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.
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
An Earth-sized exoplanet with a Mercury-like compositionSérgio Sacani
Earth, Venus, Mars and some extrasolar terrestrial planets1
have a mass and radius that is consistent with a mass fraction
of about 30% metallic core and 70% silicate mantle2
. At the
inner frontier of the Solar System, Mercury has a completely
different composition, with a mass fraction of about 70%
metallic core and 30% silicate mantle3
. Several formation or
evolution scenarios are proposed to explain this metal-rich
composition, such as a giant impact4, mantle evaporation5
or the depletion of silicate at the inner edge of the protoplanetary
disk6. These scenarios are still strongly debated.
Here, we report the discovery of a multiple transiting planetary
system (K2-229) in which the inner planet has a radius
of 1.165 ± 0.066 Earth radii and a mass of 2.59 ± 0.43 Earth
masses. This Earth-sized planet thus has a core-mass fraction
that is compatible with that of Mercury, although it was
expected to be similar to that of Earth based on host-star
chemistry7
. This larger Mercury analogue either formed with
a very peculiar composition or has evolved, for example, by
losing part of its mantle. Further characterization of Mercurylike
exoplanets such as K2-229 b will help to put the detailed
in situ observations of Mercury (with MESSENGER and
BepiColombo8) into the global context of the formation and
evolution of solar and extrasolar terrestrial planets.
The Variable Detection of Atmospheric Escape around the Young, Hot Neptune AU...Sérgio Sacani
This document summarizes observations from the Hubble Space Telescope of the young hot Neptune exoplanet AU Mic b, which orbits the nearby M dwarf star AU Mic. The observations aimed to detect atmospheric escape of neutral hydrogen through absorption in the stellar Lyman-alpha emission line. Two visits were obtained, one in 2020 and one in 2021, corresponding to transits of the planet. A stellar flare was observed and removed from the first visit data. In the second visit, absorption was detected in the blue wing of the Lyman-alpha line 2.5 hours before the white light transit, indicating the presence of high-velocity neutral hydrogen escaping the planet's atmosphere and traveling toward the observer. Estimates place the column density of this material
This document summarizes a blind HI survey of the southern Milky Way zone of avoidance conducted with the Parkes radio telescope. The survey detected 883 galaxies at Galactic longitudes 212° < l < 36° and latitudes |b| < 5° to a sensitivity of 6 mJy per 27 km/s channel. Fifty-one percent of detections had known optical/near-infrared counterparts, while 27% had new counterparts identified. The survey delineated large-scale structures in the Puppis and Great Attractor regions for the first time. Several newly identified galaxy concentrations and clusters were revealed that help trace the Great Attractor Wall.
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
Artigo que descreve a descoberta do exoplaneta Kepler-432b, um exoplaneta mais massivo que Júpiter que orbita uma estrela gigante vermelha bem próximo e numa órbita extremamente alongada.
The extremely high albedo of LTT 9779 b revealed by CHEOPSSérgio Sacani
Optical secondary eclipse measurements of small planets can provide a wealth of information about the reflective properties
of these worlds, but the measurements are particularly challenging to attain because of their relatively shallow depth. If such signals
can be detected and modeled, however, they can provide planetary albedos, thermal characteristics, and information on absorbers in
the upper atmosphere.
Aims. We aim to detect and characterize the optical secondary eclipse of the planet LTT 9779 b using the CHaracterising ExOPlanet
Satellite (CHEOPS) to measure the planetary albedo and search for the signature of atmospheric condensates.
Methods. We observed ten secondary eclipses of the planet with CHEOPS. We carefully analyzed and detrended the light curves using
three independent methods to perform the final astrophysical detrending and eclipse model fitting of the individual and combined light
curves.
Results. Each of our analysis methods yielded statistically similar results, providing a robust detection of the eclipse of LTT 9779 b
with a depth of 115±24 ppm. This surprisingly large depth provides a geometric albedo for the planet of 0.80+0.10
−0.17, consistent with
estimates of radiative-convective models. This value is similar to that of Venus in our own Solar System. When combining the eclipse
from CHEOPS with the measurements from TESS and Spitzer, our global climate models indicate that LTT 9779 b likely has a super
metal-rich atmosphere, with a lower limit of 400× solar being found, and the presence of silicate clouds. The observations also reveal
hints of optical eclipse depth variability, but these have yet to be confirmed.
Conclusions. The results found here in the optical when combined with those in the near-infrared provide the first steps toward
understanding the atmospheric structure and physical processes of ultrahot Neptune worlds that inhabit the Neptune desert.
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
An Earth-sized exoplanet with a Mercury-like compositionSérgio Sacani
Earth, Venus, Mars and some extrasolar terrestrial planets1
have a mass and radius that is consistent with a mass fraction
of about 30% metallic core and 70% silicate mantle2
. At the
inner frontier of the Solar System, Mercury has a completely
different composition, with a mass fraction of about 70%
metallic core and 30% silicate mantle3
. Several formation or
evolution scenarios are proposed to explain this metal-rich
composition, such as a giant impact4, mantle evaporation5
or the depletion of silicate at the inner edge of the protoplanetary
disk6. These scenarios are still strongly debated.
Here, we report the discovery of a multiple transiting planetary
system (K2-229) in which the inner planet has a radius
of 1.165 ± 0.066 Earth radii and a mass of 2.59 ± 0.43 Earth
masses. This Earth-sized planet thus has a core-mass fraction
that is compatible with that of Mercury, although it was
expected to be similar to that of Earth based on host-star
chemistry7
. This larger Mercury analogue either formed with
a very peculiar composition or has evolved, for example, by
losing part of its mantle. Further characterization of Mercurylike
exoplanets such as K2-229 b will help to put the detailed
in situ observations of Mercury (with MESSENGER and
BepiColombo8) into the global context of the formation and
evolution of solar and extrasolar terrestrial planets.
The Variable Detection of Atmospheric Escape around the Young, Hot Neptune AU...Sérgio Sacani
This document summarizes observations from the Hubble Space Telescope of the young hot Neptune exoplanet AU Mic b, which orbits the nearby M dwarf star AU Mic. The observations aimed to detect atmospheric escape of neutral hydrogen through absorption in the stellar Lyman-alpha emission line. Two visits were obtained, one in 2020 and one in 2021, corresponding to transits of the planet. A stellar flare was observed and removed from the first visit data. In the second visit, absorption was detected in the blue wing of the Lyman-alpha line 2.5 hours before the white light transit, indicating the presence of high-velocity neutral hydrogen escaping the planet's atmosphere and traveling toward the observer. Estimates place the column density of this material
This document summarizes a blind HI survey of the southern Milky Way zone of avoidance conducted with the Parkes radio telescope. The survey detected 883 galaxies at Galactic longitudes 212° < l < 36° and latitudes |b| < 5° to a sensitivity of 6 mJy per 27 km/s channel. Fifty-one percent of detections had known optical/near-infrared counterparts, while 27% had new counterparts identified. The survey delineated large-scale structures in the Puppis and Great Attractor regions for the first time. Several newly identified galaxy concentrations and clusters were revealed that help trace the Great Attractor Wall.
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
Artigo que descreve a descoberta do exoplaneta Kepler-432b, um exoplaneta mais massivo que Júpiter que orbita uma estrela gigante vermelha bem próximo e numa órbita extremamente alongada.
The extremely high albedo of LTT 9779 b revealed by CHEOPSSérgio Sacani
Optical secondary eclipse measurements of small planets can provide a wealth of information about the reflective properties
of these worlds, but the measurements are particularly challenging to attain because of their relatively shallow depth. If such signals
can be detected and modeled, however, they can provide planetary albedos, thermal characteristics, and information on absorbers in
the upper atmosphere.
Aims. We aim to detect and characterize the optical secondary eclipse of the planet LTT 9779 b using the CHaracterising ExOPlanet
Satellite (CHEOPS) to measure the planetary albedo and search for the signature of atmospheric condensates.
Methods. We observed ten secondary eclipses of the planet with CHEOPS. We carefully analyzed and detrended the light curves using
three independent methods to perform the final astrophysical detrending and eclipse model fitting of the individual and combined light
curves.
Results. Each of our analysis methods yielded statistically similar results, providing a robust detection of the eclipse of LTT 9779 b
with a depth of 115±24 ppm. This surprisingly large depth provides a geometric albedo for the planet of 0.80+0.10
−0.17, consistent with
estimates of radiative-convective models. This value is similar to that of Venus in our own Solar System. When combining the eclipse
from CHEOPS with the measurements from TESS and Spitzer, our global climate models indicate that LTT 9779 b likely has a super
metal-rich atmosphere, with a lower limit of 400× solar being found, and the presence of silicate clouds. The observations also reveal
hints of optical eclipse depth variability, but these have yet to be confirmed.
Conclusions. The results found here in the optical when combined with those in the near-infrared provide the first steps toward
understanding the atmospheric structure and physical processes of ultrahot Neptune worlds that inhabit the Neptune desert.
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.
AT2023fhn (the Finch): a Luminous Fast Blue Optical Transient at a large offs...Sérgio Sacani
Luminous Fast Blue Optical Transients (LFBOTs) - the prototypical example being AT 2018cow - are a rare class of events
whose origins are poorly understood. They are characterised by rapid evolution, featureless blue spectra at early times, and
luminous X-ray and radio emission. LFBOTs thus far have been found exclusively at small projected offsets from star-forming
host galaxies. We present Hubble Space Telescope, Gemini, Chandra and Very Large Array observations of a new LFBOT,
AT 2023fhn. The Hubble Space Telescope data reveal a large offset (> 3.5 half-light radii) from the two closest galaxies, both
at redshift 𝑧 ∼ 0.24. The location of AT 2023fhn is in stark contrast with previous events, and demonstrates that LFBOTs can
occur in a range of galactic environments.
A precise water_abundance_measurement_for_the_hot_jupiter_wasp_43bSérgio Sacani
This document presents a precise measurement of the water abundance in the atmosphere of the exoplanet WASP-43b using transmission and thermal emission spectroscopy from the Hubble Space Telescope. The key findings are:
1) The water content of WASP-43b's atmosphere is consistent with solar composition at planetary temperatures, ranging from 0.4 to 3.5 times the solar water abundance.
2) This metallicity measurement extends the trend seen in the solar system of lower metal enrichment for higher mass planets.
3) Measuring a planet's water content constrains its formation location in the protoplanetary disk and provides insight into planetary formation models.
Measurements of the_near_nucleus_coma_of_comet_67_p_churyumov_gerasimenko_wit...Sérgio Sacani
Artigo descreve descoberta feita pelo instrumento Alice da sonda Rosetta no cometa 67P/Churyumov-Gerasimenko, das moléculas de água e dióxido de carbono quebradas que pairam pela atmosfera do cometa.
