Exoplanets in protoplanetary disks cause localized deviations from Keplerian velocity in channel maps of
molecular line emission. Current methods of characterizing these deviations are time consuming,and there is no
unified standard approach. We demonstrate that machine learning can quickly and accurately detect the presence of
planets. We train our model on synthetic images generated from simulations and apply it to real observations to
identify forming planets in real systems. Machine-learning methods, based on computer vision, are not only
capable of correctly identifying the presence of one or more planets, but they can also correctly constrain the
location of those planets.
Locating Hidden Exoplanets in ALMA Data Using Machine LearningSérgio Sacani
Exoplanets in protoplanetary disks cause localized deviations from Keplerian velocity in channel
maps of molecular line emission. Current methods of characterizing these deviations are time consuming, and there is no unified standard approach. We demonstrate that machine learning can quickly
and accurately detect the presence of planets. We train our model on synthetic images generated from
simulations and apply it to real observations to identify forming planets in real systems. Machine
learning methods, based on computer vision, are not only capable of correctly identifying the presence
of one or more planets, but they can also correctly constrain the location of those planets.
ASTRONOMICAL OBJECTS DETECTION IN CELESTIAL BODIES USING COMPUTER VISION ALGO...csandit
Computer vision, astronomy, and astrophysics function quite productively together to the point where they are completely logical for each other. Out of computer vision algorithms the
progress of astronomy and astrophysics would have slowed down to reasonably a deadlock. The new researches and calculations can lead to more information as well as higher quality of data. Consequently, an organized view on planetary surfaces can change all in the long run. A new
discovery would be a puzzling complexity or a possible branching of paths, yet the quest to know more about the celestial bodies by dint of computer vision algorithms will continue. The detection of astronomical objects in celestial bodies is a challenging task. This paper presents
an implementation of how to detect astronomical objects in celestial bodies using computer vision algorithm with satisfactory performance. It also puts forward some observations linked
among computer vision, astronomy, and astrophysics.
3D-Spatiotemporal forecasting the expansion of supernova shells using deep le...Sérgio Sacani
Supernova (SN) plays an important role in galaxy formation and evolution. In high-resolution galaxy simulations using massively
parallel computing, short integration time-steps for SNe are serious bottlenecks. This is an urgent issue that needs to be resolved
for future higher-resolution galaxy simulations. One possible solution would be to use the Hamiltonian splitting method, in
which regions requiring short time-steps are integrated separately from the entire system. To apply this method to the particles
affected by SNe in a smoothed particle hydrodynamics simulation, we need to detect the shape of the shell on and within which
such SN-affected particles reside during the subsequent global step in advance. In this paper, we develop a deep learning model,
3D-Memory In Memory (3D-MIM), to predict a shell expansion after a SN explosion. Trained on turbulent cloud simulations
with particle mass mgas = 1 M, the model accurately reproduces the anisotropic shell shape, where densities decrease by over
10 per cent by the explosion. We also demonstrate that the model properly predicts the shell radius in the uniform medium
beyond the training data set of inhomogeneous turbulent clouds. We conclude that our model enables the forecast of the shell
and its interior where SN-affected particles will be present.
Prospects for Detecting Gaps in Globular Cluster Stellar Streams in External ...Sérgio Sacani
Stellar streams form through the tidal disruption of satellite galaxies or globular clusters orbiting a
host galaxy. Globular cluster streams are exciting since they are thin (dynamically cold) and, therefore
sensitive to perturbations from low-mass subhalos. Since the subhalo mass function differs depending
on the dark matter composition, these gaps can provide unique constraints on dark matter models.
However, current samples are limited to the Milky Way. With its large field of view, deep imaging
sensitivity, and high angular resolution, the upcoming Nancy Grace Roman Space Telescope (Roman)
presents a unique opportunity to increase the number of observed streams and gaps significantly. This
paper presents a first exploration of the prospects for detecting gaps in streams in M31 and other
nearby galaxies with resolved stars. We simulate the formation of gaps in a Palomar-5-like stream
and generate mock observations of these gaps with background stars in M31 and the foreground Milky
Way stellar fields. We assess Roman’s ability to detect gaps out to 10 Mpc through visual inspection
and with the gap-finding tool FindTheGap. We conclude that gaps of ≈ 1.5 kpc in streams that are
created from subhalos of masses ≥ 5×106 M⊙ are detectable within a 2–3 Mpc volume in exposures of
1000s–1 hour. This volume contains ≈ 150 galaxies, including ≈ 8 galaxies with luminosities > 109 L⊙.
Large samples of stream gaps in external galaxies will open up a new era of statistical analyses of gap
characteristics in stellar streams and help constrain dark matter models.
Imaging the Milky Way with Millihertz Gravitational WavesSérgio Sacani
Modern astronomers enjoy access to all-sky images across a wide range of the electromagnetic spectrum from
long-wavelength radio to high-energy gamma rays. The most prominent feature in many of these images is our
own Galaxy, with different features revealed in each wave band. Gravitational waves (GWs) have recently been
added to the astronomers’ toolkit as a nonelectromagnetic messenger. To date, all identified GW sources have been
extra-Galactic and transient. However, the Milky Way hosts a population of ultracompact binaries (UCBs), which
radiate persistent GWs in the milliHertz band that is not observable with today’s terrestrial gravitational-wave
detectors. Space-based detectors such as the Laser Interferometer Space Antenna will measure this population and
provide a census of their location, masses, and orbital properties. In this work, we will show how this data can be
used to form a false-color image of the Galaxy that represents the intensity and frequency of the gravitational
waves produced by the UCB population. Such images can be used to study the morphology of the Galaxy, identify
interesting multimessenger sources through cross-matching, and for educational and outreach purposes.
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
Locating Hidden Exoplanets in ALMA Data Using Machine LearningSérgio Sacani
Exoplanets in protoplanetary disks cause localized deviations from Keplerian velocity in channel
maps of molecular line emission. Current methods of characterizing these deviations are time consuming, and there is no unified standard approach. We demonstrate that machine learning can quickly
and accurately detect the presence of planets. We train our model on synthetic images generated from
simulations and apply it to real observations to identify forming planets in real systems. Machine
learning methods, based on computer vision, are not only capable of correctly identifying the presence
of one or more planets, but they can also correctly constrain the location of those planets.
ASTRONOMICAL OBJECTS DETECTION IN CELESTIAL BODIES USING COMPUTER VISION ALGO...csandit
Computer vision, astronomy, and astrophysics function quite productively together to the point where they are completely logical for each other. Out of computer vision algorithms the
progress of astronomy and astrophysics would have slowed down to reasonably a deadlock. The new researches and calculations can lead to more information as well as higher quality of data. Consequently, an organized view on planetary surfaces can change all in the long run. A new
discovery would be a puzzling complexity or a possible branching of paths, yet the quest to know more about the celestial bodies by dint of computer vision algorithms will continue. The detection of astronomical objects in celestial bodies is a challenging task. This paper presents
an implementation of how to detect astronomical objects in celestial bodies using computer vision algorithm with satisfactory performance. It also puts forward some observations linked
among computer vision, astronomy, and astrophysics.
3D-Spatiotemporal forecasting the expansion of supernova shells using deep le...Sérgio Sacani
Supernova (SN) plays an important role in galaxy formation and evolution. In high-resolution galaxy simulations using massively
parallel computing, short integration time-steps for SNe are serious bottlenecks. This is an urgent issue that needs to be resolved
for future higher-resolution galaxy simulations. One possible solution would be to use the Hamiltonian splitting method, in
which regions requiring short time-steps are integrated separately from the entire system. To apply this method to the particles
affected by SNe in a smoothed particle hydrodynamics simulation, we need to detect the shape of the shell on and within which
such SN-affected particles reside during the subsequent global step in advance. In this paper, we develop a deep learning model,
3D-Memory In Memory (3D-MIM), to predict a shell expansion after a SN explosion. Trained on turbulent cloud simulations
with particle mass mgas = 1 M, the model accurately reproduces the anisotropic shell shape, where densities decrease by over
10 per cent by the explosion. We also demonstrate that the model properly predicts the shell radius in the uniform medium
beyond the training data set of inhomogeneous turbulent clouds. We conclude that our model enables the forecast of the shell
and its interior where SN-affected particles will be present.
Prospects for Detecting Gaps in Globular Cluster Stellar Streams in External ...Sérgio Sacani
Stellar streams form through the tidal disruption of satellite galaxies or globular clusters orbiting a
host galaxy. Globular cluster streams are exciting since they are thin (dynamically cold) and, therefore
sensitive to perturbations from low-mass subhalos. Since the subhalo mass function differs depending
on the dark matter composition, these gaps can provide unique constraints on dark matter models.
However, current samples are limited to the Milky Way. With its large field of view, deep imaging
sensitivity, and high angular resolution, the upcoming Nancy Grace Roman Space Telescope (Roman)
presents a unique opportunity to increase the number of observed streams and gaps significantly. This
paper presents a first exploration of the prospects for detecting gaps in streams in M31 and other
nearby galaxies with resolved stars. We simulate the formation of gaps in a Palomar-5-like stream
and generate mock observations of these gaps with background stars in M31 and the foreground Milky
Way stellar fields. We assess Roman’s ability to detect gaps out to 10 Mpc through visual inspection
and with the gap-finding tool FindTheGap. We conclude that gaps of ≈ 1.5 kpc in streams that are
created from subhalos of masses ≥ 5×106 M⊙ are detectable within a 2–3 Mpc volume in exposures of
1000s–1 hour. This volume contains ≈ 150 galaxies, including ≈ 8 galaxies with luminosities > 109 L⊙.
Large samples of stream gaps in external galaxies will open up a new era of statistical analyses of gap
characteristics in stellar streams and help constrain dark matter models.
