Showing posts with label Andromeda Galaxy. Show all posts
Showing posts with label Andromeda Galaxy. Show all posts

Thursday, February 27, 2025

New dwarf galaxy discovered in the halo of Andromeda galaxy

A series of plots showing the tentative detection of a candidate stellar overdensity (Pegasus VII) in the UNIONS photometric catalogs. Credit: arXiv (2025). DOI: 10.48550/arxiv.2502.09792


An international team of astronomers reports the discovery of a new dwarf galaxy, which they have named Pegasus VII. The newfound galaxy, which lies about 2.4 million light years away, was identified in the Ultraviolet Near-Infrared Optical Northern Survey (UNIONS). The discovery was detailed in a research paper published Feb. 13 on the arXiv preprint server.

Dwarf galaxies are low-luminosity and low-mass stellar systems, usually containing a few billion stars. Their formation and activity are thought to be heavily influenced by interactions with larger galaxies.

One of the great places to look for dwarf galaxies is the halo of the Andromeda galaxy (also known as Messier 31, or M31 for short), due to its relative proximity. UNIONS is so far the deepest available survey for exploring the far reaches of this galaxy's halo and now a team of astronomers led by Simon E. T. Smith of the University of Victoria in Canada, has found another such dwarf.

"We present the newly discovered dwarf galaxy Pegasus VII (Peg VII), a member of the M31 sub-group which has been uncovered in the ri photometric catalogs from the Ultraviolet Near-Infrared Optical Northern Survey and confirmed with follow-up imaging from both the Canada-France-Hawaii Telescope and the Gemini-North Telescope," the researchers wrote in the paper.

Pegasus VII was identified at a separation of about 1.08 million light years from the Andromeda galaxy. Therefore, Pegasus VII is just about to cross the virial radius of Andromeda and has likely been isolated up until this point.

According to the study, Pegasus VII has an absolute V-band magnitude of −5.7 mag, a central surface of 27.3 mag/arcsec2, and a physical half-light radius of approximately 577 light years. This means that Pegasus VII is the faintest known dwarf galaxy satellite of Andromeda and roughly five times larger than the most extended globular clusters in this galaxy.

The study found that Pegasus VII has an ellipticity at a level of 0.5 and this projected elongation is aligned within 18 degrees of the projected direction towards Andromeda. The astronomers suppose that the source of this elongation is a previous tidal interaction with the gravitational potential of the Andromeda galaxy.

Furthermore, the researchers calculated that Pegasus VII has a total stellar mass of 26,000 solar masses and its metallicity is at a level of -2.0 dex. The age of the dwarf galaxy was estimated to be around 10 billion years.

Summing up the results, the authors of the paper concluded that they hope to find many more dwarf galaxies in the halo of Andromeda.

"The discovery of Pegasus VII complements both the empirical and theoretical claim that a wealth of dwarf galaxy satellites remain undetected towards M31," the scientists wrote.

by Tomasz Nowakowski (Phys.org)





More information: Simon E. T. Smith et al, Deep in the Fields of the Andromeda Halo: Discovery of the Pegasus VII dwarf galaxy in UNIONS, arXiv (2025). DOI: 10.48550/arxiv.2502.09792

Journal information: arXiv

© 2025 Science X Network



Explore further


Saturday, January 18, 2025

NASA Celebrates Edwin Hubble's Discovery of a New Universe

M31 Cepheid Variable Star V1
Credits/Image: NASA, ESA, Hubble Heritage Project (STScI, AURA)
Acknowledgment: Robert Gendler

Compass Scale Image of V1 in M31
Credits/Image: NASA, ESA, Hubble Heritage Project (STScI, AURA)

Cepheid Variable Star V1 in Andromeda Galaxy
Credits/Image: NASA, ESA, Hubble Heritage Project (STScI, AURA)
Acknowledgment: Robert Gendler



For humans, the most important star in the universe is our Sun. The second-most important star is nestled inside the Andromeda galaxy. Don't go looking for it — the flickering star is 2.2 million light-years away, and is 1/100,000th the brightness of the faintest star visible to the human eye.

Yet, a century ago, its discovery by Edwin Hubble, then an astronomer at Carnegie Observatories, opened humanity's eyes as to how large the universe really is, and revealed that our Milky Way galaxy is just one of hundreds of billions of galaxies in the universe ushered in the coming-of-age for humans as a curious species that could scientifically ponder our own creation through the message of starlight. Carnegie Science and NASA are celebrating this centennial at the 245th meeting of the American Astronomical Society in Washington, D.C.

The seemingly inauspicious star, simply named V1, flung open a Pandora's box full of mysteries about time and space that are still challenging astronomers today. Using the largest telescope in the world at that time, the Carnegie-funded 100-inch Hooker Telescope at Mount Wilson Observatory in California, Hubble discovered the demure star in 1923. This rare type of pulsating star, called a Cepheid variable, is used as milepost markers for distant celestial objects. There are no tape-measures in space, but by the early 20th century Henrietta Swan Leavitt had discovered that the pulsation period of Cepheid variables is directly tied to their luminosity.

Many astronomers long believed that the edge of the Milky Way marked the edge of the entire universe. But Hubble determined that V1, located inside the Andromeda "nebula," was at a distance that far exceeded anything in our own Milky Way galaxy. This led Hubble to the jaw-dropping realization that the universe extends far beyond our own galaxy.

In fact Hubble had suspected there was a larger universe out there, but here was the proof in the pudding. He was so amazed he scribbled an exclamation mark on the photographic plate of Andromeda that pinpointed the variable star.

As a result, the science of cosmology exploded almost overnight. Hubble's contemporary, the distinguished Harvard astronomer Harlow Shapley, upon Hubble notifying him of the discovery, was devastated. "Here is the letter that destroyed my universe," he lamented to fellow astronomer Cecilia Payne-Gaposchkin, who was in his office when he opened Hubble's message.

Just three years earlier, Shapley had presented his observational interpretation of a much smaller universe in a debate one evening at the Smithsonian Museum of Natural History in Washington. He maintained that the Milky Way galaxy was so huge, it must encompass the entirety of the universe. Shapley insisted that the mysteriously fuzzy "spiral nebulae," such as Andromeda, were simply stars forming on the periphery of our Milky Way, and inconsequential.

Little could Hubble have imagined that 70 years later, an extraordinary telescope named after him, lofted hundreds of miles above the Earth, would continue his legacy. The marvelous telescope made "Hubble" a household word, synonymous with wonderous astronomy.

