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BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20161115T114500
DTEND;TZID=Europe/Rome:20161115T124500
DTSTAMP:20260405T010207
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:20161115T114500
DTEND;TZID=Europe/Rome:20161115T124500
DTSTAMP:20260405T010207
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:20161122T114500
DTEND;TZID=Europe/Rome:20161122T124500
DTSTAMP:20260405T010207
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:20161122T114500
DTEND;TZID=Europe/Rome:20161122T124500
DTSTAMP:20260405T010207
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:20161124T114500
DTEND;TZID=Europe/Rome:20161124T124500
DTSTAMP:20260405T010207
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:20161124T114500
DTEND;TZID=Europe/Rome:20161124T124500
DTSTAMP:20260405T010207
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:20161129T114500
DTEND;TZID=Europe/Rome:20161129T124500
DTSTAMP:20260405T010207
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:20260405T010207
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
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20161206T114500
DTEND;TZID=Europe/Rome:20161206T124500
DTSTAMP:20260405T010207
CREATED:20160915T090345Z
LAST-MODIFIED:20160915T090345Z
UID:1533-1481024700-1481028300@www.oa-roma.inaf.it
SUMMARY:New channels of single and binary evolution and nucleosynthesis
DESCRIPTION:In this talk I will present our new findings on an exotic group of evolved objects: post-asymptotic giant branch (post-AGB) and post-red giant branch (post-RGB) stars. These objects bear the signatures of the entire morphological and nucleosynthetic changes that occur during and prior to the red giant evolutionary phases. Therefore\, they provide excellent constraints for single and binary star evolution and nucleosynthesis. These objects have also revealed new evolutionary channels and AGB nucleosynthesis which is vital for understanding the complex chemical evolution of our Galaxy as well as external galaxies.
URL:https://www.oa-roma.inaf.it/event/seminario/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20161206T114500
DTEND;TZID=Europe/Rome:20161206T124500
DTSTAMP:20260405T010207
CREATED:20160915T090345Z
LAST-MODIFIED:20160915T090345Z
UID:4683-1481024700-1481028300@www.oa-roma.inaf.it
SUMMARY:New channels of single and binary evolution and nucleosynthesis
DESCRIPTION:In this talk I will present our new findings on an exotic group of evolved objects: post-asymptotic giant branch (post-AGB) and post-red giant branch (post-RGB) stars. These objects bear the signatures of the entire morphological and nucleosynthetic changes that occur during and prior to the red giant evolutionary phases. Therefore\, they provide excellent constraints for single and binary star evolution and nucleosynthesis. These objects have also revealed new evolutionary channels and AGB nucleosynthesis which is vital for understanding the complex chemical evolution of our Galaxy as well as external galaxies.
URL:https://www.oa-roma.inaf.it/event/seminario-8/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20161213T114500
DTEND;TZID=Europe/Rome:20161213T124500
DTSTAMP:20260405T010207
CREATED:20160729T153718Z
LAST-MODIFIED:20160729T153718Z
UID:1349-1481629500-1481633100@www.oa-roma.inaf.it
SUMMARY:Electromagnetic follow-up of gravitational wave candidates: perspectives and first results of the Italian project GRAWITA
DESCRIPTION:Detecting an electromagnetic (EM) emission associated with a gravitational wave (GW) signal is one of the main goal of the newly born gw astronomy. Merger of neutron stars and/or black holes and core-collapse of massive stars are expected to cause rapid transient EM signals like gamma-ray bursts (GRBs)\, core-collapse supernovae\, soft-gamma ray repeaters and pulsar glitches. \nThe Advanced LIGO detectors on September 14th\, for the first time\, detected a binary black hole merger (GW150914) for which a detectable electromagnetic counterpart is little expected. This detection showed that EM follow-up facilities are able to react quickly to GW signals covering radio\, optical\, near-infrared\, X-ray\, and gamma-ray wavelengths with ground- and space-based over the entire gravitational sky localization even if they have to deal with large position uncertainties up to hundreds square degrees.\nTherefore wide-field cameras and rapid follow-up observations are crucial to characterize the EM candidates and the first EM counterpart identification.\nIn this talk I want to present the activities we are currently currying on to optimize the response of the GRAWITA network of facilities to expected GW triggers and our first results. The GRAWITA project is representing an efficient operational framework capable of fast reaction on large error box triggers and direct identification and characterization of the candidates.\nAll the activities we will describe are expect to provide means and opportunities to the Italian and European astronomical communities to have a leading role in the GW astronomy and Time Domain Astronomy fields.
