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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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DTSTART:20151025T010000
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TZNAME:CEST
DTSTART:20160327T010000
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DTSTART:20161030T010000
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DTSTART:20170326T010000
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END:VTIMEZONE
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160426T114500
DTEND;TZID=Europe/Rome:20160426T124500
DTSTAMP:20260404T221128
CREATED:20160403T173332Z
LAST-MODIFIED:20160403T173332Z
UID:4662-1461671100-1461674700@www.oa-roma.inaf.it
SUMMARY:Machine learning search for gamma-ray burst afterglows in optical images
DESCRIPTION:Thanks to the rapid advances in robotic telescopes and wide field surveys\, the time domain astronomy reveals a huge number of transient detections every night. Therefore\,  automatic classification of sources in the optical images is essential. A special attention is brought to the identification of gamma-ray burst afterglows using the combined observational data from the GROND telescope and the SDSS survey. Their successful identification can lead to further follow-up observations by dedicated telescopes and for statistical studies of these transients.
URL:https://www.oa-roma.inaf.it/event/machine-learning-search-for-gamma-ray-burst-afterglows-in-optical-images-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160426T114500
DTEND;TZID=Europe/Rome:20160426T124500
DTSTAMP:20260404T221128
CREATED:20160403T173332Z
LAST-MODIFIED:20160403T173332Z
UID:995-1461671100-1461674700@www.oa-roma.inaf.it
SUMMARY:Machine learning search for gamma-ray burst afterglows in optical images
DESCRIPTION:Thanks to the rapid advances in robotic telescopes and wide field surveys\, the time domain astronomy reveals a huge number of transient detections every night. Therefore\,  automatic classification of sources in the optical images is essential. A special attention is brought to the identification of gamma-ray burst afterglows using the combined observational data from the GROND telescope and the SDSS survey. Their successful identification can lead to further follow-up observations by dedicated telescopes and for statistical studies of these transients.
URL:https://www.oa-roma.inaf.it/event/machine-learning-search-for-gamma-ray-burst-afterglows-in-optical-images/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160412T114500
DTEND;TZID=Europe/Rome:20160412T124500
DTSTAMP:20260404T221128
CREATED:20160405T045429Z
LAST-MODIFIED:20160405T045429Z
UID:1046-1460461500-1460465100@www.oa-roma.inaf.it
SUMMARY:Escape of Lyman photons from galaxies
DESCRIPTION:One of the key questions in observational cosmology is the identification of the sources responsible for cosmic\nreionization. The general consensus is that a population of faint low-mass galaxies must be responsible for the\nbulk of the ionizing photons. However\, until recently\, attempts at identifying individual galaxies showing\nLyman continuum (LyC) leakage have only found very few such galaxies\, both at high and low redshifts.\nWe recently proposed a new indirect diagnostic for LyC leakage based on the shape of the Lyman-alpha line\,\nthat I will first review (Verhamme+15).\nA breakthrough was recently achieved by our team (Izotov et al. 2016a\,b)\, detecting LyC emission in\nlow-redshift (z~0.3) luminous compact star-forming galaxies (LCGs) with high LyC escape fractions\nusing HST/COS observations. I will present these new results\, and the Lyman-alpha emission from these galaxies\,\nconfirming our theoretical predictions.\nFinally\, I will propose another complementary Lyman-alpha signature for LyC leakage\, discussing theoretical predictions\non the Lyman-alpha spatial extend of LyC emitters: LyC leakers should have no/faint Lyman-alpha halos.
URL:https://www.oa-roma.inaf.it/event/escape-of-lyman-photons-from-galaxies/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160412T114500
DTEND;TZID=Europe/Rome:20160412T124500
DTSTAMP:20260404T221128
CREATED:20160405T045429Z
LAST-MODIFIED:20160405T045429Z
UID:4663-1460461500-1460465100@www.oa-roma.inaf.it
SUMMARY:Escape of Lyman photons from galaxies
DESCRIPTION:One of the key questions in observational cosmology is the identification of the sources responsible for cosmic\nreionization. The general consensus is that a population of faint low-mass galaxies must be responsible for the\nbulk of the ionizing photons. However\, until recently\, attempts at identifying individual galaxies showing\nLyman continuum (LyC) leakage have only found very few such galaxies\, both at high and low redshifts.\nWe recently proposed a new indirect diagnostic for LyC leakage based on the shape of the Lyman-alpha line\,\nthat I will first review (Verhamme+15).\nA breakthrough was recently achieved by our team (Izotov et al. 2016a\,b)\, detecting LyC emission in\nlow-redshift (z~0.3) luminous compact star-forming galaxies (LCGs) with high LyC escape fractions\nusing HST/COS observations. I will present these new results\, and the Lyman-alpha emission from these galaxies\,\nconfirming our theoretical predictions.\nFinally\, I will propose another complementary Lyman-alpha signature for LyC leakage\, discussing theoretical predictions\non the Lyman-alpha spatial extend of LyC emitters: LyC leakers should have no/faint Lyman-alpha halos.
