Find research datasets worth reusing

opencc-by-4.0Oct 2024View details →

Reproduction package for: 'Exploring Waveform Variations among Neutron Star Ray-tracing Codes for Complex Emission Geometries'

Data files, python scripts and notebooks to reproduce the code output comparisons performed in "Exploring Waveform Variations among Neutron Star Ray-tracing Codes for Complex Emission Geometries" by Choudhury et al. (2024; <a href="https://doi.org/10.3847/1538-4357/ad7255" target="_blank" rel="noopener">ApJ 975 202</a>,  <a href="https://doi.org/10.48550/arXiv.2406.07285" target="_blank" rel="noopener">arXiv.2406.07285</a>). Please refer to the README for detailed information. N.B. The neutral hydrogen column density (${\rm N}_{\rm H}$) value is mentioned in the paper to be $0.2 \times 10^{20} {\rm cm}^{-2}$, whereas all the analyses in the paper, as reflected in this Zenodo package, actually uses ${\rm N}_{\rm H} = 2 \times 10^{20} {\rm cm}^{-2}$.

opencc-by-4.0Oct 2024View details →

Photometric detection of internal gravity waves in upper main-sequence stars. IV. Comparable stochastic low-frequency variability in SMC, LMC, and Galactic massive stars

Supporting data for peer-reviewed publication entitled: 'Photometric detection of internal gravity waves in upper main-sequence stars. IV. Comparable stochastic low-frequency variability in SMC, LMC, and Galactic massive stars', published in A&A. For the purpose of open access, the authors have applied a CC BY licence to the author accepted manuscript version and made it publicly available: <a href="https://arxiv.org/abs/2410.12726">https://arxiv.org/abs/2410.12726</a> Evolutionary models and stability window calculations courtesy of Jermyn et al. 2022 (DOI: <a href="https://iopscience.iop.org/article/10.3847/1538-4357/ac4e89">10.3847/1538-4357/ac4e89</a>) are publicly available via: <a href="https://github.com/adamjermyn/conv_trends">https://github.com/adamjermyn/conv_trends</a> TESS full-frame image data are publicly available from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute (STScI): <a href="https://archive.stsci.edu/missions-and-data/tess">https://archive.stsci.edu/missions-and-data/tess</a> TESS light curves (provided in this repository) were extracted using the publicly available tglc (Han & Brandt 2023; DOI: <a href="https://iopscience.iop.org/article/10.3847/1538-3881/acaaa7">10.3847/1538-3881/acaaa7</a>) software package: <a href="https://github.com/TeHanHunter/TESS_Gaia_Light_Curve">https://github.com/TeHanHunter/TESS_Gaia_Light_Curve </a> SLF variability parameters (provided in this repository; cf. Tables 1 and 2 of the paper) were obtained using GP regression with the publicly available celerite2 (Foreman-Mackey et al. 2017; DOI: <a href="https://iopscience.iop.org/article/10.3847/1538-3881/aa9332">10.3847/1538-3881/aa9332</a>) software package: <a href="https://celerite2.readthedocs.io/en/latest/">https://celerite2.readthedocs.io/en/latest/</a>  and confidence intervals were obtained using the publicly available pymc3 (Salvatier et al. 2016; <a href="https://doi.org/10.7717/peerj-cs.55">https://doi.org/10.7717/peerj-cs.55</a>) software package: <a href="https://github.com/pymc-devs/pymc">https://github.com/pymc-devs/pymc</a> This research was supported in part by the National Science Foundation (NSF) under Grant Number NSF PHY-1748958; the Research Foundation Flanders (FWO) with grant agreement numbers 1286521N, 11F7120N, and V411621N; UK Research and Innovation (UKRI) in the form of a Frontier Research grant under the UK government's ERC Horizon Europe funding guarantee (SYMPHONY; grant number: EP/Y031059/1); a Royal Society University Research Fellowship (URF; grant number: URF\R1\231631); and the KU Leuven Research Council (grant number C16/18/005: PARADISE).

opencc-by-4.0Aug 2021View details →

Dataset for: "Modeling the Hα Emission Surrounding Spica using the Lyman Continuum from a Gravity-darkened Central Star"

