BEGIN:VCALENDAR
VERSION:2.0
PRODID:-//Osservatorio Astronomico di Roma - ECPv6.15.19//NONSGML v1.0//EN
CALSCALE:GREGORIAN
METHOD:PUBLISH
X-ORIGINAL-URL:https://www.oa-roma.inaf.it
X-WR-CALDESC:Eventi per Osservatorio Astronomico di Roma
REFRESH-INTERVAL;VALUE=DURATION:PT1H
X-Robots-Tag:noindex
X-PUBLISHED-TTL:PT1H
BEGIN:VTIMEZONE
TZID:Europe/Rome
BEGIN:DAYLIGHT
TZOFFSETFROM:+0100
TZOFFSETTO:+0200
TZNAME:CEST
DTSTART:20170326T010000
END:DAYLIGHT
BEGIN:STANDARD
TZOFFSETFROM:+0200
TZOFFSETTO:+0100
TZNAME:CET
DTSTART:20171029T010000
END:STANDARD
BEGIN:DAYLIGHT
TZOFFSETFROM:+0100
TZOFFSETTO:+0200
TZNAME:CEST
DTSTART:20180325T010000
END:DAYLIGHT
BEGIN:STANDARD
TZOFFSETFROM:+0200
TZOFFSETTO:+0100
TZNAME:CET
DTSTART:20181028T010000
END:STANDARD
BEGIN:DAYLIGHT
TZOFFSETFROM:+0100
TZOFFSETTO:+0200
TZNAME:CEST
DTSTART:20190331T010000
END:DAYLIGHT
BEGIN:STANDARD
TZOFFSETFROM:+0200
TZOFFSETTO:+0100
TZNAME:CET
DTSTART:20191027T010000
END:STANDARD
END:VTIMEZONE
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20180206T114500
DTEND;TZID=Europe/Rome:20180206T124500
DTSTAMP:20260408T060206
CREATED:20170816T120220Z
LAST-MODIFIED:20170816T120220Z
UID:3400-1517917500-1517921100@www.oa-roma.inaf.it
SUMMARY:A Panchromatic View of High-Redshift Quasar Host Galaxies
DESCRIPTION:While it is now widely accepted that the growth of supermassive black-holes in galaxies is fundamentally linked to the process of galaxy formation\, the host galaxies of the most luminous and massive accreting black-holes or quasars are still poorly understood. Quasars out-shine their host galaxies at most wavelengths making these studies difficult\, and the space-density of luminous quasars is also such that very wide-field surveys are required to be able to assemble statistical samples. I will present new observations of the host galaxies of a population of heavily reddened\, luminous quasars at redshifts of 2-3. Exploiting wide-field optical surveys together with the dust obscuration towards the quasar line-of-sight\, we are\, for the first time\, able to probe the rest-frame UV emission from the star-forming hosts of these high-luminosity quasars. Observations of the quasar host galaxies at sub-millimetre and millimetre wavelengths with SCUBA2\, ALMA and the VLA are also revealing complex gas morphologies\, diverse interstellar medium properties and evidence for significant over-densities and major-mergers.
URL:https://www.oa-roma.inaf.it/event/talk-by-manda-banerji/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20180206T114500
DTEND;TZID=Europe/Rome:20180206T124500
DTSTAMP:20260408T060206
CREATED:20170816T120220Z
LAST-MODIFIED:20170816T120220Z
UID:4723-1517917500-1517921100@www.oa-roma.inaf.it
SUMMARY:A Panchromatic View of High-Redshift Quasar Host Galaxies
DESCRIPTION:While it is now widely accepted that the growth of supermassive black-holes in galaxies is fundamentally linked to the process of galaxy formation\, the host galaxies of the most luminous and massive accreting black-holes or quasars are still poorly understood. Quasars out-shine their host galaxies at most wavelengths making these studies difficult\, and the space-density of luminous quasars is also such that very wide-field surveys are required to be able to assemble statistical samples. I will present new observations of the host galaxies of a population of heavily reddened\, luminous quasars at redshifts of 2-3. Exploiting wide-field optical surveys together with the dust obscuration towards the quasar line-of-sight\, we are\, for the first time\, able to probe the rest-frame UV emission from the star-forming hosts of these high-luminosity quasars. Observations of the quasar host galaxies at sub-millimetre and millimetre wavelengths with SCUBA2\, ALMA and the VLA are also revealing complex gas morphologies\, diverse interstellar medium properties and evidence for significant over-densities and major-mergers.
