5. A grand tour of exoplanets

2021 ◽  
pp. 76-95
Author(s):  
Raymond T. Pierrehumbert
Keyword(s):  
Solar System ◽  
Radial Velocity ◽  
Lower Case Letter ◽  
Grand Tour ◽  
Naming Convention ◽  
Lower Case ◽  
Transit Method

‘A grand tour of exoplanets’ explores exoplanets. Since there are far too many known exoplanets already for many of them to get familiar names such as the Solar System planets have, they are identified by a two-part naming convention. The first part of the name is the star they orbit, and the second part is a lower-case letter indicating the order in which the planet associated with that star was discovered. There are two main ways that exoplanets are found: the radial velocity (RV) technique and the transit method. Planets can be characterized by their instellation and by size or mass.

The Romaunt of the Rose and Source Manuscripts

PMLA ◽  
1959 ◽  
Vol 74 (3) ◽  
pp. 178-183
Author(s):  
Ronald Sutherland
Keyword(s):  
Jean De Meun ◽  
Great Work ◽  
Roman De La Rose ◽  
Guillaume De Lorris ◽  
Lower Case Letter ◽  
Lower Case ◽  
The Family ◽  
Significant Measure ◽  
The Rose ◽  
Partial Translation

The Authorship of the Romaunt of the Rose, subject of ardent controversy for nearly a century, can at last be established beyond any significant measure of doubt, for there is a new and highly reliable kind of evidence to show that at least two men were responsible for the existing partial translation of the famed Roman de la rose into Middle English. More than 200 MSS of the original French poem, composed by Guillaume de Lorris and Jean de Meun in the thirteenth century, have been catalogued by the late Ernest Langlois. The French scholar divided these MSS into three main groups, I, II, and III, and into subgroups or families marked by capital letters; while individual MSS he designated by the family letter plus a lower-case letter, Ab, He, Ha, and so on. In consequence of Langlois' great work, scholars have been enabled to compare the ME Romaunt with the variant readings of the MSS of its French original, and as will be demonstrated below, such comparison throws revealing light upon the facts of the Romaunt's composition.

Priming within the ‘Attentional Blink’ in an RSVP Task

Perception ◽  
1996 ◽  
Vol 25 (1_suppl) ◽  
pp. 26-26
Author(s):  
F K Chua ◽  
J Goh ◽  
G Kek
Keyword(s):  
Attentional Blink ◽  
Sensory Processing ◽  
Experimental Psychology ◽  
Priming Effect ◽  
Human Perception ◽  
Weak Form ◽  
Visual Presentation ◽  
Lower Case Letter ◽  
Lower Case ◽  
Local Interference

Recent experiments (eg M M Chun and M C Potter, 1995 Journal of Experimental Psychology: Human Perception and Performance21 109 – 127; J E Raymond, K L Shapiro, and K M Arnell, 1992 Journal of Experimental Psychology: Human Perception and Performance18 849 – 860) with RSVP (rapid serial visual presentation) suggest that the attentional blink is caused by local interference. We present data from three RSVP experiments that provide further clues regarding the attentional blink. In experiment 1, subjects detected an ‘X’ and then identified a red letter; in experiment 2, subjects had to say whether the first red target was an ‘X’ and then identify a red letter. In experiment 3, subjects identified two red letters. We systematically varied the lag between the first and second targets. On half the trials, we also primed the second target by placing an identical letter in the lag one position (the position after the first target). In experiment 3, we also examined if the priming effect was semantic with a lower case letter. The first two experiments suggest that the priming effect is very short-lived and mainly sensory in nature. The priming effect disappears altogether if the first target is not present. More interestingly, we found that when subjects failed to detect the ‘X’, priming could still happen. The third experiment replicates and extends the results of the first two experiments. We also show that priming, albeit in a weak form, may still happen during the time when the attentional blink is supposed to occur. These results suggest that it is not an inhibition that causes the attentional blink and that sensory processing continues during the blink.

