DOCSLIB.ORG

Chasing the Brightest Cosmic Explosions with ROTSE-III

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Chasing the Brightest Cosmic Explosions with ROTSE-III Chasing the Brightest Cosmic Explosions with ROTSE-III by Fang Yuan A dissertation submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy (Physics) in The University of Michigan 2010 Doctoral Committee: Professor Carl W. Akerlof, Chair Professor Fred Adams Professor Timothy A. McKay Professor Bing Zhou Assistant Professor Jon M. Miller c Fang Yuan 2010 All Rights Reserved To my family ii ACKNOWLEDGEMENTS First of all, I can never express my gratitude enough to Carl Akerlof, who has taught me so much in and beyond the field of physics. Carl's wonderful mentoring has made my PhD study such an enjoyable experience. As a proud member of the ROTSE group, I am grateful to all these brilliant people, Eli Rykoff, Tim McKay, Heather Flewelling, Sarah Yost, Wiphu Rujopakarn, Don Smith and many more, that have worked with ROTSE and have made it such a superb instrument and fun project to work with. It has been a great pleasure to work with the friendly and capable observatory staffs, in particular David Doss, Toni Hanke, Tuncay Ozı¨ ¸sık and Andre Phillips. A critical part of this thesis has been made possible through collaboration with an excellent group of researchers in the University of Texas. It all began with the ingenious idea of Robert Quimby, from whom I have gained invaluable technical and mental support when starting RSVP. I am indebted to Craig Wheeler for all the wise insights and generous encouragement. I also thank Jozsef Vinko for all the kindly help. The success of RSVP has relied on the efforts from many undergraduates, including Jamie Aretakis, Dan Chamarro, Matt Sisson and Amelia Uecker. I would like to acknowledge Weikang Zheng and Shashi Pandy for taking graceful care of ROTSE when I am busy finishing up this thesis. iii I wish to thank my parents for their unconditional love and support that make me feel safe and connected whatever I do wherever I am. Finally, thank you Qiaoqiao for making me a very happy person. Part of chapter 3 of this thesis is accepted for publication in the Astrophysical Journal. Part of chapter 4 is based on Yuan & Akerlof (2008). Part of chapter 5 has been submitted to the Astrophysical Journal. iv TABLE OF CONTENTS DEDICATION : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : ii ACKNOWLEDGEMENTS : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : iii LIST OF FIGURES : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : viii LIST OF TABLES : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : x LIST OF ABBREVIATIONS : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : xi ABSTRACT : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : : xiii CHAPTER I. Introduction . 1 II. GRB and the Fireball Model . 4 2.1 Introduction . 4 2.2 Pre-Swift Phenomenology . 6 2.2.1 Prompt Burst Emission . 6 2.2.2 Afterglow . 7 2.2.3 SNe Association . 7 2.3 The Fireball Model . 8 2.3.1 Relativistic Outflow . 8 2.3.2 Emission Mechanisms . 8 2.3.3 Jets . 9 2.3.4 Very High Energy Emission . 10 2.4 The Swift-era . 12 2.4.1 Bursts Statistics . 12 2.4.2 Canonical X-ray Lightcurves . 13 2.4.3 Very Early Optical Observations . 13 2.4.4 Missing Jet Breaks? . 15 2.4.5 High Redshift Bursts . 17 2.4.6 Host . 18 2.4.7 Progenitor . 18 III. Observations of GRBs by ROTSE-III . 20 3.1 Introduction . 20 3.2 GRB 081008: from Burst to Afterglow and the Transition Phase in Between 21 v 3.2.1 Observations and Data Reduction . 22 3.2.2 Spectral and Temporal analysis . 