61 research outputs found
Vibrotactile feedback in m-commerce:Stimulating perceived control and perceived ownership to increase anticipated satisfaction
Consumers increasingly purchase through m-channels, including apps. Accordingly, marketers have enhanced immersive, sensorial aspects of m-channels, such as including vibrations while making in-app purchases. Given discrepant findings, it remains unclear whether adding such vibrotactile feedback affects consumer decision making. The present research addresses: (1) Whether adding vibrotactile feedback influences consumers' anticipated product satisfaction and purchase confidence, and (2) if so, how? Through an online pilot survey, two online experiments, and one lab experiment, this research finds that adding vibrotactile feedback to m-channels increases consumers' anticipated product satisfaction, but not purchase confidence. Moreover, perceived ownership mediates this effect, because the vibrations offer a sense of control over the product during the purchase process. This research makes several contributions. First, it documents that control elicited via vibrations offers an alternative means to psychological ownership, as opposed to imagining touch. Second, we offer this haptic route as a means to achieve the stimulation motivation driving perceived ownership, different from prior visual routes. Third, it potentially reconciles literature conflicts regarding the effect of vibrotactile feedback on consumer decision making.</p
APPleSOSS: A Producer of ProfiLEs for SOSS. Application to the NIRISS SOSS Mode
The SOSS mode of the NIRISS instrument is poised to be one of the workhorse
modes for exoplanet atmosphere observations with the newly launched James Webb
Space Telescope. One of the challenges of the SOSS mode, however, is the
physical overlap of the first two diffraction orders of the G700XD grism on the
detector. Recently, the ATOCA algorithm was developed and implemented as an
option in the official JWST pipeline, as a method to extract SOSS spectra by
decontaminating the detector -- that is, separating the first and second
orders. Here, we present APPleSOSS (A Producer of ProfiLEs for SOSS), which
generates the spatial profiles for each diffraction order upon which ATOCA
relies. We validate APPleSOSS using simulated SOSS time series observations of
WASP-52b, and compare it to ATOCA extractions using two other spatial profiles
(a best and worst case scenario on-sky), as well as a simple box extraction
performed without taking into account the order contamination. We demonstrate
that APPleSOSS traces retain a high degree of fidelity to the true underlying
spatial profiles, and therefore yield accurate extracted spectra. We further
confirm that the effects of the order contamination for relative measurements
(e.g., exoplanet transmission or emission observations) is small -- the
transmission spectrum obtained from each of our four tests, including the
contaminated box extraction, deviates by 0.1 from the
atmosphere model input into our noiseless simulations. We further confirm via a
retrieval analysis that the atmosphere parameters (metallicity and C/O)
obtained from each transmission spectrum are consistent at the 1 level
with the true underlying values.Comment: 12 pages, 9 figures. Submitted to PAS
ATOCA: an algorithm to treat order contamination. Application to the NIRISS SOSS mode
After a successful launch, the James Webb Space Telescope is preparing to
undertake one of its principal missions, the characterization of the
atmospheres of exoplanets. The Single Object Slitless Spectroscopy (SOSS) mode
of the Near Infrared Imager and Slitless Spectrograph (NIRISS) is the only
observing mode that has been specifically designed for this objective. It
features a wide simultaneous spectral range (0.6--2.8\,\micron) through two
spectral diffraction orders. However, due to mechanical constraints, these two
orders overlap slightly over a short range, potentially introducing a
``contamination'' signal in the extracted spectrum. We show that for a typical
box extraction, this contaminating signal amounts to 1\% or less over the
1.6--2.8\,\micron\ range (order 1), and up to 1\% over the 0.85--0.95\,\micron\
range (order 2). For observations of exoplanet atmospheres (transits, eclipses
or phase curves) where only temporal variations in flux matter, the
contamination signal typically biases the results by order of 1\% of the
