This deep-field view of the sky, taken by NASA's Spitzer Space Telescope, is dominated by galaxies - including some very faint, very distant ones - circled in red. The bottom right inset shows one of those distant galaxies, made visible thanks to a long-duration observation by Spitzer. The wide-field view also includes data from NASA's Hubble Space Telescope. The Spitzer observations came from the GREATS survey, short for GOODS Re-ionization Era wide-Area Treasury from Spitzer. GOODS is itself an acronym: Great Observatories Origins Deep Survey. NASA's Jet Propulsion Laboratory, Pasadena, Calif., manages the Spitzer Space Telescope mission for NASA's Science Mission Directorate, Washington. Science operations are conducted at the Spitzer Science Center at the California Institute of Technology, also in Pasadena. Caltech manages JPL for NASA. The Hubble Space Telescope is a project of international cooperation between NASA and the European Space Agency. The Space Telescope Science Institute conducts Hubble science operations. The institute is operated for NASA by the Association of Universities for Research in Astronomy, Inc., Washington, D.C.

This image from NASA's Spitzer Space Telescope shows the elliptical galaxy Messier 87 (M87), the home galaxy of the supermassive black hole recently imaged by the Event Horizon Telescope (EHT). Spitzer's infrared view shows a faint trace of a jet of material spewing to the right of the galaxy - a feature that was previously one key indicator that a supermassive black hole lived at the galaxy's center. More prominent in the image is the shockwave created by that jet. The inset in the image below shows a close-up view of the shockwave on the right side of the galaxy, as well as the shockwave from a second jet traveling to the left of the galaxy. Located about 55 million light-years from Earth, M87 has been a subject of astronomical study for more than 100 years and has been imaged by many NASA observatories, including the Hubble Space Telescope, the Chandra X-ray Observatory and NuSTAR. In 1918, astronomer Heber Curtis first noticed "a curious straight ray" extending from the galaxy's center. This bright jet (which appears to extend to the right of the galaxy) is visible in multiple wavelengths of light, from radio waves through X-rays. The jet is produced by a disk of material spinning rapidly around the black hole, and spewing in opposite directions away from the galaxy. When the particles in the jet impact the interstellar medium (the sparse material filling the space between stars in M87), they create a shockwave that radiates in infrared and radio wavelengths of light, but not visible light. The jet on the right is traveling almost directly toward Earth, and its brightness is amplified due to its high speed in our direction. But the jet's trajectory is just slightly offset from our line of sight with the galaxy, so we can still see some of the length of the jet. The shockwave begins around the point where the jet appears to curve down, highlighting the regions where the fast-moving particles are colliding with gas in the galaxy and slowing down. There is also a second jet on the left that is moving so rapidly away from us it is rendered invisible at all wavelengths. But the shockwave it creates in the interstellar medium can still be seen here. In the Spitzer image, the shockwave is on the left side of the galaxy and looks like an inverted letter "C." This image from NASA's Spitzer Space Telescope shows M87 looks like a hazy, blue space-puff. At the galaxy's center is a supermassive black hole that spews two jets of material out into space. This image shows a wide-field image of M87, also taken by NASA's Spitzer Space Telescope. The top inset shows a close-up of two shockwaves, created by a jet emanating from the galaxy's supermassive black hole. The Event Horizon Telescope recently took a close-up image of the silhouette of that black hole, shown in the second inset. Scientists are still striving for a solid theoretical understanding of how inflowing gas around black holes creates outflowing jets. Infrared light at wavelengths of 3.4 and 4.5 microns are rendered in blue and green, showing the distribution of stars, while dust features that glow brightly at 8.0 microns are shown in red. 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.