Imaging the Milky Way with Millihertz Gravitational WavesSérgio Sacani
Modern astronomers enjoy access to all-sky images across a wide range of the electromagnetic spectrum from
long-wavelength radio to high-energy gamma rays. The most prominent feature in many of these images is our
own Galaxy, with different features revealed in each wave band. Gravitational waves (GWs) have recently been
added to the astronomers’ toolkit as a nonelectromagnetic messenger. To date, all identified GW sources have been
extra-Galactic and transient. However, the Milky Way hosts a population of ultracompact binaries (UCBs), which
radiate persistent GWs in the milliHertz band that is not observable with today’s terrestrial gravitational-wave
detectors. Space-based detectors such as the Laser Interferometer Space Antenna will measure this population and
provide a census of their location, masses, and orbital properties. In this work, we will show how this data can be
used to form a false-color image of the Galaxy that represents the intensity and frequency of the gravitational
waves produced by the UCB population. Such images can be used to study the morphology of the Galaxy, identify
interesting multimessenger sources through cross-matching, and for educational and outreach purposes.
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
Detection of an atmosphere around the super earth 55 cancri eSérgio Sacani
We report the analysis of two new spectroscopic observations of the super-Earth 55 Cancri e, in the near
infrared, obtained with the WFC3 camera onboard the HST. 55 Cancri e orbits so close to its parent
star, that temperatures much higher than 2000 K are expected on its surface. Given the brightness
of 55 Cancri, the observations were obtained in scanning mode, adopting a very long scanning length
and a very high scanning speed. We use our specialized pipeline to take into account systematics
introduced by these observational parameters when coupled with the geometrical distortions of the
instrument. We measure the transit depth per wavelength channel with an average relative uncertainty
of 22 ppm per visit and nd modulations that depart from a straight line model with a 6 condence
level. These results suggest that 55 Cancri e is surrounded by an atmosphere, which is probably
hydrogen-rich. Our fully Bayesian spectral retrieval code, T -REx, has identied HCN to be the
most likely molecular candidate able to explain the features at 1.42 and 1.54 m. While additional
spectroscopic observations in a broader wavelength range in the infrared will be needed to conrm
the HCN detection, we discuss here the implications of such result. Our chemical model, developed
with combustion specialists, indicates that relatively high mixing ratios of HCN may be caused by a
high C/O ratio. This result suggests this super-Earth is a carbon-rich environment even more exotic
than previously thought.
Discovery of rotational modulations in the planetary mass companion 2m1207b i...Sérgio Sacani
Rotational modulations of brown dwarfs have recently provided powerful constraints on the properties
of ultra-cool atmospheres, including longitudinal and vertical cloud structures and cloud evolution.
Furthermore, periodic light curves directly probe the rotational periods of ultra-cool objects. We
present here, for the first time, time-resolved high-precision photometric measurements of a planetarymass
companion, 2M1207b. We observed the binary system with HST/WFC3 in two bands and with
two spacecraft roll angles. Using point spread function-based photometry, we reach a nearly photonnoise
limited accuracy for both the primary and the secondary. While the primary is consistent with
a flat light curve, the secondary shows modulations that are clearly detected in the combined light
curve as well as in di↵erent subsets of the data. The amplitudes are 1.36% in the F125W and 0.78%
in the F160W filters, respectively. By fitting sine waves to the light curves, we find a consistent period
of 10.7+1.2
−0.6 hours and similar phases in both bands. The J- and H-band amplitude ratio of 2M1207b
is very similar to a field brown dwarf that has identical spectral type but di↵erent J-H color. Importantly,
our study also measures, for the first time, the rotation period for a directly imaged extra-solar
planetary-mass companion.
A High-mass, Young Star-forming Core Escaping from Its Parental FilamentSérgio Sacani
We studied the unique kinematic properties in massive filament G352.63-1.07 at 103 au spatial scale with the dense
molecular tracers observed with the Atacama Large Millimeter/submillimeter Array. We find the central massive
core M1 (12 Me) being separated from the surrounding filament with a velocity difference of
- =- - v vsys 2 km s 1 and a transverse separation within 3″. Meanwhile, as shown in multiple dense-gas
tracers, M1 has a spatial extension closely aligned with the main filament and is connected to the filament toward
both its ends. M1 thus represents a very beginning state for a massive, young star-forming core escaping from the
parental filament, within a timescale of ∼4000 yr. Based on its kinetic energy (3.5 × 1044 erg), the core escape is
unlikely solely due to the original filament motion or magnetic field but requires more energetic events such as a
rapid intense anisotropic collapse. The released energy also seems to noticeably increase the environmental
turbulence. This may help the filament to become stabilized again.
Keck Integral-field Spectroscopy of M87 Reveals an Intrinsically Triaxial Gal...Sérgio Sacani
The three-dimensional intrinsic shape of a galaxy and the mass of the central supermassive black hole provide key
insight into the galaxy’s growth history over cosmic time. Standard assumptions of a spherical or axisymmetric
shape can be simplistic and can bias the black hole mass inferred from the motions of stars within a galaxy. Here,
we present spatially resolved stellar kinematics of M87 over a two-dimensional 250″ × 300″ contiguous field
covering a radial range of 50 pc–12 kpc from integral-field spectroscopic observations at the Keck II Telescope.
From about 5 kpc and outward, we detect a prominent 25 km s−1 rotational pattern, in which the kinematic axis
(connecting the maximal receding and approaching velocities) is 40° misaligned with the photometric major axis of
M87. The rotational amplitude and misalignment angle both decrease in the inner 5 kpc. Such misaligned and
twisted velocity fields are a hallmark of triaxiality, indicating that M87 is not an axisymmetrically shaped galaxy.
Triaxial Schwarzschild orbit modeling with more than 4000 observational constraints enabled us to determine
simultaneously the shape and mass parameters. The models incorporate a radially declining profile for the stellar
mass-to-light ratio suggested by stellar population studies. We find that M87 is strongly triaxial, with ratios of
p = 0.845 for the middle-to-long principal axes and q = 0.722 for the short-to-long principal axes, and determine
the black hole mass to be ( - ´) 5.37 0.22 10 +
0.25
0.37 9M , where the second error indicates the systematic uncertainty
associated with the distance to M87.
Measuring the Hubble constant with kilonovae using the expanding photosphere ...Sérgio Sacani
While gravitational wave (GW) standard sirens from neutron star (NS) mergers have been proposed to offer good measurements of
the Hubble constant, we show in this paper how a variation of the expanding photosphere method (EPM) or spectral-fitting expanding
atmosphere method, applied to the kilonovae (KNe) associated with the mergers, can provide an independent distance measurement
to individual mergers that is potentially accurate to within a few percent. There are four reasons why the KN-EPM overcomes the
major uncertainties commonly associated with this method in supernovae: (1) the early continuum is very well-reproduced by a
blackbody spectrum, (2) the dilution effect from electron scattering opacity is likely negligible, (3) the explosion times are exactly
known due to the GW detection, and (4) the ejecta geometry is, at least in some cases, highly spherical and can be constrained from
line-shape analysis. We provide an analysis of the early VLT/X-shooter spectra AT2017gfo showing how the luminosity distance can
be determined, and find a luminosity distance of DL = 44.5 ± 0.8 Mpc in agreement with, but more precise than, previous methods.
We investigate the dominant systematic uncertainties, but our simple framework, which assumes a blackbody photosphere, does not
account for the full time-dependent three-dimensional radiative transfer effects, so this distance should be treated as preliminary. The
luminosity distance corresponds to an estimated Hubble constant of H0 = 67.0 ± 3.6 km s−1 Mpc−1
, where the dominant uncertainty
is due to the modelling of the host peculiar velocity. We also estimate the expected constraints on H0 from future KN-EPM-analysis
with the upcoming O4 and O5 runs of the LIGO collaboration GW-detectors, where five to ten similar KNe would yield 1% precision
cosmological constraints.
Lunar Surface Model Age Derivation: Comparisons Between Automatic and Human C...Sérgio Sacani
Dating young lunar surfaces, such as impact ejecta blankets and terrains associated with recent
volcanic activities, provides critical information on the recent events that shaped the surface of the Moon.
Model age derivation of young or small areas using a crater chronology is typically achieved through manual
counting, which requires a lot of small impact craters to be tediously mapped. In this study, we present the
use of a Crater Detection Algorithm (CDA) to extract crater populations on Lunar Reconnaissance Orbiter—
Narrow Angle Camera (LRO-NAC) and Kaguya Terrain Camera images. We applied our algorithm to images
covering the ejecta blankets of four Copernican impact craters and across four young mare terrains, where
manually derived model ages were already published. Across the eight areas, 10 model ages were derived. We
assessed the reproducibility of our model using two populations for each site: (a) an unprocessed population and
(b) a population adjusted to remove contaminations of secondary and buried craters. The results showed that
unprocessed detections led to overestimating crater densities by 12%–48%, but “adjusted” populations produced
consistent results within <20% of published values in 80% of cases. Regarding the discrepancies observed, we
found no significant error in our detections that could explain the differences with crater densities manually
measured. With careful processing, we conclude that a CDA can be used to determine model ages and crater
densities for the Moon. We also emphasize that automated crater datasets need to be processed, interpreted and
used carefully, in unity with geologic reasoning. The presented approach can offer a consistent and reproducible
way to derive model ages.
Mapping the Skies of Ultracool Worlds: Detecting Storms and Spots with Extrem...Sérgio Sacani
Extremely large telescopes (ELTs) present an unparalleled opportunity to study the magnetism,
atmospheric dynamics, and chemistry of very low mass stars (VLMs), brown dwarfs, and exoplanets.
Instruments such as the Giant Magellan Telescope - Consortium Large Earth Finder (GMT/GCLEF),
the Thirty Meter Telescope’s Multi-Objective Diffraction-limited High-Resolution Infrared Spectrograph
(TMT/MODHIS), and the European Southern Observatory’s Mid-Infrared ELT Imager and Spectrograph (ELT/METIS) provide the spectral resolution and signal-to-noise (S/N) necessary to Doppler
image ultracool targets’surfaces based on temporal spectral variations due to surface inhomogeneities.
Using our publicly-available code, Imber, developed and validated in Plummer & Wang (2022), we
evaluate these instruments’abilities to discern magnetic star spots and cloud systems on a VLM star
(TRAPPIST-1); two L/T transition ultracool dwarfs (VHS J1256−1257 b and SIMP J0136+0933); and
three exoplanets (Beta Pic b and HR 8799 d and e). We find that TMT/MODHIS and ELT/METIS are
suitable for Doppler imaging the ultracool dwarfs and Beta Pic b over a single rotation. Uncertainties
for longitude and radius are typically . 10◦
, and latitude uncertainties range from ∼ 10◦
to 30◦
.