planetary atmosphere spectral features strength. To address this problem, we
developed the Algorithm to Treat Order ContAmination (ATOCA). By constructing a
linear model of each pixel on the detector, treating the underlying incident
spectrum as a free variable, ATOCA is able to perform a simultaneous extraction
of both orders. We show that, given appropriate estimates of the spatial trace
profiles, the throughputs, the wavelength solutions, as well as the spectral
resolution kernels for each order, it is possible to obtain an extracted
spectrum accurate to within 10\,ppm over the full spectral range.Comment: Submitted to PASP. 22 pages, 12 figure
Characterizing the Near-infrared Spectra of Flares from TRAPPIST-1 During JWST Transit Spectroscopy Observations
We present the first analysis of JWST near-infrared spectroscopy of stellar
flares from TRAPPIST-1 during transits of rocky exoplanets. Four flares were
observed from 0.6--2.8 m with NIRISS and 0.6--3.5 m with NIRSpec
during transits of TRAPPIST-1b, f, and g. We discover P and Br
line emission and characterize flare continuum at wavelengths from 1--3.5
m for the first time. Observed lines include H,
P-P, Br, He I 0.7062m, two Ca II
infrared triplet (IRT) lines, and the He I IRT. We observe a reversed Paschen
decrement from P-P alongside changes in the light curve shapes
of these lines. The continuum of all four flares is well-described by blackbody
emission with an effective temperature below 5300 K, lower than temperatures
typically observed at optical wavelengths. The 0.6--1 m spectra were
convolved with the TESS response, enabling us to measure the flare rate of
TRAPPIST-1 in the TESS bandpass. We find flares of 10 erg large enough
to impact transit spectra occur at a rate of 3.6 flare
d, 10 higher than previous predictions from K2. We measure
the amount of flare contamination at 2 m for the TRAPPIST-1b and f
transits to be 500450 and 2100400 ppm, respectively. We find up to
80% of flare contamination can be removed, with mitigation most effective from
1.0--2.4 m. These results suggest transits affected by flares may still be
useful for atmospheric characterization efforts.Comment: 29 pages, 17 figures, 3 tables, accepted to The Astrophysical Journa
Atmospheric Reconnaissance of TRAPPIST-1 b with JWST/NIRISS: Evidence for Strong Stellar Contamination in the Transmission Spectra
TRAPPIST-1 is a nearby system of seven Earth-sized, temperate, rocky
exoplanets transiting a Jupiter-sized M8.5V star, ideally suited for in-depth
atmospheric studies. Each TRAPPIST-1 planet has been observed in transmission
both from space and from the ground, confidently rejecting cloud-free,
hydrogen-rich atmospheres. Secondary eclipse observations of TRAPPIST-1 b with
JWST/MIRI are consistent with little to no atmosphere given the lack of heat
redistribution. Here we present the first transmission spectra of TRAPPIST-1 b
obtained with JWST/NIRISS over two visits. The two transmission spectra show
moderate to strong evidence of contamination from unocculted stellar
heterogeneities, which dominates the signal in both visits. The transmission
spectrum of the first visit is consistent with unocculted starspots and the
second visit exhibits signatures of unocculted faculae. Fitting the stellar
contamination and planetary atmosphere either sequentially or simultaneously,
we confirm the absence of cloud-free hydrogen-rich atmospheres, but cannot
assess the presence of secondary atmospheres. We find that the uncertainties
associated with the lack of stellar model fidelity are one order of magnitude
above the observation precision of 89 ppm (combining the two visits). Without
affecting the conclusion regarding the atmosphere of TRAPPIST-1 b, this
highlights an important caveat for future explorations, which calls for
additional observations to characterize stellar heterogeneities empirically
and/or theoretical works to improve model fidelity for such cool stars. This
need is all the more justified as stellar contamination can affect the search
for atmospheres around the outer, cooler TRAPPIST-1 planets for which
transmission spectroscopy is currently the most efficient technique.Comment: 26 pages, 11 figures, accepted for publication in The Astrophysical
Journal Letter
Awesome SOSS: Transmission Spectroscopy of WASP-96b with NIRISS/SOSS
The future is now - after its long-awaited launch in December 2021, JWST
began science operations in July 2022 and is already revolutionizing exoplanet
