J/A+A/608/A139 237 Lyman-alpha spectra of MUSE-Wide survey (Gronke, 2017)
Modeling 237 Lyman-alpha spectra of the MUSE-Wide survey. Gronke M. <Astron. Astrophys. 608, A139 (2017)> =2017A&A...608A.139G (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, spectra ; Models Keywords: radiative transfer - galaxies: high-redshift - line: formation - line: profiles - scattering Abstract: We compare 237 Lyman-α (Lyα) spectra of the "MUSE-Wide survey" (Herenz et al., 2017, Cat. J/A+A/606/A12) to a suite of radiative transfer simulations consisting of a central luminous source within a concentric, moving shell of neutral gas, and dust. This six parameter shell-model has been used numerously in previous studies, however, on significantly smaller data-sets. We find that the shell-model can reproduce the observed spectral shape very well - better than the also common 'Gaussian-minus-Gaussian' model which we also fitted to the dataset. Specifically, we find that ∼94% of the fits possess a goodness-of-fit value of p(chi2)>0.1. The large number of spectra allows us to robustly characterize the shell-model parameter range, and consequently, the spectral shapes typical for realistic spectra. We find that the vast majority of the Lyα spectral shapes require an outflow and only ∼5% are well-fitted through an inflowing shell. In addition, we find ∼46% of the spectra to be consistent with a neutral hydrogen column density <1017cm-2 -- suggestive of a non-negligible fraction of continuum leakers in the MUSE-Wide sample. Furthermore, we correlate the spectral against the Lyα halo properties against each other but do not find any strong correlation. Description: Shell-model parameters of the 237 Lyα spectra presented in the first instalment of the MUSE-Wide survey (Herenz et al., 2017, Cat. J/A+A/606/A12). For each spectrum, the MUSE UNIQUE ID, the p(chi2) value of the best fit, and the six shell-model parameters (plus their uncertainty) are given. In particular, for each parameter, the (16,50,84)th percentiles of the likelihood are outputted. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file sm-fits.dat 305 237 *Shell-model parameters
Note on sm-fits.dat: Suffixes -16, -50, -84 indicate the 16th, 50th and 84th percentiles of the posterior, respectively.
See also: J/A+A/606/A12 : MUSE-Wide survey: 831 emission line galaxies (Herenz+, 2017) Byte-by-byte Description of file: sm-fits.dat
Bytes Format Units Label Explanations
1- 9 I9 --- MUSE MUSE UNIQUE ID 11- 26 F16.11 km/s Dv-16 16th percentile of intrinsic shift 28- 46 F19.14 km/s Dv-50 Intrinsic shift 48- 63 F16.11 km/s Dv-84 84th percentile of intrinsic shift 65- 77 F13.10 [cm-2] logNHI-16 16th percentile of shell column density (1) 79- 91 F13.10 [cm-2] logNHI-50 Shell column density (1) 93-105 F13.10 [cm-2] logNHI-84 84th percentile of shell column density (1) 107-119 F13.11 [K] logT-16 16th percentile of effective temperature of shell (1) 121-133 F13.11 [K] logT-50 Effective temperature of shell (1) 135-147 F13.11 [K] logT-84 84th percentile of effective temperature of shell (1) 149-162 F14.10 km/s sigmai-16 16th percentile of intrinsic width of Lyα line 164-177 F14.10 km/s sigmai-50 Intrinsic width of Lya line 179-192 F14.10 km/s sigmai-84 84th percentile of intrinsic width of Lyα line 194-207 F14.12 --- taud-16 16th percentile of (absorbing) dust optical detph 209-222 F14.12 --- taud-50 (absorbing) dust optical detph 224-237 F14.12 --- taud-84 84th percentile of (absorbing) dust optical detph 239-254 F16.11 km/s vexp-16 16th percentile of expansion velocity 256-271 F16.11 km/s vexp-50 Expansion velocity (2) 273-287 F15.10 km/s vexp-84 84th percentile of expansion velocity 289-305 E17.15 --- Pchi2 p(chi^2) of the best fit
Note (1): log stands for the logarithm with base 10 Note (2): Negative values stand for inflow.
Acknowledgements: Max Gronke, maxbg(at)astro.uio.no
(End) Max Gronke [Oslo, Norway], Patricia Vannier [CDS] 25-Sep-2017
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