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1. A Uniform Analysis of Debris Disks with the Gemini Planet Imager. I. An Empirical Search for Perturbations from Planetary Companions in Polarized Light Images

Author

Katie A. Crotts, Brenda C. Matthews, Gaspard Duchêne, Thomas M. Esposito, Ruobing Dong, Justin Hom, Rebecca Oppenheimer, Malena Rice, Schuyler G. Wolff, Christine H. Chen, Clarissa R. Do Ó, Paul Kalas, Briley L. Lewis, Alycia J. Weinberger, David J. Wilner, Mark Ammons, Pauline Arriaga, Robert J. De Rosa, John H. Debes, Michael P. Fitzgerald, Eileen C. Gonzales, Dean C. Hines, Sasha Hinkley, A. Meredith Hughes, Ludmilla Kolokolova, Eve J. Lee, Ronald A. López, Bruce Macintosh, Johan Mazoyer, Stanimir Metchev, Maxwell A. Millar-Blanchaer, Eric L. Nielsen, Jenny Patience, Marshall D. Perrin, Laurent Pueyo, Fredrik T. Rantakyrö, Bin B. Ren, Glenn Schneider, Remi Soummer, and Christopher C. Stark

Subjects
Debris disks, Circumstellar disks, Exoplanets, Planetary-disk interactions, Near infrared astronomy, Astrophysics, QB460-466
Abstract

The Gemini Planet Imager (GPI) has excelled in imaging debris disks in the near-infrared. The GPI Exoplanet Survey imaged 24 debris disks in polarized H -band light, while other programs observed half of these disks in polarized J and/or K 1 bands. Using these data, we present a uniform analysis of the morphology of each disk to find asymmetries suggestive of perturbations, particularly those due to planet–disk interactions. The multiwavelength surface brightness, disk color, and geometry permit the identification of any asymmetries such as warps or disk offsets from the central star. We find that 19 of the disks in this sample exhibit asymmetries in surface brightness, disk color, disk geometry, or a combination of the three, suggesting that for this sample, perturbations, as seen in scattered light, are common. The relationship between these perturbations and potential planets in the system is discussed. We also explore correlations among stellar temperatures, ages, disk properties, and observed perturbations. We find significant trends between the vertical aspect ratio and the stellar temperature, disk radial extent, and the dust grain size distribution power law, q . We also confirm a trend between the disk color and stellar effective temperature, where the disk becomes increasingly red/neutral with increasing temperature. Such results have important implications for the evolution of debris disk systems around stars of various spectral types.

Published
2024
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2. Improving and Assessing Planet Sensitivity of the GPI Exoplanet Survey with a Forward Model Matched Filter

Author

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

Subjects
instrumentation: adaptive optics, methods: statistical, planetary systems, surveys, techniques: high angular resolution, techniques: image processing, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
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-Loéve 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 (S/N) of the recovered planets. We show that only two spectral templates are necessary to recover any young Jovian exoplanets with minimal S/N loss. We also developed a complete pipeline for the automated detection of point-source candidates, the calculation of receiver operating characteristics (ROC), contrast curves based on false positives, and completeness contours. We process in a uniform manner more than 330 data sets from the Gemini Planet Imager Exoplanet Survey 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.

Published
2017

3. THE PECULIAR DEBRIS DISK OF HD 111520 AS RESOLVED BY THE GEMINI PLANET IMAGER

Author

Draper, Zachary H, Duchêne, Gaspard, Millar-Blanchaer, Maxwell A, Matthews, Brenda C, Wang, Jason J, Kalas, Paul, Graham, James R, Padgett, Deborah, Ammons, S Mark, Bulger, Joanna, Chen, Christine, Chilcote, Jeffrey K, Doyon, René, Fitzgerald, Michael P, Follette, Kate B, Gerard, Benjamin, Greenbaum, Alexandra Z, Hibon, Pascale, Hinkley, Sasha, Macintosh, Bruce, Ingraham, Patrick, Lafrenière, David, Marchis, Franck, Marois, Christian, Nielsen, Eric L, Oppenheimer, Rebecca, Patel, Rahul, Patience, Jenny, Perrin, Marshall, Pueyo, Laurent, Rajan, Abhijith, Rameau, Julien, Sivaramakrishnan, Anand, Vega, David, Ward-Duong, Kimberly, and Wolff, Schuyler G

Subjects
circumstellar matter, stars: individual, astro-ph.EP, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract

Using the Gemini Planet Imager, we have resolved the circumstellar debris disk around HD 111520 at a projected range of ∼30-100 AU in both total and polarized H-band intensity. The disk is seen edge-on at a position angle of 165° along the spine of emission. A slight inclination and asymmetric warp are covariant and alter the interpretation of the observed disk emission. We employ three point-spread function subtraction methods to reduce the stellar glare and instrumental artifacts to confirm that there is a roughly 2:1 brightness asymmetry between the NW and SE extension. This specific feature makes HD 111520 the most extreme example of asymmetric debris disks observed in scattered light among similar highly inclined systems, such as HD 15115 and HD 106906. We further identify a tentative localized brightness enhancement and scale height enhancement associated with the disk at ∼40 AU away from the star on the SE extension. We also find that the fractional polarization rises from 10% to 40% from 0.″5 to 0.″8 from the star. The combination of large brightness asymmetry and symmetric polarization fraction leads us to believe that an azimuthal dust density variation is causing the observed asymmetry.

Published
2016

4. POINT SOURCE POLARIMETRY WITH THE GEMINI PLANET IMAGER: SENSITIVITY CHARACTERIZATION WITH T5.5 DWARF COMPANION HD 19467 B

Author

Jensen-Clem, Rebecca, Millar-Blanchaer, Max, Mawet, Dimitri, Graham, James R, Wallace, J Kent, Macintosh, Bruce, Hinkley, Sasha, Wiktorowicz, Sloane J, Perrin, Marshall D, Marley, Mark S, Fitzgerald, Michael P, Oppenheimer, Rebecca, Ammons, S Mark, Rantakyrö, Fredrik T, and Marchis, Franck

Subjects
brown dwarfs, stars: individual, techniques: high angular resolution, techniques: polarimetric, astro-ph.EP, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract

Detecting polarized light from self-luminous exoplanets has the potential to provide key information about rotation, surface gravity, cloud grain size, and cloud coverage. While field brown dwarfs with detected polarized emission are common, no exoplanet or substellar companion has yet been detected in polarized light. With the advent of high contrast imaging spectro-polarimeters such as GPI and SPHERE, such a detection may now be possible with careful treatment of instrumental polarization. In this paper, we present 28 minutes of H-band GPI polarimetric observations of the benchmark T5.5 companion HD 19467 B. We detect no polarization signal from the target, and place an upper limit on the degree of linear polarization of pCL99.73% ≤ 2.4%. We discuss our results in the context of T dwarf cloud models and photometric variability.

