Algumas das imagens mais nítidas obtidas com o Very Large Telescope do ESO revelaram pela primeira vez o que parece ser uma estrela velha a dar origem a uma nebulosa planetária em forma da borboleta. Estas observações da estrela gigante vermelha L2 Puppis, obtidas no modo ZIMPOL do recentemente instalado instrumento SPHERE, mostram também de forma clara uma companheira estelar próxima. As fases finais das estrelas continuam a suscitar muitas questões aos astrônomos, incluindo a origem de uma nebulosa bipolar como esta, com a sua estranha e complexa forma de ampulheta.
A cerca de 200 anos-luz de distância, L2 Puppis é uma das gigantes vermelhas mais próximas da Terra que se sabe ter atingido já as fases finais da sua vida. As novas observações obtidas com o modo ZIMPOL do SPHERE foram feitas no visível usando métodos de ótica adaptativa extremos, com os quais se corrigem as imagens com um grau muito mais elevado do que com a ótica adaptativa normal, permitindo assim que objetos tênues próximos de fontes de luz intensa possam ser observados com imenso detalhe. Tratam-se dos primeiros resultados publicados com este modo e os mais detalhados obtidos para uma estrela deste tipo.
O ZIMPOL consegue produzir imagens três vezes mais nítidas do que as obtidas com o Telescópio Espacial Hubble da NASA/ESA, sendo que as novas observações mostram a poeira que rodeia a L2 Puppis de forma extremamente detalhada [1]. Estes dados confirmam resultados anteriores, obtidos com o instrumento NACO, da poeira a formar um disco, o qual a partir da Terra nos aparece praticamente de perfil, mas dão-nos uma visão muito mais detalhada. A informação de polarização obtida com o ZIMPOL permitiu à equipa construir um modelo tridimensional das estruturas de poeira [2].
Science with small telescopes - exoplanetsguest8aa6ebb
The search for extrasolar planets has become one of the most attractive problems in modern astrophysics. The biggest observatories in the world are involved in this task as well as little amateur instruments. There is also a huge variety of astronomical methods used for their investigation. Here I present the projects for searching for exoplanets by transit method and our observations of the planet WASP-2b. We observed a transit on 3/4 August 2008 with a 354 mm Schmidt-Cassegrain Celestron telescope and CCD SBIG STL 11000M camera. By precise photometry made using MaximDL software we obtained the light curve of the star system. Decrease of brightness by 0.02m is detected. Analyzing our data we estimate the radius of the planet and inclination of its orbit. Our results are in good correlation with the published information in literature.
Science with small telescopes - exoplanetsguest8aa6ebb
The search for extrasolar planets has become one of the most attractive problems in modern astrophysics. The biggest observatories in the world are involved in this task as well as little amateur instruments. There is also a huge variety of astronomical methods used for their investigation. Here I present the projects for searching for exoplanets by transit method and our observations of the planet WASP-2b. We observed a transit on 3/4 August 2008 with a 354 mm Schmidt-Cassegrain Celestron telescope and CCD SBIG STL 11000M camera. By precise photometry made using MaximDL software we obtained the light curve of the star system. Decrease of brightness by 0.02m is detected. Analyzing our data we estimate the radius of the planet and inclination of its orbit. Our results are in good correlation with the published information in literature.
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 ASTRODEEP Frontier Fields catalogues II. Photometric redshifts and rest f...Sérgio Sacani
Aims. We present the first public release of photometric redshifts, galaxy rest frame properties and associated magnification values
in the cluster and parallel pointings of the first two Frontier Fields, Abell-2744 and MACS-J0416. The released catalogues aim to
provide a reference for future investigations of extragalactic populations in these legacy fields: from lensed high-redshift galaxies to
cluster members themselves.
Methods.We exploit a multiwavelength catalogue, ranging from Hubble Space Telescope (HST) to ground-based K and Spitzer IRAC,
which is specifically designed to enable detection and measurement of accurate fluxes in crowded cluster regions. The multiband
information is used to derive photometric redshifts and physical properties of sources detected either in the H-band image alone, or
from a stack of four WFC3 bands. To minimize systematics, median photometric redshifts are assembled from six dierent approaches
to photo-z estimates. Their reliability is assessed through a comparison with available spectroscopic samples. State-of-the-art lensing
models are used to derive magnification values on an object-by-object basis by taking into account sources positions and redshifts.
Results. We show that photometric redshifts reach a remarkable 3–5% accuracy. After accounting for magnification, the H-band
number counts are found to be in agreement at bright magnitudes with number counts from the CANDELS fields, while extending
the presently available samples to galaxies that, intrinsically, are as faint as H 32 33, thanks to strong gravitational lensing. The
Frontier Fields allow the galaxy stellar mass distribution to be probed, depending on magnification, at 0.5–1.5 dex lower masses with
respect to extragalactic wide fields, including sources at Mstar 107–108 M at z > 5. Similarly, they allow the detection of objects
with intrinsic star formation rates (SFRs) >1 dex lower than in the CANDELS fields reaching 0.1–1 M=yr at z 6–10.
Imaging the dust_sublimation_front_of_a_circumbinary_diskSérgio Sacani
Aims. We present the first near-IR milli-arcsecond-scale image of a post-AGB binary that is surrounded by hot circumbinary dust.
Methods. A very rich interferometric data set in six spectral channels was acquired of IRAS 08544-4431 with the new RAPID camera
on the PIONIER beam combiner at the Very Large Telescope Interferometer (VLTI). A broadband image in the H-band was reconstructed
by combining the data of all spectral channels using the SPARCO method.
Results. We spatially separate all the building blocks of the IRAS 08544-4431 system in our milliarcsecond-resolution image. Our
dissection reveals a dust sublimation front that is strikingly similar to that expected in early-stage protoplanetary disks, as well as an
unexpected flux signal of 4% from the secondary star. The energy output from this companion indicates the presence of a compact
circum-companion accretion disk, which is likely the origin of the fast outflow detected in H.
Conclusions. Our image provides the most detailed view into the heart of a dusty circumstellar disk to date. Our results demonstrate
that binary evolution processes and circumstellar disk evolution can be studied in detail in space and over time.
Evidence for pop_iii_like_stellar_populations_in_the_most_luminous_lyman_alph...Sérgio Sacani
Com o auxílio do Very Large Telescope do ESO, astrônomos descobriram a galáxia mais brilhante observada até hoje no Universo primordial e encontraram evidências fortes de que este objeto contém estrelas da primeira geração. Estas estrelas massivas e brilhantes, puramente teóricas até agora, foram as criadoras dos primeiros elementos pesados na história — os elementos necessários à formação das estrelas que nos rodeiam atualmente, os planetas que as orbitam e a vida tal como a conhecemos. A galáxia recentemente descoberta chamada CR7 é três vezes mais brilhante do que a galáxia distante mais brilhante que era conhecida até agora.
Os astrônomos desenvolveram há algum tempo a teoria da existência de uma primeira geração de estrelas - conhecidas por estrelas de População III — que teriam nascido do material primordial do Big Bang [1]. Todos os elementos químicos mais pesados — como o oxigênio, nitrogênio, carbono e ferro, que são essenciais à vida — formaram-se no interior das estrelas, o que significa que as primeiras estrelas se devem ter formado dos únicos elementos que existiam antes delas: hidrogênio, hélio e traços mínimos de lítio.
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 ASTRODEEP Frontier Fields catalogues II. Photometric redshifts and rest f...Sérgio Sacani
Aims. We present the first public release of photometric redshifts, galaxy rest frame properties and associated magnification values
in the cluster and parallel pointings of the first two Frontier Fields, Abell-2744 and MACS-J0416. The released catalogues aim to
provide a reference for future investigations of extragalactic populations in these legacy fields: from lensed high-redshift galaxies to
cluster members themselves.
Methods.We exploit a multiwavelength catalogue, ranging from Hubble Space Telescope (HST) to ground-based K and Spitzer IRAC,
which is specifically designed to enable detection and measurement of accurate fluxes in crowded cluster regions. The multiband
information is used to derive photometric redshifts and physical properties of sources detected either in the H-band image alone, or
from a stack of four WFC3 bands. To minimize systematics, median photometric redshifts are assembled from six dierent approaches
to photo-z estimates. Their reliability is assessed through a comparison with available spectroscopic samples. State-of-the-art lensing
models are used to derive magnification values on an object-by-object basis by taking into account sources positions and redshifts.
Results. We show that photometric redshifts reach a remarkable 3–5% accuracy. After accounting for magnification, the H-band
number counts are found to be in agreement at bright magnitudes with number counts from the CANDELS fields, while extending
the presently available samples to galaxies that, intrinsically, are as faint as H 32 33, thanks to strong gravitational lensing. The
Frontier Fields allow the galaxy stellar mass distribution to be probed, depending on magnification, at 0.5–1.5 dex lower masses with
respect to extragalactic wide fields, including sources at Mstar 107–108 M at z > 5. Similarly, they allow the detection of objects
with intrinsic star formation rates (SFRs) >1 dex lower than in the CANDELS fields reaching 0.1–1 M=yr at z 6–10.
Imaging the dust_sublimation_front_of_a_circumbinary_diskSérgio Sacani
Aims. We present the first near-IR milli-arcsecond-scale image of a post-AGB binary that is surrounded by hot circumbinary dust.
Methods. A very rich interferometric data set in six spectral channels was acquired of IRAS 08544-4431 with the new RAPID camera
on the PIONIER beam combiner at the Very Large Telescope Interferometer (VLTI). A broadband image in the H-band was reconstructed
by combining the data of all spectral channels using the SPARCO method.
Results. We spatially separate all the building blocks of the IRAS 08544-4431 system in our milliarcsecond-resolution image. Our
dissection reveals a dust sublimation front that is strikingly similar to that expected in early-stage protoplanetary disks, as well as an
unexpected flux signal of 4% from the secondary star. The energy output from this companion indicates the presence of a compact
circum-companion accretion disk, which is likely the origin of the fast outflow detected in H.
Conclusions. Our image provides the most detailed view into the heart of a dusty circumstellar disk to date. Our results demonstrate
that binary evolution processes and circumstellar disk evolution can be studied in detail in space and over time.
Evidence for pop_iii_like_stellar_populations_in_the_most_luminous_lyman_alph...Sérgio Sacani
Com o auxílio do Very Large Telescope do ESO, astrônomos descobriram a galáxia mais brilhante observada até hoje no Universo primordial e encontraram evidências fortes de que este objeto contém estrelas da primeira geração. Estas estrelas massivas e brilhantes, puramente teóricas até agora, foram as criadoras dos primeiros elementos pesados na história — os elementos necessários à formação das estrelas que nos rodeiam atualmente, os planetas que as orbitam e a vida tal como a conhecemos. A galáxia recentemente descoberta chamada CR7 é três vezes mais brilhante do que a galáxia distante mais brilhante que era conhecida até agora.
Os astrônomos desenvolveram há algum tempo a teoria da existência de uma primeira geração de estrelas - conhecidas por estrelas de População III — que teriam nascido do material primordial do Big Bang [1]. Todos os elementos químicos mais pesados — como o oxigênio, nitrogênio, carbono e ferro, que são essenciais à vida — formaram-se no interior das estrelas, o que significa que as primeiras estrelas se devem ter formado dos únicos elementos que existiam antes delas: hidrogênio, hélio e traços mínimos de lítio.
Large heterogeneities in_comet_67_p_as_revealed_by_active_pits_from_sinkhole_...Sérgio Sacani
Em um estudo publicado online na edição da revista Nature, 18 cavidades quase circulares foram identificadas no hemisfério norte do cometa 67P/Churyumov-Gerasimenko. As cavidades tem de dezenas a centenas de metros de diâmetro e se estendem a mais de 210 metros abaixo da superfície do cometa. Essas cavidades são ativas e provavelmente criadas por um processo de sumidouro, possivelmente acompanhado por explosões.
A sonda Rosetta da ESA tem monitorado a atividade do cometa por mais de um ano, observando como seu halo de poeira e gás cresce à medida que o cometa se move para perto do Sol ao longo de sua órbita.
De uma distância de apenas centenas de quilômetros, a sonda observa um intrigante padrão de jatos de poeira sendo emitidos do núcleo enquanto eles são ejetados para o espaço.
Mas agora, graças a imagens de alta resolução da câmera de ângulo restrito da sonda, a Optical Spectroscopic and Infrared Remote Imaging System (OSIRIS), feitas de uma distância entre 10 a 30 km do centro do cometa, alguns desses jatos puderam ser rastreados de volta à superfície do cometa, chegando até a sua fonte, é a primeira vez que isso é feito e observado.
The mass of_the_mars_sized_exoplanet_kepler_138_b_from_transit_timingSérgio Sacani
Artigo da revista Nature, descreve o trabalho de astrônomos para medir o tamanho e a massa de um exoplaneta parecido com Marte, além de caracterizar por completo o sistema planetário da estrela Kepler-138.
A smack model_of_colliding_planetesimals_and_dust_in_the_beta_pictoris_debris...Sérgio Sacani
Uma nova simulação de supercomputador da NASA do planeta e do disco de detritos ao redor da estrela Beta Pictoris revela que o movimento do planeta dirige ondas espirais através do disco, um fenômeno que gera colisões entre os detritos em órbita. Padrões nas colisões e a poeira resultante parece ser responsável por muitas feições observadas que pesquisas anteriores tinham sido incapazes de serem explicadas completamente.
A revised upper_limit_to_energy_extraction_from_a_kerr_black_holeSérgio Sacani
Uma nova simulação computacional feita pela NASA mostra que as partículas da matéria escura colidindo na extrema gravidade de um buraco negro pode produzir uma luz de raios-gamma forte e potencialmente observável. Detectando essa emissão forneceria aos astrônomos com uma nova ferramenta para entender tanto os buracos negros como a natureza da matéria escura, uma elusiva substância responsável pela maior parte da massa do universo que nem reflete, absorve ou emite luz.
