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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:20180325T010000
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BEGIN:STANDARD
TZOFFSETFROM:+0200
TZOFFSETTO:+0100
TZNAME:CET
DTSTART:20181028T010000
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BEGIN:DAYLIGHT
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TZOFFSETTO:+0200
TZNAME:CEST
DTSTART:20190331T010000
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TZOFFSETFROM:+0200
TZOFFSETTO:+0100
TZNAME:CET
DTSTART:20191027T010000
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TZOFFSETFROM:+0100
TZOFFSETTO:+0200
TZNAME:CEST
DTSTART:20200329T010000
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DTSTART:20201025T010000
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BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20191210T114500
DTEND;TZID=Europe/Rome:20191210T124500
DTSTAMP:20260405T010041
CREATED:20190723T112945Z
LAST-MODIFIED:20191204T155611Z
UID:6537-1575978300-1575981900@www.oa-roma.inaf.it
SUMMARY:Characterizing multi-phase gas outflows and their powering mechanism in nearby AGN
DESCRIPTION:Active Galactic Nuclei are thought to play a crucial role in\nthe evolution of massive galaxies. In particular\, fast outflows are\nfrequently observed in AGN covering various gas phases which may remove\na significant fraction of the gas content from the galaxies. I will\nreview the current state of research in this very active field of\nongoing research together with the advantages and disadvantages of\nprevious approaches. In particular\, I will highlight the importance of\nmulti-wavelength observations to unravel the true multi-phase nature of\noutflows by combining state-of-the-art observational facilities. In this\ncontext I will present the first results from the ongoing Close AGN\nReference Survey (CARS)\, a multi-wavelength survey of 39 luminous\nlow-redshift unobscured AGN with extensive observations from VLT/MUSE\,\nALMA\, VLA\, Chandra\, SOFIA and many more. In addition\, I will present the\nmulti-phase view of the famous ultra-luminous Quasar 3C273 where we\nunlocked a few unknown secrets.
URL:https://www.oa-roma.inaf.it/event/colloquium-bernd-husemann/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20191203T114500
DTEND;TZID=Europe/Rome:20191203T124500
DTSTAMP:20260405T010041
CREATED:20190723T160231Z
LAST-MODIFIED:20191201T160753Z
UID:6544-1575373500-1575377100@www.oa-roma.inaf.it
SUMMARY:Acoustic oscillations and dynamo action in giants
DESCRIPTION:The role of the magnetic field in determining the angular momentum  transport in stellar interior is still an open issue. Acoustic oscillations are directly affected by the presence of a large-scale magnetic field but their study can provide fundamental information on the properties of the magnetic fields in solar-like stars. As an example the case of  EK Eridani\, a slowly rotating\, overactive G8 giant\, will be presented.  Moreover the possibility to use asteroseismology to solve the  long-lasting mystery on the origin of magnetic fields in Ap stars will be discussed.
URL:https://www.oa-roma.inaf.it/event/alfio-bonanno-colloquium/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20191126T114500
DTEND;TZID=Europe/Rome:20191126T124500
DTSTAMP:20260405T010041
CREATED:20190919T100822Z
LAST-MODIFIED:20191123T102647Z
UID:6767-1574768700-1574772300@www.oa-roma.inaf.it
SUMMARY:LSST: an opportunity for the Italian Community
DESCRIPTION:We review the current status of the LSST project\, its expected performances\, the key science goals and the involvment of the Italian Community
URL:https://www.oa-roma.inaf.it/event/colloquium-giuliana-fiorentino/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20191125T080000
DTEND;TZID=Europe/Rome:20191128T170000
DTSTAMP:20260405T010041
CREATED:20191122T181336Z
LAST-MODIFIED:20191122T181336Z
UID:7116-1574668800-1574960400@www.oa-roma.inaf.it
SUMMARY:workshop Stamerra
DESCRIPTION:
URL:https://www.oa-roma.inaf.it/event/workshop-stamerra/
LOCATION:Aula Gratton
CATEGORIES:Congressi
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20191118T090000
DTEND;TZID=Europe/Rome:20191122T180000