This image from NASA's Spitzer Space Telescope shows the elliptical galaxy Messier 87 (M87), the home galaxy of the supermassive black hole recently imaged by the Event Horizon Telescope (EHT). Spitzer's infrared view shows a faint trace of a jet of material spewing to the right of the galaxy - a feature that was previously one key indicator that a supermassive black hole lived at the galaxy's center. More prominent in the image is the shockwave created by that jet. The inset in the image below shows a close-up view of the shockwave on the right side of the galaxy, as well as the shockwave from a second jet traveling to the left of the galaxy. Located about 55 million light-years from Earth, M87 has been a subject of astronomical study for more than 100 years and has been imaged by many NASA observatories, including the Hubble Space Telescope, the Chandra X-ray Observatory and NuSTAR. In 1918, astronomer Heber Curtis first noticed "a curious straight ray" extending from the galaxy's center. This bright jet (which appears to extend to the right of the galaxy) is visible in multiple wavelengths of light, from radio waves through X-rays. The jet is produced by a disk of material spinning rapidly around the black hole, and spewing in opposite directions away from the galaxy. When the particles in the jet impact the interstellar medium (the sparse material filling the space between stars in M87), they create a shockwave that radiates in infrared and radio wavelengths of light, but not visible light. The jet on the right is traveling almost directly toward Earth, and its brightness is amplified due to its high speed in our direction. But the jet's trajectory is just slightly offset from our line of sight with the galaxy, so we can still see some of the length of the jet. The shockwave begins around the point where the jet appears to curve down, highlighting the regions where the fast-moving particles are colliding with gas in the galaxy and slowing down. There is also a second jet on the left that is moving so rapidly away from us it is rendered invisible at all wavelengths. But the shockwave it creates in the interstellar medium can still be seen here. In the Spitzer image, the shockwave is on the left side of the galaxy and looks like an inverted letter "C." This image from NASA's Spitzer Space Telescope shows M87 looks like a hazy, blue space-puff. At the galaxy's center is a supermassive black hole that spews two jets of material out into space. This image shows a wide-field image of M87, also taken by NASA's Spitzer Space Telescope. The inset shows a close-up of two shockwaves, created by a jet emanating from the galaxy's supermassive black hole. Scientists are still striving for a solid theoretical understanding of how inflowing gas around black holes creates outflowing jets. Infrared light at wavelengths of 3.4 and 4.5 microns are rendered in blue and green, showing the distribution of stars, while dust features that glow brightly at 8.0 microns are shown in red. 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.

This image from NASA's Spitzer Space Telescope shows the elliptical galaxy Messier 87 (M87), the home galaxy of the supermassive black hole recently imaged by the Event Horizon Telescope (EHT). Spitzer's infrared view shows a faint trace of a jet of material spewing to the right of the galaxy - a feature that was previously one key indicator that a supermassive black hole lived at the galaxy's center. More prominent in the image is the shockwave created by that jet. The inset in the image below shows a close-up view of the shockwave on the right side of the galaxy, as well as the shockwave from a second jet traveling to the left of the galaxy. Located about 55 million light-years from Earth, M87 has been a subject of astronomical study for more than 100 years and has been imaged by many NASA observatories, including the Hubble Space Telescope, the Chandra X-ray Observatory and NuSTAR. In 1918, astronomer Heber Curtis first noticed "a curious straight ray" extending from the galaxy's center. This bright jet (which appears to extend to the right of the galaxy) is visible in multiple wavelengths of light, from radio waves through X-rays. The jet is produced by a disk of material spinning rapidly around the black hole, and spewing in opposite directions away from the galaxy. When the particles in the jet impact the interstellar medium (the sparse material filling the space between stars in M87), they create a shockwave that radiates in infrared and radio wavelengths of light, but not visible light. The jet on the right is traveling almost directly toward Earth, and its brightness is amplified due to its high speed in our direction. But the jet's trajectory is just slightly offset from our line of sight with the galaxy, so we can still see some of the length of the jet. The shockwave begins around the point where the jet appears to curve down, highlighting the regions where the fast-moving particles are colliding with gas in the galaxy and slowing down. There is also a second jet on the left that is moving so rapidly away from us it is rendered invisible at all wavelengths. But the shockwave it creates in the interstellar medium can still be seen here. In the Spitzer image, the shockwave is on the left side of the galaxy and looks like an inverted letter "C." This image from NASA's Spitzer Space Telescope shows M87 looks like a hazy, blue space-puff. At the galaxy's center is a supermassive black hole that spews two jets of material out into space. This image shows a wide-field image of M87, also taken by NASA's Spitzer Space Telescope. Scientists are still striving for a solid theoretical understanding of how inflowing gas around black holes creates outflowing jets. Infrared light at wavelengths of 3.4 and 4.5 microns are rendered in blue and green, showing the distribution of stars, while dust features that glow brightly at 8.0 microns are shown in red. 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.

