A multi-wavelength study of<i>z</i>= 3.15 Lyman-$\mathsf{\alpha}$ emitters in the GOODS South Field

Nilsson, K.; Møller, P.; Möller, Ole; Fynbo, J. P. U.; Michalowski, Michal; Watson, Derrick G.; Ledoux, C.; Rosati, P.; Pedersen, K.; Grove, L. F.

doi:10.1051/0004-6361:20066949

Cited by 115 publications

(105 citation statements)

References 72 publications

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“…It has previously been reported that LAEs have SEDs that are in many cases blue (Gawiser et al 2006(Gawiser et al , 2007Pirzkal et al 2007). Only two other surveys reported detections of red SEDs in several LAEs (Stiavelli et al 2001;Lai et al 2008), although one extremely red object was found by Nilsson et al (2007). Among the 170 objects detected in this survey, a total of 118 candidates have Vj − i + colours greater than zero, indicative of red colours, and five candidates have undefined colours due to upper limits in both bands, or only in the i + band.…”

Section: Photometrymentioning

confidence: 70%

“…13 propose that z ∼ 3 Lyα emitters may have a wide range of properties. In Nilsson et al (2007), a stacked sample of Lyα emitters at z = 3.15 were studied. Here, small masses and low dust contents were inferred, but the ages were unconstrained.…”

Section: Datementioning

confidence: 99%

“…The candidate Lyα emitters were selected according to a similar method as described in Nilsson et al (2007). The method is based on determining the equivalent width (EW) of a potential emission/absorption line located in the narrow-band wavelength range.…”

Section: Object Detection and Candidate Selectionmentioning

confidence: 99%

“…Objects with large equivalent widths (EWs) are thus selected by comparing the colours in the narrow-band image and complementary broad-band images. Spectroscopically confirmed Lyα emitters now include several hundreds of sources at redshifts z ∼ 3 (e.g., Møller & Warren 1993;Cowie & Hu 1998;Steidel et al 2000;Fynbo et al 2001Fynbo et al , 2003aMatsuda et al 2005;Venemans et al 2007;Nilsson et al 2007;Ouchi et al 2008), z ∼ 4.5 (Finkelstein et al 2007), z ∼ 5.7 (Malhotra et al 2005;Shimasaku et al 2006;Tapken et al 2006) and z ∼ 6.5 (Taniguchi et al 2005;Kashikawa et al 2006). However, in the low redshift range, between z ≈ 1.6 corresponding to the atmospheric cut-off in the UV and z ∼ 3, little progress has been made.…”

Section: Introductionmentioning

confidence: 99%

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Evolution in the properties of Lyman-αemitters from redshiftsz~ 3 toz ~ 2

Nilsson¹,

Tapken²,

Møller

et al. 2009

A&A

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156

237

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Context. Narrow-band surveys to detect Lyα emitters are powerful tools for identifying high, and very high, redshift galaxies. Although samples are increasing at redshifts z = 3−6, the nature of these galaxies is still poorly known. The number of galaxies detected at redshifts below z ∼ 3 are also small. Aims. We study the properties of z = 2.25 Lyα emitters and compare them with those of z > 3 Lyα emitters.Methods. We present narrow-band imaging made with the MPG/ESO 2.2m telescope and the WFI (Wide Field Imager) detector. Using this data, we have searched for emission-line objects. We find 170 candidate typical Lyα emitters and 17 candidates that we regard as high UV-transmission Lyα emitters. We have derived the magnitudes of these objects in 8 photometric bands from u * to K s , and studied whether they have X-ray and/or radio counterparts. Results. We demonstrate that there has been significant evolution in the properties of Lyα emitters between redshift z ∼ 3 and z = 2.25. The spread in spectral energy distributions (SEDs) at the lower redshift is larger and we detect a significant AGN contribution in the sample. The distribution of the equivalent widths is narrower than at z ∼ 3, with only a few candidates with rest-frame equivalent width above the predicted limit of 240 Å. The star formation rates derived from the Lyα emission compared to those derived from the UV emission are lower by on average a factor of ∼1.8, indicative of a significant absorption by dust. Conclusions. Lyα emitters at redshift z = 2.25 may be more evolved than Lyα emitters at higher redshift. The red SEDs imply more massive, older and/or dustier galaxies at lower redshift than observed at higher redshifts. The decrease in equivalent widths and star formation rates indicate more quiescent galaxies, with in general less star formation than in higher redshift galaxies. At z = 2.25, AGN appear to be more abundant and also to contribute more to the Lyα emitting population.

