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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.19558">arXiv:2502.19558</a> <span> [<a href="https://arxiv.org/pdf/2502.19558">pdf</a>, <a href="https://arxiv.org/format/2502.19558">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> Characterization of AF Lep b at high spectral resolution with VLT/HiRISE </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Denis%2C+A">A. Denis</a>, <a href="/search/astro-ph?searchtype=author&query=Vigan%2C+A">A. Vigan</a>, <a href="/search/astro-ph?searchtype=author&query=Costes%2C+J">J. Costes</a>, <a href="/search/astro-ph?searchtype=author&query=Chauvin%2C+G">G. Chauvin</a>, <a href="/search/astro-ph?searchtype=author&query=Radcliffe%2C+A">A. Radcliffe</a>, <a href="/search/astro-ph?searchtype=author&query=Ravet%2C+M">M. Ravet</a>, <a href="/search/astro-ph?searchtype=author&query=Balmer%2C+W">W. Balmer</a>, <a href="/search/astro-ph?searchtype=author&query=Palma-Bifani%2C+P">P. Palma-Bifani</a>, <a href="/search/astro-ph?searchtype=author&query=Petrus%2C+S">S. Petrus</a>, <a href="/search/astro-ph?searchtype=author&query=Parmentier%2C+V">V. Parmentier</a>, <a href="/search/astro-ph?searchtype=author&query=Martos%2C+S">S. Martos</a>, <a href="/search/astro-ph?searchtype=author&query=Simonnin%2C+A">A. Simonnin</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnefoy%2C+M">M. Bonnefoy</a>, <a href="/search/astro-ph?searchtype=author&query=Cadet%2C+R">R. Cadet</a>, <a href="/search/astro-ph?searchtype=author&query=Forveille%2C+T">T. Forveille</a>, <a href="/search/astro-ph?searchtype=author&query=Charnay%2C+B">B. Charnay</a>, <a href="/search/astro-ph?searchtype=author&query=Kiefer%2C+F">F. Kiefer</a>, <a href="/search/astro-ph?searchtype=author&query=Lagrange%2C+A+-">A. -M. Lagrange</a>, <a href="/search/astro-ph?searchtype=author&query=Chiavassa%2C+A">A. Chiavassa</a>, <a href="/search/astro-ph?searchtype=author&query=Stolker%2C+T">T. Stolker</a>, <a href="/search/astro-ph?searchtype=author&query=Lavail%2C+A">A. Lavail</a>, <a href="/search/astro-ph?searchtype=author&query=Godoy%2C+N">N. Godoy</a>, <a href="/search/astro-ph?searchtype=author&query=Janson%2C+M">M. Janson</a>, <a href="/search/astro-ph?searchtype=author&query=Pourcelot%2C+R">R. Pourcelot</a>, <a href="/search/astro-ph?searchtype=author&query=Delorme%2C+P">P. Delorme</a> , et al. (19 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2502.19558v1-abstract-short" style="display: inline;"> Since the recent discovery of the directly imaged super-Jovian planet AF Lep b, several studies have been conducted to characterize its atmosphere and constrain its orbital parameters. AF Lep b has a measured dynamical mass of $3.68 \pm 0.48$ MJup, a radius of $1.3 \pm 0.15$ RJup, a nearly circular orbit in spin-orbit alignment with the host star, a relatively high metallicity, and a near-solar to… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.19558v1-abstract-full').style.display = 'inline'; document.getElementById('2502.19558v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.19558v1-abstract-full" style="display: none;"> Since the recent discovery of the directly imaged super-Jovian planet AF Lep b, several studies have been conducted to characterize its atmosphere and constrain its orbital parameters. AF Lep b has a measured dynamical mass of $3.68 \pm 0.48$ MJup, a radius of $1.3 \pm 0.15$ RJup, a nearly circular orbit in spin-orbit alignment with the host star, a relatively high metallicity, and a near-solar to super-solar C/O ratio. However, key parameters such as the rotational velocity and radial velocity could not be estimated as they require high-resolution spectroscopic data that is impossible to obtain with classical spectrographs. AF Lep b was recently observed with the new HiRISE visitor instrument at the VLT, with the goal of obtaining high-resolution (R~140,000) spectroscopic observations to better constrain the orbital and atmospheric parameters of the young giant exoplanet. We compare the extracted spectrum of AF Lep b to self-consistent atmospheric models using ForMoSA. We then use our measurements of the radial velocity of the planet to provide new constraints on the orbit of the planet. From the forward modeling, we find a C/O ratio that aligns with previous low-resolution analyses, and we confirm the super-solar metallicity. We also confirm unambiguously the presence of methane in the atmosphere of the companion. Based on all available relative astrometry and radial velocity measurements of the host star, we show that two distinct orbital populations are possible for the companion. We derive the radial velocity of AF Lep b to be $10.51 \pm 1.03$ km/s, and show that this value agrees well with one of the two orbital solutions, allowing us to rule out an entire family of orbits. Additionally, assuming that the rotation and orbit are coplanar, the derived planet's rotation rate is consistent with the observed trend of increasing spin velocity with higher planet mass. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.19558v1-abstract-full').style.display = 'none'; document.getElementById('2502.19558v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.03776">arXiv:2404.03776</a> <span> [<a href="https://arxiv.org/pdf/2404.03776">pdf</a>, <a href="https://arxiv.org/format/2404.03776">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202449328">10.1051/0004-6361/202449328 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Four-of-a-kind? Comprehensive atmospheric characterisation of the HR 8799 planets with VLTI/GRAVITY </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Nasedkin%2C+E">E. Nasedkin</a>, <a href="/search/astro-ph?searchtype=author&query=Molli%C3%A8re%2C+P">P. Molli猫re</a>, <a href="/search/astro-ph?searchtype=author&query=Lacour%2C+S">S. Lacour</a>, <a href="/search/astro-ph?searchtype=author&query=Nowak%2C+M">M. Nowak</a>, <a href="/search/astro-ph?searchtype=author&query=Kreidberg%2C+L">L. Kreidberg</a>, <a href="/search/astro-ph?searchtype=author&query=Stolker%2C+T">T. Stolker</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J+J">J. J. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Balmer%2C+W+O">W. O. Balmer</a>, <a href="/search/astro-ph?searchtype=author&query=Kammerer%2C+J">J. Kammerer</a>, <a href="/search/astro-ph?searchtype=author&query=Shangguan%2C+J">J. Shangguan</a>, <a href="/search/astro-ph?searchtype=author&query=Abuter%2C+R">R. Abuter</a>, <a href="/search/astro-ph?searchtype=author&query=Amorim%2C+A">A. Amorim</a>, <a href="/search/astro-ph?searchtype=author&query=Asensio-Torres%2C+R">R. Asensio-Torres</a>, <a href="/search/astro-ph?searchtype=author&query=Benisty%2C+M">M. Benisty</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+J+-">J. -P. Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Beust%2C+H">H. Beust</a>, <a href="/search/astro-ph?searchtype=author&query=Blunt%2C+S">S. Blunt</a>, <a href="/search/astro-ph?searchtype=author&query=Boccaletti%2C+A">A. Boccaletti</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnefoy%2C+M">M. Bonnefoy</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnet%2C+H">H. Bonnet</a>, <a href="/search/astro-ph?searchtype=author&query=Bordoni%2C+M+S">M. S. Bordoni</a>, <a href="/search/astro-ph?searchtype=author&query=Bourdarot%2C+G">G. Bourdarot</a>, <a href="/search/astro-ph?searchtype=author&query=Brandner%2C+W">W. Brandner</a>, <a href="/search/astro-ph?searchtype=author&query=Cantalloube%2C+F">F. Cantalloube</a>, <a href="/search/astro-ph?searchtype=author&query=Caselli%2C+P">P. Caselli</a> , et al. (73 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.03776v2-abstract-short" style="display: inline;"> With four companions at separations from 16 to 71 au, HR 8799 is a unique target for direct imaging, presenting an opportunity for the comparative study of exoplanets with a shared formation history. Combining new VLTI/GRAVITY observations obtained within the ExoGRAVITY program with archival data, we perform a systematic atmospheric characterisation of all four planets. We explore different levels… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03776v2-abstract-full').style.display = 'inline'; document.getElementById('2404.03776v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.03776v2-abstract-full" style="display: none;"> With four companions at separations from 16 to 71 au, HR 8799 is a unique target for direct imaging, presenting an opportunity for the comparative study of exoplanets with a shared formation history. Combining new VLTI/GRAVITY observations obtained within the ExoGRAVITY program with archival data, we perform a systematic atmospheric characterisation of all four planets. We explore different levels of model flexibility to understand the temperature structure, chemistry and clouds of each planet using both petitRADTRANS atmospheric retrievals and fits to self-consistent radiative-convective equilibrium models. Using Bayesian Model Averaging to combine multiple retrievals, we find that the HR 8799 planets are highly enriched in metals, with [M/H] $\gtrsim$1, and have stellar to super-stellar C/O ratios. The C/O ratio increases with increasing separation from $0.55^{+0.12}_{-0.10}$ for d to $0.78^{+0.03}_{-0.04}$ for b, with the exception of the innermost planet which has a C/O ratio of $0.87\pm0.03$. By retrieving a quench pressure and using a disequilibrium chemistry model we derive vertical mixing strengths compatible with predictions for high-metallicity, self-luminous atmospheres. Bayesian evidence comparisons strongly favour the presence of HCN in HR 8799 c and e, as well as CH$_{4}$ in HR 8799 c, with detections at $>5蟽$ confidence. All of the planets are cloudy, with no evidence for patchiness. The clouds of c, d and e are best fit by silicate clouds lying above a deep iron cloud layer, while the clouds of the cooler HR 8799 b are more likely composed of Na$_{2}$S. With well defined atmospheric properties, future exploration of this system is well positioned to unveil further detail in these planets, extending our understanding of the composition, structure, and formation history of these siblings. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03776v2-abstract-full').style.display = 'none'; document.getElementById('2404.03776v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">45 pages, 25 figures, accepted by Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 687, A298 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.13055">arXiv:2403.13055</a> <span> [<a href="https://arxiv.org/pdf/2403.13055">pdf</a>, <a href="https://arxiv.org/format/2403.13055">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202450018">10.1051/0004-6361/202450018 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Combining Gaia and GRAVITY: Characterising five new Directly Detected Substellar Companions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Winterhalder%2C+T+O">T. O. Winterhalder</a>, <a href="/search/astro-ph?searchtype=author&query=Lacour%2C+S">S. Lacour</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%A9rand%2C+A">A. M茅rand</a>, <a href="/search/astro-ph?searchtype=author&query=Maire%2C+A+-">A. -L. Maire</a>, <a href="/search/astro-ph?searchtype=author&query=Kammerer%2C+J">J. Kammerer</a>, <a href="/search/astro-ph?searchtype=author&query=Stolker%2C+T">T. Stolker</a>, <a href="/search/astro-ph?searchtype=author&query=Pourr%C3%A9%2C+N">N. Pourr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Abuter%2C+R">R. Abuter</a>, <a href="/search/astro-ph?searchtype=author&query=Amorim%2C+A">A. Amorim</a>, <a href="/search/astro-ph?searchtype=author&query=Asensio-Torres%2C+R">R. Asensio-Torres</a>, <a href="/search/astro-ph?searchtype=author&query=Balmer%2C+W+O">W. O. Balmer</a>, <a href="/search/astro-ph?searchtype=author&query=Benisty%2C+M">M. Benisty</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+J+-">J. -P. Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Beust%2C+H">H. Beust</a>, <a href="/search/astro-ph?searchtype=author&query=Blunt%2C+S">S. Blunt</a>, <a href="/search/astro-ph?searchtype=author&query=Boccaletti%2C+A">A. Boccaletti</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnefoy%2C+M">M. Bonnefoy</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnet%2C+H">H. Bonnet</a>, <a href="/search/astro-ph?searchtype=author&query=Bordoni%2C+M+S">M. S. Bordoni</a>, <a href="/search/astro-ph?searchtype=author&query=Bourdarot%2C+G">G. Bourdarot</a>, <a href="/search/astro-ph?searchtype=author&query=Brandner%2C+W">W. Brandner</a>, <a href="/search/astro-ph?searchtype=author&query=Cantalloube%2C+F">F. Cantalloube</a>, <a href="/search/astro-ph?searchtype=author&query=Caselli%2C+P">P. Caselli</a>, <a href="/search/astro-ph?searchtype=author&query=Charnay%2C+B">B. Charnay</a> , et al. (74 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.13055v2-abstract-short" style="display: inline;"> Precise mass constraints are vital for the characterisation of brown dwarfs and exoplanets. Here we present how the combination of data obtained by Gaia and GRAVITY can help enlarge the sample of substellar companions with measured dynamical masses. We show how the Non-Single-Star (NSS) two-body orbit catalogue contained in Gaia DR3 can be used to inform high-angular-resolution follow-up observati… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.13055v2-abstract-full').style.display = 'inline'; document.getElementById('2403.13055v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.13055v2-abstract-full" style="display: none;"> Precise mass constraints are vital for the characterisation of brown dwarfs and exoplanets. Here we present how the combination of data obtained by Gaia and GRAVITY can help enlarge the sample of substellar companions with measured dynamical masses. We show how the Non-Single-Star (NSS) two-body orbit catalogue contained in Gaia DR3 can be used to inform high-angular-resolution follow-up observations with GRAVITY. Applying the method presented in this work to eight Gaia candidate systems, we detect all eight predicted companions, seven of which were previously unknown and five are of a substellar nature. Among the sample is Gaia DR3 2728129004119806464 B, which - detected at an angular separation of (34.01 $\pm$ 0.15) mas from the host - is the closest substellar companion ever imaged. This translates to a semi-major axis of (0.938 $\pm$ 0.023) AU. WT 766 B, detected at a greater angular separation, was confirmed to be on an orbit exhibiting an even smaller semi-major axis of (0.676 $\pm$ 0.008) AU. The GRAVITY data were then used to break the host-companion mass degeneracy inherent to the Gaia NSS orbit solutions as well as to constrain the orbital solutions of the respective target systems. Knowledge of the companion masses enabled us to further characterise them in terms of their ages, effective temperatures, and radii via the application of evolutionary models. The inferred ages exhibit a distinct bias towards values younger than what is to be expected based on the literature. The results serve as an independent validation of the orbital solutions published in the NSS two-body orbit catalogue and show that the combination of astrometric survey missions and high-angular-resolution direct imaging holds great promise for efficiently increasing the sample of directly imaged companions in the future, especially in the light of Gaia's upcoming DR4 and the advent of GRAVITY+. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.13055v2-abstract-full').style.display = 'none'; document.getElementById('2403.13055v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 688, A44 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.05019">arXiv:2402.05019</a> <span> [<a href="https://arxiv.org/pdf/2402.05019">pdf</a>, <a href="https://arxiv.org/format/2402.05019">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202449504">10.1051/0004-6361/202449504 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A catalogue of dual-field interferometric binary calibrators </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Nowak%2C+M">M. Nowak</a>, <a href="/search/astro-ph?searchtype=author&query=Lacour%2C+S">S. Lacour</a>, <a href="/search/astro-ph?searchtype=author&query=Abuter%2C+R">R. Abuter</a>, <a href="/search/astro-ph?searchtype=author&query=Amorim%2C+A">A. Amorim</a>, <a href="/search/astro-ph?searchtype=author&query=Asensio-Torres%2C+R">R. Asensio-Torres</a>, <a href="/search/astro-ph?searchtype=author&query=Balmer%2C+W+O">W. O. Balmer</a>, <a href="/search/astro-ph?searchtype=author&query=Benisty%2C+M">M. Benisty</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+J+-">J. -P. Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Beust%2C+H">H. Beust</a>, <a href="/search/astro-ph?searchtype=author&query=Blunt%2C+S">S. Blunt</a>, <a href="/search/astro-ph?searchtype=author&query=Boccaletti%2C+A">A. Boccaletti</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnefoy%2C+M">M. Bonnefoy</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnet%2C+H">H. Bonnet</a>, <a href="/search/astro-ph?searchtype=author&query=Bordoni%2C+M+S">M. S. Bordoni</a>, <a href="/search/astro-ph?searchtype=author&query=Bourdarot%2C+G">G. Bourdarot</a>, <a href="/search/astro-ph?searchtype=author&query=Brandner%2C+W">W. Brandner</a>, <a href="/search/astro-ph?searchtype=author&query=Cantalloube%2C+F">F. Cantalloube</a>, <a href="/search/astro-ph?searchtype=author&query=Charnay%2C+B">B. Charnay</a>, <a href="/search/astro-ph?searchtype=author&query=Chauvin%2C+G">G. Chauvin</a>, <a href="/search/astro-ph?searchtype=author&query=Chavez%2C+A">A. Chavez</a>, <a href="/search/astro-ph?searchtype=author&query=Choquet%2C+E">E. Choquet</a>, <a href="/search/astro-ph?searchtype=author&query=Christiaens%2C+V">V. Christiaens</a>, <a href="/search/astro-ph?searchtype=author&query=Cl%C3%A9net%2C+Y">Y. Cl茅net</a>, <a href="/search/astro-ph?searchtype=author&query=Foresto%2C+V+C+d">V. Coud茅 du Foresto</a>, <a href="/search/astro-ph?searchtype=author&query=Cridland%2C+A">A. Cridland</a> , et al. (75 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2402.05019v1-abstract-short" style="display: inline;"> Dual-field interferometric observations with VLTI/GRAVITY sometimes require the use of a "binary calibrator", a binary star whose individual components remain unresolved by the interferometer, with a separation between 400 and 2000 mas for observations with the Units Telescopes (UTs), or 1200 to 3000 mas for the Auxiliary Telescopes (ATs). The separation vector also needs to be predictable to with… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.05019v1-abstract-full').style.display = 'inline'; document.getElementById('2402.05019v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.05019v1-abstract-full" style="display: none;"> Dual-field interferometric observations with VLTI/GRAVITY sometimes require the use of a "binary calibrator", a binary star whose individual components remain unresolved by the interferometer, with a separation between 400 and 2000 mas for observations with the Units Telescopes (UTs), or 1200 to 3000 mas for the Auxiliary Telescopes (ATs). The separation vector also needs to be predictable to within 10 mas for proper pointing of the instrument. Up until now, no list of properly vetted calibrators was available for dual-field observations with VLTI/GRAVITY on the UTs. Our objective is to compile such a list, and make it available to the community. We identify a list of candidates from the Washington Double Star (WDS) catalogue, all with appropriate separations and brightness, scattered over the Southern sky. We observe them as part of a dedicated calibration programme, and determine whether these objects are true binaries (excluding higher multiplicities resolved interferometrically but unseen by imaging), and extract measurements of the separation vectors. We combine these new measurements with those available in the WDS to determine updated orbital parameters for all our vetted calibrators. We compile a list of 13 vetted binary calibrators for observations with VLTI/GRAVITY on the UTs, and provide orbital estimates and astrometric predictions for each of them. We show that our list guarantees that there are always at least two binary calibrators at airmass < 2 in the sky over the Paranal observatory, at any point in time. Any Principal Investigator wishing to use the dual-field mode of VLTI/GRAVITY with the UTs can now refer to this list to select an appropriate calibrator. We encourage the use of "whereistheplanet" to predict the astrometry of these calibrators, which seamlessly integrates with "p2Gravity" for VLTI/GRAVITY dual-field observing material preparation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.05019v1-abstract-full').style.display = 'none'; document.getElementById('2402.05019v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 6 figures. Submitted to A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 687, A248 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.08283">arXiv:2312.08283</a> <span> [<a href="https://arxiv.org/pdf/2312.08283">pdf</a>, <a href="https://arxiv.org/format/2312.08283">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> VLTI/GRAVITY Provides Evidence the Young, Substellar Companion HD 136164 Ab formed like a "Failed Star" </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Balmer%2C+W+O">William O. Balmer</a>, <a href="/search/astro-ph?searchtype=author&query=Pueyo%2C+L">L. Pueyo</a>, <a href="/search/astro-ph?searchtype=author&query=Lacour%2C+S">S. Lacour</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J+J">J. J. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Stolker%2C+T">T. Stolker</a>, <a href="/search/astro-ph?searchtype=author&query=Kammerer%2C+J">J. Kammerer</a>, <a href="/search/astro-ph?searchtype=author&query=Pourr%C3%A9%2C+N">N. Pourr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Nowak%2C+M">M. Nowak</a>, <a href="/search/astro-ph?searchtype=author&query=Rickman%2C+E">E. Rickman</a>, <a href="/search/astro-ph?searchtype=author&query=Blunt%2C+S">S. Blunt</a>, <a href="/search/astro-ph?searchtype=author&query=Sivaramakrishnan%2C+A">A. Sivaramakrishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Sing%2C+D">D. Sing</a>, <a href="/search/astro-ph?searchtype=author&query=Wagner%2C+K">K. Wagner</a>, <a href="/search/astro-ph?searchtype=author&query=Marleau%2C+G+-">G. -D. Marleau</a>, <a href="/search/astro-ph?searchtype=author&query=Lagrange%2C+A+-">A. -M. Lagrange</a>, <a href="/search/astro-ph?searchtype=author&query=Abuter%2C+R">R. Abuter</a>, <a href="/search/astro-ph?searchtype=author&query=Amorim%2C+A">A. Amorim</a>, <a href="/search/astro-ph?searchtype=author&query=Asensio-Torres%2C+R">R. Asensio-Torres</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+J+-">J. -P. Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Beust%2C+H">H. Beust</a>, <a href="/search/astro-ph?searchtype=author&query=Boccaletti%2C+A">A. Boccaletti</a>, <a href="/search/astro-ph?searchtype=author&query=Bohn%2C+A">A. Bohn</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnefoy%2C+M">M. Bonnefoy</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnet%2C+H">H. Bonnet</a>, <a href="/search/astro-ph?searchtype=author&query=Bordoni%2C+M+S">M. S. Bordoni</a> , et al. (71 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.08283v1-abstract-short" style="display: inline;"> Young, low-mass Brown Dwarfs orbiting early-type stars, with low mass ratios ($q\lesssim0.01$), appear intrinsically rare and present a formation dilemma: could a handful of these objects be the highest mass outcomes of ``planetary" formation channels (bottom up within a protoplanetary disk), or are they more representative of the lowest mass ``failed binaries" (formed via disk fragmentation, or c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.08283v1-abstract-full').style.display = 'inline'; document.getElementById('2312.08283v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.08283v1-abstract-full" style="display: none;"> Young, low-mass Brown Dwarfs orbiting early-type stars, with low mass ratios ($q\lesssim0.01$), appear intrinsically rare and present a formation dilemma: could a handful of these objects be the highest mass outcomes of ``planetary" formation channels (bottom up within a protoplanetary disk), or are they more representative of the lowest mass ``failed binaries" (formed via disk fragmentation, or core fragmentation)? Additionally, their orbits can yield model-independent dynamical masses, and when paired with wide wavelength coverage and accurate system age estimates, can constrain evolutionary models in a regime where the models have a wide dispersion depending on initial conditions. We present new interferometric observations of the $16\,\mathrm{Myr}$ substellar companion HD~136164~Ab (HIP~75056~Ab) with VLTI/GRAVITY and an updated orbit fit including proper motion measurements from the Hipparcos-Gaia Catalogue of Accelerations. We estimate a dynamical mass of $35\pm10\,\mathrm{M_J}$ ($q\sim0.02$), making HD~136164~Ab the youngest substellar companion with a dynamical mass estimate. The new mass and newly constrained orbital eccentricity ($e=0.44\pm0.03$) and separation ($22.5\pm1\,\mathrm{au}$) could indicate that the companion formed via the low-mass tail of the Initial Mass Function. Our atmospheric fit to the \texttt{SPHINX} M-dwarf model grid suggests a sub-solar C/O ratio of $0.45$, and $3\times$ solar metallicity, which could indicate formation in the circumstellar disk via disk fragmentation. Either way, the revised mass estimate likely excludes ``bottom-up" formation via core accretion in the circumstellar disk. HD~136164~Ab joins a select group of young substellar objects with dynamical mass estimates; epoch astrometry from future \textit{Gaia} data releases will constrain the dynamical mass of this crucial object further. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.08283v1-abstract-full').style.display = 'none'; document.getElementById('2312.08283v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in The Astronomical Journal. 9 figures, 3 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.00148">arXiv:2310.00148</a> <span> [<a href="https://arxiv.org/pdf/2310.00148">pdf</a>, <a href="https://arxiv.org/format/2310.00148">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> First VLTI/GRAVITY Observations of HIP 65426 b: Evidence for a Low or Moderate Orbital Eccentricity </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Blunt%2C+S">S. Blunt</a>, <a href="/search/astro-ph?searchtype=author&query=Balmer%2C+W+O">W. O. Balmer</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J+J">J. J. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Lacour%2C+S">S. Lacour</a>, <a href="/search/astro-ph?searchtype=author&query=Petrus%2C+S">S. Petrus</a>, <a href="/search/astro-ph?searchtype=author&query=Bourdarot%2C+G">G. Bourdarot</a>, <a href="/search/astro-ph?searchtype=author&query=Kammerer%2C+J">J. Kammerer</a>, <a href="/search/astro-ph?searchtype=author&query=Pourr%C3%A9%2C+N">N. Pourr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Rickman%2C+E">E. Rickman</a>, <a href="/search/astro-ph?searchtype=author&query=Shangguan%2C+J">J. Shangguan</a>, <a href="/search/astro-ph?searchtype=author&query=Winterhalder%2C+T">T. Winterhalder</a>, <a href="/search/astro-ph?searchtype=author&query=Abuter%2C+R">R. Abuter</a>, <a href="/search/astro-ph?searchtype=author&query=Amorim%2C+A">A. Amorim</a>, <a href="/search/astro-ph?searchtype=author&query=Asensio-Torres%2C+R">R. Asensio-Torres</a>, <a href="/search/astro-ph?searchtype=author&query=Benisty%2C+M">M. Benisty</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+J+-">J. -P. Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Beust%2C+H">H. Beust</a>, <a href="/search/astro-ph?searchtype=author&query=Boccaletti%2C+A">A. Boccaletti</a>, <a href="/search/astro-ph?searchtype=author&query=Bohn%2C+A">A. Bohn</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnefoy%2C+M">M. Bonnefoy</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnet%2C+H">H. Bonnet</a>, <a href="/search/astro-ph?searchtype=author&query=Brandner%2C+W">W. Brandner</a>, <a href="/search/astro-ph?searchtype=author&query=Cantalloube%2C+F">F. Cantalloube</a>, <a href="/search/astro-ph?searchtype=author&query=Caselli%2C+P">P. Caselli</a>, <a href="/search/astro-ph?searchtype=author&query=Charnay%2C+B">B. Charnay</a> , et al. (73 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.00148v2-abstract-short" style="display: inline;"> Giant exoplanets have been directly imaged over orders of magnitude of orbital separations, prompting theoretical and observational investigations of their formation pathways. In this paper, we present new VLTI/GRAVITY astrometric data of HIP 65426 b, a cold, giant exoplanet which is a particular challenge for most formation theories at a projected separation of 92 au from its primary. Leveraging… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.00148v2-abstract-full').style.display = 'inline'; document.getElementById('2310.00148v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.00148v2-abstract-full" style="display: none;"> Giant exoplanets have been directly imaged over orders of magnitude of orbital separations, prompting theoretical and observational investigations of their formation pathways. In this paper, we present new VLTI/GRAVITY astrometric data of HIP 65426 b, a cold, giant exoplanet which is a particular challenge for most formation theories at a projected separation of 92 au from its primary. Leveraging GRAVITY's astrometric precision, we present an updated eccentricity posterior that disfavors large eccentricities. The eccentricity posterior is still prior-dependent, and we extensively interpret and discuss the limits of the posterior constraints presented here. We also perform updated spectral comparisons with self-consistent forward-modeled spectra, finding a best fit ExoREM model with solar metallicity and C/O=0.6. An important caveat is that it is difficult to estimate robust errors on these values, which are subject to interpolation errors as well as potentially missing model physics. Taken together, the orbital and atmospheric constraints paint a preliminary picture of formation inconsistent with scattering after disk dispersal. Further work is needed to validate this interpretation. Analysis code used to perform this work is available at https://github.com/sblunt/hip65426. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.00148v2-abstract-full').style.display = 'none'; document.getElementById('2310.00148v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 14 figures. Revised and resubmitted to AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.16969">arXiv:2309.16969</a> <span> [<a href="https://arxiv.org/pdf/2309.16969">pdf</a>, <a href="https://arxiv.org/format/2309.16969">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ace629">10.3847/1538-4357/ace629 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Sudden extreme obscuration of a Sun-like main-sequence star: evolution of the circumstellar dust around ASASSN-21qj </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+J+P">Jonathan P. Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=Ertel%2C+S">Steve Ertel</a>, <a href="/search/astro-ph?searchtype=author&query=Kemper%2C+F">Francisca Kemper</a>, <a href="/search/astro-ph?searchtype=author&query=del+Burgo%2C+C">Carlos del Burgo</a>, <a href="/search/astro-ph?searchtype=author&query=Otten%2C+G+P+P+L">Gilles P. P. L. Otten</a>, <a href="/search/astro-ph?searchtype=author&query=Scicluna%2C+P">Peter Scicluna</a>, <a href="/search/astro-ph?searchtype=author&query=Zeegers%2C+S+T">Sascha T. Zeegers</a>, <a href="/search/astro-ph?searchtype=author&query=Ribas%2C+%C3%81">脕lvaro Ribas</a>, <a href="/search/astro-ph?searchtype=author&query=Morata%2C+O">Oscar Morata</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.16969v1-abstract-short" style="display: inline;"> ASASSN-21qj is a distant Sun-like star that recently began an episode of deep dimming events after no prior recorded variability. Here we examine archival and newly obtained optical and near-infrared data of this star. The deep aperiodic dimming and absence of previous infrared excess are reminiscent of KIC 8462852 (``Boyajian's Star''). The observed occultations are consistent with a circumstella… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.16969v1-abstract-full').style.display = 'inline'; document.getElementById('2309.16969v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.16969v1-abstract-full" style="display: none;"> ASASSN-21qj is a distant Sun-like star that recently began an episode of deep dimming events after no prior recorded variability. Here we examine archival and newly obtained optical and near-infrared data of this star. The deep aperiodic dimming and absence of previous infrared excess are reminiscent of KIC 8462852 (``Boyajian's Star''). The observed occultations are consistent with a circumstellar cloud of sub-micron-sized dust grains composed of amorphous pyroxene, with a minimum mass of $1.50~\pm~0.04\times10^{-9}~M_{\oplus}$ derived from the deepest occultations, and a minimum grain size of $0.29^{+0.01}_{-0.18}~渭$m assuming a power law size distribution. We further identify the first evidence of near-infrared excess in this system from NEOWISE 3.4 and 4.6~$渭$m observations. The excess emission implies a total circumstellar dust mass of around $10^{-6} M_{\oplus}$, comparable to the extreme, variable discs associated with terrestrial planet formation around young stars. The quasiperiodic recurrence of deep dips and the inferred dust temperature (ranging from 1800 to 700~K across the span of observations) independently point to an orbital distance of $\simeq$0.2~au for the dust, supporting the occulting material and excess emission being causally linked. The origin of this extended, opaque cloud is surmised to be the breakup of one or more exocometary bodies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.16969v1-abstract-full').style.display = 'none'; document.getElementById('2309.16969v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 6 figures, 1 table, published in ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 954 140 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.12390">arXiv:2309.12390</a> <span> [<a href="https://arxiv.org/pdf/2309.12390">pdf</a>, <a href="https://arxiv.org/format/2309.12390">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> First light of VLT/HiRISE: High-resolution spectroscopy of young giant exoplanets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vigan%2C+A">A. Vigan</a>, <a href="/search/astro-ph?searchtype=author&query=Morsy%2C+M+E">M. El Morsy</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+M">M. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Otten%2C+G+P+P+L">G. P. P. L. Otten</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia%2C+J">J. Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Costes%2C+J">J. Costes</a>, <a href="/search/astro-ph?searchtype=author&query=Muslimov%2C+E">E. Muslimov</a>, <a href="/search/astro-ph?searchtype=author&query=Viret%2C+A">A. Viret</a>, <a href="/search/astro-ph?searchtype=author&query=Charles%2C+Y">Y. Charles</a>, <a href="/search/astro-ph?searchtype=author&query=Zins%2C+G">G. Zins</a>, <a href="/search/astro-ph?searchtype=author&query=Murray%2C+G">G. Murray</a>, <a href="/search/astro-ph?searchtype=author&query=Costille%2C+A">A. Costille</a>, <a href="/search/astro-ph?searchtype=author&query=Paufique%2C+J">J. Paufique</a>, <a href="/search/astro-ph?searchtype=author&query=Seemann%2C+U">U. Seemann</a>, <a href="/search/astro-ph?searchtype=author&query=Houll%C3%A9%2C+M">M. Houll茅</a>, <a href="/search/astro-ph?searchtype=author&query=Anwand-Heerwart%2C+H">H. Anwand-Heerwart</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+M">M. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Abinanti%2C+A">A. Abinanti</a>, <a href="/search/astro-ph?searchtype=author&query=Balard%2C+P">P. Balard</a>, <a href="/search/astro-ph?searchtype=author&query=Baraffe%2C+I">I. Baraffe</a>, <a href="/search/astro-ph?searchtype=author&query=Benedetti%2C+J+-">J. -A. Benedetti</a>, <a href="/search/astro-ph?searchtype=author&query=Blanchard%2C+P">P. Blanchard</a>, <a href="/search/astro-ph?searchtype=author&query=Blanco%2C+L">L. Blanco</a>, <a href="/search/astro-ph?searchtype=author&query=Beuzit%2C+J+-">J. -L. Beuzit</a>, <a href="/search/astro-ph?searchtype=author&query=Choquet%2C+E">E. Choquet</a> , et al. (24 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.12390v2-abstract-short" style="display: inline;"> A major endeavor of this decade is the direct characterization of young giant exoplanets at high spectral resolution to determine the composition of their atmosphere and infer their formation processes and evolution. Such a goal represents a major challenge owing to their small angular separation and luminosity contrast with respect to their parent stars. Instead of designing and implementing comp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.12390v2-abstract-full').style.display = 'inline'; document.getElementById('2309.12390v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.12390v2-abstract-full" style="display: none;"> A major endeavor of this decade is the direct characterization of young giant exoplanets at high spectral resolution to determine the composition of their atmosphere and infer their formation processes and evolution. Such a goal represents a major challenge owing to their small angular separation and luminosity contrast with respect to their parent stars. Instead of designing and implementing completely new facilities, it has been proposed to leverage the capabilities of existing instruments that offer either high contrast imaging or high dispersion spectroscopy, by coupling them using optical fibers. In this work we present the implementation and first on-sky results of the HiRISE instrument at the very large telescope (VLT), which combines the exoplanet imager SPHERE with the recently upgraded high resolution spectrograph CRIRES using single-mode fibers. The goal of HiRISE is to enable the characterization of known companions in the $H$ band, at a spectral resolution of the order of $R = 位/螖位= 100\,000$, in a few hours of observing time. We present the main design choices and the technical implementation of the system, which is constituted of three major parts: the fiber injection module inside of SPHERE, the fiber bundle around the telescope, and the fiber extraction module at the entrance of CRIRES. We also detail the specific calibrations required for HiRISE and the operations of the instrument for science observations. Finally, we detail the performance of the system in terms of astrometry, temporal stability, optical aberrations, and transmission, for which we report a peak value of $\sim$3.9% based on sky measurements in median observing conditions. Finally, we report on the first astrophysical detection of HiRISE to illustrate its potential. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.12390v2-abstract-full').style.display = 'none'; document.getElementById('2309.12390v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 15 figures, 3 tables. Accepted in A&A on 24 October 2023</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.04403">arXiv:2309.04403</a> <span> [<a href="https://arxiv.org/pdf/2309.04403">pdf</a>, <a href="https://arxiv.org/format/2309.04403">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/acf761">10.3847/1538-4357/acf761 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> VLTI/GRAVITY Observations and Characterization of the Brown Dwarf Companion HD 72946 B </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Balmer%2C+W+O">W. O. Balmer</a>, <a href="/search/astro-ph?searchtype=author&query=Pueyo%2C+L">L. Pueyo</a>, <a href="/search/astro-ph?searchtype=author&query=Stolker%2C+T">T. Stolker</a>, <a href="/search/astro-ph?searchtype=author&query=Reggiani%2C+H">H. Reggiani</a>, <a href="/search/astro-ph?searchtype=author&query=Lacour%2C+S">S. Lacour</a>, <a href="/search/astro-ph?searchtype=author&query=Maire%2C+A+-">A. -L. Maire</a>, <a href="/search/astro-ph?searchtype=author&query=Molli%C3%A8re%2C+P">P. Molli猫re</a>, <a href="/search/astro-ph?searchtype=author&query=Nowak%2C+M">M. Nowak</a>, <a href="/search/astro-ph?searchtype=author&query=Sing%2C+D">D. Sing</a>, <a href="/search/astro-ph?searchtype=author&query=Pourr%C3%A9%2C+N">N. Pourr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Blunt%2C+S">S. Blunt</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J+J">J. J. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Rickman%2C+E">E. Rickman</a>, <a href="/search/astro-ph?searchtype=author&query=Henning%2C+T">Th. Henning</a>, <a href="/search/astro-ph?searchtype=author&query=Ward-Duong%2C+K">K. Ward-Duong</a>, <a href="/search/astro-ph?searchtype=author&query=Abuter%2C+R">R. Abuter</a>, <a href="/search/astro-ph?searchtype=author&query=Amorim%2C+A">A. Amorim</a>, <a href="/search/astro-ph?searchtype=author&query=Asensio-Torres%2C+R">R. Asensio-Torres</a>, <a href="/search/astro-ph?searchtype=author&query=Benisty%2C+M">M. Benisty</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+J+-">J. -P. Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Beust%2C+H">H. Beust</a>, <a href="/search/astro-ph?searchtype=author&query=Boccaletti%2C+A">A. Boccaletti</a>, <a href="/search/astro-ph?searchtype=author&query=Bohn%2C+A">A. Bohn</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnefoy%2C+M">M. Bonnefoy</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnet%2C+H">H. Bonnet</a> , et al. (74 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.04403v3-abstract-short" style="display: inline;"> Tension remains between the observed and modeled properties of substellar objects, but objects in binary orbits, with known dynamical masses can provide a way forward. HD 72946 B is a recently imaged brown dwarf companion to the nearby, solar type star. We achieve $\sim100~渭\mathrm{as}$ relative astrometry of HD 72946 B in the K-band using VLTI/GRAVITY, unprecedented for a benchmark brown dwarf. W… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.04403v3-abstract-full').style.display = 'inline'; document.getElementById('2309.04403v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.04403v3-abstract-full" style="display: none;"> Tension remains between the observed and modeled properties of substellar objects, but objects in binary orbits, with known dynamical masses can provide a way forward. HD 72946 B is a recently imaged brown dwarf companion to the nearby, solar type star. We achieve $\sim100~渭\mathrm{as}$ relative astrometry of HD 72946 B in the K-band using VLTI/GRAVITY, unprecedented for a benchmark brown dwarf. We fit an ensemble of measurements of the orbit using orbitize! and derive a strong dynamical mass constraint $\mathrm{M_B}=69.5\pm0.5~\mathrm{M_{Jup}}$ assuming a strong prior on the host star mass $\mathrm{M_A}=0.97\pm0.01~\mathrm{M_\odot}$ from an updated stellar analysis. We fit the spectrum of the companion to a grid of self-consistent BT-Settl-CIFIST model atmospheres, and perform atmospheric retrievals using petitRADTRANS. A dynamical mass prior only marginally influences the sampled distribution on effective temperature, but has a large influence on the surface gravity and radius, as expected. The dynamical mass alone does not strongly influence retrieved pressure-temperature or cloud parameters within our current retrieval setup. Independent of cloud prescription and prior assumptions, we find agreement within $\pm2\,蟽$ between the C/O ratio of the host ($0.52\pm0.05)$ and brown dwarf ($0.43$ to $0.63$), as expected from a molecular cloud collapse formation scenario, but our retrieved metallicities are implausibly high ($0.6-0.8$) in light of an excellent agreement of the data with the solar abundance model grid. Future work on our retrieval framework will seek to resolve this tension. Additional study of low surface-gravity objects is necessary to assess the influence of a dynamical mass prior on atmospheric analysis. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.04403v3-abstract-full').style.display = 'none'; document.getElementById('2309.04403v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in the Astrophysical Journal. 32 pages, 14 figures, 7 tables. v2&3 correct errors in co-author's affiliations, figure rendering, and some grant acknowledgements</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.14063">arXiv:2304.14063</a> <span> [<a href="https://arxiv.org/pdf/2304.14063">pdf</a>, <a href="https://arxiv.org/format/2304.14063">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202245333">10.1051/0004-6361/202245333 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Applying a temporal systematics model to vector Apodizing Phase Plate coronagraphic data: TRAP4vAPP </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Liu%2C+P">Pengyu Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Bohn%2C+A+J">Alexander J. Bohn</a>, <a href="/search/astro-ph?searchtype=author&query=Doelman%2C+D+S">David S. Doelman</a>, <a href="/search/astro-ph?searchtype=author&query=Sutlieff%2C+B+J">Ben J. Sutlieff</a>, <a href="/search/astro-ph?searchtype=author&query=Samland%2C+M">Matthias Samland</a>, <a href="/search/astro-ph?searchtype=author&query=Kenworthy%2C+M+A">Matthew A. Kenworthy</a>, <a href="/search/astro-ph?searchtype=author&query=Snik%2C+F">Frans Snik</a>, <a href="/search/astro-ph?searchtype=author&query=Birkby%2C+J+L">Jayne L. Birkby</a>, <a href="/search/astro-ph?searchtype=author&query=Biller%2C+B+A">Beth A. Biller</a>, <a href="/search/astro-ph?searchtype=author&query=Males%2C+J+R">Jared R. Males</a>, <a href="/search/astro-ph?searchtype=author&query=Morzinski%2C+K+M">Katie M. Morzinski</a>, <a href="/search/astro-ph?searchtype=author&query=Close%2C+L+M">Laird M. Close</a>, <a href="/search/astro-ph?searchtype=author&query=Otten%2C+G+P+P+L">Gilles P. P. L. Otten</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.14063v1-abstract-short" style="display: inline;"> The vector Apodizing Phase Plate (vAPP) is a pupil plane coronagraph that suppresses starlight by forming a dark hole in its point spread function (PSF). The unconventional and non-axisymmetrical PSF arising from the phase modification applied by this coronagraph presents a special challenge to post-processing techniques. We aim to implement a recently developed post-processing algorithm, temporal… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.14063v1-abstract-full').style.display = 'inline'; document.getElementById('2304.14063v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.14063v1-abstract-full" style="display: none;"> The vector Apodizing Phase Plate (vAPP) is a pupil plane coronagraph that suppresses starlight by forming a dark hole in its point spread function (PSF). The unconventional and non-axisymmetrical PSF arising from the phase modification applied by this coronagraph presents a special challenge to post-processing techniques. We aim to implement a recently developed post-processing algorithm, temporal reference analysis of planets (TRAP) on vAPP coronagraphic data. The property of TRAP that uses non-local training pixels, combined with the unconventional PSF of vAPP, allows for more flexibility than previous spatial algorithms in selecting reference pixels to model systematic noise. Datasets from two types of vAPPs are analysed: a double grating-vAPP (dgvAPP360) that produces a single symmetric PSF and a grating-vAPP (gvAPP180) that produces two D-shaped PSFs. We explore how to choose reference pixels to build temporal systematic noise models in TRAP for them. We then compare the performance of TRAP with previously implemented algorithms that produced the best signal-to-noise ratio (S/N) in companion detections in these datasets. We find that the systematic noise between the two D-shaped PSFs is not as temporally associated as expected. Conversely, there is still a significant number of systematic noise sources that are shared by the dark hole and the bright side in the same PSF. We should choose reference pixels from the same PSF when reducing the dgvAPP360 dataset or the gvAPP180 dataset with TRAP. In these datasets, TRAP achieves results consistent with previous best detections, with an improved S/N for the gvAPP180 dataset. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.14063v1-abstract-full').style.display = 'none'; document.getElementById('2304.14063v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 10 figures, accepted to A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 674, A115 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.05559">arXiv:2303.05559</a> <span> [<a href="https://arxiv.org/pdf/2303.05559">pdf</a>, <a href="https://arxiv.org/format/2303.05559">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/acbd4b">10.3847/1538-3881/acbd4b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Improved companion mass limits for Sirius A with thermal infrared coronagraphy using a vector-apodizing phase plate and time-domain starlight-subtraction techniques </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Long%2C+J+D">Joseph D. Long</a>, <a href="/search/astro-ph?searchtype=author&query=Males%2C+J+R">Jared R. Males</a>, <a href="/search/astro-ph?searchtype=author&query=Haffert%2C+S+Y">Sebastiaan Y. Haffert</a>, <a href="/search/astro-ph?searchtype=author&query=Pearce%2C+L">Logan Pearce</a>, <a href="/search/astro-ph?searchtype=author&query=Marley%2C+M+S">Mark S. Marley</a>, <a href="/search/astro-ph?searchtype=author&query=Morzinski%2C+K+M">Katie M. Morzinski</a>, <a href="/search/astro-ph?searchtype=author&query=Close%2C+L+M">Laird M. Close</a>, <a href="/search/astro-ph?searchtype=author&query=Otten%2C+G+P+P+L">Gilles P. P. L. Otten</a>, <a href="/search/astro-ph?searchtype=author&query=Snik%2C+F">Frans Snik</a>, <a href="/search/astro-ph?searchtype=author&query=Kenworthy%2C+M+A">Matthew A. Kenworthy</a>, <a href="/search/astro-ph?searchtype=author&query=Keller%2C+C+U">Christoph U. Keller</a>, <a href="/search/astro-ph?searchtype=author&query=Hinz%2C+P">Philip Hinz</a>, <a href="/search/astro-ph?searchtype=author&query=Monnier%2C+J+D">John D. Monnier</a>, <a href="/search/astro-ph?searchtype=author&query=Weinberger%2C+A">Alycia Weinberger</a>, <a href="/search/astro-ph?searchtype=author&query=Tolls%2C+V">Volker Tolls</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.05559v1-abstract-short" style="display: inline;"> We use observations with the infrared-optimized MagAO system and Clio camera in 3.9 $渭$m light to place stringent mass constraints on possible undetected companions to Sirius A. We suppress the light from Sirius A by imaging it through a grating vector-apodizing phase plate coronagraph with 180-degree dark region (gvAPP-180). To remove residual starlight in post-processing, we apply a time-domain… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.05559v1-abstract-full').style.display = 'inline'; document.getElementById('2303.05559v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.05559v1-abstract-full" style="display: none;"> We use observations with the infrared-optimized MagAO system and Clio camera in 3.9 $渭$m light to place stringent mass constraints on possible undetected companions to Sirius A. We suppress the light from Sirius A by imaging it through a grating vector-apodizing phase plate coronagraph with 180-degree dark region (gvAPP-180). To remove residual starlight in post-processing, we apply a time-domain principal-components-analysis-based algorithm we call PCA-Temporal (PCAT), which uses eigen-time-series rather than eigen-images to subtract starlight. By casting the problem in terms of eigen-time-series, we reduce the computational cost of post-processing the data, enabling the use of the fully sampled dataset for improved contrast at small separations. We also discuss the impact of retaining fine temporal sampling of the data on final contrast limits. We achieve post-processed contrast limits of $1.5 \times 10^{-6}$ to $9.8 \times 10^{-6}$ outside of 0.75 arcsec which correspond to planet masses of 2.6 to 8.0 $M_J$. These are combined with values from the recent literature of high-contrast imaging observations of Sirius to synthesize an overall completeness fraction as a function of mass and separation. After synthesizing these recent studies and our results, the final completeness analysis rules out 99% of $\ge 9 \ M_J$ planets from 2.5-7 AU. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.05559v1-abstract-full').style.display = 'none'; document.getElementById('2303.05559v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 22 figures, accepted to AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.07354">arXiv:2208.07354</a> <span> [<a href="https://arxiv.org/pdf/2208.07354">pdf</a>, <a href="https://arxiv.org/format/2208.07354">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> XPipeline: Starlight subtraction at scale for MagAO-X </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Long%2C+J+D">Joseph D. Long</a>, <a href="/search/astro-ph?searchtype=author&query=Males%2C+J+R">Jared R. Males</a>, <a href="/search/astro-ph?searchtype=author&query=Haffert%2C+S+Y">Sebastiaan Y. Haffert</a>, <a href="/search/astro-ph?searchtype=author&query=Close%2C+L+M">Laird M. Close</a>, <a href="/search/astro-ph?searchtype=author&query=Morzinski%2C+K+M">Katie M. Morzinski</a>, <a href="/search/astro-ph?searchtype=author&query=Van+Gorkom%2C+K">Kyle Van Gorkom</a>, <a href="/search/astro-ph?searchtype=author&query=Lumbres%2C+J">Jennifer Lumbres</a>, <a href="/search/astro-ph?searchtype=author&query=Foster%2C+W">Warren Foster</a>, <a href="/search/astro-ph?searchtype=author&query=Hedglen%2C+A">Alexander Hedglen</a>, <a href="/search/astro-ph?searchtype=author&query=Kautz%2C+M">Maggie Kautz</a>, <a href="/search/astro-ph?searchtype=author&query=Rodack%2C+A">Alex Rodack</a>, <a href="/search/astro-ph?searchtype=author&query=Schatz%2C+L">Lauren Schatz</a>, <a href="/search/astro-ph?searchtype=author&query=Miller%2C+K">Kelsey Miller</a>, <a href="/search/astro-ph?searchtype=author&query=Doelman%2C+D">David Doelman</a>, <a href="/search/astro-ph?searchtype=author&query=Bos%2C+S">Steven Bos</a>, <a href="/search/astro-ph?searchtype=author&query=Kenworthy%2C+M+A">Matthew A. Kenworthy</a>, <a href="/search/astro-ph?searchtype=author&query=Snik%2C+F">Frans Snik</a>, <a href="/search/astro-ph?searchtype=author&query=Otten%2C+G+P+P+L">Gilles P. P. L. Otten</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2208.07354v1-abstract-short" style="display: inline;"> MagAO-X is an extreme adaptive optics (ExAO) instrument for the Magellan Clay 6.5-meter telescope at Las Campanas Observatory in Chile. Its high spatial and temporal resolution can produce data rates of 1 TB/hr or more, including all AO system telemetry and science images. We describe the tools and architecture we use for commanding, telemetry, and science data transmission and storage. The high d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.07354v1-abstract-full').style.display = 'inline'; document.getElementById('2208.07354v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.07354v1-abstract-full" style="display: none;"> MagAO-X is an extreme adaptive optics (ExAO) instrument for the Magellan Clay 6.5-meter telescope at Las Campanas Observatory in Chile. Its high spatial and temporal resolution can produce data rates of 1 TB/hr or more, including all AO system telemetry and science images. We describe the tools and architecture we use for commanding, telemetry, and science data transmission and storage. The high data volumes require a distributed approach to data processing, and we have developed a pipeline that can scale from a single laptop to dozens of HPC nodes. The same codebase can then be used for both quick-look functionality at the telescope and for post-processing. We present the software and infrastructure we have developed for ExAO data post-processing, and illustrate their use with recently acquired direct-imaging data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.07354v1-abstract-full').style.display = 'none'; document.getElementById('2208.07354v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">From work presented at the SPIE Astronomical Telescopes and Instrumentation 2022 meeting</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.04867">arXiv:2208.04867</a> <span> [<a href="https://arxiv.org/pdf/2208.04867">pdf</a>, <a href="https://arxiv.org/format/2208.04867">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202244727">10.1051/0004-6361/202244727 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Direct discovery of the inner exoplanet in the HD206893 system. Evidence for deuterium burning in a planetary-mass companion </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hinkley%2C+S">S. Hinkley</a>, <a href="/search/astro-ph?searchtype=author&query=Lacour%2C+S">S. Lacour</a>, <a href="/search/astro-ph?searchtype=author&query=Marleau%2C+G+-">G. -D. Marleau</a>, <a href="/search/astro-ph?searchtype=author&query=Lagrange%2C+A+M">A. M. Lagrange</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J+J">J. J. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Kammerer%2C+J">J. Kammerer</a>, <a href="/search/astro-ph?searchtype=author&query=Cumming%2C+A">A. Cumming</a>, <a href="/search/astro-ph?searchtype=author&query=Nowak%2C+M">M. Nowak</a>, <a href="/search/astro-ph?searchtype=author&query=Rodet%2C+L">L. Rodet</a>, <a href="/search/astro-ph?searchtype=author&query=Stolker%2C+T">T. Stolker</a>, <a href="/search/astro-ph?searchtype=author&query=Balmer%2C+W+-">W. -O. Balmer</a>, <a href="/search/astro-ph?searchtype=author&query=Ray%2C+S">S. Ray</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnefoy%2C+M">M. Bonnefoy</a>, <a href="/search/astro-ph?searchtype=author&query=Molli%C3%A8re%2C+P">P. Molli猫re</a>, <a href="/search/astro-ph?searchtype=author&query=Lazzoni%2C+C">C. Lazzoni</a>, <a href="/search/astro-ph?searchtype=author&query=Kennedy%2C+G">G. Kennedy</a>, <a href="/search/astro-ph?searchtype=author&query=Mordasini%2C+C">C. Mordasini</a>, <a href="/search/astro-ph?searchtype=author&query=Abuter%2C+R">R. Abuter</a>, <a href="/search/astro-ph?searchtype=author&query=Aigrain%2C+S">S. Aigrain</a>, <a href="/search/astro-ph?searchtype=author&query=Amorim%2C+A">A. Amorim</a>, <a href="/search/astro-ph?searchtype=author&query=Asensio-Torres%2C+R">R. Asensio-Torres</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Benisty%2C+M">M. Benisty</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+J+-">J. -P. Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Beust%2C+H">H. Beust</a> , et al. (89 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2208.04867v5-abstract-short" style="display: inline;"> Long term precise radial velocity (RV) monitoring of the nearby star HD206893, as well as anomalies in the system proper motion, have suggested the presence of an additional, inner companion in the system. Here we describe the results of a multi-epoch search for the companion responsible for this RV drift and proper motion anomaly using the VLTI/GRAVITY instrument. Utilizing information from ongoi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.04867v5-abstract-full').style.display = 'inline'; document.getElementById('2208.04867v5-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.04867v5-abstract-full" style="display: none;"> Long term precise radial velocity (RV) monitoring of the nearby star HD206893, as well as anomalies in the system proper motion, have suggested the presence of an additional, inner companion in the system. Here we describe the results of a multi-epoch search for the companion responsible for this RV drift and proper motion anomaly using the VLTI/GRAVITY instrument. Utilizing information from ongoing precision RV measurements with the HARPS spectrograph, as well as Gaia host star astrometry, we report a high significance detection of the companion HD206893c over three epochs, with clear evidence for Keplerian orbital motion. Our astrometry with $\sim$50-100 $渭$arcsec precision afforded by GRAVITY allows us to derive a dynamical mass of 12.7$^{+1.2}_{-1.0}$ M$_{\rm Jup}$ and an orbital separation of 3.53$^{+0.08}_{-0.06}$ au for HD206893c. Our fits to the orbits of both companions in the system utilize both Gaia astrometry and RVs to also provide a precise dynamical estimate of the previously uncertain mass of the B component, and therefore derive an age of $155\pm15$ Myr. We find that theoretical atmospheric/evolutionary models incorporating deuterium burning for HD206893c, parameterized by cloudy atmospheres provide a good simultaneous fit to the luminosity of both HD206893B and c. In addition to utilizing long-term RV information, this effort is an early example of a direct imaging discovery of a bona fide exoplanet that was guided in part with Gaia astrometry. Utilizing Gaia astrometry is expected to be one of the primary techniques going forward to identify and characterize additional directly imaged planets. Lastly, this discovery is another example of the power of optical interferometry to directly detect and characterize extrasolar planets where they form at ice-line orbital separations of 2-4\,au. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.04867v5-abstract-full').style.display = 'none'; document.getElementById('2208.04867v5-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.06436">arXiv:2207.06436</a> <span> [<a href="https://arxiv.org/pdf/2207.06436">pdf</a>, <a href="https://arxiv.org/format/2207.06436">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> Connecting SPHERE and CRIRES+ for the characterisation of young exoplanets at high spectral resolution: status update of VLT/HiRISE </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vigan%2C+A">A. Vigan</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+M">M. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Morsy%2C+M+E">M. El Morsy</a>, <a href="/search/astro-ph?searchtype=author&query=Muslimov%2C+E">E. Muslimov</a>, <a href="/search/astro-ph?searchtype=author&query=Viret%2C+A">A. Viret</a>, <a href="/search/astro-ph?searchtype=author&query=Zins%2C+G">G. Zins</a>, <a href="/search/astro-ph?searchtype=author&query=Murray%2C+G">G. Murray</a>, <a href="/search/astro-ph?searchtype=author&query=Costille%2C+A">A. Costille</a>, <a href="/search/astro-ph?searchtype=author&query=Otten%2C+G+P+P+L">G. P. P. L. Otten</a>, <a href="/search/astro-ph?searchtype=author&query=Seemann%2C+U">U. Seemann</a>, <a href="/search/astro-ph?searchtype=author&query=Anwand-Heerwart%2C+H">H. Anwand-Heerwart</a>, <a href="/search/astro-ph?searchtype=author&query=Dohlen%2C+K">K. Dohlen</a>, <a href="/search/astro-ph?searchtype=author&query=Blanchard%2C+P">P. Blanchard</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia%2C+J">J. Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Charles%2C+Y">Y. Charles</a>, <a href="/search/astro-ph?searchtype=author&query=Tchoubaklian%2C+N">N. Tchoubaklian</a>, <a href="/search/astro-ph?searchtype=author&query=Ely%2C+T">T. Ely</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+M">M. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Paufique%2C+J">J. Paufique</a>, <a href="/search/astro-ph?searchtype=author&query=Beuzit%2C+J+-">J. -L. Beuzit</a>, <a href="/search/astro-ph?searchtype=author&query=Houll%C3%A9%2C+M">M. Houll茅</a>, <a href="/search/astro-ph?searchtype=author&query=Costes%2C+J">J. Costes</a>, <a href="/search/astro-ph?searchtype=author&query=Pourcelot%2C+R">R. Pourcelot</a>, <a href="/search/astro-ph?searchtype=author&query=Baraffe%2C+I">I. Baraffe</a>, <a href="/search/astro-ph?searchtype=author&query=Dorn%2C+R">R. Dorn</a> , et al. (10 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2207.06436v1-abstract-short" style="display: inline;"> New generation exoplanet imagers on large ground-based telescopes are highly optimised for the detection of young giant exoplanets in the near-infrared, but they are intrinsically limited for their characterisation by the low spectral resolution of their integral field spectrographs ($R<100$). High-dispersion spectroscopy at $R \gg 10^4$ would be a powerful tool for the characterisation of these p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.06436v1-abstract-full').style.display = 'inline'; document.getElementById('2207.06436v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.06436v1-abstract-full" style="display: none;"> New generation exoplanet imagers on large ground-based telescopes are highly optimised for the detection of young giant exoplanets in the near-infrared, but they are intrinsically limited for their characterisation by the low spectral resolution of their integral field spectrographs ($R<100$). High-dispersion spectroscopy at $R \gg 10^4$ would be a powerful tool for the characterisation of these planets, but there is currently no high-resolution spectrograph with extreme adaptive optics and coronagraphy that would enable such characterisation. With project HiRISE we propose to use fiber coupling to combine the capabilities of two flagship instruments at the Very Large Telescope in Chile: the exoplanet imager SPHERE and the high-resolution spectrograph CRIRES+. The coupling will be implemented at the telescope in early 2023. We provide a general overview of the implementation of HiRISE, of its assembly, integration and testing (AIT) phase in Europe, and a brief assessment of its expected performance based on the final hardware. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.06436v1-abstract-full').style.display = 'none'; document.getElementById('2207.06436v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to SPIE Astronomical Telescopes + Instrumentation 2022, Adaptive Optics Systems VIII, Paper 12185-27</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.00425">arXiv:2206.00425</a> <span> [<a href="https://arxiv.org/pdf/2206.00425">pdf</a>, <a href="https://arxiv.org/format/2206.00425">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243097">10.1051/0004-6361/202243097 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> In-depth direct imaging and spectroscopic characterization of the young Solar System analog HD 95086 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Desgrange%2C+C">C. Desgrange</a>, <a href="/search/astro-ph?searchtype=author&query=Chauvin%2C+G">G. Chauvin</a>, <a href="/search/astro-ph?searchtype=author&query=Christiaens%2C+V">V. Christiaens</a>, <a href="/search/astro-ph?searchtype=author&query=Cantalloube%2C+F">F. Cantalloube</a>, <a href="/search/astro-ph?searchtype=author&query=Lefranc%2C+L+-">L. -X. Lefranc</a>, <a href="/search/astro-ph?searchtype=author&query=Coroller%2C+H+L">H. Le Coroller</a>, <a href="/search/astro-ph?searchtype=author&query=Rubini%2C+P">P. Rubini</a>, <a href="/search/astro-ph?searchtype=author&query=Otten%2C+G+P+P+L">G. P. P. L. Otten</a>, <a href="/search/astro-ph?searchtype=author&query=Beust%2C+H">H. Beust</a>, <a href="/search/astro-ph?searchtype=author&query=Bonavita%2C+M">M. Bonavita</a>, <a href="/search/astro-ph?searchtype=author&query=Delorme%2C+P">P. Delorme</a>, <a href="/search/astro-ph?searchtype=author&query=Devinat%2C+M">M. Devinat</a>, <a href="/search/astro-ph?searchtype=author&query=Gratton%2C+R">R. Gratton</a>, <a href="/search/astro-ph?searchtype=author&query=Lagrange%2C+A+-">A. -M. Lagrange</a>, <a href="/search/astro-ph?searchtype=author&query=Langlois%2C+M">M. Langlois</a>, <a href="/search/astro-ph?searchtype=author&query=Mesa%2C+D">D. Mesa</a>, <a href="/search/astro-ph?searchtype=author&query=Milli%2C+J">J. Milli</a>, <a href="/search/astro-ph?searchtype=author&query=Szul%C3%A1gyi%2C+J">J. Szul谩gyi</a>, <a href="/search/astro-ph?searchtype=author&query=Nowak%2C+M">M. Nowak</a>, <a href="/search/astro-ph?searchtype=author&query=Rodet%2C+L">L. Rodet</a>, <a href="/search/astro-ph?searchtype=author&query=Rojo%2C+P">P. Rojo</a>, <a href="/search/astro-ph?searchtype=author&query=Petrus%2C+S">S. Petrus</a>, <a href="/search/astro-ph?searchtype=author&query=Janson%2C+M">M. Janson</a>, <a href="/search/astro-ph?searchtype=author&query=Henning%2C+T">T. Henning</a>, <a href="/search/astro-ph?searchtype=author&query=Kral%2C+Q">Q. Kral</a> , et al. (26 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2206.00425v1-abstract-short" style="display: inline;"> Context. HD 95086 is a young nearby Solar System analog hosting a giant exoplanet orbiting at 57 au from the star between an inner and outer debris belt. The existence of additional planets has been suggested as the mechanism that maintains the broad cavity between the two belts. Aims. We present a dedicated monitoring of HD 95086 with the VLT/SPHERE instrument to refine the orbital and atmosphe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.00425v1-abstract-full').style.display = 'inline'; document.getElementById('2206.00425v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.00425v1-abstract-full" style="display: none;"> Context. HD 95086 is a young nearby Solar System analog hosting a giant exoplanet orbiting at 57 au from the star between an inner and outer debris belt. The existence of additional planets has been suggested as the mechanism that maintains the broad cavity between the two belts. Aims. We present a dedicated monitoring of HD 95086 with the VLT/SPHERE instrument to refine the orbital and atmospheric properties of HD 95086 b, and to search for additional planets in this system. Methods. SPHERE observations, spread over ten epochs from 2015 to 2019 and including five new datasets, were used. Combined with archival observations, from VLT/NaCo (2012-2013) and Gemini/GPI (2013-2016), the extended set of astrometric measurements allowed us to refine the orbital properties of HD 95086 b. We also investigated the spectral properties and the presence of a circumplanetary disk around HD 95086 b by using the special fitting tool exploring the diversity of several atmospheric models. In addition, we improved our detection limits in order to search for a putative planet c via the K-Stacker algorithm. Results. We extracted for the first time the JH low-resolution spectrum of HD 95086 b by stacking the six best epochs, and confirm its very red spectral energy distribution. Combined with additional datasets from GPI and NaCo, our analysis indicates that this very red color can be explained by the presence of a circumplanetary disk around planet b, with a range of high-temperature solutions (1400-1600 K) and significant extinction (Av > 10 mag), or by a super-solar metallicity atmosphere with lower temperatures (800-1300 K), and small to medium amount of extinction (Av < 10 mag). We do not find any robust candidates for planet c, but give updated constraints on its potential mass and location. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.00425v1-abstract-full').style.display = 'none'; document.getElementById('2206.00425v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">29 pages, 20 figures, A&A, accepted</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 664, A139 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.12280">arXiv:2205.12280</a> <span> [<a href="https://arxiv.org/pdf/2205.12280">pdf</a>, <a href="https://arxiv.org/format/2205.12280">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243408">10.1051/0004-6361/202243408 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Validation of strategies for coupling exoplanet PSFs into single-mode fibres for high-dispersion coronagraphy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Morsy%2C+M+E">M. El Morsy</a>, <a href="/search/astro-ph?searchtype=author&query=Vigan%2C+A">A. Vigan</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+M">M. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Otten%2C+G+P+P+L">G. P. P. L. Otten</a>, <a href="/search/astro-ph?searchtype=author&query=Choquet%2C+E">E. Choquet</a>, <a href="/search/astro-ph?searchtype=author&query=Madec%2C+F">F. Madec</a>, <a href="/search/astro-ph?searchtype=author&query=Costille%2C+A">A. Costille</a>, <a href="/search/astro-ph?searchtype=author&query=Sauvage%2C+J+-">J. -F. Sauvage</a>, <a href="/search/astro-ph?searchtype=author&query=Dohlen%2C+K">K. Dohlen</a>, <a href="/search/astro-ph?searchtype=author&query=Muslimov%2C+E">E. Muslimov</a>, <a href="/search/astro-ph?searchtype=author&query=Pourcelot%2C+R">R. Pourcelot</a>, <a href="/search/astro-ph?searchtype=author&query=Floriot%2C+J">J. Floriot</a>, <a href="/search/astro-ph?searchtype=author&query=Benedetti%2C+J+-">J. -A. Benedetti</a>, <a href="/search/astro-ph?searchtype=author&query=Blanchard%2C+P">P. Blanchard</a>, <a href="/search/astro-ph?searchtype=author&query=Balard%2C+P">P. Balard</a>, <a href="/search/astro-ph?searchtype=author&query=Murray%2C+G">G. Murray</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2205.12280v1-abstract-short" style="display: inline;"> On large ground-based telescopes, the combination of extreme adaptive optics (ExAO) and coronagraphy with high-dispersion spectroscopy (HDS), sometimes referred to as high-dispersion coronagraphy (HDC), is starting to emerge as a powerful technique for the direct characterisation of giant exoplanets. The high spectral resolution not only brings a major gain in terms of accessible spectral features… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.12280v1-abstract-full').style.display = 'inline'; document.getElementById('2205.12280v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.12280v1-abstract-full" style="display: none;"> On large ground-based telescopes, the combination of extreme adaptive optics (ExAO) and coronagraphy with high-dispersion spectroscopy (HDS), sometimes referred to as high-dispersion coronagraphy (HDC), is starting to emerge as a powerful technique for the direct characterisation of giant exoplanets. The high spectral resolution not only brings a major gain in terms of accessible spectral features but also enables a better separation of the stellar and planetary signals. Ongoing projects such as Keck/KPIC, Subaru/REACH, and VLT/HiRISE base their observing strategy on the use of a few science fibres, one of which is dedicated to sampling the planet's signal, while the others sample the residual starlight in the speckle field. The main challenge in this approach is to blindly centre the planet's point spread function (PSF) accurately on the science fibre, with an accuracy of less than 0.1 $位/D$ to maximise the coupling efficiency. In the context of the HiRISE project, three possible centring strategies are foreseen, either based on retro-injecting calibration fibres to localise the position of the science fibre or based on a dedicated centring fibre. We implemented these three approaches, and we compared their centring accuracy using an upgraded setup of the MITHiC high-contrast imaging testbed, which is similar to the setup that will be adopted in HiRISE. Our results demonstrate that reaching a specification accuracy of 0.1 $位/D$ is extremely challenging regardless of the chosen centring strategy. It requires a high level of accuracy at every step of the centring procedure, which can be reached with very stable instruments. We studied the contributors to the centring error in the case of MITHiC and we propose a quantification for some of the most impacting terms. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.12280v1-abstract-full').style.display = 'none'; document.getElementById('2205.12280v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 667, A171 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.10671">arXiv:2109.10671</a> <span> [<a href="https://arxiv.org/pdf/2109.10671">pdf</a>, <a href="https://arxiv.org/format/2109.10671">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202141889">10.1051/0004-6361/202141889 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The mass of Beta Pictoris c from Beta Pictoris b orbital motion </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lacour%2C+S">S. Lacour</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J+J">J. J. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Rodet%2C+L">L. Rodet</a>, <a href="/search/astro-ph?searchtype=author&query=Nowak%2C+M">M. Nowak</a>, <a href="/search/astro-ph?searchtype=author&query=Shangguan%2C+J">J. Shangguan</a>, <a href="/search/astro-ph?searchtype=author&query=Beust%2C+H">H. Beust</a>, <a href="/search/astro-ph?searchtype=author&query=Lagrange%2C+A+-">A. -M. Lagrange</a>, <a href="/search/astro-ph?searchtype=author&query=Abuter%2C+R">R. Abuter</a>, <a href="/search/astro-ph?searchtype=author&query=Amorim%2C+A">A. Amorim</a>, <a href="/search/astro-ph?searchtype=author&query=Asensio-Torres%2C+R">R. Asensio-Torres</a>, <a href="/search/astro-ph?searchtype=author&query=Benisty%2C+M">M. Benisty</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+J+-">J. -P. Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Blunt%2C+S">S. Blunt</a>, <a href="/search/astro-ph?searchtype=author&query=Boccaletti%2C+A">A. Boccaletti</a>, <a href="/search/astro-ph?searchtype=author&query=Bohn%2C+A">A. Bohn</a>, <a href="/search/astro-ph?searchtype=author&query=Bolzer%2C+M+-">M. -L. Bolzer</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnefoy%2C+M">M. Bonnefoy</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnet%2C+H">H. Bonnet</a>, <a href="/search/astro-ph?searchtype=author&query=Bourdarot%2C+G">G. Bourdarot</a>, <a href="/search/astro-ph?searchtype=author&query=Brandner%2C+W">W. Brandner</a>, <a href="/search/astro-ph?searchtype=author&query=Cantalloube%2C+F">F. Cantalloube</a>, <a href="/search/astro-ph?searchtype=author&query=Caselli%2C+P">P. Caselli</a>, <a href="/search/astro-ph?searchtype=author&query=Charnay%2C+B">B. Charnay</a>, <a href="/search/astro-ph?searchtype=author&query=Chauvin%2C+G">G. Chauvin</a>, <a href="/search/astro-ph?searchtype=author&query=Choquet%2C+E">E. Choquet</a> , et al. (74 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2109.10671v1-abstract-short" style="display: inline;"> We aim to demonstrate that the presence and mass of an exoplanet can now be effectively derived from the astrometry of another exoplanet. We combined previous astrometry of $尾$ Pictoris b with a new set of observations from the GRAVITY interferometer. The orbital motion of $尾$ Pictoris b is fit using Markov chain Monte Carlo simulations in Jacobi coordinates. The inner planet, $尾$ Pictoris c, was… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.10671v1-abstract-full').style.display = 'inline'; document.getElementById('2109.10671v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.10671v1-abstract-full" style="display: none;"> We aim to demonstrate that the presence and mass of an exoplanet can now be effectively derived from the astrometry of another exoplanet. We combined previous astrometry of $尾$ Pictoris b with a new set of observations from the GRAVITY interferometer. The orbital motion of $尾$ Pictoris b is fit using Markov chain Monte Carlo simulations in Jacobi coordinates. The inner planet, $尾$ Pictoris c, was also reobserved at a separation of 96\,mas, confirming the previous orbital estimations. From the astrometry of planet b only, we can (i) detect the presence of $尾$ Pictoris c and (ii) constrain its mass to $10.04^{+4.53}_{-3.10}\,M_{\rm Jup}$. If one adds the astrometry of $尾$ Pictoris c, the mass is narrowed down to $9.15^{+1.08}_{-1.06}\,M_{\rm Jup}$. The inclusion of radial velocity measurements does not affect the orbital parameters significantly, but it does slightly decrease the mass estimate to $8.89^{+0.75}_{-0.75}\,M_{\rm Jup}$. With a semimajor axis of $2.68\pm0.02$\,au, a period of $1221\pm15$ days, and an eccentricity of $0.32\pm0.02$, the orbital parameters of $尾$ Pictoris c are now constrained as precisely as those of $尾$ Pictoris b. The orbital configuration is compatible with a high-order mean-motion resonance (7:1). The impact of the resonance on the planets' dynamics would then be negligible with respect to the secular perturbations, which might have played an important role in the eccentricity excitation of the outer planet. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.10671v1-abstract-full').style.display = 'none'; document.getElementById('2109.10671v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted in A&A Letter</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 654, L2 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.08249">arXiv:2106.08249</a> <span> [<a href="https://arxiv.org/pdf/2106.08249">pdf</a>, <a href="https://arxiv.org/format/2106.08249">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202140749">10.1051/0004-6361/202140749 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> GRAVITY K-band spectroscopy of HD 206893 B: brown dwarf or exoplanet </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kammerer%2C+J">J. Kammerer</a>, <a href="/search/astro-ph?searchtype=author&query=Lacour%2C+S">S. Lacour</a>, <a href="/search/astro-ph?searchtype=author&query=Stolker%2C+T">T. Stolker</a>, <a href="/search/astro-ph?searchtype=author&query=Molli%C3%A8re%2C+P">P. Molli猫re</a>, <a href="/search/astro-ph?searchtype=author&query=Sing%2C+D+K">D. K. Sing</a>, <a href="/search/astro-ph?searchtype=author&query=Nasedkin%2C+E">E. Nasedkin</a>, <a href="/search/astro-ph?searchtype=author&query=Kervella%2C+P">P. Kervella</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J+J">J. J. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Ward-Duong%2C+K">K. Ward-Duong</a>, <a href="/search/astro-ph?searchtype=author&query=Nowak%2C+M">M. Nowak</a>, <a href="/search/astro-ph?searchtype=author&query=Abuter%2C+R">R. Abuter</a>, <a href="/search/astro-ph?searchtype=author&query=Amorim%2C+A">A. Amorim</a>, <a href="/search/astro-ph?searchtype=author&query=Asensio-Torres%2C+R">R. Asensio-Torres</a>, <a href="/search/astro-ph?searchtype=author&query=Baub%C3%B6ck%2C+M">M. Baub枚ck</a>, <a href="/search/astro-ph?searchtype=author&query=Benisty%2C+M">M. Benisty</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+J+-">J. -P. Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Beust%2C+H">H. Beust</a>, <a href="/search/astro-ph?searchtype=author&query=Blunt%2C+S">S. Blunt</a>, <a href="/search/astro-ph?searchtype=author&query=Boccaletti%2C+A">A. Boccaletti</a>, <a href="/search/astro-ph?searchtype=author&query=Bohn%2C+A">A. Bohn</a>, <a href="/search/astro-ph?searchtype=author&query=Bolzer%2C+M+-">M. -L. Bolzer</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnefoy%2C+M">M. Bonnefoy</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnet%2C+H">H. Bonnet</a>, <a href="/search/astro-ph?searchtype=author&query=Brandner%2C+W">W. Brandner</a>, <a href="/search/astro-ph?searchtype=author&query=Cantalloube%2C+F">F. Cantalloube</a> , et al. (72 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2106.08249v1-abstract-short" style="display: inline;"> We aim to reveal the nature of the reddest known substellar companion HD 206893 B by studying its near-infrared colors and spectral morphology and by investigating its orbital motion. We fit atmospheric models for giant planets and brown dwarfs and perform spectral retrievals with petitRADTRANS and ATMO on the observed GRAVITY, SPHERE, and GPI spectra of HD 206893 B. To recover its unusual spectra… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.08249v1-abstract-full').style.display = 'inline'; document.getElementById('2106.08249v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.08249v1-abstract-full" style="display: none;"> We aim to reveal the nature of the reddest known substellar companion HD 206893 B by studying its near-infrared colors and spectral morphology and by investigating its orbital motion. We fit atmospheric models for giant planets and brown dwarfs and perform spectral retrievals with petitRADTRANS and ATMO on the observed GRAVITY, SPHERE, and GPI spectra of HD 206893 B. To recover its unusual spectral features, we include additional extinction by high-altitude dust clouds made of enstatite grains in the atmospheric model fits. We also infer the orbital parameters of HD 206893 B by combining the $\sim 100~渭\text{as}$ precision astrometry from GRAVITY with data from the literature and constrain the mass and position of HD 206893 C based on the Gaia proper motion anomaly of the system. The extremely red color and the very shallow $1.4~渭\text{m}$ water absorption feature of HD 206893 B can be fit well with the adapted atmospheric models and spectral retrievals. Altogether, our analysis suggests an age of $\sim 3$-$300~\text{Myr}$ and a mass of $\sim 5$-$30~\text{M}_\text{Jup}$ for HD 206893 B, which is consistent with previous estimates but extends the parameter space to younger and lower-mass objects. The GRAVITY astrometry points to an eccentric orbit ($e = 0.29^{+0.06}_{-0.11}$) with a mutual inclination of $< 34.4~\text{deg}$ with respect to the debris disk of the system. While HD 206893 B could in principle be a planetary-mass companion, this possibility hinges on the unknown influence of the inner companion on the mass estimate of $10^{+5}_{-4}~\text{M}_\text{Jup}$ from radial velocity and Gaia as well as a relatively small but significant Argus moving group membership probability of $\sim 61\%$. However, we find that if the mass of HD 206893 B is $< 30~\text{M}_\text{Jup}$, then the inner companion HD 206893 C should have a mass between $\sim 8$-$15~\text{M}_\text{Jup}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.08249v1-abstract-full').style.display = 'none'; document.getElementById('2106.08249v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 19 figures, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 652, A57 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2104.12078">arXiv:2104.12078</a> <span> [<a href="https://arxiv.org/pdf/2104.12078">pdf</a>, <a href="https://arxiv.org/format/2104.12078">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ac224e">10.3847/1538-3881/ac224e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> TOI-1431b/MASCARA-5b: A Highly Irradiated Ultra-Hot Jupiter Orbiting One of the Hottest & Brightest Known Exoplanet Host Stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Addison%2C+B+C">Brett Christopher Addison</a>, <a href="/search/astro-ph?searchtype=author&query=Knudstrup%2C+E">Emil Knudstrup</a>, <a href="/search/astro-ph?searchtype=author&query=Wong%2C+I">Ian Wong</a>, <a href="/search/astro-ph?searchtype=author&query=Hebrard%2C+G">Guillaume Hebrard</a>, <a href="/search/astro-ph?searchtype=author&query=Dorval%2C+P">Patrick Dorval</a>, <a href="/search/astro-ph?searchtype=author&query=Snellen%2C+I">Ignas Snellen</a>, <a href="/search/astro-ph?searchtype=author&query=Albrecht%2C+S">Simon Albrecht</a>, <a href="/search/astro-ph?searchtype=author&query=Bello-Arufe%2C+A">Aaron Bello-Arufe</a>, <a href="/search/astro-ph?searchtype=author&query=Almenara%2C+J">Jose-Manuel Almenara</a>, <a href="/search/astro-ph?searchtype=author&query=Boisse%2C+I">Isabelle Boisse</a>, <a href="/search/astro-ph?searchtype=author&query=Bonfils%2C+X">Xavier Bonfils</a>, <a href="/search/astro-ph?searchtype=author&query=Dalal%2C+S">Shweta Dalal</a>, <a href="/search/astro-ph?searchtype=author&query=Demangeon%2C+O">Olivier Demangeon</a>, <a href="/search/astro-ph?searchtype=author&query=Hoyer%2C+S">Sergio Hoyer</a>, <a href="/search/astro-ph?searchtype=author&query=Kiefer%2C+F">Flavien Kiefer</a>, <a href="/search/astro-ph?searchtype=author&query=Santos%2C+N+C">N. C. Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Nowak%2C+G">Grzegorz Nowak</a>, <a href="/search/astro-ph?searchtype=author&query=Luque%2C+R">Rafael Luque</a>, <a href="/search/astro-ph?searchtype=author&query=Stangret%2C+M">Monika Stangret</a>, <a href="/search/astro-ph?searchtype=author&query=Palle%2C+E">Enric Palle</a>, <a href="/search/astro-ph?searchtype=author&query=Tronsgaard%2C+R">Rene Tronsgaard</a>, <a href="/search/astro-ph?searchtype=author&query=Antoci%2C+V">Victoria Antoci</a>, <a href="/search/astro-ph?searchtype=author&query=Buchhave%2C+L+A">Lars A. Buchhave</a>, <a href="/search/astro-ph?searchtype=author&query=Gunther%2C+M+N">Maximilian N. Gunther</a>, <a href="/search/astro-ph?searchtype=author&query=Daylan%2C+T">Tansu Daylan</a> , et al. (48 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2104.12078v2-abstract-short" style="display: inline;"> We present the discovery of a highly irradiated and moderately inflated ultra-hot Jupiter, TOI-1431b/MASCARA-5b (HD 201033b), first detected by NASA's Transiting Exoplanet Survey Satellite mission (TESS) and the Multi-site All-Sky CAmeRA (MASCARA). The signal was established to be of planetary origin through radial velocity measurements obtained using SONG, SOPHIE, FIES, NRES, and EXPRES, which sh… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.12078v2-abstract-full').style.display = 'inline'; document.getElementById('2104.12078v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.12078v2-abstract-full" style="display: none;"> We present the discovery of a highly irradiated and moderately inflated ultra-hot Jupiter, TOI-1431b/MASCARA-5b (HD 201033b), first detected by NASA's Transiting Exoplanet Survey Satellite mission (TESS) and the Multi-site All-Sky CAmeRA (MASCARA). The signal was established to be of planetary origin through radial velocity measurements obtained using SONG, SOPHIE, FIES, NRES, and EXPRES, which show a reflex motion of $K=294.1\pm1.1$ m s$^{-1}$. A joint analysis of the TESS and ground-based photometry and radial velocity measurements reveals that TOI-1431b has a mass of $M_{p}=3.12\pm0.18$ $\rm{M_J}$ ($990\pm60$ M$_{\oplus}$), an inflated radius of $R_{p}=1.49\pm0.05$ $\rm{R_J}$ ($16.7\pm0.6$ R$_{\oplus}$), and an orbital period of $P=2.650237\pm0.000003$ d. Analysis of the spectral energy distribution of the host star reveals that the planet orbits a bright ($\mathrm{V}=8.049$ mag) and young ($0.29^{+0.32}_{-0.19}$ Gyr) Am type star with $T_{\rm eff}=7690^{+400}_{-250}$ $\rm{K}$, resulting in a highly irradiated planet with an incident flux of $\langle F \rangle=7.24^{+0.68}_{-0.64}\times$10$^9$ erg s$^{-1}$ cm$^{-2}$ ($5300^{+500}_{-470}\mathrm{S_{\oplus}}$) and an equilibrium temperature of $T_{eq}=2370\pm70$ K. TESS photometry also reveals a secondary eclipse with a depth of $127^{+4}_{-5}$ppm as well as the full phase curve of the planet's thermal emission in the red-optical. This has allowed us to measure the dayside and nightside temperature of its atmosphere as $T_\mathrm{day}=3004\pm64$ K and $T_\mathrm{night}=2583\pm63$ K, the second hottest measured nightside temperature. The planet's low day/night temperature contrast ($\sim$420 K) suggests very efficient heat transport between the dayside and nightside hemispheres. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.12078v2-abstract-full').style.display = 'none'; document.getElementById('2104.12078v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in the Astronomical Journal. 39 pages, 18 figures, and 4 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2104.11251">arXiv:2104.11251</a> <span> [<a href="https://arxiv.org/pdf/2104.11251">pdf</a>, <a href="https://arxiv.org/format/2104.11251">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202140479">10.1051/0004-6361/202140479 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Direct imaging and spectroscopy of exoplanets with the ELT/HARMONI high-contrast module </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Houll%C3%A9%2C+M">Mathis Houll茅</a>, <a href="/search/astro-ph?searchtype=author&query=Vigan%2C+A">Arthur Vigan</a>, <a href="/search/astro-ph?searchtype=author&query=Carlotti%2C+A">Alexis Carlotti</a>, <a href="/search/astro-ph?searchtype=author&query=Choquet%2C+%C3%89">脡lodie Choquet</a>, <a href="/search/astro-ph?searchtype=author&query=Cantalloube%2C+F">Faustine Cantalloube</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+M+W">Mark W. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Sauvage%2C+J">Jean-Fran莽ois Sauvage</a>, <a href="/search/astro-ph?searchtype=author&query=Schwartz%2C+N">Noah Schwartz</a>, <a href="/search/astro-ph?searchtype=author&query=Otten%2C+G+P+P+L">Gilles P. P. L. Otten</a>, <a href="/search/astro-ph?searchtype=author&query=Baraffe%2C+I">Isabelle Baraffe</a>, <a href="/search/astro-ph?searchtype=author&query=Emsenhuber%2C+A">Alexandre Emsenhuber</a>, <a href="/search/astro-ph?searchtype=author&query=Mordasini%2C+C">Christoph Mordasini</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2104.11251v1-abstract-short" style="display: inline;"> Combining high-contrast imaging with medium-resolution spectroscopy has been shown to significantly boost the direct detection of exoplanets. HARMONI, one of the first-light instruments to be mounted on ESO's ELT, will be equipped with a single-conjugated adaptive optics system to reach the diffraction limit of the ELT in H and K bands, a high-contrast module dedicated to exoplanet imaging, and a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.11251v1-abstract-full').style.display = 'inline'; document.getElementById('2104.11251v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.11251v1-abstract-full" style="display: none;"> Combining high-contrast imaging with medium-resolution spectroscopy has been shown to significantly boost the direct detection of exoplanets. HARMONI, one of the first-light instruments to be mounted on ESO's ELT, will be equipped with a single-conjugated adaptive optics system to reach the diffraction limit of the ELT in H and K bands, a high-contrast module dedicated to exoplanet imaging, and a medium-resolution (up to R = 17 000) optical and near-infrared integral field spectrograph. Combined together, these systems will provide unprecedented contrast limits at separations between 50 and 400 mas. In this paper, we estimate the capabilities of the HARMONI high-contrast module for the direct detection of young giant exoplanets. We use an end-to-end model of the instrument to simulate observations based on realistic observing scenarios and conditions. We analyze these data with the so-called "molecule mapping" technique combined to a matched-filter approach, in order to disentangle the companions from the host star and tellurics, and increase the S/N of the planetary signal. We detect planets above 5-sigma at contrasts up to 16 mag and separations down to 75 mas in several spectral configurations of the instrument. We show that molecule mapping allows the detection of companions up to 2.5 mag fainter compared to state-of-the-art high-contrast imaging techniques based on angular differential imaging. We also demonstrate that the performance is not strongly affected by the spectral type of the host star, and that we reach close sensitivities for the best three quartiles of observing conditions at Armazones, which means that HARMONI could be used in near-critical observations during 60 to 70% of telescope time at the ELT. Finally, we simulate planets from population synthesis models to further explore the parameter space that HARMONI and its high-contrast module will soon open. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.11251v1-abstract-full').style.display = 'none'; document.getElementById('2104.11251v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A (14 pages, 9 figures)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 652, A67 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2104.11211">arXiv:2104.11211</a> <span> [<a href="https://arxiv.org/pdf/2104.11211">pdf</a>, <a href="https://arxiv.org/format/2104.11211">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1364/AO.422155">10.1364/AO.422155 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The vector-apodizing phase plate coronagraph: design, current performance, and future development </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Doelman%2C+D+S">D. S. Doelman</a>, <a href="/search/astro-ph?searchtype=author&query=Snik%2C+F">F. Snik</a>, <a href="/search/astro-ph?searchtype=author&query=Por%2C+E+H">E. H. Por</a>, <a href="/search/astro-ph?searchtype=author&query=Bos%2C+S+P">S. P. Bos</a>, <a href="/search/astro-ph?searchtype=author&query=Otten%2C+G+P+P+L">G. P. P. L. Otten</a>, <a href="/search/astro-ph?searchtype=author&query=Kenworthy%2C+M">M. Kenworthy</a>, <a href="/search/astro-ph?searchtype=author&query=Haffert%2C+S+Y">S. Y. Haffert</a>, <a href="/search/astro-ph?searchtype=author&query=Wilby%2C+M">M. Wilby</a>, <a href="/search/astro-ph?searchtype=author&query=Bohn%2C+A+J">A. J. Bohn</a>, <a href="/search/astro-ph?searchtype=author&query=Sutlieff%2C+B+J">B. J. Sutlieff</a>, <a href="/search/astro-ph?searchtype=author&query=Miller%2C+K">K. Miller</a>, <a href="/search/astro-ph?searchtype=author&query=Ouellet%2C+M">M. Ouellet</a>, <a href="/search/astro-ph?searchtype=author&query=de+Boer%2C+J">J. de Boer</a>, <a href="/search/astro-ph?searchtype=author&query=Keller%2C+C+U">C. U. Keller</a>, <a href="/search/astro-ph?searchtype=author&query=Escuti%2C+M+J">M. J. Escuti</a>, <a href="/search/astro-ph?searchtype=author&query=Shi%2C+S">S. Shi</a>, <a href="/search/astro-ph?searchtype=author&query=Warriner%2C+N+Z">N. Z. Warriner</a>, <a href="/search/astro-ph?searchtype=author&query=Hornburg%2C+K+J">K. J. Hornburg</a>, <a href="/search/astro-ph?searchtype=author&query=Birkby%2C+J+L">J. L. Birkby</a>, <a href="/search/astro-ph?searchtype=author&query=Males%2C+J">J. Males</a>, <a href="/search/astro-ph?searchtype=author&query=Morzinski%2C+K+M">K. M. Morzinski</a>, <a href="/search/astro-ph?searchtype=author&query=Close%2C+L+M">L. M. Close</a>, <a href="/search/astro-ph?searchtype=author&query=Codona%2C+J">J. Codona</a>, <a href="/search/astro-ph?searchtype=author&query=Long%2C+J">J. Long</a>, <a href="/search/astro-ph?searchtype=author&query=Schatz%2C+L">L. Schatz</a> , et al. (28 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2104.11211v2-abstract-short" style="display: inline;"> Over the last decade, the vector-apodizing phase plate (vAPP) coronagraph has been developed from concept to on-sky application in many high-contrast imaging systems on 8-m class telescopes. The vAPP is an geometric-phase patterned coronagraph that is inherently broadband, and its manufacturing is enabled only by direct-write technology for liquid-crystal patterns. The vAPP generates two coronagra… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.11211v2-abstract-full').style.display = 'inline'; document.getElementById('2104.11211v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.11211v2-abstract-full" style="display: none;"> Over the last decade, the vector-apodizing phase plate (vAPP) coronagraph has been developed from concept to on-sky application in many high-contrast imaging systems on 8-m class telescopes. The vAPP is an geometric-phase patterned coronagraph that is inherently broadband, and its manufacturing is enabled only by direct-write technology for liquid-crystal patterns. The vAPP generates two coronagraphic PSFs that cancel starlight on opposite sides of the point spread function (PSF) and have opposite circular polarization states. The efficiency, that is the amount of light in these PSFs, depends on the retardance offset from half-wave of the liquid-crystal retarder. Using different liquid-crystal recipes to tune the retardance, different vAPPs operate with high efficiencies ($>96\%$) in the visible and thermal infrared (0.55 $渭$m to 5 $渭$m). Since 2015, seven vAPPs have been installed in a total of six different instruments, including Magellan/MagAO, Magellan/MagAO-X, Subaru/SCExAO, and LBT/LMIRcam. Using two integral field spectrographs installed on the latter two instruments, these vAPPs can provide low-resolution spectra (R$\sim$30) between 1 $渭$m and 5 $渭$m. We review the design process, development, commissioning, on-sky performance, and first scientific results of all commissioned vAPPs. We report on the lessons learned and conclude with perspectives for future developments and applications. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.11211v2-abstract-full').style.display = 'none'; document.getElementById('2104.11211v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">38 pages, 17 figures, accepted for publication in Applied Optics, added NSF grant acknowledgement</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2103.15844">arXiv:2103.15844</a> <span> [<a href="https://arxiv.org/pdf/2103.15844">pdf</a>, <a href="https://arxiv.org/format/2103.15844">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202040157">10.1051/0004-6361/202040157 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Calibration of residual aberrations in exoplanet imagers with large numbers of degrees of freedom </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pourcelot%2C+R">Rapha毛l Pourcelot</a>, <a href="/search/astro-ph?searchtype=author&query=Vigan%2C+A">Arthur Vigan</a>, <a href="/search/astro-ph?searchtype=author&query=Dohlen%2C+K">Kjetil Dohlen</a>, <a href="/search/astro-ph?searchtype=author&query=Rouz%C3%A9%2C+B">Bastien Rouz茅</a>, <a href="/search/astro-ph?searchtype=author&query=Sauvage%2C+J">Jean-Fran莽ois Sauvage</a>, <a href="/search/astro-ph?searchtype=author&query=Morsy%2C+M+E">Mona El Morsy</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+M">Maxime Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=N%27Diaye%2C+M">Mamadou N'Diaye</a>, <a href="/search/astro-ph?searchtype=author&query=Caillat%2C+A">Amandine Caillat</a>, <a href="/search/astro-ph?searchtype=author&query=Choquet%2C+%C3%89">脡lodie Choquet</a>, <a href="/search/astro-ph?searchtype=author&query=Otten%2C+G+P+P+L">Gilles P. P. L. Otten</a>, <a href="/search/astro-ph?searchtype=author&query=Abbinanti%2C+A">Alain Abbinanti</a>, <a href="/search/astro-ph?searchtype=author&query=Balard%2C+P">Philippe Balard</a>, <a href="/search/astro-ph?searchtype=author&query=Carbillet%2C+M">Marcel Carbillet</a>, <a href="/search/astro-ph?searchtype=author&query=Blanchard%2C+P">Philippe Blanchard</a>, <a href="/search/astro-ph?searchtype=author&query=Hulin%2C+J">J茅r茅my Hulin</a>, <a href="/search/astro-ph?searchtype=author&query=Robert%2C+%C3%89">脡milie Robert</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2103.15844v1-abstract-short" style="display: inline;"> Imaging faint objects, such as exoplanets or disks, around nearby stars is extremely challenging because host star images are dominated by the telescope diffraction pattern. Using a coronagraph is an efficient solution for removing diffraction but requires an incoming wavefront with good quality to maximize starlight rejection. On the ground, the most advanced exoplanet imagers use extreme adaptiv… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.15844v1-abstract-full').style.display = 'inline'; document.getElementById('2103.15844v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.15844v1-abstract-full" style="display: none;"> Imaging faint objects, such as exoplanets or disks, around nearby stars is extremely challenging because host star images are dominated by the telescope diffraction pattern. Using a coronagraph is an efficient solution for removing diffraction but requires an incoming wavefront with good quality to maximize starlight rejection. On the ground, the most advanced exoplanet imagers use extreme adaptive optics (ExAO) systems that are based on a deformable mirror (DM) with a large number of actuators to efficiently compensate for high-order aberrations and provide diffraction-limited images. While several exoplanet imagers with DMs using around 1500 actuators are now routinely operating on large telescopes to observe gas giant planets, future systems may require a tenfold increase in the number of degrees of freedom to look for rocky planets. In this paper, we explore wavefront correction with a secondary adaptive optics system that controls a very large number of degrees of freedom that are not corrected by the primary ExAO system. Using Marseille Imaging Testbed for High Contrast (MITHiC), we implement a second stage of adaptive optics with ZELDA, a Zernike wavefront sensor, and a spatial light modulator (SLM) to compensate for the phase aberrations of the bench downstream residual aberrations from adaptive optics. We demonstrate that their correction up to 137 cycles per pupil with nanometric accuracy is possible, provided there is a simple distortion calibration of the pupil and a moderate wavefront low-pass filtering. We also use ZELDA for a fast compensation of ExAO residuals, showing its promising implementation as a second-stage correction for the observation of rocky planets around nearby stars. Finally, we present images with a classical Lyot coronagraph on MITHiC and validate our ability to reach its theoretical performance with our calibration. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.15844v1-abstract-full').style.display = 'none'; document.getElementById('2103.15844v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 649, A170 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.07098">arXiv:2101.07098</a> <span> [<a href="https://arxiv.org/pdf/2101.07098">pdf</a>, <a href="https://arxiv.org/format/2101.07098">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1117/12.2561667">10.1117/12.2561667 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The ExoGRAVITY project: using single mode interferometry to characterize exoplanets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lacour%2C+S">S. Lacour</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J+J">J. J. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Nowak%2C+M">M. Nowak</a>, <a href="/search/astro-ph?searchtype=author&query=Pueyo%2C+L">L. Pueyo</a>, <a href="/search/astro-ph?searchtype=author&query=Eisenhauer%2C+F">F. Eisenhauer</a>, <a href="/search/astro-ph?searchtype=author&query=Lagrange%2C+A+-">A. -M. Lagrange</a>, <a href="/search/astro-ph?searchtype=author&query=Molli%C3%A8re%2C+P">P. Molli猫re</a>, <a href="/search/astro-ph?searchtype=author&query=Abuter%2C+R">R. Abuter</a>, <a href="/search/astro-ph?searchtype=author&query=Amorim%2C+A">A. Amorim</a>, <a href="/search/astro-ph?searchtype=author&query=Asensio-Torres%2C+R">R. Asensio-Torres</a>, <a href="/search/astro-ph?searchtype=author&query=Baub%C3%B6ck%2C+M">M. Baub枚ck</a>, <a href="/search/astro-ph?searchtype=author&query=Benisty%2C+M">M. Benisty</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+J+P">J. P. Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Beust%2C+H">H. Beust</a>, <a href="/search/astro-ph?searchtype=author&query=Blunt%2C+S">S. Blunt</a>, <a href="/search/astro-ph?searchtype=author&query=Boccaletti%2C+A">A. Boccaletti</a>, <a href="/search/astro-ph?searchtype=author&query=Bohn%2C+A">A. Bohn</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnefoy%2C+M">M. Bonnefoy</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnet%2C+H">H. Bonnet</a>, <a href="/search/astro-ph?searchtype=author&query=Brandner%2C+W">W. Brandner</a>, <a href="/search/astro-ph?searchtype=author&query=Cantalloube%2C+F">F. Cantalloube</a>, <a href="/search/astro-ph?searchtype=author&query=Caselli%2C+P">P. Caselli</a>, <a href="/search/astro-ph?searchtype=author&query=Charnay%2C+B">B. Charnay</a>, <a href="/search/astro-ph?searchtype=author&query=Chauvin%2C+G">G. Chauvin</a>, <a href="/search/astro-ph?searchtype=author&query=Choquet%2C+E">E. Choquet</a> , et al. (67 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2101.07098v2-abstract-short" style="display: inline;"> Combining adaptive optics and interferometric observations results in a considerable contrast gain compared to single-telescope, extreme AO systems. Taking advantage of this, the ExoGRAVITY project is a survey of known young giant exoplanets located in the range of 0.1'' to 2'' from their stars. The observations provide astrometric data of unprecedented accuracy, being crucial for refining the orb… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.07098v2-abstract-full').style.display = 'inline'; document.getElementById('2101.07098v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.07098v2-abstract-full" style="display: none;"> Combining adaptive optics and interferometric observations results in a considerable contrast gain compared to single-telescope, extreme AO systems. Taking advantage of this, the ExoGRAVITY project is a survey of known young giant exoplanets located in the range of 0.1'' to 2'' from their stars. The observations provide astrometric data of unprecedented accuracy, being crucial for refining the orbital parameters of planets and illuminating their dynamical histories. Furthermore, GRAVITY will measure non-Keplerian perturbations due to planet-planet interactions in multi-planet systems and measure dynamical masses. Over time, repetitive observations of the exoplanets at medium resolution ($R=500$) will provide a catalogue of K-band spectra of unprecedented quality, for a number of exoplanets. The K-band has the unique properties that it contains many molecular signatures (CO, H$_2$O, CH$_4$, CO$_2$). This allows constraining precisely surface gravity, metallicity, and temperature, if used in conjunction with self-consistent models like Exo-REM. Further, we will use the parameter-retrieval algorithm petitRADTRANS to constrain the C/O ratio of the planets. Ultimately, we plan to produce the first C/O survey of exoplanets, kick-starting the difficult process of linking planetary formation with measured atomic abundances. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.07098v2-abstract-full').style.display = 'none'; document.getElementById('2101.07098v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">SPIE 2020, invited talk</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.04187">arXiv:2101.04187</a> <span> [<a href="https://arxiv.org/pdf/2101.04187">pdf</a>, <a href="https://arxiv.org/format/2101.04187">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/abdb2d">10.3847/1538-3881/abdb2d <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraining the Nature of the PDS 70 Protoplanets with VLTI/GRAVITY </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J+J">J. J. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Vigan%2C+A">A. Vigan</a>, <a href="/search/astro-ph?searchtype=author&query=Lacour%2C+S">S. Lacour</a>, <a href="/search/astro-ph?searchtype=author&query=Nowak%2C+M">M. Nowak</a>, <a href="/search/astro-ph?searchtype=author&query=Stolker%2C+T">T. Stolker</a>, <a href="/search/astro-ph?searchtype=author&query=De+Rosa%2C+R+J">R. J. De Rosa</a>, <a href="/search/astro-ph?searchtype=author&query=Ginzburg%2C+S">S. Ginzburg</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+P">P. Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Abuter%2C+R">R. Abuter</a>, <a href="/search/astro-ph?searchtype=author&query=Amorim%2C+A">A. Amorim</a>, <a href="/search/astro-ph?searchtype=author&query=Asensio-Torres%2C+R">R. Asensio-Torres</a>, <a href="/search/astro-ph?searchtype=author&query=Baubck%2C+M">M. Baubck</a>, <a href="/search/astro-ph?searchtype=author&query=Benisty%2C+M">M. Benisty</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+J+P">J. P. Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Beust%2C+H">H. Beust</a>, <a href="/search/astro-ph?searchtype=author&query=Beuzit%2C+J+-">J. -L. Beuzit</a>, <a href="/search/astro-ph?searchtype=author&query=Blunt%2C+S">S. Blunt</a>, <a href="/search/astro-ph?searchtype=author&query=Boccaletti%2C+A">A. Boccaletti</a>, <a href="/search/astro-ph?searchtype=author&query=Bohn%2C+A">A. Bohn</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnefoy%2C+M">M. Bonnefoy</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnet%2C+H">H. Bonnet</a>, <a href="/search/astro-ph?searchtype=author&query=Brandner%2C+W">W. Brandner</a>, <a href="/search/astro-ph?searchtype=author&query=Cantalloube%2C+F">F. Cantalloube</a>, <a href="/search/astro-ph?searchtype=author&query=Caselli%2C+P">P. Caselli</a>, <a href="/search/astro-ph?searchtype=author&query=Charnay%2C+B">B. Charnay</a> , et al. (79 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2101.04187v2-abstract-short" style="display: inline;"> We present K-band interferometric observations of the PDS 70 protoplanets along with their host star using VLTI/GRAVITY. We obtained K-band spectra and 100 $渭$as precision astrometry of both PDS 70 b and c in two epochs, as well as spatially resolving the hot inner disk around the star. Rejecting unstable orbits, we found a nonzero eccentricity for PDS 70 b of $0.17 \pm 0.06$, a near-circular orbi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.04187v2-abstract-full').style.display = 'inline'; document.getElementById('2101.04187v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.04187v2-abstract-full" style="display: none;"> We present K-band interferometric observations of the PDS 70 protoplanets along with their host star using VLTI/GRAVITY. We obtained K-band spectra and 100 $渭$as precision astrometry of both PDS 70 b and c in two epochs, as well as spatially resolving the hot inner disk around the star. Rejecting unstable orbits, we found a nonzero eccentricity for PDS 70 b of $0.17 \pm 0.06$, a near-circular orbit for PDS 70 c, and an orbital configuration that is consistent with the planets migrating into a 2:1 mean motion resonance. Enforcing dynamical stability, we obtained a 95% upper limit on the mass of PDS 70 b of 10 $M_\textrm{Jup}$, while the mass of PDS 70 c was unconstrained. The GRAVITY K-band spectra rules out pure blackbody models for the photospheres of both planets. Instead, the models with the most support from the data are planetary atmospheres that are dusty, but the nature of the dust is unclear. Any circumplanetary dust around these planets is not well constrained by the planets' 1-5 $渭$m spectral energy distributions (SEDs) and requires longer wavelength data to probe with SED analysis. However with VLTI/GRAVITY, we made the first observations of a circumplanetary environment with sub-au spatial resolution, placing an upper limit of 0.3~au on the size of a bright disk around PDS 70 b. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.04187v2-abstract-full').style.display = 'none'; document.getElementById('2101.04187v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">30 pages, 9 figures, Accepted for publication in AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.02274">arXiv:2011.02274</a> <span> [<a href="https://arxiv.org/pdf/2011.02274">pdf</a>, <a href="https://arxiv.org/ps/2011.02274">ps</a>, <a href="https://arxiv.org/format/2011.02274">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202039250">10.1051/0004-6361/202039250 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Properties of the Hyades, the eclipsing binary HD27130, and the oscillating red giant $蔚$ Tau </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Brogaard%2C+K">K. Brogaard</a>, <a href="/search/astro-ph?searchtype=author&query=Pak%C5%A1tien%C4%97%2C+E">E. Pak拧tien臈</a>, <a href="/search/astro-ph?searchtype=author&query=Grundahl%2C+F">F. Grundahl</a>, <a href="/search/astro-ph?searchtype=author&query=Mikolaitis%2C+%C5%A0">艩. Mikolaitis</a>, <a href="/search/astro-ph?searchtype=author&query=Tautvai%C5%A1ien%C4%97%2C+G">G. Tautvai拧ien臈</a>, <a href="/search/astro-ph?searchtype=author&query=Slumstrup%2C+D">D. Slumstrup</a>, <a href="/search/astro-ph?searchtype=author&query=Talens%2C+G+J+J">G. J. J. Talens</a>, <a href="/search/astro-ph?searchtype=author&query=VandenBerg%2C+D+A">D. A. VandenBerg</a>, <a href="/search/astro-ph?searchtype=author&query=Miglio%2C+A">A. Miglio</a>, <a href="/search/astro-ph?searchtype=author&query=Arentoft%2C+T">T. Arentoft</a>, <a href="/search/astro-ph?searchtype=author&query=Kjeldsen%2C+H">H. Kjeldsen</a>, <a href="/search/astro-ph?searchtype=author&query=Janulis%2C+R">R. Janulis</a>, <a href="/search/astro-ph?searchtype=author&query=Drazdauskas%2C+A">A. Drazdauskas</a>, <a href="/search/astro-ph?searchtype=author&query=Marchini%2C+A">A. Marchini</a>, <a href="/search/astro-ph?searchtype=author&query=Minkevi%C4%8Di%C5%ABt%C4%97%2C+R">R. Minkevi膷i奴t臈</a>, <a href="/search/astro-ph?searchtype=author&query=Stonkut%C4%97%2C+E">E. Stonkut臈</a>, <a href="/search/astro-ph?searchtype=author&query=Bagdonas%2C+V">V. Bagdonas</a>, <a href="/search/astro-ph?searchtype=author&query=Andersen%2C+M+F">M. Fredslund Andersen</a>, <a href="/search/astro-ph?searchtype=author&query=Jessen-Hansen%2C+J">J. Jessen-Hansen</a>, <a href="/search/astro-ph?searchtype=author&query=Pall%C3%A9%2C+P+L">P. L. Pall茅</a>, <a href="/search/astro-ph?searchtype=author&query=Dorval%2C+P">P. Dorval</a>, <a href="/search/astro-ph?searchtype=author&query=Snellen%2C+I+A+G">I. A. G. Snellen</a>, <a href="/search/astro-ph?searchtype=author&query=Otten%2C+G+P+P+L">G. P. P. L. Otten</a>, <a href="/search/astro-ph?searchtype=author&query=White%2C+T+R">T. R. White</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2011.02274v1-abstract-short" style="display: inline;"> Eclipsing binary stars allow derivation of accurate and precise masses and radii. When they reside in star clusters, properties of even higher precision, along with additional information, can be extracted. Asteroseismology of solar-like oscillations offers similar possibilities for single stars. We improve the previously established properties of the Hyades eclipsing binary HD27130 and re-assess… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.02274v1-abstract-full').style.display = 'inline'; document.getElementById('2011.02274v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.02274v1-abstract-full" style="display: none;"> Eclipsing binary stars allow derivation of accurate and precise masses and radii. When they reside in star clusters, properties of even higher precision, along with additional information, can be extracted. Asteroseismology of solar-like oscillations offers similar possibilities for single stars. We improve the previously established properties of the Hyades eclipsing binary HD27130 and re-assess the asteroseismic properties of the giant star $蔚$ Tau. The physical properties of these members of the Hyades are then used to constrain the helium content and age of the cluster. New multi-colour light curves were combined with multi-epoch radial velocities to yield masses and radii of HD27130. $T_{\rm eff}$ was derived from spectroscopy and photometry, and verified using the Gaia parallax. We estimate the cluster age from re-evaluated asteroseismic properties of $蔚$ Tau while using HD27130 to constrain the helium content. The masses and radii, and $T_{\rm eff}$ of HD 27130 were found to be $M=1.0245\pm0.0024 M_{\odot}$, $R=0.9226\pm0.015 R_{\odot}$, $T_{\rm eff}=5650\pm50$ K for the primary, and $M=0.7426\pm0.0016 M_{\odot}$, $R=0.7388\pm0.026 R_{\odot}$, $T_{\rm eff}=4300\pm100$ K for the secondary component. Our re-evaluation of $蔚$ Tau suggests that the previous literature estimates are trustworthy, and that the Hipparcos parallax is more reliable than the Gaia DR2 parallax. The helium content of HD27130 and thus of the Hyades is found to be $Y=0.27$ but with significant model dependence. Correlations with the adopted metallicity results in a robust helium enrichment law with $\frac{螖Y}{螖Z}$ close to 1.2. We estimate the age of the Hyades to be 0.9 $\pm$ 0.1 (stat) $\pm$ 0.1 (sys) Gyr in slight tension with recent age estimates based on the cluster white dwarfs. (abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.02274v1-abstract-full').style.display = 'none'; document.getElementById('2011.02274v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 8 figures, accepted for publication in Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 645, A25 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2009.01841">arXiv:2009.01841</a> <span> [<a href="https://arxiv.org/pdf/2009.01841">pdf</a>, <a href="https://arxiv.org/format/2009.01841">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202038517">10.1051/0004-6361/202038517 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Direct characterization of young giant exoplanets at high spectral resolution by coupling SPHERE and CRIRES+ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Otten%2C+G+P+P+L">G. P. P. L. Otten</a>, <a href="/search/astro-ph?searchtype=author&query=Vigan%2C+A">A. Vigan</a>, <a href="/search/astro-ph?searchtype=author&query=Muslimov%2C+E">E. Muslimov</a>, <a href="/search/astro-ph?searchtype=author&query=N%27Diaye%2C+M">M. N'Diaye</a>, <a href="/search/astro-ph?searchtype=author&query=Choquet%2C+E">E. Choquet</a>, <a href="/search/astro-ph?searchtype=author&query=Seemann%2C+U">U. Seemann</a>, <a href="/search/astro-ph?searchtype=author&query=Dohlen%2C+K">K. Dohlen</a>, <a href="/search/astro-ph?searchtype=author&query=Houll%C3%A9%2C+M">M. Houll茅</a>, <a href="/search/astro-ph?searchtype=author&query=Cristofari%2C+P">P. Cristofari</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+M+W">M. W. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Charles%2C+Y">Y. Charles</a>, <a href="/search/astro-ph?searchtype=author&query=Baraffe%2C+I">I. Baraffe</a>, <a href="/search/astro-ph?searchtype=author&query=Beuzit%2C+J+-">J. -L. Beuzit</a>, <a href="/search/astro-ph?searchtype=author&query=Costille%2C+A">A. Costille</a>, <a href="/search/astro-ph?searchtype=author&query=Dorn%2C+R">R. Dorn</a>, <a href="/search/astro-ph?searchtype=author&query=Morsy%2C+M+E">M. El Morsy</a>, <a href="/search/astro-ph?searchtype=author&query=Kasper%2C+M">M. Kasper</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+M">M. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Mordasini%2C+C">C. Mordasini</a>, <a href="/search/astro-ph?searchtype=author&query=Pourcelot%2C+R">R. Pourcelot</a>, <a href="/search/astro-ph?searchtype=author&query=Reiners%2C+A">A. Reiners</a>, <a href="/search/astro-ph?searchtype=author&query=Sauvage%2C+J+-">J. -F. Sauvage</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2009.01841v2-abstract-short" style="display: inline;"> Studies of atmospheres of directly imaged exoplanets 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 s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.01841v2-abstract-full').style.display = 'inline'; document.getElementById('2009.01841v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.01841v2-abstract-full" style="display: none;"> Studies of atmospheres of directly imaged exoplanets 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 SPHERE and CRIRES+ at the VLT for spectral characterization of directly imaged planets. Using end-to-end simulations of HiRISE we determine the S/N of the detection of molecular species for known exoplanets 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 $尾$ Pic or 51 Eri. 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 two-hour integration times between 50-350 mas for hosts with $H<8.5$ and between 50-700 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. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.01841v2-abstract-full').style.display = 'none'; document.getElementById('2009.01841v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 17 figures. 2 tables. Originally accepted for publication in A&A. Revised version after error in sky background was discovered (too high) and corrected in proofing stage. Revisions made in Abstract, Sections 3-6 and Figures 6-12,C1,C2 that address the changes in performance. Resubmitted to A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2006.09394">arXiv:2006.09394</a> <span> [<a href="https://arxiv.org/pdf/2006.09394">pdf</a>, <a href="https://arxiv.org/format/2006.09394">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202038325">10.1051/0004-6361/202038325 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Retrieving scattering clouds and disequilibrium chemistry in the atmosphere of HR 8799e </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Molli%C3%A8re%2C+P">P. Molli猫re</a>, <a href="/search/astro-ph?searchtype=author&query=Stolker%2C+T">T. Stolker</a>, <a href="/search/astro-ph?searchtype=author&query=Lacour%2C+S">S. Lacour</a>, <a href="/search/astro-ph?searchtype=author&query=Otten%2C+G+P+P+L">G. P. P. L. Otten</a>, <a href="/search/astro-ph?searchtype=author&query=Shangguan%2C+J">J. Shangguan</a>, <a href="/search/astro-ph?searchtype=author&query=Charnay%2C+B">B. Charnay</a>, <a href="/search/astro-ph?searchtype=author&query=Molyarova%2C+T">T. Molyarova</a>, <a href="/search/astro-ph?searchtype=author&query=Nowak%2C+M">M. Nowak</a>, <a href="/search/astro-ph?searchtype=author&query=Henning%2C+T">Th. Henning</a>, <a href="/search/astro-ph?searchtype=author&query=Marleau%2C+G+-">G. -D. Marleau</a>, <a href="/search/astro-ph?searchtype=author&query=Semenov%2C+D+A">D. A. Semenov</a>, <a href="/search/astro-ph?searchtype=author&query=van+Dishoeck%2C+E">E. van Dishoeck</a>, <a href="/search/astro-ph?searchtype=author&query=Eisenhauer%2C+F">F. Eisenhauer</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia%2C+P">P. Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+R+G">R. Garcia Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Girard%2C+J+H">J. H. Girard</a>, <a href="/search/astro-ph?searchtype=author&query=Greenbaum%2C+A+Z">A. Z. Greenbaum</a>, <a href="/search/astro-ph?searchtype=author&query=Hinkley%2C+S">S. Hinkley</a>, <a href="/search/astro-ph?searchtype=author&query=Kervella%2C+P">P. Kervella</a>, <a href="/search/astro-ph?searchtype=author&query=Kreidberg%2C+L">L. Kreidberg</a>, <a href="/search/astro-ph?searchtype=author&query=Maire%2C+A+-">A. -L. Maire</a>, <a href="/search/astro-ph?searchtype=author&query=Nasedkin%2C+E">E. Nasedkin</a>, <a href="/search/astro-ph?searchtype=author&query=Pueyo%2C+L">L. Pueyo</a>, <a href="/search/astro-ph?searchtype=author&query=Snellen%2C+I+A+G">I. A. G. Snellen</a>, <a href="/search/astro-ph?searchtype=author&query=Vigan%2C+A">A. Vigan</a> , et al. (3 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2006.09394v2-abstract-short" style="display: inline;"> Clouds are ubiquitous in exoplanet atmospheres and represent a challenge for the model interpretation of their spectra. Complex cloud models are too numerically costly for generating a large number of spectra, while more efficient models may be too strongly simplified. We aim to constrain the atmospheric properties of the directly imaged planet HR 8799e with a free retrieval approach. We use our r… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.09394v2-abstract-full').style.display = 'inline'; document.getElementById('2006.09394v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.09394v2-abstract-full" style="display: none;"> Clouds are ubiquitous in exoplanet atmospheres and represent a challenge for the model interpretation of their spectra. Complex cloud models are too numerically costly for generating a large number of spectra, while more efficient models may be too strongly simplified. We aim to constrain the atmospheric properties of the directly imaged planet HR 8799e with a free retrieval approach. We use our radiative transfer code petitRADTRANS for generating spectra, which we couple to the PyMultiNest tool. We added the effect of multiple scattering which is important for treating clouds. Two cloud model parameterizations are tested: the first incorporates the mixing and settling of condensates, the second simply parameterizes the functional form of the opacity. In mock retrievals, using an inadequate cloud model may result in atmospheres that are more isothermal and less cloudy than the input. Applying our framework on observations of HR 8799e made with the GPI, SPHERE and GRAVITY, we find a cloudy atmosphere governed by disequilibrium chemistry, confirming previous analyses. We retrieve that ${\rm C/O}=0.60_{-0.08}^{+0.07}$. Other models have not yet produced a well constrained C/O value for this planet. The retrieved C/O values of both cloud models are consistent, while leading to different atmospheric structures: cloudy, or more isothermal and less cloudy. Fitting the observations with the self-consistent Exo-REM model leads to comparable results, while not constraining C/O. With data from the most sensitive instruments, retrieval analyses of directly imaged planets are possible. The inferred C/O ratio of HR 8799e is independent of the cloud model and thus appears to be a robust. This C/O is consistent with stellar, which could indicate that the HR 8799e formed outside the CO$_2$ or CO iceline. As it is the innermost planet of the system, this constraint could apply to all HR 8799 planets. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.09394v2-abstract-full').style.display = 'none'; document.getElementById('2006.09394v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A, 28 pages, 13 figures, updated author list</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 640, A131 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1906.05254">arXiv:1906.05254</a> <span> [<a href="https://arxiv.org/pdf/1906.05254">pdf</a>, <a href="https://arxiv.org/format/1906.05254">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201936082">10.1051/0004-6361/201936082 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MASCARA-3b: A hot Jupiter transiting a bright F7 star in an aligned orbit </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hjorth%2C+M">M. Hjorth</a>, <a href="/search/astro-ph?searchtype=author&query=Albrecht%2C+S">S. Albrecht</a>, <a href="/search/astro-ph?searchtype=author&query=Talens%2C+G+J+J">G. J. J. Talens</a>, <a href="/search/astro-ph?searchtype=author&query=Grundahl%2C+F">F. Grundahl</a>, <a href="/search/astro-ph?searchtype=author&query=Justesen%2C+A+B">A. B. Justesen</a>, <a href="/search/astro-ph?searchtype=author&query=Otten%2C+G+P+P+L">G. P. P. L. Otten</a>, <a href="/search/astro-ph?searchtype=author&query=Antoci%2C+V">V. Antoci</a>, <a href="/search/astro-ph?searchtype=author&query=Dorval%2C+P">P. Dorval</a>, <a href="/search/astro-ph?searchtype=author&query=Foxell%2C+E">E. Foxell</a>, <a href="/search/astro-ph?searchtype=author&query=Andersen%2C+M+F">M. Fredslund Andersen</a>, <a href="/search/astro-ph?searchtype=author&query=Murgas%2C+F">F. Murgas</a>, <a href="/search/astro-ph?searchtype=author&query=Palle%2C+E">E. Palle</a>, <a href="/search/astro-ph?searchtype=author&query=Stuik%2C+R">R. Stuik</a>, <a href="/search/astro-ph?searchtype=author&query=Snellen%2C+I+A+G">I. A. G. Snellen</a>, <a href="/search/astro-ph?searchtype=author&query=Van+Eylen%2C+V">V. Van Eylen</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1906.05254v2-abstract-short" style="display: inline;"> We report the discovery of MASCARA-3b, a hot Jupiter orbiting its bright (V = 8.33) late F-type host every $5.55149\pm 0.00001$ days in an almost circular orbit ($e = 0.050^{+0.020}_{-0.017}$). This is the fourth exoplanet discovered with the Multi-site All-Sky CAmeRA (MASCARA), and the first of these that orbits a late-type star. Follow-up spectroscopic measurements were obtained in and out of tr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.05254v2-abstract-full').style.display = 'inline'; document.getElementById('1906.05254v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1906.05254v2-abstract-full" style="display: none;"> We report the discovery of MASCARA-3b, a hot Jupiter orbiting its bright (V = 8.33) late F-type host every $5.55149\pm 0.00001$ days in an almost circular orbit ($e = 0.050^{+0.020}_{-0.017}$). This is the fourth exoplanet discovered with the Multi-site All-Sky CAmeRA (MASCARA), and the first of these that orbits a late-type star. Follow-up spectroscopic measurements were obtained in and out of transit with the Hertzsprung SONG telescope. Combining the MASCARA photometry and SONG radial velocities reveals a radius and mass of $1.36\pm 0.05$ $R_{\text{Jup}}$ and $4.2\pm 0.2$ $M_{\text{Jup}}$. In addition, SONG spectroscopic transit observations were obtained on two separate nights. From analyzing the mean out-of-transit broadening function, we obtain $v\sin i_{\star} = 20.4\pm 0.4$ km s$^{-1}$. In addition, investigating the Rossiter-McLaughlin effect, as observed in the distortion of the stellar lines directly and through velocity anomalies, we find the projected obliquity to be $位= 1.2^{+8.2}_{-7.4}$ deg, which is consistent with alignment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.05254v2-abstract-full').style.display = 'none'; document.getElementById('1906.05254v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 June, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 7 figures, 6 tables; accepted in A&A. Updated for the accepted and proof-readed version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 631, A76 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1904.02733">arXiv:1904.02733</a> <span> [<a href="https://arxiv.org/pdf/1904.02733">pdf</a>, <a