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1. The First Flight of the Marshall Grazing Incidence X-Ray Spectrometer (MaGIXS)

Author

Sabrina L. Savage, Amy R. Winebarger, Ken Kobayashi, P. S. Athiray, Dyana Beabout, Leon Golub, Robert W. Walsh, Brent Beabout, Stephen Bradshaw, Alexander R. Bruccoleri, Patrick R. Champey, Peter Cheimets, Jonathan Cirtain, Edward E. DeLuca, Giulio Del Zanna, Jaroslav Dudík, Anthony Guillory, Harlan Haight, Ralf K. Heilmann, Edward Hertz, William Hogue, Jeffery Kegley, Jeffery Kolodziejczak, Chad Madsen, Helen Mason, David E. McKenzie, Jagan Ranganathan, Katharine K. Reeves, Bryan Robertson, Mark L. Schattenburg, Jorg Scholvin, Richard Siler, Paola Testa, Genevieve D. Vigil, Harry P. Warren, Benjamin Watkinson, Bruce Weddendorf, and Ernest Wright

Subjects
Spectroscopy, Solar active regions, Solar x-ray emission, Solar coronal heating, Solar corona, Active solar corona, Astrophysics, QB460-466
Abstract

The Marshall Grazing Incidence X-ray Spectrometer (MaGIXS) sounding rocket experiment launched on 2021 July 30 from the White Sands Missile Range in New Mexico. MaGIXS is a unique solar observing telescope developed to capture X-ray spectral images of coronal active regions in the 6–24 Å wavelength range. Its novel design takes advantage of recent technological advances related to fabricating and optimizing X-ray optical systems, as well as breakthroughs in inversion methodologies necessary to create spectrally pure maps from overlapping spectral images. MaGIXS is the first instrument of its kind to provide spatially resolved soft X-ray spectra across a wide field of view. The plasma diagnostics available in this spectral regime make this instrument a powerful tool for probing solar coronal heating. This paper presents details from the first MaGIXS flight, the captured observations, the data processing and inversion techniques, and the first science results.

Published
2023
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2. The Imaging X-ray Polarimetry Explorer (IXPE)

Author

Martin C. Weisskopf, Brian Ramsey, Stephen L. O’Dell, Allyn Tennant, Ronald Elsner, Paolo Soffita, Ronaldo Bellazzini, Enrico Costa, Jeffery Kolodziejczak, Victoria Kaspi, Fabio Mulieri, Herman Marshall, Giorgio Matt, and Roger Romani

Subjects
Physics, QC1-999
Abstract

The Imaging X-ray Polarimetry Explorer (IXPE) expands observation space by simultaneously adding polarization to the array of X-ray source properties currently measured (energy, time, and location). IXPE will thus open new dimensions for understanding how X-ray emission is produced in astrophysical objects, especially in systems under extreme physical conditions. Keywords: X-ray astronomy, X-ray polarimetry, X-ray imaging

Published
2016
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3. Assembly of the FOXSI-4 Mirror Modules

Author

Stephen D. Bongiorno, Wayne H. Baumgartner, Jeffery Kolodziejczak, Charles G. Davis, Jagan Ranganathan, Nicholas Thomas, Jeff E Mccracken, and Danielle Gurgew

Subjects
Optics
Abstract

The Focusing Optics X-ray Solar Imager 4 (FOXSI 4) is a heliophysics sounding rocket experiment that is currently in its fourth launch campaign. The payload is comprised of seven 2 m focal length X-ray telescopes, which each consist of a grazing incidence mirror module that focuses x-rays onto an imaging detector. For this fourth flight, Marshall Space Flight Center (MSFC) designed, built, and tested three new high-angular-resolution optics. This paper describes the design and assembly of the FOXSI 4 mirror modules.

