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BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171003T114500
DTEND;TZID=Europe/Rome:20171003T124500
DTSTAMP:20260404T213646
CREATED:20170728T201245Z
LAST-MODIFIED:20170728T201245Z
UID:3349-1507031100-1507034700@www.oa-roma.inaf.it
SUMMARY:First black holes: observability and growth
DESCRIPTION:The first black hole seeds ​likely ​formed when the Universe was younger than 500 Myr​ old.\n​They play​ an important role ​in​ the growth of early (z=7) supermassive black holes. While ​much ​progress ha​s​ been made in understanding their formation and growth\, their observational signatures remain largely unexplored. As a result\, ​we are yet to ​detect ​these​ sources. ​We​ present a novel photometric method to identify black hole seed candidates in deep multi-wavelength surveys. The method relies on infrared and X-ray observations and selects​ the only two objects with a robust X-ray detection found in the CANDELS/GOODS-S survey with a photometric redshift z>6. To date\, these selected objects represent the most promising black hole seed candidates\, possibly formed via the direct collapse black hole scenario. While this result is based on the best photometric observations of high-z sources available to date\, additional ​gains are​ expected from deeper spectroscopic and X-ray data. For this reason\, ​we ​explore the role ​that ​JWST ​will play in the ​detect​on of ​the first black holes​ in ​the ​U​niverse.\nMoreover\, we present a novel probabilistic model for black hole growth: our results have important implications for the conditions that facilitate efficient black hole growth\, particularly at early cosmic epochs. By bringing in a precise definition of “growth probability”\, our finding clearly demonstrates quantitatively the generally-accepted concept that the super-massive black holes that we observed at z=7 are the “luckiest” members of the ensemble of high-z black holes. Our formalism has significant and broad ​consequences​ for upcoming observations of high-redshift quasars.
URL:https://www.oa-roma.inaf.it/event/simar-fabio-pacucci/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171003T114500
DTEND;TZID=Europe/Rome:20171003T124500
DTSTAMP:20260404T213646
CREATED:20170728T201245Z
LAST-MODIFIED:20170728T201245Z
UID:4712-1507031100-1507034700@www.oa-roma.inaf.it
SUMMARY:First black holes: observability and growth
DESCRIPTION:The first black hole seeds ​likely ​formed when the Universe was younger than 500 Myr​ old.\n​They play​ an important role ​in​ the growth of early (z=7) supermassive black holes. While ​much ​progress ha​s​ been made in understanding their formation and growth\, their observational signatures remain largely unexplored. As a result\, ​we are yet to ​detect ​these​ sources. ​We​ present a novel photometric method to identify black hole seed candidates in deep multi-wavelength surveys. The method relies on infrared and X-ray observations and selects​ the only two objects with a robust X-ray detection found in the CANDELS/GOODS-S survey with a photometric redshift z>6. To date\, these selected objects represent the most promising black hole seed candidates\, possibly formed via the direct collapse black hole scenario. While this result is based on the best photometric observations of high-z sources available to date\, additional ​gains are​ expected from deeper spectroscopic and X-ray data. For this reason\, ​we ​explore the role ​that ​JWST ​will play in the ​detect​on of ​the first black holes​ in ​the ​U​niverse.\nMoreover\, we present a novel probabilistic model for black hole growth: our results have important implications for the conditions that facilitate efficient black hole growth\, particularly at early cosmic epochs. By bringing in a precise definition of “growth probability”\, our finding clearly demonstrates quantitatively the generally-accepted concept that the super-massive black holes that we observed at z=7 are the “luckiest” members of the ensemble of high-z black holes. Our formalism has significant and broad ​consequences​ for upcoming observations of high-redshift quasars.