URL:https://www.oa-roma.inaf.it/event/escape-of-lyman-photons-from-galaxies-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160405T114500
DTEND;TZID=Europe/Rome:20160405T124500
DTSTAMP:20260404T221128
CREATED:20160317T061919Z
LAST-MODIFIED:20160317T061919Z
UID:544-1459856700-1459860300@www.oa-roma.inaf.it
SUMMARY:The final wind: stars in retirement
DESCRIPTION:Catastrophic mass loss is at the heart of 90% of all stellar\ndeath. Low and intermediate mass stars lose their hydrogen envelope\nwhile on the Asymptotic Giant Branch stars. At the end\, there is\ninsufficient hydrogen left and the star rapidly evolves into a white\ndwarf\, briefly illuminating a planetary nebula on the way. The ejected\ngas can be used to study the superwind\, the nuclear burning and dredge\nup processes in the star\, and even (with some difficulties) the star\nformation histories of the dying stellar population. In this talk I\nwill discuss the planetary nebulae of the Galactic bulge\, briefly\nmention AGB stars in globular clusters\, and finally discuss the origin\nof the mysterious AGB J-type stars\, believed to be the cause of the\nA+B grains in the proto-solar system.
URL:https://www.oa-roma.inaf.it/event/the-final-wind-stars-in-retirement/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160405T114500
DTEND;TZID=Europe/Rome:20160405T124500
DTSTAMP:20260404T221128
CREATED:20160317T061919Z
LAST-MODIFIED:20160317T061919Z
UID:4657-1459856700-1459860300@www.oa-roma.inaf.it
SUMMARY:The final wind: stars in retirement
DESCRIPTION:Catastrophic mass loss is at the heart of 90% of all stellar\ndeath. Low and intermediate mass stars lose their hydrogen envelope\nwhile on the Asymptotic Giant Branch stars. At the end\, there is\ninsufficient hydrogen left and the star rapidly evolves into a white\ndwarf\, briefly illuminating a planetary nebula on the way. The ejected\ngas can be used to study the superwind\, the nuclear burning and dredge\nup processes in the star\, and even (with some difficulties) the star\nformation histories of the dying stellar population. In this talk I\nwill discuss the planetary nebulae of the Galactic bulge\, briefly\nmention AGB stars in globular clusters\, and finally discuss the origin\nof the mysterious AGB J-type stars\, believed to be the cause of the\nA+B grains in the proto-solar system.
URL:https://www.oa-roma.inaf.it/event/the-final-wind-stars-in-retirement-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160331T114500
DTEND;TZID=Europe/Rome:20160331T124500
DTSTAMP:20260404T221128
CREATED:20160321T061529Z
LAST-MODIFIED:20160321T061529Z
UID:572-1459424700-1459428300@www.oa-roma.inaf.it
SUMMARY:AGN feedback studies: combining SINFONI and ALMA
DESCRIPTION:From a mere ornament in the center of the galaxy\, the Super Massive\nBlack Holes (SMBHs) turned in a potential major actor in shaping the\nfinal stellar mass of its host via the so-called AGN feedback. From\nthe observations there is mounting evidence that AGN outflows are\nubiquitous\, but what is still largely missing are observational proofs\nof the impact that such AGN-driven outflows have on their hosts. I\nwill discuss two complementary approaches to tackle this topic.\nThe first involve the use of Integral Field Spectroscopy in the\nnear-infrared to use kinematical maps of the ionized gas\, as traced by\nthe [OIII] line\, to constrain the energetics of AGN outflows. Our\ngroup has already obtained several results using SINFONI and it has\nnow started a more systematical study via a recently approved Large\nProgramme at VLT. The second approach involve the use of ALMA band-3 observations to\nmeasure molecular gas masses\, via the 12CO(2-1) transition line\, in a\nrepresentative sample of ‘main-sequence’ z~ 1.5 AGNs. We compare the\nstar-formation efficiency and gas fraction of their hosts with those of inactive\ngalaxies in the same range of stellar masses\, SFR and redshifts.