Published
2023

5. X-ray Polarization Reveals the Precessions of the Neutron Star in Hercules X-1

Author

Jeremy Heyl, Victor Doroshenko, Denis González-Caniulef, Ilaria Caiazzo, Juri Poutanen, Alexander Mushtukov, Sergey Tsygankov, Demet Kirmizibayrak, Matteo Bachetti, George Pavlov, Iván Agudo, Lucio Antonelli, Luca Baldini, Wayne Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolo Di Lalla, Alessandro Di Marco, Immacolata Donnarumma, Michal Dovciak, Steven Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier Garcia, Shuichi Gunji, Wataru Iwakiri, Svetlana Jorstad, Philip Kaaret, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery Kolodziejczak, Henric Krawczynski, Fabio La Monaca, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frederic Marin, Andrea Marinucci, Alan Marscher, Herman Marshall, Francesco Massaro, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Fabio Muleri, Michela Negro, C.-Y. Ng, Stephen O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, Abel Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Simonetta Puccetti, Brian Ramsey, John Rankin, Ajay Ratheesh, Oliver Roberts, Roger Romani, Carmelo Sgro, Patrick Slane, Paolo Soffitta, Gloria Spandre, Doug Swartz, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn Tennant, Nicholas Thomas, Francesco Tombesi, Alessio Trois, Roberto Turolla, Jacco Vink, Martin Weisskopf, Kinwah Wu, Fei Xie, and Silvia Zane

Abstract

In an X-ray pulsar, a neutron star accretes matter from a stellar companion through an accretion disk. The high magnetic field of the rotating neutron star disrupts the inner edge of the disc, funneling the gas to flow onto the magnetic poles on its surface. Hercules X-1 is in many ways the prototypical X-ray pulsar; it shows persistent X-ray emission and it resides with its companion HZ Her, a two-solar-mass star, at about 7~kpc from Earth1. Its emission varies on three distinct timescales2 the neutron star rotates every 1.2~seconds, it is eclipsed by its companion each 1.7~days, and the system exhibits a superorbital period of 35~days which has remained remarkably stable since its discovery3. Several lines of evidence point to the source of this variation as the precession of the accretion disc4,5, the precession of the neutron star6,7 or both8. Despite the many hints over the past fifty years, the precession of the neutron star itself has yet not been confirmed or refuted. We here present X-ray polarization measurements with the Imaging X-ray Polarimetry Explorer9 (IXPE) which probe the spin geometry of the neutron star. These observations provide direct evidence that the 35-day-period is set by the free precession of the neutron star crust, which has the important implication that its moment of inertia eigenvalues differ fractionally by a few parts per ten million10. Furthermore, we find indications that the basic spin geometry of the neutron star is altered by torques on timescale of a few hundred days.

Published
2023
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6. The First Flight of the Marshall Grazing Incidence X-ray Spectrometer (MaGIXS)

Author

Sabrina L. Savage, Amy R. Winebarger, Ken Kobayashi, P. S. Athiray, Dyana Beabout, Leon Golub, Robert W. Walsh, Brent Beabout, Stephen Bradshaw, Alexander R. Bruccoleri, Patrick R. Champey, Peter Cheimets, Jonathan Cirtain, Edward E. DeLuca, Giulio Del Zanna, Jaroslav Dudík, Anthony Guillory, Harlan Haight, Ralf K. Heilmann, Edward Hertz, William Hogue, Jeffery Kegley, Jeffery Kolodziejczak, Chad Madsen, Helen Mason, David E. McKenzie, Jagan Ranganathan, Katharine K. Reeves, Bryan Robertson, Mark L. Schattenburg, Jorg Scholvin, Richard Siler, Paola Testa, Genevieve D. Vigil, Harry P. Warren, Benjamin Watkinson, Bruce Weddendorf, Ernest Wright, Savage, SL [0000-0002-6172-0517], Winebarger, AR [0000-0002-5608-531X], Kobayashi, K [0000-0003-1057-7113], Athiray, PS [0000-0002-4454-147X], Golub, L [0000-0001-9638-3082], Walsh, RW [0000-0002-1025-9863], Bradshaw, S [0000-0002-3300-6041], Bruccoleri, AR [0000-0001-5927-3300], Champey, PR [0000-0002-7139-6191], DeLuca, EE [0000-0001-7416-2895], Del Zanna, G [0000-0002-4125-0204], Dudík, J [0000-0003-1308-7427], Heilmann, RK [0000-0001-9980-5295], Hertz, E [0000-0002-6747-9648], Madsen, C [0000-0001-8775-913X], Mason, H [0000-0002-6418-7914], McKenzie, DE [0000-0002-9921-7757], Reeves, KK [0000-0002-6903-6832], Schattenburg, ML [0000-0001-6932-2612], Testa, P [0000-0002-0405-0668], Vigil, GD [0000-0002-7219-1526], Warren, HP [0000-0001-6102-6851], and Apollo - University of Cambridge Repository

