adsabs/AstroCLIMB huggingface dataset:
Paper: NICER Observations of Thermonuclear Bursts from 4U 1728-34: Detection of Oscillations prior to the Onset of Two Bursts
Authors: Z. Funda Bostancı, Tuğba Boztepe, Tolga Güver, Tod E. Strohmayer, Yuri Cavecchi, Ersin Göğüş, Diego Altamirano, Peter Bult, Deepto Chakrabarty, Sebastien Guillot, Gaurava K. Jaisawal, Christian Malacaria, Giulio C. Mancuso, Andrea Sanna, Jean H. Swank
Figure caption: Upper panels: under the assumption that there are oscillations at 356.1 Hz, 367.0 Hz, and 359.0 Hz, the evolution of the fractional rms amplitudes (black lines) is shown together with the burst light curves (red lines) in the 0.5–12, 0.5–6, and 6–12 keV bands for bursts 1, 3, and 10 (panels from left to right), respectively. Amplitudes are calculated in 1 s intervals for bursts 1 and 10 and in 2 s intervals for burst 3. Arrows indicate upper limits. The amplitudes are high in two bins (2 or 4 s for bursts 1 and 3) just before burst onset, then drop below the detection level during the burst peak. The horizontal blue dashed lines show the average values of rms amplitude calculated using the 100 s interval before the onset for bursts 1 and 3, and the 30 s interval before the onset for burst 10. Lower panels: phase-folded light curves (squares and stars with the error bars) obtained by folding 1 s intervals for bursts 1 and 10, and 2 s intervals for burst 3. The best-fitting sinusoidal models (solid lines) for the bins just before the onset (red) and the peak (blue) are also shown. Phase-folded light curves were normalized by constant values from the best-fitting sinusoidal models, for clarity.
Paper: FRAMEx. IV. Mechanical Feedback from the Active Galactic Nucleus in NGC 3079
Authors: Luis C. Fernandez, Nathan J. Secrest, Megan C. Johnson, Travis C. Fischer
Figure caption: From our 6 GHz VLBA observations using our model fitting of radio core components A and B. Images are 64 × 64 mas, centered on the core component A. The color bar is in units of mJy beam−1. The green ellipse is the convolved beam. Top row: untapered observation on 2020 May 19 with included 15× rms contours. Both the middle and bottom row images are tapered to 48 Mλ in the uv plane to constrain the data as close to a circular convolved beam with included 10× rms contours. Middle row: observation on 2020 January 27. Bottom row: observation on 2020 May 19.
Paper: NICER Observations of Thermonuclear Bursts from 4U 1728-34: Detection of Oscillations prior to the Onset of Two Bursts
Authors: Z. Funda Bostancı, Tuğba Boztepe, Tolga Güver, Tod E. Strohmayer, Yuri Cavecchi, Ersin Göğüş, Diego Altamirano, Peter Bult, Deepto Chakrabarty, Sebastien Guillot, Gaurava K. Jaisawal, Christian Malacaria, Giulio C. Mancuso, Andrea Sanna, Jean H. Swank
Figure caption: 0.5–10 keV light curves of detected thermonuclear X-ray bursts with contours of the candidate oscillations listed in Table 4. For bursts 4 and 10 we detect oscillations at two different frequencies; we therefore show these bursts twice. The vertical lines show the start time, the e-folding time, and the decay length, defined as the time over which the count rate declines to 10% of the peak.
Paper: NICER Observations of Thermonuclear Bursts from 4U 1728-34: Detection of Oscillations prior to the Onset of Two Bursts
Authors: Z. Funda Bostancı, Tuğba Boztepe, Tolga Güver, Tod E. Strohmayer, Yuri Cavecchi, Ersin Göğüş, Diego Altamirano, Peter Bult, Deepto Chakrabarty, Sebastien Guillot, Gaurava K. Jaisawal, Christian Malacaria, Giulio C. Mancuso, Andrea Sanna, Jean H. Swank
Figure caption: Upper panels: light curves of the X-ray bursts with a bin size of 0.5 s (black), where we modified the time axis of the plots to begin at the peak and contours of dynamical power spectra showing burst oscillations for bursts 1, 10, and 11 from 4U 1728−34 (from left to right). Contours refer to Z 2 ≥ 10 (blue) and ≥15 (red) up to the maximum with steps of 2. Lower panels: pulse profiles calculated using the 2 s interval together with the best-fitting sinusoidal model (blue line).
