User:Marshallsumter/Radiation astronomy2/Radios

This image has the radio image of Greg Taylor, NRAO, overlain on the X-ray image from Chandra. The radio source Hydra A originates in a galaxy near the center of the cluster. Optical observations show a few hundred galaxies in the cluster. Credit: NASA/CXC/SAO; Radio: NRAO.{{free media}}

Radio astronomy studies radiation with wavelengths greater than approximately one millimeter. Radio astronomy is different from most other forms of observational astronomy in that the observed radio waves can be treated as waves rather than as discrete photons. Hence, it is relatively easier to measure both the amplitude and phase of radio waves, whereas this is not as easily done at shorter wavelengths.

Although some radio waves are produced by astronomical objects in the form of thermal emission, most of the radio emission that is observed from Earth is seen in the form of synchrotron radiation, which is produced when electrons oscillate around magnetic fields. Additionally, a number of spectral lines produced by interstellar gas, notably the hydrogen spectral line at 21 cm, are observable at radio wavelengths.

Astronomy

Main resource: Radiation astronomy/Astronomy

Sunset over four telescopes of the Mauna Kea Observatories is pictured, from left to right: the Subaru Telescope, the twin Keck I and II telescopes, and the NASA Infrared Telescope Facility. Credit: Alan L.{{free media}}

With its high altitude, dry environment, and stable airflow, Mauna Kea's summit is one of the best sites in the world for astronomical observation, and one of the most controversial. Since the creation of an access road in 1964, thirteen telescopes funded by eleven countries have been constructed at the summit. The Mauna Kea Observatories are used for scientific research across the electromagnetic spectrum from visible light to radio, and comprise one of the world's largest facilities of their type. Their construction on a "sacred landscape", replete with endangered species and ongoing cultural practices, continues to be a topic of debate and protest. Studies are underway to determine their effect on the summit ecology, particularly on the rare Wēkiu bug. It was designated a National Natural Landmark in 1972.

There are nine telescopes working in the visible and infrared spectrum, three in the submillimeter spectrum, and one in the radio spectrum, with mirrors or dishes ranging from 0.9 m (3.0 ft) to 25 m (82 ft).

Telescope domes have a slit or other opening in the roof that can be opened during observing, and closed when the telescope is not in use. In most cases, the entire upper portion of the telescope dome can be rotated to allow the instrument to observe different sections of the night sky. Radio telescopes usually do not have domes.

Radios

File:RadioNightSky.jpg

This composite picture shows the radio sky above an old optical photograph of the NRAO site in Green Bank, WV. Credit: NRAO.{{fairuse}}

"This composite picture [at right] shows the radio sky above an old optical photograph of the NRAO site in Green Bank, WV. The former 300 Foot Telescope (the large dish standing between the three 85 foot interferometer telescopes on the left and the 140 Foot Telescope on the right) made this 4.85 GHz radio image, which is about 45 degrees across. Increasing radio brightness is indicated by lighter shades to indicate how the sky would appear to someone with a "radio eye" 300 feet in diameter."

"The visible and radio skies reveal quite different "parallel universes" sharing the same space. Most bright stars are undetectable at radio wavelengths, and many strong radio sources are optically faint or invisible. Familiar objects like the Sun and planets can look quite different through the radio and optical windows. The extended radio sources spread along a band from the lower left to the upper right in this picture lie in the outer Milky Way. The brightest irregularly shaped sources are clouds of hydrogen ionized by luminous young stars. Such stars quickly exhaust their nuclear fuel, collapse, and explode as supernovae, whose remnants appear as faint radio rings. Unlike the nearby (distances < 1000 light years) stars visible to the human eye, almost none of the myriad "radio stars" (unresolved radio sources) scattered across the sky are actually stars. Most are extremely luminous radio galaxies or quasars, and their average distance is over 5,000,000,000 light years. Radio waves travel at the speed of light, so distant extragalactic sources appear today as they actually were billions of years ago. Radio galaxies and quasars are beacons carrying information about galaxies and their environs, everywhere in the observable universe and ever since the first galaxies were formed."

Radio waves are a type of electromagnetic radiation with wavelengths in the electromagnetic spectrum longer than infrared light. Radio waves have frequencies from 300 Gigahertz (GHz) to as low as 3 Kilohertz (kHz), and corresponding wavelengths from 1 millimeter to 100 kilometers.

Theoretical radio astronomy

At approximately 2 degrees on a side (the full moon is about 1/2 degree across), or about 1000 light years at the distance of the center of the Milky Way, the image is shown in false color with brightness indicating areas of intense radio emission, and surrounding dark areas indicating less intense radio emission. Credit: N. E. Kassim, D. S. Briggs, T. J. W. Lazio, T. N. LaRosa, J. Imamura (NRL/RSD).{{free media}}

Dark lines near the center of the image are artifacts of the image processing. The concentration of radio sources along a diagonal line through the image reveals the disk-like shape of the Milky Way viewed edge-on.

Def. the "branch of astronomy which utilizes radio waves through the use of radio telescopes to study celestial bodies and occurrences" is called radio astronomy, or radioastronomy.

Entities

Main resource: Radiation astronomy/Entities

Nikola Tesla, the father of radio and radio astronomy; is pictured holding a gas-filled phosphor-coated light bulb which he developed in the 1890s, and was illuminated without wires by an electromagnetic field from a "Tesla Coil". Credit: Unknown author.{{free media}}

"The supersensitive receiver invented by Tesla to track electrical storms also was the first manmade device to detect radio signals coming from the cosmos, over thirty years before a Bell Laboratories researcher, Karl Jansky, picked up similar signals and came to be recognized as the "father of radio astronomy"."

Radars

Main resources: Radiation astronomy/Radars and Radar astronomy

This image shows the early planetary radar at Pluton, USSR, 1960. Credit: Rumlin.{{free media}}

Radar astronomy is a technique of observing nearby astronomical objects by reflecting microwaves off target objects and analyzing the echoes. This research has been conducted for six decades. Radar astronomy differs from radio astronomy in that the latter is a passive observation and the former an active one. Radar systems have been used for a wide range of solar system studies. The radar transmission may either be pulsed or continuous.

The extremely accurate astrometry provided by radar is critical in long-term predictions of asteroid-Earth impacts, as illustrated by the object 99942 Apophis. In particular, optical observations measure very accurately where an object appears on the sky, but cannot measure the distance accurately at all. Radar, on the other hand, directly measures the distance to the object (and how fast it is changing). The combination of optical and radar observations normally allows the prediction of orbits at least decades, and sometimes centuries, into the future.

The maximum range of astronomy by radar is very limited, and is confined to the solar system. This is because the signal strength drops off very steeply with distance to the target, the small fraction of incident flux that is reflected by the target, and the limited strength of transmitters. It is also necessary to have a relatively good ephemeris of the target before observing it.

At right is an image of the Pluton radar complex used for radar astronomy since 1960.

Radio occultations

The diagram Illustrates radio occultation and refraction. Credit: MPRennie.{{free media}}

Radio occultation (RO) is a remote sensing technique used for measuring the physical properties of a planetary atmosphere. It relies on the detection of a change in a radio signal as it passes through the planet's atmosphere i.e. as it is occulted by the atmosphere. When electromagnetic radiation passes through the atmosphere it is refracted. The magnitude of the refraction depends on the gradient of refractivity normal to the path, which in turn depends on the gradients of density and the water vapour. The effect is most pronounced when the radiation traverses a long atmospheric limb path. At radio frequencies the amount of bending cannot be measured directly, instead the bending can be calculated using the Doppler shift of the signal given the geometry of the emitter and receiver. The amount of bending can be related to the refractive index by using an Abel transform on the formula relating bending angle to refractivity. In the case of the neutral atmosphere (below the ionosphere) information on the atmosphere's temperature, pressure and water vapour can be derived, hence radio occultation data has applications in meteorology.

"As a spacecraft travels through the solar system, a targeted radio signal sent back to Earth can be aimed through the ionosphere of a nearby planet. Plasma in the ionosphere causes small but detectable changes in the signal that allow scientists to learn about the upper atmosphere."

Microwaves

Main resources: Radiation astronomy/Microwaves and Microwave astronomy

This sample radio receiver component was constructed at the Rutherford Appleton Laboratory, Chilton in Wiltshire. Credit: Science Museum London / Science and Society Picture Library.{{free media}}

Microwaves, a subset of radio waves, have wavelengths ranging from as long as one meter to as short as one millimeter, or equivalently, with frequencies between 300 MHz (0.3 GHz) and 300 GHz. This broad definition includes both UHF and EHF (millimeter waves), and various sources use different boundaries. In all cases, microwave includes the entire SHF band (3 to 30 GHz, or 10 to 1 cm) at minimum, with RF engineering often putting the lower boundary at 1 GHz (30 cm), and the upper around 100 GHz (3 mm).

The COBE is launched into Earth orbit on November 18, 1989. The WMAP is launched on June 30, 2001, into orbit at the Lagrange 2 location. Both satellites have aboard detectors designed to perform microwave astronomy, as these are limited to only the microwave band.

The Gravity Recovery and Climate Experiment (GRACE) mission uses a microwave ranging system to accurately measure changes in the speed and distance between two identical spacecraft flying in a polar orbit about 220 kilometers (140 mi) apart, 500 kilometers (310 mi) above Earth. The ranging system is sensitive enough to detect separation changes as small as 10 micrometres (approximately one-tenth the width of a human hair) over a distance of 220 kilometers.

As the twin GRACE satellites circle the globe 15 times a day, they sense minute variations in Earth's gravitational pull. When the first satellite passes over a region of slightly stronger gravity, a gravity anomaly, it is pulled slightly ahead of the trailing satellite. This causes the distance between the satellites to increase. The first spacecraft then passes the anomaly, and slows down again; meanwhile the following spacecraft accelerates, then decelerates over the same point.

By measuring the constantly changing distance between the two satellites and combining that data with precise positioning measurements from Global Positioning System (GPS) instruments, a detailed map of Earth's gravity [can be constructed].

Continua

Main resource: Radiation astronomy/Continua

This is a Hubble Space Telescope image of the Crab Nebula showing the diffuse blue region. Credit: NASA, ESA, J. Hester and A. Loll (Arizona State University).{{free media}}

Like X-rays, the gamma-ray continuum can arise from bremsstrahlung, black-body radiation, synchrotron radiation, or what is called inverse Compton scattering of lower-energy photons by relativistic electrons, knock-on collisions of fast protons with atomic electrons, and atomic recombination, with or without additional electron transitions.

