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1,584 results for “stars”
FIGURE 1 in New brittlestars (Echinodermata: Ophiuroidea) from New Zealand waters
FIGURE 1: Ophiolebes comatulina n. sp. holotype, disc diameter 5 mm. A: dorsal, B: ventral. Ophiolycus farquhari n. sp. disc diameter 6 mm. C: dorsal, D: ventral. Ophiolepis biscalata n. sp. holotype, disc diameter 16 mm. E: dorsal, F: ventral.
FIGURE 3 in New brittlestars (Echinodermata: Ophiuroidea) from New Zealand waters
FIGURE 3: Amphiophiura bakeri n. sp. holotype, disc diameter 9.5 mm. A: dorsal, B: ventral; paratype, C: dorsal (SEM), D: ventral (SEM). Ophiura (Ophiuroglypha) verrucosa n. sp. holotype, disc diameter 17 mm, E: dorsal, F: ventral.
FIGURE 6 in New brittlestars (Echinodermata: Ophiuroidea) from New Zealand waters
FIGURE 6: Ophiura (Dictenophiura) spinicantha n. sp. holotype, disc diameter 16 mm. A: dorsal, B: ventral, E: armbase. Ophiura (Dictenophiura) platyacantha n. sp. holotype, disc diameter 14 mm., C: dorsal, D: ventral, F: armbase.
ariedel/young_catalog: The Catalog of Suspected Nearby Young Stars (2016.1118)
<p>This is the Catalog of Suspected Young Stars from Riedel et al. (2017) (at time of paper submission).</p> <p>The catalog is meant to contain astrometric, photometric, and basic spectroscopic information for all stars EVER reported as being young (and nearby, with a rough outer limit of 100 parsecs plus the Pleiades and stars in the Octans moving group (both extend beyond 100 parsecs) plus field stars included in papers presenting young stars, or considered and rejected in those papers. Basically, if the star's youth was ever under consideration, this catalog should have it.</p> <p>The catalog currently contains 5350 stars, in a one-line-per-star format, with 388 columns. Every quantity has an associated reference, nearly all quantities have uncertainties, and most quantities have upper limit/lower limit/joint/deblended flags. The master file is actually an OpenDocument (.ods) spreadsheet which has the following improvements over the .csv file:</p> <p>Color-coded sections In-sheet calculations for derived quantities like Mean RV, Mean Parallax, and most photometric colors. Properties of companions that were simply copied from the primary star are in bold. For instance, if all that's known is that the star is a binary, EVERYTHING should be bolded. The procedure upon discovering a companion is to copy the entire primary star's line and bold it, and then replace those values with the ones specific to the secondary. Note that the OpenDocument and Excel files have two extra header lines as compared to the CSV</p> <p>The .csv file is probably easier to read into a program. Code for using Python 2.7+ and Astropy 0.4+ to produce a Python table is below:</p> <p>from astropy.io import ascii</p> <p>catalog = ascii.read(infilename)</p> <p>Buyer beware: This is a work in progress. There is missing data (no lithium data for The Pleiades yet; I haven't added the papers; nearly no Hyades at all because I haven't added the papers yet). Multiplicity is incomplete. The Bold/Unbolded method of dealing with multiples is not consistently applied, and I intend to supplant it with flags on every data value.</p> <p>Earlier versions exist for the purposes of reproducing prior work but are far less complete and correct; versions prior to 2016.0704 have fewer objects; versions prior to 2016.0116 do not have headers that comply with AAS journal standards.</p> <p>Comments and suggestions are welcome.</p>
Star Formation In Nearby Clouds (SFiNCs): X-ray And Infrared Source Catalogs And Membership. SPCM Atlas Dataset.