Paper: NICER Observations of Thermonuclear Bursts from 4U 1728-34: Detection of Oscillations prior to the Onset of Two Bursts
Authors: Z. Funda Bostancı, Tuğba Boztepe, Tolga Güver, Tod E. Strohmayer, Yuri Cavecchi, Ersin Göğüş, Diego Altamirano, Peter Bult, Deepto Chakrabarty, Sebastien Guillot, Gaurava K. Jaisawal, Christian Malacaria, Giulio C. Mancuso, Andrea Sanna, Jean H. Swank
Figure caption: Frequencies of the detected oscillations as a function of time since the peak of a burst. Only the oscillations that were selected in Section 3.2.1 are shown. The red dashed line shows the 363 Hz level. The color scale shows Z 2 values, while the size of the symbols grows with increasing fractional rms amplitude.
Paper: NICER Observations of Thermonuclear Bursts from 4U 1728-34: Detection of Oscillations prior to the Onset of Two Bursts
Authors: Z. Funda Bostancı, Tuğba Boztepe, Tolga Güver, Tod E. Strohmayer, Yuri Cavecchi, Ersin Göğüş, Diego Altamirano, Peter Bult, Deepto Chakrabarty, Sebastien Guillot, Gaurava K. Jaisawal, Christian Malacaria, Giulio C. Mancuso, Andrea Sanna, Jean H. Swank
Figure caption: Distribution of maximum Z 2 values obtained from all 73 NICER observations of 4U 1728−34, in the energy ranges 0.5–12 keV (left) and 6–12 keV (right). The red dashed lines show the maximum Z 2 values measured from the oscillations prior to the bursts in the related energy band.
Paper: NICER Observations of Thermonuclear Bursts from 4U 1728-34: Detection of Oscillations prior to the Onset of Two Bursts
Authors: Z. Funda Bostancı, Tuğba Boztepe, Tolga Güver, Tod E. Strohmayer, Yuri Cavecchi, Ersin Göğüş, Diego Altamirano, Peter Bult, Deepto Chakrabarty, Sebastien Guillot, Gaurava K. Jaisawal, Christian Malacaria, Giulio C. Mancuso, Andrea Sanna, Jean H. Swank
Figure caption: Values of touchdown flux (orange dots) and/or peak flux (blue squares) measured here compared with the average value of touchdown flux presented by Güver et al. (2012a), which is shown with the red solid line together with the systematic uncertainties shown with black dashed lines.
Paper: NICER Observations of Thermonuclear Bursts from 4U 1728-34: Detection of Oscillations prior to the Onset of Two Bursts
Authors: Z. Funda Bostancı, Tuğba Boztepe, Tolga Güver, Tod E. Strohmayer, Yuri Cavecchi, Ersin Göğüş, Diego Altamirano, Peter Bult, Deepto Chakrabarty, Sebastien Guillot, Gaurava K. Jaisawal, Christian Malacaria, Giulio C. Mancuso, Andrea Sanna, Jean H. Swank
Figure caption: Histograms of values of peak flux, blackbody temperature, and blackbody radius assuming a source distance of 5.31 kpc in the MINBAR catalog together with the same values measured with NICER for 10 bursts (black stars) reported here.
Paper: Planetary Engulfment Prognosis within the ρ CrB System
Authors: Stephen R. Kane
Figure caption: The final predicted stages of MS evolution for ρ CrB based on the MIST model described in Section 3, showing the evolution of stellar mass (top panel), radius (middle panel), and luminosity (bottom panel). The model depicts the transition through the RGB, horizontal branch, and AGB. The vertical dotted line indicates the current stellar age, and the gray shaded region represents the 1σ uncertainty on that age.
Paper: Planetary Engulfment Prognosis within the ρ CrB System
Authors: Stephen R. Kane
Figure caption: HZ and planetary orbits in the ρ CrB system, where the orbits are labeled by planet designation. The inner edge of the OHZ is shown in green and can be seen in the corners of the figure beyond the orbit of planet d. The scale of the figure is 1.77 au along each side.
