The Hy-Redshift Universe: Galaxy Formation and Evolution at High Redshift

Bunker, Andrew J.; Breugel, W. J. M. van

doi:10.2172/793845

Cited by 58 publications

(3 citation statements)

References 139 publications

(261 reference statements)

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“…The cluster magnification has fortuitously afforded us detailed spectral and spatial information of a very faint and presumably otherwise typical examples of galaxies at z > 4. We have obtained higher resolution longslit spectra for one of these objects, revealing spatial and spectral detail of the Lya and metal lines along the lengths of the N and S arcs Bunker et al, 1998a) and also near-IR Keck images useful for exploring the role of dust and for a good estimate of the luminosity (Bunker et al, 1998a). The rarity of luminous high redshift galaxies and the requirement of a high magnification for useful spectroscopic follow-up means that such searches will be slow, but well rewarded by detailed information on galaxies at otherwise inaccessibly-early times.…”

Section: Resultsmentioning

confidence: 99%

A faint galaxy redshift survey behind massive clusters

Frye

1999

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This thesis is concerned with the gravitational lensing effect by massive galaxy clusters. We have explored a new technique for measuring galaxy masses and for detecting high-z galaxies by their optical colors. A redshift survey has been obtained at the Keck for a magnitude limited sample of objects (1 < 23) behind three clusters, A1689, A2390 and A2218 within a radius of 0.5kfpc. For each cluster we see both a clear trend of increasing flux and redshift towards the center. This behavior is the result of image magnifications, such that at fixed redshift one sees further down the luminosity function. The gradient of this magnification is, unlike measurements of image distortion, sensitive to the mass profile, and found to depart strongly from a pure isothermal halo. We have found that VW color selection can be used effectively as a discriminant for finding high-z galaxies behind clusters and present five 4.1 < z < 5.1 spectra which are of very high quality due to their high mean magnification of w 20, showing strong, visibly-saturated interstellar metal lines in some cases. Also, We have also investigated the radio ring lens PKS 1830-211, locating the Contents

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Section: Resultsmentioning

confidence: 99%

A faint galaxy redshift survey behind massive clusters

Frye

1999

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“…Investigations of the faint radio source population (e.g., Windhorst et al 1999;Kondapally et al 2021) have clearly established that very sensitive optical datasets are required in order to identify counterparts for the vast bulk of the radio population. This is a consequence of the fact that many faint radio sources are either at very high redshift, or are heavily obscured, or both (e.g., Smolčić et al 2017;Whittam et al 2022).…”

Section: Introductionmentioning

confidence: 99%

EMU/GAMA: Radio-detected galaxies are more obscured than optically selected galaxies

Ahmed,

Hopkins,

Ware

et al. 2024

Publ. Astron. Soc. Aust.

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We demonstrate the importance of radio selection in probing heavily obscured galaxy populations. We combine Evolutionary Map of the Universe (EMU) Early Science data in the Galaxy and Mass Assembly (GAMA) G23 field with the GAMA data, providing optical photometry and spectral line measurements, together withWide-field Infrared Survey Explorer (WISE) infrared (IR) photometry, providing IR luminosities and colours. We investigate the degree of obscuration in star forming galaxies, based on the Balmer decrement (BD), and explore how this trend varies, over a redshift range of 0 < z < 0.345. We demonstrate that the radio detected population has on average higher levels of obscuration than the parent optical sample, arising through missing the lowest BD and lowest mass galaxies, which are also the lower star formation rate (SFR) and metallicity systems. We discuss possible explanations for this result, including speculation around whether it might arise from steeper stellar initial mass functions in low mass, low SFR galaxies.

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“…During the past decade our observational knowledge of the evolution of galaxies to high redshift has considerably improved (Bunker & van Breugel 1999). On larger scales recent observations of the cosmic microwave background have given a greater confidence in the validity of the standard cosmological models (de Bernardis et al 2000).…”

Section: Introductionmentioning

confidence: 99%

Numerical simulation of the formation of a spiral galaxy

Williams

Nelson²

2001

A&A

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Abstract. A simulation is described in which the numerical galaxy formed compares favourably in every measurable respect with contemporary bright spiral galaxies, including the formation of a distinct stellar bulge and large scale spiral arm shocks in the gas component. This is achieved in spite of the fact that only idealized proto-galactic initial conditions were used, and only simple phenomenological prescriptions for the physics of the interstellar medium (ISM) and star formation were implemented. In light of the emphasis in recent literature on the importance of the link between galaxy formation and models of the universe on cosmological scales, on the details of the physics of the ISM and star formation, and on apparent problems therein, the implications of this result are discussed.

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The Hy-Redshift Universe: Galaxy Formation and Evolution at High Redshift

Cited by 58 publications

References 139 publications

A faint galaxy redshift survey behind massive clusters

A faint galaxy redshift survey behind massive clusters

EMU/GAMA: Radio-detected galaxies are more obscured than optically selected galaxies

Numerical simulation of the formation of a spiral galaxy

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