28 3.2.3 Discussion . 37 3.2.4 Conclusions . 45 3.3 Other GRBs Observed by ROTSE-III . 47 3.3.1 Data Reduction . 47 3.3.2 GRB 071025 . 49 3.3.3 GRB/XRF 080330 . 52 3.3.4 GRB 080413A . 54 3.3.5 GRB 080603B . 56 3.3.6 GRB 080607 . 58 3.3.7 GRB 080703 . 61 3.3.8 GRB 080804 . 62 3.3.9 GRB 080928 . 64 3.3.10 GRB 081029 . 66 3.3.11 GRB 081121 . 68 3.4 Early Behavior of GRBs . 70 3.4.1 High Energy Observations . 70 3.4.2 Optical and X-ray Spectra . 70 3.4.3 Optical and Hard X-ray (BAT) Spectra . 71 3.4.4 Conclusion . 73 IV. ROTSE Supernova Verification Project . 74 4.1 Introduction . 74 4.2 Science Goals . 76 4.2.1 Ultra-luminous SNe . 76 4.2.2 SNe Ia . 81 4.3 Image Subtraction by Cross-Convolution . 86 4.3.1 Mathematical Method . 87 4.3.2 Computational Methods . 90 4.3.3 Operational Experience . 96 4.4 Transient Search Pipeline . 97 4.4.1 Target Fields Selection . 97 4.4.2 Construction of References and Bad Pixel Maps . 104 4.4.3 Data Flow and Automated Candidate Filtering . 106 4.4.4 Web Scan and Follow-up Schedules . 107 V. RSVP supernovae . 111 5.1 Introduction . 111 5.2 ROTSE-III Observations of the SNe . 112 5.2.1 Data Reduction . 112 5.2.2 Discoveries and Photometry . 112 5.2.3 SN 2007gr . 112 5.2.4 SN 2007if . 129 5.2.5 SN 2007is . 130 5.2.6 SN 2007iu . 130 5.2.7 SN 2007kh . 130 5.2.8 SN 2007nq . 131 5.2.9 SN 2007ob . 131 5.2.10 SN 2007op . 132 5.2.11 SN 2007qc . 132 5.2.12 SN 2007qe . 132 vi 5.2.13 SN 2007rx . 133 5.2.14 SN 2007sp . 133 5.2.15 SN 2007su . 133 5.2.16 SN 2007sw . 134 5.2.17 SN 2008E . 134 5.2.18 SN 2008ab . 134 5.2.19 SN 2008ac . 135 5.2.20 SN 2008ad . 135 5.2.21 SN 2008am . 135 5.2.22 SN 2008ar . 137 5.2.23 SN 2008bg . 137 5.2.24 SN 2008bj . 137 5.2.25 SN 2008by . 138 5.2.26 SN 2008bz . 138 5.2.27 SN 2008cw . 138 5.2.28 SN 2008dx . 139 5.2.29 ROTSE3 J125642.7+273041 . ..
Load more

Recommended publications
  • Progressive Redshifts in the Late-Time Spectra of Type IA Supernovae
    Dartmouth College Dartmouth Digital Commons Dartmouth Scholarship Faculty Work 8-9-2016 Progressive Redshifts in the Late-Time Spectra of Type IA Supernovae C. S. Black Dartmouth College R. A. Fesen Dartmouth College J. T. Parrent Harvard-Smithsonian Center for Astrophysics Follow this and additional works at: https://digitalcommons.dartmouth.edu/facoa Part of the Astrophysics and Astronomy Commons Dartmouth Digital Commons Citation Black, C. S.; Fesen, R. A.; and Parrent, J. T., "Progressive Redshifts in the Late-Time Spectra of Type IA Supernovae" (2016). Dartmouth Scholarship. 1806. https://digitalcommons.dartmouth.edu/facoa/1806 This Article is brought to you for free and open access by the Faculty Work at Dartmouth Digital Commons. It has been accepted for inclusion in Dartmouth Scholarship by an authorized administrator of Dartmouth Digital Commons. For more information, please contact [email protected]. DRAFT VERSION AUGUST 9, 2016 Preprint typeset using LATEX style emulateapj v. 5/2/11 PROGRESSIVE RED SHIFTS IN THE LATE-TIME SPECTRA OF TYPE IA SUPERNOVAE C. S. BLACK1 , R. A. FESEN1 , & J. T. PARRENT2 16127 Wilder Lab, Department of Physics & Astronomy, Dartmouth College, Hanover, NH 03755 and 2Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA Draft version August 9, 2016 ABSTRACT We examine the evolution of late-time, optical nebular features of Type Ia supernovae (SNe Ia) using a sample consisting of 160 spectra of 27 normal SNe Ia taken from the literature as well as unpublished spectra of SN 2008Q and ASASSN-14lp. Particular attention was given to nebular features between 4000-6000 Å in terms of temporal changes in width and central wavelength.
