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The ALHAMBRA survey: tight dependence of the optical mass-to-light ratio on galaxy colour up to z = 1.5

  • López-Sanjuan, C.
  • Díaz-García, L. A.
  • Cenarro, A. J.
  • Fernández-Soto, A.
  • Viironen, K.
  • Molino, A.
  • Benítez, N.
  • Cristóbal-Hornillos, D.
  • Moles, M.
  • Varela, J.
  • Arnalte-Mur, P.
  • Ascaso, B.
  • Castander, F. J.
  • Cerviño, M.
  • Delgado, R. M. González
  • Husillos, C.
  • Márquez, I.
  • Masegosa, J.
  • Del Olmo, A.
  • Pović, M.
  • And 1 more
Published Article
Publication Date
May 09, 2018
Submission Date
May 09, 2018
DOI: 10.1051/0004-6361/201833402
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Our goal is to characterise the dependence of the optical mass-to-light ratio on galaxy colour up to z = 1.5, expanding the redshift range explored in previous work. From the ALHAMBRA redshifts, stellar masses, and rest-frame luminosities provided by the MUFFIT code, we derive the mass-to-light ratio vs. colour relation (MLCR) both for quiescent and star-forming galaxies. The intrinsic relation and its physical dispersion are derived with a Bayesian inference model. The rest-frame i-band mass-to-light ratio of quiescent and star-forming galaxies presents a tight correlation with the rest-frame (g - i) colour up to z = 1.5. Such MLCR is linear for quiescent galaxies and quadratic for star-forming galaxies. The intrinsic dispersion in these relations is 0.02 dex for quiescent galaxies and 0.06 dex for star-forming ones. The derived MLCRs do not present a significant redshift evolution and are compatible with previous local results in the literature. Finally, these tight relations also hold for g- and r-band luminosities. The derived MLCRs in ALHAMBRA can be used to predict the mass-to-light ratio from a rest-frame optical colour up to z = 1.5. These tight correlations do not change with redshift, suggesting that galaxies have evolved along the derived relations during the last 9 Gyr.

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