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World desk7 min

How Astronomers Use Webb and Hubble to Study Star-Forming Regions

Hubble traces young stars, glowing gas and jets; Webb’s infrared observations reveal more of the stars and dusty material hidden inside stellar nurseries. Together, images and spectra provide complementary evidence about star formation.
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Astronomers use Hubble and the James Webb Space Telescope together because each reveals a different part of a star-forming region. Hubble’s ultraviolet and visible observations show young stars, glowing gas and jets; Webb’s near- and mid-infrared observations reveal more of the stars and dusty material hidden inside clouds. Comparing images and spectra across these wavelengths helps scientists build a more complete picture than any single view can provide.

Why use two telescopes to study star formation?

Stars form inside clouds of gas and dust. As a young star takes shape, it can illuminate nearby gas, drive outflows and affect the material around it. But the cloud that gives rise to a star can also hide it: dust scatters or absorbs much visible light, making an embedded young star difficult to see in an optical image. Infrared light is less hindered by dust, so observations at infrared wavelengths can reveal features that visible-light observations miss. Infrared observations still have limits; they do not pass through every cloud without obstruction. NASA explains the difference in its overview of infrared astronomy.

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Hubble and Webb are therefore complementary observatories, not competing versions of the same instrument. Hubble observes ultraviolet, visible and some near-infrared light. Webb is optimized for near- and mid-infrared observations. Their different wavelength coverage brings different stars, gas and dust into view, letting astronomers compare the visible effects of star formation with structures deeper in the dusty region.

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What does each telescope reveal?

Observatory Wavelength coverage emphasized in star-formation studies What the observations can show
Hubble Ultraviolet and visible light, with some near-infrared capability Young stars that shine brightly in ultraviolet light; visible structure in clouds; ionized gas illuminated by young stars; and shock waves associated with jets. Some near-infrared light can escape from embedded regions. NASA describes these uses in its overview of Hubble observations of star birth.
Webb Near- and mid-infrared light Near-infrared observations can reveal very young stars within dusty stellar nurseries; mid-infrared observations help astronomers study dust and cooler material. NASA describes Webb’s infrared role in its star lifecycle overview.

The contrast is especially clear in NASA’s comparison of the Pillars of Creation. In Hubble’s visible-light view, dust blocks much of what lies inside the pillars. Webb’s near-infrared NIRCam view shows more structure and embedded stars, while Webb’s mid-infrared view emphasizes dusty material. The images differ because each wavelength responds to different material and processes—not because one is a complete picture and the other is an incomplete one.

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How do Webb and Hubble work together?

A multiwavelength study starts with a scientific question. Astronomers might want to locate young stars, examine how those stars affect the surrounding cloud, or investigate the properties of material within a nebula. They select observations that address the question, then compare what appears in each wavelength band. A bright feature in one image may be faint, obscured or absent in another because the telescopes are tracing different parts of the region.

1. Map the visible activity

Hubble’s ultraviolet and visible observations can show young stars and the gas they illuminate. They can also reveal cloud structure, ionized material and shock waves from jets. These views help astronomers examine the exposed effects of young stars and how those effects extend into nearby gas. Hubble’s near-infrared capability can add information from some regions where visible light has difficulty escaping.

2. Look for stars and material concealed by dust

Webb’s near-infrared observations can uncover young stars that are difficult to see in visible light because they are embedded in dusty surroundings. Its mid-infrared observations provide another way to study dust and cooler material. NASA describes Webb’s infrared capability as allowing it to “probe deeply into star-forming regions to study the conditions that lead to new stellar systems” in its Science with Webb overview.

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3. Compare features across wavelengths

When astronomers compare images, they can see which features are shared across bands and which become prominent only at particular wavelengths. A structure visible in Hubble’s optical view may trace illuminated or ionized gas, while a feature prominent in Webb’s infrared view may be associated with embedded stars or dusty material. The comparison provides context: a single image shows the emission and absorption captured by its filters, not every component of the region.

4. Choose an instrument mode for the question

Webb’s instruments include cameras and spectrographs with specialized observing modes. NIRCam provides near-infrared imaging; MIRI observes mid-infrared light and has camera and spectrograph capability; NIRSpec and NIRISS provide additional near-infrared spectroscopy modes. These instruments are not interchangeable in every respect. Astronomers select a mode according to what they need to measure, as outlined in NASA’s guide to Webb’s scientific instruments.