URL:https://www.oa-roma.inaf.it/event/electromagnetic-follow-up-of-gravitational-wave-candidates-perspectives-and-first-results-of-the-italian-project-grawita/
LOCATION:RM
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20161213T114500
DTEND;TZID=Europe/Rome:20161213T124500
DTSTAMP:20260405T010207
CREATED:20160729T153718Z
LAST-MODIFIED:20160729T153718Z
UID:4678-1481629500-1481633100@www.oa-roma.inaf.it
SUMMARY:Electromagnetic follow-up of gravitational wave candidates: perspectives and first results of the Italian project GRAWITA
DESCRIPTION:Detecting an electromagnetic (EM) emission associated with a gravitational wave (GW) signal is one of the main goal of the newly born gw astronomy. Merger of neutron stars and/or black holes and core-collapse of massive stars are expected to cause rapid transient EM signals like gamma-ray bursts (GRBs)\, core-collapse supernovae\, soft-gamma ray repeaters and pulsar glitches. \nThe Advanced LIGO detectors on September 14th\, for the first time\, detected a binary black hole merger (GW150914) for which a detectable electromagnetic counterpart is little expected. This detection showed that EM follow-up facilities are able to react quickly to GW signals covering radio\, optical\, near-infrared\, X-ray\, and gamma-ray wavelengths with ground- and space-based over the entire gravitational sky localization even if they have to deal with large position uncertainties up to hundreds square degrees.\nTherefore wide-field cameras and rapid follow-up observations are crucial to characterize the EM candidates and the first EM counterpart identification.\nIn this talk I want to present the activities we are currently currying on to optimize the response of the GRAWITA network of facilities to expected GW triggers and our first results. The GRAWITA project is representing an efficient operational framework capable of fast reaction on large error box triggers and direct identification and characterization of the candidates.\nAll the activities we will describe are expect to provide means and opportunities to the Italian and European astronomical communities to have a leading role in the GW astronomy and Time Domain Astronomy fields.
URL:https://www.oa-roma.inaf.it/event/electromagnetic-follow-up-of-gravitational-wave-candidates-perspectives-and-first-results-of-the-italian-project-grawita-2/
LOCATION:RM
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20161220T114500
DTEND;TZID=Europe/Rome:20161220T124500
DTSTAMP:20260405T010207
CREATED:20160915T090842Z
LAST-MODIFIED:20160915T090842Z
UID:4684-1482234300-1482237900@www.oa-roma.inaf.it
SUMMARY:Chemical properties of distant Milky Way halo stars from current and future spectroscopic surveys
DESCRIPTION:The study of elemental abundances of long-lived individual stars is one of the pillars of Galactic Archaeology\, as a powerful way for retrieving information on the stars birth environment.\nThrough this approach\, it has already been established that the inner Milky Way halo cannot have formed solely from the disruption of satellite galaxies experiencing as low an initial star formation rate as in the surviving Milky Way satellites.\nHowever\, the growing observational evidence for a dual nature of the Milky Way stellar halo raises the question of whether the elemental abundances of inner halo stars can be considered as representative of the whole Milky Way halo and if the inner and outer halo were formed through different dominant mechanisms.\nIn this talk I will present our investigation of the\nchemical properties of the outer Milky Way halo\, based on abundances of large samples of distant halo stars\, both from SDSS-DR13\nand proprietary spectroscopic campaigns at VLT\, Magellan and HET. I will conclude with a\ndiscussion of the prospects that future Galactic Archaeology surveys such as with the WHT/WEAVE spectrograph will open up for the study of the Milky Way halo properties.
