The Stratospheric Observatory for Infrared Astronomy (SOFIA) has returned to its usual base of operations after a month of science observations in the Southern Hemisphere. The observatory was temporarily based out of Christchurch International Airport in New Zealand.
The Stratospheric Observatory for Infrared Astronomy (SOFIA) returns to NASA’s Armstrong Flight Research Center Building 703 on Aug. 11 after a productive month of science flights out of Christchurch International Airport in New Zealand. Credit: NASA/Joshua Fisher
SOFIA arrived Thursday, Aug. 11 at NASA Armstrong Flight Research Center’s Building 703 in Palmdale, California, and plans to resume science flights Monday, Aug. 22.
SOFIA had been scheduled to remain longer in New Zealand before severe weather caused damage to the aircraft, requiring the mission to adjust its science observation plans and cancel the remainder of the deployment. During its time in the Southern Hemisphere, SOFIA observed and studied a wide range of celestial objects and phenomena, like cosmic magnetic fields, the structure of the Milky Way, and the origin of cosmic rays.
An inspection and assessment of the aircraft determined SOFIA may safely return to science flights for the remainder of the mission, following minor repairs and a safety checkout flight conducted in New Zealand. The mission will conclude no later than Sept. 30.
The Stratospheric Observatory for Infrared Astronomy (SOFIA) is adjusting its science observation plans and canceling the remainder of its Southern Hemisphere deployment following damage to the aircraft caused by severe weather on Monday, July 18. SOFIA is currently operating out of Christchurch International Airport in New Zealand to better observe celestial objects in the southern skies.
SOFIA at Christchurch International Airport, New Zealand. Credit: NASA/SOFIA/G. Perryman
The SOFIA team has determined the needed repairs will take at least three weeks, eliminating the possibility of conducting the remaining science observation flights that were planned from New Zealand through August 7.
SOFIA arrived in New Zealand on June 18 and had a successful and productive month of science flights. Using two instruments, HAWC+ and GREAT, SOFIA observed and studied a wide range of celestial objects and phenomena, like cosmic magnetic fields, structure of the Milky Way, and the origin of cosmic rays.
During the deployment, the SOFIA team also took part in multiple outreach events, sharing information about the observatory and its science with students in grades K-12, youth groups, museum attendees, and members of the aerospace industry.
The aircraft will return to its usual base of operations in Palmdale, California, and resume science flights after repairs are complete.
The Stratospheric Observatory for Infrared Astronomy (SOFIA) is down for maintenance after being damaged by a storm that affected the area around Christchurch International Airport in New Zealand on Monday, July 18.
During the severe weather event, high winds caused the stairs outside the aircraft to shift, causing light damage to the front of the aircraft, as well as the stairs themselves. There were no injuries to any staff. The aircraft damage is being assessed, repair plans are moving forward, and new stairs are being delivered. During this time, the mission’s science observation schedule will be reassessed, as SOFIA is unable to continue normal operations until the repairs are complete and stairs are available.
SOFIA currently is operating out of Christchurch International Airport to better observe celestial objects in the Southern Hemisphere. Updates to the status of SOFIA will be shared once available.
Within the Orion Nebula is a massive set of stars known as the Trapezium stars. The winds from the Trapezium stars blow a bubble of dust and gas in the area in front of them, called Orion’s Veil. The majority of Orion’s Veil is sparse, with most of its gas lying in the bubble’s wall. The wall, or Orion’s Veil shell, is about a light-year thick and expanding toward us – and recent observations by the Stratospheric Observatory for Infrared Astronomy (SOFIA) German REceiver for Astronomy at Terahertz Frequencies (GREAT) have identified some unexpected features in it.