TRAPPIST-1’s edge-on inclination and low υ sin i provide a challenge for all three instruments while
GMT/GCLEF and the HR 8799 planets may require observations over multiple rotations. We compare
the spectroscopic technique, photometry-only inference, and the combination of the two. We find
combining spectroscopic and photometric observations can lead to improved Bayesian inference of
surface inhomogeneities and offers insight into whether ultracool atmospheres are dominated by spotted
or banded features.
The Possible Tidal Demise of Kepler’s First Planetary SystemSérgio Sacani
We present evidence of tidally-driven inspiral in the Kepler-1658 (KOI-4) system, which consists of a giant planet
(1.1RJ, 5.9MJ) orbiting an evolved host star (2.9Re, 1.5Me). Using transit timing measurements from Kepler,
Palomar/WIRC, and TESS, we show that the orbital period of Kepler-1658b appears to be decreasing at a rate = -
+ P 131 22
20 ms yr−1
, corresponding to an infall timescale P P » 2.5 Myr. We consider other explanations for the
data including line-of-sight acceleration and orbital precession, but find them to be implausible. The observed
period derivative implies a tidal quality factor
¢ = ´ -
+ Q 2.50 10 0.62
0.85 4, in good agreement with theoretical
predictions for inertial wave dissipation in subgiant stars. Additionally, while it probably cannot explain the entire
inspiral rate, a small amount of planetary dissipation could naturally explain the deep optical eclipse observed for
the planet via enhanced thermal emission. As the first evolved system with detected inspiral, Kepler-1658 is a new
benchmark for understanding tidal physics at the end of the planetary life cycle
Hubble Asteroid Hunter III. Physical properties of newly found asteroidsSérgio Sacani
Context. Determining the size distribution of asteroids is key to understanding the collisional history and evolution of the inner Solar System. Aims. We aim to improve our knowledge of the size distribution of small asteroids in the main belt by determining the parallaxes of newly detected asteroids in the Hubble Space Telescope (HST) archive and subsequently their absolute magnitudes and sizes. Methods. Asteroids appear as curved trails in HST images because of the parallax induced by the fast orbital motion of the spacecraft. Taking into account the trajectory of this latter, the parallax effect can be computed to obtain the distance to the asteroids by fitting simulated trajectories to the observed trails. Using distance, we can obtain the absolute magnitude of an object and an estimation of its size assuming an albedo value, along with some boundaries for its orbital parameters. Results. In this work, we analyse a set of 632 serendipitously imaged asteroids found in the ESA HST archive. Images were captured with the ACS/WFC and WFC3/UVIS instruments. A machine learning algorithm (trained with the results of a citizen science project) was used to detect objects in these images as part of a previous study. Our raw data consist of 1031 asteroid trails from unknown objects, not matching any entries in the Minor Planet Center (MPC) database using their coordinates and imaging time. We also found 670 trails from known objects (objects featuring matching entries in the MPC). After an accuracy assessment and filtering process, our analysed HST asteroid set consists of 454 unknown objects and 178 known objects. We obtain a sample dominated by potential main belt objects featuring absolute magnitudes (H) mostly between 15 and 22 mag. The absolute magnitude cumulative distribution logN(H > H0) ∝ αlog(H0) confirms the previously reported slope change for 15 < H < 18, from α ≈ 0.56 to α ≈ 0.26, maintained in our case down to absolute magnitudes of around H ≈ 20, and therefore expanding the previous result by approximately two magnitudes. Conclusions. HST archival observations can be used as an asteroid survey because the telescope pointings are statistically randomly oriented in the sky and cover long periods of time. They allow us to expand the current best samples of astronomical objects at no extra cost in regard to telescope time.
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.
Titan’s Topography and Shape at the Endof the Cassini MissionSérgio Sacani
With the conclusion of the Cassini mission, we present an updated topographic map of Titan,including all the available altimetry, SARtopo, and stereophotogrammetry topographic data sets availablefrom the mission. We use radial basis func tions to interpolate the sparse data set, which covers only ∼9%of Titan’s global area. The most notable updates to the topography include higher coverage of the polesof Titan, improved fits to the global shape, and a finer resolution of the global interpolation. We alsopresent a statistical analysis of the error in the derived products and perform a global minimization on aprofile-by-profile basis to account for observed biases in the input data set. We find a greater flattening ofTitan than measured, additional topographic rises in Titan’s southern hemisphere and better constrain thepossible locations of past and present liquids on Titan’s surface.
The build up_of_the_c_d_halo_of_m87_evidence_for_accretion_in_the_last_gyrSérgio Sacani
Observações recentes obtidas com o Very Large Telescope do ESO mostraram que Messier 87, a galáxia elíptica gigante mais próximo de nós, engoliu uma galáxia inteira de tamanho médio no último bilhão de anos. Uma equipe de astrônomos conseguiu pela primeira vez seguir o movimento de 300 nebulosas planetárias brilhantes, encontrando evidências claras deste evento e encontrando também excesso de radiação emitida pelos restos da vítima completamente desfeita.
Direct Measure of Radiative And Dynamical Properties Of An Exoplanet AtmosphereSérgio Sacani
Two decades after the discovery of 51Pegb, the formation processes and atmospheres of short-period gas giants
remain poorly understood. Observations of eccentric systems provide key insights on those topics as they can
illuminate how a planet’s atmosphere responds to changes in incident flux. We report here the analysis of multi-day
multi-channel photometry of the eccentric (e ~ 0.93) hot Jupiter HD80606b obtained with the Spitzer Space
Telescope. The planet’s extreme eccentricity combined with the long coverage and exquisite precision of new
periastron-passage observations allow us to break the degeneracy between the radiative and dynamical timescales
of HD80606b’s atmosphere and constrain its global thermal response. Our analysis reveals that the atmospheric
layers probed heat rapidly (∼4 hr radiative timescale) from<500 to 1400 K as they absorb ~20% of the incoming
stellar flux during the periastron passage, while the planet’s rotation period is 93 35
85
-
+ hr, which exceeds the predicted
pseudo-synchronous period (40 hr).
Key words: methods: numerical – planet–star interactions – planets and satellites: atmospheres – planets and
satellites: dynamical evolution and stability – planets and satellites: individual (HD 80606 b) – techniques:
photometric
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.
More Related Content
Similar to Locating Hidden Exoplanets in ALMA Data Using Machine Learning
Detection of an atmosphere around the super earth 55 cancri eSérgio Sacani
We report the analysis of two new spectroscopic observations of the super-Earth 55 Cancri e, in the near
infrared, obtained with the WFC3 camera onboard the HST. 55 Cancri e orbits so close to its parent
star, that temperatures much higher than 2000 K are expected on its surface. Given the brightness
of 55 Cancri, the observations were obtained in scanning mode, adopting a very long scanning length
and a very high scanning speed. We use our specialized pipeline to take into account systematics
introduced by these observational parameters when coupled with the geometrical distortions of the
instrument. We measure the transit depth per wavelength channel with an average relative uncertainty
of 22 ppm per visit and nd modulations that depart from a straight line model with a 6 condence
level. These results suggest that 55 Cancri e is surrounded by an atmosphere, which is probably
hydrogen-rich. Our fully Bayesian spectral retrieval code, T -REx, has identied HCN to be the
most likely molecular candidate able to explain the features at 1.42 and 1.54 m. While additional
spectroscopic observations in a broader wavelength range in the infrared will be needed to conrm
the HCN detection, we discuss here the implications of such result. Our chemical model, developed
with combustion specialists, indicates that relatively high mixing ratios of HCN may be caused by a
high C/O ratio. This result suggests this super-Earth is a carbon-rich environment even more exotic
than previously thought.
Discovery of rotational modulations in the planetary mass companion 2m1207b i...Sérgio Sacani
Rotational modulations of brown dwarfs have recently provided powerful constraints on the properties
of ultra-cool atmospheres, including longitudinal and vertical cloud structures and cloud evolution.
Furthermore, periodic light curves directly probe the rotational periods of ultra-cool objects. We
present here, for the first time, time-resolved high-precision photometric measurements of a planetarymass
companion, 2M1207b. We observed the binary system with HST/WFC3 in two bands and with
two spacecraft roll angles. Using point spread function-based photometry, we reach a nearly photonnoise
limited accuracy for both the primary and the secondary. While the primary is consistent with
a flat light curve, the secondary shows modulations that are clearly detected in the combined light
curve as well as in di↵erent subsets of the data. The amplitudes are 1.36% in the F125W and 0.78%
in the F160W filters, respectively. By fitting sine waves to the light curves, we find a consistent period
of 10.7+1.2
−0.6 hours and similar phases in both bands. The J- and H-band amplitude ratio of 2M1207b
is very similar to a field brown dwarf that has identical spectral type but di↵erent J-H color. Importantly,
our study also measures, for the first time, the rotation period for a directly imaged extra-solar
planetary-mass companion.
A High-mass, Young Star-forming Core Escaping from Its Parental FilamentSérgio Sacani
We studied the unique kinematic properties in massive filament G352.63-1.07 at 103 au spatial scale with the dense
molecular tracers observed with the Atacama Large Millimeter/submillimeter Array. We find the central massive
core M1 (12 Me) being separated from the surrounding filament with a velocity difference of
- =- - v vsys 2 km s 1 and a transverse separation within 3″. Meanwhile, as shown in multiple dense-gas
tracers, M1 has a spatial extension closely aligned with the main filament and is connected to the filament toward
both its ends. M1 thus represents a very beginning state for a massive, young star-forming core escaping from the
parental filament, within a timescale of ∼4000 yr. Based on its kinetic energy (3.5 × 1044 erg), the core escape is
unlikely solely due to the original filament motion or magnetic field but requires more energetic events such as a
rapid intense anisotropic collapse. The released energy also seems to noticeably increase the environmental
turbulence. This may help the filament to become stabilized again.
