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9 results for “Young stellar objects”
Confusion matrices for theoretical young stellar object models
<p>This is a data table supplementing the following publication: </p> <p><em><strong>A framework for modeling the evolution of young stellar objects </strong></em>(Richardson et al. 2025, accepted to ApJ).</p> <p>It contains a set of confusion matrices comparing the evolutionary stages and classes of radiative transfer YSO models selected by proximity to protostellar evolutionary tracks. Models are included in a matrix based on their correspondence to particular modeled accretion histories, zero-age stellar masses, ages, mass accretion efficiencies, and levels of detectability (defined using flux in the ALMA Band 6 wavelength range). Details on the construction and use of the table are contained in the accompanying README file, and more information about the matrices is contained in Section 4.2 of the companion paper.</p> <p>The YSO models populating these matrices are from Richardson et al. (2024); information on them is contained in the <a href="https://ui.adsabs.harvard.edu/abs/2024ApJ...961..188R/abstract" target="_blank" rel="noopener">companion work</a> and <a href="https://zenodo.org/records/10522816" target="_blank" rel="noopener">data release</a>.</p>
An updated modular set of synthetic spectral energy distributions for young stellar objects
<p>These are the models released with the following publication:</p> <p><strong><em>An updated modular set of synthetic spectral energy distributions for young stellar objects</em></strong> (<a href="https://ui.adsabs.harvard.edu/abs/2024ApJ...961..188R/abstract" target="_blank" rel="noopener">Richardson et al. 2024</a>).</p> <p>This is a set of young stellar object (YSO) models with associated spectral energy distributions (SEDs) calculated through radiative transfer. It is a significant update to the data published alongside Robitaille (2017, R17). It contains the parameters shaping each model and adds the newly calculated parameters of envelope mass, average dust temperature, disk stability, and line-of-sight extinction. It also makes explicit quantities, such as source luminosity, that were left implicit in the previous release. This set also convolves the SEDs with several new filters, primarily those on the James Webb Space Telescope, and adds a script to facilitate convolution of these models with additional filters as desired by users. All data included in Version 1.1 of the R17 set (the most recent) are included here.</p> <p>Like their predecessors, these models are versioned. Updates will be released as more models are completed or other changes are made.</p> <p>Files unzip to r+24_models-{version}/{geometry}. "files.tar.gz" contains scripts for SED convolution and main sequence comparison, the opacity to absorption of dust used in the radiative transfer calculations, main sequence T/L values used for results in the accompanying work, and reference material for the contents of the dataset and latest version.</p> <p>The primary use of these models is as templates for SED fitting. The R17 models were structured for use with the <a href="https://sedfitter.readthedocs.io/en/stable/" target="_blank" rel="noopener">sedfitter</a> python package, which enables fitting and analysis of the fit results. For a version of sedfitter which accommodates the new additions, use <a href="https://github.com/richardson-t/sedfitter/tree/dev" target="_blank" rel="noopener">this fork</a>.</p>
JWST convolutions for a modular set of synthetic SEDs for young stellar objects (Robitaille, 2017)
<p>This is a companion to the models released alongside the publication:</p> <p><em>A modular set of synthetic spectral energy distributions for young stellar objects</em>, Robitaille (2017)</p> <p>The models are convolved with JWST filters taken from the SVO’s filter profile service. Some models with rotationally flattened envelopes (i.e. geometries with<strong> u</strong>)<strong> </strong>not present in the original model grid have since been completed; their convolved SEDs are included here.</p> <p>Files unzip to {geometry}/convolved/JWST/{SVO_filtername}.fits.</p> <p>This is a subset of the information included in https://doi.org/10.5281/zenodo.8114592.</p>
A modular set of synthetic spectral energy distributions for young stellar objects - Robitaille (2017) - v1.1 [Hyperion files]