DTSTAMP:20260405T010041
CREATED:20190111T102035Z
LAST-MODIFIED:20190111T102139Z
UID:5155-1574067600-1574445600@www.oa-roma.inaf.it
SUMMARY:Lithium in the Universe: to Be or not to Be
DESCRIPTION:
URL:https://www.oa-roma.inaf.it/event/lithium-in-the-universe-to-be-or-not-to-be/
LOCATION:OAR Monte Porzio Catone – aula Gratton\, Via Frascati 33\, Roma\, RM\, 00136\, Italia
CATEGORIES:Congressi
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20191115T160000
DTEND;TZID=Europe/Rome:20191115T170000
DTSTAMP:20260405T010041
CREATED:20191108T072725Z
LAST-MODIFIED:20191108T075652Z
UID:7070-1573833600-1573837200@www.oa-roma.inaf.it
SUMMARY:Dal Sole a Sedna: una passeggiata per il sistema solare\, e uno sguardo più in là
DESCRIPTION:Dal 1959 ad oggi più di cento sonde spaziali hanno lasciato la Terra verso la Luna e lo spazio profondo. Queste appendici robotica dei nostri sensi hanno visitato tutti i pianeti e i principali satelliti del sistema solare\, rivelando una straordinaria e inattesa varietà di forme e fenomeni. Ripercorrere vent’anni di scoperte sarà un tributo all’ingegno di quanti le hanno rese possibili. Grazie alle immagini più belle raccolte negli ultimi anni\, la conferenza ripercorrerà le scoperte più significative nell’esplorazione del sistema solare\, gettando infine uno sguardo ai pianeti delle stelle vicine. Forse tra questi ne esiste qualcuno che ospita la vita? Come trovarlo?
URL:https://www.oa-roma.inaf.it/event/dal-sole-a-sedna-una-passeggiata-per-il-sistema-solare-e-uno-sguardo-piu-in-la/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20191114T114500
DTEND;TZID=Europe/Rome:20191114T124500
DTSTAMP:20260405T010041
CREATED:20191023T064535Z
LAST-MODIFIED:20191031T064029Z
UID:7011-1573731900-1573735500@www.oa-roma.inaf.it
SUMMARY:Lithium in the local Volume
DESCRIPTION:We present our recent study on the chemical evolution of lithium in the thin disc of the Milky Way.\nWe found that the best agreement with the observed Li abundances in the thin disc is obtained\nconsidering novae as the main source of lithium. We assumed a delay time of ≈1 Gyr  for nova\nproduction and an effective 7Li yield of 1.8(± 0.6)×10−5 Msun over the whole nova lifetime.\nThe possibility to check our detailed assumptions on lithium production on other stellar systems\, such\nas the satellites of our Milky Way\, is seriously hampered by their distance from us. In these  systems\ndwarf stars (where the original lithium can be measured) are too faint to detect lithium lines.\nHowever\, thanks to the Gaia mission\, it was recently possible to disentangle the stars of a disrupted\ndwarf galaxy in the Galactic halo (called Enceladus or Galactic sausage). Adopting a chemical evolution\nmodel able to match the chemical enrichment in alpha elements and the metallicity distribution function\nof Enceladus\, we present our prediction for the lithium abundance of the stars of this disrupted galaxy.
URL:https://www.oa-roma.inaf.it/event/colloquium-gabriele-cescutti/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20191108T114500
DTEND;TZID=Europe/Rome:20191108T124500
DTSTAMP:20260405T010041
CREATED:20191105T085225Z
LAST-MODIFIED:20191105T085225Z
UID:7038-1573213500-1573217100@www.oa-roma.inaf.it
SUMMARY:The ultraluminous X-ray pulsar NGC 5907 ULX-1 and its nebula
DESCRIPTION:Ultraluminous X-ray pulsars are accretion-powered pulsars whose X-ray\nluminosity\, if isotropic\, largely exceeds their Eddington limit. Only a handful\nare known to date and NGC 5907 ULX-1\, distant 17 Mpc from us\, is the most luminous of them\,\nat 1e41 erg/s 500 times its Eddington limit. We constrained through\npulsar timing its orbit and spin behavior\, estimating a 5d orbital period and a spin-up\ntime <40 yr. We detected an extended X-ray feature surrounding the source: likely a young and\npowerful bubble driven by the wind from the accreting pulsar system. The nebula\nhas been powered at ~1e41 erg/s for ~70 kyr proving that a highly super-Eddington\nregime can be sustained for much longer than the spin-up time of the pulsar.\nI will present the current status of the observations and understanding of this system\nand the prospects to solve the still open problems it raises.