<p>The SPCM (SFiNCs Possible Cluster Member) Atlas dataset accompanies the article entitled ``Star Formation In Nearby Clouds (SFiNCs): X-ray And Infrared Source Catalogs And Membership,'' by Getman, Broos, Kuhn, Feigelson, Richert, Ota, Bate, and Garmire, to appear in The Astrophysical Journal Supplement Series. The paper is also available on-line on astro-ph at: https://arxiv.org/abs/1612.05282 . SPCM Atlas is a collection of 25 PDF files. Four pdf files are associated with the SFiNCs star forming region (SFR) Cep OB3b, and 21 pdf files are associated with the remaining 21 SFiNCs SFRs. Full description of SPCM Atlas is given in the Appendix B section of the article. This upload is superseded by a new version, http://doi.org/10.5281/zenodo.345398 .</p>
2MASS star counts for Gaia TGAS selection function
<p>This file contains star counts from the 2MASS point-source catalog (Skrutskie et al. 2006) for the purpose of determining the selection function of the Gaia DR1 Tycho-Astrometric Solution (Gaia collaboration et al. 2016; Lindegren et al. 2016). Counts are computed as a function of sky position (at HEALPix level 5 in RA, Dec), J-Ks color and a custom magnitude [J_T = J + (J − Ks )^2 + 2.5 (J − Ks )]. This file is designed to be used with the https://github.com/jobovy/gaia_tools package.</p> <p>The counts were performed using the following SQL query on a database that contains the full 2MASS PSC and a table that contains the HEALPix index of all stars in the 2MASS PSC at HEALPix level 12 in Ra, Dec (keys hp12index and pts_key in table twomass_psc_hp12):</p> <blockquote> <p>select floor((j_m+(j_m-k_m)*(j_m-k_m)+2.5*(j_m-k_m))*10), \ </p> <p>floor((j_m-k_m+0.05)/1.05*3), floor(hp12index/16384), count(*) as count \ </p> <p>from twomass_psc, twomass_psc_hp12 \ </p> <p>where (twomass_psc.pts_key = twomass_psc_hp12.pts_key \ </p> <p>AND (ph_qual like 'A__' OR (rd_flg like '1__' OR rd_flg like '3__')) \ </p> <p>AND (ph_qual like '__A' OR (rd_flg like '__1' OR rd_flg like '__3')) \ </p> <p>AND use_src='1' AND ext_key is null \ </p> <p>AND (j_m-k_m) > -0.05 AND (j_m-k_m) < 1.0 AND j_m < 13.5 AND j_m > 2) \ </p> <p>group by floor((j_m+(j_m-k_m)*(j_m-k_m)+2.5*(j_m-k_m))*10), \ </p> <p>floor((j_m-k_m+0.05)/1.05*3),floor(hp12index/16384) \ </p> <p>order by floor((j_m+(j_m-k_m)*(j_m-k_m)+2.5*(j_m-k_m))*10) ASC; </p> </blockquote> <p> </p>
An observed population of intermediate-mass helium stars that have been stripped in binaries - theoretical, computational and observational data
<p>This Zenodo repository contains the observational and computational data presented in the manuscript "An observed population of intermediate-mass helium stars stripped in binaries" by Drout, Götberg, Ludwig, Groh, de Mink, O'Grady and Smith.</p><p>We organize the data as follows:</p><ul><li>The stacked spectra presented in Figures S16-S21 are located in stacked_spectra.tar.gz, which contains a text file for each star. The text files have three columns that correspond to wavelength in Angstrom, normalized counts, and errors, respectively.<br> </li><li>The spectral model grid computed based on binary evolutionary model output and presented in detail in the Supplementary information section S1.2.1, is labeled with names starting S121. The file S121_evol_based_006_absolute_magnitudes.txt contains the absolute AB magnitudes for the models in UV and optical filters. The .tar.gz S121_evol_based_006_spectra.tar.gz contains files with the full spectral energy distribution and normalized spectra of each model. The .tar.gz S121_evol_based_006_complete_models.tar.gz contains the full CMFGEN models.<br> </li><li>For the stellar atmosphere model grid presented in Supplementary material section S1.2.2, we refer to the Zenodo repository 10.5281/zenodo.7976200, which is made available in association with the second paper in our series. We note that we used a subset of that grid in the article associated with this Zenodo repository. We refer to section S1.2.2 for more details.<br> </li><li>The spectral models demonstrating the mass loss rate variations in Supplementary information section S1.2.3 are presented here with names starting with S123. There is one file containing the absolute magnitudes (S123_mdot_variation_absolute_magnitudes.txt), the S123_mdot_variation_spectra.tar.gz contains the spectral energy distributions and normalized spectra for each of the models, and the S123_mdot_variation_complete_models.tar.gz contains the full CMFGEN models.