NASA will share a new image or spectrum from the James Webb Space Telescope at least every other week on the mission’s blog. This week, check the blog on Thursday, Dec. 1 at 11 a.m. EST for new images highlighting one of Saturn’s moons.
In the meantime, learn more about what to expect as Webb observations make their way from raw data to published, peer-reviewed science.
News Media Contacts
Alise Fisher
Headquarters, Washington
202-358-2546 alise.m.fisher@nasa.gov
Laura Betz
Goddard Space Flight Center, Greenbelt, Md.
301-286-9030 laura.e.betz@nasa.gov
Micrometeoroid strikes are an unavoidable aspect of operating any spacecraft. NASA’s James Webb Space Telescope was engineered to withstand continual bombardment from these dust-sized particles moving at extreme velocities, to continue to generate groundbreaking science far into the future.
“We have experienced 14 measurable micrometeoroid hits on our primary mirror, and are averaging one to two per month, as anticipated. The resulting optical errors from all but one of these were well within what we had budgeted and expected when building the observatory,” said Mike Menzel, Webb lead mission systems engineer at NASA’s Goddard Space Flight Center in Greenbelt, Maryland. “One of these was higher than our expectations and prelaunch models; however, even after this event our current optical performance is still twice as good as our requirements.”
To ensure all parts of the observatory continue to perform at their best, NASA convened a working group of optics and micrometeoroid experts from NASA Goddard‘s Webb team, the telescope’s mirror manufacturer, the Space Telescope Science Institute, and the NASA Meteoroid Environment Office at NASA’s Marshall Space Flight Center in Huntsville, Alabama. After thorough analysis, the team concluded the higher-energy impact observed in May was a rare statistical event both in terms of energy, and in hitting a particularly sensitive location on Webb’s primary mirror. To minimize future impacts of this magnitude, the team has decided that future observations will be planned to face away from what is now known as the ‘micrometeoroid avoidance zone.’
“Micrometeoroids that strike the mirror head on (moving opposite the direction the telescope is moving) have twice the relative velocity and four times the kinetic energy, so avoiding this direction when feasible will help extend the exquisite optical performance for decades,” said Lee Feinberg, Webb optical telescope element manager at NASA Goddard. This does not mean that these areas of the sky cannot be observed, only that observations of those objects will be more safely made at a different time in the year when Webb is in a different location in its orbit. Observations that are time critical, such as solar system targets, will still be done in the micrometeoroid avoidance zone if required. This adjustment to how Webb observations are scheduled will have a long-term statistical benefit.
The team will implement the micrometeoroid avoidance zone starting with Webb’s second year of science, or “Cycle 2.” More information and guidance for Cycle 2 is available on JWST Observer News.
-Thaddeus Cesari, NASA’s Goddard Space Flight Center
Editor’s Note: This post highlights data from Webb science in progress, which has not yet been through the peer-review process.
We spoke with Kristen McQuinn of Rutgers University, one of the lead scientists on Webb Early Release Science (ERS) program 1334, focused on resolved stellar populations. These are large groups of stars – including stars within the dwarf galaxy Wolf–Lundmark–Melotte (WLM) – that are close enough for Webb to differentiate between individual stars, but far enough for Webb to capture a large number of stars at once.
A portion of the dwarf galaxy Wolf–Lundmark–Melotte (WLM) captured by the Spitzer Space Telescope’s Infrared Array Camera (left) and the James Webb Space Telescope’s Near-Infrared Camera (right). The images demonstrate Webb’s remarkable ability to resolve faint stars outside the Milky Way. The Spitzer image shows 3.6-micron light in cyan and 4.5-micron in orange (IRAC1 and IRAC2). The Webb image includes 0.9-micron light shown in blue, 1.5-micron in cyan, 2.5-micron in yellow, and 4.3-micron in red (filters F090W, F150W, F250M, and F430M). Download the full-resolution version from the Space Telescope Science Institute. SCIENCE CREDIT: NASA, ESA, CSA, STScI, and Kristen McQuinn (Rutgers University). IMAGE PROCESSING: Alyssa Pagan (STScI).
So, tell us a bit about this galaxy, WLM. What’s interesting about it?
WLM is a dwarf galaxy in our galactic neighborhood. It’s fairly close to the Milky Way (only about 3 million light-years from Earth), but it’s also relatively isolated. We think WLM hasn’t interacted with other systems, which makes it really nice for testing our theories of galaxy formation and evolution. Many of the other nearby galaxies are intertwined and entangled with the Milky Way, which makes them harder to study.
