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X-WR-CALNAME:Osservatorio Astronomico di Roma
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X-WR-CALDESC:Eventi per Osservatorio Astronomico di Roma
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TZID:Europe/Rome
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TZNAME:CEST
DTSTART:20160327T010000
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TZNAME:CET
DTSTART:20161030T010000
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DTSTART:20170326T010000
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DTSTART:20181028T010000
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BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20170207T114500
DTEND;TZID=Europe/Rome:20170207T124500
DTSTAMP:20260417T042416
CREATED:20160906T125157Z
LAST-MODIFIED:20160906T125157Z
UID:1357-1486467900-1486471500@www.oa-roma.inaf.it
SUMMARY:High-contrast imaging observations of exoplanets: current status and future
DESCRIPTION:Thanks to notable advancements in adaptive optics combined with\ncoronagraphic observational strategies\, high-contrast imaging techniques\nare rapidly progressing in the current years. The exploration of the\nsub-stellar regime via direct imaging\, hampered so far by technical limitations\, is starting to provide us with a powerful tool\, thanks to the advent of new-generation instruments\, such as e.g.\, GPI or ScEXAO. SPHERE at VLT is a new facility that combining extreme adaptive optics with coronagraphy\, dual-band imaging\, and integral field spectroscopy has recently started its operations and aims at revealing relatively massive exoplanets at few tenths of arcsecond separations and contrasts better than 10^6. In this contribution I will present recent results obtained with SPHERE in the framework of the exoplanet detection and characterisation. Moreover\, I will present a new system for coronagraphy with high-order adaptive optics that will be operating at LBT by the end of 2018: SHARK. This system will provide coronagraphic observations from visual to NIR bands\, granting a very powerful tool that is not currently available for any other instrument in the world. Finally\, I will discuss the employment of a brand-new technique that combines high-contrast imaging with high-dispersion spectroscopy\, allowing in principle to reach contrasts down to 10^10. In the era of E-ELT\, this will open the way to investigating earth-like planets in the habitable zones of their parent stars.
URL:https://www.oa-roma.inaf.it/event/high-contrast-imaging-observations-of-exoplanets-current-status-and-future/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20170207T114500
DTEND;TZID=Europe/Rome:20170207T124500
DTSTAMP:20260417T042416
CREATED:20160906T125157Z
LAST-MODIFIED:20160906T125157Z
UID:4681-1486467900-1486471500@www.oa-roma.inaf.it
SUMMARY:High-contrast imaging observations of exoplanets: current status and future
DESCRIPTION:Thanks to notable advancements in adaptive optics combined with\ncoronagraphic observational strategies\, high-contrast imaging techniques\nare rapidly progressing in the current years. The exploration of the\nsub-stellar regime via direct imaging\, hampered so far by technical limitations\, is starting to provide us with a powerful tool\, thanks to the advent of new-generation instruments\, such as e.g.\, GPI or ScEXAO. SPHERE at VLT is a new facility that combining extreme adaptive optics with coronagraphy\, dual-band imaging\, and integral field spectroscopy has recently started its operations and aims at revealing relatively massive exoplanets at few tenths of arcsecond separations and contrasts better than 10^6. In this contribution I will present recent results obtained with SPHERE in the framework of the exoplanet detection and characterisation. Moreover\, I will present a new system for coronagraphy with high-order adaptive optics that will be operating at LBT by the end of 2018: SHARK. This system will provide coronagraphic observations from visual to NIR bands\, granting a very powerful tool that is not currently available for any other instrument in the world. Finally\, I will discuss the employment of a brand-new technique that combines high-contrast imaging with high-dispersion spectroscopy\, allowing in principle to reach contrasts down to 10^10. In the era of E-ELT\, this will open the way to investigating earth-like planets in the habitable zones of their parent stars.
URL:https://www.oa-roma.inaf.it/event/high-contrast-imaging-observations-of-exoplanets-current-status-and-future-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20170214T143000
DTEND;TZID=Europe/Rome:20170214T153000
DTSTAMP:20260417T042416
CREATED:20160915T090957Z
LAST-MODIFIED:20160915T090957Z
UID:4685-1487082600-1487086200@www.oa-roma.inaf.it
SUMMARY:A main sequence for quasars
DESCRIPTION:The last 15 years have seen a major step forward in the analysis of optical UV spectroscopic data of large quasar samples.  Multivariate statistical approaches have proved to be especially helpful\, as they have led to the definition of systematic trends (first and second eigenvector derived from Principal Component Analysis) in observed properties that are the basis of physical and dynamical modeling of quasar structure. In this talk I will discuss the empirical correlates of the so-called quasar “main sequence” associated with the quasar eigenvector 1\, its governing physical parameters\, as well as luminosity effects associated with the second eigenvector.  I will also briefly discuss  quasars in a segment of the main sequence which includes the strongest FeII emitters. These sources show a small dispersion around a well-defined Eddington ratio value\, a property which makes them potential “Eddington standard candles”.
URL:https://www.oa-roma.inaf.it/event/seminario-3-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20170214T143000
DTEND;TZID=Europe/Rome:20170214T153000
DTSTAMP:20260417T042416
CREATED:20160915T090957Z
LAST-MODIFIED:20160915T090957Z
UID:1539-1487082600-1487086200@www.oa-roma.inaf.it
SUMMARY:A main sequence for quasars
DESCRIPTION:The last 15 years have seen a major step forward in the analysis of optical UV spectroscopic data of large quasar samples.  Multivariate statistical approaches have proved to be especially helpful\, as they have led to the definition of systematic trends (first and second eigenvector derived from Principal Component Analysis) in observed properties that are the basis of physical and dynamical modeling of quasar structure. In this talk I will discuss the empirical correlates of the so-called quasar “main sequence” associated with the quasar eigenvector 1\, its governing physical parameters\, as well as luminosity effects associated with the second eigenvector.  I will also briefly discuss  quasars in a segment of the main sequence which includes the strongest FeII emitters. These sources show a small dispersion around a well-defined Eddington ratio value\, a property which makes them potential “Eddington standard candles”.
