal conditions. Rather than erasing the Moon’s influence, this experiment embraces it—showing how celestial light sources interact, layer by layer, to paint the night sky not as it is ideally imagined, but as it is truly experienced.
Equipment Used
Telescope: Celestron NexStar Evo 9.25 (235mm f/10 Schmidt-Cassegrain)
Camera: ZWO ASI2600MC Pro
Mount: Sky-Watcher EQ-6R Pro Computerized Equatorial Mount
Guide Scope: ZWO 30F4 Mini Guide Scope
Guide Camera: ZWO ASI462MC
Optics: Starizona HyperStar 4 HS4-C9.25
Focuser: ZWO Electronic Automatic Focuser (EAF-5V)
Controller: ZWO ASIAIR Plus Wi-Fi Camera Controller
Filter: Optolong L-Pro 2″ Multiband Pass Filter
Additional Tools: Samsung Cellular Phone, Memory Card
Edited Spitzer Space Telescope image of the region around Rho Ophiuchi, showing lots of nebulae and stars. Color/processing variant.
Original caption: Newborn stars peek out from beneath their natal blanket of dust in this dynamic image of the Rho Ophiuchi dark cloud from NASA's Spitzer Space Telescope. Called "Rho Oph" by astronomers, it's one of the closest star-forming regions to our own solar system. Located near the constellations Scorpius and Ophiuchus, the nebula is about 407 light years away from Earth.
Rho Oph is a complex made up of a large main cloud of molecular hydrogen, a key molecule allowing new stars to form from cold cosmic gas, with two long streamers trailing off in different directions. Recent studies using the latest X-ray and infrared observations reveal more than 300 young stellar objects within the large central cloud. Their median age is only 300,000 years, very young compared to some of the universe's oldest stars, which are more than 12 billion years old.
This false-color image of Rho Oph's main cloud, Lynds 1688, was created with data from Spitzer's infrared array camera, which has the highest spatial resolution of Spitzer's three imaging instruments, and its multiband imaging photometer, best for detecting cooler
materials. Blue represents 3.6-micron light; green shows light of 8 microns; and red is 24-micron light. The multiple wavelengths reveal different aspects of the dust surrounding and between the embedded stars, yielding information about the stars and their birthplace.
The colors in this image reflect the relative temperatures and evolutionary states of the various stars. The youngest stars are surrounded by dusty disks of gas from which they, and their potential planetary systems, are forming. These young disk systems show up as red in this image. Some of these young stellar objects are surrounded by their own compact nebulae. More evolved stars, which have shed their natal material, are blue.
The infrared portrait of the Small Magellanic Cloud, taken by NASA's Spitzer Space Telescope, reveals the stars and dust in this galaxy as never seen before. The Small Magellanic Cloud is a nearby satellite galaxy to our Milky Way galaxy, approximately 200,000 light-years away.
The image shows the main body of the Small Magellanic Cloud, which is comprised of the "bar" and "wing" on the left and the "tail" extending to the right. The bar contains both old stars (in blue) and young stars lighting up their natal dust (green/red). The wing mainly contains young stars. The tail contains only gas, dust and newly formed stars. Spitzer data has confirmed that the tail region was recently torn off the main body of the galaxy. Two of the tail clusters, which are still embedded in their birth clouds, can be seen as red dots.
In addition, the image contains a galactic globular cluster in the lower left (blue cluster of stars) and emission from dust in our own galaxy (green in the upper right and lower right corners).
The data in this image are being used by astronomers to study the lifecycle of dust in the entire galaxy: from the formation in stellar atmospheres, to the reservoir containing the present day interstellar medium, and the dust consumed in forming new stars. The dust being formed in old, evolved stars (blue stars with a red tinge) is measured using mid-infrared wavelengths. The present day interstellar dust is weighed by measuring the intensity and color of emission at longer infrared wavelengths. The rate at which the raw material is being consumed is determined by studying ionized gas regions and the younger stars (yellow/red extended regions). The Small Magellanic Cloud, and its companion galaxy the Large Magellanic Cloud, are the two galaxies where this type of study is possible, and the research could not be done without Spitzer.
This image was captured by Spitzer's multiband imaging photometer, with 24-micron light colored blue; 70-micron light colored green and 160-micron light colored red. The blue, green, and red colors trace hot, warm and cool dust emission, respectively.
The image was taken as part of the Spitzer Legacy program known as SAGE-SMC: Surveying the Agents of Galaxy Evolution in the Tidally-Stripped, Low Metallicity Small Magellanic Cloud.
Image credit: NASA/JPL-Caltech/STScI
OK, lemme talk a little about yet another chapter in my continuing education concerning things I apparently decided not to appreciate until I was past 50.
