Constraints on a Universal Stellar Initial Mass Function from Ultraviolet to Near-Infrared Galaxy Luminosity Densities

By I. Baldry, Karl Glazebrook. 2003

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In Astronomy and Astrophysics

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Galaxy bimodality versus stellar mass and environment (2006, methodology): “Note with the IMF and mass-to-light ratios used in this paper, Ωstars ≈ 0.002 (cf. Persic & Salucci 1992; Baldry & Glazebrook 2003; Nagamine et al. 2006). c© 2006 RAS, MNRAS 000, 1–19 Figure A1.”
MODELING THE EXTRAGALACTIC BACKGROUND LIGHT FROM STARS AND DUST (2009, methodology): “Baldry & Glazebrook (2003) fit local luminosity density data to find a preferred IMF, which is similar to a Salpeter IMF abovem = 0.5 (ξ(m) ∝ m−2.2) but flatter below this mass (ξ(m) ∝ m−1.5).”
Ultraviolet to Mid-Infrared Observations of Star-forming Galaxies at z ~ 2: Stellar Masses and Stellar Populations (2005, methodology): “…IMF to facilitate comparison with other work (e.g., Cole et al. 2001; Shapley et al. 2001); use of the Chabrier (2003) IMF, the IMF proposed by Baldry & Glazebrook (2003), or the “diet” Salpeter IMF used by Bell et al. (2003), would reduce the inferred stellar masses by a factor of ∼ 1.5− 1.8.”
Star formation and mass assembly in high-redshift galaxies (2009, methodology): “Masses and SFRs of Juneau et al. (2005) were instead renormalized from a Baldry & Glazebrook (2003) to a Salpeter (1955) IMF using the factors 1.82 (Juneau et al. 2005) and 2 (Hopkins & Beacom 2006).”
Toward Understanding Massive Star Formation (2007, result): “Even population studies at moderate to high redshift are consistent with the assumption of a Salpeter power law (e.g., Baldry & Glazebrook 2003).”
THE STAR FORMATION HISTORY OF MASS-SELECTED GALAXIES IN THE COSMOS FIELD (2010, methodology): “…from the Astronomical Imaging Processing System (AIPS) (see Schinnerer et al. 2007, for 22 Logarithmic masses and SFRs based on a Salpeter (1955) IMF, a Kroupa (2001) IMF and a Baldry & Glazebrook (2003) IMF are converted to the Chabrier scale by adding -0.24 dex, 0 dex and 0.02 dex, respectively.”
Semi-analytic modelling of the extragalactic background light and consequences for extragalactic gamma-ray spectra: Modelling of the EBL and gamma-ray spectra (2012, methodology): “The authors favour their model (‘C’) with a Baldry & Glazebrook (2003) IMF and star formation history from Hopkins & Beacom (2006) with Cole et al. (2001) parametrization.”
The rising star formation histories of distant galaxies and implications for gas accretion with time (2010, result): “This is similar to the findings of Baldry & Glazebrook (2003) based on SFHs derived from the UV to IR luminosity densities of low-redshift galaxies.”
Galaxy and Mass Assembly (GAMA): the star formation rate dependence of the stellar initial mass function (2011, background): “The IMF is often parametrized as one or more power laws, describing the number of stars within a given mass interval, dNdM ∝ mα with α defining the slope for the mass range of interest (Salpeter 1955; Baldry & Glazebrook 2003).”
THE COSMIC CORE-COLLAPSE SUPERNOVA RATE DOES NOT MATCH THE MASSIVE-STAR FORMATION RATE (2011, background): “These choices are applicable for the Salpeter A IMF, which is a modified Salpeter IMF with a turnover below 1M⊙ (Baldry & Glazebrook 2003).”
Reconstructing the star formation history of the Milky Way disc(s) from chemical abundances (2014, methodology): “We chose the popular IMFs of Salpeter (1955) and Kroupa (2001), the historically important Scalo (1998) IMF, and for illustrative purposes the IMF of Baldry & Glazebrook (2003).”
Evolution of the Intergalactic Opacity: Implications for the Ionizing Background, Cosmic Star Formation, and Quasar Activity (2008, methodology): “To the luminosity density measurements, dust corrections (where necessary), SFR calibrations, and IMF assumptions are applied to derive the star formation history.”
The galaxy stellar mass-star formation rate relation: evidence for an evolving stellar initial mass function? (2007, background): “…the most careful work on trying to reconcile fossil light measures with redshift-integrated measures of stellar mass. Extending the analyses of Baldry & Glazebrook (2003) and Hopkins & Beacom (2006) by including extragalactic background light (EBL) constraints, they found that no standard IMF…”
Improved constraints on the expansion rate of the Universe up to z ∼ 1.1 from the spectroscopic evolution of cosmic chronometers (2012, methodology): “0n and Hδ, in the range 0.6 < z < 1.2 and with masses M > 1010.2M ⊙. Stellar masses have been derived from template ﬁts to the multicolor photometry [54], assuming a Baldry et al. (2003) IMF [55]. Masses have been scaled by -0.03 dex to convert them to a Chabrier IMF [42, 53]. ETGs have bee”
Evidence for a Nonuniversal Stellar Initial Mass Function from the Integrated Properties of SDSS Galaxies (2007, background): “For example, the Miller & Scalo (1979) and Scalo (1986) solar neighborhood IMFs are rejected by integrated light approaches, i.e., Kennicutt (1983, hereafter K83), Kennicutt et al. (1994, hereafter KTC94), and Baldry & Glazebrook (2003).”
The Stellar Mass Assembly of Galaxies from z = 0 to z = 4: Analysis of a Sample Selected in the Rest-Frame Near-Infrared with Spitzer (2007, methodology): “For example, a Kroupa et al. (1993) IMF (as the one used in Borch et al. 2006) predicts stellar masses smaller than ours by a factor of ∼1.7, or a Baldry & Glazebrook (2003) IMF (used in, for example, Glazebrook et al. 2004) predicts also smaller masses by a factor of ∼1.8.”
Gravitationally lensed quasars and supernovae in future wide-field optical imaging surveys (2010, methodology): “…of core-collapse SNe is simply proportional to the cosmic star formation rate: ncc(z) = CccρSFR(z), (16) where Ccc = 0.0132 M−1 was derived assuming that core-collapse SNe are produced in the stellar mass range 8 M 50 M , together with the initial mass function of Baldry & Glazebrook (2003).”
Cosmic Star Formation History and Its Dependence on Galaxy Stellar Mass (2004, unknown): “Throughout this paper, we adopt the Baldry & Glazebrook (2003) (BG03) Initial Mass Function (IMF), which has a very similar slope to the Salpeter (1955) IMF at high masses and provides a good fit to cosmic and galaxy colors locally.”
On the galaxy stellar mass function, the mass-metallicity relation, and the implied baryonic mass function (2008, methodology): “Baldry & Glazebrook (2003) give a range from 0.035 to 0.063 from fitting to the local cosmic luminosity densities (over a range of IMFs but similar to those used here in terms of M/L) and Nagamine et al. (2006) found 0.051 ± 0.009 from fitting to various data including the extragalactic background…”