The average dust attenuation curve at <i>z</i> ∼ 1.3 based on <i>HST</i> grism surveys

Battisti, Andrew; Bagley, Micaela; Baronchelli, Ivano; Dai, Y. Sophia; Henry, Alaina; Malkan, M. A.; Alavi, Anahita; Calzetti, Daniela; Colbert, James; McCarthy, Patrick J.; Mehta, Vihang; Rafelski, Marc; Scarlata, Claudia; Shivaei, Irene; Wisnioski, Emily

doi:10.1093/mnras/stac1052

Cited by 12 publications

(3 citation statements)

References 110 publications

(193 reference statements)

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“…After rejecting the cases with bad fits (𝜒 2 > 2𝜎), we compare the uncertainties of 𝑧 phot , 𝑀 * and SFR derived from UV to near-IR photo-z fitting to those results from fitting the full available SED in the top panels of Figure 8. As expected (Battisti et al 2022), the non-IR fits tend to come with larger measurement uncertainties because fewer observations are available to constrain the models. For 𝑧 phot and 𝑀 * , including the IR bands only leads to a relatively small improvement (i.e., decrease) in the uncertainty.…”

Section: Contribution Of Including Ir Data To the Uncertainties Of 𝑀 ...supporting

confidence: 52%

Exploring the Intrinsic Scatter of the Star-Forming Galaxy Main Sequence at redshift 0.5 to 3.0

Huang,

Battisti,

Grasha

et al. 2023

Preprint

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Previous studies have shown that the normalization and scatter of the galaxy 'main sequence' (MS), the relation between star formation rate (SFR) and stellar mass (𝑀 * ), evolves over cosmic time. However, such studies often rely on photometric redshifts and/or only rest-frame UV to near-IR data, which may underestimate the SFR and 𝑀 * uncertainties. We use MAGPHYS+photo-z to fit the UV to radio spectral energy distributions of 12,380 galaxies in the COSMOS field at 0.5 < 𝑧 < 3.0 and self-consistently include photometric redshift uncertainties on the derived SFR and 𝑀 * . We quantify the effect on the observed MS scatter from (1) photometric redshift uncertainties (which are minor) and ( 2) fitting only rest-frame ultraviolet to near-infrared observations (which are severe). At fixed redshift and 𝑀 * , we find that the intrinsic MS scatter for our sample of galaxies is 1.4 to 2.6 times larger than the measurement uncertainty. The average intrinsic MS scatter has decreased by 0.1 dex from 𝑧 = 0.5 to ∼ 2.0. At low-𝑧, the trend between the intrinsic MS scatter and 𝑀 * follows a functional form similar to an inverse stellar mass-halo mass relation (SMHM; 𝑀 * /𝑀 halo vs 𝑀 * ), with a minimum in intrinsic MS scatter at log(𝑀 * /𝑀 ) ∼ 10.25 and larger scatter at both lower and higher 𝑀 * ; while this distribution becomes flatter for high-𝑧. The SMHM is thought to be a consequence of feedback effects and this similarity may suggest a link between galaxy feedback and the intrinsic MS scatter. These results favor a slight evolution in the intrinsic MS scatter with both redshift and mass.

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Section: Contribution Of Including Ir Data To the Uncertainties Of 𝑀 ...supporting

confidence: 52%

Exploring the Intrinsic Scatter of the Star-Forming Galaxy Main Sequence at redshift 0.5 to 3.0

Huang,

Battisti,

Grasha

et al. 2023

Preprint

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“…Vast samples of galaxies with multiple Balmer emission-line measurements exist in the local Universe, from surveys such as the Sloan Digital Sky Survey (SDSS; Abazajian et al 2009), and including both integrated spectra and spatially resolved emission-line maps (e.g., Belfiore et al 2018;Ellison et al 2018). Large samples of Balmer decrements and dust-corrected Hα SFRs (SFR(Hα)) were assembled for the first time at z > 1 with the advent of the Hubble Space Telescope (HST)/WFC3 IR grism (Domínguez et al 2013;Price et al 2014;Battisti et al 2022) as well as multi-object near-IR spectrographs on 8-10 m class ground-based telescopes (Reddy et al 2015). These measurements were used to trace the so-called "main sequence" of galaxy formation during the epoch of peak SFR density in the Universe (Shivaei et al 2015), constrain the nature of nebular dust attenuation and ISM geometry (Reddy et al 2015(Reddy et al , 2020Shivaei et al 2020), describe the spatially resolved growth of galaxy disks (Nelson et al 2016), and investigate the relationship between dust attenuation and stellar mass (Shapley et al 2022).…”

Section: Introductionmentioning

confidence: 99%

JWST/NIRSpec Balmer-line Measurements of Star Formation and Dust Attenuation at z ∼ 3–6