A very luminous_magnetar_powered_supernova_associated_with_an_ultra_long_gamm...Sérgio Sacani
Observações obtidas nos Observatórios de La Silla e Paranal no Chile demonstraram pela primeira vez que existe uma ligação entre uma explosão de raios gama de longa duração e uma explosão de supernova de brilho incomum. Os resultados mostram que a supernova não teve origem em decaimento radioativo, como se esperava, mas sim em campos magnéticos muito fortes decaindo em torno de um objeto exótico conhecido como magnetar. Os resultados serão publicados em 9 de julho de 2015 na revista Nature.
As explosões de raios gama constituem um dos eventos associados às maiores explosões que ocorreram desde o Big Bang. São detectadas por telescópios em órbita sensíveis a este tipo de radiação altamente energética, a qual não consegue penetrar a atmosfera terrestre, e são igualmente observadas a maiores comprimentos de onda por outros telescópios, situados tanto no espaço como no solo.
As explosões de raios gama duram tipicamente alguns segundos, mas em casos muito raros podem ocorrer durante horas. Uma destas explosões de longa duração foi captada pelo satélite Swift a 9 de dezembro de 2011 e chamada GRB 111209A. Foi simultaneamente uma das mais longas e mais brilhantes explosões de raios gama jáobservada.
The atacama cosmology_telescope_measuring_radio_galaxy_bias_through_cross_cor...Sérgio Sacani
A radiação cósmica de micro-ondas aponta para a matéria escura invisível, marcando o ponto onde jatos de material viajam a velocidades próximas da velocidade da luz, de acordo com uma equipe internacional de astrônomos. O principal autor do estudo, Rupert Allison da Universidade de Oxford apresentou os resultados no dia 6 de Julho de 2015 no National Astronomy Meeting em Venue Cymru, em Llandudno em Wales.
Atualmente, ninguém sabe ao certo do que a matéria escura é feita, mas ela é responsável por cerca de 26% do conteúdo de energia do universo, com galáxias massivas se formando em densas regiões de matéria escura. Embora invisível, a matéria escura se mostra através do efeito gravitacional – uma grande bolha de matéria escura puxa a matéria normal (como elétrons, prótons e nêutrons) através de sua própria gravidade, eventualmente se empacotando conjuntamente para criar as estrelas e galáxias inteiras.
Muitas das maiores dessas são galáxias ativas com buracos negros supermassivos em seus centros. Alguma parte do gás caindo diretamente na direção do buraco negro é ejetada como jatos de partículas e radiação. As observações feitas com rádio telescópios mostram que esses jatos as vezes se espalham por milhões de anos-luz desde a galáxia – mais distante até mesmo do que a extensão da própria galáxia.
Os cientistas esperam que os jatos possam viver em regiões onde existe um excesso de concentração da matéria escura, maior do que o da média. Mas como a matéria escura é invisível, testar essa ideia não é algo tão direto.
The distribution and_annihilation_of_dark_matter_around_black_holesSérgio Sacani
Uma nova simulação computacional feita pela NASA mostra que as partículas da matéria escura colidindo na extrema gravidade de um buraco negro pode produzir uma luz de raios-gamma forte e potencialmente observável. Detectando essa emissão forneceria aos astrônomos com uma nova ferramenta para entender tanto os buracos negros como a natureza da matéria escura, uma elusiva substância responsável pela maior parte da massa do universo que nem reflete, absorve ou emite luz.
A measurement of_the_black_hole_mass_in_ngc_1097_using_almaSérgio Sacani
Artigo descreve a maneira como os astrônomos usaram pela primeira vez o ALMA para medir a massa de um buraco negro supermassivo no interior de uma galáxias espiral barrada.
Variability in a_young_lt_transition_planetary_mass_objectSérgio Sacani
Padrões climáticos num misterioso mundo além do nosso Sistema Solar tem sido revelado pela primeira vez, sugere um estudo.
Camadas de nuvens, feitas de poeira quente e gotículas de ferro derretido, foram detectadas num objeto parecido com um planeta descoberto a 75 anos-luz de distância da Terra, dizem os pesquisadores.
As descobertas poderiam melhorar a habilidade dos cientistas de descobrir se condições em planetas distantes seriam capazes de sustentar a vida.
Uma equipe de pesquisadores liderada pela Universidade de Edimburgo, usou um telescópio no Chile para estudar o sistema climático de um mundo distante, conhecido como PSO J318.5-22, que estima-se tenha cerca de 20 milhões de anos de vida.
Os pesquisadores capturaram centenas de imagens infravermelhas do objeto enquanto ele rotacionava em torno do seu próprio eixo num período de 5 horas. Comparando o brilho do PSO J318.5-22, com corpos vizinhos, a equipe descobriu que ele era coberto por múltiplas camadas de nuvens finas e espessas. Essas nuvens causaram as mudanças no brilho do mundo distante enquanto ele executava o seu movimento de rotação, dizem os cientistas.
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
SPECTROSCOPIC CONFIRMATION OF THE EXISTENCE OF LARGE, DIFFUSE GALAXIES IN THE...Sérgio Sacani
We recently identified a population of low surface brightness objects in the field of the z = 0.023 Coma cluster,
using the Dragonfly Telephoto Array. Here we present Keck spectroscopy of one of the largest of these “ultradiffuse
galaxies” (UDGs), confirming that it is a member of the cluster. The galaxy has prominent absorption
features, including the Ca II H+K lines and the G-band, and no detected emission lines. Its radial velocity of
cz=6280±120 km s−1 is within the 1σ velocity dispersion of the Coma cluster. The galaxy has an effective
radius of 4.3 ± 0.3 kpc and a Sérsic index of 0.89 ± 0.06, as measured from Keck imaging. We find no indications
of tidal tails or other distortions, at least out to a radius of ∼2re. We show that UDGs are located in a previously
sparsely populated region of the size—magnitude plane of quiescent stellar systems, as they are ∼6 mag fainter
than normal early-type galaxies of the same size. It appears that the luminosity distribution of large quiescent
galaxies is not continuous, although this could largely be due to selection effects. Dynamical measurements are
needed to determine whether the dark matter halos of UDGs are similar to those of galaxies with the same
luminosity or to those of galaxies with the same size.
Peekaboo: the extremely metal poor dwarf galaxy HIPASS J1131–31Sérgio Sacani
The dwarf irregular galaxy HIPASS J1131–31 was discovered as a source of HI emission
at low redshift in such close proximity of a bright star that we call it Peekaboo. The galaxy
resolves into stars in images with Hubble Space Telescope, leading to a distance estimate
of 6.8 ± 0.7 Mpc. Spectral optical observations with the Southern African Large Telescope
reveal HIPASS J1131–31 to be one of the most extremely metal-poor galaxies known with
the gas-phase oxygen abundance 12+log(O/H) = 6.99±0.16 dex via the direct [OIII] 4363 line
method and 6.87±0.07 dex from the two strong line empirical methods. The red giant branch
of the system is tenuous compared with the prominence of the features of young populations in
the color-magnitude diagram, inviting speculation that star formation in the galaxy only began
in the last few Gyr
Artigo que descreve a descoberta do exoplaneta Kepler-432b, um exoplaneta mais massivo que Júpiter que orbita uma estrela gigante vermelha bem próximo e numa órbita extremamente alongada.
- Astrônomos descobriram que uma pequena estrela, do tamanho de Júpiter, possui uma tempestade muito parecida com a Grande Mancha Vermelha e que está ali, persistente por dois anos.
- Enquanto nos planetas, esse tipo de característica é normal, em estrelas essa é a melhor evidência encontrada até hoje.
- A estrela é chamada de W1906+40 e pertence a uma classe de objetos frios chamados de Anãs-L.
- Elas são consideradas estrelas pois fundem átomos e geram luz, como o Sol faz, enquanto que as anãs marrons são conhecidas como estrelas que falharam, pois elas não possuem o processo de fusão atômica em seu interior.
- Nesse novo estudo os astrônomos foram capazes de verificar as mudanças na atmosfera da estrela por dois anos. A técnica usada foi semelhante à de detecção de exoplanetas, analisando a curva de luz da estrela, que apresentava quedas, mas que não era por questão de planetas.
- Os astrônomos usaram o Spitzer e estudaram a luz infravermelha da estrela, que revelou uma gigantesca mancha escura que não era uma mancha magnética estelar, mas sim uma tempestade com um diâmetro equivalente ao de 3 Terras. O spitzer foi capaz de estudar camadas diferentes da atmosfera da estrela e esses dados junto com os dados do Kepler, revelaram com clareza a tempestade estelar.
- Futuras observações serão realizadas usando os dois equipamentos para tentar identificar esse tipo de tempestade em anãs marrons, por exemplo, e tentar descobrir se esse tipo de fenômeno é muito comum, ou é raro no universo.
A surge of light at the birth of a supernovaSérgio Sacani
It is difficult to establish the properties of massive stars that explode
as supernovae1,2
. The electromagnetic emission during the first
minutes to hours after the emergence of the shock from the stellar
surface conveys important information about the final evolution
and structure of the exploding star3–6. However, the unpredictable
nature of supernova events hinders the detection of this brief initial
phase7–9. Here we report the serendipitous discovery of a newly
born, normal type IIb supernova (SN 2016gkg)10, which reveals a
rapid brightening at optical wavelengths of about 40 magnitudes
per day. The very frequent sampling of the observations allowed
us to study in detail the outermost structure of the progenitor of
the supernova and the physics of the emergence of the shock. We
develop hydrodynamical models of the explosion that naturally
account for the complete evolution of the supernova over distinct
phases regulated by different physical processes. This result
suggests that it is appropriate to decouple the treatment of the
shock propagation from the unknown mechanism that triggers
the explosion.
Detection of solar_like_oscillations_in_relies_of_the_milk_way_asteroseismolo...Sérgio Sacani
Asteroseismic constraints on K giants make it possible to infer radii, masses and ages of tens
of thousands of field stars. Tests against independent estimates of these properties are however
scarce, especially in the metal-poor regime. Here, we report the detection of solar-like
oscillations in 8 stars belonging to the red-giant branch and red-horizontal branch of the globular
cluster M4. The detections were made in photometric observations from the K2 Mission
during its Campaign 2. Making use of independent constraints on the distance, we estimate
masses of the 8 stars by utilising different combinations of seismic and non-seismic inputs.
When introducing a correction to the Δν scaling relation as suggested by stellar models, for
RGB stars we find excellent agreement with the expected masses from isochrone fitting, and
with a distance modulus derived using independent methods. The offset with respect to independent
masses is lower, or comparable with, the uncertainties on the average RGB mass
(4 − 10%, depending on the combination of constraints used). Our results lend confidence to
asteroseismic masses in the metal poor regime. We note that a larger sample will be needed
to allow more stringent tests to be made of systematic uncertainties in all the observables
(both seismic and non-seismic), and to explore the properties of RHB stars, and of different
populations in the cluster.
A reflective, metal-rich atmosphere for GJ 1214b from its JWST phase curveSérgio Sacani
There are no planets intermediate in size between Earth and Neptune in our Solar System, yet these objects are found around a
substantial fraction of other stars [1]. Population statistics show that
close-in planets in this size range bifurcate into two classes based
on their radii [2, 3]. It is hypothesized that the group with larger
radii (referred to as “sub-Neptunes”) is distinguished by having
hydrogen-dominated atmospheres that are a few percent of the total
mass of the planets [4]. GJ 1214b is an archetype sub-Neptune that
has been observed extensively using transmission spectroscopy to
test this hypothesis [5–14]. However, the measured spectra are featureless, and thus inconclusive, due to the presence of high-altitude
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GJ 1214b Phase Curve 3
aerosols in the planet’s atmosphere. Here we report a spectroscopic thermal phase curve of GJ 1214b obtained with JWST in the
mid-infrared. The dayside and nightside spectra (average brightness
temperatures of 553 ± 9 and 437 ± 19 K, respectively) each show > 3σ
evidence of absorption features, with H2O as the most likely cause in
both. The measured global thermal emission implies that GJ 1214b’s
Bond albedo is 0.51 ± 0.06. Comparison between the spectroscopic
phase curve data and three-dimensional models of GJ 1214b reveal
a planet with a high metallicity atmosphere blanketed by a thick
and highly reflective layer of clouds or haze.
Confirmation of the_planetary_microlensing_signal_and_star_and_planet_mass_de...Sérgio Sacani
O Telescópio Espacial Hubble e o Observatório W. M. Keck, no Havaí, fizeram confirmações independentes de um exoplaneta orbitando sua estrela central de uma distância bem grande. O planeta foi descoberto através de uma técnica chamada de microlente gravitacional.
Essa descoberta traz uma nova peça para o processo de caçada de exoplanetas: para descobrir planetas longe de suas estrelas, como Júpiter e Saturno estão do Sol. Os resultados obtidos pelo Hubble e pelo Keck apareceram em dois artigos da edição de 30 de Julho de 2015 do The Astrophysical Journal.
A grande maioria dos exoplanetas catalogados são aqueles localizados bem perto de suas estrelas, isso acontece porque as técnicas atuais de se caçar exoplanetas favorecem a descoberta de planetas com curtos períodos orbitais. Mas esse não é o caso da técnica de microlente gravitacional, que pode encontrar planetas mais frios e mais distantes com órbitas de longo período que outros métodos não são capazes de detectar.
