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PRODID:-//Osservatorio Astronomico di Roma - ECPv6.15.20//NONSGML v1.0//EN
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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
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TZID:Europe/Rome
BEGIN:DAYLIGHT
TZOFFSETFROM:+0100
TZOFFSETTO:+0200
TZNAME:CEST
DTSTART:20150329T010000
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TZOFFSETTO:+0100
TZNAME:CET
DTSTART:20151025T010000
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TZOFFSETTO:+0200
TZNAME:CEST
DTSTART:20160327T010000
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TZOFFSETFROM:+0200
TZOFFSETTO:+0100
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DTSTART:20161030T010000
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TZOFFSETFROM:+0100
TZOFFSETTO:+0200
TZNAME:CEST
DTSTART:20170326T010000
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DTSTART:20171029T010000
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END:VTIMEZONE
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20161108T114500
DTEND;TZID=Europe/Rome:20161108T124500
DTSTAMP:20260428T153004
CREATED:20160727T120724Z
LAST-MODIFIED:20160727T120724Z
UID:4676-1478605500-1478609100@www.oa-roma.inaf.it
SUMMARY:AGILE highlights in gamma-ray astrophysics and the hunt for GW counterparts
DESCRIPTION:
URL:https://www.oa-roma.inaf.it/event/agile-highlights-in-gamma-ray-astrophysics-and-the-hunt-for-gw-counterparts-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20161108T114500
DTEND;TZID=Europe/Rome:20161108T124500
DTSTAMP:20260428T153004
CREATED:20160727T120724Z
LAST-MODIFIED:20160727T120724Z
UID:1341-1478605500-1478609100@www.oa-roma.inaf.it
SUMMARY:AGILE highlights in gamma-ray astrophysics and the hunt for GW counterparts
DESCRIPTION:
URL:https://www.oa-roma.inaf.it/event/agile-highlights-in-gamma-ray-astrophysics-and-the-hunt-for-gw-counterparts/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20161110T114500
DTEND;TZID=Europe/Rome:20161110T124500
DTSTAMP:20260428T153004
CREATED:20161004T044403Z
LAST-MODIFIED:20161004T044403Z
UID:1727-1478778300-1478781900@www.oa-roma.inaf.it
SUMMARY:Can supermassive black holes influence the evolution of galaxies?
DESCRIPTION:Powerful winds driven by active galactic nuclei (AGN) are often invoked to play a fundamental role in the evolution of both supermassive black holes (SMBHs) and their host galaxies\, quenching star formation and explaining the tight SMBH-galaxy relations. A strong support of this “quasar mode” feedback came from the recent X-ray observations of a mildly relativistic accretion disk winds in an ultraluminous infrared galaxies and their connection with a large-scale molecular outflows\, providing a direct link between the SMBH and the gas out of which stars form. Spectroscopic observations\, especially in the X-ray band\, show that such accretion disk winds may be common in local AGN and quasars. However\, their origin and characteristics are still not fully understood. Detailed theoretical models and simulations focused on radiation\, magnetohydrodynamic (MHD) or a combination of these two processes to investigate the possible acceleration mechanisms and dynamics of these winds. Some of these models have been directly compared to X-ray spectra\, providing important insights into the wind physics. Fundamental improvements on these studies will come from the unprecedented energy resolution and sensitivity of upcoming X-ray missions\, such as Athena\, and the synergy with future large facilities at other wavelengths\, such as ALMA\, E-ELT\, SKA.
URL:https://www.oa-roma.inaf.it/event/can-supermassive-black-holes-influence-the-evolution-of-galaxies/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20161110T114500
DTEND;TZID=Europe/Rome:20161110T124500
DTSTAMP:20260428T153004
CREATED:20161004T044403Z
LAST-MODIFIED:20161004T044403Z
UID:4691-1478778300-1478781900@www.oa-roma.inaf.it
SUMMARY:Can supermassive black holes influence the evolution of galaxies?