Subjects
Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, 5101 Astronomical Sciences, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 51 Physical Sciences, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

The Marshall Grazing Incidence X-ray Spectrometer (MaGIXS) sounding rocket experiment launched on July 30, 2021 from the White Sands Missile Range in New Mexico. MaGIXS is a unique solar observing telescope developed to capture X-ray spectral images, in the 6 - 24 Angstrom wavelength range, of coronal active regions. Its novel design takes advantage of recent technological advances related to fabricating and optimizing X-ray optical systems as well as breakthroughs in inversion methodologies necessary to create spectrally pure maps from overlapping spectral images. MaGIXS is the first instrument of its kind to provide spatially resolved soft X-ray spectra across a wide field of view. The plasma diagnostics available in this spectral regime make this instrument a powerful tool for probing solar coronal heating. This paper presents details from the first MaGIXS flight, the captured observations, the data processing and inversion techniques, and the first science results., 20 pages, 18 figures

Published
2022

7. When the Milky Way hosted a quasar

Author

Frederic Marin, Eugene Churazov, Ildar Khabibullin, Riccardo Ferrazzoli, Laura Di Gesu, Thibault Barnouin, Alessandro Di Marco, Riccardo Middei, Alexey Vikhlinin, Enrico Costa, Paolo Soffitta, Fabio Muleri, Rashid Sunyaev, William Forman, Ralph Kraft, Stefano Bianchi, Immacolata Donnarumma, Pierre-Olivier Petrucci, Teruaki Enoto, Iván Agudo, Lucio Antonelli, Matteo Bachetti, Luca Baldini, Wayne Baumgartner, Ronaldo Bellazzini, Stephen Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolo Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Niccolo Di Lalla, Victor Doroshenko, Michal Dovciak, Steven Ehlert, Yuri Evangelista, Sergio Fabiani, Javier Garcia, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Adam Ingram, Wataru Iwakiri, Svetlana Jorstad, Philip Kaaret, Vladimir Karas, Takao Kitaguchi, Jeffery Kolodziejczak, Henric Krawczynski, Fabio La Monaca, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Andrea Marinucci, Alan Marscher, Herman Marshall, Francesco Massaro, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Michela Negro, C.-Y. Ng, Stephen O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George Pavlov, Abel Peirson, Matteo Perri, Melissa Pesce-Rollins, Maura Pilia, Andrea Possenti, Juri Poutanen, Simonetta Puccetti, Brian Ramsey, John Rankin, Ajay Ratheesh, Oliver Roberts, Roger Romani, Carmelo Sgro, Patrick Slane, Gloria Spandre, Doug Swartz, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn Tennant, Nicholas Thomas, Francesco Tombesi, Alessio Trois, Sergey Tsygankov, Roberto Turolla, Jacco Vink, Martin Weisskopf, Kinwah Wu, Fei Xie, and Silvia Zane

