It's the talk I gave in the Pucon Symposium 2015 about the Next Generation Fornax Survey and the discovery of a large number of dwarf galaxies in the Fornax cluster.
The neowise discovered_comet_population_and_the_co_co2_production_ratesSérgio Sacani
Após o seu lançamento em 2009, a sonda NEOWISE da NASA já observou 163 cometas durante a missão primária WISE/NEOWISE. Essa amostra do telescópio espacial representa a maior pesquisa infravermelha de cometas já feitas até o momento. Os dados dessa pesquisa estão dando uma nova ideia sobre a poeira, o tamanho dos núcleos do cometa, e a taxa de produção dos gases difíceis de serem observados como dióxido de carbono e monóxido de carbono. Os resultados do censo do NEOWISE dos cometas foram recentemente publicados no Astrophysical Journal.
O monóxido de carbono (CO) e o dióxido de carbono (CO2) são moléculas comuns encontradas no ambiente do início do Sistema Solar, e nos cometas. Na maior parte das circunstâncias, a sublimação do gelo de água provavelmente guia a atividade nos cometas quando eles chegam perto do Sol, mas em distâncias maiores e em temperaturas mais frias, outras moléculas como o CO e o CO2 podem ser os principais guias. O dióxido e o monóxido de carbono são moléculas difíceis de serem detectadas da terra, devido a abundância dessas moléculas na própria atmosfera terrestre que podem obscurecer o sinal. A sonda NEOWISE vaga além da atmosfera da Terra, fazendo essas medidas dos gases emitidos pelos cometas possíveis.
“Essa é a primeira vez que nós observamos essa grande evidência estatística do monóxido de carbono obtida enquanto o gás do cometa é emitido quando ele está mais distante do Sol”, disse James Bauer, vice-principal pesquisador da missão NEOWISE do Laboratório de Propulsão a Jato da NASA em Pasadena, na Califórnia, e autor do artigo. “Emitindo o que é provavelmente monóxido de carbono além de 4 Unidades Astronômicas, ou seja, 600 milhões de quilômetros, isso nos mostra que os cometas podem ter guardado a maior parte dos gases quando eles se formaram, e ficaram ali guardados por bilhões de anos. A maioria dos cometas que nós observamos ativos além das 4 Unidades Astronômicas, são cometas de períodos longos, cometas com períodos orbitais maiores que 200 anos que gastam a maior parte da sua vida além da órbita de Netuno”.
O telescópio de rastreio VISTA do ESO encontrou uma horda de galáxias massivas anteriormente ocultas por poeira, que existiram quando o Universo era ainda bebê. Ao descobrir e estudar uma grande quantidade deste tipo de galáxias, os astrônomos descobriram, exatamente e pela primeira vez, quando é que tais monstros apareceram pela primeira vez no Universo.
O simples fato de contar o número de galáxias que existem em determinada área do céu permite aos astrônomos testar teorias de formação e evolução galática. No entanto, uma tarefa aparentemente tão fácil torna-se mais difícil quando tentamos contar galáxias cada vez mais distantes e tênues e é mais complicada ainda devido ao fato das galáxias mais brilhantes e fáceis de observar — as mais massivas no Universo — se tornarem mais raras à medida que os astrônomos observam o passado do Universo, enquanto que as galáxias menos brilhantes, mas muito mais numerosas, são ainda mais difíceis de detectar.
Uma equipe de astrônomos liderada por Karina Caputi do Instituto Astronômico Kapteyn da Universidade de Groningen, descobriu muitas galáxias distantes que não tinham sido detectadas anteriormente. A equipe utilizou imagens do rastreioUltraVISTA, um dos seis projetos que usam o VISTA para mapear o céu no infravermelho próximo, e fez um censo das galáxias tênues quando a idade do Universo estava compreendida entre 0,75 e 2,1 bilhões de anos.
The operational environment and rotational acceleration of asteroid (101955) ...Sérgio Sacani
During its approach to asteroid (101955) Bennu, NASA’s Origins, Spectral Interpretation,
Resource Identification, and Security-Regolith Explorer (OSIRIS-REx) spacecraft surveyed
Bennu’s immediate environment, photometric properties, and rotation state. Discovery of
a dusty environment, a natural satellite, or unexpected asteroid characteristics would have
had consequences for the mission’s safety and observation strategy. Here we show that
spacecraft observations during this period were highly sensitive to satellites (sub-meter
scale) but reveal none, although later navigational images indicate that further investigation is
needed. We constrain average dust production in September 2018 from Bennu’s surface
to an upper limit of 150 g s–1 averaged over 34 min. Bennu’s disk-integrated photometric
phase function validates measurements from the pre-encounter astronomical campaign.
We demonstrate that Bennu’s rotation rate is accelerating continuously at 3.63 ± 0.52 × 10–6
degrees day–2, likely due to the Yarkovsky–O’Keefe–Radzievskii–Paddack (YORP) effect, with
evolutionary implications.
A radiation belt of energetic protonslocated between Saturn and its ringsSérgio Sacani
Most magnetized planetsare known to possess radiation belts, wherehigh-energy charged particles are trapped inlarge numbers. The possibility that a radiationbelt could exist also in the confined regionbetween Saturn and its main rings has beenproposed on the basis of remote sensing obser-vations and simulations. It was not until thefinal 5 months of the Cassini mission that in situmeasurements were obtained from this regionwith the Magnetosphere Imaging Instrument(MIMI). This paper provides an overview ofthese measurements andtheir interpretation.
The neowise discovered_comet_population_and_the_co_co2_production_ratesSérgio Sacani
Após o seu lançamento em 2009, a sonda NEOWISE da NASA já observou 163 cometas durante a missão primária WISE/NEOWISE. Essa amostra do telescópio espacial representa a maior pesquisa infravermelha de cometas já feitas até o momento. Os dados dessa pesquisa estão dando uma nova ideia sobre a poeira, o tamanho dos núcleos do cometa, e a taxa de produção dos gases difíceis de serem observados como dióxido de carbono e monóxido de carbono. Os resultados do censo do NEOWISE dos cometas foram recentemente publicados no Astrophysical Journal.