URL:https://www.oa-roma.inaf.it/event/simar-fabio-pacucci-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171010T113000
DTEND;TZID=Europe/Rome:20171010T123000
DTSTAMP:20260404T213646
CREATED:20170728T201510Z
LAST-MODIFIED:20170728T201510Z
UID:4713-1507635000-1507638600@www.oa-roma.inaf.it
SUMMARY:L'utilità della Scienza inutile
DESCRIPTION:Se i risultati scientifici finanziati con i soldi dei contribuenti sono “beni pubblici”\, è utile o addirittura etico spendere miliardi per cercare una particella elementare? O per andare a visitare un satellite di Giove o cercare l’acqua su Marte? O per osservare una galassia ai confini dell’Universo? In altre parole\, è utile finanziare la ricerca di base? E se sì\, con che risorse? E per fare quale tipo di ricerca?\nLa competizione è diventata una delle maggiori forze trainanti per la ricerca. Ma siamo sicuri che il modello “competition-driven science” sia davvero quello migliore?\nDi più\, sta cambiando il concetto stesso di conoscenza? Siamo sicuri che sia ancora valido e applicabile oggi il “metodo scientifico” introdotto da Galileo più di 400 anni fa?\nLe risposte a tutte queste domande non sono scontate\, anzi\, possono contenere molte sorprese non tutte piacevoli o rassicuranti\, risposte tra le quali cercheremo di orientarci usando un punto di vista non sempre convenzionale.\nLa presentazione\, in Italiano\, è aperta a tutto il personale\, anche ai non specialisti del settore.
URL:https://www.oa-roma.inaf.it/event/lutilita-della-scienza-inutile-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171010T113000
DTEND;TZID=Europe/Rome:20171010T123000
DTSTAMP:20260404T213646
CREATED:20170728T201510Z
LAST-MODIFIED:20170728T201510Z
UID:3352-1507635000-1507638600@www.oa-roma.inaf.it
SUMMARY:L'utilità della Scienza inutile
DESCRIPTION:Se i risultati scientifici finanziati con i soldi dei contribuenti sono “beni pubblici”\, è utile o addirittura etico spendere miliardi per cercare una particella elementare? O per andare a visitare un satellite di Giove o cercare l’acqua su Marte? O per osservare una galassia ai confini dell’Universo? In altre parole\, è utile finanziare la ricerca di base? E se sì\, con che risorse? E per fare quale tipo di ricerca?\nLa competizione è diventata una delle maggiori forze trainanti per la ricerca. Ma siamo sicuri che il modello “competition-driven science” sia davvero quello migliore?\nDi più\, sta cambiando il concetto stesso di conoscenza? Siamo sicuri che sia ancora valido e applicabile oggi il “metodo scientifico” introdotto da Galileo più di 400 anni fa?\nLe risposte a tutte queste domande non sono scontate\, anzi\, possono contenere molte sorprese non tutte piacevoli o rassicuranti\, risposte tra le quali cercheremo di orientarci usando un punto di vista non sempre convenzionale.\nLa presentazione\, in Italiano\, è aperta a tutto il personale\, anche ai non specialisti del settore.
URL:https://www.oa-roma.inaf.it/event/lutilita-della-scienza-inutile/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171017T114500
DTEND;TZID=Europe/Rome:20171017T124500
DTSTAMP:20260404T213646
CREATED:20170728T201627Z
LAST-MODIFIED:20170728T201627Z
UID:3354-1508240700-1508244300@www.oa-roma.inaf.it
SUMMARY:The primitive small bodies: from the origin of the solar system to the origin of life
DESCRIPTION:The so-called “primitive” small bodies (carbonaceous asteroids\, centaurs\, comets\, trans-Neptunian objects) have formed in the water- and organic-rich outer regions of the protoplanetary disk. They carry information on a number of evolutionary processes which have taken place since the solar system formation\, and\, in particular\, they are considered as the most probable source of terrestrial prebiotic material.\nIn this talk\, I will present the results of a 30-night observing programme carried out at the ESO-NTT in 2015-2017\, the first-ever spectroscopic survey dedicated to the “small” (up to a few hundred meters) near-Earth asteroids (NEAs). Noteworthy\, smaller asteroids could deposit prebiotic material on the early Earth in a more efficient way\, without massive water vaporization and destruction of organic molecules as in the case of larger impacts.\nI will also discuss about the ongoing sample return missions from primitive NEAs Ryugu and Bennu\, that will be reached in 2018 by the Hayabusa 2 (JAXA) and OSIRIS-REx (NASA) spacecrafts\, respectively. Such missions will be fundamental to assess if the organic compounds contained in primitive asteroids can indeed be associated with the formation of life on Earth.\nFinally\, I will report about a long-term observational programme aimed to investigate the composition and cometary activity of centaurs\, a transitional population between the trans-Neptunian regions and the inner solar system. It is to be reminded that the impact of Centaur-like objects might have significantly contributed to the delivery of noble gases and amino-acids to the early Earth.
