Where stars form

Inside - out growth and coherent star formation from HSTHα maps of 3200 galaxies across the main sequence at 0.7 <z <1.5

Erica June Nelson, Pieter G. Van Dokkum, Natascha M. Förster Schreiber, Marijn Franx, Gabriel B. Brammer, Ivelina G. Momcheva, Stijn Wuyts, Katherine E. Whitaker, Rosalind E. Skelton, Mattia Fumagalli, Christopher C. Hayward, Mariska Kriek, Ivo Labbé, Joel Leja, Hans Walter Rix, Linda J. Tacconi, Arjen Van Der Wel, Frank C. Van Den Bosch, Pascal A. Oesch, Claire Dickey & 1 others Johannes Ulf Lange

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Abstract

We present Hα maps at 1 kpc spatial resolution for star-forming galaxies at z ∼ 1, made possible by the Wide Field Camera 3 grism on Hubble Space Telescope (HST). Employing this capability over all five 3D-HST/CANDELS fields provides a sample of 3200 galaxies enabling a division into subsamples based on stellar mass and star formation rate (SFR). By creating deep stacked Hα images, we reach surface brightness limits of 1 × 10-18 erg s-1 cm-2 arcsec-2, allowing us to map the distribution of ionized gas to ∼10 kpc for typical L∗ galaxies at this epoch. We find that the spatial extent of the Hα distribution increases with stellar mass as r = 1.5 (M/1010 M)0.23 kpc. The Hα emission is more extended than the stellar continuum emission, consistent with inside-out assembly of galactic disks. This effect grows stronger with mass as r/r = 1.1(M/1010 M)0.054. We map the Hα distribution as a function of SFR(IR+UV) and find evidence for "coherent star formation" across the SFR-M plane: above the main sequence (MS), Hα is enhanced at all radii; below the MS, Hα is depressed at all radii. This suggests that at all masses the physical processes driving the enhancement or suppression of star formation act throughout the disks of galaxies. At high masses (1010.5 <M/M <1011), above the MS, Hα is particularly enhanced in the center, potentially building bulges and/or supermassive black holes. Below the MS, a strong central dip in the EW(Hα), as well as the inferred specific SFR, appears. Importantly, though, across the entirety of the SFR-M plane, the absolute SFR as traced by Hα is always centrally peaked, even in galaxies below the MS.

Original languageEnglish
Article number27
JournalAstrophysical Journal
Volume828
Issue number1
DOIs
Publication statusPublished - 1 Sep 2016

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star formation rate
Hubble Space Telescope
star formation
galaxies
stars
stellar mass
radii
ionized gases
erg
division
rate
dip
brightness
spatial resolution
assembly
cameras
time measurement
retarding
continuums
augmentation

Keywords

  • galaxies: evolution
  • galaxies: formation
  • galaxies: high-redshift
  • galaxies: star formation
  • galaxies: structure

Cite this

Nelson, E. J., Van Dokkum, P. G., Förster Schreiber, N. M., Franx, M., Brammer, G. B., Momcheva, I. G., ... Lange, J. U. (2016). Where stars form: Inside - out growth and coherent star formation from HSTHα maps of 3200 galaxies across the main sequence at 0.7 <z <1.5. Astrophysical Journal, 828(1), [27]. https://doi.org/10.3847/0004-637X/828/1/27

Where stars form : Inside - out growth and coherent star formation from HSTHα maps of 3200 galaxies across the main sequence at 0.7 <z <1.5. / Nelson, Erica June; Van Dokkum, Pieter G.; Förster Schreiber, Natascha M.; Franx, Marijn; Brammer, Gabriel B.; Momcheva, Ivelina G.; Wuyts, Stijn; Whitaker, Katherine E.; Skelton, Rosalind E.; Fumagalli, Mattia; Hayward, Christopher C.; Kriek, Mariska; Labbé, Ivo; Leja, Joel; Rix, Hans Walter; Tacconi, Linda J.; Van Der Wel, Arjen; Van Den Bosch, Frank C.; Oesch, Pascal A.; Dickey, Claire; Lange, Johannes Ulf.

In: Astrophysical Journal, Vol. 828, No. 1, 27, 01.09.2016.

