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23 results for “emission lines”
The [CII] 158 μm line emission in high-redshift galaxies: Data Set
<p>This data set contains all data tables associated to the publication: "The [CII] 158 μm line emission in high-redshift galaxies"; A&A Lagache, Cousin, Chatzikos 2018. Please cite it if you use those data.</p>
Emission line models for the lowest mass core-collapse supernovae - I. Case study of a 9 M⊙ one-dimensional neutrino-driven explosion
<p>Model spectra of the 9 Msun iron-core model, and the pure H toy model, 200-600d. Distance 10 Mpc assumed.</p>
What can we learn about transients from the 21 cm line emission in their environments?
<p>I present the result of an observational campaign to map the 21 cm atomic hydrogen line in host galaxies of supernovae (SNe), long gamma-ray bursts (GRBs), and fast radio bursts (FRBs). For all analysed hosts of type Ic-BL SNe and GRBs we found off-centre gas concentrations close to the GRB/SN positions and irregular velocity fields. This suggests a recent gas inflow. This is consistent with GRB/SN progenitors being born when a galaxy accretes metal-poor gas from the intergalactic medium, and opens a possibility to use GRB/SN hosts to study gas accretion. This supports a very massive model for their progenitors. Similarly, the host galaxies of FRBs exhibit very asymmetric 21 cm lines, suggesting a connection between the birth of FRB progenitors and galaxy interactions. On the other hand, the host galaxy of the unusual transient AT 2018cow (the first fast blue optical transient, FBOT) does not exhibit such features, which suggests that its progenitor may not have been a massive star. </p>
Data from "CO Line Emission Surfaces and Vertical Structure in Mid-Inclination Protoplanetary Disks"
<p>CO line emission image cubes ("[DISK]_CO_cube.fits"), line+continuum image cubes ("[DISK]_CO_cube_wcont.fits"), and zeroth moment maps ("[DISK]_CO_M0.fits") associated with Law et al., 2022, "CO Line Emission Surfaces and Vertical Structure in Mid-Inclination Protoplanetary Disks," The Astrophysical Journal</p> <p>CO line emission image cubes from the DSHARP ALMA Large Program (for HD 142666, MY Lup, GW Lup, WaOph 6, DoAr 25) can be found at: https://bulk.cv.nrao.edu/almadata/lp/DSHARP/ and are not included here.</p> <p>The raw data are available on the ALMA archive (see Table 1 in the paper for a listing of the relevant ALMA project codes).</p>
Paranal Airglow Line And Continuum Emission (PALACE) model: data and code of v1.0
<p>This data and code release is related to the article "PALACE v1.0: Paranal Airglow Line And Continuum Emission model", which has been published in Geoscientific Model Development, Vol. 18, 2025 (https://doi.org/10.5194/gmd-18-4353-2025).<br>The release consists of three .zip files:<br>PMD.zip: 436 ASCII files with data that were used to build and evaluate the model. More details in PMD/pmd_README.txt.<br>PALACE.zip: Python/Cython code for the calculation of the model. More details in PALACE/README.txt.<br>test.zip: Test output of the code for the default parameters (.dat file in alternative ASCII format).</p>
The nebular spectra of SN 2012aw and constraints on stellar nucleosynthesis from oxygen emission lines
<p>Spectral models of M_ZAMS = 12, 15, 19, 25 Msun progenitors, all epochs.</p>
Data for the paper "Effective Emission Heights of Various OH Lines From X-shooter and SABER Observations of a Passing Quasi-2-Day Wave"
<p>The provided ASCII tables are related to the paper "Effective Emission Heights of Various OH Lines From X-shooter and SABER Observations of a Passing Quasi-2-Day Wave", which has been published in Journal of Geophysical Research: Atmospheres, Vol. 127, 2022 (DOI: 10.1029/2022JD036610).</p>
Data from "Mapping Protoplanetary Disk Vertical Structure with CO Isotopologue Line Emission"
<p>CO isotopologue line emission image cubes ("[DISK]_[LINE]_cube.fits"), line+continuum image cubes ("[DISK]_[LINE]_cube_wcont.fits"), and zeroth moment maps ("[DISK]_[LINE]_M0.fits") associated with Law et al., 2023, "Mapping Protoplanetary Disk Vertical Structure with CO Isotopologue Line Emission," The Astrophysical Journal</p> <p>The raw data are available on the ALMA archive (see Table 2 in the paper for a listing of the relevant ALMA project codes).</p>