Keck Integral-field Spectroscopy of M87 Reveals an Intrinsically Triaxial Gal...Sérgio Sacani
The three-dimensional intrinsic shape of a galaxy and the mass of the central supermassive black hole provide key
insight into the galaxy’s growth history over cosmic time. Standard assumptions of a spherical or axisymmetric
shape can be simplistic and can bias the black hole mass inferred from the motions of stars within a galaxy. Here,
we present spatially resolved stellar kinematics of M87 over a two-dimensional 250″ × 300″ contiguous field
covering a radial range of 50 pc–12 kpc from integral-field spectroscopic observations at the Keck II Telescope.
From about 5 kpc and outward, we detect a prominent 25 km s−1 rotational pattern, in which the kinematic axis
(connecting the maximal receding and approaching velocities) is 40° misaligned with the photometric major axis of
M87. The rotational amplitude and misalignment angle both decrease in the inner 5 kpc. Such misaligned and
twisted velocity fields are a hallmark of triaxiality, indicating that M87 is not an axisymmetrically shaped galaxy.
Triaxial Schwarzschild orbit modeling with more than 4000 observational constraints enabled us to determine
simultaneously the shape and mass parameters. The models incorporate a radially declining profile for the stellar
mass-to-light ratio suggested by stellar population studies. We find that M87 is strongly triaxial, with ratios of
p = 0.845 for the middle-to-long principal axes and q = 0.722 for the short-to-long principal axes, and determine
the black hole mass to be ( - ´) 5.37 0.22 10 +
0.25
0.37 9M , where the second error indicates the systematic uncertainty
associated with the distance to M87.
Measuring the Hubble constant with kilonovae using the expanding photosphere ...Sérgio Sacani
While gravitational wave (GW) standard sirens from neutron star (NS) mergers have been proposed to offer good measurements of
the Hubble constant, we show in this paper how a variation of the expanding photosphere method (EPM) or spectral-fitting expanding
atmosphere method, applied to the kilonovae (KNe) associated with the mergers, can provide an independent distance measurement
to individual mergers that is potentially accurate to within a few percent. There are four reasons why the KN-EPM overcomes the
major uncertainties commonly associated with this method in supernovae: (1) the early continuum is very well-reproduced by a
blackbody spectrum, (2) the dilution effect from electron scattering opacity is likely negligible, (3) the explosion times are exactly
known due to the GW detection, and (4) the ejecta geometry is, at least in some cases, highly spherical and can be constrained from
line-shape analysis. We provide an analysis of the early VLT/X-shooter spectra AT2017gfo showing how the luminosity distance can
be determined, and find a luminosity distance of DL = 44.5 ± 0.8 Mpc in agreement with, but more precise than, previous methods.
We investigate the dominant systematic uncertainties, but our simple framework, which assumes a blackbody photosphere, does not
account for the full time-dependent three-dimensional radiative transfer effects, so this distance should be treated as preliminary. The
luminosity distance corresponds to an estimated Hubble constant of H0 = 67.0 ± 3.6 km s−1 Mpc−1
, where the dominant uncertainty
is due to the modelling of the host peculiar velocity. We also estimate the expected constraints on H0 from future KN-EPM-analysis
with the upcoming O4 and O5 runs of the LIGO collaboration GW-detectors, where five to ten similar KNe would yield 1% precision
cosmological constraints.
Lunar Surface Model Age Derivation: Comparisons Between Automatic and Human C...Sérgio Sacani
Dating young lunar surfaces, such as impact ejecta blankets and terrains associated with recent
volcanic activities, provides critical information on the recent events that shaped the surface of the Moon.
Model age derivation of young or small areas using a crater chronology is typically achieved through manual
counting, which requires a lot of small impact craters to be tediously mapped. In this study, we present the
use of a Crater Detection Algorithm (CDA) to extract crater populations on Lunar Reconnaissance Orbiter—
Narrow Angle Camera (LRO-NAC) and Kaguya Terrain Camera images. We applied our algorithm to images
covering the ejecta blankets of four Copernican impact craters and across four young mare terrains, where
manually derived model ages were already published. Across the eight areas, 10 model ages were derived. We
assessed the reproducibility of our model using two populations for each site: (a) an unprocessed population and
(b) a population adjusted to remove contaminations of secondary and buried craters. The results showed that
unprocessed detections led to overestimating crater densities by 12%–48%, but “adjusted” populations produced
consistent results within <20% of published values in 80% of cases. Regarding the discrepancies observed, we
found no significant error in our detections that could explain the differences with crater densities manually
measured. With careful processing, we conclude that a CDA can be used to determine model ages and crater
densities for the Moon. We also emphasize that automated crater datasets need to be processed, interpreted and
used carefully, in unity with geologic reasoning. The presented approach can offer a consistent and reproducible
way to derive model ages.
Mapping the Skies of Ultracool Worlds: Detecting Storms and Spots with Extrem...Sérgio Sacani
Extremely large telescopes (ELTs) present an unparalleled opportunity to study the magnetism,
atmospheric dynamics, and chemistry of very low mass stars (VLMs), brown dwarfs, and exoplanets.
Instruments such as the Giant Magellan Telescope - Consortium Large Earth Finder (GMT/GCLEF),
the Thirty Meter Telescope’s Multi-Objective Diffraction-limited High-Resolution Infrared Spectrograph
(TMT/MODHIS), and the European Southern Observatory’s Mid-Infrared ELT Imager and Spectrograph (ELT/METIS) provide the spectral resolution and signal-to-noise (S/N) necessary to Doppler
image ultracool targets’surfaces based on temporal spectral variations due to surface inhomogeneities.
Using our publicly-available code, Imber, developed and validated in Plummer & Wang (2022), we
evaluate these instruments’abilities to discern magnetic star spots and cloud systems on a VLM star
(TRAPPIST-1); two L/T transition ultracool dwarfs (VHS J1256−1257 b and SIMP J0136+0933); and
three exoplanets (Beta Pic b and HR 8799 d and e). We find that TMT/MODHIS and ELT/METIS are
suitable for Doppler imaging the ultracool dwarfs and Beta Pic b over a single rotation. Uncertainties
for longitude and radius are typically . 10◦
, and latitude uncertainties range from ∼ 10◦
to 30◦
.
TRAPPIST-1’s edge-on inclination and low υ sin i provide a challenge for all three instruments while
GMT/GCLEF and the HR 8799 planets may require observations over multiple rotations. We compare
the spectroscopic technique, photometry-only inference, and the combination of the two. We find
combining spectroscopic and photometric observations can lead to improved Bayesian inference of
surface inhomogeneities and offers insight into whether ultracool atmospheres are dominated by spotted
or banded features.
The Possible Tidal Demise of Kepler’s First Planetary SystemSérgio Sacani
We present evidence of tidally-driven inspiral in the Kepler-1658 (KOI-4) system, which consists of a giant planet
(1.1RJ, 5.9MJ) orbiting an evolved host star (2.9Re, 1.5Me). Using transit timing measurements from Kepler,
Palomar/WIRC, and TESS, we show that the orbital period of Kepler-1658b appears to be decreasing at a rate = -
+ P 131 22
20 ms yr−1
, corresponding to an infall timescale P P » 2.5 Myr. We consider other explanations for the
data including line-of-sight acceleration and orbital precession, but find them to be implausible. The observed
period derivative implies a tidal quality factor
¢ = ´ -
+ Q 2.50 10 0.62
0.85 4, in good agreement with theoretical
predictions for inertial wave dissipation in subgiant stars. Additionally, while it probably cannot explain the entire
inspiral rate, a small amount of planetary dissipation could naturally explain the deep optical eclipse observed for
the planet via enhanced thermal emission. As the first evolved system with detected inspiral, Kepler-1658 is a new
benchmark for understanding tidal physics at the end of the planetary life cycle
Hubble Asteroid Hunter III. Physical properties of newly found asteroidsSérgio Sacani
Context. Determining the size distribution of asteroids is key to understanding the collisional history and evolution of the inner Solar System. Aims. We aim to improve our knowledge of the size distribution of small asteroids in the main belt by determining the parallaxes of newly detected asteroids in the Hubble Space Telescope (HST) archive and subsequently their absolute magnitudes and sizes. Methods. Asteroids appear as curved trails in HST images because of the parallax induced by the fast orbital motion of the spacecraft. Taking into account the trajectory of this latter, the parallax effect can be computed to obtain the distance to the asteroids by fitting simulated trajectories to the observed trails. Using distance, we can obtain the absolute magnitude of an object and an estimation of its size assuming an albedo value, along with some boundaries for its orbital parameters. Results. In this work, we analyse a set of 632 serendipitously imaged asteroids found in the ESA HST archive. Images were captured with the ACS/WFC and WFC3/UVIS instruments. A machine learning algorithm (trained with the results of a citizen science project) was used to detect objects in these images as part of a previous study. Our raw data consist of 1031 asteroid trails from unknown objects, not matching any entries in the Minor Planet Center (MPC) database using their coordinates and imaging time. We also found 670 trails from known objects (objects featuring matching entries in the MPC). After an accuracy assessment and filtering process, our analysed HST asteroid set consists of 454 unknown objects and 178 known objects. We obtain a sample dominated by potential main belt objects featuring absolute magnitudes (H) mostly between 15 and 22 mag. The absolute magnitude cumulative distribution logN(H > H0) ∝ αlog(H0) confirms the previously reported slope change for 15 < H < 18, from α ≈ 0.56 to α ≈ 0.26, maintained in our case down to absolute magnitudes of around H ≈ 20, and therefore expanding the previous result by approximately two magnitudes. Conclusions. HST archival observations can be used as an asteroid survey because the telescope pointings are statistically randomly oriented in the sky and cover long periods of time. They allow us to expand the current best samples of astronomical objects at no extra cost in regard to telescope time.
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.
Titan’s Topography and Shape at the Endof the Cassini MissionSérgio Sacani
With the conclusion of the Cassini mission, we present an updated topographic map of Titan,including all the available altimetry, SARtopo, and stereophotogrammetry topographic data sets availablefrom the mission. We use radial basis func tions to interpolate the sparse data set, which covers only ∼9%of Titan’s global area. The most notable updates to the topography include higher coverage of the polesof Titan, improved fits to the global shape, and a finer resolution of the global interpolation. We alsopresent a statistical analysis of the error in the derived products and perform a global minimization on aprofile-by-profile basis to account for observed biases in the input data set. We find a greater flattening ofTitan than measured, additional topographic rises in Titan’s southern hemisphere and better constrain thepossible locations of past and present liquids on Titan’s surface.