Published
2016

5. DIRECT IMAGING OF AN ASYMMETRIC DEBRIS DISK IN THE HD 106906 PLANETARY SYSTEM

Author

Kalas, Paul G, Rajan, Abhijith, Wang, Jason J, Millar-Blanchaer, Maxwell A, Duchene, Gaspard, Chen, Christine, Fitzgerald, Michael P, Dong, Ruobing, Graham, James R, Patience, Jennifer, Macintosh, Bruce, Murray-Clay, Ruth, Matthews, Brenda, Rameau, Julien, Marois, Christian, Chilcote, Jeffrey, De Rosa, Robert J, Doyon, René, Draper, Zachary H, Lawler, Samantha, Ammons, S Mark, Arriaga, Pauline, Bulger, Joanna, Cotten, Tara, Follette, Katherine B, Goodsell, Stephen, Greenbaum, Alexandra, Hibon, Pascale, Hinkley, Sasha, Hung, Li-Wei, Ingraham, Patrick, Konapacky, Quinn, Lafreniere, David, Larkin, James E, Long, Douglas, Maire, Jérôme, Marchis, Franck, Metchev, Stan, Morzinski, Katie M, Nielsen, Eric L, Oppenheimer, Rebecca, Perrin, Marshall D, Pueyo, Laurent, Rantakyrö, Fredrik T, Ruffio, Jean-Baptiste, Saddlemyer, Leslie, Savransky, Dmitry, Schneider, Adam C, Sivaramakrishnan, Anand, Soummer, Rémi, Song, Inseok, Thomas, Sandrine, Vasisht, Gautam, Ward-Duong, Kimberly, Wiktorowicz, Sloane J, and Wolff, Schuyler G

Subjects
circumstellar matter, infrared: stars, stars: individual, techniques: high angular resolution, astro-ph.EP, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract

We present the first scattered light detections of the HD 106906 debris disk using the Gemini/Gemini Planet Imager in the infrared and Hubble Space Telescope (HST)/Advanced Camera for Surveys in the optical. HD 106906 is a 13 Myr old F5V star in the Sco-Cen association, with a previously detected planet-mass candidate HD 106906b projected 650 AU from the host star. Our observations reveal a near edge-on debris disk that has a central cleared region with radius ∼50 AU, and an outer extent >500 AU. The HST data show that the outer regions are highly asymmetric, resembling the "needle" morphology seen for the HD 15115 debris disk. The planet candidate is oriented ∼21° away from the position angle of the primary's debris disk, strongly suggesting non-coplanarity with the system. We hypothesize that HD 106906b could be dynamically involved in the perturbation of the primary's disk, and investigate whether or not there is evidence for a circumplanetary dust disk or cloud that is either primordial or captured from the primary. We show that both the existing optical properties and near-infrared colors of HD 106906b are weakly consistent with this possibility, motivating future work to test for the observational signatures of dust surrounding the planet.

Published
2015

6. β PICTORIS’ INNER DISK IN POLARIZED LIGHT AND NEW ORBITAL PARAMETERS FOR β PICTORIS b

Author

Millar-Blanchaer, Maxwell A, Graham, James R, Pueyo, Laurent, Kalas, Paul, Dawson, Rebekah I, Wang, Jason, Perrin, Marshall D, moon, Dae-Sik, Macintosh, Bruce, Ammons, S Mark, Barman, Travis, Cardwell, Andrew, Chen, Christine H, Chiang, Eugene, Chilcote, Jeffrey, Cotten, Tara, De Rosa, Robert J, Draper, Zachary H, Dunn, Jennifer, Duchêne, Gaspard, Esposito, Thomas M, Fitzgerald, Michael P, Follette, Katherine B, Goodsell, Stephen J, Greenbaum, Alexandra Z, Hartung, Markus, Hibon, Pascale, Hinkley, Sasha, Ingraham, Patrick, Jensen-Clem, Rebecca, Konopacky, Quinn, Larkin, James E, Long, Douglas, Maire, Jérôme, Marchis, Franck, Marley, Mark S, Marois, Christian, Morzinski, Katie M, Nielsen, Eric L, Palmer, David W, Oppenheimer, Rebecca, Poyneer, Lisa, Rajan, Abhijith, Rantakyrö, Fredrik T, Ruffio, Jean-Baptiste, Sadakuni, Naru, Saddlemyer, Leslie, Schneider, Adam C, Sivaramakrishnan, Anand, Soummer, Remi, Thomas, Sandrine, Vasisht, Gautam, Vega, David, Wallace, J Kent, Ward-Duong, Kimberly, Wiktorowicz, Sloane J, and Wolff, Schuyler G

Subjects
astrometry, planet-disk interactions, planets and satellites: individual, techniques: polarimetric, astro-ph.EP, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract

We present H-band observations of β Pic with the Gemini Planet Imager's (GPI's) polarimetry mode that reveal the debris disk between ∼0.″3 (6 AU) and ∼1.″7 (33 AU), while simultaneously detecting β Pic b. The polarized disk image was fit with a dust density model combined with a Henyey-Greenstein scattering phase function. The best-fit model indicates a disk inclined to the line of sight () with a position angle (PA) (slightly offset from the main outer disk, ), that extends from an inner disk radius of to well outside GPI's field of view. In addition, we present an updated orbit for β Pic b based on new astrometric measurements taken in GPI's spectroscopic mode spanning 14 months. The planet has a semimajor axis of , with an eccentricity The PA of the ascending node is offset from both the outer main disk and the inner disk seen in the GPI image. The orbital fit constrains the stellar mass of β Pic to Dynamical sculpting by β Pic b cannot easily account for the following three aspects of the inferred disk properties: (1) the modeled inner radius of the disk is farther out than expected if caused by β Pic b; (2) the mutual inclination of the inner disk and β Pic b is when it is expected to be closer to zero; and (3) the aspect ratio of the disk () is larger than expected from interactions with β Pic b or self-stirring by the disk's parent bodies.

Published
2015

7. POLARIMETRY WITH THE GEMINI PLANET IMAGER: METHODS, PERFORMANCE AT FIRST LIGHT, AND THE CIRCUMSTELLAR RING AROUND HR 4796A

Author

Perrin, Marshall D, Duchene, Gaspard, Millar-Blanchaer, Max, Fitzgerald, Michael P, Graham, James R, Wiktorowicz, Sloane J, Kalas, Paul G, Macintosh, Bruce, Bauman, Brian, Cardwell, Andrew, Chilcote, Jeffrey, De Rosa, Robert J, Dillon, Daren, Doyon, René, Dunn, Jennifer, Erikson, Darren, Gavel, Donald, Goodsell, Stephen, Hartung, Markus, Hibon, Pascale, Ingraham, Patrick, Kerley, Daniel, Konapacky, Quinn, Larkin, James E, Maire, Jérôme, Marchis, Franck, Marois, Christian, Mittal, Tushar, Morzinski, Katie M, Oppenheimer, BR, Palmer, David W, Patience, Jennifer, Poyneer, Lisa, Pueyo, Laurent, Rantakyrö, Fredrik T, Sadakuni, Naru, Saddlemyer, Leslie, Savransky, Dmitry, Soummer, Rémi, Sivaramakrishnan, Anand, Song, Inseok, Thomas, Sandrine, Wallace, J Kent, Wang, Jason J, and Wolff, Schuyler G

Subjects
circumstellar matter, instrumentation: adaptive optics, instrumentation: high angular resolution, instrumentation: polarimeters, polarization, stars: individual, astro-ph.EP, astro-ph.IM, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract

We present the first results from the polarimetry mode of the Gemini Planet Imager (GPI), which uses anew integral field polarimetry architecture to provide high contrast linear polarimetry with minimal systematic biases between the orthogonal polarizations. We describe the design, data reduction methods, and performance of polarimetry with GPI. Point-spread function (PSF) subtraction via differential polarimetry suppresses unpolarized starlight by a factor of over 100, and provides sensitivity to circumstellar dust reaching the photon noise limit for these observations. in the case of the circumstellar disk around HR 4796A,GPI's advanced adaptive optics system reveals the disk clearly even prior to PSF subtraction. In polarized light, the disk is seen all the way in to its semi-minor axis for the first time. The disk exhibits surprisingly strong asymmetry in polarized intensity, with the west side ≳9 times brighter than the east side despite the fact that the east side is slightly brighter in total intensity. Based on a synthesis of the total and polarized intensities, we now believe that the west side is closer to us, contrary to most prior interpretations. Forward scattering by relatively large silicate dust particles leads to the strong polarized intensity on thewest side, and the ring must be slightly optically thick in order to explain the lower brightness in total intensity there. These findings suggest that the ring is geometrically narrow and dynamically cold, perhaps shepherded by larger bodies in the same manner as Saturn's Fring.

Published
2015

8. A Uniform Analysis of Debris Disks with the Gemini Planet Imager. I. An Empirical Search for Perturbations from Planetary Companions in Polarized Light Images

Author

Crotts, Katie A., primary, Matthews, Brenda C., additional, Duchêne, Gaspard, additional, Esposito, Thomas M., additional, Dong, Ruobing, additional, Hom, Justin, additional, Oppenheimer, Rebecca, additional, Rice, Malena, additional, Wolff, Schuyler G., additional, Chen, Christine H., additional, Do Ó, Clarissa R., additional, Kalas, Paul, additional, Lewis, Briley L., additional, Weinberger, Alycia J., additional, Wilner, David J., additional, Ammons, Mark, additional, Arriaga, Pauline, additional, De Rosa, Robert J., additional, Debes, John H., additional, Fitzgerald, Michael P., additional, Gonzales, Eileen C., additional, Hines, Dean C., additional, Hinkley, Sasha, additional, Hughes, A. Meredith, additional, Kolokolova, Ludmilla, additional, Lee, Eve J., additional, López, Ronald A., additional, Macintosh, Bruce, additional, Mazoyer, Johan, additional, Metchev, Stanimir, additional, Millar-Blanchaer, Maxwell A., additional, Nielsen, Eric L., additional, Patience, Jenny, additional, Perrin, Marshall D., additional, Pueyo, Laurent, additional, Rantakyrö, Fredrik T., additional, Ren, Bin B., additional, Schneider, Glenn, additional, Soummer, Remi, additional, and Stark, Christopher C., additional

Published
2024
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11. Integral Field Spectroscopy with the Solar Gravitational Lens

Author

Alexander Madurowicz and Bruce Macintosh

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

The prospect of combining integral field spectroscopy with the solar gravitational lens (SGL) to spectrally and spatially resolve the surfaces and atmospheres of extrasolar planets is investigated. The properties of hyperbolic orbits visiting the focal region of the SGL are calculated analytically, demonstrating trade offs between departure velocity and time of arrival, as well as gravity assist maneuvers and heliocentric angular velocity. Numerical integration of the solar barycentric motion demonstrates that navigational acceleration of $\textrm{d}v \lesssim 80 \frac{\textrm{m}}{\textrm{s}} + 6.7 \frac{\textrm{m}}{\textrm{s}} \frac{t}{\textrm{year}}$ is needed to obtain and maintain alignment. Obtaining target ephemerides of sufficient precision is an open problem. The optical properties of an oblate gravitational lens are reviewed, including calculations of the magnification and the point-spread function that forms inside a telescope. Image formation for extended, incoherent sources is discussed when the projected image is smaller than, approximately equal to, and larger than the critical caustic. Sources of contamination which limit observational SNR are considered in detail, including the sun, the solar corona, the host star, and potential background objects. A noise mitigation strategy of spectrally and spatially separating the light using integral field spectroscopy is emphasized. A pseudoinverse-based image reconstruction scheme demonstrates that direct reconstruction of an Earth-like source from \textit{single} measurements of the Einstein ring is possible when the critical caustic and observed SNR are sufficiently large. In this arrangement, a mission would not require multiple telescopes or navigational symmetry breaking, enabling continuous monitoring of the atmospheric composition and dynamics on other planets., 34 pages, 21 figures, accepted to ApJ

Published
2022
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14. An Exo–Kuiper Belt with an Extended Halo around HD 191089 in Scattered Light

Author

Ren, Bin, primary, Choquet, Élodie, additional, Perrin, Marshall D., additional, Duchêne, Gaspard, additional, Debes, John H., additional, Pueyo, Laurent, additional, Rice, Malena, additional, Chen, Christine, additional, Schneider, Glenn, additional, Esposito, Thomas M., additional, Poteet, Charles A., additional, Wang, Jason J., additional, Ammons, S. Mark, additional, Ansdell, Megan, additional, Arriaga, Pauline, additional, Bailey, Vanessa P., additional, Barman, Travis, additional, Bruzzone, Juan Sebastián, additional, Bulger, Joanna, additional, Chilcote, Jeffrey, additional, Cotten, Tara, additional, De Rosa, Robert J., additional, Doyon, Rene, additional, Fitzgerald, Michael P., additional, Follette, Katherine B., additional, Goodsell, Stephen J., additional, Gerard, Benjamin L., additional, Graham, James R., additional, Greenbaum, Alexandra Z., additional, Hagan, J. Brendan, additional, Hibon, Pascale, additional, Hines, Dean C., additional, Hung, Li-Wei, additional, Ingraham, Patrick, additional, Kalas, Paul, additional, Konopacky, Quinn, additional, Larkin, James E., additional, Macintosh, Bruce, additional, Maire, Jérôme, additional, Marchis, Franck, additional, Marois, Christian, additional, Mazoyer, Johan, additional, Ménard, François, additional, Metchev, Stanimir, additional, Millar-Blanchaer, Maxwell A., additional, Mittal, Tushar, additional, Moerchen, Margaret, additional, Nielsen, Eric L., additional, N’Diaye, Mamadou, additional, Oppenheimer, Rebecca, additional, Palmer, David, additional, Patience, Jennifer, additional, Pinte, Christophe, additional, Poyneer, Lisa, additional, Rajan, Abhijith, additional, Rameau, Julien, additional, Rantakyrö, Fredrik T., additional, Ruffio, Jean-Baptiste, additional, Ryan, Dominic, additional, Savransky, Dmitry, additional, Schneider, Adam C., additional, Sivaramakrishnan, Anand, additional, Song, Inseok, additional, Soummer, Rémi, additional, Stark, Christopher, additional, Thomas, Sandrine, additional, Vigan, Arthur, additional, Wallace, J. Kent, additional, Ward-Duong, Kimberly, additional, Wiktorowicz, Sloane, additional, Wolff, Schuyler, additional, Ygouf, Marie, additional, and Norman, Colin, additional

Published
2019
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15. TESS Hunt for Young and Maturing Exoplanets (THYME): A Planet in the 45 Myr Tucana–Horologium Association