No global pluto_like_atmosphere_on_dwarf_planet_makemake_from_a_stellar_occul...Sérgio Sacani
1. A stellar occultation event was observed involving the dwarf planet Makemake on April 23, 2011 using multiple telescopes.
2. Analysis of the light curves from the event showed abrupt disappearances and reappearances of the star, indicating Makemake has no global atmosphere at an upper limit of 4-12 nanobar surface pressure.
3. The occultation data was used to determine Makemake has dimensions of 1,430±9 km by 1,502±45 km, implying a high geometric albedo of 0.77±0.03. This rules out a low density and suggests Makemake is in hydrostatic equilibrium as an oblate spheroid.
The document describes the SuperWASP project, which uses two robotic telescopes (SuperWASP-N and SuperWASP-S) to search for transiting exoplanets. As of February 2015, SuperWASP had discovered 98 exoplanets, making it the most successful ground-based exoplanet survey. It discusses the history of exoplanet detection, details the SuperWASP instrumentation and detection method, and reviews its discoveries and role alongside space-based missions like Kepler.
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
Uma espetacular colisão de galáxias foi descoberta além da Via Láctea. O sistema mais próximo já descoberto, a identificação foi anunciada por uma equipe de astrônomos liderada pelo Professor Quentin Parker da Universidade de Hong Kong e pelo Professor Albert Zijlstra na Universidade de Manchester.
A galáxia está a 30 milhões de anos-luz de distância, o que significa que ela é relativamente próxima. Ela foi chamada de Roda de Kathryn, em homenagem à sua semelhança com o famoso fogo de artifício e também em homenagem à esposa do coautor do trabalho.
Esses sistemas são muito raros e nascem da colisão entre duas galáxias de tamanhos similares. As ondas de choque geradas na colisão comprimem o reservatório de gás em cada galáxia e disparam a formação de novas estrelas. Isso cria um espetacular anel de intensa emissão, e ilumina o sistema, do mesmo modo que a Roda Catherine ilumina a noite num show de fogos de artifício.
As galáxias crescem através de colisões, mas é raro registrar esse processo acontecendo, e é extremamente raro ver o anel da colisão em progresso. Pouco mais de 20 sistemas com anéis completos são conhecidos.
This document presents an analysis of transit spectroscopy observations of three exoplanets - WASP-12 b, WASP-17 b, and WASP-19 b - using the Wide Field Camera 3 instrument on the Hubble Space Telescope. The observations achieved almost photon-limited precision but uncertainties in the transit depths were increased by the uneven sampling of the light curves. The final transit spectra for all three planets are consistent with the presence of a water absorption feature at 1.4 microns, though the amplitude is smaller than expected from previous Spitzer observations possibly due to hazes. Due to degeneracies between models, the data cannot unambiguously constrain the atmospheric compositions without additional observations.
Is the atmosphere of the ultra-hot Jupiter WASP-121 b variable?Sérgio Sacani
We present a comprehensive analysis of the Hubble Space Telescope observations of the atmosphere
of WASP-121 b, a ultra-hot Jupiter. After reducing the transit, eclipse, and phase-curve observations
with a uniform methodology and addressing the biases from instrument systematics, sophisticated
atmospheric retrievals are used to extract robust constraints on the thermal structure, chemistry, and
cloud properties of the atmosphere. Our analysis shows that the observations are consistent with a
strong thermal inversion beginning at ∼104 Pa on the dayside, solar to subsolar metallicity Z (i.e.,
−0.77 < log(Z) < 0.05), and super-solar C/O ratio (i.e., 0.59 < C/O < 0.87). More importantly,
utilizing the high signal-to-noise ratio and repeated observations of the planet, we identify the following
unambiguous time-varying signals in the data: i) a shift of the putative hotspot offset between the
two phase-curves and ii) varying spectral signatures in the transits and eclipses. By simulating the
global dynamics of WASP-121 b atmosphere at high-resolution, we show that the identified signals are
consistent with quasi-periodic weather patterns, hence atmospheric variability, with signatures at the
level probed by the observations (∼5% to ∼10%) that change on a timescale of ∼5 planet days; in
the simulations, the weather patterns arise from the formation and movement of storms and fronts,
causing hot (as well as cold) patches of atmosphere to deform, separate, and mix in time.
This document describes observations of the Seyfert 1 galaxy Mrk 509 using the Cosmic Origins Spectrograph (COS) on the Hubble Space Telescope (HST). The observations detected absorption features in the ultraviolet spectrum, which are attributed to outflowing gas from the active galactic nucleus as well as gas in the galaxy's interstellar medium and halo. The COS observations provide higher signal-to-noise and resolution than previous observations, detecting additional complexity in the absorption features. Variability in some features constrains the distances of absorbing gas components to be less than 250 pc and 1.5 kpc from the active nucleus. The absorption lines only partially cover the emission from the active nucleus, possibly due to
MUSE sneaks a peek at extreme ram-pressure stripping events. I. A kinematic s...Sérgio Sacani
- MUSE observations of the galaxy ESO137-001 reveal an extended gaseous tail over 30 kpc long traced by H-alpha emission, providing evidence of an extreme ram pressure stripping event as the galaxy falls into the massive Norma galaxy cluster.
- Analysis of the H-alpha kinematics and stellar velocity field show that ram pressure has removed the interstellar medium from the outer disk while the primary tail is still fed by gas from the galaxy center, with gravitational interactions not appearing to be the main mechanism of gas removal.
- The stripped gas retains evidence of the disk's rotational velocity out to around 20 kpc downstream, indicating the galaxy is moving radially along the plane of the sky, while
This document describes observations of the galaxy ESO137-001 using the MUSE instrument on the VLT. The key points are:
1) MUSE observations reveal an extended gas tail stretching over 30 kpc from the galaxy, tracing ongoing ram pressure stripping as it falls into the Norma galaxy cluster.
2) Analysis of the gas kinematics and stellar velocity field show that ram pressure has removed the interstellar medium from the outer disk while the primary tail is still fed by gas from the galaxy center.
3) The stripped gas retains evidence of the disk's rotational velocity out to 20 kpc downstream, indicating the galaxy is moving radially through the cluster. Beyond this the gas shows greater turbulence,
Eccentricity from transit_photometry_small_planets_in_kepler_multi_planet_sys...Sérgio Sacani
Artigo descreve estudo que mostra que a órbita dos exoplanetas terrestres são na sua maioria órbitas circulares, o que é bom para se procurar por vida e o que vem causando uma revolução no entendimento sobre os sistemas de exoplanteas.
The document summarizes findings from the Microwave Instrument on the Rosetta Orbiter (MIRO) regarding the subsurface properties and early activity of comet 67P/Churyumov-Gerasimenko. Key points:
- MIRO detected water vapor emissions from the comet beginning in early June 2014 and measured the total water production rate, which varied from 0.3 kg/s to 1.2 kg/s between June and August.
- Water outgassing displayed periodic variations correlated with the comet's 12.4-hour rotation period and seemed to originate primarily from the comet's "neck" region.
- Subsurface temperatures measured by MIRO showed seasonal and diurnal variations, indicating radiation
This document summarizes the results of a 180 ks Chandra-LETGS observation of Mrk 509 as part of a larger multi-wavelength campaign. The observation detected several absorption features in the X-ray spectrum originating from an ionized absorber, including ions with three distinct ionization degrees. The lowest ionized component is slightly redshifted and not in pressure equilibrium with the others, likely belonging to the host galaxy's interstellar medium. The other two components are outflowing at velocities of around -200 and -455 km/s. Simultaneous HST-COS observations detected 13 UV kinematic components, and at least three can be associated with the X-ray components, providing evidence that the UV and X-
TEMPORAL EVOLUTION OF THE HIGH-ENERGY IRRADIATION AND WATER CONTENT OF TRAPPI...Sérgio Sacani
The ultracool dwarf star TRAPPIST-1 hosts seven Earth-size transiting planets, some of which could
harbour liquid water on their surfaces. UV observations are essential to measure their high-energy
irradiation, and to search for photodissociated water escaping from their putative atmospheres. Our
new observations of TRAPPIST-1 Ly-α line during the transit of TRAPPIST-1c show an evolution of
the star emission over three months, preventing us from assessing the presence of an extended hydrogen
exosphere. Based on the current knowledge of the stellar irradiation, we investigated the likely history
of water loss in the system. Planets b to d might still be in a runaway phase, and planets within the
orbit of TRAPPIST-1g could have lost more than 20 Earth oceans after 8 Gyr of hydrodynamic escape.
However, TRAPPIST-1e to h might have lost less than 3 Earth oceans if hydrodynamic escape stopped
once they entered the habitable zone. We caution that these estimates remain limited by the large
uncertainty on the planet masses. They likely represent upper limits on the actual water loss because
our assumptions maximize the XUV-driven escape, while photodissociation in the upper atmospheres
should be the limiting process. Late-stage outgassing could also have contributed significant amounts
of water for the outer, more massive planets after they entered the habitable zone. While our results
suggest that the outer planets are the best candidates to search for water with the JWST, they also
highlight the need for theoretical studies and complementary observations in all wavelength domains
to determine the nature of the TRAPPIST-1 planets, and their potential habitability.
Keywords: planetary systems - Stars: individual: TRAPPIST-1
Spirals and clumps in V960 Mon: signs of planet formation via gravitational i...Sérgio Sacani
The formation of giant planets has traditionally been divided into two pathways: core accretion and gravitational instability. However, in recent years, gravitational instability has become less favored, primarily due
to the scarcity of observations of fragmented protoplanetary disks around young stars and low occurrence rate
of massive planets on very wide orbits. In this study, we present a SPHERE/IRDIS polarized light observation
of the young outbursting object V960 Mon. The image reveals a vast structure of intricately shaped scattered
light with several spiral arms. This finding motivated a re-analysis of archival ALMA 1.3 mm data acquired
just two years after the onset of the outburst of V960 Mon. In these data, we discover several clumps of continuum emission aligned along a spiral arm that coincides with the scattered light structure. We interpret the
localized emission as fragments formed from a spiral arm under gravitational collapse. Estimating the mass of
solids within these clumps to be of several Earth masses, we suggest this observation to be the first evidence of
gravitational instability occurring on planetary scales. This study discusses the significance of this finding for
planet formation and its potential connection with the outbursting state of V960 Mon.