The radio continuum from an active galactic nucleus is always due to a jet. It shows a spectrum characteristic of synchrotron radiation.

"[T]he diffuse blue region is predominantly produced by synchrotron radiation, which is radiation given off by the curving motion of electrons in a magnetic field. The radiation corresponded to electrons moving at speeds up to half the speed of light."

A synchrotron model for the continuum spectrum of the Crab Nebula fits the radiation given off.

In the Crab Nebula X-ray spectrum there are three features that differ greatly from Scorpius X-1: its spectrum is much harder, its source diameter is in light-years (ly)s, not astronomical units (AU), and its radio and optical synchrotron emission are strong. Its overall X-ray luminosity rivals the optical emission and could be that of a nonthermal plasma. However, the Crab Nebula appears as an X-ray source that is a central freely expanding ball of dilute plasma, where the energy content is 100 times the total energy content of the large visible and radio portion, obtained from the unknown source.

Backgrounds

Main resource: Radiation astronomy/Backgrounds

The graph is of the cosmic microwave background spectrum measured by the FIRAS instrument on the COBE satellite, the most-precisely measured black body spectrum in nature, the error bars are too small to be seen even in enlarged image, and it is impossible to distinguish the data from the theoretical curve. Credit: Quantum Doughnut.{{free media}}

Cosmic microwave background (CMB) radiation (also CMBR, CBR, MBR, and relic radiation) is thermal radiation filling the observable universe almost uniformly.

Precise measurements of cosmic background radiation are critical to cosmology, since any proposed model of the universe must explain this radiation. The CMBR has a thermal black body spectrum at a temperature of 2.725 K, which peaks at the microwave range frequency of 160.2 GHz, corresponding to a 1.873 mm wavelength. This holds if measured per unit frequency, as in Planck's law. If measured instead per unit wavelength, using Wien's law, the peak is at 1.06 mm corresponding to a frequency of 283 GHz.

"The differential 850-μm counts are well described by the function

$n(S)=N_{0}/(a+S^{3.2}),$

where $S$ is the flux in mJy, $N_{0}$ = 3.0 × 10⁴ per square degree per mJy, and $a$ = 0.4 − 1.0 is chosen to match the 850-μm extragalactic background light."

Protons

Main resources: Radiation astronomy/Protons and Proton astronomy

This plot shows how fluxes of charged particles increased over a few minutes around the satellite on January 19, 2017. Credit: NOAA/NASA.{{free media}}

The new Space Environment In‐Situ Suite (SEISS) instrument onboard NOAA’s GOES-16 is working and successfully sending data back to Earth. This plot shows how fluxes of charged particles increased over a few minutes around the satellite on January 19, 2017. These particles are often associated with brilliant displays of aurora borealis at northern latitudes and australis at southern latitudes; however, they can pose a radiation hazard to astronauts and other satellites, and threaten radio communications. Information from SEISS will help NOAA's Space Weather Prediction Center provide early warning of these high flux events, so astronauts, satellite operators and others can take action to protect lives and equipment.

This SEISS data shows injections of protons and electrons observed by the Magnetospheric Particle Sensors MPS-HI and Solar and Galactic Proton Sensor (SGPS) on January 19, 2017. MPS-HI and SGPS are two of the individual sensor units on SEISS. The fluxes shown are from the MPS-HI telescopes that look radially outward from the Earth, and from the lowest-energy channel observed by the eastward-looking SGPS.

"Radio observations at 210 GHz taken by the Bernese Multibeam Radiometer for KOSMA (BEMRAK) [...] at submillimeter wavelengths [show an impulsive component that] starts simultaneously with high-energy (>200 MeV nucleon⁻¹) proton acceleration and the production of pions. The derived radio source size is compact (≤10"), and the emission is cospatial with the location of precipitating flare-accelerated >30 MeV protons as seen in γ-ray imaging."

Electrons

Main resources: Radiation astronomy/Electrons and Electron astronomy

This image shows the inner part of our galaxy, which hosts the largest and densest collection of giant molecular clouds in the Milky Way. Credit: NASA Goddard Photo and Video.{{free media}}

This image shows the inner part of our galaxy, which hosts the largest and densest collection of giant molecular clouds in the Milky Way. These vast, cool clouds contain enough dense gas and dust to form tens of millions of stars like the Sun.

The composite image includes data from the Goddard-IRAM Superconducting 2-Millimeter Observer, ESA’s Herschel satellite, the James Clerk Maxwell Telescope near the summit of Maunakea, Hawaii, and radio observations from the National Science Foundation’s Karl G. Jansky Very Large Array, located near Socorro, New Mexico. The resulting image essentially color codes different emission mechanisms.

Blue and cyan features reveal cold dust in molecular clouds where star formation is still in its infancy. Yellow features, such as the Arches filaments and the Sagittarius B1 molecular cloud, reveal the presence of ionized gas and show well-developed star factories; this light comes from electrons that are slowed but not captured by gas ions. Red and orange regions show areas where high-speed electrons spiral in a magnetic field, such as in the prominent Radio Arc and Sagittarius A, the bright source at the galaxy’s center that hosts its supermassive black hole.

"Radio observations at 210 GHz taken by the Bernese Multibeam Radiometer for KOSMA (BEMRAK) [of] high-energy particle acceleration during the energetic solar flare of 2003 October 28 [...] at submillimeter wavelengths [reveal] a gradual, long-lasting (>30 minutes) component with large apparent source sizes (~60"). Its spectrum below ~200 GHz is consistent with synchrotron emission from flare-accelerated electrons producing hard X-ray and γ-ray bremsstrahlung assuming a magnetic field strength of ≥200 G in the radio source and a confinement time of the radio-emitting electrons in the source of less than 30 s. [There is a] close correlation in time and space of radio emission with the production of pions".

Gamma rays

Main resources: Radiation astronomy/Gamma rays and Gamma-ray astronomy

This illustration shows the set-up for the most common type of gamma ray burst. Credit: NASA/Goddard Space Flight Center/ICRAR.{{free media}}

Gamma ray bursts are cosmic explosions, with radiation up to a trillion times the energy of visible light. This illustration shows the set-up for the most common type of gamma ray burst. The core of a massive star (left) has collapsed and formed a black hole. This “engine” drives a jet of particles that moves through the collapsing star and out into space at nearly the speed of light. The prompt emission, which typically lasts a minute or less, may arise from the jet’s interaction with gas near the newborn black hole and from collisions between shells of fast-moving gas within the jet (internal shock waves). The afterglow emission occurs as the leading edge of the jet sweeps up its surroundings (creating an external shock wave) and emits radiation across the spectrum for some time — months to years, in the case of radio and visible light, and many hours at the highest gamma-ray energies yet observed. These far exceed 100 billion electron volts (GeV) for two recent GRBs.

A "fading counterpart to GRB 980329 at 850 μm [has been found]. [...] the sub-millimeter flux was relatively bright. [...] The radio through sub-millimeter spectrum of GRB 980329 is well fit by a power law with index α = +0.9. However, we cannot exclude a ν^1/3 power law attenuated by synchrotron self-absorption."

Submillimeter observations

1. determine "the breaks in the radio to sub-millimeter to optical spectrum so that the spectral shape can be compared to the synchrotron models"
2. determine "the evolution of the sub-millimeter flux" and
3. look "for underlying quiescent sources that may be dusty star-forming galaxies at high redshifts."

X-rays

Main resources: Radiation astronomy/X-rays and X-ray astronomy

Pictor A is in x-rays and radio bands. Credit: ATCA, Chandra, NASA, ESA, Australian University.{{free media}}

This is a composite image of the northern part of the galaxy cluster Abell 1758 showing the effects of a collision between two smaller galaxy clusters. Credit: Joseph DePasquale.{{free media}}

In the image on the left, Chandra X-ray data (blue) reveal hot gas in the cluster and data from the Giant Metrewave Radio Telescope (GMRT) in India (pink) shows huge "halos" generated by ultra-relativistic particles and magnetic fields over vast scales. Optical data from the Digitized Sky Survey are colored gold. A study of this galaxy cluster and 31 others with Chandra and the GMRT shows that huge radio halos are generated during collisions between galaxy clusters.

"Inside [the] X-ray error box [for GRB 980329], a variable radio source VLA J070238.0+385044 was found that was similar to GRB 970508 (Taylor et al. 1998a, 1998b)."

Ultraviolets

Main resource: Radiation astronomy/Ultraviolets

This image shows two companion galaxies, NGC 4625 (top) and NGC 4618 (bottom), and their surrounding cocoons of cool hydrogen gas (purple). Credit: NASA/JPL-Caltech/Carnegie Observatories/WSRT.{{free media}}

This image shows two companion galaxies, NGC 4625 (top) and NGC 4618 (bottom), and their surrounding cocoons of cool hydrogen gas (purple). The huge set of spiral arms on NGC 4625 (blue) was discovered by the ultraviolet eyes of NASA's Galaxy Evolution Explorer. Though these arms are nearly invisible when viewed in optical light, they glow brightly in ultraviolet. This is because they are bustling with hot, newborn stars that radiate primarily ultraviolet light.

The vibrant spiral arms are also quite lengthy, stretching out to a distance four times the size of the galaxy's core. They are part of the largest ultraviolet galactic disk discovered so far.

Astronomers do not know why NGC 4625 grew arms while NGC 4618 did not. The purple nebulosity shown here illustrates that hydrogen gas - an ingredient of star formation - is diffusely distributed around both galaxies. This means that other unknown factors led to the development of the arms of NGC 4625.

Located 31 million light-years away in the constellation Canes Venatici, NGC 4625 is the closest galaxy ever seen with such a young halo of arms. It is slightly smaller than our Milky Way, both in size and mass. However, the fact that this galaxy's disk is forming stars very actively suggests that it might evolve into a more massive and mature galaxy resembling our own.

The image is composed of ultraviolet, visible-light and radio data, from the Galaxy Evolution Explorer, the California Institute of Technology's Digitized Sky Survey, and the Westerbork Synthesis Radio Telescope, the Netherlands, respectively. Near-ultraviolet light is colored green; far-ultraviolet light is colored blue; and optical light is colored red. Radio emissions are colored purple.