URL:https://www.oa-roma.inaf.it/event/seminar-by-davide-perna/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171017T114500
DTEND;TZID=Europe/Rome:20171017T124500
DTSTAMP:20260404T213646
CREATED:20170728T201627Z
LAST-MODIFIED:20170728T201627Z
UID:4714-1508240700-1508244300@www.oa-roma.inaf.it
SUMMARY:The primitive small bodies: from the origin of the solar system to the origin of life
DESCRIPTION:The so-called “primitive” small bodies (carbonaceous asteroids\, centaurs\, comets\, trans-Neptunian objects) have formed in the water- and organic-rich outer regions of the protoplanetary disk. They carry information on a number of evolutionary processes which have taken place since the solar system formation\, and\, in particular\, they are considered as the most probable source of terrestrial prebiotic material.\nIn this talk\, I will present the results of a 30-night observing programme carried out at the ESO-NTT in 2015-2017\, the first-ever spectroscopic survey dedicated to the “small” (up to a few hundred meters) near-Earth asteroids (NEAs). Noteworthy\, smaller asteroids could deposit prebiotic material on the early Earth in a more efficient way\, without massive water vaporization and destruction of organic molecules as in the case of larger impacts.\nI will also discuss about the ongoing sample return missions from primitive NEAs Ryugu and Bennu\, that will be reached in 2018 by the Hayabusa 2 (JAXA) and OSIRIS-REx (NASA) spacecrafts\, respectively. Such missions will be fundamental to assess if the organic compounds contained in primitive asteroids can indeed be associated with the formation of life on Earth.\nFinally\, I will report about a long-term observational programme aimed to investigate the composition and cometary activity of centaurs\, a transitional population between the trans-Neptunian regions and the inner solar system. It is to be reminded that the impact of Centaur-like objects might have significantly contributed to the delivery of noble gases and amino-acids to the early Earth.
URL:https://www.oa-roma.inaf.it/event/seminar-by-davide-perna-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171024T114500
DTEND;TZID=Europe/Rome:20171024T124500
DTSTAMP:20260404T213646
CREATED:20170728T201742Z
LAST-MODIFIED:20170728T201742Z
UID:3356-1508845500-1508849100@www.oa-roma.inaf.it
SUMMARY:Observations of Fast Outflows in Active Galactic Nuclei
DESCRIPTION:The presence of outflows in many Active Galaxies has been firmly established through X-ray spectroscopy over the last two decades.\nThese outflows range from the low velocity warm absorbers commonly seen in many Seyfert galaxies\, through to the\nso called ultra fast outflows\, where the outflow velocities can reach a significant fraction of c.\nUltra fast outflows were first discovered in 2003\, from the presence of highly blue-shifted absorption lines from the X-ray spectra of quasars and AGN. The observational evidence for fast outflows will be reviewed\, as well as their wider properties and potential for feedback into the host galaxies of AGN. New data from large programs on the fast outflows\, such as PDS 456 and PG 1211+143\, will be shown\, the former showing a fast wide angle outflow\, while both AGN show highly variable outflows which may respond to the ionising continuum.\nThe evidence for fast soft X-ray absorption as well as the possible driving mechanisms of the winds will also be discussed.
URL:https://www.oa-roma.inaf.it/event/seminar-by-james-reeves/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171024T114500
DTEND;TZID=Europe/Rome:20171024T124500
DTSTAMP:20260404T213646
CREATED:20170728T201742Z
LAST-MODIFIED:20170728T201742Z
UID:4715-1508845500-1508849100@www.oa-roma.inaf.it
SUMMARY:Observations of Fast Outflows in Active Galactic Nuclei
DESCRIPTION:The presence of outflows in many Active Galaxies has been firmly established through X-ray spectroscopy over the last two decades.\nThese outflows range from the low velocity warm absorbers commonly seen in many Seyfert galaxies\, through to the\nso called ultra fast outflows\, where the outflow velocities can reach a significant fraction of c.\nUltra fast outflows were first discovered in 2003\, from the presence of highly blue-shifted absorption lines from the X-ray spectra of quasars and AGN. The observational evidence for fast outflows will be reviewed\, as well as their wider properties and potential for feedback into the host galaxies of AGN. New data from large programs on the fast outflows\, such as PDS 456 and PG 1211+143\, will be shown\, the former showing a fast wide angle outflow\, while both AGN show highly variable outflows which may respond to the ionising continuum.\nThe evidence for fast soft X-ray absorption as well as the possible driving mechanisms of the winds will also be discussed.