An elevation of 0.1 light-seconds for the optical jet base in an accreting Ga...Sérgio Sacani
Relativistic plasma jets are observed in many systems that
host accreting black holes. According to theory, coiled magnetic
fields close to the black hole accelerate and collimate the
plasma, leading to a jet being launched1–3. Isolating emission
from this acceleration and collimation zone is key to measuring
its size and understanding jet formation physics. But this
is challenging because emission from the jet base cannot
easily be disentangled from other accreting components. Here,
we show that rapid optical flux variations from an accreting
Galactic black-hole binary are delayed with respect to X-rays
radiated from close to the black hole by about 0.1 seconds, and
that this delayed signal appears together with a brightening
radio jet. The origin of these subsecond optical variations
has hitherto been controversial4–8. Not only does our work
strongly support a jet origin for the optical variations but it
also sets a characteristic elevation of ≲ 103 Schwarzschild
radii for the main inner optical emission zone above the black
hole9, constraining both internal shock10 and magnetohydrodynamic11
models. Similarities with blazars12,13 suggest that jet
structure and launching physics could potentially be unified
under mass-invariant models. Two of the best-studied jetted
black-hole binaries show very similar optical lags8,14,15, so this
size scale may be a defining feature of such systems.
The binding of cosmological structures by massless topological defectsSérgio Sacani
Assuming spherical symmetry and weak field, it is shown that if one solves the Poisson equation or the Einstein field
equations sourced by a topological defect, i.e. a singularity of a very specific form, the result is a localized gravitational
field capable of driving flat rotation (i.e. Keplerian circular orbits at a constant speed for all radii) of test masses on a thin
spherical shell without any underlying mass. Moreover, a large-scale structure which exploits this solution by assembling
concentrically a number of such topological defects can establish a flat stellar or galactic rotation curve, and can also deflect
light in the same manner as an equipotential (isothermal) sphere. Thus, the need for dark matter or modified gravity theory is
mitigated, at least in part.
EWOCS-I: The catalog of X-ray sources in Westerlund 1 from the Extended Weste...Sérgio Sacani
Context. With a mass exceeding several 104 M⊙ and a rich and dense population of massive stars, supermassive young star clusters
represent the most massive star-forming environment that is dominated by the feedback from massive stars and gravitational interactions
among stars.
Aims. In this paper we present the Extended Westerlund 1 and 2 Open Clusters Survey (EWOCS) project, which aims to investigate
the influence of the starburst environment on the formation of stars and planets, and on the evolution of both low and high mass stars.
The primary targets of this project are Westerlund 1 and 2, the closest supermassive star clusters to the Sun.
Methods. The project is based primarily on recent observations conducted with the Chandra and JWST observatories. Specifically,
the Chandra survey of Westerlund 1 consists of 36 new ACIS-I observations, nearly co-pointed, for a total exposure time of 1 Msec.
Additionally, we included 8 archival Chandra/ACIS-S observations. This paper presents the resulting catalog of X-ray sources within
and around Westerlund 1. Sources were detected by combining various existing methods, and photon extraction and source validation
were carried out using the ACIS-Extract software.
Results. The EWOCS X-ray catalog comprises 5963 validated sources out of the 9420 initially provided to ACIS-Extract, reaching a
photon flux threshold of approximately 2 × 10−8 photons cm−2
s
−1
. The X-ray sources exhibit a highly concentrated spatial distribution,
with 1075 sources located within the central 1 arcmin. We have successfully detected X-ray emissions from 126 out of the 166 known
massive stars of the cluster, and we have collected over 71 000 photons from the magnetar CXO J164710.20-455217.
More Related Content
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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.
AT2023fhn (the Finch): a Luminous Fast Blue Optical Transient at a large offs...Sérgio Sacani
Luminous Fast Blue Optical Transients (LFBOTs) - the prototypical example being AT 2018cow - are a rare class of events
whose origins are poorly understood. They are characterised by rapid evolution, featureless blue spectra at early times, and
luminous X-ray and radio emission. LFBOTs thus far have been found exclusively at small projected offsets from star-forming
host galaxies. We present Hubble Space Telescope, Gemini, Chandra and Very Large Array observations of a new LFBOT,
AT 2023fhn. The Hubble Space Telescope data reveal a large offset (> 3.5 half-light radii) from the two closest galaxies, both
at redshift 𝑧 ∼ 0.24. The location of AT 2023fhn is in stark contrast with previous events, and demonstrates that LFBOTs can
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A precise water_abundance_measurement_for_the_hot_jupiter_wasp_43bSérgio Sacani
This document presents a precise measurement of the water abundance in the atmosphere of the exoplanet WASP-43b using transmission and thermal emission spectroscopy from the Hubble Space Telescope. The key findings are:
1) The water content of WASP-43b's atmosphere is consistent with solar composition at planetary temperatures, ranging from 0.4 to 3.5 times the solar water abundance.
2) This metallicity measurement extends the trend seen in the solar system of lower metal enrichment for higher mass planets.
3) Measuring a planet's water content constrains its formation location in the protoplanetary disk and provides insight into planetary formation models.
Measurements of the_near_nucleus_coma_of_comet_67_p_churyumov_gerasimenko_wit...Sérgio Sacani
Artigo descreve descoberta feita pelo instrumento Alice da sonda Rosetta no cometa 67P/Churyumov-Gerasimenko, das moléculas de água e dióxido de carbono quebradas que pairam pela atmosfera do cometa.
No global pluto_like_atmosphere_on_dwarf_planet_makemake_from_a_stellar_occul...Sérgio Sacani
1. A stellar occultation event was observed involving the dwarf planet Makemake on April 23, 2011 using multiple telescopes.
2. Analysis of the light curves from the event showed abrupt disappearances and reappearances of the star, indicating Makemake has no global atmosphere at an upper limit of 4-12 nanobar surface pressure.
3. The occultation data was used to determine Makemake has dimensions of 1,430±9 km by 1,502±45 km, implying a high geometric albedo of 0.77±0.03. This rules out a low density and suggests Makemake is in hydrostatic equilibrium as an oblate spheroid.
The document describes the SuperWASP project, which uses two robotic telescopes (SuperWASP-N and SuperWASP-S) to search for transiting exoplanets. As of February 2015, SuperWASP had discovered 98 exoplanets, making it the most successful ground-based exoplanet survey. It discusses the history of exoplanet detection, details the SuperWASP instrumentation and detection method, and reviews its discoveries and role alongside space-based missions like Kepler.
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
Uma espetacular colisão de galáxias foi descoberta além da Via Láctea. O sistema mais próximo já descoberto, a identificação foi anunciada por uma equipe de astrônomos liderada pelo Professor Quentin Parker da Universidade de Hong Kong e pelo Professor Albert Zijlstra na Universidade de Manchester.
A galáxia está a 30 milhões de anos-luz de distância, o que significa que ela é relativamente próxima. Ela foi chamada de Roda de Kathryn, em homenagem à sua semelhança com o famoso fogo de artifício e também em homenagem à esposa do coautor do trabalho.
Esses sistemas são muito raros e nascem da colisão entre duas galáxias de tamanhos similares. As ondas de choque geradas na colisão comprimem o reservatório de gás em cada galáxia e disparam a formação de novas estrelas. Isso cria um espetacular anel de intensa emissão, e ilumina o sistema, do mesmo modo que a Roda Catherine ilumina a noite num show de fogos de artifício.
As galáxias crescem através de colisões, mas é raro registrar esse processo acontecendo, e é extremamente raro ver o anel da colisão em progresso. Pouco mais de 20 sistemas com anéis completos são conhecidos.
This document presents an analysis of transit spectroscopy observations of three exoplanets - WASP-12 b, WASP-17 b, and WASP-19 b - using the Wide Field Camera 3 instrument on the Hubble Space Telescope. The observations achieved almost photon-limited precision but uncertainties in the transit depths were increased by the uneven sampling of the light curves. The final transit spectra for all three planets are consistent with the presence of a water absorption feature at 1.4 microns, though the amplitude is smaller than expected from previous Spitzer observations possibly due to hazes. Due to degeneracies between models, the data cannot unambiguously constrain the atmospheric compositions without additional observations.
Is the atmosphere of the ultra-hot Jupiter WASP-121 b variable?Sérgio Sacani
We present a comprehensive analysis of the Hubble Space Telescope observations of the atmosphere
of WASP-121 b, a ultra-hot Jupiter. After reducing the transit, eclipse, and phase-curve observations
with a uniform methodology and addressing the biases from instrument systematics, sophisticated
atmospheric retrievals are used to extract robust constraints on the thermal structure, chemistry, and
cloud properties of the atmosphere. Our analysis shows that the observations are consistent with a
strong thermal inversion beginning at ∼104 Pa on the dayside, solar to subsolar metallicity Z (i.e.,
−0.77 < log(Z) < 0.05), and super-solar C/O ratio (i.e., 0.59 < C/O < 0.87). More importantly,
utilizing the high signal-to-noise ratio and repeated observations of the planet, we identify the following
unambiguous time-varying signals in the data: i) a shift of the putative hotspot offset between the
two phase-curves and ii) varying spectral signatures in the transits and eclipses. By simulating the
global dynamics of WASP-121 b atmosphere at high-resolution, we show that the identified signals are
consistent with quasi-periodic weather patterns, hence atmospheric variability, with signatures at the
level probed by the observations (∼5% to ∼10%) that change on a timescale of ∼5 planet days; in
the simulations, the weather patterns arise from the formation and movement of storms and fronts,
causing hot (as well as cold) patches of atmosphere to deform, separate, and mix in time.
This document describes observations of the Seyfert 1 galaxy Mrk 509 using the Cosmic Origins Spectrograph (COS) on the Hubble Space Telescope (HST). The observations detected absorption features in the ultraviolet spectrum, which are attributed to outflowing gas from the active galactic nucleus as well as gas in the galaxy's interstellar medium and halo. The COS observations provide higher signal-to-noise and resolution than previous observations, detecting additional complexity in the absorption features. Variability in some features constrains the distances of absorbing gas components to be less than 250 pc and 1.5 kpc from the active nucleus. The absorption lines only partially cover the emission from the active nucleus, possibly due to
MUSE sneaks a peek at extreme ram-pressure stripping events. I. A kinematic s...Sérgio Sacani
- MUSE observations of the galaxy ESO137-001 reveal an extended gaseous tail over 30 kpc long traced by H-alpha emission, providing evidence of an extreme ram pressure stripping event as the galaxy falls into the massive Norma galaxy cluster.
- Analysis of the H-alpha kinematics and stellar velocity field show that ram pressure has removed the interstellar medium from the outer disk while the primary tail is still fed by gas from the galaxy center, with gravitational interactions not appearing to be the main mechanism of gas removal.
- The stripped gas retains evidence of the disk's rotational velocity out to around 20 kpc downstream, indicating the galaxy is moving radially along the plane of the sky, while
This document describes observations of the galaxy ESO137-001 using the MUSE instrument on the VLT. The key points are:
1) MUSE observations reveal an extended gas tail stretching over 30 kpc from the galaxy, tracing ongoing ram pressure stripping as it falls into the Norma galaxy cluster.
