CLEAR: Paschen-$β$ Star Formation Rates and Dust Attenuation of Low Redshift Galaxies

Cleri, Nikko J.; Trump, Jonathan R.; Backhaus, Bren E.; Momcheva, Ivelina; Papovich, Casey; Simons, Raymond C.; Weiner, Benjamin J.; Estrada-Carpenter, Vicente; Finkelstein, Steven L.; Giavalisco, Mauro; Ji, Zhiyuan; Jung, Intae; Matharu, Jasleen; Martínez, Félix; Sturm, Megan R.

doi:10.48550/arxiv.2009.00617

Cited by 6 publications

(9 citation statements)

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“…Previous work on the metallicities, ages, and formation histories of massive galaxies at 1 < z < 2 has been published in Estrada-Carpenter et al (2019, and the gas-phase metallicity gradients of star-forming galaxies is investigated in Simons et al (2020). Also, Cleri et al (2020) studied Paschen-β as a star-formation rate indicator in low redshift galaxies, using the CLEAR dataset.…”

Section: Clear Hst/grism Surveymentioning

confidence: 99%

CLEAR: Boosted Ly$α$ Transmission of the Intergalactic Medium in UV bright Galaxies

Jung,

Papovich,

Finkelstein

et al. 2021

Preprint

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Reionization is an inhomogeneous process, thought to begin in small ionized bubbles of the intergalactic medium (IGM) around overdense regions of galaxies. Recent Lyman-alpha (Lyα) studies during the epoch of reionization show growing evidence that ionized bubbles formed earlier around brighter galaxies, suggesting higher IGM transmission of Lyα from these galaxies. We investigate this problem using IR slitless spectroscopy from the Hubble Space Telescope (HST) Wide-Field Camera 3 (WFC3) G102 grism observations of 148 galaxies selected via photometric redshifts at 6.0 < z < 8.2. These galaxies have spectra extracted from the CANDELS Lyα Emission at Reionization (CLEAR) survey. We combine the CLEAR data for 275 galaxies with the Keck/DEIMOS+MOSFIRE dataset from the Texas Spectroscopic Search for Lyα Emission at the End of Reionization Survey. We then constrain the Lyα equivalent-width (EW) distribution at 6.0 < z < 8.2, which is described by an exponential form, dN/dEW ∝ exp(-EW)/W 0 , with the characteristic e-folding scale width (W 0 ). We confirm a significant drop of the Lyα strength (or W 0 ) at z > 6. Furthermore, we compare the redshift evolution of W 0 between galaxies at different UV luminosities. The UV-bright (M UV < −21, or L UV > L * ) galaxies show weaker evolution with a decrease of 0.4 (±0.2) dex in W 0 at z > 6 while UV-faint (M UV > −21, or L UV < L * ) galaxies exhibit a significant drop by a factor of 0.7-0.8 (±0.2) dex in W 0 from z < 6 to z > 6. Our results add to the accumulating evidence that UV-bright galaxies exhibit boosted Lyα transmission in the IGM, suggesting that reionization completes sooner in regions proximate to galaxies of higher UV luminosity.

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Section: Clear Hst/grism Surveymentioning

confidence: 99%

CLEAR: Boosted Ly$α$ Transmission of the Intergalactic Medium in UV bright Galaxies

Jung,

Papovich,

Finkelstein

et al. 2021

Preprint

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“…Morelli et al (2020) probed that the index behaviour in the cool IRTF stars is driven by temperature, with no trends with surface gravity and metallicity. Cleri et al (2020) showed that the Paβ index could adopted as a tracer of the star formation rate in galaxies, showing a similar (and somewhat even better) behaviour with respect to the Hα and Hβ indicators. This supports our findings (Fig.…”

Section: Trends With the Metal Indicesmentioning

confidence: 76%

Near-infrared spectroscopic indices for unresolved stellar populations. II. Index measurements