URL:https://www.oa-roma.inaf.it/event/seminario-2-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20161220T114500
DTEND;TZID=Europe/Rome:20161220T124500
DTSTAMP:20260405T010207
CREATED:20160915T090842Z
LAST-MODIFIED:20160915T090842Z
UID:1537-1482234300-1482237900@www.oa-roma.inaf.it
SUMMARY:Chemical properties of distant Milky Way halo stars from current and future spectroscopic surveys
DESCRIPTION:The study of elemental abundances of long-lived individual stars is one of the pillars of Galactic Archaeology\, as a powerful way for retrieving information on the stars birth environment.\nThrough this approach\, it has already been established that the inner Milky Way halo cannot have formed solely from the disruption of satellite galaxies experiencing as low an initial star formation rate as in the surviving Milky Way satellites.\nHowever\, the growing observational evidence for a dual nature of the Milky Way stellar halo raises the question of whether the elemental abundances of inner halo stars can be considered as representative of the whole Milky Way halo and if the inner and outer halo were formed through different dominant mechanisms.\nIn this talk I will present our investigation of the\nchemical properties of the outer Milky Way halo\, based on abundances of large samples of distant halo stars\, both from SDSS-DR13\nand proprietary spectroscopic campaigns at VLT\, Magellan and HET. I will conclude with a\ndiscussion of the prospects that future Galactic Archaeology surveys such as with the WHT/WEAVE spectrograph will open up for the study of the Milky Way halo properties.
URL:https://www.oa-roma.inaf.it/event/seminario-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20170110T114500
DTEND;TZID=Europe/Rome:20170110T124500
DTSTAMP:20260405T010207
CREATED:20161005T041307Z
LAST-MODIFIED:20161005T041307Z
UID:1730-1484048700-1484052300@www.oa-roma.inaf.it
SUMMARY:Radial metallicity gradients of disk galaxies: The emission-line probes
DESCRIPTION:The metallicity of stellar and interstellar probes thorough disk galaxies\, including our own\, is distributed non-uniformly\, showing typically shallow radial metallicity gradients where the metallicity decreases radially\, inside out.  Ultimately\, the chemical evolution models need to be constrained by observations to determine the existence and extent of gradient slope and evolution\, which in turn are linked to the formation and evolution of the galaxy.\nThe use of emission-line probes to test metallicity gradients takes advantage of the brightness of the nebular emission lines\, and of the fact that the two major nebular probes\, planetary nebulae (PNe) and HII regions\, probe different epochs since galaxy formation. The limitation is that direct abundances are within observational reach only in the Local Universe.  On the Galactic side\, additional complications are added to the problem by the uncertainty of the PN distance scale.\nIn this talk I review the radial metallicity gradients background and main observational results\, the latest direct metallicity gradient determinations in the Galaxy and beyond\, the Gaia solution to the PN distance problem\, and the foreseen advances of this field with the next generation of observational capabilities.