Opticals

Main resources: Radiation astronomy/Opticals and Optical astronomy

The scale of Cen A's giant radio-emitting lobes stretch more than 1.4 million light-years. Credit: NASA/DOE/Fermi LAT Collaboration, Capella Observatory, and Ilana Feain, Tim Cornwell, and Ron Ekers (CSIRO/ATNF), R. Morganti (ASTRON), and N. Junkes (MPIfR).{{free media}}

Image of Odd radio circle ORC J2103-6200 (green) from 2022 by the MeerKAT telescope superimposed on an optical image from the Dark Energy Survey. Credit: Jayanne English.{{free media}}

It takes the addition of radio data (orange) to fully appreciate the scale of Cen A's giant radio-emitting lobes, which stretch more than 1.4 million light-years. Gamma-rays from Fermi's Large Area Telescope (purple) and an image of the galaxy in visible light are also included in this composite.

The image on the left is of an Odd radio circle ORC J2103-6200 by the MeerKAT telescope superimposed on an optical image from the Dark Energy Survey.

An Odd Radio Circle (ORC) is a very large, (over 50 thousand times the diameter of our very own Milky Way ~ 3 Million Light-years) unexplained astronomical object that, at radio wavelengths, is highly circular and brighter along its edges. As of 27 April 2021, there have been five such objects (and possibly six more) observed. The observed ORCs are bright at radio wavelengths, but are not visible at visible, infrared or X-ray wavelengths. This is due to the physical process producing this radiation, which is thought to be synchrotron radiation. Three of the ORCs contain optical galaxies in their centers, suggesting that the galaxies might have formed these objects.

By optical astronomy, optical observations measure very accurately where an object appears on the sky, but cannot measure the distance accurately at all.

Visuals

Main resource: Radiation astronomy/Visuals

The images have information about how the ring structure differs both with distance from the planet and with position around the equatorial circle. Credit: NASA/JPL/Space Science Institute.{{free media}}

Cassini instruments provide complementary information about the structure of Saturn's rings. Narrow and wide angle cameras provide images in the visible region of the electromagnetic spectrum much like a digital camera does. The images have information about how the ring structure differs both with distance from the planet and with position around the equatorial circle. However, resolution is usually limited to few kilometers at best.

Radio and stellar occultations of the rings also provide important information about ring structure, but only along a one-dimensional track through the rings. The radial resolution can be as fine as 50 meters (164 feet). An "image" is then constructed by assuming circular symmetry over the ring region of interest. Color is usually added to encode other information related to the observed structure.

This image compares structure of Saturn's rings observed by these two approaches. The upper half is a natural color mosaic of images of the illuminated side of the rings by the Cassini narrow-angle camera (see PIA06175). The bottom simulated image is constructed from a radio occultation observation conducted on May 3, 2005. For another view created using this process, see PIA07872. Color in the lower image is used to represent information about ring particle sizes.

Three simultaneous radio signals of 0.94, 3.6, and 13 centimeter wavelength (Ka-, X-, and S-bands) were sent from Cassini through the rings to Earth. The observed change of each signal as Cassini moved behind the rings provided a profile of the distribution of ring material as a function of distance from Saturn, or an optical depth profile. This simulated image was constructed from the measured optical depth profiles.

Shades of purple, primarily over most of the middle ring, the B ring, and the inner portion of the outer ring, the A ring, indicate regions where there is a lack of particles less than 5 centimeters (about 2 inches) in diameter. Green and blue shades indicate regions where there are particles of sizes smaller than 5 centimeters (2 inches) and 1 centimeter (less than one third of an inch), respectively, primarily in the outer A ring and within most of the inner ring, the C ring. The saturated broad white band near the middle of the B ring is the densest region of the rings, over which two of the three radio signals were blocked at 10-kilometer (6-mile) resolution, preventing accurate color representation. From other evidence in the radio observations, all ring regions appear to be populated by a broad range particle size distribution that extends to boulder sizes (several to many meters across).

Reds

Main resource: Radiation astronomy/Reds

This image shows a composite view of the giant elliptical galaxy NGC 5044. Credit: NASA Chandra/Digitised Sky Survey/Southern Observatory for Astrophysical Research/Very Large Array.{{free media}}

The stellar component, as observed at optical wavelengths, is shown in white at the centre of the image. The other stars scattered around the image are foreground stars from our own Galaxy. The galaxy is embedded in a hot atmosphere of ionised hydrogen gas, which is shown in blue. With temperatures up to tens of millions of K, the hot gas shines brightly in X-rays and was observed using NASA's Chandra X-ray Observatory. Observations show that some of the hot gas cools down and flows towards the centre of the galaxy. There, the cold gas may condense and form stars, unless it is reheated or expelled from the galaxy by other agents. The filamentary network shown in red is warm hydrogen gas, as observed in the H-alpha emission line at a rest wavelength of 656.28 nm with the Southern Observatory for Astrophysical Research (SOAR) telescope in Chile. When observed in radio wavelengths, this galaxy appears only as the weak source shown in violet at the centre of the image, which belies the moderately active black hole sitting at the centre of the galaxy. The radio observations were performed with NRAO's Very Large Array (VLA). A team of astronomers has observed NGC 5044 and other nearby giant elliptical galaxies using ESA's Herschel Space Observatory, to try to figure out why galaxies of this type do not form stars. Spectroscopic observations obtained with Herschel showed that, contrary to previous belief, NGC 5044 contains plenty of cold gas – the raw material to form stars. The same holds true for most of the giant elliptical galaxies that the team observed. A multi-wavelength study suggests that, while hot gas cools down in these galaxies, stars do not form because of feedback from the central supermassive black hole, which stirs up the gas preventing it from turning into stars.

Infrareds

Main resources: Radiation astronomy/Infrareds and Infrared astronomy

This technique of creating "multi wavelength" images allows seeing how X-rays fit with data of other types of light, such as optical, radio, and infrared. Credit: NASA/STScI.{{free media}}

"It was not until after the variable radio source was discovered that infrared observations [of GRB 980329] found a fading counterpart (Klose et al. 1998; Palazzi et al. 1998; Metzger 1998): this indicated that the optical extinction was significant for this source (Larkin et al. 1998; Taylor et al. 1998b), and/or the redshift was large (Fruchter 1999)."

Submillimeters

Main resources: Radiation astronomy/Submillimeters and Submillimeter astronomy

File:Whirlpool M51-pr.jpg

This is a composite image of the Whirlpool Galaxy (also known as M51). Credit: Joint Astronomy Centre, University of British Columbia and NASA/HST (STScI).{{fairuse}}

The image at right is a "composite image of the Whirlpool Galaxy (also known as M51). The green image is from the Hubble Space Telescope and shows the optical wavelength. The submillimetre light detected by SCUBA-2 is shown in red (850 microns) and blue (450 microns). The Whirlpool Galaxy lies at an estimated distance of 31 million light years from Earth in the constellation Canes Venatici."

Hydrogens

Main resource: Chemicals/Hydrogens

The hydrogen line, 21 centimeter line or HI line refers to the electromagnetic radiation spectral line that is created by a change in the energy state of neutral hydrogen atoms. This electromagnetic radiation is at the precise frequency of 1420.40575177 [megahertz] MHz, which is equivalent to the vacuum wavelength of 21.10611405413 cm in free space. This wavelength or frequency falls within the microwave radio region of the electromagnetic spectrum, and it is observed frequently in radio astronomy, since those radio waves can penetrate the large clouds of interstellar cosmic dust that are opaque to visible light.

Sun

Main resources: Stars/Sun and Sun (star)

The Sun as seen in radio waves from 17 GHz down to 80 MHz. Credit: Patrick McCauley.{{free media}}

One composite is graphed of the last 30 years of solar variability. Credit: Robert A. Rohde.{{free media}}

From left to right in the right hand image, the observations were recorded by the Nobeyama Radioheliograph (NoRH), Very Large Array (VLA), Nancay Radioheliograph (NRH), and Murchison Widefield Array (MWA). The NoRH and MWA images were taken on the same day, and the VLA and NRH are on different days. The NoRH and VLA images are in false color, and the NRH and MWA images are in grayscale. The first two on the left are dominated by gyromagnetic emission from the chromosphere, transition region, and low-corona, while the three images on the right are dominated by thermal bremsstrahlung emission from the corona, with lower frequencies being generated at larger heights above the surface. Solid circles in the right three panels correspond to the size of the Sun seen in visible light.

The parts of the Sun above the photosphere are referred to collectively as the solar atmosphere. They can be viewed with telescopes operating across the electromagnetic spectrum, from radio through visible light to gamma rays, and comprise five principal zones: the temperature minimum, the chromosphere, the transition region, the corona, and the heliosphere.

At right is a radio image of the Sun at 4.6 GHz. "The brightest discrete radio source is the Sun, but it is much less dominant than it is in visible light. The radio sky is always dark, even when the Sun is up, because atmospheric dust doesn't scatter radio waves, whose wavelengths are much longer than the dust particles."

"The quiet Sun at 4.6 GHz imaged by the [Very Large Array] VLA with a resolution of 12 arcsec, or about 8400 km on the surface of the Sun. The brightest features (red) in this false-color image have brightness temperatures ~ 10⁶ K and coincide with sunspots. The green features are cooler and show where the Sun's atmosphere is very dense. At this frequency the radio-emitting surface of the Sun has an average temperature of 3 x 10⁴ K, and the dark blue features are cooler yet. The blue slash crossing the bottom of the disk is a feature called a filament channel, where the Sun's atmosphere is very thin: it marks the boundary of the South Pole of the Sun. The radio Sun is somewhat bigger than the optical Sun: the solar limb (the edge of the disk) in this image is about 20000 km above the optical limb."

Direct measurements of radio emissions from the Sun at 10.7 cm also provide a proxy of solar activity [at second right] that can be measured from the ground since the Earth's atmosphere is transparent at this wavelength.

The general direction of the solar apex is southwest of the star Vega near the constellation of Hercules. There are several coordinates for the solar apex. The visual coordinates (as obtained by visual observation of the apparent motion) [are] right ascension (RA) 18^h 28^m 0^s and declination (dec) of 30° North (in galactic coordinates: 56.24° longitude, 22.54° latitude). The radioastronomical position is RA 18^h 03^m 50.2^s and dec 30° 00′ 16.8″ (galactic coordinates: 58.87° longitude, 17.72° latitude).

Mercury

Main resource: Rocks/Rocky objects/Mercury

This is a radar image of Mercury's north polar region acquired by the Arecibo Observatory in 1991 combined with images from MESSENGER. Credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington/National Astronomy and Ionosphere Center, Arecibo Observatory.{{free media}}

Radar astronomy of Mercury "[i]mproved [the] value for the distance from the earth [included] [r]otational period, libration, [and] surface mapping, [especially] of [the] polar regions.