2) Analysis of the gas kinematics and stellar velocity field show that ram pressure has removed the interstellar medium from the outer disk while the primary tail is still fed by gas from the galaxy center.
3) The stripped gas retains evidence of the disk's rotational velocity out to 20 kpc downstream, indicating the galaxy is moving radially through the cluster. Beyond this the gas shows greater turbulence,
Eccentricity from transit_photometry_small_planets_in_kepler_multi_planet_sys...Sérgio Sacani
Artigo descreve estudo que mostra que a órbita dos exoplanetas terrestres são na sua maioria órbitas circulares, o que é bom para se procurar por vida e o que vem causando uma revolução no entendimento sobre os sistemas de exoplanteas.
The document summarizes findings from the Microwave Instrument on the Rosetta Orbiter (MIRO) regarding the subsurface properties and early activity of comet 67P/Churyumov-Gerasimenko. Key points:
- MIRO detected water vapor emissions from the comet beginning in early June 2014 and measured the total water production rate, which varied from 0.3 kg/s to 1.2 kg/s between June and August.
- Water outgassing displayed periodic variations correlated with the comet's 12.4-hour rotation period and seemed to originate primarily from the comet's "neck" region.
- Subsurface temperatures measured by MIRO showed seasonal and diurnal variations, indicating radiation
This document summarizes the results of a 180 ks Chandra-LETGS observation of Mrk 509 as part of a larger multi-wavelength campaign. The observation detected several absorption features in the X-ray spectrum originating from an ionized absorber, including ions with three distinct ionization degrees. The lowest ionized component is slightly redshifted and not in pressure equilibrium with the others, likely belonging to the host galaxy's interstellar medium. The other two components are outflowing at velocities of around -200 and -455 km/s. Simultaneous HST-COS observations detected 13 UV kinematic components, and at least three can be associated with the X-ray components, providing evidence that the UV and X-
TEMPORAL EVOLUTION OF THE HIGH-ENERGY IRRADIATION AND WATER CONTENT OF TRAPPI...Sérgio Sacani
The ultracool dwarf star TRAPPIST-1 hosts seven Earth-size transiting planets, some of which could
harbour liquid water on their surfaces. UV observations are essential to measure their high-energy
irradiation, and to search for photodissociated water escaping from their putative atmospheres. Our
new observations of TRAPPIST-1 Ly-α line during the transit of TRAPPIST-1c show an evolution of
the star emission over three months, preventing us from assessing the presence of an extended hydrogen
exosphere. Based on the current knowledge of the stellar irradiation, we investigated the likely history
of water loss in the system. Planets b to d might still be in a runaway phase, and planets within the
orbit of TRAPPIST-1g could have lost more than 20 Earth oceans after 8 Gyr of hydrodynamic escape.
However, TRAPPIST-1e to h might have lost less than 3 Earth oceans if hydrodynamic escape stopped
once they entered the habitable zone. We caution that these estimates remain limited by the large
uncertainty on the planet masses. They likely represent upper limits on the actual water loss because
our assumptions maximize the XUV-driven escape, while photodissociation in the upper atmospheres
should be the limiting process. Late-stage outgassing could also have contributed significant amounts
of water for the outer, more massive planets after they entered the habitable zone. While our results
suggest that the outer planets are the best candidates to search for water with the JWST, they also
highlight the need for theoretical studies and complementary observations in all wavelength domains
to determine the nature of the TRAPPIST-1 planets, and their potential habitability.
Keywords: planetary systems - Stars: individual: TRAPPIST-1
Spirals and clumps in V960 Mon: signs of planet formation via gravitational i...Sérgio Sacani
The formation of giant planets has traditionally been divided into two pathways: core accretion and gravitational instability. However, in recent years, gravitational instability has become less favored, primarily due
to the scarcity of observations of fragmented protoplanetary disks around young stars and low occurrence rate
of massive planets on very wide orbits. In this study, we present a SPHERE/IRDIS polarized light observation
of the young outbursting object V960 Mon. The image reveals a vast structure of intricately shaped scattered
light with several spiral arms. This finding motivated a re-analysis of archival ALMA 1.3 mm data acquired
just two years after the onset of the outburst of V960 Mon. In these data, we discover several clumps of continuum emission aligned along a spiral arm that coincides with the scattered light structure. We interpret the
localized emission as fragments formed from a spiral arm under gravitational collapse. Estimating the mass of
solids within these clumps to be of several Earth masses, we suggest this observation to be the first evidence of
gravitational instability occurring on planetary scales. This study discusses the significance of this finding for
planet formation and its potential connection with the outbursting state of V960 Mon.
An elevation of 0.1 light-seconds for the optical jet base in an accreting Ga...Sérgio Sacani
Relativistic plasma jets are observed in many systems that
host accreting black holes. According to theory, coiled magnetic
fields close to the black hole accelerate and collimate the
plasma, leading to a jet being launched1–3. Isolating emission
from this acceleration and collimation zone is key to measuring
its size and understanding jet formation physics. But this
is challenging because emission from the jet base cannot
easily be disentangled from other accreting components. Here,
we show that rapid optical flux variations from an accreting
Galactic black-hole binary are delayed with respect to X-rays
radiated from close to the black hole by about 0.1 seconds, and
that this delayed signal appears together with a brightening
radio jet. The origin of these subsecond optical variations
has hitherto been controversial4–8. Not only does our work
strongly support a jet origin for the optical variations but it
also sets a characteristic elevation of ≲ 103 Schwarzschild
radii for the main inner optical emission zone above the black
hole9, constraining both internal shock10 and magnetohydrodynamic11
models. Similarities with blazars12,13 suggest that jet
structure and launching physics could potentially be unified
under mass-invariant models. Two of the best-studied jetted
black-hole binaries show very similar optical lags8,14,15, so this
size scale may be a defining feature of such systems.
Similar to WASP-69b’s Escaping Envelope Is Confined to a Tail Extending at Least 7 Rp (20)
The binding of cosmological structures by massless topological defectsSérgio Sacani
Assuming spherical symmetry and weak field, it is shown that if one solves the Poisson equation or the Einstein field
equations sourced by a topological defect, i.e. a singularity of a very specific form, the result is a localized gravitational
field capable of driving flat rotation (i.e. Keplerian circular orbits at a constant speed for all radii) of test masses on a thin
spherical shell without any underlying mass. Moreover, a large-scale structure which exploits this solution by assembling
concentrically a number of such topological defects can establish a flat stellar or galactic rotation curve, and can also deflect
light in the same manner as an equipotential (isothermal) sphere. Thus, the need for dark matter or modified gravity theory is
mitigated, at least in part.
EWOCS-I: The catalog of X-ray sources in Westerlund 1 from the Extended Weste...Sérgio Sacani
Context. With a mass exceeding several 104 M⊙ and a rich and dense population of massive stars, supermassive young star clusters
represent the most massive star-forming environment that is dominated by the feedback from massive stars and gravitational interactions
among stars.
Aims. In this paper we present the Extended Westerlund 1 and 2 Open Clusters Survey (EWOCS) project, which aims to investigate
the influence of the starburst environment on the formation of stars and planets, and on the evolution of both low and high mass stars.
The primary targets of this project are Westerlund 1 and 2, the closest supermassive star clusters to the Sun.
Methods. The project is based primarily on recent observations conducted with the Chandra and JWST observatories. Specifically,
the Chandra survey of Westerlund 1 consists of 36 new ACIS-I observations, nearly co-pointed, for a total exposure time of 1 Msec.
Additionally, we included 8 archival Chandra/ACIS-S observations. This paper presents the resulting catalog of X-ray sources within
and around Westerlund 1. Sources were detected by combining various existing methods, and photon extraction and source validation
were carried out using the ACIS-Extract software.
Results. The EWOCS X-ray catalog comprises 5963 validated sources out of the 9420 initially provided to ACIS-Extract, reaching a
photon flux threshold of approximately 2 × 10−8 photons cm−2
s
−1
. The X-ray sources exhibit a highly concentrated spatial distribution,
with 1075 sources located within the central 1 arcmin. We have successfully detected X-ray emissions from 126 out of the 166 known
massive stars of the cluster, and we have collected over 71 000 photons from the magnetar CXO J164710.20-455217.
The debris of the ‘last major merger’ is dynamically youngSérgio Sacani
The Milky Way’s (MW) inner stellar halo contains an [Fe/H]-rich component with highly eccentric orbits, often referred to as the
‘last major merger.’ Hypotheses for the origin of this component include Gaia-Sausage/Enceladus (GSE), where the progenitor
collided with the MW proto-disc 8–11 Gyr ago, and the Virgo Radial Merger (VRM), where the progenitor collided with the
MW disc within the last 3 Gyr. These two scenarios make different predictions about observable structure in local phase space,
because the morphology of debris depends on how long it has had to phase mix. The recently identified phase-space folds in Gaia
DR3 have positive caustic velocities, making them fundamentally different than the phase-mixed chevrons found in simulations
at late times. Roughly 20 per cent of the stars in the prograde local stellar halo are associated with the observed caustics. Based
on a simple phase-mixing model, the observed number of caustics are consistent with a merger that occurred 1–2 Gyr ago.
We also compare the observed phase-space distribution to FIRE-2 Latte simulations of GSE-like mergers, using a quantitative
measurement of phase mixing (2D causticality). The observed local phase-space distribution best matches the simulated data
1–2 Gyr after collision, and certainly not later than 3 Gyr. This is further evidence that the progenitor of the ‘last major merger’
did not collide with the MW proto-disc at early times, as is thought for the GSE, but instead collided with the MW disc within
the last few Gyr, consistent with the body of work surrounding the VRM.
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.
Or: Beyond linear.
Abstract: Equivariant neural networks are neural networks that incorporate symmetries. The nonlinear activation functions in these networks result in interesting nonlinear equivariant maps between simple representations, and motivate the key player of this talk: piecewise linear representation theory.
Disclaimer: No one is perfect, so please mind that there might be mistakes and typos.
dtubbenhauer@gmail.com
Corrected slides: dtubbenhauer.com/talks.html
Remote Sensing and Computational, Evolutionary, Supercomputing, and Intellige...University of Maribor
Slides from talk:
Aleš Zamuda: Remote Sensing and Computational, Evolutionary, Supercomputing, and Intelligent Systems.
11th International Conference on Electrical, Electronics and Computer Engineering (IcETRAN), Niš, 3-6 June 2024
Inter-Society Networking Panel GRSS/MTT-S/CIS Panel Session: Promoting Connection and Cooperation
https://www.etran.rs/2024/en/home-english/
The ability to recreate computational results with minimal effort and actionable metrics provides a solid foundation for scientific research and software development. When people can replicate an analysis at the touch of a button using open-source software, open data, and methods to assess and compare proposals, it significantly eases verification of results, engagement with a diverse range of contributors, and progress. However, we have yet to fully achieve this; there are still many sociotechnical frictions.