URL:https://www.oa-roma.inaf.it/event/the-ultraluminous-x-ray-pulsar-ngc-5907-ulx-1-and-its-nebula/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20191105T114500
DTEND;TZID=Europe/Rome:20191105T124500
DTSTAMP:20260405T010041
CREATED:20191016T061058Z
LAST-MODIFIED:20191030T155258Z
UID:6926-1572954300-1572957900@www.oa-roma.inaf.it
SUMMARY:The impact of AGB stars on the life of stellar systems
DESCRIPTION:During the latest phases of their lives\, low-intermediate mass stars (M<8Msun) evolve through the Asymptotic Giant branch (AGB) phase. Although very rapid\, the AGB phase represents a crucial step for the chemical evolution of the system where these stars form. The reason is that AGB stars undergo an advanced nucleosynthesis and experiment dredge-up events\, while they progressively lose the majority of their mass through stellar winds. Furthermore\, the low temperature and high densisty of their stellar winds prove extremely favourable conditions for dust condensation in the circumstellar envelopes. All the reprocessed gas and dust lost by the AGB stars enrich the insterstellar medium of the host system. Detailed modelling of these complex physical processes are essential to reconstruct the impact that these stars had on the history of formation and chemical evolution of stellar clusters and galaxies. In this talk I will present how the latest generation of AGB+dust evolutionary models has been recently used to this scope in different environments: from globular clusters\, to unveil the origine of multiple populations\, to Local Group dwarf galaxies\, to infer star formation history and dust production rate.
URL:https://www.oa-roma.inaf.it/event/colloquium-flavia-dellagli/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20191029T114500
DTEND;TZID=Europe/Rome:20191029T124500
DTSTAMP:20260405T010041
CREATED:20191020T043613Z
LAST-MODIFIED:20191020T043613Z
UID:6990-1572349500-1572353100@www.oa-roma.inaf.it
SUMMARY:Post-AGB stars as tracers of the origin of elements in the Universe
DESCRIPTION:The chemical evolution of galaxies is governed by the chemical yields from stars\, especially from Asymptotic Giant Branch (AGB) stars. This underlines the importance of understanding how AGB stars produce their elements by obtaining accurate stellar nucleosynthetic yields. Although AGB nucleosynthesis has general validity\, critical uncertainties (such as the treatment of convective-driven mixing processes and mass loss) exist in current stellar models. Observations from Post-Asymptotic Giant Branch (post-AGB) stars serve as excellent tools to confront predictions from a dedicated suite of stellar models\, quantify the strongest discrepancies\, and eliminate crucial uncertainties that hamper stellar modelling. Our recent studies of post-AGB stars have shown an intriguing chemical diversity that ranges from stars that are extremely enriched in carbon and s-process elements to the discovery of the first post-AGB star with no traces of carbon nor s-process elements. Additionally\, our studies have also shown that AGB nucleosynthesis is significantly affected by a binary companion. These results reflect the complexity that surrounds the element production in AGB stars. In this talk\, I will present the intriguing chemical diversity observed in post-AGB stars and its implications on element/isotope production in AGB stars and stellar nucleosynthetic yields.
URL:https://www.oa-roma.inaf.it/event/post-agb-stars-as-tracers-of-the-origin-of-elements-in-the-universe/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20191022T114500
DTEND;TZID=Europe/Rome:20191022T124500
DTSTAMP:20260405T010041
CREATED:20191007T104849Z
LAST-MODIFIED:20191008T082548Z
UID:6886-1571744700-1571748300@www.oa-roma.inaf.it
SUMMARY:Linear spectropolarimetry in stars different than the Sun: what can we learn?
