ABSTRACT
The James Webb Space Telescope will allow to spectroscopically study an unprecedented number of galaxies deep into the reionization era, notably by detecting O iiiλλ4959, 5007, and H β ...nebular emission lines. To efficiently prepare such observations, we photometrically select a large sample of galaxies at z ∼ 8 and study their rest-frame optical emission lines. Combining data from the GOODS Re-ionization Era wide-Area Treasury from Spitzer (GREATS) survey and from HST we perform spectral energy distribution (SED) fitting, using synthetic SEDs from a large grid of photoionization models. The deep Spitzer/IRAC data combined with our models exploring a large parameter space enables to constrain the O iii + H β fluxes and equivalent widths for our sample, as well as the average physical properties of z ∼ 8 galaxies, such as the ionizing photon production efficiency with $\log (\xi _\mathrm{ion}/\mathrm{erg}^{-1}\mathrm{Hz})\ge 25.77$. We find a relatively tight correlation between the O iii + H β and UV luminosity, which we use to derive for the first time the O iiiλλ4959, 5007 + H β luminosity function (LF) at z ∼ 8. The z ∼ 8 O iii + H β LF is higher at all luminosities compared to lower redshift, as opposed to the UV LF, due to an increase of the O iii + H β luminosity at a given UV luminosity from z ∼ 3 to z ∼ 8. Finally, using the O iii + H β LF, we make predictions for JWST/NIRSpec number counts of z ∼ 8 galaxies. We find that the current wide-area extragalactic legacy fields are too shallow to use JWST at maximal efficiency for z ∼ 8 spectroscopy even at 1 h depth and JWST pre-imaging to ≳30 mag will be required.
To gain insight on the mass assembly and place constraints on the star formation history (SFH) of Lyman break galaxies (LBGS), it is important to accurately determine their properties. We estimate ...how nebular emission and different SFHs affect parameter estimation of LBGs. We present a homogeneous, detailed analysis of the spectral energy distribution (SED) of similar4700 LBGs from the GOODS-MUSIC catalogue with deep multi-wavelength photometry from the U band to 8pm to determine stellar mass, age, dust attenuation, and star formation rate. Using our SED fitting tool, which takes into account nebular emission, we explore a wide parameter space. We also explore a set of different star formation histories. The physical parameters of approximately two thirds of high redshift galaxies are significantly modified when we account for nebular emission. The SED models, which include nebular emission shed new light on the properties of LBGs with numerous important implications.
Continuing interest and more developments in recent years indicated that it would be useful to update Banea and da Silva paper entitled “Adhesively bonded joints in composite materials: an overview”. ...This paper presents an updated review of adhesively bonded joints in composite materials, which covers articles published from 2009 to 2016. The main parameters that affect the performance of bonded joints such as surface treatment, joint configuration, geometric and material parameters, failure mode etc. are discussed. The environmental factors such as pre-bond moisture, moisture and temperature are also discussed in detail and how they affect the durability of adhesive joints. Lots of shortcomings were resolved during the last years by developing new materials, new methods and models. However, there is still a potential to evaluate and identify the best possible combination of parameters which would give the best performance of composite bonded joints.
The low uniformity in light distribution provided by conventional lighting systems installed in laying poultry can compromise the productive performance and egg quality of laying hens. Thus, the aim ...of the current study is to evaluate the effect of a linear lighting system with light-emitting diode (LED strip) on the productive performance and egg quality of laying hens, by comparing it to the conventional LED lamp lighting system. The study used Hy-Line Brown hens from a commercial production unit. Hen-day egg production (%), mortality rate (%), egg weight (g), albumen height (mm), Haugh unit, eggshell thickness, eggshell strength, and thermal-environment conditions were evaluated from the 19th to the 48th wk of age. The results have shown that LED strips were capable of improving egg production (P < 0.05) in comparison to LED lamps. Egg quality was not affected (P > 0.05) by the evaluated lighting systems throughout the experimental period. Results of the current study indicate that the homogeneous illuminance distribution provided by the linear LED strip lighting system at different cage floors improved egg production in comparison to the conventional LED lamp lighting system.
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•A new catalyst from waste pineapple leaves was used in the biodiesel synthesis.•98.92% of conversion was obtained when applying 4 wt% of the new catalyst.•High conversions were ...obtained in only 30 min of reaction time.•Conversions higher than 85% were obtained after the fourth catalyst recycling cycle.