DESCRIPTION:Powerful winds driven by active galactic nuclei (AGN) are often invoked to play a fundamental role in the evolution of both supermassive black holes (SMBHs) and their host galaxies\, quenching star formation and explaining the tight SMBH-galaxy relations. A strong support of this “quasar mode” feedback came from the recent X-ray observations of a mildly relativistic accretion disk winds in an ultraluminous infrared galaxies and their connection with a large-scale molecular outflows\, providing a direct link between the SMBH and the gas out of which stars form. Spectroscopic observations\, especially in the X-ray band\, show that such accretion disk winds may be common in local AGN and quasars. However\, their origin and characteristics are still not fully understood. Detailed theoretical models and simulations focused on radiation\, magnetohydrodynamic (MHD) or a combination of these two processes to investigate the possible acceleration mechanisms and dynamics of these winds. Some of these models have been directly compared to X-ray spectra\, providing important insights into the wind physics. Fundamental improvements on these studies will come from the unprecedented energy resolution and sensitivity of upcoming X-ray missions\, such as Athena\, and the synergy with future large facilities at other wavelengths\, such as ALMA\, E-ELT\, SKA.
URL:https://www.oa-roma.inaf.it/event/can-supermassive-black-holes-influence-the-evolution-of-galaxies-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20161115T114500
DTEND;TZID=Europe/Rome:20161115T124500
DTSTAMP:20260428T153004
CREATED:20161014T114652Z
LAST-MODIFIED:20161014T114652Z
UID:4697-1479210300-1479213900@www.oa-roma.inaf.it
SUMMARY:Extreme-Adaptive-Optics observations of protostellar jets
DESCRIPTION:The ejection of matter in form of protostellar jets/outflows plays a fundamental role in the star-formation process as it is tightly connected to the mass accretion mechanism and is expected to directly affect the evolution of the circumstellar disk in which planet formation occurs. Since the typical angular scales of the jet-formation region are of the order of tens of mas for the closest star-forming regions\, such region has so far remained unknown from an observational point of view. New instruments equipped with extreme Adaptive Optics systems offer now the opportunity to observe the jets as close as possible to the driving sources so as to gather crucial pieces of information on the ejection process and its connection to the disk.\nIn this context\, I will present the first VLT/SPHERE observations jets from a young object. Using the ZIMPOL instrument we have taken optical images of the young binary Z CMa\, which is composed by two eruptive variables: a Herbig star showing recurrent EXor-like outbursts and a FUor source\, both driving a jet. The morphology of the two jets\, which we trace down to ~70 mas\, looks fairly different: the Herbig star appears to emit a poorly collimated compact flow\, while the FU Ori drives a highly collimated precessing jet.\nFor the FUor jet\, we discuss the mechanism responsible for the observed jet precession and we provide the first direct measurement of the mass ejection rate and of the ejection efficiency in a FUor source\, which we can compare to the same quantities measured in other classes of young stellar objects.\nFinally\, I will give an overview of what we can expect for protostellar jet observations with other upcoming extreme-AO instruments\, such as SHARK at LBT.
URL:https://www.oa-roma.inaf.it/event/extreme-adaptive-optics-observations-of-protostellar-jets-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20161115T114500
DTEND;TZID=Europe/Rome:20161115T124500
DTSTAMP:20260428T153004
CREATED:20161014T114652Z
LAST-MODIFIED:20161014T114652Z
UID:1776-1479210300-1479213900@www.oa-roma.inaf.it
SUMMARY:Extreme-Adaptive-Optics observations of protostellar jets
DESCRIPTION:The ejection of matter in form of protostellar jets/outflows plays a fundamental role in the star-formation process as it is tightly connected to the mass accretion mechanism and is expected to directly affect the evolution of the circumstellar disk in which planet formation occurs. Since the typical angular scales of the jet-formation region are of the order of tens of mas for the closest star-forming regions\, such region has so far remained unknown from an observational point of view. New instruments equipped with extreme Adaptive Optics systems offer now the opportunity to observe the jets as close as possible to the driving sources so as to gather crucial pieces of information on the ejection process and its connection to the disk.\nIn this context\, I will present the first VLT/SPHERE observations jets from a young object. Using the ZIMPOL instrument we have taken optical images of the young binary Z CMa\, which is composed by two eruptive variables: a Herbig star showing recurrent EXor-like outbursts and a FUor source\, both driving a jet. The morphology of the two jets\, which we trace down to ~70 mas\, looks fairly different: the Herbig star appears to emit a poorly collimated compact flow\, while the FU Ori drives a highly collimated precessing jet.\nFor the FUor jet\, we discuss the mechanism responsible for the observed jet precession and we provide the first direct measurement of the mass ejection rate and of the ejection efficiency in a FUor source\, which we can compare to the same quantities measured in other classes of young stellar objects.\nFinally\, I will give an overview of what we can expect for protostellar jet observations with other upcoming extreme-AO instruments\, such as SHARK at LBT.
