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We present the results of a sim 60-hour multiband observational campaign with the Atacama Large Millimeter Array targeting a spectroscopically confirmed and lensed galaxy at $z=6.07$, first identified during the ALMA Lensing Cluster Survey (ALCS). We sampled the dust continuum emission from rest frame 90 to 370 mu m at six different frequencies and set constraining upper limits on the molecular gas line emission and content by targeting the and transitions in two lensed images with $ Complementing these submillimeter observations with deep optical and near-IR photometry and spectroscopy with we find this galaxy to form stars at a rate of $ SFR 50-70$<!PCT!> of which is obscured by dust. This is consistent with what one would predict for a $M_ object by extrapolating the relation between the fraction of the obscured star formation rate and stellar mass at $z<2.5$ and with observations of IR-detected objects at $5<z<7$. The light-weighted dust temperature of dust K is similar to that of more massive galaxies at similar redshifts, although with large uncertainties and with possible negative gradients. We measure a dust mass of dust 10^6 \, M_ and, by combining and a dynamical estimate, a gas mass of gas Their ratio ($ DGR $) is in good agreement with predictions from models and empirical relations in the literature. The dust-to-stellar mass fraction of $f_ dust 0.002$ and the young stellar age ($100-200$ Myr) are consistent with efficient dust production via supernovae, as predicted by existing models and simulations of dust evolution. Also, the expected number density of galaxies with at $z=6$ from a subset of these models is in agreement with the observational estimate that we set from the parent ALCS survey. The combination of gravitational lensing and deep multiwavelength observations allowed us to probe luminosity and mass regimes up to two orders of magnitude lower than what has been explored so far for field galaxies at similar redshifts. Our results serve as a benchmark for future observational endeavors of the high-redshift and faint galaxy population that might have driven the reionization of the Universe.
We present the results of a sim 60-hour multiband observational campaign with the Atacama Large Millimeter Array targeting a spectroscopically confirmed and lensed galaxy at $z=6.07$, first identified during the ALMA Lensing Cluster Survey (ALCS). We sampled the dust continuum emission from rest frame 90 to 370 mu m at six different frequencies and set constraining upper limits on the molecular gas line emission and content by targeting the and transitions in two lensed images with $ Complementing these submillimeter observations with deep optical and near-IR photometry and spectroscopy with we find this galaxy to form stars at a rate of $ SFR 50-70$<!PCT!> of which is obscured by dust. This is consistent with what one would predict for a $M_ object by extrapolating the relation between the fraction of the obscured star formation rate and stellar mass at $z<2.5$ and with observations of IR-detected objects at $5<z<7$. The light-weighted dust temperature of dust K is similar to that of more massive galaxies at similar redshifts, although with large uncertainties and with possible negative gradients. We measure a dust mass of dust 10^6 \, M_ and, by combining and a dynamical estimate, a gas mass of gas Their ratio ($ DGR $) is in good agreement with predictions from models and empirical relations in the literature. The dust-to-stellar mass fraction of $f_ dust 0.002$ and the young stellar age ($100-200$ Myr) are consistent with efficient dust production via supernovae, as predicted by existing models and simulations of dust evolution. Also, the expected number density of galaxies with at $z=6$ from a subset of these models is in agreement with the observational estimate that we set from the parent ALCS survey. The combination of gravitational lensing and deep multiwavelength observations allowed us to probe luminosity and mass regimes up to two orders of magnitude lower than what has been explored so far for field galaxies at similar redshifts. Our results serve as a benchmark for future observational endeavors of the high-redshift and faint galaxy population that might have driven the reionization of the Universe.
Planetary nebulae (PNe) have three main components: a central star (CS), ionized gas, and dust in the nebula. Each contains critical chemical fingerprints of the PN's evolution, which serve as tracers of the evolution, nucleosynthesis, and dust production that occurred during the preceding asymptotic giant branch (AGB) phase. We aim to build a bridge to link the PN phase to the evolution of progenitors, to better understand the dust production and mass-loss mechanism during the final AGB phase. Here we present a comprehensive study of nine Large Magellanic Cloud spherical or elliptical PNe whose observations from the UV through the IR are available in the literature. We characterize nebulae and CSs, finding information necessary to reconstruct the evolutionary history of mass-loss and dust production, such as as the amount of gas that makes up the nebula and the dust that surrounds the CS. We compared the observed energy distribution of the selected PNe to that obtained from photoionization modeling, taking the presence of dust into account. The physical and chemical parameters of the CSs were then compared with predictions from the evolutionary tracks. We characterize the source, assigning a progenitor, early-AGB mass to each CS. We estimate the mass of the nebula and the dust-to-gas ratio. For five objects, we find evidence for the presence of a near-IR bump, which would indicate the presence of hot dust.
We present Atacama Large Millimetre/submillimetre Array (ALMA) observations of the [O iii] 88 μm emission of a sample of thirteen galaxies at z = 6 to 7.6 selected as [C ii]-emitting companion sources of quasars. To disentangle the origins of the luminous Oxygen line in the z > 6 Universe, we looked at emission-line galaxies that are selected through an excellent star-formation tracer [C ii] with star-formation rates between 9 and 162 $\rm {\rm M}_{\odot }/yr$. Direct observations reveal [O iii] emission in just a single galaxy ($L_\mathrm{[O\, \small {III}]}/L_\mathrm{[C\, \small {II}]}$ = 2.3), and a stacked image shows no [O iii] detection, providing deep upper limits on the $L_\mathrm{[O\, \small {III}]}/L_\mathrm{[C\, \small {II}]}$ ratios in the z > 6 Universe ($L_\mathrm{[O\, \small {III}]}/L_\mathrm{[C\, \small {II}]}$ < 1.2 at 3σ). While the fidelity of this sample is high, no obvious optical/near-infrared counterpart is seen in the JWST imaging available for four galaxies. Additionally accounting for low-z CO emitters, line stacking shows that our sample-wide result remains robust: The enhanced $L_\mathrm{[O\, \small {III}]}/L_\mathrm{[C\, \small {II}]}$ reported in the first billion years of the Universe is likely due to the selection towards bright, blue Lyman-break galaxies with high surface star-formation rates or young stellar populations. The deep upper limit on the rest-frame 90 μm continuum emission (<141μJy at 3σ), implies a low average dust temperature (Tdust ≲ 30 K) and high dust mass (Mdust ∼ 108 M⊙). As more normal galaxies are explored in the early Universe, synergy between JWST and ALMA is fundamental to further investigate the ISM properties of the a broad range of samples of high-z galaxies.
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