Find research datasets worth reusing

opencc-by-3.0Jul 2013View details →

Fig. 20 in Temporary expansion to shelf depths rather than an onshore-offshore trend: the shallow-water rise and demise of the modern deep-sea brittle star family Ophiacanthidae (Echinodermata: Ophiuroidea)

Fig. 20. Fossil lateral arm plates (LAPs) of ophiacanthid brittle stars in external (a) and internal (b) views and articulated arm fragment. 1-2. Ophiogaleus dorecki (Hess, 1962) comb. nov. from the late Pliensbachian (Early Jurassic) of Seewen, Switzerland. 1. NHMB M11214, proximal LAP. 2. NHMB M11215, distal LAP. 3-5. Ophiogaleus stans sp. nov. from the early Bathonian (Middle Jurassic) of La Pouza, France. 3. GZG.INV.78615 (holotype), proximal LAP. 4. GZG.INV.78616 (paratype), median LAP. 5. GZG.INV.78617 (paratype), distal LAP. 6-7. Ophiogaleus sp. nov. innom 2 from the Callovian (Middle Jurassic) of Jumara, India. 6. GZG.INV.78619, proximal LAP. 7. GZG.INV.78620, distal LAP. 8-10. Ophiogaleus constrictus (Hess, 1966) comb. nov. from the late Oxfordian (Late Jurassic) of Savigna, France. 8. GZG.INV.78624, proximal LAP. 9. GZG.INV.78625, distal LAP. 10. GZG.INV.78626, proximal arm fragment in ventral (a) and dorsal (b) views. One common scale bar per species except for 10.

opencc-by-4.0May 2020View details →

Variability of OB stars from TESS southern Sectors 1-13 and high-resolution IACOB and OWN spectroscopy

Typical MESA and GYRE inlists associated with <a href="https://arxiv.org/abs/2005.09658">Burssens et al. 2020</a>. MESA v. 12155, GYRE version v. 5.2. Context: Lack of high-precision long-term continuous photometric data for large samples of stars has prevented the large-scale exploration of pulsational variability in the OB star regime. As a result, the candidates for in-depth asteroseismic modelling remained limited to a few tens of dwarfs. The TESS nominal space mission has surveyed the southern sky, including parts of the galactic plane, yielding continuous data of at least 27 d for hundreds of OB stars. Aims: We aim to couple TESS data in the southern sky with ground-based spectroscopy to study the variability in two dimensions, mass and evolution. We focus mainly on the presence of coherent pulsation modes that may or may not be present in the predicted theoretical instability domains and unravel all frequency behaviour in the amplitude spectra of the TESS data. Methods: We compose a sample of 98 OB-type stars observed by TESS in Sectors 1-13 and with available multi-epoch, high-resolution spectroscopy gathered by the IACOB and OWN surveys. We present the short-cadence 2-min light curves of dozens of OB-type stars, that have one or more spectra in the IACOB or OWN database. Based on these light curves and their Lomb-Scargle periodograms we perform variability classification and frequency analysis. We place the stars in the spectroscopic Hertzsprung-Russell diagram to interpret the variability in an evolutionary context. Results: We deduce diverse origins of the mmag-level variability found in all of the 98 OB stars in the TESS data. We find among the sample several new variable stars, including three hybrid pulsators, three eclipsing binaries, high frequency modes in a Be star, and potential heat-driven pulsations in two Oe stars.  Conclusions: We identify stars for which future asteroseismic modelling is possible, provided mode identification is achieved. By comparing the position of the variables to theoretical instability strips we discuss the current shortcomings in non-adiabatic pulsation theory, and the distribution of pulsators in the upper Hertzsprung-Russell diagram.

opencc-by-4.0Jul 2020View details →

Datasets for "Hall cascade with fractional magnetic helicity in neutron star crusts"

