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1. Using AI for Wave-front Estimation with the Rubin Observatory Active Optics System

Author

John Franklin Crenshaw, Andrew J. Connolly, Joshua E. Meyers, J. Bryce Kalmbach, Guillem Megias Homar, Tiago Ribeiro, Krzysztof Suberlak, Sandrine Thomas, and Te-Wei Tsai

Subjects
Neural networks, Multiple mirror telescopes, Optical telescopes, Astronomical optics, Astronomical instrumentation, Astronomy, QB1-991
Abstract

The Vera C. Rubin Observatory will, over a period of 10 yr, repeatedly survey the southern sky. To ensure that images generated by Rubin meet the quality requirements for precision science, the observatory will use an active-optics system (AOS) to correct for alignment and mirror surface perturbations introduced by gravity and temperature gradients in the optical system. To accomplish this, Rubin will use out-of-focus images from sensors located at the edge of the focal plane to learn and correct for perturbations to the wave front. We have designed and integrated a deep-learning (DL) model for wave-front estimation into the AOS pipeline. In this paper, we compare the performance of this DL approach to Rubin’s baseline algorithm when applied to images from two different simulations of the Rubin optical system. We show the DL approach is faster and more accurate, achieving the atmospheric error floor both for high-quality images and low-quality images with heavy blending and vignetting. Compared to the baseline algorithm, the DL model is 40× faster, the median error 2× better under ideal conditions, 5× better in the presence of vignetting by the Rubin camera, and 14× better in the presence of blending in crowded fields. In addition, the DL model surpasses the required optical quality in simulations of the AOS closed loop. This system promises to increase the survey area useful for precision science by up to 8%. We discuss how this system might be deployed when commissioning and operating Rubin.

Published
2024
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2. Testing the Interaction between a Substellar Companion and a Debris Disk in the HR 2562 System

Author

Stella Yimiao Zhang, Gaspard Duchêne, Robert J. De Rosa, Megan Ansdell, Quinn Konopacky, Thomas Esposito, Eugene Chiang, Malena Rice, Brenda Matthews, Paul Kalas, Bruce Macintosh, Franck Marchis, Stan Metchev, Jenny Patience, Julien Rameau, Kimberly Ward-Duong, Schuyler Wolff, Michael P. Fitzgerald, Vanessa P. Bailey, Travis S. Barman, Joanna Bulger, Christine H. Chen, Jeffrey K. Chilcotte, Tara Cotten, René Doyon, Katherine B. Follette, Benjamin L. Gerard, Stephen Goodsell, James R. Graham, Alexandra Z. Greenbaum, Pascale Hibon, Li-Wei Hung, Patrick Ingraham, Jérôme Maire, Mark S. Marley, Christian Marois, Maxwell A. Millar-Blanchaer, Eric L. Nielsen, Rebecca Oppenheimer, David W. Palmer, Marshall D. Perrin, Lisa A. Poyneer, Laurent Pueyo, Abhijith Rajan, Fredrik T. Rantakyrö, Jean-Baptiste Ruffio, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Inseok Song, Remi Soummer, Sandrine Thomas, Jason J. Wang, and Sloane J. Wiktorowicz

Subjects
Debris disks, Substellar companion stars, Brown dwarfs, Orbit determination, Gravitational interaction, Astronomy, QB1-991
Abstract

The HR 2562 system is a rare case where a brown dwarf companion resides in a cleared inner hole of a debris disk, offering invaluable opportunities to study the dynamical interaction between a substellar companion and a dusty disk. We present the first ALMA observation of the system as well as the continued Gemini Planet Imager monitoring of the companion’s orbit with six new epochs from 2016 to 2018. We update the orbital fit, and in combination with absolute astrometry from GAIA, place a 3 σ upper limit of 18.5 M _J on the companion’s mass. To interpret the ALMA observations, we used radiative transfer modeling to determine the disk properties. We find that the disk is well resolved and nearly edge-on. While the misalignment angle between the disk and the orbit is weakly constrained, due to the short orbital arc available, the data strongly support a (near) coplanar geometry for the system. Furthermore, we find that the models that describe the ALMA data best have inner radii that are close to the companion’s semimajor axis. Including a posteriori knowledge of the system’s SED further narrows the constraints on the disk’s inner radius and places it at a location that is in reasonable agreement with (possibly interior to) predictions from existing dynamical models of disk truncation by an interior substellar companion. HR 2562 has the potential over the next few years to become a new test bed for dynamical interaction between a debris disk and a substellar companion.

Published
2023
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3. Rubin Observatory Commissioning Camera: summit integration

Author

Brian Stalder, Kevin Reil, Christian Aguilar, Claudio Araya, Anthony Borstad, Boyd Bowdish, Myung Cho, Stephen Cisneros, Chuck Claver, Julio Constanzo, Giovanni Corvetto, Holger Drass, Frossie Economou, Erik Dennihy, Alan Eisner, Juan Fabrega, Angelo Fausti Neto, Merlin Fisher-Levine, Ivan Gonzalez, Ronald Harris, Diane Hascall, Justine Haupt, Josh Hoblitt, James Howard, Mike Huffer, Tim Jenness, David Jiménez Mejías, Brian Johnson, Tony Johnson, K. Simon Krughoff, Craig Lage, Travis Lange, Ming Liang, Juan Lopez, Margaux Lopez, Robert Lupton, Guido Maulen, Felipe Menanteau, Neill Mills, Glenn Morris, Freddy Munoz, Homer Neal, Douglas R. Neill, Scott Newbry, Andrei Nomerotski, Dmitry Onoprienko, Ian Ordenes, Juan Orellana, Shawn Osier, HyeYun Park, Stephen Pietrowicz, Andrés Alejandro Plazas Malagón, Gary Poczulp, Brian Qiu, Bruno Quint, Heinrich Reinking, Michael Reuter, Tiago Ribeiro, Rodrigo Rojas, Sandra Romero, Rafe Schindler, Bill Schoening, Jacques Sebag, Alysha Shugart, Cristian Silva, Ioana Sotuela, Anthony Tache, Diego Tapia, John G. Thayer, Sandrine Thomas, Roberto Tighe, Tei-Wei Tsai, Max Turri, Anthony Tyson, Luis Vergara, Christopher Walter, Oliver Wiecha, and Van Xiong

Published
2022

4. Multiband Polarimetric Imaging of HR 4796A with the Gemini Planet Imager

Author

Pauline Arriaga, Michael P. Fitzgerald, Gaspard Duchêne, Paul Kalas, Maxwell A. Millar-Blanchaer, Marshall D. Perrin, Christine H. Chen, Johan Mazoyer, Mark Ammons, Vanessa P. Bailey, Trafis S. Barman, Joanna Bulger, Jeffrey K. Chilcote, Tara Cotten, Robert J. De Rosa, Rene Doyon, Thomas M. Esposito, Katherine B. Follette, Benjamin L. Gerard, Stephen Goodsell, James R. Graham, Alexandra Z. Greenbaum, Pascale Hibon, Justin Hom, Li-Wei Hung, Patrick Ingraham, Quinn M. Konopacky, Bruce A. Macintosh, Jérôme Maire, Franck Marchis, Mark S. Marley, Christian Marois, Stanimir Metchev, Eric L. Nielsen, Rebecca Oppenheimer, David W. Palmer, Jenny Patience, Lisa A. Poyneer, Laurent Pueyo, Abhijith Rajan, Julien Rameau, Fredrik T. Rantakyrö, Jean-Baptiste Ruffio, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Inseok Song, Remi Soummer, Sandrine Thomas, Jason J. Wang, Kimberly Ward-Duong, and Schuyler G. Wolff

Published
2020
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5. The Gemini Planet Imager View of the HD 32297 Debris Disk

Author

Gaspard Duchêne, Malena Rice, Justin Hom, Joseph Zalesky, Thomas M. Esposito, Maxwell A. Millar-Blanchaer, Bin Ren, Paul Kalas, Michael P. Fitzgerald, Pauline Arriaga, Sebastian Bruzzone, Joanna Bulger, Christine H. Chen, Eugene Chiang, Tara Cotten, Ian Czekala, Robert J. De Rosa, Ruobing Dong, Zachary H. Draper, Katherine B. Follette, James R. Graham, Li-Wei Hung, Ronald Lopez, Bruce Macintosh, Brenda C. Matthews, Johan Mazoyer, Stan Metchev, Jennifer Patience, Marshall D. Perrin, Julien Rameau, Inseok Song, Kevin Stahl, Jason Wang, Schuyler Wolff, Ben Zuckerman, S. Mark Ammons, Vanessa P. Bailey, Travis Barman, Jeffrey Chilcote, Rene Doyon, Benjamin L. Gerard, Stephen J. Goodsell, Alexandra Z. Greenbaum, Pascale Hibon, Patrick Ingraham, Quinn Konopacky, Jérôme Maire, Franck Marchis, Mark S. Marley, Christian Marois, Eric L. Nielsen, Rebecca Oppenheimer, David Palmer, Lisa Poyneer, Laurent Pueyo, Abhijith Rajan, Fredrik T. Rantakyrö, Jean-Baptiste Ruffio, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Rémi Soummer, Sandrine Thomas, and Kimberley Ward-Duong

Published
2020
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6. The Gemini Planet Imager Exoplanet Survey: Dynamical Mass of the Exoplanet β Pictoris b from Combined Direct Imaging and Astrometry

Author

Eric L. Nielsen, Robert J. De Rosa, Jason J. Wang, Johannes Sahlmann, Paul Kalas, Gaspard Duchêne, Julien Rameau, Mark S. Marley, Didier Saumon, Bruce Macintosh, Maxwell A. Millar-Blanchaer, Meiji M. Nguyen, S. Mark Ammons, Vanessa P. Bailey, Travis Barman, Joanna Bulger, Jeffrey Chilcote, Tara Cotten, Rene Doyon, Thomas M. Esposito, Michael P. Fitzgerald, Katherine B. Follette, Benjamin L. Gerard, Stephen J. Goodsell, James R. Graham, Alexandra Z. Greenbaum, Pascale Hibon, Li-Wei Hung, Patrick Ingraham, Quinn Konopacky, James E. Larkin, Jérôme Maire, Franck Marchis, Christian Marois, Stanimir Metchev, Rebecca Oppenheimer, David Palmer, Jennifer Patience, Marshall Perrin, Lisa Poyneer, Laurent Pueyo, Abhijith Rajan, Fredrik T. Rantakyrö, Jean-Baptiste Ruffio, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Inseok Song, Remi Soummer, Sandrine Thomas, J. Kent Wallace, Kimberly Ward-Duong, Sloane Wiktorowicz, and Schuyler Wolff

Published
2020
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7. An Updated Visual Orbit of the Directly Imaged Exoplanet 51 Eridani b and Prospects for a Dynamical Mass Measurement with Gaia

Author

Robert J. De Rosa, Eric L. Nielsen, Jason J. Wang, S. Mark Ammons, Gaspard Duchêne, Bruce Macintosh, Julien Rameau, Vanessa P. Bailey, Travis Barman, Joanna Bulger, Jeffrey Chilcote, Tara Cotten, Rene Doyon, Thomas M. Esposito, Michael P. Fitzgerald, Katherine B. Follette, Benjamin L. Gerard, Stephen J. Goodsell, James R. Graham, Alexandra Z. Greenbaum, Pascale Hibon, Justin Hom, Li-Wei Hung, Patrick Ingraham, Paul Kalas, Quinn Konopacky, James E. Larkin, Jérôme Maire, Franck Marchis, Mark S. Marley, Christian Marois, Stanimir Metchev, Maxwell A. Millar-Blanchaer, Rebecca Oppenheimer, David Palmer, Jennifer Patience, Marshall Perrin, Lisa Poyneer, Laurent Pueyo, Abhijith Rajan, Fredrik T. Rantakyrö, Bin Ren, Jean-Baptiste Ruffio, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Inseok Song, Remi Soummer, Melisa Tallis, Sandrine Thomas, J. Kent Wallace, Kimberly Ward-Duong, Sloane Wiktorowicz, and Schuyler Wolff

Published
2019
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8. Detection of a Low-mass Stellar Companion to the Accelerating A2IV Star HR 1645

Author

Robert J. De Rosa, Eric L. Nielsen, Julien Rameau, Gaspard Duchêne, Alexandra Z. Greenbaum, Jason J. Wang, S. Mark Ammons, Vanessa P. Bailey, Travis Barman, Joanna Bulger, Jeffrey Chilcote, Tara Cotten, Rene Doyon, Thomas M. Esposito, Michael P. Fitzgerald, Katherine B. Follette, Benjamin L. Gerard, Stephen J. Goodsell, James R. Graham, Pascale Hibon, Justin Hom, Li-Wei Hung, Patrick Ingraham, Paul Kalas, Quinn Konopacky, James E. Larkin, Bruce Macintosh, Jérôme Maire, Franck Marchis, Mark S. Marley, Christian Marois, Stanimir Metchev, Maxwell A. Millar-Blanchaer, Rebecca Oppenheimer, David Palmer, Jennifer Patience, Marshall Perrin, Lisa Poyneer, Laurent Pueyo, Abhijith Rajan, Fredrik T. Rantakyrö, Bin Ren, Jean-Baptiste Ruffio, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Inseok Song, Remi Soummer, Melisa Tallis, Sandrine Thomas, J. Kent Wallace, Kimberly Ward-Duong, Sloane Wiktorowicz, and Schuyler Wolff

Published
2019
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9. Special Section Guest Editorial: Extremely Large Telescopes

Author

Sandrine Thomas, Gelys Trancho, Elise Vernet, and Tony Travouillon

Subjects
Space and Planetary Science, Control and Systems Engineering, Mechanical Engineering, Astronomy and Astrophysics, Instrumentation, Electronic, Optical and Magnetic Materials
Published
2022

10. A low-mass companion desert among intermediate-mass visual binaries: The scaled-up counterpart to the brown dwarf desert

Author

Gaspard Duchêne, Jner Tzern Oon, Robert J De Rosa, Patrick Kantorski, Brandon Coy, Jason J Wang, Sandrine Thomas, Jenny Patience, Laurent Pueyo, Eric L Nielsen, and Quinn Konopacky

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract

We present a high-contrast imaging survey of intermediate-mass (1.75--4.5 $M_\odot$) stars to search for the most extreme stellar binaries, i.e., for the lowest mass stellar companions. Using adaptive optics at the Lick and Gemini observatories, we observed 169 stars and detected 24 candidates companions, 16 of which are newly discovered and all but three are likely or confirmed physical companions. Despite obtaining sensitivity down to the substellar limit for 75\% of our sample, we do not detect any companion below 0.3 $M_\odot$, strongly suggesting that the distribution of stellar companions is truncated at a mass ratio of $q_\mathrm{min} \gtrsim0.075$. Combining our results with known brown dwarf companions, we identify a low-mass companion desert to intermediate mass stars in the range $0.02\lesssim q \lesssim0.05$, which quantitatively matches the known brown dwarf desert among solar-type stars. We conclude that the formation mechanism for multiple systems operates in a largely scale-invariant manner and precludes the formation of extremely uneven systems, likely because the components of a proto-binary accrete most of their mass after the initial cloud fragmentation. Similarly, the mechanism to form "planetary" ($q \lesssim 0.02$) companions likely scales linearly with stellar mass, probably as a result of the correlation between the masses of stars and their protoplanetary disks. Finally, we predict the existence of a sizable population of brown dwarf companions to low-mass stars and of a rising population of planetary-mass objects towards $\approx 1\,M_\mathrm{Jup}$ around solar-type stars. Improvements on current instrumentation will test these predictions., Comment: Accepted for publication in MNRAS; 23 pages, 17 figures

Published
2022
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11. The Gemini Planet Imager Exoplanet Survey: Giant Planet and Brown Dwarf Demographics from 10 to 100 au

Author

Eric L. Nielsen, Robert J. De Rosa, Bruce Macintosh, Jason J. Wang, Jean-Baptiste Ruffio, Eugene Chiang, Mark S. Marley, Didier Saumon, Dmitry Savransky, S. Mark Ammons, Vanessa P. Bailey, Travis Barman, Célia Blain, Joanna Bulger, Adam Burrows, Jeffrey Chilcote, Tara Cotten, Ian Czekala, Rene Doyon, Gaspard Duchêne, Thomas M. Esposito, Daniel Fabrycky, Michael P. Fitzgerald, Katherine B. Follette, Jonathan J. Fortney, Benjamin L. Gerard, Stephen J. Goodsell, James R. Graham, Alexandra Z. Greenbaum, Pascale Hibon, Sasha Hinkley, Lea A. Hirsch, Justin Hom, Li-Wei Hung, Rebekah Ilene Dawson, Patrick Ingraham, Paul Kalas, Quinn Konopacky, James E. Larkin, Eve J. Lee, Jonathan W. Lin, Jérôme Maire, Franck Marchis, Christian Marois, Stanimir Metchev, Maxwell A. Millar-Blanchaer, Katie M. Morzinski, Rebecca Oppenheimer, David Palmer, Jennifer Patience, Marshall Perrin, Lisa Poyneer, Laurent Pueyo, Roman R. Rafikov, Abhijith Rajan, Julien Rameau, Fredrik T. Rantakyrö, Bin Ren, Adam C. Schneider, Anand Sivaramakrishnan, Inseok Song, Remi Soummer, Melisa Tallis, Sandrine Thomas, Kimberly Ward-Duong, and Schuyler Wolff