A 3D model of the Orion Nebula shows Orion’s Veil shell as a bluish gas surrounding the nebula depicted in red and yellow. Researchers using SOFIA found a protrusion in the shell, which could allow gas and dust to escape beyond the shell. Credit: NASA, ESA, Frank Summers (STScI), Greg T. Bacon (STScI), Lisa Frattare (STScI), Zolt G. Levay (STScI), K. Litaker (STScI). Acknowledgment: Axel Mellinger, Robert Gendler, Rogelio B. Andreo
“The bubble – with a diameter of approximately seven light-years – should be an almost sphere-like structure, but we found a protrusion in its northwestern part,” said Ümit Kavak, a postdoctoral researcher at SOFIA based out of NASA’s Ames Research Center in California’s Silicon Valley, who is the lead author on a recent paper describing the studies.
The SOFIA observations show ionized carbon emission in this protrusion, which Kavak used to determine its size, structure, and how it is expanding, in hopes of uncovering its origins and future.
Shaped like a “U” lying on its side, the protrusion extends well beyond Orion’s Veil shell. It is a likely spot for the shell to pierce, and the protrusion’s chimney-like top seems to imply it already has.
Schematic picture of the protrusion (green lines, center right) and outflows of ionized carbon extending beyond the protrusion — where the shell has likely been pierced — overlaid on a Wide-field Infrared Survey Explorer image of the region. Credit: NASA/JPL-Caltech/WISE Team; Kavak et al.
“When you breach the Veil shell, you effectively start stirring a cosmic soup of gas and dust by adding turbulence,” Kavak said.
“This isn’t the most appetizing soup, but it’s one of the ways to form new stars or limit future star formation,” added Alexander Tielens, a researcher at Leiden University and another author on the paper.
This turbulence affects the density, temperature, and chemistry of its surrounding region, which may ultimately lead to the creation or destruction of star formation sites.
The group also identified a second, weaker protrusion, which they plan to investigate further in a future publication. Together, these protrusions affect the entire morphology of the Orion Nebula.
SOFIA is a joint project of NASA and the German Space Agency at DLR. DLR provides the telescope, scheduled aircraft maintenance, and other support for the mission. NASA’s Ames Research Center in California’s Silicon Valley manages the SOFIA program, science, and mission operations in cooperation with the Universities Space Research Association, headquartered in Columbia, Maryland, and the German SOFIA Institute at the University of Stuttgart. The aircraft is maintained and operated by NASA’s Armstrong Flight Research Center Building 703, in Palmdale, California. SOFIA achieved full operational capability in 2014, and the mission will conclude no later than Sept. 30, 2022. SOFIA will continue its regular operations until then, including science flights and a deployment to New Zealand this summer.
After a two-year hiatus, SOFIA has returned to Christchurch, New Zealand, for a long deployment. About once a year, SOFIA temporarily moves its operating home to better observe celestial objects in the Southern Hemisphere.
SOFIA taxiing on the ramp at Christchurch International Airport in 2017. Image Credit: NASA/SOFIA/Waynne Williams
There is always a high demand from the SOFIA scientific community to observe the southern skies, and SOFIA has been working to meet those needs. This year, we already deployed once to Santiago, Chile, for a quick, two-week deployment to observe the Large Magellanic Cloud. Now SOFIA is heading back to New Zealand for the seventh and final time.
“We are thrilled to be returning to Christchurch to continue to study and discover the infrared universe,” said Naseem Rangwala, the SOFIA project scientist.
SOFIA has made 12 deployments over its operational lifetime, generally leaving Palmdale, California, to observe celestial objects and phenomena not visible from its home skies. We observed occultations in Florida and New Zealand, as well as atomic oxygen in Earth’s atmosphere, stellar feedback, and magnetic fields from German soil.
Christchurch is often SOFIA’s home-away-from-home when deploying overseas. This time, SOFIA plans to conduct 32 flights to observe a wide range of celestial objects and phenomena, like cosmic magnetic fields, stellar feedback, and cosmic rays, using two instruments, HAWC+ and GREAT.