Abstract

The Galactic Center harbors diffuse X-ray emission co-spatial with giant molecular clouds and featuring hard X-ray spectra with a prominent fluorescent iron line at 6.4 keV [1–3]. These spectral properties are characteristic of the reflected emission from a neutral gas illuminated by X-rays. However, there are no persistent X-ray sources in that region that are bright enough to provide the required illumination level. Moreover, the observed diffuse emission is variable on time scales of years [4, 5], implying that the primary source of X-rays must be variable, too. The most exciting and far-reaching scenario is that a very powerful flare from the central supermassive black hole of the Milky Way, Sgr A*, provided the required flux of X-ray photons, when for a period shorter than a few years it became at least five orders of magnitude brighter than is typically observed today. Even if the primary emission was unpolarized, the reflected emission should be polarized in the direction perpendicular to the scattering plane with the degree of polarization being set by the scattering angle. Therefore, by measuring X-ray polarization one can infer the direction towards the primary source and, simultaneously, the mutual positions in space of the source and the cloud [6]. Here, we report the detection of X-ray polarization from the Galactic Center region obtained by the recently launched Imaging X-ray Polarimetry Explorer (IXPE) mission. For a large region where Chandra and XMM-Newton identify spectral signatures of the reflection, IXPE measures a polarization degree of 31% ± 11% with a polarization angle -48° ± 11° for the scattered continuum. The latter corroborates the conjecture that Sgr A* is the primary source of illuminating photons, while the former implies that some 200 years ago our Galactic Center hosted an extremely bright active galactic nucleus, on par with the ones found in Seyfert galaxies, though only for a short time.

Published
2022
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8. Angling for X-ray pulsar geometry with polarimetry

Author

Victor Doroshenko, Juri Poutanen, Sergey Tsygankov, Valery Suleimanov, Matteo Bachetti, Ilaria Caiazzo, Enrico Costa, Alessandro Di Marco, Jeremy Heyl, Fabio La Monaca, Fabio Muleri, Alexander Mushtukov, George Pavlov, Brian Ramsey, John Rankin, Andrea Santangelo, Paolo Soffitta, Ruediger Staubert, Martin Weisskopf, Silvia Zane, Iván Agudo, Lucio Antonelli, Luca Baldini, Wayne Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen Bongiorno, Raffaella Bonino, Niccolò Bucciantini, Alessandro Brez, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Immacolata Donnarumma, Michal Dovciak, Steven Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana Jorstad, Vladimir Karas, Takao Kitaguchi, Jeffery Kolodziejczak, Henric Krawczynski, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan Marscher, Herman Marshall, Francesco Massaro, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, C.-Y. Ng, Stephen O'Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, Abel Peirson, Matteo Perri, Melissa Pesce-Rollins, Maura Pilia, Andrea Possenti, Simonetta Puccetti, Ajay Ratheesh, Roger Romani, Carmelo Sgro, Patrick Slane, Gloria Spandre, Rashid Sunyaev, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn Tennant, Nicolas Thomas, Francesco Tombesi, Alessio Trois, Roberto Turolla, Jacco Vink, Kinwah Wu, and Fei Xie

Abstract

Using observations of X-ray pulsar Her X-1 by the Imaging X-ray Polarimetry Explorer, we report on a highly significant detection of the polarization signal from an accreting neutron star. The observed degree of the linear polarization of ∼ 10% is found to be far below theoretical expectations for this object, and stays low throughout the spin cycle of the pulsar. Both the polarization degree and the angle exhibit variability with pulse phase, which allowed us to measure the pulsar spin position angle and magnetic obliquity of the neutron star, which is an essential step towards detailed modeling of the intrinsic emission of X-ray pulsars. Combining our results with the optical polarimetric data, we find that the spin axis of the neutron star and the angular momentum of the binary orbit are misaligned by at least ∼20 deg, which is a strong argument in support of the models explaining stability of the observed super-orbital variability with the precession of the neutron star.

Published
2022
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9. Toward the fabrication of a 5-μm-resolution Wolter microscope for the National Ignition Facility (invited)

Author

Patrick R. Champey, Jeffery Kolodziejczak, Bernard Kozioziemski, Jacqueline Davis, Charles Griffith, Tom Kester, Kiranmayee Kilaru, Amy Meekham, Joe Menapace, Brian Ramsey, Oliver J. Roberts, Javier Sanchez, Panini Singam, W. Scott Smith, Chet Speegle, Mark Stahl, Tayyab Suratwala, Nick Thomas, Mark Young, and Julia K. Vogel

Subjects
Instrumentation
Abstract

Advancements in computer-controlled polishing, metrology, and replication have led to an x-ray mirror fabrication process that is capable of producing high-resolution Wolter microscopes. We present the fabrication and test of a nickel–cobalt replicated full-shell x-ray mirror that was electroformed from a finely figured and polished mandrel. This mandrel was designed for an 8-m source-to-detector-distance microscope, with 10× magnification, and was optimized to reduce shell distortions that occur within 20 mm of the shell ends. This, in combination with an improved replication tooling design and refined bath parameters informed by a detailed COMSOL Multiphysics® model, has led to reductions in replication errors in the mirrors. Mandrel surface fabrication was improved by implementing a computer-controlled polishing process that corrected the low-frequency mandrel figure error and achieved