Author

Newton, Elisabeth R., primary, Mann, Andrew W., additional, Tofflemire, Benjamin M., additional, Pearce, Logan, additional, Rizzuto, Aaron C., additional, Vanderburg, Andrew, additional, Martinez, Raquel A., additional, Wang, Jason J., additional, Ruffio, Jean-Baptiste, additional, Kraus, Adam L., additional, Johnson, Marshall C., additional, Thao, Pa Chia, additional, Wood, Mackenna L., additional, Rampalli, Rayna, additional, Nielsen, Eric L., additional, Collins, Karen A., additional, Dragomir, Diana, additional, Hellier, Coel, additional, Anderson, D. R., additional, Barclay, Thomas, additional, Brown, Carolyn, additional, Feiden, Gregory, additional, Hart, Rhodes, additional, Isopi, Giovanni, additional, Kielkopf, John F., additional, Mallia, Franco, additional, Nelson, Peter, additional, Rodriguez, Joseph E., additional, Stockdale, Chris, additional, Waite, Ian A., additional, Wright, Duncan J., additional, Lissauer, Jack J., additional, Ricker, George R., additional, Vanderspek, Roland, additional, Latham, David W., additional, Seager, S., additional, Winn, Joshua N., additional, Jenkins, Jon M., additional, Bouma, Luke G., additional, Burke, Christopher J., additional, Davies, Misty, additional, Fausnaugh, Michael, additional, Li, Jie, additional, Morris, Robert L., additional, Mukai, Koji, additional, Villaseñor, Joel, additional, Villeneuva, Steven, additional, De Rosa, Robert J., additional, Macintosh, Bruce, additional, Mengel, Matthew W., additional, Okumura, Jack, additional, and Wittenmyer, Robert A., additional

Published
2019
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16. SHAPED PUPIL DESIGN FOR THE GEMINI PLANET IMAGER

Author

Bruce Macintosh, Eric Cady, Rémi Soummer, and N. Jeremy Kasdin

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), High contrast, Computer science, business.industry, FOS: Physical sciences, Astronomy and Astrophysics, Pupil, law.invention, Starlight, Telescope, Optics, Apodization, Space and Planetary Science, law, Planet, Gemini Planet Imager, Astrophysics - Instrumentation and Methods for Astrophysics, business, Instrumentation and Methods for Astrophysics (astro-ph.IM), Coronagraph, Astrophysics - Earth and Planetary Astrophysics
Abstract

The Gemini Planet Imager (GPI) is an instrument designed for the Gemini South telescope to image young Jupiter-mass planets in the infrared. To achieve the high contrast needed for this, it employs an apodized pupil Lyot coronagraph (APLC) to remove most of the starlight. Current designs use a partially-transmitting apodizer in the pupil; we examine the use of binary apodizations in the form of starshaped shaped pupils, and present a design that could achieve comparable performance, along with a series of design guidelines for creating shaped pupil versions of APLCs in other systems., Comment: 20 pages, 7 figures, accepted for publication in ApJ

Published
2009
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17. Gas and Dust Associated with the Strange, Isolated Star BP Piscium

Author

Christian Marois, Alycia J. Weinberger, Barry Zuckerman, Marshall D. Perrin, G. W. Marcy, Patrick Palmer, Inseok Song, James R. Graham, David J. Wilner, Bruce Macintosh, Eric E. Becklin, Joseph H. Rhee, Michael S. Bessell, C. Melis, T. Forveille, Joel H. Kastner, Travis Barman, David S. Meier, Laboratoire d'Astrophysique de Grenoble (LAOG), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Star (graph theory), 01 natural sciences, Luminosity, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Conjunction (astronomy), Astrophysics (astro-ph), Astronomy and Astrophysics, Accretion (astrophysics), T Tauri star, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Variable star, Low Mass
Abstract

We have carried out a multiwavelength observational campaign demonstrating some of the remarkable properties of the infrared-bright variable star BP Psc. Surrounded by a compact dusty, gaseous disk, this little-studied late-G (or early-K) type star emits about 75% of its detected energy flux at infrared wavelengths. Evidence for accretion of gas in conjunction with narrow bi-polar jets and Herbig-Haro objects is apparently consistent with classification of BP Psc as a pre-main sequence star, as postulated in most previous studies. If young, then BP Psc would be one of the nearest and oldest known classical T Tauri stars. However, such an evolutionary classification encounters various problems that are absent or much less severe if BP Psc is instead a luminosity class III post-main sequence star. In this case, it would be the first known example of a first ascent giant surrounded by a massive molecular disk with accompanying rapid gas accretion and prominent jets and HH objects. In this model, the genesis of the massive dusty gaseous disk could be a consequence of the envelopment of a low mass companion star. Properties in the disk may be conducive to the current formation of planets, a gigayear or more after the formation of BP Psc itself., Accepted for Astrophysical Journal New version with minor changes: includes fixing a typo on the 3rd line of the paragraph that follows Equa 4 and adding a new reference (Nordhaus and Blackman 2006)

Published
2008
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18. Individual, Model-independent Masses of the Closest Known Brown Dwarf Binary to the Sun

Author

Garcia, E. Victor, primary, Ammons, S. Mark, additional, Salama, Maissa, additional, Crossfield, Ian, additional, Bendek, Eduardo, additional, Chilcote, Jeffrey, additional, Garrel, Vincent, additional, Graham, James R., additional, Kalas, Paul, additional, Konopacky, Quinn, additional, Lu, Jessica R., additional, Macintosh, Bruce, additional, Marin, Eduardo, additional, Marois, Christian, additional, Nielsen, Eric, additional, Neichel, Benoît, additional, Pham, Don, additional, De Rosa, Robert J., additional, Ryan, Dominic M., additional, Service, Maxwell, additional, and Sivo, Gaetano, additional

Published
2017
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19. The Core of NGC 6240 from Keck Adaptive Optics andHubble Space TelescopeNICMOS Observations

Author

Bruce Macintosh, Gabriela Canalizo, L. Raschke, Glenn Schneider, David Whysong, Claire E. Max, and Robert Antonucci

Subjects
Physics, Hydrogen molecule, Astronomy and Astrophysics, Astrophysics, law.invention, Telescope, Core (optical fiber), medicine.anatomical_structure, Space and Planetary Science, law, Young star, Hubble space telescope, medicine, Adaptive optics, Nucleus, Line (formation)
Abstract

We present results of near infrared imaging of the disk-galaxy-merger NGC 6240 using adaptive optics on the Keck II Telescope and reprocessed archival data from NICMOS on the Hubble Space Telescope. Both the North and South nuclei of NGC 6240 are clearly elongated, with considerable sub-structure within each nucleus. In K' band there are at least two point-sources within the North nucleus; we tentatively identify the south-western point-source within the North nucleus as the position of one of the two AGNs. Within the South nucleus, the northern sub-nucleus is more highly reddened. Based upon the nuclear separation measured at 5 GHz, we suggest that the AGN in the South nucleus is still enshrouded in dust at K' band, and is located slightly to the north of the brightest point in K' band. Within the South nucleus there is strong H2 1-0 S(1) line emission from the northern sub-nucleus, contrary to the conclusions of previous seeing-limited observations. Narrowband H2 emission-line images show that a streamer or ribbon of excited molecular hydrogen connects the North and South nuclei. We suggest that this linear feature corresponds to a bridge of gas connecting the two nuclei, as seen in computer simulations of mergers. Many point-like regions are seen around the two nuclei. These are most prominent at 1.1 microns with NICMOS, and in K'-band with Keck adaptive optics. We suggest that these point-sources represent young star clusters formed in the course of the merger.

