Health Implications of 2,3,7,8-Tetrachlorodibenzo-p-dioxin Exposure in Primates

Allen, James; Miller, John P.

doi:10.1007/978-1-4615-8948-8_32

Cited by 11 publications

(5 citation statements)

References 11 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The F -test provides a quantitative means of judging the relative likelihood of different structural decompositions. There are of course other approaches (e.g., Allen et al 2006), but the F -test seems to be a powerful and straightforward approach as we show below. For each model we estimate the reduced χ 2 using the fit residuals and the number of resolution elements per fit, n res , in this instance estimated as n res = n pixels /(πΘ 2 ), where n pixels is the number of unmasked (object) pixels used in the fit and Θ is the r-band seeing half-width at half maximum (HWHM) in pixels.…”

Section: Selecting the Appropriate Model With The F-statisticmentioning

confidence: 93%

A Catalog of Bulge+disk Decompositions and Updated Photometry for 1.12 Million Galaxies in the Sloan Digital Sky Survey

Simard

Mendel

Patton

et al. 2011

ApJS

641

1,147

View full text Add to dashboard Cite

We perform two-dimensional, point-spread-function-convolved, bulge+disk decompositions in the g and r bandpasses on a sample of 1,123,718 galaxies from the Legacy area of the Sloan Digital Sky Survey Data Release Seven. Four different decomposition procedures are investigated which make improvements to sky background determinations and object deblending over the standard SDSS procedures that lead to more robust structural parameters and integrated galaxy magnitudes and colors, especially in crowded environments. We use a set of science-based quality assurance metrics, namely, the disk luminosity-size relation, the galaxy color-magnitude diagram, and the galaxy central (fiber) colors to show the robustness of our structural parameters. The best procedure utilizes simultaneous, two-bandpass decompositions. Bulge and disk photometric errors remain below 0.1 mag down to bulge and disk magnitudes of g 19 and r 18.5. We also use and compare three different galaxy fitting models: a pure Sérsic model, an n b = 4 bulge + disk model, and a Sérsic (free n b ) bulge + disk model. The most appropriate model for a given galaxy is determined by the F-test probability. All three catalogs of measured structural parameters, rest-frame magnitudes, and colors are publicly released here. These catalogs should provide an extensive comparison set for a wide range of observational and theoretical studies of galaxies.

show abstract

Section: Selecting the Appropriate Model With The F-statisticmentioning

confidence: 93%

A Catalog of Bulge+disk Decompositions and Updated Photometry for 1.12 Million Galaxies in the Sloan Digital Sky Survey

Simard

Mendel

Patton

et al. 2011

ApJS

641

1,147

View full text Add to dashboard Cite

show abstract

“…Therefore, these three groups correspond to our two component galaxies. Additionally Binggeli & Cameron have a type V, which has a deficiency of flux in the center compared to an exponential profile (also see Allen et al 2006). These models might be to some degree represented in our models with an outer component with n < 1.…”

Section: Comparison With More Massive Galaxiesmentioning

confidence: 99%

A Near-Infrared Census of the Multicomponent Stellar Structure of Early-Type Dwarf Galaxies in the Virgo Cluster

Janz

Laurikainen

Lisker

et al. 2014

ApJ

117

View full text Add to dashboard Cite

The fraction of star-forming to quiescent dwarf galaxies varies from almost infinity in the field to zero in the centers of rich galaxy clusters. What is causing this pronounced morphology-density relation? What do quiescent dwarf galaxies look like when studied in detail, and what conclusions can be drawn about their formation mechanism? Here we study a nearly magnitudecomplete sample (−19 < M r < −16 mag) of 121 Virgo cluster early types with deep near-infrared images from the SMAKCED project. We fit two-dimensional models with optional inner and outer components, as well as bar and lens components (in ∼15% of the galaxies), to the galaxy images. While a single Sérsic function may approximate the overall galaxy structure, it does not entirely capture the light distribution of two-thirds of our galaxies, for which multi-component models provide a better fit. This fraction of complex galaxies shows a strong dependence on luminosity, being larger for brighter objects. We analyze the global and component-specific photometric scaling relations of early-type dwarf galaxies and discuss similarities with bright early and late types. The dwarfs' global galaxy parameters show scaling relations that are similar to those of bright disk galaxies. The inner components are mostly fitted with Sérsic n values close to 1. At a given magnitude they are systematically larger than the bulges of spirals, suggesting that they are not ordinary bulges. We argue that the multi-component structures in early-type dwarfs are mostly a phenomenon inherent to the disks, and may indeed stem from environmental processing.