Published
2022
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10. The Imaging X-ray polarimetry explorer (IXPE): Technical overview III

Author

Paolo Soffitta, Primo Attina', Luca Baldini, Mattia Barbanera, Wayne H. Baumgartner, Ronaldo Bellazzini, Jeff Bladt, Stephen D. Bongiorno, Alessandro Brez, Simone Castellano, Rita Carpentiero, Marco Castronuovo, Luca Cavalli, Elisabetta Cavazzuti, Fabio D' Amico, Saverio Citraro, Enrico Costa, William D. Deininger, ELisa D' Alba, Ettore Del Monte, Kutis L. Diets, Niccolo' Di Lalla, Alessandro Di Marco, Guseppe Di Persio, Immacolata Donnarumma, Ronald F. Elsner, Sergio Fabiani, Riccardo Ferrazzoli, Larry Guy, William Kalinowski, Jeffery Kolodziejczak, Luca Latronico, Carlo Lefevre, Paolo Lorenzi, Leonardo Lucchesi, Simone Maldera, Alberto Manfreda, Elio Mangraviti, Herman L. Marshall, James Masciarelli, Giorgio Matt, Massimo Minuti, Fabio Muleri, Hikmat Nasimi, Barbara Negri, Alessio Nuti, Leonardo Orsini, Darren Osborne, Maura Pilia, Matteo Perri, Melissa Pesce-Rollins, Colin Peterson, Michele Pinchera, Simonetta Puccetti, Brian Ramsey, Ajay Ratheesh, Roger W. Romani, Paolo Sarra, Francesco Santoli, Andrea Sciortino, Carmelo Sgro', Brian T. Smith, Gloria Spandre, Allyn F. Tennant, Antonino Tobia, Alessio Trois, Marco Vimercati, Jeffrey Wedmnore, Martin C. Weisskopf, Fei Xie, Francesco Zanetti, Cheryl Alexander, D. Zachery Allen, Fabrizio Amici, L. Angelo Antonelli, Spencer Antoniak, Matteo Bachetti, Raffaella Bonino, Fabio Borotto, Shawn Breeding, Daniele Brienza, H. Kyle Bygott, Claudia Cardelli, Marco Ceccanti, Mauro Centrone, Yuri Evangelista, MacKenzie Ferrie, Brent Forsyth, Michele Foster, Eli Gurnee, Grant Hibbard, Sandra R. Johnson, Erik Kelly, Kiranmayee Kilaru, Fabio La Monaca, Shelley Le Roy, Pasqualino Loffredo, Guido Magazzu', Marco Marengo, Alessandra Marrocchesi, Francesco Massaro, Alfredo Morbidini, Jeffrey McCracken, Michael McEachen, Paolo Mereu, Scott Mitchell, Ikuyuki Mitsuishi, Federico Mosti, Michela Nigro, Chiara Oppedisano, Richard Pacheco, alessandro Paggi, Steven D. Pavelitz, Cristina Pentz, Raffaele Piazzolla, Brad Porter, Alessandro Profeti, Jaganathan Ranganathan, John Rankin, Noah Root, Alda Rubini, Stephanie Ruswick, Javier Sanchez, Emanuele Scalise, Sara Schindhelm, Chet O. Speegle, Toru Tamagawa, Marcello Tardiola, Amy L. Walden, Bruce Weddendorf, David Welch, Michael Head, Stuart Gray, Rondal Mize, Stephen L. O'Dell, Christopher Schroeder, Nicholas E. Thomas, Randy M. Bagget, David Dolan, Kevin Ferrant, Joseph Footdale, Benjamin Garelick, Samantha Johnson, and Timothy Seek