Summary: This deposit supplements the manuscript, "Modeling the Hα Emission Surrounding Spica using the Lyman Continuum from a Gravity-darkened Central Star", accepted to the Astrophysical Journal. The tar.gz archive file contains an example Cloudy script and associated data. The complete listing of the files included in this archive file are given here:       ReadMe                                          Documentation file     example_cloudy_input_file.txt        Cloudy script     spica_i=100_V5_solar.ascii            Spica input stellar spectral energy distribution     spica_i=110_V5_solar.ascii            Spica input stellar spectral energy distribution     spica_i=116_V5_solar.ascii            Spica input stellar spectral energy distribution     spica_i=120_V5_solar.ascii            Spica input stellar spectral energy distribution     spica_i=130_V5_solar.ascii            Spica input stellar spectral energy distribution     spica_i=140_V5_solar.ascii            Spica input stellar spectral energy distribution     spica_i=150_V5_solar.ascii            Spica input stellar spectral energy distribution     spica_i=160_V5_solar.ascii            Spica input stellar spectral energy distribution     spica_i=170_V5_solar.ascii            Spica input stellar spectral energy distribution     spica_i=180_V5_solar.ascii            Spica input stellar spectral energy distribution     spica_i=90_V5_solar.ascii              Spica input stellar spectral energy distribution   System requirements: The input script and SED files correspond to Cloudy code version 17.02:         Codebase: <a href="https://trac.nublado.org/">https://trac.nublado.org/</a>         Primary documentation: Ferland et al. (<a href="https://ui.adsabs.harvard.edu/abs/2017RMxAA..53..385F/abstract">2017RMxAA..53..385F</a>; arXiv:<a href="https://arxiv.org/abs/1705.10877">1705.10877</a>)   Additional documentation provided in the ReadMe file.

opencc-by-4.0May 2021View details →

Constraining scalar-tensor theories by neutron star-balck hole gravitational wave events

This data release corresponds to the paper "Constraining scalar-tensor theories by neutron star-balck hole gravitational wave events" (<a href="https://arxiv.org/abs/2105.13644">arXiv:2105.13644</a>). In this paper, we consider three specific models of scalar-tensor theories, including the Brans-Dicke theory (BD), the theory with scalarization phenomena proposed by Damour and Esposito-Far\`{e}se (DEF), and Screened Modified Gravity (SMG). From all 4 possible NSBH events so far, we use two of them to place the constraints. The other two are excluded in this work due to the possible unphysical deviations. Four equations of state (EoSs), sly, alf2, H4 and mpa1, are used to derive the scalar charges of neutron stars for BD and DEF. The constraints are obtained by performing the full Bayesian inference with the help of the open source software <a href="https://git.ligo.org/lscsoft/bilby">Bilby</a>. This dataset contains all posterior samples of the runs discussed in the paper. The models and EoSs can be read form the filenames for the runs of BD and DEF. The files of "*_half_dipole.json" correspond to the runs for constraining the dipole radiation without considering specific model parameters. All files are JSON format which is the default output format of <a href="https://git.ligo.org/lscsoft/bilby">Bilby</a>. They are human readable and also can be processed or visualized by <a href="https://git.ligo.org/lscsoft/bilby">Bilby</a> or <a href="https://git.ligo.org/lscsoft/pesummary">PESummary</a> conveniently.

opencc-by-4.0Sep 2021View details →

Impact of the PSR J0740+6620 radius constraint on the properties of high-density matter : Weighted Monte Carlo samples for neutron star observables

This data release contains weighted Monte Carlo samples associated with Legred, Chatziioannou, Essick, Han, and Landry, 2021 "Impact of PSR J0740+6620 radius constraint on the properties of high-density matter" Phys. Rev. D 104, 063003; doi:10.1103/PhysRevD.104.063003

opencc-by-4.0Sep 2021View details →

The immature Homo naledi ilium from the Lesedi Chamber, Rising Star Cave, South Africa