Paper: Planetary Engulfment Prognosis within the ρ CrB System
Authors: Stephen R. Kane
Figure caption: Distance from the host star in au for the stellar evolution off the MS over 7 × 108 yr (top panel) and 107 yr (bottom panel). The radius of the star is shown as a blue line, and the dashed lines show the semimajor axes of the known planets. The location of the fluid-body Roche limit of the star is indicated by the dotted line.
Paper: Spectroscopic Detection of Alfvénic Waves in the Chromospheric Fibrils of a Solar-quiet Region
Authors: Hannah Kwak, Jongchul Chae, Eun-Kyung Lim, Kyoung-Sun Lee, Donguk Song, Heesu Yang
Figure caption: (a) A map of chromospheric intensity obtained from MLSI. The cyan line marks the selected fibril for detailed analysis in (b), (c), and (d). The contours in blue indicate the LOS magnetic field strengths of −30 and −200 G, and the contours in red indicate magnetic field strengths of 30 and 200 G. The darker shades of each color represent stronger magnetic field strength. (b) and (c) Time–distance plots of the LOS velocity and temperature constructed along the cyan line in the chromospheric intensity map (panel (a)). The velocity and temperature signals have been bandpass-filtered with periods from 1.5 to 22 minutes. (d) Temporal variations of the LOS velocity (green) and temperature (violet) at the position marked with a yellow dashed line in the time–distance plots (panels (b) and (c)).
Paper: Spectroscopic Detection of Alfvénic Waves in the Chromospheric Fibrils of a Solar-quiet Region
Authors: Hannah Kwak, Jongchul Chae, Eun-Kyung Lim, Kyoung-Sun Lee, Donguk Song, Heesu Yang
Figure caption: Left: SDO/HMI LOS magnetogram of a quiet-Sun region taken at 17:29:15 UT (t = 41 minutes) on 2020 July 30. The yellow dashed rectangle represents the FOV of the FISS. Middle: FISS Hα–4 Å raster image. Right: Hα line center image. The blue and red contours represent LOS magnetic field strengths of −200 and 200 G, respectively.
Paper: Spectroscopic Detection of Alfvénic Waves in the Chromospheric Fibrils of a Solar-quiet Region
Authors: Hannah Kwak, Jongchul Chae, Eun-Kyung Lim, Kyoung-Sun Lee, Donguk Song, Heesu Yang
Figure caption: The top panels display the Hα intensity and LOS velocity maps acquired from the MLSI. The following panels show the velocity maps filtered by different period bands, i.e., 3, 5, 10, and longer than 30 minutes periods. During the 20 minute time interval, 131 wave packets were detected. The arrows indicate detected wave packets, with their centers positioned at the midpoint between two selected points used for cross-correlation analysis. The direction of the arrows indicates the wave propagation direction. The length of the arrows represents the propagation speed, which is proportional to c 1/3. The propagation speeds range from 21 to 405 km s−1. The colors of the arrows indicate the wave packets belonging to different period bands. The light green arrows represent 3 minute waves, medium green arrows represent 5 minute waves, and dark green arrows represent 10 minute waves.
Paper: Spectroscopic Detection of Alfvénic Waves in the Chromospheric Fibrils of a Solar-quiet Region
Authors: Hannah Kwak, Jongchul Chae, Eun-Kyung Lim, Kyoung-Sun Lee, Donguk Song, Heesu Yang
Figure caption: Stacked histograms of period P (top), propagation speed c (middle), and velocity amplitude V (bottom). For period, the values are divided into outward waves and inward waves. For propagation speed and velocity amplitude, the values are grouped into three bands based on their periods: 3, 5, and 10 minute bands.
Paper: Identifying Physical Structures in Our Galaxy with Gaussian Mixture Models: An Unsupervised Machine Learning Technique
Authors: M. Tiwari, R. Kievit, S. Kabanovic, L. Bonne, F. Falasca, C. Guevara, R. Higgins, M. Justen, R. Karim, Ü. Kavak, C. Pabst, M. W. Pound, N. Schneider, R. Simon, J. Stutzki, M. Wolfire, A. G. G. M. Tielens
Figure caption: Using the GMM described in Kabanovic et al. (2022), BIC vs. n input plot (left panel) and domain map (right panel) for NGC 1977, RCW 120, and RCW 49.