What looks like a red butterfly in space is in reality a nursery for hundreds of baby stars, revealed in this infrared image from NASA's Spitzer Space Telescope. Officially named W40, the butterfly is a nebula - a giant cloud of gas and dust in space where new stars may form. The butterfly's two "wings" are giant bubbles of hot, interstellar gas blowing from the hottest, most massive stars in this region. The material that forms W40's wings was ejected from a dense cluster of stars that lies between the wings in the image. The hottest, most massive of these stars, W40 IRS 1a, lies near the center of the star cluster. W40 is about 1,400 light-years from the Sun, about the same distance as the well-known Orion nebula, although the two are almost 180 degrees apart in the sky. They are two of the nearest regions in which massive stars - with masses upwards of 10 times that of the Sun - have been observed to be forming. The W40 star-forming region was observed as part of a Spitzer Legacy Survey, and the resulting mosaic image was published as part of the MYStIX (Massive Young stellar clusters Study in Infrared and X-rays) survey of young stellar objects. The Spitzer picture is composed of four images taken with the telescope's Infrared Array Camera (IRAC) in different wavelengths of infrared light: 3.6, 4.5, 5.8 and 8.0 m (shown as blue, green, orange and red). Organic molecules made of carbon and hydrogen, called polycyclic aromatic hydrocarbons (PAHs), are excited by interstellar radiation and become luminescent at wavelengths near 8.0 microns, giving the nebula its reddish features. Stars are brighter at the shorter wavelengths, giving them a blue tint. Some of the youngest stars are surrounded by dusty disks of material, which glow with a yellow or red hue. NASA's Jet Propulsion Laboratory, Pasadena, California, manages the Spitzer Space Telescope mission for NASA's Science Mission Directorate, Washington. Science operations are conducted at the Spitzer Science Center at Caltech in Pasadena, California. Spacecraft operations are based at Lockheed Martin Space Systems Company, Littleton, Colorado. Data are archived at the Infrared Science Archive housed at the Infrared Processing and Analysis Center at Caltech. Caltech manages JPL for NASA.

This image shows two merging galaxies known as Arp 302, also called VV 340. In these images, different colors correspond to different wavelengths of infrared light. Blue and green are wavelengths both strongly emitted by stars. Red is a wavelength mostly emitted by dust.

This image shows the merger of two galaxies, known as NGC 6786 (right) and UGC 11415 (left), also collectively called VII Zw 96. It is composed of images from three Spitzer Infrared Array Camera (IRAC) channels: IRAC channel 1 in blue, IRAC channel 2 in green and IRAC channel 3 in red.

This image shows the merger of two galaxies, known as NGC 7752 (larger) and NGC 7753 (smaller), also collectively called Arp86. In these images, different colors correspond to different wavelengths of infrared light. Blue and green are wavelengths both strongly emitted by stars. Red is a wavelength mostly emitted by dust.

This image of supernova remnant G54.1+0.3 includes radio, infrared and X-ray light. The saturated yellow point at the center of the image indicates strong X-ray source at the center of the supernova remnant. This is an incredibly dense object called a neutron star, which can form as a star runs out of fuel to keep it inflated, and the unsupported material collapses down on to the star's core. G54.1+0.3 contains a special type of neutron star called a pulsar, which emits particularly bright radio and X-ray emissions. The blue and green emissions show the presence of dust, including silica. The red hues correspond to radio data from the Karl G. Jansky Very Large Array; green corresponds to 70 m wavelength infrared light from the European Space Agency's Herschel Space Observatory; blue corresponds to 24 m wavelength infrared light from the Multiband Imaging Photometer (MIPS) instrument on NASA's Spitzer Space Telescope; yellow corresponds to X-ray data from the Chandra X-ray Observatory.

The Cat's Paw Nebula, imaged here by NASA's Spitzer Space Telescope, is a star-forming region inside the Milky Way Galaxy and is located in the constellation Scorpius. Its distance from Earth is estimated to be between 1.3 kiloparsecs (about 4,200 light years) to 1.7 kiloparsecs (about 5,500 light years). The image was taken as part of the Galactic Legacy Infrared Midplane Survey Extraordinaire (GLIMPSE), a survey of the Milky Way Galaxy. It was taken using Spitzer's Infrared Array Camera (IRAC). The colors correspond with wavelengths of 3.6 microns (blue), 4.5 microns (green), and 8 microns (red). The bright, cloudlike band running left to right across the image shows the presence of gas and dust that can collapse to form new stars. The black filaments running through the nebula are particularly dense regions of gas and dust. The entire star-forming region is thought to be between 24 and 27 parsecs (80-90 light years) across.New stars may heat up the pressurized gas surrounding them causing the gas to expand and form "bubbles".