To use any of these data, please cite: Cofran Z, VanSickle C, Valenzuela R, García-Martínez D, Walker CS, Hawks J, Zipfel B, Williams SA, & Berger LR. 2022. The immature Homo naledi ilium from the Lesedi Chamber, Rising Star Cave, South Africa. American Journal of Biological Anthropology 179:3–17. (https://onlinelibrary.wiley.com/doi/full/10.1002/ajpa.24522) Lesedi Ilium Landmark Dataset_R1.csv = A comma separated values (.csv) format file containing 148 3D landmarks describing shape of the right ilium, for 23 immature humans, Australopithecus fossils MLD 7 and MLD 25, and two reconstructions of the Homo naledi fossil U.W. 102a-138. The first naledi reconstruction utilizes a reference template based on MLD 7 and MLD 25, and the second reconstruction is based on the average of the human ilia. The .csv file contains columns for individual ID, landmark name, and the x-, y-, and z-coordinates of the landmark, and each row is a unique landmark coordinate. Lesedi_Ilium_Height_Data.csv = A comma separated values (.csv) format file containing developmental stage and iliac height (in mm) for 43 humans, U.W. 102a-138, and three Australopithecus fossils (MLD 7, MLD 25, and the left and right sides of Sts 14). A 3D mesh of the U.W. 102a-138 ilium is available on Morphosource: https://www.morphosource.org/concern/media/000383216?locale=en

opencc-by-4.0Jan 2023View details →

Brown Dwarfs are Violet: Python Tools for the Estimation of Human-eye Colors of Stars and Substellar Objects

The accompanying files include a Python Jupyter notebook (and associated data files read in by the Python code) that carry out the calculations described by Cranmer (2023), talk 246.05 presented at the 241st Meeting of the American Astronomical Society (AAS) in Seattle, Washington. The abstract of the talk is provided here: There has always been interest in the perceived colors of the stars.  They were key to the development of the H-R diagram, and they are also used widely in educational and public-outreach imagery.  Thus, it is useful to develop software tools to compute these colors, as accurately as possible, from spectral energy distributions.  This presentation follows up on an RNAAS paper (<a href="https://ui.adsabs.harvard.edu/abs/2021RNAAS...5..201C/abstract">Cranmer 2021</a>) that presented a collection of objective (CIE coordinate) and subjective (RGB triple) colors for main-sequence stars and brown dwarfs.  A new empirical method of converting from CIE to RGB values is described, and results for various stellar spectra are presented.  Although brown dwarfs over a wide range of effective temperatures (400 to 2000 K) emit most of their flux in the infrared, their visible spectra often exhibit a local maximum around a strong dip in the Na I cross section at 0.4-0.5 microns.  Thus, they may appear purple to human eyes.  Also, the hottest (O-type) main-sequence stars may appear even "bluer than the blue sky" because of Paschen continuum absorption.  This presentation will update earlier stellar and brown-dwarf color estimates using more recently published synthetic spectra, and it will also investigate the effects of atmospheric absorption, over a range of air-mass values, on these perceived colors.  Python Jupyter notebooks that carry out these calculations will be uploaded to the Zenodo repository for open-access distribution. NOTE 1: The algorithms described here, for computing RGB triples, ought to be considered as preliminary results in ongoing research; i.e., they need additional testing and validation by comparing to the results of other more established ways of converting astronomical spectra to perceived colors. NOTE 2: These files follow on from those provided in another Zenodo upload associated with the 2021 RNAAS paper: <a href="https://doi.org/10.5281/zenodo.5293307">https://doi.org/10.5281/zenodo.5293307</a>

opencc-by-4.0Feb 2023View details →

Suomi 100 satellite's images: The auroral and the star images

Spacecraft: Suomi 100 Instrument: Camera <ul> <li>White light RGB camera</li> <li>Resolution: 2048 x 1536 pixels</li> <li>Angle of view: 43.6° x 33.4° (horizontal x vertical)</li> </ul> On-board data processing: <ul> <li>Debayering</li> <li>Color correction</li> <li>Gamma correction (gamma=2.2, gamma-break: 0.1)</li> <li>JPEG compression</li> </ul> Data: Three images     1. The auroral image: Original (ID: 001229, rotated 180°) <ul> <li>File: img001229.jpg</li> <li>Imaging time: January 22, 2019, 18:08:20 UT</li> <li>Location: 62.17°N, 47.64°E, 582865 m (WGS84)</li> <li>Attitude: heading -31.21°, tilt 68.89°, roll -1.85°</li> <li>Integration time: 2.4 seconds</li> <li>Sensor gain: x128</li> </ul>     2. The auroral image: Processed version (see Knuuttila et al., JoSS, 2022, for details) <ul> <li>File: img001229_processed.png</li> <li>Inverted on-board data processing (excl. debayering)</li> <li>Subtracted the star image (ID: 001264) to compensate warm pixel effec</li> </ul>     3. The original star image used for background subtraction (ID: 001264) <ul> <li>File: img001264.jpg</li> <li>Imaging time: January 23, 2019, 18:13 UT</li> <li>Attitude: declination -1.3°, right ascension 97.1°, celestial north clock angle -21.8° (J2000)</li> <li>Integration time: 1.6 seconds</li> <li>Sensor gain: x32</li> </ul>

