The Rest-Frame Far-Ultraviolet Morphologies of Star-Forming Galaxies at z ~ 1.5 and 4

By J. Lotz, P. Madau, M. Giavalisco, Joel R. Primack, H. Ferguson. 2006

161 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Computer Vision and Pattern Recognition

View Paper: https://www.semanticscholar.org/paper/e3e49f88f599ef1341384a0200059d1db2384f17

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Citations in the corpus

GEMS: Galaxy Fitting Catalogs and Testing Parametric Galaxy Fitting Codes: GALFIT and GIM2D (2007, background): “…of total brightness, galaxy half-light size, and structure, using metrics which do not depend on a galaxy, having a structure well-described by any particular functional form (e.g., Petrosian 1976; Abraham et al. 2 Häußler et al. 1996; Bershady, Jangren & Conselice 2000; Lotz et al. 2006).”
BULGE AND CLUMP EVOLUTION IN HUBBLE ULTRA DEEP FIELD CLUMP CLUSTERS, CHAINS AND SPIRAL GALAXIES (2008, background): “…more massive at higher redshifts, partly because of bandshifting of UV-bright regions into the optical bands, and partly because of an increased importance of interactions in the young universe (e.g., Abraham et al. 1996a, 1996b; Conselice et al. 2005; Elmegreen & Elmegreen 2005; Lotz et al. 2006).”
CONSTRAINTS ON THE ASSEMBLY AND DYNAMICS OF GALAXIES. I. DETAILED REST-FRAME OPTICAL MORPHOLOGIES ON KILOPARSEC SCALE OF z ∼ 2 STAR-FORMING GALAXIES (2010, methodology): “Accordingly, we also followed a non-parametric approach to characterize in detail morphologies of our galaxies, measuring the Gini,M20, and Multiplicity coefficients, which have been introduced and applied by Abraham et al. (2003), Lotz et al. (2004, 2006), and Law et al. (2007a).”
EVIDENCE FOR UBIQUITOUS COLLIMATED GALACTIC-SCALE OUTFLOWS ALONG THE STAR-FORMING SEQUENCE AT z ∼ 0.5 (2013, methodology): “For galaxies in the EGS, we use segmentation maps generated from the sum of the V606 and i814 images provided by J. Lotz and described in Lotz et al. (2006).”
MOST SUBMILLIMETER GALAXIES ARE MAJOR MERGERS (2010, background): “High-redshift galaxies are clumpy and irregular, which may either be the result of on-going mergers (Lotz et al. 2006; Conselice et al. 2008), or the consequence of clumpy star formation in a kinematically more coherent structure such as an underlying rotating disk (Förster-Schreiber et al. 2006,…”
HYDRODYNAMICS OF HIGH-REDSHIFT GALAXY COLLISIONS: FROM GAS-RICH DISKS TO DISPERSION-DOMINATED MERGERS AND COMPACT SPHEROIDS (2010, background): “First, determinations of the merger rate from highredshift surveys are usually based on irregular structures or disturbed kinematics (e.g., Conselice et al. 2003; Lotz et al. 2006, 2008; Overzier et al. 2010; Jogee et al. 2009; López-Sanjuan et al. 2009; Puech 2010).”
SPECTROSCOPIC OBSERVATIONS OF LYMAN BREAK GALAXIES AT REDSHIFTS ∼4, 5, AND 6 IN THE GOODS-SOUTH FIELD (2009, methodology): “…1996a,b), including studies of their morphology and size (Giavalisco et al. 1996; Papovich et al. 2003; Ravindranath et al. 2006; Law et al. 2007; Lotz et al. 2006; Ferguson et al. 2004), their ages and stellar masses (Papovich et al. 2000; Shapley et al. 2000; Dickinson et al. 2003a), their…”
Resolved Galaxies in the Hubble Ultra Deep Field: Star Formation in Disks at High Redshift (2007, background): “The resulting rest-frame UV intensity profile could differ from the rest-frame B-band profile if there is a red bulge or other old component in the disk that is not prominent in the rest-frame UV (Giavalisco et al. 1996; Kuchinski et al. 2000; Lotz et al. 2006).”
The Physical Nature of Rest-UV Galaxy Morphology during the Peak Epoch of Galaxy Formation (2006, unknown): “13 kpc at the redshift of our sample, similar to previous analyses (Conselice et al. 2003a, LPM04, Lotz et al. 2006) whose selection radii Figure 2 (continued) range up to about 10 kpc. Based on visual analysis of ACS and ground-based color maps, this appears to be the optimal choice of distance…”
THE MAJOR AND MINOR GALAXY MERGER RATES AT z < 1.5 (2011, background): “Extremely deep images (i.e. the Hubble Ultra Deep Field; Beckwith et al. 2006) can give asymmetry values 0.05− 0.10 higher than lower signal-to-noise images of the same galaxy (Shi et al. 2009; Lotz et al. 2006).”
THE KILOPARSEC-SCALE KINEMATICS OF HIGH-REDSHIFT STAR-FORMING GALAXIES (2009, background): “Morphologies As demonstrated by numerous authors (e.g. Abraham et al. 1996; Conselice et al. 2005; Elmegreen et al. 2005; Lotz et al. 2006; Law et al. 2007b) the morphological structure of galaxies at redshift z & 2 is highly irregular and frequently composed of multiple spatially separated…”
THE PERSISTENCE OF COOL GALACTIC WINDS IN HIGH STELLAR MASS GALAXIES BETWEEN z ∼ 1.4 AND ∼1 (2009, methodology): “These are nonparametric measurements described in Lotz et al. (2004, 2006).”
The Herschel census of infrared SEDs through cosmic time (2013, result): “Morphological studies of IR-luminous galaxies have presented contrasting results – e.g. Bell et al. (2005) and Lotz et al. (2006) report that more than half of LIRGs at z > 0.7 are gas-rich isolated spirals, whereas other studies (e.g. Le Fevre et al. 2000; Cassata et al. 2005; Bridge et al. 2007;…”
Galaxy Zoo Green Peas: discovery of a class of compact extremely star-forming galaxies (2009, background): “Many of these high redshift galaxies show disturbed morphologies (Ravindranathet al. 2006; Lotz et al. 2006), like those seen in the HST images of the star-forming Peas in Figure 7.”
The Relation between Quasar and Merging Galaxy Luminosity Functions and the Merger-driven Star Formation History of the Universe (2006, methodology): “In future samples that determine the MGLF by uniform, automated selection criteria (see, e.g., Lotz et al. 2006), our comparisons can be made more precise by inferring tmerge a priori from the simulations and directly measuring fgas in optical samples.”