J/MNRAS/471/267 Lyα fluxes of HDFS 2.91<z<6.64 sources (Drake+, 2017)
MUSE deep-fields: the Ly α luminosity function in the
Hubble Deep Field-South at 2.91 < z < 6.64.
Drake A.B., Guiderdoni B., Blaizot J., Wisotzki L., Herenz E.C., Garel T.,
Richard J., Bacon R., Bina D., Cantalupo S., Contini T., Den Brok M.,
Hashimoto T., Marino R.A., Pello R., Schaye J., Schmidt K.B.
<Mon. Not. R. Astron. Soc., 471, 267-278 (2017)>
=2017MNRAS.471..267D 2017MNRAS.471..267D (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, spectra ; Redshifts ; H I data
Keywords: surveys - galaxies: evolution - galaxies: formation -
galaxies: high-redshift -
galaxies: luminosity functions, mass function -
cosmology: observations
Abstract:
We present the first estimate of the Lyα luminosity function
using blind spectroscopy from the Multi Unit Spectroscopic Explorer,
MUSE, in the Hubble Deep Field-South. Using automatic source-detection
software, we assemble a homogeneously detected sample of 59 Lyα
emitters covering a flux range of -18.0<log10(F)←16.3(erg/s/cm2),
corresponding to luminosities of 41.4<log10(L)<42.8(erg/s). As
recent studies have shown, Lyα fluxes can be underestimated by
a factor of 2 or more via traditional methods, and so we undertake a
careful assessment of each object's Lyα flux using a
curve-of-growth analysis to account for extended emission. We describe
our self-consistent method for determining the completeness of the
sample, and present an estimate of the global Ly α luminosity
function between redshifts 2.91<z<6.64 using the 1/Vmax estimator.
We find that the luminosity function is higher than many number
densities reported in the literature by a factor of 2-3, although our
result is consistent at the 1σ level with most of these studies.
Our observed luminosity function is also in good agreement with
predictions from semi-analytic models, and shows no evidence for
strong evolution between the high- and low-redshift halves of the
data. We demonstrate that one's approach to Lyα flux estimation
does alter the observed luminosity function, and caution that accurate
flux assessments will be crucial in measurements of the faint-end
slope. This is a pilot study for the Lyα luminosity function in
the MUSE deep-fields, to be built on with data from the Hubble Ultra
Deep Field that will increase the size of our sample by almost a
factor of 10.
Description:
During the final MUSE commissioning run in 2014 July, we performed a
deep integration on the HDFS for a total of 27h, using the standard
wavelength range 4750-9300Å.
We use a new reduction of the cube optimized for the detection of
faint emission-line objects.
We therefore choose to implement a single method of source detection
allowing us to apply homogeneous selection criteria across the field,
and to apply these same criteria in our fake source recovery
experiment.
Our chosen software, 'MUSELET' (J. Richard), has been optimized
for the detection of line emission, and has been extensively tested on
both blank and cluster fields.
We apply this method to Bacon et al. (2015, J/A+A/575/A75) sources.
We present the 59 objects detected automatically with MUSELET.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 74 59 Various flux estimates for all 59 objects
detected automatically with MUSELET
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See also:
J/A+A/575/A75 : MUSE 3D view of HDF-S (Bacon+, 2015)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- ID ID of the object in Bacon et al. (2015,
J/A+A/575/A75), [BBR2015] NNN in Simbad
5- 12 F8.4 deg RAdeg MUSELET right ascension (J2000)
14- 21 F8.4 deg DEdeg MUSELET declination (J2000)
23- 29 F7.2 0.1nm lambdaObs Peak wavelength of MUSELET's detection
31- 34 F4.2 --- zLya Lyα redshifts
36- 40 F5.2 10-21W/m2 FluxB15 Lyα Flux from Bacon et al. (2015,
Cat. J/A+A/575/A75)
42- 46 F5.2 10-21W/m2 FluxW16 ?=- Lyα Flux from Wisotzki
(2016A&A...587A..98W 2016A&A...587A..98W)
48- 52 F5.2 10-21W/m2 Flux2 This work 2 arcsec aperture Lyα
flux estimate
54- 57 F4.2 10-21W/m2 e_Flux2 rms uncertainty on Flux2
59- 63 F5.2 10-21W/m2 FluxCoG Curve of growth Lyα flux estimate
from this work
65- 69 F5.2 10-21W/m2 e_FluxCoG rms uncertainty on FluxCoG
71- 74 F4.2 arcsec Diam Diameter of the aperture within which we
make the flux measurement in the
curve-of-growth analysis
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 15-May-2020