O monóxido de carbono (CO) e o dióxido de carbono (CO2) são moléculas comuns encontradas no ambiente do início do Sistema Solar, e nos cometas. Na maior parte das circunstâncias, a sublimação do gelo de água provavelmente guia a atividade nos cometas quando eles chegam perto do Sol, mas em distâncias maiores e em temperaturas mais frias, outras moléculas como o CO e o CO2 podem ser os principais guias. O dióxido e o monóxido de carbono são moléculas difíceis de serem detectadas da terra, devido a abundância dessas moléculas na própria atmosfera terrestre que podem obscurecer o sinal. A sonda NEOWISE vaga além da atmosfera da Terra, fazendo essas medidas dos gases emitidos pelos cometas possíveis.
“Essa é a primeira vez que nós observamos essa grande evidência estatística do monóxido de carbono obtida enquanto o gás do cometa é emitido quando ele está mais distante do Sol”, disse James Bauer, vice-principal pesquisador da missão NEOWISE do Laboratório de Propulsão a Jato da NASA em Pasadena, na Califórnia, e autor do artigo. “Emitindo o que é provavelmente monóxido de carbono além de 4 Unidades Astronômicas, ou seja, 600 milhões de quilômetros, isso nos mostra que os cometas podem ter guardado a maior parte dos gases quando eles se formaram, e ficaram ali guardados por bilhões de anos. A maioria dos cometas que nós observamos ativos além das 4 Unidades Astronômicas, são cometas de períodos longos, cometas com períodos orbitais maiores que 200 anos que gastam a maior parte da sua vida além da órbita de Netuno”.
O telescópio de rastreio VISTA do ESO encontrou uma horda de galáxias massivas anteriormente ocultas por poeira, que existiram quando o Universo era ainda bebê. Ao descobrir e estudar uma grande quantidade deste tipo de galáxias, os astrônomos descobriram, exatamente e pela primeira vez, quando é que tais monstros apareceram pela primeira vez no Universo.
O simples fato de contar o número de galáxias que existem em determinada área do céu permite aos astrônomos testar teorias de formação e evolução galática. No entanto, uma tarefa aparentemente tão fácil torna-se mais difícil quando tentamos contar galáxias cada vez mais distantes e tênues e é mais complicada ainda devido ao fato das galáxias mais brilhantes e fáceis de observar — as mais massivas no Universo — se tornarem mais raras à medida que os astrônomos observam o passado do Universo, enquanto que as galáxias menos brilhantes, mas muito mais numerosas, são ainda mais difíceis de detectar.
Uma equipe de astrônomos liderada por Karina Caputi do Instituto Astronômico Kapteyn da Universidade de Groningen, descobriu muitas galáxias distantes que não tinham sido detectadas anteriormente. A equipe utilizou imagens do rastreioUltraVISTA, um dos seis projetos que usam o VISTA para mapear o céu no infravermelho próximo, e fez um censo das galáxias tênues quando a idade do Universo estava compreendida entre 0,75 e 2,1 bilhões de anos.
The operational environment and rotational acceleration of asteroid (101955) ...Sérgio Sacani
During its approach to asteroid (101955) Bennu, NASA’s Origins, Spectral Interpretation,
Resource Identification, and Security-Regolith Explorer (OSIRIS-REx) spacecraft surveyed
Bennu’s immediate environment, photometric properties, and rotation state. Discovery of
a dusty environment, a natural satellite, or unexpected asteroid characteristics would have
had consequences for the mission’s safety and observation strategy. Here we show that
spacecraft observations during this period were highly sensitive to satellites (sub-meter
scale) but reveal none, although later navigational images indicate that further investigation is
needed. We constrain average dust production in September 2018 from Bennu’s surface
to an upper limit of 150 g s–1 averaged over 34 min. Bennu’s disk-integrated photometric
phase function validates measurements from the pre-encounter astronomical campaign.
We demonstrate that Bennu’s rotation rate is accelerating continuously at 3.63 ± 0.52 × 10–6
degrees day–2, likely due to the Yarkovsky–O’Keefe–Radzievskii–Paddack (YORP) effect, with
evolutionary implications.
A radiation belt of energetic protonslocated between Saturn and its ringsSérgio Sacani
Most magnetized planetsare known to possess radiation belts, wherehigh-energy charged particles are trapped inlarge numbers. The possibility that a radiationbelt could exist also in the confined regionbetween Saturn and its main rings has beenproposed on the basis of remote sensing obser-vations and simulations. It was not until thefinal 5 months of the Cassini mission that in situmeasurements were obtained from this regionwith the Magnetosphere Imaging Instrument(MIMI). This paper provides an overview ofthese measurements andtheir interpretation.
-Neutrino-
It's believed that modern physics nothing can travel faster than the speed of light. The astonishing results of the experiment seem to show that elementary particle Neutrinos, Can. It’s the most spread particles and the lightest. Neutrino is a hardly reacting with matter, It can travel right through the earth without interacting, As an example 70 billion Neutrinos per square second continue coming from the sun. These Neutrino parts traveled through the Earth Crust to the detection point and they synchronized between the 2 points to the nearest Nanno second (A billion of a second) in this distance, they discovered that the neutrino were 60 seconds ahead of what light takes to cover this distance. It's the first time we have an experimental evidence something faster than light and that will make a major change in physics as we know it now.
The most luminous_galaxies_discovered_by_wiseSérgio Sacani
Artigo descreve estudo feito por astrônomos e com a ajuda da sonda WISE da NASA para identificar as galáxias do tipo ELIRGs, entre elas a mais luminosa galáxia do universo, com um buraco negro gigantesco em seu interior e localizada a cerca de 12.8 bilhões de anos de distância da Terra.
