An Ejecta Kinematics Study of Kepler’s Supernova Remnant with High-Resolution Chandra HETG Spectroscopy

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dc.contributor.authorMillard, Matthew J.
dc.contributor.authorBhalerao, Jayant
dc.contributor.authorPark, Sangwook
dc.contributor.authorSato, Toshiki
dc.contributor.authorHughes, John P.
dc.contributor.authorSlane, Patrick
dc.contributor.authorPatnaude, Daniel
dc.contributor.authorBurrows, David
dc.contributor.authorBadenes, Carles
dc.date.accessioned2020-01-30T18:11:13Z
dc.date.available2020-01-30T18:11:13Z
dc.date.issued2019-05-16
dc.description.abstractWe report measurements of the bulk radial velocity from a sample of small, metal-rich ejecta knots in Kepler's Supernova Remnant (SNR). We measure the Doppler shift of the He-like Si Kα line center energy in the spectra of these knots from our Chandra High-Energy Transmission Grating Spectrometer (HETGS) observation to estimate their radial velocities. We estimate high radial velocities of up to ∼ 8,000 km s⁻¹ for some of these ejecta knots. We also measure proper motions for our sample based on the archival Chandra Advanced CCD Imaging Spectrometer (ACIS) data taken in 2000, 2006, and 2014. Our measured radial velocities and proper motions indicate that some of these ejecta knots are nearly freely-expanding after ∼ 400 years since the explosion. The fastest moving knots showed proper motions up to ∼ 0.2 arcseconds per year. Based on our radial velocity measurements, we estimate a distance to Kepler's SNR, d ∼ 4.8 to 8.2 kpc. We find that the ejecta knots in our sample have an average space velocity of ∣Vₛ∣∼ 4,600 km s⁻¹ (at a distance of 6 kpc). We note that 8 out of the 15 ejecta knots from our sample show a statistically significant (at the 90% confidence level) redshifted spectrum, compared to only 2 with a blueshifted spectrum, suggesting an asymmetry in the ejecta distribution in Kepler's SNR along the line of sight.en_US
dc.description.sponsorshipThis work has been supported in part by NASA Chandra Grants GO6-17060X and AR7-18006X. J.P.H. acknowledges support for supernova remnant research from NASA grant NNX15AK71G to Rutgers University. T.S. was supported by the Japan Society for the Promotion of Science (JSPS) KAKENHI Grant Number JP19K14739 and the Special Postdoctoral Researchers Program in RIKEN.en_US
dc.description.urihttps://arxiv.org/abs/1905.04475en_US
dc.format.extent14 pagesen_US
dc.genrejournal articles preprintsen_US
dc.identifierdoi:10.13016/m25atl-xc5i
dc.identifier.citationMillard, Matthew J.; Bhalerao, Jayant; Park, Sangwook; Sato, Toshiki; Hughes, John P.; Slane, Patrick; Patnaude, Daniel; Burrows, David; Badenes, Carles; An Ejecta Kinematics Study of Kepler’s Supernova Remnant with High-Resolution Chandra HETG Spectroscopy; High Energy Astrophysical Phenomena (2019); https://arxiv.org/abs/1905.04475en_US
dc.identifier.urihttp://hdl.handle.net/11603/17195
dc.language.isoen_USen_US
dc.relation.isAvailableAtThe University of Maryland, Baltimore County (UMBC)
dc.relation.ispartofUMBC Physics Department Collection
dc.rightsThis item is likely protected under Title 17 of the U.S. Copyright Law. Unless on a Creative Commons license, for uses protected by Copyright Law, contact the copyright holder or the author.
dc.subjectradial velocityen_US
dc.subjectSupernova Remnant (SNR)en_US
dc.subjectdoppler shiften_US
dc.subjectHigh-Energy Transmission Grating Spectrometer (HETGS)en_US
dc.titleAn Ejecta Kinematics Study of Kepler’s Supernova Remnant with High-Resolution Chandra HETG Spectroscopyen_US
dc.typeTexten_US

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