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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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BEGIN:VTIMEZONE
TZID:Europe/Rome
BEGIN:DAYLIGHT
TZOFFSETFROM:+0100
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TZNAME:CEST
DTSTART:20160327T010000
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TZOFFSETTO:+0100
TZNAME:CET
DTSTART:20161030T010000
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TZOFFSETTO:+0200
TZNAME:CEST
DTSTART:20170326T010000
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DTSTART:20171029T010000
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DTSTART:20180325T010000
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DTSTART:20181028T010000
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BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171107T114500
DTEND;TZID=Europe/Rome:20171107T124500
DTSTAMP:20260406T233435
CREATED:20170728T201847Z
LAST-MODIFIED:20170728T201847Z
UID:4716-1510055100-1510058700@www.oa-roma.inaf.it
SUMMARY:The BH mass - galaxy scaling relations in the local Universe: what is the role of type 2 AGN?
DESCRIPTION:Coevolutionary models that link the growth of supermassive black holes (BHs) and of their host galaxies are based on the observations of tight scaling relations between the BH mass and some properties of the host bulge. These relations have been calibrated thanks to the direct measurements of the BH mass in local galaxies and are extremely important\, used to measure BH masses at high redshift and to determine the distribution of accreted mass\, i.e. the black hole mass function.\nHowever\, these relations seem to be biased in favour of the more massive BHs\, due to a bias in the resolution of the BH sphere of influence. Hence\, there is urgent need to explore the full distribution of BH masses\, accumulating sources below 1e+7 solar masses.\nI here present the results from a systematic study performed using deep NIR (VLT and LBT) spectroscopy of a sample of ~40 type 2 active galactic nuclei (AGN)\, drawn from the complete SWIFT/BAT 70-month hard (14-195 keV) X-ray catalogue. Thanks to our new virial relation based on unbiased physical quantities\, i.e. hard X-ray luminosity and Paβ emission line FWHM\, we have been able to measure for the first time in a virial way the supermassive black hole masses of type 2 AGN\, whose values have been up today estimated using indirect proxies (e.g. from scaling relations). With direct virial masses for type 2 AGN\, we discuss\, for the first time\, if the BH-host galaxy scaling relations hold for type 2 AGN\, thus putting a missing piece to the AGN/galaxy co-evolution puzzle.
URL:https://www.oa-roma.inaf.it/event/seminar-by-federica-ricci-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171107T114500
DTEND;TZID=Europe/Rome:20171107T124500
DTSTAMP:20260406T233435
CREATED:20170728T201847Z
LAST-MODIFIED:20170728T201847Z
UID:3358-1510055100-1510058700@www.oa-roma.inaf.it
SUMMARY:The BH mass - galaxy scaling relations in the local Universe: what is the role of type 2 AGN?
DESCRIPTION:Coevolutionary models that link the growth of supermassive black holes (BHs) and of their host galaxies are based on the observations of tight scaling relations between the BH mass and some properties of the host bulge. These relations have been calibrated thanks to the direct measurements of the BH mass in local galaxies and are extremely important\, used to measure BH masses at high redshift and to determine the distribution of accreted mass\, i.e. the black hole mass function.\nHowever\, these relations seem to be biased in favour of the more massive BHs\, due to a bias in the resolution of the BH sphere of influence. Hence\, there is urgent need to explore the full distribution of BH masses\, accumulating sources below 1e+7 solar masses.\nI here present the results from a systematic study performed using deep NIR (VLT and LBT) spectroscopy of a sample of ~40 type 2 active galactic nuclei (AGN)\, drawn from the complete SWIFT/BAT 70-month hard (14-195 keV) X-ray catalogue. Thanks to our new virial relation based on unbiased physical quantities\, i.e. hard X-ray luminosity and Paβ emission line FWHM\, we have been able to measure for the first time in a virial way the supermassive black hole masses of type 2 AGN\, whose values have been up today estimated using indirect proxies (e.g. from scaling relations). With direct virial masses for type 2 AGN\, we discuss\, for the first time\, if the BH-host galaxy scaling relations hold for type 2 AGN\, thus putting a missing piece to the AGN/galaxy co-evolution puzzle.
URL:https://www.oa-roma.inaf.it/event/seminar-by-federica-ricci/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171114T114500
DTEND;TZID=Europe/Rome:20171114T124500
DTSTAMP:20260406T233435
CREATED:20170816T115844Z
LAST-MODIFIED:20170816T115844Z
UID:3396-1510659900-1510663500@www.oa-roma.inaf.it
SUMMARY:Main Sequence Multiple Populations in Large Magellanic Cloud Globular Clusters
DESCRIPTION:Six Large Magellanic Cloud (LMC) globular clusters (GCs) (NGC 1466\, NGC 1841\, NGC 2210\, NGC 2257\, Hodge 11\, and Reticulum) have been analyzed for multiple stellar populations with the Hubble Space Telescope (GO-14164). This is the first such study for ancient (ages > 13 Gyr) clusters in the LMC. We find that five out of the six GCs examined show evidence for multiple populations in the main sequence. One cluster (Hodge 11) shows irregularities in its horizontal branch that may indicate the presence of a 0.1 dex internal helium abundance spread.
