Self-homotopy equivalences of $H_*(-;\bold Z/p)$-local spaces

Møller, Jesper M.

doi:10.2996/kmj/1138039038

Cited by 85 publications

(110 citation statements)

References 9 publications

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“…Hunstead, Pettini & Fletcher 1990;Noterdaeme et al 2012a), (narrow-band) imaging (e.g. Smith, Cohen & Bradley 1986;Møller & Warren 1993;Kulkarni et al 2001;Fumagalli et al 2014) and integral field spectroscopy (e.g. Christensen et al 2007;Péroux et al 2011;Bouché et al 2012;Jorgenson & Wolfe 2014).…”

Section: Galaxy Counterparts Of Metal-rich Dlas 2739mentioning

confidence: 99%

Galaxy counterparts of metal-rich damped Lyα absorbers: the case of J205922.4−052842★

Hartoog

Fynbo

Kaper

et al. 2015

Monthly Notices of the Royal Astronomical Society

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Disclaimer/Complaints regulationsIf you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the material inaccessible and/or remove it from the website. Please Ask the Library: http://uba.uva.nl/en/contact, or a letter to: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. You will be contacted as soon as possible. ABSTRACTWe present observations of three new sources in the European Southern Observatory VLT/Xshooter survey dedicated to the detection of the emitting counterparts of damped Lyα (DLA) systems towards bright quasars (QSOs). The aim is to bridge the observational gap between absorption (i.e. DLAs) and emission-selected galaxies at z ∼ 2.2-2.5, in order to get a more complete picture of (proto)galaxies around this epoch. The hypothesis is that because DLA galaxies fulfil metallicity-velocity width and luminosity-metallicity relations, highmetallicity DLAs are more likely to be detected in emission. The region around each QSO is covered with slits (1. We conclude that focusing on metal-rich DLAs is a good way to find counterparts, but the non-detections at high metallicity (e.g. that of the DLA in J105744.5+062914) show that there is not a one-to-one relationship, and cautions us to not naively apply the properties of the DLA counterparts to all metal-rich DLAs.

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Section: Galaxy Counterparts Of Metal-rich Dlas 2739mentioning

confidence: 99%

Galaxy counterparts of metal-rich damped Lyα absorbers: the case of J205922.4−052842★

Hartoog

Fynbo

Kaper

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…It is seen from Table 3 that our survey found a larger space a The true 5σ level for this study is fainter, but only objects brighter than this limit were included in the catalog (Pettini, private communication). References : (1) Møller & Warren (1993); Warren & Møller (1996); (3) Hu et al (1998); (4) ; (5) Kudritzki et al (2000); (6) Steidel et al (2000); (7) Fynbo et al (2000) and this paper.…”

Section: Space Densitymentioning

confidence: 99%

“…The pre-imaging B-band images and the I-band images were BIAS subtracted and flat-fielded using standard techniques and the individual reduced images were combined using the σ-clipping algorithm described in Møller & Warren (1993). The combined images reach 5(2)σ detection limits in 1 arcsec 2 circular apertures of 25.9(26.9) in the I-band and 26.7(27.7) in the B-band (both in the AB-system).…”

Section: Data Reductionmentioning

confidence: 99%

“…Several studies have shown that Lyα narrow-band imaging is an alternative technique to identify high redshift galaxies (Møller & Warren 1993;Francis et al 1995;Pascarelle et al 1996;Pascarelle et al 1998;Hu et al 1998;Fynbo et al 1999Fynbo et al , 2000Kudritzki et al 2000;Kurk et al 2000;Pentericci et al 2000;Steidel et al 2000;Roche et al 2000;Rhoads et al 2000). So far it has not been considered efficient enough to seriously compete with the LBG technique, but it does have the advantage that spectroscopic confirmation is not limited by the broad band flux.…”

Section: Introductionmentioning

confidence: 99%

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Probing the faint end of the Galaxy luminosity function at $\vec{z}=$ 3 with Lyαemission