URL:https://www.oa-roma.inaf.it/event/seminar-by-james-reeves-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171031T114500
DTEND;TZID=Europe/Rome:20171031T124500
DTSTAMP:20260404T213646
CREATED:20170907T063500Z
LAST-MODIFIED:20170907T063500Z
UID:3435-1509450300-1509453900@www.oa-roma.inaf.it
SUMMARY:The first CEMP-no star in the Sculptor dwarf spheroidal galaxy
DESCRIPTION:The origin of carbon-enhanced metal-poor (CEMP) stars and their possible\nconnection with the chemical elements produced by the first stellar\ngeneration is still highly debated. Recently\, the first CEMP-no star in\nthe Sculptor dwarf spheroidal was discovered at an iron abundance of\n[Fe/H] = 8722;2.03 ± 0.10. Since Sculptor is one of the best studied\ndwarf galaxies in the Local Group\, it is surprising that until now\, only\none CEMP-no star has been found in this galaxy. The available observations\nsuggest that the fraction of CEMP stars in Sculptor is lower than in the\nGalactic halo. To understand this apparent discrepancy between different\nenvironments\, I will discuss the CEMP-no fraction in Sculptor\, and other\ndwarf galaxies in general.
URL:https://www.oa-roma.inaf.it/event/seminar-by-asa-skuladottir/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171031T114500
DTEND;TZID=Europe/Rome:20171031T124500
DTSTAMP:20260404T213646
CREATED:20170907T063500Z
LAST-MODIFIED:20170907T063500Z
UID:4727-1509450300-1509453900@www.oa-roma.inaf.it
SUMMARY:The first CEMP-no star in the Sculptor dwarf spheroidal galaxy
DESCRIPTION:The origin of carbon-enhanced metal-poor (CEMP) stars and their possible\nconnection with the chemical elements produced by the first stellar\ngeneration is still highly debated. Recently\, the first CEMP-no star in\nthe Sculptor dwarf spheroidal was discovered at an iron abundance of\n[Fe/H] = 8722;2.03 ± 0.10. Since Sculptor is one of the best studied\ndwarf galaxies in the Local Group\, it is surprising that until now\, only\none CEMP-no star has been found in this galaxy. The available observations\nsuggest that the fraction of CEMP stars in Sculptor is lower than in the\nGalactic halo. To understand this apparent discrepancy between different\nenvironments\, I will discuss the CEMP-no fraction in Sculptor\, and other\ndwarf galaxies in general.
URL:https://www.oa-roma.inaf.it/event/seminar-by-asa-skuladottir-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171107T114500
DTEND;TZID=Europe/Rome:20171107T124500
DTSTAMP:20260404T213646
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:20171107T114500
DTEND;TZID=Europe/Rome:20171107T124500
DTSTAMP:20260404T213646
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:20171114T114500
DTEND;TZID=Europe/Rome:20171114T124500
DTSTAMP:20260404T213646
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:20171114T114500
DTEND;TZID=Europe/Rome:20171114T124500
DTSTAMP:20260404T213646
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:20171121T114500
DTEND;TZID=Europe/Rome:20171121T124500
DTSTAMP:20260404T213646
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:20260404T213646
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:20260404T213646
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:20171128T114500
DTEND;TZID=Europe/Rome:20171128T124500
DTSTAMP:20260404T213646
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:20171130T114500
DTEND;TZID=Europe/Rome:20171130T124500
DTSTAMP:20260404T213646
CREATED:20171127T182520Z
LAST-MODIFIED:20171127T182520Z
UID:4737-1512042300-1512045900@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-3/
LOCATION:OAR Monte Porzio Catone – aula Gratton\, Via Frascati 33\, Roma\, RM\, 00136\, Italia
ORGANIZER;CN="OAR":MAILTO:info@oa-roma.inaf.it
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171130T114500
DTEND;TZID=Europe/Rome:20171130T124500
DTSTAMP:20260404T213646
CREATED:20171127T182520Z
LAST-MODIFIED:20171127T182520Z
UID:3774-1512042300-1512045900@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/
LOCATION:OAR Monte Porzio Catone – aula Gratton\, Via Frascati 33\, Roma\, RM\, 00136\, Italia
ORGANIZER;CN="OAR":MAILTO:info@oa-roma.inaf.it
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171130T114500
DTEND;TZID=Europe/Rome:20171130T124500
DTSTAMP:20260404T213646
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:20260404T213646
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