Research output: Contribution to journalArticle

Nelson, EJ, Van Dokkum, PG, Förster Schreiber, NM, Franx, M, Brammer, GB, Momcheva, IG, Wuyts, S, Whitaker, KE, Skelton, RE, Fumagalli, M, Hayward, CC, Kriek, M, Labbé, I, Leja, J, Rix, HW, Tacconi, LJ, Van Der Wel, A, Van Den Bosch, FC, Oesch, PA, Dickey, C & Lange, JU 2016, 'Where stars form: Inside - out growth and coherent star formation from HSTHα maps of 3200 galaxies across the main sequence at 0.7 <z <1.5', Astrophysical Journal, vol. 828, no. 1, 27. https://doi.org/10.3847/0004-637X/828/1/27
Nelson, Erica June ; Van Dokkum, Pieter G. ; Förster Schreiber, Natascha M. ; Franx, Marijn ; Brammer, Gabriel B. ; Momcheva, Ivelina G. ; Wuyts, Stijn ; Whitaker, Katherine E. ; Skelton, Rosalind E. ; Fumagalli, Mattia ; Hayward, Christopher C. ; Kriek, Mariska ; Labbé, Ivo ; Leja, Joel ; Rix, Hans Walter ; Tacconi, Linda J. ; Van Der Wel, Arjen ; Van Den Bosch, Frank C. ; Oesch, Pascal A. ; Dickey, Claire ; Lange, Johannes Ulf. / Where stars form : Inside - out growth and coherent star formation from HSTHα maps of 3200 galaxies across the main sequence at 0.7 <z <1.5. In: Astrophysical Journal. 2016 ; Vol. 828, No. 1.
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abstract = "We present Hα maps at 1 kpc spatial resolution for star-forming galaxies at z ∼ 1, made possible by the Wide Field Camera 3 grism on Hubble Space Telescope (HST). Employing this capability over all five 3D-HST/CANDELS fields provides a sample of 3200 galaxies enabling a division into subsamples based on stellar mass and star formation rate (SFR). By creating deep stacked Hα images, we reach surface brightness limits of 1 × 10-18 erg s-1 cm-2 arcsec-2, allowing us to map the distribution of ionized gas to ∼10 kpc for typical L∗ galaxies at this epoch. We find that the spatial extent of the Hα distribution increases with stellar mass as rHα = 1.5 (M∗/1010 M⊙)0.23 kpc. The Hα emission is more extended than the stellar continuum emission, consistent with inside-out assembly of galactic disks. This effect grows stronger with mass as rHα/r∗ = 1.1(M∗/1010 M⊙)0.054. We map the Hα distribution as a function of SFR(IR+UV) and find evidence for {"}coherent star formation{"} across the SFR-M∗ plane: above the main sequence (MS), Hα is enhanced at all radii; below the MS, Hα is depressed at all radii. This suggests that at all masses the physical processes driving the enhancement or suppression of star formation act throughout the disks of galaxies. At high masses (1010.5 <M∗/M⊙ <1011), above the MS, Hα is particularly enhanced in the center, potentially building bulges and/or supermassive black holes. Below the MS, a strong central dip in the EW(Hα), as well as the inferred specific SFR, appears. Importantly, though, across the entirety of the SFR-M∗ plane, the absolute SFR as traced by Hα is always centrally peaked, even in galaxies below the MS.",
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AU - Nelson, Erica June

AU - Van Dokkum, Pieter G.

AU - Förster Schreiber, Natascha M.

AU - Franx, Marijn

AU - Brammer, Gabriel B.

AU - Momcheva, Ivelina G.

AU - Wuyts, Stijn

AU - Whitaker, Katherine E.

AU - Skelton, Rosalind E.

AU - Fumagalli, Mattia

AU - Hayward, Christopher C.

AU - Kriek, Mariska

AU - Labbé, Ivo

AU - Leja, Joel

AU - Rix, Hans Walter

AU - Tacconi, Linda J.

AU - Van Der Wel, Arjen

AU - Van Den Bosch, Frank C.

AU - Oesch, Pascal A.

AU - Dickey, Claire

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KW - galaxies: formation

KW - galaxies: high-redshift

KW - galaxies: star formation

KW - galaxies: structure

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