Synthetic Emission Line Catalog and High-Resolution SEDs for SPHEREx Galaxy Simulations
<p><strong>Overview:</strong></p> <p>This repository contains the synthetic galaxy models derived from multi-wavelength photometry in the COSMOS field (166k galaxies over 1.27 sq. deg., 18 < i < 25) and from the GAMA survey (44k galaxies over 217 sq. deg., i < 18). These encompass a representative sample of galaxies SPHEREx will observe, and should be applicable for other surveys as well.</p> <ul> <li>Synthetic emission line strengths in the rest-frame optical/near-infrared (H-alpha, H-beta, Paschen-alpha, [OIII], [OII], [NII], [SII])</li> <li>High-resolution SEDs (0.1 - 8 micron), which are produced by 1) fitting a library of 160 galaxy templates to multi-band photometry and 2) inserting emission lines with strengths predicted by an empirical model that depends on galaxy type, redshift and stellar mass.</li> </ul> <p>These products were made using the modeling framework <strong>C</strong>onditional <strong>LI</strong>ne <strong>P</strong>ainting on <strong>S</strong>ynthetic <strong>S</strong>pectra (<em>CLIPonSS</em>), the details of which are summarized in Feder+2023b (<a href="https://arxiv.org/abs/2312.04636">arXiv link here</a>). The synthetic emission line catalog is validated against a variety of LF measurements, line ratio trends and direct line comparisons. </p> <p><strong>Data description:</strong></p> <p><em><strong>High-resolution SEDs</strong></em>: The SEDs are stored in .FITS files, for which each galaxy SED has its own Header Data Unit (HDU). This format was chosen due to the fact that the wavelength sampling for the 160 galaxy empirical and model-based templates varies, i.e., we do not perform any interpolation onto a homogenized wavelength grid. In cases where emission lines are added but the continuum template resolution is coarse, the resolution is increased in the vicinity of the emission line(s) to adequately sample the line profiles. Each galaxy's HDU is indexed by its Farmer ID (for COSMOS) or alternatively its uberID (GAMA). The COSMOS SEDs are split into three files for relative ease of access, while the GAMA sources are all in one file.</p> <p><em><strong>Emission line catalogs:</strong></em> The emission line catalogs are stored in .csv format with the following information:</p> <p>Tractor_ID (or uberID) [integer]: Unique identifier for each source</p> <p>RA/DEC [float, in degrees]: Celestial coordinates</p> <p>imag [AB]: i-band magnitude</p> <p>mass_best [float]: log-stellar masses estimated through SED fitting process</p> <p>ebv [float]: Galaxy intrinsic dust extinction (ranging from ebv=0 to 1)</p> <p>redshift [float]: Best-fit redshift from COSMOS2020 (GAMA) catalogs</p> <p>bfit_tid [integer]: Best fit template ID from library of templates</p> <p>dustlaw [integer]: Best fit dust law (1=Prevot, 2=Calzetti, 3=Seaton, 4=Allen, 5=Fitzpatrick)</p> <p>L_{line} [float, erg s-1]: Line luminosities from empirical model</p> <p>F_{line} [float, erg cm-2 s-1]: Line fluxes from empirical model</p> <p>ew_ha [float, Angstrom]: Equivalent width of H-alpha from empirical model</p> <p><strong><em>Fitting templates: </em></strong>We include the 31 model-based templates and 129 empirical templates from Brown+2014. In the Brown templates we have removed any relevant lines that were directly measured in the initial spectra, however we do not fit for/remove PAH features. These can serve as the basis for other empirically based galaxy simulations with different emission line prescriptions.</p> <p>Any questions regarding the use of these data products or related issues can be directed to Richard Feder (link to <a href="https://richardfeder.github.io/">personal website</a>). </p> <p> </p>
Database of emission lines
Open the record for dataset details and reuse information.
CO emission line spectra of the detected IRAM 30m CO-CAVITY galaxies.
