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By NASA
5 min read
Preparations for Next Moonwalk Simulations Underway (and Underwater)
A super pressure balloon with the EUSO-2 payload is prepared for launch from Wānaka, New Zealand, during NASA’s campaign in 2023.NASA/Bill Rodman NASA’s Scientific Balloon Program has returned to Wānaka, New Zealand, for two scheduled flights to test and qualify the agency’s super pressure balloon technology. These stadium-sized, heavy-lift balloons will travel the Southern Hemisphere’s mid-latitudes for planned missions of 100 days or more.
Launch operations are scheduled to begin in late March from Wānaka Airport, NASA’s dedicated launch site for mid-latitude, ultra long-duration balloon missions.
“We are very excited to return to New Zealand for this campaign to officially flight qualify the balloon vehicle for future science investigations,” said Gabriel Garde, chief of NASA’s Balloon Program Office at the agency’s Wallops Flight Facility in Virginia. “Our dedicated team both in the field and at home has spent years in preparation for this opportunity, and it has been through their hard work, fortitude, and passion that we are back and fully ready for the upcoming campaign.”
While the primary flight objective is to test and qualify the super pressure balloon technology, the flights will also host science missions and technology demonstrations. The High-altitude Interferometer Wind Observation (HIWIND), led by High Altitude Observatory, National Center for Atmospheric Research in Boulder, Colorado, will fly as a mission of opportunity on the first flight. The HIWIND payload will measure neutral wind in the part of Earth’s atmosphere called the thermosphere. Understanding these winds will help scientists predict changes in the ionosphere, which can affect communication and navigation systems. The second flight will support several piggyback missions of opportunity, or smaller payloads, including:
Compact Multichannel Imaging Camera (CoMIC), led by University of Massachusetts Lowell, will study and measure how Earth’s atmosphere scatters light at high altitudes and will measure airglow, specifically the red and green emissions. High-altitude Infrasound from Geophysical Sources (HIGS), led by NASA’s Jet Propulsion Laboratory and Sandia National Laboratories, will measure atmospheric pressure to collect signals of geophysical events on Earth such as earthquakes and volcanic eruptions. These signals will help NASA as it develops the ability to measure seismic activity on Venus from high-altitude balloons. Measuring Ocean Acoustics North of Antarctica (MOANA), led by Sandia National Laboratories and Swedish Institute of Space Physics, aims to capture sound waves in Earth’s stratosphere with frequencies below the limit of human hearing. NASA’s Balloon Program Office at the agency’s Wallops Flight Facility is leading two technology demonstrations on the flight. The INterim Dynamics Instrumentation for Gondolas (INDIGO) is a data recorder meant to measure the shock of the gondola during the launch, termination, and landing phases of flight. The Sensor Package for Attitude, Rotation, and Relative Observable Winds – 7 (SPARROW-7), will demonstrate relative wind measurements using an ultrasonic device designed for the balloon float environment that measures wind speed and direction. NASA’s 18.8-million-cubic-foot (532,000-cubic-meter) helium-filled super pressure balloon, when fully inflated, is roughly the size of Forsyth-Barr Stadium in Dunedin, New Zealand, which has a seating capacity of more than 35,000. The balloon will float at an altitude of around 110,000 feet (33.5 kilometers), more than twice the altitude of a commercial airplane. Its flight path is determined by the speed and direction of wind at its float altitude.
The balloon is a closed system design to prevent gas release. It offers greater stability at float altitude with minimum altitude fluctuations during the day to night cycle compared to a zero pressure balloon. This capability will enable future missions to affordably access the near-space environment for long-duration science and technology research from the Southern Hemisphere’s mid-latitudes, including nighttime observations.
The public is encouraged to follow real-time tracking of the balloons’ paths as they circle the globe on the agency’s Columbia Scientific Balloon Facility website. Launch and tracking information will be shared across NASA’s social media platforms and the NASA Wallops blog.
NASA’s return to Wānaka marks the sixth super pressure balloon campaign held in New Zealand since the agency began balloon operations there in 2015. The launches are conducted in collaboration with the Queenstown Airport Corporation, Queenstown Lake District Council, New Zealand Space Agency, and Airways New Zealand.
“We are especially grateful to our local hosts, partners, and collaborators who have been with us from the beginning and are critical to the success of these missions and this campaign,” said Garde.
NASA’s Wallops Flight Facility in Virginia manages the agency’s scientific balloon flight program with 10 to 16 flights each year from launch sites worldwide. Peraton, which operates NASA’s Columbia Scientific Balloon Facility in Palestine, Texas, provides mission planning, sustaining engineering services, and field operations for NASA’s scientific balloon program. The Columbia team has launched more than 1,700 scientific balloons over some 40 years of operations. NASA’s balloons are fabricated by Aerostar. The NASA Scientific Balloon Program is funded by the NASA Headquarters Science Mission Directorate Astrophysics Division.
For more information on NASA’s Scientific Balloon Program, visit:
www.nasa.gov/scientificballoons.
By Olivia Littleton
NASA’s Wallops Flight Facility, Wallops Island, Va.
