Author
Katie M. Morzinski
Other affiliations: National Science Foundation, Lawrence Livermore National Laboratory, University of California, Santa Cruz
Bio: Katie M. Morzinski is an academic researcher from University of Arizona. The author has contributed to research in topics: Exoplanet & Adaptive optics. The author has an hindex of 55, co-authored 215 publications receiving 9280 citations. Previous affiliations of Katie M. Morzinski include National Science Foundation & Lawrence Livermore National Laboratory.
Papers published on a yearly basis
Papers
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Stanford University1, Lawrence Livermore National Laboratory2, University of California, Berkeley3, University of Toronto4, National Research Council5, Space Telescope Science Institute6, University of Arizona7, Princeton University8, University of California, Los Angeles9, Arizona State University10, University of California, Santa Cruz11, Université de Montréal12, Search for extraterrestrial intelligence13, Ames Research Center14, American Museum of Natural History15, Cornell University16, University of Georgia17, California Institute of Technology18, Johns Hopkins University19
TL;DR: Observations ofBeta Pictoris clearly detect the planet, Beta Pictoris b, in a single 60-s exposure with minimal postprocessing, and fitting the Keplerian orbit of Beta Pic b using the new position together with previous astrometry gives a factor of 3 improvement in most parameters over previous solutions.
Abstract: The Gemini Planet Imager is a dedicated facility for directly imaging and spectroscopically characterizing extrasolar planets. It combines a very high-order adaptive optics system, a diffraction-suppressing coronagraph, and an integral field spectrograph with low spectral resolution but high spatial resolution. Every aspect of the Gemini Planet Imager has been tuned for maximum sensitivity to faint planets near bright stars. During first-light observations, we achieved an estimated H band Strehl ratio of 0.89 and a 5-σ contrast of 10(6) at 0.75 arcseconds and 10(5) at 0.35 arcseconds. Observations of Beta Pictoris clearly detect the planet, Beta Pictoris b, in a single 60-s exposure with minimal postprocessing. Beta Pictoris b is observed at a separation of 434 ± 6 milliarcseconds (mas) and position angle 211.8 ± 0.5°. Fitting the Keplerian orbit of Beta Pic b using the new position together with previous astrometry gives a factor of 3 improvement in most parameters over previous solutions. The planet orbits at a semimajor axis of [Formula: see text] near the 3:2 resonance with the previously known 6-AU asteroidal belt and is aligned with the inner warped disk. The observations give a 4% probability of a transit of the planet in late 2017.
754 citations
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Lawrence Livermore National Laboratory1, Stanford University2, University of California, Berkeley3, University of Arizona4, University of California, San Diego5, Ames Research Center6, University of Victoria7, Herzberg Institute of Astrophysics8, Space Telescope Science Institute9, Arizona State University10, Université de Montréal11, Los Alamos National Laboratory12, University of California, Los Angeles13, University of Western Ontario14, Subaru15, University of Hertfordshire16, Princeton University17, University of Toronto18, Centre national de la recherche scientifique19, University of Chicago20, University of California, Santa Cruz21, Durham University22, University of Exeter23, University of Georgia24, Stony Brook University25, University of California, Santa Barbara26, American Museum of Natural History27, University of Chile28, Universities Space Research Association29, Cornell University30, University of Toledo31, California Institute of Technology32
TL;DR: Using the Gemini Planet Imager, a Jupiter-like planet is discovered orbiting the ~20-million-year-old star 51 Eridani at a projected separation of 13 astronomical units and has a methane signature and is probably the smallest exoplanet that has been directly imaged.
Abstract: Directly detecting thermal emission from young extrasolar planets allows measurement of their atmospheric compositions and luminosities, which are influenced by their formation mechanisms. Using the Gemini Planet Imager, we discovered a planet orbiting the ~20-million-year-old star 51 Eridani at a projected separation of 13 astronomical units. Near-infrared observations show a spectrum with strong methane and water-vapor absorption. Modeling of the spectra and photometry yields a luminosity (normalized by the luminosity of the Sun) of 1.6 to 4.0 × 10(-6) and an effective temperature of 600 to 750 kelvin. For this age and luminosity, "hot-start" formation models indicate a mass twice that of Jupiter. This planet also has a sufficiently low luminosity to be consistent with the "cold-start" core-accretion process that may have formed Jupiter.