The build up_of_the_c_d_halo_of_m87_evidence_for_accretion_in_the_last_gyrSérgio Sacani
Observações recentes obtidas com o Very Large Telescope do ESO mostraram que Messier 87, a galáxia elíptica gigante mais próximo de nós, engoliu uma galáxia inteira de tamanho médio no último bilhão de anos. Uma equipe de astrônomos conseguiu pela primeira vez seguir o movimento de 300 nebulosas planetárias brilhantes, encontrando evidências claras deste evento e encontrando também excesso de radiação emitida pelos restos da vítima completamente desfeita.
Direct Measure of Radiative And Dynamical Properties Of An Exoplanet AtmosphereSérgio Sacani
Two decades after the discovery of 51Pegb, the formation processes and atmospheres of short-period gas giants
remain poorly understood. Observations of eccentric systems provide key insights on those topics as they can
illuminate how a planet’s atmosphere responds to changes in incident flux. We report here the analysis of multi-day
multi-channel photometry of the eccentric (e ~ 0.93) hot Jupiter HD80606b obtained with the Spitzer Space
Telescope. The planet’s extreme eccentricity combined with the long coverage and exquisite precision of new
periastron-passage observations allow us to break the degeneracy between the radiative and dynamical timescales
of HD80606b’s atmosphere and constrain its global thermal response. Our analysis reveals that the atmospheric
layers probed heat rapidly (∼4 hr radiative timescale) from<500 to 1400 K as they absorb ~20% of the incoming
stellar flux during the periastron passage, while the planet’s rotation period is 93 35
85
-
+ hr, which exceeds the predicted
pseudo-synchronous period (40 hr).
Key words: methods: numerical – planet–star interactions – planets and satellites: atmospheres – planets and
satellites: dynamical evolution and stability – planets and satellites: individual (HD 80606 b) – techniques:
photometric
Similar to Locating Hidden Exoplanets in ALMA Data Using Machine Learning (20)
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.
Efficient spin-up of Earth System Models usingsequence accelerationSérgio Sacani
Marine and terrestrial biogeochemical models are key components of the Earth System Models (ESMs) used toproject future environmental changes. However, their slow adjustment time also hinders effective use of ESMsbecause of the enormous computational resources required to integrate them to a pre-industrial equilibrium. Here,a solution to this "spin-up" problem based on "sequence acceleration", is shown to accelerate equilibration of state-of-the-art marine biogeochemical models by over an order of magnitude. The technique can be applied in a "blackbox" fashion to existing models. Even under the challenging spin-up protocols used for Intergovernmental Panelon Climate Change (IPCC) simulations, this algorithm is 5 times faster. Preliminary results suggest that terrestrialmodels can be similarly accelerated, enabling a quantification of major parametric uncertainties in ESMs, improvedestimates of metrics such as climate sensitivity, and higher model resolution than currently feasible.
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/
Cancer cell metabolism: special Reference to Lactate PathwayAADYARAJPANDEY1
Normal Cell Metabolism:
Cellular respiration describes the series of steps that cells use to break down sugar and other chemicals to get the energy we need to function.
Energy is stored in the bonds of glucose and when glucose is broken down, much of that energy is released.
Cell utilize energy in the form of ATP.
The first step of respiration is called glycolysis. In a series of steps, glycolysis breaks glucose into two smaller molecules - a chemical called pyruvate. A small amount of ATP is formed during this process.
Most healthy cells continue the breakdown in a second process, called the Kreb's cycle. The Kreb's cycle allows cells to “burn” the pyruvates made in glycolysis to get more ATP.
The last step in the breakdown of glucose is called oxidative phosphorylation (Ox-Phos).
It takes place in specialized cell structures called mitochondria. This process produces a large amount of ATP. Importantly, cells need oxygen to complete oxidative phosphorylation.
If a cell completes only glycolysis, only 2 molecules of ATP are made per glucose. However, if the cell completes the entire respiration process (glycolysis - Kreb's - oxidative phosphorylation), about 36 molecules of ATP are created, giving it much more energy to use.
IN CANCER CELL:
Unlike healthy cells that "burn" the entire molecule of sugar to capture a large amount of energy as ATP, cancer cells are wasteful.
Cancer cells only partially break down sugar molecules. They overuse the first step of respiration, glycolysis. They frequently do not complete the second step, oxidative phosphorylation.
This results in only 2 molecules of ATP per each glucose molecule instead of the 36 or so ATPs healthy cells gain. As a result, cancer cells need to use a lot more sugar molecules to get enough energy to survive.
Unlike healthy cells that "burn" the entire molecule of sugar to capture a large amount of energy as ATP, cancer cells are wasteful.
Cancer cells only partially break down sugar molecules. They overuse the first step of respiration, glycolysis. They frequently do not complete the second step, oxidative phosphorylation.
This results in only 2 molecules of ATP per each glucose molecule instead of the 36 or so ATPs healthy cells gain. As a result, cancer cells need to use a lot more sugar molecules to get enough energy to survive.
introduction to WARBERG PHENOMENA:
WARBURG EFFECT Usually, cancer cells are highly glycolytic (glucose addiction) and take up more glucose than do normal cells from outside.
Otto Heinrich Warburg (; 8 October 1883 – 1 August 1970) In 1931 was awarded the Nobel Prize in Physiology for his "discovery of the nature and mode of action of the respiratory enzyme.
WARNBURG EFFECT : cancer cells under aerobic (well-oxygenated) conditions to metabolize glucose to lactate (aerobic glycolysis) is known as the Warburg effect. Warburg made the observation that tumor slices consume glucose and secrete lactate at a higher rate than normal tissues.
This presentation explores a brief idea about the structural and functional attributes of nucleotides, the structure and function of genetic materials along with the impact of UV rays and pH upon them.
A brief information about the SCOP protein database used in bioinformatics.
The Structural Classification of Proteins (SCOP) database is a comprehensive and authoritative resource for the structural and evolutionary relationships of proteins. It provides a detailed and curated classification of protein structures, grouping them into families, superfamilies, and folds based on their structural and sequence similarities.
What is greenhouse gasses and how many gasses are there to affect the Earth.moosaasad1975
What are greenhouse gasses how they affect the earth and its environment what is the future of the environment and earth how the weather and the climate effects.
Introduction:
RNA interference (RNAi) or Post-Transcriptional Gene Silencing (PTGS) is an important biological process for modulating eukaryotic gene expression.
It is highly conserved process of posttranscriptional gene silencing by which double stranded RNA (dsRNA) causes sequence-specific degradation of mRNA sequences.
dsRNA-induced gene silencing (RNAi) is reported in a wide range of eukaryotes ranging from worms, insects, mammals and plants.
This process mediates resistance to both endogenous parasitic and exogenous pathogenic nucleic acids, and regulates the expression of protein-coding genes.
What are small ncRNAs?
micro RNA (miRNA)
short interfering RNA (siRNA)
Properties of small non-coding RNA:
Involved in silencing mRNA transcripts.
Called “small” because they are usually only about 21-24 nucleotides long.
Synthesized by first cutting up longer precursor sequences (like the 61nt one that Lee discovered).
Silence an mRNA by base pairing with some sequence on the mRNA.
Discovery of siRNA?
The first small RNA:
In 1993 Rosalind Lee (Victor Ambros lab) was studying a non- coding gene in C. elegans, lin-4, that was involved in silencing of another gene, lin-14, at the appropriate time in the
development of the worm C. elegans.
Two small transcripts of lin-4 (22nt and 61nt) were found to be complementary to a sequence in the 3' UTR of lin-14.
Because lin-4 encoded no protein, she deduced that it must be these transcripts that are causing the silencing by RNA-RNA interactions.
Types of RNAi ( non coding RNA)
MiRNA
Length (23-25 nt)
Trans acting
Binds with target MRNA in mismatch
Translation inhibition
Si RNA
Length 21 nt.
Cis acting
Bind with target Mrna in perfect complementary sequence
Piwi-RNA
Length ; 25 to 36 nt.
Expressed in Germ Cells
Regulates trnasposomes activity
MECHANISM OF RNAI:
First the double-stranded RNA teams up with a protein complex named Dicer, which cuts the long RNA into short pieces.
Then another protein complex called RISC (RNA-induced silencing complex) discards one of the two RNA strands.
The RISC-docked, single-stranded RNA then pairs with the homologous mRNA and destroys it.
THE RISC COMPLEX:
RISC is large(>500kD) RNA multi- protein Binding complex which triggers MRNA degradation in response to MRNA
Unwinding of double stranded Si RNA by ATP independent Helicase
Active component of RISC is Ago proteins( ENDONUCLEASE) which cleave target MRNA.
DICER: endonuclease (RNase Family III)
Argonaute: Central Component of the RNA-Induced Silencing Complex (RISC)
One strand of the dsRNA produced by Dicer is retained in the RISC complex in association with Argonaute
ARGONAUTE PROTEIN :
1.PAZ(PIWI/Argonaute/ Zwille)- Recognition of target MRNA
2.PIWI (p-element induced wimpy Testis)- breaks Phosphodiester bond of mRNA.)RNAse H activity.
MiRNA:
The Double-stranded RNAs are naturally produced in eukaryotic cells during development, and they have a key role in regulating gene expression .
Professional air quality monitoring systems provide immediate, on-site data for analysis, compliance, and decision-making.
Monitor common gases, weather parameters, particulates.
This pdf is about the Schizophrenia.
For more details visit on YouTube; @SELF-EXPLANATORY;
https://www.youtube.com/channel/UCAiarMZDNhe1A3Rnpr_WkzA/videos
Thanks...!
2. have no planets in them to address any class imbalance (i.e.,
not having an equal number of “at least one planet” class and
“no planet” class simulations) while ensuring diversity in the
number of planets. After sampling the stellar mass for use in
the simulation, stellar temperatures and radii, both of which are
used in the radiative transfer calculations, are determined using
isochrones calculated by Siess et al. (2000).
2.1. Hydrodynamical Simulations
We run 1000 3D smoothed particle hydrodynamics (SPH)
simulations using the PHANTOM (Price et al. 2018) code.