Published
2019
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12. Performance of the Gemini Planet Imager Non-redundant Mask and Spectroscopy of Two Close-separation Binaries: HR 2690 and HD 142527

Author

Alexandra Z. Greenbaum, Anthony Cheetham, Anand Sivaramakrishnan, Fredrik T. Rantakyrö, Gaspard Duchêne, Peter Tuthill, Robert J. De Rosa, Rebecca Oppenheimer, Bruce Macintosh, S. Mark Ammons, Vanessa P. Bailey, Travis Barman, Joanna Bulger, Andrew Cardwell, Jeffrey Chilcote, Tara Cotten, Rene Doyon, Michael P. Fitzgerald, Katherine B. Follette, Benjamin L. Gerard, Stephen J. Goodsell, James R. Graham, Pascale Hibon, Li-Wei Hung, Patrick Ingraham, Paul Kalas, Quinn Konopacky, James E. Larkin, Jérôme Maire, Franck Marchis, Mark S. Marley, Christian Marois, Stanimir Metchev, Maxwell A. Millar-Blanchaer, Katie M. Morzinski, Eric L. Nielsen, David Palmer, Jennifer Patience, Marshall Perrin, Lisa Poyneer, Laurent Pueyo, Abhijith Rajan, Julien Rameau, Naru Sadakuni, Dmitry Savransky, Adam C. Schneider, Inseok Song, Remi Soummer, Sandrine Thomas, J. Kent Wallace, Jason J. Wang, Kimberly Ward-Duong, Sloane Wiktorowicz, and Schuyler Wolff

Published
2019
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13. Rubin Observatory primary tertiary mirror cell assembly: Optical testing of the fully assembled mirror support

Author

Christopher Contaxis, Hubert M. Martin, Adrian R. Loeff, Steven C. West, Stephanie Meyen, Chuck Claver, Douglas R. Neill, M. T. Tuell, K. Kenagy, Bo Xin, William W. Hubler, Sandrine Thomas, and Edward Hileman

Subjects
Surface (mathematics), Materials science, Observatory, Optical testing, Primary (astronomy), Mechanical engineering, Bending, Actuator, Cell assembly, Finite element method
Abstract

The Vera C. Rubin Observatory Primary Tertiary Mirror (M1M3), together with the fully-assembled mirror support system, underwent two optical testing campaigns at the University of Arizona Richard F. Caris Mirror Lab. The objectives of the testing campaigns were: (1) optimizing the M1M3 surfaces with support forces, and (2) characterizing how the surfaces respond to actuator forces, including measuring the bending modes and single actuator influence functions. Both objectives were successfully achieved. The differences between the measured bending modes and the Finite Element Analysis (FEA) predicted modes were shown to be less than a few percent. The surface optimizations routinely resulted in Root-Mean-Square (RMS) surface errors below 30 nm for M1 and M3, simultaneously. The entire system was shown to be robust and repeatable. In this paper, we present the results of the optical testing and the analyses performed using the data acquired.

Published
2020

14. Vera C. Rubin Observatory: Telescope and site status

Author

Patrick Ingraham, Shawn P. Callahan, Bo Xin, Tomislav Vucina, Freddy Muñoz, Tiago Ribeiro, Jeffrey D. Barr, Roberto Tighe, B. Stalder, Juan Fabrega, Douglas R. Neill, Sandrine Thomas, Jacques Sebag, Andy W. Clements, Felipe Daruich, Eduardo P. Serrano, and William J. Gressler

Subjects
Engineering, business.industry, Integration testing, Large Synoptic Survey Telescope, DIMM, law.invention, Telescope, law, Observatory, Astronomical interferometer, Telescope mount, business, Spectrograph, Remote sensing
Abstract

The Vera C. Rubin Observatory (Rubin Obs) (formerly Large Synoptic Survey Telescope - LSST) is an 8.4-m telescope, now under construction in Chile. In the last couple of years, the telescope has achieved tremendous progress, though like many other projects, progress has been curtailed for over six months due to the worldwide pandemic. This paper provides the high-level status of each of the telescope's subsystem. The summit facility (Cerro Pachon) and base facility (La Serena) have been substantially completed. The dome is expected to be finished by October of 2021, which will also allow the completion of integration and testing of the Telescope Mount Assembly (TMA). The integration and verification of the TMA is planned to be completed by the end of 2021. The two mirror systems, M1M3 and M2, have been fully tested under interferometers, showing they both satisfy their performance requirement, and both have been received at the summit facility. The M2 mirror has been successfully coated with protected aluminum, which is the first scientific coating produced by the new Rubin coating plant. The M1M3 mirror is planned to be coated with the same plant at the beginning of 2022. The auxiliary telescope and its principal spectrograph instrument, which will allow for real-time atmospheric characterization, has been commissioned. The Rubin environment awareness system (EAS), which includes the DIMM, weather station, all-sky camera, and facility environmental control, is operational. Significant progress has been made on the software for all of the above-mentioned subsystems, as well as the comprehensive telescope control system and the telescope operator interfaces.

Published
2020

15. Vera C. Rubin Observatory auxiliary telescope commissioning as a control system pathfinder

Author

Patrick J. Ingraham, Andy W. Clements, Tiago Ribeiro, Michael A. Reuter, Merlin Fisher-Levine, Joshua Hoblitt, Robert H. Lupton, Sandrine Thomas, Christopher W. Stubbs, Kirk Arndt, Nick Callahan, CHarles F. Claver, Franco Colleoni, Luis Corral, Peter Doherty, Frossie Economou, Angel Fausti, Tim Jeness, Htut Khine, Simon Krughoff, Nicholas Mondrik, Felipe Menanteau, David J. Mills, William O'Mullane, Kevin A. Reil, Mario Rivera, Brian Stalder, Jacques Sebag, Ian Shipsey, Roberto Tighe, Adam J. Thornton, Andres Villalobos, and Oliver Wiecha

Published
2020

16. LSST primary tertiary mirror cell assembly: Integration and functional testing

Author

Tomislav Vucina, Edward Stover, Dave Mills, Christian Aguilar, Bo Xin, Freddy Muñoz, Brian Johnson, Oli Wiecha, Edward Hileman, Juan Lopez, Christopher Contaxis, Claudio Araya, Ron Harris, Douglas R. Neill, Gary Muller, Michael Booth, Franco Colleoni, Felipe Daruich, Ian Ordenes, Jacques Sebag, Jeff Urban, Eric Coughlin, Sandrine Thomas, Constanza Araujo, Neill Mills, Andy W. Clements, and Garry Knight

Subjects
Interferometry, Optics, Observatory, Primary (astronomy), business.industry, Optical surface, Active optics, Support system, Telescope mount, business, Cell assembly, Geology
Abstract

The Vera C. Rubin Observatory is currently under construction on Cerro Pachon, in Chile. It was designed to conduct a 10-year multi-band survey of the southern sky with frequent re-visits (with both an intra- and extra-night cadence) to identify transient and moving objects. The mirror cell assembly was designed in Tucson, Arizona by the Rubin Observatory engineering department, and was tested twice in Tucson. The first testing campaign was performed at CAID industries, where the mirror cell was fabricated, using a steel mirror surrogate that has the same geometry and mass of the glass mirror2,4. The glass mirror is a single monolith that contains both the primary and tertiary mirrors on a single substrate. The testing results confirmed that the mirror support system was performing within the design specifications, and that it was safe to install the glass mirror on the cell. The second test campaign was performed at the Richard F. Caris Mirror Lab of the University of Arizona using the actual glass mirror16. This test campaign was performed under the test tower, which contains a vibration insensitive interferometer to measure mirror figure. This confirmed the mirror support system could achieve proper optical surface figure control for both primary and tertiary mirrors. After successful test campaigns at CAID, and the mirror Lab, the mirror cell assembly was disassembled, packed and shipped to the Rubin Observatory site at the Cerro Pachon summit in Chile. Upon arrival, the mirror cell has been integrated with the mirror surrogate once again to perform the third test campaign that confirmed the system has arrived safe and operational to the summit. This integrated system will be tested on the telescope mount assembly to verify that it still meets it requirements under the effects of variations in gravitational orientation, and dynamic (slewing) loads.

Published
2020

17. The Shack-Hartmann wavefront sensor for the Rubin Observatory

Author

Sandrine Thomas, Jerome Ballesta, Rafael Meyer, Guillaume Tison, and Jacques Sebag

Subjects
Aperture, business.industry, Computer science, Linearity, Wavefront sensor, law.invention, Telescope, Optics, Observatory, law, Calibration, Sensitivity (control systems), business, Shack–Hartmann wavefront sensor
Abstract

A measurement platform including a Shack-Hartmann Wavefront Sensor (SHWFS) has been designed, integrated and tested at Imagine Optic, Orsay France and delivered to the Rubin Observatory (previously known as the LSST). This instrument will be used for the initial on-axis optical alignment and testing of the LSST telescope. The optical configuration of the Rubin Telescope without the presence of the main LSST camera requires advanced capabilities in term of quantities of aberrations to measure, linearity, accuracy and sensitivity for usage on a natural star. The HASO 128 GE 2, available from Imagine Optic, was identified as the most relevant WFS to meet all those requirements. In that paper, we provide details about the simulations that led to the choice of the HASO 128 GE 2. We also provide the specifics regarding the opto-mechanical design allowing the relay imaging of the pupil compatible with the fast aperture of the telescope, a reference source for the on-site calibration of the system and the optical output made available for a viewer camera.

Published
2020

18. Rubin Observatory active optics system status

Author

Andrew J. Connolly, Douglas R. Neill, Charles F. Claver, Tiago Ribeiro, Chris Suberlak, Bo Xin, Sandrine Thomas, J. Bryce Kalmbach, and Tei-Wei Tsai

Subjects
Wavefront, Computer science, business.industry, Field of view, Active optics, Wavefront sensor, law.invention, Telescope, Interferometry, Cardinal point, Optics, Observatory, law, business
Abstract

The Vera C. Rubin Observatory is now under construction on Cerro Pachon in Chile. This ground-based facility is designed to conduct the Legacy Survey of Space and Time (LSST), which is a decade-long time-domain optical survey of the night sky. The system aberrations introduced by temperature gradients, hysteresis and other non-predictable errors can prevent the telescope from delivering a consistently high-quality image over its 3.5 degrees field of view, necessary to the LSST scientific goals. Therefore, the active optics system (AOS) uses a combination of an open-loop and a closed-loop correction. The AOS open-loop is planned to correct for typical gravity variations while the AOS closed-loop will correct the real-time (within 30s) system aberrations. The components used for this task consist mainly of: two mirrors with active support systems (M1M3 and M2), two hexapods and curvature wavefront sensors integrated to the focal plane of the science detector. By the beginning of 2019, both M1 and M3 mirrors had been extensively tested using interferometry techniques, providing necessary measurements to refine our Finite Element models. This will help to achieve higher image quality when integrating all mirrors on the telescope. Progress has also been made on the active optics pipeline, which allows for conversion of the wavefront sensor images into corrective data for the mirrors and hexapods. In this paper, we will present the main results from the mirror testing as well as predicted performance of the AOS using these results. Finally, we will discuss the test plan for commissioning the AOS on the telescope.

Published
2020

19. Multiband Polarimetric Imaging of HR 4796A with the Gemini Planet Imager

Author

Katherine B. Follette, Sandrine Thomas, Adam C. Schneider, Inseok Song, Trafis S. Barman, Michael P. Fitzgerald, Benjamin L. Gerard, Robert J. De Rosa, Justin Hom, Pauline Arriaga, Eric L. Nielsen, Jérôme Maire, K. Ward-Duong, Thomas M. Esposito, Anand Sivaramakrishnan, Vanessa P. Bailey, Bruce Macintosh, Tara Cotten, Rémi Soummer, Rebecca Oppenheimer, Stephen J. Goodsell, Schuyler Wolff, Paul Kalas, Gaspard Duchêne, Pascale Hibon, Quinn Konopacky, Laurent Pueyo, Dmitry Savransky, Abhijith Rajan, Christian Marois, Jeffrey Chilcote, J. Patience, Maxwell A. Millar-Blanchaer, Christine Chen, Stanimir Metchev, Fredrik T. Rantakyrö, Johan Mazoyer, Alexandra Z. Greenbaum, Joanna Bulger, René Doyon, Franck Marchis, Julien Rameau, Jason J. Wang, James R. Graham, David Palmer, Patrick Ingraham, Jean-Baptiste Ruffio, Marshall D. Perrin, Lisa Poyneer, Mark Ammons, Li Wei Hung, Mark S. Marley, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)

Subjects
Brightness, 010504 meteorology & atmospheric sciences, Population, Phase (waves), Near infrared astronomy, FOS: Physical sciences, Astrophysics, 01 natural sciences, Luminosity, polarimetry (1278), Debris disks, 0103 physical sciences, Polarimetry, Gemini Planet Imager, circumstellar dust (236), education, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), [PHYS]Physics [physics], education.field_of_study, Debris disk, Scattering, near infrared astronomy (1093), Astronomy and Astrophysics, debris disks (363), coronagraphic imaging (313), Wavelength, Circumstellar dust, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Circumstellar disks, Astrophysics::Earth and Planetary Astrophysics, Coronagraphic imaging, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], circumstellar disks (235), Astrophysics - Earth and Planetary Astrophysics
Abstract

HR4796A hosts a well-studied debris disk with a long history due to its high fractional luminosity and favorable inclination lending itself well to both unresolved and resolved observations. We present new J- and K1-band images of the resolved debris disk HR4796A taken in the polarimetric mode of the Gemini Planet Imager (GPI). The polarized intensity features a strongly forward scattered brightness distribution and is undetected at the far side of the disk. The total intensity is detected at all scattering angles and also exhibits a strong forward scattering peak. We use a forward modelled geometric disk in order to extract geometric parameters, polarized fraction and total intensity scattering phase functions for these data as well as H-band data previously taken by GPI. We find the polarized phase function becomes increasingly more forward scattering as wavelength increases. We fit Mie and distribution of hollow spheres grain (DHS) models to the extracted functions. We find that while it is possible to describe generate a satisfactory model for the total intensity using a DHS model, but not with a Mie model. We find that no single grain population of DHS or Mie grains of arbitrary composition can simultaneously reproduce the polarized fraction and total intensity scattering phase functions, indicating the need for more sophisticated grain models., Comment: Accepted for publication in AJ. 3 tables, 11 figures

Published
2020

20. The Gemini Planet Imager view of the HD 32297 debris disk

Author

Bruce Macintosh, Joseph Zalesky, Julien Rameau, Kevin Stahl, Malena Rice, Franck Marchis, Quinn Konopacky, Ronald Lopez, Benjamin L. Gerard, James R. Graham, Stephen J. Goodsell, Schuyler Wolff, Inseok Song, Patrick Ingraham, Eugene Chiang, K. Ward-Duong, Abhijith Rajan, Jennifer Patience, Li-Wei Hung, S. Metchev, Pauline Arriaga, Bin Ren, Justin Hom, Zachary H. Draper, Jean-Baptiste Ruffio, Rémi Soummer, Marshall D. Perrin, Thomas M. Esposito, Jérôme Maire, Fredrik T. Rantakyrö, Christian Marois, Dmitry Savransky, Barry Zuckerman, Vanessa P. Bailey, Katherine B. Follette, Gaspard Duchêne, Anand Sivaramakrishnan, Jeffrey Chilcote, Sandrine Thomas, Lisa Poyneer, J. Bulger, Adam C. Schneider, Mark S. Marley, Johan Mazoyer, Laurent Pueyo, Ruobing Dong, Brenda C. Matthews, Tara Cotten, Pascale Hibon, Jason J. Wang, Rebecca Oppenheimer, Travis Barman, Eric L. Nielsen, Michael P. Fitzgerald, Alexandra Z. Greenbaum, S. Mark Ammons, René Doyon, Paul Kalas, Maxwell A. Millar-Blanchaer, Christine Chen, Robert J. De Rosa, Ian Czekala, David Palmer, Sebastian Bruzzone, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)

Subjects
010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Debris disks, 0103 physical sciences, Gemini Planet Imager, Surface brightness, circumstellar dust (236), 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), [PHYS]Physics [physics], Physics, Debris disk, Scattering, Astronomy and Astrophysics, Polarization (waves), Starlight, debris disks (363), Circumstellar dust, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Halo, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract

We present new $H$-band scattered light images of the HD 32297 edge-on debris disk obtained with the Gemini Planet Imager (GPI). The disk is detected in total and polarized intensity down to a projected angular separation of 0.15", or 20au. On the other hand, the large scale swept-back halo remains undetected, likely a consequence of its markedly blue color relative to the parent body belt. We analyze the curvature of the disk spine and estimate a radius of $\approx$100au for the parent body belt, smaller than past scattered light studies but consistent with thermal emission maps of the system. We employ three different flux-preserving post-processing methods to suppress the residual starlight and evaluate the surface brightness and polarization profile along the disk spine. Unlike past studies of the system, our high fidelity images reveal the disk to be highly symmetric and devoid of morphological and surface brightness perturbations. We find the dust scattering properties of the system to be consistent with those observed in other debris disks, with the exception of HR 4796. Finally, we find no direct evidence for the presence of a planetary-mass object in the system., Comment: Accepted for publication in the Astronomical Journal

Published
2020

21. Debris Disk Results from the Gemini Planet Imager Exoplanet Survey's Polarimetric Imaging Campaign

Author

Tara Cotten, Jean-Baptiste Ruffio, Kimberly Ward-Duong, Rebecca Oppenheimer, David Palmer, Pauline Arriaga, Bin Ren, Jérôme Maire, Inseok Song, Zachary H. Draper, Julien Rameau, Travis Barman, James R. Graham, Justin Hom, Jeffrey Chilcote, Sebastian Bruzzone, Joanna Bulger, Dmitry Savransky, Ronald Lopez, Rémi Soummer, Robert J. De Rosa, Laurent Pueyo, Michael P. Fitzgerald, Bruce Macintosh, Abhijith Rajan, Paul Kalas, Jason J. Wang, Sasha Hinkley, Stan Metchev, Alexandra Z. Greenbaum, Fredrik T. Rantakyrö, Eric L. Nielsen, Mark S. Marley, Kevin Stahl, Maxwell A. Millar-Blanchaer, Ruobing Dong, Pascale Hibon, Ian Czekala, Li-Wei Hung, Sandrine Thomas, Eugene Chiang, Stephen J. Goodsell, Schuyler Wolff, Quinn Konopacky, Adam C. Schneider, Franck Marchis, Christine Chen, S. Mark Ammons, René Doyon, Jennifer Patience, Vanessa P. Bailey, Malena Rice, Thomas M. Esposito, Christian Marois, Anand Sivaramakrishnan, Johan Mazoyer, Barry Zuckerman, Gaspard Duchêne, Marshall D. Perrin, Patrick Ingraham, Lisa Poyneer, Megan Ansdell, Katherine B. Follette, Benjamin L. Gerard, and Brenda C. Matthews

Subjects
010504 meteorology & atmospheric sciences, Polarimetry, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Integral field spectrograph, 0103 physical sciences, Radiative transfer, Astrophysics::Solar and Stellar Astrophysics, Gemini Planet Imager, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Debris disk, Astronomy and Astrophysics, Exoplanet, Stars, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Circumstellar dust, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the results of a ${\sim}4$-year direct imaging survey of 104 stars to resolve and characterize circumstellar debris disks in scattered light as part of the Gemini Planet Imager Exoplanet Survey. We targeted nearby (${\lesssim}150$ pc), young (${\lesssim}500$ Myr) stars with high infrared excesses ($L_{\mathrm{IR}} / L_\star > 10^{-5}$), including 38 with previously resolved disks. Observations were made using the Gemini Planet Imager high-contrast integral field spectrograph in $H$-band (1.6 $��$m) coronagraphic polarimetry mode to measure both polarized and total intensities. We resolved 26 debris disks and three protoplanetary/transitional disks. Seven debris disks were resolved in scattered light for the first time, including newly presented HD 117214 and HD 156623, and we quantified basic morphologies of five of them using radiative transfer models. All of our detected debris disks but HD 156623 have dust-poor inner holes, and their scattered-light radii are generally larger than corresponding radii measured from resolved thermal emission and those inferred from spectral energy distributions. To assess sensitivity, we report contrasts and consider causes of non-detections. Detections were strongly correlated with high IR excess and high inclination, although polarimetry outperformed total intensity angular differential imaging for detecting low inclination disks (${\lesssim} 70 ��$). Based on post-survey statistics, we improved upon our pre-survey target prioritization metric predicting polarimetric disk detectability. We also examined scattered-light disks in the contexts of gas, far-IR, and millimeter detections. Comparing $H$-band and ALMA fluxes for two disks revealed tentative evidence for differing grain properties. Finally, we found no preference for debris disks to be detected in scattered light if wide-separation substellar companions were present., arXiv resubmission with typographical corrections. Accepted for publication in AJ. 19 figures, 7 tables

Published
2020

22. HD 165054: an astrometric calibration field for high-contrast imagers in Baade's Window

Author

Travis Barman, Inseok Song, Franck Marchis, James R. Graham, Michael P. Fitzgerald, Jeffrey Chilcote, Sloane Wiktorowicz, Paul Kalas, James E. Larkin, David Palmer, Julien Rameau, Fredrik T. Rantakyrö, Stephen J. Goodsell, Schuyler Wolff, Patrick Ingraham, Gaspard Duchêne, Marshall D. Perrin, Bruce Macintosh, Meiji M. Nguyen, Abhijith Rajan, Robert J. De Rosa, Laurent Pueyo, Li Wei Hung, Katherine B. Follette, Jason J. Wang, Lisa Poyneer, Bin Ren, Anand Sivaramakrishnan, Christian Marois, Stanimir Metchev, René Doyon, Quinn Konopacky, J. Kent Wallace, Sandrine Thomas, Rémi Soummer, Kimberly Ward-Duong, Adam C. Schneider, Dmitry Savransky, Alexandra Z. Greenbaum, Maxwell A. Millar-Blanchaer, Mark S. Marley, Thomas M. Esposito, Eric L. Nielsen, Rebecca Oppenheimer, Joanna Bulger, Vanessa P. Bailey, Melisa Tallis, Pascale Hibon, Tara Cotten, Jennifer Patience, Jean-Baptiste Ruffio, Jérôme Maire, Benjamin L. Gerard, and Justin Hom

Subjects
astronomical instrumentation, Proper motion, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Baade's Window, Bulge, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Gemini Planet Imager, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, astronomy data reduction, direct imaging, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Astrometry, Galactic plane, Stars, Space and Planetary Science, astrometry, Astrophysics::Earth and Planetary Astrophysics, Parallax, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

We present a study of the HD 165054 astrometric calibration field that has been periodically observed with the Gemini Planet Imager. HD 165054 is a bright star within Baade's Window, a region of the galactic plane with relatively low extinction from interstellar dust. HD 165054 was selected as a calibrator target due to the high number density of stars within this region ($\sim 3$ stars per square arcsecond with $H, 25 pages, 12 figures

Published
2020

23. Revised astrometric calibration of the Gemini Planet Imager

Author

Jennifer Patience, Jean-Baptiste Ruffio, Laurent Pueyo, Inseok Song, Stanimir Metchev, Jeffrey Chilcote, Travis Barman, S. Mark Ammons, René Doyon, Sloane Wiktorowicz, James R. Graham, Katherine B. Follette, Meiji M. Nguyen, Rebecca Oppenheimer, Robert J. De Rosa, Maxwell A. Millar-Blanchaer, Bruce Macintosh, Vanessa P. Bailey, Michael P. Fitzgerald, Fredrik T. Rantakyrö, Stephen J. Goodsell, Schuyler Wolff, Jason J. Wang, Kimberly Ward-Duong, Mark S. Marley, Gaspard Duchêne, Lisa Poyneer, Rémi Soummer, Tara Cotten, Marshall D. Perrin, Dmitry Savransky, Pascale Hibon, Quinn Konopacky, Li-Wei Hung, Alexandra Z. Greenbaum, Abhijith Rajan, Franck Marchis, Anand Sivaramakrishnan, D. M. Palmer, Paul Kalas, Christian Marois, Julien Rameau, Benjamin L. Gerard, James E. Larkin, Joanna Bulger, Sandrine Thomas, Thomas M. Esposito, Adam C. Schneider, Patrick Ingraham, Eric L. Nielsen, Jérôme Maire, and J. Kent Wallace

Subjects
FOS: Physical sciences, 01 natural sciences, 010309 optics, astrometric calibration, 0103 physical sciences, Calibration, Gemini Planet Imager, 010303 astronomy & astrophysics, Instrumentation, Instrumentation and Methods for Astrophysics (astro-ph.IM), Zenith, Physics, High contrast, Mechanical Engineering, Astronomy, Astronomy and Astrophysics, Astrometry, Position angle, Electronic, Optical and Magnetic Materials, Stars, high-contrast imaging, Space and Planetary Science, Control and Systems Engineering, Astrophysics - Instrumentation and Methods for Astrophysics, data processing, Data reduction
Abstract

We present a revision to the astrometric calibration of the Gemini Planet Imager (GPI), an instrument designed to achieve the high contrast at small angular separations necessary to image substellar and planetary-mass companions around nearby, young stars. We identified several issues with the GPI Data Reduction Pipeline (DRP) that significantly affected the determination of angle of north in reduced GPI images. As well as introducing a small error in position angle measurements for targets observed at small zenith distances, this error led to a significant error in the previous astrometric calibration that has affected all subsequent astrometric measurements. We present a detailed description of these issues, and how they were corrected. We reduced GPI observations of calibration binaries taken periodically since the instrument was commissioned in 2014 using an updated version of the DRP. These measurements were compared to observations obtained with the NIRC2 instrument on Keck II, an instrument with an excellent astrometric calibration, allowing us to derive an updated plate scale and north offset angle for GPI. This revised astrometric calibration should be used to calibrate all measurements obtained with GPI for the purposes of precision astrometry., Comment: 36 pages, 17 figures, accepted for publication in the Journal of Astronomical Telescopes, Instruments, and Systems. Updated version includes revisions made during the referee process

Published
2020

24. An updated visual orbit of the directly imaged exoplanet 51 Eridani b and prospects for a dynamical mass measurement with Gaia

Author

Sloane Wiktorowicz, Marshall D. Perrin, Laurent Pueyo, Bin Ren, Melisa Tallis, Jean-Baptiste Ruffio, Pascale Hibon, Rémi Soummer, James E. Larkin, Jason J. Wang, Inseok Song, Jérôme Maire, Benjamin L. Gerard, Bruce Macintosh, Justin Hom, Fredrik T. Rantakyrö, Gaspard Duchêne, Julien Rameau, Abhijith Rajan, Maxwell A. Millar-Blanchaer, David Palmer, Dmitry Savransky, Anand Sivaramakrishnan, Lisa Poyneer, Eric L. Nielsen, Quinn Konopacky, Franck Marchis, Robert J. De Rosa, Christian Marois, Stephen J. Goodsell, Schuyler Wolff, J. Kent Wallace, Jeffrey Chilcote, James R. Graham, J. Bulger, Katherine B. Follette, Patrick Ingraham, Jennifer Patience, Tara Cotten, Sandrine Thomas, Adam C. Schneider, Stanimir Metchev, Alexandra Z. Greenbaum, S. Mark Ammons, René Doyon, Travis Barman, Michael P. Fitzgerald, Paul Kalas, Rebecca Oppenheimer, K. Ward-Duong, Thomas M. Esposito, Vanessa P. Bailey, Li Wei Hung, and Mark S. Marley

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Physics, exoplanet dynamics, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Astrometry, 01 natural sciences, Exoplanet, Orbit, Acceleration, Stars, 13. Climate action, Space and Planetary Science, Planet, coronographic imaging, 0103 physical sciences, astrometry, Gemini Planet Imager, Circular orbit, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

We present a revision to the visual orbit of the young, directly-imaged exoplanet 51 Eridani b using four years of observations with the Gemini Planet Imager. The relative astrometry is consistent with an eccentric ($e=0.53_{-0.13}^{+0.09}$) orbit at an intermediate inclination ($i=136_{-11}^{+10}$\,deg), although circular orbits cannot be excluded due to the complex shape of the multidimensional posterior distribution. We find a semi-major axis of $11.1_{-1.3}^{+4.2}$\,au and a period of $28.1_{-4.9}^{+17.2}$\,yr, assuming a mass of 1.75\,M$_{\odot}$ for the host star. We find consistent values with a recent analysis of VLT/SPHERE data covering a similar baseline. We investigated the potential of using absolute astrometry of the host star to obtain a dynamical mass constraint for the planet. The astrometric acceleration of 51~Eri derived from a comparison of the {\it Hipparcos} and {\it Gaia} catalogues was found to be inconsistent at the 2--3$\sigma$ level with the predicted reflex motion induced by the orbiting planet. Potential sources of this inconsistency include a combination of random and systematic errors between the two astrometric catalogs or the signature of an additional companion within the system interior to current detection limits. We also explored the potential of using {\it Gaia} astrometry alone for a dynamical mass measurement of the planet by simulating {\it Gaia} measurements of the motion of the photocenter of the system over the course of the extended eight-year mission. We find that such a measurement is only possible ($>98$\% probability) given the most optimistic predictions for the {\it Gaia} scan astrometric uncertainties for bright stars, and a high mass for the planet ($\gtrsim3.6$\,M$_{\rm Jup}$)., Comment: 17 pages, 11 figures. Accepted for publication in the Astronomical Journal

Published
2019

25. An Exo-Kuiper Belt and An Extended Halo around HD 191089 in Scattered Light

Author

Pauline Arriaga, Bin Ren, Sloane Wiktorowicz, Alexandra Z. Greenbaum, Rémi Soummer, Arthur Vigan, Christophe Pinte, Robert J. De Rosa, Inseok Song, Laurent Pueyo, Jean-Baptiste Ruffio, Johan Mazoyer, Fredrik T. Rantakyrö, Juan Sebastián Bruzzone, Thomas M. Esposito, Tara Cotten, Patrick Ingraham, Travis Barman, Christopher C. Stark, Sandrine Thomas, J. Kent Wallace, Magaret Moerchen, Jeffrey Chilcote, Julien Rameau, Franck Marchis, Adam C. Schneider, Megan Ansdell, Malena Rice, Christian Marois, Li-Wei Hung, Stanimir Metchev, Lisa Poyneer, Bruce Macintosh, Charles A. Poteet, S. Mark Ammons, René Doyon, James E. Larkin, Kimberly Ward-Duong, Tushar Mittal, Pascale Hibon, Gaspard Duchene, Michael P. Fitzgerald, Quinn Konopacky, Maxwell A. Millar-Blanchaer, Glenn Schneider, Joanna Bulger, Jérôme Maire, Mamadou N'Diaye, Katherine B. Follette, Rebecca Oppenheimer, J. Brendan Hagan, James R. Graham, Eric L. Nielsen, Marie Ygouf, Christine Chen, Paul Kalas, Jennifer Patience, Abhijith Rajan, Marshall D. Perrin, Stephen J. Goodsell, Schuyler Wolff, Anand Sivaramakrishnan, Dean C. Hines, Vanessa P. Bailey, Dmitry Savransky, Elodie Choquet, D. M. Palmer, John H. Debes, Jason J. Wang, Francois Menard, Dominic M. Ryan, Colin Norman, Benjamin L. Gerard, Department of Physics and Astronomy [Baltimore], Johns Hopkins University (JHU), Department of Mathematics and Statistics [Baltimore], Loyola University [Maryland, Baltimore], Caltech Department of Astronomy [Pasadena], California Institute of Technology (CALTECH), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, Space Telescope Science Institute (STSci), Department of Astronomy [Berkeley], University of California [Berkeley], University of California-University of California, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Yale University [New Haven], Steward Observatory, University of Arizona, Lawrence Livermore National Laboratory (LLNL), Department of Physics and Astronomy [UCLA, Los Angeles], University of California [Los Angeles] (UCLA), Lunar and Planetary Laboratory [Tucson] (LPL), University of Western Ontario (UWO), Subaru Telescope, National Astronomical Observatory of Japan (NAOJ), University of Notre Dame [Indiana] (UND), University of Georgia [USA], Institut de Recherche sur les Exoplanètes (iREX), Université de Montréal [Montréal], Amherst College, Gemini Observatory [Southern Operations Center], Association of Universities for Research in Astronomy (AURA), University of Victoria [Canada] (UVIC), National Research Council of Canada (NRC), Department of Astronomy [Ann Arbor], University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Natural Sounds and Night Skies Division, Large Synoptic Survey Telescope (LSST), Search for Extraterrestrial Intelligence Institute (SETI), University of California [San Diego] (UC San Diego), University of California, Kavli Institute for Particle Astrophysics and Cosmology (KIPAC), Stanford University [Stanford], Department of Physics and Astronomy [Stony Brook], Stony Brook University [SUNY] (SBU), State University of New York (SUNY)-State University of New York (SUNY), Department of Earth and Planetary Science [UC Berkeley] (EPS), American Geophysical Union, Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), American Museum of Natural History (AMNH), Arizona State University [Tempe] (ASU), School of Physics and Astronomy [Clayton], Monash University [Clayton], Department of Astronomy [Ithaca], Cornell University, Department of Astronomy and Astrophysics [UCSC Santa Cruz], University of California [Santa Cruz] (UCSC), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Infrared Processing and Analysis Center (IPAC), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), NASA-California Institute of Technology (CALTECH), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université de Montréal (UdeM), Stanford University, Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Cornell University [New York], University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), University of California (UC), American Geophysical Union [Washington], Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), University of California [Santa Cruz] (UC Santa Cruz), and Universiteit Leiden