astronomy. The Early Release Observations (ERO) program was designed to provide
the first images and spectra from JWST, covering a multitude of science cases
and using multiple modes of each on-board instrument. Here, we present
transmission spectroscopy observations of the hot-Saturn WASP-96b with the
Single Object Slitless Spectroscopy (SOSS) mode of the Near Infrared Imager and
Slitless Spectrograph, observed as part of the ERO program. As the SOSS mode
presents some unique data reduction challenges, we provide an in-depth
walk-through of the major steps necessary for the reduction of SOSS data:
including background subtraction, correction of 1/f noise, and treatment of the
trace order overlap. We furthermore offer potential routes to correct for field
star contamination, which can occur due to the SOSS mode's slitless nature. By
comparing our extracted transmission spectrum with grids of atmosphere models,
we find an atmosphere metallicity between 1x and 5x solar, and a solar
carbon-to-oxygen ratio. Moreover, our models indicate that no grey cloud deck
is required to fit WASP-96b's transmission spectrum, but find evidence for a
slope shortward of 0.9m, which could either be caused by enhanced Rayleigh
scattering or the red wing of a pressure-broadened Na feature. Our work
demonstrates the unique capabilities of the SOSS mode for exoplanet
transmission spectroscopy and presents a step-by-step reduction guide for this
new and exciting instrument.Comment: MNRAS, in press. Updated to reflect published versio
A chemical survey of exoplanets with ARIEL
Thousands of exoplanets have now been discovered with a huge range of masses, sizes and orbits: from rocky Earth-like planets to large gas giants grazing the surface of their host star. However, the essential nature of these exoplanets remains largely mysterious: there is no known, discernible pattern linking the presence, size, or orbital parameters of a planet to the nature of its parent star. We have little idea whether the chemistry of a planet is linked to its formation environment, or whether the type of host star drives the physics and chemistry of the planet’s birth, and evolution. ARIEL was conceived to observe a large number (~1000) of transiting planets for statistical understanding, including gas giants, Neptunes, super-Earths and Earth-size planets around a range of host star types using transit spectroscopy in the 1.25–7.8 μm spectral range and multiple narrow-band photometry in the optical. ARIEL will focus on warm and hot planets to take advantage of their well-mixed atmospheres which should show minimal condensation and sequestration of high-Z materials compared to their colder Solar System siblings. Said warm and hot atmospheres are expected to be more representative of the planetary bulk composition. Observations of these warm/hot exoplanets, and in particular of their elemental composition (especially C, O, N, S, Si), will allow the understanding of the early stages of planetary and atmospheric formation during the nebular phase and the following few million years. ARIEL will thus provide a representative picture of the chemical nature of the exoplanets and relate this directly to the type and chemical environment of the host star. ARIEL is designed as a dedicated survey mission for combined-light spectroscopy, capable of observing a large and well-defined planet sample within its 4-year mission lifetime. Transit, eclipse and phase-curve spectroscopy methods, whereby the signal from the star and planet are differentiated using knowledge of the planetary ephemerides, allow us to measure atmospheric signals from the planet at levels of 10–100 part per million (ppm) relative to the star and, given the bright nature of targets, also allows more sophisticated techniques, such as eclipse mapping, to give a deeper insight into the nature of the atmosphere. These types of observations require a stable payload and satellite platform with broad, instantaneous wavelength coverage to detect many molecular species, probe the thermal structure, identify clouds and monitor the stellar activity. The wavelength range proposed covers all the expected major atmospheric gases from e.g. H2O, CO2, CH4 NH3, HCN, H2S through to the more exotic metallic compounds, such as TiO, VO, and condensed species. Simulations of ARIEL performance in conducting exoplanet surveys have been performed – using conservative estimates of mission performance and a full model of all significant noise sources in the measurement – using a list of potential ARIEL targets that incorporates the latest available exoplanet statistics. The conclusion at the end of the Phase A study, is that ARIEL – in line with the stated mission objectives – will be able to observe about 1000 exoplanets depending on the details of the adopted survey strategy, thus confirming the feasibility of the main science objectives.Peer reviewedFinal Published versio