Inspired by David Donoho's vision, this talk aims to revisit the three crucial pillars of frictionless reproducibility (data sharing, code sharing, and competitive challenges) with the perspective of deep software variability.
Our observation is that multiple layers — hardware, operating systems, third-party libraries, software versions, input data, compile-time options, and parameters — are subject to variability that exacerbates frictions but is also essential for achieving robust, generalizable results and fostering innovation. I will first review the literature, providing evidence of how the complex variability interactions across these layers affect qualitative and quantitative software properties, thereby complicating the reproduction and replication of scientific studies in various fields.
I will then present some software engineering and AI techniques that can support the strategic exploration of variability spaces. These include the use of abstractions and models (e.g., feature models), sampling strategies (e.g., uniform, random), cost-effective measurements (e.g., incremental build of software configurations), and dimensionality reduction methods (e.g., transfer learning, feature selection, software debloating).
I will finally argue that deep variability is both the problem and solution of frictionless reproducibility, calling the software science community to develop new methods and tools to manage variability and foster reproducibility in software systems.
Exposé invité Journées Nationales du GDR GPL 2024
ANAMOLOUS SECONDARY GROWTH IN DICOT ROOTS.pptxRASHMI M G
Abnormal or anomalous secondary growth in plants. It defines secondary growth as an increase in plant girth due to vascular cambium or cork cambium. Anomalous secondary growth does not follow the normal pattern of a single vascular cambium producing xylem internally and phloem externally.
Nucleophilic Addition of carbonyl compounds.pptxSSR02
Nucleophilic addition is the most important reaction of carbonyls. Not just aldehydes and ketones, but also carboxylic acid derivatives in general.
Carbonyls undergo addition reactions with a large range of nucleophiles.
Comparing the relative basicity of the nucleophile and the product is extremely helpful in determining how reversible the addition reaction is. Reactions with Grignards and hydrides are irreversible. Reactions with weak bases like halides and carboxylates generally don’t happen.
Electronic effects (inductive effects, electron donation) have a large impact on reactivity.
Large groups adjacent to the carbonyl will slow the rate of reaction.
Neutral nucleophiles can also add to carbonyls, although their additions are generally slower and more reversible. Acid catalysis is sometimes employed to increase the rate of addition.
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/
ESPP presentation to EU Waste Water Network, 4th June 2024 “EU policies driving nutrient removal and recycling
and the revised UWWTD (Urban Waste Water Treatment Directive)”
When I was asked to give a companion lecture in support of ‘The Philosophy of Science’ (https://shorturl.at/4pUXz) I decided not to walk through the detail of the many methodologies in order of use. Instead, I chose to employ a long standing, and ongoing, scientific development as an exemplar. And so, I chose the ever evolving story of Thermodynamics as a scientific investigation at its best.
Conducted over a period of >200 years, Thermodynamics R&D, and application, benefitted from the highest levels of professionalism, collaboration, and technical thoroughness. New layers of application, methodology, and practice were made possible by the progressive advance of technology. In turn, this has seen measurement and modelling accuracy continually improved at a micro and macro level.
Perhaps most importantly, Thermodynamics rapidly became a primary tool in the advance of applied science/engineering/technology, spanning micro-tech, to aerospace and cosmology. I can think of no better a story to illustrate the breadth of scientific methodologies and applications at their best.
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.
2. note that the photometric observations do not contain velocity
information.
In this paper, we provide a new view of the WASP-69b
outflow using Keck/NIRSPEC. Relative to CARMENES,
NIRSPEC collects more photons per transit, resulting in a
higher signal-to-noise (S/N) and allows for a more detailed
examination of the tail geometry and velocity structure.
We describe our Keck/NIRSPEC observations in Section 2.
We explain the data reduction process in Section 3. We
characterize the strength, time dependence, and velocity
structure of the outflow in Section 4. We estimate the mass-
loss rate in Section 5. We discuss comparisons with previous
observations and place our observations of WASP-69b in the
broader context of He I detections in Section 6. Finally, we
conclude in Section 7 with a discussion of our WASP-69b
interpretation and potential future work on this system as well
as others.
2. Observations
On 2019 July 12 UT, we observed the transit of WASP-69b
(see Table 1 for system parameters) using Keck/NIRSPEC
(McLean et al. 1998; Martin et al. 2018). We used the
NIRSPEC-1 filter (λ = 9470–11210 Å) and the 0 28 × 12″ slit,
which provides a resolving power of R = 40,000; at the He
feature, this corresponds to Δλ = 0.3 Å or Δv = 7.5 km s−1
.
Following previous works, we removed the “thin” blocking
filter to eliminate CCD fringing in the Y-band. On 2022 August
2 UT we observed WASP-69 again using the same setup and
reduction listed throughout this paper. However, due to a time-
scheduling error, we did not observe the transit of WASP-69b.
However, this did allow us to obtain an out-of-transit baseline
for WASP-69, which we use to further constrain He I
variability in the stellar atmosphere. These observations
occurred during orbital phase f = [−0.30, − 0.22] compared
to the transit midpoint at phase of f = 0.
We scheduled our observations using the ephemeris of
Casasayas-Barris et al. (2017). The transit midpoint occurred at
12:20 UT with ± 2.1 minute midpoint uncertainty. We used the
ABBA nod-dithering technique to remove signal from the
background and collected 104 exposures of WASP-69 with
integration times of 149 s from UT = 09:25–14:44. The first
observation began 108 minutes before ingress when the target
was at airmass = 1.44; the last observation ended when the
target was at airmass = 1.46. We lost guiding on two frames in
the WASP-69 sequence during egress. Additionally, we
observed two nearby rapidly rotating A0V stars for telluric
calibration at the beginning and end of the WASP-69 observing
sequence: HIP102631 (airmass = 1.35, v sin(i) = 142 km s−1
)
and HIP105315 (B9V, airmass = 1.62, v sin(i) = 200 km s−1
).
3. Data Reduction
We reduced 104 raw observations using the NIRSPEC
Reduction Package, REDSPEC (Kim et al. 2015).4
We focused
Table 1
WASP-69b: Physical, Orbital, and System Parameters
Parameter Unit Value Reference
Teff [K] 4700 ± 50 Casasayas-Barris et al. (2017)
Age [Gyr] 7.0 Casasayas-Barris et al. (2017)
Fe/H ... 0.150 ± 0.080 Bonomo et al. (2017)
Må [Me] 0.826 ± 0.029 Casasayas-Barris et al. (2017)
Rå [Re] 0.813 ± 0.028 Casasayas-Barris et al. (2017)
v sin(iå) [km s−1
] 2.20 ± 0.40 Casasayas-Barris et al. (2017)
log g [cm s−2
] 4.50 ± 0.15 Stassun et al. (2017)
γ [km s−1
] −9.62826 ± 0.00023 Anderson et al. (2014)
Mp [MJ] 0.2600 ± 0.0185 Casasayas-Barris et al. (2017)
Rp [RJ] 1.057 ± 0.017 Casasayas-Barris et al. (2017)
Teq [K] 963 ± 18 Casasayas-Barris et al. (2017)
Kp [m s−1
] 38.1 ± 2.4 Casasayas-Barris et al. (2017)
a [au] 0.04525 ± 0.00075 Casasayas-Barris et al. (2017)
a/Rå ... 12.00 ± 0.46 Casasayas-Barris et al. (2017)
Tc [BKJD] 915.8334 ± 0.0002 Casasayas-Barris et al. (2017)
P [d] 3.8681390 ± 0.0000017 Casasayas-Barris et al. (2017)
T14 [hr] 2.23 ± 0.023 Casasayas-Barris et al. (2017)
ip [deg] 86.71 ± 0.20 Casasayas-Barris et al. (2017)
e ... 0 Casasayas-Barris et al. (2017)
b ... 0.686 ± 0.023 Casasayas-Barris et al. (2017)
Figure 1. The two calibration stars, HIP102631 (red) and HIP105315 (orange),
are shown here with a slight offset. The nearby telluric absorption features at
10835.9 and 10837.8 Å are marked with blue. A representative WASP-69
exposure is shown in black and conveys the spectral region, instrument
resolution, and signal-to-noise ratio. The three dashed gray lines indicate the
He I 10830 Å triplet vacuum rest wavelengths. The main core of the profile
comes from the 10833.22 and 10833.31 Å features, which are blended. The
weaker singlet is located at 10832.06 Å.
4
https://github.com/Keck-DataReductionPipelines/NIRSPEC-Data-
Reduction-Pipeline
2
The Astrophysical Journal, 960:123 (9pp), 2024 January 10 Tyler et al.
3. on échelle order 70, which encompasses the He I triplet
transition lines. In this work, we adopt a vacuum wavelength
scale for the He I triplet transitions (10832.06, 10833.22, and
10833.31 Å). We established our laboratory wavelength
solution using Neon, Argon, Xenon, and Krypton arc lamps
provided by NIRSPEC website.5
We derived an initial wavelength solution and reduced each
AB and BA nod pair into single, combined 1D frames. We
used the suggested S/N measurement formula for the 2018
NIRSPEC update and report a S/N of ≈55 per reduced pixel.
Due to the target hopping off of the slit mentioned in the
previous section, there is a small gap of missing data in our
time series that occurs just as the the planet begins egress.
We used REDSPEC to identify bad pixels and cosmic-ray
hits and interpolated over them using a cubic spline.
We used the calibration star spectra to identify telluric
features in the target spectrum and inspect for contamination of
the He I profile. We identify nearby H2O absorption lines at
10835.9 and 10837.8 Å, but they do not interfere with the
absorbing He I band as shown in Figure 1.
We shifted the spectra to the stellar rest frame by cross-
correlating each spectrum with a PHOENIX stellar template
model (Husser et al. 2013) with the following parameters:
Teff = 4700 K; log(g) = 4.5; [M/H] = 0.0). We masked out the
He I absorbing region (10830–10835 Å) as well as any telluric
features so they do not influence our spectral registration.
We fit the resulting cross-correlation function peaks with
Gaussian profiles and determined velocity shifts for each
spectrum. These shifts ranged from 19 to 21 km s−1
and
included barycentric Doppler shifts and instrument variability.
With our observations now shifted into the stellar rest frame,
we co-added the spectra into three distinct bins: pre-transit, in-
transit, and post-transit (see Table 2). We computed the average
spectrum for each bin and plot the composite spectra and
corresponding shifts in Figure 2. To interpret the outflow with
respect to the WASP-69b, we now calculate the projected
velocity of the planet and shift the spectra into the planetary
rest frame.