The Cat's Paw Nebula, imaged here by NASA's Spitzer Space Telescope, lies inside the Milky Way Galaxy and is located in the constellation Scorpius. Its distance from Earth is estimated to be between 1.3 kiloparsecs (about 4,200 light years) to 1.7 kiloparsecs (about 5,500 light years). The bright, cloudlike band running left to right across the image shows the presence of gas and dust that can collapse to form new stars. The black filaments running through the nebula are particularly dense regions of gas and dust. The entire star-forming region is thought to be between 24 and 27 parsecs (80-90 light years) across.The stars that form inside the nebula heat up the pressurized gas surrounding them, such that the gas may expand and form "bubbles," which appear red in this image. Asymmetric bubbles may "burst," creating U-shaped features. The green areas show regions where radiation from hot stars collided with large molecules and small dust grains called polycyclic aromatic hydocarbons (PAHs), causing them to fluoresce. This image was compiled using data from two Spitzer instruments, the Infrared Array Camera (IRAC) and the Multiband Imaging Photometer (MIPS). The colors correspond with wavelengths of 3.6 microns (blue), 4.5 microns (cyan), 8 microns (green) and 24 microns (red).

These simulated views of the ultrahot Jupiter WASP-121b show what the planet might look like to the human eye from five different vantage points, illuminated to different degrees by its parent star. The images were created using a computer simulation being used to help scientists understand the atmospheres of these ultra-hot planets. Ultrahot Jupiters reflect almost no light, rather like charcoal. However, the daysides of ultrahot Jupiters have temperatures of between 3600F and 5400F (2000C and 3000C), so the planets produce their own glow, like a hot ember. The orange color in this simulated image is thus from the planet's own heat. The computer model was based on observations of WASP-121b conducted using NASA's Spitzer and Hubble space telescopes.

Thin, red veins of energized gas mark the location of the supernova remnant HBH3 in this image from NASA's Spitzer Space Telescope. The puffy, white feature in the image is a portion of the star forming regions W3, W4 and W5. Infrared wavelengths of 3.6 microns have been mapped to blue, and 4.5 microns to red. The white color of the star-forming region is a combination of both wavelengths, while the HBH3 filaments radiate only at the longer 4.5 micron wavelength. NASA's Jet Propulsion Laboratory, Pasadena, California, manages the Spitzer Space Telescope mission for NASA's Science Mission Directorate, Washington. Science operations are conducted at the Spitzer Science Center at Caltech in Pasadena, California. Spacecraft operations are based at Lockheed Martin Space Systems Company, Littleton, Colorado. Data are archived at the Infrared Science Archive housed at the Infrared Processing and Analysis Center at Caltech. Caltech manages JPL for NASA.

A diagram showing the components of the TDE observed in Arp299B. (Not to scale). The supermassive black hole at the center of the galaxy is surrounded by a highly dense medium, and embedded in a dusty torus. Most of the optical and X-ray emissions produced by the event were absorbed, and re-emitted at infrared (IR) wavelengths due to the existence of polar dust. A few months after the detection at IR wavelengths, the TDE was detected at radio wavelengths with the help of a very sensitive array of radio telescopes.

An image of the galaxy Arp299B, which is undergoing a merging process with Arp299A (the galaxy to the left), captured by NASA's Hubble space telescope. The inset features an artist's illustration of a tidal disruption event (TDE), which occurs when a star passes fatally close to a supermassive black hole. A TDE was recently observed near the center of Arp299B.

An artist's concept of a tidal disruption event (TDE) that happens when a star passes fatally close to a supermassive black hole, which reacts by launching a relativistic jet.

