Euclid Telescope Reveals a 5 Billion Solar Mass Black Hole in Galaxy NGC 1272

Core Concepts

The Euclid telescope's high-resolution imaging enabled the discovery of a massive black hole in galaxy NGC 1272, highlighting the importance of core size, rather than velocity dispersion, in identifying galaxies hosting the most massive black holes.

Abstract

Bibliographic Information:

Saglia, R., Mehrgan, K., de Nicola, S., et al. (2024). Euclid: The rb-M∗ relation as a function of redshift. I. The 5 × 10^9 M⊙ black hole in NGC 1272. Astronomy & Astrophysics manuscript no. NGC1272Euclid3.

Research Objective:

This research paper presents the first Euclid telescope-based dynamical mass determination of a supermassive black hole, focusing on NGC 1272, the second most luminous elliptical galaxy in the Perseus cluster. The study aims to demonstrate the efficacy of utilizing core size as a predictor of black hole mass in massive elliptical galaxies.

Methodology:

The researchers combined Euclid VIS photometry data from the Early Release Observations of the Perseus cluster with VIRUS spectroscopic observations from the Hobby-Eberly Telescope. They analyzed the surface brightness profile of NGC 1272 to determine its core size and employed both axisymmetric and triaxial Schwarzschild models to dynamically estimate the black hole mass and other galactic parameters.

Key Findings:

• The Euclid VIS image revealed a core in NGC 1272 with a size of 1.29 arcseconds or 0.45 kpc.
• Dynamical modeling determined a black hole mass of (5 ± 3) × 10^9 M⊙, consistent with predictions based on the MBH-rb correlation but significantly larger than estimates from the MBH-σ relation.
• The study found that NGC 1272's core size is a more accurate indicator of its black hole mass than its velocity dispersion.

Main Conclusions:

The authors conclude that the core size of massive elliptical galaxies, formed through dry mergers and subsequent core scouring, serves as a reliable indicator of the mass of their central black holes. This finding has significant implications for identifying galaxies hosting the most massive black holes, especially those with lower velocity dispersions, which may not be accurately represented by the MBH-σ relation.

Significance:

This research highlights the capabilities of the Euclid telescope in studying the dynamics of galaxies and accurately determining black hole masses. The findings emphasize the importance of core size as a key parameter in understanding the evolution of massive elliptical galaxies and their central black holes.

Limitations and Future Research:

The study acknowledges limitations due to the positioning of the IFU during observations, resulting in uneven coverage of the galaxy. Future research with more comprehensive data coverage and extending to higher redshifts is suggested to further validate the relationship between core size and black hole mass in a wider range of galaxies.

Stats

The core size of NGC 1272 is 1.′′29±0.′′07 or 0.45 kpc.
The black hole mass of NGC 1272 is (5 ± 3) × 10^9 M⊙.
The stellar mass of NGC 1272 is 9 × 10^11 M⊙.
The luminosity of NGC 1272 is 1.3 × 10^11 L⊙.
The velocity dispersion within the half-luminosity radius (σe) is 247 ± 3 km s−1.
The mass deficit (Mdef) expelled from the core during its formation is 1.9 × 10^10 M⊙, or 3.8 MBH.

Quotes

Key Insights Distilled From

Euclid: The $r_{\rm b}$-$M_\ast$ relation as a function of redshift. I. The $5 \times 10^9 M_\odot$ black hole in NGC 1272

by R. Saglia (1... at arxiv.org 11-05-2024

https://arxiv.org/pdf/2411.01927.pdf

Deeper Inquiries

How will the Euclid Wide and Deep Surveys contribute to our understanding of black hole formation and evolution in the early Universe?

The Euclid Wide and Deep Surveys promise to revolutionize our understanding of black hole formation and evolution in the early Universe in several key ways:

Unprecedented Sample Size: Euclid's wide-area coverage will enable the identification of a statistically significant sample of massive elliptical galaxies, including the rare high-redshift ones. This vast sample size will be crucial for studying the demographics of black holes across cosmic time, allowing astronomers to trace the evolution of the black hole mass function and its connection to galaxy evolution.
Resolving Cores at High Redshift: Euclid's high spatial resolution is essential for resolving the cores of galaxies at high redshift. This is crucial for measuring core radii (rb), a key parameter tightly correlated with black hole mass (MBH) through the MBH-rb relation. By measuring rb for a large sample of galaxies at different redshifts, Euclid will provide crucial data points to constrain the evolution of this relation and shed light on the co-evolution of black holes and their host galaxies.
Probing the Early Growth of Black Holes: The depth of the Euclid surveys will allow us to probe the properties of galaxies and their central black holes at high redshift (z~1), corresponding to an epoch when the Universe was significantly younger. This will provide valuable insights into the early growth phases of supermassive black holes, a period that is currently poorly constrained. By studying the MBH-rb relation at these early epochs, Euclid can help us understand the mechanisms responsible for the rapid growth of black holes in the early Universe.
Synergy with Other Surveys: Euclid's observations will be highly synergistic with other multi-wavelength surveys, such as those conducted with the James Webb Space Telescope (JWST) and the Atacama Large Millimeter/submillimeter Array (ALMA). Combining Euclid's data with these complementary datasets will provide a more holistic view of black hole growth and galaxy evolution, allowing astronomers to study the interplay between star formation, black hole accretion, and the properties of the intergalactic medium.
In summary, the Euclid Wide and Deep Surveys will provide a unique and powerful dataset for studying black hole formation and evolution in the early Universe. By combining wide-area coverage, high spatial resolution, and significant depth, Euclid will enable the discovery and characterization of a vast sample of galaxies and their central black holes, providing crucial insights into the co-evolution of these fascinating objects across cosmic time.

