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Title: THE RELATION BETWEEN DYNAMICAL MASS-TO-LIGHT RATIO AND COLOR FOR MASSIVE QUIESCENT GALAXIES OUT TO z ∼ 2 AND COMPARISON WITH STELLAR POPULATION SYNTHESIS MODELS

Abstract

We explore the relation between the dynamical mass-to-light ratio (M/L) and rest-frame color of massive quiescent galaxies out to z ∼ 2. We use a galaxy sample with measured stellar velocity dispersions in combination with Hubble Space Telescope and ground-based multi-band photometry. Our sample spans a large range in log M {sub dyn}/L {sub g} (of 1.6 dex) and log M {sub dyn}/L {sub K} (of 1.3 dex). There is a strong, approximately linear correlation between the M/L for different wavebands and rest-frame color. The root-mean-square scatter in log M {sub dyn}/L residuals implies that it is possible to estimate the M/L with an accuracy of ∼0.25 dex from a single rest-frame optical color. Stellar population synthesis (SPS) models with a Salpeter stellar initial mass function (IMF) cannot simultaneously match M {sub dyn}/L {sub g} versus (g – z){sub rest-frame} and M {sub dyn}/L {sub K} versus (g – K){sub rest-frame}. By changing the slope of the IMF we are still unable to explain the M/L of the bluest and reddest galaxies. We find that an IMF with a slope between α = 2.35 and α = 1.35 provides the best match. We also explore a broken IMF with amore » Salpeter slope at M < 1 M {sub ☉} and M > 4 M {sub ☉} and a slope α in the intermediate region. The data favor a slope of α = 1.35 over α = 2.35. Nonetheless, our results show that variations between different SPS models are comparable to the IMF variations. In our analysis we assume that the variation in M/L and color is driven by differences in age, and that other contributions (e.g., metallicity evolution, dark matter) are small. These assumptions may be an important source of uncertainty as galaxies evolve in more complex ways.« less

Authors:
;  [1];  [2];  [3];  [4]
  1. Leiden Observatory, Leiden University, P.O. Box 9513, 2300 RA Leiden (Netherlands)
  2. Astronomy Department, University of California at Berkeley, Berkeley, CA 94720 (United States)
  3. Steward Observatory, University of Arizona, Tucson, AZ 85721 (United States)
  4. Department of Astronomy, Yale University, P.O. Box 208101, New Haven, CT 06520-8101 (United States)
Publication Date:
OSTI Identifier:
22364413
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 799; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; APPROXIMATIONS; COLOR; COMPARATIVE EVALUATIONS; CORRELATIONS; GALACTIC EVOLUTION; GALAXIES; MASS; METALLICITY; NONLUMINOUS MATTER; PHOTOMETRY; SPACE; STAR EVOLUTION; TELESCOPES; VARIATIONS; VISIBLE RADIATION

Citation Formats

Van de Sande, Jesse, Franx, Marijn, Kriek, Mariska, Bezanson, Rachel, and Van Dokkum, Pieter G. THE RELATION BETWEEN DYNAMICAL MASS-TO-LIGHT RATIO AND COLOR FOR MASSIVE QUIESCENT GALAXIES OUT TO z ∼ 2 AND COMPARISON WITH STELLAR POPULATION SYNTHESIS MODELS. United States: N. p., 2015. Web. doi:10.1088/0004-637X/799/2/125.
Van de Sande, Jesse, Franx, Marijn, Kriek, Mariska, Bezanson, Rachel, & Van Dokkum, Pieter G. THE RELATION BETWEEN DYNAMICAL MASS-TO-LIGHT RATIO AND COLOR FOR MASSIVE QUIESCENT GALAXIES OUT TO z ∼ 2 AND COMPARISON WITH STELLAR POPULATION SYNTHESIS MODELS. United States. https://doi.org/10.1088/0004-637X/799/2/125
Van de Sande, Jesse, Franx, Marijn, Kriek, Mariska, Bezanson, Rachel, and Van Dokkum, Pieter G. 2015. "THE RELATION BETWEEN DYNAMICAL MASS-TO-LIGHT RATIO AND COLOR FOR MASSIVE QUIESCENT GALAXIES OUT TO z ∼ 2 AND COMPARISON WITH STELLAR POPULATION SYNTHESIS MODELS". United States. https://doi.org/10.1088/0004-637X/799/2/125.
@article{osti_22364413,
title = {THE RELATION BETWEEN DYNAMICAL MASS-TO-LIGHT RATIO AND COLOR FOR MASSIVE QUIESCENT GALAXIES OUT TO z ∼ 2 AND COMPARISON WITH STELLAR POPULATION SYNTHESIS MODELS},
author = {Van de Sande, Jesse and Franx, Marijn and Kriek, Mariska and Bezanson, Rachel and Van Dokkum, Pieter G.},
abstractNote = {We explore the relation between the dynamical mass-to-light ratio (M/L) and rest-frame color of massive quiescent galaxies out to z ∼ 2. We use a galaxy sample with measured stellar velocity dispersions in combination with Hubble Space Telescope and ground-based multi-band photometry. Our sample spans a large range in log M {sub dyn}/L {sub g} (of 1.6 dex) and log M {sub dyn}/L {sub K} (of 1.3 dex). There is a strong, approximately linear correlation between the M/L for different wavebands and rest-frame color. The root-mean-square scatter in log M {sub dyn}/L residuals implies that it is possible to estimate the M/L with an accuracy of ∼0.25 dex from a single rest-frame optical color. Stellar population synthesis (SPS) models with a Salpeter stellar initial mass function (IMF) cannot simultaneously match M {sub dyn}/L {sub g} versus (g – z){sub rest-frame} and M {sub dyn}/L {sub K} versus (g – K){sub rest-frame}. By changing the slope of the IMF we are still unable to explain the M/L of the bluest and reddest galaxies. We find that an IMF with a slope between α = 2.35 and α = 1.35 provides the best match. We also explore a broken IMF with a Salpeter slope at M < 1 M {sub ☉} and M > 4 M {sub ☉} and a slope α in the intermediate region. The data favor a slope of α = 1.35 over α = 2.35. Nonetheless, our results show that variations between different SPS models are comparable to the IMF variations. In our analysis we assume that the variation in M/L and color is driven by differences in age, and that other contributions (e.g., metallicity evolution, dark matter) are small. These assumptions may be an important source of uncertainty as galaxies evolve in more complex ways.},
doi = {10.1088/0004-637X/799/2/125},
url = {https://www.osti.gov/biblio/22364413}, journal = {Astrophysical Journal},
issn = {0004-637X},
number = 2,
volume = 799,
place = {United States},
year = {Sun Feb 01 00:00:00 EST 2015},
month = {Sun Feb 01 00:00:00 EST 2015}
}