Probing the Magnetic Universe
While in New Zealand, SOFIA will observe magnetic fields in our galaxy, the Milky Way, pictured here from a previous study with another SOFIA instrument. Image credit: NASA/SOFIA/JPL-Caltech/ESA/Herschel.
Sticking relatively close to our cosmic home, SOFIA will start by investigating our galaxy, the Milky Way. A team of researchers is mapping the magnetic fields within the Milky Way’s central regions. These data will complement a previous Legacy Program that made mid-infrared images of the Milky Way. This work is similar to other cosmic magnetic field studies that map the shape and strength of this invisible force in othergalaxies. SOFIA can detect cosmic magnetic fields on many scales, including star formation scales, especially along filaments.
SOFIA will also be looking at magnetic fields in filaments of material in our galaxy. These filaments are thread-like structures full of cold gas and dust. Most stars form in these dark rivers of material. A team of scientists will be investigating how magnetic fields play a role in star formation in filaments.
Stars Blowing Bubbles and a Barometer for Cosmic Rays
SOFIA in Christchurch, New Zealand, during its 2019 deployment with the staff and crew of the observatory. Image credit: NASA/Waynne Williams.
After HAWC+ finishes up probing the magnetic universe, SOFIA’s operations team will swap the instrument for the German PI-led GREAT instrument. GREAT does a wide variety of studies including looking at stellar feedback – how some stars can affect the regions around them. Young massive stars create huge winds that blow out into the surrounding dusty material, sometimes blowing celestial bubbles. As they do this, the stellar winds plow into the material and sometimes can trigger or quench star formation. Scientists want to understand when and why star formation is turned on or off.
GREAT, like the radio in your car, can be tuned to be sensitive to specific signals. During the New Zealand deployment, it will be set to register hydride molecules. These molecules were some of the first types that formed in our universe, and, even now, they are sometimes created in other environments. When scientists detect hydrides, they can use them as sensitive barometers for the presence of cosmic rays, high energy particles that travel close to the speed of light.
Hydride molecules form in very specific circumstances, and, usually, scientists can determine their production rate. At the same time, these molecules are quite delicate and can easily be destroyed by passing cosmic rays. Understanding the balance between their production and destruction can provide clues to the abundance of cosmic rays.
Scientists have measured the cosmic rays produced by our Sun and understand them very well, but do not fully understand cosmic rays that originate from outside our solar system. Using hydride molecules, researchers will investigate how abundant cosmic rays are in environments outside our solar system.
Many of the key celestial objects for astronomers, like the center of the Milky Way, are either visible only from the Southern Hemisphere or more easily observed from these latitudes. Three years after SOFIA achieved first light in 2010, the observatory made its first trip to New Zealand. Now, nine years later and with six previous trips to Christchurch, this will be SOFIA’s last international deployment.
NASA and DLR recently announced the conclusion of the SOFIA mission. SOFIA will operate for the rest of fiscal year 2022, before entering an orderly shutdown process on October 1, 2022.
“We are committed to delivering a strong finish for this unique astrophysics mission, from a place of strength and pride, by giving our scientific community as much data as possible from the Southern Hemisphere,” Dr. Rangwala said. Moving forward, SOFIA’s data will be available in NASA’s public archives for astronomers worldwide to use.
SOFIA is a joint project of NASA and the German Space Agency at DLR. DLR provides the telescope, scheduled aircraft maintenance, and other support for the mission. NASA’s Ames Research Center in California’s Silicon Valley manages the SOFIA program, science, and mission operations in cooperation with the Universities Space Research Association, headquartered in Columbia, Maryland, and the German SOFIA Institute at the University of Stuttgart. The aircraft is maintained and operated by NASA’s Armstrong Flight Research Center Building 703, in Palmdale, California.
Hidden behind a dark band of dust known as the Great Rift, the Cygnus-X star formation region is more than a bit of a mystery. Astronomers haven’t quite figured out what the molecular clouds in Cygnus-X are doing, and why, but observations from the Stratospheric Observatory for Infrared Astronomy (SOFIA) may help.