So this is a clone of the Demeter Compulator optical compressor.
I've owned a couple of compressors over the years and have never really been a fan. I had a TC Electronic Sustain+Parametric Equalizer pedal for decades. I mainly used it as an EQ to drive a little growl-y peak into my amp, but the compressor part of the pedal was usually annoying to me. It seemed to suck a lot of the life out of anything I played and you could hear it bringing up the level as stuff decayed. I also had a Scholz Sustainor for years and never really cared much for the compressor in that thing, either, although it wasn't as annoying as the TC box. I also use the Multipressor software multiband compressor for computer remaster-y stuff, which I've done with old live recordings. That thing is magic. You can target ranges and completely change the overall tonal balance of a mix without resorting to EQ. It's probably my favorite plugin. I even ran Jean-Luc Ponty's, 'Egocentric Molucules' through it because I've always hated the mix. I was able to make that track SO much better in so little time that it seemed like some kind of voodoo.
Anyway, I decided I'd try an optical compressor. Right out of the gate, the thing was breaking up when I'd bang out a chord. It has an internal trimmer, though, so you can adapt it to various instruments. I had to turn that trimmer almost all the way down to use my Junior without getting distortion, so my guess is that this box was designed for Strat players. Either that, or guys with humbuckers just don't cotton to no squishee-squeezy bidness. In any case, by the time I had it working properly I was all ready to hate it.
Except it's really transparent. It's kind of like you aren't running an effect at all, except at the same time it's like I'm just freakin' awesome. Havin' one of those good nights where everything rings out like I want it to and my technique is better than normal.
I'm not experienced enough to know better at this point, but I feel like I could leave this thing on all the time. I wonder if there's some kind of Compressors Anonymous for people who won't shut these things off?
So...uh...cool.
BTW, you can see how it's set. The left knob is set for unity gain, which was pretty high, IMO. Not much more travel there if I'd wanted to boost things a little. The right knob is compression and that seems pretty awesome just a little to the left of noon. I'm just learning to hear what this thing does, so that may be high and I'm just not hearing anything ugly because my ears are still learning its wicked ways, but that sounds pretty awesome to me right now.
Edited Spitzer Space Telescope image of the region around Rho Ophiuchi, showing lots of nebulae and stars.
Original caption: Newborn stars peek out from beneath their natal blanket of dust in this dynamic image of the Rho Ophiuchi dark cloud from NASA's Spitzer Space Telescope. Called "Rho Oph" by astronomers, it's one of the closest star-forming regions to our own solar system. Located near the constellations Scorpius and Ophiuchus, the nebula is about 407 light years away from Earth.
Rho Oph is a complex made up of a large main cloud of molecular hydrogen, a key molecule allowing new stars to form from cold cosmic gas, with two long streamers trailing off in different directions. Recent studies using the latest X-ray and infrared observations reveal more than 300 young stellar objects within the large central cloud. Their median age is only 300,000 years, very young compared to some of the universe's oldest stars, which are more than 12 billion years old.
This false-color image of Rho Oph's main cloud, Lynds 1688, was created with data from Spitzer's infrared array camera, which has the highest spatial resolution of Spitzer's three imaging instruments, and its multiband imaging photometer, best for detecting cooler
materials. Blue represents 3.6-micron light; green shows light of 8 microns; and red is 24-micron light. The multiple wavelengths reveal different aspects of the dust surrounding and between the embedded stars, yielding information about the stars and their birthplace.
The colors in this image reflect the relative temperatures and evolutionary states of the various stars. The youngest stars are surrounded by dusty disks of gas from which they, and their potential planetary systems, are forming. These young disk systems show up as red in this image. Some of these young stellar objects are surrounded by their own compact nebulae. More evolved stars, which have shed their natal material, are blue.
Fabricada en material transpirable multibanda con dos bandas cruzadas, ballenas verticales en la espalda y cierre velcro delantero. La faja de color beige incorpora una placa lumbar extraíble de foam para dar calor en dicha zona o retirarse si no se precisa. Comodidad de uso y tacto suave en contacto con la piel. Tratamientos pre y post-quirúrgicos.
Para más información: www.exclusivasiglesias.com/es/product/ortesis-tronco/faja...
This image layout compares visible (left) and infrared views of the North America nebula, taken by the Digitized Sky Survey and NASA's Spitzer Space Telescope, respectively..
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The nebula is named after its resemblance to the North America content in visible light. This visible view highlights the eastern seaboard and Gulf of Mexico regions. In infrared light, the continent disappears. The "Mexican Riviera" -- the west coast of Mexico -- seems to invert in texture and brightness, as does the "neck" region of the Pelican nebula, named for its resemblance to a pelican. This nebula can be seen to the right of the North America nebula in the visible image. The Gulf of Mexico transforms from a dark cloud into a "river" of hundreds of young stars..
