adsabs/AstroCLIMB huggingface dataset:
Paper: A Search for Lensed Lyα Emitters within the Early HETDEX Data Set
Authors: Isaac H. Laseter, Steven L. Finkelstein, Micaela J. Bagley, Dustin M. Davis, Karl Gebhardt, Caryl Gronwall, Robin Ciardullo, Gregory R. Zeimann, Erin Mentuch Cooper, Daniel Farrow
Figure caption: Color–magnitude diagram for all SDSS galaxies between the spectroscopic redshift range of 0.4 ≲ z ≲ 0.7. The region between the red lines designates the foreground galaxy sample. The bottom, leftward tail of the CMD consists of predominantly blue, star-forming galaxies and QSO interlopers. The foreground galaxy sample region was chosen to eliminate star-forming galaxies that could contaminate the sample. If any of our chosen potential lens systems exhibited emission lines from the lens galaxy, they were eliminated from the candidate catalog in the analysis stage, which is discussed in Section 3.3.
Paper: A Search for Lensed Lyα Emitters within the Early HETDEX Data Set
Authors: Isaac H. Laseter, Steven L. Finkelstein, Micaela J. Bagley, Dustin M. Davis, Karl Gebhardt, Caryl Gronwall, Robin Ciardullo, Gregory R. Zeimann, Erin Mentuch Cooper, Daniel Farrow
Figure caption: 20181225v008-9900000001. Top Left: Two best VIRUS fibers, pixel flats, smoothed VIRUS fibers, and weighted sum of fibers. Top Middle: Gaussian fit to emission line. Top Right: Best available imaging on location of lensed LAE candidate. Bottom: Full spectrum of lensed LAE candidate. The yellow box with a dashed line denotes the location of Lyα.
Paper: A Search for Lensed Lyα Emitters within the Early HETDEX Data Set
Authors: Isaac H. Laseter, Steven L. Finkelstein, Micaela J. Bagley, Dustin M. Davis, Karl Gebhardt, Caryl Gronwall, Robin Ciardullo, Gregory R. Zeimann, Erin Mentuch Cooper, Daniel Farrow
Figure caption: Distribution of foreground galaxy redshift and magnification. The three dotted lines represent the magnification cutoff for strong lensing, intermediate lensing, and weak lensing. As can be seen in the histogram to the right, a substantial sample of our candidates are in the strong lensing regime. The histogram presented above the scatter plot represents the foreground redshift distribution.
Paper: A Search for Lensed Lyα Emitters within the Early HETDEX Data Set
Authors: Isaac H. Laseter, Steven L. Finkelstein, Micaela J. Bagley, Dustin M. Davis, Karl Gebhardt, Caryl Gronwall, Robin Ciardullo, Gregory R. Zeimann, Erin Mentuch Cooper, Daniel Farrow
Figure caption: Distribution of source galaxy redshift and magnification, with dotted lines and histograms representing the same info from Figure 5.
Paper: A Search for Lensed Lyα Emitters within the Early HETDEX Data Set
Authors: Isaac H. Laseter, Steven L. Finkelstein, Micaela J. Bagley, Dustin M. Davis, Karl Gebhardt, Caryl Gronwall, Robin Ciardullo, Gregory R. Zeimann, Erin Mentuch Cooper, Daniel Farrow
Figure caption: 20181115v016-9900030004. Top Left: Two best VIRUS fibers, pixel flats, smoothed VIRUS fibers, and weighted sum of fibers. Top Middle: Gaussian fit to emission line. Top Right: Best available imaging on location of lensed LAE candidate. Bottom: Full spectrum of lensed LAE candidate. The yellow box with a dashed line denotes the location of Lyα.