These mysteries relate to the fact that Cygnus-X is a difficult region to study. Two of its clouds – DR21 and W75N – clearly have separate gas velocities, but which cloud is in front of the other, and whether or not the two clouds are colliding, are open questions. Dan Clemens, an astronomer at Boston University, is the principal investigator on a project using SOFIA to examine Cygnus-X and the effects of magnetic fields on its clouds and cloud filaments. Details of these studies were presented at the June 2022 meeting of the American Astronomical Society.
Cygnus-X northeast region. Background image was constructed from Herschel SPIRE 250um in red, Herschel PACS 70um in green, and Spitzer MIPS 24um in blue. Red polygon indicates region surveyed for near-infrared, H-band (1.6um) stellar polarizations. Cyan segments indicate the magnetic field orientations derived from those NIR polarizations. Dashed white curves highlight filaments and sub-filaments cataloged by Hennemann et al. (2012) and new filaments and subfilaments from this study. The green polygon shows the DR21 Ridge region surveyed using SOFIA HAWC+ E-band (214um) polarization and the inscribed smaller magenta polygon shows the corresponding HAWC+ A-band (52um) polarization surveyed region. Credit: Herschel/Spitzer/SOFIA/Hennemann et al./Clemens et al.
“You can think of it as a pasta bowl with all these threads going in,” said Clemens. “Which pasta is in front of which pasta? Are there separate piles of pasta, or are they interacting piles of pasta that cause stars to form?”
On top of this, the presence of magnetic fields adds further complexity. What these magnetic fields are doing – whether they are passive participants in the clouds’ dynamics or helping to direct mass flows – is a question the SOFIA data may help answer by looking at small-scale filaments within the clouds.
Using SOFIA’s High-resolution Airborne Wideband Camera Plus (HAWC+), Clemens and his team zoomed in on Cygnus-X to look at the polarizations of the filaments at far-infrared wavelengths. These polarizations indicate the directions of the small-scale magnetic fields in the region, which the researchers use to determine the role the fields are playing.
“We want to ascertain the nature of the magnetic fields along these filaments, where they begin, and where they end,” Clemens said. “This will help test our best star formation models and notions.”
Most modern theories of star formation hint that magnetic fields may be channeling gas flows within molecular clouds toward a central hub, where massive star formation occurs. The SOFIA observations will reveal the magnetic fields in filaments within the clouds, helping to verify the idea that fine, weak magnetic fields can control how stars form.
According to the team’s analysis, there appear to be four distinct layers of gas and dust between us and the northern region of Cygnus-X. Whether or not these layers are interacting will affect their understanding of SOFIA’s magnetic field data. As such, Clemens and his collaborators will need to determine which cloud is in front of the other, and if they are going to collide, before the SOFIA data – and supporting wider-field, ground-based, near-infrared data – describing the magnetic fields can be effectively interpreted.
SOFIA is a joint project of NASA and the German Space Agency at DLR. DLR provides the telescope, scheduled aircraft maintenance, and other support for the mission. NASA’s Ames Research Center in California’s Silicon Valley manages the SOFIA program, science, and mission operations in cooperation with the Universities Space Research Association, headquartered in Columbia, Maryland, and the German SOFIA Institute at the University of Stuttgart. The aircraft is maintained and operated by NASA’s Armstrong Flight Research Center Building 703, in Palmdale, California. SOFIA achieved full operational capability in 2014, and the mission will conclude no later than Sept. 30, 2022. SOFIA will continue its regular operations until then, including science flights and a deployment to New Zealand this summer.
“One of the key goals, when you think about modern astronomy, considers the life cycle of molecular material,” said Arshia Jacob, an astronomer at Johns Hopkins University. Diffuse atomic gas becomes dense molecular gas, which ultimately forms stars and stellar systems, and continues to evolve over time. Though astronomers understand much of this process, there are a lot of missing pieces.