DESCRIPTION:Polarimetry is considered as an important searching tool in Astronomy and it deserves to be a standard observational technique for a variety of astrophysical contexts: from stellar photospheric inhomogeneities to protoplanetary nebulae\, as well as in the exoplanet research field. Despite this\, however\, the difficulties involved in the measurements and in the theoretical interpretation made this technique not as widespread as it deserves. In this talk I will review the results of my research about the diagnostic potential of optical high resolution linear spectropolarimetry in stars different than the Sun.  At this purpose\, after an introduction on the observational technique\, I will focus on the polarised spectrum of the post-AGB binary system 89 Herculis: from the very inner regions of the stellar envelope to the first observational evidence of a micro-Gauss level magnetic field. Finally\, I will discuss on the applicability and future prospect of this technique in the more general context of stellar physics.
URL:https://www.oa-roma.inaf.it/event/colloquium-manuele-ganci/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20191015T114500
DTEND;TZID=Europe/Rome:20191015T134500
DTSTAMP:20260405T010041
CREATED:20190913T082524Z
LAST-MODIFIED:20191008T061431Z
UID:6725-1571139900-1571147100@www.oa-roma.inaf.it
SUMMARY:Horizontal Branch morphologies in the age of multi-band photometry
DESCRIPTION:The Horizontal Branch (HB) stars have always played a crucial role in the study of the galactic globular clusters (GC). They are the direct offspring of the low mass\, Red Giant Branch (RGB) stars and the final product of the helium flash taking place at the Tip of the RGB. The colour and the luminosity of a HB star are tied to its mass which\, in turn\, is tied to the mass of the star undergoing the flash. The sensitivity of this value to the chemistry of the cluster allows for a large variety of HB morphologies which is one of the culprits that led to the discovery of the multiple populations phenomenon. A leap forward in our understanding of GCs has been made when recent works\, based on a large collection of HST data\, measured\, albeit indirectly\, the helium abundance in a large collection of GCs\, allowing the characterization of these old stellar populations in unprecedented ways. In spite of this richness of information\, however\, we still lack the key to fully understand the populations hosted along the HB\, especially due to the complex interplay between the parameters regulating their evolution. In this talk\, I will provide a review of the current state of the HB study and discuss how the synergy with the recent advancements in the field of multi-band photometry can provide solutions to some new and decades-old problems.
URL:https://www.oa-roma.inaf.it/event/colloquium-marco-tailo/
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20191010T114500
DTEND;TZID=Europe/Rome:20191010T124500
DTSTAMP:20260405T010041
CREATED:20191004T065258Z
LAST-MODIFIED:20191004T065258Z
UID:6873-1570707900-1570711500@www.oa-roma.inaf.it
SUMMARY:Dynamic relations in sampled processes
DESCRIPTION:I will start my talk by a short description of a historical connection between my university\, Shanghai Jiao Tong University (SJTU)\, and Collegio Romano. There is an interesting chain from Clavius\, who led the Gregorian calendar reform\, via Matteo Ricci and Xu Guangqi\, the first modern scientist of China\, to the founding of the two elite universities on Shanghai\, Fudan and SJTU. The technical part of my talk is based on joint work with Tryphon Georgiou. Linear dynamical relations that may exist in continuous-time\, or at some natural sampling rate\, are not directly discernable at reduced observational sampling rates. Indeed\, at reduced rates\, matrix-valued spectral densities of vector-valued time series have maximal rank and thereby cannot be used to ascertain potential dynamic relations between their entries. This hitherto undeclared source of inaccuracies appears to plague off-the-shelf identification techniques seeking remedy in hypothetical observational noise. In this paper we explain the exact relation between stochastic models at different sampling rates and show how to construct stochastic models at the finest time scale that data allows. We then point out that the correct number of dynamical dependences can only be ascertained by considering stochastic models at this finest time scale\, which in general is faster than the observational sampling rate.