<p>These are the input and output files for the radiative transfer code (Hyperion) for the model sets presented in</p> <p><em>A modular set of synthetic spectral energy distributions for young stellar objects</em>, Robitaille (2017)</p> <p>Each model set is provided as a single tar file. Each tar file expands to <strong>grids-1.1/<set name></strong>, so if you expand all tar files in the same folder, you will end up with a single <strong>grids-1.1</strong> folder with 18 sub-folders, one for each model set.</p> <p>For a given model set, the files are as follows:</p> <ul> <li>grids-1.1/<set name>/input - input Hyperion files</li> <li>grids-1.1/<set name>/log - log files from Hyperion</li> <li>grids-1.1/<set name>/output - output Hyperion files</li> <li>grids-1.1/<set name>/par - parameters for each model</li> <li>grids-1.1/<set name>/ranges.conf - ranges of parameters varied in the model set</li> <li>grids-1.1/<set name>/parameters.hdf5 - table of parameters for all models</li> <li>grids-1.1/<set name>/d03_5.5_3.0_A_sub.hdf5 - dust file used for the models</li> </ul> <p>Given the large number of models for some of the model sets, the models are not all stored directly inside the par, input, output or log directories - instead these directories contain folders formed from the first two characters (forced to lowercase) of the names of the models they contain. For example, a3 contains all models whose name starts with a3 or A3. This was done to avoid having too many files in a single folder which can cause issues on certain file systems.</p> <p>For the Hyperion input and output files, in some cases an _sed file is present. In these cases, the output SEDs (and polarization spectra) should be read from the _sed file, not the original output file. This is the case for all models that are in a set for which the ambient medium was present, as described in §4.2.3 of Robitaille (2017). Furthermore, in some cases the SED file is called _sed_noscat to indicate that scattering was not included, as described in §5.1 of Robitaille (2017).</p> <p>To avoid taking up too much disk space, the Hyperion HDF5 input/output files use external links to refer to each other and to the dust file. To make sure the links work, you should do all operations with the input/output files from the directory containing <strong>grids-1.1</strong>. For example, to open a Hyperion output file, you would need to do (in Python):</p> <p> In [1]: from hyperion.model import ModelOutput</p> <p> In [2]: mo = ModelOutput('grids-1.1/s---s-i/output/a3/A3kQmQtj.rtout')</p> <p>A notebook with examples of reading in the output files can be found here:</p> <p>https://github.com/hyperion-rt/paper-2017-sed-models/blob/master/notebook_raw/reading_raw_files.ipynb</p> <p>More information on using Hyperion, including reading input/output files, can also be found at http://docs.hyperion-rt.org</p> <p>For <strong>announcements</strong> of new versions of these models, you can subscribe to the following mailing list:</p> <p>https://groups.google.com/forum/#!forum/protostars</p> <p>For <strong>questions or issues</strong> using these models, you can open a GitHub issue in the companion repository:</p> <p>https://github.com/hyperion-rt/paper-2017-sed-models/issues/new</p>
THE NATURE OF X-RAYS FROM YOUNG STELLAR OBJECTS IN THE ORION NEBULA CLUSTER - A Chandra HETGS Legacy Project
<p><span>This first release provides the community with a first cut of confusion cleaned X-ray spectra of the Orion Nebula Cluster observed with the HETG onboard the Chandra X-ray Observatory. The data were taken starting in 1999 until 2021. <br><br>The confusion cleaning is based on several aspects of sources for confusion, which includes cluster point sources intersecting with grating dispersions, grating arms intersecting each other in CCD space, as well as grating dispersion overlaps prohibiting proper order sorting. The latter is a major effect and resulted in sometimes severe data losses. In the first release, our automated procedure took care of the vast majority of point sources and grating arm intersections. With respect to the dispersion arm overlaps, in this release we took a statistical approach optimizing the agreement of all four grating dispersion arms in the merged data to agree within a 1 sigma statistical uncertainty over 90% of the bandpass between 2 and 15 Angstrom. For that we used the zero order flux fractions of the interfering sources as the driving parameter. <br><br>There are still many caveats and rooms for improvement, which we will address in upcoming releases, which include the treatment of the increasing background at high dispersion, improve extraction efficiency, exclude observations with non-detections before confusion cleaning, include possible new detections, investigate the 5 A excess