Jacob is the lead author on a recent paper characterizing the interstellar medium in the Milky Way using SOFIA, the Stratospheric Observatory for Infrared Astronomy, to fill in some of these missing pieces. By studying six hydrides, which are molecules or molecular ions in which one or more hydrogen atoms are bound to a heavier atom through shared electron pairs, Jacob and her collaborators hope to better understand how molecular clouds form and evolve.
W3, one of the 25 Milky Way regions the HyGAL project will study, is seen as the glowing white area in the upper right of this image of the Heart and Soul Nebulae, taken by NASA’s Wide-field Infrared Survey Explorer (WISE). SOFIA looked at the abundances of six hydride molecules in W3, the spectra of two of which are shown in the box at left. Image credit: Nebulae: NASA/JPL-Caltech/UCLA; Spectra: Jacob et al.
Hydrides are useful to astronomers because they are very sensitive tracers of different phases of the interstellar medium, and their chemistry is relatively straightforward. Moreover, hydride observations provide measurements of the amount of material present.
The multi-investigator SOFIA project Hydrides in the Galaxy (HyGAL) uses a diverse selection of hydride molecules, allowing different processes to be monitored while complementing other observations. For example, one of the hydrides studied, argonium, can only form in regions that are almost purely atomic gas, so detecting argonium is indicative of a low molecular content in its surrounding environment. Other hydride molecules can indicate the presence of dense gas, intense cosmic radiation, turbulence, and more.
“Hydrides are small, but we can understand so much from them. Small molecules, big impact,” Jacob said.
In the first stage of the project, the group compared the hydride abundances in three regions of the Milky Way: two star-forming regions, W3(OH) and W3 IRS5, and a young stellar object, NGC 7538 IRS1. Though the average properties of these first three sources are similar, the full HyGAL project plans to study a total of 25 regions. With the remaining 22 sources covering distances from the inner galaxy all the way to the outer galaxy, they expect vastly different results.
“The sources are very different: Some of them are older, some have more chemical enrichment, some are younger and still forming stars,” Jacob said. “All of these will affect the nature of molecules that are formed, like their abundances, for example.”
Moving away from the galactic center, the transitions from atomic to molecular gas change, and the cosmic ray ionization rates vary vastly, which will result in differences in the ratios of molecules present and other properties. This will help astronomers understand the diversity of environments within the Milky Way.
“Imagine you’re moving into a cloud. At each stage, you’re seeing different molecules, reflecting changes in the cloud properties as it gets denser,” Jacob said. “Through this project, we’re filling in the properties of this transition.”
Currently, there have only been a handful of bright sources emitting a broad range of radiation that have been studied in this way, all concentrated in the inner galaxy. The SOFIA data will more than double the existing data, providing additional answers about the structure, dynamics, and chemistry of these clouds and where the dense material comes from.
SOFIA is the only facility presently capable of accessing the frequency range necessary for these observations at the required resolution. The German REceiver Astronomy at Terahertz Frequencies (GREAT) instrument aboard SOFIA allows five frequencies to be monitored simultaneously, each tuned to five of the six hydrides in question to determine the makeup of the cloud sources. These are complemented by studies at radio wavelengths with observatories such as the Karl G. Jansky Very Large Array near Socorro, New Mexico.
“The idea is to give us not only information about the sources themselves, but also information about the different spiral arms they cross, making this truly a study over galactic scales,” Jacob said.