opencc-by-4.0May 2023View details →

THE StellaR PAth WP1: Sun-as-a-star plasma Emission Measure Distributions

This folder contains a set of plasma Emission Measure Distributions (EMDs) vs. temperature, derived from observations of the solar corona with the Soft X-ray Telescope (SXT) on board the solar satellite Yohkoh, and the prescription to build EMDs for coronae of solar-type stars with different activity levels, including both quiescent and flaring components. For details read the Description PDF file.

opencc-by-4.0Jun 2023View details →

Three-component modelling of O-rich AGB star winds I. Effects of drift using forsterite – dataset

The data provided here include all parameter files, log files, and a set of the binary output files that are the basis for the publication in A&A. The file 'file_listing.txt' contains a complete list of files and directories in all gzipped tar files. Each individual gzipped tar file is formatted as follows:  Mm.m_Ll.ll_Ttttt.tar.gz where  m.m  :: the assumed mass of the model, in solar masses  l.ll :: The assumed luminosity, in log10(solar luminosities)  tttt :: The effective temperature of the star, in Kelvin. The contents of the tar files vary according to the model, but here is the general directory structure:  nodr/  :: non-drift / PC models  drift/ :: drift models  nodr/init  drift/init :: Initial model files created using John Connor. File suffixes are the following:  .par :: Plain-text parameter file that contains all parameters that are          different from the respective default value in the model.      Consequently, to see what parameters were actually used, it is      necessary to look in the log file (see below).  .bin :: Binary file that contains output of converged models. Each model is          stored in two versions, first the previous time step and then the      current time step (having access to the model code T-800, data of both      time steps are needed to restart model calculations at that time      step).          The initial model file only contains one model; where the previous      time step data are the same as the current time step data.          We provide a tool to read this file, see below.          Note! These files can get pretty large and are therefore only        available for a smaller number of the models in the Zenodo dataset.        Please ask the corresponding author for the missing files is the        need should appear.  .log :: Plain-text log file that shows the used model parameters and a number          of key properties for each converged model.      The encoding of this file is UTF-8.  .inf :: Plain-text secondary log file that contains the header of the          [primary] log file as well as timing information.      The encoding of this file is UTF-8.  .tpb :: Secondary binary file that contains a number of properties specified          at the outer boundary, typically for each consecutive time step.          We provide a tool to read this file, see below.  .lis :: Plain-text file with the iteration history. Unavailable here.  .liv :: Plain-text file with values specified for a number of properties at          each gridpoint. Unavailable here.  .inp :: Plain-text file that is used to launch a model; some are present.          This file is automatically generated by the tool that launches T-800      and is typically removed when T-800 launches. Unavailable here.  .eps :: Encapsulated PostScript file created by John Connor when calculating          the initial model. Model evolution structure - file endings before the suffix:  _rlx :: Files related to relaxing the T-800 calculations on the initial model          created by John Connor.  _exp :: Files related to expanding the initially compact model to using the          full radial domain.  _fix :: Files related to the intermediate stage where calculations are changed          from expansion to outflow.            _out :: Files related to the outflow stage of the calculations; this is what          you want to look at to see the wind evolution. Results in the paper      are calculated using these data.  Note! Some outflow stage calculations continue the evolution of the previous    set of files. The underlying reason for continued calculations is typically    that the calculated time interval is too short. Such files are typically    given the extension '_cont.lin_out', '_cont2.lin_out', etc. Stored data in the binary files:  The binary files (suffix '.bin') contain the full radial structure in the  following 10 (PC models) or 11 (drift models) primary variables:    mr: radius    mm: integrated [gas] mass    md: gas density    mu: gas velocity    me: internal energy    mj: radiative energy    mh: radiative flux    n0: dust moment, forsterite (Fo)    nm: number density of magnesium atoms    ns: number density of silicon atoms    v0: dust velocity, forsterite (only drift models)  Other properties are derived from these primary variables using auxiliary code  that isn't part of this dataset. Load files:   Two tools are provided here that can load the binary data files using the   Interactive Data Language (IDL):   sc_load_bin (for files with the suffix '.bin'):     Loads the full content of a T-800 binary file and returns a structure     with the data.   sc_load_tpb (for files with the suffix '.tpb'):     Loads the full content of a T-800 'tpb' binary file and returns a     structure with the data.     Note! Due to the way models run on clusters, this file is sometimes       incomplete; this happens when the model code T-800 is stopped as the       cluster-specific walltime is reached. If this is the case, it is       necessary to use the binary file instead, where data are saved       typically every 20:th time step.   Alternative tools for use with Python and Julia could be considered for   writing, but where not yet available when this dataset was made public.   Please contact the corresponding author for a current status on this issue.