Table 2
Observations
Target Observation Date of observation Start Time End Time Airmass range Nobs texp S/N per pixel range
(UT) (UT) (s)
HIP102631 Telluric Std 2019-07-12 09:09 09:12 1.36–1.34 4 50 50
WASP-69 Pre-Transit 2019-07-12 09:25 11:06 1.44–1.14 34 149 35–60
WASP-69 In-Transit 2019-07-12 11:09 13:32 1.13–1.19 42 149 50–62
WASP-69 Post-Transit 2019-07-12 13:36 14:47 1.20–1.48 24 149 51–58
HIP105315 Telluric Std 2019-07-12 14:59 15:06 1.6–1.64 4 100 50
WASP-69 Out-of-Transit 2022-08-02 05:58 13:45 1.07–3.47 74 149 25–42
Figure 2. Colors in the main panel show the depth of each normalized spectrum relative to a master template made up of all pre-transit observations, i.e., 1.0
corresponds to no excess absorption. Missing data are gray, and the vertical white lines encompass the defined He I bandwidth (see Section 2 for further details). The
top panel shows the green master spectrum for WASP-69 and the orange HIP105315 telluric standard spectrum for which we have applied an arbitrary vertical offset
for clarity. Telluric absorption features are indicated with blue vertical lines and coincide with the transient vertical artifacts in the plot. The right panel shows the
velocity shift between the PHOENIX model and each frame.
5
https://www2.keck.hawaii.edu/inst/nirspec/lines.html
3
The Astrophysical Journal, 960:123 (9pp), 2024 January 10 Tyler et al.
4. 4. Results
In Figure 3, we show the normalized pre-transit, in-transit,
and post-transit absorption profiles in the He I band with
respect to the central rest wavelength positions of the He I
triplet. Excess absorption is clearly visible in-transit and post-
transit. The difference in absorption depth and width of the
bluer wing of the profile is evident.
In Figure 4, we plot the relative absorption intensity in both
the stellar and planetary rest frames. The first through fourth
contact points are shown as well as the central positions of the
He I 10830 Å triplet. We report an average in-transit absorption
depth of 2.7% ± 0.4%. We estimated the uncertainty over the
He I 10830 Å bandwidth [10831.58–10833.99 Å] by measuring
the standard deviation of the average normalized intensity in
neighboring bins of equal extent in time and wavelength. This
dispersion captures the photon-counting statistics and instru-
mental errors associated with variations in wavelength solution
and line profile. Assuming a spherical outflow geometry, the
relative absorption depth tells us about the extent to which the
extended exosphere is enveloping the planet.
We computed the velocity of the He I triplet by modeling the
profile of the line with 3 Gaussians, each corresponding to the
three central wavelengths of the metastable He I transition. We
fixed the relative heights and wavelength between the
transitions and allowed two parameters to vary: the total depth
and the central wavelength. During the in-transit observations,
we detect a net blueshift of −5.9 ± 1.0 km s−1
. This radial
velocity shift in the absorption profile can trace the bulk
velocity structure of the outflowing He I.
We can see that the excess absorption continues for the entire
post-transit sequence (1.28 hr). Furthermore, the absorbing He I
is blueshifted for the duration of the transit and accelerates
away from the star. This excess He I absorption post-transit is
consistent with a “comet-like” tail of helium trailing the planet
and continuing to absorb stellar photons while being
accelerated away from the planet and toward the observer
due to stellar winds. As the planet has traveled over 7 Rp
beyond the disk, a continually thinning column of He I is still
detected.
These tails are shaped by stellar winds that interact with the
planetary outflow and redirect material around the planet,
radially away from the star (MacLeod & Oklopčić 2022).
McCann et al. (2019) showed that the degree to which the
planetary outflow is shaped is a function of orbital velocity,
Figure 3. The He I feature is deeper in-transit (blue spectrum) and post-transit (red spectrum) compared to pre-transit (black spectrum). Gray dashed lines represent the
central rest wavelengths in the stellar rest frame.
Figure 4. Left: same as Figure 2 but detailing the He I triplet. T1, T2, T3, and T4 label the four transit contact times. The three white dashed lines represent the expected
motion of the He I transition lines in the stellar rest frame due to the predicted planetary velocity. Right: same as left but shifted into the planetary rest frame. Two
separate helium bandpasses used to sum up the helium light curve are plotted as vertical orange solid line and red dotted lines. The orange vertical lines represent our
preferred bandpass. The red dotted lines are comparable to the bandpass used in other data sets.
4
The Astrophysical Journal, 960:123 (9pp), 2024 January 10 Tyler et al.
5. intrinsic planetary wind velocity, and stellar wind strength—
which can be variable itself. While weak stellar winds cannot
confine the planetary outflow, a strong stellar wind can
suppress the outflow and redirect the majority of the out-
gassed material into the tail. Observational evidence of this was
first seen in Lyα detections, the most extreme for the hot-
Neptune GJ436b (Lavie et al. 2017) which has a hydrogen tail
that continues absorbing for several hours after the optical
transit ends.
The time asymmetry of the absorption profile is consistent
with interactions between planetary outflows and strong
stellar winds (MacLeod & Oklopčić 2022). In general, a
planetary outflow will form a bow shock at the point where
the outflow ram pressure ρv2
equals the ram pressure of the
stellar wind. Multiple groups have shown that for sufficiently
strong stellar winds, the planetary outflow can be suppressed
below the sonic surface and completely redirected around the
planet and toward the tail (Wang & Dai 2021a; MacLeod &
Oklopčić 2022).
To probe the extent of the absorption, we computed the
equivalent width for the spectral time series. We defined the
He I absorbing band [10831.58–10833.99 Å] to include the full
wavelength range where excess absorption is detected
(Figure 2).
We report a maximum EW just after mid-transit of
40.7 mÅ ± 6.8 mÅ. During the transit (T14), we find an average
equivalent width (EW) of 27.8 mÅ ± 2.5 mÅ. As shown in
Figure 5, the post-transit equivalent width never returns to the
pre-transit baseline. We compute an average EW of
15.4 mÅ ± 3.9 mÅ during the post-transit phase. Here the time
asymmetry can be seen clearly, and in the last observation
(1.28 hr after T4) we report an EW 5% higher than the pre-
transit average.
Simulations show that stellar winds can not only cause time
asymmetry in the relative equivalent width absorption of the
He I feature but also shift the peak of maximal absorption
relative to the optical point of conjunction (Wang &
Dai 2021a; MacLeod & Oklopčić 2022). After the peak
absorption, the decrease in absorption transitions in to a more
gradual return to the pre-transit baseline that can take several
hours.
Assuming a circular orbit, we calculate WASP-69b’s orbital
velocity vorb = 2π ap/P = 127.3 ± 1.5 km s−1
. In the 1.28 hr
of post-transit observations that we detect continued absorp-
tion, the planet travels ∼ 5.9 × 105
km. Assuming all of the
helium we are seeing is confined to a partial annulus at the
orbital separation of the planet, we set a minimum limit on the
length of the He I tail 7.5 Rp. The Roche lobe for WASP-69b
is located at ≈2.7 Rp, but the tail extends well beyond that
limit and is unbound from the gravitational influence of the
planet. A simple diagram of the transit chord can be seen in
Figure 6.
Figure 5. Equivalent width variations over the course of the night. The red
dashed lines represent the four contact points, and the horizontal orange dashed
line shows the pre-transit baseline, which is not recovered. The maximal depth
is slightly delayed compared to mid-transit, as predicted by modeling strong
stellar wind interactions that shape planetary outflows.
Figure 6. Transit chord and top-down view of the WASP-69 system presented to scale. Left: transit chord view from Keck. The four contact points, T1, T2, T3, and T4
are represented with vertical black dashed lines and the absorbing He I is light blue. The red dashed line represents the final predicted position of the planet
corresponding to the last observation in the spectral time series after traveling over 7 Rp (1.28 hr) beyond the disk of the star from the perspective of the observer.
Right: top-down view of the system. The He I tail can be seen accelerating toward the observer on the lower right of the panel.
5
The Astrophysical Journal, 960:123 (9pp), 2024 January 10 Tyler et al.
6. 5. Mass-loss Rate Estimate
One of the main goals for tracing He I is to quantitatively
measure mass-loss rates in real time. A detailed model of this
outflow would include effects like Coriolis force and advection
coupled with a 3D radiative transfer scheme and is beyond the
scope of this work (see, e.g., Wang & Dai 2021b). Here, we
offer two estimates of the mass-loss rate of WASP-69b: (1) an
order-of-magnitude estimate following the method of Zhang
et al. (2022) and (2) an estimate assuming a 1D Parker-like
outflow.
5.1. Order of Magnitude
We assumed that most of the planetary outflow is optically
thin, which is consistent with the weakness of the singlet
centered near 10832 Å. We then take the optical depth from
star to observer to be
t l s l
= l
n P , 1
He
( ) ( ) ( )
where nHe is the column density of metastable helium atoms,
P(λ) is the line profile with ò l l =
-¥
+¥
P d 1
( ) , and the
absorption cross section is σλ ≡ p l
e g f m c
l l e
2
0
2 2
( ) ( ). Here, e
is the electron charge, me is the electron mass, gl is the
statistical weight for the lower level, fl is the oscillator strengths
of the three lines (0.059, 0.179, and 0.299, respectively;
Kramida et al. 2022), and λ0 is the rest wavelength of the
absorbing spectral line. Assuming the optically thin limit where
1 − e− τ
≈ τ, we integrate over λ and obtain the standard
equation for equivalent width:
s
=
l l
W N . 2
( )
Defining the average equivalent width Wavg, we can solve for
the total number of metastable helium atoms NHe S
3
2 by
integrating over and dividing by the cross-sectional area of
the star:
s p
l
=
=
=
=
l
l
l
W
dS
W dS
W dS W dS
N W R
N
R m c
e g f
W
1
. 3
e
l l
avg
avg
He S avg
2
He S
2 2
2
0
2 avg
3
2
3
2
*
*
∬
∬
∬ ∬
( )
Using our calculated EW measurement for Wavg, we
calculate = ´
N 3.1 10
He S
32
3
2 , which we can convert into a
total amount of helium, assuming metastable helium comprises
10−6
of total helium nuclei. This fraction assumes an optimistic
case that applies to early K-type stars (as shown in
Oklopčić 2019). Assuming primordial mass and number
composition ratios for helium to hydrogen, 3:1 and 9:1
respectively, we estimate the total mass of the planetary
outflow in helium and hydrogen to be mtot = 1 × 1016
g. With
this mass estimate, we can estimate a total mass-loss rate
mtot/τ, where the replenishment lifetime for observable He I
atoms crossing the stellar disk is τ = Rå/cs and where cs is the
sound speed. We adopt 10 km s−1
, which is consistent with a
typical sound speed for planets with these outflows. Our order-
of-magnitude mass-loss estimate is t
= = Å
M m M
1
tot
Gyr−1
or 1.8 × 1011
g s−1
.
