Beneath the Night Sky in a Galaxy (Not Too) Far Away – Technology Org

Kristen McQuinn of Rutgers University, one of the lead scientists in Webb Early Release Science (ERS) program 1334, focused on resolved stellar populations, in this interview from NASA discusses a large groups of stars – including stars within the dwarf galaxy Wolf-Lundmark- Melotte (WLM) – 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 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 credit: 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 nice to test our theories of galaxy formation and evolution. Many other nearby galaxies are intertwined and entangled with the Milky Way, making 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 galactic winds. Although WLM has been forming stars recentlyThroughout cosmic time, 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 skyat the Milky Wayfrom 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 brightness.

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 Webb’s 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 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 measurement parameters. 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 the Director’s Discretionary Early Release Science program 1334.

Source: National Aeronautics and Space Administration


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