Today, NASA's Hubble Space Telescope pushes the frontiers of knowledge over 10 times farther than Edwin Hubble could ever see. The space telescope has lifted the curtain on a compulsive universe full of active stars, colliding galaxies, and runaway black holes, among the celestial fireworks of the interplay between matter and energy.

Edwin Hubble was the first astronomer to take the initial steps that would ultimately lead to the Hubble Space Telescope, revealing a seemingly infinite ocean of galaxies. He thought that, despite their abundance, galaxies came in just a few specific shapes: pinwheel spirals, football-shaped ellipticals, and oddball irregular galaxies. He thought these might be clues to galaxy evolution – but the answer had to wait for the Hubble Space Telescope's legendary Hubble Deep Field in 1994.

The most impactful finding that Edwin Hubble's analysis showed was that the farther the galaxy is, the faster it appears to be receding from Earth. The universe looked like it was expanding like a balloon. This was based on Hubble tying galaxy distances to the reddening of light — the redshift – that proportionally increased the father away the galaxies are.

The redshift data were first collected by Lowell Observatory astronomer Vesto Slipher, who spectroscopically studied the "spiral nebulae" a decade before Hubble. Slipher did not know they were extragalactic, but Hubble made the connection. Slipher first interpreted his redshift data an example of the Doppler effect. This phenomenon is caused by light being stretched to longer, redder wavelengths if a source is moving away from us. To Slipher, it was curious that all the spiral nebulae appeared to be moving away from Earth.

Two years prior to Hubble publishing his findings, the Belgian physicist and Jesuit priest Georges Lemaître analyzed the Hubble and Slifer observations and first came to the conclusion of an expanding universe. This proportionality between galaxies' distances and redshifts is today termed Hubble–Lemaître's law. Because the universe appeared to be uniformly expanding, Lemaître further realized that the expansion rate could be run back into time – like rewinding a movie – until the universe was unimaginably small, hot and dense. It wasn't until 1949 that the term "big bang" came into fashion.

This was a relief to Edwin Hubble's contemporary, Albert Einstein, who deduced the universe could not remain stationary without imploding under gravity's pull. The rate of cosmic expansion is now known as the Hubble Constant

Ironically, Hubble himself never fully accepted the runaway universe as an interpretation of the redshift data. He suspected that some unknown physics phenomenon was giving the illusion that the galaxies were flying away from each other. He was partly right in that Einstein's theory of special relativity explained redshift as an effect of time-dilation that is proportional to the stretching of expanding space. The galaxies only appear to be zooming through the universe. Space is expanding instead.

After decades of precise measurements, the Hubble telescope came along to nail down the expansion rate precisely, giving the universe an age of 13.8 billion years. This required establishing the first rung of what astronomers call the "cosmic distance ladder" needed to build a yardstick to far-flung galaxies. They are cousins to V1, Cepheid variable stars that the Hubble telescope can detect out to over 100 times farther from Earth than the star Edwin Hubble first found.

Astrophysics was turned on its head again in 1998 when the Hubble telescope and other observatories discovered that the universe was expanding at an ever-faster rate, through a phenomenon dubbed "dark energy." Einstein first toyed with this idea of a repulsive form of gravity in space, calling it the cosmological constant

Even more mysteriously, the current expansion rate appears to be different than what modern cosmological models of the developing universe would predict, further confounding theoreticians. Today astronomers are wrestling with the idea that whatever is accelerating the universe may be changing over time. NASA's Roman Space Telescope, with the ability to do large cosmic surveys, should lead to new insights into the behavior of dark matter and dark energy. Roman will likely measure the Hubble constant via lensed supernovae.

This grand century-long adventure, plumbing depths of the unknown, began with Hubble photographing a large smudge of light, the Andromeda galaxy, at the Mount Wilson Observatory high above Los Angeles.

In short, Edwin Hubble is the man who wiped away the ancient universe and discovered a new universe that would shrink humanity's self-perception into being an insignificant speck in the cosmos.

The Hubble Space Telescope has been operating for over three decades and continues to make ground-breaking discoveries that shape our fundamental understanding of the universe. Hubble is a project of international cooperation between NASA and ESA (European Space Agency). NASA’s Goddard Space Flight Center in Greenbelt, Maryland, manages the telescope and mission operations. Lockheed Martin Space, based in Denver, also supports mission operations at Goddard. The Space Telescope Science Institute in Baltimore, which is operated by the Association of Universities for Research in Astronomy, conducts Hubble science operations for NASA.




About This Release

Credits: Media Contact:

Ray Villard
Space Telescope Science Institute, Baltimore, Maryland

Permissions: Content Use Policy

Contact Us: Direct inquiries to the News Team.

Related Links and Documents



Friday, January 10, 2025

Prime Focus Spectrograph on the Subaru Telescope to Begin Science Operations in February

Example of data obtained by PFS observing celestial objects in the Andromeda Galaxy region. On the left, the positions of the PFS fibers configured to observe individual celestial objects are marked by circles on an image of the Andromeda Galaxy taken with HSC (Hyper Suprime-Cam) (Credit: NAOJ). The cyan rectangle represents the field of view of the multi-object spectrograph DEIMOS in operation at W. M. Keck Observatory for comparison. On the right, a magnified image of the observed celestial object is shown, along with the spectra obtained by PFS. (Credit: PFS Project/Kavli IPMU/NAOJ). Download image (4.5MB)



Researchers have finished equipping the Subaru Telescope with a new special “compound eye,” culminating several years of effort. This new eye is an instrument featuring approximately 2,400 prisms scattered across the extremely wide field of view available at the Subaru Telescope’s primary focus, allowing for simultaneous spectroscopic observation of thousands of celestial objects. This unrivaled capability will help researchers precisely understand the formation and evolution of galaxies and the Universe. Among 8-meter-class telescopes, the Subaru Telescope is the most competitive with the largest survey capability in the world. This instrument, the Prime Focus Spectrograph (PFS), will be ready to begin scientific operations in February 2025.

PFS will be one of the flagship instruments of the “Subaru Telescope 2.0” era. Taking advantage of the Subaru Telescope’s ultrawide field of view, approximately 1.3 degrees in diameter at the prime focus, and world-renowned large light-gathering power, PFS will position 2,400 fibers to collect light from celestial objects and simultaneously obtain spectra across the entire visible light range and part of the near-infrared band. Just like the compound eyes of insects, each facet (fiber) focuses on a different direction to cover a wide area while perceiving the colors of light from that direction. This highly ambitious instrument will dramatically enhance the Subaru Telescope’s spectroscopic observation efficiency.

