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Investigating the Unusual Spectroscopic Time-Evolution in SN 2012Fr∗
Draft version October 4, 2018 Typeset using LATEX default style in AASTeX62 Investigating the Unusual Spectroscopic Time-Evolution in SN 2012fr∗ Christopher Cain,1, 2, 3 E. Baron,2, 4, 5 M. M. Phillips,6 Carlos Contreras,7, 8 Chris Ashall,9 Maximilian D. Stritzinger,8 Christopher R. Burns,10 Anthony L. Piro,10 Eric Y. Hsiao,9, 7, 8 P. Hoeflich,9 Kevin Krisciunas,11 and Nicholas B. Suntzeff11 1Azusa Pacific University 901 E Alosta Ave, Azusa, California, 91702, USA 2University of Oklahoma 440 W. Brooks, Rm 100, Norman, Oklahoma, 73019, USA 3Department of Physics and Astronomy, University of California, Riverside, CA 92521, USA 4Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg, Germany 5Visiting Astronomer, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark. 6Las Campanas Observatory, Carnegie Observatories Casilla 601, La Serena, Chile 7Las Campanas Observatory, Carnegie Observatories, Casilla 601, La Serena, Chile 8Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark. 9Department of Physics, Florida State University, Tallahassee, FL 32306, USA 10Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA 91101, USA 11George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Department of Physics and Astronomy, Texas A&M University, College Station, TX 77843, USA (Received ; Revised ; Accepted ) Submitted to ApJ ABSTRACT The type Ia supernova (SN) 2012fr displayed an unusual combination of its Si II λλ5972, 6355 fea- tures. This includes the ratio of their pseudo equivalent widths, placing it at the border of the Shallow Silicon (SS) and Core Normal (CN) spectral subtype in the Branch diagram, while the Si IIλ6355 expansion velocities places it as a High-Velocity (HV) object in the Wang et al. -
Curriculum Vitae - 24 March 2020
Dr. Eric E. Mamajek Curriculum Vitae - 24 March 2020 Jet Propulsion Laboratory Phone: (818) 354-2153 4800 Oak Grove Drive FAX: (818) 393-4950 MS 321-162 [email protected] Pasadena, CA 91109-8099 https://science.jpl.nasa.gov/people/Mamajek/ Positions 2020- Discipline Program Manager - Exoplanets, Astro. & Physics Directorate, JPL/Caltech 2016- Deputy Program Chief Scientist, NASA Exoplanet Exploration Program, JPL/Caltech 2017- Professor of Physics & Astronomy (Research), University of Rochester 2016-2017 Visiting Professor, Physics & Astronomy, University of Rochester 2016 Professor, Physics & Astronomy, University of Rochester 2013-2016 Associate Professor, Physics & Astronomy, University of Rochester 2011-2012 Associate Astronomer, NOAO, Cerro Tololo Inter-American Observatory 2008-2013 Assistant Professor, Physics & Astronomy, University of Rochester (on leave 2011-2012) 2004-2008 Clay Postdoctoral Fellow, Harvard-Smithsonian Center for Astrophysics 2000-2004 Graduate Research Assistant, University of Arizona, Astronomy 1999-2000 Graduate Teaching Assistant, University of Arizona, Astronomy 1998-1999 J. William Fulbright Fellow, Australia, ADFA/UNSW School of Physics Languages English (native), Spanish (advanced) Education 2004 Ph.D. The University of Arizona, Astronomy 2001 M.S. The University of Arizona, Astronomy 2000 M.Sc. The University of New South Wales, ADFA, Physics 1998 B.S. The Pennsylvania State University, Astronomy & Astrophysics, Physics 1993 H.S. Bethel Park High School Research Interests Formation and Evolution -
Curriculum Vitae Avishay Gal-Yam