    [Show full text]
  • Copyright by Robert Michael Quimby 2006 the Dissertation Committee for Robert Michael Quimby Certifies That This Is the Approved Version of the Following Dissertation
    Copyright by Robert Michael Quimby 2006 The Dissertation Committee for Robert Michael Quimby certifies that this is the approved version of the following dissertation: The Texas Supernova Search Committee: J. Craig Wheeler, Supervisor Peter H¨oflich Carl Akerlof Gary Hill Pawan Kumar Edward L. Robinson The Texas Supernova Search by Robert Michael Quimby, A.B., M.A. DISSERTATION Presented to the Faculty of the Graduate School of The University of Texas at Austin in Partial Fulfillment of the Requirements for the Degree of DOCTOR OF PHILOSOPHY THE UNIVERSITY OF TEXAS AT AUSTIN December 2006 Acknowledgments I would like to thank J. Craig Wheeler, Pawan Kumar, Gary Hill, Peter H¨oflich, Rob Robinson and Christopher Gerardy for their support and advice that led to the realization of this project and greatly improved its quality. Carl Akerlof, Don Smith, and Eli Rykoff labored to install and maintain the ROTSE-IIIb telescope with help from David Doss, making this project possi- ble. Finally, I thank Greg Aldering, Saul Perlmutter, Robert Knop, Michael Wood-Vasey, and the Supernova Cosmology Project for lending me their image subtraction code and assisting me with its installation. iv The Texas Supernova Search Publication No. Robert Michael Quimby, Ph.D. The University of Texas at Austin, 2006 Supervisor: J. Craig Wheeler Supernovae (SNe) are popular tools to explore the cosmological expan- sion of the Universe owing to their bright peak magnitudes and reasonably high rates; however, even the relatively homogeneous Type Ia supernovae are not intrinsically perfect standard candles. Their absolute peak brightness must be established by corrections that have been largely empirical.
    [Show full text]
  • On the Progenitors of Type Ia Supernovae
    Physics & Astronomy Faculty Publications Physics and Astronomy 2-21-2018 On the Progenitors of Type Ia Supernovae Mario Livio University of Nevada, Las Vegas; The Weizmann Institute of Science, [email protected] Paolo Mazzali The Weizmann Institute of Science; Liverpool John Moores University Follow this and additional works at: https://digitalscholarship.unlv.edu/physastr_fac_articles Part of the Astrophysics and Astronomy Commons Repository Citation Livio, M., Mazzali, P. (2018). On the Progenitors of Type Ia Supernovae. Physics Reports, 736 1-23. http://dx.doi.org/10.1016/j.physrep.2018.02.002 This Article is protected by copyright and/or related rights. It has been brought to you by Digital Scholarship@UNLV with permission from the rights-holder(s). You are free to use this Article in any way that is permitted by the copyright and related rights legislation that applies to your use. For other uses you need to obtain permission from the rights-holder(s) directly, unless additional rights are indicated by a Creative Commons license in the record and/ or on the work itself. This Article has been accepted for inclusion in Physics & Astronomy Faculty Publications by an authorized administrator of Digital Scholarship@UNLV. For more information, please contact [email protected]. On the Progenitors of Type Ia SupernovaeI Mario Livio1,2, Paolo Mazzali2,3 Abstract We review all the models proposed for the progenitor systems of Type Ia super- novae and discuss the strengths and weaknesses of each scenario when confronted with observations. We show that all scenarios encounter at least a few serious difficulties, if taken to represent a comprehensive model for the progenitors of all Type Ia supernovae (SNe Ia).