URL:https://www.oa-roma.inaf.it/event/agn-feedback-studies-combining-sinfoni-and-alma/
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160331T114500
DTEND;TZID=Europe/Rome:20160331T124500
DTSTAMP:20260404T221128
CREATED:20160321T061529Z
LAST-MODIFIED:20160321T061529Z
UID:4660-1459424700-1459428300@www.oa-roma.inaf.it
SUMMARY:AGN feedback studies: combining SINFONI and ALMA
DESCRIPTION:From a mere ornament in the center of the galaxy\, the Super Massive\nBlack Holes (SMBHs) turned in a potential major actor in shaping the\nfinal stellar mass of its host via the so-called AGN feedback. From\nthe observations there is mounting evidence that AGN outflows are\nubiquitous\, but what is still largely missing are observational proofs\nof the impact that such AGN-driven outflows have on their hosts. I\nwill discuss two complementary approaches to tackle this topic.\nThe first involve the use of Integral Field Spectroscopy in the\nnear-infrared to use kinematical maps of the ionized gas\, as traced by\nthe [OIII] line\, to constrain the energetics of AGN outflows. Our\ngroup has already obtained several results using SINFONI and it has\nnow started a more systematical study via a recently approved Large\nProgramme at VLT. The second approach involve the use of ALMA band-3 observations to\nmeasure molecular gas masses\, via the 12CO(2-1) transition line\, in a\nrepresentative sample of ‘main-sequence’ z~ 1.5 AGNs. We compare the\nstar-formation efficiency and gas fraction of their hosts with those of inactive\ngalaxies in the same range of stellar masses\, SFR and redshifts.
URL:https://www.oa-roma.inaf.it/event/agn-feedback-studies-combining-sinfoni-and-alma-2/
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160329T114500
DTEND;TZID=Europe/Rome:20160329T124500
DTSTAMP:20260404T221128
CREATED:20160317T062407Z
LAST-MODIFIED:20160317T062407Z
UID:546-1459251900-1459255500@www.oa-roma.inaf.it
SUMMARY:Substructures in protostellar discs: spirals\, gaps and warps
DESCRIPTION:The advent of high resolution imaging of protostellar discs\, both in the sub-mm (thanks to ALMA) and in the near infrared\, has radically changed our understanding of the evolution of such discs and of the planet formation process occuring within them. While in the past disc were modeled as simplified\, axi-symmetric structures\, often characterized by simple radial power-law for density and temperature\, we now need more advanced modeling\, able to describe the substructures observed. Such modeling needs to take into account both the gas component\, that dominates the dynamics and the line emission\, and the dust\, which is responsible for the continuum mm band emission. Here\, I present several aspects of such modeling. I will discuss the theory and some hydrodynamical simulations describing: (a) spiral density waves\, for example induced by gravitational instabilities in young and massive discs; (b) gaps induced by the presence of a forming planet in the disc\, with particular emphasis on the spectacular case of HL Tau\, that we have recently successfully modeled; (c) warps\, which are expected to develop in circumbinary discs\, or in discs where a planet has been put on a very inclined orbit.