URL:https://www.oa-roma.inaf.it/event/talk-by-manda-banerji-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20180213T114500
DTEND;TZID=Europe/Rome:20180213T124500
DTSTAMP:20260408T060206
CREATED:20170911T152627Z
LAST-MODIFIED:20170911T152627Z
UID:3447-1518522300-1518525900@www.oa-roma.inaf.it
SUMMARY:Electromagnetic Counterparts of Gravitational Waves
DESCRIPTION:Compact binary systems composed by neutron stars (NS) and black holes (BH) are one of the principal sources of gravitational waves (GW) in the terrestrial interferometers frequency range (10 Hz -1 kHz). While BH binary coalescences are not expected in general to be accompanied by any electromagnetic signal\, detectable electromagnetic counterparts\, such as Short Gamma-Ray Bursts (SGRB) and Kilonovae\, could follow binary NS and NS-BH mergers.\nThe recent join GW and electromagnetic observation of a binary NS coalescence (GW170817) marked the down of multimessenger astronomy era that open a new way to explore the high energetic universe and test the fundamental physics under extreme conditions.\nThe coincident detection of gravitational and electromagnetic radiation is important because these messengers carry different and complementary informations: while from a GW detection it is possible to infer the masses and the spins of the binary progenitors\, electromagnetic emission is essential to localize the source\, thus enabling the host galaxy identification.\nIn this talk I will show how a joint detection of SGRB and GW from a NS-BH progenitor could be used to measure the neutron star radius and thus constrain the dense matter equation of state.\nI will also provide a brief description of isotropic electromagnetic counterpart of compact binary coalescence such as Kilonova and Spindown powered transients.
URL:https://www.oa-roma.inaf.it/event/seminar-by-stefano-ascenzi/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20180213T114500
DTEND;TZID=Europe/Rome:20180213T124500
DTSTAMP:20260408T060206
CREATED:20170911T152627Z
LAST-MODIFIED:20170911T152627Z
UID:4729-1518522300-1518525900@www.oa-roma.inaf.it
SUMMARY:Electromagnetic Counterparts of Gravitational Waves
DESCRIPTION:Compact binary systems composed by neutron stars (NS) and black holes (BH) are one of the principal sources of gravitational waves (GW) in the terrestrial interferometers frequency range (10 Hz -1 kHz). While BH binary coalescences are not expected in general to be accompanied by any electromagnetic signal\, detectable electromagnetic counterparts\, such as Short Gamma-Ray Bursts (SGRB) and Kilonovae\, could follow binary NS and NS-BH mergers.\nThe recent join GW and electromagnetic observation of a binary NS coalescence (GW170817) marked the down of multimessenger astronomy era that open a new way to explore the high energetic universe and test the fundamental physics under extreme conditions.\nThe coincident detection of gravitational and electromagnetic radiation is important because these messengers carry different and complementary informations: while from a GW detection it is possible to infer the masses and the spins of the binary progenitors\, electromagnetic emission is essential to localize the source\, thus enabling the host galaxy identification.\nIn this talk I will show how a joint detection of SGRB and GW from a NS-BH progenitor could be used to measure the neutron star radius and thus constrain the dense matter equation of state.\nI will also provide a brief description of isotropic electromagnetic counterpart of compact binary coalescence such as Kilonova and Spindown powered transients.
