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X-ORIGINAL-URL:https://www.oa-roma.inaf.it
X-WR-CALDESC:Eventi per Osservatorio Astronomico di Roma
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DTSTART:20160327T010000
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DTSTART:20161030T010000
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BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20170307T114500
DTEND;TZID=Europe/Rome:20170307T124500
DTSTAMP:20260426T120652
CREATED:20161114T095348Z
LAST-MODIFIED:20161114T095348Z
UID:1977-1488887100-1488890700@www.oa-roma.inaf.it
SUMMARY:From the first stars to the first quasars
DESCRIPTION:Observations of the most luminous quasars at redshift z>6 reveal the existence of numerous supermassive black holes (SMBHs\, > 10^9 Msun) already in place about twelve billion years ago. The growth of these first SMBHs is still a major challenge for theoretical models. If it starts from black hole (BH) remnants of Population III stars (light seeds with mass ~100 Msun)\, it requires super-Eddington accretion. An alternative route is to start from heavy seeds formed by the direct collapse of gas on to a ~10^5 Msun BH. In addition\, the interstellar medium (ISM) of the galaxies hosting these quasars are observed to be chemically mature systems\, with metallicities Z>Zsun and dust masses >10^8 Msun\, similar to that of more evolved\, local galaxies. The connection between the rapid growth of the SMBHs and the fast chemical evolution of the host galaxy is one of the most puzzling issues for theoretical models.\nI will present the results of our cosmological\, data constrained semi-analytic model in which we investigate the relative role of light and heavy seeds as BH progenitors of the first SMBHs\, self-consistently following the evolution of the chemical properties (metals and dust abundance) in the host galaxies ISM.
URL:https://www.oa-roma.inaf.it/event/seminario-rosa-valiante/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20170307T114500
DTEND;TZID=Europe/Rome:20170307T124500
DTSTAMP:20260426T120652
CREATED:20161114T095348Z
LAST-MODIFIED:20161114T095348Z
UID:4699-1488887100-1488890700@www.oa-roma.inaf.it
SUMMARY:From the first stars to the first quasars
DESCRIPTION:Observations of the most luminous quasars at redshift z>6 reveal the existence of numerous supermassive black holes (SMBHs\, > 10^9 Msun) already in place about twelve billion years ago. The growth of these first SMBHs is still a major challenge for theoretical models. If it starts from black hole (BH) remnants of Population III stars (light seeds with mass ~100 Msun)\, it requires super-Eddington accretion. An alternative route is to start from heavy seeds formed by the direct collapse of gas on to a ~10^5 Msun BH. In addition\, the interstellar medium (ISM) of the galaxies hosting these quasars are observed to be chemically mature systems\, with metallicities Z>Zsun and dust masses >10^8 Msun\, similar to that of more evolved\, local galaxies. The connection between the rapid growth of the SMBHs and the fast chemical evolution of the host galaxy is one of the most puzzling issues for theoretical models.\nI will present the results of our cosmological\, data constrained semi-analytic model in which we investigate the relative role of light and heavy seeds as BH progenitors of the first SMBHs\, self-consistently following the evolution of the chemical properties (metals and dust abundance) in the host galaxies ISM.
URL:https://www.oa-roma.inaf.it/event/seminario-rosa-valiante-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20170314T114500
DTEND;TZID=Europe/Rome:20170314T124500
DTSTAMP:20260426T120652
CREATED:20160909T044857Z
LAST-MODIFIED:20160909T044857Z
UID:1387-1489491900-1489495500@www.oa-roma.inaf.it
SUMMARY:Highly Ionized X-ray Absorbers in AGNs and their Energetic: the case of NGC 4051
DESCRIPTION:Highly ionized absorbers are found in 50% of type 1 Seyferts and QSOs. They presence\, along our line of sight\, imprints a number of absorption lines from highly ionized metals in the far UV and X-ray spectral bands\, like FeX-XVII\, CIV-VI\, OVI-OVIII\, NeVII-X\, etc. These absorption lines are always detected blue-shifted compared to the host galaxy reference system\, which implies that the ionized material is being ejected from the nucleus and driven outwards\, possibly by the AGN radiation pressure. Outflow velocities span a wide range\, from few hundreds to few thousands km/s in the so called Narrow-Absorption Line (NAL) and/or Warm Absorber objects\, to non negligible fractions of the speed of light in UV Broad Absorption Line (BAL) or X-ray Ultra-Fast Outflows (UFOs). These outflows are believed to be photo-ionized by the central source and their energetic depends on their mass outflow rate which\, in turn\, depends on the volume density n_e of the material\, which is difficult to measure because degenerate with the square of the distance R of the absorber from the photo-ionizing source.\nIn this talk\, after a brief overview of the phenomenon\, I will show how time-evolving photo-ionization works and how it can be used to break the degeneracy between the absorber volume density n_e and its distance R from the central engine. I will then present the particularly fortunate case of NGC 4051 and show the puzzling results of the analysis performed here at OAR of the long 2009 XMM-Newton monitoring of this source.
