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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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DTSTART:20160327T010000
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DTSTART:20161030T010000
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DTSTART:20170326T010000
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DTSTART:20171029T010000
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BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20170110T114500
DTEND;TZID=Europe/Rome:20170110T124500
DTSTAMP:20260414T035059
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:20170110T114500
DTEND;TZID=Europe/Rome:20170110T124500
DTSTAMP:20260414T035059
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:20170117T114500
DTEND;TZID=Europe/Rome:20170117T124500
DTSTAMP:20260414T035059
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:20260414T035059
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:20260414T035059
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:20260414T035059
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:20260414T035059
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:20260414T035059
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:20260414T035059
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:20170131T114500
DTEND;TZID=Europe/Rome:20170131T124500
DTSTAMP:20260414T035059
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
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