The hyperplane of early-type galaxies: using stellar population properties to increase the precision and accuracy of the fundamental plane as a distance indicator

ABSTRACT We use deep spectroscopy from the SAMI (Sydney-AAO Multi-object Integral) Galaxy Survey to explore the precision of the fundamental plane (FP) of early-type galaxies as a distance indicator for future single-fibre spectroscopy surveys. We study the optimal trade-off between sample size and...

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Veröffentlicht in:Monthly notices of the Royal Astronomical Society 2024-08, Vol.532 (2), p.1775-1795
Hauptverfasser: D’Eugenio, Francesco, Colless, Matthew, van der Wel, Arjen, Vaughan, Sam P, Said, Khaled, van de Sande, Jesse, Bland-Hawthorn, Joss, Bryant, Julia J, Croom, Scott M, López-Sánchez, Ángel R, Lorente, Nuria P F, Maiolino, Roberto, Taylor, Edward N
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container_end_page 1795
container_issue 2
container_start_page 1775
container_title Monthly notices of the Royal Astronomical Society
container_volume 532
creator D’Eugenio, Francesco
Colless, Matthew
van der Wel, Arjen
Vaughan, Sam P
Said, Khaled
van de Sande, Jesse
Bland-Hawthorn, Joss
Bryant, Julia J
Croom, Scott M
López-Sánchez, Ángel R
Lorente, Nuria P F
Maiolino, Roberto
Taylor, Edward N
description ABSTRACT We use deep spectroscopy from the SAMI (Sydney-AAO Multi-object Integral) Galaxy Survey to explore the precision of the fundamental plane (FP) of early-type galaxies as a distance indicator for future single-fibre spectroscopy surveys. We study the optimal trade-off between sample size and signal-to-noise ratio (SNR), and investigate which additional observables can be used to construct hyperplanes with smaller intrinsic scatter than the FP. We add increasing levels of random noise (parametrized as effective exposure time) to the SAMI spectra to study the effect of increasing measurement uncertainties on the FP- and hyperplane-inferred distances. We find that, using direct-fit methods, the values of the FP and hyperplane best-fitting coefficients depend on the spectral SNR, and reach asymptotic values for a mean $\langle \mathrm{ SNR} \rangle =40\, \mathrm{\mathring{\rm A}}^{-1}$. As additional variables for the FP we consider three stellar-population observables: light-weighted age, stellar mass-to-light ratio, and a novel combination of Lick indices ($I_\mathrm{age}$). For an $\langle \mathrm{ SNR} \rangle =45~\mathrm{\mathring{\rm A}}^{-1}$ (equivalent to 1-h exposure on a 4-m telescope), all three hyperplanes outperform the FP as distance indicators. Being an empirical spectral index, $I_\mathrm{age}$ avoids the model-dependent uncertainties and bias underlying age and mass-to-light ratio measurements, yet yields a 10 per cent reduction of the median distance uncertainty compared to the FP. We also find that, as a by-product, the $I_\mathrm{age}$ hyperplane removes most of the reported environment bias of the FP. After accounting for the different SNR, these conclusions also apply to a 50 times larger sample from SDSS-III (Sloan Digital Sky Survey). However, in this case, only $\mathrm{ age}$ removes the environment bias.
doi_str_mv 10.1093/mnras/stae1582
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subjects Aerial surveys
Age
Asymptotic methods
Bias
Galaxies
Hyperplanes
Noise measurement
Random noise
Signal to noise ratio
Sky surveys (astronomy)
Spectrum analysis
Stellar age
Stellar mass
Uncertainty
title The hyperplane of early-type galaxies: using stellar population properties to increase the precision and accuracy of the fundamental plane as a distance indicator
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