Multi-Messenger Observations of a Binary Neutron Star Merger
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The Minor Planet Bulletin
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 36, NUMBER 3, A.D. 2009 JULY-SEPTEMBER 77. PHOTOMETRIC MEASUREMENTS OF 343 OSTARA Our data can be obtained from http://www.uwec.edu/physics/ AND OTHER ASTEROIDS AT HOBBS OBSERVATORY asteroid/. Lyle Ford, George Stecher, Kayla Lorenzen, and Cole Cook Acknowledgements Department of Physics and Astronomy University of Wisconsin-Eau Claire We thank the Theodore Dunham Fund for Astrophysics, the Eau Claire, WI 54702-4004 National Science Foundation (award number 0519006), the [email protected] University of Wisconsin-Eau Claire Office of Research and Sponsored Programs, and the University of Wisconsin-Eau Claire (Received: 2009 Feb 11) Blugold Fellow and McNair programs for financial support. References We observed 343 Ostara on 2008 October 4 and obtained R and V standard magnitudes. The period was Binzel, R.P. (1987). “A Photoelectric Survey of 130 Asteroids”, found to be significantly greater than the previously Icarus 72, 135-208. reported value of 6.42 hours. Measurements of 2660 Wasserman and (17010) 1999 CQ72 made on 2008 Stecher, G.J., Ford, L.A., and Elbert, J.D. (1999). “Equipping a March 25 are also reported. 0.6 Meter Alt-Azimuth Telescope for Photometry”, IAPPP Comm, 76, 68-74. We made R band and V band photometric measurements of 343 Warner, B.D. (2006). A Practical Guide to Lightcurve Photometry Ostara on 2008 October 4 using the 0.6 m “Air Force” Telescope and Analysis. Springer, New York, NY. located at Hobbs Observatory (MPC code 750) near Fall Creek, Wisconsin. -
1. Budorcas Taxicolor Tibetanus Milne-Edwards.- a Horn of an Adult and Skins and Skulls of Two Very Young Animals, Tai-Pa-Shiang, August 16 and October 25
59.9(51.4) Article XXIX.- MAMMALS FROM SHEN-SI PROVINCE, CHINA. By J. A. ALLEN. A small collection of mammals from Mount Tai-pai, Shen-si Province, China, recently acquired by the Museum through Mr. Alan Owston of Yokohama, contains several species of interest. It comprises 55 specimens, representing 16 species, some of which appear to be undescribed. The material is rather poorly prepared, the skulls having been left in the skins, and when removed were found to be more or less mutilated, some of them lacking the whole of the postorbital portion. The collection is of interest as coming from a hitherto unexplored locality, the Tai-pa-shiang mountains, on the western border of Shen-si, which are said to reach an altitude of about 11,000 feet. The specimens are mostly labeled simply "Tai-pa- shiang," with the sex of the specimen and date of collection, but a few are labeled as from "Yumonko, foot of Tai-pa-shiang," and others are marked "Si-Tai-pa-shiang." In no case is the altitude indicated. 1. Budorcas taxicolor tibetanus Milne-Edwards.- A horn of an adult and skins and skulls of two very young animals, Tai-pa-shiang, August 16 and October 25. The two specimens are respectively male and female, and differ much in color, the male having the body, except the ventral surface and the dorsal stripe, pale yellowish, the dorsal stripe, the ventral surface and limbs dark dull reddish brown; top of nose and edge of ears blackish. The other has the body nearly white, with the underparts and limbs dark brown; the dorsal stripe is dark brown only over the shoulders, and black mixed with white on the top of the neck and posterior two-thirds of the dorsal line; black hairs are also appearing on the limbs. -
Ligo-India Proposal for an Interferometric Gravitational-Wave Observatory