    [Show full text]
  • Arxiv:0709.0302V1 [Astro-Ph] 3 Sep 2007 N Ro,M,414 USA 48104, MI, Arbor, Ann USA As(..Mcayne L 01.Sc Aeilcudslow Could Material Such Some 2001)
    DRAFT VERSION NOVEMBER 4, 2018 Preprint typeset using LATEX style emulateapj v. 03/07/07 SN 2005AP: A MOST BRILLIANT EXPLOSION ROBERT M. QUIMBY1,GREG ALDERING2,J.CRAIG WHEELER1,PETER HÖFLICH3,CARL W. AKERLOF4,ELI S. RYKOFF4 Draft version November 4, 2018 ABSTRACT We present unfiltered photometric observations with ROTSE-III and optical spectroscopic follow-up with the HET and Keck of the most luminous supernova yet identified, SN 2005ap. The spectra taken about 3 days before and 6 days after maximum light show narrow emission lines (likely originating in the dwarf host) and absorption lines at a redshift of z =0.2832, which puts the peak unfiltered magnitude at −22.7 ± 0.1 absolute. Broad P-Cygni features corresponding to Hα, C III,N III, and O III, are further detected with a photospheric velocity of ∼ 20,000kms−1. Unlike other highly luminous supernovae such as 2006gy and 2006tf that show slow photometric evolution, the light curve of SN 2005ap indicates a 1-3 week rise to peak followed by a relatively rapid decay. The spectra also lack the distinct emission peaks from moderately broadened (FWHM ∼ 2,000kms−1) Balmer lines seen in SN 2006gyand SN 2006tf. We briefly discuss the origin of the extraordinary luminosity from a strong interaction as may be expected from a pair instability eruption or a GRB-like engine encased in a H/He envelope. Subject headings: Supernovae, SN 2005ap 1. INTRODUCTION the ultra-relativistic flow and thus mask the gamma-ray bea- Luminous supernovae (SNe) are most commonly associ- con announcing their creation, unlike their stripped progeni- ated with the Type Ia class, which are thought to involve tor cousins.
    [Show full text]
  • LIKE SN 1991T OR SN 2007If? Ju-Jia Zhang1,2,3, Xiao-Feng Wang3, Michele Sasdelli4,5, Tian-Meng Zhang6, Zheng-Wei Liu7, Paolo A
    The Astrophysical Journal, 817:114 (13pp), 2016 February 1 doi:10.3847/0004-637X/817/2/114 © 2016. The American Astronomical Society. All rights reserved. A LUMINOUS PECULIAR TYPE IA SUPERNOVA SN 2011HR: MORE LIKE SN 1991T OR SN 2007if? Ju-Jia Zhang1,2,3, Xiao-Feng Wang3, Michele Sasdelli4,5, Tian-Meng Zhang6, Zheng-Wei Liu7, Paolo A. Mazzali4,5, Xiang-Cun Meng1,2, Keiichi Maeda8,9, Jun-Cheng Chen3, Fang Huang3, Xu-Lin Zhao3, Kai-Cheng Zhang3, Qian Zhai1,2,10, Elena Pian11,12, Bo Wang1,2, Liang Chang1,2, Wei-Min Yi1,2, Chuan-Jun Wang1,2,10, Xue-Li Wang1,2, Yu-Xin Xin1,2, Jian-Guo Wang1,2, Bao-Li Lun1,2, Xiang-Ming Zheng1,2, Xi-Liang Zhang1,2, Yu-Feng Fan1,2, and Jin-Ming Bai1,2 1 Yunnan Observatories (YNAO), Chinese Academy of Sciences, Kunming 650011, China; [email protected] 2 Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650011, China 3 Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing 100084, China; [email protected] 4 Astrophysics Research Institute, Liverpool John Moores University, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UK 5 Max-Planck Institute fur Astrophysics, D-85748 Garching, Germany 6 National Astronomical Observatories of China (NAOC), Chinese Academy of Sciences, Beijing 100012, China 7 Argelander-Institut für Astronomie, Auf dem Hügel 71, D-53121, Bonn, Germany 8 Department of Astronomy, Kyoto University, Kyoto, 606-8502, Japan 9 Kavli Institute for the Physics and Mathematics of the Universe
    [Show full text]
  • Virgo the Virgin
    Virgo the Virgin Virgo is one of the constellations of the zodiac, the group tion Virgo itself. There is also the connection here with of 12 constellations that lies on the ecliptic plane defined “The Scales of Justice” and the sign Libra which lies next by the planets orbital orientation around the Sun. Virgo is to Virgo in the Zodiac. The study of astronomy had a one of the original 48 constellations charted by Ptolemy. practical “time keeping” aspect in the cultures of ancient It is the largest constellation of the Zodiac and the sec- history and as the stars of Virgo appeared before sunrise ond - largest constellation after Hydra. Virgo is bordered by late in the northern summer, many cultures linked this the constellations of Bootes, Coma Berenices, Leo, Crater, asterism with crops, harvest and fecundity. Corvus, Hydra, Libra and Serpens Caput. The constella- tion of Virgo is highly populated with galaxies and there Virgo is usually depicted with angel - like wings, with an are several galaxy clusters located within its boundaries, ear of wheat in her left hand, marked by the bright star each of which is home to hundreds or even thousands of Spica, which is Latin for “ear of grain”, and a tall blade of galaxies. The accepted abbreviation when enumerating grass, or a palm frond, in her right hand. Spica will be objects within the constellation is Vir, the genitive form is important for us in navigating Virgo in the modern night Virginis and meteor showers that appear to originate from sky. Spica was most likely the star that helped the Greek Virgo are called Virginids.