The harps n-rocky_planet_search_hd219134b_transiting_rocky_planetSérgio Sacani
Usando o espectrógrafo HARPS-N acoplado ao Telescopio Nazionale Galileo no Observatório de Roque de Los Muchachos, nas Ilhas Canárias, os astrônomos descobriram três exoplanetas, classificados como Super-Terras e um gigante gasoso orbitando uma estrela próxima, chamada de HD 219134.
A HD 219134, também conhecida como HR 8832 é uma estrela do tipo anã-K de quinta magnitude, localizada a aproximadamente 21 anos-luz de distância da Terra, na constelação de Cassiopeia.
A estrela é levemente mais fria e menos massiva que o nosso sol. Ela é tão brilhante que pode ser observada a olho nu.
O sistema planetário HD 219134, abriga um planeta gigante gasoso externo e três planetas internos classificados como super-Terras, um dos quais transita em frente à estrela.
O Telescópio Espacial Hubble das agências NASA e ESA registrou a imagem pela primeira vez da explosão prevista de uma supernova. O reaparecimento da supernova Refsdal foi calculado a partir de diferentes modelos de aglomerados de galáxias, cuja imensa gravidade está entortando a luz da supernova.
Muitas estrelas terminam a sua vida com uma explosão, mas somente poucas dessas explosões estelares têm sido registradas no ato que acontecem. Quando isso acontece, é pura sorte, pelo menos até agora. No dia 11 de Dezembro de 2015, os astrônomos não somente fizeram a imagem de uma supernova em ação, como também observaram quando e onde ela estava prevista para acontecer.
A supernova, apelidada de Refsdal, foi registrada no aglomerado de galáxias, conhecido como MACS J1149.5+2223. Enquanto que a luz do aglomerado gasta cerca de cinco bilhões de anos para chegar até nós, a supernova explodiu muito tempo antes, a aproximadamente 10 bilhões de anos atrás.
A história da Refsdal começou em Novembro de 2014, quando os cientistas registraram quatro imagens separadas da supernova num raro arranjo conhecido como Cruz de Einstein, ao redor de uma galáxia dentro do MACS J1149.5+2223. A ilusão de óptica cósmica ocorreu devido ao fato da massa de uma única galáxia dentro do aglomerado estar entortando e ampliando a luz da distante explosão estelar, num processo conhecido como lente gravitacional.
Galaxy and mass_assembly_gama_panchromatic_data_release_and__the_low_energy_b...Sérgio Sacani
Uma equipe internacional de astrônomos estudou mais de 200 000 galáxias e mediu a energia gerada numa enorme região do espaço com a maior precisão até hoje. Este estudo representa a estimativa mais completa de produção de energia no Universo próximo. A equipe confirmou que a energia produzida nesta região do Universo de hoje é apenas cerca de metade da produzida há dois bilhões de anos atrás e descobriu que este enfraquecimento ocorre em todos os comprimentos de onda que vão desde o ultravioleta ao infravermelho longínquo. O Universo está morrendo lentamente.
O estudo envolve muitos dos telescópios mais poderosos do mundo, incluindo o VISTA e o VST — os telescópios de rastreio do ESO, instalados no Observatório do Paranal, no Chile. Observações de suporte foram obtidas por dois telescópios espaciais operados pela NASA (GALEX e WISE) e por um outro pertencente à Agência Espacial Europeia (Herschel) [1].
Este trabalho realizou-se no âmbito do projeto Galaxy And Mass Assembly (GAMA), o maior rastreio já realizado em múltiplos comprimentos de onda.
“Usamos tantos telescópios terrestres e espaciais quanto nos foi possível para medir a produção de energia de cerca de 200 000 galáxias ao longo do maior intervalo de comprimentos de onda possível,” disse Simon Driver (ICRAR, The University of Western Australia), que lidera a enorme equipe GAMA.
Chandra deep observation_of_xdcpj004402033_a_massive_galaxy_cluster_at_z_1_5Sérgio Sacani
Artigo apresenta os resultados obtidos pelo Chandra ao medir com precisão a massa do mais massivo aglomerado de galáxias do universo distante, o Aglomerado Gioiello.
Academic Research: 25 Tools and Resources to Help You Write a Good Paperacademicresearch
Academic research is the integral part of education process, and it is a common struggle among students. Check the following tools to make your paper stand out! Visit: http://papers4.sale/academic-research-write-good-paper/
-Neutrino-
It's believed that modern physics nothing can travel faster than the speed of light. The astonishing results of the experiment seem to show that elementary particle Neutrinos, Can. It’s the most spread particles and the lightest. Neutrino is a hardly reacting with matter, It can travel right through the earth without interacting, As an example 70 billion Neutrinos per square second continue coming from the sun. These Neutrino parts traveled through the Earth Crust to the detection point and they synchronized between the 2 points to the nearest Nanno second (A billion of a second) in this distance, they discovered that the neutrino were 60 seconds ahead of what light takes to cover this distance. It's the first time we have an experimental evidence something faster than light and that will make a major change in physics as we know it now.
The most luminous_galaxies_discovered_by_wiseSérgio Sacani
Artigo descreve estudo feito por astrônomos e com a ajuda da sonda WISE da NASA para identificar as galáxias do tipo ELIRGs, entre elas a mais luminosa galáxia do universo, com um buraco negro gigantesco em seu interior e localizada a cerca de 12.8 bilhões de anos de distância da Terra.
The harps n-rocky_planet_search_hd219134b_transiting_rocky_planetSérgio Sacani
Usando o espectrógrafo HARPS-N acoplado ao Telescopio Nazionale Galileo no Observatório de Roque de Los Muchachos, nas Ilhas Canárias, os astrônomos descobriram três exoplanetas, classificados como Super-Terras e um gigante gasoso orbitando uma estrela próxima, chamada de HD 219134.
A HD 219134, também conhecida como HR 8832 é uma estrela do tipo anã-K de quinta magnitude, localizada a aproximadamente 21 anos-luz de distância da Terra, na constelação de Cassiopeia.