In "1991, the Arecibo radio telescope in Puerto Rico detected unusually radar-bright patches at Mercury's poles, spots that reflected radio waves in the way one would expect if there were water ice [denoted in the image at right by yellow areas]. Many of these patches corresponded to the location of large impact craters mapped by the Mariner 10 spacecraft in the 1970s."

"Images from the spacecraft's Mercury Dual Imaging System taken in 2011 and earlier this year confirmed that radar-bright features at Mercury's north and south poles are within shadowed regions on Mercury's surface, findings that are consistent with the water-ice hypothesis."

"The neutron data indicate that Mercury's radar-bright polar deposits contain, on average, a hydrogen-rich layer more than tens of centimeters thick beneath a surficial layer 10 to 20 centimeters thick that is less rich in hydrogen".

"The buried layer has a hydrogen content consistent with nearly pure water ice."

"These reflectance anomalies are concentrated on poleward-facing slopes and are spatially collocated with areas of high radar backscatter postulated to be the result of near-surface water ice".

"Correlation of observed reflectance with modeled temperatures indicates that the optically bright regions are consistent with surface water ice."

MESSENGER's Mercury Laser Altimeter (MLA) data "show that the spatial distribution of regions of high radar backscatter is well matched by the predicted distribution of thermally stable water ice".

Venus

Using an imaging radar technique, the Magellan spacecraft was able to lift the veil from the face of Venus and produce this spectacular high resolution image of the planet's surface. Red, in this false-color map, represents mountains, while blue represents valleys. Credit: Magellan Team, JPL, NASA.{{free media}}

This is a false color image of Venus produced from a global radar view of the surface by the Magellan probe while radar imaging between 1990-1994. Credit: NASA.{{free media}}

The first un-ambiguous detection of Venus was made by the Jet Propulsion Laboratory (JPL) on 10 March 1961. A correct measurement of the AU soon followed.

"The advantages of radar in planetary astronomy result from (1) the observer's control of all the attributes of the coherent signal used to illuminate the target, especially the wave form's time/frequency modulation and polarization; (2) the ability of radar to resolve objects spatially via measurements of the distribution of echo power in time delay and Doppler frequency; (3) the pronounced degree to which delay-Doppler measurements constrain orbits and spin vectors; and (4) centimeter-to-meter wavelengths, which easily penetrate optically opaque planetary clouds and cometary comae, permit investigation of near-surface macrostructure and bulk density, and are sensitive to high concentrations of metal or, in certain situations, ice."

When viewed using radio astronomy, the resulting radar image, at left, shows that just beneath the cloud layers is a rocky object.

Earth

Main resource: Rocks/Rocky objects/Earth

This is a shaded relief map of Antarctica developed from RADARSAT Synthetic Aperture Radar data. Credit: U.S. National Oceanic & Atmospheric Administration.{{free media}}

Numerous airborne and spacecraft radars have mapped the entire planet, for various purposes. One example is the Shuttle Radar Topography Mission, which mapped the entire Earth at 30 m resolution.

At right is a shaded relief map of Antarctica developed from RADARSAT Synthetic Aperture Radar data. RADARSAT is a Canadian satellite.

Moon

Mosaic image of the lunar south pole as taken by Clementine: note permanent polar shadow. Credit: NASA/JPL-Caltech.{{free media}}

The Moon's north pole is shown during the summer. Credit: NASA/GSFC/Arizona State University.{{free media}}

File:Nsmoonpole.s.jpeg

This is a radar image of the Moon's south pole made with the Arecibo Planetary Radar. Credit: N. J. Stacy.{{fairuse}}

Goldstone radar image of the craters at the Moon's south pole. Credit: JeanLucMargot.{{free media}}

This image shows the variations in the lunar gravity field as measured by NASA's Gravity Recovery and Interior Laboratory (GRAIL) during the primary mapping mission from March to May 2012. Credit: NASA/JPL-Caltech/MIT/GSFC.{{free media}}

File:Moon at 850 microns.gif

Thermal emission from the Moon is shown at 850 microns. Credit: NRAO.{{fairuse}}

File:Moon at 70 cm radar.jpg

This is an Arecibo/GBT λ = 70 cm bistatic radar image of the lunar north pole. Credit: Arecibo/GBT.{{fairuse}}

"The moon is comparatively close and was detected by radar, soon after the invention of the technique, in 1946. Measurements included surface roughness and later mapping of shadowed regions near the poles.

"Very precise microwave measurements between two spacecraft, named Ebb and Flow, were used to map gravity with high precision and high spatial resolution. The field shown resolves blocks on the surface of about 12 miles (20 kilometres) and measurements are three to five orders of magnitude improved over previous data. Red corresponds to mass excesses and blue corresponds to mass deficiencies. The map shows more small-scale detail on the far side of the moon compared to the nearside because the far side has many more small craters."

"Twin NASA probes orbiting Earth's moon have generated the highest resolution gravity field map of any celestial body. The new map, created by the Gravity Recovery and Interior Laboratory (GRAIL) mission, is allowing scientists to learn about the moon's internal structure and composition in unprecedented detail. Data from the two washing machine-sized spacecraft also will provide a better understanding of how Earth and other rocky planets in the solar system formed and evolved."

"The gravity field map reveals an abundance of features never before seen in detail, such as tectonic structures, volcanic landforms, basin rings, crater central peaks and numerous simple, bowl-shaped craters. Data also show the moon's gravity field is unlike that of any terrestrial planet in our solar system."

""What this map tells us is that more than any other celestial body we know of, the moon wears its gravity field on its sleeve," said GRAIL Principal Investigator Maria Zuber of the Massachusetts Institute of Technology in Cambridge. "When we see a notable change in the gravity field, we can sync up this change with surface topography features such as craters, rilles or mountains.""

"According to Zuber, the moon's gravity field preserves the record of impact bombardment that characterized all terrestrial planetary bodies and reveals evidence for fracturing of the interior extending to the deep crust and possibly the mantle. This impact record is preserved, and now precisely measured, on the moon. The probes revealed the bulk density of the moon's highland crust is substantially lower than generally assumed. This low-bulk crustal density agrees well with data obtained during the final Apollo lunar missions in the early 1970s, indicating that local samples returned by astronauts are indicative of global processes."

""With our new crustal bulk density determination, we find that the average thickness of the moon's crust is between 21 and 27 miles (34 and 43 kilometres), which is about 6 to 12 miles (10 to 20 kilometres) thinner than previously thought," said Mark Wieczorek, GRAIL co-investigator at the Institut de Physique du Globe de Paris. "With this crustal thickness, the bulk composition of the moon is similar to that of Earth. This supports models where the moon is derived from Earth materials that were ejected during a giant impact event early in solar system history.""

"The map was created by the spacecraft transmitting radio signals to define precisely the distance between them as they orbit the moon in formation. As they fly over areas of greater and lesser gravity caused by visible features, such as mountains and craters, and masses hidden beneath the lunar surface, the distance between the two spacecraft will change slightly."

""We used gradients of the gravity field in order to highlight smaller and narrower structures than could be seen in previous datasets," said Jeff Andrews-Hanna, a GRAIL guest scientist with the Colorado School of Mines in Golden. "This data revealed a population of long, linear gravity anomalies, with lengths of hundreds of kilometres, crisscrossing the surface. These linear gravity anomalies indicate the presence of dikes, or long, thin, vertical bodies of solidified magma in the subsurface. The dikes are among the oldest features on the moon, and understanding them will tell us about its early history.""

"Clementine orbited the Moon in 1994 for 71 days, mapping the Moon globally in 11 wavelengths and measuring its topography by laser ranging. [... The] bistatic radar experiment (so-called because the spacecraft transmitted while we listened to the echoes on Earth) found evidence in the dark areas near the south pole of the Moon for material with high circular polarization ratio [CPR]".

"Meanwhile, astronomers on Earth began publishing results questioning the Clementine and Lunar Prospector [1998-2000] results. With the giant Arecibo radiotelescope, radar images were taken from the Earth. They found radar reflections with high CPR lying in both permanent darkness and in sunlit areas. Ice is not stable in sunlight, so they postulated that all high CPR is caused by surface roughness; if any ice is at the lunar poles, it must be in a finely disseminated form, invisible to radar mapping."

The experiment from Clemintine "was bistatic, i.e., the transmitter and receiver were in different places. Bistatic radar has the advantage of observing reflections through the phase angle, the angle between transmitted and received radio rays [...]. This phase dependence is important. It’s similar to the effect one gets from looking at a bicycle reflector at just the right angle: at certain angles, the internal planes in the transparent plastic align and a very bright reflection is seen. Similarly, in both radio and visible wavelengths on the Moon, we see an “opposition surge”, an apparent increase in brightness looking directly down from the sun (zero phase). Clementine orbited the Moon such that we could observe its phase dependence [...] and we specifically looked for this “opposition surge”, called the Coherent Backscatter Opposition Effect (CBOE). CBOE is particularly valuable to identify ice on planetary surfaces."

"Clementine transmitted right circular polarized (RCP) radio and we listened on Earth in both right- and left-circular polarized (LCP) channels. The ratio of power received in these two channels is called the circular polarization ratio (CPR). The dry, equatorial Moon has CPR less than one, but the icy satellites of Jupiter all have CPR greater than one. We know these objects have surfaces of water ice; in this case, the ice acts as a radio-transparent media in which waves penetrate the ice, are scattered and reflected multiple times, and returned such that some of the waves are received in the same polarization sense as they are sent—they have CPR greater than unity"

"The problem with CPR alone is that we can also get high values from very rough surfaces, such as a rough, blocky lava flow, which has angles that form many small corner reflectors. In this case, a radio wave could hit a rock face (changing RCP into LCP) and then bounce over to another rock face (changing the LCP back into RCP) and hence to the receiver [...]. This “double-bounce” effect also creates high CPR in that “same sense” reflections could mimic the enhanced CPR one gets from ice targets."

At lower right is an image using the Goldstone DSS-14 antenna as a transmitter and the DSS-13 as a receiver, a form of radar interferometry. The cross for the south pole in the Arecibo image is in the Shackleton crater of the Goldstone image.

At fourth right is an image of the Moon using its thermal emission at 850 microns.

"The Moon and planets are not detectable by reflected solar radiation at radio wavelengths. However, they all emit thermal radiation, and Jupiter is a strong nonthermal source as well. If the Sun were suddenly switched off, the planets would remain radio sources for a long time, slowly fading as they cooled. At first glance, the λ = 0.85 mm radio image of the Moon [at second right] looks familiar, but there are differences from the visible Moon."

