On a Formula for Correcting Statistics for the Effects of a known Probable Error of Observation

Eddinǵton, A. S.

doi:10.1093/mnras/73.5.359

Cited by 479 publications

(379 citation statements)

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“…More sources are intrinsically faint than bright, and therefore, more of those faint sources scatter towards higher flux densities than bright sources scatter down towards lower flux densities. This Eddington boosting (first described by Eddington, 1913) assumes that fainter sources are more numerous than brighter sources. The second form of boosting comes from confusion noise, as discussed in § 3.1, which is caused by sources below the detection threshold contributing flux to sources above the detection threshold.…”

Section: Estimating Deboosted Flux Densitiesmentioning

confidence: 99%

Dusty star-forming galaxies at high redshift

2014

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Far-infrared and submillimeter wavelength surveys have now established the important role of dusty, star-forming galaxies (DSFGs) in the assembly of stellar mass and the evolution of massive galaxies in the Universe. The brightest of these galaxies have infrared luminosities in excess of 10 13 L with implied star-formation rates of thousands of solar masses per year. They represent the most intense starbursts in the Universe, yet many are completely optically obscured. Their easy detection at submm wavelengths is due to dust heated by ultraviolet radiation of newly forming stars. When summed up, all of the dusty, star-forming galaxies in the Universe produce an infrared radiation field that has an equal energy density as the direct starlight emission from all galaxies visible at ultraviolet and optical wavelengths. The bulk of this infrared extragalactic background light emanates from galaxies as diverse as gas-rich disks to mergers of intense starbursting galaxies. Major advances in far-infrared instrumentation in recent years, both spacebased and ground-based, has led to the detection of nearly a million DSFGs, yet our understanding of the underlying astrophysics that govern the start and end of the dusty starburst phase is still in nascent stage. This review is aimed at summarizing the current status of DSFG studies, focusing especially on the detailed characterization of the bestunderstood subset (submillimeter galaxies, who were summarized in the last review of this field over a decade ago, Blain et al. 2002), but also the selection and characterization of more recently discovered DSFG populations. We review DSFG population statistics, their physical properties including dust, gas and stellar contents, their environments, and current theoretical models related to the formation and evolution of these galaxies.

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Section: Estimating Deboosted Flux Densitiesmentioning

confidence: 99%

Dusty star-forming galaxies at high redshift

2014

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“…Both Duncan et al (2014) and Grazian et al (2015) utilize data collected from the Cosmic Assembly Near-infrared Deep ExtragaLactic Survey (CANDELS; Grogin et al 2011;Koekemoer et al 2011) GOODS South field with stellar masses directly obtained from SED fitting of combined optical and near-infrared space-based observations, and include the effects of both nebular line and continuum emission. In addition, Grazian et al (2015) include a detailed treatment of the effects of Eddington bias (Eddington 1913) on the normalization and slope of their derived mass functions. Whilst Song et al (2016) also utilize CANDELS infrared data, they instead carry out a hybrid SED stacking technique to derive a redshift dependent stellar mass-UV luminosity relation which is then combined with measured UV luminosity functions to estimate the galaxy stellar mass function.…”

Section: Model Calibrationmentioning

confidence: 99%

Dark-ages reionization and galaxy formation simulation – III. Modelling galaxy formation and the epoch of reionization

Mutch

Geil

Poole

et al. 2016

Mon. Not. R. Astron. Soc.

141

160

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We introduce Meraxes, a new, purpose-built semi-analytic galaxy formation model designed for studying galaxy growth during reionization. Meraxes is the first model of its type to include a temporally and spatially coupled treatment of reionization and is built upon a custom (100 Mpc) 3 N -body simulation with high temporal and mass resolution, allowing us to resolve the galaxy and star formation physics relevant to early galaxy formation. Our fiducial model with supernova feedback reproduces the observed optical depth to electron scattering and evolution of the galaxy stellar mass function between z=5 and 7, predicting that a broad range of halo masses contribute to reionization. Using a constant escape fraction and global recombination rate, our model is unable to simultaneously match the observed ionizing emissivity at z < ∼ 6. However, the use of an evolving escape fraction of 0.05-0.1 at z∼6, increasing towards higher redshift, is able to satisfy these three constraints. We also demonstrate that photoionization suppression of low mass galaxy formation during reionization has only a small effect on the ionization history of the inter-galactic medium. This lack of 'selfregulation' arises due to the already efficient quenching of star formation by supernova feedback. It is only in models with gas supply-limited star formation that reionization feedback is effective at regulating galaxy growth. We similarly find that reionization has only a small effect on the stellar mass function, with no observationally detectable imprint at M * >10 7.5 M . However, patchy reionization has significant effects on individual galaxy masses, with variations of factors of 2-3 at z=5 that correlate with environment.

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“…We also correct  for Eddington (1913) bias, which can boost the [O III]λ4363 line flux for galaxies near the adopted S/ N = 3 limit. Since there is a direct relation between  and T e , this bias can result in higher T e .…”

Section: T E and Metallicity Determinationsmentioning

confidence: 99%

“…For this reason, we determine upper limit  values by adopting [O III]λ4363 fluxes that correspond to S/ N = 2.5 for those with /  < 2 S N 3, 1.5 for /  < 1 S N 2, and 1.0 for / < S N 1. For the [O III]λ4363 non-detected sample, we do not apply the Eddington (1913) bias correction because the lack of a detection suggests that the bias is weak. The derived upper limits on T e span 0.8×10 4 -3×10 4 K, and are provided in Table 14.…”

Section: T E and Metallicity Determinationsmentioning

confidence: 99%

The Metal Abundances Across Cosmic Time (     ) Survey. I. Optical Spectroscopy in the Subaru Deep Field

Ly¹,

Malhotra²,

Malkan³

et al. 2016

ApJS

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Deep rest-frame optical spectroscopy is critical for characterizing and understanding the physical conditions and properties of the ionized gas in galaxies. Here, we present a new spectroscopic survey called "Metal Abundances across Cosmic Time" or  , which will obtain rest-frame optical spectra for ∼3000 emission-line galaxies. This paper describes the optical spectroscopy that has been conducted with MMT/Hectospec and Keck/DEIMOS for ≈1900 z = 0.1-1 emission-line galaxies selected from our narrowband and intermediate-band imaging in the Subaru Deep Field. In addition, we present a sample of 164 galaxies for which we have measured the weak [O III] λ4363 line (66 with at least 3σ detections and 98 with significant upper limits). This nebular emission line determines the gas-phase metallicity by measuring the electron temperature of the ionized gas. This paper presents the optical spectra, emission-line measurements, interstellar properties (e.g., metallicity, gas density), and stellar properties (e.g., star formation rates, stellar mass). Paper II of the  survey (Ly et al.) presents the first results on the stellar mass-gas metallicity relation at z1 using the sample with [O III]λ4363 measurements.

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On a Formula for Correcting Statistics for the Effects of a known Probable Error of Observation

Cited by 479 publications

References 0 publications

Dusty star-forming galaxies at high redshift

Dusty star-forming galaxies at high redshift

Dark-ages reionization and galaxy formation simulation – III. Modelling galaxy formation and the epoch of reionization

The Metal Abundances Across Cosmic Time (     ) Survey. I. Optical Spectroscopy in the Subaru Deep Field

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