A estrela é levemente mais fria e menos massiva que o nosso sol. Ela é tão brilhante que pode ser observada a olho nu.
O sistema planetário HD 219134, abriga um planeta gigante gasoso externo e três planetas internos classificados como super-Terras, um dos quais transita em frente à estrela.
O Telescópio Espacial Hubble das agências NASA e ESA registrou a imagem pela primeira vez da explosão prevista de uma supernova. O reaparecimento da supernova Refsdal foi calculado a partir de diferentes modelos de aglomerados de galáxias, cuja imensa gravidade está entortando a luz da supernova.
Muitas estrelas terminam a sua vida com uma explosão, mas somente poucas dessas explosões estelares têm sido registradas no ato que acontecem. Quando isso acontece, é pura sorte, pelo menos até agora. No dia 11 de Dezembro de 2015, os astrônomos não somente fizeram a imagem de uma supernova em ação, como também observaram quando e onde ela estava prevista para acontecer.
A supernova, apelidada de Refsdal, foi registrada no aglomerado de galáxias, conhecido como MACS J1149.5+2223. Enquanto que a luz do aglomerado gasta cerca de cinco bilhões de anos para chegar até nós, a supernova explodiu muito tempo antes, a aproximadamente 10 bilhões de anos atrás.
A história da Refsdal começou em Novembro de 2014, quando os cientistas registraram quatro imagens separadas da supernova num raro arranjo conhecido como Cruz de Einstein, ao redor de uma galáxia dentro do MACS J1149.5+2223. A ilusão de óptica cósmica ocorreu devido ao fato da massa de uma única galáxia dentro do aglomerado estar entortando e ampliando a luz da distante explosão estelar, num processo conhecido como lente gravitacional.
Galaxy and mass_assembly_gama_panchromatic_data_release_and__the_low_energy_b...Sérgio Sacani
Uma equipe internacional de astrônomos estudou mais de 200 000 galáxias e mediu a energia gerada numa enorme região do espaço com a maior precisão até hoje. Este estudo representa a estimativa mais completa de produção de energia no Universo próximo. A equipe confirmou que a energia produzida nesta região do Universo de hoje é apenas cerca de metade da produzida há dois bilhões de anos atrás e descobriu que este enfraquecimento ocorre em todos os comprimentos de onda que vão desde o ultravioleta ao infravermelho longínquo. O Universo está morrendo lentamente.
O estudo envolve muitos dos telescópios mais poderosos do mundo, incluindo o VISTA e o VST — os telescópios de rastreio do ESO, instalados no Observatório do Paranal, no Chile. Observações de suporte foram obtidas por dois telescópios espaciais operados pela NASA (GALEX e WISE) e por um outro pertencente à Agência Espacial Europeia (Herschel) [1].
Este trabalho realizou-se no âmbito do projeto Galaxy And Mass Assembly (GAMA), o maior rastreio já realizado em múltiplos comprimentos de onda.
“Usamos tantos telescópios terrestres e espaciais quanto nos foi possível para medir a produção de energia de cerca de 200 000 galáxias ao longo do maior intervalo de comprimentos de onda possível,” disse Simon Driver (ICRAR, The University of Western Australia), que lidera a enorme equipe GAMA.
Chandra deep observation_of_xdcpj004402033_a_massive_galaxy_cluster_at_z_1_5Sérgio Sacani
Artigo apresenta os resultados obtidos pelo Chandra ao medir com precisão a massa do mais massivo aglomerado de galáxias do universo distante, o Aglomerado Gioiello.
Academic Research: 25 Tools and Resources to Help You Write a Good Paperacademicresearch
Academic research is the integral part of education process, and it is a common struggle among students. Check the following tools to make your paper stand out! Visit: http://papers4.sale/academic-research-write-good-paper/
The muse 3_d_view_of_the_hubble_deep_field_southSérgio Sacani
Artigo mostra como foram as observações feitas com o MUSE, o novo instrumento do VLT do campo profundo do Hubble. Além de descobrir 20 novos objetos, o MUSE conseguiu medir as propriedades das galáxias e até representar as mais próximas em 3 dimensões.
The Large Interferometer For Exoplanets (LIFE): the science of characterising...Advanced-Concepts-Team
Studying the atmospheres of a statistically significant number of rocky, terrestrial exoplanets - including the search for habitable and potentially inhabited planets - is one of the major goals of exoplanetary science and possibly the most challenging question in 21st century astrophysics. However, despite being at the top of the agenda of all major space agencies and ground-based observatories, none of the currently planned projects or missions worldwide has the technical capabilities to achieve this goal. In this talk we present new results from the LIFE Mission initiative, which addresses this issue by investigating the scientific potential of a mid infrared nulling interferometer observatory. Here we will focus on the mission's yield estimates, our simulator software as well as various exemplary science cases such as observing Earth- and Venus-twins or searching for phosphine in exoplanetary atmospheres.
Venus cloud discontinuity in 2022 The first long-term study with uninterrupte...Sérgio Sacani
First identified in 2016 by the Japan Aerospace eXploration Agency (JAXA) Akatsuki mission, the discontinuity or disruption is a recurrent wave observed to propagate over decades at the deeper clouds of Venus (47–56 km above the surface), while its
absence at the top of the clouds (∼70 km) suggests that it dissipates at the upper clouds and contributes to the maintenance of the
puzzling atmospheric superrotation of Venus through wave-mean flow interaction.
Aims. Taking advantage of the campaign of ground-based observations undertaken in coordination with the Akatsuki mission from
December 2021 until July 2022, we undertook the longest uninterrupted monitoring of the cloud discontinuity to date to obtain a
pioneering long-term characterisation of its main properties and to better constrain its recurrence and lifetime.
Methods. The dayside upper, middle, and nightside lower clouds were studied with images acquired by the Akatsuki Ultraviolet
Imager (UVI), amateur observers, and SpeX at the NASA Infrared Telescope Facility (IRTF). Hundreds of images were inspected in
search of the discontinuity events and to measure key properties such as its dimensions, orientation, and rotation period.