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Last Updated Mar 14, 2025 EditorOlivia F. LittletonContactOlivia F. Littletonolivia.f.littleton@nasa.govLocationWallops Flight Facility Related Terms
Scientific Balloons Astrophysics Astrophysics Division Goddard Space Flight Center Wallops Flight Facility Explore More
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By European Space Agency
The European Space Agency is releasing the first catalogue of astronomical data from the Euclid space telescope, including three new enormous image mosaics with zoom-ins. Follow the reveal live on Wednesday 19 March at 11:00 BST / 12:00 CET.
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By European Space Agency
The European Space Agency has unveiled the ESA Space HPC, a new resource for space in Europe. ESA Director General Josef Aschbacher was joined by ESA Council Chair Renato Krpoun and ASI president Teodoro Valente to cut the ribbon at ESA’s establishment in Italy, ESRIN.
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By European Space Agency
Help us uncover the secrets of the Sun! Our Solar Orbiter spacecraft has been watching the Sun since February 2020. With five years’ worth of data waiting to be explored, it’s time to dig in. The new ‘Solar Radio Burst Tracker’ Zooniverse project is ready for you.
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By NASA
Explore This Section Webb News Latest News Latest Images Blog (offsite) Awards X (offsite – login reqd) Instagram (offsite – login reqd) Facebook (offsite- login reqd) Youtube (offsite) Overview About Who is James Webb? Fact Sheet Impacts+Benefits FAQ Science Overview and Goals Early Universe Galaxies Over Time Star Lifecycle Other Worlds Observatory Overview Launch Orbit Mirrors Sunshield Instrument: NIRCam Instrument: MIRI Instrument: NIRSpec Instrument: FGS/NIRISS Optical Telescope Element Backplane Spacecraft Bus Instrument Module Multimedia About Webb Images Images Videos What is Webb Observing? 3d Webb in 3d Solar System Podcasts Webb Image Sonifications Team International Team People Of Webb More For the Media For Scientists For Educators For Fun/Learning 6 Min Read NASA’s Webb Peers Deeper into Mysterious Flame Nebula
This collage of images from the Flame Nebula shows a near-infrared light view from NASA’s Hubble Space Telescope on the left, while the two insets at the right show the near-infrared view taken by NASA’s James Webb Space Telescope. Credits:
NASA, ESA, CSA, M. Meyer (University of Michigan), A. Pagan (STScI) The Flame Nebula, located about 1,400 light-years away from Earth, is a hotbed of star formation less than 1 million years old. Within the Flame Nebula, there are objects so small that their cores will never be able to fuse hydrogen like full-fledged stars—brown dwarfs.
Brown dwarfs, often called “failed stars,” over time become very dim and much cooler than stars. These factors make observing brown dwarfs with most telescopes difficult, if not impossible, even at cosmically short distances from the Sun. When they are very young, however, they are still relatively warmer and brighter and therefore easier to observe despite the obscuring, dense dust and gas that comprises the Flame Nebula in this case.
NASA’s James Webb Space Telescope can pierce this dense, dusty region and see the faint infrared glow from young brown dwarfs. A team of astronomers used this capability to explore the lowest mass limit of brown dwarfs within the Flame Nebula. The result, they found, were free-floating objects roughly two to three times the mass of Jupiter, although they were sensitive down to 0.5 times the mass of Jupiter.
“The goal of this project was to explore the fundamental low-mass limit of the star and brown dwarf formation process. With Webb, we’re able to probe the faintest and lowest mass objects,” said lead study author Matthew De Furio of the University of Texas at Austin.
Image A: Flame Nebula: Hubble and Webb Observations
This collage of images from the Flame Nebula shows a near-infrared light view from NASA’s Hubble Space Telescope on the left, while the two insets at the right show the near-infrared view taken by NASA’s James Webb Space Telescope. Much of the dark, dense gas and dust, as well as the surrounding white clouds within the Hubble image, have been cleared in the Webb images, giving us a view into a more translucent cloud pierced by the infrared-producing objects within that are young stars and brown dwarfs. Astronomers used Webb to take a census of the lowest-mass objects within this star-forming region.
The Hubble image on the left represents light at wavelengths of 1.05 microns (filter F105W) as blue, 1.3 microns (F130N) as green, and 1.39 microns (F129M) as red. The two Webb images on the right represent light at wavelengths of 1.15 microns and 1.4 microns (filters F115W and F140M) as blue, 1.82 microns (F182M) as green, 3.6 microns (F360M) as orange, and 4.3 microns (F430M) as red. NASA, ESA, CSA, M. Meyer (University of Michigan), A. Pagan (STScI) Smaller Fragments
The low-mass limit the team sought is set by a process called fragmentation. In this process large molecular clouds, from which both stars and brown dwarfs are born, break apart into smaller and smaller units, or fragments.
