Vanderbilt University, Nashville, TN (United States); National Science Foundation (NSF), Alexandria, VA (United States)
Vanderbilt University, Nashville, TN (United States); Swinburne University of Technology, Hawthorn, VIC (Australia); ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) (Australia)
This paper represents an effort to provide robust constraints on the galaxy–halo connection and simultaneously test the Planck ΛCDM cosmology using a fully numerical model of small-scale galaxy clustering. We explore two extensions to the standard Halo Occupation Distribution model: assembly bias, whereby halo occupation depends on both halo mass and the larger environment, and velocity bias, whereby galaxy velocities do not perfectly trace the velocity of the dark matter within the halo. Moreover, we incorporate halo mass corrections to account for the impact of baryonic physics on the halo population. We identify an optimal set of clustering measurements to constrain this "decorated" HOD model for both low- and high-luminosity galaxies in SDSS DR7. We find that, for low-luminosity galaxies, a model with both assembly bias and velocity bias provides the best fit to the clustering measurements, with no tension remaining in the fit. In this model, we find evidence for both central and satellite galaxy assembly bias at the 99% and 95% confidence levels, respectively. In addition, we find evidence for satellite galaxy velocity bias at the 99.9% confidence level. For high-luminosity galaxies, we find no evidence for either assembly bias or velocity bias, but our model exhibits significant tension with SDSS measurements. We find that all of these conclusions still stand when we include the effects of baryonic physics on the halo mass function, suggesting that the tension we find for high-luminosity galaxies may be due to a problem with our assumed cosmological model.
Beltz-Mohrmann, Gillian D., et al. "Toward Accurate Modeling of Galaxy Clustering on Small Scales: Halo Model Extensions and Lingering Tension." The Astrophysical Journal, vol. 948, no. 2, May. 2023. https://doi.org/10.3847/1538-4357/acc576
Beltz-Mohrmann, Gillian D., Szewciw, Adam O., Berlind, Andreas A., & Sinha, Manodeep (2023). Toward Accurate Modeling of Galaxy Clustering on Small Scales: Halo Model Extensions and Lingering Tension. The Astrophysical Journal, 948(2). https://doi.org/10.3847/1538-4357/acc576
Beltz-Mohrmann, Gillian D., Szewciw, Adam O., Berlind, Andreas A., et al., "Toward Accurate Modeling of Galaxy Clustering on Small Scales: Halo Model Extensions and Lingering Tension," The Astrophysical Journal 948, no. 2 (2023), https://doi.org/10.3847/1538-4357/acc576
@article{osti_2332730,
author = {Beltz-Mohrmann, Gillian D. and Szewciw, Adam O. and Berlind, Andreas A. and Sinha, Manodeep},
title = {Toward Accurate Modeling of Galaxy Clustering on Small Scales: Halo Model Extensions and Lingering Tension},
annote = {This paper represents an effort to provide robust constraints on the galaxy–halo connection and simultaneously test the Planck ΛCDM cosmology using a fully numerical model of small-scale galaxy clustering. We explore two extensions to the standard Halo Occupation Distribution model: assembly bias, whereby halo occupation depends on both halo mass and the larger environment, and velocity bias, whereby galaxy velocities do not perfectly trace the velocity of the dark matter within the halo. Moreover, we incorporate halo mass corrections to account for the impact of baryonic physics on the halo population. We identify an optimal set of clustering measurements to constrain this "decorated" HOD model for both low- and high-luminosity galaxies in SDSS DR7. We find that, for low-luminosity galaxies, a model with both assembly bias and velocity bias provides the best fit to the clustering measurements, with no tension remaining in the fit. In this model, we find evidence for both central and satellite galaxy assembly bias at the 99% and 95% confidence levels, respectively. In addition, we find evidence for satellite galaxy velocity bias at the 99.9% confidence level. For high-luminosity galaxies, we find no evidence for either assembly bias or velocity bias, but our model exhibits significant tension with SDSS measurements. We find that all of these conclusions still stand when we include the effects of baryonic physics on the halo mass function, suggesting that the tension we find for high-luminosity galaxies may be due to a problem with our assumed cosmological model.},
doi = {10.3847/1538-4357/acc576},
url = {https://www.osti.gov/biblio/2332730},
journal = {The Astrophysical Journal},
issn = {ISSN 0004-637X},
number = {2},
volume = {948},
place = {United States},
publisher = {IOP Publishing},
year = {2023},
month = {05}}
Argonne National Laboratory (ANL), Argonne, IL (United States)
Sponsoring Organization:
Alfred P. Sloan Foundation; Max Planck Society; National Aeronautic and Space Administration (NASA); National Science Foundation (NSF); USDOE Office of Science
Grant/Contract Number:
AC02-06CH11357
OSTI ID:
2332730
Journal Information:
The Astrophysical Journal, Journal Name: The Astrophysical Journal Journal Issue: 2 Vol. 948; ISSN 0004-637X