Spanning nearly 15 years with support from industrial partners around the world, the development of PFS has been led by an international collaboration of over 20 research institutions in Japan, the U.S., France, Brazil, Taiwan, Germany, and China. Notably, the University of Tokyo Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI) has taken the lead in proposing and developing the instrument as well as planning large-sky survey observations, with the goal of testing various theoretical models about the formation of the Universe. The National Astronomical Observatory of Japan (NAOJ) has also played a central role, participating in the development of the instrument and overseeing the coordination of the project, while also being responsible for the acceptance and operation of the instrument

The PFS team plans to carry out a large-sky survey program over the next five or so years, utilizing a total of 360 nights of telescope time. This survey will take spectra of millions of distant galaxies, as well as hundreds of thousands of stars in the Milky Way and our neighboring Andromeda Galaxy.




Related Link(s)


Sunday, September 01, 2024

NASA's Roman Space Telescope to Investigate Galactic Fossils

Halo of the Andromeda Galaxy (Illustration)
Credits: Illustration: NASA, Joseph Olmsted (STScI)



The universe is a dynamic, ever-changing place where galaxies are dancing, merging together, and shifting appearance. Unfortunately, because these changes take millions or billions of years, telescopes can only provide snapshots, squeezed into a human lifetime.

However, galaxies leave behind clues to their history and how they came to be. NASA’s upcoming Nancy Grace Roman Space Telescope will have the capacity to look for these fossils of galaxy formation with high-resolution imaging of galaxies in the nearby universe.

Astronomers, through a grant from NASA, are designing a set of possible observations called RINGS (the Roman Infrared Nearby Galaxies Survey) that would collect these remarkable images, and the team is producing publicly available tools that the astronomy community can use once Roman launches and starts taking data. The RINGS survey is a preliminary concept that may or may not be implemented during Roman’s science mission.

Roman is uniquely prepared for RINGS due to its resolution akin to NASA’s Hubble Space Telescope and its wide field of view – 200 times that of Hubble in the infrared – making it a sky survey telescope that complements Hubble’s narrow-field capabilities.

Galactic Archaeologists

Scientists can only look at brief instances in the lives of evolving galaxies that eventually lead to the fully formed galaxies around us today. As a result, galaxy formation can be difficult to track

Luckily, galaxies leave behind hints of their evolution in their stellar structures, almost like how organisms on Earth can leave behind imprints in rock. These galactic “fossils” are groups of ancient stars that hold the history of the galaxy’s formation and evolution, including the chemistry of the galaxy when those stars formed.

Such cosmic fossils are of particular interest to Robyn Sanderson, the deputy principal investigator of RINGS at the University of Pennsylvania in Philadelphia. She describes the process of analyzing stellar structures in galaxies as “like going through an excavation and trying to sort out bones and put them back together.”

Roman’s high resolution will allow scientists to pick out these galactic fossils, using structures ranging from long tidal tails on a galaxy’s outskirts to stellar streams within the galaxy. These large-scale structures, which Roman is uniquely capable of capturing, can give clues to a galaxy’s merger history. The goal, says Sanderson, is to “reassemble these fossils in order to look back in time and understand how these galaxies came to be.”

Shedding Light on Dark Matter

RINGS will also enable further investigations of one of the most mysterious substances in the universe: dark matter, an invisible form of matter that makes up most of a galaxy’s mass. A particularly useful class of objects for testing dark matter theories are ultra-faint dwarf galaxies. According to Raja GuhaThakurta of the University of California, Santa Cruz, "Ultra faint dwarf galaxies are so dark matter-dominated that they have very little normal matter for star formation. With so few stars being created, ultra-faint galaxies can essentially be seen as pure blobs of dark matter to study.”

Roman, thanks to its large field of view and high resolution, will observe these ultra-faint galaxies to help test multiple theories of dark matter. With these new data, the astronomical community will come closer to finding the truth about this unobservable dark matter that vastly outweighs visible matter: dark matter makes up about 80% of the universe’s matter while normal matter comprises the remaining 20%.

Ultra-faint galaxies are far from the only test of dark matter. Often, just looking in an average-sized galaxy’s backyard is enough. Structures in the halo of stars surrounding a galaxy often give hints to the amount of dark matter present. However, due to the sheer size of galactic halos (they are often 15-20 times as big as the galaxy itself), current telescopes are deeply inefficient at observing them.

At the moment, the only fully resolved galactic halos scientists have to go on are our own Milky Way and Andromeda, our neighbor galaxy. Ben Williams, the principal investigator of RINGS at the University of Washington in Seattle, describes how Roman’s power will amend this problem: “We only have reliable measurements of the Milky Way and Andromeda, because those are close enough that we can get measurements of a large number of stars distributed across their stellar halos. So, with Roman, all of a sudden we’ll have 100 or more of these fully resolved galaxies.”

When Roman launches by May 2027, it is expected to fundamentally alter how scientists understand galaxies. In the process, it will shed some light on our own home galaxy. The Milky Way is easy to study up close, but we do not have a large enough selfie stick to take a photo of our entire galaxy and its surrounding halo. RINGS shows what Roman is capable of should such a survey be approved. By studying the nearby universe, RINGS can examine galaxies similar in size and age to the Milky Way, and shed light on how we came to be here.

About the mission

The Nancy Grace Roman Space Telescope is managed at NASA’s Goddard Space Flight Center in Greenbelt, Maryland, with participation by NASA's Jet Propulsion Laboratory and Caltech/IPAC in Southern California, the Space Telescope Science Institute in Baltimore, and a science team comprising scientists from various research institutions. The primary industrial partners are BAE Systems, Inc. in Boulder, Colorado; L3Harris Technologies in Rochester, New York; and Teledyne Scientific & Imaging in Thousand Oaks, California.



Tuesday, January 09, 2024

When one plus one (eventually) equals one

Arp 122, NGC 6040, NGC 6041
Two spiral galaxies are merging together at the right side of the image. One is seen face-on and is circular in shape. The other seems to lie in front of the first one. This galaxy is seen as a disc tilted away from the viewer and it is partially warped. In the lower-left corner, cut off by the frame, a large elliptical galaxy appears as light radiating from a point. Various small galaxies cover the background. Credit: ESA/Hubble & NASA, J. Dalcanton, Dark Energy Survey/DOE/FNAL/DECam/CTIO/NOIRLab/NSF/AURA. Acknowledgement: L. Shatz

This Hubble Picture of the Week features Arp 122, a peculiar galaxy that in fact comprises two galaxies — NGC 6040, the tilted, warped spiral galaxy and LEDA 59642, the round, face-on spiral — that are in the midst of a collision. This dramatic cosmic encounter is located at the very safe distance of roughly 570 million light-years from Earth. Peeking in at the corner is the elliptical galaxy NGC 6041, a central member of the galaxy cluster that Arp 122 resides in, but otherwise not participating in this monster merger.