<pre>The run directories contain time series and spectra as text files and other secondary data as idl save files. They can be read directly with the corresponding idl routines that are in the directory run_directories/run_idl. The run directories can be used to rerun the cases with the Pencil Code (https://github.com/pencil-code).</pre>

opencc-by-4.0Jun 2020View details →

Brazil STAR Project Microgrid Monitoring Data

Contains monitoring data from microgrids deployed in rural areas of the State of Amazonas, Brazil. The data collections started in January of 2018 and ended in March 2019. Contained in the folder CSVs.zip are data from four housing units (denoted as STAR-A, STAR-B, STAR-C and STAR-D) consisting of: 1) Battery information, 2) Solar photovoltaic (PV) generation information, and 3) Measurements from individual appliance monitors (IAMs). Folders are named in the format YYYY-MM-DD-STAR-X_SYS, where 1) YYYY is the year, 2) MM is the month, 3) DD is the day, 4) STAR-X is indicator for the housing unit, i.e., STAR-A, STAR-B, STAR-C, or STAR-D. 5) SYS denotes the "system" and refers to one of the following: Battery, PV, or IAM. The files YYYY-MM-DD-STAR-X_Battery contain the following information in their columns in the order presented: 1) Timestamp 2) Battery current (mA) 3) Ampere-hours (mAh) 4) State of Charge (SOC) (%) 5) Number of charge cycles 6) Number of full discharges 7) Battery voltage (mV) 8) Battery power (W) 9) Amount of discharge energy (0.01 kWh) 10) Amount of charge energy (0.01 kWh) The files YYYY-MM-DD-STAR-X_PV contain the following information in their columns in the order presented: 1) Timestamp 2) Panel voltage (mV) 3) Panel power (W) 4) Energy generated (0.01 kWh) 5) Battery state of operation: 0(Off); 1(Low power); 2(Fault); 3(Bulk); 4(Absorption); 5(Float); 6(Inverting) The files YYYY-MM-DD-STAR-X_IAM contain the following information in their columns in the order presented: 1) Timestamp 2) Real power (W) 3) Reactive power (W) 4) Voltage (unknown unit) 5) IAM ID

opencc-by-4.0Sep 2020View details →

Reflectance and emission spectra of Earth-like planets orbiting red giant stars

Spectra of red giant stellar hosts and reflectance/emission planetary spectra as described in Kozakis & Kaltenegger (2020).  File names and content are explained in 0readme.txt.  Please email theakozakis@gmail.com with any questions.

opencc-by-4.0Oct 2020View details →

Three-component modelling of C-rich AGB-star winds V. – dataset

The provided data include all parameter files, binary output files, and log files that are the basis for the publication in MNRAS. 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_CtOc.cc.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.  c.cc :: The carbon-to-oxygen excess, in log10(n_C/n_H-n_O/n_H)+12 The contents 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 all used parameters it is necessary to look in      the log file (see below).  .bin :: Binary file that contains converged models. Each model is stored in          two versions, first the previous time step and then the current time      step (both 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.          The format of this file is explained below.          Note! These files can get pretty large and are therefore only        available for a smaller number of the models here. Please ask the        corresponding author for the missing files should the need 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.  .tpb :: Secondary binary file that contains a number of properties specified          at the outer boundary, typically for each consecutive time step.  .lis :: Plain-text file with the iteration history. Available for some files.  .liv :: Plain-text file with values specified for a number of properties at          each gridpoint. Available for a smaller number of files.  .inp :: Plain-text file that is used to launch a model; some are still there.  .eps :: Encapsulated PostScript files 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. 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-4.0Oct 2020View details →

Data for the Paper "Digital color codes of stars"

Data for the paper "Digital color codes of stars" by Jan-Vincent Harre and René Heller. Our code "spec2col.py" can be found at <a href="https://github.com/janvincentharre/spec2col">GitHub</a>.

Fig. 6 in Discometra luberonensis sp. nov. (Crinoidea, Himerometridae), a new feather star from the Late Burdigalian

Fig. 6. Calices of Discometra rhodanica (Fontannes, 1877) from Picabrier. A. Aboral oblique view of centrodorsal, largest specimen (MHNL 20.062686). B. Adoral oblique view, smallest specimen (MHNL 20.062688). C–D. Specimen of intermediate size (MHNL 20.062687). C. Adoral oblique view. D. Aboral oblique view. Scale bars = 1 mm.

