Narrow‐Angle Astrometry with theSpace Interferometry Mission: The Search for Extrasolar Planets. I. Detection and Characterization of Single Planets

2002 ◽  
Vol 114 (801) ◽  
pp. 1173-1196 ◽  
Author(s):  
A. Sozzetti ◽  
S. Casertano ◽  
R. A. Brown ◽  
M. G. Lattanzi
Keyword(s):  
Extrasolar Planets ◽  
Narrow Angle

Direct detection and characterization of extrasolar planets: The Mariotti space interferometer

Icarus ◽  
2005 ◽  
Vol 178 (2) ◽  
pp. 570-588 ◽  
Author(s):  
Bertrand Mennesson ◽  
Alain Léger ◽  
Marc Ollivier
Keyword(s):  
Extrasolar Planets ◽  
Direct Detection ◽  
Space Interferometer

scholarly journals Direct characterization of young giant exoplanets at high spectral resolution by coupling SPHERE and CRIRES+

2021 ◽  
Vol 646 ◽  
pp. A150
Author(s):  
G. P. P. L. Otten ◽  
A. Vigan ◽  
E. Muslimov ◽  
M. N’Diaye ◽  
E. Choquet ◽  
...  
Keyword(s):  
Spectral Resolution ◽  
Extrasolar Planets ◽  
Signal To Noise Ratio ◽  
Detection Limits ◽  
Spectral Lines ◽  
High Spectral Resolution ◽  
Contrast Imaging ◽  
High Contrast Imaging ◽  
The Impact

Studies of atmospheres of directly imaged extrasolar planets with high-resolution spectrographs have shown that their characterization is predominantly limited by noise on the stellar halo at the location of the studied exoplanet. An instrumental combination of high-contrast imaging and high spectral resolution that suppresses this noise and resolves the spectral lines can therefore yield higher quality spectra. We study the performance of the proposed HiRISE fiber coupling between the direct imager SPHERE and the spectrograph CRIRES+ at the Very Large Telescope for spectral characterization of directly imaged planets. Using end-to-end simulations of HiRISE we determine the signal-to-noise ratio (S/N) of the detection of molecular species for known extrasolar planets in H and K bands, and compare them to CRIRES+. We investigate the ultimate detection limits of HiRISE as a function of stellar magnitude, and we quantify the impact of different coronagraphs and of the system transmission. We find that HiRISE largely outperforms CRIRES+ for companions around bright hosts like β Pictoris or 51 Eridani. For an H = 3.5 host, we observe a gain of a factor of up to 16 in observing time with HiRISE to reach the same S/N on a companion at 200 mas. More generally, HiRISE provides better performance than CRIRES+ in 2 h integration times between 50 and 350 mas for hosts with H < 8.5 and between 50 and 700 mas for H < 7. For fainter hosts like PDS 70 and HIP 65426, no significant improvements are observed. We find that using no coronagraph yields the best S/N when characterizing known exoplanets due to higher transmission and fiber-based starlight suppression. We demonstrate that the overall transmission of the system is in fact the main driver of performance. Finally, we show that HiRISE outperforms the best detection limits of SPHERE for bright stars, opening major possibilities for the characterization of future planetary companions detected by other techniques.

scholarly journals Imaging and Characterization of Extrasolar Planets with the Next Generation of Space Telescopes

Geosciences ◽  
2018 ◽  
Vol 8 (12) ◽  
pp. 442
Author(s):  
Ana I. Gómez de Castro
Keyword(s):  
Extrasolar Planets ◽  
Current Status ◽  
Next Generation ◽  
Special Issue ◽  
Space Telescopes ◽  
Large Space ◽  
Design Studies ◽  
Pros And Cons ◽  
Nm Range

The study and characterization of the exoplanets’ atmospheres and composition is in its infancy. The large facilities that will make feasible to image an exo-Earth are currently under study. This contribution to the special issue on “detection and characterization of extrasolar planets” is a summary on the current status of the design studies to build large space-based facilities working in the 100–3000 nm range for this purpose. The three basic designs: Fresnel imagers, starshades, and coronagraphs on large space telescopes are described. An outline of the pros and cons for each design is provided. The relevance of transmission spectroscopy to characterize exoplanets atmospheres is pointed out.

scholarly journals Optical interferometry from the Earth

2009 ◽  
Vol 5 (S261) ◽  
pp. 277-285 ◽  
Author(s):  
Andreas Quirrenbach
Keyword(s):  
Black Hole ◽  
Extrasolar Planets ◽  
Optical Interferometry ◽  
Orbital Parameters ◽  
Narrow Angle ◽  
Angle Measurements ◽  
The Earth ◽  
Optical Interferometers