"The darker right edge of the Moon is not being illuminated by the Sun, but it still emits radio waves because it does not cool to absolute zero during the lunar night. A subtler point is that the radio emission is not produced at the visible surface; it emerges from a layer about ten wavelengths thick. As a result, monthly temperature variations of the Moon decrease with increasing wavelength. These wavelength-dependent temperature variations encode information about the conductivity and heat capacity of the rocky and dusty outer layers of the Moon."

"Radar images like the one [at fifth right] were recently used to search for water ice trapped in cold craters near the lunar poles."

The ESA Lunar Lander Mission Lunar Dust Environment and Plasma Package: "Observe radio spectrum (with an additional goal to prepare for future radiation astronomy activities.)"

Interplanetary mediums

Main resource: Interplanetary medium

Interplanetary scintillation refers to random fluctuations in the intensity of radio waves of celestial origin, on the timescale of a few seconds. It is analogous to the twinkling one sees looking at stars in the sky at night, but in the radio part of the electromagnetic spectrum rather than the visible one. Interplanetary scintillation is the result of radio waves traveling through fluctuations in the density of the electron and protons that make up the solar wind.

Scintillation occurs as a result of variations in the refractive index of the medium through which waves are traveling. The solar wind is a plasma, composed primarily of electrons and lone protons, and the variations in the index of refraction are caused by variations in the density of the plasma. Different indices of refraction result in phase changes between waves traveling through different locations, which results in interference. As the waves interfere, both the frequency of the wave and its angular size are broadened, and the intensity varies.

Mars

This image shows a cross-section of a portion of the north polar ice cap of Mars. Credit: NASA.{{free media}}

File:Martian Ionosphere MARSIS release 4A.jpg

This plot, called an ionogram, shows data from sounding Mars' ionosphere with the Mars Advanced Radar for Subsurface and Ionospheric Sounding (MARSIS). Credit: ASI/NASA/ESA/Univ. of Rome/Univ. of Iowa/JPL.{{fairuse}}

This image is a SHARAD subsurface radargram of Mars. Credit: NASA/JPL-Caltech/ASI/University of Rome/Washington Universtiy in St. Louis.{{free media}}

Mapping of surface roughness [has been performed] from Arecibo Observatory. The Mars Express mission carries a ground-penetrating radar.

The image at right "shows a cross-section of a portion of the north polar ice cap of Mars, derived from data acquired by the Mars Reconnaissance Orbiter's Shallow Radar (SHARAD), one of six instruments on the spacecraft. The data depict the region's internal ice structure, with annotations describing different layers. The ice depicted in this graphic is approximately 2 kilometers (1.2 miles) thick and 250 kilometers (155 miles) across. White lines show reflection of the radar signal back to the spacecraft. Each line represents a place where a layer sits on top of another. Scientists study how thick the pancake-like layers are, where they bulge and how they tilt up or down to understand what the surface of the ice sheet was like in the past as each new layer was deposited."

The image at left, "called an ionogram, shows data from sounding Mars' ionosphere with the Mars Advanced Radar for Subsurface and Ionospheric Sounding (MARSIS). The horizontal axis is the frequency of the pulse. The left vertical axis is the time delay after transmitting the pulse, with time increasing downward. The right vertical axis is a conversion of time delay to distance, showing the apparent range to the reflection point. The intensity of the received signal at any given frequency and apparent range is indicated by the color, with dark blue being the least intense and green being the most intense."

"The green echo at an apparent range of about 800 kilometers (497 miles) from 2.5 to 5.5 megahertz is the reflected signal from the surface of Mars. The curved bright green feature with an apparent range varying from about 600 to 750 kilometers (373 to 466 miles) at frequencies from about 0.7 to 1.8 megahertz is the echo from the top side of the ionosphere. A second echo of the ionosphere, at an apparent range of about 100 kilometers (62 miles) is labeled "Oblique ionospheric echo." Such echoes are believed to come from distorted structures in the ionosphere caused by the magnetic fields in the crust of Mars."

"MARSIS is an instrument on the European Space Agency's Mars Express orbiter."

At lower right is a "radargram from the Shallow Subsurface Radar instrument (SHARAD)".

The "Shallow Subsurface Radar instrument (SHARAD) on NASA's Mars Reconnaissance Orbiter [radargram] is shown in the upper-right panel and reveals detailed structure in the polar layered deposits of the south pole of Mars."

"The sounding radar collected the data presented here during orbit 1334 of the mission, on Nov. 8, 2006."

"The horizontal scale in the radargram is distance along the ground track. It can be referenced to the ground track map shown in the lower right. The radar traversed from about 75 to 85 degrees south latitude, or about 590 kilometers (370 miles). The ground track map shows elevation measured by the Mars Orbiter Laser Altimeter on NASA's Mars Global Surveyor orbiter. Green indicates low elevation; reddish-white indicates higher elevation. The traverse proceeds up onto a plateau formed by the layers."

"The vertical scale on the radargram is time delay of the radar signals reflected back to Mars Reconnaissance Orbiter from the surface and subsurface. For reference, using an assumed velocity of the radar waves in the subsurface, time is converted to depth below the surface at one place: about 1,500 meters (5,000 feet) to one of the deeper subsurface reflectors. The color scale varies from black for weak reflections to white for strong reflections."

"The middle panel shows mapping of the major subsurface reflectors, some of which can be traced for a distance of 100 kilometers (60 miles) or more. The layers are not all horizontal and the reflectors are not always parallel to one another. Some of this is due to variations in surface elevation, which produce differing velocity path lengths for different reflector depths. However, some of this behavior is due to spatial variations in the deposition and removal of material in the layered deposits, a result of the recent climate history of Mars."

"The Shallow Subsurface Radar was provided by the Italian Space Agency (ASI). Its operations are led by the University of Rome and its data are analyzed by a joint U.S.-Italian science team."

Asteroids

Main resource: Rocks/Rocky objects/Asteroids

File:2012 LZ1.jpg

This image is of asteroid 2012 LZ1 by the Arecibo Observatory in Puerto Rico using the Arecibo Planetary Radar. Credit: Arecibo Observatory.{{fairuse}}

This is a Goldstone radar image of asteroid 4179 Toustatis. Credit: Steve Ostro, JPL.{{free media}}

The image at the top right is of asteroid 2012 LZ1.

"On Sunday, June 10, a potentially hazardous asteroid thought to have been 500 meters (0.31 miles) wide was discovered by Siding Spring Observatory in New South Wales, Australia. Fortunately for us, asteroid 2012 LZ1 drifted safely by, coming within 14 lunar distances from Earth on Thursday, June 14."

"Asteroid 2012 LZ1 is actually bigger than thought… in fact, it is quite a lot bigger. 2012 LZ1 is one kilometer wide (0.62 miles), double the initial estimate."

Asteroid "2012 LZ1′s surface is really dark, reflecting only 2-4 percent of the light that hits it — this contributed to the underestimated initial optical observations. Looking for an asteroid the shade of charcoal isn’t easy."

“This object turned out to be quite a bit bigger than we expected, which shows how important radar observations can be, because we’re still learning a lot about the population of asteroids”.

“The sensitivity of our radar has permitted us to measure this asteroid’s properties and determine that it will not impact the Earth at least in the next 750 years”.

The extremely accurate astrometry provided by radar is critical in long-term predictions of asteroid-Earth impacts, as illustrated by the object 99942 Apophis.

At right is a Goldstone radar image of the asteroid 4179 Toutatis on November 26, 1996.

The "images were recorded at NASA's Deep Space Network 70-meter and 34-meter radio/radar antennas in Goldstone, CA, and the 305-meter Arecibo Radio Telescope in Puerto Rico."

"It's amazing that the shape of Toutatis can be determined so accurately from ground-based observations".

"This technology will provide us with startling, close-up views of thousands of asteroids that orbit near the Earth."

"We used the computer to mathematically create a three- dimensional model of the surface and rotation of Toutatis".

"It's as though we put a clay model in space and molded it until it matched the appearance of the actual asteroid."

"The video is of particular interest as Toutatis nears Earth and makes its closest approach on Friday, Nov. 29, when it will pass by at a distance of 3.3 million miles (5.3 million kilometers), or about 14 times the distance from the Earth to the Moon. In 2004, Toutatis will pass only four lunar distances from Earth, closer than any known Earth- approaching object expected to pass by in the next 60 years."

"Toutatis poses no significant threat to Earth, at least for a few hundred years".

"The discovery that we live in an asteroid swarm is important for the future of humanity".

"These leftover debris from planetary formation can teach us a good deal about the formation of our Solar System. Asteroids also contain valuable minerals and many are the cheapest possible destinations for space missions."

Jupiter

Main resource: Jupiter

File:Jupiter radio image.jpg

This VLA image of Jupiter doesn't look like a planetary disk at all. Credit: NRAO.{{fairuse}}

In 1955, Bernard Burke and Kenneth Franklin detected bursts of radio signals coming from Jupiter at 22.2 MHz. The period of these bursts matched the rotation of the planet, and they were also able to use this information to refine the rotation rate. Radio bursts from Jupiter were found to come in two forms: long bursts (or L-bursts) lasting up to several seconds, and short bursts (or S-bursts) that had a duration of less than a hundredth of a second.

Forms of decametric radio signals from Jupiter:

• bursts (with a wavelength of tens of meters) vary with the rotation of Jupiter, and are influenced by interaction of Io with Jupiter's magnetic field.
• emission (with wavelengths measured in centimeters) was first observed by Frank Drake and Hein Hvatum in 1959. The origin of this signal was from a torus-shaped belt around Jupiter's equator. This signal is caused by cyclotron radiation from electrons that are accelerated in Jupiter's magnetic field.

Between September and November 23, 1963, Jupiter is detected by radar astronomy.

"The dense atmosphere makes a penetration to a hard surface (if indeed one exists at all) very unlikely. In fact, the JPL results imply a correlation of the echo with Jupiter ... which corresponds to the upper (visible) atmosphere. ... Further observations will be needed to clarify the current uncertainties surrounding radar observations of Jupiter."

"Although in 1963 some claimed to have detected echoes from Jupiter, these were quite weak and have not been verified by later experiments."

"A search for radar echoes from Jupiter at 430 MHz during the oppositions of 1964 and 1965 failed to yield positive results, despite a sensitivity several orders of magnitude better than employed by other groups in earlier (1963) attempts at higher frequencies. ... [I]t might be suspected that meteorological disturbances of a random nature were involved, and that the echoes might be returned only in exceptional circumstances. Further support for this point of view may be gleaned from the fact that JPL found positive results for only 1 (centered at 32° System I longitude) of the 8 longitude regions investigated in 1963 (Goldstein 1964) and, in fact, had no success during their observations in 1964 (see comment by Goldstein following Dyce 1965)."