Fig. 5 in Discometra luberonensis sp. nov. (Crinoidea, Himerometridae), a new feather star from the Late Burdigalian

Fig. 5. Late Burdigalian specimens attributed to Discometra rhodanica (Fontannes, 1877) by de Loriol (1897). A–B. Neotype of D. rhodanica from Notre-Dame du Château (MASR 2020.5011). A. Oblique aboral view of centrodorsal. B. Oblique adoral view of calyx (arrow = sub-rectangular low ridge). C–E. Unidentified Comatulidae Fleming, 1928. C. Adoral face of a centrodorsal from Entrechaux – ʻFerme Pieʼ (MHNL 20.062689). D-E. Radial circlet from Notre-Dame du Château (MASR 2020.5021). Scale bars = 1 mm.

Fig. 1 in Discometra luberonensis sp. nov. (Crinoidea, Himerometridae), a new feather star from the Late Burdigalian

Fig. 1. The Miocene Rhône-Provence Gulf (modified from Philippe 1998: fig.1). A = submarine or emerging shoals; B = limit of the Rhône-Provence Gulf; C = estimated limit of the Burdigalian transgression. Sites with Discometra Gislèn, 1924 cited in the text are indicated as follows: black star = Ménerbes-Lacoste Plateau; 1 = Bollène; 2 = Les Angles; 3 = Caumont-sur-Durance (Picabrier); 4 = Notre-Dame du Château; 5 = Entrechaux.

Fig. 4 in Discometra luberonensis sp. nov. (Crinoidea, Himerometridae), a new feather star from the Late Burdigalian

Fig. 4. Cross sections near aboral surface of radial circlet showing Y-shaped coelomic canals in the genus Discometra Gislèn, 1924. A. Discometra rhodanica (Fontannes, 1877). B. Discometra eggenburgensis (Schaffer, 1912). Modified from Sieverts-Doreck (1961) in which A was modified from Fontannes (1880).

Fig. 3 in Discometra luberonensis sp. nov. (Crinoidea, Himerometridae), a new feather star from the Late Burdigalian

Fig. 3. Centrodorsal and radials in Himerometridae A.H. Clark, 1908. A–D. Himerometra robustipinna (Carpenter, 1881) (MNHN-IE-2012-862). A. Adoral side of centrodorsal. B. Cirrus sockets on lateral face of centrodorsal. C–D. Radials. C. Adoral view showing vermiculate grooves on inner face. D. Distal articular facet. E. Discometra rhodanica (Fontannes, 1877) from Picabrier (MHNL 20.062687), cirrus sockets on centrodorsal. Scale bars: A–D = 1 mm; E = 0.5 mm.

Fig. 2 in Discometra luberonensis sp. nov. (Crinoidea, Himerometridae), a new feather star from the Late Burdigalian

Fig. 2. Aboral view of the proximal crown and centrodorsal in three genera of Himerometridae A.H. Clark, 1908. A–F. Discometra luberonensis sp. nov., Late Burdigalian of Ménerbes-Lacoste Plateau. A–B. Holotype (MHNL 20.062682). C–D. Paratype (MHNL 20.056148). E–F. Paratype (MHNL 20-056151). G–H. Extant species of Himerometridae from western Pacific. G. Himerometra robustipinna (Carpenter, 1881) (MNHN-IE-2012-862). H. Heterometra savignii (Müller, 1841) (MNHN-IE-2016-1381). Scale bars: A–G = 10 mm; H = 5 mm.

opencc-zeroJul 2016View details →

How loud are neutron star mergers?