This graph presents known properties of the seven TRAPPIST-1 exoplanets (labeled b through h), showing how they stack up to the inner rocky worlds in our own solar system. The horizontal axis shows the level of illumination that each planet receives from its host star. TRAPPIST-1 is a mere 9 percent the mass of our Sun, and its temperature is much cooler. But because the TRAPPIST-1 planets orbit so closely to their star, they receive comparable levels of light and heat to Earth and its neighboring planets. The vertical axis shows the densities of the planets. Density, calculated based on a planet's mass and volume, is the first important step in understanding a planets composition. The plot shows that the TRAPPIST-1 planet densities range from being similar to Earth and Venus at the upper end, down to values comparable to Mars at the lower end. The relative sizes of the planets are indicated by the circles. The masses and densities of the TRAPPIST-1 planets were determined by careful measurements of slight variations in the timings of their orbits using extensive observations made by NASAs Spitzer and Kepler space telescopes, in combination with data from Hubble and a number of ground-based telescopes. These measurements are the most precise to date for any system of exoplanets. By comparing these measurements with theoretical models of how planets form and evolve, researchers have determined that they are all rocky in overall composition. Estimates suggest the lower-density planets could have large quantities of water -- as much as 5 percent by mass for TRAPPIST-1d. Earth, in comparison, has only about 0.02 percent of its mass in the form of water.

This artist's concept shows what the TRAPPIST-1 planetary system may look like, based on available data about the planets' diameters, masses and distances from the host star, as of February 2018. This image represents an updated version of one originally created in 2017. The planets' appearances were re-imagined based on a 2018 study using additional observations from NASA's Spitzer and Kepler space telescopes, in addition to previous data from Spitzer, the ground-based TRAPPIST (TRAnsiting Planets and PlanetesImals Small Telescope) telescope and other ground-based observatories. The system was named for the TRAPPIST telescope. The new analysis concludes that the seven planets of TRAPPIST-1 are all rocky, and some could contain significant amounts of water. TRAPPIST-1 is an ultra-cool dwarf star in the constellation Aquarius, and its planets orbit very close to it. The form that water would take on TRAPPIST-1 planets would depend on the amount of heat they receive from their star, which is a mere 9 percent as massive as our Sun. Planets closest to the star are more likely to host water in the form of atmospheric vapor, while those farther away may have water frozen on their surfaces as ice. TRAPPIST-1e is the rockiest planet of them all, but still is believed to have the potential to host some liquid water. In this illustration, the relative sizes of the planets and their host star, an ultracool dwarf, are all shown to scale.

This artist's concept shows what the TRAPPIST-1 planetary system may look like, based on available data about the planets' diameters, masses and distances from the host star, as of February 2018. This image represents an updated version of one originally created in 2017. The planets' appearances were re-imagined based on a 2018 study using additional observations from NASA's Spitzer and Kepler space telescopes, in addition to previous data from Spitzer, the ground-based TRAPPIST (TRAnsiting Planets and PlanetesImals Small Telescope) telescope and other ground-based observatories. The system was named for the TRAPPIST telescope. The new analysis concludes that the seven planets of TRAPPIST-1 are all rocky, and some could contain significant amounts of water. TRAPPIST-1 is an ultra-cool dwarf star in the constellation Aquarius, and its planets orbit very close to it. The form that water would take on TRAPPIST-1 planets would depend on the amount of heat they receive from their star, which is a mere 9 percent as massive as our Sun. Planets closest to the star are more likely to host water in the form of atmospheric vapor, while those farther away may have water frozen on their surfaces as ice. TRAPPIST-1e is the rockiest planet of them all, but still is believed to have the potential to host some liquid water. In this illustration, the relative sizes of the planets and their host star, an ultracool dwarf, are all shown to scale.

This illustration shows the seven Earth-size planets of TRAPPIST-1, an exoplanet system about 40 light-years away, based on data current as of February 2018. The image shows the planets relative sizes but does not represent their orbits to scale. The art highlights possibilities for how the surfaces of these intriguing worlds might look based on their newly-calculated properties. The seven planets of TRAPPIST-1 are all Earth-sized and terrestrial. TRAPPIST-1 is an ultra-cool dwarf star in the constellation Aquarius, and its planets orbit very close to it.