Galactic collisions and mergers are monumentally energetic and dramatic events, but they take place on a very slow timescale. For example, the Milky Way is on track to collide with its nearest galactic neighbour, the Andromeda Galaxy (M31), but these two galaxies have a good four billion years to go before they actually meet. The process of colliding and merging will not be a quick one either: it might take hundreds of millions of years to unfold. These collisions take so long because of the truly massive distances involved.

Galaxies are composed of stars and their solar systems, dust and gas. In galactic collisions, therefore, these constituent components may experience enormous changes in the gravitational forces acting on them. In time, this completely changes the structure of the two (or more) colliding galaxies, and sometimes ultimately results in a single, merged galaxy. That may well be what results from the collision pictured in this image. Galaxies that result from mergers are thought to have a regular or elliptical structure, as the merging process disrupts more complex structures (such as those observed in spiral galaxies). It would be fascinating to know what Arp 122 will look like once this collision is complete . . . but that will not happen for a long, long time.



Friday, October 13, 2023

LINER on collision course


Two galaxies are prominent among many much smaller background galaxies in the darkness of space. The larger galaxy is an elliptical galaxy, radiating light in a perfectly even sphere from a bright centre. The smaller galaxy is a barred spiral, with arms that are wispy like fog connected to a bar crossing the galaxy’s shining core. The shape of the arms makes the smaller galaxy notably squarish. Credit: ESA/Hubble & NASA, M. West

This Picture of the Week prominently features two galaxies: NGC 3558 in the lower left, and LEDA 83465 in the upper right. Both galaxies lie roughly 450 million light years from Earth. The two galaxies are separated from one another by a distance of roughly 150 000 light years, which might sound vast, until we consider that our nearest galactic neighbour — the Andromeda galaxy — is a whopping 2.5 million light years distant from the Milky Way galaxy. In galactic terms, the two galaxies pictured here are practically on top of one another.

This is because they belong to a crowded and chaotic galaxy cluster known as Abell 1185, which is packed with galaxies that are interacting with one another via gravity. These galactic interactions have sometimes led to dramatic results, such as galaxies being torn apart completely. This fate has not befallen NGC 3558, which currently retains its integrity as both an elliptical galaxy and a low-ionisation nuclear emission-line region, or LINER. In fact, it probably attained its present form by devouring smaller galaxies in the cluster — galaxies much like LEDA 83465.

LINERs are a particular type of galactic nucleus or core, and are distinguished by the chemical fingerprints written into the light that they emit. As their name suggests, LINERs emit light which suggests that many of the atoms and molecules within these galactic cores have either been weakly ionised or not ionised at all. Ionisation is the process by which atoms or molecules lose or gain electrons. In galaxies, it is driven by a variety of processes — from shockwaves travelling through galaxies, to radiation from massive stars or from hot gas in accretion discs. In the case of LINERs, this means that many of the atoms and molecules within the galaxies have lost either a single electron, or have retained all their electrons. The mechanism that drives this weak ionisation in LINERs such as NGC 3558 is still debated amongst astronomers.



Wednesday, August 16, 2023

A New Way to Constrain Dark Energy


This ultraviolet mosaic of our galactic neighbor, the Andromeda Galaxy, is constructed from observations by NASA's Swift Observatory. Credit:
NASA/Swift/Stefan Immler (GSFC) and Erin Grand (UMCP)

The cosmological constant, once rued by Einstein as his greatest blunder, is back in style. Researchers have used an entirely new method to determine the value of this constant — thought to be related to dark energy — using a galaxy in our cosmic backyard.


An image of anisotropies in the cosmic microwave background. The Planck satellite studied the cosmic microwave background to measure several important cosmological parameters. Credit:
ESA and the Planck Collaboration

Accounting for Acceleration

Our universe is expanding, and that expansion is accelerating, propelled by a mysterious quantity known as dark energy. Many researchers suspect that dark energy is an explanation for the cosmological constant, a quantity tacked onto the equations of Einstein’s theory of gravity. Initially included as a way to make the equations describe a static, non-expanding universe, Einstein scrapped the constant when the universe was revealed to be expanding. With the discovery that this expansion is actually accelerating, the cosmological constant is back in vogue, but with a new purpose.

Researchers have devised a number of ways to measure quantities relevant to the cosmological constant. For example, the Planck mission mapped the tiny imperfections and non-uniformities in the cosmic microwave background — the oldest light in the universe — to measure the cosmological constant on a global scale. But as with all active areas of research, it’s important to make measurements in multiple ways to test our theories from all angles. How might we probe the cosmological constant on an entirely different scale?


An illustration of the Local Group of galaxies, which contains the Milky Way and Andromeda, as well as some of its near neighbors. Click to enlarge. Credit:
Antonio Ciccolella; CC BY 4.0

Local Solutions to Global Questions

David Benisty, Anne-Christine Davis, and Wyn Evans (University of Cambridge) used pairs of galaxies locked in a gravitational dance to place constraints on the value of the cosmological constant. Their method hinges on the fact that the fabric of spacetime, from the space between the stars to the gaps between galaxies, is expanding under the influence of dark energy. This means that encoded within the orbital motions of any gravitationally bound galaxy pair is the subtle pressure of dark energy, forcing the galaxies apart as gravity pulls them together.

Benisty and collaborators analytically solved the two-body problem that describes the orbits of the Milky Way and its most massive neighbor, Andromeda, and accounts for the repulsive influence of dark energy. In doing so, they constrained the value of the cosmological constant over a few million light-years — a much smaller scale than the Planck mission, which drew its conclusions from the cosmic microwave background that suffuses the entire sky.


Constraints on the cosmological constant, Λ, compared to the constraints determined from Planck data. Future measurements, such as with JWST, are anticipated to greatly improve the constraint placed by the binary galaxy method. Credit: Adapted from
Benisty et al. 2023

Upper Limits and Other Applications

The team’s findings agreed with the results from the Planck mission, finding an upper limit on the value of the cosmological constant equal to 5.44 times the value measured by Planck. While the constraint is not particularly stringent, Benisty and coauthors anticipate that more precise data will allow them to narrow the constraint in the future. In particular, stellar positions measured by JWST will improve our estimates of Andromeda’s mass, which is one of the largest sources of uncertainty.