Results. We succeeded in tracking the discontinuity at the middle clouds during 109 days without interruption. The discontinuity
exhibited properties nearly identical to measurements in 2016 and 2020, with an orientation of 91◦ ± 8
◦
, length of 4100 ± 800 km,
width of 500 ± 100 km, and a rotation period of 5.11 ± 0.09 days. Ultraviolet images during 13–14 June 2022 suggest that the
discontinuity may have manifested at t
Matter ejections behind the highs and lows of the transitional millisecond pu...Sérgio Sacani
Transitional millisecond pulsars are an emerging class of sources linking low-mass X-ray binaries to millisecond radio pulsars in
binary systems. These pulsars alternate between a radio pulsar state and an active low-luminosity X-ray disc state. During the active
state, these sources exhibit two distinct emission modes (high and low) that alternate unpredictably, abruptly, and incessantly. X-ray
to optical pulsations are observed only during the high mode. Knowledge of the root reason for this puzzling behaviour remains
elusive. This paper presents the results of the most extensive multi-wavelength campaign ever conducted on the transitional pulsar
prototype, PSR J1023+0038, covering from radio to X-rays. The campaign was carried out over two nights in June 2021, and involved
12 different telescopes and instruments including XMM-Newton, HST, VLT/FORS2 (in polarimetric mode), ALMA, VLA and FAST.
By modelling the broadband spectral energy distributions in both emission modes, we show that the mode switches are caused by
changes in the innermost region of the accretion disc. These changes trigger the emission of discrete mass ejections, which occur on
top of a compact jet, as testified by the detection of at least one short-duration millimetre flare with A
Beyond the Kuiper Belt Edge: New High Perihelion Trans-Neptunian Objects With...Sérgio Sacani
We are conducting a survey for distant solar system objects beyond the Kuiper
Belt edge ( 50 AU) with new wide-field cameras on the Subaru and CTIO tele-
scopes. We are interested in the orbits of objects that are decoupled from the
giant planet region in order to understand the structure of the outer solar sys-
tem, including whether a massive planet exists beyond a few hundred AU as first
reported in Trujillo and Sheppard (2014). In addition to discovering extreme
trans-Neptunian objects detailed elsewhere, we have found several objects with
high perihelia (q > 40 AU) that differ from the extreme and inner Oort cloud
objects due to their moderate semi-major axes (50 < a < 100 AU) and eccen-
tricities (e . 0.3). Newly discovered objects 2014 FZ71 and 2015 FJ345 have
the third and fourth highest perihelia known after Sedna and 2012 VP113, yet
their orbits are not nearly as eccentric or distant. We found several of these high
perihelion but moderate orbit objects and observe that they are mostly near Nep-
tune mean motion resonances and have significant inclinations (i > 20 degrees).
These moderate objects likely obtained their unusual orbits through combined
interactions with Neptune’s mean motion resonances and the Kozai resonance,
similar to the origin scenarios for 2004 XR190. We also find the distant 2008
ST291 has likely been modified by the MMR+KR mechanism through the 6:1
Neptune resonance. We discuss these moderately eccentric, distant objects along
with some other interesting low inclination outer classical belt objects like 2012
FH84 discovered in our ongoing survey.
Observation of Io’s Resurfacing via Plume Deposition Using Ground-based Adapt...Sérgio Sacani
Since volcanic activity was first discovered on Io from Voyager images in 1979, changes
on Io’s surface have been monitored from both spacecraft and ground-based telescopes.
Here, we present the highest spatial resolution images of Io ever obtained from a groundbased telescope. These images, acquired by the SHARK-VIS instrument on the Large
Binocular Telescope, show evidence of a major resurfacing event on Io’s trailing hemisphere. When compared to the most recent spacecraft images, the SHARK-VIS images
show that a plume deposit from a powerful eruption at Pillan Patera has covered part
of the long-lived Pele plume deposit. Although this type of resurfacing event may be common on Io, few have been detected due to the rarity of spacecraft visits and the previously low spatial resolution available from Earth-based telescopes. The SHARK-VIS instrument ushers in a new era of high resolution imaging of Io’s surface using adaptive
optics at visible wavelengths.
Fleeting Small-scale Surface Magnetic Fields Build the Quiet-Sun CoronaSérgio Sacani
Arch-like loop structures filled with million Kelvin hot plasma form the building blocks of the quiet-Sun corona.
Both high-resolution observations and magnetoconvection simulations show the ubiquitous presence of magnetic
fields on the solar surface on small spatial scales of ∼100 km. However, the question of how exactly these quietSun coronal loops originate from the photosphere and how the magnetic energy from the surface is channeled to
heat the overlying atmosphere is a long-standing puzzle. Here we report high-resolution photospheric magnetic
field and coronal data acquired during the second science perihelion of Solar Orbiter that reveal a highly dynamic
magnetic landscape underlying the observed quiet-Sun corona. We found that coronal loops often connect to
surface regions that harbor fleeting weaker, mixed-polarity magnetic field patches structured on small spatial
scales, and that coronal disturbances could emerge from these areas. We suggest that weaker magnetic fields with
fluxes as low as 1015 Mx and/or those that evolve on timescales less than 5 minutes are crucial to understanding
the coronal structuring and dynamics.