Paper: The Dust Sublimation Region of the Type 1 AGN NGC 4151 at a Hundred Microarcsecond Scale as Resolved by the CHARA Array Interferometer
Authors: Makoto Kishimoto, Matthew Anderson, Theo ten Brummelaar, Christopher Farrington, Robert Antonucci, Sebastian Hönig, Florentin Millour, Konrad R. W. Tristram, Gerd Weigelt, Laszlo Sturmann, Judit Sturmann, Gail Schaefer, Nic Scott
Figure caption: Thin-ring radius implied by each visibility observed (after the small correction for the putative AD component), plotted along the PA of the corresponding baseline. The PA of the optical polarization (94°), indicative of the system polar axis, is shown as the inner dashed–solid line, while the PA of the linear radio jet structure (84°; components D1/D2/D3 over 50 mas scale; Mundell et al. 2003) is indicated with the outer dashed–solid line segments.
Paper: The Dust Sublimation Region of the Type 1 AGN NGC 4151 at a Hundred Microarcsecond Scale as Resolved by the CHARA Array Interferometer
Authors: Makoto Kishimoto, Matthew Anderson, Theo ten Brummelaar, Christopher Farrington, Robert Antonucci, Sebastian Hönig, Florentin Millour, Konrad R. W. Tristram, Gerd Weigelt, Laszlo Sturmann, Judit Sturmann, Gail Schaefer, Nic Scott
Figure caption: Observed visibility squared V 2 as a function of projected baselines. In addition to our CHARA Array data at ∼30 m and ∼200−250 m baselines, we also plotted visibilities observed at Keck interferometer (Kishimoto et al. 2013 and references therein). V 2 for Gaussian with HWHM of 0.3 and 0.4 mas are also plotted for reference in dotted and dashed curves, respectively.
Paper: The Dust Sublimation Region of the Type 1 AGN NGC 4151 at a Hundred Microarcsecond Scale as Resolved by the CHARA Array Interferometer
Authors: Makoto Kishimoto, Matthew Anderson, Theo ten Brummelaar, Christopher Farrington, Robert Antonucci, Sebastian Hönig, Florentin Millour, Konrad R. W. Tristram, Gerd Weigelt, Laszlo Sturmann, Judit Sturmann, Gail Schaefer, Nic Scott
Figure caption: Sampled uv points, color-coded with observed visibility squared.
Paper: Comparison of Two Methods for Deriving the Magnetic Field in a Filament Channel
Authors: T. A. Kucera, M. Luna, T. Török, K. Muglach, J. T. Karpen, C. Downs, X. Sun, B. J. Thompson, H. R. Gilbert
Figure caption: RBSL flux rope used to model the magnetic field of filament F2. (a) Footprint locations (circles) and axis (red line) of the rope in a top-down view, prior to MHD relaxation. The green line shows the PIL section at 1.005 R ⊙ that was used to construct the axis; B  r (r = 1 R ⊙) is shown in blue/red colors. Scales are solar longitude and latitude in degrees, respectively. (b) Magnetic-field lines after MHD relaxation (arbitrary colors) as viewed from Earth at 04:28 UT on 2014 May 30 (see Figure 7(a)). The field of view is slightly larger than in (a); B  r (r = 1 R ⊙) is shown in gray scale.
Paper: Comparison of Two Methods for Deriving the Magnetic Field in a Filament Channel
Authors: T. A. Kucera, M. Luna, T. Török, K. Muglach, J. T. Karpen, C. Downs, X. Sun, B. J. Thompson, H. R. Gilbert
Figure caption: Histogram showing in green the distribution of the radii of curvature of the dipped field lines in the RBSL model and the corresponding periods calculated with Equation (2). The yellow histogram values represent the periods measured from the F2 oscillations listed in Table 1.
Paper: Comparison of Two Methods for Deriving the Magnetic Field in a Filament Channel
Authors: T. A. Kucera, M. Luna, T. Török, K. Muglach, J. T. Karpen, C. Downs, X. Sun, B. J. Thompson, H. R. Gilbert
Figure caption: Schematic defining the criteria used to compare a model flux-rope field line (blue solid line) and an observed oscillation in the plane of the sky (brown solid line). D is the distance between the center of the dip in a given model field line (solid blue circle) and the location along the oscillation track corresponding to the equilibrium position of the plasma (solid brown circle). The angle α measures the angle between the respective tangents to the field line at the dip (blue dashed line) and to the track at the equilibrium point (brown dashed line).