URL:https://www.oa-roma.inaf.it/event/substructures-in-protostellar-discs-spirals-gaps-and-warps/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160329T114500
DTEND;TZID=Europe/Rome:20160329T124500
DTSTAMP:20260404T221128
CREATED:20160317T062407Z
LAST-MODIFIED:20160317T062407Z
UID:4659-1459251900-1459255500@www.oa-roma.inaf.it
SUMMARY:Substructures in protostellar discs: spirals\, gaps and warps
DESCRIPTION:The advent of high resolution imaging of protostellar discs\, both in the sub-mm (thanks to ALMA) and in the near infrared\, has radically changed our understanding of the evolution of such discs and of the planet formation process occuring within them. While in the past disc were modeled as simplified\, axi-symmetric structures\, often characterized by simple radial power-law for density and temperature\, we now need more advanced modeling\, able to describe the substructures observed. Such modeling needs to take into account both the gas component\, that dominates the dynamics and the line emission\, and the dust\, which is responsible for the continuum mm band emission. Here\, I present several aspects of such modeling. I will discuss the theory and some hydrodynamical simulations describing: (a) spiral density waves\, for example induced by gravitational instabilities in young and massive discs; (b) gaps induced by the presence of a forming planet in the disc\, with particular emphasis on the spectacular case of HL Tau\, that we have recently successfully modeled; (c) warps\, which are expected to develop in circumbinary discs\, or in discs where a planet has been put on a very inclined orbit.
URL:https://www.oa-roma.inaf.it/event/substructures-in-protostellar-discs-spirals-gaps-and-warps-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160322T114500
DTEND;TZID=Europe/Rome:20160322T124500
DTSTAMP:20260404T221128
CREATED:20160317T062227Z
LAST-MODIFIED:20160317T062227Z
UID:4658-1458647100-1458650700@www.oa-roma.inaf.it
SUMMARY:High ionisation absorption in low mass X-ray binaries
DESCRIPTION:The advent of the new generation of X-ray telescopes yielded a significant step forward in our understanding of ionised absorption generated in the accretion discs of X-ray binaries. It appears now clear that these relatively weak and narrow absorption features\, sporadically present in the X-ray spectra of some systems\, are actually the signature of equatorial outflows\, which might carry away more matter than that being accreted. Therefore\, they play a major role in the accretion phenomenon. These outflows (or ionised atmospheres) are ubiquitous during the softer states but absent during the power-law dominated\, hard states\, suggesting a strong link with the state of the inner accretion disc\, presence of the radio-jet and the properties of the central source. I will review the current understanding of this field.
URL:https://www.oa-roma.inaf.it/event/high-ionisation-absorption-in-low-mass-x-ray-binaries-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160322T114500
DTEND;TZID=Europe/Rome:20160322T124500
DTSTAMP:20260404T221128
CREATED:20160317T062227Z
LAST-MODIFIED:20160317T062227Z
UID:545-1458647100-1458650700@www.oa-roma.inaf.it
SUMMARY:High ionisation absorption in low mass X-ray binaries
DESCRIPTION:The advent of the new generation of X-ray telescopes yielded a significant step forward in our understanding of ionised absorption generated in the accretion discs of X-ray binaries. It appears now clear that these relatively weak and narrow absorption features\, sporadically present in the X-ray spectra of some systems\, are actually the signature of equatorial outflows\, which might carry away more matter than that being accreted. Therefore\, they play a major role in the accretion phenomenon. These outflows (or ionised atmospheres) are ubiquitous during the softer states but absent during the power-law dominated\, hard states\, suggesting a strong link with the state of the inner accretion disc\, presence of the radio-jet and the properties of the central source. I will review the current understanding of this field.
URL:https://www.oa-roma.inaf.it/event/high-ionisation-absorption-in-low-mass-x-ray-binaries/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160315T114500
DTEND;TZID=Europe/Rome:20160315T124500
DTSTAMP:20260404T221128
CREATED:20160216T154302Z
LAST-MODIFIED:20160216T154302Z
UID:453-1458042300-1458045900@www.oa-roma.inaf.it
SUMMARY:Cool\, luminous stars to probe chemistry & kinematics in dusty-extincted stellar systems
DESCRIPTION:Evolved\, cool giants and supergiants are among the brightest stars in any stellar system and are\neasily observable out to large distances.\nWhen observed at infrared wavelengths\, these cool stars can be also used to probe the stellar content\nin environments severely obscured by dust\, such as the central regions of galaxies.\nProgress in our astrophysical comprehension of the stellar content in such extreme environments\ngoes together with the technological advance of IR instrumentation.\nIn this talk I will first present briefly the IR instrument context over the last two decades\,\nand then I will review some of the most recent results in probing stellar chemistry\nand kinematics in the center of the Milky Way and in nearby galaxies.