URL:https://www.oa-roma.inaf.it/event/talk-by-christina-gilligan/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171114T114500
DTEND;TZID=Europe/Rome:20171114T124500
DTSTAMP:20260406T233435
CREATED:20170816T115844Z
LAST-MODIFIED:20170816T115844Z
UID:4721-1510659900-1510663500@www.oa-roma.inaf.it
SUMMARY:Main Sequence Multiple Populations in Large Magellanic Cloud Globular Clusters
DESCRIPTION:Six Large Magellanic Cloud (LMC) globular clusters (GCs) (NGC 1466\, NGC 1841\, NGC 2210\, NGC 2257\, Hodge 11\, and Reticulum) have been analyzed for multiple stellar populations with the Hubble Space Telescope (GO-14164). This is the first such study for ancient (ages > 13 Gyr) clusters in the LMC. We find that five out of the six GCs examined show evidence for multiple populations in the main sequence. One cluster (Hodge 11) shows irregularities in its horizontal branch that may indicate the presence of a 0.1 dex internal helium abundance spread.
URL:https://www.oa-roma.inaf.it/event/talk-by-christina-gilligan-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171121T114500
DTEND;TZID=Europe/Rome:20171121T124500
DTSTAMP:20260406T233435
CREATED:20170728T201958Z
LAST-MODIFIED:20170728T201958Z
UID:4717-1511264700-1511268300@www.oa-roma.inaf.it
SUMMARY:Fibrillar Structures in the Solar Chromosphere
DESCRIPTION:I present observations of dynamic\, slender bright fibrils seen in high-quality narrow-band Ca II H images from the SuFI instrument onboard the SUNRISE balloon-borne solar observatory. We have shown that these slender Ca II H fibrils (SCFs) map magnetic fields in the low solar chromosphere derived from magnetostatic extrapolation of the photospheric field obtained with SUNRISE/IMaX and SDO/HMI. Our analysis reveals the prevalence of both kink and sausage waves in the SCFs\, propagating at high-frequencies (up to 30 mHz)\, with speeds on the order of 9-15 km/s. The estimated energy flux (~ 15 kW/m^2) carried by the observed waves is marginally enough to heat the chromosphere (and perhaps the corona). Characteristics of these waves differ from those reported for other fibrillar structures\, which\, however\, were observed mainly in the upper solar chromosphere.\nFurthermore\, I present observations of fibrillar structures through the mid-to-high solar chromosphere from coordinated observations of an active region with the Interface Region Imaging Spectrograph (IRIS) explorer and the Atacama Large Millimeter/submillimeter Array (ALMA). This provides us with temperature distributions of the entire field of view at multiple chromospheric heights\, and in particular\, of the fibrillar structures. A detail comparison between fibrillar structures simultaneously observed at several millimetre and ultraviolet bands of\, e.g.\, ALMA 1.3 mm as well as IRIS Mg II h & k\, Si IV\, C II\, and O I has provided us with new insights into the nature of these thread-like structures.
URL:https://www.oa-roma.inaf.it/event/seminar-by-shahin-jafarzadeh-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171121T114500
DTEND;TZID=Europe/Rome:20171121T124500
DTSTAMP:20260406T233435
CREATED:20170728T201958Z
LAST-MODIFIED:20170728T201958Z
UID:3360-1511264700-1511268300@www.oa-roma.inaf.it
SUMMARY:Fibrillar Structures in the Solar Chromosphere
DESCRIPTION:I present observations of dynamic\, slender bright fibrils seen in high-quality narrow-band Ca II H images from the SuFI instrument onboard the SUNRISE balloon-borne solar observatory. We have shown that these slender Ca II H fibrils (SCFs) map magnetic fields in the low solar chromosphere derived from magnetostatic extrapolation of the photospheric field obtained with SUNRISE/IMaX and SDO/HMI. Our analysis reveals the prevalence of both kink and sausage waves in the SCFs\, propagating at high-frequencies (up to 30 mHz)\, with speeds on the order of 9-15 km/s. The estimated energy flux (~ 15 kW/m^2) carried by the observed waves is marginally enough to heat the chromosphere (and perhaps the corona). Characteristics of these waves differ from those reported for other fibrillar structures\, which\, however\, were observed mainly in the upper solar chromosphere.\nFurthermore\, I present observations of fibrillar structures through the mid-to-high solar chromosphere from coordinated observations of an active region with the Interface Region Imaging Spectrograph (IRIS) explorer and the Atacama Large Millimeter/submillimeter Array (ALMA). This provides us with temperature distributions of the entire field of view at multiple chromospheric heights\, and in particular\, of the fibrillar structures. A detail comparison between fibrillar structures simultaneously observed at several millimetre and ultraviolet bands of\, e.g.\, ALMA 1.3 mm as well as IRIS Mg II h & k\, Si IV\, C II\, and O I has provided us with new insights into the nature of these thread-like structures.