Probing the innermost_regions_of_agn_jets_and_their_magnetic_fields_with_radi...Sérgio Sacani
Desde 1974, observações feitas com o chamado Long Baseline Interferometry, ou VLBI, combinaram sinais de um objeto cósmico recebidos em diferentes rádio telescópios espalhados pelo globo para criar uma antena com o tamanho equivalente à maior separação entre elas. Isso fez com que fosse possível fazer imagens com uma nitidez sem precedentes, com uma resolução 1000 vezes melhor do que Hubble consegue na luz visível. Agora, uma equipe internacional de astrônomos quebrou todos os recordes combinando 15 rádio telescópios na Terra e a antena de rádio da missão RadioAstron, da agência espacial russa, na órbita da Terra. O trabalho, liderado pelo Instituto de Astrofísica de Andalucía, o IAA-CSIC, forneceu novas ideias sobre a natureza das galáxias ativas, onde um buraco negro extremamente massivo engole a matéria ao redor enquanto simultaneamente emite um par de jatos de partículas de alta energia e campos magnéticos a velocidades próximas da velocidade da luz.
Observações feitas no comprimento de onda das micro-ondas são essenciais para explorar esses jatos, já que os elétrons de alta energia se movendo em campos magnéticos são mais proficientes em produzir micro-ondas. Mas a maioria das galáxias ativas com jatos brilhantes estão a bilhões de anos-luz de distância da Terra, de modo que esses jatos são minúsculos no céu. Desse modo a alta resolução é essencial para observar esses jatos em ação e então revelar fenômenos como as ondas de choque e a turbulência que controla o quanto de luz é produzida num dado tempo. “Combinando pela primeira vez rádio telescópios na Terra com rádio telescópios no espaço, operando na máxima resolução, tem permitido que a nossa equipe crie uma antena que tem um tamanho equivalente a 8 vezes o diâmetro da Terra, correspondendo a 20 micro arcos de segundo”, disse José L; Gómez, o líder da equipe no Instituto de Astrofísica de Andalucía, IAA-CSIC.
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.
Earliest Galaxies in the JADES Origins Field: Luminosity Function and Cosmic ...Sérgio Sacani
We characterize the earliest galaxy population in the JADES Origins Field (JOF), the deepest
imaging field observed with JWST. We make use of the ancillary Hubble optical images (5 filters
spanning 0.4−0.9µm) and novel JWST images with 14 filters spanning 0.8−5µm, including 7 mediumband filters, and reaching total exposure times of up to 46 hours per filter. We combine all our data
at > 2.3µm to construct an ultradeep image, reaching as deep as ≈ 31.4 AB mag in the stack and
30.3-31.0 AB mag (5σ, r = 0.1” circular aperture) in individual filters. We measure photometric
redshifts and use robust selection criteria to identify a sample of eight galaxy candidates at redshifts
z = 11.5 − 15. These objects show compact half-light radii of R1/2 ∼ 50 − 200pc, stellar masses of
M⋆ ∼ 107−108M⊙, and star-formation rates of SFR ∼ 0.1−1 M⊙ yr−1
. Our search finds no candidates
at 15 < z < 20, placing upper limits at these redshifts. We develop a forward modeling approach to
infer the properties of the evolving luminosity function without binning in redshift or luminosity that
marginalizes over the photometric redshift uncertainty of our candidate galaxies and incorporates the
impact of non-detections. We find a z = 12 luminosity function in good agreement with prior results,
and that the luminosity function normalization and UV luminosity density decline by a factor of ∼ 2.5
from z = 12 to z = 14. We discuss the possible implications of our results in the context of theoretical
models for evolution of the dark matter halo mass function.
THE IMPORTANCE OF MARTIAN ATMOSPHERE SAMPLE RETURN.Sérgio Sacani
The return of a sample of near-surface atmosphere from Mars would facilitate answers to several first-order science questions surrounding the formation and evolution of the planet. One of the important aspects of terrestrial planet formation in general is the role that primary atmospheres played in influencing the chemistry and structure of the planets and their antecedents. Studies of the martian atmosphere can be used to investigate the role of a primary atmosphere in its history. Atmosphere samples would also inform our understanding of the near-surface chemistry of the planet, and ultimately the prospects for life. High-precision isotopic analyses of constituent gases are needed to address these questions, requiring that the analyses are made on returned samples rather than in situ.
Multi-source connectivity as the driver of solar wind variability in the heli...Sérgio Sacani
The ambient solar wind that flls the heliosphere originates from multiple
sources in the solar corona and is highly structured. It is often described
as high-speed, relatively homogeneous, plasma streams from coronal
holes and slow-speed, highly variable, streams whose source regions are
under debate. A key goal of ESA/NASA’s Solar Orbiter mission is to identify
solar wind sources and understand what drives the complexity seen in the
heliosphere. By combining magnetic feld modelling and spectroscopic
techniques with high-resolution observations and measurements, we show
that the solar wind variability detected in situ by Solar Orbiter in March
2022 is driven by spatio-temporal changes in the magnetic connectivity to
multiple sources in the solar atmosphere. The magnetic feld footpoints
connected to the spacecraft moved from the boundaries of a coronal hole
to one active region (12961) and then across to another region (12957). This
is refected in the in situ measurements, which show the transition from fast
to highly Alfvénic then to slow solar wind that is disrupted by the arrival of
a coronal mass ejection. Our results describe solar wind variability at 0.5 au
but are applicable to near-Earth observatories.
Gliese 12 b: A Temperate Earth-sized Planet at 12 pc Ideal for Atmospheric Tr...Sérgio Sacani
Recent discoveries of Earth-sized planets transiting nearby M dwarfs have made it possible to characterize the
atmospheres of terrestrial planets via follow-up spectroscopic observations. However, the number of such planets
receiving low insolation is still small, limiting our ability to understand the diversity of the atmospheric
composition and climates of temperate terrestrial planets. We report the discovery of an Earth-sized planet
transiting the nearby (12 pc) inactive M3.0 dwarf Gliese 12 (TOI-6251) with an orbital period (Porb) of 12.76 days.
The planet, Gliese 12 b, was initially identified as a candidate with an ambiguous Porb from TESS data. We
confirmed the transit signal and Porb using ground-based photometry with MuSCAT2 and MuSCAT3, and
validated the planetary nature of the signal using high-resolution images from Gemini/NIRI and Keck/NIRC2 as
well as radial velocity (RV) measurements from the InfraRed Doppler instrument on the Subaru 8.2 m telescope
and from CARMENES on the CAHA 3.5 m telescope. X-ray observations with XMM-Newton showed the host
star is inactive, with an X-ray-to-bolometric luminosity ratio of log 5.7 L L X bol » - . Joint analysis of the light
curves and RV measurements revealed that Gliese 12 b has a radius of 0.96 ± 0.05 R⊕,a3σ mass upper limit of
3.9 M⊕, and an equilibrium temperature of 315 ± 6 K assuming zero albedo. The transmission spectroscopy metric
(TSM) value of Gliese 12 b is close to the TSM values of the TRAPPIST-1 planets, adding Gliese 12 b to the small
list of potentially terrestrial, temperate planets amenable to atmospheric characterization with JWST.
Gliese 12 b, a temperate Earth-sized planet at 12 parsecs discovered with TES...Sérgio Sacani
We report on the discovery of Gliese 12 b, the nearest transiting temperate, Earth-sized planet found to date. Gliese 12 is a
bright (V = 12.6 mag, K = 7.8 mag) metal-poor M4V star only 12.162 ± 0.005 pc away from the Solar system with one of the
lowest stellar activity levels known for M-dwarfs. A planet candidate was detected by TESS based on only 3 transits in sectors
42, 43, and 57, with an ambiguity in the orbital period due to observational gaps. We performed follow-up transit observations
with CHEOPS and ground-based photometry with MINERVA-Australis, SPECULOOS, and Purple Mountain Observatory,
as well as further TESS observations in sector 70. We statistically validate Gliese 12 b as a planet with an orbital period of
12.76144 ± 0.00006 d and a radius of 1.0 ± 0.1 R⊕, resulting in an equilibrium temperature of ∼315 K. Gliese 12 b has excellent
future prospects for precise mass measurement, which may inform how planetary internal structure is affected by the stellar
compositional environment. Gliese 12 b also represents one of the best targets to study whether Earth-like planets orbiting cool
stars can retain their atmospheres, a crucial step to advance our understanding of habitability on Earth and across the galaxy.
The importance of continents, oceans and plate tectonics for the evolution of...Sérgio Sacani
Within the uncertainties of involved astronomical and biological parameters, the Drake Equation
typically predicts that there should be many exoplanets in our galaxy hosting active, communicative
civilizations (ACCs). These optimistic calculations are however not supported by evidence, which is
often referred to as the Fermi Paradox. Here, we elaborate on this long-standing enigma by showing
the importance of planetary tectonic style for biological evolution. We summarize growing evidence
that a prolonged transition from Mesoproterozoic active single lid tectonics (1.6 to 1.0 Ga) to modern
plate tectonics occurred in the Neoproterozoic Era (1.0 to 0.541 Ga), which dramatically accelerated
emergence and evolution of complex species. We further suggest that both continents and oceans
are required for ACCs because early evolution of simple life must happen in water but late evolution
of advanced life capable of creating technology must happen on land. We resolve the Fermi Paradox
(1) by adding two additional terms to the Drake Equation: foc
(the fraction of habitable exoplanets
with significant continents and oceans) and fpt
(the fraction of habitable exoplanets with significant
continents and oceans that have had plate tectonics operating for at least 0.5 Ga); and (2) by
demonstrating that the product of foc
and fpt
is very small (< 0.00003–0.002). We propose that the lack
of evidence for ACCs reflects the scarcity of long-lived plate tectonics and/or continents and oceans on
exoplanets with primitive life.
A Giant Impact Origin for the First Subduction on EarthSérgio Sacani
Hadean zircons provide a potential record of Earth's earliest subduction 4.3 billion years ago. Itremains enigmatic how subduction could be initiated so soon after the presumably Moon‐forming giant impact(MGI). Earlier studies found an increase in Earth's core‐mantle boundary (CMB) temperature due to theaccumulation of the impactor's core, and our recent work shows Earth's lower mantle remains largely solid, withsome of the impactor's mantle potentially surviving as the large low‐shear velocity provinces (LLSVPs). Here,we show that a hot post‐impact CMB drives the initiation of strong mantle plumes that can induce subductioninitiation ∼200 Myr after the MGI. 2D and 3D thermomechanical computations show that a high CMBtemperature is the primary factor triggering early subduction, with enrichment of heat‐producing elements inLLSVPs as another potential factor. The models link the earliest subduction to the MGI with implications forunderstanding the diverse tectonic regimes of rocky planets.
Climate extremes likely to drive land mammal extinction during next supercont...Sérgio Sacani
Mammals have dominated Earth for approximately 55 Myr thanks to their
adaptations and resilience to warming and cooling during the Cenozoic. All
life will eventually perish in a runaway greenhouse once absorbed solar
radiation exceeds the emission of thermal radiation in several billions of
years. However, conditions rendering the Earth naturally inhospitable to
mammals may develop sooner because of long-term processes linked to
plate tectonics (short-term perturbations are not considered here). In
~250 Myr, all continents will converge to form Earth’s next supercontinent,
Pangea Ultima. A natural consequence of the creation and decay of Pangea
Ultima will be extremes in pCO2 due to changes in volcanic rifting and
outgassing. Here we show that increased pCO2, solar energy (F⨀;
approximately +2.5% W m−2 greater than today) and continentality (larger
range in temperatures away from the ocean) lead to increasing warming
hostile to mammalian life. We assess their impact on mammalian
physiological limits (dry bulb, wet bulb and Humidex heat stress indicators)
as well as a planetary habitability index. Given mammals’ continued survival,
predicted background pCO2 levels of 410–816 ppm combined with increased
F⨀ will probably lead to a climate tipping point and their mass extinction.
The results also highlight how global landmass configuration, pCO2 and F⨀
play a critical role in planetary habitability.
Constraints on Neutrino Natal Kicks from Black-Hole Binary VFTS 243Sérgio Sacani
The recently reported observation of VFTS 243 is the first example of a massive black-hole binary
system with negligible binary interaction following black-hole formation. The black-hole mass (≈10M⊙)
and near-circular orbit (e ≈ 0.02) of VFTS 243 suggest that the progenitor star experienced complete
collapse, with energy-momentum being lost predominantly through neutrinos. VFTS 243 enables us to
constrain the natal kick and neutrino-emission asymmetry during black-hole formation. At 68% confidence
level, the natal kick velocity (mass decrement) is ≲10 km=s (≲1.0M⊙), with a full probability distribution
that peaks when ≈0.3M⊙ were ejected, presumably in neutrinos, and the black hole experienced a natal
kick of 4 km=s. The neutrino-emission asymmetry is ≲4%, with best fit values of ∼0–0.2%. Such a small
neutrino natal kick accompanying black-hole formation is in agreement with theoretical predictions.
Detectability of Solar Panels as a TechnosignatureSérgio Sacani
In this work, we assess the potential detectability of solar panels made of silicon on an Earth-like
exoplanet as a potential technosignature. Silicon-based photovoltaic cells have high reflectance in the
UV-VIS and in the near-IR, within the wavelength range of a space-based flagship mission concept
like the Habitable Worlds Observatory (HWO). Assuming that only solar energy is used to provide
the 2022 human energy needs with a land cover of ∼ 2.4%, and projecting the future energy demand
assuming various growth-rate scenarios, we assess the detectability with an 8 m HWO-like telescope.
Assuming the most favorable viewing orientation, and focusing on the strong absorption edge in the
ultraviolet-to-visible (0.34 − 0.52 µm), we find that several 100s of hours of observation time is needed
to reach a SNR of 5 for an Earth-like planet around a Sun-like star at 10pc, even with a solar panel
coverage of ∼ 23% land coverage of a future Earth. We discuss the necessity of concepts like Kardeshev
Type I/II civilizations and Dyson spheres, which would aim to harness vast amounts of energy. Even
with much larger populations than today, the total energy use of human civilization would be orders of
magnitude below the threshold for causing direct thermal heating or reaching the scale of a Kardashev
Type I civilization. Any extraterrrestrial civilization that likewise achieves sustainable population
levels may also find a limit on its need to expand, which suggests that a galaxy-spanning civilization
as imagined in the Fermi paradox may not exist.