URL:https://www.oa-roma.inaf.it/event/extreme-adaptive-optics-observations-of-protostellar-jets/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20161122T114500
DTEND;TZID=Europe/Rome:20161122T124500
DTSTAMP:20260428T153004
CREATED:20160801T142752Z
LAST-MODIFIED:20160801T142752Z
UID:1350-1479815100-1479818700@www.oa-roma.inaf.it
SUMMARY:A hard X-ray view of non-local AGNs
DESCRIPTION:The Cosmic X-ray Background (CXB) provides a record of cosmic accretion history\nonto actively accreting supermassive black holes. The direct resolution of the\nCXB into discrete sources can therefore provide a census of AGN populations\nacross cosmic time.\nPopulation synthesis models are able to explain the CXB as mixture of AGN\npopulations with different luminosities and obscuration degree provided a\nconsistent population of heavily obscured AGN\, called Compton Thick (CT)\,\nexpected to contribute significantly (20-30%) to the CXB peak at 20-30 keV\, is\npostulated. Unfortunately\, several parameter degeneracies in the modelings at\nenergies > 10 keV result in an order of magnitude uncertainty in the estimation\nof the fraction of CT AGN. Furthermore\, the direct detection of these sources at\n 10 keV\,\nis capable of resolving a sizable part (>~ 30%) of the CXB at energies around\nits peak of emissivity and of obtaining a direct and almost unobscured view of\nobscured AGN up to z~3 therefore starting to address the main concerns in the\nmodelings of the CXB.  In this regard I will report on the first spectral\ncharacterization of these AGN populations\, through broad-band (0.5-24 keV)\nspectral analysis of a hard-band selected sample of AGN from the NuSTAR survey\nprogram.
URL:https://www.oa-roma.inaf.it/event/the-nustar-view-of-non-local-agns/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20161122T114500
DTEND;TZID=Europe/Rome:20161122T124500
DTSTAMP:20260428T153004
CREATED:20160801T142752Z
LAST-MODIFIED:20160801T142752Z
UID:4679-1479815100-1479818700@www.oa-roma.inaf.it
SUMMARY:A hard X-ray view of non-local AGNs
DESCRIPTION:The Cosmic X-ray Background (CXB) provides a record of cosmic accretion history\nonto actively accreting supermassive black holes. The direct resolution of the\nCXB into discrete sources can therefore provide a census of AGN populations\nacross cosmic time.\nPopulation synthesis models are able to explain the CXB as mixture of AGN\npopulations with different luminosities and obscuration degree provided a\nconsistent population of heavily obscured AGN\, called Compton Thick (CT)\,\nexpected to contribute significantly (20-30%) to the CXB peak at 20-30 keV\, is\npostulated. Unfortunately\, several parameter degeneracies in the modelings at\nenergies > 10 keV result in an order of magnitude uncertainty in the estimation\nof the fraction of CT AGN. Furthermore\, the direct detection of these sources at\n 10 keV\,\nis capable of resolving a sizable part (>~ 30%) of the CXB at energies around\nits peak of emissivity and of obtaining a direct and almost unobscured view of\nobscured AGN up to z~3 therefore starting to address the main concerns in the\nmodelings of the CXB.  In this regard I will report on the first spectral\ncharacterization of these AGN populations\, through broad-band (0.5-24 keV)\nspectral analysis of a hard-band selected sample of AGN from the NuSTAR survey\nprogram.
URL:https://www.oa-roma.inaf.it/event/the-nustar-view-of-non-local-agns-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20161124T114500
DTEND;TZID=Europe/Rome:20161124T124500
DTSTAMP:20260428T153004
CREATED:20161122T161639Z
LAST-MODIFIED:20161122T161639Z
UID:4701-1479987900-1479991500@www.oa-roma.inaf.it
SUMMARY:Storia della nascita e la sorte dei “telescopi Mussolini"
DESCRIPTION:In May 1938\, during the state visit to Italy Hitler asked Mussolini “to accept as a token of our reverence and friendship a Zeiss telescope and the complete equipment of an observatory”. This equipment included three big telescopes (a 26-inch refractor\, a 1-m Schmidt refractor and a double astrograph) with three domes and auxiliary apparatus (a new-type transit instrument\, a registering microphotometer\,  a comparator etc). All telescopes together with domes were going to be produced by Zeiss.  It was decided to build the National Astronomical Observatory in Monte Porzio Catone for hosting the astronomical equipment. However\, due to the WWII tragic events these plans were not fulfilled. Three domes for big telescopes (with necessary motors for rising floor and moving roof) were completed\, moved to Italy and mounted. However\, after 8 September\, 1943 they were unmounted and moved back to Germany to the Zeiss factory. The domes and  auxiliary  instruments were distributed between German observatories. Three big telescopes were not paid by the German government and stayed in the Zeiss factory. They never came to Italy. In 1945 these telescopes were taken to the Soviet Union as war reparation. They were sent to Soviet observatories those most affected by the war.
