Peter D. Mitchell
How well can we really estimate the stellar masses of galaxies from broad-band photometry?
Mitchell, Peter D.; Lacey, Cedric G; Baugh, Carlton M; Cole, S
Professor Cedric Lacey firstname.lastname@example.org
Professor Carlton Baugh email@example.com
Professor Shaun Cole firstname.lastname@example.org
Director of the Institute for Computational Cosmology
The estimated stellar masses of galaxies are widely used to characterize how the galaxy population evolves over cosmic time. If stellar masses can be estimated in a robust manner, free from any bias, global diagnostics such as the stellar mass function can be used to constrain the physics of galaxy formation. We explore how galaxy stellar masses, estimated by fitting broad-band spectral energy distributions (SEDs) with stellar population models, can be biased as a result of commonly adopted assumptions for the star formation and chemical enrichment histories, recycled fractions and dust attenuation curves of galaxies. We apply the observational technique of broad-band SED fitting to model galaxy SEDs calculated by the theoretical galaxy formation model GALFORM, isolating the effect of each of these assumptions. We find that, averaged over the entire galaxy population, the common assumption of exponentially declining star formation histories does not, by itself, adversely affect stellar mass estimation. However, we also show that this result does not hold when considering galaxies that have undergone a recent burst of star formation. We show that fixing the metallicity in SED fitting or using sparsely sampled metallicity grids can introduce mass-dependent systematics into stellar mass estimates. We find that the common assumption of a star–dust geometry corresponding to a uniform foreground dust screen can cause the stellar masses of dusty model galaxies to be significantly underestimated. Finally, we show that stellar mass functions recovered by applying SED fitting to model galaxies at high redshift can differ significantly in both shape and normalization from the intrinsic mass functions predicted by a given model. In particular, the effects of dust can reduce the normalization at the high-mass end by up to 0.6 dex in some cases. Given these differences, our methodology of using stellar masses estimated from model galaxy SEDs offers a new, self-consistent way to compare model predictions with observations. We conclude that great care should be taken when comparing theoretical galaxy formation models to observational results based on the estimated stellar masses of high-redshift galaxies.
Mitchell, P. D., Lacey, C. G., Baugh, C. M., & Cole, S. (2013). How well can we really estimate the stellar masses of galaxies from broad-band photometry?. Monthly Notices of the Royal Astronomical Society, 435(1), 87-114. https://doi.org/10.1093/mnras/stt1280
|Journal Article Type||Article|
|Publication Date||Oct 11, 2013|
|Deposit Date||May 14, 2014|
|Publicly Available Date||May 20, 2014|
|Journal||Monthly Notices of the Royal Astronomical Society|
|Publisher||Royal Astronomical Society|
|Peer Reviewed||Peer Reviewed|
|Keywords||Galaxies, Fundamental parameters, Stellar content.|
Published Journal Article
This article has been published in the Monthly Notices of the Royal Astronomical Society <br /> © 2013 The Authors.<br /> Published by Oxford University Press on behalf of The Royal Astronomical Society. All rights reserved.
You might also like
Galaxy clustering from the bottom up: A Streaming Model emulator I
Towards an accurate model of small-scale redshift-space distortions in modified gravity
Fast full N-body simulations of generic modified gravity: derivative coupling models
Halo merger tree comparison: impact on galaxy formation models