Jet reorientation in central galaxies of clusters and groups: insights from V...Sérgio Sacani
Recent observations of galaxy clusters and groups with misalignments between their central AGN jets
and X-ray cavities, or with multiple misaligned cavities, have raised concerns about the jet – bubble
connection in cooling cores, and the processes responsible for jet realignment. To investigate the
frequency and causes of such misalignments, we construct a sample of 16 cool core galaxy clusters and
groups. Using VLBA radio data we measure the parsec-scale position angle of the jets, and compare
it with the position angle of the X-ray cavities detected in Chandra data. Using the overall sample
and selected subsets, we consistently find that there is a 30% – 38% chance to find a misalignment
larger than ∆Ψ = 45◦ when observing a cluster/group with a detected jet and at least one cavity. We
determine that projection may account for an apparently large ∆Ψ only in a fraction of objects (∼35%),
and given that gas dynamical disturbances (as sloshing) are found in both aligned and misaligned
systems, we exclude environmental perturbation as the main driver of cavity – jet misalignment.
Moreover, we find that large misalignments (up to ∼ 90◦
) are favored over smaller ones (45◦ ≤ ∆Ψ ≤
70◦
), and that the change in jet direction can occur on timescales between one and a few tens of Myr.
We conclude that misalignments are more likely related to actual reorientation of the jet axis, and we
discuss several engine-based mechanisms that may cause these dramatic changes.
The solar dynamo begins near the surfaceSérgio Sacani
The magnetic dynamo cycle of the Sun features a distinct pattern: a propagating
region of sunspot emergence appears around 30° latitude and vanishes near the
equator every 11 years (ref. 1). Moreover, longitudinal flows called torsional oscillations
closely shadow sunspot migration, undoubtedly sharing a common cause2. Contrary
to theories suggesting deep origins of these phenomena, helioseismology pinpoints
low-latitude torsional oscillations to the outer 5–10% of the Sun, the near-surface
shear layer3,4. Within this zone, inwardly increasing differential rotation coupled with
a poloidal magnetic field strongly implicates the magneto-rotational instability5,6,
prominent in accretion-disk theory and observed in laboratory experiments7.
Together, these two facts prompt the general question: whether the solar dynamo is
possibly a near-surface instability. Here we report strong affirmative evidence in stark
contrast to traditional models8 focusing on the deeper tachocline. Simple analytic
estimates show that the near-surface magneto-rotational instability better explains
the spatiotemporal scales of the torsional oscillations and inferred subsurface
magnetic field amplitudes9. State-of-the-art numerical simulations corroborate these
estimates and reproduce hemispherical magnetic current helicity laws10. The dynamo
resulting from a well-understood near-surface phenomenon improves prospects
for accurate predictions of full magnetic cycles and space weather, affecting the
electromagnetic infrastructure of Earth.
Extensive Pollution of Uranus and Neptune’s Atmospheres by Upsweep of Icy Mat...Sérgio Sacani
In the Nice model of solar system formation, Uranus and Neptune undergo an orbital upheaval,
sweeping through a planetesimal disk. The region of the disk from which material is accreted by
the ice giants during this phase of their evolution has not previously been identified. We perform
direct N-body orbital simulations of the four giant planets to determine the amount and origin of solid
accretion during this orbital upheaval. We find that the ice giants undergo an extreme bombardment
event, with collision rates as much as ∼3 per hour assuming km-sized planetesimals, increasing the
total planet mass by up to ∼0.35%. In all cases, the initially outermost ice giant experiences the
largest total enhancement. We determine that for some plausible planetesimal properties, the resulting
atmospheric enrichment could potentially produce sufficient latent heat to alter the planetary cooling
timescale according to existing models. Our findings suggest that substantial accretion during this
phase of planetary evolution may have been sufficient to impact the atmospheric composition and
thermal evolution of the ice giants, motivating future work on the fate of deposited solid material.
Exomoons & Exorings with the Habitable Worlds Observatory I: On the Detection...Sérgio Sacani
The highest priority recommendation of the Astro2020 Decadal Survey for space-based astronomy
was the construction of an observatory capable of characterizing habitable worlds. In this paper series
we explore the detectability of and interference from exomoons and exorings serendipitously observed
with the proposed Habitable Worlds Observatory (HWO) as it seeks to characterize exoplanets, starting
in this manuscript with Earth-Moon analog mutual events. Unlike transits, which only occur in systems
viewed near edge-on, shadow (i.e., solar eclipse) and lunar eclipse mutual events occur in almost every
star-planet-moon system. The cadence of these events can vary widely from ∼yearly to multiple events
per day, as was the case in our younger Earth-Moon system. Leveraging previous space-based (EPOXI)
lightcurves of a Moon transit and performance predictions from the LUVOIR-B concept, we derive
the detectability of Moon analogs with HWO. We determine that Earth-Moon analogs are detectable
with observation of ∼2-20 mutual events for systems within 10 pc, and larger moons should remain
detectable out to 20 pc. We explore the extent to which exomoon mutual events can mimic planet
features and weather. We find that HWO wavelength coverage in the near-IR, specifically in the 1.4 µm
water band where large moons can outshine their host planet, will aid in differentiating exomoon signals
from exoplanet variability. Finally, we predict that exomoons formed through collision processes akin
to our Moon are more likely to be detected in younger systems, where shorter orbital periods and
favorable geometry enhance the probability and frequency of mutual events.
Emergent ribozyme behaviors in oxychlorine brines indicate a unique niche for...Sérgio Sacani
Mars is a particularly attractive candidate among known astronomical objects
to potentially host life. Results from space exploration missions have provided
insights into Martian geochemistry that indicate oxychlorine species, particularly perchlorate, are ubiquitous features of the Martian geochemical landscape. Perchlorate presents potential obstacles for known forms of life due to
its toxicity. However, it can also provide potential benefits, such as producing
brines by deliquescence, like those thought to exist on present-day Mars. Here
we show perchlorate brines support folding and catalysis of functional RNAs,
while inactivating representative protein enzymes. Additionally, we show
perchlorate and other oxychlorine species enable ribozyme functions,
including homeostasis-like regulatory behavior and ribozyme-catalyzed
chlorination of organic molecules. We suggest nucleic acids are uniquely wellsuited to hypersaline Martian environments. Furthermore, Martian near- or
subsurface oxychlorine brines, and brines found in potential lifeforms, could
provide a unique niche for biomolecular evolution.
Continuum emission from within the plunging region of black hole discsSérgio Sacani
The thermal continuum emission observed from accreting black holes across X-ray bands has the potential to be leveraged as a
powerful probe of the mass and spin of the central black hole. The vast majority of existing ‘continuum fitting’ models neglect
emission sourced at and within the innermost stable circular orbit (ISCO) of the black hole. Numerical simulations, however,
find non-zero emission sourced from these regions. In this work, we extend existing techniques by including the emission
sourced from within the plunging region, utilizing new analytical models that reproduce the properties of numerical accretion
simulations. We show that in general the neglected intra-ISCO emission produces a hot-and-small quasi-blackbody component,
but can also produce a weak power-law tail for more extreme parameter regions. A similar hot-and-small blackbody component
has been added in by hand in an ad hoc manner to previous analyses of X-ray binary spectra. We show that the X-ray spectrum
of MAXI J1820+070 in a soft-state outburst is extremely well described by a full Kerr black hole disc, while conventional
models that neglect intra-ISCO emission are unable to reproduce the data. We believe this represents the first robust detection of
intra-ISCO emission in the literature, and allows additional constraints to be placed on the MAXI J1820 + 070 black hole spin
which must be low a• < 0.5 to allow a detectable intra-ISCO region. Emission from within the ISCO is the dominant emission
component in the MAXI J1820 + 070 spectrum between 6 and 10 keV, highlighting the necessity of including this region. Our
continuum fitting model is made publicly available.
WASP-69b’s Escaping Envelope Is Confined to a Tail Extending at Least 7 RpSérgio Sacani
Studying the escaping atmospheres of highly irradiated exoplanets is critical for understanding the physical
mechanisms that shape the demographics of close-in planets. A number of planetary outflows have been observed
as excess H/He absorption during/after transit. Such an outflow has been observed for WASP-69b by multiple
groups that disagree on the geometry and velocity structure of the outflow. Here, we report the detection of this
planet’s outflow using Keck/NIRSPEC for the first time. We observed the outflow 1.28 hr after egress until the
target set, demonstrating the outflow extends at least 5.8 × 105 km or 7.5 Rp This detection is significantly longer
than previous observations, which report an outflow extending ∼2.2 planet radii just 1 yr prior. The outflow is
blueshifted by −23 km s−1 in the planetary rest frame. We estimate a current mass-loss rate of 1 M⊕ Gyr−1
. Our
observations are most consistent with an outflow that is strongly sculpted by ram pressure from the stellar wind.
However, potential variability in the outflow could be due to time-varying interactions with the stellar wind or
differences in instrumental precision.
X-rays from a Central “Exhaust Vent” of the Galactic Center ChimneySérgio Sacani
Using deep archival observations from the Chandra X-ray Observatory, we present an analysis of
linear X-ray-emitting features located within the southern portion of the Galactic center chimney,
and oriented orthogonal to the Galactic plane, centered at coordinates l = 0.08◦
, b = −1.42◦
. The
surface brightness and hardness ratio patterns are suggestive of a cylindrical morphology which may
have been produced by a plasma outflow channel extending from the Galactic center. Our fits of the
feature’s spectra favor a complex two-component model consisting of thermal and recombining plasma
components, possibly a sign of shock compression or heating of the interstellar medium by outflowing
material. Assuming a recombining plasma scenario, we further estimate the cooling timescale of this
plasma to be on the order of a few hundred to thousands of years, leading us to speculate that a
sequence of accretion events onto the Galactic Black Hole may be a plausible quasi-continuous energy
source to sustain the observed morphology
hematic appreciation test is a psychological assessment tool used to measure an individual's appreciation and understanding of specific themes or topics. This test helps to evaluate an individual's ability to connect different ideas and concepts within a given theme, as well as their overall comprehension and interpretation skills. The results of the test can provide valuable insights into an individual's cognitive abilities, creativity, and critical thinking skills
ISI 2024: Application Form (Extended), Exam Date (Out), EligibilitySciAstra
The Indian Statistical Institute (ISI) has extended its application deadline for 2024 admissions to April 2. Known for its excellence in statistics and related fields, ISI offers a range of programs from Bachelor's to Junior Research Fellowships. The admission test is scheduled for May 12, 2024. Eligibility varies by program, generally requiring a background in Mathematics and English for undergraduate courses and specific degrees for postgraduate and research positions. Application fees are ₹1500 for male general category applicants and ₹1000 for females. Applications are open to Indian and OCI candidates.
Richard's aventures in two entangled wonderlandsRichard Gill
Since the loophole-free Bell experiments of 2020 and the Nobel prizes in physics of 2022, critics of Bell's work have retreated to the fortress of super-determinism. Now, super-determinism is a derogatory word - it just means "determinism". Palmer, Hance and Hossenfelder argue that quantum mechanics and determinism are not incompatible, using a sophisticated mathematical construction based on a subtle thinning of allowed states and measurements in quantum mechanics, such that what is left appears to make Bell's argument fail, without altering the empirical predictions of quantum mechanics. I think however that it is a smoke screen, and the slogan "lost in math" comes to my mind. I will discuss some other recent disproofs of Bell's theorem using the language of causality based on causal graphs. Causal thinking is also central to law and justice. I will mention surprising connections to my work on serial killer nurse cases, in particular the Dutch case of Lucia de Berk and the current UK case of Lucy Letby.
Comparing Evolved Extractive Text Summary Scores of Bidirectional Encoder Rep...University of Maribor
Slides from:
11th International Conference on Electrical, Electronics and Computer Engineering (IcETRAN), Niš, 3-6 June 2024
Track: Artificial Intelligence
https://www.etran.rs/2024/en/home-english/
Phenomics assisted breeding in crop improvementIshaGoswami9
As the population is increasing and will reach about 9 billion upto 2050. Also due to climate change, it is difficult to meet the food requirement of such a large population. Facing the challenges presented by resource shortages, climate
change, and increasing global population, crop yield and quality need to be improved in a sustainable way over the coming decades. Genetic improvement by breeding is the best way to increase crop productivity. With the rapid progression of functional
genomics, an increasing number of crop genomes have been sequenced and dozens of genes influencing key agronomic traits have been identified. However, current genome sequence information has not been adequately exploited for understanding
the complex characteristics of multiple gene, owing to a lack of crop phenotypic data. Efficient, automatic, and accurate technologies and platforms that can capture phenotypic data that can
be linked to genomics information for crop improvement at all growth stages have become as important as genotyping. Thus,
high-throughput phenotyping has become the major bottleneck restricting crop breeding. Plant phenomics has been defined as the high-throughput, accurate acquisition and analysis of multi-dimensional phenotypes
during crop growing stages at the organism level, including the cell, tissue, organ, individual plant, plot, and field levels. With the rapid development of novel sensors, imaging technology,
and analysis methods, numerous infrastructure platforms have been developed for phenotyping.
Seminar of U.V. Spectroscopy by SAMIR PANDASAMIR PANDA
Spectroscopy is a branch of science dealing the study of interaction of electromagnetic radiation with matter.
Ultraviolet-visible spectroscopy refers to absorption spectroscopy or reflect spectroscopy in the UV-VIS spectral region.
Ultraviolet-visible spectroscopy is an analytical method that can measure the amount of light received by the analyte.