URL:https://www.oa-roma.inaf.it/event/seminario-letizia-stanghellini/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20170110T114500
DTEND;TZID=Europe/Rome:20170110T124500
DTSTAMP:20260405T010207
CREATED:20161005T041307Z
LAST-MODIFIED:20161005T041307Z
UID:4692-1484048700-1484052300@www.oa-roma.inaf.it
SUMMARY:Radial metallicity gradients of disk galaxies: The emission-line probes
DESCRIPTION:The metallicity of stellar and interstellar probes thorough disk galaxies\, including our own\, is distributed non-uniformly\, showing typically shallow radial metallicity gradients where the metallicity decreases radially\, inside out.  Ultimately\, the chemical evolution models need to be constrained by observations to determine the existence and extent of gradient slope and evolution\, which in turn are linked to the formation and evolution of the galaxy.\nThe use of emission-line probes to test metallicity gradients takes advantage of the brightness of the nebular emission lines\, and of the fact that the two major nebular probes\, planetary nebulae (PNe) and HII regions\, probe different epochs since galaxy formation. The limitation is that direct abundances are within observational reach only in the Local Universe.  On the Galactic side\, additional complications are added to the problem by the uncertainty of the PN distance scale.\nIn this talk I review the radial metallicity gradients background and main observational results\, the latest direct metallicity gradient determinations in the Galaxy and beyond\, the Gaia solution to the PN distance problem\, and the foreseen advances of this field with the next generation of observational capabilities.
URL:https://www.oa-roma.inaf.it/event/seminario-letizia-stanghellini-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20170117T114500
DTEND;TZID=Europe/Rome:20170117T124500
DTSTAMP:20260405T010207
CREATED:20161005T041443Z
LAST-MODIFIED:20161005T041443Z
UID:4693-1484653500-1484657100@www.oa-roma.inaf.it
SUMMARY:Sensing the Universe in colour; Kinetic Inductance Detectors for optical and near-IR astronomy
DESCRIPTION:I will describe the ongoing work in the development of Microwave Kinetic Inductance Detectors (MKIDs) for optical and infra-red astronomy. These super-conducting devices represent an important step towards the development of the ‘ultimate detector’; one that can measure the position\, energy and arrival time of a photon. I will describe the operating principles of the devices and their current status. I will present the current MKID-based optical/IR instruments and show results from recent science demonstration runs. Finally\, I will discuss the future promise of the technology and highlight some of the areas of astronomical instrumentation where they could have a transformational impact and our program at Oxford to exploit these devices.
URL:https://www.oa-roma.inaf.it/event/seminario-kieran-obrien-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20170117T114500
DTEND;TZID=Europe/Rome:20170117T124500
DTSTAMP:20260405T010207
CREATED:20161005T041443Z
LAST-MODIFIED:20161005T041443Z
UID:1732-1484653500-1484657100@www.oa-roma.inaf.it
SUMMARY:Sensing the Universe in colour; Kinetic Inductance Detectors for optical and near-IR astronomy
DESCRIPTION:I will describe the ongoing work in the development of Microwave Kinetic Inductance Detectors (MKIDs) for optical and infra-red astronomy. These super-conducting devices represent an important step towards the development of the ‘ultimate detector’; one that can measure the position\, energy and arrival time of a photon. I will describe the operating principles of the devices and their current status. I will present the current MKID-based optical/IR instruments and show results from recent science demonstration runs. Finally\, I will discuss the future promise of the technology and highlight some of the areas of astronomical instrumentation where they could have a transformational impact and our program at Oxford to exploit these devices.
URL:https://www.oa-roma.inaf.it/event/seminario-kieran-obrien/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20170124T080000
DTEND;TZID=Europe/Rome:20170124T170000
DTSTAMP:20260405T010207
CREATED:20161005T041628Z
LAST-MODIFIED:20161005T041628Z
UID:1734-1485244800-1485277200@www.oa-roma.inaf.it
SUMMARY:Protoplanetary disk evolution: the key to planet formation
DESCRIPTION:The evolution of protoplanetary disks in young stellar clusters is regulated by the interplay of various physical processes\, such as accretion and winds\, and by the interactions with other stars in the cluster. Accretion and winds are best studied spectroscopically. Instruments like the VLT/X-Shooter spectrograph allow us to observe simultaneously the signatures of the accretion process\, such as the UV-excess and the emission lines\, together with lines tracing winds and outflows\, such as helium lines and forbidden lines. At the same time\, these spectra allow us to robustly derive the physical parameters of the central objects\, such as their temperature and their mass. These processes relate to the disk mass and size\, which can nowadays be studied with ALMA. Finally\, the coming Gaia data releases will open the field to new studies of dynamical evolution of stars in young clusters by means of kinematical modelling.\nI will report on the stellar\, accretion\, and wind properties derived with X-Shooter of the complete samples of low-mass stars in the Lupus and Chamaeleon star forming regions\, and discuss the dependence of stellar and accretion parameters with the disk properties obtained with ALMA surveys in these regions. I will present the results of the study of some peculiar dipping young stars recently discovered. Finally\, I will show how we can use Gaia data to study young clusters and the effect of interactions on the evolution of disks.
