CLEAR: The Evolution of Spatially Resolved Star Formation in Galaxies between 0.5 ≲ z ≲ 1.7 Using Hα Emission Line Maps

Matharu, Jasleen; Papovich, Casey; Simons, Raymond C.; Momcheva, Ivelina; Brammer, Gabriel; Ji, Zhiyuan; Backhaus, Bren E.; Cleri, Nikko J.; Estrada-Carpenter, Vicente; Finkelstein, Steven L.; Finlator, Kristian; Giavalisco, Mauro; Jung, Intae; Muzzin, Adam; Nelson, Erica J.; Pillepich, Annalisa; Trump, Jonathan R.; Weiner, Benjamin J.

doi:10.3847/1538-4357/ac8471

Cited by 19 publications

(34 citation statements)

References 161 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…4). Matharu et al (2022) found that size measurements in CANDELS-like HST imaging are less reliable for galaxies at these redshifts with M * 10 9 M (primarily this is because the sizes of the galaxies are small and approaching the resolution limit of the HST WFC3 image.). We therefore apply this mass limit to our study here.…”

Section: Sample Selectionmentioning

confidence: 99%

“…We use galfit (Peng et al 2002(Peng et al , 2010 for the morphology measurements following the two-galfit-run approach from Matharu et al (2019Matharu et al ( , 2022, which leads to a high level of agreement with published size measurements (see more details in Matharu et al 2019). For each galaxy, we create 10 × 10 cutouts of NUV-, PAHbands and F160W and associated error images, centered on its F160W coordinates.…”

Section: The Morphology Measurementsmentioning

confidence: 99%

“…Tracking spatially resolved star formation in galaxies will provide insight into this structural/size evolution, thus, their link to the dominant stellar buildup of galaxies and quenching mechanisms. Indeed, studies found that ongoing star formation traced by Hα emission occurs in disks that are more extended than those occupied by existing stars in SFGs in the redshift range of z ∼ 0.5 − 2.7 (Nelson et al 2012;Tacchella et al 2015;Nelson et al 2016a;Wilman et al 2020;Matharu et al 2022), while the extent of star formation and stellar disks are found to be the same in the local universe (James et al 2009;Fossati et al 2013). However, dust obscuration posts an immense challenge in uncovering star-formation activities via spatially resolved galaxy studies.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

CEERS: Spatially Resolved UV and mid-IR Star Formation in Galaxies at 0.2 < z < 2.5: The Picture from the Hubble and James Webb Space Telescopes

Shen¹,

Papovich²,

Yang³

et al. 2023

Preprint

View full text Add to dashboard Cite

We present the mid-IR (MIR) morphologies for 70 star-forming galaxies (SFGs) at 0.2 < z < 2.5 with stellar mass M * > 10 9 M using JWST MIRI observations from the Cosmic Evolution Early Release Science survey (CEERS). The MIRI bands span the MIR (7.7-21 µm), enabling us to measure the effective radii (R eff ) and Sérsic indexes of these SFGs at rest-frame 6.2 and 7.7 µm, which contain strong emission from Polycyclic aromatic hydrocarbon (PAH) features, a well-established tracer of star formation in galaxies. We compare the PAH-band morphologies to those in rest-frame Near-UV (NUV) using HST ACS/F435W or ACS/F606W and optical/near-IR using HST WFC3/F160W imaging from UVCANDELS and CANDELS, where the NUV-band and F160W trace the profile of (unobscured) massive stars and the stellar continuum, respectively. The R eff of galaxies in the PAHband are slightly smaller (∼10%) than those in F160W for more massive galaxies with M * 10 9.5 M at z ≤ 1.2 and with M * 10 10 M at z ≥ 1.2, but the PAH-band and F160W have a similar fractions of light within 1 kpc. In contrast, the R eff of galaxies in the NUV-band are larger, with lower fractions of light within 1 kpc compared to the F160W for galaxies at z ≤ 1.2. Using the MIRI data to estimate the surface density of the IR-based SFR, we find the correlation between the IR-based SFR surface density and stellar mass has a steeper slope than that of the UV-based surface density and stellar mass, suggesting galaxies with higher stellar masses having increasing amounts of obscured fraction of star formation in their inner regions. This paper demonstrates how the high-angular resolution data from JWST /MIRI can reveal new information about the morphology of obscured-star formation.

show abstract

Section: Sample Selectionmentioning

confidence: 99%

Section: The Morphology Measurementsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

CEERS: Spatially Resolved UV and mid-IR Star Formation in Galaxies at 0.2 < z < 2.5: The Picture from the Hubble and James Webb Space Telescopes

Shen¹,

Papovich²,

Yang³

et al. 2023

Preprint

View full text Add to dashboard Cite

show abstract

“…The CLEAR spectra have been used to study the metallicities, ages, and formation histories of massive high-redshift galaxies (Estrada-Carpenter et al 2019Simons et al 2021) and appraise Paschen-β as an SFR indicator in low-redshift galaxies (Cleri et al 2022). Matharu et al (2022) used spatially resolved Hα emission-line maps of star-forming galaxies to study the evolution of gradients in galaxy assembly. Jung et al (2022) used CLEAR to study the evolution of the strength of Lyα emission at 6.5 < z < 8.2.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

“…Spatially resolving Hα gives the profile of star formation within a galaxy. This gives us information about whether a galaxy is formed inside-out or outside-in by comparing to the galaxy's stellar continuum (Nelson et al 2012(Nelson et al , 2016a(Nelson et al , 2021Matharu et al 2022). Spatially resolving the Balmer decrement (Hα/Hβ) measures the profile of dust attenuation within a galaxy.…”