<br> </li><li>The spectral model grid computed based on main-sequence evolutionary model output and presented in detail in the Supplementary information section S1.3.1, is labeled with names starting S131. The file S131_MS_evol_based_006_absolute_magnitudes.tar.gz contains three files with the absolute AB magnitudes for the models in the UV and optical filters, each file corresponding to either 20%, 60%, or 90% through the main-sequence evolution and labeled f20, f60, and f90, respectively. S131_MS_evol_based_006_spectra.tar.gz contains three folders labeled f20, f60 and f90, which each contains the SEDs (in Flambda and ABmag) and normalized spectra for the corresponding models. The files S131_MS_evol_based_006_complete_models_fX0.tar.gz contain the complete CMFGEN models.<br> </li><li>The custom index files we use for astrometry.net in section S3.1.1 are located in the zip file called S311_astrometry_index_files.zip. This information was used to recalculate the astrometry on the Swift UVOT images of the Magellanic Clouds.<br> </li><li>To make Figure 2B, we calculated the equivalent widths for a set of models assuming a signal-to-noise ratio of 35. This procedure is described in Section S3.7.2. In Figure2B_Model_EWs.zip, we provide three files that each contain these modeled equivalent widths for (1) stripped star models, (2) OB star models, and (3) composite models. <br> </li><li>To make Figure S7 (see also Sections S1.2.3 and S2.2), which is similar to Figure 2B, but presents the effects of varying the wind mass loss of stripped stars, we used a similar set of modeled equivalent widths as when we produced Figure 2B. These modeled equivalent widths are provided in FigureS7_Model_EWs.zip. <br> </li><li>To make Figure 3, we calculated equivalent widths for the model grid described in Section S1.2.2 and the TLUSTY OB star grids (see Section S1.3.2) assuming a signal-to-noise ratio of 100. These model equivalent widths are provided in the file called Figure3_Model_EWs.zip. </li></ul>
Planetary perturbers: Flaring star-planet interactions in Kepler and TESS
<p>This data set contains:</p> <p>a. almost 13,000 de-trended Kepler and TESS light curves used in the publication with the same title (Ilin et al. 2024). Each light curve is a fits file with the Kepler or TESS identifier, Quarter or Sector, and, if there are multiuple light curves per Quarter/Sector, the number of the light curve. The light curves can be read with any fits file handler (e.g., astropy), or with the lightkurve package. Each light curve contains arrays for the flux, detrended flux, time, and orbital phase of the innermost planet. Note that for transiting planets the orbital phase is set to zero around transit midtime, while for non-transiting planets, the phase zero is set arbitrarily. There is no particular reason for splitting the data in the zip files except for easier upload.</p> <p>b. Tables 1-4 from Ilin et al. (2024). Tables 1 and 3 are combined into one. Each table includes a description of its columns at the top.</p> <p><a href="https://ui.adsabs.harvard.edu/abs/2024MNRAS.527.3395I/abstract"><strong>Ilin et al. (2024)</strong></a> Ilin, E., Poppenhäger, K., Chebly, J., Ilić, N., Alvarado-Gómez, J.~D.</p> <p>Planetary perturbers: flaring star-planet interactions in Kepler and TESS.</p> <p>Monthly Notices of the Royal Astronomical Society 527, 3395–3417.</p> <p>doi:10.1093/mnras/stad3398</p>
LBT/PEPSI Spectropolarimetry of the Exoplanet Host Star 51 Peg
<p>Reduced observations of the exoplanet host star 51 Peg from the Large Binocular Telescope (LBT) using the Potsdam Echelle Polarimetric and Spectroscopic Instrument (PEPSI) on 12 nights between 2022 November 18 and 2022 December 3.</p>
Fig.ç3.R elationships of (A) barbel length and (B) pectoral- n length to standard length in Upeneus guttatus (closed symbols: stars from Japan, squares from Indo–West Paci c) and U. japonicus (open circles). in First Records of the Two-tone Goatfish, Upeneus guttatus, from Japan, and Comparisons with U. japonicus (Perciformes: Mullidae)
Fig.ç3.R elationships of (A) barbel length and (B) pectoral- n length to standard length in Upeneus guttatus (closed symbols: stars from Japan, squares from Indo–West Paci c) and U. japonicus (open circles).
Fig. 2 in Diet And Feeding In The Sea Star Astropecten Indicus (Döderlein, 1888)
Fig. 2. Examples of 16 prey types found in the stomachs of Astropecten indicus (n = 69) collected in Singapore. The white bar at the bottom right of each item = 1 mm. *Cerithium sp. was dead before ingestion.
Fig. 5 in Diet And Feeding In The Sea Star Astropecten Indicus (Döderlein, 1888)
Fig. 5. Scatter plot showing the relationship between number of prey items ingested and Astropecten indicus (n=20) arm length after 24 h.
