Stephan’s Quintet is a visual grouping of five galaxies located in the constellation Pegasus. Together, they are also known as the Hickson Compact Group 92 (HCG 92). Although called a “quintet,” only four of the galaxies are truly close together and caught up in a cosmic dance. The fifth and leftmost galaxy, called NGC 7320, is well in the foreground compared with the other four.
Tight groups like this may have been more common in the early universe when their superheated, infalling material may have fueled very energetic black holes called quasars. Even today, the topmost galaxy in the group – NGC 7319 – harbors an active galactic nucleus, a supermassive black hole 24 million times the mass of the Sun. It is actively accreting material and puts out light energy equivalent to 40 billion Suns.
Scientists using NASA’s James Webb Space Telescope studied the active galactic nucleus in great detail with the Medium-Resolution Spectrometer (MRS), which is part of the Mid-Infrared Instrument (MIRI). The spectrometer features integral field units (IFUs) – a combination of a camera and spectrograph. These IFUs provided the Webb team with a “data cube,” or collection of images of the galactic core’s spectral features.
Using IFUs, scientists can measure spatial structures, determine the velocity of those structures, and get a full range of spectral data. Much like medical magnetic resonance imaging (MRI), the IFUs allow scientists to “slice and dice” the information into many images for detailed study.
MIRI’s MRS pierced through the shroud of dust near the active galactic nucleus to measure the bright emission from hot gas being ionized by powerful winds and radiation from the black hole. The instrument saw the gas near the supermassive black hole in wavelengths never studied before in so much detail, and it was able to determine its velocity.
Some of these key emission features are shown in this image. In each case, the blue-colored regions indicate movement toward the viewer and orange-colored regions represent movement away from the viewer. The argon and neon lines are from hot spots of super-heated gas that is highly ionized by the powerful radiation and winds from the supermassive black hole. The molecular hydrogen line is from colder dense gas in the central regions of the galaxy and entrained in the outflowing wind. The velocities are measured by shifts in the wavelengths of a given emission line feature.
MIRI was contributed by ESA and NASA, with the instrument designed and built by a consortium of nationally funded European Institutes (The MIRI European Consortium) in partnership with JPL and the University of Arizona.
For a full array of Webb’s first images and spectra, including downloadable files, please visit: https://webbtelescope.org/news/first-images
Credits
Image
NASA, ESA, CSA, STScI
| About The Object | |
|---|---|
| Object Name | Stephan’s Quintet, Hickson Compact Group (HCG) 92 |
| Object Description | Interacting Galaxy Group |
| R.A. Position | 22:35:57.49 |
| Dec. Position | 33:57:36.0 |
| Constellation | Pegasus |
| Distance | 290 million light-years (89 million parsecs) |
| About The Data | |
| Data Description | This image was created with Webb data from proposal . It is part of Webb Early Release Observations. The Early Release Observations and associated materials were developed, executed, and compiled by the ERO production team: Jaclyn Barrientes, Claire Blome, Hannah Braun, Matthew Brown, Margaret Carruthers, Dan Coe, Joseph DePasquale, Nestor Espinoza, Macarena Garcia Marin, Karl Gordon, Alaina Henry, Leah Hustak, Andi James, Ann Jenkins, Anton Koekemoer, Stephanie LaMassa, David Law, Alexandra Lockwood, Amaya Moro-Martin, Susan Mullally, Alyssa Pagan, Dani Player, Klaus Pontoppidan, Charles Proffitt, Christine Pulliam, Leah Ramsay, Swara Ravindranath, Neill Reid, Massimo Robberto, Elena Sabbi, Leonardo Ubeda. The EROs were also made possible by the foundational efforts and support from the JWST instruments, STScI planning and scheduling, Data Management teams, and Office of Public Outreach. |
| Instrument | NIRCam, MIRI |
| About The Object | |
|---|---|
| Object Name | A name or catalog number that astronomers use to identify an astronomical object. |
| Object Description | The type of astronomical object. |
| R.A. Position | Right ascension – analogous to longitude – is one component of an object's position. |
| Dec. Position | Declination – analogous to latitude – is one component of an object's position. |
| Constellation | One of 88 recognized regions of the celestial sphere in which the object appears. |
| Distance | The physical distance from Earth to the astronomical object. Distances within our solar system are usually measured in Astronomical Units (AU). Distances between stars are usually measured in light-years. Interstellar distances can also be measured in parsecs. |
| Dimensions | The physical size of the object or the apparent angle it subtends on the sky. |
| About The Data | |
| Data Description |
|
| Instrument | The science instrument used to produce the data. |
| Exposure Dates | The date(s) that the telescope made its observations and the total exposure time. |
| Filters | The camera filters that were used in the science observations. |
| About The Image | |
| Image Credit | The primary individuals and institutions responsible for the content. |
| Publication Date | The date and time the release content became public. |
| Color Info | A brief description of the methods used to convert telescope data into the color image being presented. |
| Orientation | The rotation of the image on the sky with respect to the north pole of the celestial sphere. |
