In other words, by not taking the effect of Laniakea into account, the Hubble tension seemed smaller than it actually is. These new results show that the tension is 2% – 3% greater than we thought.
Yes, accounting for the Laniakea Supercluster could make the Hubble tension even larger. The Hubble tension is one of the great unsolved mysteries of cosmology. It stems from our inability to pin down the precise rate of cosmic expansion.
The Laniakea Supercluster is the galaxy supercluster that is home to the Milky Way and approximately 100,000 other nearby galaxies. A team of researchers recently uncovered that the influence of the Laniakea Supercluster upon our measurements is more influential than once thought. This revelation prompts a recalculation of the Hubble tension, exposing a 2-3% underestimation of the cosmic fray.
The Hubble tension is also known as the H0 discrepancy. The discrepancy between the H0 values measured from the local distance ladder and from the CMB is the most serious challenge to the standard ACDM model
Here are some structures that are larger than the Laniakea Supercluster:
- Shapley Supercluster The largest structure in the local universe, containing more than 8,000 galaxies and with a mass of more than 10 million billion times that of the sun
- Hercules–Corona Borealis Great Wall The largest known structure in the observable universe, measuring approximately 10 billion light-years in length
- South Pole Wall A newly identified structure that lies immediately beyond the Laniakea Supercluster
- Saraswati A supercluster that is over 650 million light years in diameter
The reduced Hubble constant, h, is defined as H0/100, where H0 is the present-day Hubble parameter. The Hubble constant is calculated by comparing distance values to the apparent recessional velocity of the target galaxies.
The exact value of the Hubble constant is somewhat uncertain, but is generally believed to be around 70 kilometers per second for every megaparsec in distance, km/sec/Mpc. The current best direct measurement of the Hubble constant is 73.8 km/sec/Mpc (give or take 2.4 km/sec/Mpc including, both random and systematic errors), corresponding to a 3% uncertainty.
The Hubble parameter is defined as the rate of change of the distance between two points in the universe, divided by the distance between those two points. The Hubble parameter is getting smaller because the denominator is getting bigger more quickly than the numerator
Here are some structures outside the Laniakea Supercluster:
- Shapley, Hercules, Coma, and Perseus–Pisces: These are complexes of galaxies outside the Laniakea Supercluster
- South Pole Wall: This newly identified structure wraps the region like an arm, with the densest part in the direction of the Earth’s South Pole
- Taurus Void: This is a vast, near-empty region of space situated between the Perseus–Pisces Supercluster and the Virgo Supercluster
The Laniakea Supercluster is a constituent part of the Pisces–Cetus Supercluster Complex, a galaxy filament.
The Hubble tension is a problem in cosmology that occurs when measuring the Hubble constant, or the rate of the universe’s expansion, two different ways. The two methods yield different answers:
- Late universe Measurements using calibrated distance ladder techniques have converged on a value of approximately 73 (km/s)/Mpc.
- Early universe Techniques based on measurements of the cosmic microwave background have become available since 2000, and these agree on a value near 67.7 (km/s)/Mpc.
The Hubble tension is arguably the most pressing problem in cosmology today. The most exciting possibility is that the tension is a clue about something we are missing in our understanding of the cosmos.
Early dark energy (EDE) offers a solution to the Hubble tension
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