System properties, such as stellar mass, disk properties,
observational resolution, etc., were LHC-sampled from
Table 1. A significant percentage (25%) of these simulations
were withheld for testing. Each simulation uses 106
SPH particles and evolves for 100 orbits. A given planet’s
accretion radius is set to one-fourth of its Hill radius. The
surface density profile is set to Σ ∝ R− p
, and the sound speed is
set to cs ∝ R− q
.
2.2. Velocity Channel Maps
The simulation results are used to create velocity channel
maps in only 13
CO to keep the size of the parameter space
manageable, although 12
CO and C18
O are also reasonable
choices. The channel maps are created using the MCFOST
radiative transfer code (Pinte et al. 2006, 2009). For each
simulation, multiple points between 10 and 100 orbits are
chosen randomly. Since one-third of the simulations have no
planets, six snapshots are chosen from each of those
simulations while only two snapshots are chosen for simula-
tions with planets. This eliminates the class imbalance. From
each snapshot, a velocity channel cube is made using either the
13
CO J 2 → 1 (220.4 GHz) or 3 → 2 (330.6 GHz) transition,
which is randomly sampled. These transitions are used because
they were also used to identify the planets in HD 163296 and
HD 97048 (Pinte et al. 2018, 2019). The final result is a
velocity cube, where each velocity channel is an image with
600 × 600 pixels at a resolution of 1 au pixel−1
. This velocity
cube is used as the model input. Channel maps are calculated
using 108
photon packets. The dust-to-gas ratio is 1:100, and
dust is composed of carbon and silicates (Draine & Lee 1984).
Stellar radii and temperatures are calculated with isochrones
given by Siess et al. (2000) using the LHC-sampled masses and
ages. A spherical beam is used.
2.3. Simulated Observations
The velocity channel maps are convolved spatially and
spectrally, and noise is added by LHC sampling from Table 1.
rms noise is added independently for each pixel, which more
faithfully replicates observational effects such as hot pixels.
This method results in an average rms of ∼10% for each image.
Except for the specific values, this process largely follows
that done in Terry et al. (2022). Figures 1 and 2 show the
results of convolving selected velocity channels for a disk with
and without a planet, respectively. Figure 1 shows that, while
the perturbation is strongest in the velocity channel that covers
the planet (rightmost column), the perturbation is not
necessarily completely localized and can be visible in distant
regions of the disk. This is an expected behavior. The deviation
is strongest at the location of the planet, but the spiral wake
leaves further imprints as it disperses throughout the disk.
By itself, a single velocity channel is poorly suited for our
method. Only a few channels display kinks, and channels with
kinks can neighbor the exact channel containing the planet. We
therefore stack all C velocity channels into a single image of
dimension (H × W × C), where H and W are the height and
width of the image (600 × 600 pixels for these purposes).
The number of velocity channels in an observation varies but
mostly falls in the range ∼40–80 channels that cover the disk
(Andrews et al. 2018; Öberg et al. 2021). We therefore use
C = 47, 61, and 75 channels for each observation. The number
of channels must be odd to cover the disk symmetrically and
still retain the systemic (Δv = 0) channel. The input velocity of
the simulated channels ranges from |Δv| = |vsystemic − v| „ 2.5
km s−1
to fully cover the disk.
2.4. Machine-learning Models
The input for all models is a (600 × 600 × C) image, and
their output is a two-component vector with softmax activation
(Goodfellow et al. 2016). The softmax function maps the
output vector such that the sum of the components equals one.
Each component can be interpreted as the predicted probability
Table 1
Simulation Parameter Ranges for the LHC Sampling and the Stage at Which They Were Applied
Parameter Variable Minimum Value Maximum Value Use
Number of planets N 0 4 PHANTOM, MCFOST
Disk Inner Radius (au) Rout 150 250 PHANTOM, MCFOST
Disk Outer Radius Rin 0.1Rout 0.1Rout PHANTOM, MCFOST
Planetary Mass (M⊕) Mplanet 5 120 PHANTOM, MCFOST
Stellar Mass (Me) Må 0.5 2.0 PHANTOM, MCFOST
Planet Semimajor Axis (au) a Rin + 0.2Rout Rin + 0.8Rout PHANTOM
Mass Ratio Mdisk / Må 5 × 10−4
10−2
PHANTOM
Disk Viscosity αSS 5 × 10−4
2.5 × 10−3
PHANTOM
Surface Density Profile (Σ = Σ0R− p
) p 0.1 1.0 PHANTOM
Sound Speed Profile (cs = cs,0R− q
) q 0.1 0.75 PHANTOM
Stellar Age (Myr) t 0.5 5.0 MCFOST
Inclination (degrees) i 10 80 MCFOST
Azimuth (degrees) f 0 360 MCFOST
Distance (pc) d 100 200 MCFOST
Spectral Resolution (km s−1
) δv 0.01 0.1 Synthetic Observations
Spatial Resolution (arcseconds) ″ 0.025 0.25 Synthetic Observations
rms Noise (%) δ 0.05 20 Synthetic Observations
2
The Astrophysical Journal, 941:192 (10pp), 2022 December 20 Terry et al.
3. that the input belongs to the corresponding class (i.e., “contains
at least one planet” class or “does not contain a planet” class).
An Adam optimizer (Kingma & Ba 2014) is used to add
momentum, which remembers previous gradients, and gradient
scaling to a simple gradient descent algorithm. This helps
escape local minima and improves the speed and range of
convergence. The cross-entropy loss (Hinton et al. 1995)
penalizes confident predictions that are incorrect. Training
stops when there is no improvement in the validation loss after
eight complete epochs, i.e., eight sweeps through the
training data.
Multiple architectures are used to compare performance on
two tasks: predicting if the system hosts at least one planet and
determining its azimuthal location.
Figure 1. Example raw (top row) and convolved, noisy (bottom row) channel maps in a disk with a planet present. The planet (circled in white) is visible as a kink in
the right column. The opposite velocity channel is shown in the left column, and the systemic channel is shown in the middle column. The beam size is indicated in the
bottom middle image (solid white circle). This disk is one of the smallest and farthest simulated and is observed with some of the worst spatial resolutions, which is
why the beam is so large.
Figure 2. Example raw (top row) and convolved, noisy (bottom row) channel maps in a disk without a planet present. The beam size is indicated in the bottom middle
image.
3
The Astrophysical Journal, 941:192 (10pp), 2022 December 20 Terry et al.
4. We use two different models based on PyTorch (Paszke et al.
2019) implementations: EfficientNetV2 (Tan & Le 2021) and
RegNet (Xu et al. 2022). Neither model uses the default
hyperparameters or pretrained weights.
EfficientNetV2 is an updated version of EfficientNet (Tan &
Le 2019) that maximizes performance and minimizes the
number of trainable parameters and training time. RegNet, on
the other hand, seeks to maximize performance by adding
variants of convolutional recurrent neural networks to ResNet
(He et al. 2016). This can extract greater spatial information at
the cost of significantly more trainable parameters.
We perform Bayesian hyperparameter tuning using WANDB
(Biewald 2020) to find separate sets of hyperparameters that
minimize the validation loss for C = 47, 61, and 75. The
default parameters for these sweeps are based on default
versions “EfficientNetV2 S” and “RegNetY 16GF.”
Each architecture is evaluated for accuracy and area under
the receiver operating characteristic curve (AUC; Hanley &
McNeil 1982). Accuracy in this context is defined as whether a
model correctly predicted that a system with planet(s) has at
least one planet and similarly for systems with no planets. We
choose AUC because it gives a robust measure of the
performance of the model across different decision thresholds,
i.e., the softmax threshold required to claim the presence of a
planet. Substantial confidence is required to claim a planet
detection, but setting the decision threshold too high can lead to
false negatives. False positives may be more acceptable
because further analysis can overrule them, whereas a false
negative may lead to no further analysis and result in the planet
not being detected. The optimum threshold for this boundary is
open for discussion by the community. We show multiple
thresholds (50%, 75%, 90%, and 95%) in Figures 3 and 4 to
demonstrate how the threshold for claiming the presence of at
least one planet affects the results.
While some protoplanetary disks exhibit gaps in the
continuum that are highly suggestive of a planet, this does
not help one find the azimuthal location. Planet-induced non-
Keplerian kinks tend to be strongest near the planet, so our
model must determine if and where the kink is in our data in
order to give information on the azimuthal location.
One simple approach to this is to look at the activations
inside the model itself. The activation strengths highlight
regions that the model finds particularly informative for
classification. EfficientNetV2 uses SiLU activations (Elfwing
et al. 2018), and RegNet uses ReLU (Glorot et al. 2011). We
use mean-subtracted activations to achieve this. For a given
pixel with an activation value x, the mean-subtracted activation
¢
x is defined as ¢ = - á ñ
∣ ∣
x x x , where 〈x〉 is the mean activation
over the entire image. Activations occur most strongly at the
location of the strongest deviation from Keplerianity, i.e.,
the kink.
3. Results and Discussion
3.1. Machine-learning Models
We train six models in total: an EfficientNetV2 and a
RegNet, each for 47, 61, and 75 velocity channels. Using a
typical decision threshold of 0.5, each model, other than the 47-
channel RegNet, has an accuracy of at least 93%. When this
decision threshold is increased to 0.95, four models have an
accuracy of at least 92%. Five models have an AUC of at least
0.98. This confirms that our models have learned to correctly
detect the presence of planets using kinematic signatures.
Table 2 shows the number of parameters as well as relevant
performance measures for each final model. All EfficientNetV2
models converge to a similar number of trainable parameters,
whereas the number of parameters for the RegNets increases
sharply with the number of channels. RegNet is a larger and
more complicated architecture, so this is expected. The
performance of the RegNet models varies widely compared
to the EfficientNetV2 models. The accuracy of EfficientNetV2
models varies by at most 8%, whereas RegNet varies by as
much as 31%. By all performance metrics, while the average
EfficientNetV2 outperforms the average RegNet, the 61-
channel RegNet outperforms all other models.