Subjects
010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Phase (waves), FOS: Physical sciences, techniques: image processing, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Ring (chemistry), stars: individual (HD 191089), 01 natural sciences, Power law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Debris disk, Range (particle radiation), Scattering, protoplanetary disks, Astronomy and Astrophysics, stars: imaging, Astrophysics - Solar and Stellar Astrophysics, radiative transfer, 13. Climate action, Space and Planetary Science, Halo, Astrophysics::Earth and Planetary Astrophysics, Intensity (heat transfer), Astrophysics - Earth and Planetary Astrophysics
Abstract

We have obtained Hubble Space Telescope STIS and NICMOS, and Gemini/GPI scattered light images of the HD 191089 debris disk. We identify two spatial components: a ring resembling Kuiper Belt in radial extent (FWHM: ${\sim}$25 au, centered at ${\sim}$46 au), and a halo extending to ${\sim}$640 au. We find that the halo is significantly bluer than the ring, consistent with the scenario that the ring serves as the "birth ring" for the smaller dust in the halo. We measure the scattering phase functions in the 30{\deg}-150{\deg} scattering angle range and find the halo dust is both more forward- and backward-scattering than the ring dust. We measure a surface density power law index of -0.68${\pm}$0.04 for the halo, which indicates the slow-down of the radial outward motion of the dust. Using radiative transfer modeling, we attempt to simultaneously reproduce the (visible) total and (near-infrared) polarized intensity images of the birth ring. Our modeling leads to mutually inconsistent results, indicating that more complex models, such as the inclusion of more realistic aggregate particles, are needed., Comment: 29 pages, 18 figures, ApJ accepted

Published
2019

26. Performance of the Gemini Planet Imager Non-Redundant Mask and spectroscopy of two close-separation binaries HR 2690 and HD 142527

Author

Tara Cotten, Abhijith Rajan, Mark S. Marley, Rebecca Oppenheimer, Franck Marchis, Inseok Song, Vanessa P. Bailey, Stanimir Metchev, James R. Graham, Pascale Hibon, Stephen J. Goodsell, Schuyler Wolff, Joanna Bulger, Robert J. De Rosa, S. Mark Ammons, Jeffrey Chilcote, René Doyon, Kimberly Ward-Duong, Alexandra Z. Greenbaum, Naru Sadakuni, Lisa Poyneer, Eric L. Nielsen, Dmitry Savransky, Andrew Cardwell, Anand Sivaramakrishnan, Katie M. Morzinski, Laurent Pueyo, Sandrine Thomas, Peter G. Tuthill, Adam C. Schneider, Christian Marois, Patrick Ingraham, Sloane Wiktorowicz, Katherine B. Follette, Maxwell A. Millar-Blanchaer, Gaspard Duchêne, Li-Wei Hung, Marshall D. Perrin, Bruce Macintosh, Fredrik T. Rantakyrö, Jennifer Patience, Quinn Konopacky, David Palmer, Benjamin L. Gerard, Rémi Soummer, Travis Barman, J. Kent Wallace, Jason J. Wang, Michael P. Fitzgerald, Paul Kalas, James E. Larkin, Julien Rameau, Anthony Cheetham, and Jérôme Maire

Subjects
Physics, FOS: Physical sciences, techniques: high angular resolution, Astronomy, Astronomy and Astrophysics, instrumentation: adaptive optics, 01 natural sciences, Exoplanet, Astronomical instrumentation, 010309 optics, Graduate research, stars: individual (HR 2690, HD 142527), Space and Planetary Science, 0103 physical sciences, Gemini Planet Imager, National laboratory, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics
Abstract

The Gemini Planet Imager (GPI) contains a 10-hole non-redundant mask (NRM), enabling interferometric resolution in complement to its coronagraphic capabilities. The NRM operates both in spectroscopic (integral field spectrograph, henceforth IFS) and polarimetric configurations. NRM observations were taken between 2013 and 2016 to characterize its performance. Most observations were taken in spectroscopic mode with the goal of obtaining precise astrometry and spectroscopy of faint companions to bright stars. We find a clear correlation between residual wavefront error measured by the AO system and the contrast sensitivity by comparing phase errors in observations of the same source, taken on different dates. We find a typical 5-$\sigma$ contrast sensitivity of $2-3~\times~10^{-3}$ at $\sim\lambda/D$. We explore the accuracy of spectral extraction of secondary components of binary systems by recovering the signal from a simulated source injected into several datasets. We outline data reduction procedures unique to GPI's IFS and describe a newly public data pipeline used for the presented analyses. We demonstrate recovery of astrometry and spectroscopy of two known companions to HR 2690 and HD 142527. NRM+polarimetry observations achieve differential visibility precision of $\sigma\sim0.4\%$ in the best case. We discuss its limitations on Gemini-S/GPI for resolving inner regions of protoplanetary disks and prospects for future upgrades. We summarize lessons learned in observing with NRM in spectroscopic and polarimetric modes., Comment: Accepted to AJ, 22 pages, 14 figures

Published
2019

27. The Gemini Planet Imager Exoplanet Survey: Giant Planet and Brown Dwarf Demographics From 10-100 AU

Author

Eric L. Nielsen, Robert J. De Rosa, Bruce Macintosh, Jason J. Wang, Jean-Baptiste Ruffio, Eugene Chiang, Mark S. Marley, Didier Saumon, Dmitry Savransky, S. Mark Ammons, Vanessa P. Bailey, Travis Barman, Célia Blain, Joanna Bulger, Adam Burrows, Jeffrey Chilcote, Tara Cotten, Ian Czekala, Rene Doyon, Gaspard Duchêne, Thomas M. Esposito, Daniel Fabrycky, Michael P. Fitzgerald, Katherine B. Follette, Jonathan J. Fortney, Benjamin L. Gerard, Stephen J. Goodsell, James R. Graham, Alexandra Z. Greenbaum, Pascale Hibon, Sasha Hinkley, Lea A. Hirsch, Justin Hom, Li-Wei Hung, Rebekah Ilene Dawson, Patrick Ingraham, Paul Kalas, Quinn Konopacky, James E. Larkin, Eve J. Lee, Jonathan W. Lin, Jérôme Maire, Franck Marchis, Christian Marois, Stanimir Metchev, Maxwell A. Millar-Blanchaer, Katie M. Morzinski, Rebecca Oppenheimer, David Palmer, Jennifer Patience, Marshall Perrin, Lisa Poyneer, Laurent Pueyo, Roman R. Rafikov, Abhijith Rajan, Julien Rameau, Fredrik T. Rantakyrö, Bin Ren, Adam C. Schneider, Anand Sivaramakrishnan, Inseok Song, Remi Soummer, Melisa Tallis, Sandrine Thomas, Kimberly Ward-Duong, Schuyler Wolff, Nielsen, EL [0000-0001-6975-9056], De Rosa, RJ [0000-0002-4918-0247], Macintosh, B [0000-0003-1212-7538], Wang, JJ [0000-0003-0774-6502], Ruffio, JB [0000-0003-2233-4821], Chiang, E [0000-0002-6246-2310], Marley, MS [0000-0002-5251-2943], Saumon, D [0000-0001-6800-3505], Savransky, D [0000-0002-8711-7206], Mark Ammons, S [0000-0001-5172-7902], Bailey, VP [0000-0002-5407-2806], Barman, T [0000-0002-7129-3002], Bulger, J [0000-0003-4641-2003], Burrows, A [0000-0002-3099-5024], Chilcote, J [0000-0001-6305-7272], Cotten, T [0000-0003-0156-3019], Czekala, I [0000-0002-1483-8811], Esposito, TM [0000-0002-0792-3719], Fabrycky, D [0000-0003-3750-0183], Fitzgerald, MP [0000-0002-0176-8973], Follette, KB [0000-0002-7821-0695], Fortney, JJ [0000-0002-9843-4354], Gerard, BL [0000-0003-3978-9195], Goodsell, SJ [0000-0002-4144-5116], Greenbaum, AZ [0000-0002-7162-8036], Hibon, P [0000-0003-3726-5494], Hinkley, S [0000-0001-8074-2562], Hung, LW [0000-0003-1498-6088], Ilene Dawson, R [0000-0001-9677-1296], Ingraham, P [0000-0003-3715-8138], Konopacky, Q [0000-0002-9936-6285], Larkin, JE [0000-0001-7687-3965], Lee, EJ [0000-0002-1228-9820], Marchis, F [0000-0001-7016-7277], Marois, C [0000-0002-4164-4182], Metchev, S [0000-0003-3050-8203], Millar-Blanchaer, MA [0000-0001-6205-9233], Morzinski, KM [0000-0002-1384-0063], Oppenheimer, R [0000-0001-7130-7681], Perrin, M [0000-0002-3191-8151], Rafikov, RR [0000-0002-0012-1609], Rajan, A [0000-0002-9246-5467], Rameau, J [0000-0003-0029-0258], Rantakyrö, FT [0000-0002-9667-2244], Ren, B [0000-0003-1698-9696], Schneider, AC [0000-0002-6294-5937], Sivaramakrishnan, A [0000-0003-1251-4124], Song, I [0000-0002-5815-7372], Soummer, R [0000-0003-2753-2819], Tallis, M [0000-0002-5917-6524], Thomas, S [0000-0002-9121-3436], Ward-Duong, K [0000-0002-4479-8291], Wolff, S [0000-0002-9977-8255], and Apollo - University of Cambridge Repository

Subjects
planets and satellites: detection, 010504 meteorology & atmospheric sciences, Stellar mass, detection [planets and satellites], Brown dwarf, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, adaptive optics [instrumentation], Astronomy & Astrophysics, instrumentation: adaptive optics, 01 natural sciences, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, planetary systems, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Mass distribution, Giant planet, Astronomy and Astrophysics, Exoplanet, Stars, 13. Climate action, Space and Planetary Science, astro-ph.EP, Astrophysics::Earth and Planetary Astrophysics, Planetary mass, Astronomical and Space Sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

We present a statistical analysis of the first 300 stars observed by the Gemini Planet Imager Exoplanet Survey (GPIES). This subsample includes six detected planets and three brown dwarfs; from these detections and our contrast curves we infer the underlying distributions of substellar companions with respect to their mass, semi-major axis, and host stellar mass. We uncover a strong correlation between planet occurrence rate and host star mass, with stars M $>$ 1.5 $M_\odot$ more likely to host planets with masses between 2-13 M$_{\rm Jup}$ and semi-major axes of 3-100 au at 99.92% confidence. We fit a double power-law model in planet mass (m) and semi-major axis (a) for planet populations around high-mass stars (M $>$ 1.5M$_\odot$) of the form $\frac{d^2 N}{dm da} \propto m^\alpha a^\beta$, finding $\alpha$ = -2.4 $\pm$ 0.8 and $\beta$ = -2.0 $\pm$ 0.5, and an integrated occurrence rate of $9^{+5}_{-4}$% between 5-13 M$_{\rm Jup}$ and 10-100 au. A significantly lower occurrence rate is obtained for brown dwarfs around all stars, with 0.8$^{+0.8}_{-0.5}$% of stars hosting a brown dwarf companion between 13-80 M$_{\rm Jup}$ and 10-100 au. Brown dwarfs also appear to be distributed differently in mass and semi-major axis compared to giant planets; whereas giant planets follow a bottom-heavy mass distribution and favor smaller semi-major axes, brown dwarfs exhibit just the opposite behaviors. Comparing to studies of short-period giant planets from the RV method, our results are consistent with a peak in occurrence of giant planets between ~1-10 au. We discuss how these trends, including the preference of giant planets for high-mass host stars, point to formation of giant planets by core/pebble accretion, and formation of brown dwarfs by gravitational instability., Comment: 52 pages, 18 figures. AJ in press

Published
2019

28. LSST: from Science Drivers to Reference Design and Anticipated Data Products

Author

Željko Ivezić, Steven M. Kahn, J. Anthony Tyson, Bob Abel, Emily Acosta, Robyn Allsman, David Alonso, Yusra AlSayyad, Scott F. Anderson, John Andrew, James Roger P. Angel, George Z. Angeli, Reza Ansari, Pierre Antilogus, Constanza Araujo, Robert Armstrong, Kirk T. Arndt, Pierre Astier, Éric Aubourg, Nicole Auza, Tim S. Axelrod, Deborah J. Bard, Jeff D. Barr, Aurelian Barrau, James G. Bartlett, Amanda E. Bauer, Brian J. Bauman, Sylvain Baumont, Ellen Bechtol, Keith Bechtol, Andrew C. Becker, Jacek Becla, Cristina Beldica, Steve Bellavia, Federica B. Bianco, Rahul Biswas, Guillaume Blanc, Jonathan Blazek, Roger D. Blandford, Josh S. Bloom, Joanne Bogart, Tim W. Bond, Michael T. Booth, Anders W. Borgland, Kirk Borne, James F. Bosch, Dominique Boutigny, Craig A. Brackett, Andrew Bradshaw, William Nielsen Brandt, Michael E. Brown, James S. Bullock, Patricia Burchat, David L. Burke, Gianpietro Cagnoli, Daniel Calabrese, Shawn Callahan, Alice L. Callen, Jeffrey L. Carlin, Erin L. Carlson, Srinivasan Chandrasekharan, Glenaver Charles-Emerson, Steve Chesley, Elliott C. Cheu, Hsin-Fang Chiang, James Chiang, Carol Chirino, Derek Chow, David R. Ciardi, Charles F. Claver, Johann Cohen-Tanugi, Joseph J. Cockrum, Rebecca Coles, Andrew J. Connolly, Kem H. Cook, Asantha Cooray, Kevin R. Covey, Chris Cribbs, Wei Cui, Roc Cutri, Philip N. Daly, Scott F. Daniel, Felipe Daruich, Guillaume Daubard, Greg Daues, William Dawson, Francisco Delgado, Alfred Dellapenna, Robert de Peyster, Miguel de Val-Borro, Seth W. Digel, Peter Doherty, Richard Dubois, Gregory P. Dubois-Felsmann, Josef Durech, Frossie Economou, Tim Eifler, Michael Eracleous, Benjamin L. Emmons, Angelo Fausti Neto, Henry Ferguson, Enrique Figueroa, Merlin Fisher-Levine, Warren Focke, Michael D. Foss, James Frank, Michael D. Freemon, Emmanuel Gangler, Eric Gawiser, John C. Geary, Perry Gee, Marla Geha, Charles J. B. Gessner, Robert R. Gibson, D. Kirk Gilmore, Thomas Glanzman, William Glick, Tatiana Goldina, Daniel A. Goldstein, Iain Goodenow, Melissa L. Graham, William J. Gressler, Philippe Gris, Leanne P. Guy, Augustin Guyonnet, Gunther Haller, Ron Harris, Patrick A. Hascall, Justine Haupt, Fabio Hernandez, Sven Herrmann, Edward Hileman, Joshua Hoblitt, John A. Hodgson, Craig Hogan, James D. Howard, Dajun Huang, Michael E. Huffer, Patrick Ingraham, Walter R. Innes, Suzanne H. Jacoby, Bhuvnesh Jain, Fabrice Jammes, James Jee, Tim Jenness, Garrett Jernigan, Darko Jevremović, Kenneth Johns, Anthony S. Johnson, Margaret W. G. Johnson, R. Lynne Jones, Claire Juramy-Gilles, Mario Jurić, Jason S. Kalirai, Nitya J. Kallivayalil, Bryce Kalmbach, Jeffrey P. Kantor, Pierre Karst, Mansi M. Kasliwal, Heather Kelly, Richard Kessler, Veronica Kinnison, David Kirkby, Lloyd Knox, Ivan V. Kotov, Victor L. Krabbendam, K. Simon Krughoff, Petr Kubánek, John Kuczewski, Shri Kulkarni, John Ku, Nadine R. Kurita, Craig S. Lage, Ron Lambert, Travis Lange, J. Brian Langton, Laurent Le Guillou, Deborah Levine, Ming Liang, Kian-Tat Lim, Chris J. Lintott, Kevin E. Long, Margaux Lopez, Paul J. Lotz, Robert H. Lupton, Nate B. Lust, Lauren A. MacArthur, Ashish Mahabal, Rachel Mandelbaum, Thomas W. Markiewicz, Darren S. Marsh, Philip J. Marshall, Stuart Marshall, Morgan May, Robert McKercher, Michelle McQueen, Joshua Meyers, Myriam Migliore, Michelle Miller, David J. Mills, Connor Miraval, Joachim Moeyens, Fred E. Moolekamp, David G. Monet, Marc Moniez, Serge Monkewitz, Christopher Montgomery, Christopher B. Morrison, Fritz Mueller, Gary P. Muller, Freddy Muñoz Arancibia, Douglas R. Neill, Scott P. Newbry, Jean-Yves Nief, Andrei Nomerotski, Martin Nordby, Paul O’Connor, John Oliver, Scot S. Olivier, Knut Olsen, William O’Mullane, Sandra Ortiz, Shawn Osier, Russell E. Owen, Reynald Pain, Paul E. Palecek, John K. Parejko, James B. Parsons, Nathan M. Pease, J. Matt Peterson, John R. Peterson, Donald L. Petravick, M. E. Libby Petrick, Cathy E. Petry, Francesco Pierfederici, Stephen Pietrowicz, Rob Pike, Philip A. Pinto, Raymond Plante, Stephen Plate, Joel P. Plutchak, Paul A. Price, Michael Prouza, Veljko Radeka, Jayadev Rajagopal, Andrew P. Rasmussen, Nicolas Regnault, Kevin A. Reil, David J. Reiss, Michael A. Reuter, Stephen T. Ridgway, Vincent J. Riot, Steve Ritz, Sean Robinson, William Roby, Aaron Roodman, Wayne Rosing, Cecille Roucelle, Matthew R. Rumore, Stefano Russo, Abhijit Saha, Benoit Sassolas, Terry L. Schalk, Pim Schellart, Rafe H. Schindler, Samuel Schmidt, Donald P. Schneider, Michael D. Schneider, William Schoening, German Schumacher, Megan E. Schwamb, Jacques Sebag, Brian Selvy, Glenn H. Sembroski, Lynn G. Seppala, Andrew Serio, Eduardo Serrano, Richard A. Shaw, Ian Shipsey, Jonathan Sick, Nicole Silvestri, Colin T. Slater, J. Allyn Smith, R. Chris Smith, Shahram Sobhani, Christine Soldahl, Lisa Storrie-Lombardi, Edward Stover, Michael A. Strauss, Rachel A. Street, Christopher W. Stubbs, Ian S. Sullivan, Donald Sweeney, John D. Swinbank, Alexander Szalay, Peter Takacs, Stephen A. Tether, Jon J. Thaler, John Gregg Thayer, Sandrine Thomas, Adam J. Thornton, Vaikunth Thukral, Jeffrey Tice, David E. Trilling, Max Turri, Richard Van Berg, Daniel Vanden Berk, Kurt Vetter, Francoise Virieux, Tomislav Vucina, William Wahl, Lucianne Walkowicz, Brian Walsh, Christopher W. Walter, Daniel L. Wang, Shin-Yawn Wang, Michael Warner, Oliver Wiecha, Beth Willman, Scott E. Winters, David Wittman, Sidney C. Wolff, W. Michael Wood-Vasey, Xiuqin Wu, Bo Xin, Peter Yoachim, Hu Zhan, Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Université Paris Diderot - Paris 7 (UPD7), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire des matériaux avancés (LMA), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Centre National de la Recherche Scientifique (CNRS), Centre de Calcul de l'IN2P3 (CC-IN2P3), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Instituto de RadioAstronomía Milimétrica (IRAM), Centre National de la Recherche Scientifique (CNRS), LSST, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne (UCA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), and Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2)