Subjects
Physics, X-ray, Optics, business.industry, X-ray, Polarimetry, Astrophysics, Optics, Gas Pixel Detector, Polarimetry, business, Astrophysics, Gas Pixel Detector
Published
2020

11. Kepler-22b: a 2.4 Earth-radius Planet in the Habitable Zone of a Sun-like Star

Author

William J. Borucki, David G. Koch, Natalie Batalha, Stephen T. Bryson, Jason Rowe, Francois Fressin, Guillermo Torres, Douglas A. Caldwell, Jørgen Christensen-Dalsgaard, William D. Cochran, Edna DeVore, Thomas N. Gautier, John C. Geary, Ronald Gilliland, Alan Gould, Steve B. Howell, Jon M. Jenkins, David W. Latham, Jack J. Lissauer, Geoffrey W. Marcy, Dimitar Sasselov, Alan Boss, David Charbonneau, David Ciardi, Lisa Kaltenegger, Laurance Doyle, Andrea K. Dupree, Eric B. Ford, Jonathan Fortney, Matthew J. Holman, Jason H. Steffen, Fergal Mullally, Martin Still, Jill Tarter, Sarah Ballard, Lars A. Buchhave, Josh Carter, Jessie L. Christiansen, Brice-Olivier Demory, Jean-Michel Désert, Courtney Dressing, Michael Endl, Daniel Fabrycky, Debra Fischer, Michael R. Haas, Christopher Henze, Elliott Horch, Andrew W. Howard, Howard Isaacson, Hans Kjeldsen, John Asher Johnson, Todd Klaus, Jeffery Kolodziejczak, Thomas Barclay, Jie Li, Søren Meibom, Andrej Prsa, Samuel N. Quinn, Elisa V. Quintana, Paul Robertson, William Sherry, Avi Shporer, Peter Tenenbaum, Susan E. Thompson, Joseph D. Twicken, Jeffrey Van Cleve, William F. Welsh, Sarbani Basu, William Chaplin, Andrea Miglio, Steven D. Kawaler, Torben Arentoft, Dennis Stello, Travis S. Metcalfe, Graham A. Verner, Christoffer Karoff, Mia Lundkvist, Mikkel N. Lund, Rasmus Handberg, Yvonne Elsworth, Saskia Hekker, Daniel Huber, Timothy R. Bedding, William Rapin, and Low Energy Astrophysics (API, FNWI)

Subjects
Physics, Earth and Planetary Astrophysics (astro-ph.EP), Kepler-22b, 520 Astronomy, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Radius, Earth radius, Orbit, Photometry (astronomy), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Planet, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Kepler-62e, Circumstellar habitable zone, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract

A search of the time-series photometry from NASA's Kepler spacecraft reveals a transiting planet candidate orbiting the 11th magnitude G5 dwarf KIC 10593626 with a period of 290 days. The characteristics of the host star are well constrained by high-resolution spectroscopy combined with an asteroseismic analysis of the Kepler photometry, leading to an estimated mass and radius of 0.970 +/- 0.060 MSun and 0.979 +/- 0.020 RSun. The depth of 492 +/- 10ppm for the three observed transits yields a radius of 2.38 +/- 0.13 REarth for the planet. The system passes a battery of tests for false positives, including reconnaissance spectroscopy, high-resolution imaging, and centroid motion. A full BLENDER analysis provides further validation of the planet interpretation by showing that contamination of the target by an eclipsing system would rarely mimic the observed shape of the transits. The final validation of the planet is provided by 16 radial velocities obtained with HIRES on Keck 1 over a one year span. Although the velocities do not lead to a reliable orbit and mass determination, they are able to constrain the mass to a 3{\sigma} upper limit of 124 MEarth, safely in the regime of planetary masses, thus earning the designation Kepler-22b. The radiative equilibrium temperature is 262K for a planet in Kepler-22b's orbit. Although there is no evidence that Kepler-22b is a rocky planet, it is the first confirmed planet with a measured radius to orbit in the Habitable Zone of any star other than the Sun., Comment: Accepted to ApJ

Published
2012
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12. Characteristics of Planetary Candidates Observed by Kepler. II. Analysis of the First Four Months of Data