    [Show full text]
  • Are Superluminous Supernovae Powered by Collision Or By
    Are Superluminous Supernovae Powered By Collision Or By Millisecond Magnetars? Shlomo Dado1 and Arnon Dar1 ABSTRACT Using our previously derived simple analytic expression for the bolometric light curves of supernovae, we demonstrate that the collision of the fast de- bris of ordinary supernova explosions with relatively slow-moving shells from pre-supernova eruptions can produce the observed bolometric light curves of su- perluminous supernovae (SLSNe) of all types. These include both, those which can be explained as powered by spinning-down millisecond magnetars and those which cannot. That and the observed close similarity between the bolometric light-curves of SLSNe and ordinary interacting SNe suggest that SLSNe are pow- ered mainly by collisions with relatively slow moving circumstellar shells from pre-supernova eruptions rather than by the spin-down of millisecond magnetars born in core collapse supernova explosions. Subject headings: supernovae: general 1. Introduction For a long time, it has been widely believed that the observed luminosity of all known types of supernova (SN) explosions is powered by one or more of the following sources: radioactive decay of freshly-synthesized elements, typically 56Ni (Colgate and McKee 1969; Colgate et al. 1980), heat deposited in the envelope of a supergiant star by the explosion arXiv:1312.5273v1 [astro-ph.HE] 18 Dec 2013 shock (Grassberg et al. 1971), and interaction between the SN debris and the circumstellar wind environment (Chevalier 1982). Recently, however, a new type of SNe, superluminous SNe (SLSNe) whose peak luminosity exceeds 1044 ergs per second, much brighter than that of the brightest normal thermonuclear supernovae (type Ia) and core collapse supernova (types Ib/c and II) was discovered by modern supernova surveys.
    [Show full text]
  • 121012-AAS-221 Program-14-ALL, Page 253 @ Preflight
    221ST MEETING OF THE AMERICAN ASTRONOMICAL SOCIETY 6-10 January 2013 LONG BEACH, CALIFORNIA Scientific sessions will be held at the: Long Beach Convention Center 300 E. Ocean Blvd. COUNCIL.......................... 2 Long Beach, CA 90802 AAS Paper Sorters EXHIBITORS..................... 4 Aubra Anthony ATTENDEE Alan Boss SERVICES.......................... 9 Blaise Canzian Joanna Corby SCHEDULE.....................12 Rupert Croft Shantanu Desai SATURDAY.....................28 Rick Fienberg Bernhard Fleck SUNDAY..........................30 Erika Grundstrom Nimish P. Hathi MONDAY........................37 Ann Hornschemeier Suzanne H. Jacoby TUESDAY........................98 Bethany Johns Sebastien Lepine WEDNESDAY.............. 158 Katharina Lodders Kevin Marvel THURSDAY.................. 213 Karen Masters Bryan Miller AUTHOR INDEX ........ 245 Nancy Morrison Judit Ries Michael Rutkowski Allyn Smith Joe Tenn Session Numbering Key 100’s Monday 200’s Tuesday 300’s Wednesday 400’s Thursday Sessions are numbered in the Program Book by day and time. Changes after 27 November 2012 are included only in the online program materials. 1 AAS Officers & Councilors Officers Councilors President (2012-2014) (2009-2012) David J. Helfand Quest Univ. Canada Edward F. Guinan Villanova Univ. [email protected] [email protected] PAST President (2012-2013) Patricia Knezek NOAO/WIYN Observatory Debra Elmegreen Vassar College [email protected] [email protected] Robert Mathieu Univ. of Wisconsin Vice President (2009-2015) [email protected] Paula Szkody University of Washington [email protected] (2011-2014) Bruce Balick Univ. of Washington Vice-President (2010-2013) [email protected] Nicholas B. Suntzeff Texas A&M Univ. suntzeff@aas.org Eileen D. Friel Boston Univ. [email protected] Vice President (2011-2014) Edward B. Churchwell Univ. of Wisconsin Angela Speck Univ. of Missouri [email protected] [email protected] Treasurer (2011-2014) (2012-2015) Hervey (Peter) Stockman STScI Nancy S.
