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Radio multibandas, de bulbos,siendo un gran adelante, en los 50`s, ya que podian captar estaciones de diferentes paises, aunque la mayoria era en su idima origina, como tambien se escuchaban señales de telegrafo entre otros.
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.
Saturn's moon Titan is one of the most difficult objects to figure out true colors. To begin with, its surface is simply impossible to observe in the visible range because of the haze. Sufficiently transparent spectral bands begin only in the infrared, which means that only for the infrared it is possible to create a global map. Fortunately, we have Huygens landing probe, whose data was processed by Erich Karkoschka and Stefan E. Schröder [1]. The figure 6 was run through my program TrueColorTools (requiring some modifications along the way). The multiband images were interpolated and extrapolated (to blue range) there to a spectral cube and then convolved with the sensitivity of the human eye.
Having surface panoramas with a known color processing, all that is left is to extend that color to some infrared map. The best available option was a map from B. Seignovert et al. [2], which was first rid of artifacts and manually cleaned of pixilization. The Huygens landing site was selected from this map and matched to a previously processed projection of it in visible colors.
Now we need to find an unknown transformation over a piece of the infrared map so that it produces something as close as possible to the corresponding piece of the visible map, and then apply the found transformation to the entire infrared map. Assuming linearity of the transformation, it can be written in the form IR · X + C = VIS, where IR is a known 3-vector of some pixel color, X is an unknown 3x3 color transformation matrix, C is an unknown 3-vector and VIS is the resulted visible color 3-vector. The linearity assumption can be justified if the surface spectra in the visible and infrared are highly correlated with each other (which is true), but the infrared map used [2] contains nonlinear color transformations to highlight geologic features. Therefore, it was renormalized as follows before processing: R′ = G · B = 2.03/1.08 μm, G′ = R · B = 1.59/1.08 μm, B′ = B = 1.27/1.08 μm.
It turns out that we do not know the 3x3+3=12 parameters of X and C responsible for color conversion. They were found in 12-dimensional space as a result of optimization over all the landing site pieces pixels by the MNC method in Python. There was an attempt to add another matrix with quadratic form, but it failed: the result was too optimized and unrealistic.
Unfortunately, Huygens was only able to capture a small region of the surface, only one of two variations in the coloration of the dunes. Therefore, the unknown color of the second type of dunes had to be handpicked based on the assumption that there were no sharp brightness gradients on the surface, and run the optimization with this patch of handpicked influence. The color of the lakes is also handpicked, no suitable theoretical data has been found. Without these assumptions, the texture map cannot be completed. That's about as close to maximum color realism as we can achieve right now.
Lake delineations were obtained separately using radar data [3], which had noise and missing data. These regions were manually reconstructed from infrared data from Cassini, and the infrared map [2] itself was pre-warped to match the radar data (reprojected from the polar stereographic projection with another Python script).
Thanks to Pedro J. and Chara for their help and support!
History
August 2025: the Titan color map series was updated in accordance with the color processing updates in TrueColorTools (Tikhonov regularization for spectral reconstruction, color spaces management).
Contrast is slightly increased due to the darker presumed visible color of the second type of dunes.
January 2026: Did a little research on the color of liquid methane and ethane under Titan surface conditions. Turns out they're likely transparent, see this paper. The spherical albedo color was calculated from the refractive index "n" from [4] by integrating the Fresnel equations. The script makes the average color of the lakes calculated taking into account map distortions.
Info
Simple cylindrical projection, center longitude 0°.
Gamma corrected, albedo corrected.
Sources
[2] B. Seignovert et al. (2019). Titan's global map combining VIMS and ISS mosaics (1.1). CaltechDATA
[4] Martonchik & Orton (1994). Optical constants of liquid and solid methane
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IC 4603: A Celestial Marvel
Image Description: IC 4603, a stunning reflection nebula, showcases the intricate beauty of interstellar dust and gas. Located in the constellation Scorpius, this nebula is a reflection of the light from nearby stars.
Image Capture Details:
This image was captured using a Celestron Nexstar Evolution 9.25 telescope with a Starizona Hypestar 4H4-C92.5 reducer, paired with a ZWO ASI2600MC Pro camera. The mount used was a Sky-Watcher EQ-6R Pro, guided by a ZWO 30f4 Mini Scope and ZWO ASI462MC Planetary Camera. An Optolong L-Pro 2" multiband pass filter was employed to enhance the image quality. The exposure time was 300 seconds.
Image Processing:
The image was stacked using DeepSkyStacker and processed in PixInsight and Adobe Photoshop.