opencc-by-4.0Jul 2023View details →

Magellan/M2FS and MMT/Hectochelle Spectroscopy of Dwarf Galaxies and Faint Star Clusters within the Galactic Halo

m2fs_HiRes_catalog_public.fits: public catalog of measurements derived from spectroscopic observations of individual targets with the Magellan/M2FS spectrograph in HiRes configuration m2fs_MedRes_catalog_public.fits: public catalog of measurements derived from spectroscopic observations of individual targets with the Magellen/M2FS spectrograph in MedRes configuration hecto_catalog_public.fits: public catalog of measurements derived from spectroscopic observations of individual targets with the MMT/Hectochelle spectrograph fits_files.tar.gz: Supplementary data products, including all sky-subtracted spectra from individual targets and best-fitting model spectra. template_spectra.tar.gz: synthetic template spectra (columns are wavelength in air (Angstroms), normalized flux)

opencc-by-4.0Jun 2022View details →

Introducing MADYS: the Manifold Age Determination for Young Stars | Full model database

Complete database of stellar and substellar evolutionary models employed in the Manifold Age Determination for Young Stars (MADYS). For a description of the tool, please refer to the main paper. For a detailed description of individual files, it is advised to use the ad-hoc functions provided within the published package. Bibliographic reference: arxiv:2206.02446 GitHub repository: https://github.com/vsquicciarini/madys

opencc-by-4.0Sep 2023View details →

X-ray and optical light curves of the M dwarf dipper star TIC 234284556

We observed the star TIC 234284556 with XMM-Newton in soft X-rays and in the optical for ca. 35 hours (127.8 ks), starting 2022-04-16 22:58:46, ObsID 0881050101. We provide here two extracted soft X-ray light curves (energy band 0.2-2 keV) collected with XMM-Newton's PN camera, namely for a circular extraction region with 20 arcsec radius centered on the position of the M dwarf star TIC 234284556 (pn_lca_02_2.fits) with 100 seconds time binning, and a background light curve with the same energy range and time binning extracted for a PN background region with a three times larger radius (pn_lcabg_02_2.fits). We also provide optical light curves in the V band, collected with XMM-Newton's Optical Monitor with 10 seconds cadence (file names P0881050101OMS0**TIMESR0000.FIT). A barycentric correction, using the XMM-SAS task "barycen", has been applied to the PN and OM time columns. The time coordinate is given in seconds since BJD 2450814.5 (1998-01-01 00:00:00).

opencc-by-4.0Aug 2023View details →

Data Release: "LIGO-Virgo-KAGRA's Oldest Black Holes: Probing star formation at cosmic noon with GWTC-3"

This repository contains the data behind the figures presented in v2 of "LIGO-Virgo-KAGRA's Oldest Black Holes: Probing star formation at cosmic noon with GWTC-3" (<a href="https://ui.adsabs.harvard.edu/link_gateway/2023arXiv230715824F/arxiv:2307.15824">arXiv:2307.15824</a>), to appear in ApJL.The csv files (in Output.zip) and the h5 files contain the data products. The three Jupyter notebooks include code for plotting the figures and calculating the summary statistics that appear in the paper.

opencc-by-4.0Aug 2015View details →

Data for: Discovery of low-metallicity stars in the central parsec of the Milky Way

Spectroscopic data from Stostad et al. (2015) and Do et al. (2015). This file contains K-band spectra from the Gemini NIFS instrument of stars in the central parsec of the Galactic center. The files are in FITS format. Additional descriptions are in in Stostad et al. (2015).  If using this data, please cite Do et al. (2015) and Stostad et al. (2015) https://ui.adsabs.harvard.edu/abs/2015ApJ...808..106S/abstract https://ui.adsabs.harvard.edu/abs/2015ApJ...809..143D/abstract   Contributors to the creation of the spectra from this dataset include: Tuan Do Morten Stostad

opencc-by-4.0Mar 2020View details →

Reproduction package for the paper "The effects of surface fossil magnetic fields on massive star evolution - II. Implementation of magnetic braking in MESA and implications for the evolution of surface rotation in OB stars "