Another interesting and important thing about WLM is that its gas is similar to the gas that made up galaxies in the early universe. It’s fairly unenriched, chemically speaking. (That is, it’s poor in elements heavier than hydrogen and helium.)
This is because the galaxy has lost many of these elements through something we call galactic winds. Although WLM has been forming stars recently – throughout cosmic time, really – and those stars have been synthesizing new elements, some of the material gets expelled from the galaxy when the massive stars explode. Supernovae can be powerful and energetic enough to push material out of small, low-mass galaxies like WLM.
This makes WLM super interesting in that you can use it to study how stars form and evolve in small galaxies like those in the ancient universe.
You arranged to show this image at a planetarium. How did you feel when you saw the image projected on the dome?
It was just inspiring. It really was incredible. I will never look at these images the same again. Seeing this on the dome, it was like looking up at our own night sky – at the Milky Way – from a dark site. I could imagine that we were standing on a planet in the WLM galaxy and looking up at its night sky.
We can see a myriad of individual stars of different colors, sizes, temperatures, ages, and stages of evolution; interesting clouds of nebular gas within the galaxy; foreground stars with Webb’s diffraction spikes; and background galaxies with neat features like tidal tails. It’s really a gorgeous image.
And, of course, the view is far deeper and better than our eyes could possibly see. Even if you were looking out from a planet in the middle of this galaxy, and even if you could see infrared light, you would need bionic eyes to be able to see what Webb sees.
What are you trying to find out by studying WLM?
The main science focus is to reconstruct the star formation history of this galaxy. Low-mass stars can live for billions of years, which means that some of the stars that we see in WLM today formed in the early universe. By determining the properties of these low-mass stars (like their ages), we can gain insight into what was happening in the very distant past. It’s very complementary to what we learn about the early formation of galaxies by looking at high-redshift systems, where we see the galaxies as they existed when they first formed.
The Early Release Science programs were designed to highlight Webb’s capabilities and help astronomers prepare for future observations. How are you supporting other astronomers with this work?
In a few ways. We’re checking the calibration of the NIRCam instrument itself. We’re checking our stellar evolution models. And we’re developing software to measure star brightnesses.
We already studied this exact same field very carefully with Hubble. Now we’re looking at the near-infrared light with Webb, and we’re using WLM as a sort of standard for comparison (like you would use in a lab) to help us make sure we understand the Webb observations. We want to make sure we’re measuring the stars’ brightnesses really, really accurately and precisely. We also want to make sure that we understand our stellar evolution models in the near-infrared.
Our team is also charged with developing a public software tool to measure the brightness of all the resolved stars in the NIRCam images. This is a non-proprietary tool that everyone will be able to use. We are developing and testing the software, and optimizing the parameters used for measurements. This is a bedrock tool for astronomers around the world. If you want to do anything with resolved stars that are crowded together on the sky, you need a tool like this.
About the Author
Kristen McQuinn is an assistant professor in the Department of Physics and Astronomy at Rutgers University, and co-investigator on Director’s Discretionary Early Release Science program 1334.
The James Webb Space Telescope’s Mid-Infrared Instrument (MIRI) has four observing modes. On Aug. 24, after measuring increased friction in one of the grating wheels used in MIRI’s medium resolution spectrometry (MRS) mode, the Webb team paused science observations using this specific mode. Since then, a team of experts has carried out an in-depth investigation that has reviewed instrument design as well as historical and postlaunch data.
The team concluded the issue is likely caused by increased contact forces between sub-components of the wheel central bearing assembly under certain conditions. Based on this, the team developed and vetted a plan for how to use the affected mechanism during science operations.
An engineering test was executed Wednesday, Nov. 2, that successfully demonstrated predictions for wheel friction. Webb will resume MIRI MRS science observations by Saturday, Nov. 12, starting with a unique opportunity to observe Saturn’s polar regions, just before they become unobservable by Webb for the next 20 years. The team will schedule additional MRS science observations, initially at a limited cadence, following a plan to keep the affected wheel in balance, monitor wheel health, and prepare MIRI MRS for a return to full science operations.
NASA will share a new image or spectrum from the James Webb Space Telescope at least every other week on the mission’s blog. This week, check the blog on Wednesday, Nov. 9 at 11 a.m. EST for a new image highlighting a nearby dwarf galaxy.
In the meantime, learn more about what to expect as Webb observations make their way from raw data to published, peer-reviewed science.