URL:https://www.oa-roma.inaf.it/event/dynamic-relations-in-sampled-processes/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20191003T114500
DTEND;TZID=Europe/Rome:20191003T124500
DTSTAMP:20260405T010041
CREATED:20190902T141633Z
LAST-MODIFIED:20190926T090644Z
UID:6683-1570103100-1570106700@www.oa-roma.inaf.it
SUMMARY:Early galaxy formation and its large-scale effects
DESCRIPTION:Galaxy formation in the first billion years mark a time of great upheaval in the history of the Universe: as the first sources of light\, these galaxies ended the ‘cosmic dark ages’ and produced the first photons that could break apart the hydrogen atoms suffusing all of space starting the process of cosmic reionization. As the earliest building blocks\, the galaxies that formed in the first billion years also determine the physical properties of all subsequent galaxy populations. I will start by introducing the reionization process and detail the reasons foe which the history and topology of reionization remain debated. I will then show how cross-correlations of 21cm data with the underlying galaxy population\, in the forthcoming era of 21cm cosmology\, will yield tantalising constraints on the average intergalactic medium ionization state as well as the reionization toplogy (outside-in versus inside-out). Time permitting\, I will try to give a flavour of how the assembly of early galaxies\, accessible with the forthcoming James Webb Space Telescope\, can provide a powerful testbed for Dark Matter models beyond “Cold Dark Matter”.
URL:https://www.oa-roma.inaf.it/event/colloquium-pratika-dayal/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20191001T114500
DTEND;TZID=Europe/Rome:20191001T124500
DTSTAMP:20260405T010041
CREATED:20190612T065612Z
LAST-MODIFIED:20190612T065612Z
UID:6287-1569930300-1569933900@www.oa-roma.inaf.it
SUMMARY:colloquium - Chris Sneden
DESCRIPTION:
URL:https://www.oa-roma.inaf.it/event/colloquium-chris-sneden/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20190926T114500
DTEND;TZID=Europe/Rome:20190926T124500
DTSTAMP:20260405T010041
CREATED:20190612T065845Z
LAST-MODIFIED:20190925T064343Z
UID:6291-1569498300-1569501900@www.oa-roma.inaf.it
SUMMARY:Modeling stellar winds on the asymptotic giant branch accurately
DESCRIPTION:I present the latest progress on our ongoing work with our state-of-the-art\nmodels of stellar winds of asymptotic giant branch stars. I will both depict\nfeatures and assumptions of our model code T-800 and show some of the results\nthat set our work apart; because\, results are in several a case drastically\ndifferent from earlier results. In particular\, I focus on effects of\ngas-to-dust drift and higher-than-before spatial resolution.
URL:https://www.oa-roma.inaf.it/event/chris-sandin-colloquium/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20190924T143000
DTEND;TZID=Europe/Rome:20190924T153000
DTSTAMP:20260405T010041
CREATED:20190612T065744Z
LAST-MODIFIED:20190913T070536Z
UID:6289-1569335400-1569339000@www.oa-roma.inaf.it
SUMMARY:Lars Mattsson - colloquium
DESCRIPTION:
URL:https://www.oa-roma.inaf.it/event/lars-mattsson-colloquium/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20190916T114500
DTEND;TZID=Europe/Rome:20190916T124500
DTSTAMP:20260405T010041
CREATED:20190730T120235Z
LAST-MODIFIED:20190910T150513Z
UID:6567-1568634300-1568637900@www.oa-roma.inaf.it
SUMMARY:Absorption and accretion properties of local Active Galactic Nuclei
DESCRIPTION:Active Galactic Nuclei (AGN) are powered by accretion onto supermassive black holes and\, besides being among the most luminous sources of radiation in the Universe\, are also widely believed to play an important role in the evolution of their host galaxies.\nX-ray emission is an ubiquitous property of AGN and\, being produced within a few gravitational radii from the supermassive black hole\, can provide fundamental information about the structure and geometry of the circumnuclear material\, as well as on the characteristics of the accretion flow. In my talk I will present recent studies of the obscuration and accretion properties of local AGN in the X-ray band\, focussing on the results obtained from the Swift/BAT AGN Spectroscopic Survey. \n 