Published
2005
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20. Mid-Infrared Observations of van Maanen 2: No Substellar Companion

Author

Jay Farihi, Bruce Macintosh, and Eric E. Becklin

Subjects
Physics, Solar mass, Line-of-sight, Infrared, Astrophysics (astro-ph), Brown dwarf, FOS: Physical sciences, White dwarf, Astronomy and Astrophysics, Astrophysics, Wavelength, Space and Planetary Science, Magnitude (astronomy), Jupiter mass
Abstract

The results of a comprehensive infrared imaging search for the putative 0.06 solar mass astrometric companion to the 4.4 pc white dwarf van Mannen 2 are reported. Adaptive optics images acquired at 3.8 microns reveal a diffraction limited core of 0.09" and no direct evidence of a secondary. Models predict that at 5 Gyr, a 50 jupiter mass brown dwarf would be only 1 magnitude fainter than van Maanen 2 at this wavelength and the astrometric analysis suggested a separation of 0.2". In the case of a chance alignment along the line of sight, a 0.4 mag excess should be measured. An independent photometric observation at the same wavelength reveals no excess. In addition, there exist published ISO observations of van Maanen 2 at 6.8 and 15.0 microns which are consistent with photospheric flux of a 6750 K white dwarf. If recent brown dwarf models are correct, there is no substellar companion with T > 500 K., 11 pages, 3 figures, 1 table, accepted to ApJ Letters

Published
2004
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21. A Multiwavelength Scattered Light Analysis of the Dust Grain Population in the GG Tauri Circumbinary Ring

Author

Bruce Macintosh, C. McCabe, Gaspard Duchêne, and Andrea M. Ghez

Subjects
Physics, education.field_of_study, Scattering, Molecular cloud, Astrophysics (astro-ph), Population, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Protoplanetary disk, Polarization (waves), Interstellar medium, Grain growth, Wavelength, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, education, Astrophysics::Galaxy Astrophysics
Abstract

We present the first 3.8 micron image of the dusty ring surrounding the young binary system GG Tau, obtained with the W. M. Keck II 10m telescope's adaptive optics system. This is the longest wavelength at which the ring has been detected in scattered light so far, allowing a multi-wavelength analysis of the scattering properties of the dust grains present in this protoplanetary disk in combination with previous, shorter wavelengths, HST images. We find that the scattering phase function of the dust grains in the disk is only weakly dependent on the wavelength. This is inconsistent with dust models inferred from observations of the interstellar medium or dense molecular clouds. In particular, the strongly forward-throwing scattering phase function observed at 3.8 micron implies a significant increase in the population of large (>~1 micron) grains, which provides direct evidence for grain growth in the ring. However, the grain size distribution required to match the 3.8 micron image of the ring is incompatible with its published 1 micron polarization map, implying that the dust population is not uniform throughout the ring. We also show that our 3.8 micron scattered light image probes a deeper layer of the ring than previous shorter wavelength images, as demonstrated by a shift in the location of the inner edge of the disk's scattered light distribution between 1 and 3.8 micron. We therefore propose a stratified structure for the ring in which the surface layers, located ~50 AU above the ring midplane, contain dust grains that are very similar to those found in dense molecular clouds, while the region of the ring located ~25 AU from the midplane contains significantly larger grains. This stratified structure is likely the result of vertical dust settling and/or preferred grain growth in the densest parts of the ring., 34 pages, 6 figures, accepted for publication in Astrophysical Journal

Published
2004
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22. Titan’s Clouds from Gemini and Keck Adaptive Optics Imaging

Author

Bruce Macintosh, Christopher P. McKay, Henry G. Roe, and I. de Pater

Subjects
Physics, Convection, Solar System, Haze, Infrared, Astronomy, Astronomy and Astrophysics, Astrobiology, Troposphere, symbols.namesake, Space and Planetary Science, Planet, Physics::Space Physics, symbols, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Adaptive optics, Titan (rocket family), Physics::Atmospheric and Oceanic Physics, Astrophysics::Galaxy Astrophysics
Abstract

Using adaptive optics on the Gemini and Keck II telescopes, we found a thin haze and discrete clouds in Titan’s south polar troposphere. The discrete clouds vary on timescales of a few hours. We propose a seasonal mechanism to explain the formation of this spring polar tropospheric haze. Assuming that the clouds are located in or above the haze, we suggest that convection within this haze layer triggers methane condensation; subsequent latent heat release leads to vigorous convection and formation of transient clouds. Our results have significant implications for planning the Cassini mission flybys of Titan. Subject headings: infrared: solar system — instrumentation: adaptive optics — planets and satellites: individual (Titan)

Published
2002
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23. Speckle Decorrelation and Dynamic Range in Speckle Noise–limited Imaging

Author

Anand Sivaramakrishnan, Bruce Macintosh, Philip E. Hodge, and James P. Lloyd

Subjects
Physics, business.industry, Dynamic range, Astrophysics::Instrumentation and Methods for Astrophysics, Phase (waves), Physics::Optics, Astronomy and Astrophysics, Speckle noise, Speckle decorrelation, Residual, Speckle pattern, Noise, Computer Science::Graphics, Optics, Space and Planetary Science, Background distribution, business
Abstract

The useful dynamic range of an image in the diffraction-limited regime is usually limited by speckles caused by residual phase errors in the optical system forming the image. The technique of speckle decorrelation involves introducing many independent realizations of additional phase error into a wave front during one speckle lifetime, changing the instantaneous speckle pattern. A commonly held assumption is that this results in the speckles being "moved around" at the rate at which the additional phase screens are applied. The intention of this exercise is to smooth the speckles out into a more uniform background distribution during their persistence time, thereby enabling companion detection around bright stars to be photon noise limited rather than speckle limited. We demonstrate analytically why this does not occur and confirm this result with numerical simulations. We show that the original speckles must persist and that the technique of speckle decorrelation merely adds more noise to the original speckle noise, thereby degrading the dynamic range of the image.