Dynamic versus Static Designation

2005 ◽  
Vol 13 ◽  
pp. 998-999
Author(s):  
Dimitri Pourbaix
Keyword(s):  
Data Structure ◽  
Radial Velocity ◽  
Orbital Period ◽  
Recent Progress ◽  
The Past ◽  
Lower Case ◽  
History Of ◽  
The Cross ◽  
Cross Reference

AbstractShould the designation of the components of a system reflect its known hierarchy or rather the history of their discovery? With the recent progress in, say, radial velocity techniques, the old famous order in which components were used to be discovered (inner to outer components for spectroscopic systems) is somehow altered. In the past, capital letters were used for visual companions and lower case letters for spectroscopic components and there was almost no overlap between the two groups. The situation has changed from both ends of the orbital period interval. In some rare cases, we think letters should be re-distributed and re-assigned in order to reflect the structure of the system. With an adequate choice of the data structure, such a change of the companion designation is rather straightforward to implement in modern databases (such as SB9). The only foreseen drawback is related to the cross-reference with some old papers: the letter B would not designate the same component in a 1970 paper and in a 2003 one. For instance, the former secondary of an SB2 system might now refer to the unseen companion and an astrometric triple.

scholarly journals The TROY project

2018 ◽  
Vol 618 ◽  
pp. A42 ◽  
Author(s):  
J. Lillo-Box ◽  
A. Leleu ◽  
H. Parviainen ◽  
P. Figueira ◽  
M. Mallonn ◽  
...  
Keyword(s):  
Solar System ◽  
Radial Velocity ◽  
Parameter Space ◽  
Planet Formation ◽  
Planetary System ◽  
Lagrangian Points ◽  
Formation And Evolution ◽  
Observing Techniques

Context.Co-orbital bodies are the byproduct of planet formation and evolution, as we know from the solar system. Although planet-size co-orbitals do not exists in our planetary system, dynamical studies show that they can remain stable for long periods of time in the gravitational well of massive planets. Should they exist, their detection is feasible with the current instrumentation.Aims.In this paper, we present new ground-based observations searching for these bodies co-orbiting with nine close-in (P< 5 days) planets, using various observing techniques. The combination of all of these techniques allows us to restrict the parameter space of any possible trojan in the system.Methods.We used multi-technique observations, comprised of radial velocity, precision photometry, and transit timing variations, both newly acquired in the context of the TROY project and publicly available, to constrain the presence of planet-size trojans in the Lagrangian points of nine known exoplanets.Results.We find no clear evidence of trojans in these nine systems through any of the techniques used down to the precision of the observations. However, this allows us to constrain the presence of any potential trojan in the system, especially in the trojan mass or radius vs. libration amplitude plane. In particular, we can set upper mass limits in the super-Earth mass regime for six of the studied systems.

scholarly journals Precision Radial Velocities in the Near Infrared with TEDI

2008 ◽  
Vol 4 (S253) ◽  
pp. 157-161 ◽  
Author(s):  
James P. Lloyd ◽  
Agnieszka Czeszumska ◽  
Jerry Edelstein ◽  
David Erskine ◽  
Michael Feuerstein ◽  
...  
Keyword(s):  
Radial Velocity ◽  
Near Infrared ◽  
Radial Velocities ◽  
Velocity Measurements ◽  
M Dwarfs ◽  
Low Mass Stars ◽  
Habitable Zones ◽  
Low Mass ◽  
Transit Method

AbstractThe TEDI (TripleSpec - Exoplanet Discovery Instrument) is a dedicated instrument for the near-infrared radial velocity search for planetary companions to low-mass stars with the goal of achieving meters-per-second radial velocity precision. Heretofore, such planet searches have been limited almost entirely to the optical band and to stars that are bright in this band. Consequently, knowledge about planetary companions to the populous but visibly faint low-mass stars is limited. In addition to the opportunity afforded by precision radial velocity searches directly for planets around low mass stars, transits around the smallest M dwarfs offer a chance to detect the smallest possible planets in the habitable zones of the parent stars. As has been the the case with followup of planet candidates detected by the transit method requiring radial velocity confirmation, the capability to undertake efficient precision radial velocity measurements of mid-late M dwarfs will be required. TEDI has been commissioned on the Palomar 200” telescope in December 2007, and is currently in a science verification phase.