January 27, 2017 Curriculum Vitae Avishay Gal-Yam Personal Name: Avishay Gal-Yam Current address: Department of Particle Physics and Astrophysics, Weizmann Institute of Science, 76100 Rehovot, Israel. Telephones: home: 972-8-9464749, work: 972-8-9342063, Fax: 972-8-9344477 e-mail: [email protected] Born: March 15, 1970, Israel Family status: Married + 3 Citizenship: Israeli Education 1997-2003: Ph.D., School of Physics and Astronomy, Tel-Aviv University, Israel. Advisor: Prof. Dan Maoz 1994-1996: B.Sc., Magna Cum Laude, in Physics and Mathematics, Tel-Aviv University, Israel. (1989-1993: Military service.) Positions 2013- : Head, Physics Core Facilities Unit, Weizmann Institute of Science, Israel. 2012- : Associate Professor, Weizmann Institute of Science, Israel. 2008- : Head, Kraar Observatory Program, Weizmann Institute of Science, Israel. 2007- : Visiting Associate, California Institute of Technology. 2007-2012: Senior Scientist, Weizmann Institute of Science, Israel. 2006-2007: Postdoctoral Scholar, California Institute of Technology. 2003-2006: Hubble Postdoctoral Fellow, California Institute of Technology. 1996-2003: Physics and Mathematics Research and Teaching Assistant, Tel Aviv University. Honors and Awards 2012: Kimmel Award for Innovative Investigation. 2010: Krill Prize for Excellence in Scientific Research. 2010: Isreali Physical Society (IPS) Prize for a Young Physicist (shared with E. Nakar). 2010: German Federal Ministry of Education and Research (BMBF) ARCHES Prize. 2010: Levinson Physics Prize. 2008: The Peter and Patricia Gruber Award. 2007: European Union IRG Fellow. 2006: “Citt`adi Cefal`u"Prize. 2003: Hubble Fellow. 2002: Tel Aviv U. School of Physics and Astronomy award for outstanding achievements. 2000: Colton Fellow. 2000: Tel Aviv U. School of Physics and Astronomy research and teaching excellence award. -
In-Depth Study of Photometric Variability and Radiative Timescales for Atmospheric Evolution in Four L Dwarfs
Weather on Other Worlds IV: In-Depth Study of Photometric Variability and Radiative Timescales for Atmospheric Evolution in Four L Dwarfs Item Type text; Electronic Thesis Authors Flateau, Davin C. Publisher The University of Arizona. Rights Copyright © is held by the author. Digital access to this material is made possible by the University Libraries, University of Arizona. Further transmission, reproduction or presentation (such as public display or performance) of protected items is prohibited except with permission of the author. Download date 30/09/2021 07:25:39 Link to Item http://hdl.handle.net/10150/594630 WEATHER ON OTHER WORLDS IV: IN-DEPTH STUDY OF PHOTOMETRIC VARIABILITY AND RADIATIVE TIMESCALES FOR ATMOSPHERIC EVOLUTION IN FOUR L DWARFS by Davin C. Flateau A Thesis Submitted to the Faculty of the DEPARTMENT OF PLANETARY SCIENCES In Partial Fulfillment of the Requirements For the Degree of MASTER OF SCIENCE In the Graduate College THE UNIVERSITY OF ARIZONA 2015 2 STATEMENT BY AUTHOR This thesis has been submitted in partial fulfillment of requirements for an advanced degree at the University of Arizona and is deposited in the University Library to be made available to borrowers under rules of the Library. Brief quotations from this thesis are allowable without special permission, provided that accurate acknowledgment of the source is made. Requests for permission for extended quotation from or reproduction of this manuscript in whole or in part may be granted by the head of the major department or the Dean of the Graduate College when in his or her judgment the proposed use of the material is in the interests of scholarship. -
A Review on Substellar Objects Below the Deuterium Burning Mass Limit: Planets, Brown Dwarfs Or What?