The use of Nauplii and metanauplii artemia in aquaculture (brine shrimp).pptxMAGOTI ERNEST
Although Artemia has been known to man for centuries, its use as a food for the culture of larval organisms apparently began only in the 1930s, when several investigators found that it made an excellent food for newly hatched fish larvae (Litvinenko et al., 2023). As aquaculture developed in the 1960s and ‘70s, the use of Artemia also became more widespread, due both to its convenience and to its nutritional value for larval organisms (Arenas-Pardo et al., 2024). The fact that Artemia dormant cysts can be stored for long periods in cans, and then used as an off-the-shelf food requiring only 24 h of incubation makes them the most convenient, least labor-intensive, live food available for aquaculture (Sorgeloos & Roubach, 2021). The nutritional value of Artemia, especially for marine organisms, is not constant, but varies both geographically and temporally. During the last decade, however, both the causes of Artemia nutritional variability and methods to improve poorquality Artemia have been identified (Loufi et al., 2024).
Brine shrimp (Artemia spp.) are used in marine aquaculture worldwide. Annually, more than 2,000 metric tons of dry cysts are used for cultivation of fish, crustacean, and shellfish larva. Brine shrimp are important to aquaculture because newly hatched brine shrimp nauplii (larvae) provide a food source for many fish fry (Mozanzadeh et al., 2021). Culture and harvesting of brine shrimp eggs represents another aspect of the aquaculture industry. Nauplii and metanauplii of Artemia, commonly known as brine shrimp, play a crucial role in aquaculture due to their nutritional value and suitability as live feed for many aquatic species, particularly in larval stages (Sorgeloos & Roubach, 2021).
Salas, V. (2024) "John of St. Thomas (Poinsot) on the Science of Sacred Theol...Studia Poinsotiana
I Introduction
II Subalternation and Theology
III Theology and Dogmatic Declarations
IV The Mixed Principles of Theology
V Virtual Revelation: The Unity of Theology
VI Theology as a Natural Science
VII Theology’s Certitude
VIII Conclusion
Notes
Bibliography
All the contents are fully attributable to the author, Doctor Victor Salas. Should you wish to get this text republished, get in touch with the author or the editorial committee of the Studia Poinsotiana. Insofar as possible, we will be happy to broker your contact.
ANAMOLOUS SECONDARY GROWTH IN DICOT ROOTS.pptxRASHMI M G
Abnormal or anomalous secondary growth in plants. It defines secondary growth as an increase in plant girth due to vascular cambium or cork cambium. Anomalous secondary growth does not follow the normal pattern of a single vascular cambium producing xylem internally and phloem externally.
Toxic effects of heavy metals : Lead and Arsenicsanjana502982
Heavy metals are naturally occuring metallic chemical elements that have relatively high density, and are toxic at even low concentrations. All toxic metals are termed as heavy metals irrespective of their atomic mass and density, eg. arsenic, lead, mercury, cadmium, thallium, chromium, etc.
The dust disk_and_companion_of_the_nearby_agb_star_l2_puppis
1. Astronomy & Astrophysics manuscript no. L2Pup_SPHERE_v2r1 c ESO 2015
May 4, 2015
The dust disk and companion of the nearby AGB star L2 Puppis
SPHERE/ZIMPOL polarimetric imaging at visible wavelengths
P. Kervella1, 2, M. Montargès2, 3, E. Lagadec4, S. T. Ridgway5, X. Haubois6, J. H. Girard6, K. Ohnaka7, G. Perrin2, and
A. Gallenne8
1
Unidad Mixta Internacional Franco-Chilena de Astronomía (UMI 3386), CNRS/INSU, France & Departamento de Astronomía,
Universidad de Chile, Camino El Observatorio 1515, Las Condes, Santiago, Chile, e-mail: pkervell@das.uchile.cl.
2
LESIA (UMR 8109), Observatoire de Paris, CNRS, UPMC, Université Paris-Diderot, PSL Research University, 5 place Jules
Janssen, 92195 Meudon, France, e-mail: pierre.kervella@obspm.fr.
3
Institut de Radio-Astronomie Millimétrique, 300 rue de la Piscine, 38406 St Martin d’Hères, France.
4
Laboratoire Lagrange (UMR 7293), Université de Nice-Sophia Antipolis, CNRS, Observatoire de la Côte d’Azur, Bd de
l’Observatoire, B.P. 4229, F-06304 Nice cedex 4, France.
5
National Optical Astronomy Observatories, 950 North Cherry Avenue, Tucson, AZ 85719, USA.
6
European Southern Observatory, Alonso de Córdova 3107, Casilla 19001, Santiago 19, Chile.
7
Instituto de Astronomía, Universidad Católica del Norte, Avenida Angamos 0610, Antofagasta, Chile.
8
Universidad de Concepción, Departamento de Astronomía, Casilla 160-C, Concepción, Chile.
Received ; Accepted
ABSTRACT
The bright southern star L2 Pup is a particularly prominent asymptotic giant branch (AGB) star, located at a distance of only 64 pc.
We report new adaptive optics observations of L2 Pup at visible wavelengths with the SPHERE/ZIMPOL instrument of the VLT that
confirm the presence of the circumstellar dust disk discovered recently by Kervella et al. (2014b). This disk is seen almost almost
edge-on, at an inclination of 82◦
. The signature of its three-dimensional structure is clearly observed in the map of the degree of
linear polarization pL. We identify the inner rim of the disk through its polarimetric signature at a radius of 6 AU from the AGB star.
The ZIMPOL intensity images in the V and R bands also reveal a close-in secondary source at a projected separation of 2 AU from
the primary. The identification of the spectral type of this companion is uncertain due to the strong reddening from the disk, but its
photometry suggests that it is a late K giant, of comparable mass to the AGB star. We present refined physical parameters for the
dust disk derived using the RADMC-3D radiative transfer code. We also interpret the pL map using a simple polarization model to
infer the three-dimensional structure of the envelope. Interactions between the inner binary system and the disk apparently form spiral
structures that propagate along the orthogonal axis to the disk to form streamers. Two dust plumes propagating orthogonally to the
disk are also detected. They originate in the inner stellar system, and are possibly related to the interaction of the wind of the two stars
with the material in the disk. Based on the morphology of the envelope of L2 Pup, we propose that this star is at an early stage of the
formation of a bipolar planetary nebula.
Key words. Stars: individual: HD 56096; Stars: imaging; Stars: AGB and post-AGB; Stars: circumstellar matter; Techniques: high
angular resolution; Techniques: polarimetric
1. Introduction
Evolved stars are important contributors to the enrichment of
heavy elements in the interstellar medium, and more generally
to the chemical evolution of the Universe. As they are much
more numerous than high mass stars, the low and intermedi-
ate mass stars (1 − 8 M ) play a particularly important role.
L2 Puppis (HD 56096, HIP 34922, HR 2748) is an asymptotic
giant branch (AGB) Mira-like variable, with an uncertain mass
estimated at 0.7 M by Lykou et al. (2015), 1.7 M by Dumm
& Schild (1998) and 2 M by Kervella et al. (2014b). This is
probably the second nearest known AGB star at d = 64 pc
(π = 15.61 ± 0.99 mas, van Leeuwen 2007), i.e. only 9 pc far-
ther than R Dor and 30% closer than Mira. It is also one of the
brightest, at mV ≈ 7 and mK ≈ −1.5. L2 Pup is therefore a partic-
ularly prominent benchmark object to monitor the final stages of
Based on observations made with ESO telescopes at Paranal Obser-
vatory, under ESO Science Verification program 60.A-9367(A).
the evolution of moderately massive stars. Kervella et al. (2014b)
obtained in 2013 a series of NACO images in 12 narrow-band fil-
ters covering λ = 1.0−4.0 µm. They revealed a dust lane in front
of the star that exhibits a high opacity in the J band and becomes
translucent in the H and K bands. In the L band, thermal emis-
sion from the dust disk was also detected, as well as a large loop
extending to more than 10 AU. New observations by Lykou et al.
(2015) using the sparse aperture masking mode of NACO con-
firmed the observed structures. From aperture-synthesis imag-
ing combining NACO and VLTI/AMBER, Ohnaka et al. (2015)
identified clumpy dust clouds and also confirm the presence of
an elongated central emission in the East-West direction. They
also reveal that the southern half of the central star is severely
obscured by the nearly edge-on disk. The hypothesis proposed
by Kervella et al. (2014b) is that the circumstellar dust of L2 Pup
is distributed in a disk seen at an almost edge-on inclination of
84◦
. This disk may act as a collimator for the AGB star mass loss.
However, the true three-dimensional (3D) geometry of the enve-
Article number, page 1 of 12
2. A&A proofs: manuscript no. L2Pup_SPHERE_v2r1
lope was not constrained by the NACO infrared images. More-
over, and although the large dust loop observed in the L band
pointed at the presence of a companion, it remained undetected
in the NACO images.
In the present work, we report diffraction limited polarimet-
ric images at visible wavelengths from the SPHERE/ZIMPOL
adaptive optics system (Sect. 2). The resulting intensity and de-
gree of linear polarization maps allow us to address two ques-
tions: (1) what is the 3D geometry of the dust distribution around
L2 Pup? and (2) is L2 Pup a binary star? After an analysis of the
images (Sect. 3), we discuss the implications in Sect. 4.
2. Observations and data reduction
2.1. Observations
The Spectro-Polarimetric High-contrast Exoplanet REsearch
(SPHERE, Beuzit et al. 2008) is a high performance adaptive
optics system (Fusco et al. 2014) installed at the Nasmyth focus
of the Unit Telescope 3 of the Very Large Telescope. We ob-
served L2 Pup on the night of 7 December 2014 using SPHERE
and the Zurich IMaging POLarimeter (ZIMPOL, Roelfsema
et al. 2014) during the Science Verification of the instrument.
We observed L2 Pup and a point spread function (PSF) calibra-
tor, β Col (HD 39425, spectral type K1III) in the polarimetric P2
mode. β Col also acts as a photometric calibrator as it belongs to
the catalogues by Bordé et al. (2002) and Cohen et al. (1999).
The ZIMPOL instrument includes two cameras that allow for si-
multaneous observations at two different wavelengths. We used
the V (for camera 1, hereafter referred to as cam1) and NR (cam2)
filters, that have respective central wavelengths of λV = 554.0
and λR = 645.9 nm, and full width half maximum bandwidths
of 80.6 and 56.7 nm. The list of observations is given in Table 1.
The observations of L2 Pup were taken both with and without
Lyot coronagraph (V_CLC_S_WF). The PSF reference β Col was
observed only without coronagraph, and through the ND2 neutral
density filter, that has a photometric transmission of 0.61% in V
and 0.76% in NR
1
.
We processed the raw cubes using the ZIMPOL data reduc-
tion pipeline, in its pre-release version 0.14.02
. The observations
resulted in 24 data cubes for observations #1 and #2 (Table 1),
containing the frames recorded with the two cameras, and 48
cubes for observation #3. Each of these cubes was processed
separately using the pipeline to produce Stokes +Q, −Q, +U and
−U frames for each of the two cameras, together with their asso-
ciated intensity frames IQ and IU. The resulting average frames
were then precisely aligned and derotated using custom python
routines. We observed a fixed rotation offset of 3◦
clockwise of
cam2 images relative to cam1 taken as the reference in the fol-
lowing. The vertical axis of cam1 is oriented North-South, with
North up and East to the left (all images are oriented following
this convention in the present work). Examples of the resulting
images of L2 Pup and the PSF calibrator are presented in Fig. 1.
The images obtained with the Lyot coronagraph did not show a
significant improvement in the detection of the faint extensions
of the disk, while the presence of the occulter created perturba-
tions to the wings of the PSF. As a result, the coronagraphic in-
tensity images are poorly suited for deconvolution (Fig. 2), and
we did not consider them further in this work. Fortunately, the
polarimetric parameters of the coronagraphic observations are
1
According to the SPHERE User Manual version P95.2.
2
Downloadable from ftp://ftp.eso.org/pub/dfs/pipelines/
sphere/
NR band (646 nm)
PSF
Fig. 1. Non-deconvolved intensity image of L2 Pup in the NR band, with
a square root intensity scale (in ADU) and a field of view of 0.91 ×
0.91 . The PSF (β Col) is shown as an insert at the same scale.
Fig. 2. Top: Comparison of the image of L2 Pup in the NR band without
coronagraph (left) and the image in the same filter with coronagraph
(right). Bottom: Same images after deconvolution (20 steps of IRAF’s
lucy algorithm). The logarithmic color scales have been matched tak-
ing into account the different exposure times. The field of view is
0.91 × 0.91 .
of excellent quality, as the PSF wing signature is naturally sub-
tracted during the computation of the Stokes Q and U maps. We
will therefore consider the coronagraphic pL maps together with
the non-coronagraphic versions in order to check for the stability
of the polarimetric measurement.
2.2. Polarimetric quantities and deconvolution
From the average +Q, −Q, +U, −U, IQ and IU frames, we de-
rive the degree of linear polarization pL, the polarization electric-
Article number, page 2 of 12
3. P. Kervella et al.: SPHERE/ZIMPOL observations of L2 Puppis
Table 1. Log of the SPHERE/ZIMPOL observations of L2 Pup and its associated PSF calibrator, β Col.
# MJD Star Coronagraph DIT NDIT Dither Polar Total exp. Seeing AM
[s] cycles [s] [”]
1 56998.3024 β Col No 1.2 16 × 2 6 1 230.4 0.74 1.11
2 56998.3229 L2 Pup No 1.2 50 × 2 6 1 720 0.77 1.08
3 56998.3558 L2 Pup Yes 12 4 × 2 6 2 1152 0.67 1.14
Notes. MJD is the average modified julian date of the exposures. DIT is the individual exposure time of the SPHERE frames, and NDIT is the
total number of frames recorded. Dither is the number of dithering positions, and AM is the airmass.