URL:https://www.oa-roma.inaf.it/event/seminar-by-shahin-jafarzadeh/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171128T114500
DTEND;TZID=Europe/Rome:20171128T124500
DTSTAMP:20260406T233435
CREATED:20171016T082254Z
LAST-MODIFIED:20171016T082254Z
UID:3639-1511869500-1511873100@www.oa-roma.inaf.it
SUMMARY:The other 95%: insights from strong gravitational lensing
DESCRIPTION:In the standard cosmological model ninety-five percent of the energy content of the universe consists of dark energy and dark matter. Even though their abundance seems well determined\, very little is known about their fundamental nature. I will describe how we can learn about the physics of the dark sector by studying in detail its gravitational effect on the trajectories of photons as they travel across the universe\, a phenomenon known as strong gravitational lensing. In the first part of the talk\, I will use strong gravitational lenses with a time variable background source to measure the expansion rate of the universe (Hubble constant) to 3.8% precision. This result is completely independent of the local distance ladder and the cosmic microwave background\, and thus provides a new opportunity to understand whether the tension between the two arises from systematic uncertainties or may be indicative of new physics. In the second part of the talk I will describe how strong lensing can be used to detect the presence of dark subhalos independent of their stellar content. This measurement tests a fundamental prediction of the cold dark matter model\, i.e. that galaxies should be surrounded by large numbers of dark satellite subhalos. Proof that such satellites do not exist would force a revision of the model in favor of more exotic alternatives like warm dark matter. I will conclude by discussing the exciting future of strong lensing as a tool for cosmology\, in light of the huge numbers of strong lenses that are being discovered in the current generation of wide field astronomical surveys.
URL:https://www.oa-roma.inaf.it/event/seminar-by-tommaso-treu/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171128T114500
DTEND;TZID=Europe/Rome:20171128T124500
DTSTAMP:20260406T233435
CREATED:20171016T082254Z
LAST-MODIFIED:20171016T082254Z
UID:4733-1511869500-1511873100@www.oa-roma.inaf.it
SUMMARY:The other 95%: insights from strong gravitational lensing
DESCRIPTION:In the standard cosmological model ninety-five percent of the energy content of the universe consists of dark energy and dark matter. Even though their abundance seems well determined\, very little is known about their fundamental nature. I will describe how we can learn about the physics of the dark sector by studying in detail its gravitational effect on the trajectories of photons as they travel across the universe\, a phenomenon known as strong gravitational lensing. In the first part of the talk\, I will use strong gravitational lenses with a time variable background source to measure the expansion rate of the universe (Hubble constant) to 3.8% precision. This result is completely independent of the local distance ladder and the cosmic microwave background\, and thus provides a new opportunity to understand whether the tension between the two arises from systematic uncertainties or may be indicative of new physics. In the second part of the talk I will describe how strong lensing can be used to detect the presence of dark subhalos independent of their stellar content. This measurement tests a fundamental prediction of the cold dark matter model\, i.e. that galaxies should be surrounded by large numbers of dark satellite subhalos. Proof that such satellites do not exist would force a revision of the model in favor of more exotic alternatives like warm dark matter. I will conclude by discussing the exciting future of strong lensing as a tool for cosmology\, in light of the huge numbers of strong lenses that are being discovered in the current generation of wide field astronomical surveys.
URL:https://www.oa-roma.inaf.it/event/seminar-by-tommaso-treu-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171130T114500
DTEND;TZID=Europe/Rome:20171130T124500
DTSTAMP:20260406T233435
CREATED:20171128T071804Z
LAST-MODIFIED:20171128T071804Z
UID:3776-1512042300-1512045900@www.oa-roma.inaf.it
SUMMARY:Oumuamua\, the first asteroid coming from another planetary system
DESCRIPTION:The discovery of 1I/’Oumuamua\, the first interstellar object found\ntransiting in our Solar System\, provided astronomers with an extremely\nunusual new target\, and with a few surprises. We will briefly present\nthe discovery story and the unique properties of this new temporary\nvisitor of our Solar System.
URL:https://www.oa-roma.inaf.it/event/oumuamua-the-first-asteroid-coming-from-another-planetary-system-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171130T114500
DTEND;TZID=Europe/Rome:20171130T124500
DTSTAMP:20260406T233435
CREATED:20171128T071804Z
LAST-MODIFIED:20171128T071804Z
UID:4738-1512042300-1512045900@www.oa-roma.inaf.it
SUMMARY:Oumuamua\, the first asteroid coming from another planetary system
DESCRIPTION:The discovery of 1I/’Oumuamua\, the first interstellar object found\ntransiting in our Solar System\, provided astronomers with an extremely\nunusual new target\, and with a few surprises. We will briefly present\nthe discovery story and the unique properties of this new temporary\nvisitor of our Solar System.
URL:https://www.oa-roma.inaf.it/event/oumuamua-the-first-asteroid-coming-from-another-planetary-system-2-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
END:VCALENDAR