INTERPRETING THE EVOLUTION OF THE SIZE-LUMINOSITY RELATION FOR DISK GALAXIES FROM REDSHIFT 1 TO THE PRESENT

2010/11/01 by Alyson Brooks, A. M. Brooks, A. R. Solomon +15 · 98 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Electrical and Electromagnetic Research #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy formation and evolution #Halo #Redshift #Stellar mass #Stellar population #Surface brightness fluctuation #Thick disk #Tully–Fisher relation #astro-ph.CO #astro-ph.GA

paper · pdf · doi:10.1088/0004-637x/728/1/51

published in The Astrophysical Journal 728(1), 51 (IOP Publishing) · Version resubmitted to ApJ, after referee's comments

arxiv created 2010/11/01 · openalex publication_date 2011/01/19 · arxiv updated 2015/05/20 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/06

Abstract

A sample of very high resolution cosmological disk galaxy simulations is used to investigate the evolution of galaxy disk sizes back to redshift 1 within the ΛCDM cosmology. Artificial images in the rest-frame B band are generated, allowing for a measurement of disk scale lengths using surface brightness profiles as observations would, and avoiding any assumption that light must follow mass as previous models have assumed. We demonstrate that these simulated disks are an excellent match to the observed magnitude–size relation for both local disks and for disks at z = 1 in the magnitude/mass range of overlap. We disentangle the evolution seen in the population as a whole from the evolution of individual disk galaxies. In agreement with observations, our simulated disks undergo roughly 1.5 mag arcsec −2 of surface brightness dimming since z = 1. We find evidence that evolution in the magnitude–size plane varies by mass, such that galaxies with M * ⩾ 10 9 M ☉ undergo more evolution in size than luminosity, while dwarf galaxies tend to evolve potentially more in luminosity. The disks grow in such a way as to stay on roughly the same stellar-mass–size relation with time. Finally, due to an evolving stellar-mass–star-formation-rate (SFR) relation, a galaxy at a given stellar mass (or size) at z = 1 will reside in a more massive halo and have a higher SFR, and thus a higher luminosity, than a counterpart of the same stellar mass at z = 0.

Citations

• Galaxies in a simulated ΛCDM Universe - I. Cold mode and hot cores
• A fundamental relation between mass, star formation rate and metallicity in local and high-redshift galaxies
• Scalelength of disc galaxies
• Modelling angular momentum history in dark matter haloes
• The angular momentum content of dwarf galaxies: new challenges for the theory of galaxy formation
• Large Disklike Galaxies at High Redshift
• On the Origin of Exponential Disks at High Redshift
• The Angular Momentum Distribution of Gas and Dark Matter in Galactic Halos
• The reversal of the star formation-density relation in the distant universe
• The Energy Output of the Universe from 0.1 to 1000 μm
• Core condensation in heavy halos: a two-stage theory for galaxy formation and clustering
• CONNECTING GALAXIES, HALOS, AND STAR FORMATION RATES ACROSS COSMIC TIME
• Origin of the Angular Momentum of Galaxies
• A theory of the interstellar medium - Three components regulated by supernova explosions in an inhomogeneous substrate
• Damped Lyman α systems in galaxy formation simulations
• The UV‐Optical Color Magnitude Diagram. II. Physical Properties and Morphological Evolution On and Off of a Star‐forming Sequence
• Star Formation, Supernova Feedback, and the Angular Momentum Problem in Numerical Cold Dark Matter Cosmogony: Halfway There?
• Dependence of Halo Properties on Interaction History, Environment, and Cosmology
• Do mergers spin-up dark matter haloes?
• K-Corrections and Filter Transformations in the Ultraviolet, Optical, and Near-Infrared
• The angular momentum of dark haloes: merger and accretion effects
• Molecular Hydrogen and Global Star Formation Relations in Galaxies
• Starburst99: Synthesis Models for Galaxies with Active Star Formation
• The Baryon Content of Extremely Low Mass Dwarf Galaxies
• The star formation history ofK-selected galaxies
• Effects of supernova feedback on the formation of galaxy discs
• The Origin and Evolution of the Mass-Metallicity Relationship for Galaxies: Results from Cosmological N -Body Simulations
• The formation and assembly of a typical star-forming galaxy at redshift z ≈ 3
• Disk Evolution sincez ∼ 1 in a CDM Universe
• Cosmic Evolution of Stellar Disk Truncations: Fromz ∼ 1 to the Local Universe
• Dark Halo and Disk Galaxy Scaling Laws in Hierarchical Universes
• High Galactic latitude polarized emission at 1.4 GHz and implications for cosmic microwave background observations
• Towards a resolution of the galactic spin crisis: mergers, feedback and spin segregation
• The Size Evolution of High-Redshift Galaxies
• Star formation and feedback in smoothed particle hydrodynamic simulations – I. Isolated galaxies
• Can gas prevent the destruction of thin stellar discs by minor mergers?
• Multiwavelength Study of Massive Galaxies atz∼2. I. Star Formation and Galaxy Growth
• HIGH-RESOLUTION ROTATION CURVES AND GALAXY MASS MODELS FROM THINGS
• Scaling Relations of Spiral Galaxies
• FIVE-YEARWILKINSON MICROWAVE ANISOTROPY PROBEOBSERVATIONS: COSMOLOGICAL INTERPRETATION
• How galaxies lose their angular momentum
• SINGS: TheSIRTFNearby Galaxies Survey
• Dark Matter and Stellar Mass in the Luminous Regions of Disk Galaxies
• Modelling galaxies with a 3d multi-phase ISM
• The Geneva-Copenhagen survey of the Solar neighbourhood

Cited by

• Edge-on Galaxies in the Hubble Ultra Deep Field