LIGO-INDIA PROPOSAL FOR AN INTERFEROMETRIC GRAVITATIONAL-WAVE OBSERVATORY IndIGO Indian Initiative in Gravitational-wave Observations PROPOSAL FOR LIGO-INDIA !"#!$ Indian Initiative in Gravitational wave Observations http://www.gw-indigo.org II Title of the Project LIGO-INDIA Proposal of the Consortium for INDIAN INITIATIVE IN GRAVITATIONAL WAVE OBSERVATIONS IndIGO to Department of Atomic Energy & Department of Science and Technology Government of India IndIGO Consortium Institutions Chennai Mathematical Institute IISER, Kolkata IISER, Pune IISER, Thiruvananthapuram IIT Madras, Chennai IIT, Kanpur IPR, Bhatt IUCAA, Pune RRCAT, Indore University of Delhi (UD), Delhi Principal Leads Bala Iyer (RRI), Chair, IndIGO Consortium Council Tarun Souradeep (IUCAA), Spokesperson, IndIGO Consortium Council C.S. Unnikrishnan (TIFR), Coordinator Experiments, IndIGO Consortium Council Sanjeev Dhurandhar (IUCAA), Science Advisor, IndIGO Consortium Council Sendhil Raja (RRCAT) Ajai Kumar (IPR) Anand Sengupta(UD) 10 November 2011 PROPOSAL FOR LIGO-INDIA II PROPOSAL FOR LIGO-INDIA LIGO-India EXECUTIVE SUMMARY III PROPOSAL FOR LIGO-INDIA IV PROPOSAL FOR LIGO-INDIA This proposal by the IndIGO consortium is for the construction and subsequent 10- year operation of an advanced interferometric gravitational wave detector in India called LIGO-India under an international collaboration with Laser Interferometer Gravitational–wave Observatory (LIGO) Laboratory, USA. The detector is a 4-km arm-length Michelson Interferometer with Fabry-Perot enhancement arms, and aims to detect fractional changes in the arm-length smaller than 10-23 Hz-1/2 . The task of constructing this very sophisticated detector at the limits of present day technology is facilitated by the amazing opportunity offered by the LIGO Laboratory and its international partners to provide the complete design and all the key components required to build the detector as part of the collaboration. -
The Multi-Messenger Discovery and Observation of a Binary Neutron Star
The Astrophysical Journal Letters, 848:L12 (59pp), 2017 October 20 https://doi.org/10.3847/2041-8213/aa91c9 © 2017. The American Astronomical Society. All rights reserved. Multi-messenger Observations of a Binary Neutron Star Merger LIGO Scientific Collaboration and Virgo Collaboration, Fermi GBM, INTEGRAL, IceCube Collaboration, AstroSat Cadmium Zinc Telluride Imager Team, IPN Collaboration, The Insight-Hxmt Collaboration, ANTARES Collaboration, The Swift Collaboration, AGILE Team, The 1M2H Team, The Dark Energy Camera GW-EM Collaboration and the DES Collaboration, The DLT40 Collaboration, GRAWITA: GRAvitational Wave Inaf TeAm, The Fermi Large Area Telescope Collaboration, ATCA: Australia Telescope Compact Array, ASKAP: Australian SKA Pathfinder, Las Cumbres Observatory Group, OzGrav, DWF (Deeper, Wider, Faster Program),AST3, and CAASTRO Collaborations, The VINROUGE Collaboration, MASTER Collaboration, J-GEM, GROWTH, JAGWAR, Caltech- NRAO, TTU-NRAO, and NuSTAR Collaborations,Pan-STARRS,TheMAXITeam,TZACConsortium, KU Collaboration, Nordic Optical Telescope, ePESSTO, GROND, Texas Tech University, SALT Group, TOROS: Transient Robotic Observatory of the South Collaboration, The BOOTES Collaboration, MWA: Murchison Widefield Array, The CALET Collaboration, IKI-GW Follow-up Collaboration, H.E.S.S. Collaboration, LOFAR Collaboration, LWA: Long Wavelength Array, HAWC Collaboration, The Pierre Auger Collaboration, ALMA Collaboration, Euro VLBI Team, Pi of the Sky Collaboration, The Chandra Team at McGill University, DFN: Desert Fireball Network, ATLAS, High Time Resolution Universe Survey, RIMAS and RATIR, and SKA South Africa/MeerKAT (See the end matter for the full list of authors.) Received 2017 October 3; revised 2017 October 6; accepted 2017 October 6; published 2017 October 16 Abstract On 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. -
View Print Program (Pdf)
PROGRAM November 3 - 5, 2016 Hosted by Sigma Pi Sigma, the physics honor society 2016 Quadrennial Physics Congress (PhysCon) 1 31 Our students are creating the future. They have big, bold ideas and they come to Florida Polytechnic University looking for ways to make their visions a reality. Are you the next? When you come to Florida Poly, you’ll be welcomed by students and 3D faculty who share your passion for pushing the boundaries of science, PRINTERS technology, engineering and math (STEM). Florida’s newest state university offers small classes and professors who work side-by-side with students on real-world projects in some of the most advanced technology labs available, so the possibilities are endless. FLPOLY.ORG 2 2016 Quadrennial Physics Congress (PhysCon) Contents Welcome ........................................................................................................................... 