Subjects
010504 meteorology & atmospheric sciences, Astronomy, observational [methods], Field of view, Astrophysics, 7. Clean energy, 01 natural sciences, law.invention, law, size distribution, sagittarius dwarf galaxy, 010303 astronomy & astrophysics, stars: general, media_common, Physics, Reference design, general [stars], gamma-ray bursts, Astrophysics (astro-ph), observations [cosmology], proper motion stars, ia supernovae, astrometry, methods: observational, Astronomical and Space Sciences, Physical Chemistry (incl. Structural), Milky Way, media_common.quotation_subject, Dark matter, FOS: Physical sciences, Large Synoptic Survey Telescope, Astronomy & Astrophysics, milky-way tomography, Primary mirror, Telescope, surveys, astro-ph, 0103 physical sciences, Galaxy: general, general [Galaxy], 0105 earth and related environmental sciences, dark-energy constraints, Organic Chemistry, Astronomy and Astrophysics, Space and Planetary Science, Sky, tidal disruption events, cosmology: observations, digital sky survey, lensing power spectrum, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

(Abridged) We describe here the most ambitious survey currently planned in the optical, the Large Synoptic Survey Telescope (LSST). A vast array of science will be enabled by a single wide-deep-fast sky survey, and LSST will have unique survey capability in the faint time domain. The LSST design is driven by four main science themes: probing dark energy and dark matter, taking an inventory of the Solar System, exploring the transient optical sky, and mapping the Milky Way. LSST will be a wide-field ground-based system sited at Cerro Pach\'{o}n in northern Chile. The telescope will have an 8.4 m (6.5 m effective) primary mirror, a 9.6 deg$^2$ field of view, and a 3.2 Gigapixel camera. The standard observing sequence will consist of pairs of 15-second exposures in a given field, with two such visits in each pointing in a given night. With these repeats, the LSST system is capable of imaging about 10,000 square degrees of sky in a single filter in three nights. The typical 5$\sigma$ point-source depth in a single visit in $r$ will be $\sim 24.5$ (AB). The project is in the construction phase and will begin regular survey operations by 2022. The survey area will be contained within 30,000 deg$^2$ with $\delta, Comment: 57 pages, 32 color figures, version with high-resolution figures available from https://www.lsst.org/overview

Published
2019

29. Imaging the 44 au Kuiper Belt Analog Debris Ring around HD 141569A with GPI Polarimetry

Author

Juan Sebastián Bruzzone, Stanimir Metchev, Gaspard Duchêne, Maxwell A. Millar-Blanchaer, Ruobing Dong, Thomas M. Esposito, Jason J. Wang, James R. Graham, Johan Mazoyer, Schuyler Wolff, S. Mark Ammons, Adam C. Schneider, Alexandra Z. Greenbaum, Brenda C. Matthews, Pauline Arriaga, Vanessa P. Bailey, Travis Barman, Joanna Bulger, Jeffrey Chilcote, Tara Cotten, Robert J. De Rosa, Rene Doyon, Michael P. Fitzgerald, Katherine B. Follette, Benjamin L. Gerard, Stephen J. Goodsell, Pascale Hibon, Justin Hom, Li-Wei Hung, Patrick Ingraham, Paul Kalas, Quinn Konopacky, James E. Larkin, Bruce Macintosh, Jérôme Maire, Franck Marchis, Christian Marois, Katie M. Morzinski, Eric L. Nielsen, Rebecca Oppenheimer, David Palmer, Rahul Patel, Jennifer Patience, Marshall Perrin, Lisa Poyneer, Laurent Pueyo, Abhijith Rajan, Julien Rameau, Fredrik T. Rantakyrö, Dmitry Savransky, Anand Sivaramakrishnan, Inseok Song, Remi Soummer, Sandrine Thomas, J. Kent Wallace, Kimberly Ward-Duong, and Sloane Wiktorowicz

Subjects
coronographic imaging (313), 010504 meteorology & atmospheric sciences, Polarimetry, FOS: Physical sciences, Astrophysics, 01 natural sciences, polarimetry (1278), Coincident, 0103 physical sciences, Thermal, Radiative transfer, direct imaging (387), Gemini Planet Imager, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Spiral galaxy, astronomical techniques (1684), Astronomy and Astrophysics, debris disks (363), Astrophysics - Solar and Stellar Astrophysics, Thin disk, 13. Climate action, Space and Planetary Science, Millimeter, Astrophysics - Earth and Planetary Astrophysics, circumstellar disks (235)
Abstract

We present the first polarimetric detection of the inner disk component around the pre-main sequence B9.5 star HD 141569A. Gemini Planet Imager H-band (1.65 micron) polarimetric differential imaging reveals the highest signal-to-noise ratio detection of this ring yet attained and traces structure inwards to 0.25" (28 AU at a distance of 111 pc). The radial polarized intensity image shows the east side of the disk, peaking in intensity at 0.40" (44 AU) and extending out to 0.9" (100 AU). There is a spiral arm-like enhancement to the south, reminiscent of the known spiral structures on the outer rings of the disk. The location of the spiral arm is coincident with 12CO J=3-2 emission detected by ALMA, and hints at a dynamically active inner circumstellar region. Our observations also show a portion of the middle dusty ring at ~220 AU known from previous observations of this system. We fit the polarized H-band emission with a continuum radiative transfer Mie model. Our best-fit model favors an optically thin disk with a minimum dust grain size close to the blow-out size for this system: evidence of on-going dust production in the inner reaches of the disk. The thermal emission from this model accounts for virtually all of the far-infrared and millimeter flux from the entire HD 141569A disk, in agreement with the lack of ALMA continuum and CO emission beyond ~100 AU. A remaining 8-30 micron thermal excess a factor of ~2 above our model argues for a yet-unresolved warm innermost 5-15 AU component of the disk., 16 pages, 8 figures, accepted at AJ

Published
2020

30. First Resolved Scattered-light Images of Four Debris Disks in Scorpius-Centaurus with the Gemini Planet Imager

Author

Kezman Saboi, Barry Zuckerman, Gaspard Duchêne, Pauline Arriaga, Sloane J. Wiktorowicz, Inseok Song, Marshall D. Perrin, Bin Ren, Tara Cotten, Christine Chen, Julien Rameau, Lisa Poyneer, Jeffrey Chilcote, Schuyler Wolff, Abhijith Rajan, James R. Graham, Paul Kalas, Dmitry Savransky, Justin Hom, Hannah Jang-Condell, Jennifer Patience, James E. Larkin, Jason J. Wang, Vanessa P. Bailey, Patrick Ingraham, Melisa Tallis, Thomas M. Esposito, Rebecca Oppenheimer, J. Kent Wallace, David Palmer, Katherine B. Follette, Bruce Macintosh, Elisabeth Matthews, Mark S. Marley, Pascale Hibon, Sandrine Thomas, Travis Barman, Quinn Konopacky, Adam C. Schneider, Robert J. De Rosa, Jérôme Maire, Christian Marois, Eric L. Nielsen, Michael P. Fitzgerald, Rémi Soummer, Johan Mazoyer, Alexandra Z. Greenbaum, Kadin Worthen, Brenda C. Matthews, S. Goodsell, Fredrik T. Rantakyrö, Anand Sivaramakrishnan, Stanimir Metchev, S. Mark Ammons, René Doyon, Maxwell A. Millar-Blanchaer, Franck Marchis, Laurent Pueyo, Kimberly Ward-Duong, and Joanna Bulger

Subjects
Brightness, circumstellar matter (241), 010504 meteorology & atmospheric sciences, Continuum (design consultancy), FOS: Physical sciences, Astrophysics, planetary system formation (1257), 01 natural sciences, Planet, 0103 physical sciences, direct imaging (387), Gemini Planet Imager, circumstellar dust (236), 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Debris disk, near infrared astronomy (1093), Astronomy and Astrophysics, Planetary system, debris disks (363), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Circumstellar dust, Millimeter, Astrophysics - Earth and Planetary Astrophysics, circumstellar disks (235)
Abstract

We present the first spatially resolved scattered-light images of four debris disks around members of the Scorpius-Centaurus (Sco-Cen) OB Association with high-contrast imaging and polarimetry using the Gemini Planet Imager (GPI). All four disks are resolved for the first time in polarized light and one disk is also detected in total intensity. The three disks imaged around HD 111161, HD 143675, and HD 145560 are symmetric in both morphology and brightness distribution. The three systems span a range of inclinations and radial extents. The disk imaged around HD 98363 shows indications of asymmetries in morphology and brightness distribution, with some structural similarities to the HD 106906 planet-disk system. Uniquely, HD 98363 has a wide co-moving stellar companion Wray 15-788 with a recently resolved disk with very different morphological properties. HD 98363 A/B is the first binary debris disk system with two spatially resolved disks. All four targets have been observed with ALMA, and their continuum fluxes range from one non-detection to one of the brightest disks in the region. With the new results, a total of 15 A/F-stars in Sco-Cen have resolved scattered light debris disks, and approximately half of these systems exhibit some form of asymmetry. Combining the GPI disk structure results with information from the literature on millimeter fluxes and imaged planets reveals a diversity of disk properties in this young population. Overall, the four newly resolved disks contribute to the census of disk structures measured around A/F-stars at this important stage in the development of planetary systems., Comment: 20 pages, 9 figures

Published
2020

31. Direct Imaging of the HD 35841 Debris Disk: A Polarized Dust Ring from Gemini Planet Imager and an Outer Halo from HST/STIS

Author

Bruce Macintosh, Juan Sebastián Bruzzone, Abhijith Rajan, Julien Rameau, Quinn Konopacky, Jérôme Maire, Pauline Arriaga, Bin Ren, Lisa Poyneer, Inseok Song, Rémi Soummer, Sandrine Thomas, Adam C. Schneider, Rebecca Oppenheimer, Christine Chen, Paul Kalas, James R. Graham, Alexandra Z. Greenbaum, David Palmer, J. Kent Wallace, James E. Larkin, Jason J. Wang, Sloane J. Wiktorowicz, Robert J. De Rosa, Eugene Chiang, Gaspard Duchêne, Thomas M. Esposito, Stephen J. Goodsell, Laurent Pueyo, Schuyler Wolff, Joanna Bulger, Marshall D. Perrin, Eric L. Nielsen, Patrick Ingraham, Pascale Hibon, Jeffrey Chilcote, Vanessa P. Bailey, Tara Cotten, Johan Mazoyer, Stanimir Metchev, Dominic M. Ryan, S. Mark Ammons, Kimberly Ward-Duong, Dmitry Savransky, René Doyon, Li-Wei Hung, Maxwell A. Millar-Blanchaer, Franck Marchis, Jennifer Patience, Malena Rice, Elodie Choquet, Travis Barman, Michael P. Fitzgerald, Christian Marois, Fredrik T. Rantakyrö, Anand Sivaramakrishnan, Megan Ansdell, Katherine B. Follette, Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Department of Mathematics [Berkeley], University of California [Berkeley], University of California-University of California, Search for Extraterrestrial Intelligence Institute (SETI), Caltech Department of Astronomy [Pasadena], California Institute of Technology (CALTECH), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Johns Hopkins University (JHU), Space Telescope Science Institute (STSci), Department of Physics and Astronomy [UCLA, Los Angeles], University of California [Los Angeles] (UCLA), Department of Earth and Planetary Science [UC Berkeley] (EPS), Kavli Institute for Particle Astrophysics and Cosmology (KIPAC), Stanford University, Physics and Astronomy Department, Amherst College, European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Laboratoire Universitaire d'Astrophysique de Nice (LUAN), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Arizona State University [Tempe] (ASU), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), California Institute of Technology (CALTECH)-NASA, Stanford University [Stanford], and Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, 01 natural sciences, circumstellar matter, 010305 fluids & plasmas, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Gemini Planet Imager, Surface brightness, planetary systems [infrared], 010303 astronomy & astrophysics, individual [stars], Astrophysics::Galaxy Astrophysics, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Debris disk, Scattering, high angular resolution [techniques], Astronomy and Astrophysics, Planetary system, Radiation pressure, 13. Climate action, Space and Planetary Science, astro-ph.EP, Spectral energy distribution, Halo, Astrophysics::Earth and Planetary Astrophysics, Astronomical and Space Sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

We present new high resolution imaging of a light-scattering dust ring and halo around the young star HD 35841. Using spectroscopic and polarimetric data from the Gemini Planet Imager in H-band (1.6 microns), we detect the highly inclined (i=85 deg) ring of debris down to a projected separation of ~12 au (~0.12") for the first time. Optical imaging from HST/STIS shows a smooth dust halo extending outward from the ring to >140 au (>1.4"). We measure the ring's scattering phase function and polarization fraction over scattering angles of 22-125 deg, showing a preference for forward scattering and a polarization fraction that peaks at ~30% near the ansae. Modeling of the scattered-light disk indicates that the ring spans radii of ~60-220 au, has a vertical thickness similar to that of other resolved dust rings, and contains grains as small as 1.5 microns in diameter. These models also suggest the grains have a low porosity, are more likely to consist of carbon than astrosilicates, and contain significant water ice. The halo has a surface brightness profile consistent with that expected from grains pushed by radiation pressure from the main ring onto highly eccentric but still bound orbits. We also briefly investigate arrangements of a possible inner disk component implied by our spectral energy distribution models, and speculate about the limitations of Mie theory for doing detailed analyses of debris disk dust populations., Accepted to AJ. 22 pages, 11 figures, 3 tables

Published
2018

32. V&V planning and execution in an integrated model-based engineering environment using MagicDraw, Syndeia, and JIRA

Author

Tim Jenness, Wil O'Mullane, Brian M. Selvy, Austin Roberts, Andrew Serio, Sandrine Thomas, Charles F. Claver, Rob Bovill, Michael A. Reuter, Brian Van Klaveren, Gabriele Comoretto, Manas Bajaj, Dirk Zwemer, and Jacques Sebag

Subjects
Test case, Software, Test management, Computer science, Systems Modeling Language, business.industry, Synchronization (computer science), Model-based systems engineering, Systems modeling, Test plan, Software engineering, business
Abstract

This paper describes the evolution of the processes, methodologies and tools developed and utilized on the Large Synoptic Survey Telescope (LSST) project that provide a complete end-to-end environment for verification planning, execution, and reporting. LSST utilizes No Magic’s MagicDraw Cameo Systems Modeler tool as the core tool for systems modeling, a Jira-based test case/test procedure/test plan tool called Test Management for Jira for verification execution, and Intercax’s Syndeia tool for bi-directional synchronization of data between Cameo Systems Modeler and Jira. Several additional supporting tools and services are also described to round out a complete solution. The paper describes the project’s needs, overall software platform architecture, and customizations developed to provide the end to- end solution.