Benisty and collaborators also used their method to place constraints on other theories of gravity. While these constraints were less restrictive than those placed on the cosmological constant, the technique is still valuable as it constrains modified gravity on scales of millions of light-years rather than the solar-system-sized scales from previous work.

Citation

“Constraining Dark Energy from the Local Group Dynamics,” David Benisty et al 2023 ApJL 953 L2. doi:10.3847/2041-8213/ace90b

Monday, January 30, 2023

The Curious Case of the Dwarf Galaxy Pegasus W


What appears to be a normal field of stars is actually an ultra-faint dwarf galaxy; this Hubble Space Telescope image shows just the stars belonging to the tiny galaxy Leo IV, with the background galaxies removed. Credit: NASA, ESA, and T. Brown (STScI)

Title: Pegasus W: An Ultra-Faint Dwarf Galaxy Outside the Halo of M31 Not Quenched by Reionization
Authors: Kristen B. McQuinn et al.
First Author’s Institution: Rutgers University
Status: Accepted to ApJ


Our local patch of the universe is populated by a number of galaxies — the so-called “Local Group,” consisting of our very own Milky Way, the similar-in-mass Andromeda Galaxy (Messier 31), and between 50 and 100 known “dwarf” or low-mass galaxies. The faintest, least massive of these, termed ultra-faint dwarfs, range in mass from a few thousand solar masses down to just a few hundred solar masses! Ultra-faint dwarfs in the Local Group are of immense interest to astronomers, since they can be used to study a variety of phenomena ranging from dark matter dynamics to stellar feedback, and from chemical evolution to ram pressure stripping. Owing to the low mass and weak gravitational potentials of ultra-faint dwarfs, these various physical processes often have outsize effects on their stars and gas, making them ideal objects for study.

Today’s authors report the discovery of a new ultra-faint dwarf named Pegasus W and analyse some of its interesting properties. Most ultra-faint dwarfs are extremely difficult to detect as they are faint and often diffuse — in fact, looking at a simple image of one may not even reveal its presence, as Figure 1 shows! Therefore, they are often detected by looking for statistical overdensities of stars in large sky surveys, and that’s exactly how Pegasus W was discovered from Dark Energy Spectroscopic Instrument (DESI) data. The authors of today’s article then followed up with Hubble Space Telescope imaging to study the stellar populations in the galaxy.


Figure 1: Left-hand panel shows a Hubble Space Telescope image of the area of the sky where Pegasus W is located. The right panel shows a view of the stellar density distribution, with the contours highlighting the over-density of stars that indicates the presence of Pegasus W. Credit: Adapted from McQuinn et al. 2023

Pegasus W is about 3 million light-years from the Milky Way. It’s closer to Andromeda, but still outside Andromeda’s virial radius (a measure of how far a galaxy’s gravitational influence extends). Therefore, it is not considered a satellite of Andromeda but rather an isolated ultra-faint dwarf galaxy. It is also quite faint, with a V-band absolute magnitude of about −7.2 and an estimated stellar mass of only 6.5 x 104 solar masses!

One of the most important properties of a galaxy is its star formation history — a fossil record of how it assembled and grew over time. Local Group dwarf galaxies are especially well suited for star formation history studies because of how nearby they are. The Local Group is the only place in the entire universe where we can get resolved photometry (imaging) of the individual stars in a galaxy, whereas for all other galaxies farther away we can only observe their starlight as an unresolved blob! This is key for measuring accurate star formation histories, since resolved stellar imaging allows us to build a colour–magnitude diagram for a galaxy — a plot of all its stars comparing their luminosities to their temperatures. After constructing a galaxy’s colour–magnitude diagram, we can fit stellar evolution models to it to figure out how old its various stellar populations are, and this allows us to reverse-engineer the entire record of how it formed its stars over cosmic time!

Figure 2 shows how this analysis was carried out for Pegasus W. The top-left panel shows the observed colour–magnitude diagram for the galaxy, with the top right being the best-fit diagram from stellar evolution modelling. The bottom left shows the residuals (i.e., what results from subtracting the model from the data). The residual significance diagram on the bottom right shows a checkerboard pattern, which indicates that the model is a good fit.


Figure 2: Top left: Observed colour–magnitude diagram for Pegasus W from resolved stellar imaging. Top right: Colour–magnitude diagram reconstruction using stellar evolution models. Bottom left: Residual resulting from subtracting the model from the data. Bottom right: Residual significance diagram showing that the model is a good fit. Credit: McQuinn et al. 2023
 
Figure 3 shows the star formation history that the authors inferred for Pegasus W. The y axis shows the fraction of its final stellar mass, and the x axis shows lookback time from present day (right-hand side being present day and the left-hand edge representing the Big Bang). The red curve shows the growth of Pegasus W’s stellar mass over time, with the orange shaded region representing the uncertainty on the star formation history.
 

Figure 3: Star formation history for Pegasus W, showing the fraction of its present-day stellar mass at various points in time from the Big Bang (left-hand edge) to present day (right-hand edge). The orange shaded region represents the error on the star formation history, while the grey shaded region represents the epoch of reionisation. Credit: McQuinn et al. 2023

 
The authors note what is most unique about Pegasus W: most ultra-faint dwarfs known to date have very short star formation histories at very early times. That is, most ultra-faint dwarfs formed all their stars at early cosmic times and were quenched (ceased forming stars) over 10 billion years ago. Astronomers believe that this early quenching was likely due to cosmic reionisation, when the hydrogen gas in the universe went from neutral to ionised due to radiation from the first stars and galaxies. However, as Figure 3 shows, Pegasus W does not appear to have quenched during reionisation (indicated by the vertical grey shaded region) and continued forming stars well after!

The puzzle of Pegasus W’s star formation history is likely to generate significant debate amongst astronomers studying galaxy evolution and reionisation. The authors note that better photometric data and perhaps even spectroscopy would help improve the uncertainty on the star formation history measurements, and that JWST is likely to help shed more light on this mystery in coming years.

Original astrobite edited by Isabella Trierweiler.

By Astrobites





About the author, Pratik Gandhi:

I’m a 3rd-year astrophysics PhD student at UC Davis, originally from Mumbai, India. I study galaxy formation and evolution, and am really excited about the use of both simulations and observations in the study of galaxies. I am interested in science communication, teaching, and social issues in academia. Also a huge fan of Star Trek, with Deep Space Nine and The Next Generation being my favourites!