4 Unifying Fields: Science Driving Innovation .......................................................................... 7 Daily Schedules ............................................................................................................. 9-11 PhysCon Sponsors .............................................................................................................12 Planning Committee & Staff ................................................................................................13 About the Society of Physics Students and Sigma Pi Sigma ���������������������������������������������������13 Previous Sigma Pi Sigma -
The Perils of Complacency
THE PERILS OF COMPLACENCYTHE PERILS : America at a Tipping Point in Science & Engineering : America at a Tipping Point THE PERILS OF COMPLACENCY America at a Tipping Point in Science & Engineering An Update to Restoring the Foundation: The Vital Role of Research in Preserving the American Dream AMERICAN ACADEMY OF ARTS & SCIENCES AMERICAN ACADEMY THE PERILS OF COMPLACENCY America at a Tipping Point in Science & Engineering An Update to Restoring the Foundation: The Vital Role of Research in Preserving the American Dream american academy of arts & sciences Cambridge, Massachusetts This report and its supporting data were finalized in April 2020. While some new data have been released since then, the report’s findings and recommendations remain valid. Please note that Figure 1 was based on nsf analysis, which used existing oecd purchasing power parity (ppp) to convert U.S. and Chinese financial data.oecd adjusted its ppp factors in May 2020. The new factors for China affect the curves in the figure, pushing the China-U.S. crossing point toward the end of the decade. This development is addressed in Appendix D. © 2020 by the American Academy of Arts & Sciences All rights reserved. isbn: 0- 87724- 134- 1 This publication is available online at www.amacad.org/publication/perils-of-complacency. The views expressed in this report are those held by the contributors and are not necessarily those of the Officers and Members of the American Academy of Arts and Sciences. Please direct inquiries to: American Academy of Arts and Sciences 136 Irving Street Cambridge, Massachusetts 02138- 1996 Telephone: 617- 576- 5000 Email: [email protected] Website: www.amacad.org Contents Acknowledgments 5 Committee on New Models for U.S. -
Multi-Messenger Observations of a Binary Neutron Star Merger
DRAFT VERSION OCTOBER 6, 2017 Typeset using LATEX twocolumn style in AASTeX61 MULTI-MESSENGER OBSERVATIONS OF A BINARY NEUTRON STAR MERGER LIGO SCIENTIFIC COLLABORATION,VIRGO COLLABORATION AND PARTNER ASTRONOMY GROUPS (Dated: October 6, 2017) ABSTRACT On August 17, 2017 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB170817A) with a time-delay of 1.7swith respect to the merger ⇠ time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg2 at a luminosity distance +8 of 40 8 Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range− 0.86 to 2.26 M . An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT2017gfo) in NGC 4993 (at 40 Mpc) less ⇠ than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1-m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over 10 days. Following early non-detections, X-ray and radio emission were discovered at the ⇠ transient’s position 9 and 16 days, respectively, after the merger. -
Asteroid Regolith Weathering: a Large-Scale Observational Investigation