"This VLA image of Jupiter [at right] doesn't look like a planetary disk at all. Most of the radio emission is synchrotron radiation from electrons in Jupiter's magnetic field."

Saturn

In this simulated image of Saturn's rings, color is used to present information about ring particle sizes in different regions based on the measured attenuations of three radio signals. Credit: NASA / Jet Propulsion Lab.{{free media}}

"Three simultaneous radio signals at wavelengths of 0.94, 3.6, and 13 centimeters (Ka-, X-, and S-bands) were sent from Cassini through the rings to Earth. The observed change of each signal as Cassini moved behind the rings provided a profile of the distribution of ring material and an optical depth profile."

"This simulated image was constructed from the measured optical depth profiles of the Cassini Division and ring A. It depicts the observed structure at about 10 kilometers (6 miles) in resolution. The image shows the same ring A region depicted in a similar image (Multiple Eyes of Cassini), using a different color scheme to enhance the view of a remarkable array of over 40 wavy features called 'density waves' uncovered in the May 3 radio occultation throughout ring A."

"Color is used to represent information about ring particle sizes based on the measured effects of the three radio signals. Shades of red [purple] indicate regions where there is a lack of particles less than 5 centimeters (about 2 inches) in diameter. Green and blue shades indicate regions where there are particles of sizes smaller than 5 centimeters (2 inches) and 1 centimeter (less than one third of an inch), respectively."

"Note the gradual increase in shades of green towards the outer edge of ring A. It indicates gradual increase in the abundance of 5-centimeter (2-inch) and smaller particles. Note also the blue shades in the vicinity of the Keeler gap (the narrow dark band near the edge of ring A). They indicate increased abundance of even smaller particles of diameter less than a centimeter. Frequent collisions between large ring particles in this dynamically active region likely fragment the larger particles into more numerous smaller ones."

Titan

This Cassini false-color mosaic shows all synthetic-aperture radar images to date of Titan's north polar region. Credit: NASA / JPL / USGS.{{free media}}

This is a radar image of the Titan surface taken on July 22, 2006, from the Cassini probe. Credit: NASA/JPL/USGS.{{free media}}

Radar detection of Titan from Arecibo Observatory, [included] mapping of Titan's surface.

"This Cassini false-color mosaic [at right] shows all synthetic-aperture radar images to date of Titan's north polar region. Approximately 60 percent of Titan's north polar region, above 60 degrees north latitude, is now mapped with radar. About 14 percent of the mapped region is covered by what is interpreted as liquid hydrocarbon lakes."

"Features thought to be liquid are shown in blue and black, and the areas likely to be solid surface are tinted brown. The terrain in the upper left of this mosaic is imaged at lower resolution than the remainder of the image".

"Most of the many lakes and seas seen so far are contained in this image, including the largest known body of liquid on Titan. These seas are most likely filled with liquid ethane, methane and dissolved nitrogen."

"Many bays, islands and presumed tributary networks are associated with the seas. The large feature in the upper right center of this image is at least 100,000 square kilometers (40,000 square miles) in area, greater in extent than Lake Superior (82,000 square kilometers or 32,000 square miles), one of Earth's largest lakes. This Titan feature covers a greater fraction of the surface, at least 0.12 percent, than the Black Sea, Earth's largest terrestrial inland sea, at 0.085 percent. Larger seas may exist, as it is probable that some of these bodies are connected, either in areas unmapped by radar or under the surface (see PIA08365)."

"Of the 400 observed lakes and seas, 70 percent of their area is taken up by large "seas" greater than 26,000 square kilometers (10,000 square miles)."

In the second image at right is another radar image of Titan's surface. "The existence of oceans or lakes of liquid methane on Saturn's moon Titan was predicted more than 20 years ago. But with a dense haze preventing a closer look it has not been possible to confirm their presence. Until the Cassini flyby of July 22, 2006, that is."

"Radar imaging data from the flyby, published this week in the journal Nature, provide convincing evidence for large bodies of liquid. This image, used on the journal's cover, gives a taste of what Cassini saw. Intensity in this colorized image is proportional to how much radar brightness is returned, or more specifically, the logarithm of the radar backscatter cross-section. The colors are not a representation of what the human eye would see."

"The lakes, darker than the surrounding terrain, are emphasized here by tinting regions of low backscatter in blue. Radar-brighter regions are shown in tan. The strip of radar imagery is foreshortened to simulate an oblique view of the highest latitude region, seen from a point to its west."

"This radar image was acquired by the Cassini radar instrument in synthetic aperture mode on July 22, 2006. The image is centered near 80 degrees north, 35 degrees west and is about 140 kilometers (84 miles) across. Smallest details in this image are about 500 meters (1,640 feet) across."

"The Permittivity, Waves and Altimetry (PWA) sensor on the Huygens Atmosphere Structure Instrument (HASI) detected an extremely low frequency (ELF) radio wave during the descent. It was oscillating very slowly for a radio wave, just 36 times a second, and increased slightly in frequency as the probe reached lower altitudes."

Pluto

New Horizons has found that Pluto’s atmosphere has an unexpectedly low surface pressure. Credit: NASA/JHUAPL/SwRI.{{free media}}

Observations with the New Horizons’ REX radio experiment, made about one hour after closest approach to Pluto on July 14, reveal that the atmospheric surface pressure is about half the value previously inferred from Earth-based observations.

Pluto’s atmosphere may be changing before our eyes. Measurements with NASA’s New Horizons spacecraft have revealed that Pluto’s atmosphere has an unexpectedly low surface pressure compared to that derived from previous observations. One explanation for the low pressure is that about half of Pluto’s atmosphere may have recently frozen onto the planet’s surface. If confirmed, it could indicate that further decreases in pressure may soon be in store. The pressure measurement is the first ever obtained for the surface of Pluto. It was made by REX, the spacecraft’s radio experiment, about one hour after New Horizons’ closest approach to Pluto on July 14. In a carefully-planned observation that had never before been attempted, two radio dishes on Earth--part of NASA’s Deep Space Network-- beamed radio waves precisely timed to reach Pluto just as New Horizons passed behind the dwarf planet.

The radio waves traveled through Pluto’s atmosphere en route to the spacecraft and were bent, or refracted, by the atmospheric gases. The amount of bending -- which appears as a shift in the frequency of the radio waves -- revealed that the gas pressure at Pluto’s surface was only 1/100-thousandth that of the pressure on the surface of Earth. That’s about half the amount calculated from previous Earth-based observations.

Interstellar medium

Main resource: Interstellar medium

File:HIsky.jpg

Interstellar gas in our Galaxy emits spectral lines as well as continuum noise. Credit: NRAO.{{fairuse}}

Radio astronomy has resulted in the detection of over a hundred interstellar species, including radicals and ions, and organic (i.e. carbon-based) compounds, such as alcohols, acids, aldehydes, and ketones. One of the most abundant interstellar molecules, and among the easiest to detect with radio waves (due to its strong electric dipole moment), is CO (carbon monoxide). In fact, CO is such a common interstellar molecule that it is used to map out molecular regions. The radio observation of perhaps greatest human interest is the claim of interstellar glycine, the simplest amino acid, but with considerable accompanying controversy. One of the reasons why this detection [is] controversial is that although radio (and some other methods like rotational spectroscopy) are good for the identification of simple species with large dipole moments, they are less sensitive to more complex molecules, even something relatively small like amino acids.

"Interstellar gas in our Galaxy [shown at right] emits spectral lines as well as continuum noise. Neutral hydrogen (HI) gas is ubiquitous in the disk. The brightness of the λ ~ 21 cm hyperfine line at ~ 1420.4 MHz is proportional to the column density of HI along the line of sight and is nearly independent of the gas temperature. It is not affected by dust absorption, so we can see the HI throughout our Galaxy and nearby external galaxies."

"Red indicates directions of high HI column density, while blue and black show areas with little hydrogen. The figure is centered on the Galactic center and Galactic longitude increases to the left. Some of the hydrogen loops outline old supernova remnants."

Molecular clouds

The Orion Nebula is the defining Galactic HII region and has been well studied over a wide range of wavelengths. Credit: Debra Shepherd, Ron Maddalena, and Joe McMullin, NRAO/AUI.{{free media}}

The Orion Nebula is the defining Galactic HII region and has been well studied over a wide range of wavelengths. The top left image shows observations made with the Robert C. Byrd Green Bank Telescope (GBT) of extended emission at 3.6 cm wavelength from ionized gas in the Orion Nebula. The brightest feature with a box around it is M42 (NGC 1976), a thin blister of ionized gas on the surface of the OMC-1 molecular cloud. Winds from luminous stars in the Trapezium cluster ablate the surface of the cloud, ejecting cloud material into the diffuse interstellar medium. M43 (NGC 1982) is just above the northeastern rim of M42 (the circular feature above and slightly to the left of the box). The top right image was made with the Very Large Array (VLA) at the same wavelength as the GBT image. A wealth of detail showing the complex inner structure of the ionized gas is visible with the VLA. The bottom image was created by combining the GBT and VLA images to get a better picture of what the center of the nebula looks like. It combines the power of both instruments: the GBT's sensitivity to extended structure and the VLA's ability to see fine detail.

The figure shows the GBT image in the upper left displayed from 0 to 119.4 Jy/beam. The OTF mosaic has an RMS of 10 mJy/beam and a maximum of 119.4 Jy/beam. The dynamic range of the image is 11,900 - the highest dynamic range ever achieved by a single dish telescope. The total flux is 430 Jy. The VLA image (upper right) is displayed on a linear stretch from 0 to 0.83 Jy/beam. The mosaic has an RMS of 6.1 mJy/beam, a maximum of 0.83 Jy/beam, and a minimum of -0.027 Jy/beam. The total flux is 189 Jy -- less than half the total flux measured with the GBT. The combined GBT+VLA image (bottom center) was created using an "image feathering technique in which each image was automatically Fourier transformed to the uv-plane, weighted appropriately, combined, and then Fourier transformed back to the image plane. The resulting image has a peak flux density of 1.82 Jy/beam, an RMS of 10 mJy/beam, and a total flux of 415 Jy.

G0.253+0.016 was probed "with another network of telescopes, the Combined Array for Research in Millimeter-wave Astronomy [CARMA] in California."