Fig. 3. Comparison of the IQ (left) and IU (right) images of the PSF star
β Col. The grey scale is identical between the two images, and the field
of view is 0.113 × 0.113 .
vector position angle θ and the intensity map I using:
q =
[+Q] − [−Q]
2 IQ
, u =
[+U] − [−U]
2 IU
(1)
pL = q2 + u2, θ = arctan
q
u
, I =
IQ + IU
2
. (2)
We deconvolved the intensity and pL images of L2 Pup using
the β Col intensity maps I as the dirty beams, and the Lucy-
Richardson (L-R) algorithm implemented in the IRAF3
software
package. We checked that the small differences between the IQ
and IU images of the PSF star (Fig. 3) do not introduce artefacts
in the deconvolution process when using the average intensity
image I as the dirty beam. McNeil & Moody (2005) showed that
the Lucy-Richardson algorithm preserves the photometric accu-
racy of the original images relatively well compared to other
classical algorithms. We stopped the L-R deconvolution after
80 iterations (uniformly for both cameras), as the deconvolved
images do not show a significant evolution for additional pro-
cessing steps. The resulting I and pL deconvolved frames are
presented in Fig. 4. The quality of the AO correction and the
stability of the atmospheric seeing during the observations (Ta-
ble 1) results in a very good aptitude of the L2 Pup images for
deconvolution. On the PSF calibrator β Col, we measure a Strehl
ratio S ≈ 30% in the V filter, and S = 40 to 45% in the NR fil-
ter. This is equivalent to the Strehl ratios obtained with NACO
respectively in the J and H bands, in good atmospheric condi-
tions. The measured full width at half maximum (FWHM) of
the PSF image is approximately 16.5×18 mas in the V band and
17 × 20 mas in the NR band.
The pL maps show clearly the presence of four maxima lo-
cated on the side, below and above the dark dust lane. This be-
havior is typical of light scattering in a thick circumstellar dust
disk, as the light is scattered and transmitted on both sides of the
disk, with a maximum polarization for a scattering angle close
to 90◦
(see Sect. 3.2 for a further discussion).
3
http://iraf.noao.edu
Table 2. Photometry of L2 Pup and its companion.
Star mV mR
β Col (calibrator) 3.12 ± 0.01 2.27 ± 0.01
L2 Pup (total) 7.03 ± 0.05 5.54 ± 0.05
Disk only 7.36 ± 0.10 5.97 ± 0.10
L2 Pup A 8.72 ± 0.10 6.93 ± 0.10
L2 Pup B 10.29 ± 0.10 8.75 ± 0.10
2.3. Pixel scale and field orientation
We aligned the cam2 images on the orientation of cam1 by rotat-
ing them by 3 deg counter clockwise, as described in Sect. 2.1.
We adopt a pixel scale of 3.628 ± 0.036 mas pix−1
and a posi-
tion angle of the vertical axis with respect to North of 357.95 ±
0.55 deg for both cam1 and cam2. These parameters were de-
rived from commissioning observations of several astrometric
reference sources by Ch. Ginski (private communication), in-
cluding five astrometric binaries with high quality orbital solu-
tions and the quadruple system θ1
Ori B.
3. Analysis
3.1. Photometry and astrometry
From the ZIMPOL images, the total flux of L2 Pup and its close
envelope (within 0.5 of the central source) relative to β Col is
estimated to fL2 Pup/ fβ Col = 0.027 ± 0.001 in the V band and
fL2 Pup/fβ Col = 0.049 ± 0.002 in the NR band. Although ZIM-
POL’s NR filter has a narrower bandpass than the standard R fil-
ter, we consider here that they are equivalent. The V and R mag-
nitudes of β Col were taken from Morel & Magnenat (1978).
The central source appears noticeably elongated in the
ZIMPOL intensity images (Fig. 5), and after deconvolution,
a secondary source is detected, as shown in Fig. 6. The as-
trometric position of the fainter source relative to the cen-
tral AGB star in both the V and NR images is found to
be: ∆x, ∆y = +9 ± 1 pix, +1 ± 1 pix , corresponding to
[∆α, ∆δ] = [32.7 ± 3.6 mas, −3.6 ± 3.6 mas], and a projected
separation of 32.9 ± 3.6 mas, or 2.1 ± 0.2 AU considering the
Hipparcos parallax. Due to the high geometrical inclination and
thickness of the disk, it is likely that part of the photosphere of
the AGB star is obscured (Kervella et al. 2014b). This effect
could bias the apparent astrometric position, as well as that of
the companion. However, considering that the vector direction
between the AGB star and its companion is mostly aligned with
the major axis of the disk, the relative position of the two objects
should only be mildly affected.
The photometry of the different parts of the L2 Pup system is
listed in Table 2. The majority of the flux in the V and NR bands
is scattered light coming from the disk, as the contribution of the
Article number, page 3 of 12
4. A&A proofs: manuscript no. L2Pup_SPHERE_v2r1
5 AU
V band (554 nm)
100 mas
N
E
NR band (646 nm)
Fig. 4. Top: Deconvolved intensity images of L2 Pup in the V (left) and NR (right) bands (logarithmic intensity scale, in ADU). Middle: Decon-
volved map of the degree of linear polarization pL in the V (left) and NR (right) bands from the non-coronagraphic observations (linear intensity
scale). Bottom: pL in the V (left) and NR (right) bands from the coronagraphic frames (linear intensity scale). The field of view is 0.60 × 0.60 .
Article number, page 4 of 12
5. P. Kervella et al.: SPHERE/ZIMPOL observations of L2 Puppis
Fig. 5. Non-deconvolved intensity images in NR of the central source
of L2 Pup (left) and the PSF calibrator β Col (right). The grey scale is
linear between the minimum and maximum value of each image, and
the field of view is 0.151 × 0.151 .
V (554 nm)
30 mas
N
E
NR (646 nm)
Fig. 6. Position of L2 Pup and its companion in the deconvolved V
(left) and NR (right) intensity images. The positions of the two stars
are marked with crosses. The field of view is 0.227 × 0.227 .
two stars to the total flux of the system reaches only 26% in V
and 32% in NR. To isolate the photometric contribution of the
secondary source L2 Pup B, we first subtracted the radial median
profile (centered on the primary star) from the deconvolved im-
ages to remove the flux contribution of the background. We then
measured the integrated flux over a disk with a radius of 4 pix-
els, as shown in Fig. 7, and we subtracted the background flux
measured on the opposite side of the central star. This second
background subtraction is intended to remove the scattered light
contribution by the disk. To estimate the flux from L2 Pup A, we
adopted the same approach, but we considered the deconvolved
image without radial median subtraction, and we subtracted the
background from the same background region as for L2 Pup B
(Fig. 7). We obtain a flux ratio of fV(B)/ fV(A) = 24 ± 10% in
the V band and fNR(B)/ fNR(A) = 19 ± 10% in the NR band. The
stated error bars are conservative, to take into account the uncer-
tainty in the neutral density filter transmission, deconvolved flux
distribution and estimation of the background level, that may not
be homogeneous between the eastern and western sides of the
disk. This translates into ±0.1 mag uncertainties for the individ-
ual components (disk, A and B), and we adopt ±0.05 mag error
bars for the integrated photometry of the whole system.
The two objects L2 Pup A and B appear relatively faint and
red in color. This is caused by the considerable wavelength de-
pendent absorption of the light as it passes through the disk.
Considering the geometrical configuration of the disk and binary
system, the reddening should however be similar for the two ob-
jects. Therefore, the difference in apparent V magnitude that we
measure (∆mV = 1.6) should be close to the difference in abso-
lute V magnitude between the two objects. A discussion of the
properties of L2 Pup B is presented in Sect. 4.1.
30 mas
N
E
V (554 nm)
Fig. 7. Radial median subtracted image of L2 Pup’s companion in the V
band. The photometry of L2 Pup B is computed from the integration of
the flux enclosed in the solid circle, while the background is estimated
in the dashed circle. The positions of the two stars are marked with
crosses, and the field of view is 0.227 × 0.227 .
3.2. Polarization model and 3D structure of the disk
To map the cold dust, we take advantage of the high scattering
and polarizing efficiency of the dust in the visible domain. The
basic principle of our approach is to derive the scattering angle
θ of the light on the dust from the measured degree of linear
polarization pL. For that purpose, we have to assume a polariza-
tion model pL(θ), following the method employed by Kervella
et al. (2014a) to map the 3D structure of the dusty envelope of
the long-period Cepheid RS Pup. The nature of the dust has an
impact on its polarization curve, in particular on the maximum
value of pL (hereafter pmax) and also on the angle of maximum
polarization (θmax). The consistently high maximum value of pL
in L2 Pup’s envelope indicates that the dust grain physical prop-
erties are probably comparable to those of RS Pup. The typical
Milky Way dust models exhibit lower maximum values of pL
(20 to 30%, Draine 2003). However, laboratory experiments by
Volten et al. (2007) show very high degrees of linear polariza-
tion (up to pL ≈ 50% to 100% in the visible) on light scattered
by fluffy dust grains (see also Shen et al. 2009), which may be
present around L2 Pup.
We observe in the deconvolved polarization maps presented
in Fig. 4 a value of pmax(V) = 0.46 and pmax(NR) = 0.61 for the
non-coronagraphic images. The coronagraphic images present
comparable but slightly lower maxima of pmax(V) = 0.42 and
pmax(NR) = 0.58. These figures are of the same order as the
pmax = 0.52 ± 0.02 value observed by Kervella et al. (2014a) in
the V band in the light scattering nebula surrounding RS Pup, as
well as by Sparks et al. (2008) in the dusty nebula of V838 Mon
(pmax ≈ 0.50, also in the V band).
For the present analysis of L2 Pup’s polarization, we thus
adopt the scaled “Draine” polarization model of the Milky Way
dust presented by Kervella et al. (2014a), with pmax(V) = 0.42 ±
0.02 and pmax(NR) = 0.58±0.02. The polarization for this model
peaks at a scattering angle of θmax = 92◦
. The chosen pmax values
were measured on the average pL maps of the non-coronagraphic
and coronagraphic frames, and the error bars cover the range of
values between the frames. The statistical errors are significantly
smaller, but the deconvolution process introduces an additional
Article number, page 5 of 12
6. A&A proofs: manuscript no. L2Pup_SPHERE_v2r1
0%
10%
20%
30%
40%
50%
60%
70%
0 10 20 30 40 50 60 70 80 90 100 110 120
DegreeoflinearpolarizationpL
Scattering angle Theta (degrees)
pMax=0.58
pMax=0.42
Fig. 8. Adopted polarization models pL(θ) for the V band (dashed curve)
and the NR band (solid curve).
uncertainty that we take into account conservatively. The result-
ing pL(θ) model curves are presented in Fig. 8. The fact that
the pmax value is smaller in the V band than in the NR band is in
agreement with the existing light scattering models. For instance,
the Milky Way dust model4
presented by Draine (2003) for a to-
tal to selective extinction parameter RV = AV/E(B − V) = 3.1
gives pmax = 0.236 at λ = 547 nm, and pmax = 0.273 at
λ = 649 nm. Kervella et al. (2014a) presents a more detailed
discussion of the choice of polarization model.
In our simple approach, we assume that the scattering angle
is lower than or equal to θmax, i.e. that the scattering occurs in
the forward direction. The reason for this choice is that at vis-
ible wavelengths, forward scattering is far more efficient than
backward scattering. This means that the majority of the scat-
tered light we observe around L2 Pup comes from dust located
between us and the AGB star, rather than behind the star. How-
ever, for scattering angles close to 90◦
, there is an unresolvable
ambiguity whether the material is located closer or farther to us
than the star. In other words, we assume that the dust is located
in front of the “plane of the sky”, defined as the imaginary plane
perpendicular to the line of sight passing through the central star,
rather than behind.
We also make the assumption that the stellar light is scattered
only once on the dust grains before reaching us. This is clearly
a simplification, but this hypothesis should be valid for the inner
parts of the disk, that exhibit the strongest scattered light surface
brightness. Since the scattering from the disk is generated on the
inside of the bipolar cone, and we are on the outside of the cone,
the emission from the inner surface could likely be rescattered
in the passage through the cone walls. However, the dust column
density in these walls is apparently small, and the effect of this
second forward scattering of the already polarized light from the
inner disk is therefore not expected to change significantly the
degree of linear polarization. Another simplification of our com-
putation of the scattering angle θ is that we consider both stars A
and B together as a single source. As we are mostly interested in
scattering that occurs in the disk and other features at a typical
radius of 10 AU, the two stars are mostly seen as a single source
by the light scattering dust. Moreover, the flux contribution of
B is limited to less than a quarter of that of the AGB star in the
ZIMPOL wavelength bands.
4
Data available from https://www.astro.princeton.edu/
~draine/dust/scat.html
Table 3. Grid parameters of the RADMC-3D simulation
Parameter Value
Inner radius 3 AU
Outer radius 100 AU
Number of points in radius direction 500
Maximum meridional angle 0.8 rad
Number of points in meridional angle 120
Azimuthal direction Invariant
Wavelength interval limits (µm) [0.1, 1, 10, 100]
Number of points in each interval [100, 50, 20]
Knowing the projected radius r (in AU) of each point in the
disk relative to the central star (from the angular separation and
the parallax) and the scattering angle θ, we can compute its alti-
tude expressed (in AU) in front of the plane of the sky:
z = r tan
π
2
− θ . (3)
To compute θ, we first average the pL maps obtained with and
without coronagraph, that gave very similar polarization degrees
(Fig. 4), and then computed the altitude maps separately for each
camera. The values of z have been computed only where the SNR
of pL is larger than 5, and pL > 0.5%.
