scholarly journals Exoplanet mass estimation for a sample of targets for the Ariel mission

2021 ◽  
Author(s):  
J. R. Barnes ◽  
C. A. Haswell
Keyword(s):  
Radial Velocity ◽  
Input Parameter ◽  
Noise Sources ◽  
Time Commitment ◽  
Low Mass ◽  
Time Required ◽  
Fixed Input ◽  
The Impact ◽  
Quadrature Sampling

AbstractAriel’s ambitious goal to survey a quarter of known exoplanets will transform our knowledge of planetary atmospheres. Masses measured directly with the radial velocity technique are essential for well determined planetary bulk properties. Radial velocity masses will provide important checks of masses derived from atmospheric fits or alternatively can be treated as a fixed input parameter to reduce possible degeneracies in atmospheric retrievals. We quantify the impact of stellar activity on planet mass recovery for the Ariel mission sample using Sun-like spot models scaled for active stars combined with other noise sources. Planets with necessarily well-determined ephemerides will be selected for characterisation with Ariel. With this prior requirement, we simulate the derived planet mass precision as a function of the number of observations for a prospective sample of Ariel targets. We find that quadrature sampling can significantly reduce the time commitment required for follow-up RVs, and is most effective when the planetary RV signature is larger than the RV noise. For a typical radial velocity instrument operating on a 4 m class telescope and achieving 1 m s−1 precision, between ~17% and ~ 37% of the time commitment is spent on the 7% of planets with mass Mp < 10 M⊕. In many low activity cases, the time required is limited by asteroseismic and photon noise. For low mass or faint systems, we can recover masses with the same precision up to ~3 times more quickly with an instrumental precision of ~10 cm s−1.

scholarly journals Disentangling planetary orbits from stellar activity in radial-velocity surveys

2014 ◽  
Vol 13 (2) ◽  
pp. 155-157 ◽  
Author(s):  
R. D. Haywood ◽  
A. Collier Cameron ◽  
D. Queloz ◽  
S.C.C. Barros ◽  
M. Deleuil ◽  
...  
Keyword(s):  
Radial Velocity ◽  
High Accuracy ◽  
Stellar Surface ◽  
Stellar Activity ◽  
The Earth ◽  
Planetary Orbits ◽  
Low Mass ◽  
Do So

AbstractThe majority of extra-solar planets have been discovered (or confirmed after follow-up) through radial-velocity (RV) surveys. Using ground-based spectrographs such as High Accuracy Radial Velocity Planetary Search (HARPS) and HARPS-North, it is now possible to detect planets that are only a few times the mass of the Earth. However, the presence of dark spots on the stellar surface produces RV signals that are very similar in amplitude to those caused by orbiting low-mass planets. Disentangling these signals has thus become the biggest challenge in the detection of Earth-mass planets using RV surveys. To do so, we use the star's lightcurve to model the RV variations produced by spots. Here we present this method and show the results of its application to CoRoT-7.

scholarly journals Periodic transit timing variations and refined system parameters of the exoplanet XO-6b

2019 ◽  
Author(s):  
Zoltán Garai ◽  
Theodor Pribulla ◽  
Richard Komžík ◽  
Emil Kundra ◽  
Ľubomír Hambálek ◽  
...  
Keyword(s):  
Radial Velocity ◽  
Rotating Stars ◽  
Velocity Measurements ◽  
Orbital Parameters ◽  
Orbit Inclination ◽  
Consistent Solution ◽  
Low Mass ◽  
Academy Of Sciences ◽  
Fast Rotating

Abstract Only a few exoplanets are known to orbit around fast rotating stars. One of them is XO-6b, which orbits an F5V-type star. Shortly after the discovery, we started multicolor photometric and radial-velocity follow-up observations of XO-6b, using the telescopes of Astronomical Institute of the Slovak Academy of Sciences. Our main scientific goals were to better characterize the planetary system and to search for transit timing variations. We refined several planetary and orbital parameters. Based on our measurements, the planet XO-6b seems to be about 10% larger, which is, however, only about 2σ difference, but its orbit inclination angle, with respect to the plane of the sky, seems to be significantly smaller, than it was determined originally by the discoverers. In this case we found about 9.5σ difference. Moreover, we observed periodic transit timing variations of XO-6b with a semi-amplitude of about 14 min and with a period of about 450 days. There are two plausible explanations of such transit timing variations: (1) a third object in the system XO-6 causing light-time effect, or (2) resonant perturbations between the transiting planet XO-6b and another unknown low-mass planet in this system. From the O-C diagram we derived that the assumed third object in the system should have a stellar mass, therefore significant variations are expected in the radial-velocity measurements of XO-6. Since this is not the case, and since all attempts to fit radial velocities and O-C data simultaneously failed to provide a consistent solution, more realistic is the second explanation.