geosciences Review A Review on Substellar Objects below the Deuterium Burning Mass Limit: Planets, Brown Dwarfs or What? José A. Caballero Centro de Astrobiología (CSIC-INTA), ESAC, Camino Bajo del Castillo s/n, E-28692 Villanueva de la Cañada, Madrid, Spain; [email protected] Received: 23 August 2018; Accepted: 10 September 2018; Published: 28 September 2018 Abstract: “Free-floating, non-deuterium-burning, substellar objects” are isolated bodies of a few Jupiter masses found in very young open clusters and associations, nearby young moving groups, and in the immediate vicinity of the Sun. They are neither brown dwarfs nor planets. In this paper, their nomenclature, history of discovery, sites of detection, formation mechanisms, and future directions of research are reviewed. Most free-floating, non-deuterium-burning, substellar objects share the same formation mechanism as low-mass stars and brown dwarfs, but there are still a few caveats, such as the value of the opacity mass limit, the minimum mass at which an isolated body can form via turbulent fragmentation from a cloud. The least massive free-floating substellar objects found to date have masses of about 0.004 Msol, but current and future surveys should aim at breaking this record. For that, we may need LSST, Euclid and WFIRST. Keywords: planetary systems; stars: brown dwarfs; stars: low mass; galaxy: solar neighborhood; galaxy: open clusters and associations 1. Introduction I can’t answer why (I’m not a gangstar) But I can tell you how (I’m not a flam star) We were born upside-down (I’m a star’s star) Born the wrong way ’round (I’m not a white star) I’m a blackstar, I’m not a gangstar I’m a blackstar, I’m a blackstar I’m not a pornstar, I’m not a wandering star I’m a blackstar, I’m a blackstar Blackstar, F (2016), David Bowie The tenth star of George van Biesbroeck’s catalogue of high, common, proper motion companions, vB 10, was from the end of the Second World War to the early 1980s, and had an entry on the least massive star known [1–3]. -
Asymmetries in Sn 2014J Near Maximum Light Revealed Through Spectropolarimetry
ASYMMETRIES IN SN 2014J NEAR MAXIMUM LIGHT REVEALED THROUGH SPECTROPOLARIMETRY Item Type Article Authors Porter, Amber; Leising, Mark D.; Williams, G. Grant; Milne, P. A.; Smith, Paul; Smith, Nathan; Bilinski, Christopher; Hoffman, Jennifer L.; Huk, Leah; Leonard, Douglas C. Citation ASYMMETRIES IN SN 2014J NEAR MAXIMUM LIGHT REVEALED THROUGH SPECTROPOLARIMETRY 2016, 828 (1):24 The Astrophysical Journal DOI 10.3847/0004-637X/828/1/24 Publisher IOP PUBLISHING LTD Journal The Astrophysical Journal Rights © 2016. The American Astronomical Society. All rights reserved. Download date 27/09/2021 22:28:24 Item License http://rightsstatements.org/vocab/InC/1.0/ Version Final published version Link to Item http://hdl.handle.net/10150/622057 The Astrophysical Journal, 828:24 (12pp), 2016 September 1 doi:10.3847/0004-637X/828/1/24 © 2016. The American Astronomical Society. All rights reserved. ASYMMETRIES IN SN 2014J NEAR MAXIMUM LIGHT REVEALED THROUGH SPECTROPOLARIMETRY Amber L. Porter1, Mark D. Leising1, G. Grant Williams2,3, Peter Milne2, Paul Smith2, Nathan Smith2, Christopher Bilinski2, Jennifer L. Hoffman4, Leah Huk4, and Douglas C. Leonard5 1 Department of Physics and Astronomy, Clemson University, 118 Kinard Laboratory, Clemson, SC 29634, USA; [email protected] 2 Steward Observatory, University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721, USA 3 MMT Observatory, P.O. Box 210065, University of Arizona, Tucson, AZ 85721-0065, USA 4 Department of Physics and Astronomy, University of Denver, 2112 East Wesley Avenue, Denver, CO 80208, USA 5 Department of Astronomy, San Diego State University, PA-210, 5500 Campanile Drive, San Diego, CA 92182-1221, USA Received 2016 February 14; revised 2016 May 11; accepted 2016 May 12; published 2016 August 24 ABSTRACT We present spectropolarimetric observations of the nearby Type Ia supernova SN 2014J in M82 over six epochs: +0, +7, +23, +51, +77, +109, and +111 days with respect to B-band maximum. -