Published
2018

33. LSST telescope and site status

Author

Andrew Serio, Sandrine Thomas, Jacques Sebag, Douglas R. Neill, Francisco Delgado, Grissel Coleman, and William J. Gressler

Subjects
010309 optics, 0103 physical sciences, 010303 astronomy & astrophysics, 01 natural sciences
Published
2018

34. GPI Spectra of HR 8799 c, d, and e from 1.5 to 2.4 μm with KLIP Forward Modeling

Author

Sloane Wiktorowicz, Marshall D. Perrin, Benjamin L. Gerard, Pauline Arriaga, K. Ward-Duong, Jérôme Maire, Stanimir Metchev, Inseok Song, Adam Burrows, James R. Graham, Vanessa P. Bailey, Rémi Soummer, Alexandra Z. Greenbaum, René Doyon, Laurent Pueyo, Jennifer Patience, Katherine B. Follette, Jean-Baptiste Ruffio, Eric L. Nielsen, Patrick Ingraham, Abhijith Rajan, Anand Sivaramakrishnan, J. Kent Wallace, Mark S. Marley, Li-Wei Hung, Robert J. De Rosa, Megan Ansdell, Pascale Hibon, Rebecca Oppenheimer, Sandrine Thomas, Adam C. Schneider, Lisa Poyneer, Christian Marois, Gaspard Duchene, David Palmer, Dmitry Savransky, Fredrik T. Rantakyrö, Andrew Norton, Stephen J. Goodsell, Maxwell A. Millar-Blanchaer, Schuyler Wolff, Bruce Macintosh, Jeffrey Chilcote, Quinn Konopacky, Jason J. Wang, Julien Rameau, Jonathan Aguilar, James E. Larkin, Joanna Bulger, Tara Cotten, Franck Marchis, Travis Barman, Michael P. Fitzgerald, and Paul Kalas

Subjects
Physics, gaseous planets [planets and satellites], Brown dwarf, Astronomy and Astrophysics, Astrophysics, Astronomy & Astrophysics, Stellar classification, Klip, 01 natural sciences, Low Gravity, Spectral line, 010309 optics, HR 8799 e, 13. Climate action, Space and Planetary Science, Error bar, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, 010303 astronomy & astrophysics, individual [stars], Astronomical and Space Sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

We explore KLIP forward modeling spectral extraction on Gemini Planet Imager coronagraphic data of HR 8799, using PyKLIP and show algorithm stability with varying KLIP parameters. We report new and re-reduced spectrophotometry of HR 8799 c, d, and e in H & K bands. We discuss a strategy for choosing optimal KLIP PSF subtraction parameters by injecting simulated sources and recovering them over a range of parameters. The K1/K2 spectra for HR 8799 c and d are similar to previously published results from the same dataset. We also present a K band spectrum of HR 8799 e for the first time and show that our H-band spectra agree well with previously published spectra from the VLT/SPHERE instrument. We show that HR 8799 c and d show significant differences in their H & K spectra, but do not find any conclusive differences between d and e or c and e, likely due to large error bars in the recovered spectrum of e. Compared to M, L, and T-type field brown dwarfs, all three planets are most consistent with mid and late L spectral types. All objects are consistent with low gravity but a lack of standard spectra for low gravity limit the ability to fit the best spectral type. We discuss how dedicated modeling efforts can better fit HR 8799 planets' near-IR flux and discuss how differences between the properties of these planets can be further explored., Comment: Accepted to AJ, 25 pages, 16 Figures

Published
2018

35. 1–2.4 μm near-IR spectrum of the giant planet β Pictoris b obtained with the gemini planet imager

Author

Andrew Norton, Bruce Macintosh, James E. Larkin, Abhijith Rajan, Zachary H. Draper, James R. Graham, Li-Wei Hung, Quinn Konopacky, Jennifer Patience, Donald T. Gavel, Markus Hartung, Jérôme Maire, Robert J. De Rosa, Rebecca Oppenheimer, Travis Barman, Fredrik T. Rantakyrö, Maxwell A. Millar-Blanchaer, Julien Rameau, Stephen J. Goodsell, Schuyler Wolff, Adam Burrows, Rémi Soummer, Kimberly Ward-Duong, Patrick Ingraham, Katie M. Morzinski, Gaspard Duchene, David Palmer, Andrew Cardwell, Katherine B. Follette, J. Kent Wallace, Michael P. Fitzgerald, Jennifer Dunn, Vanessa P. Bailey, Andrew Serio, Brian J. Bauman, Sandrine Thomas, Dmitry Savransky, Paul Kalas, Leslie Saddlemyer, Adam C. Schneider, Jeffrey Chilcote, Lisa Poyneer, Anand Sivaramakrishnan, Pascale Hibon, Stanimir Metchev, Sebastian Bruzzone, Alexandra Z. Greenbaum, René Doyon, Christine Chen, Joanna Bulger, Inseok Song, Daren Dillon, Jason J. Wang, Tara Cotten, Darren Erikson, Eric L. Nielsen, Naru Sadakuni, Franck Marchis, Mark S. Marley, Jeffrey Vargas, Christian Marois, Sloane Wiktorowicz, Marshall D. Perrin, and Laurent Pueyo

Subjects
010504 meteorology & atmospheric sciences, Brown dwarf, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, adaptive optics [instrumentation], Astronomy & Astrophysics, 01 natural sciences, Luminosity, 0103 physical sciences, Beta Pictoris, Astrophysics::Solar and Stellar Astrophysics, Gemini Planet Imager, planetary systems, 010303 astronomy & astrophysics, individual [stars], Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Giant planet, Astronomy and Astrophysics, Radius, Effective temperature, Surface gravity, 13. Climate action, Space and Planetary Science, astro-ph.EP, spectroscopic [techniques], Astrophysics::Earth and Planetary Astrophysics, Astronomical and Space Sciences
Abstract

Using the Gemini Planet Imager (GPI) located at Gemini South, we measured the near-infrared (1.0-2.4 micron) spectrum of the planetary companion to the nearby, young star $\beta$ Pictoris. We compare the spectrum obtained with currently published model grids and with known substellar objects and present the best matching models as well as the best matching observed objects. Comparing the empirical measurement of the bolometric luminosity to evolutionary models, we find a mass of $12.9\pm0.2$ $\mathcal{M}_\mathrm{Jup}$, an effective temperature of $1724\pm15$ K, a radius of $1.46\pm0.01$ $\mathcal{R}_\mathrm{Jup}$, and a surface gravity of $\log g = 4.18\pm0.01$ [dex] (cgs). The stated uncertainties are statistical errors only, and do not incorporate any uncertainty on the evolutionary models. Using atmospheric models, we find an effective temperature of $1700-1800$ K and a surface gravity of $\log g = 3.5$-$4.0$ [dex] depending upon model. These values agree well with other publications and with "hot-start" predictions from planetary evolution models. Further, we find that the spectrum of $\beta$ Pic b best matches a low-surface gravity L2$\pm$1 brown dwarf. Finally comparing the spectrum to field brown dwarfs we find the the spectrum best matches 2MASS J04062677-381210 and 2MASS J03552337+1133437.

Published
2018

36. Dynamical Constraints on the HR 8799 Planets with GPI

Author

Kimberly Ward-Duong, Gaspard Duchêne, Alexandra Z. Greenbaum, David Palmer, Daniel C. Fabrycky, Jason J. Wang, Jean-Baptiste Ruffio, Robert J. De Rosa, Travis Barman, Franck Marchis, Li Wei Hung, Jeffrey Chilcote, Michael P. Fitzgerald, J. Kent Wallace, Eugene Chiang, Rebekah I. Dawson, Paul Kalas, Stephen J. Goodsell, Julien Rameau, Schuyler Wolff, James E. Larkin, Tara Cotten, Christian Marois, Patrick Ingraham, Jérôme Maire, Sloane J. Wiktorowicz, Pauline Arriaga, Stanimir Metchev, Thomas M. Esposito, Jennifer Patience, Dmitry Savransky, S. Mark Ammons, René Doyon, Laurent Pueyo, Rémi Soummer, Benjamin L. Gerard, Joanna Bulger, Vanessa P. Bailey, Maxwell A. Millar-Blanchaer, Lisa Poyneer, Eric L. Nielsen, Anand Sivaramakrishnan, Rebecca Oppenheimer, Bruce Macintosh, Quinn Konopacky, Katherine B. Follette, Pascale Hibon, Fredrik T. Rantakyrö, Inseok Song, James R. Graham, Sandrine Thomas, Adam C. Schneider, Abhijith Rajan, Marshall D. Perrin, and Mark S. Marley

Subjects
Gemini Observatory, Physics, Earth and Planetary Astrophysics (astro-ph.EP), 010308 nuclear & particles physics, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Astrometry, 01 natural sciences, Space and Planetary Science, Planet, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, National laboratory, 010303 astronomy & astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

The HR 8799 system uniquely harbors four young super-Jupiters whose orbits can provide insights into the system's dynamical history and constrain the masses of the planets themselves. Using the Gemini Planet Imager (GPI), we obtained down to one milliarcsecond precision on the astrometry of these planets. We assessed four-planet orbit models with different levels of constraints and found that assuming the planets are near 1:2:4:8 period commensurabilities, or are coplanar, does not worsen the fit. We added the prior that the planets must have been stable for the age of the system (40 Myr) by running orbit configurations from our posteriors through $N$-body simulations and varying the masses of the planets. We found that only assuming the planets are both coplanar and near 1:2:4:8 period commensurabilities produces dynamically stable orbits in large quantities. Our posterior of stable coplanar orbits tightly constrains the planets' orbits, and we discuss implications for the outermost planet b shaping the debris disk. A four-planet resonance lock is not necessary for stability up to now. However, planet pairs d and e, and c and d, are each likely locked in two-body resonances for stability if their component masses are above $6~M_{\rm{Jup}}$ and $7~M_{\rm{Jup}}$, respectively. Combining the dynamical and luminosity constraints on the masses using hot-start evolutionary models and a system age of $42 \pm 5$~Myr, we found the mass of planet b to be $5.8 \pm 0.5~M_{\rm{Jup}}$, and the masses of planets c, d, and e to be $7.2_{-0.7}^{+0.6}~M_{\rm{Jup}}$ each., 21 pages, 10 figures, accepted to AJ

Published
2018

37. Demonstration of broadband contrast at 1.2 $\lambda$/D and greater for the EXCEDE Starlight Suppression System

Author

Sandrine Thomas, Julien Lozi, Ruslan Belikov, Eduardo Bendek, Troy T. Hix, Dana H. Lynch, Olivier Guyon, Peter T. Zell, Dan Sirbu, Eugene Pluzhnik, and Glenn Schneider

Subjects
Wavefront, Physics, business.industry, Mechanical Engineering, Astronomy and Astrophysics, Wavefront sensor, 01 natural sciences, Deformable mirror, Exoplanet, Electronic, Optical and Magnetic Materials, law.invention, Starlight, 010309 optics, Optics, Apodization, Space and Planetary Science, Control and Systems Engineering, law, 0103 physical sciences, business, Astrophysics - Instrumentation and Methods for Astrophysics, 010303 astronomy & astrophysics, Instrumentation, Coronagraph, Circumstellar habitable zone
Abstract

The EXoplanetary Circumstellar Environments and Disk Explorer (EXCEDE) science mission concept uses a visible-wavelength Phase-Induced Amplitude Apodization (PIAA) coronagraph to enable high-contrast imaging of circumstellar debris systems and some giant planets at angular separations reaching into the habitable zones of some of the nearest stars. We report on the experimental results obtained in the vacuum chamber at the Lockheed Martin Advanced Technology Center in 10% broadband light centered about 650 nm, with a median contrast of $1 \times 10^{-5}$ between 1.2 and 2.0 $\lambda$/D simultaneously with $3 \times 10^{-7}$ contrast between 2 and 11 $\lambda/D$ for a single-sided dark hole using a deformable mirror (DM) upstream of the PIAA coronagraph. These results are stable and repeatable as demonstrated by three measurements runs with DM settings set from scratch and maintained on the best 90% out of the 1000 collected frames. We compare the reduced experimental data with simulation results from modeling observed experimental limits; observed performance is consistent with uncorrected low-order modes not estimated by the Low Order Wavefront Sensor (LOWFS). Modeled sensitivity to bandwidth and residual tip/tilt modes is well-matched to the experiment., Comment: 47 pages (double-spaced), 14 figures

Published
2017

38. Characterizing 51 Eri b from 1 to 5 μm: A Partly Cloudy Exoplanet

Author

Alexandra Z. Greenbaum, Robert J. De Rosa, David Palmer, Rahul Patel, Sandrine Thomas, Adam C. Schneider, David Lafrenière, Paul Kalas, Jean-Baptiste Ruffio, Bruce Macintosh, Gautam Vasisht, Kimberly Ward-Duong, Gaspard Duchene, Mara Johnson-Groh, Inseok Song, Travis Barman, Tara Cotten, Dmitry Savransky, Jonathan J. Fortney, Lisa Poyneer, Quinn Konopacky, Michael P. Fitzgerald, Maxwell A. Millar-Blanchaer, Caroline V. Morley, Ian Czekala, Franck Marchis, Fredrik T. Rantakyrö, Christian Marois, Marshall D. Perrin, Jeffrey Chilcote, James R. Graham, Thomas M. Esposito, Pascale Hibon, Abhijith Rajan, Jason J. Wang, Jennifer Patience, Pauline Arriaga, Patrick Ingraham, Anand Sivaramakrishnan, Didier Saumon, Rebecca Oppenheimer, Julien Rameau, Stanimir Metchev, Jérôme Maire, Sloane J. Wiktorowicz, S. Mark Ammons, René Doyon, Mark S. Marley, Katie M. Morzinski, Stephen J. Goodsell, Schuyler Wolff, Li-Wei Hung, Eric L. Nielsen, Joanna Bulger, Laurent Pueyo, Vanessa P. Bailey, James E. Larkin, Adam Burrows, Rémi Soummer, J. Kent Wallace, and Katherine B. Follette

Subjects
gaseous planets [planets and satellites], 010504 meteorology & atmospheric sciences, Metallicity, Brown dwarf, Astrophysics, adaptive optics [instrumentation], Astronomy & Astrophysics, 01 natural sciences, Photometry (optics), Planet, 0103 physical sciences, Gemini Planet Imager, composition [planets and satellites], 010303 astronomy & astrophysics, individual [stars], 0105 earth and related environmental sciences, Physics, Astronomy and Astrophysics, Effective temperature, atmospheres [planets and satellites], Surface gravity, Exoplanet, 13. Climate action, Space and Planetary Science, individual (51 Eridani) [stars], astro-ph.EP, Astronomical and Space Sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

We present spectro-photometry spanning 1-5 $\mu$m of 51 Eridani b, a 2-10 M$_\text{Jup}$ planet discovered by the Gemini Planet Imager Exoplanet Survey. In this study, we present new $K1$ (1.90-2.19 $\mu$m) and $K2$ (2.10-2.40 $\mu$m) spectra taken with the Gemini Planet Imager as well as an updated $L_P$ (3.76 $\mu$m) and new $M_S$ (4.67 $\mu$m) photometry from the NIRC2 Narrow camera. The new data were combined with $J$ (1.13-1.35 $\mu$m) and $H$ (1.50-1.80 $\mu$m) spectra from the discovery epoch with the goal of better characterizing the planet properties. 51 Eri b photometry is redder than field brown dwarfs as well as known young T-dwarfs with similar spectral type (between T4-T8) and we propose that 51 Eri b might be in the process of undergoing the transition from L-type to T-type. We used two complementary atmosphere model grids including either deep iron/silicate clouds or sulfide/salt clouds in the photosphere, spanning a range of cloud properties, including fully cloudy, cloud free and patchy/intermediate opacity clouds. Model fits suggest that 51 Eri b has an effective temperature ranging between 605-737 K, a solar metallicity, a surface gravity of $\log$(g) = 3.5-4.0 dex, and the atmosphere requires a patchy cloud atmosphere to model the SED. From the model atmospheres, we infer a luminosity for the planet of -5.83 to -5.93 ($\log L/L_{\odot}$), leaving 51 Eri b in the unique position as being one of the only directly imaged planet consistent with having formed via cold-start scenario. Comparisons of the planet SED against warm-start models indicates that the planet luminosity is best reproduced by a planet formed via core accretion with a core mass between 15 and 127 M$_{\oplus}$., Comment: 27 pages, 19 figures, Accepted for publication in The Astronomical Journal