Shapley,

Sanders,

Reddy

et al. 2023

ApJ

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We present an analysis of the star formation rates (SFRs) and dust attenuation properties of star-forming galaxies at 2.7 ≤ z < 6.5 drawn from the Cosmic Evolution Early Release Science Survey. Our analysis is based on JWST/NIRSpec Micro-Shutter Assembly R ∼ 1000 spectroscopic observations covering approximately 1–5 μm. Our primary rest-frame optical spectroscopic measurements are Hα/Hβ Balmer decrements, which we use as an indicator of nebular dust attenuation. In turn, we use Balmer decrements to obtain dust-corrected Hα-based SFRs (i.e., SFR(Hα)). We construct the relationship between SFR(Hα) and stellar mass (M *) in three bins of redshift (2.7 ≤ z < 4.0, 4.0 ≤ z < 5.0, and 5.0 ≤ z < 6.5), which represents the first time the star-forming main sequence has been traced at these redshifts using direct spectroscopic measurements of Balmer emission as a proxy for SFR. In tracing the relationship between SFR(Hα) and M * back to such early times (z > 3), it is essential to use a conversion factor between Hα and SFR that accounts for the subsolar metallicity prevalent among distant galaxies. We also use measured Balmer decrements to investigate the relationship between dust attenuation and stellar mass out to z ∼ 6. The lack of significant redshift evolution in attenuation at fixed stellar mass, previously confirmed using Balmer decrements out to z ∼ 2.3, appears to hold out to z ∼ 6.5. Given the rapidly evolving gas, dust, and metal content of star-forming galaxies at fixed mass, this lack of significant evolution in attenuation provides an ongoing challenge to explain.

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“…Observations from ground-based multiobject near-IR spectrographs (e.g., Keck/MOSFIRE, the Very Large Telescope (VLT)/KMOS) and space-based facilities (e.g., the Hubble Space Telescope (HST)/WFC3 grism) have yielded measurements of hydrogen recombination lines and nebular reddening for thousands of galaxies up to z ∼ 2.6 (e.g., Förster Schreiber et al 2009;Kashino et al 2013;Price et al 2014;Reddy et al 2015;De Barros et al 2016;Shivaei et al 2020b;Reddy et al 2020;Rezaee et al 2021;Battisti et al 2022). There is a general consensus from these studies that, on average, the nebular reddening exceeds that of the stellar continuum, where the difference in reddening may correlate with SFR, specific SFR (sSFR), stellar mass, and/or gas-phase metallicity.…”

Section: Introductionmentioning

confidence: 99%

Paschen-line Constraints on Dust Attenuation and Star Formation at z ∼ 1–3 with JWST/NIRSpec

Reddy

Topping

Shapley

et al. 2023

ApJ

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We use medium-resolution JWST/NIRSpec observations from the Cosmic Evolution Early Release Science Survey to place the first constraints on dust attenuation and star formation based on Paschen lines for a sizable sample of 63 galaxies at redshifts z = 1.0–3.1. Our analysis indicates strong correlations between the Balmer decrement, Hα/Hβ, and line ratios that include Paschen lines (i.e., Paα/Hβ, Paβ/Hβ, and the Paschen decrement, Paα/Paβ), suggesting that the former is sensitive to the overall dust obscuration toward H ii regions in high-redshift galaxies. The line ratios are used to derive nebular reddening, E(B − V)neb, and star formation rates (SFRs). There is marginal evidence that the SFRs deduced from Paschen lines may exceed by ≈25% those derived from Balmer lines alone, suggesting the presence of star formation that is optically thick in Balmer lines, though deeper observations are needed to confirm this result. Using the Paschen-line constraints on the bolometric SFRs, we reevaluate the relationship between dust obscuration and UV spectral slope, and find a reddening of the UV continuum that, on average, follows the SMC extinction curve. This analysis highlights the need for deeper spectroscopy of more representative samples to evaluate nebular dust attenuation and bolometric SFRs in high-redshift galaxies, and their relationship to the reddening of the UV continuum.

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The average dust attenuation curve at z ∼ 1.3 based on HST grism surveys

Cited by 12 publications

References 110 publications

Exploring the Intrinsic Scatter of the Star-Forming Galaxy Main Sequence at redshift 0.5 to 3.0

Exploring the Intrinsic Scatter of the Star-Forming Galaxy Main Sequence at redshift 0.5 to 3.0

JWST/NIRSpec Balmer-line Measurements of Star Formation and Dust Attenuation at z ∼ 3–6

Paschen-line Constraints on Dust Attenuation and Star Formation at z ∼ 1–3 with JWST/NIRSpec

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