href="https://arxiv.org/format/1904.02733">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201935611">10.1051/0004-6361/201935611 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MASCARA-4 b/bRing-1b - A retrograde hot Jupiter around the bright A3V star HD 85628 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dorval%2C+P">P. Dorval</a>, <a href="/search/astro-ph?searchtype=author&query=Talens%2C+G+J+J">G. J. J. Talens</a>, <a href="/search/astro-ph?searchtype=author&query=Otten%2C+G+P+P+L">G. P. P. L. Otten</a>, <a href="/search/astro-ph?searchtype=author&query=Brahm%2C+R">R. Brahm</a>, <a href="/search/astro-ph?searchtype=author&query=Jord%C3%A1n%2C+A">A. Jord谩n</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzi%2C+L">L. Vanzi</a>, <a href="/search/astro-ph?searchtype=author&query=Zapata%2C+A">A. Zapata</a>, <a href="/search/astro-ph?searchtype=author&query=Henry%2C+T">T. Henry</a>, <a href="/search/astro-ph?searchtype=author&query=Paredes%2C+L">L. Paredes</a>, <a href="/search/astro-ph?searchtype=author&query=Jao%2C+W+C">W. C. Jao</a>, <a href="/search/astro-ph?searchtype=author&query=James%2C+H">H. James</a>, <a href="/search/astro-ph?searchtype=author&query=Hinojosa%2C+R">R. Hinojosa</a>, <a href="/search/astro-ph?searchtype=author&query=Bakos%2C+G+A">G. A. Bakos</a>, <a href="/search/astro-ph?searchtype=author&query=Csubry%2C+Z">Z. Csubry</a>, <a href="/search/astro-ph?searchtype=author&query=Bhatti%2C+W">W. Bhatti</a>, <a href="/search/astro-ph?searchtype=author&query=Suc%2C+V">V. Suc</a>, <a href="/search/astro-ph?searchtype=author&query=Osip%2C+D">D. Osip</a>, <a href="/search/astro-ph?searchtype=author&query=Mamajek%2C+E+E">E. E. Mamajek</a>, <a href="/search/astro-ph?searchtype=author&query=Mellon%2C+S+N">S. N. Mellon</a>, <a href="/search/astro-ph?searchtype=author&query=Wyttenbach%2C+A">A. Wyttenbach</a>, <a href="/search/astro-ph?searchtype=author&query=Stuik%2C+R">R. Stuik</a>, <a href="/search/astro-ph?searchtype=author&query=Kenworthy%2C+M">M. Kenworthy</a>, <a href="/search/astro-ph?searchtype=author&query=Bailey%2C+J">J. Bailey</a>, <a href="/search/astro-ph?searchtype=author&query=Ireland%2C+M">M. Ireland</a>, <a href="/search/astro-ph?searchtype=author&query=Crawford%2C+S">S. Crawford</a> , et al. (3 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1904.02733v1-abstract-short" style="display: inline;"> In this paper, we aim to characterize a transiting planetary candidate in the southern skies found in the combined MASCARA and bRing data sets of HD 85628, an A3V star of V = 8.2 mag at a distance 172 pc, to confirm its planetary nature. The candidate was originally detected in data obtained jointly with the MASCARA and bRing instruments using a BLS search for transit events. Further photometry wa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.02733v1-abstract-full').style.display = 'inline'; document.getElementById('1904.02733v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.02733v1-abstract-full" style="display: none;"> In this paper, we aim to characterize a transiting planetary candidate in the southern skies found in the combined MASCARA and bRing data sets of HD 85628, an A3V star of V = 8.2 mag at a distance 172 pc, to confirm its planetary nature. The candidate was originally detected in data obtained jointly with the MASCARA and bRing instruments using a BLS search for transit events. Further photometry was taken by the 0.7 m CHAT, and radial velocity measurements with FIDEOS on the ESO 1.0 m Telescope. High resolution spectra during a transit were taken with CHIRON on the SMARTS 1.5 m telescope to target the Doppler shadow of the candidate. We confirm the existence of a hot Jupiter transiting the bright A3V star HD 85628, which we co-designate as MASCARA-4b and bRing-1b. It is in a 2.824 day orbit, with an estimated planet radius of $1.53 ^{0.07}_{0.04}$ $R_{\rm{Jup}}$ and an estimated planet mass of $3.1 \pm 0.9$ $M_{\rm{Jup}}$, putting it well within the planet mass regime.. The CHAT observations show a partial transit, reducing the probability that the transit was around a faint background star. The CHIRON observations show a clear Doppler shadow, implying that the transiting object is in a retrograde orbit with $|位| = 247.5 \pm 1.6 $\textdegree. The planet orbits at at a distance of 0.047 $\pm$ 0.004 AU from the star and has a zero-albedo equilibrium temperature of 2100 $\pm$ 100 K. In addition, we find that HD 85628 has a previously unreported stellar companion star in the Gaia DR2 data demonstrating common proper motion and parallax at 4.3 arcsecond separation (projected separation $\sim$740 AU), and with absolute magnitude consistent with being a K/M dwarf. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.02733v1-abstract-full').style.display = 'none'; document.getElementById('1904.02733v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 8 figures, submitted to A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 635, A60 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1807.04361">arXiv:1807.04361</a> <span> [<a href="https://arxiv.org/pdf/1807.04361">pdf</a>, <a href="https://arxiv.org/format/1807.04361">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> The hunt for Sirius Ab: Comparison of algorithmic sky and PSF estimation performance in deep coronagraphic thermal-IR high contrast imaging </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Long%2C+J+D">Joseph D. Long</a>, <a href="/search/astro-ph?searchtype=author&query=Males%2C+J+R">Jared R. Males</a>, <a href="/search/astro-ph?searchtype=author&query=Morzinski%2C+K+M">Katie M. Morzinski</a>, <a href="/search/astro-ph?searchtype=author&query=Close%2C+L+M">Laird M. Close</a>, <a href="/search/astro-ph?searchtype=author&query=Snik%2C+F">Frans Snik</a>, <a href="/search/astro-ph?searchtype=author&query=Kenworthy%2C+M+A">Matthew A. Kenworthy</a>, <a href="/search/astro-ph?searchtype=author&query=Otten%2C+G+P+P+L">Gilles P. P. L. Otten</a>, <a href="/search/astro-ph?searchtype=author&query=Monnier%2C+J">John Monnier</a>, <a href="/search/astro-ph?searchtype=author&query=Tolls%2C+V">Volker Tolls</a>, <a href="/search/astro-ph?searchtype=author&query=Weinberger%2C+A">Alycia Weinberger</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1807.04361v1-abstract-short" style="display: inline;"> Despite promising astrometric signals, to date there has been no success in direct imaging of a hypothesized third member of the Sirius system. Using the Clio instrument and MagAO adaptive optics system on the Magellan Clay 6.5 m telescope, we have obtained extensive imagery of Sirius through a vector apodizing phase plate (vAPP) coronagraph in a narrowband filter at 3.9 microns. The vAPP coronagr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.04361v1-abstract-full').style.display = 'inline'; document.getElementById('1807.04361v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1807.04361v1-abstract-full" style="display: none;"> Despite promising astrometric signals, to date there has been no success in direct imaging of a hypothesized third member of the Sirius system. Using the Clio instrument and MagAO adaptive optics system on the Magellan Clay 6.5 m telescope, we have obtained extensive imagery of Sirius through a vector apodizing phase plate (vAPP) coronagraph in a narrowband filter at 3.9 microns. The vAPP coronagraph and MagAO allow us to be sensitive to planets much less massive than the limits set by previous non-detections. However, analysis of these data presents challenges due to the target's brightness and unique characteristics of the instrument. We present a comparison of dimensionality reduction techniques to construct background illumination maps for the whole detector using the areas of the detector that are not dominated by starlight. Additionally, we describe a procedure for sub-pixel alignment of vAPP data using a physical-optics-based model of the coronagraphic PSF. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.04361v1-abstract-full').style.display = 'none'; document.getElementById('1807.04361v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 July, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 4 figures. Submitted to Proceedings of SPIE Astronomical Telescopes + Instrumentation, Adaptive Optics Systems VI</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1806.10618">arXiv:1806.10618</a> <span> [<a href="https://arxiv.org/pdf/1806.10618">pdf</a>, <a href="https://arxiv.org/format/1806.10618">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Bringing high-spectral resolution to VLT/SPHERE with a fibre coupling to VLT/CRIRES+ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vigan%2C+A">A. Vigan</a>, <a href="/search/astro-ph?searchtype=author&query=Otten%2C+G+P+P+L">G. P. P. L. Otten</a>, <a href="/search/astro-ph?searchtype=author&query=Muslimov%2C+E">E. Muslimov</a>, <a href="/search/astro-ph?searchtype=author&query=Dohlen%2C+K">K. Dohlen</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+M+W">M. W. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Seemann%2C+U">U. Seemann</a>, <a href="/search/astro-ph?searchtype=author&query=Beuzit%2C+J+-">J. -L. Beuzit</a>, <a href="/search/astro-ph?searchtype=author&query=Dorn%2C+R">R. Dorn</a>, <a href="/search/astro-ph?searchtype=author&query=Kasper%2C+M">M. Kasper</a>, <a href="/search/astro-ph?searchtype=author&query=Mouillet%2C+D">D. Mouillet</a>, <a href="/search/astro-ph?searchtype=author&query=Baraffe%2C+I">I. Baraffe</a>, <a href="/search/astro-ph?searchtype=author&query=Reiners%2C+A">A. Reiners</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1806.10618v1-abstract-short" style="display: inline;"> Atmospheric composition provides essential markers of the most fundamental properties of giant exoplanets, such as their formation mechanism or internal structure. New-generation exoplanet imagers, like VLT/SPHERE or Gemini/GPI, have been designed to achieve very high contrast (>15 mag) at small angular separations ($<$0.5\as) for the detection of young giant planets in the near-infrared, but they… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.10618v1-abstract-full').style.display = 'inline'; document.getElementById('1806.10618v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1806.10618v1-abstract-full" style="display: none;"> Atmospheric composition provides essential markers of the most fundamental properties of giant exoplanets, such as their formation mechanism or internal structure. New-generation exoplanet imagers, like VLT/SPHERE or Gemini/GPI, have been designed to achieve very high contrast (>15 mag) at small angular separations ($<$0.5\as) for the detection of young giant planets in the near-infrared, but they only provide very low spectral resolutions ($R<100$) for their characterization. High-dispersion spectroscopy at resolutions up to $10^5$ is one of the most promising pathways for the detailed characterization of exoplanets, but it is currently out of reach for most directly imaged exoplanets because current high-dispersion spectrographs in the near-infrared lack coronagraphs to attenuate the stellar signal and the spatial resolution necessary to resolve the planet. Project HiRISE (High-Resolution Imaging and Spectroscopy of Exoplanets) ambitions to develop a demonstrator that will combine the capabilities of two flagship instruments installed on the ESO Very Large Telescope, the high-contrast exoplanet imager SPHERE and the high-resolution spectrograph CRIRES+, with the goal of answering fundamental questions on the formation, composition and evolution of young planets. In this work, we will present the project, the first set of realistic simulations and the preliminary design of the fiber injection unit that will be implemented in SPHERE. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.10618v1-abstract-full').style.display = 'none'; document.getElementById('1806.10618v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 June, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 12 figures. Proceeding of the SPIE Astronomical Telescopes + Instrumentation Conference, 10 - 15 June 2018</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1806.02247">arXiv:1806.02247</a> <span> [<a href="https://arxiv.org/pdf/1806.02247">pdf</a>, <a href="https://arxiv.org/format/1806.02247">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201833142">10.1051/0004-6361/201833142 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Studying bright variable stars with the Multi-site All-Sky CAmeRA (MASCARA) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Burggraaff%2C+O">O. Burggraaff</a>, <a href="/search/astro-ph?searchtype=author&query=Talens%2C+G+J+J">G. J. J. Talens</a>, <a href="/search/astro-ph?searchtype=author&query=Spronck%2C+J">J. Spronck</a>, <a href="/search/astro-ph?searchtype=author&query=Lesage%2C+A+-">A. -L. Lesage</a>, <a href="/search/astro-ph?searchtype=author&query=Stuik%2C+R">R. Stuik</a>, <a href="/search/astro-ph?searchtype=author&query=Otten%2C+G+P+P+L">G. P. P. L. Otten</a>, <a href="/search/astro-ph?searchtype=author&query=Van+Eylen%2C+V">V. Van Eylen</a>, <a href="/search/astro-ph?searchtype=author&query=Pollacco%2C+D">D. Pollacco</a>, <a href="/search/astro-ph?searchtype=author&query=Snellen%2C+I+A+G">I. A. G. Snellen</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1806.02247v1-abstract-short" style="display: inline;"> The Multi-site All-Sky CAmeRA (MASCARA) aims to find the brightest transiting planet systems by monitoring the full sky at magnitudes $4<V<8.4$, taking data every 6.4 seconds. The northern station has been operational on La Palma since February 2015. These data can also be used for other scientific purposes, such as the study of variable stars. In this paper we aim to assess the value of MASCARA d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.02247v1-abstract-full').style.display = 'inline'; document.getElementById('1806.02247v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1806.02247v1-abstract-full" style="display: none;"> The Multi-site All-Sky CAmeRA (MASCARA) aims to find the brightest transiting planet systems by monitoring the full sky at magnitudes $4<V<8.4$, taking data every 6.4 seconds. The northern station has been operational on La Palma since February 2015. These data can also be used for other scientific purposes, such as the study of variable stars. In this paper we aim to assess the value of MASCARA data for studying variable stars by determining to what extent known variable stars can be recovered and characterised, and how well new, unknown variables can be discovered. We used the first 14 months of MASCARA data, consisting of the light curves of 53 401 stars with up to one million flux points per object. All stars were cross-matched with the VSX catalogue to identify known variables. The MASCARA light curves were searched for periodic flux variability using generalised Lomb-Scargle periodograms. If significant variability of a known variable was detected, the found period and amplitude were compared with those listed in the VSX database. If no previous record of variability was found, the data were phase folded to attempt a classification. Of the 1919 known variable stars in the MASCARA sample with periods $0.1<P<10$ days, amplitudes $>2\%$, and that have more than 80 hours of data, $93.5\%$ are recovered. In addition, the periods of $210$ stars without a previous VSX record were determined, and $282$ candidate variable stars were newly identified. The O'Connell effect is seen in seven eclipsing binaries, of which two have no previous record of this effect. MASCARA data are very well suited to study known variable stars. They also serve as a powerful means to find new variables among the brightest stars in the sky. Follow-up is required to ensure that the observed variability does not originate from faint background objects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.02247v1-abstract-full').style.display = 'none'; document.getElementById('1806.02247v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 June, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 22 figures, Accepted for publication in A&A, tables and >3000 light curves will be available on CDS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 617, A32 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1805.03102">arXiv:1805.03102</a> <span> [<a href="https://arxiv.org/pdf/1805.03102">pdf</a>, <a href="https://arxiv.org/format/1805.03102">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201832963">10.1051/0004-6361/201832963 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Na I and H$伪$ absorption features in the atmosphere of MASCARA-2b/KELT-20b </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Casasayas-Barris%2C+N">N. Casasayas-Barris</a>, <a href="/search/astro-ph?searchtype=author&query=Palle%2C+E">E. Palle</a>, <a href="/search/astro-ph?searchtype=author&query=Yan%2C+F">F. Yan</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+G">G. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Albrecht%2C+S">S. Albrecht</a>, <a href="/search/astro-ph?searchtype=author&query=Nortmann%2C+L">L. Nortmann</a>, <a href="/search/astro-ph?searchtype=author&query=Van+Eylen%2C+V">V. Van Eylen</a>, <a href="/search/astro-ph?searchtype=author&query=Snellen%2C+I">I. Snellen</a>, <a href="/search/astro-ph?searchtype=author&query=Talens%2C+G+J+J">G. J. J. Talens</a>, <a href="/search/astro-ph?searchtype=author&query=Hernandez%2C+J+I+G">J. I. Gonzalez Hernandez</a>, <a href="/search/astro-ph?searchtype=author&query=Rebolo%2C+R">R. Rebolo</a>, <a href="/search/astro-ph?searchtype=author&query=Otten%2C+G+P+P+L">G. P. P. L. Otten</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1805.03102v1-abstract-short" style="display: inline;"> We have used the HARPS-North high resolution spectrograph ($\mathcal{R}$=115 000) at TNG to observe one transit of the highly irradiated planet MASCARA-2b/KELT-20b. Using only one transit observation, we are able to clearly resolve the spectral features of the atomic sodium (Na I) doublet and the H$伪$ line in its atmosphere, measuring absorption depths of 0.17$\pm$0.03$\%$ and 0.59$\pm$0.08$\%$ fo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.03102v1-abstract-full').style.display = 'inline'; document.getElementById('1805.03102v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1805.03102v1-abstract-full" style="display: none;"> We have used the HARPS-North high resolution spectrograph ($\mathcal{R}$=115 000) at TNG to observe one transit of the highly irradiated planet MASCARA-2b/KELT-20b. Using only one transit observation, we are able to clearly resolve the spectral features of the atomic sodium (Na I) doublet and the H$伪$ line in its atmosphere, measuring absorption depths of 0.17$\pm$0.03$\%$ and 0.59$\pm$0.08$\%$ for a 0.75 $脜$ passband, respectively. These absorptions are corroborated with the transmission measured from their respective transmission light curves, which show a large Rossiter-McLaughlin effect. In case of H$伪$, this absorption corresponds to an effective radius of $R_位/R_P$=1.20$\pm$0.04. While the S/N of the final transmission spectrum is not sufficient to adjust different temperature profiles to the lines, we find that higher temperatures than the equilibrium are needed to explain the lines contrast. Particularly, we find that the Na I lines core require a temperature of T=4210$\pm$180K and that H$伪$ requires T=4330$\pm$520K. MASCARA-2b, like other planets orbiting A-type stars, receives a large amount of UV energy from its host star. This energy excites the atomic hydrogen and produces H$伪$ absorption, leading to the expansion and abrasion of the atmosphere. The study of other Balmer lines in the transmission spectrum would allow the determination of the atmospheric temperature profile and the calculation of the lifetime of the atmosphere. In the case of MASCARA-2b, residual features are observed in the H$尾$ and H$纬$ lines, but they are not statistically significant. More transit observations are needed to confirm our findings in Na I and H$伪$, and to build up enough S/N to explore the presence of H$尾$ and H$纬$ planetary absorptions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.03102v1-abstract-full').style.display = 'none'; document.getElementById('1805.03102v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 May, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 12 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 616, A151 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1707.04262">arXiv:1707.04262</a> <span> [<a href="https://arxiv.org/pdf/1707.04262">pdf</a>, <a href="https://arxiv.org/format/1707.04262">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201731282">10.1051/0004-6361/201731282 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MASCARA-1 b: A hot Jupiter transiting a bright $m_V=8.3$ A-star in a misaligned orbit </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Talens%2C+G+J+J">G. J. J. Talens</a>, <a href="/search/astro-ph?searchtype=author&query=Albrecht%2C+S">S. Albrecht</a>, <a href="/search/astro-ph?searchtype=author&query=Spronck%2C+J+F+P">J. F. P. Spronck</a>, <a href="/search/astro-ph?searchtype=author&query=Lesage%2C+A+-">A. -L. Lesage</a>, <a href="/search/astro-ph?searchtype=author&query=Otten%2C+G+P+P+L">G. P. P. L. Otten</a>, <a href="/search/astro-ph?searchtype=author&query=Stuik%2C+R">R. Stuik</a>, <a href="/search/astro-ph?searchtype=author&query=Van+Eylen%2C+V">V. Van Eylen</a>, <a href="/search/astro-ph?searchtype=author&query=Van+Winckel%2C+H">H. Van Winckel</a>, <a href="/search/astro-ph?searchtype=author&query=Pollacco%2C+D">D. Pollacco</a>, <a href="/search/astro-ph?searchtype=author&query=McCormac%2C+J">J. McCormac</a>, <a href="/search/astro-ph?searchtype=author&query=Grundahl%2C+F">F. Grundahl</a>, <a href="/search/astro-ph?searchtype=author&query=Andersen%2C+M+F">M. Fredslund Andersen</a>, <a href="/search/astro-ph?searchtype=author&query=Antoci%2C+V">V. Antoci</a>, <a href="/search/astro-ph?searchtype=author&query=Snellen%2C+I+A+G">I. A. G Snellen</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1707.04262v2-abstract-short" style="display: inline;"> We report the discovery of MASCARA-1 b, the first exoplanet discovered with the Multi-site All-Sky CAmeRA (MASCARA). It is a hot Jupiter orbiting a bright $m_V=8.3$, rapidly rotating ($v\sin i_\star > 100~\rm{km~s}^{-1}$) A8 star with a period of $2.148780\pm8\times10^{-6} ~\rm{days}$. The planet has a mass and radius of $3.7\pm0.9~\rm{M}_{\rm{Jup}}$ and $1.5\pm0.3~\rm{R}_{\rm{Jup}}$, respectively… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.04262v2-abstract-full').style.display = 'inline'; document.getElementById('1707.04262v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1707.04262v2-abstract-full" style="display: none;"> We report the discovery of MASCARA-1 b, the first exoplanet discovered with the Multi-site All-Sky CAmeRA (MASCARA). It is a hot Jupiter orbiting a bright $m_V=8.3$, rapidly rotating ($v\sin i_\star > 100~\rm{km~s}^{-1}$) A8 star with a period of $2.148780\pm8\times10^{-6} ~\rm{days}$. The planet has a mass and radius of $3.7\pm0.9~\rm{M}_{\rm{Jup}}$ and $1.5\pm0.3~\rm{R}_{\rm{Jup}}$, respectively. As with most hot Jupiters transiting early-type stars we find a misalignment between the planet orbital axis and the stellar spin axis, which may be signature of the formation and migration histories of this family of planets. MASCARA-1 b has a mean density of $1.5\pm0.9~\rm{g~cm^{-3}}$ and an equilibrium temperature of $2570^{+50}_{-30}~\rm{K}$, one of the highest temperatures known for a hot Jupiter to date. The system is reminiscent of WASP-33, but the host star lacks apparent delta-scuti variations, making the planet an ideal target for atmospheric characterization. We expect this to be the first of a series of hot Jupiters transiting bright early-type stars that will be discovered by MASCARA. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.04262v2-abstract-full').style.display = 'none'; document.getElementById('1707.04262v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 March, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 July, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 5 figures, Published in A&A. A typo in the value of the spectroscopic impact parameter was corrected</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 606, A73 (2017) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1707.01500">arXiv:1707.01500</a> <span> [<a href="https://arxiv.org/pdf/1707.01500">pdf</a>, <a href="https://arxiv.org/format/1707.01500">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201731512">10.1051/0004-6361/201731512 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MASCARA-2 b: A hot Jupiter transiting the $m_V=7.6$ A-star HD185603 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Talens%2C+G+J+J">G. J. J. Talens</a>, <a href="/search/astro-ph?searchtype=author&query=Justesen%2C+A+B">A. B. Justesen</a>, <a href="/search/astro-ph?searchtype=author&query=Albrecht%2C+S">S. Albrecht</a>, <a href="/search/astro-ph?searchtype=author&query=McCormac%2C+J">J. McCormac</a>, <a href="/search/astro-ph?searchtype=author&query=Van+Eylen%2C+V">V. Van Eylen</a>, <a href="/search/astro-ph?searchtype=author&query=Otten%2C+G+P+P+L">G. P. P. L. Otten</a>, <a href="/search/astro-ph?searchtype=author&query=Murgas%2C+F">F. Murgas</a>, <a href="/search/astro-ph?searchtype=author&query=Palle%2C+E">E. Palle</a>, <a href="/search/astro-ph?searchtype=author&query=Pollacco%2C+D">D. Pollacco</a>, <a href="/search/astro-ph?searchtype=author&query=Stuik%2C+R">R. Stuik</a>, <a href="/search/astro-ph?searchtype=author&query=Spronck%2C+J+F+P">J. F. P. Spronck</a>, <a href="/search/astro-ph?searchtype=author&query=Lesage%2C+A+-">A. -L. Lesage</a>, <a href="/search/astro-ph?searchtype=author&query=Grundahl%2C+F">F. Grundahl</a>, <a href="/search/astro-ph?searchtype=author&query=Andersen%2C+M+F">M. Fredslund Andersen</a>, <a href="/search/astro-ph?searchtype=author&query=Antoci%2C+V">V. Antoci</a>, <a href="/search/astro-ph?searchtype=author&query=Snellen%2C+I+A+G">I. A. G. Snellen</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1707.01500v2-abstract-short" style="display: inline;"> In this paper we present MASCARA-2 b, a hot Jupiter transiting the $m_V=7.6$ A2 star HD 185603. Since early 2015, MASCARA has taken more than 1.6 million flux measurements of the star, corresponding to a total of almost 3000 hours of observations, revealing a periodic dimming in the flux with a depth of $1.3\%$. Photometric follow-up observations were performed with the NITES and IAC80 telescopes… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.01500v2-abstract-full').style.display = 'inline'; document.getElementById('1707.01500v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1707.01500v2-abstract-full" style="display: none;"> In this paper we present MASCARA-2 b, a hot Jupiter transiting the $m_V=7.6$ A2 star HD 185603. Since early 2015, MASCARA has taken more than 1.6 million flux measurements of the star, corresponding to a total of almost 3000 hours of observations, revealing a periodic dimming in the flux with a depth of $1.3\%$. Photometric follow-up observations were performed with the NITES and IAC80 telescopes and spectroscopic measurements were obtained with the Hertzsprung SONG telescope. We find MASCARA-2 b orbits HD 185603 with a period of $3.474119^{+0.000005}_{-0.000006}~\rm{days}$ at a distance of $0.057 \pm 0.006~\rm{AU}$, has a radius of $1.83 \pm 0.07~\rm{R}_{\rm{J}}$ and place a $99\%$ upper limit on the mass of $< 17~\rm{M}_{\rm{J}}$. HD 185603 is a rapidly rotating early-type star with an effective temperature of $8980^{+90}_{-130}~\rm{K}$ and a mass and radius of $1.89^{+0.06}_{-0.05}~M_\odot$, $1.60 \pm 0.06~R_\odot$, respectively. Contrary to most other hot Jupiters transiting early-type stars, the projected planet orbital axis and stellar spin axis are found to be aligned with $位=0.6 \pm 4^\circ$. The brightness of the host star and the high equilibrium temperature, $2260 \pm 50~\rm{K}$, of MASCARA-2 b make it a suitable target for atmospheric studies from the ground and space. Of particular interest is the detection of TiO, which has recently been detected in the similarly hot planets WASP-33 b and WASP-19 b. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.01500v2-abstract-full').style.display = 'none'; document.getElementById('1707.01500v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 February, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 July, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 4 figures, Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 612, A57 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1702.04193">arXiv:1702.04193</a> <span> [<a href="https://arxiv.org/pdf/1702.04193">pdf</a>, <a href="https://arxiv.org/format/1702.04193">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/834/2/175">10.3847/1538-4357/834/2/175 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> On-sky performance analysis of the vector Apodizing Phase Plate coronagraph on MagAO/Clio2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Otten%2C+G+P+P+L">Gilles P. P. L. Otten</a>, <a href="/search/astro-ph?searchtype=author&query=Snik%2C+F">Frans Snik</a>, <a href="/search/astro-ph?searchtype=author&query=Kenworthy%2C+M+A">Matthew A. Kenworthy</a>, <a href="/search/astro-ph?searchtype=author&query=Keller%2C+C+U">Christoph U. Keller</a>, <a href="/search/astro-ph?searchtype=author&query=Males%2C+J+R">Jared R. Males</a>, <a href="/search/astro-ph?searchtype=author&query=Morzinski%2C+K+M">Katie M. Morzinski</a>, <a href="/search/astro-ph?searchtype=author&query=Close%2C+L+M">Laird M. Close</a>, <a href="/search/astro-ph?searchtype=author&query=Codona%2C+J+L">Johanan L. Codona</a>, <a href="/search/astro-ph?searchtype=author&query=Hinz%2C+P+M">Philip M. Hinz</a>, <a href="/search/astro-ph?searchtype=author&query=Hornburg%2C+K+J">Kathryn J. Hornburg</a>, <a href="/search/astro-ph?searchtype=author&query=Brickson%2C+L+L">Leandra L. Brickson</a>, <a href="/search/astro-ph?searchtype=author&query=Escuti%2C+M+J">Michael J. Escuti</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1702.04193v1-abstract-short" style="display: inline;"> We report on the performance of a vector apodizing phase plate coronagraph that operates over a wavelength range of $2-5 渭$m and is installed in MagAO/Clio2 at the 6.5 m Magellan Clay telescope at Las Campanas Observatory, Chile. The coronagraph manipulates the phase in the pupil to produce three beams yielding two coronagraphic point-spread functions (PSFs) and one faint leakage PSF. The phase pa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1702.04193v1-abstract-full').style.display = 'inline'; document.getElementById('1702.04193v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1702.04193v1-abstract-full" style="display: none;"> We report on the performance of a vector apodizing phase plate coronagraph that operates over a wavelength range of $2-5 渭$m and is installed in MagAO/Clio2 at the 6.5 m Magellan Clay telescope at Las Campanas Observatory, Chile. The coronagraph manipulates the phase in the pupil to produce three beams yielding two coronagraphic point-spread functions (PSFs) and one faint leakage PSF. The phase pattern is imposed through the inherently achromatic geometric phase, enabled by liquid crystal technology and polarization techniques. The coronagraphic optic is manufactured using a direct-write technique for precise control of the liquid crystal pattern, and multitwist retarders for achromatization. By integrating a linear phase ramp to the coronagraphic phase pattern, two separated coronagraphic PSFs are created with a single pupil-plane optic, which makes it robust and easy to install in existing telescopes. The two coronagraphic PSFs contain a 180$^\circ$ dark hole on each side of a star, and these complementary copies of the star are used to correct the seeing halo close to the star. To characterize the coronagraph, we collected a dataset of a bright ($m_L=0-1$) nearby star with $\sim$1.5 hr of observing time. By rotating and optimally scaling one PSF and subtracting it from the other PSF, we see a contrast improvement by 1.46 magnitudes at $3.5 位/D$. With regular angular differential imaging at 3.9 $渭$m, the MagAO vector apodizing phase plate coronagraph delivers a $5蟽螖$ mag contrast of 8.3 ($=10^{-3.3}$) at 2 $位/D$ and 12.2 ($=10^{-4.8}$) at $3.5 位/D$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1702.04193v1-abstract-full').style.display = 'none'; document.getElementById('1702.04193v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 February, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published in ApJ. 8 figures, 1 table. Received 2016 June 17; revised 2016 November 3; accepted 2016 November 28; published 2017 January 12</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal, Volume 834, Issue 2, article id. 175, 11 pp. (2017) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1702.03931">arXiv:1702.03931</a> <span> [<a href="https://arxiv.org/pdf/1702.03931">pdf</a>, <a href="https://arxiv.org/format/1702.03931">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201630319">10.1051/0004-6361/201630319 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Multi-site All-Sky CAmeRA: Finding transiting exoplanets around bright ($m_V < 8$) stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Talens%2C+G+J+J">G. J. J. Talens</a>, <a href="/search/astro-ph?searchtype=author&query=Spronck%2C+J+F+P">J. F. P. Spronck</a>, <a href="/search/astro-ph?searchtype=author&query=Lesage%2C+A+-">A. -L. Lesage</a>, <a href="/search/astro-ph?searchtype=author&query=Otten%2C+G+P+P+L">G. P. P. L. Otten</a>, <a href="/search/astro-ph?searchtype=author&query=Stuik%2C+R">R. Stuik</a>, <a href="/search/astro-ph?searchtype=author&query=Pollacco%2C+D">D. Pollacco</a>, <a href="/search/astro-ph?searchtype=author&query=Snellen%2C+I+A+G">I. A. G Snellen</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1702.03931v1-abstract-short" style="display: inline;"> This paper describes the design, operations, and performance of the Multi-site All-Sky CAmeRA (MASCARA). Its primary goal is to find new exoplanets transiting bright stars, $4 < m_V < 8$, by monitoring the full sky. MASCARA consists of one northern station on La Palma, Canary Islands (fully operational since February 2015), one southern station at La Silla Observatory, Chile (operational from earl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1702.03931v1-abstract-full').style.display = 'inline'; document.getElementById('1702.03931v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1702.03931v1-abstract-full" style="display: none;"> This paper describes the design, operations, and performance of the Multi-site All-Sky CAmeRA (MASCARA). Its primary goal is to find new exoplanets transiting bright stars, $4 < m_V < 8$, by monitoring the full sky. MASCARA consists of one northern station on La Palma, Canary Islands (fully operational since February 2015), one southern station at La Silla Observatory, Chile (operational from early 2017), and a data centre at Leiden Observatory in the Netherlands. Both MASCARA stations are equipped with five interline CCD cameras using wide field lenses (24 mm focal length) with fixed pointings, which together provide coverage down to airmass 3 of the local sky. The interline CCD cameras allow for back-to-back exposures, taken at fixed sidereal times with exposure times of 6.4 sidereal seconds. The exposures are short enough that the motion of stars across the CCD does not exceed one pixel during an integration. Astrometry and photometry are performed on-site, after which the resulting light curves are transferred to Leiden for further analysis. The final MASCARA archive will contain light curves for ${\sim}70,000$ stars down to $m_V=8.4$, with a precision of $1.5\%$ per 5 minutes at $m_V=8$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1702.03931v1-abstract-full').style.display = 'none'; document.getElementById('1702.03931v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 February, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 12 figures, Accepted for publication in A&A. See also http://mascara1.strw.leidenuniv.nl/</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 601, A11 (2017) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1412.0660">arXiv:1412.0660</a> <span> [<a href="https://arxiv.org/pdf/1412.0660">pdf</a>, <a href="https://arxiv.org/format/1412.0660">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1364/OE.22.030287">10.1364/OE.22.030287 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Performance characterization of a broadband vector Apodizing Phase Plate coronagraph </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Otten%2C+G+P+P+L">G. P. P. L. Otten</a>, <a href="/search/astro-ph?searchtype=author&query=Snik%2C+F">F. Snik</a>, <a href="/search/astro-ph?searchtype=author&query=Kenworthy%2C+M+A">M. A. Kenworthy</a>, <a href="/search/astro-ph?searchtype=author&query=Miskiewicz%2C+M+N">M. N. Miskiewicz</a>, <a href="/search/astro-ph?searchtype=author&query=Escuti%2C+M+J">M. J. Escuti</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1412.0660v1-abstract-short" style="display: inline;"> One of the main challenges for the direct imaging of planets around nearby stars is the suppression of the diffracted halo from the primary star. Coronagraphs are angular filters that suppress this diffracted halo. The Apodizing Phase Plate coronagraph modifies the pupil-plane phase with an anti-symmetric pattern to suppress diffraction over a 180 degree region from 2 to 7 位/D and achieves a mean… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.0660v1-abstract-full').style.display = 'inline'; document.getElementById('1412.0660v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1412.0660v1-abstract-full" style="display: none;"> One of the main challenges for the direct imaging of planets around nearby stars is the suppression of the diffracted halo from the primary star. Coronagraphs are angular filters that suppress this diffracted halo. The Apodizing Phase Plate coronagraph modifies the pupil-plane phase with an anti-symmetric pattern to suppress diffraction over a 180 degree region from 2 to 7 位/D and achieves a mean raw contrast of 10^-4 in this area, independent of the tip-tilt stability of the system. Current APP coronagraphs implemented using classical phase techniques are limited in bandwidth and suppression region geometry (i.e. only on 1 side of the star). In this paper, we show the vector-APP (vAPP) whose phase pattern is implemented by the orientation of patterned liquid crystals. Beam-splitting according to circular polarization states produces two, complementary PSFs with dark holes on either side. We have developed a prototype vAPP that consists of a stack of 3 twisting liquid crystal layers with a bandwidth of 500-900 nm. We characterize the properties of this device using reconstructions of the pupil-plane pattern, and of the ensuing PSF structures. By imaging the pupil between crossed and parallel polarizers we reconstruct the fast axis pattern, transmission, and retardance of the vAPP, and use this as input for a PSF model. This model includes aberrations of the laboratory set-up, and matches the measured PSF, which shows a raw contrast of 10^-3.8 between 2 and 7 位/D in a 135 degree wedge. The vAPP coronagraph is relatively easy to manufacture and can be implemented together with a broadband quarter-wave plate and Wollaston prism in a pupil wheel in high-contrast imaging instruments. The manufacturing techniques permit the application of phase patterns with deeper contrasts inside the dark holes and enables unprecedented spectral bandwidths for phase-manipulation coronagraphy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.0660v1-abstract-full').style.display = 'none'; document.getElementById('1412.0660v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 December, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 19 figures, 1 table</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Optics Express, Vol. 22, Issue 24, pp. 30287-30314 (2014) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1305.5544">arXiv:1305.5544</a> <span> [<a href="https://arxiv.org/pdf/1305.5544">pdf</a>, <a href="https://arxiv.org/ps/1305.5544">ps</a>, <a href="https://arxiv.org/format/1305.5544">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/771/2/109">10.1088/0004-637X/771/2/109 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Rayleigh scattering in the atmosphere of GJ1214b </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=de+Mooij%2C+E+J+W">Ernst J. W. de Mooij</a>, <a href="/search/astro-ph?searchtype=author&query=Brogi%2C+M">Matteo Brogi</a>, <a href="/search/astro-ph?searchtype=author&query=de+Kok%2C+R+J">Remco J. de Kok</a>, <a href="/search/astro-ph?searchtype=author&query=Snellen%2C+I+A+G">Ignas A. G Snellen</a>, <a href="/search/astro-ph?searchtype=author&query=Croll%2C+B">Bryce Croll</a>, <a href="/search/astro-ph?searchtype=author&query=Jayawardhana%2C+R">Ray Jayawardhana</a>, <a href="/search/astro-ph?searchtype=author&query=Hoekstra%2C+H">Henk Hoekstra</a>, <a href="/search/astro-ph?searchtype=author&query=Otten%2C+G+P+P+L">Gilles P. P. L. Otten</a>, <a href="/search/astro-ph?searchtype=author&query=Bekkers%2C+D+H">David H. Bekkers</a>, <a href="/search/astro-ph?searchtype=author&query=Haffert%2C+S+Y">Sebastiaan Y. Haffert</a>, <a href="/search/astro-ph?searchtype=author&query=van+Houdt%2C+J+J">Josha. J. van Houdt</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1305.5544v1-abstract-short" style="display: inline;"> We investigate the atmosphere of GJ1214b, a transiting super-Earth planet with a low mean density, by measuring its transit depth as a function of wavelength in the blue optical portion of the spectrum. It is thought that this planet is either a mini-Neptune, consisting of a rocky core with a thick, hydrogen-rich atmosphere, or a planet with a composition dominated by water. Most observations favo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1305.5544v1-abstract-full').style.display = 'inline'; document.getElementById('1305.5544v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1305.5544v1-abstract-full" style="display: none;"> We investigate the atmosphere of GJ1214b, a transiting super-Earth planet with a low mean density, by measuring its transit depth as a function of wavelength in the blue optical portion of the spectrum. It is thought that this planet is either a mini-Neptune, consisting of a rocky core with a thick, hydrogen-rich atmosphere, or a planet with a composition dominated by water. Most observations favor a water-dominated atmosphere with a small scale-height, however, some observations indicate that GJ1214b could have an extended atmosphere with a cloud layer muting the molecular features. In an atmosphere with a large scale-height, Rayleigh scattering at blue wavelengths is likely to cause a measurable increase in the apparent size of the planet towards the blue. We observed the transit of GJ1214b in the B-band with the FOcal Reducing Spectrograph (FORS) at the Very Large Telescope (VLT) and in the g-band with both ACAM on the William Hershel Telescope (WHT) and the Wide Field Camera (WFC) at the Isaac Newton Telescope (INT). We find a planet-to-star radius ratio in the B-band of 0.1162+/-0.0017, and in the g-band 0.1180+/-0.0009 and 0.1174+/-0.0017 for the WHT & INT observations respectively. These optical data do not show significant deviations from previous measurements at longer wavelengths. In fact, a flat transmission spectrum across all wavelengths best describes the combined observations. When atmospheric models are considered a small scale-height water-dominated model fits the data best. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1305.5544v1-abstract-full').style.display = 'none'; document.getElementById('1305.5544v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 May, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ</span> </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns 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