2019MNRAS.488..706H -
Mon. Not. R. Astron. Soc., 488, 706-719 (2019/September-1)
Constraining Lyman-alpha spatial offsets at 3 < z < 5.5 from VANDELS slit spectroscopy.
HOAG A., TREU T., PENTERICCI L., AMORIN R., BOLZONELLA M., BRADAC M., CASTELLANO M., CULLEN F., FYNBO J.P.U., GARILLI B., GUAITA L., HATHI N., HENRY A., JONES T., MASON C., McLEOD D., McLURE R., MORISHITA T., POZZETTI L., SCHAERER D., SCHMIDT K.B., TALIA M. and THOMAS R.
Abstract (from CDS):
We constrain the distribution of spatially offset Lyman-alpha emission (Ly α) relative to rest-frame ultraviolet emission in ∼300 high redshift (3 < z < 5.5) Lyman-break galaxies (LBGs) exhibiting Ly α emission from VANDELS, a VLT/VIMOS slit-spectroscopic survey of the CANDELS Ultra Deep Survey and Chandra Deep Field South fields (≃0.2 deg2 total). Because slit spectroscopy only provides one spatial dimension, we use Bayesian inference to recover the underlying two-dimensional Ly α spatial offset distribution. We model the distribution using a two-dimensional circular Gaussian, defined by a single parameter σ_r,Ly α_, the standard deviation expressed in polar coordinates. Over the entire redshift range of our sample (3 < z < 5.5), we find σr,Lyα=1.70+0.09–0.08 kpc (68per cent conf.), corresponding to ∼0′′.25 at <z> = 4.5. We also find that σ_r,Ly α_ decreases significantly with redshift. Because Ly α spatial offsets can cause slit losses, the decrease in σ_r,Ly α_ with redshift can partially explain the increase in the fraction of Ly α emitters observed in the literature over this same interval, although uncertainties are still too large to reach a strong conclusion. If σ_r,Ly α_ continues to decrease into the reionization epoch, then the decrease in Ly α transmission from galaxies observed during this epoch might require an even higher neutral hydrogen fraction than what is currently inferred. Conversely, if spatial offsets increase with the increasing opacity of the intergalactic medium, slit losses may explain some of the drop in Ly α transmission observed at z > 6. Spatially resolved observations of Ly α and UV continuum at 6 < z < 8 are needed to settle the issue.
NAME Chandra Deep Field-South
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ra dec : right ascension and declination (unit and frame defined according to your Output Options)
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[error ellipse] : measurement uncertainty, on (ra,dec) if the positional angle is 90 degrees, on (majaxis,minaxis) otherwise (in mas at defined epoch in the original catalogue),
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Syntax of coordinates is : "ra dec (wtype) [error ellipse] quality bibcode" :
ra dec : right ascension and declination (unit and frame defined according to your Output Options)
Grey values are increasing the original precision due to the computation of frame transformations
(wtype) : wavelength class for the origin of the coordinates (Rad, mm, IR, Optical, UV, Xray, Gam)
[error ellipse] : measurement uncertainty, on (ra,dec) if the positional angle is 90 degrees, on (majaxis,minaxis) otherwise (in mas at defined epoch in the original catalogue),
position angle (in degrees North celestial pole to East)
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03 30 22.4 -27 58 35
[
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Syntax of coordinates is : "ra dec (wtype) [error ellipse] quality bibcode" :
ra dec : right ascension and declination (unit and frame defined according to your Output Options)
Grey values are increasing the original precision due to the computation of frame transformations
(wtype) : wavelength class for the origin of the coordinates (Rad, mm, IR, Optical, UV, Xray, Gam)
[error ellipse] : measurement uncertainty, on (ra,dec) if the positional angle is 90 degrees, on (majaxis,minaxis) otherwise (in mas at defined epoch in the original catalogue),
position angle (in degrees North celestial pole to East)
quality : flag of quality
E ≥ 10"
D : 1-10" (and some old data)
C : 0.1-1"
B : 0.01-0.1" + 2MASS, Tyc
A : VLBI, Hipparcos
bibcode : bibcode of the coordinates reference
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223.5732 -54.4374
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15.84 15.84 ~ (~) D
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