The redshift evolution of QSO heavy-element absorption systems

Steidel, Charles C.

doi:10.1086/133065

Cited by 13 publications

(7 citation statements)

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“…What is really encouraging is that the qualitative behavior of the ''star formation luminosity density'' with epoch mimics the behavior of the space density of luminous QSOs (23), and is consistent with the timescales seen for the chemical enrichment in QSO absorption line systems (1,34,(41)(42)(43)(44). The upshot is that, if one were asked to pinpoint the ''Epoch of Galaxy Formation,'' one could arguably say that it is now seen directly, in the redshift range 3.5 տ z տ 1, and that the ''onset'' of massive galaxy formation appears to be in the range zϳ3.5-4.…”

Section: The Hdf and The Global History Of Star Formationsupporting

confidence: 60%

Galaxies and large scale structure at high redshifts

Steidel

1998

Proc. Natl. Acad. Sci. U.S.A.

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It is now straightforward to assemble large samples of very high redshift (z ϳ 3) field galaxies selected by their pronounced spectral discontinuity at the rest frame Lyman limit of hydrogen (at 912 Å). This makes possible both statistical analyses of the properties of the galaxies and the first direct glimpse of the progression of the growth of their large-scale distribution at such an early epoch. Here I present a summary of the progress made in these areas to date and some preliminary results of and future plans for a targeted redshift survey at z ‫؍‬ 2.7-3.4. Also discussed is how the same discovery method may be used to obtain a ''census'' of star formation in the high redshift Universe, and the current implications for the history of galaxy formation as a function of cosmic epoch.

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Section: The Hdf and The Global History Of Star Formationsupporting

confidence: 60%

Galaxies and large scale structure at high redshifts

Steidel

1998

Proc. Natl. Acad. Sci. U.S.A.

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“…We can now rule this scenario out in PKS 0537−286, and note the chance coincidence of such a system out to z = 3 is ∼20-30% (e.g. Steidel 1992). …”

Section: Discussionmentioning

confidence: 92%

The first XMM-Newton spectrum of a high redshift quasar - PKS 0537-286

Reeves

Turner

Bennie

et al. 2001

A&A

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Abstract. We present XMM-Newton observations of the high redshift (z = 3.104), radio-loud quasar PKS 0537−286. The EPIC CCD cameras provide the highest signal-to-noise spectrum of a high-z quasar to date. The EPIC observations show that PKS 0537−286 is extremely X-ray luminous (LX = 2 10 47 erg s −1 ), with an unusually hard X-ray spectrum (Γ = 1.27± 0.02). The flat power-law emission extends over the whole observed energy range (0.4 to 40 keV in the quasar rest frame); there is no evidence of intrinsic absorption, which has been claimed in PKS 0537−286 and other high z quasars. However, there is evidence for weak Compton reflection. A redshifted iron K line, observed at 1.5 keV -corresponding to ∼6.15 keV in the quasar rest frame -is detected at 95% confidence. If confirmed, this is the most distant iron K line known. The line equivalent width is small (33 eV), consistent with the "X-ray Baldwin effect" observed in other luminous quasars. The reflected continuum is also weak (R ∼ < 0.25). We find the overall spectral energy distribution of PKS 0537−286 is dominated by the X-ray emission, which, together with the flat power-law and weak reflection features, suggests that the X-radiation from PKS 0537−286 is dominated by inverse Compton emission associated with a face-on relativistic jet.

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“…Of particular relevance for estimating the attenuation just below 912 Å are the statistics for LLSs (N H i 10 17.2 ). For these systems, we assume a power-law distribution in column-density, proportional to N 2.04 (Songaila & Cowie 2010), with a total number per unit redshift at z ∼ 3 of dN/dz ≈ 2 (Songaila & Cowie 2010;Stengler-Larrea et al 1995;Steidel 1992). Randomly generated absorbers are then applied to the unabsorbed continuum of each model sightline until the total number of absorbers is equal to a random Poisson realization of the integral of the absorber column-density and redshift distributions over the relevant ranges in column density (N H i = 10 12 -10 22 cm −2 ) and redshift (z = 1.7 − z source , where z source is the redshift of the target galaxy).…”

Section: Igm Absorption Of Lyman-continuum Fluxmentioning

confidence: 99%

NARROWBAND IMAGING OF ESCAPING LYMAN-CONTINUUM EMISSION IN THE SSA22 FIELD^,

Nestor

Shapley

Steidel

et al. 2011

ApJ

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138

242

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We present the results of an ultradeep, narrowband imaging survey for Lyman-continuum (LyC) emission at z ∼ 3 in the SSA22a field. We employ a custom narrowband filter centered at λ = 3640 Å (NB3640), which probes the LyC region for galaxies at z 3.06. We also analyze new and archival NB4980 imaging tuned to the wavelength of the Lyα emission line at z = 3.09, and archival broadband B, V, and R images of the non-ionizing UV continuum. Our NB3640 images contain 26 z 3.06 Lyman break galaxies (LBGs) as well as a set of 130 Lyα emitters (LAEs), identified by their excess NB4980 flux relative to the BV continuum. Six LBGs and 28 LAEs are detected in the NB3640 image. LBGs appear to span a range of NB3640-R colors, while LAEs appear bimodal in their NB3640-R properties. We estimate average UV-to-LyC flux density ratios, corrected for foreground contamination and intergalactic medium absorption, finding F UV /F LyC * , we estimate a galaxy contribution to the intergalactic hydrogen ionization rate that is consistent with independent estimates based on the Lyα forest opacity at z 3. If we assume that F UV /F LyC LAE corr holds at the faintest luminosities, the galaxy contribution significantly exceeds that inferred from the Lyα forest. We interpret our results in terms of a model where LyC photons escape over only ∼10%-20% of solid angle. When advantageously oriented, a galaxy will exhibit a low UV-to-LyC ratio, an effect enhanced for more compact galaxies. This model, however, does not adequately explain the extremely blue NB3640-R colors measured for some LAEs in our sample. Further follow-up study of these faint LAEs is crucial, given the potentially important contribution similar objects make to the process of reionization.

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The redshift evolution of QSO heavy-element absorption systems

Abstract: ABSTRACT. Recent results on the evolution of various classes of QSO heavy-element absorption-line systems are summarized. A general scenario for interpreting the observed evolution is suggested, with emphasis on the implications for the evolution of gas in galaxies from z=4 to the present.

Cited by 13 publications

References 22 publications

Galaxies and large scale structure at high redshifts

Galaxies and large scale structure at high redshifts

The first XMM-Newton spectrum of a high redshift quasar - PKS 0537-286

NARROWBAND IMAGING OF ESCAPING LYMAN-CONTINUUM EMISSION IN THE SSA22 FIELD^,

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The redshift evolution of QSO heavy-element absorption systems

Cited by 13 publications

References 22 publications

Galaxies and large scale structure at high redshifts

Galaxies and large scale structure at high redshifts

The first XMM-Newton spectrum of a high redshift quasar - PKS 0537-286

NARROWBAND IMAGING OF ESCAPING LYMAN-CONTINUUM EMISSION IN THE SSA22 FIELD,

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NARROWBAND IMAGING OF ESCAPING LYMAN-CONTINUUM EMISSION IN THE SSA22 FIELD^,