scholarly journals Developmental Patterns in Elemental Reading Skills: Visual Discrimination of Primary-Type Upper-Case and Lower-Case Letters

1970 ◽  
Vol 3 (4) ◽  
pp. 6-13 ◽  
Author(s):  
P. C. Smythe ◽  
R. G. Stennett ◽  
Madeline Hardy ◽  
H. R. Wilson
Keyword(s):  
Visual Discrimination ◽  
Reading Skills ◽  
Analytic Solution ◽  
Age Groups ◽  
Future Research ◽  
Lower Case Letter ◽  
Developmental Patterns ◽  
Lower Case ◽  
Visual Matching ◽  
Primary Type

Two hundred children in grades K-3 were administered visual, matching-to-sample tasks involving, (a) upper-case primary type and (b) lower-case primary type. Each upper- or lower-case letter was embedded in a display along with the three letters that had been rated as maximally similar to it in form. Performance was analyzed by calculating the percentage of students in each of four age groups correctly discriminating each item. This analysis revealed clear developmental trends and also showed performance to be higher on upper-than on lower-case letters. An ancillary, factor analytic solution was also computed and is discussed. Implications both for future research and concerning the style of type used in beginning readers are presented.

scholarly journals Developmental Patterns in Elemental Skills: Knowledge of Upper-Case and Lower-Case Letter Names

1970 ◽  
Vol 3 (3) ◽  
pp. 24-33 ◽  
Author(s):  
P. C. Smythe ◽  
R. G. Stennett ◽  
Madeline Hardy ◽  
H. R. Wilson
Keyword(s):  
Rank Order ◽  
Lower Case Letter ◽  
Developmental Patterns ◽  
Letter Naming ◽  
Letter Frequency ◽  
Lower Case ◽  
Letter Names ◽  
Primary Type ◽  
Relationship Of ◽  
The Relationship

Two hundred children in grades K-3 were administered a test designed to assess knowledge of letter names in both upper- and lower-case primary type. Children exhibited better knowledge of upper- than lower-case letter names. Rank order, correlational analyses performed to determine the relationship of letter naming to visual discrimination and letter frequency revealed different patterns for upper- and lower-case letters. A subsequent, factor analytic treatment of the data also suggested differences in upper- and lower-case letter naming. Results are related to reading readiness norms and pedagogical implications are dealt with briefly.

scholarly journals specphot: a comparison of spectroscopic and photometric exoplanet follow-up methods

2020 ◽  
Vol 495 (1) ◽  
pp. 734-742 ◽  
Author(s):  
Benjamin F Cooke ◽  
Don Pollacco
Keyword(s):  
Radial Velocity ◽  
Doppler Shift ◽  
Planetary System ◽  
Signal To Noise Ratio ◽  
High Accuracy ◽  
Signal To Noise ◽  
Shift Method ◽  
System Parameters ◽  
Transit Method

ABSTRACT We set out a simulation to explore the follow-up of exoplanet candidates. We look at comparing photometric (transit method) and spectroscopic (Doppler shift method) techniques using three instruments: Next-Generation Transit Survey, High-Accuracy Radial-velocity Planetary Search, and CORALIE. We take into account the precision of follow-up and required observing time in attempt to rank each method for a given set of planetary system parameters. The methods are assessed on two criteria: signal-to-noise ratio (S/N) of the detection and follow-up time before characterization. We find that different follow-up techniques are preferred for different regions of parameter space. For S/N, we find that the ratio of spectroscopic to photometric S/N for a given system goes like $R_{\rm p}/P^{{1}/{3}}$. For follow-up time, we find that photometry is favoured for the shortest period systems (&lt;10 d) as well as systems with small planet radii. Spectroscopy is then preferred for systems with larger radius, and thus more massive planets (given our assumed mass–radius relationship). Finally, we attempt to account for the availability of telescopes and weight the two methods accordingly.

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