University of Tennessee, Knoxville TRACE: Tennessee Research and Creative Exchange Doctoral Dissertations Graduate School 5-2019 Asteroid Regolith Weathering: A Large-Scale Observational Investigation Eric Michael MacLennan University of Tennessee, [email protected] Follow this and additional works at: https://trace.tennessee.edu/utk_graddiss Recommended Citation MacLennan, Eric Michael, "Asteroid Regolith Weathering: A Large-Scale Observational Investigation. " PhD diss., University of Tennessee, 2019. https://trace.tennessee.edu/utk_graddiss/5467 This Dissertation is brought to you for free and open access by the Graduate School at TRACE: Tennessee Research and Creative Exchange. It has been accepted for inclusion in Doctoral Dissertations by an authorized administrator of TRACE: Tennessee Research and Creative Exchange. For more information, please contact [email protected]. To the Graduate Council: I am submitting herewith a dissertation written by Eric Michael MacLennan entitled "Asteroid Regolith Weathering: A Large-Scale Observational Investigation." I have examined the final electronic copy of this dissertation for form and content and recommend that it be accepted in partial fulfillment of the equirr ements for the degree of Doctor of Philosophy, with a major in Geology. Joshua P. Emery, Major Professor We have read this dissertation and recommend its acceptance: Jeffrey E. Moersch, Harry Y. McSween Jr., Liem T. Tran Accepted for the Council: Dixie L. Thompson Vice Provost and Dean of the Graduate School (Original signatures are on file with official studentecor r ds.) Asteroid Regolith Weathering: A Large-Scale Observational Investigation A Dissertation Presented for the Doctor of Philosophy Degree The University of Tennessee, Knoxville Eric Michael MacLennan May 2019 © by Eric Michael MacLennan, 2019 All Rights Reserved. -
Aqueous Alteration on Main Belt Primitive Asteroids: Results from Visible Spectroscopy1
Aqueous alteration on main belt primitive asteroids: results from visible spectroscopy1 S. Fornasier1,2, C. Lantz1,2, M.A. Barucci1, M. Lazzarin3 1 LESIA, Observatoire de Paris, CNRS, UPMC Univ Paris 06, Univ. Paris Diderot, 5 Place J. Janssen, 92195 Meudon Pricipal Cedex, France 2 Univ. Paris Diderot, Sorbonne Paris Cit´e, 4 rue Elsa Morante, 75205 Paris Cedex 13 3 Department of Physics and Astronomy of the University of Padova, Via Marzolo 8 35131 Padova, Italy Submitted to Icarus: November 2013, accepted on 28 January 2014 e-mail: [email protected]; fax: +33145077144; phone: +33145077746 Manuscript pages: 38; Figures: 13 ; Tables: 5 Running head: Aqueous alteration on primitive asteroids Send correspondence to: Sonia Fornasier LESIA-Observatoire de Paris arXiv:1402.0175v1 [astro-ph.EP] 2 Feb 2014 Batiment 17 5, Place Jules Janssen 92195 Meudon Cedex France e-mail: [email protected] 1Based on observations carried out at the European Southern Observatory (ESO), La Silla, Chile, ESO proposals 062.S-0173 and 064.S-0205 (PI M. Lazzarin) Preprint submitted to Elsevier September 27, 2018 fax: +33145077144 phone: +33145077746 2 Aqueous alteration on main belt primitive asteroids: results from visible spectroscopy1 S. Fornasier1,2, C. Lantz1,2, M.A. Barucci1, M. Lazzarin3 Abstract This work focuses on the study of the aqueous alteration process which acted in the main belt and produced hydrated minerals on the altered asteroids. Hydrated minerals have been found mainly on Mars surface, on main belt primitive asteroids and possibly also on few TNOs. These materials have been produced by hydration of pristine anhydrous silicates during the aqueous alteration process, that, to be active, needed the presence of liquid water under low temperature conditions (below 320 K) to chemically alter the minerals. -
The Basic Physics of the Binary Black Hole Merger GW150914