URL:https://www.oa-roma.inaf.it/event/seminar-by-stefano-ascenzi-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20180220T114500
DTEND;TZID=Europe/Rome:20180220T124500
DTSTAMP:20260408T060206
CREATED:20171016T082422Z
LAST-MODIFIED:20171016T082422Z
UID:3641-1519127100-1519130700@www.oa-roma.inaf.it
SUMMARY:Lyα-Lyman Continuum connection in 3.5 ≤ z ≤ 4.3 star-forming galaxies from the VUDS survey
DESCRIPTION:Understanding the processes that led to the reionization of the Universe is among the most challenging tasks of modern extra-galactic astronomy. The main responsible for this phenomenon are thought to be high redshift star-forming galaxies. However\, it is very difficult to constrain their contribution and only few detections of Lyman Continuum (LyC) emitters have been reported so far. Following theoretical models\, several so-called indirect indicators of LyC radiation have been proposed\, such as a strong Lyα emission\, a large OIII/OII ratio\, the compactness of the UV continuum and others. Using these pre-selection criteria has indeed proved to be a powerful method to identify LyC leakers at low redshift but there is a lack of consistent studies that relates these indicators to the LyC emission at high redshifts.\nWe have used ultra-deep spectra from the Vimos Ultra Deep Survey (VUDS) to investigate the LyC properties of z~4 star-forming galaxies. We initially investigated the LyC emission from a stack of ~33 sources free from foreground contamination\, selected after a very careful cleaning procedure based on the inspection of multi-wavelength high resolution HST imaging. We found for this sample a mean fesc\,rel=0.09±0.04 with no individual detections. We also observed a tentative correlation between the individual limits given in the LyC flux and the EW of the Lyα emission line. To better investigate this trend and other expected correlations with LyC properties of high redshift galaxies\, we then analysed a much larger sample of more than 200 objects also from the VUDS survey. We found evidence that LyC is strongly related to a large Lyα EW and to the UV compactness\, in agreement with theoretical expectations and observational studies at low redshift. In addition we found that galaxies with a small Lyα spatial extent have higher LyC flux compared to the rest of the population: such a correlation had never been analysed before and seems even stronger than the correlation with high Lyα EW and small UV effective radius.
URL:https://www.oa-roma.inaf.it/event/seminar-by-francesca-marchi/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20180220T114500
DTEND;TZID=Europe/Rome:20180220T124500
DTSTAMP:20260408T060206
CREATED:20171016T082422Z
LAST-MODIFIED:20171016T082422Z
UID:4734-1519127100-1519130700@www.oa-roma.inaf.it
SUMMARY:Lyα-Lyman Continuum connection in 3.5 ≤ z ≤ 4.3 star-forming galaxies from the VUDS survey
DESCRIPTION:Understanding the processes that led to the reionization of the Universe is among the most challenging tasks of modern extra-galactic astronomy. The main responsible for this phenomenon are thought to be high redshift star-forming galaxies. However\, it is very difficult to constrain their contribution and only few detections of Lyman Continuum (LyC) emitters have been reported so far. Following theoretical models\, several so-called indirect indicators of LyC radiation have been proposed\, such as a strong Lyα emission\, a large OIII/OII ratio\, the compactness of the UV continuum and others. Using these pre-selection criteria has indeed proved to be a powerful method to identify LyC leakers at low redshift but there is a lack of consistent studies that relates these indicators to the LyC emission at high redshifts.\nWe have used ultra-deep spectra from the Vimos Ultra Deep Survey (VUDS) to investigate the LyC properties of z~4 star-forming galaxies. We initially investigated the LyC emission from a stack of ~33 sources free from foreground contamination\, selected after a very careful cleaning procedure based on the inspection of multi-wavelength high resolution HST imaging. We found for this sample a mean fesc\,rel=0.09±0.04 with no individual detections. We also observed a tentative correlation between the individual limits given in the LyC flux and the EW of the Lyα emission line. To better investigate this trend and other expected correlations with LyC properties of high redshift galaxies\, we then analysed a much larger sample of more than 200 objects also from the VUDS survey. We found evidence that LyC is strongly related to a large Lyα EW and to the UV compactness\, in agreement with theoretical expectations and observational studies at low redshift. In addition we found that galaxies with a small Lyα spatial extent have higher LyC flux compared to the rest of the population: such a correlation had never been analysed before and seems even stronger than the correlation with high Lyα EW and small UV effective radius.
URL:https://www.oa-roma.inaf.it/event/seminar-by-francesca-marchi-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;VALUE=DATE:20180227
DTEND;VALUE=DATE:20180228
DTSTAMP:20260408T060206
CREATED:20180220T120259Z
LAST-MODIFIED:20180220T120259Z
UID:4023-1519689600-1519775999@www.oa-roma.inaf.it
SUMMARY:Assemblea del Personale.