URL:https://www.oa-roma.inaf.it/event/x-ray-ionized-absorbers-of-agn-and-their-variability/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20170314T114500
DTEND;TZID=Europe/Rome:20170314T124500
DTSTAMP:20260426T120652
CREATED:20160909T044857Z
LAST-MODIFIED:20160909T044857Z
UID:4682-1489491900-1489495500@www.oa-roma.inaf.it
SUMMARY:Highly Ionized X-ray Absorbers in AGNs and their Energetic: the case of NGC 4051
DESCRIPTION:Highly ionized absorbers are found in 50% of type 1 Seyferts and QSOs. They presence\, along our line of sight\, imprints a number of absorption lines from highly ionized metals in the far UV and X-ray spectral bands\, like FeX-XVII\, CIV-VI\, OVI-OVIII\, NeVII-X\, etc. These absorption lines are always detected blue-shifted compared to the host galaxy reference system\, which implies that the ionized material is being ejected from the nucleus and driven outwards\, possibly by the AGN radiation pressure. Outflow velocities span a wide range\, from few hundreds to few thousands km/s in the so called Narrow-Absorption Line (NAL) and/or Warm Absorber objects\, to non negligible fractions of the speed of light in UV Broad Absorption Line (BAL) or X-ray Ultra-Fast Outflows (UFOs). These outflows are believed to be photo-ionized by the central source and their energetic depends on their mass outflow rate which\, in turn\, depends on the volume density n_e of the material\, which is difficult to measure because degenerate with the square of the distance R of the absorber from the photo-ionizing source.\nIn this talk\, after a brief overview of the phenomenon\, I will show how time-evolving photo-ionization works and how it can be used to break the degeneracy between the absorber volume density n_e and its distance R from the central engine. I will then present the particularly fortunate case of NGC 4051 and show the puzzling results of the analysis performed here at OAR of the long 2009 XMM-Newton monitoring of this source.
URL:https://www.oa-roma.inaf.it/event/x-ray-ionized-absorbers-of-agn-and-their-variability-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20170321T114500
DTEND;TZID=Europe/Rome:20170321T124500
DTSTAMP:20260426T120652
CREATED:20161009T045023Z
LAST-MODIFIED:20161009T045023Z
UID:1750-1490096700-1490100300@www.oa-roma.inaf.it
SUMMARY:Dwarf Galaxies - Fossils of Galaxy Evolution
DESCRIPTION:Dwarf galaxies are the most common type of galaxy in the Universe and\ninclude the most dark-matter-dominated objects known.  They offer\nintriguing insights into evolutionary processes at low halo masses\nand low metallicities.  Moreover\, as survivors of a once much more\nnumerous population of building blocks of larger galaxies\, they are\nkey to understanding very early star formation processes.  The Local\nGroup and particularly the Milky Way’s dwarf galaxy entourage offer\nus the unique possibility to compare in detail dwarf and Galactic\npopulations. This is an important step towards quantifying the\nmagnitude and time scales of dwarf contributions to the build-up of\nthe Milky Way and allows us to test predictions of cosmological\ntheories and hierarchical structure formation
URL:https://www.oa-roma.inaf.it/event/seminario-eva-grebel/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20170321T114500
DTEND;TZID=Europe/Rome:20170321T124500
DTSTAMP:20260426T120652
CREATED:20161009T045023Z
LAST-MODIFIED:20161009T045023Z
UID:4696-1490096700-1490100300@www.oa-roma.inaf.it
SUMMARY:Dwarf Galaxies - Fossils of Galaxy Evolution
DESCRIPTION:Dwarf galaxies are the most common type of galaxy in the Universe and\ninclude the most dark-matter-dominated objects known.  They offer\nintriguing insights into evolutionary processes at low halo masses\nand low metallicities.  Moreover\, as survivors of a once much more\nnumerous population of building blocks of larger galaxies\, they are\nkey to understanding very early star formation processes.  The Local\nGroup and particularly the Milky Way’s dwarf galaxy entourage offer\nus the unique possibility to compare in detail dwarf and Galactic\npopulations. This is an important step towards quantifying the\nmagnitude and time scales of dwarf contributions to the build-up of\nthe Milky Way and allows us to test predictions of cosmological\ntheories and hierarchical structure formation
URL:https://www.oa-roma.inaf.it/event/seminario-eva-grebel-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
END:VCALENDAR