Brightest Cluster Galaxies Survey
Credit: X-ray: NASA/CXC/MIT/M. Calzadilla el al.; Optical: NASA/ESA/STScI;
Image Processing: NASA/CXC/SAO/N. Wolk & J. Major
These four images represent a sample of galaxy clusters that are part of the largest and most complete study to learn what triggers stars to form in the universe’s biggest galaxies, as described in our latest press release. This research, made using NASA’s Chandra X-ray Observatory and other telescopes, showed that the conditions for stellar conception in these exceptionally massive galaxies have not changed over the last ten billion years.
Galaxy clusters are the largest objects in the universe held together by gravity and contain huge amounts of hot gas seen in X-rays. This hot gas weighs several times the total mass of all the stars in all the hundreds of galaxies typically found in galaxy clusters. In the four galaxy cluster images in this graphic, X-rays from hot gas detected by Chandra are in purple and optical data from NASA’s Hubble Space Telescope, mostly showing galaxies in the clusters, are yellow and cyan.
Credit: X-ray: NASA/CXC/SAO; IR (Spitzer): NASA/JPL-Caltech; IR (Webb): NASA/ESA/CSA/STScI
Experts created two new visual and auditory experiences to explore the complexity and beauty of a compact galaxy group known as Stephan’s Quintet. The guided three-dimensional visualization surveys the galaxies — their structures, characteristics, and interactions — captured in multiple wavelengths of light by some of NASA’s great observatories. The sonifications scan two-dimensional images of the quintet, translating the data into sound to reveal the depth and richness this intricate environment holds.
Using data gathered by NASA’s Hubble Space Telescope, Spitzer Space Telescope, Chandra X-ray Observatory, and James Webb Space Telescope, astronomers and visualization specialists from across several institutions came together to create two new unique sensory experiences of a compact group of galaxies known as Stephan’s Quintet: a video guiding viewers through a three-dimensional visualization of the galaxies, and audio tracks based on two-dimensional observation images. These add to the previously-developed multi-wavelength images, large tactile/audio display table, and small tactile images, bolstering the overall sensory experience of Stephan’s Quintet.
Credit: X-ray: Chandra: NASA/SAO/Univ. of Alabama/M. S. Mirakhor et al.; XMM: ESA/XMM-Newton;
Optical: SDSS; Image processing: N. Wolk
A group of galaxies is plunging into the Coma galaxy cluster and leaving behind an enormous tail of superheated gas. Astronomers have confirmed this is the longest known tail behind a galaxy group and used it to gain a deeper understanding of how galaxy clusters – some of the largest structures in the universe – grow to their enormous sizes.
NGC 346, NGC 1672, M74 & M16
Credit: X-ray: Chandra: NASA/CXC/SAO, XMM: ESA/XMM-Newton; IR: JWST: NASA/ESA/CSA/STScI, Spitzer: NASA/JPL/CalTech; Optical: Hubble: NASA/ESA/STScI, ESO; Image Processing: L. Frattare, J. Major, N. Wolk, and K. Arcand
Four composite images deliver dazzling views from NASA's Chandra X-ray Observatory and James Webb Space Telescope of two galaxies, a nebula, and a star cluster. Each image combines Chandra's X-rays — a form of high-energy light — with infrared data from previously released Webb images, both of which are invisible to the unaided eye. Data from NASA's Hubble Space Telescope (optical light) and retired Spitzer Space Telescope (infrared), plus the European Space Agency's XMM-Newton (X-ray) and the European Southern Observatory's New Technology Telescope (optical) is also used. These cosmic wonders and details are made available by mapping the data to colors that humans can perceive.
Credit: X-ray: NASA/CXC/The Ohio State Univ/S. Lopez et al.; H-alpha and Optical: NSF/NOIRLab/AURA/KPNO/CTIO; Infrared: NASA/JPL-Caltech/Spitzer/D. Dale et al; Full Field Optical: ESO/La Silla Observatory.