URL:https://www.oa-roma.inaf.it/event/seminario-carlo-manara/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20170124T080000
DTEND;TZID=Europe/Rome:20170124T170000
DTSTAMP:20260405T010207
CREATED:20161005T041628Z
LAST-MODIFIED:20161005T041628Z
UID:4694-1485244800-1485277200@www.oa-roma.inaf.it
SUMMARY:Protoplanetary disk evolution: the key to planet formation
DESCRIPTION:The evolution of protoplanetary disks in young stellar clusters is regulated by the interplay of various physical processes\, such as accretion and winds\, and by the interactions with other stars in the cluster. Accretion and winds are best studied spectroscopically. Instruments like the VLT/X-Shooter spectrograph allow us to observe simultaneously the signatures of the accretion process\, such as the UV-excess and the emission lines\, together with lines tracing winds and outflows\, such as helium lines and forbidden lines. At the same time\, these spectra allow us to robustly derive the physical parameters of the central objects\, such as their temperature and their mass. These processes relate to the disk mass and size\, which can nowadays be studied with ALMA. Finally\, the coming Gaia data releases will open the field to new studies of dynamical evolution of stars in young clusters by means of kinematical modelling.\nI will report on the stellar\, accretion\, and wind properties derived with X-Shooter of the complete samples of low-mass stars in the Lupus and Chamaeleon star forming regions\, and discuss the dependence of stellar and accretion parameters with the disk properties obtained with ALMA surveys in these regions. I will present the results of the study of some peculiar dipping young stars recently discovered. Finally\, I will show how we can use Gaia data to study young clusters and the effect of interactions on the evolution of disks.
URL:https://www.oa-roma.inaf.it/event/seminario-carlo-manara-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20170127T114500
DTEND;TZID=Europe/Rome:20170127T124500
DTSTAMP:20260405T010207
CREATED:20170116T074703Z
LAST-MODIFIED:20170116T074703Z
UID:2316-1485517500-1485521100@www.oa-roma.inaf.it
SUMMARY:The mystery of Fast Radio Bursts: are we closer to the solution?
DESCRIPTION:With the recent firm localization of the host galaxy of the Fast Radio\nBurst FRB 121102\, the solution to the mystery of these peculiar signals\nmight be getting closer. FRB 121102 is\, however\, the only one showing\nrepeating pulses\, leaving open the possibility that more classes\, hence\ndifferent progenitors\, of FRBs exist. In this talk I will give\, following\nthe timeline of their observational milestones\, an overview of FRBs. I\nwill presenting their main observational features\, some of the many\ntheoretical models suggested to explain their characteristics\, and some\npossible use of FRBs as cosmological probes.
URL:https://www.oa-roma.inaf.it/event/the-mystery-of-fast-radio-bursts-are-we-closer-to-the-solution/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20170127T114500
DTEND;TZID=Europe/Rome:20170127T124500
DTSTAMP:20260405T010207
CREATED:20170116T074703Z
LAST-MODIFIED:20170116T074703Z
UID:4703-1485517500-1485521100@www.oa-roma.inaf.it
SUMMARY:The mystery of Fast Radio Bursts: are we closer to the solution?
