Simple rules with complex outcomes

Hughes, G.; Andújar, José Luis González

doi:10.1038/387241a0

Cited by 12 publications

(15 citation statements)

References 7 publications

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“…The shot-noise contribution can be reduced by observing at high resolution and masking out pixels with fluxes above some threshold. Fluctuation analyses of point-source cleaned SCUBA maps have been done by two groups (Hughes et al 1998, Borys, Chapman & Scott 1998. However, at these sub-arcminute angular scales, the wash-out factor is very large, and the correlated component is expected to be very small.…”

Section: Discussionmentioning

confidence: 99%

“…A compelling explanation is thermal emission by the interstellar dust of high-redshift galaxies, heated by their internal optical and ultraviolet (UV) star-light. A handful (∼ 30) of sources with the expected properties have been resolved in several SCUBA images at 850µm, reported in several papers (Hughes et al 1998, Barger et al 1998, Eales et al 1999, Holland et al 1998) and summarized by Scott & White (1999), and another handful at 175µm with the ISOPHOT instrument on board the Infrared Space Observatory (ISO) . According to Hughes et al (1998) and , sources brighter than 2mJy comprise at least 25% of the background at 850µm (350 GHz).…”

Section: Introductionmentioning

confidence: 97%

“…Guiderdoni et al 1998, Blain et al 1999a. One way of improving our understanding of this background is to observe the sky with deep exposures at high angular resolution, to determine the number counts of discrete sources (Hughes et al 1998, Barger et al 1998, Eales et al 1999, Holland et al 1998, and the redshift distribution of the contributing sources (e.g. Barger et al 1999b, Blain et al 1999c).…”

Section: Introductionmentioning

confidence: 99%

“…Two have been conclusively identified as such (Frayer et al 1998). Hughes et al (1998), observing in the Hubble Deep Field (HDF), identified tentative optical star-burst galaxy counterparts for all five of their sources brighter than 2mJy; four of them with redshifts between 3 and 4 and one with z ≃ 0.9. These identifications are not yet conclusive, due to the coarse angular resolution of SCUBA, and the possibility remains that many of the sources are dust-enshrouded quasars, rather than galaxies (see, e.g.…”

Section: Introductionmentioning

confidence: 99%

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Correlations in the Far‐Infrared Background

Haiman

Knox

2000

ApJ

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We compute the expected angular power spectrum of the cosmic Far Infrared Background (FIRB). We find that the signal due to source correlations dominates the shot-noise for ℓ < ∼ 1000 and results in anisotropies with rms amplitudes ( ℓ(ℓ + 1)C ℓ /2π) between 5% and 10% of the mean for l > ∼ 150. The angular power spectrum depends on several unknown quantities, such as the UV flux density evolution, optical properties of the dust, biasing of the sources of the FIRB, and cosmological parameters. However, when we require our models to reproduce the observed DC level of the FIRB, we find that the anisotropy is at least a few percent in all cases. This anisotropy is detectable with proposed instruments, and its measurement will provide strong constraints on models of galaxy evolution and large-scale structure at redshifts up to at least z ∼ 5.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 97%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Correlations in the Far‐Infrared Background

Haiman

Knox

2000

ApJ

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“…Pettini et al 1998). Recent detections of star forming galaxies in the submm band also suggest rather high SFR of > ∼ 2 × 10 −1 h M ⊙ yr −1 Mpc −3 at z ∼ 2 − 4 (Smail, Ivison & Blain 1997;Hughes et al 1998;Berger et al 1998). More detailed discussion on this subject should await higher precision data from future infrared observations.…”

Section: Cosmological Implicationsmentioning

confidence: 90%

Formation of Subgalactic Clouds under Ultraviolet Background Radiation

Kitayama

Ikeuchi

2000

ApJ

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The effects of the UV background radiation on the formation of sub-galactic clouds are studied by means of one-dimensional hydrodynamical simulations. The radiative transfer of the ionizing photons due to the absorption by HI, HeI and HeII, neglecting the emission, is explicitly taken into account. We find that the complete suppression of collapse occurs for the clouds with circular velocities typically in the range V c ∼ 15 − 40 km s −1 and the 50% reduction in the cooled gas mass with V c ∼ 20 − 55 km s −1 . These values depend most sensitively on the collapse epoch of the cloud, the shape of the UV spectrum, and the evolution of the UV intensity. Compared to the optically thin case, previously investigated by Thoul & Weinberg (1996), the absorption of the external UV photon by the intervening medium systematically lowers the above threshold values by ∆V c ∼ 5 km s −1 . Whether the gas can contract or keeps expanding is roughly determined by the balance between the gravitational force and the thermal pressure gradient when it is maximally exposed to the external UV flux. Based on our simulation results, we discuss a number of implications on galaxy formation, cosmic star formation history, and the observations of quasar absorption lines. In Appendix, we derive analytical formulae for the photoionization coefficients and heating rates, which incorporate the frequency/direction-dependent transfer of external photons.

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