Can Webb see through dust?

Webb can observe infrared light that is less hindered by dust than visible light, making it possible to detect some stars and structures hidden in optical images. “Less hindered” is not the same as unobstructed: dense material can still absorb or block light, and a feature’s visibility depends on the wavelength and the material along the line of sight. Webb also does not make dust disappear. Its mid-infrared observations can help astronomers study dusty material itself.

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It is useful to think of infrared observations as changing the view rather than simply removing a veil. Dust may obscure a background star in one band, emit or affect the signal in another, and coexist with gas and stars that produce their own light. A Webb image can therefore reveal embedded objects while also emphasizing the dust around them. The result complements visible and ultraviolet views rather than replacing them.

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What can infrared images reveal about star formation?

Infrared images can help astronomers identify young stars within dusty stellar nurseries and examine the distribution of material that is hard to study in visible light. Near- and mid-infrared observations are not identical: Webb’s near-infrared view can reveal embedded stars and structure, while its mid-infrared view helps bring dusty and cooler material into focus. Comparing both with Hubble’s ultraviolet and visible views helps distinguish the exposed effects of young stars from activity occurring deeper inside the cloud.

NASA’s FAQ gives broad wavelength ranges of approximately 0.7–5 micrometers for near-infrared, 5–30 micrometers for mid-infrared, and 30–1000 micrometers for far infrared. These are general band descriptions, not instrument-performance limits. Webb is sensitive to near- and mid-infrared radiation; the broad ranges should not be used as substitutes for an instrument’s technical specifications. The figures are listed in NASA’s Webb FAQs.

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Images are often displayed as color composites, but a displayed color may represent a filter or wavelength band rather than the color a human eye would see. This matters when interpreting a multiwavelength image: its colors are a way to encode measurements for viewing, and the mapping between wavelength and displayed color determines what a particular hue means. Unless an image’s documentation establishes otherwise, its colors should not be treated as a literal view of the nebula’s appearance to the human eye.

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What do astronomers learn from spectra?

An image maps the position and apparent structure of light in a region. A spectrum separates light by wavelength, giving astronomers another kind of evidence: how the light varies across those wavelengths. Spectroscopy can be used to investigate properties such as composition, temperature and motion. It helps answer questions that an image’s shape or color alone cannot settle.

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Webb’s spectrographs and observing modes allow astronomers to select an approach suited to a particular question. For example, a study that needs spectral information uses a spectroscopic mode rather than relying only on a camera image. The precise result depends on the observation and its analysis; the general ability to study a property is not evidence that a particular molecule or value was measured in every nebula. NASA describes the capabilities and modes of Webb’s instruments in its instrument guide.

How do young stars change their surroundings?

Young stars do not merely form within clouds; their ultraviolet radiation and winds can alter the surrounding material. They may disrupt and disperse parts of a cloud. In some circumstances, the pressure from these effects can compress gas and contribute to further star formation. NASA’s overview of Webb’s star-formation discoveries describes both possible outcomes.

That range of effects is important when interpreting images. A bright edge, shell or compressed-looking feature does not, by itself, prove that a particular star triggered a new generation of stars. Astronomers use observations and physical analysis to assess whether a region is being disrupted, compressed or affected in another way. Hubble’s views of illuminated gas and shocks, combined with Webb’s views of embedded stars and dust, provide complementary clues, but the interpretation depends on the evidence for that specific region.

Why a single image is not the whole story

Every observation is shaped by what the telescope detects, the wavelength band selected and the method used. A visible image may emphasize illuminated gas or young stars while missing objects buried in dust. An infrared image may reveal those objects yet give a different emphasis to dust and cooler material. A spectrum adds wavelength-dependent information that an image does not provide in the same way. These are different measurements, not alternate aesthetic treatments of an identical scene.

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For that reason, the most useful question is not which telescope produces the “best” picture. It is what the observation is designed to reveal. Hubble can trace ultraviolet, visible and some near-infrared signals from young stars and their surroundings; Webb can add near- and mid-infrared views of embedded stars and dusty material. Together, their observations help astronomers investigate both the visible effects of star formation and the regions that dust makes harder to examine.

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