SOFIA is a joint project of NASA and the German Space Agency at DLR. DLR provides the telescope, scheduled aircraft maintenance, and other support for the mission. NASA’s Ames Research Center in California’s Silicon Valley manages the SOFIA program, science, and mission operations in cooperation with the Universities Space Research Association, headquartered in Columbia, Maryland, and the German SOFIA Institute at the University of Stuttgart. The aircraft is maintained and operated by NASA’s Armstrong Flight Research Center Building 703, in Palmdale, California. SOFIA achieved full operational capability in 2014, and the mission will conclude no later than Sept. 30, 2022. SOFIA will continue its regular operations until then, including science flights and a deployment to New Zealand this summer.
With its observations of a special pair of stars at a special moment in their lives, the Stratospheric Observatory for Infrared Astronomy (SOFIA) is shedding new light on stardust.
Over an interval of 387 days, a giant star in the constellation Aquarius periodically has a dramatic change in its brightness. This is because the star falls into a category called Mira variables, which pulsate over long periods and surround themselves in a shell of dust.
But this isn’t just any Mira variable. The star is one of two in a binary star system known as R Aquarii, where it has a companion white dwarf. The two orbit one another, and the white dwarf crosses in front of the Mira variable every 43.6 years, causing an eclipse from the perspective of a viewer on Earth.
This composite image of R Aquarii resembles a ring of fire over a black field, with a glowing purple “S” flowing through it. Near the center of the image, in the middle of the ring and the “S” wave, is a twinkle of bright white, which is the Mira variable in R Aquarii. The white dwarf is very faint and contributes very little to the optical emission. However, the purple wave is the result of a jet that is powered by the white dwarf accreting dust produced by the Mira variable. The smokey red circles are evidence of explosive events that occurred several hundred years ago. Overlain atop the composite image of R Aquarii is a set of five plots indicating the energy emitted by the system. SOFIA acquired four of the data sets, while the strong purple plot is data from the Infrared Space Observatory from 1996, when R Aquarii’s emission was strongest. The strength also depends on the phase of the binary star system’s eclipse, so it does not increase each successive year, exactly: the flux fell between 2018 and 2019. Credit: NASA/CSC/SAO/STScI/Palomar Observatory/DSS/NSF/NRAO/VLA/LCO/IMACS/MMTF/Sankrit et al.
There’s another thing that’s special about R Aquarii: The periastron, or the point in the orbit where the two stars are closest to each other, happens during the eclipse. This means that as the eclipse occurs – and the pair gets dimmer and dimmer, overall – the white dwarf and the Mira variable get closer and closer together. The white dwarf accretes more and more of the dust surrounding the Mira variable, and, because of this optimal geometry, we get to watch this process occur.
Since 2016, SOFIA, a joint project of NASA and the German Space Agency at DLR, has been monitoring the onset of the eclipse, which started in 2018, with periastron expected to occur in 2023. The flow of dust can be inferred at mid-infrared wavelengths, and SOFIA’s infrared camera, FORCAST, has just the right angular resolution to watch.
By combining what they know about the system – the distance between the two stars, the fact that an eclipse is ongoing, and predictions of how much dust there is – astronomers can figure out the balance between the amount of dust escaping the Mira variable and how much is being accreted by the white dwarf. These are “both very big questions,” said Ravi Sankrit, an astronomer at the Space Telescope Science Institute in Baltimore and first author on a recent paper about SOFIA’s 2018 and 2019 observations of R Aquarii.
“It’s an opportunity to see it in a unique way, because the material that’s being accreted isn’t obscured by the Mira, it’s right out in front,” added Steven Goldman, a scientist with Universities Space Research Association, based at NASA’s Ames Research Center in California’s Silicon Valley. Goldman is a co-author on the paper, which looks at how the onset of the eclipse is beginning to affect the dust surrounding the system.
Since the two stars move from being very far apart to very close to one another, their dust is constantly changing. Continued mid-infrared monitoring is required to fully understand how the dust is affected by the stars’ orbit.
“Binarity, winds, jet formation, mass loss, and accretion are fundamental astrophysics,” Sankrit said. “So, the real excitement here is that you’re getting something that is on a human timescale probing very fundamental aspects of astrophysics.”