September 21, 2016 The basic physics of the binary black hole merger GW150914 The LIGO Scientific Collaboration and The Virgo Collaboration¤ The first direct gravitational-wave detection was made by the Advanced Laser Interferometer Gravitational Wave Observatory on September 14, 2015. The GW150914 signal was strong enough to be apparent, without using any waveform model, in the filtered detec- tor strain data. Here those features of the signal visible in these data are used, along with only such concepts from Newtonian physics and general relativity as are ac- cessible to anyone with a general physics background. The simple analysis presented here is consistent with the fully general-relativistic analyses published else- Figure 1 The instrumental strain data in the Livingston detec- where, in showing that the signal was produced by the tor (blue) and Hanford detector (red), as shown in Figure 1 of inspiral and subsequent merger of two black holes. The [1]. Both have been bandpass- and notch-filtered. The Hanford black holes were each of approximately 35M , still strain has been shifted back in time by 6.9 ms and inverted. ¯ Times shown are relative to 09:50:45 Coordinated Universal orbited each other as close as 350 km apart and sub- » Time (UTC) on September 14, 2015. sequently merged to form a single black hole. Similar reasoning, directly from the data, is used to roughly es- timate how far these black holes were from the Earth, A black hole is a region of space-time where the gravita- and the energy that they radiated in gravitational waves. -
Observational Constraints on the Optical and Near-Infrared Emission from the Neutron Star–Black Hole Binary Merger Candidate S190814bv? K
A&A 643, A113 (2020) Astronomy https://doi.org/10.1051/0004-6361/202037669 & c K. Ackley et al. 2020 Astrophysics Observational constraints on the optical and near-infrared emission from the neutron star–black hole binary merger candidate S190814bv? K. Ackley1, L. Amati2, C. Barbieri3,4,5 , F. E. Bauer6,7,8 , S. Benetti9, M. G. Bernardini3, K. Bhirombhakdi10, M. T. Botticella11, M. Branchesi12,13, E. Brocato14,15, S. H. Bruun16, M. Bulla17, S. Campana3, E. Cappellaro9, A. J. Castro-Tirado18, K. C. Chambers19, S. Chaty20,21, T.-W. Chen22,23, R. Ciolfi9,24, A. Coleiro20, C. M. Copperwheat25, S. Covino3, R. Cutter26, F. D’Ammando27, P. D’Avanzo3, G. De Cesare2, V. D’Elia14,28, M. Della Valle11, L. Denneau19, M. De Pasquale29, V. S. Dhillon30,31, M. J. Dyer30, N. Elias-Rosa9,32, P. A. Evans33, R. A. J. Eyles-Ferris33, A. Fiore9,34, M. Fraser35, A. S. Fruchter10, J. P. U. Fynbo36,37, L. Galbany38, C. Gall16, D. K. Galloway1, F. I. Getman11, G. Ghirlanda3, J. H. Gillanders39, A. Gomboc40, B. P. Gompertz26, C. González-Fernández41, S. González-Gaitán42, A. Grado11, G. Greco43,44, M. Gromadzki45, P. J. Groot46,47,48,49 , C. P. Gutiérrez50, T. Heikkilä51, K. E. Heintz52, J. Hjorth16, Y.-D. Hu18,38, M. E. Huber19, C. Inserra53, L. Izzo16, J. Japelj54, A. Jerkstrand22, Z. P. Jin55, P. G. Jonker46,56, E. Kankare51, D. A. Kann18, M. Kennedy57, S. Kim6,58, S. Klose59, E. C. Kool22, R. Kotak51, H. Kuncarayakti51,60, G. P. Lamb33, G. Leloudas61, A. J. Levan26,46,??, F. Longo62, T. -
The Minor Planet Bulletin
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 38, NUMBER 2, A.D. 2011 APRIL-JUNE 71. LIGHTCURVES OF 10452 ZUEV, (14657) 1998 YU27, AND (15700) 1987 QD Gary A. Vander Haagen Stonegate Observatory, 825 Stonegate Road Ann Arbor, MI 48103 [email protected] (Received: 28 October) Lightcurve observations and analysis revealed the following periods and amplitudes for three asteroids: 10452 Zuev, 9.724 ± 0.002 h, 0.38 ± 0.03 mag; (14657) 1998 YU27, 15.43 ± 0.03 h, 0.21 ± 0.05 mag; and (15700) 1987 QD, 9.71 ± 0.02 h, 0.16 ± 0.05 mag. Photometric data of three asteroids were collected using a 0.43- meter PlaneWave f/6.8 corrected Dall-Kirkham astrograph, a SBIG ST-10XME camera, and V-filter at Stonegate Observatory. The camera was binned 2x2 with a resulting image scale of 0.95 arc- seconds per pixel. Image exposures were 120 seconds at –15C. Candidates for analysis were selected using the MPO2011 Asteroid Viewing Guide and all photometric data were obtained and analyzed using MPO Canopus (Bdw Publishing, 2010). Published asteroid lightcurve data were reviewed in the Asteroid Lightcurve Database (LCDB; Warner et al., 2009). The magnitudes in the plots (Y-axis) are not sky (catalog) values but differentials from the average sky magnitude of the set of comparisons. The value in the Y-axis label, “alpha”, is the solar phase angle at the time of the first set of observations. All data were corrected to this phase angle using G = 0.15, unless otherwise stated.