Tuesday, July 05, 2022

Gemini North Spies Ultra-Faint Fossil Galaxy Discovered on Outskirts of Andromeda

PR Image noirlab2214a
The ultra-faint dwarf galaxy Pegasus V

PR Image noirlab2214b
The ultra-faint dwarf galaxy Pegasus V (circled)


Videos

Cosmoview Episode 46: Gemini North Spies Ultra-Faint Fossil Galaxy Discovered on Outskirts of Andromeda
Cosmoview Episode 46: Gemini North Spies Ultra-Faint Fossil Galaxy Discovered on Outskirts of Andromeda
CosmoView Episodio 46: Descubren nueva galaxia en imágenes tomadas en Cerro Tololo
CosmoView Episodio 46: Descubren nueva galaxia en imágenes tomadas en Cerro Tololo 
 


NSF’s NOIRLab facilities reveal a relict of the earliest galaxies

An unusual ultra-faint dwarf galaxy has been discovered on the outer fringes of the Andromeda Galaxy thanks to the sharp eyes of an amateur astronomer examining archival data processed by NSF’s NOIRLab’s Community Science and Data Center. Follow-up by professional astronomers using the International Gemini Observatory, a Program of NSF’s NOIRLab, revealed that the dwarf galaxy — Pegasus V — contains very few heavier elements and is likely to be a fossil of the first galaxies.

An unusual ultra-faint dwarf galaxy has been discovered on the edge of the Andromeda Galaxy using several facilities of NSF's NOIRLab. The galaxy, called Pegasus V, was first detected as part of a systematic search for Andromeda dwarfs coordinated by David Martinez-Delgado from the Instituto de Astrofísica de Andalucía, Spain, when amateur astronomer Giuseppe Donatiello found an interesting ‘smudge’ in data in a DESI Legacy Imaging Surveys image [1]. The image was taken with the US Department of Energy-fabricated Dark Energy Camera on the Víctor M. Blanco 4-meter Telescope at Cerro Tololo Inter-American Observatory (CTIO). The data were processed through the Community Pipeline which is operated by NOIRLab's Community Science and Data Center (CSDC). 

Follow-up deeper observations by astronomers using the larger, 8.1-meter Gemini North telescope with the GMOS instrument, revealed faint stars in Pegasus V, confirming that it is an ultra-faint dwarf galaxy on the outskirts of the Andromeda Galaxy. Gemini North in Hawai‘i is one half of the International Gemini Observatory.

The observations with Gemini revealed that the galaxy appears to be extremely deficient in heavier elements compared to similar dwarf galaxies, meaning that it is very old and likely to be a fossil of the first galaxies in the Universe.

“We have found an extremely faint galaxy whose stars formed very early in the history of the Universe," commented Michelle Collins, an astronomer at the University of Surrey, UK and lead author of the paper announcing this discovery. “This discovery marks the first time a galaxy this faint has been found around the Andromeda Galaxy using an astronomical survey that wasn't specifically designed for the task.”

The faintest galaxies are considered to be fossils of the very first galaxies that formed, and these galactic relics contain clues about the formation of the earliest stars. While astronomers expect the Universe to be teeming with faint galaxies like Pegasus V [2], they have not yet discovered nearly as many as their theories predict. If there are truly fewer faint galaxies than predicted this would imply a serious problem with astronomers' understanding of cosmology and dark matter. 

Discovering examples of these faint galaxies is therefore an important endeavor, but also a difficult one. Part of the challenge is that these faint galaxies are extremely tricky to spot, appearing as just a few sparse stars hidden in vast images of the sky.

The trouble with these extremely faint galaxies is that they have very few of the bright stars which we typically use to identify them and measure their distances,” explained Emily Charles, a PhD student at the University of Surrey who was also involved in the study. “Gemini’s 8.1-meter mirror allowed us to find faint, old stars which enabled us both to measure the distance to Pegasus V and to determine that its stellar population is extremely old.”

The strong concentration of old stars that the team found in Pegasus V suggests that the object is likely a fossil of the first galaxies. When compared with the other faint galaxies around Andromeda, Pegasus V seems uniquely old and metal-poor, indicating that its star formation ceased very early indeed. 

“We hope that further study of Pegasus V’s chemical properties will provide clues into the earliest periods of star formation in the Universe,” concluded Collins. “This little fossil galaxy from the early Universe may help us understand how galaxies form, and whether our understanding of dark matter is correct.”

“The public-access Gemini North telescope provides an array of capabilities for community astronomers,” said Martin Still, Gemini Program Officer at the National Science Foundation. “In this case, Gemini supported this international team to confirm the presence of the dwarf galaxy, associate it physically with the Andromeda Galaxy, and determine the metal-deficient nature of its evolved stellar population."

Upcoming astronomical facilities are set to shed more light on faint galaxies. Pegasus V was witness to a time in the history of the Universe known as reionization, and other objects dating back to this time will soon be observed with NASA’s James Webb Space Telescope. Astronomers also hope to discover other such faint galaxies in the future using Vera C. Rubin Observatory, a Program of NSF's NOIRLab. Rubin Observatory will conduct an unprecedented, decade-long survey of the optical sky called the Legacy Survey of Space and Time (LSST).

 Source: NSF’s National Optical-Infrared Astronomy Research Laboratory (NOIRLab)/News

 



Notes

[1] The DESI Legacy Imaging Surveys were conducted to identify targets for the Dark Energy Spectroscopic Instrument (DESI) operations. These surveys comprise a unique blend of three projects that have observed a third of the night sky: the Dark Energy Camera Legacy Survey (DECaLS), observed by the DOE-built Dark Energy Camera (DECam) on the Víctor M. Blanco 4-meter Telescope at Cerro Tololo Inter-American Observatory (CTIO) in Chile; the Mayall z-band Legacy Survey (MzLS), by the Mosaic3 camera on the Nicholas U. Mayall 4-meter Telescope at Kitt Peak National Observatory (KPNO); and the Beijing-Arizona Sky Survey (BASS) by the 90Prime camera on the Bok 2.3-meter Telescope, which is owned and operated by the University of Arizona and located at KPNO. CTIO and KPNO are Programs of NSF's NOIRLab.

[2] Pegasus V is so named because it is the fifth dwarf galaxy discovered located in the constellation Pegasus. The on-sky separation between Pegasus V and the Andromeda Galaxy is about 18.5 degrees.




More Information

This research was presented in a paper entitled “Pegasus V — a newly discovered ultra-faint dwarf galaxy on the outskirts of Andromeda” to appear in Monthly Notices of the Royal Astronomical Society.