The physics Sankrit, Goldman, and their team are uncovering is applicable to more than just R Aquarii. There are hundreds of other similar binaries, and those are just the ones we know of. These other binary systems are likely experiencing the same phenomenon but aren’t oriented correctly for us to be able to see their periastron and the changes in their surrounding dust.
SOFIA is a joint project of NASA and the German Space Agency at DLR. DLR provides the telescope, scheduled aircraft maintenance, and other support for the mission. NASA’s Ames Research Center in California’s Silicon Valley manages the SOFIA program, science, and mission operations in cooperation with the Universities Space Research Association, headquartered in Columbia, Maryland, and the German SOFIA Institute at the University of Stuttgart. The aircraft is maintained and operated by NASA’s Armstrong Flight Research Center Building 703, in Palmdale, California. SOFIA achieved full operational capability in 2014, and the mission will conclude no later than Sept. 30, 2022. SOFIA will continue its regular operations until then, including science flights and a deployment to New Zealand this summer.
During flights in August 2018 and July 2019, planetary scientists used the Stratospheric Observatory for Infrared Astronomy (SOFIA), a joint project of NASA and the German Space Agency at DLR, to study the atmospheric circulation on Jupiter – for the first time during the planet’s northern winter.
Left: Optical image of Jupiter taken by the Hubble Space Telescope. Right: SOFIA image of Jupiter demonstrating the variation in its brightness temperature with latitude. The two images show Jupiter in approximately the same orientation. Image credit: Left: NASA/ESA; Right: NASA/SOFIA/de Pater et al., 2021
To do so, they looked at hydrogen.
Hydrogen molecules – H2 – can be arranged in two different ways, known as parahydrogen and orthohydrogen. The two orientations have distinct energies, so determining the ratio of parahydrogen to orthohydrogen can tell astronomers about the overall temperature.
The researchers looked at the concentration of parahydrogen and orthohydrogen at altitudes just above Jupiter’s main cloud deck. They discovered that, around the equator, warm gas is rising into the atmosphere. At the north and south poles, however, the opposite is occurring: Cold gas from the higher, cooler levels of the atmosphere is traveling downward.
“This gives a sense of the general circulation: rising at the equator, sinking near the poles,” said Imke de Pater, lead author on a recent paper in the Planetary Science Journal describing the observations.
Jupiter’s atmosphere had been looked at through the lens of hydrogen before – by SOFIA in 2014, and by NASA’s Voyager 1 and 2 in 1979 – but only during the northern Jovian summer. The current observations were the first ever taken during Jupiter’s northern winter, about half a Jovian year after the 2014 SOFIA studies. This comparison illustrated how Jupiter’s poles change with the seasons, showing that its far north remains cooler than its far south, regardless of time of year.
Jupiter’s northern and southern hemispheres are known to have an asymmetric aerosol distribution, so this temperature imbalance between its two poles is likely an effect of its asymmetry.
In studying Jupiter, de Pater and her colleagues also saw four other objects that had entered SOFIA’s field of view and the data collected: Jupiter’s four largest moons, known collectively as its Galilean satellites – Io, Europa, Ganymede, and Callisto.
“We were surprised that we actually captured all four satellites, and could determine their brightness temperature,” de Pater said.
Thanks to this pleasant surprise, the group could clearly see how the moons’ temperatures decrease with depth in their subsurface layers. These temperature changes can eventually be used to determine the composition, density, and other properties inside the satellites.
The satellites all have unique characteristics – ranging from water ice on Europa, to heavy craters on the ancient Callisto, to extreme volcanic activity on Io – making their material makeup particularly interesting to investigate.
Jupiter and its moons are too bright to be observed by the long wavelength channels on the James Webb Space Telescope as they can saturate the instrument, and they cannot be measured from the ground due to Earth’s atmosphere blocking a large amount of mid-infrared radiation. SOFIA’s unique access to the mid-infrared, therefore, enables these measurements and provides critical information about Jupiter and its moons.