Fig. 3. a in Diet And Feeding In The Sea Star Astropecten Indicus (Döderlein, 1888)
Fig. 3. a) Number of Astropecten indicus that chose with-shell and without-shell Umbonium vestiarium and Musculista senhousia prey (n=30). b) Mean number + S.E. of prey ingested at 2 h and at 24 h. Differences between light and dark bars are significant for both a) and b).
Contact tracing of binary stars: Pathways to stellar mergers (online data)
<p><strong># Data for Henneco et al. (2024)</strong></p> <p>This repository contains the input files required to reproduce the MESAbinary models from Henneco et al. (2024). It also contains the full machine-readable version of Table G.1. For an overview of the quantities in each column, we refer to the notes underneath Table G.1 in the paper.</p> <p>MESA r12778<br>MESA SDK 20.3.2</p> <p><strong>## MESA_inlists</strong></p> <p>- <strong>inlist1</strong>: inlist for the initially more massive primary star</p> <p>- <strong>inlist2</strong>: inlist for the initially less massive secondary star</p> <p>-<strong> inlist_project</strong>: inlist for the binary system</p> <p> </p> <p><strong>## run_extras</strong></p> <p>- <strong>run_star_extras.f</strong>: subroutines and functions for the individual stars</p> <p>- <strong>run_binary_extras.f</strong>: subroutines and functions for the binary system</p> <p> </p> <p><strong>## MESA_ZAMS_models</strong></p> <p>Precomputed ZAMS models read in through <strong>inlist1</strong> and <strong>inlist2</strong>.</p> <p> </p> <p><strong>## table_G1_full.txt</strong></p> <p>Full machine-readable version of Table G.1.<br> </p> <p><strong>## MESA_models_output</strong></p> <p>Detailed output of the MESAbinary calculations. <em>Will be added in due time.</em></p>
Kinematic data and mathematical modeling of sea star locomotion
<p>It is unclear how animals with radial symmetry control locomotion without a brain. Using a combination of experiments, mathematical modeling, and robotics, we tested the extent to which this control emerges in sea stars from the local control of their hundreds of feet and their mechanical interactions with the body. We discovered that these animals (<em>Protoreaster nodosus</em>) compensate for an experimental increase in their submerged weight by recruiting more feet that synchronize in the power stroke of the locomotor cycle. Mathematical modeling replicated this response to loading in the absence of nervous communication and demonstrated how the body weight serves as a regulator of recruitment. We built a robotic sea star with an array of independently-controlled actuators that were also recruited in greater numbers under higher loads due to their collective mechanics. These findings demonstrate that an array of actuators in biological and robotic systems are capable of cooperative transport with dynamic adjustments to loading. This form of distributed control contrasts the conventional view of animal locomotion as governed by the central nervous system and offers inspiration for the design of engineered devices with arrays of actuators.</p>
A Study of Primordial Very Massive Star Evolution II: Stellar Rotation and Gamma-Ray Burst Progenitors
<p>Wind ejecta tables of rotating very massive stars from the paper:</p> <p><a href="https://iopscience.iop.org/article/10.3847/1538-4357/ad1185">A Study of Primordial Very Massive Star Evolution II: Stellar Rotation and Gamma-Ray Burst Progenitors</a></p>
Star Trails
<p>Honorable mention in the 2023 IAU OAE Astrophotography Contest, category Still images with smartphones-mobile devices: Star Trails, by Govind Gurjar.</p> <p>Taken in the darkness of Panotiya, Amartiya village, India, this image from October 2022 showcases beautiful star trails painting the night sky, receiving an honourable mention in the category of Still images taken exclusively with smartphones/mobile devices. With only a smartphone and a tripod, the photographer captured these trails — visual evidence of our planet's rotation, as each streak represents the apparent movement of the stars as the Earth spins, creating a captivating cosmic choreography of light. The distinct colours of the stars — some gleaming blue, others whitish — hint at their varying temperatures and compositions. Additionally, a subtle streak of an aeroplane momentarily intersects the timeless dance of the stars, juxtaposing the serene heavens with the bustling activity of life below.</p> <p>Credit: Govind Gurjar/IAU OAE (<a href="https://creativecommons.org/licenses/by/4.0/legalcode">CC BY 4.0</a>)</p>
Star Trail in the Southern Hemisphere with Bortle 4 Scale Light Pollution