On Earth, wind can transport particles of dust and debris across the planet, with sand from the Sahara ending up in the Caribbean or volcanic ash from Iceland being deposited in Greenland. Wind can also have a big impact on the ecology and environment of a galaxy, just like on Earth, but on much larger and more dramatic scales.
A new study using NASA's Chandra X-ray Observatory shows the effects of powerful winds launched from the center of a nearby galaxy, NGC 253, located 11.4 million light-years from Earth. This galactic wind is composed of gas with temperatures of millions of degrees that glows in X-rays. An amount of hot gas equivalent to about two million Earth masses blows away from the galaxy's center every year.
NGC 253 is a spiral galaxy, making it similar to our Milky Way. However, stars are forming in NGC 253 about two to three times more quickly than in our home galaxy. Some of these young stars are massive and generate a wind by ferociously blowing gas from their surfaces. Even more powerful winds are unleashed when, later in their relatively short lives, these stars explode as supernovae, and hurl waves of material out into space.
We are happy to welcome Valentina Missaglia as a guest blogger. She is the first author of the paper that is the subject of our latest press release. She is currently a postdoctoral researcher at the Institute of Astrophysics — FORTH in Heraklion (Crete) in the SMILE (“Search for Milli-LEnses”) group, recently funded by an ERC grant, that aims at investigating the nature of dark matter through observations of gravitational lenses on milli-arcsecond scales. Valentina earned her Ph.D. from the University of Turin (Italy) and her research focuses on radio and X-ray emission from radio-loud active galactic nuclei (which contain supermassive black holes that are rapidly pulling in material, producing intense radio waves) and how these sources interact with the surrounding medium. Before starting her Ph.D. in 2019, Valentina was a visiting student at the Center of Astrophysics | Harvard & Smithsonian, where she collaborated with Dr. Ralph Kraft on observations of galaxy clusters performed with NASA’s Chandra X-ray Observatory.
Looking at the night sky with the naked eye, we can only see an infinitesimal part of what the Universe contains, and the largest part cannot even be “seen”. Radio wavelengths have gifted us some of the most fascinating astronomical sources: radio-loud active galactic nuclei in the centers of galaxies, which can produce jets that extend way farther out from the optical galaxy itself.
The most powerful radio sources in the northern hemisphere are listed in a well- studied catalog, the Third Cambridge Catalog (3C), which contains the source we investigated with multiwavelength observations: 3C 297. This source appeared very intriguing in observations performed with Chandra in 2016. Therefore, we requested more time to better investigate features that we uncovered thanks to this first short observation, such as hot, X-ray emitting gas around our source.
SDSS J011522.18+001518.5 and SDSS J155627.74+241758.9
Credit: X-ray: NASA/CXC/SAO/D. Kim et al.; Optical/IR: Legacy Surveys/D. Lang (Perimeter Institute)
This panel of images represents a survey that used data from NASA’s Chandra X-ray Observatory to uncover hundreds of previously “hidden” black holes. This result helps astronomers conduct a more accurate census of supermassive black holes that exist in the centers of most large galaxies, as reported in our latest press release.
This graphic shows two of the galaxies from the new study, with Chandra X-ray data in purple and optical data from the Sloan Digital Sky Survey (SDSS) in red, green and blue. These black holes were found in galaxies that are dim in optical light, but bright in X-rays. Astronomers have dubbed these “XBONGs” (for X-ray bright, optically normal galaxies). While scientists have been aware of XBONGs for several decades, an explanation for their unusual properties has been unclear.
We are happy to welcome Vivienne Baldassare as our guest blogger. Vivienne is an Assistant Professor of Physics and Astronomy at Washington State University, and led the paper that is the subject of our latest press release. Her work is mainly focused on searching for the smallest supermassive black holes in order to learn more about black hole formation and growth. Prior to her current position, she was a NASA Einstein fellow at Yale University. She earned her PhD in Astronomy & Astrophysics from the University of Michigan in 2017, and a bachelor's degree in Physics from CUNY Hunter College in 2012.