Paper: X-Ray and Radio Observations of Central Black Holes in Nearby Low-mass Early-type Galaxies: Preliminary Evidence for Low Eddington Fractions
Authors: Ryan Urquhart, Lauren I. McDermott, Jay Strader, Anil C. Seth, Laura Chomiuk, Nadine Neumayer, Dieu D. Nguyen, Evangelia Tremou
Figure caption: The core of NGC 5102, as imaged by (a) Chandra/ACIS in the 0.3–7 keV band; (b) Hubble Space Telescope/Wide Field Camera 2 (HST/WFC2) in the F569W filter (the 0.″9 red and green error circles indicate the X-ray positions of the nuclear and non-nuclear X-ray sources, respectively); (c) Australia Telescope Compact Array (ATCA) in the 6B configuration at 1.6 GHz; (d) ATCA in the 6B configuration at 2.6 GHz; (e) ATCA in the 1.5D configuration at 1.6 GHz; (f) ATCA in the 1.5D configuration at 2.6 GHz; (g) ATCA in the 6A configuration at 1.6 GHz; (h) ATCA in the 6A configuration at 2.6 GHz; (i) Australia Square Kilometer Array Pathfinder at 0.9 GHz; (j) Very Large Array (VLA) at 6 GHz. In the radio images, the red cross indicates the Gaia position of the nuclear source, and the FWHM extent of the synthesized beam is plotted as a white ellipse in the bottom left corner. The Gaia position is not included in panel (i) due to the uncertain astrometry. Green contours are set at ﹩2\sqrt{{2}^{n}}\times \sigma ﹩, where σ is the local rms and n = 1, 2, 3, 4....
Paper: X-Ray and Radio Observations of Central Black Holes in Nearby Low-mass Early-type Galaxies: Preliminary Evidence for Low Eddington Fractions
Authors: Ryan Urquhart, Lauren I. McDermott, Jay Strader, Anil C. Seth, Laura Chomiuk, Nadine Neumayer, Dieu D. Nguyen, Evangelia Tremou
Figure caption: Left: spectral index map for the ATCA/1.5D image, centered on the core of NGC 5102. Right: error on spectral index. Green contours taken from Figure 1(e) for reference.
Paper: Proper Motions, Orbits, and Tidal Influences of Milky Way Dwarf Spheroidal Galaxies
Authors: Andrew B. Pace, Denis Erkal, Ting S. Li
Figure caption: Comparison between the orbital direction and spatial orientation of the dSphs. Symbols and colors follow Figure 5. (Left) Difference between the reflex-corrected proper motion (i.e., the orbital direction) and the position angle (i.e., spatial orientation) ∣θ  μ  − θ xy∣ vs. the pericenter. When ∣θ  μ  − θ xy∣ ∼ 0, the orbit and major axis of the dSph are aligned. The blue error bar is from the reflex-corrected proper motion, and the black error bar is due to the distribution in the position angle. (Center left) ∣θ  μ  − θ xy∣ vs. ellipticity of the dSph. (Center right) Histogram of ∣θ  μ  − θ xy∣ for the same sample. To simulate errors we draw from each dSph’s ∣θ  μ  − θ xy∣ distribution 1000 times. The black bins are a subset of dSphs with smaller uncertainties. There is an excess of dSphs aligned with their orbital motion. (Right) Histogram of ∣θ  μ  − θ xy∣ but separated by ellipticity. The blue bins are the elongated sample (ϵ > 0.4). There is a clear preference for systems with large ellipticity to align with their orbital direction.
Paper: Proper Motions, Orbits, and Tidal Influences of Milky Way Dwarf Spheroidal Galaxies
Authors: Andrew B. Pace, Denis Erkal, Ting S. Li
Figure caption: Comparison of the pericenter (r peri) with and without the LMC influence (left panel and right panel, respectively) vs. the average density within the half-light radius calculated from the stellar kinematics (ρ 1/2). The black line shows twice the enclosed MW density as a function of the radius. If the satellite sits below this line, its Jacobi radius will be larger than the half-light radius, and it will likely be tidal disrupting. Satellites near or below the curve are labeled. Orange symbols denote dSphs, which are clearly tidally disrupting: Ant II, Sgr, and Tuc III. Green symbols denote dSphs that are potentially undergoing tidal disruption and near the MW average density: Boo I, Boo III, Cra II, Gru II, Seg 2, and Tuc IV (see text for details).