Figure 3 shows the confusion matrix, which describes the
distribution of correct and incorrect predictions, for all models
applied to the withheld test set. Panel (a) shows the results
using a 50% decision threshold, i.e., a planet is predicted if the
confidence is over 50%. Panels (b), (c), and (d) show the same
for cutoffs of 75%, 90%, and 95%. Figure 4 gives several
relevant metrics for model performance and all ROC curves.
Claiming a planet is present should come with high confidence,
so a 50% decision threshold is not necessarily what should be
used in practice. It is encouraging that, for all other models than
the 47-channel RegNet, there are no qualitative changes in the
results when a higher decision threshold is used; the main effect
is simply increasing the number of false negatives and
decreasing the number of false positives.
If there are multiple planets in a disk, then multiple kinks
may be present. It is therefore prudent to check that the quality
of the predictions does not depend on the number of planets in
the disk. We check the possibility of this dependence by
calculating the accuracy for each model for disks with a given
number of planets. Figure 5 gives the results of these
calculations. The p-values from Pearson correlation tests
shown in Figure 6 demonstrate that only the 47-channel
RegNet using a decision threshold of 50% has a statistically
significant relationship between accuracy and the number of
planets (p < 0.05). While the 47-channel RegNet using a
decision threshold of 95% does not have a statistically
significant relationship, it is clear that the performance is
worse when there are planets, i.e., there are many false
negatives. This is in line with this model’s relatively low AUC
and Figure 3. The performance of all other models does not
differ significantly with the number of planets.
3.2. Simulation Activations
Many disks do not show obvious signs of planets, either in
continuum or line emission. Inspecting the activations of the
disks helps overcome this. Figure 7 shows the result from a
disk that is difficult to classify by eye. The models predict the
presence of an exoplanet with high confidence, activating on a
subset of channels that are deemed important by the model.
This gives information on the azimuthal location, and the radial
location may be inferred by either the location with the
strongest kink or coincident gaps in continuum images.
Panels (c) and (d) in Figure 7 show the raw and convolved
velocity channels, respectively. If one were simply inspecting
the velocity channels by eye, it would be trivially easy to miss
the kink even in the unconvolved data. The convolved, noisy
data show essentially no sign of the planets. Despite lacking
any clear signatures that can be observed visually, the models
4
The Astrophysical Journal, 941:192 (10pp), 2022 December 20 Terry et al.
5. Figure 3. Confusion matrix from withheld test set for all models. The x-axis is the percentage of disks in that class that were predicted accordingly. (a) Using a 50%
decision threshold. (b) Using a 75% decision threshold. (c) Using a 90% decision threshold. (d) Using a 95% decision threshold. The top left and bottom right blocks
of each panel show the counts of true negatives and true positives, respectively. The top right and bottom left blocks of a panel show the false positives and false
negatives, respectively. A perfectly accurate model will have no entries in the top right and bottom left.
Figure 4. Left: various metrics calculated from the withheld test set for all models. Right: corresponding receiver operating characteristic (ROC) curves. Error bars
show 95% confidence intervals that are calculated by bootstrapping each metric 1000 times using random selections of 80% of the test data. The percentages next to
the accuracy labels denote the decision threshold.
5
The Astrophysical Journal, 941:192 (10pp), 2022 December 20 Terry et al.
6. correctly classify the disks and locate the planets. This
demonstrates that our models are able to accurately find
planets that the by-eye method may fail to find.
Figure 8 shows a typical activation for a disk with no planet.
The entire disk is activated equally, indicating that there is no
localized region that exhibits behaviors indicative of a planet.
3.3. Application to Real Observations
Next, we demonstrate the effectiveness of our model by
applying it to real telescope observations. Kinematic detections
of planets have been demonstrated for many disks (Pinte et al.
2020), but here we focus on the HD 163296 and HD 97048
disks as a proof of concept (Pinte et al. 2018, 2019). Using the
same data as Pinte et al. (2018, 2019), we demonstrate that our
models replicate the prediction and estimated location of the
forming exoplanet. Figure 9(a) shows the HD 97048 in
continuum, and Figure 9(b) shows the velocity channel with
the planet’s signature circled.
Table 3 shows the softmax values for the observations. For
HD 97048, all RegNet models correctly predict a planet with
>95% confidence. Two EfficientNetV2 models correctly
predict a planet with 85% confidence. Figure 9 shows that
the velocity channels that contain the planet are strongly
activated. The activation in Figure 9(d) is strong on the planet
itself rather than simply the entire velocity channel.
The results for HD 163296 are not as confident, but the two
best-performing models predict the presence of at least one
planet with over 99% confidence.
Table 2
Final Model Descriptions and Metrics
Model Parameters Accuracy (50%) Accuracy (95%) AUC
(millions) (%) (%)
EfficientNetV2: 47 Channels 20.2 97 ± 0.5 96 ± 0.5 0.99 ± 0.002
EfficientNetV2: 61 Channels 20.2 97 ± 0.5 94 ± 0.7 0.99 ± 0.003
EfficientNetV2: 75 Channels 20.2 93 ± 0.7 88 ± 0.9 0.98 ± 0.003
RegNet: 47 Channels 51.0 78 ± 1.1 65 ± 1.3 0.86 ± 0.010
RegNet: 61 Channels 62.8 98 ± 0.4 96 ± 0.6 >0.99 ± 0.001
RegNet: 75 Channels 114 95 ± 0.6 92 ± 0.7 0.98 ± 0.003
Note. 95% confidence intervals are calculated by bootstrapping each metric 1000 times using random selections of 80% of the test data. The percentages next to the
accuracy labels denote the decision threshold.
Figure 5. Accuracy of all models for a given number of planets. Left: 50% decision threshold. Right: 95% decision threshold.
Figure 6. p-values from testing the correlation between accuracy and the
number of planets at different decision thresholds. The dashed black line is
p = 0.05, which is the standard cutoff for statistical significance.
6
The Astrophysical Journal, 941:192 (10pp), 2022 December 20 Terry et al.
7. Both classes of the models perform better when there are
more input channels, a trend not seen for HD 97048. A possible
explanation is the fact that there are about twice as many
velocity channels that cover HD 163296 when compared to HD
97048. While HD 97048 has roughly 75 channels covering the
disk, HD 163296 has roughly 150. All models applied to HD
163296 must therefore combine significantly more velocity
channels, which may decrease their ability to extract informa-
tion from the images. The activation structure tends to be less
informative, perhaps for the similar reasons, so it is omitted.
Despite this limitation, the high confidence of some of the
models should encourage a human observer to seriously
scrutinize the kinematic structure.
3.4. Limitations and Future Work
Our work comes with several limitations. All simulations
were run with SPH, so we did not demonstrate that our
methods would also be applicable to data from grid-based
codes. However, there is typically a qualitative agreement
between results from SPH- and grid-based methods (De Val-
Borro et al. 2006; Agertz et al. 2007). A good direction for
future work would be to train on simulation data from a variety
Figure 7. (a) Mean-subtracted activations using the 47-channel EfficientNetV2. The innermost planet has M = 0.28MJ, the second planet has M = 0.20MJ, the third
planet has M = 0.36MJ, and the outermost planet has M = 0.02MJ. (b) Disk column density after an azimuthal rotation of f = 131° and inclined by i = 36°. (c)
Unconvolved velocity channel with the most obvious kink. (d) Corresponding convolved velocity channel. Based on the kink, the approximate location of the planet
causing the most significant kink is in the white circle. The planets were correctly predicted with a confidence of >99%.
Figure 8. (a) Typical example of mean-subtracted activations for a disk with no
planet. (b) Disk column density after an azimuthal rotation of f = 153° and
inclined by i = 13°.
7
The Astrophysical Journal, 941:192 (10pp), 2022 December 20 Terry et al.
8. of hydrodynamics codes and check that the same results can be
obtained.
Any differences in performance of the models between the
codes, e.g., if the models consistently performed better on
SPH data, would be difficult to interpret, and the cause could be
hard to identify. It is possible that the method of domain
adaptation (Ben-David et al. 2010), which has already found
success in astronomy (Vilalta et al. 2019; Alexander et al.
2021; Ćiprijanović et al. 2022), could be used to encourage the
models to overcome any differences between data sets. This is
an avenue that is ripe for exploration in future work.
In order to keep the parameter space manageable and
demonstrate a proof of concept in this work, we therefore
trained on data produced by only one hydrodynamics code
(PHANTOM).
The absence of true image segmentation (Minaee et al. 2022)
or object detection (Zhao et al. 2019) during training is another
limitation that requires addressing in future work. While we
present results in the form of activation structures that suggest
the location(s) of the planet(s), these activations neither always
perfectly coincide with the planets nor capture all planets. User
analysis is required in order to pinpoint the radial (and
sometimes azimuthal) location(s) of the planets even with the
information given by the activation structures. The main utility
of the presented models is therefore to give a user an indication
as to whether a planet is present and motivate and direct the
analysis of the velocity channels. Segmentation and object
detection would address these shortcomings by precisely
pinpointing the location(s) of the planet(s) without any
necessary further analysis.
The assertion of a vertically isothermal disk is a simplifying
assumption that is commonly used in simulations of proto-
planetary disks (see, e.g., Dipierro et al. 2015; Pinte et al.
Figure 9. (a) HD 97048 at 885 μm. (b) Δv = 0.96 km s−1
channel. Bottom: mean-subtracted activations from two different layers for HD 97048 using the 47-channel
RegNet. The estimated planet location is given inside the white circle. The beams for the observations are given in the bottom right corner of panels (a) and (b).
Table 3
Prediction Confidences for All Models Tested on HD 97048 and HD 163296
Model HD 97048 Softmax HD 163296 Softmax
EffecientNetV2: 47 Channels 85% 37%
EffecientNetV2: 61 Channels 89% 69%
EffecientNetV2: 75 Channels 64% 73%
RegNet: 47 Channels >99% 74%
RegNet: 61 Channels 96% >99%
RegNet: 75 Channels >99% >99%
8
The Astrophysical Journal, 941:192 (10pp), 2022 December 20 Terry et al.
9. 2019). It has been demonstrated that the dispersion relation and
morphology of the planet’s signature can change significantly if
the disk is vertically stratified (Ogilvie & Lubow 2002; Juhász
& Rosotti 2018).