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171205T114500
DTEND;TZID=Europe/Rome:20171205T124500
DTSTAMP:20260404T213646
CREATED:20170816T120046Z
LAST-MODIFIED:20170816T120046Z
UID:3398-1512474300-1512477900@www.oa-roma.inaf.it
SUMMARY:Mass loss of AGB stars and RSG in the Magellanic Clouds
DESCRIPTION:I will discuss recent work that I am involved in regarding the determination of\nthe mass-loss rates (MLRs)  of a significant sample of Asymptotic Giant Branch stars and\nRed Supergiants in the Magellanic Clouds. This mostly involves modelling the\nspectral energy distributions to obtain dust MLRs\, but we also used ALMA to detect CO emission\nin a few LMC objects. I will also discuss possible ways forward in this field
URL:https://www.oa-roma.inaf.it/event/talk-by-martin-groenewegen/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171205T114500
DTEND;TZID=Europe/Rome:20171205T124500
DTSTAMP:20260404T213646
CREATED:20170816T120046Z
LAST-MODIFIED:20170816T120046Z
UID:4722-1512474300-1512477900@www.oa-roma.inaf.it
SUMMARY:Mass loss of AGB stars and RSG in the Magellanic Clouds
DESCRIPTION:I will discuss recent work that I am involved in regarding the determination of\nthe mass-loss rates (MLRs)  of a significant sample of Asymptotic Giant Branch stars and\nRed Supergiants in the Magellanic Clouds. This mostly involves modelling the\nspectral energy distributions to obtain dust MLRs\, but we also used ALMA to detect CO emission\nin a few LMC objects. I will also discuss possible ways forward in this field
URL:https://www.oa-roma.inaf.it/event/talk-by-martin-groenewegen-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171212T114500
DTEND;TZID=Europe/Rome:20171212T124500
DTSTAMP:20260404T213646
CREATED:20170821T062018Z
LAST-MODIFIED:20170821T062018Z
UID:3408-1513079100-1513082700@www.oa-roma.inaf.it
SUMMARY:High contrast imaging and the search for young exo-planets
DESCRIPTION:High contrast imaging has enormously progressed in the last twenty years\, thanks to the development of extreme AO\, efficient coronagraph\, and various differential imaging techniques. The two frontier instruments are GPI at Gemini South and SPHERE at VLT. We are now routinely achieving contrast of better than 10^5 with a record of 4×10^6 at separations below 0.5 arcsec\, This has allowed the discovery and characterization of about a dozen young planets\, of a couple of dozens of brown dwarfs\, and direct detection of several tens disks in scattered light. These data open new windows on the very early phases of planet formation\, when disks are still present. Both theory and data indicate that while clearly planets form in the late phase of the protostellar disks\, the relation between disk and planets is very complex. Also\, the spectra we are obtaining for the young planets indicate systematic differences between young and old objects with similar temperature. I will briefly present the technological and scientific aspects of this very new and exciting science
URL:https://www.oa-roma.inaf.it/event/seminar-by-raffaele-gratton/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171212T114500
DTEND;TZID=Europe/Rome:20171212T124500
DTSTAMP:20260404T213646
CREATED:20170821T062018Z
LAST-MODIFIED:20170821T062018Z
UID:4724-1513079100-1513082700@www.oa-roma.inaf.it
SUMMARY:High contrast imaging and the search for young exo-planets
DESCRIPTION:High contrast imaging has enormously progressed in the last twenty years\, thanks to the development of extreme AO\, efficient coronagraph\, and various differential imaging techniques. The two frontier instruments are GPI at Gemini South and SPHERE at VLT. We are now routinely achieving contrast of better than 10^5 with a record of 4×10^6 at separations below 0.5 arcsec\, This has allowed the discovery and characterization of about a dozen young planets\, of a couple of dozens of brown dwarfs\, and direct detection of several tens disks in scattered light. These data open new windows on the very early phases of planet formation\, when disks are still present. Both theory and data indicate that while clearly planets form in the late phase of the protostellar disks\, the relation between disk and planets is very complex. Also\, the spectra we are obtaining for the young planets indicate systematic differences between young and old objects with similar temperature. I will briefly present the technological and scientific aspects of this very new and exciting science