Paper: Proper Motions, Orbits, and Tidal Influences of Milky Way Dwarf Spheroidal Galaxies
Authors: Andrew B. Pace, Denis Erkal, Ting S. Li
Figure caption: Correlation plots of dSphs in terms of their densities, ellipticities, pericenters, and half-light radii. Symbols and colors are the same as Figure 5. Left panel: ellipticity (ϵ) vs. average dSph density divided by the average MW density at the dSph’s pericenter (ρ 1/2/ρ MW(r = r peri)). Center panel: ellipticity (ϵ) vs. pericenter (r peri). Right panel: half-light radius (r 1/2) vs. pericenter (r peri). There is no clear trend for the pericenter or the average density ratio with the ellipticity (left and middle panels). The dSphs with evidence of tidal disruption and the smallest ρ 1/2/ρ MW(r = r peri) ratios have larger half-light radii at a fixed pericenter than the general dSph population (right panel).
Paper: Proper Motions, Orbits, and Tidal Influences of Milky Way Dwarf Spheroidal Galaxies
Authors: Andrew B. Pace, Denis Erkal, Ting S. Li
Figure caption: Distance to the LMC vs. relative velocity at each satellite’s previous closest LMC approach (left) and current distance vs. current relative velocity (right). Red symbols denote the candidate LMC satellite population (Car II, Car III, Hyi I, Hor I, Phx II, Ret II). The black line is the LMC escape velocity curve with M LMC = 13.8 × 1010 M ⊙. The satellite with the closest approach is Tuc IV (gold circle), which is not considered an LMC satellite due to its large relative velocity. Currently, Sgr II (green symbol) is closer to the MW than the LMC and is more likely to be associated with the MW. The five satellites at large distances with low relative velocities (they are Dra, Dra II, UMi, Cra II, Car I) are not bound to the LMC. Most of them are closer to the MW at the time of closest approach.
Paper: Proper Motions, Orbits, and Tidal Influences of Milky Way Dwarf Spheroidal Galaxies
Authors: Andrew B. Pace, Denis Erkal, Ting S. Li
Figure caption: Results of the mixture model for four dSphs, from top to bottom: Boo III, CB, Hyd II, and UMi. The four rows are the spatial distribution (tangent plane), the proper motion (vector point diagram), a DECam-based color–magnitude diagram (not included for UMi), and a Gaia color–magnitude diagram. Points with membership probability p > 0.01 are colored according to their probability; the rest are considered MW foreground stars and are shown as gray points. The red arrow points toward the Galactic center, and the orange arrow is the direction of the reflex-corrected proper motion, which is approximately equal to the orbital motion. Two ellipses are included in the spatial distribution at one and three times the half-light radius.
Paper: Proper Motions, Orbits, and Tidal Influences of Milky Way Dwarf Spheroidal Galaxies
Authors: Andrew B. Pace, Denis Erkal, Ting S. Li
Figure caption: Color–magnitude selection based on spectroscopic members (see Tables 1, 4 for citations). (Left) DECam-based selection. The same filter is used for most of the DECam dSphs. (Middle) PS1-based selection. The filter is expanded at faint magnitudes based on photometric errors. (Right) Gaia-based selection for Dra. A similar selection is made based on spectroscopic members for the other bright dSphs.
Paper: Proper Motions, Orbits, and Tidal Influences of Milky Way Dwarf Spheroidal Galaxies
Authors: Andrew B. Pace, Denis Erkal, Ting S. Li
Figure caption: Phase-space diagram for the MW dSphs where the x-axis shows the distance to the Galactic center (GC) and the y-axis shows the total velocity in 3D, where positive (negative) indicates that the dSph is moving away from (toward) the GC. The black lines represent the escape velocity of the MW.