Author

William J. Borucki, David G. Koch, Gibor Basri, Natalie Batalha, Timothy M. Brown, Stephen T. Bryson, Douglas Caldwell, Jørgen Christensen-Dalsgaard, William D. Cochran, Edna DeVore, Edward W. Dunham, Thomas N. Gautier, John C. Geary, Ronald Gilliland, Alan Gould, Steve B. Howell, Jon M. Jenkins, David W. Latham, Jack J. Lissauer, Geoffrey W. Marcy, Jason Rowe, Dimitar Sasselov, Alan Boss, David Charbonneau, David Ciardi, Laurance Doyle, Andrea K. Dupree, Eric B. Ford, Jonathan Fortney, Matthew J. Holman, Sara Seager, Jason H. Steffen, Jill Tarter, William F. Welsh, Christopher Allen, Lars A. Buchhave, Jessie L. Christiansen, Bruce D. Clarke, Santanu Das, Jean-Michel Désert, Michael Endl, Daniel Fabrycky, Francois Fressin, Michael Haas, Elliott Horch, Andrew Howard, Howard Isaacson, Hans Kjeldsen, Jeffery Kolodziejczak, Craig Kulesa, Jie Li, Philip W. Lucas, Pavel Machalek, Donald McCarthy, Phillip MacQueen, Søren Meibom, Thibaut Miquel, Andrej Prsa, Samuel N. Quinn, Elisa V. Quintana, Darin Ragozzine, William Sherry, Avi Shporer, Peter Tenenbaum, Guillermo Torres, Joseph D. Twicken, Jeffrey Van Cleve, Lucianne Walkowicz, Fred C. Witteborn, and Martin Still

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Radius, 01 natural sciences, Earth radius, Physics::Geophysics, Jupiter, Kepler-47, 13. Climate action, Space and Planetary Science, Physics::Space Physics, 0103 physical sciences, Kepler-62, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Circumstellar habitable zone, Kepler-62e, Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences, Kepler-62c
Abstract

On 1 February 2011 the Kepler Mission released data for 156,453 stars observed from the beginning of the science observations on 2 May through 16 September 2009. There are 1235 planetary candidates with transit like signatures detected in this period. These are associated with 997 host stars. Distributions of the characteristics of the planetary candidates are separated into five class-sizes; 68 candidates of approximately Earth-size (radius < 1.25 Earth radii), 288 super-Earth size (1.25 Earth radii < radius < 2 Earth radii), 662 Neptune-size (2 Earth radii < radius < 6 Earth radii), 165 Jupiter-size (6 Earth radii < radius < 15 Earth radii), and 19 up to twice the size of Jupiter (15 Earth radii < radius < 22 Earth radii). In the temperature range appropriate for the habitable zone, 54 candidates are found with sizes ranging from Earth-size to larger than that of Jupiter. Five are less than twice the size of the Earth. Over 74% of the planetary candidates are smaller than Neptune. The observed number versus size distribution of planetary candidates increases to a peak at two to three times Earth-size and then declines inversely proportional to area of the candidate. Our current best estimates of the intrinsic frequencies of planetary candidates, after correcting for geometric and sensitivity biases, are 6% for Earth-size candidates, 7% for super-Earth size candidates, 17% for Neptune-size candidates, and 4% for Jupiter-size candidates. Multi-candidate, transiting systems are frequent; 17% of the host stars have multi-candidate systems, and 33.9% of all the candidates are part of multi-candidate systems., 106 pages, 15 figures, contains tables of candidates. Submitted to ApJ

Published
2011
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13. CHARACTERISTICS OFKEPLERPLANETARY CANDIDATES BASED ON THE FIRST DATA SET