The team is composed of Michelle L. M. Collins (Physics Department, University of Surrey, UK), Emily J. E. Charles (Physics Department, University of Surrey, UK), David Martínez-Delgado (Instituto de Astrofísica de Andalucía, Spain), Matteo Monelli (Instituto de Astrofísica de Canarias (IAC) and Universidad de La Laguna, Spain), Noushin Karim (Physics Department, University of Surrey, UK), Giuseppe Donatiello (UAI – Unione Astrofili Italiani, Italy), Erik J. Tollerud (Space Telescope Science Institute, USA), Walter Boschin (Instituto de Astrofísica de Canarias (IAC), Universidad de La Laguna, and Fundación G. Galilei - INAF (Telescopio Nazionale Galileo), Spain).

NSF’s NOIRLab (National Optical-Infrared Astronomy Research Laboratory), the US center for ground-based optical-infrared astronomy, operates the international Gemini Observatory (a facility of NSF, NRC–Canada, ANID–Chile, MCTIC–Brazil, MINCyT–Argentina, and KASI–Republic of Korea), Kitt Peak National Observatory (KPNO), Cerro Tololo Inter-American Observatory (CTIO), the Community Science and Data Center (CSDC), and Vera C. Rubin Observatory (operated in cooperation with the Department of Energy’s SLAC National Accelerator Laboratory). It is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with NSF and is headquartered in Tucson, Arizona. The astronomical community is honored to have the opportunity to conduct astronomical research on Iolkam Du’ag (Kitt Peak) in Arizona, on Maunakea in Hawai‘i, and on Cerro Tololo and Cerro Pachón in Chile. We recognize and acknowledge the very significant cultural role and reverence that these sites have to the Tohono O'odham Nation, to the Native Hawaiian community, and to the local communities in Chile, respectively.




Links



Contacts:

Michelle Collins
University of Surrey
Email:
m.collins@surrey.ac.uk

Amanda Kocz
Communications Manager
NSF’s NOIRLab
Tel: +1 520 318 8591
Email:
amanda.kocz@noirlab.edu



Friday, December 25, 2020

Primordial black holes and the search for dark matter from the multiverse

Fig1. Baby universes branching off of our universe shortly after the Big Bang appear to us as black holes.
Credit:Kavli IPMU


Fig2. Hyper Suprime-Cam (HSC) is a gigantic digital camera on the Subaru Telescope
Credit:HSC project / NAOJ


Fig3. The Subaru Telescope in Hawaii.
Credit:NAOJ

Fig4. A star in the Andromeda galaxy temporarily becomes brighter if a primordial black hole passes in front of the star, focusing its light in accordance with the theory of gravity. (Credit: Kavli IPMU/HSC Collaboration)
 
The Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU) is home to many interdisciplinary projects which benefit from the synergy of a wide range of expertise available at the institute. One such project is the study of black holes that could have formed in the early universe, before stars and galaxies were born.  

Such primordial black holes (PBHs) could account for all or part of dark matter, be responsible for some of the observed gravitational waves signals, and seed supermassive black holes found in the center of our Galaxy and other galaxies. They could also play a role in the synthesis of heavy elements when they collide with neutron stars and destroy them, releasing neutron-rich material. In particular, there is an exciting possibility that the mysterious dark matter, which accounts for most of the matter in the universe, is composed of primordial black holes. The 2020 Nobel Prize in physics was awarded to a theorist, Roger Penrose, and two astronomers, Reinhard Genzel and Andrea Ghez, for their discoveries that confirmed the existence of black holes. Since black holes are known to exist in nature, they make a very appealing candidate for dark matter. 

The recent progress in fundamental theory, astrophysics, and astronomical observations in search of PBHs has been made by an international team of particle physicists, cosmologists and astronomers, including Kavli IPMU members Alexander Kusenko, Misao Sasaki, Sunao Sugiyama, Masahiro Takada and Volodymyr Takhistov.

To learn more about primordial black holes, the research team looked at the early universe for clues. The early universe was so dense that any positive density fluctuation of more than 50 percent would create a black hole. However, cosmological perturbations that seeded galaxies are known to be much smaller. Nevertheless, a number of processes in the early universe could have created the right conditions for the black holes to form.  

One exciting possibility is that primordial black holes could form from the “baby universes” created during inflation, a period of rapid expansion that is believed to be responsible for seeding the structures we observe today, such as galaxies and clusters of galaxies. During inflation, baby universes can branch off of our universe. A small baby (or “daughter”) universe would eventually collapse, but the large amount of energy released in the small volume causes a black hole to form.  

An even more peculiar fate awaits a bigger baby universe. If it is bigger than some critical size, Einstein's theory of gravity allows the baby universe to exist in a state that appears different to an observer on the inside and the outside. An internal observer sees it as an expanding universe, while an outside observer (such as us) sees it as a black hole. In either case, the big and the small baby universes are seen by us as primordial black holes, which conceal the underlying structure of multiple universes behind their “event horizons.” The event horizon is a boundary below which everything, even light, is trapped and cannot escape the black hole. 

In their paper, the team described a novel scenario for PBH formation and showed that the black holes from the “multiverse” scenario can be found using the Hyper Suprime-Cam (HSC) of the 8.2m Subaru Telescope, a gigantic digital camera - - the management of which Kavli IPMU has played a crucial role - - near the 4,200 meter summit of Mt. Mauna Kea in Hawaii. Their work is an exciting extension of the HSC search of PBH that Masahiro Takada, a Principal Investigator at the Kavli IPMU, and his team are pursuing. The HSC team has recently reported leading constraints on the existence of PBHs in Niikura, Takada et. al. Nature Astronomy 3, 524–534 (2019)

Why was the HSC indispensable in this research? The HSC has a unique capability to image the entire Andromeda galaxy every few minutes. If a black hole passes through the line of sight to one of the stars, the black hole’s gravity bends the light rays and makes the star appear brighter than before for a short period of time. The duration of the star’s brightening tells the astronomers the mass of the black hole. With HSC observations, one can simultaneously observe one hundred million stars, casting a wide net for primordial black holes that may be crossing one of the lines of sight.  

The first HSC observations have already reported a very intriguing candidate event consistent with a PBH from the “multiverse,” with a black hole mass comparable to the mass of the Moon. Encouraged by this first sign, and guided by the new theoretical understanding, the team is conducting a new round of observations to extend the search and to provide a definitive test of whether PBHs from the multiverse scenario can account for all dark matter.  