575 citations
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Stanford University1, Lawrence Livermore National Laboratory2, University of California, Berkeley3, University of Arizona4, University of California, San Diego5, Ames Research Center6, Herzberg Institute of Astrophysics7, University of Victoria8, Space Telescope Science Institute9, Arizona State University10, Université de Montréal11, Los Alamos National Laboratory12, University of California, Los Angeles13, University of Western Ontario14, Subaru15, University of Hertfordshire16, Princeton University17, University of Toronto18, Centre national de la recherche scientifique19, University of Chicago20, University of California, Santa Cruz21, Durham University22, University of Exeter23, University of Georgia24, Stony Brook University25, University of California, Santa Barbara26, American Museum of Natural History27, University of Chile28, Universities Space Research Association29, Cornell University30, University of Toledo31, California Institute of Technology32
TL;DR: In this paper, the Gemini Planet Imager was used to detect a planet orbiting the star 51 Eridani at a projected separation of 13 astronomical units, with a spectrum with strong methane and water vapor absorption.
Abstract: Directly detecting thermal emission from young extrasolar planets allows measurement of their atmospheric composition and luminosity, which is influenced by their formation mechanism. Using the Gemini Planet Imager, we discovered a planet orbiting the \$sim$20 Myr-old star 51 Eridani at a projected separation of 13 astronomical units. Near-infrared observations show a spectrum with strong methane and water vapor absorption. Modeling of the spectra and photometry yields a luminosity of L/LS=1.6-4.0 x 10-6 and an effective temperature of 600-750 K. For this age and luminosity, "hot-start" formation models indicate a mass twice that of Jupiter. This planet also has a sufficiently low luminosity to be consistent with the "cold- start" core accretion process that may have formed Jupiter.
375 citations
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TL;DR: In this paper, adaptive optics observations of LkCa 15 that probe within the disk clearing are reported, with accurate source positions over multiple epochs spanning 2009-2015, infer the presence of multiple companions on Keplerian orbits.
Abstract: Exoplanet detections have revolutionized astronomy, offering new insights into solar system architecture and planet demographics. While nearly 1,900 exoplanets have now been discovered and confirmed, none are still in the process of formation. Transition disks, protoplanetary disks with inner clearings best explained by the influence of accreting planets, are natural laboratories for the study of planet formation. Some transition disks show evidence for the presence of young planets in the form of disk asymmetries or infrared sources detected within their clearings, as in the case of LkCa 15 (refs 8, 9). Attempts to observe directly signatures of accretion onto protoplanets have hitherto proven unsuccessful. Here we report adaptive optics observations of LkCa 15 that probe within the disk clearing. With accurate source positions over multiple epochs spanning 2009-2015, we infer the presence of multiple companions on Keplerian orbits. We directly detect Hα emission from the innermost companion, LkCa 15 b, evincing hot (about 10,000 kelvin) gas falling deep into the potential well of an accreting protoplanet.
356 citations
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Stanford University1, University of California, Berkeley2, California Institute of Technology3, Ames Research Center4, Los Alamos National Laboratory5, Cornell University6, Lawrence Livermore National Laboratory7, University of Arizona8, National Research Council9, National Institutes of Natural Sciences, Japan10, Princeton University11, University of Notre Dame12, University of Georgia13, Université de Montréal14, University of Grenoble15, University of Chicago16, University of California, Los Angeles17, Amherst College18, University of California, Santa Cruz19, University of Victoria20, University of Michigan21, European Southern Observatory22, University of Exeter23, Arizona State University24, United States Geological Survey25, Pennsylvania State University26, Search for extraterrestrial intelligence27, University of California, San Diego28, Stony Brook University29, University of Western Ontario30, American Museum of Natural History31, Space Telescope Science Institute32, University of Cambridge33, Johns Hopkins University34, Leiden University35
TL;DR: Nielsen et al. as discussed by the authors presented a statistical analysis of the first 300 stars observed by the Gemini Planet Imager Exoplanet Survey (GPEES) to infer the underlying distributions of substellar companions with respect to their mass, semimajor axis, and host stellar mass.