Fragmentation is highly dependent on several factors with the balance between temperature, thermal pressure, and gravity being among the most important. More specifically, as fragments contract under the force of gravity, their cores heat up. If a core is massive enough, it will begin to fuse hydrogen. The outward pressure created by that fusion counteracts gravity, stopping collapse and stabilizing the object (then known as a star). However, fragments whose cores are not compact and hot enough to burn hydrogen continue to contract as long as they radiate away their internal heat.
“The cooling of these clouds is important because if you have enough internal energy, it will fight that gravity,” says Michael Meyer of the University of Michigan. “If the clouds cool efficiently, they collapse and break apart.”
Fragmentation stops when a fragment becomes opaque enough to reabsorb its own radiation, thereby stopping the cooling and preventing further collapse. Theories placed the lower limit of these fragments anywhere between one and ten Jupiter masses. This study significantly shrinks that range as Webb’s census counted up fragments of different masses within the nebula.
“As found in many previous studies, as you go to lower masses, you actually get more objects up to about ten times the mass of Jupiter. In our study with the James Webb Space Telescope, we are sensitive down to 0.5 times the mass of Jupiter, and we are finding significantly fewer and fewer things as you go below ten times the mass of Jupiter,” De Furio explained. “We find fewer five-Jupiter-mass objects than ten-Jupiter-mass objects, and we find way fewer three-Jupiter-mass objects than five-Jupiter-mass objects. We don’t really find any objects below two or three Jupiter masses, and we expect to see them if they are there, so we are hypothesizing that this could be the limit itself.”
Meyer added, “Webb, for the first time, has been able to probe up to and beyond that limit. If that limit is real, there really shouldn’t be any one-Jupiter-mass objects free-floating out in our Milky Way galaxy, unless they were formed as planets and then ejected out of a planetary system.”
Image B: Low Mass Objects within the Flame Nebula in Infrared Light
This near-infrared image of a portion of the Flame Nebula from NASA’s James Webb Space Telescope highlights three low-mass objects, seen in the insets to the right. These objects, which are much colder than protostars, require the sensitivity of Webb’s instruments to detect them. These objects were studied as part of an effort to explore the lowest mass limit of brown dwarfs within the Flame Nebula.
The Webb images represent light at wavelengths of 1.15 microns and 1.4 microns (filters F115W and F140M) as blue, 1.82 microns (F182M) as green, 3.6 microns (F360M) as orange, and 4.3 microns (F430M) as red. NASA, ESA, CSA, STScI, M. Meyer (University of Michigan) Building on Hubble’s Legacy
Brown dwarfs, given the difficulty of finding them, have a wealth of information to provide, particularly in star formation and planetary research given their similarities to both stars and planets. NASA’s Hubble Space Telescope has been on the hunt for these brown dwarfs for decades.
Even though Hubble can’t observe the brown dwarfs in the Flame Nebula to as low a mass as Webb can, it was crucial in identifying candidates for further study. This study is an example of how Webb took the baton—decades of Hubble data from the Orion Molecular Cloud Complex—and enabled in-depth research.
“It’s really difficult to do this work, looking at brown dwarfs down to even ten Jupiter masses, from the ground, especially in regions like this. And having existing Hubble data over the last 30 years or so allowed us to know that this is a really useful star-forming region to target. We needed to have Webb to be able to study this particular science topic,” said De Furio.
“It’s a quantum leap in our capabilities between understanding what was going on from Hubble. Webb is really opening an entirely new realm of possibilities, understanding these objects,” explained astronomer Massimo Robberto of the Space Telescope Science Institute.
This team is continuing to study the Flame Nebula, using Webb’s spectroscopic tools to further characterize the different objects within its dusty cocoon.
“There’s a big overlap between the things that could be planets and the things that are very, very low mass brown dwarfs,” Meyer stated. “And that’s our job in the next five years: to figure out which is which and why.”
These results are accepted for publication in The Astrophysical Journal Letters.
Image C (Animated): Flame Nebula (Hubble and Webb Comparison)
This animated image alternates between a Hubble Space Telescope and a James Webb Space Telescope observation of the Flame Nebula, a nearby star-forming nebula less than 1 million years old. In this comparison, three low-mass objects are highlighted. In Hubble’s observation, the low-mass objects are hidden by the region’s dense dust and gas. However, the objects are brought out in the Webb observation due to Webb’s sensitivity to faint infrared light. NASA, ESA, CSA, Alyssa Pagan (STScI) The James Webb Space Telescope is the world’s premier space science observatory. Webb is solving mysteries in our solar system, looking beyond to distant worlds around other stars, and probing the mysterious structures and origins of our universe and our place in it. Webb is an international program led by NASA with its partners, ESA (European Space Agency) and CSA (Canadian Space Agency).
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Media Contacts
Laura Betz – laura.e.betz@nasa.gov
NASA’s Goddard Space Flight Center, Greenbelt, Md.
Matthew Brown – mabrown@stsci.edu
Space Telescope Science Institute, Baltimore, Md.
Christine Pulliam – cpulliam@stsci.edu
Space Telescope Science Institute, Baltimore, Md.
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Last Updated Mar 10, 2025 Editor Marty McCoy Contact Laura Betz laura.e.betz@nasa.gov Related Terms
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