BEGIN:VCALENDAR VERSION:2.0 PRODID:-//Osservatorio Astronomico di Roma - ECPv6.15.19//NONSGML v1.0//EN CALSCALE:GREGORIAN METHOD:PUBLISH X-WR-CALNAME:Osservatorio Astronomico di Roma X-ORIGINAL-URL:https://www.oa-roma.inaf.it X-WR-CALDESC:Eventi per Osservatorio Astronomico di Roma REFRESH-INTERVAL;VALUE=DURATION:PT1H X-Robots-Tag:noindex X-PUBLISHED-TTL:PT1H BEGIN:VTIMEZONE TZID:Europe/Rome BEGIN:DAYLIGHT TZOFFSETFROM:+0100 TZOFFSETTO:+0200 TZNAME:CEST DTSTART:20220327T010000 END:DAYLIGHT BEGIN:STANDARD TZOFFSETFROM:+0200 TZOFFSETTO:+0100 TZNAME:CET DTSTART:20221030T010000 END:STANDARD BEGIN:DAYLIGHT TZOFFSETFROM:+0100 TZOFFSETTO:+0200 TZNAME:CEST DTSTART:20230326T010000 END:DAYLIGHT BEGIN:STANDARD TZOFFSETFROM:+0200 TZOFFSETTO:+0100 TZNAME:CET DTSTART:20231029T010000 END:STANDARD BEGIN:DAYLIGHT TZOFFSETFROM:+0100 TZOFFSETTO:+0200 TZNAME:CEST DTSTART:20240331T010000 END:DAYLIGHT BEGIN:STANDARD TZOFFSETFROM:+0200 TZOFFSETTO:+0100 TZNAME:CET DTSTART:20241027T010000 END:STANDARD END:VTIMEZONE BEGIN:VEVENT DTSTART;TZID=Europe/Rome:20231107T113000 DTEND;TZID=Europe/Rome:20231107T123000 DTSTAMP:20260408T045730 CREATED:20230725T142148Z LAST-MODIFIED:20231027T055053Z UID:12052-1699356600-1699360200@www.oa-roma.inaf.it SUMMARY:colloquium Gregory Sloan: Carbon stars and dust in the Universe DESCRIPTION:Intermediate-mass stars become carbon-rich in the final phases of their\nlives as stars.  As they die\, carbon stars produce significant\nquantities of carbon-rich dust\, and they dominate the dust production in nearby\nmetal-poor galaxies like the Magellanic Clouds.  Infrared spectroscopy\nof carbon stars in these galaxies and our own reveals that (1) the\ninitial metallicity of a carbon star has little influence on how much\ndust it will produce\, and (2) the transition to strong pulsations in the\natmospheres of these stars leads to high rates of mass loss and dust\nproduction\, which will end the life of the star and eject most of its\nmass back into its host galaxy.  Stellar modeling shows that at lower\nmetallicity\, stars evolve more quickly\, and higher-mass stars can\nbecome carbon stars.  Carbon-rich dust has now been detected in\ngalaxies with redshifts up to 7\, or only 800 million years after the\nBig Bang.  While carbon stars can evolve in this time\, higher-mass\nobjects such as core-collapse supernovae or Wolf-Rayet stars are often\ninvoked as the likely source of that dust.  Nonetheless\, the available\nevidence points to carbon stars as the most likely culprit. URL:https://www.oa-roma.inaf.it/event/colloquium-greg-sloan/ LOCATION:Aula Gratton CATEGORIES:Seminari ORGANIZER;CN="Flavia Dell'Agli":MAILTO:flavia.dellagli@inaf.it END:VEVENT BEGIN:VEVENT DTSTART;TZID=Europe/Rome:20231113T113000 DTEND;TZID=Europe/Rome:20231113T123000 DTSTAMP:20260408T045730 CREATED:20231027T042658Z LAST-MODIFIED:20231027T042715Z UID:12389-1699875000-1699878600@www.oa-roma.inaf.it SUMMARY:colloquium - Richard de Grijs: Unveiling the complexities of massive star clusters DESCRIPTION:Around the turn of the last century\, star clusters of all kinds were considered ‘simple’ stellar populations. Over the past decades\, this situation has changed dramatically. At the same time\, star clusters are among the brightest stellar population components and\, as such\, they are visible out to much greater distances than individual stars\, even the brightest\, so that understanding the intricacies of star cluster composition and their evolution is imperative for understanding stellar populations and the evolution of galaxies as a whole. In this brief review of where the field has moved to in recent years\, we place particular emphasis on the properties and importance of the effects of rapid stellar rotation\, and the presence of multiplicity among the red-giant-branch populations in Magellanic Cloud star clusters with ages up to a few billion years. URL:https://www.oa-roma.inaf.it/event/colloqium-richard-de-grijs-unveiling-the-complexities-of-massive-star-clusters/ LOCATION:Aula Gratton CATEGORIES:Seminari END:VEVENT BEGIN:VEVENT DTSTART;TZID=Europe/Rome:20231114T113000 DTEND;TZID=Europe/Rome:20231114T123000 DTSTAMP:20260408T045730 CREATED:20230619T141534Z LAST-MODIFIED:20231018T153147Z UID:11813-1699961400-1699965000@www.oa-roma.inaf.it SUMMARY:colloquium - Davide Massari: Globular clusters as tracers of the Milky Way assembly history DESCRIPTION:The combination of stellar proper motions measured by the Gaia mission with spectroscopic radial velocities has recently enabled the precise determination of the orbits of Milky Way stars and globular clusters. The information on their dynamics\, coupled with existing chemical information\, has allowed us to unravel many unknowns on their origin and evolution\, as well as on the assembly history of the Milky Way itself. In this talk I will present the most recent results on this topic\, focusing on how globular clusters can be superior tracers of the Milky Way build-up\, and introducing a project\, named CARMA\, that aims at using globular cluster ages to characterise the most important merger events experienced by our Galaxy URL:https://www.oa-roma.inaf.it/event/colloquium-davide-massari/ LOCATION:Aula Gratton CATEGORIES:Seminari ORGANIZER;CN="Flavia Dell'Agli":MAILTO:flavia.dellagli@inaf.it END:VEVENT BEGIN:VEVENT DTSTART;TZID=Europe/Rome:20231121T113000 DTEND;TZID=Europe/Rome:20231121T123000 DTSTAMP:20260408T045730 CREATED:20231109T090747Z LAST-MODIFIED:20231109T091233Z UID:12500-1700566200-1700569800@www.oa-roma.inaf.it SUMMARY:colloquium - Mario Llerena: Probing the extreme ISM of extreme emission line galaxies at z~4-9 DESCRIPTION:Over the past decades\, several studies have discovered a population of galaxies that undergo very strong star formation events. They are called extreme emission line galaxies (EELGs) and are characterized by typically high EWs which are driven by elevated specific star formation rates in low mass galaxies with subsolar metallicities and little dust. Such extreme systems are rare in the local universe\, but the number density of EELGs increases with increasing redshift. Such starburst galaxies are currently presumed strongly to be the main drivers of Hydrogen reionization over 5.5 < z < 15\, which serves to motivate many of the searches for high-z EELGs as well. I will present the physical properties of a sample of ~1000 EELGs at 4