SOFIA is a joint project of NASA and the German Space Agency at DLR. DLR provides the telescope, scheduled aircraft maintenance, and other support for the mission. NASA’s Ames Research Center in California’s Silicon Valley manages the SOFIA program, science, and mission operations in cooperation with the Universities Space Research Association, headquartered in Columbia, Maryland, and the German SOFIA Institute at the University of Stuttgart. The aircraft is maintained and operated by NASA’s Armstrong Flight Research Center Building 703, in Palmdale, California.
Most stars in spiral galaxies form within the galaxy’s arms. Building the “skeletons” of these galaxies are galactic bones, long filaments that outline the densest parts of the arms.
A map shows the direction of magnetic fields in the G47 bone overlain atop an image of the G47 filament as seen by the Herschel Space Observatory. The red and yellow areas are high-density regions of dust and gas. Credit: G47: ESA/Herschel/PACS/SPIRE/Ke Wang et al. 2015; Polarization map: Stephens et al., 2022
At the largest scales, the magnetic fields of a galaxy follow its spiral arms. Fields in the bones were accordingly believed to be aligned with respect to the bone, but research from the Stratospheric Observatory for Infrared Astronomy (SOFIA), a joint project of NASA and the German Space Agency at DLR, hints that this is generally not the case. The magnetic fields do not follow the spiral shape of the galaxy’s arms, nor are they in general perpendicular to the bones.
“Before SOFIA, it was difficult to image magnetic fields at high resolution over the entirety of the bones,” said Ian Stephens, an astrophysicist at Worcester State University. “We are now able to get so many independent measurements of the magnetic field direction across these bones, allowing us to really delve into the importance of the magnetic field in these massive filamentary clouds.”
Stephens is part of the Filaments Extremely Long and Dark: a MAgnetic Polarization Survey (FIELDMAPS) project, the first attempt to map the magnetic field of any galactic bone in its entirety. Of the ten bones the group plans to map, the first project completed by FIELDMAPS is that of G47, a giant filamentary bone within the Milky Way that is 200 light-years in length and 5 light-years in width.
“Magnetic fields…can potentially set the rate at which stars form in a cloud. They can also guide the flow of gas, shape the bones, and affect the quantity and size of the densest pockets of gas that will eventually collapse to form stars,” Stephens said. “By mapping the orientation of the fields, we can estimate the relative importance of the magnetic field to that of gravity to quantify how much magnetic fields affect the star formation process.”
The researchers did just that and were able to determine that the magnetic fields are strong enough to prevent gas in many areas from succumbing to gravitational collapse to form stars. They found the magnetic fields in the G47 bone were complex, changing directions frequently – though in the densest areas, they trended perpendicular to the bone. This means the parallel fields from the less dense regions are feeding material into the denser regions, where fields play a key role in the star formation rate by impeding the birth of new stars.
FIELDMAPS used the HAWC+ polarimeter aboard SOFIA, which determines the alignment of dust, allowing astrophysicists to sense the direction of the magnetic field so it can be observed from afar. This enabled the largest and most detailed maps ever made of magnetic fields across galactic bones.
The group has more galactic bones to analyze, which they plan to compare with computer simulations of spiral galaxies. Together, these results will help develop a more thorough description of the role of magnetic fields in spiral galaxies’ arms.
SOFIA is a joint project of NASA and the German Space Agency at DLR. DLR provides the telescope, scheduled aircraft maintenance, and other support for the mission. NASA’s Ames Research Center in California’s Silicon Valley manages the SOFIA program, science, and mission operations in cooperation with the Universities Space Research Association, headquartered in Columbia, Maryland, and the German SOFIA Institute at the University of Stuttgart. The aircraft is maintained and operated by NASA’s Armstrong Flight Research Center Building 703, in Palmdale, California.