From the Sun to solar-type stars: radial velocity, photometry, astrometry and logR′HK time series for late-F to early-K old stars

2019 ◽  
Vol 15 (S354) ◽  
pp. 286-294
Author(s):  
Nadège Meunier ◽  
Anne-Marie Lagrange
Keyword(s):  
Radial Velocity ◽  
Large Range ◽  
Magnetic Activity ◽  
Activity Levels ◽  
The Sun ◽  
Lower Mass ◽  
Solar Type ◽  
Low Mass ◽  
Average Activity ◽  
The Impact

AbstractSolar simulations and observations showed that the detection of Earth twins around Sun-like stars is difficult in radial velocities with current methods techniques. The Sun has proved to be very useful to test processes, models, and analysis methods. The convective blueshift effect, dominating for the Sun, decreases towards lower mass stars, providing more suitable conditions to detect low mass planets. We describe the basic processes at work and how we extended a realistic solar model of radial velocity, photometry, astrometry and LogR′HK variability, using a coherent grid of stellar parameters covering a large range in mass and average activity levels. We present selected results concerning the impact of magnetic activity on Earth-mass planet detectability as a function of stellar type. We show how such realistic simulations can help characterizing the effect of stellar activity on RV and astrometric exoplanet detection.

scholarly journals The impact of stellar jitter on the confirmation of transiting exoplanet candidates around Solar-like stars

2008 ◽  
Vol 4 (S253) ◽  
pp. 506-507
Author(s):  
Brandon Tingley ◽  
Frank Grundahl ◽  
Hans Kjeldsen
Keyword(s):  
Time Series ◽  
Monte Carlo ◽  
Monte Carlo Simulations ◽  
Signal Detection ◽  
Radial Velocity ◽  
Good Description ◽  
Sampling Rate ◽  
Upper Limits ◽  
The Impact

AbstractThe radial velocity technique is commonly used to classify transiting exoplanet candidates. However, stars are intrinsically noisy in radial velocity. No good description of this noise has yet been proffered, although activity in general has been suggested as the source, making it impossible to evaluate its effect on signal detection. In this poster, we propose an activity-based model that incorporates both light and dark stellar spots, capable of producing both photometric and radial velocity time series. We demonstrate its consistency with both SOHO/VIRGO photometry and SOHO/GOLF radial velocities. We then use this model to establish lower and upper limits on the effects of intrinsic stellar noise on the metal lines used to follow up transit candidates, making use of Monte Carlo simulations. Based on these results, we can suggest an optimal observational sampling rate.

scholarly journals Impact of endovascular pedal arteries revascularization on wound healing in patients with critical limb ischemia

2020 ◽  
Vol 7 (11) ◽  
pp. 3633
Author(s):  
Mohamed M. El Yamany ◽  
Hatem M. Mohamed ◽  
Meera R. Boulos ◽  
Sherif A. Raffat
Keyword(s):  
Wound Healing ◽  
Critical Limb Ischemia ◽  
Wound Care ◽  
Limb Ischemia ◽  
Arterial Disease ◽  
University Hospital ◽  
Endovascular Revascularization ◽  
Time Required ◽  
The Impact

Background: Critical limb ischemia (CLI) is the final consequence of peripheral arterial disease (PAD). The management of this complex patient population often warrants a multidisciplinary approach with collaboration between endovascular interventionist, vascular surgeons, podiatrist, infectious disease, and wound care specialist. Objective of the study was to evaluate the impact of endovascular pedal arteries revascularization on wound healing in patients with critical limb ischemia.Methods: This was an interventional study conducted on 30 consecutive CLI patients underwent infra-genicular endovascular revascularization who attended to the outpatient department and emergency, Suez Canal university hospital complaining of symptoms of critical lower limb ischemia involving the foot (rest pain, ulcer and gangrene), during the period study from June 2017 till January 2019. Full detailed history, full examination, lab investigation, radiological imaging was done.Results: The pain intensity decreased from 7 to 4 post-procedural at 2nd day post-op, then to 3 at one week follow up and then it totally disappeared at one month follow up visit. The remaining patients who had incomplete PAA reported faster relieve of pain and more dramatic improve over time as it was totally relieved post procedural by time of discharge. The overall mean time required to achieve wound healing was 15±8 weeks.Conclusion: Successful pedal artery revascularization significantly improved wound healing in patients with CLI. Endovascular revascularization is effective to facilitate healing of wounds in CLI and can be performed without significant complications.

