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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)
(End) Max Gronke [Oslo, Norway], Patricia Vannier [CDS] 25-Sep-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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