Published
2002
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24. DISCOVERY OF A SUBSTELLAR COMPANION TO THE NEARBY DEBRIS DISK HOST HR 2562

Author

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

Published
2016
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25. SPECTROSCOPIC CHARACTERIZATION OF HD 95086 b WITH THE GEMINI PLANET IMAGER

Author

De Rosa, Robert J., primary, Rameau, Julien, additional, Patience, Jenny, additional, Graham, James R., additional, Doyon, René, additional, Lafrenière, David, additional, Macintosh, Bruce, additional, Pueyo, Laurent, additional, Rajan, Abhijith, additional, Wang, Jason J., additional, Ward-Duong, Kimberly, additional, Hung, Li-Wei, additional, Maire, Jérôme, additional, Nielsen, Eric L., additional, Ammons, S. Mark, additional, Bulger, Joanna, additional, Cardwell, Andrew, additional, Chilcote, Jeffrey K., additional, Galvez, Ramon L., additional, Gerard, Benjamin L., additional, Goodsell, Stephen, additional, Hartung, Markus, additional, Hibon, Pascale, additional, Ingraham, Patrick, additional, Johnson-Groh, Mara, additional, Kalas, Paul, additional, Konopacky, Quinn M., additional, Marchis, Franck, additional, Marois, Christian, additional, Metchev, Stanimir, additional, Morzinski, Katie M., additional, Oppenheimer, Rebecca, additional, Perrin, Marshall D., additional, Rantakyrö, Fredrik T., additional, Savransky, Dmitry, additional, and Thomas, Sandrine, additional

Published
2016
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26. CONSTRAINTS ON THE ARCHITECTURE OF THE HD 95086 PLANETARY SYSTEM WITH THE GEMINI PLANET IMAGER

Author

Rameau, Julien, primary, Nielsen, Eric L., additional, Rosa, Robert J. De, additional, Blunt, Sarah C., additional, Patience, Jenny, additional, Doyon, René, additional, Graham, James R., additional, Lafrenière, David, additional, Macintosh, Bruce, additional, Marchis, Franck, additional, Bailey, Vanessa, additional, Chilcote, Jeffrey K., additional, Duchene, Gaspard, additional, Esposito, Thomas M., additional, Hung, Li-Wei, additional, Konopacky, Quinn M., additional, Maire, Jérôme, additional, Marois, Christian, additional, Metchev, Stanimir, additional, Perrin, Marshall D., additional, Pueyo, Laurent, additional, Rajan, Abhijith, additional, Savransky, Dmitry, additional, Wang, Jason J., additional, Ward-Duong, Kimberly, additional, Wolff, Schuyler G., additional, Ammons, S. Mark, additional, Hibon, Pascale, additional, Ingraham, Patrick, additional, Kalas, Paul, additional, Morzinski, Katie M., additional, Oppenheimer, Rebecca, additional, Rantakyearö, Fredrik T., additional, and Thomas, Sandrine, additional

Published
2016
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27. THE PECULIAR DEBRIS DISK OF HD 111520 AS RESOLVED BY THE GEMINI PLANET IMAGER

Author

Patrick Ingraham, Franck Marchis, Benjamin L. Gerard, Abhijith Rajan, Christine Chen, David Vega, Joanna Bulger, S. Mark Ammons, James R. Graham, René Doyon, Kimberly Ward-Duong, Pascale Hibon, Schuyler Wolff, Gaspard Duchêne, Marshall D. Perrin, Katherine B. Follette, Jennifer Patience, Bruce Macintosh, Maxwell A. Millar-Blanchaer, Jeffrey Chilcote, Brenda C. Matthews, Rahul Patel, Anand Sivaramakrishnan, Michael P. Fitzgerald, Julian Rameau, Christian Marois, Paul Kalas, Laurent Pueyo, Eric L. Nielsen, David Lafrenière, Deborah L. Padgett, Jason J. Wang, Zachary H. Draper, Rebecca Oppenheimer, Sasha Hinkley, and Alexandra Z. Greenbaum

Subjects
Brightness, media_common.quotation_subject, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astronomy & Astrophysics, Physical Chemistry, Atomic, circumstellar matter, 01 natural sciences, Asymmetry, 010309 optics, Particle and Plasma Physics, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Nuclear, Gemini Planet Imager, 010303 astronomy & astrophysics, individual [stars], Astrophysics::Galaxy Astrophysics, media_common, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Debris disk, individual (HD 111520) [stars], Molecular, Astronomy and Astrophysics, Scale height, Polarization (waves), Position angle, Azimuth, Space and Planetary Science, astro-ph.EP, Astrophysics::Earth and Planetary Astrophysics, Astronomical and Space Sciences, Astrophysics - Earth and Planetary Astrophysics, Physical Chemistry (incl. Structural)
Abstract

Using the Gemini Planet Imager (GPI), we have resolved the circumstellar debris disk around HD 111520 at a projected range of ~30-100 AU in both total and polarized $H$-band intensity. The disk is seen edge-on at a position angle of ~165$^{\circ}$ along the spine of emission. A slight inclination or asymmetric warping are covariant and alters the interpretation of the observed disk emission. We employ 3 point spread function (PSF) subtraction methods to reduce the stellar glare and instrumental artifacts to confirm that there is a roughly 2:1 brightness asymmetry between the NW and SE extension. This specific feature makes HD 111520 the most extreme examples of asymmetric debris disks observed in scattered light among similar highly inclined systems, such as HD 15115 and HD 106906. We further identify a tentative localized brightness enhancement and scale height enhancement associated with the disk at ~40 AU away from the star on the SE extension. We also find that the fractional polarization rises from 10 to 40% from 0.5" to 0.8" from the star. The combination of large brightness asymmetry and symmetric polarization fraction leads us to believe that an azimuthal dust density variation is causing the observed asymmetry., Comment: 9 pages, 8 Figures, 1 table, Accepted to ApJ

Published
2016
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28. THE PDS 66 CIRCUMSTELLAR DISK AS SEEN IN POLARIZED LIGHT WITH THE GEMINI PLANET IMAGER

Author

Wolff, Schuyler G., primary, Perrin, Marshall, additional, Millar-Blanchaer, Maxwell A., additional, Nielsen, Eric L., additional, Wang, Jason, additional, Cardwell, Andrew, additional, Chilcote, Jeffrey, additional, Dong, Ruobing, additional, Draper, Zachary H., additional, Duchêne, Gaspard, additional, Fitzgerald, Michael P., additional, Goodsell, Stephen J., additional, Grady, Carol A., additional, Graham, James R., additional, Greenbaum, Alexandra Z., additional, Hartung, Markus, additional, Hibon, Pascale, additional, Hines, Dean C., additional, Hung, Li-Wei, additional, Kalas, Paul, additional, Macintosh, Bruce, additional, Marchis, Franck, additional, Marois, Christian, additional, Pueyo, Laurent, additional, Rantakyrö, Fredrik T., additional, Schneider, Glenn, additional, Sivaramakrishnan, Anand, additional, and Wiktorowicz, Sloane J., additional

Published
2016
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29. FIRST SCATTERED-LIGHT IMAGE OF THE DEBRIS DISK AROUND HD 131835 WITH THE GEMINI PLANET IMAGER

Author

Hung, Li-Wei, primary, Duchêne, Gaspard, additional, Arriaga, Pauline, additional, Fitzgerald, Michael P., additional, Maire, Jérôme, additional, Marois, Christian, additional, Millar-Blanchaer, Maxwell A., additional, Bruzzone, Sebastian, additional, Rajan, Abhijith, additional, Pueyo, Laurent, additional, Kalas, Paul G., additional, De Rosa, Robert J., additional, Graham, James R., additional, Konopacky, Quinn, additional, Wolff, Schuyler G., additional, Ammons, S. Mark, additional, Chen, Christine H., additional, Chilcote, Jeffrey K., additional, Draper, Zachary H., additional, Esposito, Thomas M., additional, Gerard, Benjamin, additional, Goodsell, Stephen, additional, Greenbaum, Alexandra, additional, Hibon, Pascale, additional, Hinkley, Sasha, additional, Macintosh, Bruce, additional, Marchis, Franck, additional, Metchev, Stanimir, additional, Nielsen, Eric L., additional, Oppenheimer, Rebecca, additional, Patience, Jennifer L., additional, Perrin, Marshall D., additional, Rantakyrö, Fredrik T., additional, Sivaramakrishnan, Anand, additional, Wang, Jason J., additional, Ward-Duong, Kimberly, additional, and Wiktorowicz, Sloane J., additional