URL:https://www.oa-roma.inaf.it/event/storia-della-nascita-e-la-sorte-dei-telescopi-mussolini-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20161124T114500
DTEND;TZID=Europe/Rome:20161124T124500
DTSTAMP:20260428T153004
CREATED:20161122T161639Z
LAST-MODIFIED:20161122T161639Z
UID:2030-1479987900-1479991500@www.oa-roma.inaf.it
SUMMARY:Storia della nascita e la sorte dei “telescopi Mussolini"
DESCRIPTION:In May 1938\, during the state visit to Italy Hitler asked Mussolini “to accept as a token of our reverence and friendship a Zeiss telescope and the complete equipment of an observatory”. This equipment included three big telescopes (a 26-inch refractor\, a 1-m Schmidt refractor and a double astrograph) with three domes and auxiliary apparatus (a new-type transit instrument\, a registering microphotometer\,  a comparator etc). All telescopes together with domes were going to be produced by Zeiss.  It was decided to build the National Astronomical Observatory in Monte Porzio Catone for hosting the astronomical equipment. However\, due to the WWII tragic events these plans were not fulfilled. Three domes for big telescopes (with necessary motors for rising floor and moving roof) were completed\, moved to Italy and mounted. However\, after 8 September\, 1943 they were unmounted and moved back to Germany to the Zeiss factory. The domes and  auxiliary  instruments were distributed between German observatories. Three big telescopes were not paid by the German government and stayed in the Zeiss factory. They never came to Italy. In 1945 these telescopes were taken to the Soviet Union as war reparation. They were sent to Soviet observatories those most affected by the war.
URL:https://www.oa-roma.inaf.it/event/storia-della-nascita-e-la-sorte-dei-telescopi-mussolini/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20161129T114500
DTEND;TZID=Europe/Rome:20161129T124500
DTSTAMP:20260428T153004
CREATED:20161110T081903Z
LAST-MODIFIED:20161110T081903Z
UID:4698-1480419900-1480423500@www.oa-roma.inaf.it
SUMMARY:Da Halley a Rosetta: esplorazione delle comete
DESCRIPTION:Le analisi compositive dei nuclei cometari esplorati da vicino ( Halley/Giotto\, Borrelly/DS1\, Stardust/Wild-2\, Tempel1/Deep Impact\, soprattutto 67P-CG/Rosetta) hanno fornito informazioni decisive sull’origine delle comete\,  sul meccanismo della loro attività emissiva\, sulla loro possibile fonte di  molecole prebiologiche verso  ambienti planetari abitabili.\nTutto questo è riassunto per la prima volta in un libro recentemente pubblicato da Hoepli (L’ ESPLORAZIONE DELLE COMETE\, da Halley a Rosetta).
URL:https://www.oa-roma.inaf.it/event/da-halley-a-rosetta-esplorazione-delle-comete-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20161129T114500
DTEND;TZID=Europe/Rome:20161129T124500
DTSTAMP:20260428T153004
CREATED:20161110T081903Z
LAST-MODIFIED:20161110T081903Z
UID:1973-1480419900-1480423500@www.oa-roma.inaf.it
SUMMARY:Da Halley a Rosetta: esplorazione delle comete
DESCRIPTION:Le analisi compositive dei nuclei cometari esplorati da vicino ( Halley/Giotto\, Borrelly/DS1\, Stardust/Wild-2\, Tempel1/Deep Impact\, soprattutto 67P-CG/Rosetta) hanno fornito informazioni decisive sull’origine delle comete\,  sul meccanismo della loro attività emissiva\, sulla loro possibile fonte di  molecole prebiologiche verso  ambienti planetari abitabili.\nTutto questo è riassunto per la prima volta in un libro recentemente pubblicato da Hoepli (L’ ESPLORAZIONE DELLE COMETE\, da Halley a Rosetta).
URL:https://www.oa-roma.inaf.it/event/da-halley-a-rosetta-esplorazione-delle-comete/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
END:VCALENDAR