<p>Winner in the 2023 IAU OAE Astrophotography Contest, category Still images with smartphones-mobile devices: Star Trail in the Southern Hemisphere with Bortle 4 Scale Light Pollution, by Slamat Riyadi.</p> <p>This breathtaking photo, captured under the clear night sky of Linggamekar Village, Cilimus, Kuningan, West Java, Indonesia on 25 June 2020, displays star trails sweeping across the southern hemisphere’s heavens. The star trails are due to Earth’s rotation causing the apparent motion of stars, creating these mesmerising arcs of light when followed over extended periods. Here, the point the stars rotate around (the South Celestial Pole) is close to the horizon, as the image was taken close to the equator. The photographer used the star trail feature on a smartphone, which captured a series of images over an extended period and stacked them together. The striking tree in the foreground adds depth to the image, contrasting the celestial motion above with its Earthly stillness, while also masking some of the surrounding light pollution. Different parts of the world offer diverse and stunning perspectives on the night sky, emphasising the importance of preserving dark skies everywhere.</p> <p>Credit: Slamat Riyadi/IAU OAE (<a href="https://creativecommons.org/licenses/by/4.0/legalcode">CC BY 4.0</a>)</p>
Star Trails of the Forbidden City
<p>Honorable mention in the 2023 IAU OAE Astrophotography Contest, category Still images with smartphones-mobile devices: Star Trails of the Forbidden City, by Stephanie Ziyi Ye.</p> <p>Beneath the celestial ballet of star trails that weave their way across the night sky, the Beijing Forbidden City stands as a testament to ancient celestial connections in this image captured in March 2022. Designed with a cosmic alignment in mind, the palace echoes the orientation of the North Star, also known as Polaris, a celestial anchor that has long guided navigators and symbolised steadiness in the sky. It was believed that the Emperor embodied the earthly representation of this pole star, bridging the realms between heaven and earth. In this harmonious one-hour exposure captured with a smartphone, the streaks of stars trace their nightly journey across the firmament, converging toward the North Star, reflecting the precision of both architectural design and celestial paths. The image receives an honourable mention in the category of Still images taken exclusively with smartphones/mobile devices.</p> <p>Credit: Stephanie Ziyi Ye/IAU OAE (<a href="https://creativecommons.org/licenses/by/4.0/legalcode">CC BY 4.0</a>)</p>
Stellar properties of observed stars stripped in binaries in the Magellanic Clouds - Observations and Results
<p>This Zenodo repository is one of three Zenodo repositories related to the article "Stellar properties of observed stars stripped in binaries in the Magellanic Clouds" by Y. Götberg, M.R. Drout, A.P. Ji, J.H. Groh, B.A. Ludwig, P.A. Crowther, N. Smith, A. de Koter, and S.E. de Mink. In the article, we analyze the optical spectra of ten stars and measure their stellar properties using spectral fitting. This repository contains observational data and the resulting measurements for the stellar properties of the stars analyzed in the article, along with best fit spectral models and spectral models used to estimate the wind mass loss rate of the stars. Below, we describe the content in more detail:</p> <ul> <li><strong>0_ReadMe.txt</strong>: A text file where we describe some more details regarding the content.</li> <li><strong>S2_stacked_stellar_spectra.tar.gz (4.6 MB):</strong> The spectra we use for obtaining stellar properties for the observed stars.</li> <li><strong>Table2.txt</strong>: the apparent AB magnitudes with associated errors for the stars we analyze in the paper.</li> <li><strong>Table3.txt</strong>: the stellar properties for the stars we analyze in the paper. These parameters are obtained by spectral fitting.</li> <li><strong>S5_spectra_best_fit_models.tar.gz (14 MB):</strong> The spectral energy distributions and normalized spectra for the best-fit models, recomputed such that the radius and bolometric luminosity also matches. This tarball contains best-fit spectra for all of the stars in text-files labeled with the format SED_StarX_xxx.txt (~70 MB when inflated). The stellar parameters are presented in Section 5.</li> <li><strong>S5_full_best_fit_models.tar.gz (1.9 GB):</strong> The full CMFGEN version of the best-fit models for each individual star. This tarball contains a tarball for each star, which when inflated becomes ~250-550 MB each. </li> <li><strong>S7_spectra_mdot_models (31 MB): </strong>The spectral energy distributions and normalized spectra for the models used in the mass-loss analysis that we present in Section 7.</li> <li><strong>S7_full_mdot_models (3.5 GB):</strong> The full CMFGEN version of the spectral models used for the mass-loss rate variation presented in section 7 (excluding the best-fit models, which are provided separately).</li> </ul>
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