Published
2015
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30. ASTROMETRIC CONFIRMATION AND PRELIMINARY ORBITAL PARAMETERS OF THE YOUNG EXOPLANET 51 ERIDANI b WITH THE GEMINI PLANET IMAGER

Author

Rosa, Robert J. De, primary, Nielsen, Eric L., additional, Blunt, Sarah C., additional, Graham, James R., additional, Konopacky, Quinn M., additional, Marois, Christian, additional, Pueyo, Laurent, additional, Rameau, Julien, additional, Ryan, Dominic M., additional, Wang, Jason J., additional, Bailey, Vanessa, additional, Chontos, Ashley, additional, Fabrycky, Daniel C., additional, Follette, Katherine B., additional, Macintosh, Bruce, additional, Marchis, Franck, additional, Ammons, S. Mark, additional, Arriaga, Pauline, additional, Chilcote, Jeffrey K., additional, Cotten, Tara H., additional, Doyon, René, additional, Duchêne, Gaspard, additional, Esposito, Thomas M., additional, Fitzgerald, Michael P., additional, Gerard, Benjamin, additional, Goodsell, Stephen J., additional, Greenbaum, Alexandra Z., additional, Hibon, Pascale, additional, Ingraham, Patrick, additional, Johnson-Groh, Mara, additional, Kalas, Paul G., additional, Lafrenière, David, additional, Maire, Jerome, additional, Metchev, Stanimir, additional, Millar-Blanchaer, Maxwell A., additional, Morzinski, Katie M., additional, Oppenheimer, Rebecca, additional, Patel, Rahul I., additional, Patience, Jennifer L., additional, Perrin, Marshall D., additional, Rajan, Abhijith, additional, Rantakyrö, Fredrik T., additional, Ruffio, Jean-Baptiste, additional, Schneider, Adam C., additional, Sivaramakrishnan, Anand, additional, Song, Inseok, additional, Tran, Debby, additional, Vasisht, Gautam, additional, Ward-Duong, Kimberly, additional, and Wolff, Schuyler G., additional

Published
2015
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31. GEMINI PLANET IMAGER OBSERVATIONS OF THE AU MICROSCOPII DEBRIS DISK: ASYMMETRIES WITHIN ONE ARCSECOND

Author

Wang, Jason J., primary, Graham, James R., additional, Pueyo, Laurent, additional, Nielsen, Eric L., additional, Millar-Blanchaer, Max, additional, Rosa, Robert J. De, additional, Kalas, Paul, additional, Ammons, S. Mark, additional, Bulger, Joanna, additional, Cardwell, Andrew, additional, Chen, Christine, additional, Chiang, Eugene, additional, Chilcote, Jeffrey K., additional, Doyon, René, additional, Draper, Zachary H., additional, Duchêne, Gaspard, additional, Esposito, Thomas M., additional, Fitzgerald, Michael P., additional, Goodsell, Stephen J., additional, Greenbaum, Alexandra Z., additional, Hartung, Markus, additional, Hibon, Pascale, additional, Hinkley, Sasha, additional, Hung, Li-Wei, additional, Ingraham, Patrick, additional, Larkin, James E., additional, Macintosh, Bruce, additional, Maire, Jerome, additional, Marchis, Franck, additional, Marois, Christian, additional, Matthews, Brenda C., additional, Morzinski, Katie M., additional, Oppenheimer, Rebecca, additional, Patience, Jenny, additional, Perrin, Marshall D., additional, Rajan, Abhijith, additional, Rantakyrö, Fredrik T., additional, Sadakuni, Naru, additional, Serio, Andrew, additional, Sivaramakrishnan, Anand, additional, Soummer, Rémi, additional, Thomas, Sandrine, additional, Ward-Duong, Kimberly, additional, Wiktorowicz, Sloane J., additional, and Wolff, Schuyler G., additional

Published
2015
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32. βPICTORIS’ INNER DISK IN POLARIZED LIGHT AND NEW ORBITAL PARAMETERS FORβPICTORISb

Author

Millar-Blanchaer, Maxwell A., primary, Graham, James R., additional, Pueyo, Laurent, additional, Kalas, Paul, additional, Dawson, Rebekah I., additional, Wang, Jason, additional, Perrin, Marshall D., additional, moon, Dae-Sik, additional, Macintosh, Bruce, additional, Ammons, S. Mark, additional, Barman, Travis, additional, Cardwell, Andrew, additional, Chen, Christine H., additional, Chiang, Eugene, additional, Chilcote, Jeffrey, additional, Cotten, Tara, additional, Rosa, Robert J. De, additional, Draper, Zachary H., additional, Dunn, Jennifer, additional, Duchêne, Gaspard, additional, Esposito, Thomas M., additional, Fitzgerald, Michael P., additional, Follette, Katherine B., additional, Goodsell, Stephen J., additional, Greenbaum, Alexandra Z., additional, Hartung, Markus, additional, Hibon, Pascale, additional, Hinkley, Sasha, additional, Ingraham, Patrick, additional, Jensen-Clem, Rebecca, additional, Konopacky, Quinn, additional, Larkin, James E., additional, Long, Douglas, additional, Maire, Jérôme, additional, Marchis, Franck, additional, Marley, Mark S., additional, Marois, Christian, additional, Morzinski, Katie M., additional, Nielsen, Eric L., additional, Palmer, David W., additional, Oppenheimer, Rebecca, additional, Poyneer, Lisa, additional, Rajan, Abhijith, additional, Rantakyrö, Fredrik T., additional, Ruffio, Jean-Baptiste, additional, Sadakuni, Naru, additional, Saddlemyer, Leslie, additional, Schneider, Adam C., additional, Sivaramakrishnan, Anand, additional, Soummer, Remi, additional, Thomas, Sandrine, additional, Vasisht, Gautam, additional, Vega, David, additional, Wallace, J. Kent, additional, Ward-Duong, Kimberly, additional, Wiktorowicz, Sloane J., additional, and Wolff, Schuyler G., additional

Published
2015
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33. CHARACTERIZING THE ATMOSPHERES OF THE HR8799 PLANETS WITH HST /WFC3

Author

Rajan, Abhijith, primary, Barman, Travis, additional, Soummer, Rémi, additional, Hagan, J. Brendan, additional, Patience, Jennifer, additional, Pueyo, Laurent, additional, Choquet, Élodie, additional, Konopacky, Quinn, additional, Macintosh, Bruce, additional, and Marois, Christian, additional

Published
2015
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36. SCATTERED LIGHT FROM DUST IN THE CAVITY OF THE V4046 Sgr TRANSITION DISK

Author

Motohide Tamura, Valerie Rapson, Joel H. Kastner, Bruce Macintosh, Max Millar-Blanchaer, Dean C. Hines, and Sean M. Andrews

