Sizes of LYα-emitting galaxies and their rest-frame ultraviolet components at z = 3.1

Nicholas A. Bond, Eric Gawiser, Caryl Gronwall, Robin Ciardullo, Martin Altmann, Kevin Schawinski

Research output: Contribution to journalArticle

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Abstract

We present a rest-frame ultraviolet analysis of ∼ 120 z ∼3.1 Lyman Alpha Emitters (LAEs) in the Extended Chandra Deep Field South. Using Hubble Space Telescope (HST) images taken as part of the Galaxy Evolution From Morphology and SEDS (GEMS) survey, Great Observatories Origins Deep Survey (GOODS), and Hubble Ultradeep Field surveys, we analyze the sizes of LAEs, as well as the spatial distribution of their components, which are defined as distinct clumps of UV-continuum emission. We set an upper limit of ∼1 kpc (∼0″.1) on the rms offset between the centroids of the continuum and Lyα emission. The SFRs of LAE components inferred from the rest-frame ultraviolet continuum range from ∼0.1 M yr-1 to ∼5 M yr-1. A subsample of LAEs with coverage in multiple surveys (at different imaging depths) suggests that one needs a signal-to-noise ratio, S/N ≳30, in order to make a robust estimate of the half-light radius of an LAE system. The majority of LAEs have observed half-light radii ≲2 kpc, and LAE components typically have observed half-light radii ≲1.5 kpc (≲020). Although only 50% of the detected LAE components are resolved at GOODS depth, the brightest (V ≲ 26.3) are all resolved in both GOODS and GEMS. Since we find little evidence for a correlation between the rest-UV sizes and magnitudes of LAEs, the majority should be resolved in a deeper survey at the 005 angular resolution of the HST. Most of the multi-component LAEs identified in shallow frames become connected in deeper images, suggesting that the majority of the rest-UV "clumps" are individual star-forming regions within a single system.

Original languageEnglish (US)
Pages (from-to)639-649
Number of pages11
JournalAstrophysical Journal
Volume705
Issue number1
DOIs
StatePublished - Jan 1 2009

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emitters
galaxies
observatory
observatories
clumps
continuums
Hubble Space Telescope
radii
signal-to-noise ratio
field survey
spatial distribution
angular resolution
centroids
signal to noise ratios
stars
estimates

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Keywords

  • Cosmology: Observations
  • Galaxies: Formation
  • Galaxies: High-redshift
  • Galaxies: Structure

Cite this

Bond, Nicholas A. ; Gawiser, Eric ; Gronwall, Caryl ; Ciardullo, Robin ; Altmann, Martin ; Schawinski, Kevin. / Sizes of LYα-emitting galaxies and their rest-frame ultraviolet components at z = 3.1. In: Astrophysical Journal. 2009 ; Vol. 705, No. 1. pp. 639-649.
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abstract = "We present a rest-frame ultraviolet analysis of ∼ 120 z ∼3.1 Lyman Alpha Emitters (LAEs) in the Extended Chandra Deep Field South. Using Hubble Space Telescope (HST) images taken as part of the Galaxy Evolution From Morphology and SEDS (GEMS) survey, Great Observatories Origins Deep Survey (GOODS), and Hubble Ultradeep Field surveys, we analyze the sizes of LAEs, as well as the spatial distribution of their components, which are defined as distinct clumps of UV-continuum emission. We set an upper limit of ∼1 kpc (∼0″.1) on the rms offset between the centroids of the continuum and Lyα emission. The SFRs of LAE components inferred from the rest-frame ultraviolet continuum range from ∼0.1 M ⊙ yr-1 to ∼5 M ⊙ yr-1. A subsample of LAEs with coverage in multiple surveys (at different imaging depths) suggests that one needs a signal-to-noise ratio, S/N ≳30, in order to make a robust estimate of the half-light radius of an LAE system. The majority of LAEs have observed half-light radii ≲2 kpc, and LAE components typically have observed half-light radii ≲1.5 kpc (≲020). Although only 50{\%} of the detected LAE components are resolved at GOODS depth, the brightest (V ≲ 26.3) are all resolved in both GOODS and GEMS. Since we find little evidence for a correlation between the rest-UV sizes and magnitudes of LAEs, the majority should be resolved in a deeper survey at the 005 angular resolution of the HST. Most of the multi-component LAEs identified in shallow frames become connected in deeper images, suggesting that the majority of the rest-UV {"}clumps{"} are individual star-forming regions within a single system.",
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Sizes of LYα-emitting galaxies and their rest-frame ultraviolet components at z = 3.1. / Bond, Nicholas A.; Gawiser, Eric; Gronwall, Caryl; Ciardullo, Robin; Altmann, Martin; Schawinski, Kevin.