Capture Location:
Desert Bloom Observatory, AZ, USA
Technical Details:
Telescope: Celestron Nexstar Evolution 9.25
Reducer: Starizona Hypestar 4H4-C92.5
Camera: ZWO ASI2600MC Pro
Mount: Sky-Watcher EQ-6R Pro
Guidescope: ZWO 30f4 Mini Scope
Guide Camera: ZWO ASI462MC Planetary Camera
Filter: Optolong L-Pro 2" multiband pass filter
Exposure: 300 seconds
Valle Orco, Parco nazionale del Gran Paradiso - Piemonte/Valle d'Aosta - Italia
AUTOPANO PRO 1.40RC2 Linux ed.
Pano-20 immagini-9113x2906-proiezione Spherical-interpolazione Bicubic Sharper-unione Multiband
The destructive results of a mighty supernova explosion reveal themselves in a delicate blend of infrared and X-ray light, as seen in this image from NASA’s Spitzer Space Telescope and Chandra X-Ray Observatory, and the European Space Agency's XMM-Newton.
The bubbly cloud is an irregular shock wave, generated by a supernova that would have been witnessed on Earth 3,700 years ago. The remnant itself, called Puppis A, is around 7,000 light-years away, and the shock wave is about 10 light-years across.
The pastel hues in this image reveal that the infrared and X-ray structures trace each other closely. Warm dust particles are responsible for most of the infrared light wavelengths, assigned red and green colors in this view. Material heated by the supernova’s shock wave emits X-rays, which are colored blue. Regions where the infrared and X-ray emissions blend together take on brighter, more pastel tones.
The shock wave appears to light up as it slams into surrounding clouds of dust and gas that fill the interstellar space in this region.
From the infrared glow, astronomers have found a total quantity of dust in the region equal to about a quarter of the mass of our sun. Data collected from Spitzer’s infrared spectrograph reveal how the shock wave is breaking apart the fragile dust grains that fill the surrounding space.
Supernova explosions forge the heavy elements that can provide the raw material from which future generations of stars and planets will form. Studying how supernova remnants expand into the galaxy and interact with other material provides critical clues into our own origins.
Infrared data from Spitzer’s multiband imaging photometer (MIPS) at wavelengths of 24 and 70 microns are rendered in green and red. X-ray data from XMM-Newton spanning an energy range of 0.3 to 8 keV (kiloelectron volts) are shown in blue.
Cuando se trata de corregir una imagen multibanda lo más importante es eliminar el efecto de sombra causado por la topografÃa, porque las sombras distorsionan las clasificaciones que se le puedan hacer a los pÃxeles. Para una imagen hiperespectral esa sombra no es relevante, porque lo más importante es identificar los patrones de absorción o reflectancia a distintos anchos de banda.
Siempre me equivoco en algo al dibujar. Necesito encontrar la forma de llegar a formas que resulten bien, que no tengan esos errores que distorsionan mi señal. No puedo dejar de insistir. Quiero aprender.
Hoy tuve que dibujar un luche en el suelo de la Escuela para una actividad de la escuela de dirigentes rurales. Ese luche salió misteriosamente parecido a la portada de la primera edición de Rayuela, de la editorial Eudeba. Pero en vez del Cielo que estaba en el último espacio dibujado en ese libro, se encontraba el Tiempo. Y nos costó lograr llegar a él con las piedritas.
Canciones descubiertas y escuchadas una y otra vez: la enredadera- leo quinteros/ azucar café- manuel garcÃa.
The NASA CE318-N Sun Sky photometer at the Mesa Lakes Ranger Station. The multiband photometer operates at daytime and takes optical measurements to provide quantification and physical-optical characterization of the aerosols.
U.S. Marine Corps Cpl. Jan Kamphuis, participating in Weapons and Tactics Instructor (WTI) 1-15 Course from Marine Air Control Squadron (MACS) 2 Detachment B, Marine Aircraft Group (MAG) 28, 2nd Marine Aircraft Wing (MAW), uses a portable radio communications 117F multiband manpack radio to communicate with a KC-130J Hercules aircraft on Stoval Auxiliary Landing Field, Yuma County, Ariz., Sept. 23, 2014. WTI is a seven week training event hosted by Marine Aviation and Weapon Tactics Squadron (MAWTS-1) cadre. MAWTS-1 provides standardized advanced tactical training and certification of unit instructor qualifications to support Marine Aviation Training and Readiness and assists in developing and employing aviation weapons and tactics. (U.S. Marine Corps photo by Cpl. Allison J. Herman, COMCAM/Released)