View allAll Photos Tagged multiband
Stewart Warner Tombstone tube radio (Hammond Museum) - this has multicolour - multiband edge lit dial -beautiful when lit
Edited Spitzer Space Telescope PR image of the Cepheus C and Cepheus B region and associated nebula. Color/processing variant.
Image source: photojournal.jpl.nasa.gov/catalog/PIA23126
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, found here.
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.
For more information on Spitzer, visit:
www.nasa.gov/spitzer and www.spitzer.caltech.edu/
Image Credit:
NASA/JPL-Caltech
Image Addition Date:
2019-05-30
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.
Top-down: Kroma intercom panel, Blackmagic Design router controller, tc.electronic multiband compressor/finalizer
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
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
This pirate tin houses a 1:1 ferrite balun and feeds a trap multiband dipole antenna in my living room / hallway
Edited Spitzer Space Telescope image of the stars Cepheus C and Cepheus B. Color/processing 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.
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.
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)
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...
I got my "General" class amateur radio license in January, but had only been using a short-distance (up to 30 miles) VHF/UHF handheld radio until recently. I got this HF/VHF/UHF multiband radio a couple weeks ago to operate on the HF bands (160m to 6m wavelength). Even though my antenna is installed temporarily indoors through my second floor bedrooms, it is working quite well. My farthest contact is Germany, over 4,000 miles away, using only 75W of power, on the 17m band in phone SSB mode.
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.
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
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.
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.
Para más información: www.exclusivasiglesias.com/es/product/ortesis-tronco/faja...
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.
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.
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.
Created from RAW data of spitzer space telescope
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) is combined with camera data at 8.0 microns (green) and 3.6 microns (blue).
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.
The core is less blueish as compared to original spitzer image to show the delicate spiral structures around the core. I needed to scale up the 24 micron image , so red halos appear but i used minimum filter to reduce this artifact, but extensive use caused a loos in data in this channel so i used it moderately
It is a five channel composite,
3.6 , 4.5 , 5.8 , 8.0 and 24 microns.
Credits: Bipradeep Saha / NASA / SHA
The Pinwheel galaxy, otherwise known as Messier 101, sports bright reddish edges in this new infrared image from NASA's Spitzer Space Telescope. Research from Spitzer has revealed that this outer red zone lacks organic molecules present in the rest of the galaxy. The red and blue spots outside of the spiral galaxy are either foreground stars or more distant galaxies.
The organics, called polycyclic aromatic hydrocarbons, are dusty, carbon-containing molecules that help in the formation of stars. On Earth, they are found anywhere combustion reactions take place, such as barbeque pits and exhaust pipes. Scientists also believe this space dust has the potential to be converted into the stuff of life.
Spitzer found that the polycyclic aromatic hydrocarbons decrease in concentration toward the outer portion of the Pinwheel galaxy, then quickly drop off and are no longer detected at its very outer rim. According to astronomers, there's a threshold at the rim where the organic material is being destroyed by harsh radiation from stars. Radiation is more damaging at the far reaches of a galaxy because the stars there have less heavy metals, and metals dampen the radiation.
The findings help researchers understand how stars can form in these harsh environments, where polycyclic aromatic hydrocarbons are lacking. Under normal circumstances, the polycyclic aromatic hydrocarbons help cool down star-forming clouds, allowing them to collapse into stars. In regions like the rim of the Pinwheelas well as the very early universestars form without the organic dust. Astronomers don't know precisely how this works, so the rim of the Pinwheel provides them with a laboratory for examining the process relatively close up.
In this image, infrared light with a wavelength of 3.6 microns is colored blue; 8-micron light is green; and 24-micron light is red. All three of Spitzer's instruments were used in the study: the infrared array camera, the multiband imaging photometer and the infrared spectrograph.
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)
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)
Band alumni, parents, and friends gathered before Multibands to enjoy great company, drinks, and hors d’oeuvres. The 2017 recipients of the Band Alumni Scholarship and the 2017 Minuteman Band Hall of Fame class were honored and attendees got the first look at a special portrait of legendary former Minuteman Band announcer Jim MacRostie — as well as the band’s new uniforms!
The atomic bomb dropped on Nagasaki was actually intended for Kokura but due to heavy cloud over Kokura the next target is Nagasaki.
This image from NASA's Spitzer Space Telescope shows infant stars "hatching" in the head of the hunter constellation, Orion. Astronomers suspect that shockwaves from a supernova explosion in Orion's head, nearly three million years ago, may have initiated this newfound birth..
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The region featured in this Spitzer image is called Barnard 30. It is located approximately 1,300 light-years away and sits on the right side of Orion's head, just north of the massive star Lambda Orionis..
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Wisps of green in the cloud are organic molecules called polycyclic aromatic hydrocarbons (PAHs). PAHs are formed anytime carbon-based materials are burned incompletely. On Earth, they can be found in the sooty exhaust from automobile and airplane engines. They also coat the grills where charcoal-broiled meats are cooked..
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Tints of orange-red in the cloud are dust particles warmed by the newly forming stars. The reddish-pink dots at the top of the cloud are very young stars embedded in a cocoon of cosmic gas and dust. Blue spots throughout the image are background Milky Way along this line of sight..
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This composite includes data from Spitzer's infrared array camera instrument, and multiband imaging photometer instrument. Light at 4.5 microns is shown as blue, 8.0 microns is green, and 24 microns is red.