Challenges for Implementing an Ecosystem Approach to Fisheries Management
The ecosystem approach is being promoted as the foundation of solutions to the unsustainability of fisheries. However, because the ecosystem approach is broadly inclusive, the science for its implementation is often considered to be overly complex and difficult. When the science needed for an ecosystem approach to fisheries is perceived this way, science products cannot keep pace with fisheries critics, thus encouraging partisan political interference in fisheries management and proliferation of “faith-based solutions. In this paper we argue that one way to effectively counter politicization of fisheries decision-making is to ensure that new ecosystem-based approaches in fisheries are viewed only as an emergent property of innovation in science and policy. We organize our essay using three major themes to focus the discussion: empirical, jurisdictional, and societal challenges. We undertake at least partial answers to the following questions: (1) has conventional fisheries management really failed?; (2) can short-comings in conventional fisheries management be augmented with new tools, such as allocation of rights?; (3) is the Ecosystem Approach to Fisheries (EAF) equivalent to Ecosystem-Based Management?; and (4) is restoration of degraded ecosystems a necessary component of an EAF
A roadmap to the efficient and robust characterization of temperate terrestrial planet atmospheres with JWST
Ultra-cool dwarf stars are abundant, long-lived, and uniquely suited to
enable the atmospheric study of transiting terrestrial companions with JWST.
Amongst them, the most prominent is the M8.5V star TRAPPIST-1 and its seven
planets, which have been the favored targets of eight JWST Cycle 1 programs.
While Cycle 1 observations have started to yield preliminary insights into the
planets, they have also revealed that their atmospheric exploration requires a
better understanding of their host star. Here, we propose a roadmap to
characterize the TRAPPIST-1 system -- and others like it -- in an efficient and
robust manner. We notably recommend that -- although more challenging to
schedule -- multi-transit windows be prioritized to constrain stellar
heterogeneities and gather up to 2 more transits per JWST hour spent.
We conclude that in such systems planets cannot be studied in isolation by
small programs, thus large-scale community-supported programs should be
supported to enable the efficient and robust exploration of terrestrial
exoplanets in the JWST era
Enabling planetary science across light-years. Ariel Definition Study Report
Ariel, the Atmospheric Remote-sensing Infrared Exoplanet Large-survey, was adopted as the fourth medium-class mission in ESA's Cosmic Vision programme to be launched in 2029. During its 4-year mission, Ariel will study what exoplanets are made of, how they formed and how they evolve, by surveying a diverse sample of about 1000 extrasolar planets, simultaneously in visible and infrared wavelengths. It is the first mission dedicated to measuring the chemical composition and thermal structures of hundreds of transiting exoplanets, enabling planetary science far beyond the boundaries of the Solar System. The payload consists of an off-axis Cassegrain telescope (primary mirror 1100 mm x 730 mm ellipse) and two separate instruments (FGS and AIRS) covering simultaneously 0.5-7.8 micron spectral range. The satellite is best placed into an L2 orbit to maximise the thermal stability and the field of regard. The payload module is passively cooled via a series of V-Groove radiators; the detectors for the AIRS are the only items that require active cooling via an active Ne JT cooler. The Ariel payload is developed by a consortium of more than 50 institutes from 16 ESA countries, which include the UK, France, Italy, Belgium, Poland, Spain, Austria, Denmark, Ireland, Portugal, Czech Republic, Hungary, the Netherlands, Sweden, Norway, Estonia, and a NASA contribution
- …