Paper: Proper Motions, Orbits, and Tidal Influences of Milky Way Dwarf Spheroidal Galaxies
Authors: Andrew B. Pace, Denis Erkal, Ting S. Li
Figure caption: Comparison of the orbital pericenter and apocenter of dSphs with a large relative change (>25% in either) in MW potentials with (orange points) and without (blue points) the presence of the LMC.
Paper: Collimation of the Relativistic Jet in the Quasar 3C 273
Authors: Hiroki Okino, Kazunori Akiyama, Keiichi Asada, José L. Gómez, Kazuhiro Hada, Mareki Honma, Thomas P. Krichbaum, Motoki Kino, Hiroshi Nagai, Uwe Bach, Lindy Blackburn, Katherine L. Bouman, Andrew Chael, Geoffrey B. Crew, Sheperd S. Doeleman, Vincent L. Fish, Ciriaco Goddi, Sara Issaoun, Michael D. Johnson, Svetlana Jorstad, Shoko Koyama, Colin J. Lonsdale, Ru-Sen Lu, Ivan Martí-Vidal, Lynn D. Matthews, Yosuke Mizuno, Kotaro Moriyama, Masanori Nakamura, Hung-Yi Pu, Eduardo Ros, Tuomas Savolainen, Fumie Tazaki, Jan Wagner, Maciek Wielgus, Anton Zensus
Figure caption: Multifrequency images of 3C 273 jets with the HSA at 43, 22, and 15 GHz and the VLBA at 1.7 GHz. Each panel shows the mean top-set image at each frequency restored by the circular Gaussian beam with the beam solid angle of the uniform-weighting beam size in Table 1. The lowest contour levels are 6.5 mJy beam−1 at 43 GHz, 8.2 mJy beam−1 at 22 GHz, 7.1 mJy beam−1 at 15 GHz, and 11.6 mJy beam−1 at 1.7 GHz. The contours for all images are multiplied by a factor of 2. The lowest contour level of each image is estimated from the mean residual image rms of the top-set reconstructions.
Paper: Collimation of the Relativistic Jet in the Quasar 3C 273
Authors: Hiroki Okino, Kazunori Akiyama, Keiichi Asada, José L. Gómez, Kazuhiro Hada, Mareki Honma, Thomas P. Krichbaum, Motoki Kino, Hiroshi Nagai, Uwe Bach, Lindy Blackburn, Katherine L. Bouman, Andrew Chael, Geoffrey B. Crew, Sheperd S. Doeleman, Vincent L. Fish, Ciriaco Goddi, Sara Issaoun, Michael D. Johnson, Svetlana Jorstad, Shoko Koyama, Colin J. Lonsdale, Ru-Sen Lu, Ivan Martí-Vidal, Lynn D. Matthews, Yosuke Mizuno, Kotaro Moriyama, Masanori Nakamura, Hung-Yi Pu, Eduardo Ros, Tuomas Savolainen, Fumie Tazaki, Jan Wagner, Maciek Wielgus, Anton Zensus
Figure caption: The inner-jet image of 3C 273 obtained with the GMVA observation including ALMA at 86 GHz. Here we show the mean of the top-set reconstructions restored at the resolution with a uniform weighting scheme. The image is restored with a circular beam of 57 μas (indicated in the bottom left corner) corresponding to the geometric mean of the uniform-weighting beam of 61 × 52 μas. The peak intensity is 0.69 Jy beam−1. The contours are multiplies by factors of 2, from the lowest contour level of 6.5 mJy beam−1.