5.2. One-dimensional Parker Model
As an alternative to our order-of-magnitude estimate, we use
p-winds (Dos Santos et al. 2022) to estimate a mass-loss rate
by fitting a Parker wind model to our observations. p-winds
is an open-source code that implements the 1D model
described by Oklopčić & Hirata (2018) and Lampón et al.
(2020) and takes as input the stellar XUV spectrum and the
observed Helium transmission spectrum.
As noted, the 1D model is insufficient for modeling outflows
with significant asymmetry; however, it is a useful point of
comparison to our order-of-magnitude model and to previous
observations. Since the X-ray and ultraviolet (XUV) spectrum
of WASP-69 is not known, we obtained the MUSCLES XUV
spectrum (λ = 10–1000 Å hν = 1200–12 eV) of similar star
HD85512 (K5) as a proxy for WASP-69. The MUSCLES
spectra are observed XUV fluxes at Earth, which are then
scaled to the appropriate semimajor axis for WASP-69b.
With p-winds, we derived a sound speed of 9 km s−1
at the
sonic point, which occurs at ∼3 Rp. For a Parker-type
hydrodynamic wind, this effectively represents the regime
where the pressure-driven flow is no longer being controlled by
the planet's gravity. We derived a temperature in this part of the
thermosphere of 9900 ± 900 K. We found the total fraction of
helium in the metastable state to be 5.4 × 10−6
, in agreement
with the optimistic case for the environment around a K-type
star (Oklopčić 2019). The estimated mass-loss rate for the 1D
model is mtot/τ = 1 M⊕ Gyr−1
(2.0 × 1011
g s−1
).
We note as a sanity check that the assumptions made in our
order-of-magnitude estimate are comparable with the
p-winds 1D results. Given the difference in these
approaches, the agreement is better than expected, and we
trust both methods at the order-of-magnitude level.
Assuming a constant orbital distance and stellar output over
time, the current mass-loss rate suggests that WASP-69b has
lost ∼ 7 M⊕ over the course of the system’s ∼ 7 Gyr lifetime.
At the current rate, WASP-69b (92 M⊕) is not at risk of losing
its envelope before the end of the lifetime of the system.
In the 2022 out-of-transit spectrum for WASP-69, which can
be seen in Figure 7, we measured a variability over the main
core of the stellar He I triplet of 0.29% throughout the night.
These variations fall below our noise floor. We report a pre-
transit EW average in 2019 of 0.23 ± 0.03Å. We compare this
to the averaged EW we measured for the 2022 WASP-69 out-
of-transit time series of 0.18 ± 0.03Å. The absolute difference
in EW between both out-of-transit epochs is 0.05 ± 0.06 Å.
While we do not see any evidence for significant variation
within the night on 2022, this does not rule out more long-term
variability in the stellar He I line, or that the pre-transit EW
from 2019 was partially contaminated by the “leading arm” of
the planetary outflow.
6. Comparison to Previous Observations
Our in-transit analysis is consistent with previous CAR-
MENES observations made by Nortmann et al. (2018),
who reported a blueshift of −3.58 ± 0.23 km s−1
and
3.59% ± 0.19% excess absorption (compared to our values
−5.9 ± 1.0 km s−1
and 2.7% ± 0.4% excess absorption). We
note here that our values are measured from an average of the
entire transit (T14), whereas the CARMENES values come
from the average during T23 when the signal is the strongest.
Although our measured values are in agreement, this difference
6
The Astrophysical Journal, 960:123 (9pp), 2024 January 10 Tyler et al.
7. does result in a lower reported absorption during our analysis.
However, our post-transit results are inconsistent with their
measurements. Nortmann et al. (2018) reported an average
post-transit absorption of 0.5% and net blueshift of
−10.7 ± 1.0 km s−1
. During the same phase, we detected an
average post-transit absorption of 1.5 ± 0.2% and a net
blueshift of −23.3 ±0.9 km s−1
(Figure 8). This is a significant
difference and can be seen in the helium light-curve
comparison for the post-transit sequence in Figure 9. The
scatter in the CARMENES data is much higher than the formal
uncertainties. Note that this visualization is highly dependent
on the choice of bandpass for helium absorption. CARMENES
(R = 80,000) has a higher resolution than NIRSPEC
(R = 40,000), but it is on a 3.5 m telescope and collected
8 times fewer photons per transit. The 10 m Keck II dish
allowed us to get significantly higher S/N per pixel (∼55
compared to ∼18 for the CARMENES observations), which
likely explains the reported differences between our measure-
ments. In Figure 10 we plot our 2019 He I transmission
spectrum with the 2 nights of data provided by Nortmann et al.
(2018) during T23. The He I 10830 Å triplet is well resolved in
both sets of observations. When the signal is the strongest,
there is less discrepancy between the data sets. However, when
the He I becomes more diffuse, the S/N differences between
the two instruments is the likely cause for the observed
variability in the post-transit tail length. Vissapragada et al.
(2020) reported comparable S/N per pixel as the CARMENES
data set, so the lack of significant post-transit He I absorption in
the WIRC observations can also be explained by lower S/N
levels.
The previous CARMENES observations from Nortmann
et al. (2018) were used in a 3D Hydrodynamics model by
Wang & Dai (2021b). They reported a mass-loss rate
∼0.5 M⊕ Gyr−1
for WASP-69b but no helium tail. Those
results seem consistent with the data set they used. Similarly,
Vissapragada et al. (2020) report a mass-loss rate of
∼ 0.2 M⊕ Gyr−1
, which they computed using the same p-
winds 1D model that assumes a symmetrical planetary
outflow (Oklopčić & Hirata 2018). Our mass-loss rate estimate
Figure 7. WASP-69 out-of-transit spectral time series for 2022 August 2. We
measure a variability over the He I triplet band of 0.29% and report an average
equivalent width of 0.18 ± 0.03 Å
Figure 8. The green points show the averaged in-transit transmission
spectrum of He I 10830 Å absorption. The blue points show the averaged
post-transit transmission spectrum, which is significantly blueshifted
(−23.3 ± 1.0 km s −1
). The gray vertical masks cover nearby telluric
features, and the residuals of the models are shown in the bottom panel.
Figure 9. Helium light curves plotted from this work and 2 nights of
CARMENES observations from Nortmann et al. (2018). The NIRSPEC
observations never return to the baseline post-egress (green). The CARMENES
observations do return to the baseline helium absorption level, at least within
the achieved precision. Note that for the CARMENES data the point-to-point
scatter is significantly higher than the formal uncertainties, which suggests
systematic errors or are simply the effects of a reduced signal with lower
S/N. Plotted in black is the NIRSPEC data but with a reduced bandpass
that is consistent with the He I bandpass of Nortmann et al. (2018)
[10833.07–10833.47 Å] for a better comparison. Our preferred bandpass
(green points) [10831.58–10833.99 Å] allows us to detect lower levels of He I
absorption in the post-transit sequence due to the high S/N of NIRSPEC. Both
helium bandpasses can be seen plotted in Figure 4.
Figure 10. He I 10830 Å absorption during T2 − T3 from Nortmann et al.
(2018) and this work. For reference, the resolving limits are plotted for both
instruments. The He I 10830 Å line is clearly resolved in both cases. Thus, we
can rule out instrument resolution−dependent variability between these
data sets.
7
The Astrophysical Journal, 960:123 (9pp), 2024 January 10 Tyler et al.
8. of 1.0 M⊕ Gyr−1
is higher than both previous results but within
an order of magnitude. We require hydrodynamic 3D-modeling
for the most accurate mass-loss estimate for WASP-69b.
Spake et al. (2021) observed the WASP-107 system with
NIRSPEC and reported similar results to these. WASP-107b
(Mp = 0.1 MJ, Rp = 0.9 RJ) has a 5.7 day orbital period around
a 0.7 Me host star. They reported continued He I absorption for
over an hour post-transit, which corresponds to a He I tail
length of 5.0 × 105
km. At the time, this was the most dramatic
post-transit He I tail observed. At the lower limit of
5.8 × 105
km, the tail of WASP-69b is at least that long.
Another common indicator for the extent of He I abundance
is the equivalent height of the absorbing atmosphere (Nortmann
et al. 2018). Equivalent height is a useful parameter to
characterize the radius of the planet in the He I 10830 Å profile.
Equivalent-height is defined as d = D + -
dR R R
R p p
2 2 1 2
p
( ) ,
where Δd is the transit depth in He I. We can compare this
equivalent height to the lower atmospheric scale height
Heq = (kBTeq)/(μg), where μ = 2.3×mH, which is consistent
with a solar H–He composition, to determine how extended the
absorbing atmosphere is beyond the expected opaque limit of
the atmosphere of a planet with a given temperature.
Figure 11 shows all of the He I 10830 Å detections that we are
aware of in the literature6
and shows the 2 WASP-69b
detections plotted in orange (this work indicated with a star).
For WASP-69b, using our average absorption over the full
transit (T1 − T4) of 2.7% ± 0.4%, we compute dRp
/Heq =
66.1 ± 3.1. We note that our /Heq estimate is about ∼25%
less than the value 85.5 ± 3.6 reported by Nortmann et al.
(2018), but this is only due to a choice of when to average over
the transit chord. Nortmann et al. (2018) report the average
during T23, when the absorption is deeper. Similarly, during T23
of our time series, we measure an average absorption depth of
3.6% ± 0.5% and dRp
/Heq = 83.1 ± 3.9. While we opt to report
the standard average absorption over the course of the transit,
we note that these equivalent-height values are in agreement.
Here we highlight a practical limit for the equivalent-height
metric as a mode of comparison between He I absorption
detections. Because of the dependence on transit depth Δd,
instruments with different resolutions may not derive the same
equivalent height for the same object. As spectral resolution,
=
l
l
D
R , increases, spectral features appear narrower and
deeper. For lower resolution, the same feature will become
broadened and shallow. Thus, the transit depth for the same
system can vary across instruments (or with slit width within
the same instrument). However, what will remain constant is
the total area under the absorption curve.
We suggest a metric that translates better across observation
and instrument parameters such as “equivalent width time”
∫EWdt over the full transit/tail duration. In the case of partial
transits, an alternative measurement that would make sense is
equivalent width per unit orbital phase. This yields a single
number that would normalize comparisons across observations/
instruments in a convenient way. For our observations, we
compute ∫EWdt = 297 ± 50 Å s. We did not reanalyze other
existing data sets to compute this quantity, but such an effort
would bring additional clarity into the census of helium outflows.