One of the biggest open questions in astrophysics is “how do massive black holes form?” Our recent research with NASA’s Chandra X-ray Observatory provides support for the theory that massive black holes can form in what astronomers call nuclear star clusters.
While big galaxies have supermassive black holes at their centers, small galaxies often have a nuclear star cluster. Nuclear star clusters are extremely dense, with millions of stars packed into a region that is tens of light years across. It was once suggested that supermassive black holes and nuclear star clusters may be mutually exclusive, with the former residing in big galaxies and the latter occurring in small galaxies. However, some galaxies (like our Milky Way!) have been found to contain both. And excitingly, some theories suggest that nuclear star clusters might be able to form massive black holes.
In my first year of graduate school, I carried out a project studying the properties of nuclear star clusters. After that, I transitioned to studying massive black holes in dwarf galaxies, but have always had a soft spot for these fascinating objects. Our new study brought these two areas together.
This blog post was written by Julia Berndtsson, a Swedish physics student currently in the third year of her undergraduate studies at Princeton University in the United States. For our latest Chandra result, she collaborated with Rosanne Di Stefano at the Center for Astrophysics | Harvard & Smithsonian during her last year of high school and through the first half of her freshman year at Princeton. She is currently exploring a range of topics in physics and engineering and works with Jason Petta's group at Princeton on developing semiconducting qubits.
When one imagines a scientist, a high school student usually isn’t the first thing that comes to mind. What people may or may not know is that there are multiple summer programs aimed at students still in their secondary education to gain exposure to research in their natural sciences, and it is because of such a program I ended up joining Dr. Rosanne Di Stefano in writing a paper on the discovery of the first planet candidate in an external galaxy.
The summer before my senior year, I was admitted to the Center for Excellence in Education’s Research Science Institute where participants were matched with a research mentor and given a project to be carried out over six weeks. Meeting Rosanne for the first time had me in awe. Not only did she give the students she took on her full confidence, but she would talk with excitement both about the topics that we were examining and over the fact that you were there to work on these problems too.
We welcome Rosanne Di Stefano, an astrophysicist at the Center for Astrophysics | Harvard & Smithsonian, as our guest blogger. Her work has encompassed a broad range of astronomical systems: stars interacting within dense stellar environments, the binary evolution of possible progenitors of Type Ia supernovae, X-ray astronomy, and gravitational microlensing. In this post, she writes about her team’s finding of a possible planet candidate in M51, which is featured in our latest press release.
The discovery of a candidate planet in M51 (nicknamed the “Whirlpool” galaxy) represents several firsts. Perhaps most important, it is the first candidate planet in a distant galaxy. Since the 1750s, it has been conjectured that the dim distant nebulas, now called galaxies, are island universes: large, gravitationally-bound stellar populations similar to our home, the Milky Way. Since the work of Edwin Hubble in 1929, we have been able to study stars in other galaxies. Our discovery of the planet candidate — in a binary system called M51 ULS-1 — gives us the first peek into external populations of planetary systems, extending the reach of planet searches to distances roughly ten thousand times more distant.
The candidate planet is understood to be in the “circumbinary” orbit of a compact object (either a neutron star or a black hole) and a donor star, meaning that the donor and compact orbit one another and that the candidate planet orbits the mass center of these two. (We call it a “donor” star because the compact object is pulling material from its surface and into a disk around the neutron star or black hole.) This makes the planet candidate in M51 ULS-1 the first found to be orbiting a high-mass star. In our own Galaxy, astronomers have discovered more than 4800 planets, but the stars they orbit are less massive than about four times the mass of our own Sun. Stars can be very much more massive, however. While the exact value of the largest possible stellar mass in today’s Universe remains uncertain, it is at least 100 solar masses. The donor star in M51 ULS-1 appears to have the luminosity and spectrum of a 20 to 30 solar mass star.
Please note this is a moderated blog. No pornography, spam, profanity or discriminatory remarks are allowed. No personal attacks are allowed. Users should stay on topic to keep it relevant for the readers.
Read the privacy statement