Can the faint submillimetre galaxies be explained in the Λ cold dark matter model

By C. Baugh, C. Lacey, Carlos S. Frenk, G. Granato, Laura Silva, A. Bressan, A. Benson, Shaun Cole. 2005

572 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/348c4a0687e0f31208257b6902296548bc705b46

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Citations in the corpus

How do galaxies get their gas (2002, methodology): “While semi-analytic models and hydrodynamic simulations both predict a drop in the global star formation rate (SFR) over this redshift interval, it is difficult to explain the full order-of-magnitude reduction implied by the data (Baugh et al. 2005).”
Star formation in galaxy mergers with realistic models of stellar feedback and the interstellar medium (2012, background): “Reproducing their abundance and luminosities remains a challenge for current models of galaxy formation (Baugh et al. 2005; Swinbank et al. 2008; Younger et al. 2009a; Hayward et al. 2010, 2011; Narayanan et al. 2010).”
Submillimeter Galaxies at z ~ 2: Evidence for Major Mergers and Constraints on Lifetimes, IMF, and CO-H2 Conversion Factor (2008, methodology): “However, if bursting and quiescent star formation modes have different IMFs (as assumed by Baugh et al. 2005), and/or if the obscuration of the stars powering the far-infrared luminosity is sufficiently large, a top-heavy IMF could still be compatible with the burst component.”
Evolution of the atomic and molecular gas content of galaxies (2013, background): “Lagos et al. (2011a,b) also estimated gas partitioning into an atomic and molecular component, and implemented a H2-based star formation recipe, within the GALFORM semi-analytic model (Baugh et al. 2005; Bower et al. 2006).”
THE STELLAR INITIAL MASS FUNCTION IN EARLY-TYPE GALAXIES FROM ABSORPTION LINE SPECTROSCOPY. II. RESULTS (2012, background): “The Mach number is critical to this conclusion: the thermal Jeans mass (MJ ∝ c3s ρ −1/2, wherecs andρ are the sound speed and density, respectively) in starbursts is frequently larger than in the MW disk, and thus a simple Jeans argument would suggest that the IMF in starbursts should bebottom-light”
The LABOCA survey of the Extended Chandra Deep Field South: A photometric redshift survey of submillimetre galaxies (2010, methodology): “10, we also show the absolute H-band magnitudes of SMGs in the CDM GALFORM model (Baugh et al. 2005), which assumes a top-heavy IMF with slope x = 0.”
Dusty Star Forming Galaxies at High Redshift (2014, methodology): “However, Swinbank et al. (2008) show that the synthetic K -band and mid-IR (3–8 µm) colors of the model galaxies in the Baugh et al. (2005) model are too low by up to a factor ∼10 as compared to observed SMGs.”
Semianalytical Model of Galaxy Formation with High-Resolution N-Body Simulations (2004, background): “…is also difficult for the current SAMs to simultaneously account for the observed luminosity density at the present time and the star formation rate at zk 3 as inferred from the submillimeter sources (Chapman et al. 2002; Cowie et al. 2002; Smail et al. 2002; Borys et al. 2003; Baugh et al. 2005).”
The evolution of stellar mass and the implied star formation history (2008, result): “The possibility of alternative IMFs in galaxies with apparently very large star formation rates is also discussed in Nagashima et al. (2005), Baugh et al. (2005), Le Delliou et al. (2006), Lacey et al. (2007) who suggest a flat IMF to reconcile a number of observations with the predictions of the…”
Effects of feedback on the morphology of galaxy discs (2005, unknown): “…formation model which, however, has been claimed to ber quired to explain the properties of high redshift sub-millimeter and Lyman-break galaxies (Baugh et al. 2005), as well as the metallicity of the intracluster medium (Nagashima et al. 2005a) and of elliptical galaxies (Nagashima et al.…”
The effect of galaxy mass ratio on merger-driven starbursts (2007, background): “Many models of galaxy formation often employ merger–driven star formation as a necessary ingredient to produce bright galaxies throughout cosmic time (Guiderdoni et al. 1998; Somerville et al. 2001; Baugh et al. 2005).”
METALLICITY-DEPENDENT QUENCHING OF STAR FORMATION AT HIGH REDSHIFT IN SMALL GALAXIES (2011, unknown): “As a result, in most current models, the decline in IR at high z drives a decline in SFR density that starts much earlier than z ∼ 1− 2 (e.g. Murali et al. 2002; Hernquist & Springel 2003; Springel & Hernquist 2003; Kereš et al. 2005; Baugh et al. 2005; Bouché et al. 2010; Schaye et al. 2010).”
Astrophysical and cosmological information from large-scale submillimetre surveys of extragalactic sources (2007, methodology): “…of the SCUBA Half Degree Extragalactic Survey (SHADES), derived from rest-frame radio-mm-far IR colours, with those yielded by the four different galaxy formation models studied by van Kampen et al. (2005) and with the semi-analytic models by Baugh et al. (2005) and by Granato et al. (2004).”
How sensitive are predicted galaxy luminosities to the choice of stellar population synthesis model (2013, background): “…to simultaneously match the number counts and redshift distribution of sub-millimiter galaxies is one of the reasons that motivated the inclusion of a top-heavy IMF in bursts of star formation in the Baugh et al. (2005) model presented in this paper) and it does not assume a universal IMF.”
The rising star formation histories of distant galaxies and implications for gas accretion with time (2010, methodology): “…“smoothly” increasing SFRs because they have formation histories that involve stochastic events with discrete changes in the instantaneous SFR (e.g., Baugh et al. 2005; Finlator et al. 2006, 2007; Somerville et al. 2008), and they may experience SFHs that deviate from the average history derived…”
A primer on hierarchical galaxy formation: the semi-analytical approach (2006, methodology): “For example, using the superwind version of the Durham model, Baugh et al. (2005) were able to reproduce the number counts of sub-millimetre selected galaxies, the luminosity function of Lyman-break galaxies at z = 3 and z = 4, whilst retaining a fair match to the present day optical and far…”
An ALMA survey of the SCUBA-2 CLS UDS field: physical properties of 707 sub-millimetre galaxies (2019, background): “The redshift distribution of SMGs can provide stringent constraints on galaxy formation models, and indeed, in some instances has forced changes in the way rapidly star-forming galaxies are modelled (e.g. Baugh et al. 2005).”
Breaking the hierarchy of galaxy formation (2005, methodology): “…models that match the luminosity function at z = 0 reasonably well often predict far fewer large galaxies at high redshift than is observed (Baugh et al. 1998, 2005; Somerville, Primack & Faber 2001); on the other hand, models that give a better match to the abundance of high-redshift…”
Galaxy formation theory (2010, methodology): “For example, Gonzalez-Perez et al. (2008) extended the model of Cole et al. (2000) by assuming that some fraction, fcloud, of the dust is in the form of dense molecular clouds where thestars form (see Baugh et al. 2005).”