URL:https://www.oa-roma.inaf.it/event/colloquium-claudio-ricci/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20190625T114500
DTEND;TZID=Europe/Rome:20190625T124500
DTSTAMP:20260405T010041
CREATED:20181130T090752Z
LAST-MODIFIED:20190522T150749Z
UID:5043-1561463100-1561466700@www.oa-roma.inaf.it
SUMMARY:Unravelling the Andromeda Galaxy's most important merger
DESCRIPTION:The Andromeda Galaxy (M31)\, our nearest large galactic neighbour\, offers a unique opportunity to test how mergers affect galaxy properties. M31’s stellar halo caused by the tidal disruption of satellite galaxies is the best tracer of the galaxy’s accretion history. Despite a decade of effort in mapping out M31’s large stellar halo\, we are unable to convert M31’s stellar halo into a merger history. Here we use cosmological models of galaxy formation to show that M31’s massive and metal-rich stellar halo containing intermediate age stars implies that it merged with a large (M* ~ 2.5 x 10^10 M_sun) galaxy ~2 Gyr ago. The simulated properties of the merger debris help to interpret a broader set of observations of M31’s stellar halo and satellites than previously considered: its compact and metal-rich satellite M32 is the tidally-stripped core of the disrupted galaxy\, M31’s rotating and flattened inner stellar halo contains most of the merger\ndebris\, and the giant stellar stream is likely to have been thrown out during the merger. This accreted galaxy was the third largest member of the Local Group. This merger may explain the global burst of star formation ~2 Gyr ago in the disk of M31 in which ~1/5 of its stars were formed. Moreover\, M31’s disk and bulge were already in place before its most important merger\, suggesting that mergers of this magnitude do not dramatically affect galaxy structure.
URL:https://www.oa-roma.inaf.it/event/colloquium-alessio-marino/
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20190618T114500
DTEND;TZID=Europe/Rome:20190618T124500
DTSTAMP:20260405T010041
CREATED:20190222T092344Z
LAST-MODIFIED:20190531T163519Z
UID:5490-1560858300-1560861900@www.oa-roma.inaf.it
SUMMARY:The eye of Gaia on globular clusters dynamics
DESCRIPTION:I present the results of a survey of the kinematics of a large sample of Galactic globular clusters performed thanks to the synergy between the 2nd Gaia data release and the most extensive collection of radial velocities. This unprecedented dataset of 3D velocities of thousand of stars in more than 100 globular clusters has been used to investigate both the internal (masses\, anisotropy and rotation patterns) and the systemic dynamics (orbits\, tides) of these stellar systems providing also insight into the overall structure of the Galactic globular cluster system.
URL:https://www.oa-roma.inaf.it/event/colloquium-antonio-sollima/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20190613T114500
DTEND;TZID=Europe/Rome:20190613T124500
DTSTAMP:20260405T010041
CREATED:20190405T105451Z
LAST-MODIFIED:20190408T052554Z
UID:5898-1560426300-1560429900@www.oa-roma.inaf.it
SUMMARY:Probing Dark Matter and Dark Energy with strong gravitational lensing
DESCRIPTION:Evidence from different cosmological probes have lead to the establishment of the dark matter and dark energy paradigm. Dark matter dominates the matter budget at cosmological scales and drives the formation of structure and dark energy is responsible for the late time acceleration of the universe. To date\, these phenomenas have purely been described as gravitational effects and no other evidence have provided convincing evidence for their underlying physical nature – remaining one of the most striking mysteries the universe has not yet revealed.\nIn my talk\, I will describe the phenomena of strong gravitational lensing and how we can use this unique probe to constrain the physical nature of dark matter and dark energy. I am going to highlight recent results in both domains. I will then look in the near future and highlight the prospects of this technique with increasing sample size\, analysis techniques and instrumentation.