Homogeneous catalysts used for biodiesel synthesis have several limitations, including non-recoverability/reusability, saponification, emulsification, equipment corrosion, and environmental pollution. To overcome these limitations, we synthesized a novel catalyst via calcination of pineapple leaves waste. This catalyst was characterized by X-ray powder diffraction, X-ray fluorescence, Fourier transform infrared spectroscopy, thermogravimetric analysis, scanning electron microscopy, and soluble alkalinity measurements. The catalyst’s activity with regards to soybean oil transesterification was analyzed, and multiple process parameters (temperature, catalyst amount, reaction time, and methanol:oil molar ratio) were examined. A high catalytic activity, probably related to the 85 wt% content of alkali/alkali metals (K, Ca and Mg), was observed after a 30 min reaction time, 60 °C, 4 wt% of catalyst, oil to methanol molar ratio of 1:40, reaching an oil to biodiesel conversion above 98%. We conclude that the novel catalyst presented here is efficient, cost-effective, and sustainable, while simultaneously abundant waste is reduced.
We present VLT/X-Shooter and MUSE spectroscopy of a faint F814W = 28.60 + or - 0.33 (M sub(UV)=-17.0, low-mass (<, ~10 super(7)M sub(middo t in circle)), and compact (R sub(eff)= 62 pc) freshly ...star-forming galaxy at z= 3.1169 magnified (16x) by the Hubble Frontier Fields galaxy cluster Abell S1063. Gravitational lensing allows for a significant jump toward low-luminosity regimes, in moderately high-resolution spectroscopy (R= lambda /dlambda ~ 3000-7400). We measured C IV lambda 1548, 1550, He II lambda 1640, O IIIlambda 1661,1666, C IIIlambdalambda 1907,1909, Hbeta, OIIIlambdalambda 4959,5007 emission lines with <, ~ 50 km s super(-1) and (de-lensed) fluxes spanning the interval 1.0 x 10 super(-19)-2 x 10 super(-18) erg s super(-1) cm super(-2) at signal-to-noise ratio (S/N) = 4-30. The double-peaked Lyalpha emission with Deltanured - blue) = 280 (+ or -7) km s super(-1) and de-lensed fluxes 2.4 sub((blue)) 8.5 sub((red)) x 10 super(-18) erg s super(-1) cm super(-2)(S/N = 38 sub((blue)) 110 sub((red))) indicate a low column density of neutral hydrogen gas consistent with a highly ionized interstellar medium as also inferred from the large OIIIlambda 5007/ OIIlambda 3727 > 10 ratio. We detect C IV lambda 1548,1550 resonant doublet in emission, each component with FWHM <, ~ 45 km s super(-1) and redshifted by +51(+ or -10) km s super(-1) relative to the systemic redshift. We interpret this as nebular emission tracing an expanding optically thin interstellar medium. Both C IV lambda 1548,1550 and He II lambda 1640 suggest the presence of hot and massive stars (with a possible faint active galactic nucleus). The ultraviolet slope is remarkably blue, beta =-2.95 + or - 0.20 (F sub(lambda)= lambda super(beta)), consistent with a dust-free and young <, ~20 Myr galaxy. Line ratios suggest an oxygen abundance 12 + log(O/H) < 7.8. We are witnessing an early episode of star formation in which a relatively low N sub(H I) and negligible dust attenuation might favor a leakage of ionizing radiation. This galaxy currently represents a unique low-luminosity reference object for future studies of the reionization epoch with the James Webb Space Telescope.
Aims. We analyse the spectral energy distributions (SEDs) of the most distant galaxies discovered with the Hubble Space telescope and from the COSMOS survey and determine their physical properties, ...such as stellar age and mass, dust attenuation, and star-formation rate. Methods. We use our SED fitting tool including the effects of nebular emission to analyse three samples of z ~ 6–8 galaxies with observed magnitudes JAB ~ 23 to 29. Our models cover a wide parameter space. Results. We find that the physical parameters of most galaxies cover a wide range of acceptable values. Stellar ages, in particular, are not strongly constrained, even for objects detected longward of the Balmer break. As already pointed out earlier, the effects of nebular lines significantly affect the age determinations of star-forming galaxies at z ~ 6–8. We find no need for stellar populations with extreme metallicities or other non-standard assumptions (IMF, escape fraction) to explain the observed properties of faint z-dropout galaxies. Albeit with large uncertainties, our fit results show indications of dust attenuation in some of the z ≈ 6–8 galaxies, which have best-fit values of AV up to ~ 1. Furthermore, we find a possible trend of increasing dust attenuation with galaxy mass, and a relatively large scatter in specific star-formation rates, SFR/$M_\star$. Conclusions. The physical parameters of very high-z galaxies may be more uncertain than indicated by previous studies. Dust attenuation seems also to be present in some z ≈ 6–8 galaxies, and may be correlated with galaxy mass, as is also the case for SFR.