The results are shown in Fig. 9. We observe a deep minimum
of z on the eastern side of the A star, that we interpret in Sect. 4 as
the intersection of the inner rim of the dust disk with the plane of
the sky. A symmetric minimum with respect to A is also present.
There is a good match between the maps obtained for the two
filters, although the map in the NR band extends slightly further
than the map in the V band, thanks to the higher brightness of the
star and better polarizing efficiency of the dust in the NR band.
3.3. RADMC-3D radiative transfer modeling
3.3.1. Dust disk parameters
To determine the physical parameters of the disk of L2 Pup, we
adopt as a starting point the disk model presented by Kervella
et al. (2014b), that is based on the RADMC-3D radiative transfer
modeling tool (Dullemond 2012), in its version 0.38. This code
first computes the dust temperature using a thermal Monte Carlo
simulation (Bjorkman & Wood 2001), then it produces an image
using isotropic scattering. The parameters of the regular grid we
used are listed in Table 3. We did not use grid refinement.
As the primary component L2 Pup A dominates photomet-
rically over B in both the V and NR filters (Sect. 3.1), and to
simplify the computation while preserving the axial symmetry,
we considered the AGB primary as the single central source of
the model. Consistently with (Kervella et al. 2014b) we used
a stellar radius of 123 R , and the spectral energy distribution
(SED) was modeled using the Castelli-Kurucz library5
(Castelli
& Kurucz 2004) with the following parameters: Teff = 3500 K,
log g = 0.0 and [M/H] = 0.0. We allowed for a vertical shift of
the central star relative to the dust disk plane, and we note z
this offset, counted positively to the North. We used a flared disk
dust distribution described by the height radial distribution:
h(r) = hrout × r ×
r
rgrid, out
β
(4)
5
Available at http://www.stsci.edu/hst/observatory/crds/
castelli_kurucz_atlas.html
Article number, page 6 of 12
7. P. Kervella et al.: SPHERE/ZIMPOL observations of L2 Puppis
V band
5 AU
4
8
12
16 AU
A B
100 mas
N
E
NR band
Fig. 9. Map of the altitude of the scattering material in front of the plane
of the sky at the distance of L2 Pup, expressed in astronomical units. The
top panel shows the map derived from the V band observations while
the lower panel shows the NR band result. The positions of the AGB
star and its companion are marked with star symbols, and the location
of minimum altitude is shown with a green square. The grey scale is
linear between 0 and 16 AU, and the contour curves are separated by
increments of 4 AU from 0 to 20 AU. The field of view is 0.60 ×0.60 .
Where hrout is the ratio between h and r at the outer radius of the
grid rgrid, out, and β the flaring index. The assumed dust density
distribution is:
ρ(r, θ) = ρr(r) ρθ(r, θ) (5)
with:
ρr(r) = σout
r
rout
α
/ h(r)
√
2π , (6)
where σout is the dust density at the external radius of the disk
rout and:
ρθ(r, θ) = exp
−0.5
r
h(r)
tan
π
2
− θ
2
, (7)
Table 4. Derived parameters of the RADMC-3D dust disk model.
Derived parameter Value
z -0.5 AU
Rin 6 AU
Rout 13 AU
α -3.5
MgFeSiO4 density at Rout 5 10−4
g cm−2
MgFeSiO4 grain size 0.1 µm
MgFeSi2O3 density at Rout 9 10−4
g cm−2
MgFeSi2O3 grain size 0.3 µm
hrout 0.3
β 0.8
Disk inclination 82◦
Total dust mass 2.4 10−7
M
5 AU
V band
100 mas
N
E
NR band
Fig. 10. RADMC-3D Model image of the circumstellar disk of L2 Pup
in the V (left) and NR (right) bands. The color scale is a function of the
square root of the surface brightness (in Jy arcsec−2
).
θ being the meridional angle. Using the model parameters de-
rived by Kervella et al. (2014b) as our initial guess, we re-
produce morphologically and photometrically the observations
in the ZIMPOL filters. We used two amorphous dust species:
MgFeSiO4 (olivine) and Mg0.5Fe0.5SiO3 (pyroxene) whose spe-
cific weights are respectively 3.7 and 3.2 g cm−3
. These species
are among the most abundant in dust-forming circumstellar dust
shells (Ferrarotti & Gail 2006), and were already selected for the
modeling by Kervella et al. (2014b). Their physical properties6
were taken from Jaeger et al. (1994) and Dorschner et al. (1995).
The model parameters giving the best agreement with the
images and SED are listed in Table 4, and the corresponding
model images are represented on Fig. 10. As the RADMC-3D
model is a pure flared disk, it does not reproduce the asymmet-
ric features discussed in Sect. 4.3 (spirals, plumes). We do not
list confidence intervals for the parameters, as due to their rela-
tively large number and the computing time required to generate
a model, it is not possible to directly fit all the model parameters
together to the observables (images and SED). However, with the
two selected dust species, the solution is well defined. Changing
the grain size significantly degrades the fit. For instance, adding
smaller grains results in the dust becoming too transparent in the
red and infrared. The overall shape of the SED is also very sen-
sitive to the inclination of the disk. The fluxes in the visible and
in the infrared are well constrained by the dust densities and the
visibility of the stellar apparent disk. To match the photometry,
we need to partly see the stellar disk above the main dust band
6
Available at http://www.astro.uni-jena.de/Laboratory/
OCDB/amsilicates.html
Article number, page 7 of 12
8. A&A proofs: manuscript no. L2Pup_SPHERE_v2r1
in the NR band, as well as the light scattered on the inner rim
of the disk. But the star has to remain partially obscured for the
flux to stay at a sufficiently low level, particularly in the near in-
frared. The number of dust species remains however relatively
uncertain. Considering the NACO images alone, only the two
selected species could reproduce the flat shape of the SED from
1 to 4 µm, but additional species may also be present.
The total dust mass in the RADMC-3D disk model is
2.4 10−7
M . This low mass (equivalent to 0.08 M⊕) however
results in a relatively high dust density in the disk due to its
small geometrical dimensions. Assuming a gas-to-dust ratio of
the order of 100, this dust mass translates to a total mass includ-
ing gas of 10−5
to 10−4
M . Considering the mass loss rate of
10−9
to 10−8
M yr−1
estimated by Winters et al. (2002) from
CO line observations in the millimeter domain, this corresponds
to approximately 10 000 years of mass loss of L2 Pup at its cur-
rent rate. As we have only a limited knowledge of the physical
properties of L2 Pup B, we do not exclude that it may have con-
tributed part of the dust present in the disk.
Compared to Kervella et al. (2014b), we obtain a slightly
lower disk inclination (82◦
instead of 84◦
), that may be partly
due to the fact that we place the central star slightly below the
disk plane (by approximately one stellar radius). We also find a
significantly larger disk thickness, as the efficient scattering in
the visible and the high resolution of the ZIMPOL images al-
low us to see the dust band more clearly than in the infrared
with NACO. In the model by Kervella et al. (2014b), the density
of the dust at a radius of 13 AU is σout = 1.67 10−4
g cm−2
for
MgFeSiO4 and σout = 2.39 10−4
g cm−2
for MgFeSi2O3. These
densities are approximately 4 times smaller than those found in
the present model at the same radius Rout (Table 4). This differ-
ence can be explained by the higher visible obscuration that has
to be included in the model to match the ZIMPOL photometry.
The outer radius of the disk is smaller than in Kervella et al.
(2014b) at 13 AU. However, we do not exclude that cold dust is
present at larger distances, as the spectral energy distribution of
L2 Pup shows excess up to the radio domain.
3.3.2. Spectral energy distribution
The integrated spectral energy distribution (SED) of L2 Pup and
its envelope is presented in Fig. 11. Our new ZIMPOL photom-
etry is shown using green points. The early 2014 NACO pho-
tometry is represented by red points, while the orange curve is
the MIDI spectrum (Kervella et al. 2014b). The grey points and
curve represent the pre-dimming photometry (before 1995) and
the reddened Kurucz model with E(B − V) = 0.6, respectively.
The SED prediction by our RADMC-3D model is represented
as a cyan curve, and the Kurucz model (L2 Pup A only) used for
our modeling as a blue curve.
Before the the long-term fading that started in 1995, the
SED was relatively well modeled from the ultraviolet to the
near-infrared by a simple extinction of the Kurucz stellar SED
(Teff = 3500 K) by Milky Way dust with E(B − V) = 0.6, as
demonstrated by the grey curve and grey points in Fig. 11. In
this basic approach, the thermal emission from the disk was natu-
rally not included. For our recent (post-fading) photometry from
NACO and ZIMPOL (obtained in early and late 2014), it is not
possible to match both the near-infrared and visible photometry
using such a simple model, as E(B − V) ≈ 1.5 predicts correctly
the visible photometry but is insufficient for the near-infrared.
The RADMC-3D model by Kervella et al. (2014b) repro-
duced properly the flat shape of the SED of L2 Pup between 1
and 4 µm, as well as the silicate bump around λ = 10 µm and the
thermal emission tail at longer wavelengths. As shown in Fig. 11,
our current model gives a predicted flux at visible wavelengths
that is compatible with the ZIMPOL measurements. To reach
this agreement, we adjusted the model parameters (disk thick-
ness and inclination in particular), but the assumed dust proper-
ties are the same (composition, grain size).
4. Discussion
4.1. L2 Pup A and B
Considering the observed flux ratio between the fainter compan-
ion L2 Pup B and the AGB star A in the visible (≈ 24%), the
companion is probably a red giant star, of somewhat smaller
mass as A and in a less evolved state. Without further spectral
information on L2 Pup B, we cannot exclude that it is of non-
stellar nature (e.g. a prominent dust knot). However, the high
relative flux compared to the AGB star favors the stellar compan-
ion hypothesis, that we adopt in the following. The color of B,
(V −R)B = 1.54, is slightly bluer than that of A, (V −R)A = 1.79,
which is consistent with this interpretation. It is however difficult
to assess precisely the spectral type of the companion based on
its color alone, due to the strong circumstellar reddening.
Another approach to determine the properties of the sec-
ondary is to consider the color excess E(B−V) = 0.6 determined
by Kervella et al. (2014b) based on the photometry obtained be-
fore the fading of 1995. Using this parameter, we correct the
apparent (V − R) colors of A and B (Table 2), and we obtain
(V − R)A = 1.2 and (V − R)B = 1.0. These colors correspond to
an early M giant for A (consistent with its effective temperature)
and a late K (or very early M) giant for B. The mass of L2 Pup B
could be approximately of 1.5 M , as considering the rapidity of
giant branch (GB) evolution, to have a stellar pair on the GB and
AGB simultaneously implies that they were close in mass while
on the main sequence.
To determine the plausible orbital period of the central bi-
nary, we consider the classical relation from Kepler’s third law:
P2
orb =
4π2
r3
G (m1 + m2)
, (8)
where m1 and m2 are the two object masses, Porb the orbital
period, and r the separation between the stars (the orbits are
assumed to be circular). For equal mass components of 1.5 to
2 M , and a separation of 2 to 4 AU, we obtain orbital periods
of Porb = 1.4 to 4.6 years. To obtain a more precise estimate, we
plan to follow the apparent stellar positions through part or all of
the binary period. We note that the mass of L2 Pup is currently
uncertain, as Lykou et al. (2015) derive a low value of 0.7 M for
the AGB star from the dynamics of the SiO masers (McIntosh &
Indermuehle 2013), while Dumm & Schild (1998) and Kervella
et al. (2014b) propose values closer to 2 M . The influence of
the presence of a second star in the system on these estimates
is unclear. We postpone a more detailed discussion of the evolu-
tionary state of the L2 Pup system to a forthcoming paper.
4.2. Overall disk geometry
A comparison of the NR light intensity map with the infrared
images from Kervella et al. (2014b) is presented in Fig. 12. We
interpret the compact polarization maximum visible to the East
of L2 Pup A (marked with a green square in Fig. 9), as the in-
ner rim of the disk. It is consistently detected in both the V and
NR band polarimetric maps, and it is interesting to remark that
Article number, page 8 of 12
9. P. Kervella et al.: SPHERE/ZIMPOL observations of L2 Puppis
100 101
Wavelength (µm)
10-12
10-11
10-10
10-9
10-8
Flux(W.m−2.µm)
RADMC-3D model SPHERE
Kurucz 3500K
Kurucz with extinction
MIDI
NACO Observations
SPHERE Observations
Photometry pre-1995
Fig. 11. Spectral energy distribution of L2 Pup.
5 AU 100 mas
N
E
0.65 µm 1.24 µm 2.17 µm 4.05 µm
Fig. 12. Visible (ZIMPOL, logarithmic intensity scale) and infrared (NACO, from Kervella et al. 2014b) images (square root scale) of L2 Pup.
another pL maximum is present almost symmetrically with re-
spect to L2 Pup A. These polarization maxima and the central
star are aligned with the major axis of the disk. The radius of the
pL minimum measured from L2 Pup A is Rrim = 6.0 ± 0.2 AU.
This value is in excellent agreement with the inner rim radius of
6 AU proposed by Kervella et al. (2014b) based on the K band
image: the thermal emission from the inner rim of the disk can
be seen as an East-West segment in the 2.17 µm image presented
in Fig. 12. This radius is also consistent with the corresponding
RADMC-3D model parameter presented by these authors to re-
produce the SED. The semi major axis of the ellipse represented
in Fig. 13 is Rext = 13 AU, and the thickness of the dark dust
band is hext = 3 AU. We propose that Rext corresponds to the
external radius of the dense part of the dust disk and hext is its
thickness at its external radius.
