Version 1
: Received: 18 January 2023 / Approved: 23 January 2023 / Online: 23 January 2023 (02:12:01 CET)
How to cite:
Shamir, L. Doppler Shift Effect as a Possible Explanation to the Hubble-Lemaitre Constant Tension. Preprints2023, 2023010390. https://doi.org/10.20944/preprints202301.0390.v1
Shamir, L. Doppler Shift Effect as a Possible Explanation to the Hubble-Lemaitre Constant Tension. Preprints 2023, 2023010390. https://doi.org/10.20944/preprints202301.0390.v1
Shamir, L. Doppler Shift Effect as a Possible Explanation to the Hubble-Lemaitre Constant Tension. Preprints2023, 2023010390. https://doi.org/10.20944/preprints202301.0390.v1
APA Style
Shamir, L. (2023). Doppler Shift Effect as a Possible Explanation to the Hubble-Lemaitre Constant Tension. Preprints. https://doi.org/10.20944/preprints202301.0390.v1
Chicago/Turabian Style
Shamir, L. 2023 "Doppler Shift Effect as a Possible Explanation to the Hubble-Lemaitre Constant Tension" Preprints. https://doi.org/10.20944/preprints202301.0390.v1
Abstract
The difference in the Hubble-Lemaitre constant determined by different probes is a yet unexplained observation. This paper proposes the contention that the tension could be explained by the Doppler shift effect of Ia supernovae or Cepheids, driven by the rotational velocity of their host galaxies relative to the rotational velocity of the Milky Way. While the effect of the Doppler shift is expected to be mild, observations show that it can lead to systematic differences in the apparent brightness, and consequently the estimated distances. A simple experiment is done by repeating a previous analysis. When using the original set of supernovae, $H_o$ is 73.758$\pm$1.943 km/s/Mpc. When using a subset of supernovae such that the host galaxies rotate in the same direction as the Milky Way, $H_o$ drops sharply to 69.049$\pm$3.42 km/s/Mpc, showing a far milder tension with the $H_o$ determined by the CMB. When using a subset of Ia supernovae that rotate in the opposite direction, Ho does not decrease, but instead it increases the Ho tension to 74.182$\pm$3.2. Further analysis will be required to determine the link between Ho observed by using Ia supernovae or Cepheids and the rotational velocity of the host galaxies.
Copyright:
This is an open access article distributed under the Creative Commons Attribution License which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