    [Show full text]
  • Chilean Senate Ratifies Agreement with ESO Riccardo Giacconi, Director General of ESO
    No. 85 – September 1996 Chilean Senate Ratifies Agreement with ESO Riccardo Giacconi, Director General of ESO On 5 September 1996, the Senate within up to 10 per cent of observing government in direct negotiation with of the Republic of Chile (Second time on all present and future ESO the private claimants. Chamber of the Parliament) approved telescopes in Chile. They also will As part of this Agreement ESO will the Interpretative, Supplementary and have membership on all ESO scien- continue and increase its contributions Modifying Agreement to the Conven- tific and technical committees. Chile- to the development of Chilean astrono- tion of 1963, which regulates the rela- an and European scientific communi- my and the educational and cultural tions between the European Southern ties will henceforth share the impor- development of local communities. Observatory and its host country, the tant scientific discoveries which will ESO is indebted to the Government of Republic of Chile. be made with the VLT facility at Cerro Chile and especially to the Minister of Following formal approval by the Paranal. Foreign Relations, Don José Miguel ESO Council, it is expected that in- By this Agreement the ESO regula- Insulza, and all those who have struments of ratification could be ex- tions for local Chilean staff will be worked towards this Agreement and its changed before the end of this year. modified to incorporate the principles ratification by the Chilean Parliament. The completion of this process is a of Chilean legislation regarding collec- I wish also to recognise the contri- reason for great mutual satisfaction tive bargaining and freedom of associ- bution of all those at ESO who played as the new Agreement consolidates ation.
    [Show full text]
  • Highly Magnetized Super-Chandrasekhar White Dwarfs and Their Consequences
    Highly magnetized super-Chandrasekhar white dwarfs and their consequences Banibrata Mukhopadhyay Department of Physics Indian Institute of Science Collaborators: Upasana Das (JILA, Colorado), Mukul Bhattacharya (Texas, Austin), Sathyawageeswar Subramanian (Cambridge), Tanayveer Singh Bhatia (IISc/ANU), Subroto Mukerjee (IISc), A. R. Rao (TIFR) Stars with a stable magnetic field: from pre-main sequence to compact remnants August 28 to September 1, 2017, Brno, Czech Republic The talk is based on the following papers MUKHOPADHYAY, A. R. Rao, T. S. Bhatia, MNRAS (press), 2017 MUKHOPADHYAY, A. R. Rao, JCAP, 05, 007, 2016 S. Subramanian, MUKHOPADHYAY, MNRAS, 454, 752, 2015 U. Das, MUKHOPADHYAY, IJMPD, 24, 1544026, 2015 U. Das, MUKHOPADHYAY, JCAP, 05, 045, 2015b U. Das, MUKHOPADHYAY, JCAP, 05, 015, 2015a U. Das, MUKHOPADHYAY, Phys. Rev. D, 91, 028302, 2015c U. Das, MUKHOPADHYAY, JCAP, 06, 050, 2014a U. Das, MUKHOPADHYAY, MPLA, 29, 1450035, 2014b M. V. Vishal, MUKHOPADHYAY, Phys. Rev. C, 89, 065804, 2014 U. Das, MUKHOPADHYAY, Phys. Rev. Lett., 110, 071102, 2013a U. Das, MUKHOPADHYAY, A. R. Rao, ApJLett., 767, 14, 2013 U. Das, MUKHOPADHYAY, IJMPD, 22, 1342004, 2013b U. Das, MUKHOPADHYAY, Phys. Rev. D, 86, 041001, 2012a U. Das, MUKHOPADHYAY, IJMPD, 21, 1242001, 2012b A. Kundu, MUKHOPADHYAY, MPLA, 27, 1250084, 2012 Flow-Chart of Evolution of our Idea Since last 5 years or so, we have initiated exploring highly magnetized super-Chandrasekhar white dwarfs (B-WDs), explaining peculiar type Ia supernovae: Over-luminous Many groups joined