DESCRIPTION:RICERCATORI\, TECNICI\, AMMINISTRATIVI\, PRECARI e STRUTTURATI DELL’ INAF – OAR\n \nASSEMBLEA DEL PERSONALE\n    Martedì 27 febbraio ore 10:00\nINAF– Monte Porzio\nPer discutere di: \n1) Stabilizzazioni e Piano Fabbisogno Personale INAF 2018/2020; \n2) Contrattazione integrativa; \n3) Nuovo contratto Istruzione e Ricerca; \n4)Elezioni RSU; \n  \nSaranno presenti all’ iniziativa : \n Stefano Bernabei – Coordinatore nazionale C.d.E. INAF FLC-CGIL\nCarlo Buttarelli – Coordinatore territoriale FLC – CGIL
URL:https://www.oa-roma.inaf.it/event/assemblea-del-personale/
LOCATION:OAR Monte Porzio Catone – aula Gratton\, Via Frascati 33\, Roma\, RM\, 00136\, Italia
END:VEVENT
BEGIN:VEVENT
DTSTART;VALUE=DATE:20180227
DTEND;VALUE=DATE:20180228
DTSTAMP:20260408T060206
CREATED:20180220T120259Z
LAST-MODIFIED:20180220T120259Z
UID:4745-1519689600-1519775999@www.oa-roma.inaf.it
SUMMARY:Assemblea del Personale.
DESCRIPTION:RICERCATORI\, TECNICI\, AMMINISTRATIVI\, PRECARI e STRUTTURATI DELL’ INAF – OAR\n \nASSEMBLEA DEL PERSONALE\n    Martedì 27 febbraio ore 10:00\nINAF– Monte Porzio\nPer discutere di: \n1) Stabilizzazioni e Piano Fabbisogno Personale INAF 2018/2020; \n2) Contrattazione integrativa; \n3) Nuovo contratto Istruzione e Ricerca; \n4)Elezioni RSU; \n  \nSaranno presenti all’ iniziativa : \n Stefano Bernabei – Coordinatore nazionale C.d.E. INAF FLC-CGIL\nCarlo Buttarelli – Coordinatore territoriale FLC – CGIL
URL:https://www.oa-roma.inaf.it/event/assemblea-del-personale-2/
LOCATION:OAR Monte Porzio Catone – aula Gratton\, Via Frascati 33\, Roma\, RM\, 00136\, Italia
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20180227T114500
DTEND;TZID=Europe/Rome:20180227T124500
DTSTAMP:20260408T060206
CREATED:20170728T202348Z
LAST-MODIFIED:20170728T202348Z
UID:3366-1519731900-1519735500@www.oa-roma.inaf.it
SUMMARY:Bright and dustiest stars in the JWST era: powerful tools to constrain the recent star formation history
DESCRIPTION:With the advent of the JWST\, the horizon of our knowledgies will be amazingly enlarged\, providing an unprecedent look of a large volume of galaxies with a broad properties range. This will be possible in the IR domain where the extinction is low and bright cool evolved stars have their emission peak. This is the case of asymptotic giant branch stars (AGB)\, luminous objects and main dust producers for the galaxy. We present how the large release of AGB+dust evolutionary models developed in the last years\, will enable a detailed study of these sources in different systems. The distribution of these objects in the IR colour-magnitude diagrams is a powerful instrument to determine the recent star formation history of the galaxy in detail.
URL:https://www.oa-roma.inaf.it/event/seminar-by-flavia-dellagli/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Europe/Rome:20180227T114500
DTEND;TZID=Europe/Rome:20180227T124500
DTSTAMP:20260408T060206
CREATED:20170728T202348Z
LAST-MODIFIED:20170728T202348Z
UID:4720-1519731900-1519735500@www.oa-roma.inaf.it
SUMMARY:Bright and dustiest stars in the JWST era: powerful tools to constrain the recent star formation history
DESCRIPTION:With the advent of the JWST\, the horizon of our knowledgies will be amazingly enlarged\, providing an unprecedent look of a large volume of galaxies with a broad properties range. This will be possible in the IR domain where the extinction is low and bright cool evolved stars have their emission peak. This is the case of asymptotic giant branch stars (AGB)\, luminous objects and main dust producers for the galaxy. We present how the large release of AGB+dust evolutionary models developed in the last years\, will enable a detailed study of these sources in different systems. The distribution of these objects in the IR colour-magnitude diagrams is a powerful instrument to determine the recent star formation history of the galaxy in detail.
URL:https://www.oa-roma.inaf.it/event/seminar-by-flavia-dellagli-2/
LOCATION:Aula Gratton
CATEGORIES:Seminari
END:VEVENT
END:VCALENDAR