All seven planets discovered in orbit around the red dwarf star TRAPPIST-1 could easily fit inside the orbit of Mercury, the innermost planet of our solar system. In fact, they would have room to spare. TRAPPIST-1 also is only a fraction of the size of our Sun; it isn't much larger than Jupiter. So, the TRAPPIST-1 system's proportions look more like Jupiter and its moons than those of our solar system. The seven planets of TRAPPIST-1 are all Earth-sized and terrestrial. TRAPPIST-1 is an ultra-cool dwarf star in the constellation Aquarius, and its planets orbit very close to it. This image has artwork updated in Feb. 2018 to reflect surfaces based on more precise measurements of the planets' densities.

This chart shows, on the top row, artist concepts of the seven planets of TRAPPIST-1 with their orbital periods, distances from their star, radii, masses, densities and surface gravity as compared to those of Earth. These numbers are current as of February 2018. On the bottom row, the same numbers are displayed for the bodies of our inner solar system: Mercury, Venus, Earth and Mars. The TRAPPIST-1 planets orbit their star extremely closely, with periods ranging from 1.5 to only about 20 days. This is much shorter than the period of Mercury, which orbits our sun in about 88 days. The masses and densities of the TRAPPIST-1 planets were determined by careful measurements of slight variations in the timings of their orbits using extensive observations made by NASAs Spitzer and Kepler space telescopes, in combination with data from Hubble and a number of ground-based telescopes. These measurements are the most precise to date for any system of exoplanets. In this illustration, the relative sizes of the planets are all shown to scale.

This image of distant interacting galaxies, known collectively as Arp 142, bears an uncanny resemblance to a penguin guarding an egg. Data from NASA's Spitzer and Hubble space telescopes have been combined to show these dramatic galaxies in light that spans the visible and infrared parts of the spectrum. This dramatic pairing shows two galaxies that couldn't look more different as their mutual gravitational attraction slowly drags them closer together. The "penguin" part of the pair, NGC 2336, was probably once a relatively normal-looking spiral galaxy, flattened like a pancake with smoothly symmetric spiral arms. Rich with newly-formed hot stars, seen in visible light from Hubble as bluish filaments, its shape has now been twisted and distorted as it responds to the gravitational tugs of its neighbor. Strands of gas mixed with dust stand out as red filaments detected at longer wavelengths of infrared light seen by Spitzer. The "egg" of the pair, NGC 2937, by contrast, is nearly featureless. The distinctly different greenish glow of starlight tells the story of a population of much older stars. The absence of glowing red dust features informs us that it has long since lost its reservoir of gas and dust from which new stars can form. While this galaxy is certainly reacting to the presence of its neighbor, its smooth distribution of stars obscures any obvious distortions of its shape. Eventually these two galaxies will merge to form a single object, with their two populations of stars, gas and dust intermingling. This kind of merger was likely a significant step in the history of most large galaxies we see around us in the nearby universe, including our own Milky Way. At a distance of about 352 million light-years, these two galaxies are roughly 10 times farther away than our nearest major galactic neighbor, the Andromeda galaxy. The blue streak at the top of the image is an unrelated background galaxy that is farther away than Arp 142. Combining light from across the visible and infrared spectrums helps astronomers piece together the complex story of the life cycles of galaxies. While this image required data from both the Spitzer and Hubble telescopes to cover this range of light, NASA's upcoming James Webb Space Telescope will be able to see all of these wavelengths of light, and with dramatically better clarity.

This illustration depicts the strange case of the backwards hotspot researchers have found on the hot exoplanet known as CoRoT-2b. NASA's Spitzer Space Telescope has played an instrumental role in mapping out the temperature distributions of a handful of closely-orbiting worlds knows as hot Jupiters. In most cases, the hottest spot on the planet is found to be either at the point directly facing the near-by star or offset eastward by strong winds. In the mysterious case of exoplanet CoRoT-2b, however, the hot spot turns out to lie in the opposite direction: west of center. There are currently a number of ideas that could explain this strangely offset hot spot, including mechanisms that make the winds blow opposite the way they do in other known planets of this type.

WASP-18b is an exoplanet located 325 light-years from Earth. The planet's mass is 10 times that of Jupiter, and it orbits its star once every 23 hours. A 2017 study found that this planet has a stratosphere that's loaded with carbon dioxide, but has no signs of water. A stratosphere is a layer of atmosphere in which temperature increases with higher altitudes. The study used NASA's Spitzer and Hubble space telescopes.