Although we can confidently attribute a significant portion of
the observed variability of this system to differences in S/N
between instruments, stellar variability may also contribute.
There are at least three known sources of stellar variability that
could be causing epoch-dependent variations in the He I transit
depth/morphology/velocity structure.
The first is that the He I 10830 Å feature varies in the stellar
atmosphere. However, this seems unlikely, and we did not
measure significant relative He I absorption variability in any of
our out-of-transit observations for WASP-69.
The second source of stellar variability could come from
relative changes in output from different parts of the star’s
electromagnetic spectrum. Although the 23
S metastable state is
most efficiently populated by the EUV/FUV flux ratio of
K-type stars like WASP-69, the extent of variability of those
outputs is not well constrained. Perhaps the tail is significant,
but the fluctuating stellar EUV/FUV levels act as a sort of
variable light source behind the outflow, adjusting the contrast
of what regions of it the observer can detect. As the EUV/FUV
flux ratio becomes more favorable for the metastable state, we
can see lower regions of column density, while higher density
regions become optically thick, and vice versa.
A third source of stellar variability could come from
variations in the stellar wind strength. Work by MacLeod &
Oklopčić (2022) on modeling the extended tail for WASP-107b
demonstrates many of the features we find in our observations:
a delayed absorption peak relative to optical transit, an
asymmetrical He I light curve, and an accelerating blueshift
of gradually decreasing He I absorption hours after egress.
These traits are consistent with interactions of a planetary
outflow being suppressed and redirected due to a strong stellar
wind. This would indicate variability in the physical length of
the tail and could explain why we measured a 7.5 Rp length
tail compared to 2.2 Rp from Nortmann et al. (2018) in
observations made 1 yr prior.
Figure 11. Summary of He I 10830 Å detections. Equivalent height dRp is
normalized by the atmospheric scale height Heq and plotted vs. broadband
XUV flux the planet receives. The WASP-69b observations are both colored
orange, with the results from this work marked with a star. Note that the two
WASP-69b data points agree when the transit depth is averaged over the same
phase of the transit. Data for other known He 10830 Å detections taken from
multiple references (i.e., Kohler 2018; Nortmann et al. 2018; Salz et al. 2018;
Alonso-Floriano et al. 2019; Gaidos et al. 2020; Ninan et al. 2020; Kasper et al.
2020; Vissapragada et al. 2020; dos Santos et al. 2020; Casasayas-Barris et al.
2021; Paragas et al. 2021; Spake et al. 2021; Vissapragada et al. 2021; Kirk
et al. 2022; Orell-Miquel et al. 2022; Czesla et al. 2022; Zhang et al. 2022;
Zhang et al. 2023).
6
Kohler (2018); Nortmann et al. (2018); Salz et al. (2018); Alonso-Floriano
et al. (2019); Gaidos et al. (2020); Ninan et al. (2020); Kasper et al. (2020);
Vissapragada et al. (2020); dos Santos et al. (2020); Casasayas-Barris et al.
(2021); Paragas et al. (2021); Spake et al. (2021); Vissapragada et al. (2021);
Kirk et al. (2022); Orell-Miquel et al. (2022); Czesla et al. (2022); Zhang et al.
(2022); Zhang et al. (2023).
8
The Astrophysical Journal, 960:123 (9pp), 2024 January 10 Tyler et al.
9. It is possible that all three of the sources of stellar variability
mentioned above are linked to one another; they should all vary
with overall variations in stellar activity.
7. Conclusion
In this work, we present high-resolution transmission
spectroscopy of the metastable He I 10830 Å absorption feature
for the WASP-69b transit on 2019 July 12 UT. During the
transit (T14) we detect an average relative helium absorption
level of 2.7% ± 0.4% and a net blueshift of −5.9 ± 1.0 km s−1
.
These values are consistent with the in-transit observations
from Nortmann et al. (2018). The absorption signal is also
consistent with Vissapragada et al. (2020).
However, we detect continued post-transit absorption of
He I, which is not seen in the other observations. This extended
absorption lasts for at least 1.28 hr post-transit and never
returns to the pre-transit baseline. We set a lower limit for the
helium tail 7.5 Rp.
We attribute most of this variability to the high S/N per pixel
NIRSPEC achieves, allowing the detection of smaller amounts
of He I and over a longer period of time. While instrumental
differences surely play a role in these discrepancies, variations
within the star or complicated planetary atmosphere dynamics
could also be responsible.
The asymmetry in the helium absorption curve is consistent
with an outflow being shaped by a strong stellar wind and
requires 3D hydrodynamic modeling for the most accurate
mass-loss estimate. However, we estimate a mass-loss rate of
1 M⊕ Gyr−1
, which we trust within an order of magnitude.
Repeat observations are valuable to probe any variability in
the outflow properties, especially with different instruments.
There is likely variability stemming from multiple sources.
Neither stellar wind strength or EUV/mid-UV output varia-
bility is well understood for stars other than our Sun, so
planetary outflow observations such as these may be a useful
method for studying and constraining certain types of stellar
variability.
Acknowledgments
The helium data presented herein were obtained at the
W. M. Keck Observatory, which is operated as a scientific
partnership among the California Institute of Technology, the
University of California and the National Aeronautics and
Space Administration. The Observatory was made possible by
the generous financial support of the W. M. Keck Foundation.
We thank the referee for a thorough review that helped improve
the quality of this work.
We thank Lisa Nortmann for providing us with the
CARMENES data for WASP-69b which was helpful in
comparing results between observations. We also thank
Michael Zhang and Fei Dai for useful conversations regarding
planetary helium outflows. We would also like to thank Greg
Gilbert for helpful edits of this manuscript. D.T. is supported in
part by the Cota-Robles Fellowship at UCLA, which was
instrumental in the advancement of this research.
ORCID iDs
Dakotah Tyler https:/
/orcid.org/0000-0003-0298-4667
Erik A. Petigura https:/
/orcid.org/0000-0003-0967-2893
Antonija Oklopčić https:/
/orcid.org/0000-0002-9584-6476
Trevor J. David https:/
/orcid.org/0000-0001-6534-6246
References
Alonso-Floriano, F. J., Snellen, I. A. G., Czesla, S., et al. 2019, A&A,
629, A110
Anderson, D. R., Collier Cameron, A., Delrez, L., et al. 2014, MNRAS,
445, 1114
Bonomo, A. S., Desidera, S., Benatti, S., et al. 2017, A&A, 602, A107
Casasayas-Barris, N., Orell-Miquel, J., Stangret, M., et al. October 2021, A&A,
654, A163
Casasayas-Barris, N., Palle, E., Nowak, G., et al. 2017, A&A, 608, A135
Czesla, S., Lampón, M., Sanz-Forcada, J., et al. 2022, A&A, 657, A6
dos Santos, L. A., Ehrenreich, D., Bourrier, V., et al. 2020, A&A, 640, A29
Dos Santos, L. A., Vidotto, A. A., Vissapragada, S., et al. 2022, A&A,
659, A62
Fulton, B. J., Petigura, E. A., Howard, A. W., et al. 2017, AJ, 154, 109
Gaidos, E., Hirano, T., Mann, A. W., et al. 2020, MNRAS, 495, 650
Husser, T. O., Wende-von Berg, S., Dreizler, S., et al. 2013, A&A, 553, A6
Kasper, D., Bean, J. L., Oklopčić, A., et al. 2020, AJ, 160, 258
Kim, S., Prato, L., & McLean, I., 2015 REDSPEC: NIRSPEC data reduction,
Astrophysics Source Code Library, ascl:1507.017
Kirk, J., Dos Santos, L. A., López-Morales, M., et al. 2022, AJ, 164, 24
Kohler, S. 2018, nova pres, 4320
Kramida, A., Ralchenko, Yu., Reader, J. & NIST ASD Team 2022, NIST ASD
Team 2022, NIST Atomic Spectra Database (ver. 5.10) (Gaithersburg, MD:
National Institute of Standards and Technology), https://physics.nist.
gov/asd
Lampón, M., López-Puertas, M., Lara, L. M., et al. 2020, A&A, 636, A13
Lavie, B., Ehrenreich, D., Bourrier, V., et al. 2017, A&A, 605, L7
MacLeod, M., & Oklopčić, A. 2022, ApJ, 926, 226
Martin, E. C., Fitzgerald, M. P., McLean, I. S., et al. 2018, Proc. SPIE, 10702,
107020A
McCann, J., Murray-Clay, R. A., Kratter, K., & Krumholz, M. R. 2019, ApJ,
873, 89
McLean, I. S., Becklin, E. E., Bendiksen, O., et al. 1998, Proc. SPIE, 3354, 566
Ninan, J. P., Stefansson, G., Mahadevan, S., et al. 2020, ApJ, 894, 97
Nortmann, L., Pallé, E., Salz, M., et al. 2018, Sci, 362, 1388
Oklopčić, A. 2019, ApJ, 881, 133
Oklopčić, A., & Hirata, C. M. 2018, ApJL, 855, L11
Orell-Miquel, J., Murgas, F., Pallé, E., et al. 2022, A&A, 659, A55
Owen, J. E., & Wu, Y. 2017, ApJ, 847, 29
Paragas, K., Vissapragada, S., Knutson, H. A., & Oklopčić, A. 2021, AAS
Meeting Abstracts 237, 543.05
Petigura, E. A., Rogers, J. G., Isaacson, H., et al. 2022, AJ, 163, 179
Salz, M., Czesla, S., Schneider, P. C., et al. 2018, A&A, 620, A97
Seager, S., & Sasselov, D. D. 2000, ApJ, 537, 916
Spake, J. J., Oklopčić, A., & Hillenbrand, L. A. 2021, AJ, 162, 284
Spake, J. J., Sing, D. K., Evans, T. M., et al. 2018, Natur, 557, 68
Stassun, K. G., Collins, K. A., & Gaudi, B. S. 2017, AJ, 153, 136
Szabó, G. M., & Kiss, L. L. 2011, ApJL, 727, L44
Vidal-Madjar, A., Lecavelier des Etangs, A., Désert, J. M., et al. 2003, Natur,
422, 143
Vissapragada, S., Knutson, H. A., Jovanovic, N., et al. 2020, AJ, 159, 278
Vissapragada, S., Stefánsson, G., Greklek-McKeon, M., et al. 2021, AJ,
162, 222
Wang, L., & Dai, F. 2021a, ApJ, 914, 99
Wang, L., & Dai, F. 2021b, ApJ, 914, 98
Zhang, M., Knutson, H. A., Dai, F., et al. 2023, AJ, 165, 62
Zhang, M., Knutson, H. A., Wang, L., Dai, F., & Barragán, O. 2022, AJ,
163, 67
9
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