URL:https://www.oa-roma.inaf.it/event/seminar-by-raffaele-gratton-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171219T114500
DTEND;TZID=Europe/Rome:20171219T124500
DTSTAMP:20260404T213646
CREATED:20170927T104628Z
LAST-MODIFIED:20170927T104628Z
UID:3565-1513683900-1513687500@www.oa-roma.inaf.it
SUMMARY:Dust Production from Evolved Stars in the Local Group
DESCRIPTION:Infrared observations of nearby galaxies and the Milky Way show that there are two main sources of ISM dust: the winds of evolved stars and supernovae ejecta. However\, the total dust contribution from evolved stars relative to supernovae\, and how it changes with metallicity\, is less certain. Infrared photometric and spectroscopic Spitzer Surveys of the Large and Small Magellanic Clouds (LMC\, SMC): Surveying the Agents of Galaxy Evolution (SAGE) resulted in the discovery of thousands of evolved stars. Here\, I will describe how the composition and quantity of dust produced by these stars depends on metallicity. I will also discuss how the mid-IR stellar populations of the Magellanic Clouds can be used as a template for potential observations with JWST\, and how we have applied this to our observing programs of Local Group galaxies and SN1987A with JWST
URL:https://www.oa-roma.inaf.it/event/seminar-by-olivia-jones/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20171219T114500
DTEND;TZID=Europe/Rome:20171219T124500
DTSTAMP:20260404T213646
CREATED:20170927T104628Z
LAST-MODIFIED:20170927T104628Z
UID:4732-1513683900-1513687500@www.oa-roma.inaf.it
SUMMARY:Dust Production from Evolved Stars in the Local Group
DESCRIPTION:Infrared observations of nearby galaxies and the Milky Way show that there are two main sources of ISM dust: the winds of evolved stars and supernovae ejecta. However\, the total dust contribution from evolved stars relative to supernovae\, and how it changes with metallicity\, is less certain. Infrared photometric and spectroscopic Spitzer Surveys of the Large and Small Magellanic Clouds (LMC\, SMC): Surveying the Agents of Galaxy Evolution (SAGE) resulted in the discovery of thousands of evolved stars. Here\, I will describe how the composition and quantity of dust produced by these stars depends on metallicity. I will also discuss how the mid-IR stellar populations of the Magellanic Clouds can be used as a template for potential observations with JWST\, and how we have applied this to our observing programs of Local Group galaxies and SN1987A with JWST
URL:https://www.oa-roma.inaf.it/event/seminar-by-olivia-jones-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20180109T114500
DTEND;TZID=Europe/Rome:20180109T124500
DTSTAMP:20260404T213646
CREATED:20170728T202118Z
LAST-MODIFIED:20170728T202118Z
UID:3362-1515498300-1515501900@www.oa-roma.inaf.it
SUMMARY:Microlensing
DESCRIPTION:I will review the microlensing and pixel lensing techniques and show how they play a\nfundamental role in the searches for galactic dark matter\, in the study of the galactic structure and in\ndetecting planets around faint stars whose cahacteristics are in general not accessible to other methods.\nWe show that dedicated and well planned experiments would even allow to detect more exotic objects\nas primordial massive black holes (if any) in nearby galaxies and/or to put strong constraints on\ntheir existence.
URL:https://www.oa-roma.inaf.it/event/seminar-by-raffaella-margutti/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20180109T114500
DTEND;TZID=Europe/Rome:20180109T124500
DTSTAMP:20260404T213646
CREATED:20170728T202118Z
LAST-MODIFIED:20170728T202118Z
UID:4718-1515498300-1515501900@www.oa-roma.inaf.it
SUMMARY:Microlensing
DESCRIPTION:I will review the microlensing and pixel lensing techniques and show how they play a\nfundamental role in the searches for galactic dark matter\, in the study of the galactic structure and in\ndetecting planets around faint stars whose cahacteristics are in general not accessible to other methods.\nWe show that dedicated and well planned experiments would even allow to detect more exotic objects\nas primordial massive black holes (if any) in nearby galaxies and/or to put strong constraints on\ntheir existence.
URL:https://www.oa-roma.inaf.it/event/seminar-by-raffaella-margutti-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
END:VCALENDAR