    [Show full text]
  • Nd AAS Meeting Abstracts
    nd AAS Meeting Abstracts 101 – Kavli Foundation Lectureship: The Outreach Kepler Mission: Exoplanets and Astrophysics Search for Habitable Worlds 200 – SPD Harvey Prize Lecture: Modeling 301 – Bridging Laboratory and Astrophysics: 102 – Bridging Laboratory and Astrophysics: Solar Eruptions: Where Do We Stand? Planetary Atoms 201 – Astronomy Education & Public 302 – Extrasolar Planets & Tools 103 – Cosmology and Associated Topics Outreach 303 – Outer Limits of the Milky Way III: 104 – University of Arizona Astronomy Club 202 – Bridging Laboratory and Astrophysics: Mapping Galactic Structure in Stars and Dust 105 – WIYN Observatory - Building on the Dust and Ices 304 – Stars, Cool Dwarfs, and Brown Dwarfs Past, Looking to the Future: Groundbreaking 203 – Outer Limits of the Milky Way I: 305 – Recent Advances in Our Understanding Science and Education Overview and Theories of Galactic Structure of Star Formation 106 – SPD Hale Prize Lecture: Twisting and 204 – WIYN Observatory - Building on the 308 – Bridging Laboratory and Astrophysics: Writhing with George Ellery Hale Past, Looking to the Future: Partnerships Nuclear 108 – Astronomy Education: Where Are We 205 – The Atacama Large 309 – Galaxies and AGN II Now and Where Are We Going? Millimeter/submillimeter Array: A New 310 – Young Stellar Objects, Star Formation 109 – Bridging Laboratory and Astrophysics: Window on the Universe and Star Clusters Molecules 208 – Galaxies and AGN I 311 – Curiosity on Mars: The Latest Results 110 – Interstellar Medium, Dust, Etc. 209 – Supernovae and Neutron
    [Show full text]
  • The Ejected Mass Distribution of Type Ia Supernovae: a Significant Rate of Non-Chandrasekhar-Mass Progenitors
    View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by The Australian National University MNRAS 445, 2535–2544 (2014) doi:10.1093/mnras/stu1808 The ejected mass distribution of Type Ia supernovae: a significant rate of non-Chandrasekhar-mass progenitors R. A. Scalzo,1,2‹ A. J. Ruiter1,2,3 andS.A.Sim2,4 1Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT 2611, Australia 2ARC Centre of Excellence for All-Sky Astrophysics (CAASTRO), The Australian National University, Cotter Road, Weston Creek ACT 2611 Australia 3Max-Planck-Institut fur¨ Astrophysik, Karl-Schwarzschild-Str. 1, D-85741 Garching bei Munchen,¨ Germany 4Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, Belfast, BT7 1NN, UK Accepted 2014 September 1. Received 2014 August 21; in original form 2014 June 30 Downloaded from ABSTRACT The ejected mass distribution of Type Ia supernovae (SNe Ia) directly probes progenitor evolutionary history and explosion mechanisms, with implications for their use as cosmological probes. Although the Chandrasekhar mass is a natural mass scale for the explosion of white http://mnras.oxfordjournals.org/ dwarfs as SNe Ia, models allowing SNe Ia to explode at other masses have attracted much recent attention. Using an empirical relation between the ejected mass and the light-curve 56 width, we derive ejected masses Mej and Ni masses MNi for a sample of 337 SNe Ia with redshifts z<0.7 used in recent cosmological analyses. We use hierarchical Bayesian inference to reconstruct the joint Mej–MNi distribution, accounting for measurement errors.
    [Show full text]