Detection of an atmosphere around the super earth 55 cancri eSérgio Sacani
We report the analysis of two new spectroscopic observations of the super-Earth 55 Cancri e, in the near
infrared, obtained with the WFC3 camera onboard the HST. 55 Cancri e orbits so close to its parent
star, that temperatures much higher than 2000 K are expected on its surface. Given the brightness
of 55 Cancri, the observations were obtained in scanning mode, adopting a very long scanning length
and a very high scanning speed. We use our specialized pipeline to take into account systematics
introduced by these observational parameters when coupled with the geometrical distortions of the
instrument. We measure the transit depth per wavelength channel with an average relative uncertainty
of 22 ppm per visit and nd modulations that depart from a straight line model with a 6 condence
level. These results suggest that 55 Cancri e is surrounded by an atmosphere, which is probably
hydrogen-rich. Our fully Bayesian spectral retrieval code, T -REx, has identied HCN to be the
most likely molecular candidate able to explain the features at 1.42 and 1.54 m. While additional
spectroscopic observations in a broader wavelength range in the infrared will be needed to conrm
the HCN detection, we discuss here the implications of such result. Our chemical model, developed
with combustion specialists, indicates that relatively high mixing ratios of HCN may be caused by a
high C/O ratio. This result suggests this super-Earth is a carbon-rich environment even more exotic
than previously thought.
Alexandru Marcu - "Faculty of physics, University of Cluj"SEENET-MTP
Prof. Alexandru Marcu presented Faculty of Physics, Babes-Bolyai University, Cluj-Napoca (Romania) at the SEENET-MTP RC & EC meeting held in Timisoara (Romania), November 22, 2014.
The fornax deep_survey_with_vst_i_the_extended_and_diffuse_stellar_halo_of_ng...Sérgio Sacani
We have started a new deep, multi-imaging survey of the Fornax cluster, dubbed Fornax Deep
Survey (FDS), at the VLT Survey Telescope. In this paper we present the deep photometry inside
two square degrees around the bright galaxy NGC 1399 in the core of the cluster. We found that
the core of the Fornax cluster is characterised by a very extended and diffuse envelope surrounding
the luminous galaxy NGC 1399: we map the surface brightness out to 33 arcmin (∼ 192 kpc)
from the galaxy center and down to μg ∼ 31 mag arcsec−2 in the g band. The deep photometry
allows us to detect a faint stellar bridge in the intracluster region on the west side of NGC 1399
and towards NGC 1387. By analyzing the integrated colors of this feature, we argue that it
could be due to the ongoing interaction between the two galaxies, where the outer envelope of
NGC 1387 on its east side is stripped away. By fitting the light profile, we found that exists a
physical break radius in the total light distribution at R = 10 arcmin (∼ 58 kpc) that sets the
transition region between the bright central galaxy and the outer exponential halo, and that the
stellar halo contributes for 60% of the total light of the galaxy (Sec. 3.5). We discuss the main
implications of this work on the build-up of the stellar halo at the center of the Fornax cluster.
By comparing with the numerical simulations of the stellar halo formation for the most massive
BCGs (i.e. 13 < logM200/M⊙ < 14), we find that the observed stellar halo mass fraction is
consistent with a halo formed through the multiple accretion of progenitors with stellar mass in
the range 108 − 1011 M⊙. This might suggest that the halo of NGC 1399 has also gone through
a major merging event. The absence of a significant number of luminous stellar streams and
tidal tails out to 192 kpc suggests that the epoch of this strong interaction goes back to an early
formation epoch. Therefore, differently from the Virgo cluster, the extended stellar halo around
NGC 1399 is characterised by a more diffuse and well-mixed component, including the ICL.
Los avances tecnológicos del último siglo nos han permitido abrir nuevas ventanas de exploración y nos han ayudado a empujar las fronteras del conocimiento. Gracias a la introducción de computadores cada vez más veloces e instrumentos astronómicos cada vez más sensibles a la luz, hoy en día contamos con catálogos de cientos de millones de estrellas y galaxias que habitan en nuestro Universo. Vivimos en la Era de la información y la exploración del Universo requiere que sepamos de Astronomía, Informática y Estadística.
Global AI nights - Casos de uso de ML en AstronomiaRoberto Muñoz
Charla que dicte en el capitulo chileno de Global AI Nights en Septiembre del 2019. Se muestran dos casos de uso para observatorios astronomicos en Chile
Inserción de científicos en la industria tecnológicaRoberto Muñoz
Charla que dicté en el 1er Workshop de Innovación organizado por la Universidad de Santiago de Chile. Presento el actual escenario en latinoamerica y Chile acerca de la inserción de científicos en el sector productivo. Cierro entregando un par ce consejos a estudiantes de pregrado y posgrado en disciplinas científicas.
An invited talk I gave in the Observatorio de Cordoba in Argentina. I talk about my research in Astronomy and how I made the transition from academia to industry.
I will list the main differences between the academic and industrial research, what skills are the most valued by tech companies and how young scientists can make the move to industry as smoothly and successful as possible.
Avances y desafíos en la exploración del UniversoRoberto Muñoz
Charla que dicté en el colegio Sol de Chile de la comuna de Los Espejo en Santiago, Chile. La charla estuvo enmarcada dentro de las actividades del Día del Asteroide.
Video analytics: Mejorando la seguridad y calidad de vidaRoberto Muñoz
Charla que dicté en el evento de Internet of Things organizado por Microsoft y MetricArts en Chile. Se discute acerca de la solución tecnológica que hemos desarrollado para mejorar la seguridad en el transporte público y la ciudad.
Tutorial de Data Science que dicté en el workshop CIO Update 2016. Enseño la revolución en el procesamiento de datos, la transición al cuarto paradigma del descubrimiento científico y las herramientas comúnmente empleadas en Data Science. Charla dictada el 19 de agosto del 2016 http://www.cioupdate.cl
From astronomy to video analytics industryRoberto Muñoz
Talk I gave at the 3rd Astroengineering workshop in Santiago, Chile. Projects I'm currently involved as a researcher in an Institute of Astrophysics and a Business intelligence company.
Efficient data reduction and analysis of DECam images using multicore archite...Roberto Muñoz
A talk I gave in the workshop "Tools for astronomical big data" held in Tucson, Arizona on March 2015. My talk was about how to do data science and big data in Astronomy having a small budget.
Astronomía en la era del big data - Arica, junio del 2015Roberto Muñoz
Charla dada en la ciudad de Arica, Chile acerca de cómo la comunidad astronómica chilena se está preparando para el tsunami de datos que están generando los telescopios en territorio nacional.
