One of the universe’s most enormous black holes in the heart of the universe

In 2007, astronomers discovered the space horseshoe, a critical lending system for a galaxy about 5.5 billion light years away. The mass of the galaxy in the foreground enlarges and distorts the image of a distant background galaxy where light has been moved for billions of years before reaching us. The galaxies in the foreground and background are in perfect alignment so that they create Einstein rings.

A new study of the horseshoe shape of the universe reveals that ultra-muscular black holes (UMBH) exist in the foreground galaxy at an astounding 36 billion solar masses.

Although there is no strict definition of UMBH, the term is often used to describe ultra-high Massive Black Holes (SMBHs) with over 5 billion solar masses. SMBHS was not “discovered” in the traditional sense of words. Rather, over time, their existence became clear. And over time, more and more large scales were measured. There is a growing need for names for the largest ones. That’s how the term “super massive black hole” was born.

The discovery of extremely huge black holes in the horseshoe shape of the universe is presented in new research. It is titled “Publishing 36 billion solar mass black holes at the heart of the Cosmic Horseshoe Gravity Lens,” and the lead author is Carlos Melo Carneiro from the Universityade Federal Government of Brazil’s University. This paper is available on the ARXIV preprint server.

The physics revolution occurred in the late 20th/early 20th century, as the theory of relativity replaced Newtonian physics and pushed understanding of the universe to the next level. Rather than being separated from space and time, it became clear that they were intertwined, and that giant objects can distort spacetime.

Even light was unimmunized, and Einstein gave John Michelle’s “Dark Star” the idea of ​​a black hole that dates back to. In 1936, Einstein predicted a gravity lens, but he was not long enough to enjoy the visual evidence we enjoy today.

Now we know thousands of gravity lenses, and they have become one of the naturally occurring tools of astronomers. They exist because of the huge black holes.

The Lens Foreground Galaxy of the Cosmic Horseshoe is named LRG 3-757. This is a certain type of rare galaxy called Luminous Red Galaxy (LRG) with very bright infrared light. The LRG 3-757 is also very large, about 100 times larger than the Milky Way, and is one of the largest galaxies ever observed. Now we know that one of the most huge black holes ever detected occupy the heart of this huge galaxy.

“Supermassive black holes (SMBHs) are located at the heart of every large galaxy, and are closely connected to host galaxies through co-evolution during cosmic time,” the author wrote in his paper.

Astronomers do not find stellar black holes in the heart of large galaxies, nor do they find SMBH in the heart of d-star galaxies. There is an established link between SMBH and the host galaxy. Especially large ovals like the LRG 3-757. This study strengthens that link.

This study focuses on what is called the MBH-Sigmae relationship. It is the relationship between the mass of SMBH and the velocity dispersion of stars in galaxy bulges. Velocity variance (Sigmae) is the measurement of the velocities of stars and how much they change with their average velocity. The higher the variance of the speed, the faster and randomly the stars move.

Astronomers look at galaxies and find that the larger the SMBH, the greater the velocity dispersion. This relationship suggests a deep connection between galaxy evolution and SMBH growth. The correlation between the mass of SMBH and its galaxy velocity variance is very close, so astronomers can obtain good estimates of the mass of SMBH by measuring the velocity variance.

However, the space horseshoe-shaped UMBH is greater than the MBH-sigma e relationship suggests.

“It is expected that the largest galaxies in the universe, such as the brightest cluster galaxies (BCGs), will host the largest SMBH,” the author writes. Astronomers have discovered many UMBHs in these galaxies, including LRG 3-757. “Nevertheless, the importance of these UMBHs lies in the fact that many of them deviate from the standard linear MBH-σe relationship,” the researchers explain.

The LRG 3-757 deviates significantly from the correlation. “Our findings place space horseshoe shapes at ~1.5 sigma on the MBH-σe relationship, supporting the new trends observed in BGC and other large galaxies,” the author writes . “This suggests a more steeper MBH and σe relationship at the highest mass that could be potentially driven by different coevolutions of SMBH and its host galaxies.”

What is behind this separation of the MBH-σe relationship in large galaxies? Some stars may have been removed from the galaxy in past mergers, affecting velocity dispersion.

According to the author, LRG 3-757 could become part of a fossil group. “The horseshoe lens is unique in that it has a z = 0.44 and does not have a relatively large companion galaxy. It is probably a fossil group,” they write.

Fossil groups are large galactic groups characterized by very large galaxies at the center, often LRG. Fossil groups and LRGs represent late stages of evolution in slower activity galaxies. Most LRGs have stars, so they are “red and dead.” There is little or no intergalaxy interaction.

“Fossil groups as remnants of early galactic mergers may follow clear evolutionary pathways compared to local galaxies, potentially explaining a higher BH mass,” the authors write.

The LRG 3-757 could have experienced what is called a “scool.” Scrubs can occur when two very large galaxies merge and affect the velocity dispersion of the stars at the center of the galaxy. “In this process, binary SMBHS dynamically expels stars from the central region of the merged galaxy, effectively reducing star velocity dispersion while leaving the SMBH mass almost unchanged,” the author explains .

Another possibility is black hole/AGN feedback. When black holes are actively fed, they are called active galactic nuclei. Powerful jets and outflows from AGN can erase star formation and alter the central structure of the galaxy. This allows for the separation of SMBH growth from velocity dispersion.

“The third scenario assumes that such a UMBH could be a very bright quasar remnant.

Researchers say more observations and better models are needed “to explain the scattering of the MBH-σe relationship at the top.”

Many more observations are ongoing thanks to the Euclidean mission. “The Euclidean Mission is expected to discover hundreds of thousands of lenses over the next five years,” the author writes in his conclusion. Very large telescopes (ELTs) also contribute by allowing for more detailed dynamic studies of velocity dispersion.

“This new era of discovery promises to deepen our understanding of galaxy evolution and the interaction of balinic and DM components,” the author concludes.