Paper: Collimation of the Relativistic Jet in the Quasar 3C 273
Authors: Hiroki Okino, Kazunori Akiyama, Keiichi Asada, José L. Gómez, Kazuhiro Hada, Mareki Honma, Thomas P. Krichbaum, Motoki Kino, Hiroshi Nagai, Uwe Bach, Lindy Blackburn, Katherine L. Bouman, Andrew Chael, Geoffrey B. Crew, Sheperd S. Doeleman, Vincent L. Fish, Ciriaco Goddi, Sara Issaoun, Michael D. Johnson, Svetlana Jorstad, Shoko Koyama, Colin J. Lonsdale, Ru-Sen Lu, Ivan Martí-Vidal, Lynn D. Matthews, Yosuke Mizuno, Kotaro Moriyama, Masanori Nakamura, Hung-Yi Pu, Eduardo Ros, Tuomas Savolainen, Fumie Tazaki, Jan Wagner, Maciek Wielgus, Anton Zensus
Figure caption: Spectral index maps between pairs of neighboring frequencies labeled in the top right corner of each panel. Spectral index α is defined by I  ν  ∝ ν  α . Spectral index values in each pair were calculated from all images in the top sets of both frequencies after aligning the images using cross-correlation (Section 4.1) and averaging them. The contours in each panel represent the mean image of the lower frequency of the HSA as shown in Figure 5.
Paper: Collimation of the Relativistic Jet in the Quasar 3C 273
Authors: Hiroki Okino, Kazunori Akiyama, Keiichi Asada, José L. Gómez, Kazuhiro Hada, Mareki Honma, Thomas P. Krichbaum, Motoki Kino, Hiroshi Nagai, Uwe Bach, Lindy Blackburn, Katherine L. Bouman, Andrew Chael, Geoffrey B. Crew, Sheperd S. Doeleman, Vincent L. Fish, Ciriaco Goddi, Sara Issaoun, Michael D. Johnson, Svetlana Jorstad, Shoko Koyama, Colin J. Lonsdale, Ru-Sen Lu, Ivan Martí-Vidal, Lynn D. Matthews, Yosuke Mizuno, Kotaro Moriyama, Masanori Nakamura, Hung-Yi Pu, Eduardo Ros, Tuomas Savolainen, Fumie Tazaki, Jan Wagner, Maciek Wielgus, Anton Zensus
Figure caption:  uv coverage of the GMVA observation at 86 GHz. Baselines to ALMA are shown in red. Data are averaged at 60 s.
Paper: Collimation of the Relativistic Jet in the Quasar 3C 273
Authors: Hiroki Okino, Kazunori Akiyama, Keiichi Asada, José L. Gómez, Kazuhiro Hada, Mareki Honma, Thomas P. Krichbaum, Motoki Kino, Hiroshi Nagai, Uwe Bach, Lindy Blackburn, Katherine L. Bouman, Andrew Chael, Geoffrey B. Crew, Sheperd S. Doeleman, Vincent L. Fish, Ciriaco Goddi, Sara Issaoun, Michael D. Johnson, Svetlana Jorstad, Shoko Koyama, Colin J. Lonsdale, Ru-Sen Lu, Ivan Martí-Vidal, Lynn D. Matthews, Yosuke Mizuno, Kotaro Moriyama, Masanori Nakamura, Hung-Yi Pu, Eduardo Ros, Tuomas Savolainen, Fumie Tazaki, Jan Wagner, Maciek Wielgus, Anton Zensus
Figure caption: Standard deviation of the top-set reconstructions of GMVA 86 GHz restored with the circular Gaussian beam of 57 μas shown by the white circle in the bottom left corner. The contours represent the mean image shown in Figure 3.
Paper: Collimation of the Relativistic Jet in the Quasar 3C 273
Authors: Hiroki Okino, Kazunori Akiyama, Keiichi Asada, José L. Gómez, Kazuhiro Hada, Mareki Honma, Thomas P. Krichbaum, Motoki Kino, Hiroshi Nagai, Uwe Bach, Lindy Blackburn, Katherine L. Bouman, Andrew Chael, Geoffrey B. Crew, Sheperd S. Doeleman, Vincent L. Fish, Ciriaco Goddi, Sara Issaoun, Michael D. Johnson, Svetlana Jorstad, Shoko Koyama, Colin J. Lonsdale, Ru-Sen Lu, Ivan Martí-Vidal, Lynn D. Matthews, Yosuke Mizuno, Kotaro Moriyama, Masanori Nakamura, Hung-Yi Pu, Eduardo Ros, Tuomas Savolainen, Fumie Tazaki, Jan Wagner, Maciek Wielgus, Anton Zensus
Figure caption: The signal-to-noise ratios of visibilities on 3C 273 as a function of projected baseline length. Data are averaged at 60 s. Baselines to ALMA are shown in red.