Could alternative mechanisms, besides dry mergers, contribute to the formation of large cores in massive elliptical galaxies and influence the MBH-rb relation?

While dry mergers are considered the dominant mechanism for forming large cores in massive elliptical galaxies and establishing the MBH-rb relation, alternative mechanisms could contribute and influence this relationship:

Tidal Deposition: As mentioned in the context, tidal interactions during galaxy encounters can strip material from the outskirts of galaxies and deposit it in the central regions. This process, known as "tidal deposition," can potentially lead to the formation of cores by increasing the central mass concentration and altering the stellar orbits. However, it remains unclear whether tidal deposition alone can explain the observed tangential anisotropy in the cores of massive ellipticals, a key signature of core scouring by binary black holes.
AGN Feedback: Active galactic nuclei (AGNs) are powered by the accretion of material onto supermassive black holes, releasing tremendous amounts of energy into the surrounding gas. This energy feedback can potentially drive powerful outflows that heat and expel gas from the central regions of galaxies, creating cores. While AGN feedback is generally considered less efficient in massive ellipticals compared to their less massive counterparts, it could still play a role in shaping the central regions and influencing the MBH-rb relation, especially in galaxies with ongoing or recent AGN activity.
Multiple Mergers: The context focuses on single dry mergers. However, massive elliptical galaxies likely experience multiple merger events throughout their lifetime. The cumulative effect of multiple mergers, each potentially involving binary black hole scouring and AGN feedback, could lead to more complex core structures and influence the MBH-rb relation in ways that are not fully understood.
Cosmic Evolution of the MBH-σ Relation: The MBH-rb relation is empirically calibrated at low redshift. However, the relationship between black hole mass and velocity dispersion (MBH-σ relation) might evolve with redshift. If the MBH-σ relation was different in the early Universe, it could affect the efficiency of core scouring and the resulting MBH-rb relation.
It is important to note that these alternative mechanisms are not mutually exclusive and could act in concert with dry mergers to shape the cores of massive ellipticals. Disentangling the relative contributions of these processes is crucial for a complete understanding of core formation and the evolution of the MBH-rb relation. Future observations with Euclid, combined with sophisticated numerical simulations, will be essential for addressing this challenge.

What are the broader cosmological implications of accurately measuring black hole masses and understanding their relationship with galaxy evolution?

Accurately measuring black hole masses and understanding their relationship with galaxy evolution holds profound cosmological implications:

Constraining Galaxy Formation and Evolution Models: Supermassive black holes are now recognized as integral components of galaxies, not merely bystanders. Their growth appears intimately linked with the formation and evolution of their host galaxies. Precisely measuring black hole masses across cosmic time provides critical constraints for theoretical models of galaxy formation and evolution. By comparing observed black hole mass functions and scaling relations with model predictions, we can refine our understanding of the physical processes governing galaxy assembly, star formation, and feedback mechanisms.
Probing the Early Universe and the Growth of Structure: The relationship between black holes and galaxies provides a unique window into the early Universe. By studying the masses and properties of high-redshift black holes, we can glean information about the conditions present during the epoch of galaxy formation. This can help us understand the growth of the first galaxies and the emergence of large-scale structure in the Universe.
Testing General Relativity in Extreme Environments: Supermassive black holes represent the most extreme gravitational environments in the Universe. Accurately measuring their masses and studying their dynamics allows us to test the predictions of general relativity in strong gravity regimes. Deviations from general relativity, if observed, could point towards new physics beyond the standard model.
Understanding the Role of Feedback in Galaxy Clusters: As highlighted in the context, massive elliptical galaxies are often found at the centers of galaxy clusters. The energy released by supermassive black holes through AGN feedback can have a profound impact on the surrounding intracluster medium, influencing the formation and evolution of galaxies within the cluster. Understanding the details of this feedback mechanism is crucial for explaining the observed properties of galaxy clusters and their evolution over cosmic time.
In conclusion, accurately measuring black hole masses and deciphering their intricate relationship with galaxy evolution is not merely an astrophysical curiosity. It holds significant implications for our understanding of fundamental physics, the evolution of the cosmos, and the processes that have shaped the Universe we observe today. The Euclid mission, with its ability to probe the demographics and properties of black holes across a wide range of redshifts, will undoubtedly play a crucial role in advancing this exciting field of research.