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These pictures look different in part because infrared light can penetrate dust whereas visible light cannot. Dusty, dark clouds in the visible image become transparent in Spitzer's view. In addition, Spitzer's infrared detectors pick up the glow of dusty cocoons enveloping baby stars..
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The Spitzer image contains data from both its infrared array camera and multiband imaging photometer. Light with a wavelength of 3.6 microns has been color-coded blue; 4.5-micron light is blue-green; 5.8-micron and 8.0-micron light are green; and 24-micron light is red.
Generations of stars can be seen in this new infrared portrait from NASA's Spitzer Space Telescope. In this wispy star-forming region, called W5, the oldest stars can be seen as blue dots in the centers of the two hollow cavities (other blue dots are background and foreground stars not associated with the region). Younger stars line the rims of the cavities, and some can be seen as pink dots at the tips of the elephant-trunk-like pillars. The white knotty areas are where the youngest stars are forming. Red shows heated dust that pervades the region's cavities, while green highlights dense clouds.
W5 spans an area of sky equivalent to four full moons and is about 6,500 light-years away in the constellation Cassiopeia. The Spitzer picture was taken over a period of 24 hours.
Like other massive star-forming regions, such as Orion and Carina, W5 contains large cavities that were carved out by radiation and winds from the region's most massive stars. According to the theory of triggered star-formation, the carving out of these cavities pushes gas together, causing it to ignite into successive generations of new stars.
This image contains some of the best evidence yet for the triggered star-formation theory. Scientists analyzing the photo have been able to show that the ages of the stars become progressively and systematically younger with distance from the center of the cavities.
This is a three-color composite showing infrared observations from two Spitzer instruments. Blue represents 3.6-micron light and green shows light of 8 microns, both captured by Spitzer's infrared array camera. Red is 24-micron light detected by Spitzer's multiband imaging photometer.
This swirling landscape of stars is known as the North America nebula. In visible light, the region resembles North America, but in this new infrared view from NASA's Spitzer Space Telescope, the continent disappears.
Where did the continent go? The reason you don't see it in Spitzer's view has to do, in part, with the fact that infrared light can penetrate dust whereas visible light cannot. Dusty, dark clouds in the visible image become transparent in Spitzer's view. In addition, Spitzer's infrared detectors pick up the glow of dusty cocoons enveloping baby stars.
Clusters of young stars (about one million years old) can be found throughout the image. Slightly older but still very young stars (about 3 to 5 million years) are also liberally scattered across the complex, with concentrations near the "head" region of the Pelican nebula, which is located to the right of the North America nebula (upper right portion of this picture).
Some areas of this nebula are still very thick with dust and appear dark even in Spitzer's view. For example, the dark "river" in the lower left-center of the image -- in the Gulf of Mexico region -- are likely to be the youngest stars in the complex (less than a million years old).
The Spitzer image contains data from both its infrared array camera and multiband imaging photometer. Light with a wavelength of 3.6 microns has been color-coded blue; 4.5-micron light is blue-green; 5.8-micron and 8.0-micron light are green; and 24-micron light is red.
That's grams, obviously. The spec sheet says 65g, but I did remove a couple of links to size the bracelet.
Really comfortable to wear, this.
[jbm-20250331-q3-022]
Faja sacrolumbar semirrígida en material transpirable multibanda con dos bandas elásticas tensoras cruzadas en la parte trasera que abrochan en el delantero, ballenas verticales en la espalda y cierre velcro delantero. Incorpora una bolsa de tela en la zona lumbar para poder insertar una placa intercambiable de material termomoldeable a baja temperatura. Fuerte apoyo y contención lumbar. Transpirable y muy cómoda de usar. Lumbalgias, procesos degenerativos, debilidad y atonía muscular, hernias discales, postoperatorio.
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Soundblox® Pro Multiwave Bass Distortion
Il Soundblox Pro Multiwave Bass Distortion eredita le potenza e la chiarezza dell'originale Soundblox Multiwave Distortion ma con algoritmi che si addicono alla gamma di frequenze del basso elettrico. I bassisti combinano accordi complessi e intervalli con toni distorti - Il processo multi banda elimina l'impasto delle note e fa si che ognuna esca pulita e fedele. Il pedale ha anche la possibilità di avere il processo singola banda per avere suoni distorti più tradizionali. E' il pedale perfetto sia in studio che sul palco.