In: Astrophysical Journal, Vol. 705, No. 1, 01.01.2009, p. 639-649.

Research output: Contribution to journalArticle

TY - JOUR

T1 - Sizes of LYα-emitting galaxies and their rest-frame ultraviolet components at z = 3.1

AU - Bond, Nicholas A.

AU - Gawiser, Eric

AU - Gronwall, Caryl

AU - Ciardullo, Robin

AU - Altmann, Martin

AU - Schawinski, Kevin

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N2 - We present a rest-frame ultraviolet analysis of ∼ 120 z ∼3.1 Lyman Alpha Emitters (LAEs) in the Extended Chandra Deep Field South. Using Hubble Space Telescope (HST) images taken as part of the Galaxy Evolution From Morphology and SEDS (GEMS) survey, Great Observatories Origins Deep Survey (GOODS), and Hubble Ultradeep Field surveys, we analyze the sizes of LAEs, as well as the spatial distribution of their components, which are defined as distinct clumps of UV-continuum emission. We set an upper limit of ∼1 kpc (∼0″.1) on the rms offset between the centroids of the continuum and Lyα emission. The SFRs of LAE components inferred from the rest-frame ultraviolet continuum range from ∼0.1 M ⊙ yr-1 to ∼5 M ⊙ yr-1. A subsample of LAEs with coverage in multiple surveys (at different imaging depths) suggests that one needs a signal-to-noise ratio, S/N ≳30, in order to make a robust estimate of the half-light radius of an LAE system. The majority of LAEs have observed half-light radii ≲2 kpc, and LAE components typically have observed half-light radii ≲1.5 kpc (≲020). Although only 50% of the detected LAE components are resolved at GOODS depth, the brightest (V ≲ 26.3) are all resolved in both GOODS and GEMS. Since we find little evidence for a correlation between the rest-UV sizes and magnitudes of LAEs, the majority should be resolved in a deeper survey at the 005 angular resolution of the HST. Most of the multi-component LAEs identified in shallow frames become connected in deeper images, suggesting that the majority of the rest-UV "clumps" are individual star-forming regions within a single system.

AB - We present a rest-frame ultraviolet analysis of ∼ 120 z ∼3.1 Lyman Alpha Emitters (LAEs) in the Extended Chandra Deep Field South. Using Hubble Space Telescope (HST) images taken as part of the Galaxy Evolution From Morphology and SEDS (GEMS) survey, Great Observatories Origins Deep Survey (GOODS), and Hubble Ultradeep Field surveys, we analyze the sizes of LAEs, as well as the spatial distribution of their components, which are defined as distinct clumps of UV-continuum emission. We set an upper limit of ∼1 kpc (∼0″.1) on the rms offset between the centroids of the continuum and Lyα emission. The SFRs of LAE components inferred from the rest-frame ultraviolet continuum range from ∼0.1 M ⊙ yr-1 to ∼5 M ⊙ yr-1. A subsample of LAEs with coverage in multiple surveys (at different imaging depths) suggests that one needs a signal-to-noise ratio, S/N ≳30, in order to make a robust estimate of the half-light radius of an LAE system. The majority of LAEs have observed half-light radii ≲2 kpc, and LAE components typically have observed half-light radii ≲1.5 kpc (≲020). Although only 50% of the detected LAE components are resolved at GOODS depth, the brightest (V ≲ 26.3) are all resolved in both GOODS and GEMS. Since we find little evidence for a correlation between the rest-UV sizes and magnitudes of LAEs, the majority should be resolved in a deeper survey at the 005 angular resolution of the HST. Most of the multi-component LAEs identified in shallow frames become connected in deeper images, suggesting that the majority of the rest-UV "clumps" are individual star-forming regions within a single system.

KW - Cosmology: Observations

KW - Galaxies: Formation

KW - Galaxies: High-redshift

KW - Galaxies: Structure

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