Updated Astrometry and Masses of the LUH 16 Brown Dwarf Binary
Astronomy & Astrophysics manuscript no. 33626_corr_LAZ c ESO 2018 August 24, 2018 Updated astrometry and masses of the LUH 16 brown dwarf binary P. F. Lazorenko1 and J. Sahlmann2 1 Main Astronomical Observatory, National Academy of Sciences of the Ukraine, Zabolotnogo 27, 03680 Kyiv, Ukraine e-mail: [email protected] 2 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA Received ; accepted ABSTRACT The nearest known binary brown dwarf WISE J104915.57-531906.1AB (LUH 16) is a well-studied benchmark for our understanding of substellar objects. Previously published astrometry of LUH 16 obtained with FORS2 on the Very Large Telescope was affected by errors that limited its use in combination with other datasets, thereby hampering the determination of its accurate orbital param- eters and masses. We improve upon the calibration and analysis of the FORS2 astrometry with the help of Gaia DR2 to generate a high-precision dataset that can be combined with present and future LUH 16 astrometry. We demonstrate its use by combining it with available measurements from the Hubble Space Telescope (HST) and Gemini/GeMS and deriving updated orbital and mass parameters. Using Gaia DR2 as astrometric reference field, we derived the absolute proper motion and updated the absolute parallax of the binary to 501.557 0.082 mas. We refined the individual dynamical masses of LUH 16 to 33.5 0.3 M (component A) and ± ± Jup 28.6 0.3 MJup (component B), which corresponds to a relative precision of 1% and is three to four times more precise than previous estimates.± We found that these masses show a weak dependence on one datapoint∼ extracted from a photographic plate from 1984. -
Detection of Polarization Due to Cloud Bands in the Nearby Luhman 16 Brown Dwarf Binary
The Astrophysical Journal, 894:42 (25pp), 2020 May 1 https://doi.org/10.3847/1538-4357/ab6ef2 © 2020. The Author(s). Published by the American Astronomical Society. Detection of Polarization due to Cloud Bands in the Nearby Luhman 16 Brown Dwarf Binary Maxwell A. Millar-Blanchaer1,2,12 , Julien H. Girard3,4 , Theodora Karalidi5 , Mark S. Marley6 , Rob G. van Holstein7, Sujan Sengupta8 , Dimitri Mawet2 , Tiffany Kataria1 , Frans Snik7, Jos de Boer7 , Rebecca Jensen-Clem9 , Arthur Vigan10, and Sasha Hinkley11 1 Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USA; [email protected] 2 Department of Astronomy, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA 3 Space Telescope Science Institute, Baltimore, MD 21218, USA 4 Université Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France 5 Department of Astronomy, UC Santa Cruz, 1156 High Street, Santa Cruz, CA 95064, USA 6 NASA Ames Research Center, Mountain View, CA 94035, USA 7 Leiden Observatory, Leiden University, P.O. Box 9513, 2300 RA Leiden, The Netherlands 8 Indian Institute of Astrophysics, Koramangala 2nd Block, Bangalore 560 034, India 9 Astronomy Department, University of California, Berkeley, Berkeley, CA 94720, USA 10 Aix-Marseille Univ., CNRS, LAM, Laboratoire d’Astrophysique de Marseille, F-13013 Marseille, France 11 School of Physics, College of Engineering, Mathematics & Physical Sciences, University of Exeter, Stocker Road, Exeter, EX4 4QL, UK Received 2019 May 21; revised 2020 January 8; accepted 2020 January 13; published 2020 May 5 Abstract Brown dwarfs exhibit patchy or spatially varying banded cloud structures that are inferred through photometric and spectroscopic variability modeling techniques. -