Il musicista ha accesso a 23 tipi di distorsione, attuali e distinti, con un modalità clean boost/EQ. I tipi di curve di distorsione vanno dal "normale" overdrive per suoni classici fino al "foldback" e "octave" per suoni più aggressivi simili a tonalità synth. Ogni tipo di distorsione può essere personalizzata tramite I'equalizzatore a 7 bande, il controllo Drive e controlli di livello separati per segnali puliti e distorti. Questi avanzati controlli di suono attenuano la tendenza alla riduzione delle basse frequenze tipica di molte unita di distorsori per basso.
Sei impostazioni predefinite dall'utente, accessibili tramite tre footswitch, aiutano a richiamare in velocità ogni nuovo suono creato e l'uso di pedale di espressione rende più morbido il passaggio da un preset all'altro. Un ingresso MIDI permette l' accesso ai preset e ai parametri tramite un MIDI controller esterno, e, come tutta la produzione Soundblox, il pedale è compatibile con il controllo di movimento Hot Hand® per avere ancora più capacità espressive.
Caratteristiche:
• Ampia gamma di suoni - 23 varianti dei nostri unici algoritmi di distorsione più una modalità CLEAN BOOST + EQ.
• Processore Multibanda - Il segnale viene diviso in bande per poi essere distorto individualmente per ottenere un suono più chiaro.
• DSP ultima generazione - Digital Signal Processor proprietario della Source Audio a 56 bit, il SA601, e convertitori AD/DA a 24-bit totalmente trasparenti.
• 6 preset programmabili - Preset facili da programmare in due banchi selezionabili con i tre interruttori per un accesso veloce accesso ai suoni preferiti.
• Equalizzatore a 7 bande — Equalizzatore a 7 bande estremamente preciso, memorizzabile nei preset per un controllo del suono più accurato .
Sound Morphing - Ingresso per pedale d'espressione permette il passaggio morbido da un suono all'altro dei vari banchi di preset.
• Compatibilità MIDI - Ingresso MIDI per avere accesso dall'esterno ai preset e ai parametri
• Motion Control - tutti i pedali Soundblox™ sono "Hot Hand® Ready" e possono essere usati con qualsiasi sensore di movimento Hot Hand® in modo da estendere la compatibilità delle unità.
• Active Analog Bypass - nel modo bypass il segnale di ingresso viene completamente escluso dal DSP in modo da non avere degradazioni del segnale (zero signal degradation).
• Alimentatore a 9V incluso.
• Dimensioni: 17.8cm (profondità) x 15.25cm (larghezza) x 5cm (altezza, incluse le manopole).
Prezzo al pubblico: € 214,00 (iva esclusa).
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Distribuito in Italia da Reference Laboratory s.r.l.
Signal University students at Iron Horse University, Fort Carson, CO, receive training on the AN/PSC-5 Multiband Radio. Located at 11 installations inside and outside the United States, Signal University has instructors and training teams who deliver C4ISR training. Its curriculum helps Soldiers prepare for company- and battalion-level field training exercises and obtain specific MOS training. (U.S. Army photo)
The magnificent spiral arms of the nearby galaxy Messier 81 are highlighted in this image from NASA's Spitzer Space Telescope. Located in the northern constellation of Ursa Major (which also includes the Big Dipper), this galaxy is easily visible through binoculars or a small telescope. M81 is located at a distance of 12 million light-years.
This Spitzer infrared image is a composite mosaic obtained with the multiband imaging photometer and the infrared array camera. Thermal infrared emission at 24 microns detected by the photometer (red, bottom left inset) is combined with camera data at 8.0 microns (green, bottom center inset) and 3.6 microns (blue, bottom right inset).
The 3.6-micron near-infrared data (blue) traces the distribution of stars, although the Spitzer image is virtually unaffected by obscuring dust and reveals a very smooth stellar mass distribution, with the spiral arms relatively subdued.
As one moves to longer wavelengths, the spiral arms become the dominant feature of the galaxy. The 8-micron emission (green) is dominated by infrared light radiated by hot dust that has been heated by nearby luminous stars. Dust in the galaxy is bathed by ultraviolet and visible light from nearby stars. Upon absorbing an ultraviolet or visible-light photon, a dust grain is heated and re-emits the energy at longer infrared wavelengths. The dust particles are composed of silicates (chemically similar to beach sand), carbonaceous grains and polycyclic aromatic hydrocarbons and trace the gas distribution in the galaxy. The well-mixed gas (which is best detected at radio wavelengths) and dust provide a reservoir of raw materials for future star formation.
The 24-micron multiband imaging photometer data (red) shows emission from warm dust heated by the most luminous young stars. The infrared-bright clumpy knots within the spiral arms show where massive stars are being born in giant H II (ionized hydrogen) regions. Studying the locations of these star forming regions with respect to the overall mass distribution and other constituents of the galaxy (e.g., gas) will help identify the conditions and processes needed for star formation.