Fynbo

Møller

Thomsen³

2001

A&A

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Abstract. We present spectroscopic observations obtained with the ESO Very Large Telecope (VLT) of seven candidate Lyα emitting galaxies in the field of the radio quiet Q1205-30 at z = 3.04 previously detected with deep narrow band imaging. Based on equivalent widths and limits on line ratios we confirm that all seven objects are Lyα emitting galaxies. Deep images also obtained with the VLT in the B and I bands show that five of the seven galaxies have very faint continuum fluxes (I(AB) ≈ 26.8 and B(AB) ≈ 27.3). The star formation rates of these seven galaxies estimated from the rest-frame UV continuum around 2000Å, as probed by the I-band detections, as well as from the Lyα luminosities, are 1-4 M yr −1 assuming a Hubble constant of 65 km s −1 Mpc −1 , Ωm = 0.3, and ΩΛ = 0.7. This is 1-3 orders of magnitude lower than for other known populations of star-forming galaxies at similar redshifts (the Lyman-Break galaxies and the sub-mm selected sources). The inferred density of the objects is high, 16 ± 4 per arcmin 2 per unit redshift. This is consistent with the integrated luminosity function for Lyman-Break galaxies down to R = 27 if the fraction of Lyα emitting galaxies is ≈70% at the faint end of the luminosity function. However, if this fraction is 20% as reported for the bright end of the luminosity function then the space density in this field is significantly larger (by a factor of 3.5) than expected from the luminosity function for Lyman-Break galaxies in the HDF-North. This would be an indication that at least some radio quiet QSOs at high redshift reside in overdense environments or that the faint end slope of the high redshift luminosity function has been underestimated. We find evidence that the faint Lyα galaxies are essentially dust-free. These observations show that Lyα emission is an efficient method by which to probe the faint end of the luminosity function at high redshifts.

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“…While predicted already half a century ago (Partridge & Peebles 1967), the first detections of high-redshift Lyα emitters was not until more than 25 years later (e.g., Møller & Warren 1993;Rhoads et al 2000). They were thus preceded by groundbreaking theoretical studies -which still represent the solid foundation of our understanding of Lyα radiative transfer in astrophysical environments today (Osterbrock 1962;Adams 1972;Neufeld 1990).…”

Section: Introductionmentioning

confidence: 99%

Modeling 237 Lyman-αspectra of the MUSE-Wide survey

Grönke

2017

A&A

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We compare 237 Lyman-α (Lyα) spectra of the "MUSE-Wide survey" ) to a suite of radiative transfer simulations consisting of a central luminous source within a concentric, moving shell of neutral gas, and dust. This six parameter shell-model has been used numerously in previous studies, however, on significantly smaller datasets. We find that the shell-model can reproduce the observed spectral shape very well -better than the also common 'Gaussian-minus-Gaussian' model which we also fitted to the dataset. Specifically, we find that ∼ 94% of the fits possess a goodness-of-fit value of p(χ 2 ) > 0.1. The large number of spectra allows us to robustly characterize the shell-model parameter range, and consequently, the spectral shapes typical for realistic spectra. We find that the vast majority of the Lyα spectral shapes require an outflow and only ∼ 5% are well-fitted through an inflowing shell. In addition, we find ∼ 46% of the spectra to be consistent with a neutral hydrogen column density < 10 17 cm −2 -suggestive of a non-negligible fraction of continuum leakers in the MUSE-Wide sample. Furthermore, we correlate the spectral against the Lyα halo properties against each other but do not find any strong correlation.

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Self-homotopy equivalences of $H_*(-;\bold Z/p)$-local spaces

Cited by 85 publications

References 9 publications

Galaxy counterparts of metal-rich damped Lyα absorbers: the case of J205922.4−052842★

Galaxy counterparts of metal-rich damped Lyα absorbers: the case of J205922.4−052842★

Probing the faint end of the Galaxy luminosity function at $\vec{z}=$ 3 with Lyαemission

Modeling 237 Lyman-αspectra of the MUSE-Wide survey

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