Subjects
Physics, Solar System, Brightness, Giant planet, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Planet, Astrophysics::Solar and Stellar Astrophysics, Gemini Planet Imager, Astrophysics::Earth and Planetary Astrophysics, Halo, Circumbinary planet, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Cosmic dust
Abstract

We report the presence of scattered light from dust grains located in the giant planet formation region of the circumbinary disk orbiting the ~20-Myr-old close (~0.045 AU separation) binary system V4046 Sgr AB based on observations with the new Gemini Planet Imager (GPI) instrument. These GPI images probe to within ~7 AU of the central binary with linear spatial resolution of ~3 AU, and are thereby capable of revealing dust disk structure within a region corresponding to the giant planets in our solar system. The GPI imaging reveals a relatively narrow (FWHM ~10 AU) ring of polarized near-infrared flux whose brightness peaks at ~14 AU. This ~14 AU radius ring is surrounded by a fainter outer halo of scattered light extending to ~45 AU, which coincides with previously detected mm-wave thermal dust emission. The presence of small grains that efficiently scatter starlight well inside the mm-wavelength disk cavity supports current models of planet formation that suggest planet-disk interactions can generate pressure traps that impose strong radial variations in the particle size distribution throughout the disk., Comment: 13 pages, 4 figures, Accepted to ApJ Letters

Published
2015
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37. THE FIRST H -BAND SPECTRUM OF THE GIANT PLANET β PICTORIS b

Author

Chilcote, Jeffrey, primary, Barman, Travis, additional, Fitzgerald, Michael P., additional, Graham, James R., additional, Larkin, James E., additional, Macintosh, Bruce, additional, Bauman, Brian, additional, Burrows, Adam S., additional, Cardwell, Andrew, additional, De Rosa, Robert J., additional, Dillon, Daren, additional, Doyon, René, additional, Dunn, Jennifer, additional, Erikson, Darren, additional, Gavel, Donald, additional, Goodsell, Stephen J., additional, Hartung, Markus, additional, Hibon, Pascale, additional, Ingraham, Patrick, additional, Kalas, Paul, additional, Konopacky, Quinn, additional, Maire, Jérôme, additional, Marchis, Franck, additional, Marley, Mark S., additional, Marois, Christian, additional, Millar-Blanchaer, Max, additional, Morzinski, Katie, additional, Norton, Andrew, additional, Oppenheimer, Rebecca, additional, Palmer, David, additional, Patience, Jennifer, additional, Perrin, Marshall, additional, Poyneer, Lisa, additional, Pueyo, Laurent, additional, Rantakyrö, Fredrik T., additional, Sadakuni, Naru, additional, Saddlemyer, Leslie, additional, Savransky, Dmitry, additional, Serio, Andrew, additional, Sivaramakrishnan, Anand, additional, Song, Inseok, additional, Soummer, Rémi, additional, Thomas, Sandrine, additional, Wallace, J. Kent, additional, Wiktorowicz, Sloane, additional, and Wolff, Schuyler, additional

Published
2014
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38. GEMINI PLANET IMAGER SPECTROSCOPY OF THE HR 8799 PLANETS c AND d

Author

Ingraham, Patrick, primary, Marley, Mark S., additional, Saumon, Didier, additional, Marois, Christian, additional, Macintosh, Bruce, additional, Barman, Travis, additional, Bauman, Brian, additional, Burrows, Adam, additional, Chilcote, Jeffrey K., additional, De Rosa, Robert J., additional, Dillon, Daren, additional, Doyon, René, additional, Dunn, Jennifer, additional, Erikson, Darren, additional, Fitzgerald, Michael P., additional, Gavel, Donald, additional, Goodsell, Stephen J., additional, Graham, James R., additional, Hartung, Markus, additional, Hibon, Pascale, additional, Kalas, Paul G., additional, Konopacky, Quinn, additional, Larkin, James A., additional, Maire, Jérôme, additional, Marchis, Franck, additional, McBride, James, additional, Millar-Blanchaer, Max, additional, Morzinski, Katie M., additional, Norton, Andrew, additional, Oppenheimer, Rebecca, additional, Palmer, Dave W., additional, Patience, Jenny, additional, Perrin, Marshall D., additional, Poyneer, Lisa A., additional, Pueyo, Laurent, additional, Rantakyrö, Fredrik, additional, Sadakuni, Naru, additional, Saddlemyer, Leslie, additional, Savransky, Dmitry, additional, Soummer, Rémi, additional, Sivaramakrishnan, Anand, additional, Song, Inseok, additional, Thomas, Sandrine, additional, Kent Wallace, J., additional, Wiktorowicz, Sloane J., additional, and Wolff, Schuyler G., additional

Published
2014
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48. APODIZED PUPIL LYOT CORONAGRAPHS FOR ARBITRARY APERTURES. III. QUASI-ACHROMATIC SOLUTIONS

Author

Rémi Soummer, Bruce Macintosh, Laurent Pueyo, Anand Sivaramakrishnan, and Ben R. Oppenheimer

Subjects
Physics, business.industry, Astronomy and Astrophysics, Planetary system, law.invention, Starlight, Integral field spectrograph, Optics, Apodization, Space and Planetary Science, Achromatic lens, law, Planet, Gemini Planet Imager, business, Coronagraph
Abstract

Direct imaging and spectroscopy of young giant planets from the ground requires broadband starlight suppression with coronagraphy. It is important to minimize the coronagraph chromatic sensitivity to help remove residual speckles through post-processing of images at multiple wavelengths. The coronagraph must also be able to mitigate the effects of ground-based telescopes with central obstruction. We present new properties of the Apodized Pupil Lyot Coronagraph (APLC) that enable quasi-achromatic starlight suppression over a broad bandpass (20%) and with central obstructions. We discuss the existence of these quasi-achromatic solutions using the properties of the generalized prolate spheroidal functions, which are used to define the apodizer profile. We discuss a broadband optimization method and illustrate its parameter space in terms of inner working angle and contrast. These new APLC solutions are implemented in the Gemini Planet Imager (GPI), a new facility instrument to detect and characterize young giant planets and disks, which will be commissioned in 2011. The coronagraph design delivers a contrast better than 10–7 beyond a separation of 0.2 arcsec in the presence of Gemini's central obstruction over a 20% bandpass. The science camera is an integral field spectrograph observing in one of the Y, J, or H, or in about two-thirds of the K bandpass, at a single time. Similar solutions have also been used for the Palomar 1640 coronagraphic integral field spectrograph.

Published
2011
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50. Gas and Dust Associated with the Strange, Isolated Star BP Piscium

Author

Zuckerman, B., primary, Melis, C., additional, Song, Inseok, additional, Meier, David S., additional, Perrin, Marshall D., additional, Macintosh, Bruce, additional, Marois, Christian, additional, Weinberger, Alycia J., additional, Rhee, Joseph H., additional, Graham, James R., additional, Kastner, Joel H., additional, Palmer, Patrick, additional, Forveille, T., additional, Becklin, E. E., additional, Wilner, D. J., additional, Barman, T. S., additional, Marcy, G. W., additional, and Bessell, M. S., additional

Published
2008
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