Aims. We examine the influence of nebular continuous and line emission in high-redshift star forming galaxies on determinations of their age, formation redshift, and other properties from SED fits. ...Methods. We include nebular emission consistently with the stellar emission in our SED fitting tool and analyse differentially a sample of 10 $z \approx 6$ galaxies in the GOODS-S field studied earlier elsewhere. Results. We find that the apparent Balmer/4000 Å breaks observed in a number of $z \approx 6$ galaxies detected at $\ga $3.6 μm with IRAC/Spitzer can be mimicked by the presence of strong restframe optical emission lines, implying in particular younger ages than previously thought. Applying these models to the small sample of $z \approx 6$ galaxies, we find that this effect may lead to a typical downward revision of their stellar ages by a factor ∼3. In consequence their average formation redshift may be reduced drastically, and these objects may not have contributed to cosmic reionisation at $z>6$. Extinction and stellar mass estimates may also be somewhat modified, but to a lesser extent. Conclusions. Careful SED fits including nebular emission and treating properly uncertainties and degeneracies are necessary for more accurate determinations of the physical parameters of high-z galaxies.
Abstract
We study the spectrophotometric properties of a highly magnified (
) pair of stellar systems identified at
z
= 3.2222 behind the Hubble Frontier Field galaxy cluster MACS J0416. Five ...multiple images (out of six) have been spectroscopically confirmed by means of VLT/MUSE and VLT/X-Shooter observations. Each image includes two faint (
), young (
Myr), low-mass (
), low-metallicity (12 + Log(O/H) ≃ 7.7, or 1/10 solar), and compact (30 pc effective radius) stellar systems separated by
pc after correcting for lensing amplification. We measured several rest-frame ultraviolet and optical narrow (
km s
−1
) high-ionization lines. These features may be the signature of very hot (
K) stars within dense stellar clusters, whose dynamical mass is likely dominated by the stellar component. Remarkably, the ultraviolet metal lines are not accompanied by Ly
α
emission (e.g., C
iv
/Ly
α
), despite the fact that the Ly
α
line flux is expected to be 150 times brighter (inferred from the H
β
flux). A spatially offset, strongly magnified (
) Ly
α
emission with a spatial extent
kpc
2
is instead identified 2 kpc away from the system. The origin of such a faint emission could be the result of fluorescent Ly
α
induced by a transverse leakage of ionizing radiation emerging from the stellar systems and/or may be associated with an underlying and barely detected object (with
de-lensed). This is the first confirmed metal-line emitter at such low-luminosity and redshift without Ly
α
emission—suggesting that, at least in some cases, a non-uniform covering factor of the neutral gas might hamper the Ly
α
detection.
Abstract
We report on five compact, extremely young (<10 Myr) and blue (βUV < −2.5, Fλ = λβ) objects observed with VLT/Multi Unit Spectroscopic Explorer at redshifts 3.1169 and 3.235, in addition to ...three objects at z = 6.145. These sources are strongly magnified (3–40 times) by the Hubble Frontier Field galaxy clusters MACS J0416 and AS1063. Their delensed half-light radii (Re) are between 16 and 140 pc, the stellar masses are ≃1–20 × 106 M⊙, the magnitudes are mUV = 28.8–31.4 (−17 < MUV < −15) and specific star formation rates can be as large as ∼800 Gyr−1. Remarkably, the inferred physical properties of two objects are similar to those expected in some globular cluster formation scenarios, representing the best candidate proto-GCs discovered so far. Rest-frame optical high-dispersion spectroscopy of one of them at z = 3.1169 yields a velocity dispersion σv ≃ 20 km s−1, implying a dynamical mass dominated by the stellar mass. Another object at z = 6.145, with delensed MUV ≃ −15.3 (mUV ≃ 31.4), shows a stellar mass and a star formation rate surface density consistent with the values expected from popular GC formation scenarios. An additional star-forming region at z = 6.145, with delensed mUV ≃ 32, a stellar mass of 0.5 × 106 M⊙ and a star formation rate of 0.06 M⊙ yr−1 is also identified. These objects currently represent the faintest spectroscopically confirmed star-forming systems at z > 3, elusive even in the deepest blank fields. We discuss how proto-GCs might contribute to the ionization budget of the Universe and augment Lyα visibility during reionization. This work underlines the crucial role of JWST in characterizing the rest-frame optical and near-infrared properties of such low-luminosity high-z objects.
![The GREATS H β + [O iii] lu...](http://api.summon.serialssolutions.com/2.0.0/image/issn/XR4PS5YY4K/0035-8711/small "The GREATS H β + [O iii] luminosity function and galaxy properties at z ∼ 8: walking the way of JWST")
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