We release neutron star merger waveforms computed using fully general relativistic simulations of equal and unequal-mass binaries drawn from the galactic population. The simulations employ finite-temperature microphysical equations of state (LS220, DD2, and SFHo) and neutrino cooling. Please, see http://arxiv.org/abs/1512.06397 for details.   Each tarball refers to a simulation and contains <ul> <li>Curvature multipolar waveform \(\psi^{(4)}_{\ell m}\)</li> <li>Metric multipolar waveform \(h_{\ell m}\)</li> <li>Radiated energy and angular momentum</li> </ul> Files: <ul> <li>waveforms/Psi4_l?_m?_r200.txt <ul> <li>Columns: \(t,\ \Re{(\psi^{(4)}_{\ell m})},\ \Im{(\psi^{(4)}_{\ell m})} \)</li> </ul> </li> <li>waveforms/Rh_l?_m?_r200.txt <ul> <li>Columns: \(u/M,\ \Re{(h_{\ell m})}/M,\ \Im{(h_{\ell m})}/M,\ \Re{(\dot{h}_{\ell m})},\ \Im{(\dot{h}_{\ell m}}),\ M\omega_{\ell m},\ A_{\ell m}/M,\ \phi_{\ell m},\ t \)</li> </ul> </li> <li>waveforms/Ej_r200.txt <ul> <li>Columns: \(E_b,\ j,\ E_\text{rad},\ J_\text{rad},\ t \)</li> </ul> </li> </ul> where <ul> <li>\(t\) simulation time</li> <li>\(u\) retarded time</li> <li>\(M\) binary mass</li> <li>\(\omega_{\ell m}\) wave frequency</li> <li>\(A_{\ell m}\) wave amplitude</li> <li>\(\phi_{\ell m}\) wave phase</li> <li>\(E_\text{GW}\) radiated energy</li> <li>\(J_\text{GW}\) radiated angular momentum</li> <li>\(E_b\) binary energy</li> <li>\(j\) binary specific angular momentum</li> </ul> Please refer to the paper and references therein for the definition of the different quantities. Units \(c=G=M_\text{Sun}=1\)

FIGURE 4 in A new viviparous species of asterinid (Echinodermata, Asteroidea, Asterinidae) and a new genus to accommodate the species of pantropical exiguoid sea stars

FIGURE 4. Aboral view of the gonads of C. hystera n. sp. filled with late stage juveniles just prior to leaving the parent, Juveniles about 500 µ m.

FIGURE 3. a in A new viviparous species of asterinid (Echinodermata, Asteroidea, Asterinidae) and a new genus to accommodate the species of pantropical exiguoid sea stars

FIGURE 3. a) Colour in life Cryptasterina hystera n. sp. (at left) and Cryptasterina pentagona (at right) Photograph. M Byrne. b) Statue Bay, central Queensland. Boulder and cobble beach. Type locality for C. hystera n. sp. Photograph. S McKillup.

FIGURE 2 in A new viviparous species of asterinid (Echinodermata, Asteroidea, Asterinidae) and a new genus to accommodate the species of pantropical exiguoid sea stars

FIGURE 2. Abactinal surface of holotype of Cryptasterina hystera sp. nov. (R = 10.2 mm) Emergent young visible in the interradius to left of image.

FIGURE 2 in New brittlestars (Echinodermata: Ophiuroidea) from New Zealand waters

FIGURE 2: Renetheo felli n. gen. et sp. holotype, disc diameter 1.2 mm. A: dorsal, B: ventral, C: cleaned vertebra (SEM), D: oral region (SEM).

FIGURE 5 in New brittlestars (Echinodermata: Ophiuroidea) from New Zealand waters

FIGURE 5: Ophiocten cryptum n. sp. holotype, disc diameter 7.5 mm. A: dorsal, B: ventral. Ophiomidas aurum, n. sp. holotype, disc diameter 4.5 mm. C: dorsal, D: ventral. Ophiophyllum teplium n. sp, holotype, disc diameter 7 mm. E: dorsal, F: ventral.

FIGURE 4 in New brittlestars (Echinodermata: Ophiuroidea) from New Zealand waters

FIGURE 4: Ophiophycis richardi n. sp. holotype, disc diameter 4 mm. A: dorsal, B: ventral, E: armbase (SEM). Ophiophycis johni n. sp. holotype, disc diameter 5.5 mm. C: dorsal, D: ventral, F: armbase (SEM).