we observe in the HEG, though at low statistics, spotcheck individual observations for any residual issues. <br><br>Release 1 provides the community with an excellent starting point for addressing our identified science projects. Out of the 46 sources that were extracted, 37 resulted in valid spectral data. 7 sources have less than 1000 counts in 1st order, some of those may not yet be very useful. <br></span></p> <p> </p> <p>Each directory contains the merged cleaned spectrum and responses for<br>one source. The file "pha2" is a Type II PHA file (multiple spectra)<br>containing the four first order spectra, HEG -1, HEG +1, MEG -1, and<br>MEG +1. Headers have been edited indicate the object (OBJECT), and<br>start and stop times for the set of observations. Since the exposure<br>depends on order, due to the cleaning process, EXPOSURE is a column in<br>the data table. Some other keywords now say "MERGED" since they can<br>vary with observation.</p> <p>There is one effective area file per order (".arf" files). These have<br>also been merged by zeroing out the same regions as excluded in the<br>count spectra, and summed weighting by exposure. They also have<br>similar header edits as for the spectra.</p> <p>While the exposures in headers may say 2 Ms, the actual exposure at<br>any wavelength may be much less. This is not explicitly known, but is<br>implicit in the ignored wavelength regions in the merged counts and<br>responses.</p> <p>There is one grating response matrix (".rmf" files) per order. Since<br>all spectral extractions of all sources used the same cross-dispersion<br>region, there is no change in these files between sources. One set<br>suffices for all extractions. These are in the directory "RMFs", and<br>also for convenience have symbolic links in each source directory.</p> <p>HETG background files have also been provided, one PHA file per first<br>order, in directory HETG_Background. These have been derived from<br>long observations of blank fields. Details are provided in the<br>accompanying memo, hetg_background.pdf.</p> <p>Headers have not been designed for auto-loading of responses (that is<br>CORRFILE, RESPFILE, and BACKFILE are set to 'none').</p>
Observing substructure in circumstellar discs around massive young stellar objects
<p>Synthetic dust continuum and molecular line Atacama Large Millimetre Array (ALMA) observations of massive, self-gravitating disc models surrounding massive young stellar objects are presented here. Semi-analytic models of self-gravitating discs with spiral density waves and clumps/fragments are combined with radiative transfer models, and synthetic observations are produced using CASA software. Models presented here have different disc masses, distances, inclinations, thermal structures, dust distributions, number and orientation of spirals and fragments.<br> <br> Data is in the FITS format, with filenames starting either with 'line' (synthetic molecular line datacube) or 'cont' (synthetic continuum images), and each filename contains the model ID. Tables of model IDs and model parameters are given in files models_table_spiral.dat and models_table_spiral_fragments.dat for models without and with fragments, respectively. Starting from a fiducial disc model, model parameters were varied one by one, with the exception of disc inclination which is separately set in each model.<br> <br> For details about the model parameters, detailed presentation of methods, proposed substructure-enhancing filtering methods, discussion and predictions for the upcoming ALMA observations, see Jankovic et al. 2018 (accepted for publication in MNRAS, arxiv.org/abs/1810.11398).</p> <p> </p>
A modular set of synthetic spectral energy distributions for young stellar objects - Robitaille (2017) - v1.1
<p>These are the models released with the following publication:</p> <p><em>A modular set of synthetic spectral energy distributions for young stellar objects</em>, Robitaille (2017)</p> <p>A companion repository is available on GitHub:</p> <p>https://github.com/hyperion-rt/paper-2017-sed-models</p> <p>In particular, a notebook is provided, demonstrating how the models here can be used:</p> <p>https://github.com/hyperion-rt/paper-2017-sed-models/blob/master/notebook/using_the_models.ipynb</p> <p><strong>Note:</strong> the files here do not include polarization results, nor do they include the SEDs split by components (e.g. scattered versus direct light). The raw Hyperion output files which contain this information will be made available at a later date, and a link will be provided here.