URL:https://www.oa-roma.inaf.it/event/cool-luminous-stars-to-probe-chemistry-kinematics-in-dusty-extincted-stellar-systems/
LOCATION:Aula Gratton
CATEGORIES:Seminari
ORGANIZER;CN="OAR":MAILTO:info@oa-roma.inaf.it
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160315T114500
DTEND;TZID=Europe/Rome:20160315T124500
DTSTAMP:20260404T221128
CREATED:20160216T154302Z
LAST-MODIFIED:20160216T154302Z
UID:4655-1458042300-1458045900@www.oa-roma.inaf.it
SUMMARY:Cool\, luminous stars to probe chemistry & kinematics in dusty-extincted stellar systems
DESCRIPTION:Evolved\, cool giants and supergiants are among the brightest stars in any stellar system and are\neasily observable out to large distances.\nWhen observed at infrared wavelengths\, these cool stars can be also used to probe the stellar content\nin environments severely obscured by dust\, such as the central regions of galaxies.\nProgress in our astrophysical comprehension of the stellar content in such extreme environments\ngoes together with the technological advance of IR instrumentation.\nIn this talk I will first present briefly the IR instrument context over the last two decades\,\nand then I will review some of the most recent results in probing stellar chemistry\nand kinematics in the center of the Milky Way and in nearby galaxies.
URL:https://www.oa-roma.inaf.it/event/cool-luminous-stars-to-probe-chemistry-kinematics-in-dusty-extincted-stellar-systems-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
ORGANIZER;CN="OAR":MAILTO:info@oa-roma.inaf.it
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160301T114500
DTEND;TZID=Europe/Rome:20160301T124500
DTSTAMP:20260404T221128
CREATED:20160223T182338Z
LAST-MODIFIED:20160223T182338Z
UID:500-1456832700-1456836300@www.oa-roma.inaf.it
SUMMARY:Extreme adaptive optics at the Large Binocular Telescope
DESCRIPTION:After a brief introduction about adaptive optics and the Large Binoculare Telescope\, I will present the LBT’s extreme adaptive optic system. I will show its current capabilities\, main scientific results and the performance improvement offered by the upcoming upgrade. Finally\, I will show how the LBT AO technology impacted the design of the 8m-class and the next generation of ground based telescopes.
URL:https://www.oa-roma.inaf.it/event/extreme-adaptive-optics-at-the-large-binocular-telescope/
LOCATION:Aula Gratton
CATEGORIES:Seminari
ORGANIZER;CN="OAR":MAILTO:info@oa-roma.inaf.it
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160301T114500
DTEND;TZID=Europe/Rome:20160301T124500
DTSTAMP:20260404T221128
CREATED:20160223T182338Z
LAST-MODIFIED:20160223T182338Z
UID:4656-1456832700-1456836300@www.oa-roma.inaf.it
SUMMARY:Extreme adaptive optics at the Large Binocular Telescope
DESCRIPTION:After a brief introduction about adaptive optics and the Large Binoculare Telescope\, I will present the LBT’s extreme adaptive optic system. I will show its current capabilities\, main scientific results and the performance improvement offered by the upcoming upgrade. Finally\, I will show how the LBT AO technology impacted the design of the 8m-class and the next generation of ground based telescopes.
URL:https://www.oa-roma.inaf.it/event/extreme-adaptive-optics-at-the-large-binocular-telescope-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
ORGANIZER;CN="OAR":MAILTO:info@oa-roma.inaf.it
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160223T114500
DTEND;TZID=Europe/Rome:20160223T124500
DTSTAMP:20260404T221128
CREATED:20160216T153808Z
LAST-MODIFIED:20160216T153808Z
UID:451-1456227900-1456231500@www.oa-roma.inaf.it
SUMMARY:Linking massive black hole spin evolution to galactic dynamics
DESCRIPTION:The evolution of the spin of massive black holes (MBHs) is driven by accretion of gas and/or by black hole binary coalescences. I will discuss the physical processes involved in the MBH spin evolution\, and present the results of a semi-analytical model that manages to reproduce the distribution of spins obtained from X-ray spectroscopy.