However, the presence of any disturbance is more important
than its specific morphology. There does exist the possibility
that vertical stratification dampens the signatures to an extent
that the models’ performances appreciably decrease, but our
results demonstrate that even extremely subtle signals can be
found by the models. Regardless, a more realistic treatment of
the thermal structure may be useful in future works.
4. Conclusions
Our results show that a machine-learning model trained on
synthetic data can determine the presence and location of
forming exoplanets in real telescope observations of proto-
planetary accretion disks. We apply this model to the HD
97048 and HD 163296 systems. Multiple models predict the
presence of a planet with greater than 99% confidence in both
systems. The presence and location of the planet in HD 97048
are corroborated by activating strongly on the same location
given by Pinte et al. (2019).
Five out of six models have greater than 90% accuracy when
using a 50% decision threshold. When using a 95% decision
threshold, four out of six models have an accuracy greater than
90%. Five models have an AUC of at least 0.98. While
EfficientNetV2 and RegNet perform comparably on the
synthetic test data, RegNet outperforms EfficientNetV2 on
the real telescope observations.
This work is the first step in a series of works that use
machine learning to automate the detection and analysis of
objects within protoplanetary disks. Applying full segmenta-
tion and object-detection methods will further increase the
ability of our models to locate planets and infer properties, such
as planetary mass. We leave this work to the future. We
envision final models that can be used easily for multiple
purposes and be distributed freely throughout the community.
As Atacama Large Millimeter/submillimeter Array (ALMA)
continues to deliver larger and larger disk survey data sets, and
next-generation telescopes—such as JWST, ngVLA, and the
Square Kilometre Array (SKA)—come online, the time/cost of
analyzing more and more data will increase. Our proof-of-
concept work demonstrates that even when high confidence is
demanded, machine learning can automate this task and match
and exceed human proficiency.
We would like to thank the referee for insightful comments
that improved the paper. This paper makes use of the following
ALMA data: ADS/JAO.ALMA#2016.1.00826.S and ADS/
JAO.ALMA#2013.1.00601.S. ALMA is a partnership of ESO
(representing its member states), NSF (USA) and NINS
(Japan), together with NRC (Canada), MOST and ASIAA
(Taiwan), and KASI (Republic of Korea), in cooperation with
the Republic of Chile. The Joint ALMA Observatory is
operated by ESO, AUI/NRAO and NAOJ. The National Radio
Astronomy Observatory is a facility of the National Science
Foundation operated under cooperative agreement by Asso-
ciated Universities, Inc. SPH results are visualized using
SPLASH (Price 2007). J.T. was a participant in the 2022
Google Summer of Code program. This study was supported in
part by resources and technical expertise from the Georgia
Advanced Computing Resource Center, a partnership between
the University of Georgiaʼs Office of the Vice President for
Research and Office of the Vice President for Information
Technology.
ORCID iDs
J. P. Terry https:/
/orcid.org/0000-0002-8590-7271
C. Hall https:/
/orcid.org/0000-0002-8138-0425
S. Abreau https:/
/orcid.org/0000-0002-9426-3789
S. Gleyzer https:/
/orcid.org/0000-0002-6222-8102
References
Agertz, O., Moore, B., Stadel, J., et al. 2007, MNRAS, 380, 963
Alexander, S., Gleyzer, S., McDonough, E., Toomey, M. W., & Usai, E. 2020,
ApJ, 893, 15
Alexander, S., Gleyzer, S., Reddy, P., Tidball, M., & Toomey, M. W. 2021,
arXiv:2112.12121
Andrews, S. M., Huang, J., Pérez, L. M., et al. 2018, ApJL, 869, L41
Andrews, S. M., Wilner, D. J., Hughes, A. M., Qi, C., & Dullemond, C. P.
2009, ApJ, 700, 1502
Auddy, S., Dey, R., Lin, M.-K., Carrera, D., & Simon, J. B. 2022, ApJ, 936, 93
Auddy, S., Dey, R., Lin, M.-K., & Hall, C. 2021, ApJ, 920, 3
Barraza-Alfaro, M., Flock, M., Marino, S., & Pérez, S. 2021, A&A, 653, A113
Ben-David, S., Blitzer, J., Crammer, K., et al. 2010, Mach. Learn., 79, 151
Biewald, L. 2020, Experiment Tracking with Weights and Biaseshttps://www.
wandb.com/
Ćiprijanović, A., Kafkes, D., Snyder, G., et al. 2022, MLS&T, 3, 035007
Cireşan, D. C., Meier, U., Masci, J., Gambardella, L. M., & Schmidhuber, J.
2011, arXiv:1102.0183
De Val-Borro, M., Edgar, R. G., Artymowicz, P., et al. 2006, MNRAS,
370, 529
Dipierro, G., Price, D., Laibe, G., et al. 2015, MNRAS Lett., 453, L73
Dosovitskiy, A., Beyer, L., Kolesnikov, A., et al. 2020, arXiv:2010.11929
Draine, B. T., & Lee, H. M. 1984, ApJ, 285, 89
Elfwing, S., Uchibe, E., & Doya, K. 2018, NN, 107, 3
Glorot, X., Bordes, A., & Bengio, Y. 2011, in Proc. 14th Int. Conf. Artif. Intell.
Stat., 15, (PMLR), 315, https://proceedings.mlr.press/v15/glorot11a.html
Goodfellow, I., Bengio, Y., & Courville, A. 2016, Deep Learning (Cambridge,
MA: MIT Press) http://www.deeplearningbook.org
Hall, C., Dong, R., Teague, R., et al. 2020, ApJ, 904, 148
Hanley, J. A., & McNeil, B. J. 1982, Radiology, 143, 29
He, K., Zhang, X., Ren, S., & Sun, J. 2016, in IEEE Conf. Comput. Vision
Pattern Recognit. (CVPR) (Piscataway, NJ: IEEE), 770
Hinton, G. E., Dayan, P., Frey, B. J., & Neal, R. M. 1995, Sci, 268, 1158
Huang, J., Andrews, S. M., Dullemond, C. P., et al. 2018, ApJL, 869, L42
Jo, Y., & Kim, J.-h. 2019, MNRAS, 489, 3565
Juhász, A., & Rosotti, G. P. 2018, MNRAS Lett., 474, L32
Kingma, D. P., & Ba, J. 2014, arXiv:1412.6980
McKay, M. D., Beckman, R. J., & Conover, W. J. 1979, Technometrics, 21,
239, http://www.jstor.org/stable/1268522
Minaee, S., Boykov, Y., Porikli, F., et al. 2022, in IEEE Trans. on Pattern Anal.
Mach. Intell., 44 (Piscataway, NJ: IEEE), 3523
Möller, A., & de Boissière, T. 2020, MNRAS, 491, 4277
Öberg, K. I., Guzmán, V. V., Walsh, C., et al. 2021, ApJS, 257, 1
Ogilvie, G. I., & Lubow, S. H. 2002, MNRAS, 330, 950
Paszke, A., Gross, S., Massa, F., et al. 2019, in Advances in Neural Information
Processing Systems, 32, ed. H. Wallach et al. (Red Hook, NY: Curran
Associates, Inc.) https://proceedings.neurips.cc/paper/2019/file/
bdbca288fee7f92f2bfa9f7012727740-Paper.pdf
Pinte, C., Harries, T. J., Min, M., et al. 2009, A&A, 498, 967
Pinte, C., Ménard, F., Duchêne, G., & Bastien, P. 2006, A&A, 459, 797
Pinte, C., Price, D. J., Ménard, F., et al. 2018, ApJL, 860, L13
Pinte, C., Price, D. J., Ménard, F., et al. 2020, ApJL, 890, L9
Pinte, C., van der Plas, G., Ménard, F., et al. 2019, NatAs, 3, 1109
Price, D. J. 2007, PASA, 24, 159
Price, D. J., Wurster, J., Tricco, T. S., et al. 2018, PASA, 35, e031
Siess, L., Dufour, E., & Forestini, M. 2000, A&A, 358, 593
Simon, J. B., Hughes, A. M., Flaherty, K. M., Bai, X.-N., & Armitage, P. J.
2015, ApJ, 808, 180
Szegedy, C., Liu, W., Jia, Y., et al. 2015, in IEEE Conf. Comput. Vision
Pattern Recognit. (CVPR) (Piscataway, NJ: IEEE), 1, https://www.cv-
foundation.org/openaccess/content_cvpr_2015/html/Szegedy_Going_
Deeper_With_2015_CVPR_paper.html
9
The Astrophysical Journal, 941:192 (10pp), 2022 December 20 Terry et al.
10. Tan, M., & Le, Q. V. 2019, in Proc. 36th Int. Conf. Mach. Learn., 97,
(PMLR), 6105, https://proceedings.mlr.press/v97/tan19a.html
Tan, M., & Le, Q. V. 2021, in Proc. 38th Int. Conf. Mach. Learn., 139,
(PMLR), 10096, https://proceedings.mlr.press/v139/tan21a.html
Teague, R., Bae, J., Bergin, E. A., Birnstiel, T., & Foreman-Mackey, D. 2018,
ApJL, 860, L12
Terry, J. P., Hall, C., Longarini, C., et al. 2022, MNRAS, 510, 1671
Vaswani, A., Shazeer, N., Parmar, N., et al. 2017, in Advances in Neural
Information Processing Systems, 30 (Red Hook, NY: Curran Associates,
Inc.) https://proceedings.neurips.cc/paper/2017/file/
3f5ee243547dee91fbd053c1c4a845aa-Paper.pdf
Vilalta, R., Gupta, K. D., Boumber, D., & Meskhi, M. M. 2019, PASP, 131,
108008
Xu, J., Pan, Y., Pan, X., et al. 2022, in IEEE Trans. on Neural Networks and
Learn. Syst. (Piscataway, NJ: IEEE), 1, https://ieeexplore.ieee.org/
document/9743274
Zhao, Z.-Q., Zheng, P., Xu, S.-t., & Wu, X. 2019, in IEEE Trans. on Neural
Networks and Learn. Syst., 30 (Piscataway, NJ: IEEE), 3212
Zhou, W., Yang, Y., Yu, C., et al. 2021, NatCo, 12, 1259
10
The Astrophysical Journal, 941:192 (10pp), 2022 December 20 Terry et al.