DESCRIPTION:With the recent firm localization of the host galaxy of the Fast Radio\nBurst FRB 121102\, the solution to the mystery of these peculiar signals\nmight be getting closer. FRB 121102 is\, however\, the only one showing\nrepeating pulses\, leaving open the possibility that more classes\, hence\ndifferent progenitors\, of FRBs exist. In this talk I will give\, following\nthe timeline of their observational milestones\, an overview of FRBs. I\nwill presenting their main observational features\, some of the many\ntheoretical models suggested to explain their characteristics\, and some\npossible use of FRBs as cosmological probes.
URL:https://www.oa-roma.inaf.it/event/the-mystery-of-fast-radio-bursts-are-we-closer-to-the-solution-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20170131T114500
DTEND;TZID=Europe/Rome:20170131T124500
DTSTAMP:20260405T010207
CREATED:20160928T050312Z
LAST-MODIFIED:20160928T050312Z
UID:1722-1485863100-1485866700@www.oa-roma.inaf.it
SUMMARY:Sterile Neutrinos as Dark Matter: From Production to Predictions
DESCRIPTION:Sterile neutrinos with masses of a few keV are very\nwell-motivated Dark Matter candidates. However\, even though they have the\nperfect properties for that job\, it is unclear how to produce them in the\nearly Universe. In this talk\, I will mainly focus on how to make this\nproduction happen in the early Universe. While several proposals exist in\nthe literature\, the production aspect unfortunately suffers from several\nincorrect or at least oversimplified statements (e.g.\, that keV sterile\nneutrino Dark Matter would usually be ‘warm’). I will make an attempt to\nexplain parts of the issues and how to resolve them\, which ultimately\nleads to means to distinguish the different mechanisms via their impact on\ncosmic structure formation. While lab experiments are not well-suited to\nprobe this type of Dark Matter candidate\, cosmology and astrophysics\nprovide the tools to do so. The whole talk is supposed to be more\npedagogical than technical\, so I will avoid heavy formula whereever\npossible.
URL:https://www.oa-roma.inaf.it/event/seminario-alexander-merle/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20170131T114500
DTEND;TZID=Europe/Rome:20170131T124500
DTSTAMP:20260405T010207
CREATED:20160928T050312Z
LAST-MODIFIED:20160928T050312Z
UID:4690-1485863100-1485866700@www.oa-roma.inaf.it
SUMMARY:Sterile Neutrinos as Dark Matter: From Production to Predictions
DESCRIPTION:Sterile neutrinos with masses of a few keV are very\nwell-motivated Dark Matter candidates. However\, even though they have the\nperfect properties for that job\, it is unclear how to produce them in the\nearly Universe. In this talk\, I will mainly focus on how to make this\nproduction happen in the early Universe. While several proposals exist in\nthe literature\, the production aspect unfortunately suffers from several\nincorrect or at least oversimplified statements (e.g.\, that keV sterile\nneutrino Dark Matter would usually be ‘warm’). I will make an attempt to\nexplain parts of the issues and how to resolve them\, which ultimately\nleads to means to distinguish the different mechanisms via their impact on\ncosmic structure formation. While lab experiments are not well-suited to\nprobe this type of Dark Matter candidate\, cosmology and astrophysics\nprovide the tools to do so. The whole talk is supposed to be more\npedagogical than technical\, so I will avoid heavy formula whereever\npossible.
URL:https://www.oa-roma.inaf.it/event/seminario-alexander-merle-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20170207T114500
DTEND;TZID=Europe/Rome:20170207T124500
DTSTAMP:20260405T010207
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:20260405T010207
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:20260405T010207
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:20170214T143000
DTEND;TZID=Europe/Rome:20170214T153000
DTSTAMP:20260405T010207
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:20170221T114500
DTEND;TZID=Europe/Rome:20170221T124500
DTSTAMP:20260405T010207
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:20260405T010207
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
END:VCALENDAR