Published
2017

39. Improving and assessing planet sensitivity of the GPI exoplanet survey with a forward model matched filter

Author

Inseok Song, Lisa Poyneer, Stanimir Metchev, Jeffrey Chilcote, Patrick Ingraham, James R. Graham, Gaspard Duchêne, René Doyon, Marshall D. Perrin, Kimberly Ward-Duong, Sandrine Thomas, Bruce Macintosh, Jason J. Wang, Adam C. Schneider, Abhijith Rajan, James E. Larkin, Jean-Baptiste Ruffio, Anand Sivaramakrishnan, Maxwell A. Millar-Blanchaer, Franck Marchis, Mark S. Marley, Quinn Konopacky, Jérôme Maire, Sloane J. Wiktorowicz, Julien Rameau, Robert J. De Rosa, Fredrik T. Rantakyrö, Laurent Pueyo, Jennifer Patience, Dmitry Savransky, Stephen J. Goodsell, Schuyler Wolff, Pascale Hibon, J. Kent Wallace, Katie M. Morzinski, Katherine B. Follette, Tara Cotten, Li-Wei Hung, Rebecca Oppenheimer, Ian Czekala, Alexandra Z. Greenbaum, Christian Marois, David Palmer, Eric L. Nielsen, Pauline Arriaga, Paul Kalas, Rémi Soummer, Vanessa P. Bailey, Travis Barman, Benjamin L. Gerard, Joanna Bulger, and Michael P. Fitzgerald

Subjects
Point spread function, Computer science, statistical [methods], FOS: Physical sciences, Image processing, adaptive optics [instrumentation], Astronomy & Astrophysics, Physical Chemistry, Atomic, 01 natural sciences, 010309 optics, Particle and Plasma Physics, surveys, Distortion, 0103 physical sciences, False positive paradox, Nuclear, Gemini Planet Imager, Instrumentation and Methods for Astrophysics (astro-ph.IM), planetary systems, 010303 astronomy & astrophysics, Earth and Planetary Astrophysics (astro-ph.EP), image processing [techniques], Matched filter, high angular resolution [techniques], Astrophysics::Instrumentation and Methods for Astrophysics, Molecular, Astronomy and Astrophysics, Exoplanet, Space and Planetary Science, False positive rate, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Algorithm, Astronomical and Space Sciences, Astrophysics - Earth and Planetary Astrophysics, Physical Chemistry (incl. Structural)
Abstract

We present a new matched filter algorithm for direct detection of point sources in the immediate vicinity of bright stars. The stellar Point Spread Function (PSF) is first subtracted using a Karhunen-Lo\'eve Image Processing (KLIP) algorithm with Angular and Spectral Differential Imaging (ADI and SDI). The KLIP-induced distortion of the astrophysical signal is included in the matched filter template by computing a forward model of the PSF at every position in the image. To optimize the performance of the algorithm, we conduct extensive planet injection and recovery tests and tune the exoplanet spectra template and KLIP reduction aggressiveness to maximize the Signal-to-Noise Ratio (SNR) of the recovered planets. We show that only two spectral templates are necessary to recover any young Jovian exoplanets with minimal SNR loss. We also developed a complete pipeline for the automated detection of point source candidates, the calculation of Receiver Operating Characteristics (ROC), false positives based contrast curves, and completeness contours. We process in a uniform manner more than 330 datasets from the Gemini Planet Imager Exoplanet Survey (GPIES) and assess GPI typical sensitivity as a function of the star and the hypothetical companion spectral type. This work allows for the first time a comparison of different detection algorithms at a survey scale accounting for both planet completeness and false positive rate. We show that the new forward model matched filter allows the detection of $50\%$ fainter objects than a conventional cross-correlation technique with a Gaussian PSF template for the same false positive rate., Comment: ApJ accepted

Published
2017

40. An optical/near-infrared investigation of HD 100546 b with the Gemini Planet Imager and MagAO

Author

Michael P. Fitzgerald, Paul Kalas, Inseok Song, David Vega, James R. Graham, Thomas M. Esposito, Robert J. De Rosa, Julien Rameau, Jeffrey Chilcote, Stephen J. Goodsell, Schuyler Wolff, Laurent Pueyo, Vanessa P. Bailey, Maxwell A. Millar-Blanchaer, Bruce Macintosh, Jennifer Patience, Lisa Poyneer, Alexandra Z. Greenbaum, J. Kent Wallace, Jean-Baptiste Ruffio, Marshall D. Perrin, David Palmer, James E. Larkin, Patrick Ingraham, Li-Wei Hung, Quinn Konopacky, Jared R. Males, Stanimir Metchev, Abhijith Rajan, Pascale Hibon, René Doyon, Katherine B. Follette, Joanna Bulger, S. M. Ammons, Jérôme Maire, Dmitry Savransky, Katie M. Morzinski, Christian Marois, Laird M. Close, Kimberly Ward-Duong, Gaspard Duchene, Rebecca Oppenheimer, Sandrine Thomas, Adam C. Schneider, Fredrik T. Rantakyrö, Anand Sivaramakrishnan, Sloane J. Wiktorowicz, Rémi Soummer, Eric L. Nielsen, Franck Marchis, Tara Cotten, Mark S. Marley, Jason J. Wang, David Lafrenière, and Travis Barman

Subjects
010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Extinction (astronomy), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, adaptive optics [instrumentation], Astronomy & Astrophysics, Protoplanetary disk, 01 natural sciences, Spectral line, Luminosity, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, planetary systems, individual [stars], Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Photosphere, planet-disk interactions, Astronomy and Astrophysics, Effective temperature, Accretion (astrophysics), 13. Climate action, Space and Planetary Science, astro-ph.EP, Astrophysics::Earth and Planetary Astrophysics, Protoplanet, Astronomical and Space Sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

We present H band spectroscopic and Halpha photometric observations of HD 100546 obtained with GPI and MagAO. We detect H band emission at the location of the protoplanet HD 100546b, but show that choice of data processing parameters strongly affects the morphology of this source. It appears point-like in some aggressive reductions, but rejoins an extended disk structure in the majority of the others. Furthermore, we demonstrate that this emission appears stationary on a timescale of 4.6 yrs, inconsistent at the 2sigma level with a Keplerian clockwise orbit at 59 au in the disk plane. The H band spectrum of the emission is inconsistent with any type of low effective temperature object or accreting protoplanetary disk. It strongly suggests a scattered light origin, as it is consistent with the spectrum of the star and the spectra extracted at other locations in the disk. A non detection at the 5sigma level of HD 100546b in differential Halpha imaging places an upper limit, assuming the protoplanet lies in a gap free of extinction, on the accretion luminosity and accretion rate of 1.7E-4 Lsun and MMdot, Accepted to AJ, 10 pages, 6 figures, 1 table

Published
2017

41. Complex spiral structure in the HD 100546 transitional disk as revealed by GPI and MagAO

Author

James R. Graham, Dmitry Savransky, Ruobing Dong, Li-Wei Hung, Travis Barman, J. Kent Wallace, Patrick Ingraham, Anand Sivaramakrishnan, Jason J. Wang, Laurent Pueyo, Clare Leonard, Jared R. Males, Pascale Hibon, Stanimir Metchev, Rémi Soummer, Jeffrey Chilcote, Christian Marois, Franck Marchis, S. Mark Ammons, René Doyon, Elijah Spiro, Alexandra Z. Greenbaum, Jeffrey Fung, David Palmer, Michael P. Fitzgerald, Fredrik T. Rantakyrö, Maxwell A. Millar-Blanchaer, Katie M. Morzinski, Lisa Poyneer, Stephen J. Goodsell, Schuyler Wolff, David Vega, Katherine B. Follette, Paul Kalas, Julien Rameau, Joanna Bulger, Jennifer Patience, Tara Cotten, Rebecca Oppenheimer, Laird M. Close, James E. Larkin, Sandrine Thomas, Adam C. Schneider, Kimberly Ward-Duong, Vanessa P. Bailey, Sloane J. Wiktorowicz, Gaspard Duchêne, Jérôme Maire, Marshall D. Perrin, Wyatt Mullen, Abhijith Rajan, Robert J. De Rosa, Eric L. Nielsen, Bruce Macintosh, Quinn Konopacky, and Inseok Song

Subjects
protoplanetary disk, FOS: Physical sciences, Astrophysics, adaptive optics [instrumentation], Astronomy & Astrophysics, Rotation, 01 natural sciences, 010309 optics, planet-disk interaction, 0103 physical sciences, Gemini Planet Imager, Projection (set theory), Adaptive optics, 010303 astronomy & astrophysics, Spiral, individual [stars], Astrophysics::Galaxy Astrophysics, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Spiral galaxy, Astronomy and Astrophysics, Wavelength, Space and Planetary Science, astro-ph.EP, Substructure, Astrophysics::Earth and Planetary Astrophysics, Astronomical and Space Sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

We present optical and near-infrared high contrast images of the transitional disk HD 100546 taken with the Magellan Adaptive Optics system (MagAO) and the Gemini Planet Imager (GPI). GPI data include both polarized intensity and total intensity imagery, and MagAO data are taken in Simultaneous Differential Imaging mode at H{\alpha}. The new GPI H -band total intensity data represent a significant enhancement in sensitivity and field rotation compared to previous data sets and enable a detailed exploration of substructure in the disk. The data are processed with a variety of differential imaging techniques (polarized, angular, reference, and simultaneous differential imaging) in an attempt to identify the disk structures that are most consistent across wavelengths, processing techniques, and algorithmic parameters. The inner disk cavity at 15 au is clearly resolved in multiple datasets, as are a variety of spiral features. While the cavity and spiral structures are identified at levels significantly distinct from the neighboring regions of the disk under several algorithms and with a range of algorithmic parameters, emission at the location of HD 100546 c varies from point-like under aggressive algorithmic parameters to a smooth continuous structure with conservative parameters, and is consistent with disk emission. Features identified in the HD100546 disk bear qualitative similarity to computational models of a moderately inclined two-armed spiral disk, where projection effects and wrapping of the spiral arms around the star result in a number of truncated spiral features in forward-modeled images., Comment: accepted to AJ

Published
2017

42. Techniques for High-Contrast Imaging in Multi-Star Systems II: Multi-Star Wavefront Control

Author

Ruslan Belikov, Eduardo Bendek, Dan Sirbu, and Sandrine Thomas

Subjects
Physics, Wavefront, Angular distance, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Planetary system, 01 natural sciences, Exoplanet, Deformable mirror, 010309 optics, Stars, Cardinal point, Optics, Space and Planetary Science, 0103 physical sciences, Alpha Centauri, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, business, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics
Abstract

Direct imaging of exoplanets represents a challenge for astronomical instrumentation due to the high-contrast ratio and small angular separation between the host star and the faint planet. Multi-star systems pose additional challenges for coronagraphic instruments due to the diffraction and aberration leakage caused by companion stars. Consequently, many scientifically valuable multi-star systems are excluded from direct imaging target lists for exoplanet surveys and characterization missions. Multi-star wavefront control (MSWC) is a technique that uses a coronagraphic instrument's deformable mirror (DM) to create high-contrast regions in the focal plane in the presence of multiple stars. Our previous paper introduced the Super-Nyquist Wavefront Control (SNWC) technique that uses a diffraction grating to enable the DM to generate high-contrast regions beyond the nominal region correctable by the DM. These two techniques can be combined to generate high-contrast regions for multi-star systems at any angular separation. As a case study, a high-contrast wavefront control (WC) simulation that applies these techniques shows that the habitable region of the Alpha Centauri system can be imaged reaching at least $8 \times 10^{-9}$ mean contrast in 10\% broadband light in one-sided dark holes from 1.6-5.5$\lambda/D$., Comment: 17 pages, 8 figures, 4 tables; Submitted to ApJ; updated Table 1 and author information

Published
2017

43. Integral Field Spectroscopy of the Low-mass Companion HD 984 B with the Gemini Planet Imager

Author

Bruce Macintosh, Anand Sivaramakrishnan, Katherine B. Follette, Maxwell A. Millar-Blanchaer, Rebecca Oppenheimer, Kimberly Ward-Duong, Gaspard Duchene, Quinn Konopacky, Jeffrey Chilcote, Alexandra Z. Greenbaum, Abhijith Rajan, James E. Larkin, James R. Graham, Li-Wei Hung, Travis Barman, Fredrik T. Rantakyrö, Stanimir Metchev, Stephen J. Goodsell, Schuyler Wolff, Rémi Soummer, S. Mark Ammons, Patrick Ingraham, Robert J. De Rosa, Joanna Bulger, David Vega, René Doyon, Julien Rameau, Marshall D. Perrin, Jérôme Maire, Mara Johnson-Groh, Michael P. Fitzgerald, Sandrine Thomas, Adam C. Schneider, Dmitry Savransky, Paul Kalas, David W. Palmer, Lisa Poyneer, Vanessa P. Bailey, Pascale Hibon, Sarah Blunt, Laurent Pueyo, Inseok Song, Jason J. Wang, Tara Cotten, Jeffrey Vargas, Mark S. Marley, Christian Marois, Eric L. Nielsen, Franck Marchis, Jenny Patience, Sloane J. Wiktorowicz, and J. Kent Wallace

Subjects
Brown dwarf, FOS: Physical sciences, Astrophysics, Astronomy & Astrophysics, Stellar classification, 01 natural sciences, Spectral line, 010309 optics, Photometry (optics), 0103 physical sciences, Gemini Planet Imager, planetary systems, 010303 astronomy & astrophysics, individual [stars], Earth and Planetary Astrophysics (astro-ph.EP), Physics, Astronomy and Astrophysics, Covariance, Exoplanet, 13. Climate action, Space and Planetary Science, astro-ph.EP, individual (HD 984) [stars], Low Mass, Astronomical and Space Sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

We present new observations of the low-mass companion to HD 984 taken with the Gemini Planet Imager as a part of the Gemini Planet Imager Exoplanet Survey campaign. Images of HD 984 B were obtained in the J (1.12--1.3 micron) and H (1.50--1.80 micron) bands. Combined with archival epochs from 2012 and 2014, we fit the first orbit to the companion to find an 18 AU (70 year) orbit with a 68% confidence interval between 14 and 28 AU, an eccentricity of 0.18 with a 68% confidence interval between 0.05 and 0.47, and an inclination of 119 degrees with a 68% confidence interval between 114 degrees and 125 degrees. To address considerable spectral covariance in both spectra, we present a method of splitting the spectra into low and high frequencies to analyze the spectral structure at different spatial frequencies with the proper spectral noise correlation. Using the split spectra, we compare to known spectral types using field brown dwarf and low-mass star spectra and find a best fit match of a field gravity M6.5+/-1.5 spectral type with a corresponding temperature of 2730+120 K. Photometry of the companion yields a luminosity of log(L_bol/L_sun) = -2.88+/-0.07 dex, using DUSTY models. Mass estimates, again from DUSTY models, find an age-dependent mass of 34+/-1 to 95+/-4 M_Jup. These results are consistent with previous measurements of the object., Comment: Accepted for publication in The Astronomical Journal

Published
2017

44. Evidence That the Directly Imaged Planet HD 131399 Ab Is a Background Star

Author

Jean-Baptiste Ruffio, Étienne Artigau, Sloane J. Wiktorowicz, Patrick Ingraham, Kimberly Ward-Duong, Robert J. De Rosa, Daniel C. Fabrycky, Stanimir Metchev, Alexandra Z. Greenbaum, S. Mark Ammons, René Doyon, David Palmer, Katherine B. Follette, Jeffrey Chilcote, Jennifer Patience, Michael P. Fitzgerald, Bruce Macintosh, Tara Cotten, Maxwell A. Millar-Blanchaer, Stephen J. Goodsell, Schuyler Wolff, Julien Rameau, J. Kent Wallace, Lisa Poyneer, Dmitry Savransky, Roman R. Rafikov, Laurent Pueyo, Anand Sivaramakrishnan, Quinn Konopacky, Arthur Vigan, Li-Wei Hung, James E. Larkin, Paul Kalas, Fredrik T. Rantakyrö, Abhijith Rajan, Sasha Hinkley, Sandrine Thomas, Joanna Bulger, Eric L. Nielsen, Thomas M. Esposito, Adam C. Schneider, Jérôme Maire, Vanessa P. Bailey, Rémi Soummer, Ruth Murray-Clay, Rebecca Oppenheimer, Christian Marois, Gaspard Duchêne, Marshall D. Perrin, Rebecca Jensen-Clem, Sarah Blunt, Katie M. Morzinski, Pascale Hibon, Inseok Song, James R. Graham, Benjamin L. Gerard, Jason J. Wang, Franck Marchis, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), and Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)

