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<ri:Resource created="2015-11-19T15:32:27Z" status="active" updated="2025-06-13T15:25:00Z" version="1.2" xmlns:cs="http://www.ivoa.net/xml/ConeSearch/v1.0" xmlns:ri="http://www.ivoa.net/xml/RegistryInterface/v1.0" xmlns:vr="http://www.ivoa.net/xml/VOResource/v1.0" xmlns:vs="http://www.ivoa.net/xml/VODataService/v1.1" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xsi:schemaLocation="http://www.ivoa.net/xml/ConeSearch/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/ConeSearch.xsd http://www.ivoa.net/xml/VOResource/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/VOResource.xsd http://www.ivoa.net/xml/VODataService/v1.1 http://vo.ari.uni-heidelberg.de/docs/schemata/VODataService.xsd" xsi:type="vs:CatalogService"><title>Galactic and MC O-AGBs and RSGs stars</title><shortName>J/MNRAS/427/3209</shortName><identifier>ivo://CDS.VizieR/J/MNRAS/427/3209</identifier><altIdentifier>doi:10.26093/cds/vizier.74273209</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Jones O.C.</name></creator><creator><name>Kemper F.</name></creator><creator><name>Sargent B.A.</name></creator><creator><name>McDonald I.</name></creator><creator><name>Gielen C.</name></creator><creator><name>Woods P.M.,Sloan G.C.</name></creator><creator><name>Boyer M.L.</name></creator><creator><name>Zijlstra A.A.</name></creator><creator><name>Clayton G.C.</name></creator><creator><name>Kraemer K.E.,Srinivasan S.</name></creator><creator><name>Ruffle P.M.E.</name></creator><date role="Updated">2024-07-19T20:17:13Z</date><date role="Created">2015-11-19T15:32:27Z</date><contact><name>CDS support team</name><address>CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France</address><email>cds-question@unistra.fr</email></contact></curation><content><subject>magellanic-clouds</subject><subject>milky-way-galaxy</subject><subject>giant-stars</subject><subject>supergiant-stars</subject><subject>infrared-sources</subject><description>We investigate the occurrence of crystalline silicates in oxygen-rich evolved stars across a range of metallicities and mass-loss rates. It has been suggested that the crystalline silicate feature strength increases with increasing mass-loss rate, implying a correlation between lattice structure and wind density. To test this, we analyse Spitzer Infrared Spectrograph and Infrared Space Observatory Short Wavelength Spectrometer spectra of 217 oxygen-rich asymptotic giant branch and 98 red supergiants in the Milky Way, the Large and Small Magellanic Clouds, and Galactic globular clusters. These encompass a range of spectral morphologies from the spectrally rich which exhibit a wealth of crystalline and amorphous silicate features to 'naked' (dust-free) stars. We combine spectroscopic and photometric observations with the GRAMS grid of radiative transfer models to derive (dust) mass-loss rates and temperature. We then measure the strength of the crystalline silicate bands at 23, 28 and 33{mu}m. We detect crystalline silicates in stars with dust mass-loss rates which span over 3dex, down to rates of ~10^-9^M_{sun}_/yr. Detections of crystalline silicates are more prevalent in higher mass-loss rate objects, though the highest mass-loss rate objects do not show the 23-{mu}m feature, possibly due to the low temperature of the forsterite grains or it may indicate that the 23-{mu}m band is going into absorption due to high column density. 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