"G0.253+0.016, which is about 30 light-years long, defies the conventional wisdom that dense gas glouds should produce lots of stars. ... The cloud is 25 times more dense than the famous Orion Nebula, which is birthing stars at a furious rate. But only a few stars are being born in G0.253+0.016, and they're pretty much all runts."

"It's a very dense cloud and it doesn't form any massive stars, which is very weird".

"CARMA data showed that gas within G0.253+0.016 is zipping around 10 times faster than gas in similar clouds. G0.253+0.016 is on the verge of flying apart, with its gas churning too violently to coalesce into stars. Further, the ... cloud is full of silicon monoxide, a compound typically produced when fast-moving gas smashes into dust particles. The abnormally large amounts of silicon monoxide suggest that G0.253+0.016 may actually consist of two colliding clouds, whose impact is generating powerful shockwaves."

When surveyed at 1.1 mm as part of the Bolocam Galactic Plane Survey, "[t]he only currently known starless [massive proto-cluster] MPC is G0.253+0.016, which lies within the dense central molecular zone and is subject to greater environmental stresses than similar objects in the Galactic plane (Longmore et al. 2012)."

DR21

Hidden behind a shroud of dust in the constellation Cygnus is an exceptionally bright source of radio emission called DR21. Credit: NASA/JPL-Caltech/A. Marston (ESTEC/ESA) & A. Noriega-Crespo (SSC/Caltech).{{free media}}

Hidden behind a shroud of dust in the constellation Cygnus is an exceptionally bright source of radio emission called DR21. Visible light images reveal no trace of what is happening in this region because of heavy dust obscuration. In fact, visible light is attenuated in DR21 by a factor of more than 10,000,000,000,000,000,000,000,000,000, 000,000,000,000 (ten thousand trillion heptillion).

New images from NASA's Spitzer Space Telescope allow us to peek behind the cosmic veil and pinpoint one of the most massive natal stars yet seen in our Milky Way galaxy. The never-before-seen star is 100,000 times as bright as the Sun. Also revealed for the first time is a powerful outflow of hot gas emanating from this star and bursting through a giant molecular cloud.

This image is a large-scale mosaic assembled from individual photographs obtained with the InfraRed Array Camera (IRAC) aboard Spitzer. The image covers an area about two times that of a full moon. The mosaic is a composite of images obtained at mid-infrared wavelengths of 3.6 microns (blue), 4.5 microns (green), 5.8 microns (orange) and 8 microns (red). The brightest infrared in the center corresponds to DR21, which presumably contains a cluster of newly forming stars at a distance of 10,000 light-years.

Protruding out from DR21 toward the bottom left of the image is a gaseous outflow (green), containing both carbon monoxide and molecular hydrogen. Data from the Spitzer spectrograph, which breaks light into its constituent individual wavelengths, indicate the presence of hot steam formed as the outflow heats the surrounding molecular gas. Outflows are physical signatures of processes that create supersonic beams, or jets, of gas. They are usually accompanied by discs of material around the new star, which likely contain the materials from which future planetary systems are formed. Additional newborn stars, depicted in green, can be seen surrounding the DR21 region.

The red filaments stretching across this image denote the presence of polycyclic aromatic hydrocarbons. These organic molecules, comprised of carbon and hydrogen, are excited by surrounding interstellar radiation and become luminescent at wavelengths near 8.0 microns. The complex pattern of filaments is caused by an intricate combination of radiation pressure, gravity and magnetic fields. The result is a tapestry in which winds, outflows and turbulence move and shape the interstellar medium.

In the lower left of the mosaic is a large bubble of gas and dust, which may represent the remnants of a past generation of stars.

Perhaps the most fascinating feature in this image is a long and shadowy linear filament extending towards the 10 o'clock position of DR21. This jet of cold and dense gas, nearly 50 light-years in extent, appears in silhouette against a warmer background. This filament is too long and massive to be a stellar jet and may have formed from a pre-existing molecular cloud core sculpted by DR21's strong winds. Regardless of its true nature, this jet and the numerous other arcs and wisps of cool dust signify the interstellar turbulence normally unseen by the human eye.

Milky Way

Main resource: Milky Way

File:Allsky408.jpg

This all-sky 408 MHz continuum image is shown in Galactic coordinates. Credit: Haslam et al. 1982, A&AS, 47, 1.{{fairuse}}

File:GpaSmall.gif

The whole sky of stars (black and white) is shown with the Galactic Plane. Credit: Glen Langston.{{fairuse}}

"The cosmic static discovered by Karl Jansky is dominated by diffuse emission orginating in and near the disk of our Galaxy. The distribution of 408 MHz continuum emission shown [at right] in Galactic coordinates is expected since we are located in the disk of a galaxy similar to the edge-on galaxy NGC 4565".

"This all-sky 408 MHz continuum image [at right] is shown in Galactic coordinates, with the galactic center in the middle and the galactic disk extending horizontally from it."

Sky Full of Stars with 8.35 GHz Galactic Plane Survey in Color is shown on the left. The Galactic center, Cygnus Region and Rosette Nebula regions are highlighted. Many of the most interesting features in the Radio Sky are invisible in the star map. Radio images of the Galactic center show a line of very bright of star forming regions along the galactic plane. In the outer galaxy few stars are born.

3C 31

A pseudo-colour image is of the large-scale radio structure of the FRI radio galaxy 3C31. Credit: Martin J Hardcastle.{{free media}}

Jets and plumes are labelled.

"In 1974, radio sources were divided into two classes Fanaroff and Riley Class I (FRI), and Class II (FRII).

The distinction was originally made based on the morphology of the large-scale radio emission (the type was determined by the distance between the brightest points in the radio emission): FRI sources were brightest towards the centre, while FRII sources were brightest at the edges.

There is a reasonably sharp divide in luminosity between the two classes: FRIs were low-luminosity, FRIIs were high luminosity.

The morphology turns out to reflect the method of energy transport in the radio source. FRI objects typically have bright jets in the centre, while FRIIs have faint jets but bright hotspots at the ends of the lobes. FRIIs appear to be able to transport energy efficiently to the ends of the lobes, while FRI beams are inefficient in the sense that they radiate a significant amount of their energy away as they travel.

The FRI/FRII division depends on host-galaxy environment in the sense that the FRI/FRII transition appears at higher luminosities in more massive galaxies. FRI jets are known to be decelerating in the regions in which their radio emission is brightest,

3C 98

The pseudo-colour image is of the large-scale radio structure of the FRII radio galaxy 3C98. Credit: Martin J Hardcastle.{{free media}}

Lobes, jet and hotspot are labelled.

The hotspots that are usually seen in FRII sources are interpreted as being the visible manifestations of shocks formed when the fast, and therefore supersonic, jet (the speed of sound cannot exceed c/√3) abruptly terminates at the end of the source, and their spectral energy distributions are consistent with this picture.

3C 123

3C 123 is an elliptical radio galaxy. Credit: Unknown author.{{free media}}

3C 123 is a strong radio source. It is surrounded by three other, even weaker galaxies.

The initial estimation of the Doppler shift (z = 0.637) indicated that it is the furthest-known (then mid-70s) galaxy, located within 8 billion light years, 5 to 10 times the size of our Galaxy, and as a radio source about 4 times stronger than Cygnus A . Subsequent investigations clarified the value of about 0.218, that is, the galaxy is much closer to the Earth and is not as large as previously thought.

3C 236

3C236 galaxy is by Hubble Space Telescope, 10.8″ view. Credit: NASA, ESA.

3C 236 is a Fanaroff–Riley classification Class II (FR II) radio galaxy. It is among the largest known radio galaxies, with the radio structure having a total linear size in excess of 4.5 Mpc (15 million light years). The galaxy features a "double-double" radio morphology consisting of the giant relic 4.5 Mpc source and an inner 2 kpc active galactic nucleus (compact steep spectrum) radio source. A recent starburst episode near the nucleus may be related to the event resulting in re-ignition of active galactic nucleus, radio activity.

3C 326

A big galaxy is stealing gas right off the "back" of its smaller companion in this new image from NASA's Spitzer Space Telescope. Credit: NASA/JPL-Caltech/P. Ogle (Spitzer Science Center/Caltech).{{free media}}

The stolen gas is hot, but it might eventually cool down to make new stars and planets.

The robber galaxy, called 3C 326 North, and its victim, 3C 326 South, are located about a billion light-years away from Earth in the Serpens constellation. They are both called radio galaxies, because the relativistic jets streaming out of their centers give off a great deal of radio waves. Other dots in the picture are foreground stars and background galaxies.

When astronomers first collected data on the 3C 326 galaxies with Spitzer's infrared spectrometer, they were surprised to find that 3C 326 North is loaded with an enormous amount of hot gas, called molecular hydrogen gas, which is fuel for stars and planets. They then studied this archived picture taken with Spitzer's infrared array camera and noticed a tail of stars connecting 3C 326 North to 3C 326 South. This tail revealed that the galactic pair are gravitationally tangled and might eventually merge – and that 3C 326 North must be hoisting gas from its smaller companion.

How is 3C 326 stealing the gas? The answer is gravity. The larger 3C 326 North, which is about the same mass as our Milky Way galaxy, has more gravity so the gas from 3C 326 South falls toward it in the same way that water rolls down hill on Earth. Even in space, it seems the bullies are bigger!

This image shows infrared light of three wavelengths: 8-micron light is red; 4.5 microns is green; 3.6 microns is blue.

3C 405

This galaxy, at a distance of some 700 million light years, contains a giant bubble filled with hot, X-ray emitting gas detected by Chandra (blue). Credit: NASA/STScI.{{free media}}

Radio data from the NSF's Very Large Array (red) reveal "hot spots" about 300,000 light years out from the center of the galaxy where powerful jets emanating from the galaxy's supermassive black hole end. Visible light data (yellow) from both Hubble and the DSS complete this view.

Galaxies

Main resources: Stars/Galaxies and Galaxies

"Over the past 30 years, radioastronomy has revealed a rich variety of molecular species in the interstellar medium of our galaxy and even others."

These regions are non-luminous, save for emission of the 21-cm (1,420 MHz) region spectral line. Mapping H I emissions with a radio telescope is a technique used for determining the structure of spiral galaxies.

Recent history

The Kölner Observatorium für SubMillimeter Astronomie (KOSMA) is a 3-m radio telescope located at 3,135 m on Gornergrat near Zermatt (Switzerland) in the southern tower (nearest to the camera). Credit: Doc Searls.{{free media}}

The recent history period dates from around 1,000 b2k to present.

