Daniel Patnaude

Smithsonian Astrophysical Observatory

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Patrick Slane

Center for Astrophysics Harvard & Smithsonian

D. Milisavljević

Purdue University West Lafayette

Carles Badenes

Pittsburgh Supercomputing Center

Robert A. Fesen

Dartmouth College

J. C. Raymond

Center for Astrophysics Harvard & Smithsonian

S.-H. Lee

Kyoto University

Paul P. Plucinsky

Center for Astrophysics Harvard & Smithsonian

Donald C. Ellison

North Carolina State University

John P. Hughes

Rutgers, The State University of New Jersey

R. Margutti

University of California, Berkeley

Cooperative Institutions

University of Turku

273

University of Łódź

242

TU Dortmund University

236

Center for Astrophysics Harvard & Smithsonian

209

Niels Brock

193

Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas

188

Centre National de la Recherche Scientifique

180

University of Copenhagen

178

Universitat de Barcelona

163

Institut d'Estudis Espacials de Catalunya

163

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Evidence of a Type Ia Progenitor for Supernova Remnant 3C 397

arXiv (Cornell University) (2020)

Héctor Martínez‐Rodríguez Laura A. Lopez Katie Auchettl Carles Badenes Tyler Holland-Ashford

The explosive origin of the young supernova remnant (SNR) 3C 397 (G41.1-0.3) is debated. Its elongated morphology and proximity to a molecular cloud are suggestive of a core-collapse (CC) SN origin, yet recent X-ray studies of heavy metals show chemical yields and line centroid energies consistent with a Type Ia SN. In this paper, we analyze the full X-ray spectrum from 0.7-10 keV of 3C 397 observed with Suzaku and compare the line centroid energies, fluxes, and elemental abundances of intermediate-mass and heavy metals (Mg to Ni) to Type Ia and CC hydrodynamical model predictions. Based on the results, we conclude that 3C 397 likely arises from an energetic Type Ia explosion in a high-density ambient medium, and we show that the progenitor was a near Chandrasekhar mass white dwarf.

Line (geometry)

Chandrasekhar limit

10.48550/arxiv.2006.08681

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Citations (9)

HST Proper Motion Measurements of Supernova Remnant N132D: Center of Expansion and Age

arXiv (Cornell University) (2023)

John Banovetz D. Milisavljević Niharika Sravan Kathryn E. Weil B. M. Subrayan

We present proper motion measurements of oxygen-rich ejecta of the LMC supernova remnant N132D using two epochs of Hubble Space Telescope Advanced Camera for Surveys data spanning 16 years. The proper motions of 120 individual knots of oxygen-rich gas were measured and used to calculate a center of expansion (CoE) of $α$=05:25:01.71 and $δ$=-69:38:41.64 (J2000) with a 1-$σ$ uncertainty of 2.90 arcseconds. This new CoE measurement is 9.2 and 10.8 arcseconds from two previous CoE estimates based on the geometry of the optically emitting ejecta. We also derive an explosion age of 2770 $\pm$ 500 yr, which is consistent with recent age estimates of $\approx 2500$ yr made from 3D ejecta reconstructions. We verify our estimates of the CoE and age using a new automated procedure that detected and tracked the proper motions of 137 knots, with 73 knots that overlap with the visually identified knots. We find the proper motions of ejecta are still ballistic, despite the remnant's age, and are consistent with the notion that the ejecta are expanding into an ISM cavity. Evidence for explosion asymmetry from the parent supernova is also observed. Using the visually measured proper motion measurements and corresponding center of expansion and age, we compare N132D to other supernova remnants with proper motion ejecta studies.

Proper motion

10.48550/arxiv.2301.02128

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Astro2020 Science White Paper: Future X-ray Studies of Supernova Remnants

arXiv (Cornell University) (2019)

Brian J. Williams Katie Auchettl Carles Badenes Daniel Castro Oleg Kargaltsev

This is a white paper submitted in response to the call from the Astro2020 Decadal Survey Committee. We outline the scientific progress that will be made in the next few decades in the study of supernova remnants in the X-ray band, using observatories like Athena, Lynx, and AXIS.

White (mutation)

White paper

Near-Earth supernova

10.48550/arxiv.1904.05857

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Citations (1)

Effective area of the AXAF high-resolution camera (HRC)

Proceedings of SPIE, the International Society for Optical Engineering/Proceedings of SPIE (1998)

Daniel Patnaude Deron O. Pease Rich Donnelly M. Juda C. Jones

The Advanced X-Ray Astrophysics Facility High Resolution Camera was calibrated at NASA's X-Ray Calibration Facility during March and April 1997. We have undertaken an analysis of the effective area of the combined High Resolution Mirror Assembly/High Resolution Camera using all data presently available from these tests. In this contribution we discuss our spectral fitting of the beam-normalization detectors, our method of removing higher order contamination lines present in the spectra, and the corrections for beam non- uniformities. Using an approach based upon the mass absorption cross-section of Cesium Iodide, we determine the quantum efficiency in the microchannel plates. We model the secondary electron absorption depth as a function of energy, which we expect to be relatively smooth. This is then combined with the most recent model of the telescope to determine the ensemble effective area for the HRC. The ensemble effective area is a product of the telescope effective are, the transmission of the UV-Ion shield, and the quantum efficiency of the microchannel plates. We focus our attention on the microchannel plate quantum efficiency, using previous result for the UV-Ion shield transmission and telescope effective area. We also address future goals and concerns.