</p> <p>For <strong>announcements</strong> of new versions of these models, you can subscribe to the following mailing list:</p> <p>https://groups.google.com/forum/#!forum/protostars</p> <p>For <strong>questions or issues</strong> using these models, you can open a GitHub issue in the companion repository:</p> <p>https://github.com/hyperion-rt/paper-2017-sed-models/issues/new</p> <p><strong>MacOS X users:</strong> there is a bug in the bundled version of tar in MacOS X that causes issues when expanding some of the largest files here (this results in the <em>flux.fits</em> file being empty). To avoid this, you can use the GNU tar version which can be installed e.g. with Homebrew using <em>brew install gnu-tar</em> then using the <em>gtar</em> command instead of <em>tar</em>.</p>
RCW 38 Young Stellar Objects Catalog
This table contains some of the results from a study of the structure of the high-mass star-forming region RCW 38 and the spatial distribution of its young stellar population. Spitzer Infrared Array Camera (IRAC) photometry (3-8 micron) is combined with Two Micron All Sky Survey (2MASS) near-IR data to identify young stellar objects (YSOs) by IR-excess emission from their circumstellar material. Chandra X-ray data are used to identify class III pre-main-sequence stars lacking circumstellar material. The authors identify 624 YSOs: 23 class 0/I and 90 flat spectrum (FS) protostars, 437 class II stars, and 74 class III stars. They also identify 29 (27 new) O star candidates over the IRAC field. Seventy-two stars exhibit IR-variability, including 7 class 0/I and 12 flat spectrum YSOs. A further 177 tentative candidates are identified by their location in the IRAC [3.6] versus [3.6]-[5.8] color-magnitude diagram. The authors find strong evidence of subclustering in the region. Three subclusters were identified surrounding the central cluster, with massive and variable stars in each subcluster. The central region shows evidence of distinct spatial distributions of the protostars and pre-main-sequence stars. A previously detected IR cluster, DB2001_Obj36, has been established as a subcluster of RCW 38. This suggests that star formation in RCW 38 occurs over a more extended area than previously thought. The gas-to-dust ratio is examined using the X-ray derived hydrogen column density, NH and the K-band extinction, and found to be consistent with the diffuse interstellar medium, in contrast with Serpens and NGC 1333. The authors posit that the high photoionizing flux of massive stars in RCW 38 affects the agglomeration of the dust grains. This table contains the list of 624 young stellar objects (given in Tables 3 and 4 of the reference paper) found among the Spitzer sources in the field of RCW 38 using the two selection techniques described in Section 3 of the reference paper: (1) selection of stars with IR excesses in IR color-color diagrams, and (2) identification of X-ray luminous YSOs by comparing X-ray sources with IR detections. The latter technique was used to identify Type III YSOs lacking emission from a dusty disk. This table does NOT contain (i) the 177 candidate YSOs listed in Table 5 of the reference paper which were identified using the [3.6] versus [3.6] - [5.8] color-magnitude diagram, since contamination removal methods could not be utilized for these objects, (ii) the 24 candidate variable YSOs listed in Table 6 of the reference paper, nor (iii) 21 of the 29 candidate O-star cluster members which were listed in table 7 of the reference paper. This table was created by the HEASARC in January 2012 based on an electronic version of Tables 3 and 4 from the reference paper which were obtained from the ApJ web site. This is a service provided by NASA HEASARC .
Young Stellar Object Candidates in IC 417
IC 417 is in the Galactic Plane, and likely part of the Aur OB2 association; it is ~2 kpc away. Stock 8 is one of the densest cluster constituents; off of it to the East, there is a 'Nebulous Stream' (NS) that is dramatic in the infrared (IR). We have assembled a list of literature-identified young stellar objects (YSOs), new candidate YSOs from the NS, and new candidate YSOs from IR excesses. We vetted this list via inspection of the images, spectral energy distributions (SEDs), and color-color/color-magnitude diagrams. We placed the 710 surviving YSOs and candidate YSOs in ranked bins, nearly two-thirds of which have more than 20 points defining their SEDs. The lowest-ranked bins include stars that are confused, or likely carbon stars. There are 503 in the higher-ranked bins; half are SED Class III, and ~40% are SED Class II.
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