URL:https://www.oa-roma.inaf.it/event/simon-birrer-colloquium/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20190611T114500
DTEND;TZID=Europe/Rome:20190611T124500
DTSTAMP:20260405T010041
CREATED:20190328T073046Z
LAST-MODIFIED:20190328T073046Z
UID:5792-1560253500-1560257100@www.oa-roma.inaf.it
SUMMARY:Orlando Luongo - colloquium
DESCRIPTION:
URL:https://www.oa-roma.inaf.it/event/orlando-luongo-colloquium/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20190528T114500
DTEND;TZID=Europe/Rome:20190528T124500
DTSTAMP:20260405T010041
CREATED:20190220T133740Z
LAST-MODIFIED:20190506T221609Z
UID:5473-1559043900-1559047500@www.oa-roma.inaf.it
SUMMARY:Protoclusters of galaxies: from Planck to the Euclid and JWST era
DESCRIPTION:Clusters of galaxies are key structures for our understanding of galaxy\nevolution physics in denser environments\, for constraining the structure\nformation scenario and some cosmological parameters independantly of\nother techniques like CMB. Despite the difficulties to observe\, detect\nand model them\, there are successes in studying and using galaxy\nclusters. In the recent years\, many hight-redshift galaxy clusters (z>1)\nwere detected as well as many high-redshift protoclusters (z>1.5)\,\nprogenitors of todays’s clusters. These objects help answering crucial\nquestions like how and when the clusters formed stars ? In a\nsynchroneous way ? What is the fate of the gas in clusters ? \nAfter a review of the current status of protoclusters search and\nproperties and the latest results\, I will focus on the original program\nwe are performing with Planck\, Herschel\, Spitzer\, IRAM\, ALMA and other\nfacilities. \nWe selected an original sample of about 2000 highly star-forming\nstructures candidates in Planck\, deep in the Cosmic Infrared Background.\nSelection was not done in SZ\, but by colors of the redshifted peak of\nthermal far-infrared emission of galaxies. We observed about 200 of them\nwith Herschel/SPIRE\, about 80 of them with Spitzer/IRAC\, and about a\ndozen in the near-infrared and millimeter ranges. We have a few redshift\nconfirmations\, and I will highlight our main findings\, work in progress\,\nand perspectives of the SPHerIC subsample (Spitzer\, Planck\, Herschel\ninfrared clusters). \nA colleague said wisely about high-redshift clusters and protoclusters\nin a review talk\, « we need more than one object at a time. » Euclid and\nJWST will make evolve this field (and other) after 2021 with increasing\nstatistics and a sharp\, detailed view of these structures at the\n« cosmic noon » epoch and earlier.
URL:https://www.oa-roma.inaf.it/event/colloquium-herve-dole/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20190521T114500
DTEND;TZID=Europe/Rome:20190521T124500
DTSTAMP:20260405T010041
CREATED:20190304T101823Z
LAST-MODIFIED:20190506T221827Z
UID:5532-1558439100-1558442700@www.oa-roma.inaf.it
SUMMARY:The first image of a black hole
DESCRIPTION:I will briefly discuss how the first image of a black hole was obtained\nby the EHT collaboration. In particular\, I will describe the theoretical\naspects that have allowed us to model the dynamics of the plasma\naccreting onto the black hole and how such dynamics was used to generate\nsynthetic black-hole images. I will also illustrate how the comparison\nbetween the theoretical images and the observations has allowed us to\ndeduce the presence of a black hole in M87 and to extract information\nabout its properties. Finally\, I will describe the lessons we have\nlearned about strong-field gravity and alternatives to black holes.
URL:https://www.oa-roma.inaf.it/event/colloquium-valentina-dorazi/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20190514T114500
DTEND;TZID=Europe/Rome:20190514T124500
DTSTAMP:20260405T010041
CREATED:20180725T070555Z
LAST-MODIFIED:20180725T070555Z
UID:4176-1557834300-1557837900@www.oa-roma.inaf.it
SUMMARY:colloquium - Francoise Combes
DESCRIPTION:
URL:https://www.oa-roma.inaf.it/event/colloquium-francoise-combes/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20190514T114500
DTEND;TZID=Europe/Rome:20190514T124500
DTSTAMP:20260405T010041
CREATED:20180725T070555Z
LAST-MODIFIED:20190502T064008Z
UID:4759-1557834300-1557837900@www.oa-roma.inaf.it
SUMMARY:Molecular tori\, black hole fueling and feedback in nearby AGN
DESCRIPTION:Recent molecular line observations with ALMA in several nearby Seyferts have revealed the existence of molecular tori\, and the nature of gas flows at 10-20pc scale. At 100pc scale\, or kpc-scale\, previous work on gravitational torques had shown that only about one third of Seyfert galaxies experienced molecular inflow and central fueling\, while in most cases the gas was stalled in rings. At higher resolution\, i.e. 10-20pc scale\, it is possible now to see in some cases AGN fueling due to nuclear trailing spirals\, influenced by the black hole potential. This brings smoking gun evidence for nuclear fueling. In our sample galaxies\, the angular resolution of up to 80mas allows us to reach the BH-zone of influence and the BH mass can be derived more directly than with the M-sigma relation.