Chatty Kathy - UNC Bootcamp Final Project Presentation - Final Version - 5.23...John Andrews
SlideShare Description for "Chatty Kathy - UNC Bootcamp Final Project Presentation"
Title: Chatty Kathy: Enhancing Physical Activity Among Older Adults
Description:
Discover how Chatty Kathy, an innovative project developed at the UNC Bootcamp, aims to tackle the challenge of low physical activity among older adults. Our AI-driven solution uses peer interaction to boost and sustain exercise levels, significantly improving health outcomes. This presentation covers our problem statement, the rationale behind Chatty Kathy, synthetic data and persona creation, model performance metrics, a visual demonstration of the project, and potential future developments. Join us for an insightful Q&A session to explore the potential of this groundbreaking project.
Project Team: Jay Requarth, Jana Avery, John Andrews, Dr. Dick Davis II, Nee Buntoum, Nam Yeongjin & Mat Nicholas
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Empowering the Data Analytics Ecosystem: A Laser Focus on Value
The data analytics ecosystem thrives when every component functions at its peak, unlocking the true potential of data. Here's a laser focus on key areas for an empowered ecosystem:
1. Democratize Access, Not Data:
Granular Access Controls: Provide users with self-service tools tailored to their specific needs, preventing data overload and misuse.
Data Catalogs: Implement robust data catalogs for easy discovery and understanding of available data sources.
2. Foster Collaboration with Clear Roles:
Data Mesh Architecture: Break down data silos by creating a distributed data ownership model with clear ownership and responsibilities.
Collaborative Workspaces: Utilize interactive platforms where data scientists, analysts, and domain experts can work seamlessly together.
3. Leverage Advanced Analytics Strategically:
AI-powered Automation: Automate repetitive tasks like data cleaning and feature engineering, freeing up data talent for higher-level analysis.
Right-Tool Selection: Strategically choose the most effective advanced analytics techniques (e.g., AI, ML) based on specific business problems.
4. Prioritize Data Quality with Automation:
Automated Data Validation: Implement automated data quality checks to identify and rectify errors at the source, minimizing downstream issues.
Data Lineage Tracking: Track the flow of data throughout the ecosystem, ensuring transparency and facilitating root cause analysis for errors.
5. Cultivate a Data-Driven Mindset:
Metrics-Driven Performance Management: Align KPIs and performance metrics with data-driven insights to ensure actionable decision making.
Data Storytelling Workshops: Equip stakeholders with the skills to translate complex data findings into compelling narratives that drive action.
Benefits of a Precise Ecosystem:
Sharpened Focus: Precise access and clear roles ensure everyone works with the most relevant data, maximizing efficiency.
Actionable Insights: Strategic analytics and automated quality checks lead to more reliable and actionable data insights.
Continuous Improvement: Data-driven performance management fosters a culture of learning and continuous improvement.
Sustainable Growth: Empowered by data, organizations can make informed decisions to drive sustainable growth and innovation.
By focusing on these precise actions, organizations can create an empowered data analytics ecosystem that delivers real value by driving data-driven decisions and maximizing the return on their data investment.
Opendatabay - Open Data Marketplace.pptxOpendatabay
Opendatabay.com unlocks the power of data for everyone. Open Data Marketplace fosters a collaborative hub for data enthusiasts to explore, share, and contribute to a vast collection of datasets.
First ever open hub for data enthusiasts to collaborate and innovate. A platform to explore, share, and contribute to a vast collection of datasets. Through robust quality control and innovative technologies like blockchain verification, opendatabay ensures the authenticity and reliability of datasets, empowering users to make data-driven decisions with confidence. Leverage cutting-edge AI technologies to enhance the data exploration, analysis, and discovery experience.
From intelligent search and recommendations to automated data productisation and quotation, Opendatabay AI-driven features streamline the data workflow. Finding the data you need shouldn't be a complex. Opendatabay simplifies the data acquisition process with an intuitive interface and robust search tools. Effortlessly explore, discover, and access the data you need, allowing you to focus on extracting valuable insights. Opendatabay breaks new ground with a dedicated, AI-generated, synthetic datasets.
Leverage these privacy-preserving datasets for training and testing AI models without compromising sensitive information. Opendatabay prioritizes transparency by providing detailed metadata, provenance information, and usage guidelines for each dataset, ensuring users have a comprehensive understanding of the data they're working with. By leveraging a powerful combination of distributed ledger technology and rigorous third-party audits Opendatabay ensures the authenticity and reliability of every dataset. Security is at the core of Opendatabay. Marketplace implements stringent security measures, including encryption, access controls, and regular vulnerability assessments, to safeguard your data and protect your privacy.
The Next Generation Fornax Survey - Pucon Symposium 2015
1. Pucón Symposium 2015
Puerto Varas, Agosto 2015
Chasing ghost galaxies in the Fornax cluster
Opportunities for the Deep Learning
community
Paul Eigenthaler, Thomas Puzia, Matt Taylor,
Yasna Ordenes, Simón Angel, Maren Hempel
Ariane Lançon, Steffen Mieske, Michael Hilker,
Patrick Côté, Laura Ferrarese & NGFS team.
Roberto Muñoz
Instituto de Astrofísica
Pontificia Universidad Católica de Chile
2. Galaxy clusters
Gravitationally bound structures that contain from hundreds to
thousands of galaxies. They are dominated by dark matter (85%) and
have large amounts of hot gas (10%).
Why so interesting?
• Large amount of galaxies at the same distance
• Laboratories to study the influence of
environment
• Rare objects formed from the most overdense
peaks in the initial density field
Coma is the best studied cluster
• Distance of 100 Mpc
• More than 1,000 members
• Mass of about
Roberto Muñoz
2 ⇥ 1015
M
3. Diffuse galaxies in Coma
van Dokkum et al. (2015) published a paper with 47 new dwarf
galaxies. A couple are diffuse galaxies, sizes similar to the Milky Way
but much fainter.