Gasparri,

Morelli,

Ivanov

et al. 2021

Preprint

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We measured the equivalent width of a large set of near-infrared (NIR, 0.8-2.4 µm) line-strength indices in the XShooter medium-resolution spectra of the central regions of 14 galaxies. We found that two aluminum indices Al at 1.31 µm and Al1 at 1.67 µm and the two CO indices CO1 at 1.56 µm and CO4 at 1.64 µm are tightly correlated with the velocity dispersion. Moreover, the NIR Al and CO1 indices show strong correlations with the optical Mg2 and Mgb indices, which are usually adopted as alpha/Fe-enhancement diagnostics. The molecular FeH1 index at 1.58 µm tightly correlates with the optical Fe and [MgFe]' indices, which are used as total metallicity diagnostics. The NIR Paβ index at 1.28 µm has a behaviour similar to the optical Hβ index, which is a diagnostic of mean age. We defined two new composite indices, Al and [AlFeH], as possible candidates to be used as NIR diagnostics of total metallicity and α/Fe enhancement. The NIR Al index has a strong correlation with the optical Mg2 and Mgb indices, while the [AlFeH] index is tightly correlated with the optical Fe and [MgFe] indices. The distribution of the data points in the NIR Paβ-Al and Paβ-[AlFeH] diagrams mimic that in the optical [MgFe] -Hβ and the Mgb-Fe diagrams, which are widely used to constraint the properties of the unresolved stellar populations. We concluded that some NIR line-strength indices could be useful in studying stellar populations as well as in fine-tuning stellar population models.

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“…Observational constraints on the degree to which stars and dust are spatially coupled are difficult to obtain but recent work by Leslie et al (2018) and van der Giessen et al (2022) using the Tuffs et al (2004) model show that galaxies in both SDSS and COSMOS exhibit significant 'clumpiness' fractions, such that young stars are heavily attenuated and the overall attenuation curves are shaped by this non-uniformity in dust geometry. Paβ and Hα emission line ratios, which can be used to infer dust attenuation, have been shown to lie outside the expected relation when measured in resolved galaxies with prominent dust lanes, as demonstrated in Cleri et al (2020), indicating the need to accommodate the star-dust geometry in dust attenuation measurements.…”

Section: Understanding Variations In Dust Attenuation Curvesmentioning

confidence: 96%

“…Correlations have been found between attenuation curve shape and galaxy physical properties like stellar mass and star formation activity (e.g. Noll et al 2007Noll et al , 2009aSalim et al 2016;Battisti et al 2016Battisti et al , 2017aCorre et al 2018;Salim et al 2018;Reddy et al 2018;Cleri et al 2020;Bogdanoska & Burgarella 2020), galaxy spectral type (e.g. Kriek & Conroy 2013), morphology and observed inclination angle (e.g.…”

Section: Introductionmentioning

confidence: 99%

How Well Can We Measure Galaxy Dust Attenuation Curves? The Impact of the Assumed Star-Dust Geometry Model in SED Fitting

Lower,

Narayanan,

Leja

et al. 2022

Preprint

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One of the most common methods for inferring galaxy attenuation curves is via spectral energy distribution (SED) modeling, where the dust attenuation properties are modeled simultaneously with other galaxy physical properties. In this paper, we assess the ability of SED modeling to infer these dust attenuation curves from broadband photometry, and suggest a new flexible model that greatly improves the accuracy of attenuation curve derivations. To do this, we fit mock SEDs generated from the simba cosmological simulation with the prospector SED fitting code. We consider the impact of the commonly-assumed uniform screen model and introduce a new non-uniform screen model parameterized by the fraction of unobscured stellar light. This non-uniform screen model allows for a non-zero fraction of stellar light to remain unattenuated, resulting in a more flexible attenuation curve shape by decoupling the shape of the UV attenuation curve from the optical attenuation curve. The ability to constrain the dust attenuation curve is significantly improved with the use of a non-uniform screen model, with the median offset in UV attenuation decreasing from −0.30 dex with a uniform screen model to −0.17 dex with the non-uniform screen model. With this increase in dust attenuation modeling accuracy, we also improve the star formation rates (SFRs) inferred with the non-uniform screen model, decreasing the SFR offset on average by 0.12 dex. We discuss the efficacy of this new model, focusing on caveats with modeling star-dust geometries and the constraining power of available SED observations.

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CLEAR: Paschen-$β$ Star Formation Rates and Dust Attenuation of Low Redshift Galaxies

Cited by 6 publications

References 0 publications

CLEAR: Boosted Ly$α$ Transmission of the Intergalactic Medium in UV bright Galaxies

CLEAR: Boosted Ly$α$ Transmission of the Intergalactic Medium in UV bright Galaxies

Near-infrared spectroscopic indices for unresolved stellar populations. II. Index measurements

How Well Can We Measure Galaxy Dust Attenuation Curves? The Impact of the Assumed Star-Dust Geometry Model in SED Fitting

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