URL:https://www.oa-roma.inaf.it/event/linking-massive-black-hole-spin-evolution-to-galactic-dynamics/
LOCATION:Aula Gratton
CATEGORIES:Seminari
ORGANIZER;CN="OAR":MAILTO:info@oa-roma.inaf.it
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160223T114500
DTEND;TZID=Europe/Rome:20160223T124500
DTSTAMP:20260404T221128
CREATED:20160216T153808Z
LAST-MODIFIED:20160216T153808Z
UID:4653-1456227900-1456231500@www.oa-roma.inaf.it
SUMMARY:Linking massive black hole spin evolution to galactic dynamics
DESCRIPTION:The evolution of the spin of massive black holes (MBHs) is driven by accretion of gas and/or by black hole binary coalescences. I will discuss the physical processes involved in the MBH spin evolution\, and present the results of a semi-analytical model that manages to reproduce the distribution of spins obtained from X-ray spectroscopy.
URL:https://www.oa-roma.inaf.it/event/linking-massive-black-hole-spin-evolution-to-galactic-dynamics-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
ORGANIZER;CN="OAR":MAILTO:info@oa-roma.inaf.it
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160216T114500
DTEND;TZID=Europe/Rome:20160216T124500
DTSTAMP:20260404T221128
CREATED:20160201T094006Z
LAST-MODIFIED:20160201T094006Z
UID:431-1455623100-1455626700@www.oa-roma.inaf.it
SUMMARY:Metals outside galaxies: what do we learn from observations?
DESCRIPTION:The observed properties and evolution of galaxies in the Universe require the existence of feedback mechanisms regulating the star formation and finally quenching it. The presence of winds\, possibly transporting the gas outside the viral radius\, has been confirmed observationally in local and high redshift objects. In this talk\, I will briefly review how scientist have confirmed the presence of heavy elements outside galaxies using the observation of QSO absorption lines and I will present and discuss new results based on the highest signal-to-noise ratio\, high resolution QSO spectrum ever obtained.
URL:https://www.oa-roma.inaf.it/event/metals-outside-galaxies-what-do-we-learn-from-observations-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160216T114500
DTEND;TZID=Europe/Rome:20160216T124500
DTSTAMP:20260404T221128
CREATED:20160201T094006Z
LAST-MODIFIED:20160201T094006Z
UID:4652-1455623100-1455626700@www.oa-roma.inaf.it
SUMMARY:Metals outside galaxies: what do we learn from observations?
DESCRIPTION:The observed properties and evolution of galaxies in the Universe require the existence of feedback mechanisms regulating the star formation and finally quenching it. The presence of winds\, possibly transporting the gas outside the viral radius\, has been confirmed observationally in local and high redshift objects. In this talk\, I will briefly review how scientist have confirmed the presence of heavy elements outside galaxies using the observation of QSO absorption lines and I will present and discuss new results based on the highest signal-to-noise ratio\, high resolution QSO spectrum ever obtained.
URL:https://www.oa-roma.inaf.it/event/metals-outside-galaxies-what-do-we-learn-from-observations-2-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160209T114500
DTEND;TZID=Europe/Rome:20160209T124500
DTSTAMP:20260404T221128
CREATED:20160201T093819Z
LAST-MODIFIED:20160201T093819Z
UID:430-1455018300-1455021900@www.oa-roma.inaf.it
SUMMARY:May a single hypothesis to explain most of the mysteries of the universe?
DESCRIPTION:A single hypothesis on the properties of the gravitational interaction\nin the presence of antimatter could explain\, simultaneously: the asymmetry\nbetween matter and antimatter at cosmic level\, the inflation\, the effects attributed\nto dark matter and dark energy\, and at elementary particle level CPV and the arrow of time.
URL:https://www.oa-roma.inaf.it/event/may-a-single-hypothesis-to-explain-most-of-the-mysteries-of-the-universe/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160209T114500
DTEND;TZID=Europe/Rome:20160209T124500
DTSTAMP:20260404T221128
CREATED:20160201T093819Z
LAST-MODIFIED:20160201T093819Z
UID:4651-1455018300-1455021900@www.oa-roma.inaf.it
SUMMARY:May a single hypothesis to explain most of the mysteries of the universe?
DESCRIPTION:A single hypothesis on the properties of the gravitational interaction\nin the presence of antimatter could explain\, simultaneously: the asymmetry\nbetween matter and antimatter at cosmic level\, the inflation\, the effects attributed\nto dark matter and dark energy\, and at elementary particle level CPV and the arrow of time.