The super-Earth exoplanet 55 Cancri e, depicted with its star in this artist's concept, likely has an atmosphere thicker than Earth's, with ingredients that could be similar to those of Earth's atmosphere, according to a 2017 study using data from NASA's Spitzer Space Telescope. Scientists say the planet may be entirely covered in lava. The planet is so close to its star that one face of the planet consistently faces the star, resulting in a dayside and a nightside. NASA's Jet Propulsion Laboratory, Pasadena, California, manages the Spitzer Space Telescope mission for NASA's Science Mission Directorate, Washington. Science operations are conducted at the Spitzer Science Center at Caltech in Pasadena, California. Spacecraft operations are based at Lockheed Martin Space Systems Company, Littleton, Colorado. Data are archived at the Infrared Science Archive housed at IPAC at Caltech. Caltech manages JPL for NASA.

This artist's concept shows an exoplanet and debris disk orbiting a polluted white dwarf. White dwarfs are dim, dense remnants of stars similar to the Sun that have exhausted their nuclear fuel and blown off their outer layers. By "pollution," astronomers mean heavy elements invading the photospheres -- the outer atmospheres -- of these stars. The leading explanation is that exoplanets could push small rocky bodies toward the star, whose powerful gravity would pulverize them into dust. That dust, containing heavy elements from the torn-apart body, would then fall on the star. NASA's Spitzer Space Telescope has been instrumental in expanding the field of polluted white dwarfs orbited by hot, dusty disks. Since launch in 2004, Spitzer has confirmed about 40 of these special stars. Another space telescope, NASA's Wide-field Infrared Survey Explorer (WISE), also detected a handful, bringing the total up to about four dozen known today. Because these objects are so faint, infrared light is crucial to identifying them.

Over their individual histories, the vast majority of galaxies are thought to produce stars at relatively slow rates. This slow-and-steady pace has continually added to the overall population of stars in galaxies and, by extension, the broader universe, as illustrated along the horizontal/x-axis of this diagram. Sometimes, however, galaxies can enter a starburst phase, where they crank out new stars at rates hundreds of times faster than normal, depicted in the vertical/y-axis. Starbursting galaxies have been thought to be a rare occurrence. But a new study using NASA's Spitzer Space Telescope has revealed that in the epoch 1.5 billion years after the Big Bang, around 15 percent of galaxies were undergoing these bouts of frenzied starmakingfar more than previously evidenced. Given the number of starburst galaxies, the study finds them responsible for producing more than half of the total new stars in the early cosmic era under study. Starburst galaxies therefore likely played a major and underappreciated role in creating our universes stars.

NASAs Spitzer Space Telescope has provisionally detected the faint afterglow of the explosive merger of two neutron stars in the galaxy NGC 4993. The event, labeled GW170817, was initially detected nearly simultaneously in gravitational waves and gamma rays, but subsequent observations by many dozens of telescopes have monitored its afterglow across the entire spectrum of light. Spitzers observation on September 29th comes late in the game, just over 6 weeks after the event was first seen, but if this weak detection is verified, it will play an important role in helping astronomers understand how many of the heaviest elements in the periodic table are created in explosive neutron star mergers. This image shows the residual 4.5 micron data from Spitzer's IRAC instrument after subtracting out the light of the galaxy using an archival image that predates the event. The faint dot framed by the markers may be one of the last detections made in infrared light of this event.

NASAs Spitzer Space Telescope has provisionally detected the faint afterglow of the explosive merger of two neutron stars in the galaxy NGC 4993. The event, labeled GW170817, was initially detected nearly simultaneously in gravitational waves and gamma rays, but subsequent observations by many dozens of telescopes have monitored its afterglow across the entire spectrum of light. Spitzers observation on September 29th comes late in the game, just over 6 weeks after the event was first seen, but if this weak detection is verified, it will play an important role in helping astronomers understand how many of the heaviest elements in the periodic table are created in explosive neutron star mergers. The left panel is a color composite of the 3.6 and 4.5 micron channels of the Spitzer IRAC instrument, rendered in cyan and red. The center panel is a median-filtered color composite showing a faint red dot at the known location of the event. The right panel shows the residual 4.5 micron data after subtracting out the light of the galaxy using an archival image that predates the event.