The Kulmhotel Gornergrat, atop Gorgergrat, which is both mountain and ski slope, is also home to two observatories. The Kölner Observatorium für SubMillimeter Astronomie (KOSMA) [at right] is a 3-m radio telescope located at 3,135 m on Gornergrat near Zermatt (Switzerland) in the southern tower (nearest to the camera).

"Because of the good climatic conditions at the altitude of 3135 m (10285 ft), astronomical observatories have been located in both towers of the “Kulmhotel” at Gornergrat since 1967. In 1985, the KOSMA telescope was installed in the southern tower by the Universität zu Köln and, in the course of 1995, replaced by a new dish and mount."

"The KOSMA telescope with its receivers and spectrometers was dedicated to observe interstellar and atmospheric molecular lines in the millimeter and submillimeter wavelength range. After 25 years of a successful era came to an end (June 2nd, 2010). The 3m KOSMA Radio Telescope left the Gornergrat and joined his long journey to Yangbajing / Lhasa / Tibet."

"Chinese and German scientists are establishing an astronomical observatory in a Tibetan county 4,300 meters above sea level."

"Tibet is an ideal location because the water deficit in its air ensures superb atmospheric transparency and creates a comparatively stable environment for research in the areas of astrophysics, high-energy and atmospheric physics."

"The observatory would house a KOSMA 3-meter sub-millimeter-wave telescope, the first of its kind to be used in general astronomical observation in China."

Sciences

Main resource: Sciences

A "catalogue of 800 compact radio sources in the declination range 35° ≤ δ ≤ 75° whose positions have been measured to an rms accuracy of ~ 12 milliarcsec with the VLA [where the] observations were carried out in three sessions between 1990 February 19 and 23." is available and this primary source mentions earlier catalogues.

Balloons

Main resource: Radiation astronomy/Balloons

The E and B Experiment (EBEX) will measure the cosmic microwave background radiation of a part of the sky during two sub-orbital (high altitude) balloon flights. It is an experiment to make large, high-fidelity images of the CMB polarization anisotropies. By using a telescope which flies at over 42,000 metres high, it is possible to reduce the atmospheric absorption of microwaves to a minimum. This allows massive cost reduction compared to a satellite probe, though only a small part of the sky can be scanned and for shorter duration than a typical satellite mission such as WMAP.

EBEX was launched on 29 December, 2012, near McMurdo Station in Antarctica.

"EBEX is meant to hone in on one specific feature of the CMB light that's been predicted, but never seen — a signature called B-type polarization, thought to have been produced by the gravity waves created by the universe's extremely rapid infant expansion, which happened even before the CMB light was released."

Satellites

Main resource: Radiation astronomy/Satellites

The fairling of the Delta 1913 (D-95) is installed around Explorer 49 (RAE-B). Credit: NASA.{{free media}}

A Delta 1000 series rocket, serial number 95, sits on its pad at Cape Canaveral ready to launch the Explorer 49 spacecraft. Credit: NASA.{{free media}}

The image on the right shows the fairling of the Delta 1913 (D-95) being installed around Explorer 49 (RAE-B).

On the left, a Delta 1000 series rocket, serial number 95, sits on its pad at Cape Canaveral ready to launch the Explorer 49 spacecraft into a lunar orbit.

Explorer 49

RAE B was a radio telecope that was placed in a moon orbit. Credit: NASA.{{free media}}

Several satellites have served as observatories for radio waves and specifically for microwaves.

Explorer 49 is a 328 kilogram satellite launched on June 10, 1973 for longwave radio astronomy research. It had four 230-meter long X-shaped antenna elements, which made it one of the largest spacecraft ever built. Explorer 49 was placed into lunar orbit to provide radio astronomical measurements of the planets, the sun, and the galaxy over the frequency range of 25 kHz to 13.1 MHz.

Radio observatories

File:Arecibo Observatory Aerial View2.jpg

The Arecibo Radio Telescope, Arecibo, Puerto Rico, at 1000 feet (305 m) across, is the largest dish antenna in the world. Credit: H. Schweiker/WIYN and NOAO/AURA/NSF, NOAA.{{fairuse}}

The "Arecibo Observatory in Puerto Rico [is] the world's largest, and most sensitive, single-dish radio telescope."

"The 1,000-foot-diameter (305 meters) Arecibo telescope [... provides] access to state-of-the-art observing for scientists in radio astronomy, solar system radar and atmospheric studies, and the observatory has the unique capability for solar system and ionosphere (the atmosphere's ionized upper layers) radar remote sensing."

"It contains the largest curved focusing dish on Earth, giving Arecibo the largest electromagnetic-wave-gathering capacity. The dish surface is made of 38,778 perforated aluminum panels, each measuring about 3 by 6 feet (1 by 2 m), supported by a mesh of steel cables.

The telescope has three radar transmitters, with effective isotropic radiated powers of 20 TW at 2380 MHz, 2.5 TW (pulse peak) at 430 MHz, and 300 MW at 47 MHz. The telescope is a spherical reflector, not a parabolic reflector. To aim the telescope, the receiver is moved to intercept signals reflected from different directions by the spherical dish surface. A parabolic mirror would induce a varying astigmatism when the receiver is in different positions off the focal point, but the error of a spherical mirror is the same in every direction.

The receiver is located on a 900-ton platform which is suspended 150 m (500 ft) in the air above the dish by 18 cables running from three reinforced concrete towers, one of which is 110 m (365 ft) high and the other two of which are 80 m (265 ft) high (the tops of the three towers are at the same elevation). The platform has a 93-meter-long rotating bow-shaped track called the azimuth arm on which receiving antennas, secondary and tertiary reflectors are mounted. This allows the telescope to observe any region of the sky within a forty-degree cone of visibility about the local zenith (between −1 and 38 degrees of declination). Puerto Rico's location near the equator allows Arecibo to view all of the planets in the Solar System, though the round trip light time to objects beyond Saturn is longer than the time the telescope can track it, preventing radar observations of more distant objects.

Goldstone Deep Space Communication Complex

This is an image of the Goldstone Deep Space Communication Complex. Credit: NASA.{{free media}}

Shown at right are the three "34m (110 ft.) diameter Beam Waveguide antennas located at the Goldstone Deep Space Communications Complex, situated in the Mojave Desert in California. This is one of three complexes which comprise NASA's Deep Space Network (DSN). The DSN provides radio communications for all of NASA's interplanetary spacecraft and is also utilized for radio astronomy and radar observations of the solar system and the universe."

Radio telescopes

This 64 meter radio telescope is at Parkes Observatory Credit: John Sarkissian (CSIRO Parkes Observatory).{{free media}}

The 25.6 m telescope at Onsala Space Observatory. Credit: Moralist.{{free media}}

The 20 metre telescope is inside its radome at the Onsala Space Observatory. Credit: Anthony Rushton.{{free media}}

The LOFAR station is at Onsala Space Observatory in Sweden. Credit: Askmatl.{{free media}}

The image shows the Rapid Prototype Seti Array at Leuschner Observatory. Credit: Andrew Howard.{{free media}}

A radio telescope is a form of direction radio antenna, as used in tracking and collecting data from satellites and space probes that operates in the radio frequency portion of the electromagnetic spectrum. Radio telescopes are typically large parabolic ("dish") antennas used singly or in an array. Radio observatories are preferentially located far from major centers of population to avoid electromagnetic interference (EMI) from radio, TV, radar, and other EMI emitting devices.

"The Rapid Prototype Array [RPA] observed the Navstar/GPS satellite #35 on 10 April 2001."

"Data were obtained at 17:58 UT 10 April 2001. The expected location of the satellite at the RPA site was azimuth 68.7 deg, elevation 57.8 deg. Six antennas were used. Antenna one was pointed to put the satellite in the main beam. Antennas two through six were pointed to put the satellite at azimuth 68 and elevation 66."

"The data-taking was triggered with a rapidly rising edge to the A/D converter. The data are synchronized to approximately 100 nsec. No compensation was made for geometric or instrumental delays."

"Data were obtained in two polarizations for each antenna with 30 Msamples/sec sampling. Sample bytes were 8-bits in length. Zero voltage corresponds to approximately 127.5 counts."

"Local oscillators were set so that 1575.42 MHz was mixed to 7.5 MHz before sampling. A 10 MHz IF passband filter sets the usable range of the band from 1570 to 1580 MHz, roughly."

Radio interferometry

The diagram shows a possible layout for an astronomical interferometer, with the mirrors laid out in a parabolic arrangement (similar to the shape of a conventional telescope mirror). Credit: Bob Tubbs.{{free media}}

An astronomical interferometer is an array of telescopes or mirror segments acting together to probe structures with higher resolution by means of interferometry. The benefit of the interferometer is that the angular resolution of the instrument is nearly that of a telescope with the same aperture as a single large instrument encompassing all of the individual photon-collecting sub-components. The drawback is that it does not collect as many photons as a large instrument of that size. Thus it is mainly useful for fine resolution of the more luminous astronomer]]s.

Very Long Baseline Interferometry uses a technique related to the closure phase to combine telescopes separated by thousands of kilometers to form a radio interferometer with the resolution which would be given by a single dish which was thousands of kilometers in diameter. Astronomical interferometers can produce higher resolution astronomical images than any other type of telescope. At radio wavelengths image resolutions of a few micro-arcseconds have been obtained.

Hypotheses

Main resource: Hypotheses

1. Radio rays can be accelerated above light speed using other photons.

See also

• Gravitational astronomy
• Infrared astronomy
• Microwave astronomy
• Millimeter astronomy
• Radar astronomy
• Red astronomy
• Submillimeter astronomy
• Superluminal astronomy

Further reading

• Cox, A. N., ed (2000). Allen's Astrophysical Quantities. New York: Springer-Verlag. p. 124. ISBN 0-387-98746-0. https://books.google.com/?id=w8PK2XFLLH8C&pg=PA124. 
• F. H. Shu (1982). The Physical Universe. Mill Valley, California: University Science Books. ISBN 0-935702-05-9. 

External links

• The History of Radio Astronomy
• International Astronomical Union
• NASA/IPAC Extragalactic Database - NED
• nrao.edu National Radio Astronomy Observatory
• NASA's National Space Science Data Center
• NCBI All Databases Search
• Office of Scientific & Technical Information
• PubChem Public Chemical Database
• The SAO/NASA Astrophysics Data System
• Scirus for scientific information only advanced search
• SDSS Quick Look tool: SkyServer
• SIMBAD Astronomical Database
• Spacecraft Query at NASA
• Universal coordinate converter

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