scholarly journals Expectations for the confirmation of Proxima c from a long-term radial velocity follow-up

2020 ◽  
Vol 494 (1) ◽  
pp. 1387-1394 ◽  
Author(s):  
M Damasso ◽  
F Del Sordo
Keyword(s):  
Radial Velocity ◽  
Orbital Period ◽  
Statistical Significance ◽  
Time Range ◽  
Published Data ◽  
Case Scenario ◽  
Data Set ◽  
To Come ◽  
The Impact

ABSTRACT Proxima c, a candidate second planet orbiting Proxima Centauri, was detected with the radial velocity method. The announced long orbital period (5.21$^{+0.26}_{-0.22}$ yr), and small semi-amplitude of the induced Doppler signal (1.2 ± 0.4 $\rm{\,m\,s^{-1}}$), make this detection challenging and a target worthy of a follow-up in the years to come. We intend to evaluate the impact of future data on the statistical significance of the detection through realistic simulated radial velocities to be added to the published data set, spanning up to one orbital period of Proxima c in the time range 2019–2023. We find that the detection significance of Proxima c increases depending not only on the amount of data collected, but also on the number of instruments used, and especially on the time-span covered by the observational campaign. However, on average, we do not get strong statistical evidence, and we predict that, in the best-case scenario, in the next five years the detection of Proxima c can become significant at the 4-σ level. If instead Proxima c does not exist, the detected signal may lower its significance down to 2 σ.

scholarly journals TOI-132 b: A short-period planet in the Neptune desert transiting a V = 11.3 G-type star★

2020 ◽  
Vol 493 (1) ◽  
pp. 973-985 ◽  
Author(s):  
Matías R Díaz ◽  
James S Jenkins ◽  
Davide Gandolfi ◽  
Eric D Lopez ◽  
Maritza G Soto ◽  
...  
Keyword(s):  
Radial Velocity ◽  
Velocity Variation ◽  
Planetary Mass ◽  
Radial Velocity Variation ◽  
Short Period ◽  
Low Mass ◽  
Formation And Evolution ◽  
Level 1 ◽  
Atmospheric Mass

ABSTRACT The Neptune desert is a feature seen in the radius-period plane, whereby a notable dearth of short period, Neptune-like planets is found. Here, we report the Transiting Exoplanet Survey Satellite (TESS) discovery of a new short-period planet in the Neptune desert, orbiting the G-type dwarf TYC 8003-1117-1 (TOI-132). TESS photometry shows transit-like dips at the level of ∼1400 ppm occurring every ∼2.11 d. High-precision radial velocity follow-up with High Accuracy Radial Velocity Planet Searcher confirmed the planetary nature of the transit signal and provided a semi-amplitude radial velocity variation of 11.38 $^{+0.84}_{-0.85}$ m s−1, which, when combined with the stellar mass of 0.97 ± 0.06 M⊙, provides a planetary mass of 22.40$^{+1.90}_{-1.92}$ M⊕. Modelling the TESS light curve returns a planet radius of 3.42$^{+0.13}_{-0.14}$ R⊕, and therefore the planet bulk density is found to be 3.08$^{+0.44}_{-0.46}$ g cm−3. Planet structure models suggest that the bulk of the planet mass is in the form of a rocky core, with an atmospheric mass fraction of 4.3$^{+1.2}_{-2.3}$ per cent. TOI-132 b is a TESS Level 1 Science Requirement candidate, and therefore priority follow-up will allow the search for additional planets in the system, whilst helping to constrain low-mass planet formation and evolution models, particularly valuable for better understanding of the Neptune desert.

scholarly journals Positional Astronomy and Stellar Masses

1985 ◽  
Vol 111 ◽  
pp. 71-80
Author(s):  
W. D. Heintz
Keyword(s):  
Radial Velocity ◽  
Main Sequence ◽  
Visual Binary ◽  
Low Mass ◽  
Stellar Masses ◽  
Positional Astronomy ◽  
The Impact

In this paper are surveyed the combinations of data needed for mass determinations, the impact of radial-velocity and speckle observations, the 1983 catalog of visual-binary orbits, the current material for main-sequence and red-dwarf masses and the controversial methods and results on low mass objects.