show abstract

“…The results from these studies are consistent with models of the Spectral Energy Distribution of these systems (e.g., Popescu et al 2000;Popescu & Tuffs 2005;Pierini et al 2004;Baes et al 2003Baes et al , 2010Bianchi et al 2000;Bianchi 2007Bianchi , 2008Jonsson et al 2010) Many of the morphological features of spiral disks can be expected to change in the course of their (secular) evolution, including the scale length (Ravindranath et al 2004;Trujillo & Aguerri 2004;Kanwar et al 2008), surface brightness (Barden et al 2005;Cameron & Driver 2007;Scarlata et al 2007), and truncation radius (Trujillo & Pohlen 2005;Azzollini et al 2008) of the stellar disk, as well as the bulge-to-disk ratio (Allen et al 2006;Pannella et al 2009), and bar fraction (Jogee et al 2004; Barazza et al 2008;Sheth et al 2008). All these morphological features of the stellar disk have been explored using deep imaging surveys with the Hubble Space Telescope (HST).…”

Section: Introductionmentioning

confidence: 99%

EVOLUTION IN THE DUST LANE FRACTION OF EDGE-ONL*_VSPIRAL GALAXIES SINCEz= 0.8

Holwerda

Dalcanton

Radburn-Smith

et al. 2012

ApJ

View full text Add to dashboard Cite

The presence of a well-defined and narrow dust lane in an edge-on spiral galaxy is the observational signature of a thin and dense molecular disk, in which gravitational collapse has overcome turbulence. Using a sample of galaxies out to z∼1 extracted from the COSMOS survey, we identify the fraction of massive (L * V ) disks that display a dust lane. Our goal is to explore the evolution in the stability of the molecular ISM disks in spiral galaxies over a cosmic timescale. We check the reliability of our morphological classifications against changes in restframe wavelength, resolution, and cosmic dimming with (artificially redshifted) images of local galaxies from the Sloan Digital Sky Survey.We find that the fraction of L * V disks with dust lanes in COSMOS is consistent with the local fraction (≈ 80%) out to z ∼ 0.7. At z=0.8, the dust lane fraction is only slightly lower. A somewhat lower dust lane fraction in starbursting galaxies tentatively supports the notion that a high specific star formation rate can efficiently destroy or inhibit a dense molecular disk. A small subsample of higher redshift COSMOS galaxies display low internal reddening (E[B-V]), as well as a low incidence of dust lanes. These may be disks in which the growth of the dusty ISM disk lags behind that of the stellar disk. We note that at z=0.8, the most massive galaxies display a lower dust lane fraction than lower mass galaxies. A small contribution of recent mergers or starbursts to this most massive population may be responsible.The fact that the fraction of galaxies with dust lanes in COSMOS is consistent with little or no evolution implies that models to explain the Spectral Energy Distribution or the host galaxy dust extinction of supernovae based on local galaxies are still applicable to higher redshift spirals. It also suggests that dust lanes are long lived phenomena or can be reformed over very short time-scales.

show abstract

Health Implications of 2,3,7,8-Tetrachlorodibenzo-p-dioxin Exposure in Primates

Cited by 11 publications

References 11 publications

A Catalog of Bulge+disk Decompositions and Updated Photometry for 1.12 Million Galaxies in the Sloan Digital Sky Survey

A Catalog of Bulge+disk Decompositions and Updated Photometry for 1.12 Million Galaxies in the Sloan Digital Sky Survey

A Near-Infrared Census of the Multicomponent Stellar Structure of Early-Type Dwarf Galaxies in the Virgo Cluster

EVOLUTION IN THE DUST LANE FRACTION OF EDGE-ONL*_VSPIRAL GALAXIES SINCEz= 0.8

Contact Info

Product

Resources

About

Health Implications of 2,3,7,8-Tetrachlorodibenzo-p-dioxin Exposure in Primates

Cited by 11 publications

References 11 publications

A Catalog of Bulge+disk Decompositions and Updated Photometry for 1.12 Million Galaxies in the Sloan Digital Sky Survey

A Catalog of Bulge+disk Decompositions and Updated Photometry for 1.12 Million Galaxies in the Sloan Digital Sky Survey

A Near-Infrared Census of the Multicomponent Stellar Structure of Early-Type Dwarf Galaxies in the Virgo Cluster

EVOLUTION IN THE DUST LANE FRACTION OF EDGE-ONL*VSPIRAL GALAXIES SINCEz= 0.8

Contact Info

Product

Resources

About

EVOLUTION IN THE DUST LANE FRACTION OF EDGE-ONL*_VSPIRAL GALAXIES SINCEz= 0.8