URL:https://www.oa-roma.inaf.it/event/colloquium-francoise-combes-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20190507T114500
DTEND;TZID=Europe/Rome:20190507T124500
DTSTAMP:20260405T010041
CREATED:20180725T070642Z
LAST-MODIFIED:20180725T070642Z
UID:4178-1557229500-1557233100@www.oa-roma.inaf.it
SUMMARY:colloquium - Mauro Centrone
DESCRIPTION:
URL:https://www.oa-roma.inaf.it/event/colloquium-mauro-centrone/
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20190416T114500
DTEND;TZID=Europe/Rome:20190416T124500
DTSTAMP:20260405T010041
CREATED:20190111T094223Z
LAST-MODIFIED:20190408T153611Z
UID:5149-1555415100-1555418700@www.oa-roma.inaf.it
SUMMARY:Lithium Web in astrophysics: insights and problems
DESCRIPTION:Lithium (Li) is widely used as a test of the cosmological model\, a probe of stellar structure\, and an age indicator of young stellar clusters. It is the very element that presents deep insights\, yet many problems to astrophysics.\nI will discuss problems and puzzles that Li introduces in astrophysics\, including cosmological Li problem (and a stellar solution to it)\, Li-rich giants problem (Galactic and extraGalactic)\, Li problem in the Sun\, the Galactic Li evolution (in the thin and thick discs)\, and the interstellar Li content. \n 
URL:https://www.oa-roma.inaf.it/event/colloquium-xiaoting-fu/
LOCATION:OAR Monte Porzio Catone – aula Gratton\, Via Frascati 33\, Roma\, RM\, 00136\, Italia
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20190409T114500
DTEND;TZID=Europe/Rome:20190409T124500
DTSTAMP:20260405T010041
CREATED:20190111T092938Z
LAST-MODIFIED:20190403T123956Z
UID:5146-1554810300-1554813900@www.oa-roma.inaf.it
SUMMARY:A MUSE view of the multiple populations' chemistry in Galactic Globular Clusters
DESCRIPTION:Stars in Galactic globular clusters are known to exhibit abundance variations in specific elements such as He\, C\, N\, O\, Na\, and Al. These variations can be observed via spectroscopy but also photometrically by using CMD constructed with various filter combinations. Although these multiple populations have been\, and still are\, the subject of many investigations\, the origin of their elemental abundance variations remain rather mysterious.\nI will present some of our recent results on that topic based on the spectroscopic survey of 26 globular clusters that is currently carried out as part of the MUSE GTO time. With the MUSE survey covering the central regions of the clusters for which HST photometry is available\, we can use these photometric catalogs to separate the RGB stars into two or more populations based on their position in the pseudo-two-color diagrams. Although the MUSE spectra are of relatively low-resolution (R ~ 2500)\, by combining the spectra of the stars within a distinct populations\, we are able to study their abundance variations and relate them directly with the populations distinguished on the pseudo-two-color diagrams.
URL:https://www.oa-roma.inaf.it/event/talk-by-marylin-latour/
LOCATION:OAR Monte Porzio Catone – aula Gratton\, Via Frascati 33\, Roma\, RM\, 00136\, Italia
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20190326T114500
DTEND;TZID=Europe/Rome:20190326T124500
DTSTAMP:20260405T010041
CREATED:20181008T060951Z
LAST-MODIFIED:20181008T060951Z
UID:4432-1553600700-1553604300@www.oa-roma.inaf.it
SUMMARY:colloquium - Elena Valenti
DESCRIPTION:
URL:https://www.oa-roma.inaf.it/event/colloquium-elena-valenti/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
END:VCALENDAR