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X-WR-CALDESC:Eventi per Osservatorio Astronomico di Roma
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DTSTART:20160327T010000
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DTSTART:20161030T010000
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DTSTART:20170326T010000
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DTSTART:20180325T010000
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BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171205T114500
DTEND;TZID=Europe/Rome:20171205T124500
DTSTAMP:20260427T094928
CREATED:20170816T120046Z
LAST-MODIFIED:20170816T120046Z
UID:3398-1512474300-1512477900@www.oa-roma.inaf.it
SUMMARY:Mass loss of AGB stars and RSG in the Magellanic Clouds
DESCRIPTION:I will discuss recent work that I am involved in regarding the determination of\nthe mass-loss rates (MLRs)  of a significant sample of Asymptotic Giant Branch stars and\nRed Supergiants in the Magellanic Clouds. This mostly involves modelling the\nspectral energy distributions to obtain dust MLRs\, but we also used ALMA to detect CO emission\nin a few LMC objects. I will also discuss possible ways forward in this field
URL:https://www.oa-roma.inaf.it/event/talk-by-martin-groenewegen/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171205T114500
DTEND;TZID=Europe/Rome:20171205T124500
DTSTAMP:20260427T094928
CREATED:20170816T120046Z
LAST-MODIFIED:20170816T120046Z
UID:4722-1512474300-1512477900@www.oa-roma.inaf.it
SUMMARY:Mass loss of AGB stars and RSG in the Magellanic Clouds
DESCRIPTION:I will discuss recent work that I am involved in regarding the determination of\nthe mass-loss rates (MLRs)  of a significant sample of Asymptotic Giant Branch stars and\nRed Supergiants in the Magellanic Clouds. This mostly involves modelling the\nspectral energy distributions to obtain dust MLRs\, but we also used ALMA to detect CO emission\nin a few LMC objects. I will also discuss possible ways forward in this field
URL:https://www.oa-roma.inaf.it/event/talk-by-martin-groenewegen-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171212T114500
DTEND;TZID=Europe/Rome:20171212T124500
DTSTAMP:20260427T094928
CREATED:20170821T062018Z
LAST-MODIFIED:20170821T062018Z
UID:3408-1513079100-1513082700@www.oa-roma.inaf.it
SUMMARY:High contrast imaging and the search for young exo-planets
DESCRIPTION:High contrast imaging has enormously progressed in the last twenty years\, thanks to the development of extreme AO\, efficient coronagraph\, and various differential imaging techniques. The two frontier instruments are GPI at Gemini South and SPHERE at VLT. We are now routinely achieving contrast of better than 10^5 with a record of 4×10^6 at separations below 0.5 arcsec\, This has allowed the discovery and characterization of about a dozen young planets\, of a couple of dozens of brown dwarfs\, and direct detection of several tens disks in scattered light. These data open new windows on the very early phases of planet formation\, when disks are still present. Both theory and data indicate that while clearly planets form in the late phase of the protostellar disks\, the relation between disk and planets is very complex. Also\, the spectra we are obtaining for the young planets indicate systematic differences between young and old objects with similar temperature. I will briefly present the technological and scientific aspects of this very new and exciting science
URL:https://www.oa-roma.inaf.it/event/seminar-by-raffaele-gratton/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171212T114500
DTEND;TZID=Europe/Rome:20171212T124500
DTSTAMP:20260427T094928
CREATED:20170821T062018Z
LAST-MODIFIED:20170821T062018Z
UID:4724-1513079100-1513082700@www.oa-roma.inaf.it
SUMMARY:High contrast imaging and the search for young exo-planets
DESCRIPTION:High contrast imaging has enormously progressed in the last twenty years\, thanks to the development of extreme AO\, efficient coronagraph\, and various differential imaging techniques. The two frontier instruments are GPI at Gemini South and SPHERE at VLT. We are now routinely achieving contrast of better than 10^5 with a record of 4×10^6 at separations below 0.5 arcsec\, This has allowed the discovery and characterization of about a dozen young planets\, of a couple of dozens of brown dwarfs\, and direct detection of several tens disks in scattered light. These data open new windows on the very early phases of planet formation\, when disks are still present. Both theory and data indicate that while clearly planets form in the late phase of the protostellar disks\, the relation between disk and planets is very complex. Also\, the spectra we are obtaining for the young planets indicate systematic differences between young and old objects with similar temperature. I will briefly present the technological and scientific aspects of this very new and exciting science
URL:https://www.oa-roma.inaf.it/event/seminar-by-raffaele-gratton-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171219T114500
DTEND;TZID=Europe/Rome:20171219T124500
DTSTAMP:20260427T094928
CREATED:20170927T104628Z
LAST-MODIFIED:20170927T104628Z
UID:3565-1513683900-1513687500@www.oa-roma.inaf.it
SUMMARY:Dust Production from Evolved Stars in the Local Group
DESCRIPTION:Infrared observations of nearby galaxies and the Milky Way show that there are two main sources of ISM dust: the winds of evolved stars and supernovae ejecta. However\, the total dust contribution from evolved stars relative to supernovae\, and how it changes with metallicity\, is less certain. Infrared photometric and spectroscopic Spitzer Surveys of the Large and Small Magellanic Clouds (LMC\, SMC): Surveying the Agents of Galaxy Evolution (SAGE) resulted in the discovery of thousands of evolved stars. Here\, I will describe how the composition and quantity of dust produced by these stars depends on metallicity. I will also discuss how the mid-IR stellar populations of the Magellanic Clouds can be used as a template for potential observations with JWST\, and how we have applied this to our observing programs of Local Group galaxies and SN1987A with JWST
URL:https://www.oa-roma.inaf.it/event/seminar-by-olivia-jones/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171219T114500
DTEND;TZID=Europe/Rome:20171219T124500
DTSTAMP:20260427T094928
CREATED:20170927T104628Z
LAST-MODIFIED:20170927T104628Z
UID:4732-1513683900-1513687500@www.oa-roma.inaf.it
SUMMARY:Dust Production from Evolved Stars in the Local Group
DESCRIPTION:Infrared observations of nearby galaxies and the Milky Way show that there are two main sources of ISM dust: the winds of evolved stars and supernovae ejecta. However\, the total dust contribution from evolved stars relative to supernovae\, and how it changes with metallicity\, is less certain. Infrared photometric and spectroscopic Spitzer Surveys of the Large and Small Magellanic Clouds (LMC\, SMC): Surveying the Agents of Galaxy Evolution (SAGE) resulted in the discovery of thousands of evolved stars. Here\, I will describe how the composition and quantity of dust produced by these stars depends on metallicity. I will also discuss how the mid-IR stellar populations of the Magellanic Clouds can be used as a template for potential observations with JWST\, and how we have applied this to our observing programs of Local Group galaxies and SN1987A with JWST
URL:https://www.oa-roma.inaf.it/event/seminar-by-olivia-jones-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
END:VCALENDAR