<p>Figures show the observed spectra of the CO(1-0) and CO(2-1) emission lines of the CO-CAVITY galaxies.</p>
F-18 16 Alpha-Fluoroestradiol-Labeled Positron Emission Tomography in Predicting Response to First-Line Hormone Therapy in Patients With Stage IV Breast Cancer
ClinicalTrials.gov study NCT00602043. IPD Sharing: Not stated. Countries: 1. Publications: 1.
Evaluating the feasibility of using downwind methods to quantify point source oil and gas emissions using continuous monitoring fence-line sensors
Open the record for dataset details and reuse information.
Tables of Emission Line Spectra discovered by Active Deep Learning in LAMOST DR2
<p>Tables of emission line spectra discovered by Active Deep Learning in LAMOST DR2 spectra survey. These are referred to in an article Škoda,Podsztavek&Tvrdík "Active deep learning method for the discovery of objects of interest in large spectroscopic surveys" submitted to Astronomy and Astrophysics.</p> <p>The zipped files contain both CSV and VOTable formats, the HTML version may be opened directly in a browser. A link to an interactive spectrum plot at Strasbourg datacenter (CDS) Vizier archive may be activated from it as well in most common browsers.</p> <p>The detailed description of tables is in attached README file.</p>
AGN and stellar spectra used to produce model molecular emission lines
<p><span>Aiming to investigate the effects of stellar and AGN radiation fields to the excitation of molecular gas, we present an analysis of model CO, H</span><span><sub>2</sub>O, and OH<sup>+</sup> emission lines produced with the application of these radiation fields using MOLPOP-CEP. We find that the ratios of CO(J<sub>upp</sub>) = 11, 12, 13, 14, 15) to CO(J<sub>upp</sub>) = 1, 2, 3, 4, 5, 6, 7, 8) obtained with the application of AGN radiation are larger than the ones produced by applying stellar radiation. Similarly, some H<sub>2</sub>O and </span><span>OH<sup>+</sup> ratios obtained with AGN radiation are found to be higher than the corresponding ratios produced by applying stellar radiation field, making the line ratios a diagnostic tool to disentangle AGN from star formation. In all cases, we find that the ratios vary as a function of the molecular gas density and the scale of the radiation field, the larger the scale of the radiation field is the stronger the excitation of the molecular transitions. Also, the effect of the radiation fields is found to be dependent on the molecular gas density, indicating that the effect of the radiation fields is regulated by the physical properties that are intrinsic to the molecular gas. Thus, due to the dependency of the line ratios on the scale of the radiation fields and the effect of the radiation fields on the molecular gas density, we conclude that it is not sufficient to use a single line ratio to claim the presence of AGN contribution to the molecular gas excitation.</span></p>
ALMA detection of CO rotational line emission in red supergiant stars of the massive young star cluster RSGC1
<p>Input files and data for the MESA simulations in the paper "ALMA detection of CO rotational line emission in red supergiant stars of the massive young star cluster RSGC1". Runs where performed with version r23.05.1 of the MESA code using the MESA SDK version x86_64-linux-22.6.1. Folder named "Decin" contains the simulation with the new mass loss rate described in the paper, while the folder named NdJ contains the input files for the simulation performed with the Nieuwenhuijzen & de Jager rates.</p>
AGN and stellar spectra used to produce model molecular emission lines
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Supplementary material "Diagnosing the interstellar medium of galaxies with far-infrared emission lines I. The [C II] 158 μm line at z ∼ 0"
<p>Repository with supplementary material to the paper: "Diagnosing the interstellar medium of galaxies with far-infrared emission lines I. The [C II] 158 μm line at z ∼ 0" published in Astronomy & Astrophysics.</p> <p>It contains the final datasets of luminosity predictions for the [C II] luminosity in the different EAGLE galaxies.</p>
Corner plots of MgII emission line fits for z~6 quasars
<p>Corner plots for the MgII emission line fits for ten z~6 quasars shown in Fig. 10 from this paper: https://ui.adsabs.harvard.edu/abs/2020arXiv200201811E/abstract. Model parameters and fitting procedure are described in section 4.2.</p>
Quantifying the informativity of emission lines to infer physical conditions in giant molecular clouds
<p>Supplementary figures for Einig et al (2024).</p>
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