It is interesting to remark that the values of Rrim, Rext and
hext that were directly measured from the ZIMPOL intensity and
pL maps are respectively in very good agreement with the best
fit parameters Rin = 6 AU, Rout = 13 AU and hrout × Rout =
4 AU listed in Table 4. With the selected dust mixture and grain
size, they are the only combination that produces model images
and SED matching the observed ones. This convergence gives
confidence that the RADMC-3D model geometry is a reasonably
good match to the true dust distribution around L2 Pup.
We can check the compatibility of the radius of the inner rim
of the disk with the presence of dust by computing the equilib-
rium temperature at this distance from the AGB star. We con-
sider the absolute magnitude of L2 Pup before the fading that
occurred after 1995 (see also Sect. 4.4), MK = −2.34 and color
(V−K) = 7.0 (Bedding et al. 2002). We consider the K -band an-
gular diameter measurements of Millan-Gabet et al. (2005), by
using six stars with a similar (V −K) color at phase 0. The appar-
ent diameter for K = 0 is 7.5 ± 1 mas, and the angular diameter
of L2 Pup A is thus estimated to ≈ 22±3 mas, in agreement with
the 19 ± 1.6 mas measurement by Kervella et al. (2014b). As the
radius of the inner edge of the disk is 94±4 mas, then the ratio of
disk inner rim to stellar radius is 8.5 ± 2. Assuming the conser-
vation of energy in a spherical geometry, the rim of the disk will
have an equilibrium temperature
√
8.5 smaller than the effective
temperature of the star. The pre-dimming effective temperature
of star A from Bedding et al. (2002) is Teff = 2900 K (we neglect
the contribution of B), that gives T ≈ 1000 K at the disk inner
boundary. Assuming a higher Teff = 3500 K for the star results
in T ≈ 1200 K at the inner rim. In the absence of mineralogical
information, these is a plausible range of temperature for dust
formation (see e.g. Gail et al. 2013).
We do not identify clear signatures of shadowing effects in
the cones or on the disk from the inner system components (see
e.g. Marino et al. 2015), but such effects are difficult to disentan-
gle from dust density fluctuations in a complex envelope such as
that of L2 Pup. The overall asymmetry between the eastern and
western parts of the cones may however be caused by differential
shadowing effects, in particular if the inner rim of the disk has
an inhomogeneous dust density and scale height.
Article number, page 9 of 12
10. A&A proofs: manuscript no. L2Pup_SPHERE_v2r1
5 AU 100 mas
N
E
A B
Loop
Plume 1
Spiral 1
Spiral 2
Plume 2
Segment
3 AU
Max.
pL
Max.
pL
Max.
pL
Max.
pL
Band
Edge
Northern cone
Southern cone
Fig. 13. Nomenclature of the features observed around L2 Pup.
4.3. Specific features in the nebula
Several remarkable features are visible in the intensity maps ob-
tained with ZIMPOL and NACO. A nomenclature of these fea-
tures is presented in Fig. 13.
4.3.1. The loop and spirals
Following Kervella et al. (2014b), we define the loop as the large
thermal emission feature detected in the NACO L band images.
The loop is not clearly detected in the ZIMPOL unpolarized in-
tensity maps. Its eastern part corresponds well to the maximum
of the pL map presented in Fig. 4, and it appears to develop on
the far side of the northern cone. Its non detection in visible scat-
tered light is likely due to the inefficiency of backward scattering.
A superposed view of the NR and thermal infrared L band image
at 4.05 µm is presented in Fig. 14, to show the relative positions
of the loop and the northern cone.
A bright curved feature labeled spiral 1 in Fig. 13 is detected
in the eastern part of the disk. Its apparent origin is located at the
inner rim of the disk. Its true starting point may however be hid-
den behind the northern edge of the dust band. It is the brightest
feature in the nebula apart from the two stars and the inner rim
of the dust disk, and it is easily visible in the non-deconvolved
images of L2 Pup (Fig. 1). We also note the presence of a second
spiral (spiral 2 in Fig. 13) in the southern cone of the nebula,
whose winding orientation is the same as the loop and spiral 1,
and whose position is mostly symmetric of the loop with respect
to star A. Based on the z map (Fig. 9), the loop and also proba-
bly the two spirals seem to be physically located on the surface
of the disk and cones.
The presence of L2 Pup’s spirals indicates a behavior poten-
tially similar to that observed in the binary AGB star R Scl by
Maercker et al. (2012) using ALMA. In both cases, spirals are
observed, but the overall geometry of the envelope of R Scl is
spherical, while the geometry of that of L2 Pup is essentially
a bipolar structure. We propose that the different geometry of
L2 Pup is due to the presence of the dust disk that collimates the
stellar wind along a specific spatial axis. Maercker et al. (2012)
0.65 µm + 4.05 µm (color)
10 AU
Fig. 14. L band loop image from NACO (color scale) superimposed on
the V band ZIMPOL unpolarized intensity map (background black and
white image). The field of view is 0.60 × 0.60 .
deduced the recent mass loss history of R Scl from the spacing
of the successive windings. Other examples exist, e.g. Ramstedt
et al. (2014) reported two-dimensional spirals in the Mira binary
system. Cernicharo et al. (2015) identified a large spiral structure
in the envelope of CW Leo at arcminute scales, using the 30-m
IRAM antenna at millimeter wavelengths. Decin et al. (2015)
also detected arcs and a smaller spiral in the inner envelope of
this star from ALMA, as well as a probable companion star from
modeling of the spiral.
In the case of L2 Pup, the spirals are apparently located on
the internal surfaces of the cones, so this complicates the deter-
mination of the pitch of the spiral. The geometry of the L band
loop suggests that the initially two-dimensional spirals has been
blown away by the stellar wind, collimated by the disk, to form
two 3D streamers (to the North and South). We can roughly es-
timate the winding time scale of the loop from the spacing be-
tween the tip of the loop and the star. We measure a vertical
spacing of 10 AU between the central object and the northern
end of the loop (Fig. 14). The CO outflow velocity determined
by Winters et al. (2002) is only 3 km/s, but with a collimated
flow nearly orthogonal to the line of sight, we have to account
for a projection effect. Considering the inclination of the disk
(≈ 82◦
, see Sect. 3.3), we estimate the velocity of the outflow
to vwind = 3/ cos(82◦
) ≈ 20 km/s. This value is faster than the
10 km/s typical velocity of the material close to the photosphere
derived by Winters et al. (2002) from the SiO masers. It is qual-
itatively in agreement with the wind velocity derived by Maer-
cker et al. (2012) for R Scl. Considering vwind = 20 km/s, the
material in the loop takes 10 AU/(20 km/s) ≈ 2.5 years to move
vertically by one spiral winding. There is a large uncertainty on
whether we observe a complete winding or only a partial one, but
this duration is reasonably comparable with the plausible orbital
period of the central binary (Sect. 4.1).
Article number, page 10 of 12
11. P. Kervella et al.: SPHERE/ZIMPOL observations of L2 Puppis
4.3.2. Plumes
The extended plume 1 that emerges to the North of the disk has
its apparent origin close to the maximum of polarization, i.e. at
the location that we identify as the inner rim of the dust disk,
at a radius of 6 AU. Its signature is detected in the polarization
map, and its 3D orientation appears essentially perpendicular to
the dust disk plane (Fig. 9). The emission observed to the East of
L2 Pup A in Fig. 7 could be the result of the wind and radiation
pressure of B blowing the dusty wind of A toward the East. The
similarity in position between the tip of spiral 1 and the start of
plume 1 indicates that the plume may be ejected from this impact
point, due to the local increased heating around the location of
the shock. Finally, another speculative explanation is that a low
mass companion (possibly recently formed in the disk) is ac-
creting material expelled from the AGB star, and ejects material
through polar jets (Veras et al. 2013; Kim & Taam 2012).
Mostly parallel to plume 1, plume 2 has also a clear signature
in the pL maps (Fig. 4), and its 3D position appears again nearly
perpendicular to the disk plane, as shown in Fig. 9. Its origin can
be traced in the inner binary system, and more precisely close to
the position of the B star. One hypothesis is that plume 2 could
originate from the collision of the winds of the two stars. An-
other possibility is that part of the material expelled by the AGB
component A is accreted through Roche lobe overflow on star
B (Abate et al. 2013), inducing the formation of an accretion
disk. This process could then result in the appearance of polar
enhanced mass loss streams. The faint X-ray emission detected
by Ramstedt et al. (2012) would favor this scenario, although the
authors indicate that it may be caused by the leak of red photons
in the detector.
4.4. Long-term photometric variations of L2 Pup
The visible flux of L2 Pup is subject to relatively large long-term
variations of ≈ 2 magnitudes in V (Bedding et al. 2002), with
in particular a 5-year decrease in brightness that started around
1995, followed by a long and stable minimum. This kind of trend
in Mira stars is rare, but not unknown (Dyck et al. 1991). The
time constant of such a trend seems too long to be associated
with AGB pulsation, and to short to be related to AGB evolu-
tion. Since the stars are obscured by the disk that is seen almost
edge-on, we propose that the long-term photometric variations
of L2 Pup are caused by changes in the line-of-sight opacity of
the intervening material. Bedding et al. (2002) observed that the
visible-infrared (V − K) color increased significantly during the
dimming event that started around the year 1995, which is con-
sistent with the occultation (and associated reddening) by the
dust present in the disk. We also note that the ZIMPOL inten-
sity images show that the edges of the main dust band exhibit
an irregular shape, and that the shape of the band itself appears
slightly curved in a “V” feature. The keplerian rotation of the
disk therefore likely results in time variable occultation of the
central stars.
4.5. A future bipolar planetary nebula?
The origin of bipolar planetary nebulae (PNe) is one of the great
classic problems of modern astrophysics. Bipolar PNe present a
remarkable axial symmetry, whose origin is often attributed to
the presence of a secondary star (Lagadec & Chesneau 2014;
Soker & Livio 1989), but a companion has been detectable only
in few cases (e.g. Olofsson et al. 2015). From its position in the
HR diagram, L2 Pup appears as a relatively young AGB star, and
therefore a possible progenitor of these spectacular structures.
Our ZIMPOL observations demonstrate that the close circum-
stellar dust is distributed in a dense disk, that also hosts a com-
panion star in a tight orbit.
A possible explanation for the formation of the circumbinary
disk is that part of the dust formed in the AGB star wind is con-
fined in the orbital plane through interaction with the wind and
radiation pressure of the secondary star. Another fraction of the
mass loss could then be collimated by the flared disk and accel-
erated orthogonally to the disk plane into a bipolar flow. In this
scenario, the presence of a companion and a collimating dust
disk appear intimately tied together to explain the appearance of
a privileged spatial axis in the mass loss. An alternate hypothe-
sis is that the companion accretes material ejected by the AGB
star, forming an accretion disk and its associated jets. These jets
would then carve a bipolar cavity in the slower AGB wind (see
e.g. García-Arredondo & Frank 2004; Nordhaus & Blackman
2006). Based on the morphology of the envelope of L2 Pup that
includes jets, streamers and a flared disk, both mechanisms may
also be simultaneously active. In this framework, it appears plau-
sible that the L2 Pup system will evolve into a PN of the hour-
glass type.
5. Conclusion
The unprecedented angular resolution of the ZIMPOL images
at visible wavelengths allowed us to confirm the discovery by
Kervella et al. (2014b) of a large dust disk around L2 Pup, and
revealed the presence of a companion at a separation of only
33 mas. The potential of the ZIMPOL instrument for the study
of the close environment of objects enshrouded in dust appears
excellent, thanks to the high efficiency of light scattering at vis-
ible wavelengths. Coupled with highly precise polarimetry, the
three-dimensional structure of the envelopes can be determined
with a high degree of fidelity through radiative transfer model-
ing. Only very few binary AGB star disks have been identified to
date. The disk we observed with ZIMPOL is therefore an impor-
tant fiducial to improve our understanding of the formation of
bipolar PNe. The L2 Pup system is very favorable for observa-
tion, thanks to its proximity, and a companion is detected which
is a significant indication for the generality of the binary case.
Following e.g. the work of Maercker et al. (2012) on R Scl,
the observation of this system with ALMA will provide decisive
information on the geometry and dynamics at play in this com-
plex envelope. For instance, CO line observations will directly
test our dust disk model through the monitoring of the keplerian
motion of the gas in the disk. McIntosh & Indermuehle (2013)
identified a large velocity range in the SiO maser emission, as
well as an intriguing three-peaked spectrum (Winters et al. 2002;
Schöier et al. 2004). Interferometric imaging with the exquisite
angular resolution of the longest baselines of ALMA (compa-
rable to NACO and ZIMPOL) will probe the near circumstellar
region from where the SiO emission originates.
Acknowledgements. We are grateful to the SPHERE instrument team for the
successful execution of our observations during the Science Verification of the
instrument. We thank Dr. Julien Milli for his help with the ZIMPOL data re-
duction pipeline. We acknowledge financial support from the “Programme Na-
tional de Physique Stellaire" (PNPS) of CNRS/INSU, France. STR acknowl-
edges partial support by NASA grant NNH09AK731. AG acknowledges sup-
port from FONDECYT grant 3130361. This research received the support of
PHASE, the high angular resolution partnership between ONERA, Observatoire
de Paris, CNRS and University Denis Diderot Paris 7. PK and AG acknowledge
support of the French-Chilean exchange program ECOS-Sud/CONICYT. This
research made use of Astropy7, a community-developed core Python package
7
Available at http://www.astropy.org/
Article number, page 11 of 12
12. A&A proofs: manuscript no. L2Pup_SPHERE_v2r1
for Astronomy (Astropy Collaboration et al. 2013). We used the SIMBAD and
VIZIER databases at the CDS, Strasbourg (France), and NASA’s Astrophysics
Data System Bibliographic Services. We used the IRAF package, distributed by
the NOAO, which are operated by the Association of Universities for Research in
Astronomy, Inc., under cooperative agreement with the National Science Foun-
dation.
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