Subjects
astro-ph.SR, detection [planets and satellites], FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, adaptive optics [instrumentation], Astronomy & Astrophysics, 01 natural sciences, 010309 optics, Spitzer Space Telescope, Planet, 0103 physical sciences, Coordination network, Astrophysics::Solar and Stellar Astrophysics, European commission, 010303 astronomy & astrophysics, individual [stars], Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Physics, Earth and Planetary Astrophysics (astro-ph.EP), image processing [techniques], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astronomy, Astronomy and Astrophysics, Astrometry, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, astro-ph.EP, astrometry, spectroscopic [techniques], Astrophysics::Earth and Planetary Astrophysics, National laboratory, Astronomical and Space Sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

We present evidence that the recently discovered, directly-imaged planet HD 131399 Ab is a background star with non-zero proper motion. From new JHK1L' photometry and spectroscopy obtained with the Gemini Planet Imager, VLT/SPHERE, and Keck/NIRC2, and a reanalysis of the discovery data obtained with VLT/SPHERE, we derive colors, spectra, and astrometry for HD 131399 Ab. The broader wavelength coverage and higher data quality allow us to re-investigate its status. Its near-infrared spectral energy distribution excludes spectral types later than L0 and is consistent with a K or M dwarf, which are the most likely candidates for a background object in this direction at the apparent magnitude observed. If it were a physically associated object, the projected velocity of HD 131399 Ab would exceed escape velocity given the mass and distance to HD 131399 A. We show that HD 131399 Ab is also not following the expected track for a stationary background star at infinite distance. Solving for the proper motion and parallax required to explain the relative motion of HD 131399 Ab, we find a proper motion of 12.3 mas/yr. When compared to predicted background objects drawn from a galactic model, we find this proper motion to be high, but consistent with the top 4% fastest-moving background stars. From our analysis we conclude that HD 131399 Ab is a background K or M dwarf., 35 pages, 20 figures, Published in AJ

Published
2017

46. DYNAMICAL MASS MEASUREMENT of the YOUNG SPECTROSCOPIC BINARY V343 NORMAE AaAb RESOLVED with the GEMINI PLANET IMAGER

Author

Abhijith Rajan, Li-Wei Hung, Pascale Hibon, Dmitry Savransky, Alexandra Z. Greenbaum, Inseok Song, Katherine B. Follette, James R. Graham, Christian Marois, Franck Marchis, Paul Kalas, Sandrine Thomas, Jason J. Wang, Adam C. Schneider, Julien Rameau, Bruce Macintosh, Anand Sivaramakrishnan, Travis Barman, J. Kent Wallace, David Palmer, Jennifer Patience, Gaspard Duchêne, Laurent Pueyo, James E. Larkin, Kimberly Ward-Duong, Quinn Konopacky, Mark Ammons, Marshall D. Perrin, Mark S. Marley, Rémi Soummer, Michael P. Fitzgerald, Stanimir Metchev, Joanna Bulger, Jeffrey Chilcote, René Doyon, Vanessa P. Bailey, Rebecca Oppenheimer, Maxwell A. Millar-Blanchaer, Tara Cotten, Robert J. De Rosa, Eric L. Nielsen, Lisa Poyneer, Patrick Ingraham, Fredrik T. Rantakyrö, Schuyler Wolff, Sloane J. Wiktorowicz, and Jérôme Maire

Subjects
Physics, astro-ph.SR, detection [planets and satellites], Spatially resolved, FOS: Physical sciences, Binary number, Astronomy and Astrophysics, Astrometry, Astrophysics, Astronomy & Astrophysics, 01 natural sciences, Mass measurement, Star system, 010309 optics, Photometry (optics), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, individual (V343 Nor) [stars], 0103 physical sciences, Gemini Planet Imager, Beta Pictoris moving group, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), individual [stars], Astronomical and Space Sciences
Abstract

We present new spatially resolved astrometry and photometry from the Gemini Planet Imager of the inner binary of the young multiple star system V343 Normae, which is a member of the beta Pictoris moving group. V343 Normae comprises a K0 and mid-M star in a ~4.5 year orbit (AaAb) and a wide 10" M5 companion (B). By combining these data with archival astrometry and radial velocities we fit the orbit and measure individual masses for both components of M_Aa = 1.10 +/- 0.10 M_sun and M_Ab = 0.290 +/- 0.018 M_sun. Comparing to theoretical isochrones, we find good agreement for the measured masses and JHK band magnitudes of the two components consistent with the age of the beta Pic moving group. We derive a model-dependent age for the beta Pic moving group of 26 +/- 3 Myr by combining our results for V343 Normae with literature measurements for GJ 3305, which is another group member with resolved binary components and dynamical masses., Comment: 12 pages, 7 figures. Accepted to AJ

Published
2016

47. Imaging an 80 au radius dust ring around the F5V star HD 157587

Author

Schuyler Wolff, Sandrine Thomas, Maxwell A. Millar-Blanchaer, Adam C. Schneider, Abhijith Rajan, Christian Marois, Inseok Song, Lisa Poyneer, Laurent Pueyo, Deborah Padgett, Stanimir Metchev, Jeffrey Chilcote, S. Mark Ammons, René Doyon, Fredrik T. Rantakyrö, James R. Graham, Joanna Bulger, Dmitry Savransky, Bruce Macintosh, Jason J. Wang, Anand Sivaramakrishnan, Jennifer Patience, Li-Wei Hung, Robert J. De Rosa, Franck Marchis, Patrick Ingraham, Brenda C. Matthews, Sebastian Bruzzone, Quinn Konopacky, Eric L. Nielsen, Vanessa P. Bailey, J. Kent Wallace, James E. Larkin, Kimberly Ward-Duong, Thomas M. Esposito, Tara Cotten, Pascale Hibon, Christine Chen, Mark S. Marley, Katherine B. Follette, Rémi Soummer, David Vega, Alexandra Z. Greenbaum, Julien Rameau, David Palmer, Benjamin L. Gerard, Zachary H. Draper, Jérôme Maire, Gaspard Duchêne, Marshall D. Perrin, Dae-Sik Moon, Sloane J. Wiktorowicz, Travis Barman, Michael P. Fitzgerald, Paul Kalas, Sasha Hinkley, Mara Johnson-Groh, and Rebecca Oppenheimer

Subjects
010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Star (graph theory), Astronomy & Astrophysics, Ring (chemistry), 01 natural sciences, 0103 physical sciences, polarimetric [techniques], Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, individual [stars], 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, planet-disk interactions, Astronomy and Astrophysics, Radius, Space and Planetary Science, astro-ph.EP, Astrophysics::Earth and Planetary Astrophysics, National laboratory, Astronomical and Space Sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

We present $H$-band near-infrared polarimetric imaging observations of the F5V star HD~157587 obtained with the Gemini Planet Imager (GPI) that reveal the debris disk as a bright ring structure at a separation of $\sim$80$-$100~AU. The new GPI data complement recent HST/STIS observations that show the disk extending out to over 500~AU. The GPI image displays a strong asymmetry along the projected minor axis as well as a fainter asymmetry along the projected major axis. We associate the minor and major axis asymmetries with polarized forward scattering and a possible stellocentric offset, respectively. To constrain the disk geometry we fit two separate disk models to the polarized image, each using a different scattering phase function. Both models favor a disk inclination of $\sim 70\degr$ and a $1.5\pm0.6$ AU stellar offset in the plane of the sky along the projected major axis of the disk. We find that the stellar offset in the disk plane, perpendicular to the projected major axis is degenerate with the form of the scattering phase function and remains poorly constrained. The disk is not recovered in total intensity due in part to strong adaptive optics residuals, but we recover three point sources. Considering the system's proximity to the galactic plane and the point sources' positions relative to the disk, we consider it likely that they are background objects and unrelated to the disk's offset from the star., Comment: Updated with proper references

Published
2016

48. DISCOVERY of A SUBSTELLAR COMPANION to the NEARBY DEBRIS DISK HOST HR 2562

Author

Inseok Song, James R. Graham, Paige A. Giorla Godfrey, Paul Kalas, Anand Sivaramakrishnan, Travis Barman, David Lafrenière, Michael P. Fitzgerald, Dmitry Savransky, Bruce Macintosh, Tara Cotten, Joseph C. Filippazzo, Jason J. Wang, Patrick Ingraham, Sloane J. Wiktorowicz, Gaspard Duchêne, Julien Rameau, Marshall D. Perrin, Quinn Konopacky, Mark S. Marley, Fredrik T. Rantakyrö, Kimberly Ward-Duong, Jennifer Patience, Abhijith Rajan, David Palmer, Sandrine Thomas, Stephen J. Goodsell, Schuyler Wolff, Adam C. Schneider, Roman R. Rafikov, Lisa Poyneer, Rebecca Oppenheimer, Robert J. De Rosa, Emily L. Rice, J. Kent Wallace, Eric L. Nielsen, Katherine B. Follette, James E. Larkin, Pascale Hibon, Jérôme Maire, Rémi Soummer, Joanna Bulger, Laurent Pueyo, Alexandra Z. Greenbaum, Li-Wei Hung, Rebekah I. Dawson, Christian Marois, Vanessa P. Bailey, Maxwell A. Millar-Blanchaer, Stanimir Metchev, Sebastian Bruzzone, S. Mark Ammons, René Doyon, Franck Marchis, Jeffrey Chilcote, Brenda C. Matthews, and Thomas M. Esposito

Subjects
Physics, Earth and Planetary Astrophysics (astro-ph.EP), Debris disk, planet-disk interactions, astro-ph.SR, Brown dwarf, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, individual (HR 2562) [stars], adaptive optics [instrumentation], Astronomy & Astrophysics, 01 natural sciences, 010309 optics, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, 0103 physical sciences, astro-ph.EP, 010303 astronomy & astrophysics, Host (network), Solar and Stellar Astrophysics (astro-ph.SR), individual [stars], Astronomical and Space Sciences, Astrophysics - Earth and Planetary Astrophysics, brown dwarfs
Abstract

We present the discovery of a brown dwarf companion to the debris disk host star HR 2562. This object, discovered with the Gemini Planet Imager (GPI), has a projected separation of 20.3$\pm$0.3 au (0.618$\pm$0.004") from the star. With the high astrometric precision afforded by GPI, we have confirmed common proper motion of HR 2562B with the star with only a month time baseline between observations to more than $5\sigma$. Spectral data in $J$, $H$, and $K$ bands show morphological similarity to L/T transition objects. We assign a spectral type of L7$\pm$3 to HR 2562B, and derive a luminosity of $\log$(L$_{\rm bol}$/L$_{\odot}$)=-4.62$\pm$0.12, corresponding to a mass of 30$\pm$15 M$_{\rm Jup}$ from evolutionary models at an estimated age of the system of 300-900 Myr. Although the uncertainty in the age of the host star is significant, the spectra and photometry exhibit several indications of youth for HR 2562B. The source has a position angle consistent with an orbit in the same plane as the debris disk recently resolved with Herschel. Additionally, it appears to be interior to the debris disk. Though the extent of the inner hole is currently too uncertain to place limits on the mass of HR 2562B, future observations of the disk with higher spatial resolution may be able to provide mass constraints. This is the first brown dwarf-mass object found to reside in the inner hole of a debris disk, offering the opportunity to search for evidence of formation above the deuterium burning limit in a circumstellar disk., Comment: 10 pages, 4 figures. Accepted for publication in ApJ Letters

Published
2016

49. Using model based systems engineering for the development of the Large Synoptic Survey Telescope's operational plan

Author

M. W. G. Johnson, Ben Emmons, Sandrine Thomas, Don Petravick, Kevin Reil, Charles F. Claver, German Schumacher, Kian Tat Lim, S. L. Marshall, Brian M. Selvy, Tim Jenness, Beth Willman, Tim Axelrod, Suzanne Jacoby, and Paul J. Lotz

Subjects
Computer science, Model-based systems engineering, Stakeholder, Enterprise architecture, 02 engineering and technology, Activity diagram, Spiral model, Systems modeling, 021001 nanoscience & nanotechnology, 01 natural sciences, Concept of operations, 010309 optics, Systems Modeling Language, 0103 physical sciences, Systems engineering, Use case, Organizational structure, 0210 nano-technology, Simulation
Abstract

We† provide an overview of the Model Based Systems Engineering (MBSE) language, tool, and methodology being used in our development of the Operational Plan for Large Synoptic Survey Telescope (LSST) operations. LSST’s Systems Engineering (SE) team is using a model-based approach to operational plan development to: 1) capture the topdown stakeholders’ needs and functional allocations defining the scope, required tasks, and personnel needed for operations, and 2) capture the bottom-up operations and maintenance activities required to conduct the LSST survey across its distributed operations sites for the full ten year survey duration. To accomplish these complimentary goals and ensure that they result in self-consistent results, we have developed a holistic approach using the Sparx Enterprise Architect modeling tool and Systems Modeling Language (SysML). This approach utilizes SysML Use Cases, Actors, associated relationships, and Activity Diagrams to document and refine all of the major operations and maintenance activities that will be required to successfully operate the observatory and meet stakeholder expectations. We have developed several customized extensions of the SysML language including the creation of a custom stereotyped Use Case element with unique tagged values, as well as unique association connectors and Actor stereotypes. We demonstrate this customized MBSE methodology enables us to define: 1) the rolls each human Actor must take on to successfully carry out the activities associated with the Use Cases; 2) the skills each Actor must possess; 3) the functional allocation of all required stakeholder activities and Use Cases to organizational entities tasked with carrying them out; and 4) the organization structure required to successfully execute the operational survey. Our approach allows for continual refinement utilizing the systems engineering spiral method to expose finer levels of detail as necessary. For example, the bottom-up, Use Case-driven approach will be deployed in the future to develop the detailed work procedures required to successfully execute each operational activity.

Published
2016

50. Large Synoptic Survey Telescope mount final design

Author

Paul J. Lotz, William J. Gressler, Ricardo Moreno Rodríguez, Michael Warner, Francisco Javier Molina Romero, Alfredo Orden Martinez, Chuck Claver, Shawn P. Callahan, John Andrew, Bill Schoening, Jacques Sebag, Ismael Ruiz de Argandoña, Ed Hileman, Victor L. Krabbendam, Constanza Araujo, Sandrine Thomas, J. Barr, D. Neill, Oliver Wiecha, German Schumacher, Chuck Gessner, Marco Venturini, Gary Muller, Luis García-Marchena, George Z. Angeli, Manuel Perezagua Aguado, and José Carlos Delgado González

Subjects
Engineering, business.industry, Elevation, 02 engineering and technology, Large Synoptic Survey Telescope, 021001 nanoscience & nanotechnology, 01 natural sciences, Mount, law.invention, 010309 optics, Telescope, law, 0103 physical sciences, Telescope mount, 0210 nano-technology, business, Remote sensing
Abstract

This paper describes the status and details of the large synoptic survey telescope 1,2,3 mount assembly (TMA). On June 9 th , 2014 the contract for the design and build of the large synoptic survey telescope mount assembly (TMA) was awarded to GHESA Ingenieria y Tecnologia, S.A. and Asturfeito, S.A. The design successfully passed the preliminary design review on October 2, 2015 and the final design revi ew January 29, 2016. This paper describes the detailed design by subsystem, analytical model results, preparations being ta ken to complete the fabrication, and the transportation and installation plans to install the mount on Cerro Pachon in Chile. This large project is the culmination of work by many people and the authors would like to thank everyone that has contributed to th e success of this project. Keywords: LSST, telescope, mount, elevation, azimuth, linear drives, tape encoders, 1. INTRODUCTION The Large Synoptic Survey Telescope (LSST) is an 8.4-mete r wide-field (3.5-degree) survey telescope, which will be located on the summit of Cerro Pachon in Chile. The design of the telescope mount assembly is by GHESA Ingenieria y Tecnologia, S.A. Asturfeito, S.A, is fabricating the TMA in northern Spain is shall reinstall the mount on Cerro Pachon. The design of the mount control, camera cable wrap, and mirror covers is by IK4 Tekniker. The design and fabrication of the azimuth and elevation li near drives and capacitor bank is by Phase Motion Control. This telescope mount assembly supports the optics, camera, baffles, and the integral subsystems required to operate the telescope. This report provides an overview of the final design of the mount and all supporting subsystems.

Published
2016

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