The 10 Parsec Sample in the Gaia Era?,?? C
A&A 650, A201 (2021) Astronomy https://doi.org/10.1051/0004-6361/202140985 & c C. Reylé et al. 2021 Astrophysics The 10 parsec sample in the Gaia era?,?? C. Reylé1 , K. Jardine2 , P. Fouqué3 , J. A. Caballero4 , R. L. Smart5 , and A. Sozzetti5 1 Institut UTINAM, CNRS UMR6213, Univ. Bourgogne Franche-Comté, OSU THETA Franche-Comté-Bourgogne, Observatoire de Besançon, BP 1615, 25010 Besançon Cedex, France e-mail: [email protected] 2 Radagast Solutions, Simon Vestdijkpad 24, 2321 WD Leiden, The Netherlands 3 IRAP, Université de Toulouse, CNRS, 14 av. E. Belin, 31400 Toulouse, France 4 Centro de Astrobiología (CSIC-INTA), ESAC, Camino bajo del castillo s/n, 28692 Villanueva de la Cañada, Madrid, Spain 5 INAF – Osservatorio Astrofisico di Torino, Via Osservatorio 20, 10025 Pino Torinese (TO), Italy Received 2 April 2021 / Accepted 23 April 2021 ABSTRACT Context. The nearest stars provide a fundamental constraint for our understanding of stellar physics and the Galaxy. The nearby sample serves as an anchor where all objects can be seen and understood with precise data. This work is triggered by the most recent data release of the astrometric space mission Gaia and uses its unprecedented high precision parallax measurements to review the census of objects within 10 pc. Aims. The first aim of this work was to compile all stars and brown dwarfs within 10 pc observable by Gaia and compare it with the Gaia Catalogue of Nearby Stars as a quality assurance test. We complement the list to get a full 10 pc census, including bright stars, brown dwarfs, and exoplanets. -
Long-Term, Multiwavelength Light Curves of Ultra-Cool Dwarfs: Ii
Draft version November 28, 2016 A Preprint typeset using LTEX style emulateapj v. 03/07/07 LONG-TERM, MULTIWAVELENGTH LIGHT CURVES OF ULTRA-COOL DWARFS: II. THE EVOLVING LIGHT CURVES OF THE T2.5 SIMP 0136 & THE UNCORRELATED LIGHT CURVES OF THE M9 TVLM 513 Bryce Croll1, Philip S. Muirhead1 2, Jack Lichtman3, Eunkyu Han2, Paul A. Dalba2, Jacqueline Radigan4 Draft version November 28, 2016 ABSTRACT We present 17 nights of ground-based, near-infrared photometry of the variable L/T transition brown dwarf SIMP J013656.5+093347 and an additional 3 nights of ground-based photometry of the radio-active late M-dwarf TVLM 513-46546. Our TVLM 513-46546 photometry includes 2 nights of simultaneous, multiwavelength, ground-based photometry, in which we detect obvious J-band vari- ability, but do not detect I-band variability of similar amplitude, confirming that the variability of TVLM 513-46546 most likely arises from clouds or aurorae, rather than starspots. Our photometry of SIMP J013656.5+093347 includes 15 nights of J-band photometry that allow us to observe how the variable light curve of this L/T transition brown dwarf evolves from rotation period to rotation period, night-to-night and week-to-week. We estimate the rotation period of SIMP J013656.5+093347 as 2.406 ± 0.012 hours, and do not find evidence for obvious differential rotation. The peak-to-peak amplitude displayed by SIMP J013656.5+093347 in our light curves evolves from greater than 6% to less than 1% in a matter of days, and the typical timescale for significant evolution of the SIMP J013656.5+093347 light curve appears to be approximately <1 to 10 rotation periods. -