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Section: Photometrymentioning

confidence: 70%

Section: Datementioning

confidence: 99%

Section: Object Detection and Candidate Selectionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Evolution in the properties of Lyman-αemitters from redshiftsz~ 3 toz ~ 2

Nilsson¹,

Tapken²,

Møller

et al. 2009

A&A

Self Cite

156

237

View full text Add to dashboard Cite

show abstract

“…Problems tackled by such approaches (e.g. Acquaviva, Gawiser & Guaita (2011), Panter, Heavens & Jimenez (2003), Nilsson et al (2007), Sajina et al (2006), Johnson et al (2013), Serra et al (2011)) typically have no more than 10 dimensions. CPU time can be reduced to manageable levels at the same time as covering adequate parameter space using a variety of methods when producing a spectral fitting code.…”

Section: Introductionmentioning

confidence: 99%

firefly (Fitting IteRativEly For Likelihood analYsis): a full spectral fitting code

Wilkinson

Maraston

Goddard

et al. 2017

Monthly Notices of the Royal Astronomical Society

177

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We present a new spectral fitting code, FIREFLY, for deriving the stellar population properties of stellar systems. FIREFLY is a chi-squared minimisation fitting code that fits combinations of single-burst stellar population models to spectroscopic data, following an iterative bestfitting process controlled by the Bayesian Information Criterion. No priors are applied, rather all solutions within a statistical cut are retained with their weight. Moreover, no additive or multiplicative polynomia are employed to adjust the spectral shape. This fitting freedom is envisaged in order to map out the effect of intrinsic spectral energy distribution (SED) degeneracies, such as age, metallicity, dust reddening on galaxy properties, and to quantify the effect of varying input model components on such properties. Dust attenuation is included using a new procedure, which was tested on Integral Field Spectroscopic (IFS) data in a previous paper. The fitting method is extensively tested with a comprehensive suite of mock galaxies, real galaxies from the Sloan Digital Sky Survey and Milky Way globular clusters. We also assess the robustness of the derived properties as a function of signal-to-noise ratio and adopted wavelength range. We show that FIREFLY is able to recover age, metallicity, stellar mass and even the star formation history remarkably well down to a S/N ∼ 5, for moderately dusty systems. Code and results are publicly available at WWW.ICG.PORT.AC.UK/FIREFLY.

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Observing the First Galaxies

Dunlop

2012

The First Galaxies

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I endeavour to provide a thorough overview of our current knowledge of galaxies and their evolution during the first billion years of cosmic time, corresponding to redshifts z > 5. After first summarizing progress with the seven different techniques which have been used to date in the discovery of objects at z > 5, I focus thereafter on the two selection methods which have yielded substantial samples of galaxies at early times, namely Lyman-break and Lyman-α selection. I discuss a decade of progress in galaxy sample selection at z ≃ 5 − 8, including issues of completeness and contamination, and address some of the confusion which has been created by erroneous reports of extreme-redshift objects. Next I provide an overview of our current knowledge of the evolving ultraviolet continuum and Lyman-α galaxy luminosity functions at z ≃ 5 − 8, and discuss what can be learned from exploring the relationship between the Lyman-break and Lyman-α selected populations.

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A multi-wavelength study ofz= 3.15 Lyman-$\mathsf{\alpha}$ emitters in the GOODS South Field

Cited by 115 publications

References 72 publications

Evolution in the properties of Lyman-αemitters from redshiftsz~ 3 toz ~ 2

Evolution in the properties of Lyman-αemitters from redshiftsz~ 3 toz ~ 2

firefly (Fitting IteRativEly For Likelihood analYsis): a full spectral fitting code

Observing the First Galaxies

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