Abstract: Author(s): Nielsen, EL; De Rosa, RJ; Macintosh, B; Wang, JJ; Ruffio, JB; Chiang, E; Marley, MS; Saumon, D; Savransky, D; Mark Ammons, S; Bailey, VP; Barman, T; Blain, C; Bulger, J; Burrows, A; Chilcote, J; Cotten, T; Czekala, I; Doyon, R; Duchene, G; Esposito, TM; Fabrycky, D; Fitzgerald, MP; Follette, KB; Fortney, JJ; Gerard, BL; Goodsell, SJ; Graham, JR; Greenbaum, AZ; Hibon, P; Hinkley, S; Hirsch, LA; Hom, J; Hung, LW; Ilene Dawson, R; Ingraham, P; Kalas, P; Konopacky, Q; Larkin, JE; Lee, EJ; Lin, JW; Maire, J; Marchis, F; Marois, C; Metchev, S; Millar-Blanchaer, MA; Morzinski, KM; Oppenheimer, R; Palmer, D; Patience, J; Perrin, M; Poyneer, L; Pueyo, L; Rafikov, RR; Rajan, A; Rameau, J; Rantakyro, FT; Ren, B; Schneider, AC; Sivaramakrishnan, A; Song, I; Soummer, R; Tallis, M; Thomas, S; Ward-Duong, K; Wolff, S | Abstract: We present a statistical analysis of the first 300 stars observed by the Gemini Planet Imager Exoplanet Survey. 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, semimajor axis, and host stellar mass. We uncover a strong correlation between planet occurrence rate and host star mass, with stars M ∗ g1.5 M o more likely to host planets with masses between 2 and 13M Jup and semimajor axes of 3-100 au at 99.92% confidence. We fit a double power-law model in planet mass (m) and semimajor axis (a) for planet populations around high-mass stars (M ∗ g1.5 M o) of the form , finding α = -2.4 +0.8 and β = -2.0 +0.5, and an integrated occurrence rate of % between 5-13M Jup and 10-100 au. A significantly lower occurrence rate is obtained for brown dwarfs around all stars, with % of stars hosting a brown dwarf companion between 13-80M Jup and 10-100 au. Brown dwarfs also appear to be distributed differently in mass and semimajor axis compared to giant planets; whereas giant planets follow a bottom-heavy mass distribution and favor smaller semimajor axes, brown dwarfs exhibit just the opposite behaviors. Comparing to studies of short-period giant planets from the radial velocity method, our results are consistent with a peak in occurrence of giant planets between ∼1 and 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.
318 citations
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1,288 citations
01 Sep 1998
TL;DR: A stellar spectral flux library of wide spectral coverage and an example of its application are presented in this paper, which consists of 131 flux-calibrated spectra, encompassing all normal spectral types and luminosity classes at solar abundance, and metal-weak and metalrich F-K dwarf and G-K giant components.
Abstract: A stellar spectral flux library of wide spectral coverage and an example of its application are presented. The new library consists of 131 flux-calibrated spectra, encompassing all normal spectral types and luminosity classes at solar abundance, and metal-weak and metal-rich F-K dwarf and G-K giant components. Each library spectrum was formed by combining data from several sources overlapping in wavelength coverage. The SIMBAD database, measured colors, and line strengths were used to check that each input component has closely similar stellar type. The library has complete spectral coverage from 1150 to 10620 Afor all components and to 25000 Afor about half of them, mainly later types of solar abundance. Missing spectral coverage in the infrared currently consists of a smooth energy distribution formed from standard colors for the relevant types. The library is designed to permit inclusion of additional digital spectra, particularly of non-solar abundance stars in the infrared, as they become available. The library spectra are each given as Fl versus l, from 1150 to 25000 Ain steps of 5 A ˚. A program to combine the library spectra in the ratios appropriate to a selected isochrone is described and an example of a spectral component signature of a composite population of solar age and metallicity is illustrated. The library spectra and associated tables are available as text files by remote electronic access.
999 citations
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TL;DR: A review of the current knowledge of the occurrence of planets around other stars, their orbital distances and eccentricities, the orbital spacings and mutual inclinations in multi-planet systems, the orientation of the host star's rotation axis, and the properties of planets in binary-star systems can be found in this paper.