Paper: Discovery of Year-scale Time Variability from Thermal X-Ray Emission in Tycho’s Supernova Remnant
Authors: Masamune Matsuda, Hiroyuki Uchida, Takaaki Tanaka, Hiroya Yamaguchi, Takeshi Go Tsuru
Figure caption: Best-fit results of kT  e  for Knot1 (same as the left panel of Figure 6) and calculated time variations with assumptions of u c = 1500 km s−1 (left), 2000 km s−1 (middle), and 2500 km s−1 (right). The solid, dashed, dotted, and dashed–dotted lines represent cases of β 0 = m  e /m  p  ≃ 1/2000, 0.05, 0.08, and 0.1, respectively.
Paper: Discovery of Year-scale Time Variability from Thermal X-Ray Emission in Tycho’s Supernova Remnant
Authors: Masamune Matsuda, Hiroyuki Uchida, Takaaki Tanaka, Hiroya Yamaguchi, Takeshi Go Tsuru
Figure caption: Ion fractions of Ne9+ (top) and Mg11+ (bottom), i.e., H-like ions as a function of kT  e  and n  e  t. The dotted and solid line contours show Δχ 2 = 1.0 and 2.3 confidence levels, respectively, in 2003 (blue), 2007 (red), 2009 (green), and 2015 (white). The points represent the best-fit parameters in each year. For 2000 data, we show only the uncertainty of kT  e  since n  e  t was fixed in our analysis (see the text).
Paper: Discovery of Year-scale Time Variability from Thermal X-Ray Emission in Tycho’s Supernova Remnant
Authors: Masamune Matsuda, Hiroyuki Uchida, Takaaki Tanaka, Hiroya Yamaguchi, Takeshi Go Tsuru
Figure caption: Best-fit results of kT  e  for Knot1 (same as the left panel of Figure 6) and calculated time variations with assumptions of u c = 800 km s−1 (left), 900 km s−1 (middle), 1000 km s−1 (right). The solid, dashed–dotted, dashed, dotted, and dashed–dotted–dotted lines represent cases of β 0 = m  e /m  p  ≃ 1/2000, 0.1, 0.15, 0.2, and 0.3, respectively.
Paper: Discovery of Year-scale Time Variability from Thermal X-Ray Emission in Tycho’s Supernova Remnant
Authors: Masamune Matsuda, Hiroyuki Uchida, Takaaki Tanaka, Hiroya Yamaguchi, Takeshi Go Tsuru
Figure caption: Left: soft-band Chandra image taken in 2015 (same as the rightmost panel of Figure 2) overlaid with contours of an Hα image taken in 2012 (see the middle panel). Middle: Hα image obtained in 2012 with GHαFaS on the William Herschel Telescope (WHT; Knežević et al. 2017). Right: Hα image taken in 2008 with WFPC2 on HST (Lee et al. 2010).
Paper: Discovery of Year-scale Time Variability from Thermal X-Ray Emission in Tycho’s Supernova Remnant
Authors: Masamune Matsuda, Hiroyuki Uchida, Takaaki Tanaka, Hiroya Yamaguchi, Takeshi Go Tsuru
Figure caption: Same as Figure 9, but assuming the years 1998 (left) and 1999 (right) as t = 0 in the case of u c = 1500 km s−1.
Paper: Discovery of Year-scale Time Variability from Thermal X-Ray Emission in Tycho’s Supernova Remnant
Authors: Masamune Matsuda, Hiroyuki Uchida, Takaaki Tanaka, Hiroya Yamaguchi, Takeshi Go Tsuru
Figure caption: Same as Figure 11, but assuming the years 1996 (left) and 1998 (right) as t = 0 in the case of u c = 1000 km s−1.