Section: Introductionmentioning

confidence: 99%

CLEAR: Spatially Resolved Emission Lines and Active Galactic Nuclei at 0.6 < z < 1.3

Backhaus

Bridge

Trump

et al. 2023

ApJ

Self Cite

View full text Add to dashboard Cite

We investigate spatially resolved emission-line ratios in a sample of 219 galaxies (0.6 < z < 1.3) detected using the G102 grism on the Hubble Space Telescope Wide Field Camera 3 taken as part of the CANDELS Lyα Emission at Reionization survey to measure ionization profiles and search for low-luminosity active galactic nuclei (AGN). We analyze [O iii] and Hβ emission-line maps, enabling us to spatially resolve the [O iii]/Hβ emission-line ratio across the galaxies in the sample. We compare the [O iii]/Hβ ratio in galaxy centers and outer annular regions to measure ionization differences and investigate the potential of sources with nuclear ionization to host AGN. We investigate some of the individual galaxies that are candidates to host strong nuclear ionization and find that they often have low stellar mass and are undetected in X-rays, as expected for low-luminosity AGN in low-mass galaxies. We do not find evidence for a significant population of off-nuclear AGN or other clumps of off-nuclear ionization. We model the observed distribution of [O iii]/Hβ spatial profiles and find that most galaxies are consistent with a small or zero difference between their nuclear and off-nuclear line ratios, but 6%–16% of galaxies in the sample are likely to host nuclear [O iii]/Hβ that is ∼0.5 dex higher than in their outer regions. This study is limited by large uncertainties in most of the measured [O iii]/Hβ spatial profiles; therefore, deeper data, e.g., from deeper HST/WFC3 programs or from JWST/NIRISS, are needed to more reliably measure the spatially resolved emission-line conditions of individual high-redshift galaxies.

show abstract

CEERS: MIRI deciphers the spatial distribution of dust-obscured star formation in galaxies at 0.1 < z < 2.5

Magnelli,

Gómez-Guijarro,

Elbaz

et al. 2023

A&A

View full text Add to dashboard Cite

Aims. We study the stellar (i.e., rest-optical) and dust-obscured star-forming (i.e., rest-mid-infrared) morphologies (i.e., sizes and Sérsic indices) of star-forming galaxies (SFGs) at 0.1 < z < 2.5. Methods. We combined Hubble Space Telescope (HST) images from the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) with JWST images from the Cosmic Evolution Early Release Science (CEERS) survey to measure the stellar and dust-obscured star formation distributions of 69 SFGs. Rest-mid-infrared (rest-MIR) morphologies were determined using a Markov chain Monte Carlo (MCMC) approach applied to the sharpest Mid-InfraRed Instrument (MIRI) images (i.e., shortest wavelength) dominated by dust emission (Sνdust/Sνtotal > 75%), as inferred for each galaxy from our optical-to-far-infrared spectral energy distribution fits with CIGALE. Rest-MIR Sérsic indices were only measured for the brightest MIRI sources, that is, with a signal-to-noise (S/N) greater than 75 (35 galaxies). At a lower S/N, simulations do indeed show that simultaneous measurements of both the size and Sérsic index become less reliable. We extended our study to fainter sources (i.e., S/N > 10; 69 galaxies) by restricting our structural analysis to their rest-MIR sizes (ReMIR) and by fixing their Sérsic index to a value of one. Results. Our MIRI-selected sample corresponds to a mass-complete sample (> 80%) of SFGs down to stellar masses 109.5, 109.5, and 1010 M⊙ at z ∼ 0.3, 1, and 2, respectively. The rest-MIR Sérsic index of bright galaxies (S/N > 75) has a median value of 0.7−0.3+0.8 (the range corresponds to the 16th and 84th percentiles), which is in good agreement with their median rest-optical Sérsic indices. The Sérsic indices as well as the distribution of the axis ratio of these galaxies suggest that they have a disk-like morphology in the rest-MIR. Galaxies above the main sequence (MS) of star formation (i.e., starbursts) have rest-MIR sizes that are, on average, a factor ∼2 smaller than their rest-optical sizes (ReOpt.). The median rest-optical to rest-MIR size ratio of MS galaxies increases with their stellar mass, from 1.1−0.2+0.4 at ∼109.8 M⊙ to 1.6−0.3+1.0 at ∼1011 M⊙. This mass-dependent trend resembles the one found in the literature between the rest-optical and rest-near-infrared sizes of SFGs, suggesting that it is primarily due to radial color gradients affecting rest-optical sizes and that the sizes of the stellar and star-forming components of SFGs are, on average, consistent at all masses. There is, however, a small population of SFGs (∼15%) with a compact star-forming component embedded in a larger stellar structure, with ReOpt.c > 1.8 × ReMIR. This population could be the missing link between galaxies with an extended stellar component and those with a compact stellar component, the so-called blue nuggets.

show abstract

CLEAR: The Evolution of Spatially Resolved Star Formation in Galaxies between 0.5 ≲ z ≲ 1.7 Using Hα Emission Line Maps

Cited by 19 publications

References 161 publications

CEERS: Spatially Resolved UV and mid-IR Star Formation in Galaxies at 0.2 < z < 2.5: The Picture from the Hubble and James Webb Space Telescopes

CEERS: Spatially Resolved UV and mid-IR Star Formation in Galaxies at 0.2 < z < 2.5: The Picture from the Hubble and James Webb Space Telescopes

CLEAR: Spatially Resolved Emission Lines and Active Galactic Nuclei at 0.6 < z < 1.3

CEERS: MIRI deciphers the spatial distribution of dust-obscured star formation in galaxies at 0.1 < z < 2.5

Contact Info

Product

Resources

About