Cviewoftherestlesssn2009ip Reveals the Explosive Ejection of a Massive Star Envelope Margutti, R., Et Al
1 Peter J. Brown Office Address Contact Information M311 Mitchell Institute for Fundamental Physics and Astronomy E-mail: [email protected] Department of Physics & Astronomy, Texas A&M University Cell: (979) 402-4523 Skype: grbpeter 4242 TAMU, College Station, TX 77843 www.linkedin.com/in/peter-brown-supernova Highlights Observational Astrophysicist with experience in ground and space-based Ultraviolet and• Optical Photometry and Spectroscopy of Supernovae and other Transients Leader of Swift supernova team since 2005 and Swift Cycle 14 Key Project • PI of 5 Hubble Space Telescope Programs • Principal Investigator of External Grants Totaling over $2,600,000 • 18 Refereed, First Author Journal Articles, 140+ Coauthored Journal Articles • 2017 Texas A&M College of Science Undergraduate Research Mentoring Award • Education Ph.D. in Astronomy & Astrophysics – Pennsylvania State University August 2009 Thesis Title: “The Ultraviolet Properties of Supernovae” Thesis Advisor: Dr. P. W. A. Roming B.S. in Physics and Astronomy – Brigham Young University August 2004 Senior Thesis Title: “Observing Gamma Ray Burst Afterglows from BYU’s Orson Pratt Observatory” Thesis Advisor: Professor J. W. Moody Academic Research Scientist – Mitchell Institute, Texas A&M University 2016 – present Positions Visiting Associate Professor Spring 2020 Visiting Assistant Professor Spring 2018 Mitchell Fellow, Postdoctoral Research Associate 2012 – 2016 Supervisor: Professor Lifan Wang Postdoctoral Research Associate – University of Utah 2009 – 2012 Supervisor: Professor -
Arxiv:1708.02714V2 [Astro-Ph.SR] 12 Aug 2017 7Gemini Telescope, Colina El Pino S/N, La Serena, Chile
Individual, Model-Independent Masses of the Closest Known Brown Dwarf Binary to the Sun E. Victor Garcia1, S. Mark Ammons1, Maissa Salama2, Ian Crossfield3;4, Eduardo Bendek5, Jeffrey Chilcote6, Vincent Garrel7, James R. Graham8, Paul Kalas8, Quinn Konopacky9, Jessica R. Lu2, Bruce Macintosh10, Eduardo Marin7, Christian Marois11;12 Eric Nielsen10;13, Beno^ıtNeichel14, Don Pham1, Robert J. De Rosa8, Dominic M. Ryan8, Maxwell Service2, Gaetano Sivo7 Abstract At a distance of ∼ 2 pc, our nearest brown dwarf neighbor, Luhman 16 AB, has been exten- sively studied since its discovery 3 years ago, yet its most fundamental parameter { the masses of the individual dwarfs { has not been constrained with precision. In this work we present the full astrometric orbit and barycentric motion of Luhman 16 AB and the first precision measurements of the individual component masses. We draw upon archival observations spanning 31 years from the European Southern Observatory (ESO) Schmidt Telescope, the Deep Near-Infrared Survey of the Southern Sky (DENIS), public FORS2 data on the Very Large Telescope (VLT), and new astrometry from the Gemini South Multiconjugate Adaptive Optics System (GeMS). Finally, we include three radial velocity measurements of the two components from VLT/CRIRES, span- ning one year. With this new data sampling a full period of the orbit, we use a Markov Chain Monte Carlo algorithm to fit a 16-parameter model incorporating mutual orbit and barycen- +1:1 tric motion parameters and constrain the individual masses to be 27:9−1:0 MJ for the T dwarf +1:3 and 34:2−1:1 MJ for the L dwarf.