 

 

Paper details

Journal: Physical Review Letters
Title: Exploring Primordial Black Holes from the Multiverse with Optical Telescopes
Authors: Alexander Kusenko (1, 2), Misao Sasaki (2, 3, 4), Sunao Sugiyama (2, 5), Masahiro Takada (2), Volodymyr Takhistov (1,2), and Edoardo Vitagliano (1)

Author affiliation

1. Department of Physics and Astronomy, University of California, Los Angeles, Los Angeles, California 90095-1547, USA 
2. Kavli Institute for the Physics and Mathematics of the Universe (WPI), UTIAS The University of Tokyo, Kashiwa, Chiba 277-8583, Japan
3. Center for Gravitational Physics, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto 606-8502, Japan 
4. Leung Center for Cosmology and Particle Astrophysics, National Taiwan University, Taipei 10617, Taiwan 
5. Department of Physics, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan

DOI: https://doi.org/10.1103/PhysRevLett.125.181304  (October 30, 2020)
Abstract of the paper: (Physical Review Letters)
Preprint: (arXiv.org page)  



 

Research contact:

Alexander Kusenko
Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU)
Visiting Senior Scientist
Department of Physics & Astronomy, University of California, Los Angeles
Professor
E-mail:
kusenko@ucla.edu

Misao Sasaki
Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU)
Deputy Director
Center for Gravitational Physics, Yukawa Institute for Theoretical Physics, Kyoto University
Leung Center for Cosmology and Particle Astrophysics, National Taiwan University
E-mail
: misao.sasaki@ipmu.jp

Sunao Sugiyama
Graduate Student
Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU)
Department of Physics, The University of Tokyo
E-mail:
sunao.sugiyama@ipmu.jp

Masahiro Takada
Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU)
Principal Investigator
E-mail:
masahiro.takada@ipmu.jp

Volodymyr Takhistov
Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU)
Project Researcher / Kavli IPMU Fellow
E-mail:
volodymyr.takhistov@ipmu.jp

Media contact:

John Amari
Press officer 
Kavli Institute for the Physics and Mathematics of the Universe, The University of Tokyo
E-mail:
press@ipmu.jp
TEL: 080-4056-2767 


Monday, October 19, 2020

Anemic Star Cluster Breaks Metal-poor Record

The discovery of rbc ext8 challenges theories that massive globular star clusters could not have formed at such low metallicities. Credit: ESASky/CFHT 

Maunakea, Hawaii – In a surprising discovery, astronomers using two Maunakea Observatories – W. M. Keck Observatory and Canada-France-Hawaii Telescope (CFHT) – have found a globular star cluster in the Andromeda Galaxy that contains a record-breaking low amount of metals.

The stars in the cluster, called RBC EXT8, have on average 800 times less iron than our Sun and are three times more iron-poor than the previous globular cluster record-holder. RBC EXT8 is also extremely deficient in magnesium.

The study, led by Søren Larsen of Radboud University in the Netherlands, is published in today’s issue of the journal Science.

“I’m amazed that this remarkable star cluster was just sitting under our noses. It is one of the brightest clusters in the Andromeda galaxy and known for decades, yet no one had checked it out in detail,” said Aaron Romanowsky, a University of California Observatories (UCO) astronomer and professor at San José State University’s Physics and Astronomy Department who co-authored the study. “It shows how the universe still has many surprises for us to discover. It also reminds us to check our assumptions – in this case, it was assumed enough clusters had been investigated to know how anemic they can be.”

A globular cluster is a large, dense collection of thousands to millions of ancient stars that move together as a tight-knit group through a galaxy. Until now, astronomers thought large globular clusters had to contain a considerable amount of heavy elements.

Hydrogen and helium are the two main elements created after the Big Bang. Heavier elements such as iron and magnesium formed later. Finding a massive globular cluster like RBC EXT8 that is extremely impoverished in metals defies current formation models, calling into question some of our ideas about the birth of stars and galaxies in the young universe.

The RBC EXT8 globular cluster orbits the outskirts of the Andromeda Galaxy, a close companion to our Milky Way Galaxy, located 2.5 million light-years from Earth. Credit: ESASky/CFHT

“Our finding shows that massive globular clusters could form in the early universe out of gas with only a small ‘sprinkling’ of elements other than hydrogen and helium. This is surprising because such pristine gas was thought to be in building blocks too small to form such massive star clusters,” said Larsen.

“This discovery is exciting because the idea of a ‘metallicity floor’ for globular clusters, that must contain some minimum amount of heavy metals, underpinned so much of our thinking about how these very old star clusters formed in the early universe,” said co-author Jean Brodie, Director, Centre for Astrophysics and Supercomputing at Swinburne University and Professor Emerita of Astronomy and Astrophysics at UCO. “Our finding contradicts the standard picture and that is always fun!”

The researchers observed RBC EXT8 using Keck Observatory’s High-Resolution Echelle Spectrometer (HIRES) in October of 2019. The globular cluster was not originally on the program, but Larsen’s team had a couple of hours of observing time left and decided to aim the Keck I telescope at the cluster, whose stellar content had not yet been studied in detail. The team made spectroscopic observations to determine RBC EXT8’s metal content and used three archive images from CFHT to determine its size and estimate its mass. Their remarkable result came as quite a surprise.

“It is observationally challenging to obtain a detailed analysis of the chemical composition of globular clusters in the Andromeda Galaxy, which is in the Northern Hemisphere of the sky,” said Brodie. “The HIRES capability at Keck is uniquely well-suited to meet this challenge.”

In the future, the researchers hope to find more “metal-lite” globular clusters and solve the mystery about their origin.






About HIRES

The High-Resolution Echelle Spectrometer (HIRES) produces spectra of single objects at very high spectral resolution yet covers a wide wavelength range. It does this by separating the light into many “stripes” of spectra stacked across a mosaic of three large CCD detectors. HIRES is famous for finding exoplanets. Astronomers also use HIRES to study important astrophysical phenomena like distant galaxies and quasars, as well as find cosmological clues about the structure of the early universe, just after the Big Bang.



About W. M. Keck Observatory

The W. M. Keck Observatory telescopes are among the most scientifically productive on Earth. The two 10-meter optical/infrared telescopes on the summit of Maunakea on the Island of Hawaii feature a suite of advanced instruments including imagers, multi-object spectrographs, high-resolution spectrographs, integral-field spectrometers, and world-leading laser guide star adaptive optics systems. Some of the data presented herein were obtained at Keck Observatory, which is a private 501(c) 3 non-profit organization operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the Native Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.