Roberto Muñoz
4. Virgo and Fornax clusters
Virgo is the largest nearby galaxy cluster. It contains about 1,762
members (Binggeli et al. 1985) and is located at 16.5 Mpc
Fornax is the second closest cluster. It contains about 340 members
(Ferguson et al. 1989) and is located at 20.0 Mpc.
Roberto Muñoz
Virgo cluster in X-ray from ROSAT
(Böhringer et al. 1994)
Murakami et al. [Vol. ,
–4.0 keV) image of the Fornax cluster. The NXB was subtracted and the difference in exposure
Fornax cluster in X-ray from XMM.
(Murakami et al 2011)
5. Virgo and Fornax clusters
Virgo is the largest nearby galaxy cluster. It contains about 1,762
members (Binggeli et al. 1985) and is located at 16.5 Mpc
Fornax is the second closest cluster. It contains about 340 members
(Ferguson et al. 1989) and is located at 20.0 Mpc.
Roberto Muñoz
Virgo cluster in X-ray from ROSAT
(Böhringer et al. 1994)
Murakami et al. [Vol. ,
–4.0 keV) image of the Fornax cluster. The NXB was subtracted and the difference in exposure
Fornax cluster in X-ray from XMM.
(Murakami et al 2011)
Ferrarese et al. 2012
7. The improved uiK diagram
Roberto Muñoz
Powalka et al., in preparation
8. NGFS: Fornax cluster
The Next Generation Fornax Survey (NGFS; PI: R. Muñoz) is an
ongoing multipassband optical and NIR survey of the Fornax galaxy
cluster. It will cover the central 30 deg2 out to the virial radius and will
allow to study the GC and galaxy populations.
Roberto Muñoz
8 deg
Globular
clusters
Galaxies
9. Observations and Processing
There is no universal observational strategy neither universal image
processing pipeline. It all depends on the scientific goals of the project
and the instrument been used.
Roberto Muñoz
CTIO/DECam
1
2
3
4
5
6
7
10
13
10. Observations and Processing
There is no universal observational strategy neither universal image
processing pipeline. It all depends on the scientific goals of the project
and the instrument been used.
Roberto Muñoz
CTIO/DECam
1
2
3
4
5
6
7
10
13
11. Observations and Processing
There is no universal observational strategy neither universal image
processing pipeline. It all depends on the scientific goals of the project
and the instrument been used.
Roberto Muñoz
CTIO/DECam
1
2
3
4
5
6
7
10
13
12. Observations and Processing
There is no universal observational strategy neither universal image
processing pipeline. It all depends on the scientific goals of the project
and the instrument been used.
Roberto Muñoz
CTIO/DECam
1
2
3
4
5
6
7
10
13
13. Observations and Processing
There is no universal observational strategy neither universal image
processing pipeline. It all depends on the scientific goals of the project
and the instrument been used.
Roberto Muñoz
CTIO/DECam
1
2
3
4
5
6
7
10
13
14. Observations and Processing
There is no universal observational strategy neither universal image
processing pipeline. It all depends on the scientific goals of the project
and the instrument been used.
Roberto Muñoz
CTIO/DECam
1
2
3
4
5
6
7
10
13
15. Observations and Processing
There is no universal observational strategy neither universal image
processing pipeline. It all depends on the scientific goals of the project
and the instrument been used.
Roberto Muñoz
CTIO/DECam
1
2
3
4
5
6
7
10
13
16. Observations and Processing
There is no universal observational strategy neither universal image
processing pipeline. It all depends on the scientific goals of the project
and the instrument been used.
Roberto Muñoz
CTIO/DECam
1
2
3
4
5
6
7
10
13
17. Observations and Processing
There is no universal observational strategy neither universal image
processing pipeline. It all depends on the scientific goals of the project
and the instrument been used.
Roberto Muñoz
CTIO/DECam
1
2
3
4
5
6
7
10
13
18. Observations and Processing
There is no universal observational strategy neither universal image
processing pipeline. It all depends on the scientific goals of the project
and the instrument been used.
Roberto Muñoz
CTIO/DECam
1
2
3
4
5
6
7
10
13
24. Color image asinh
The survey is still ongoing, but we already have deep u, g and i-band
for several tiles.
Roberto Muñoz
Muñoz et al., 2015
25. Color image asinh
The survey is still ongoing, but we already have deep u, g and i-band
for several tiles.
Roberto Muñoz
Muñoz et al., 2015
26. Color image asinh
The survey is still ongoing, but we already have deep u, g and i-band
for several tiles.
Roberto Muñoz
Muñoz et al., 2015
27. Dwarfs galaxies
We have discovered 200 new dwarf galaxies just in the central 3 deg2
of the Fornax cluster. Still 27 deg2 more to explore.
Roberto Muñoz
Muñoz, Eigenthaler, Puzia,Taylor et al., 2015
28. Equivalent to IGM
between Milky Way
and Andromeda
(~780 kpc)
Milky Way
Andromeda
•~70 deg2
•u’g’r’i’z’
•~3σ past GCLF
turnover
•~26-27 mag/arcsec^2
•spatial extent of
Centaurus A’s ~300
kpc virial radius
*optical
SCABS: A Survey of Centaurus
A’s Baryonic Structures
SCABS: A Survey of Centaurus
A’s Baryonic Structures
Taylor et al.,
in preparation
29. Summary
The NGFS survey is a multi wavelength optical and NIR survey
of the Fornax cluster.
We have developed new algorithms and methods for doing
image processing of DECam data. Special focus on modelling
the spatial variations of the sky.
We have done visual classification of the central tile and it’s
exhausting. We have discovered 200 new dwarf galaxies just in
the central DECam tile.
We need to invite the community to help us with the
identification. There are opportunities for the researchers
working in deep learning to develop methods to automatise the
identification of dwarf galaxies.
Roberto Muñoz