Author

William J. Borucki, David G. Koch, Gibor Basri, Natalie Batalha, Alan Boss, Timothy M. Brown, Douglas Caldwell, Jørgen Christensen-Dalsgaard, William D. Cochran, Edna DeVore, Edward W. Dunham, Andrea K. Dupree, Thomas N. Gautier III, John C. Geary, Ronald Gilliland, Alan Gould, Steve B. Howell, Jon M. Jenkins, Hans Kjeldsen, David W. Latham, Jack J. Lissauer, Geoffrey W. Marcy, David G. Monet, Dimitar Sasselov, Jill Tarter, David Charbonneau, Laurance Doyle, Eric B. Ford, Jonathan Fortney, Matthew J. Holman, Sara Seager, Jason H. Steffen, William F. Welsh, Christopher Allen, Stephen T. Bryson, Lars Buchhave, Hema Chandrasekaran, Jessie L. Christiansen, David Ciardi, Bruce D. Clarke, Jessie L. Dotson, Michael Endl, Debra Fischer, Francois Fressin, Michael Haas, Elliott Horch, Andrew Howard, Howard Isaacson, Jeffery Kolodziejczak, Jie Li, Phillip MacQueen, Søren Meibom, Andrej Prsa, Elisa V. Quintana, Jason Rowe, William Sherry, Peter Tenenbaum, Guillermo Torres, Joseph D. Twicken, Jeffrey Van Cleve, Lucianne Walkowicz, and Hayley Wu

Subjects
Physics, Astronomy, Astronomy and Astrophysics, Kepler, Exoplanet, Data set, Jupiter, Stars, Photometry (astronomy), Space and Planetary Science, Neptune, Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

In the spring of 2009, the Kepler Mission commenced high-precision photometry on nearly 156,000 stars to determine the frequency and characteristics of small exoplanets, conduct a guest observer program, and obtain asteroseismic data on a wide variety of stars. On 15 June 2010 the Kepler Mission released data from the first quarter of observations. At the time of this publication, 706 stars from this first data set have exoplanet candidates with sizes from as small as that of the Earth to larger than that of Jupiter. Here we give the identity and characteristics of 306 released stars with planetary candidates. Data for the remaining 400 stars with planetary candidates will be released in February 2011. Over half the candidates on the released list have radii less than half that of Jupiter. The released stars include five possible multi-planet systems. One of these has two Neptune-size (2.3 and 2.5 Earth-radius) candidates with near-resonant periods.

Published
2011
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15. CHARACTERIZATION OF THE INNER KNOT OF THE CRAB: THE SITE OF THE GAMMA-RAY FLARES?

Author

Alexander Rudy, Dieter Horns, Andrea DeLuca, Jeffery Kolodziejczak, Allyn Tennant, Yajie Yuan, Rolf Buehler, Jonathon Arons, Roger Blandford, Patrizia Caraveo, Enrico Costa, Stephan Funk, Elizabeth Hays, Andrei Lobanov, Claire Max, Michael Mayer, Roberto Mignani, Stephen L. O’Dell, Roger Romani, and Marco Tavani

Subjects
CRAB Nebula, NEBULAE, SUPERNOVA 1054, PULSARS, PULSATING stars
Abstract

A particularly intriguing recent result from γ-ray astronomy missions is the detection of powerful flares from the Crab Nebula, which challenges the current understanding of pulsar wind nebulae and acceleration mechanisms. To search for the production site(s) of these flares, we conducted a multi-wavelength observing campaign using Keck, the Hubble Space Telescope (HST), and the Chandra X-ray Observatory. As the short timescales of the γ-ray flares ( day) suggest a small emitting region, the Crab’s inner knot (about 0.6 arcsec from the pulsar) is a candidate site for such flaring. This paper describes observations of the inner knot, seeking to understand its nature and possible relationship with γ-ray flares. Using singular-value decomposition, analysis of the HST images yielded results consistent with traditional methods while substantially reducing some uncertainties. These analyses show that the knot’s intrinsic properties (especially size and brightness) are correlated with its (projected) separation from the pulsar. This characterization of the inner knot helps in constraining standard shock model parameters, under the assumption that the knot lies near the shocked surface. While the standard shock model gives good agreement in several respects, two puzzles persist: (a) the observed angular size of the knot relative to the pulsar–knot separation is much smaller than expected; and (b) the variable high degree of polarization (reported by others) is difficult to reconcile with a highly relativistic downstream flow. However, the IR–optical flux of the inner knot is marginally consistent with the shock accelerating most of the Nebula’s optical-emitting particles. [ABSTRACT FROM AUTHOR]

Published
2015
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