URL:https://www.oa-roma.inaf.it/event/may-a-single-hypothesis-to-explain-most-of-the-mysteries-of-the-universe-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160202T114500
DTEND;TZID=Europe/Rome:20160202T124500
DTSTAMP:20260404T221128
CREATED:20160122T113632Z
LAST-MODIFIED:20160122T113632Z
UID:4650-1454413500-1454417100@www.oa-roma.inaf.it
SUMMARY:The early growth of (super)massive black holes
DESCRIPTION:With detections of quasars powered by increasingly massive black holes\n(BH) at increasingly early times in cosmic history over the past decade\,\nthere has been correspondingly rapid progress made on the theory of early\nBH formation and growth. I review the emerging picture of how the first\nmassive BHs formed from the primordial gas and then grew to supermassive\nscales\, and discuss the initial conditions for the formation of the\nprogenitors of these seed BHs\, the factors dictating the initial masses\nwith which they form\, and their initialstages of growth via accretion\,\nwhich may occur at super-Eddington rates.
URL:https://www.oa-roma.inaf.it/event/the-early-growth-of-supermassive-black-holes-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
ORGANIZER;CN="OAR":MAILTO:info@oa-roma.inaf.it
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160202T114500
DTEND;TZID=Europe/Rome:20160202T124500
DTSTAMP:20260404T221128
CREATED:20160122T113632Z
LAST-MODIFIED:20160122T113632Z
UID:404-1454413500-1454417100@www.oa-roma.inaf.it
SUMMARY:The early growth of (super)massive black holes
DESCRIPTION:With detections of quasars powered by increasingly massive black holes\n(BH) at increasingly early times in cosmic history over the past decade\,\nthere has been correspondingly rapid progress made on the theory of early\nBH formation and growth. I review the emerging picture of how the first\nmassive BHs formed from the primordial gas and then grew to supermassive\nscales\, and discuss the initial conditions for the formation of the\nprogenitors of these seed BHs\, the factors dictating the initial masses\nwith which they form\, and their initialstages of growth via accretion\,\nwhich may occur at super-Eddington rates.
URL:https://www.oa-roma.inaf.it/event/the-early-growth-of-supermassive-black-holes/
LOCATION:Aula Gratton
CATEGORIES:Seminari
ORGANIZER;CN="OAR":MAILTO:info@oa-roma.inaf.it
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160126T114500
DTEND;TZID=Europe/Rome:20160126T130000
DTSTAMP:20260404T221128
CREATED:20160120T103420Z
LAST-MODIFIED:20160120T103420Z
UID:384-1453808700-1453813200@www.oa-roma.inaf.it
SUMMARY:Exploring the realm of an AGN
DESCRIPTION:The environment of Active Galactic Nuclei (AGN) is the result of accretion and injection of matter in and around a supermassive black hole. Through high resolution X-ray spectroscopy of both present and future instruments\, the most extreme gas environments of the AGN can be studied. In this talk I will present our recent results on outflows and obscuration in AGN. I will also illustrate the tremendous improvement that future instruments will offer in this field.
URL:https://www.oa-roma.inaf.it/event/exploring-the-realm-of-an-agn/
LOCATION:Aula Gratton
CATEGORIES:Seminari
ORGANIZER;CN="OAR":MAILTO:info@oa-roma.inaf.it
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20160126T114500
DTEND;TZID=Europe/Rome:20160126T130000
DTSTAMP:20260404T221128
CREATED:20160120T103420Z
LAST-MODIFIED:20160120T103420Z
UID:4649-1453808700-1453813200@www.oa-roma.inaf.it
SUMMARY:Exploring the realm of an AGN
DESCRIPTION:The environment of Active Galactic Nuclei (AGN) is the result of accretion and injection of matter in and around a supermassive black hole. Through high resolution X-ray spectroscopy of both present and future instruments\, the most extreme gas environments of the AGN can be studied. In this talk I will present our recent results on outflows and obscuration in AGN. I will also illustrate the tremendous improvement that future instruments will offer in this field.
URL:https://www.oa-roma.inaf.it/event/exploring-the-realm-of-an-agn-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
ORGANIZER;CN="OAR":MAILTO:info@oa-roma.inaf.it
END:VEVENT
END:VCALENDAR