This is a reproduction package for the paper "The effects of surface fossil magnetic fields on massive star evolution - II. Implementation of magnetic braking in MESA and implications for the evolution of surface rotation in OB stars" by Keszthelyi et al. (2020), https://doi.org/10.1093/mnras/staa237

Fig. 5 in Three New Species of Dendrogaster (Crustacea: Ascothoracida) Infecting Goniasterid Sea-Stars (Echinodermata: Asteroidea) from Japan

Fig. 5. Dendrogaster tobasuii sp. nov., allotype male, total length ca. 6 mm, NSMT-Cr 26861, removed from the main branch of holotype female. A, right lateral view (arrowhead indicating point of breakage of isolated left posterior process); B, isolated left posterior process; C, main body, left lateral view (long setae of thoracic limbs and furca omitted); D, right antennule, medial view; E, left first thoracic limb (thoracopod 2), lateral view. Abbreviations: ab, abdominal segments; bs, basis; cg, claw guard; cl, terminal claw; cx, coxa; en, endopod; ex, exopod; fr, furcal rami; fs, fusion seam; I–IV, segment numbers; mx, second maxillae; sp, rudimentary proximal sensory process; th, thoracomeres.

Fig. 7 in Three New Species of Dendrogaster (Crustacea: Ascothoracida) Infecting Goniasterid Sea-Stars (Echinodermata: Asteroidea) from Japan

Fig. 7. Dendrogaster nagasakimaruae sp. nov., A–D, holotype female, mantle size 22.0 mm, NSMT-Cr 26878, removed from coelomic cavity of Nymphaster euryplax (R 60.0 mm, r 14.6 mm), East China Sea southeast of Danjo Islands, Nagasaki Prefecture (31°51.73′N, 128°29.13′E), 247–257 m depth. A, whole animal, dorsal view; B, linear scheme to indicate a pattern of mantle branching; C, left antennule, medial view; D, second maxillae, posterior view. E–F, allotype male, total length 4.5 mm, NSMT-Cr 26879, removed from the main branch of holotype female. E, whole animal, right lateral view; F, abdomen. Abbreviations: b1a, anterior primary branches; b2a, anterior secondary branches; b3a, anterior tertiary branches; b1p, posterior primary branches; b2p, posterior secondary branches; bl, basal lobe; cg, claw guard; cl, terminal claw; fr, furcal rami; fs, fusion seam; I–IV, segment numbers; mb, main branches; mp, middle piece; pp, posterior processes; sp, rudimentary proximal sensory process.

Fig. 4 in Three New Species of Dendrogaster (Crustacea: Ascothoracida) Infecting Goniasterid Sea-Stars (Echinodermata: Asteroidea) from Japan

Fig. 4. Dendrogaster tobasuii sp. nov., holotype female, mantle size 59.9 mm, NSMT-Cr 26860, removed from coelomic cavity of Mediaster arcuatus (unmeasured), Kumano-nada Sea off Owase, Mie Prefecture, Pacific coast of central Japan, about 300 m depth. A, whole animal, dorsal view; B, linear scheme to indicate a pattern of mantle branching; C, left antennule, medial view; D, fourth segment of right antennule, lateral view; E, second maxillae. Abbreviations: b1a, anterior primary branches; b2a, anterior secondary branches; b3a, anterior tertiary branches; b1p, posterior primary branches; cg, claw guard; cl, terminal claw; fs, fusion seam; I–IV, segment numbers; mb, main branches; mp, middle piece; sp, rudimentary proximal sensory process.

Fig. 3 in Three New Species of Dendrogaster (Crustacea: Ascothoracida) Infecting Goniasterid Sea-Stars (Echinodermata: Asteroidea) from Japan

Fig. 3. Dendrogaster komatsuae sp. nov., nauplius, carapace length 0.87 mm, from holotype female. A, whole animal, ventral view; B, left portion of body, ventral view. Abbreviations: a1, antennule; a2, antenna; md, mandible. Scale bar=0.3 mm.