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• W4200007105 abstract "Abstract We present and publicly release ( www.gclasshst.com ) the first spatially resolved H α maps of star-forming cluster galaxies at z ∼ 1, made possible with the Wide Field Camera 3 (WFC3) G141 grism on the Hubble Space Telescope (HST). Using a similar but updated method to 3D-HST in the field environment, we stack the H α maps in bins of stellar mass, measure the half-light radius of the H α distribution, and compare it to the stellar continuum. The ratio of the H α to stellar continuum half-light radius, <?CDATA $R[{rm{H}}alpha /{rm{C}}]=tfrac{{R}_{mathrm{eff},{rm{H}}alpha }}{{R}_{mathrm{eff},mathrm{Cont}}}$?> <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML overflow=scroll> <mml:mi>R</mml:mi> <mml:mo stretchy=false>[</mml:mo> <mml:mi mathvariant=normal>H</mml:mi> <mml:mi>α</mml:mi> <mml:mrow> <mml:mo stretchy=false>/</mml:mo> </mml:mrow> <mml:mi mathvariant=normal>C</mml:mi> <mml:mo stretchy=false>]</mml:mo> <mml:mo>=</mml:mo> <mml:mstyle displaystyle=false> <mml:mfrac> <mml:mrow> <mml:msub> <mml:mrow> <mml:mi>R</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>eff</mml:mi> <mml:mo>,</mml:mo> <mml:mi mathvariant=normal>H</mml:mi> <mml:mi>α</mml:mi> </mml:mrow> </mml:msub> </mml:mrow> <mml:mrow> <mml:msub> <mml:mrow> <mml:mi>R</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>eff</mml:mi> <mml:mo>,</mml:mo> <mml:mi>Cont</mml:mi> </mml:mrow> </mml:msub> </mml:mrow> </mml:mfrac> </mml:mstyle> </mml:math> , is smaller in the clusters by (6 ± 9)%, but statistically consistent within 1 σ uncertainties. A negligible difference in R [H α /C] with environment is surprising, given the higher quenched fractions in the clusters relative to the field. We postulate that the combination of high quenched fractions and no change in R [H α /C] with environment can be reconciled if environmental quenching proceeds rapidly. We investigate this hypothesis by performing similar analysis on the spectroscopically confirmed, recently quenched cluster galaxies. 87% have H α detections, with star formation rates 8 ± 1 times lower than star-forming cluster galaxies of similar stellar mass. Importantly, these galaxies have an R [H α /C] that is (81 ± 8)% smaller than coeval star-forming field galaxies at fixed stellar mass. This suggests the environmental quenching process occurred outside-in. We conclude that disk truncation due to ram pressure stripping is occurring in cluster galaxies at z ∼ 1, but more rapidly and/or efficiently than in z ≲ 0.5 clusters, such that the effects on R [H α /C] become observable just after the cluster galaxy has recently quenched." @default.
• W4200007105 created "2021-12-31" @default.
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• W4200007105 date "2021-12-01" @default.
• W4200007105 modified "2023-10-05" @default.
• W4200007105 title "HST/WFC3 Grism Observations of z ∼ 1 Clusters: Evidence for Rapid Outside-in Environmental Quenching from Spatially Resolved Hα Maps" @default.
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