Sound Production Treatment for Acquired Apraxia of Speech: An Examination of Dosage in Relation to Probe Performance

2020 ◽  
pp. 1-16
Author(s):  
Julie L. Wambaugh ◽  
Lydia Kallhoff ◽  
Christina Nessler
Keyword(s):  
Retrospective Analysis ◽  
Sound Production ◽  
Apraxia Of Speech ◽  
Practice Schedule ◽  
Practice Schedules ◽  
Baseline Performance ◽  
The Mean ◽  
Number Of Treatment ◽  
The Impact

Purpose This study was designed to examine the association of dosage and effects of Sound Production Treatment (SPT) for acquired apraxia of speech. Method Treatment logs and probe data from 20 speakers with apraxia of speech and aphasia were submitted to a retrospective analysis. The number of treatment sessions and teaching episodes was examined relative to (a) change in articulation accuracy above baseline performance, (b) mastery of production, and (c) maintenance. The impact of practice schedule (SPT-Blocked vs. SPT-Random) was also examined. Results The average number of treatment sessions conducted prior to change was 5.4 for SPT-Blocked and 3.9 for SPT-Random. The mean number of teaching episodes preceding change was 334 for SPT-Blocked and 179 for SPT-Random. Mastery occurred within an average of 13.7 sessions (1,252 teaching episodes) and 12.4 sessions (1,082 teaching episodes) for SPT-Blocked and SPT-Random, respectively. Comparisons of dosage metric values across practice schedules did not reveal substantial differences. Significant negative correlations were found between follow-up probe performance and the dosage metrics. Conclusions Only a few treatment sessions were needed to achieve initial positive changes in articulation, with mastery occurring within 12–14 sessions for the majority of participants. Earlier occurrence of change or mastery was associated with better follow-up performance. Supplemental Material https://doi.org/10.23641/asha.12592190

Research Participation Experiences of Informants of Suicide and Control Cases

Crisis ◽  
2010 ◽  
Vol 31 (5) ◽  
pp. 238-246 ◽  
Author(s):  
Paul W. C. Wong ◽  
Wincy S. C. Chan ◽  
Philip S. L. Beh ◽  
Fiona W. S. Yau ◽  
Paul S. F. Yip ◽  
...  
Keyword(s):  
Ethical Issues ◽  
Research Participation ◽  
Self Report ◽  
Initial Contact ◽  
Psychological Autopsy ◽  
Autopsy Study ◽  
The People ◽  
And Control ◽  
The Impact

Background: Ethical issues have been raised about using the psychological autopsy approach in the study of suicide. The impact on informants of control cases who participated in case-control psychological autopsy studies has not been investigated. Aims: (1) To investigate whether informants of suicide cases recruited by two approaches (coroners’ court and public mortuaries) respond differently to the initial contact by the research team. (2) To explore the reactions, reasons for participation, and comments of both the informants of suicide and control cases to psychological autopsy interviews. (3) To investigate the impact of the interviews on informants of suicide cases about a month after the interviews. Methods: A self-report questionnaire was used for the informants of both suicide and control cases. Telephone follow-up interviews were conducted with the informants of suicide cases. Results: The majority of the informants of suicide cases, regardless of the initial route of contact, as well as the control cases were positive about being approached to take part in the study. A minority of informants of suicide and control cases found the experience of talking about their family member to be more upsetting than expected. The telephone follow-up interviews showed that none of the informants of suicide cases reported being distressed by the psychological autopsy interviews. Limitations: The acceptance rate for our original psychological autopsy study was modest. Conclusions: The findings of this study are useful for future participants and researchers in measuring the potential benefits and risks of participating in similar sensitive research. Psychological autopsy interviews may be utilized as an active engagement approach to reach out to the people bereaved by suicide, especially in places where the postvention work is underdeveloped.

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