Microchannel plate detector

Quantum Efficiency

Microchannel

10.1117/12.331294

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Kinematic Study of Ejecta Knots in Kepler’s SNR Using The Chandra HETGS

American Astronomical Society Meeting Abstracts #231 (2018)

M. J. Millard Jayant Bhalerao Sangwook Park John P. Hughes Patrick Slane

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Three-Dimensional Kinematic Reconstruction of the Optically-Emitting, High-Velocity, Oxygen-Rich Ejecta of Supernova Remnant N132D

AAS (2020)

D. Milisavljević Charles J. Law Daniel Patnaude Paul P. Plucinsky Michael D. Gladders

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The Unprecedented Metamorphosis of Supernova 2014C: New Insights from New Observations by HST and Gemini

American Astronomical Society Meeting Abstracts #229 (2017)

D. Milisavljević Daniel Patnaude R. Margutti A. Kamble J. C. Raymond

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METAMORPHOSIS OF SN 2014C: DELAYED INTERACTION BETWEEN A HYDROGEN POOR CORE-COLLAPSE SUPERNOVA AND A NEARBY CIRCUMSTELLAR SHELL

The Astrophysical Journal (2015)

D. Milisavljević R. Margutti A. Kamble Daniel Patnaude J. C. Raymond

We present optical observations of supernova SN 2014C, which underwent an unprecedented slow metamorphosis from H-poor type Ib to H-rich type IIn over the course of one year. The observed spectroscopic evolution is consistent with the supernova having exploded in a cavity before encountering a massive shell of the progenitor star's stripped hydrogen envelope. Possible origins for the circumstellar shell include a brief Wolf-Rayet fast wind phase that overtook a slower red supergiant wind, eruptive ejection, or confinement of circumstellar material by external influences of neighboring stars. An extended high velocity Halpha absorption feature seen in near-maximum light spectra implies that the progenitor star was not completely stripped of hydrogen at the time of core collapse. Archival pre-explosion Subaru Telescope Suprime-Cam and Hubble Space Telescope Wide Field Planetary Camera 2 images of the region obtained in 2009 show a coincident source that is most likely a compact massive star cluster in NGC 7331 that hosted the progenitor system. By comparing the emission properties of the source with stellar population models that incorporate interacting binary stars we estimate the age of the host cluster to be 30 - 300 Myr, and favor ages closer to 30 Myr in light of relatively strong Halpha emission. SN 2014C is the best-observed member of a class of core-collapse supernovae that fill the gap between events that interact strongly with dense, nearby environments immediately after explosion and those that never show signs of interaction. Better understanding of the frequency and nature of this intermediate population can contribute valuable information about the poorly understood final stages of stellar evolution.

10.1088/0004-637x/815/2/120

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Citations (67)

Spectroscopic classification of optical transients

ATel (2016)

D. Milisavljević J. Parrent Daniel Patnaude A. Kamble R. Margutti

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Do Type Ia Supernovae Explode inside Planetary Nebulae?

The Astrophysical Journal (2024)

Travis Court Carles Badenes S.-H. Lee Daniel Patnaude Guillermo Garcı́a-Segura

Abstract The nature of Type Ia supernova (SN Ia) explosions remains an open issue, with several contending progenitor scenarios actively being considered. One such scenario involves an SN Ia explosion inside a planetary nebula (PN) in the aftermath of a stellar merger triggered by a common envelope (CE) episode. We examine this scenario using hydrodynamic and nonequilibrium ionization simulations of the interaction between the SN ejecta and the PN cocoon into the supernova remnant (SNR) phase, focusing on the impact of the delay between the CE episode and the SN explosion. We compare the bulk dynamics and X-ray spectra of our simulated SNRs to the observed properties of known Type Ia SNRs in the Milky Way and the Magellanic Clouds. We conclude that models where the SN explosion happens in the immediate aftermath of the CE episode (with a delay ≲1000 yr) are hard to reconcile with the observations, because the interaction with the dense PN cocoon results in ionization timescales much higher than those found in any known Type Ia SNR. Models with a longer delay between the CE episode and the SN explosion (∼10,000 yr) are closer to the observations, and may be able to explain the bulk properties of some Type Ia SNRs.

10.3847/1538-4357/ad165f

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Citations (1)