AbstractGround-based optical interferometers can perform astrometric measurements with a precision approaching 10μas between pairs of stars separated by ~10″ on the sky. These narrow-angle measurements can be used to search for extrasolar planets and to determine their orbital parameters, to characterize microlensing events, and to measure the orbits of stars around the black hole at the center of our Galaxy.

scholarly journals Occultation Spectrophotometry of Extrasolar Planets with SOFIA

2012 ◽  
Vol 8 (S293) ◽  
pp. 435-441 ◽  
Author(s):  
Daniel Angerhausen ◽  
Klaus F. Huber ◽  
Avi M. Mandell ◽  
Michael W. McElwain ◽  
Stefan Czesla ◽  
...  
Keyword(s):  
Physical Properties ◽  
Near Infrared ◽  
Extrasolar Planets ◽  
Infrared Astronomy ◽  
Future Generations ◽  
Atmospheric Transmission ◽  
Infrared Telescope ◽  
Planetary Transits

AbstractThe NASA/DLR Stratospheric Observatory for Infrared Astronomy (SOFIA), a 2.5-meter infrared telescope on board a Boeing 747-SP, will conduct 0.3 - 1,600 μm photometric, spectroscopic, and imaging observations from altitudes as high as 45,000 ft., where the average atmospheric transmission is greater than 80 percent. SOFIA's first light cameras and spectrometers, as well as future generations of instruments, will make important contributions to the characterization of the physical properties of exoplanets. Our analysis shows that optical and near-infrared photometric and spectrophotometric follow-up observations during planetary transits and eclipses will be feasible with SOFIA's instrumentation, in particular the HIPO-FLITECAM optical/NIR instruments. The airborne-based platform has unique advantages in comparison to ground- and space-based observatories in this field of research which we will outline here. Furthermore we will present two exemplary science cases, that will be conducted in SOFIA's cycle 1.

New models of Jupiter in the context of Juno and Galileo: signature of a decoupling between the atmosphere and the interior

2020 ◽  
Author(s):  
Florian Debras ◽  
Gilles Chabrier
Keyword(s):  
Extrasolar Planets ◽  
Convective Zone ◽  
Giant Planets ◽  
Atmospheric Composition ◽  
Observational Constraints ◽  
Physical Processes ◽  
Hot Jupiters ◽  
Formation And Evolution ◽  
Gas Accretion

&lt;p&gt;&lt;span lang=&quot;en-US&quot;&gt;Juno's observations of Jupiter's gravity field have revealed extremely low values for the gravitational moments that are difficult to reconcile with the high abundance of metals observed in the atmosphere by Galileo. Recent studies chose to arbitrarily get rid of one of these two constraints in order to build models of Jupiter.&lt;/span&gt;&lt;/p&gt; &lt;p&gt;&lt;span lang=&quot;en-US&quot;&gt;In this presentation, I will detail our new Jupiter structure models reconciling Juno and Galileo observational constraints. These models confirm the need to separate Jupiter into at least 4 layers: an outer convective shell, a non-convective zone of compositional change, an inner convective shell and a diluted core representing about 60 percent of the planet in radius. Compared to other studies, these models propose a new idea with important consequences: a decrease in the quantity of metals between the outer and inner convective shells. This would imply that the atmospheric composition is not representative of the internal composition of the planet, contrary to what is regularly admitted, and would strongly impact the Jupiter formation scenarios (localization, migration, accretion).&lt;/span&gt;&lt;/p&gt; &lt;p&gt;&lt;span lang=&quot;en-US&quot;&gt;In particular, the presence of an internal non-convective zone prevents mixing between the two convective envelopes. I will detail the physical processes of this semi-convective zone (layered convection or H-He immiscibility) and explain how they may persist during the evolution of the planet.&lt;/span&gt;&lt;/p&gt; &lt;p&gt;&lt;span lang=&quot;en-US&quot;&gt;These models also impose a limit mass on the compact core, which cannot be heavier than 5 Earth masses. Such a mass, lower than the runaway gas accretion minimum mass, needs to be explained in the light of our understanding of the formation and evolution of giant planets.&lt;/span&gt;&lt;/p&gt; &lt;p&gt;&lt;span lang=&quot;en-US&quot;&gt;Using these models of Jupiter, I will finally detail the application of our new understanding of the interior of this planet to giant exoplanets. At a time of direct imaging of extrasolar planets and atmospheric characterization of hot Jupiters, a good understanding of the internal processes of planets in the solar system is paramount to make the best use of all the observations.&lt;/span&gt;&lt;/p&gt;

Sign in / Sign up

Export Citation Format

Share Document