URL:https://www.oa-roma.inaf.it/event/seminario-3/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20170221T114500
DTEND;TZID=Europe/Rome:20170221T124500
DTSTAMP:20260417T042416
CREATED:20160915T091102Z
LAST-MODIFIED:20160915T091102Z
UID:1541-1487677500-1487681100@www.oa-roma.inaf.it
SUMMARY:The challenge of massive black hole binary coalescence; from galaxy formation to gravitational waves
DESCRIPTION:I will review recent progress in understanding how a pair of massive black holes can evolve from galactic scale separations\, kpc and above\, to milliparsec separations\, where gravitational wave emission takes over\nand leads to signals that should be detected by the Laser Interferometer\nSpace Antenna (LISA). I will show how\, contrary to common belief\, the\norbital decay of massive black holes in gaseous environments can be\nless efficient and more stochastic than in stellar backgrounds\, where\nthe only two processes at play are dynamical friction and 3-body\nencounters with passings stars. Novel supercomputer simulations that attempt to study orbital decay in realistic galactic hosts show that coalescence timescales\ncan become very short\, about 10 Myr\, in high redshit massive galaxies that are on their way to become quenched spheroids\, but can be longer than a\nGyr in massive star forming gas-rich disks as those observed at z > 1.\nHosts of LISA black holes are expected to have a different nature. The complex interplay between\nthe physical properties of galactic nuclei and the orbital decay process\nposes a huge challenge to computational model\, but at the same time\nholds the promise for LISA and other gravitational wave detection\nexperiments to become a powerful probe of  galaxy formation and evolution.
URL:https://www.oa-roma.inaf.it/event/seminario-4/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20170221T114500
DTEND;TZID=Europe/Rome:20170221T124500
DTSTAMP:20260417T042416
CREATED:20160915T091102Z
LAST-MODIFIED:20160915T091102Z
UID:4686-1487677500-1487681100@www.oa-roma.inaf.it
SUMMARY:The challenge of massive black hole binary coalescence; from galaxy formation to gravitational waves
DESCRIPTION:I will review recent progress in understanding how a pair of massive black holes can evolve from galactic scale separations\, kpc and above\, to milliparsec separations\, where gravitational wave emission takes over\nand leads to signals that should be detected by the Laser Interferometer\nSpace Antenna (LISA). I will show how\, contrary to common belief\, the\norbital decay of massive black holes in gaseous environments can be\nless efficient and more stochastic than in stellar backgrounds\, where\nthe only two processes at play are dynamical friction and 3-body\nencounters with passings stars. Novel supercomputer simulations that attempt to study orbital decay in realistic galactic hosts show that coalescence timescales\ncan become very short\, about 10 Myr\, in high redshit massive galaxies that are on their way to become quenched spheroids\, but can be longer than a\nGyr in massive star forming gas-rich disks as those observed at z > 1.\nHosts of LISA black holes are expected to have a different nature. The complex interplay between\nthe physical properties of galactic nuclei and the orbital decay process\nposes a huge challenge to computational model\, but at the same time\nholds the promise for LISA and other gravitational wave detection\nexperiments to become a powerful probe of  galaxy formation and evolution.
URL:https://www.oa-roma.inaf.it/event/seminario-4-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20170228T114500
DTEND;TZID=Europe/Rome:20170228T124500
DTSTAMP:20260417T042416
CREATED:20160915T091205Z
LAST-MODIFIED:20160915T091205Z
UID:1543-1488282300-1488285900@www.oa-roma.inaf.it
SUMMARY:AGB dust production: what we learn from the Local Group galaxies
DESCRIPTION:Asymptotic giant branch (AGB) stars are among the most important gas and dust polluters of the Universe. The composition and the amount of dust produced in the winds of AGB stars is strongly correlated with the evolution of the central object. Detailed knowledge of the physical structure and chemical composition Is an essential ingredient to estimate the impact of these stars in the evolution history of their host environment.\nA new release of AGB+dust models were developed in the last years to this scope. Their application in characterizing the AGB population and its contribution to the dust budget in the MCs\, as well as in dwarf galaxies of the Local Group will be discussed in this talk.
URL:https://www.oa-roma.inaf.it/event/seminario-5/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20170228T114500
DTEND;TZID=Europe/Rome:20170228T124500
DTSTAMP:20260417T042416
CREATED:20160915T091205Z
LAST-MODIFIED:20160915T091205Z
UID:4687-1488282300-1488285900@www.oa-roma.inaf.it
SUMMARY:AGB dust production: what we learn from the Local Group galaxies
DESCRIPTION:Asymptotic giant branch (AGB) stars are among the most important gas and dust polluters of the Universe. The composition and the amount of dust produced in the winds of AGB stars is strongly correlated with the evolution of the central object. Detailed knowledge of the physical structure and chemical composition Is an essential ingredient to estimate the impact of these stars in the evolution history of their host environment.\nA new release of AGB+dust models were developed in the last years to this scope. Their application in characterizing the AGB population and its contribution to the dust budget in the MCs\, as well as in dwarf galaxies of the Local Group will be discussed in this talk.
URL:https://www.oa-roma.inaf.it/event/seminario-5-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
END:VCALENDAR