Abstract: The basic geometry of the Solar System—the shapes, spacings, and orientations of the planetary orbits—has long been a subject of fascination as well as inspiration for planet-formation theories. For exoplanetary systems, those same properties have only recently come into focus. Here we review our current knowledge of the occurrence of planets around other stars, their orbital distances and eccentricities, the orbital spacings and mutual inclinations in multiplanet systems, the orientation of the host star's rotation axis, and the properties of planets in binary-star systems.
824 citations
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Stanford University1, Lawrence Livermore National Laboratory2, University of California, Berkeley3, University of Toronto4, National Research Council5, Space Telescope Science Institute6, University of Arizona7, Princeton University8, University of California, Los Angeles9, Arizona State University10, University of California, Santa Cruz11, Université de Montréal12, Search for extraterrestrial intelligence13, Ames Research Center14, American Museum of Natural History15, Cornell University16, University of Georgia17, California Institute of Technology18, Johns Hopkins University19
TL;DR: Observations ofBeta Pictoris clearly detect the planet, Beta Pictoris b, in a single 60-s exposure with minimal postprocessing, and fitting the Keplerian orbit of Beta Pic b using the new position together with previous astrometry gives a factor of 3 improvement in most parameters over previous solutions.
Abstract: The Gemini Planet Imager is a dedicated facility for directly imaging and spectroscopically characterizing extrasolar planets. It combines a very high-order adaptive optics system, a diffraction-suppressing coronagraph, and an integral field spectrograph with low spectral resolution but high spatial resolution. Every aspect of the Gemini Planet Imager has been tuned for maximum sensitivity to faint planets near bright stars. During first-light observations, we achieved an estimated H band Strehl ratio of 0.89 and a 5-σ contrast of 10(6) at 0.75 arcseconds and 10(5) at 0.35 arcseconds. Observations of Beta Pictoris clearly detect the planet, Beta Pictoris b, in a single 60-s exposure with minimal postprocessing. Beta Pictoris b is observed at a separation of 434 ± 6 milliarcseconds (mas) and position angle 211.8 ± 0.5°. Fitting the Keplerian orbit of Beta Pic b using the new position together with previous astrometry gives a factor of 3 improvement in most parameters over previous solutions. The planet orbits at a semimajor axis of [Formula: see text] near the 3:2 resonance with the previously known 6-AU asteroidal belt and is aligned with the inner warped disk. The observations give a 4% probability of a transit of the planet in late 2017.
754 citations
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Lawrence Livermore National Laboratory1, Stanford University2, University of California, Berkeley3, University of Arizona4, University of California, San Diego5, Ames Research Center6, University of Victoria7, Herzberg Institute of Astrophysics8, Space Telescope Science Institute9, Arizona State University10, Université de Montréal11, Los Alamos National Laboratory12, University of California, Los Angeles13, University of Western Ontario14, Subaru15, University of Hertfordshire16, Princeton University17, University of Toronto18, Centre national de la recherche scientifique19, University of Chicago20, University of California, Santa Cruz21, Durham University22, University of Exeter23, University of Georgia24, Stony Brook University25, University of California, Santa Barbara26, American Museum of Natural History27, University of Chile28, Universities Space Research Association29, Cornell University30, University of Toledo31, California Institute of Technology32
TL;DR: Using the Gemini Planet Imager, a Jupiter-like planet is discovered orbiting the ~20-million-year-old star 51 Eridani at a projected separation of 13 astronomical units and has a methane signature and is probably the smallest exoplanet that has been directly imaged.
Abstract: Directly detecting thermal emission from young extrasolar planets allows measurement of their atmospheric compositions and luminosities, which are influenced by their formation mechanisms. Using the Gemini Planet Imager, we discovered a planet orbiting the ~20-million-year-old star 51 Eridani at a projected separation of 13 astronomical units. Near-infrared observations show a spectrum with strong methane and water-vapor absorption. Modeling of the spectra and photometry yields a luminosity (normalized by the luminosity of the Sun) of 1.6 to 4.0 × 10(-6) and an effective temperature of 600 to 750 kelvin. For this age and luminosity, "hot-start" formation models indicate a mass twice that of Jupiter. This planet also has a sufficiently low luminosity to be consistent with the "cold-start" core-accretion process that may have formed Jupiter.
575 citations