Paper: Identifying Physical Structures in Our Galaxy with Gaussian Mixture Models: An Unsupervised Machine Learning Technique
Authors: M. Tiwari, R. Kievit, S. Kabanovic, L. Bonne, F. Falasca, C. Guevara, R. Higgins, M. Justen, R. Karim, Ü. Kavak, C. Pabst, M. W. Pound, N. Schneider, R. Simon, J. Stutzki, M. Wolfire, A. G. G. M. Tielens
Figure caption: Velocity channel maps of [C II] emission toward RCW 49. The beam size is shown in the lower right.
Paper: Identifying Physical Structures in Our Galaxy with Gaussian Mixture Models: An Unsupervised Machine Learning Technique
Authors: M. Tiwari, R. Kievit, S. Kabanovic, L. Bonne, F. Falasca, C. Guevara, R. Higgins, M. Justen, R. Karim, Ü. Kavak, C. Pabst, M. W. Pound, N. Schneider, R. Simon, J. Stutzki, M. Wolfire, A. G. G. M. Tielens
Figure caption: Velocity channel maps of [C II] emission toward RCW 120. The beam size is shown in the lower right.
Paper: Identifying Physical Structures in Our Galaxy with Gaussian Mixture Models: An Unsupervised Machine Learning Technique
Authors: M. Tiwari, R. Kievit, S. Kabanovic, L. Bonne, F. Falasca, C. Guevara, R. Higgins, M. Justen, R. Karim, Ü. Kavak, C. Pabst, M. W. Pound, N. Schneider, R. Simon, J. Stutzki, M. Wolfire, A. G. G. M. Tielens
Figure caption: Normalized average spectra of all GMM-identified clusters for NGC 1977 (left column), RCW 120 (middle column), and RCW 49 (right column). The dashed region represents the standard deviation, depicting the variation in spectral profiles for all spectra per pixel corresponding to a cluster.
Paper: Identifying Physical Structures in Our Galaxy with Gaussian Mixture Models: An Unsupervised Machine Learning Technique
Authors: M. Tiwari, R. Kievit, S. Kabanovic, L. Bonne, F. Falasca, C. Guevara, R. Higgins, M. Justen, R. Karim, Ü. Kavak, C. Pabst, M. W. Pound, N. Schneider, R. Simon, J. Stutzki, M. Wolfire, A. G. G. M. Tielens
Figure caption: Average spectra of all GMM-identified clusters for NGC 1977 (left column), RCW 120 (middle column), and RCW 49 (right column). The dashed region represents the standard deviation, depicting the variation in spectral profiles for all spectra per pixel corresponding to a cluster.
Paper: Identifying Physical Structures in Our Galaxy with Gaussian Mixture Models: An Unsupervised Machine Learning Technique
Authors: M. Tiwari, R. Kievit, S. Kabanovic, L. Bonne, F. Falasca, C. Guevara, R. Higgins, M. Justen, R. Karim, Ü. Kavak, C. Pabst, M. W. Pound, N. Schneider, R. Simon, J. Stutzki, M. Wolfire, A. G. G. M. Tielens
Figure caption: Velocity channel maps of [C II] emission toward NGC 1977. The beam size is shown in the lower right.
Paper: Identifying Physical Structures in Our Galaxy with Gaussian Mixture Models: An Unsupervised Machine Learning Technique
Authors: M. Tiwari, R. Kievit, S. Kabanovic, L. Bonne, F. Falasca, C. Guevara, R. Higgins, M. Justen, R. Karim, Ü. Kavak, C. Pabst, M. W. Pound, N. Schneider, R. Simon, J. Stutzki, M. Wolfire, A. G. G. M. Tielens
Figure caption: Domain map of NGC 1977 from an identical model to the one presented in Figure 3, however instead of assigning each pixel to the cluster to which it has the largest probability of belonging, we only plot points with a probability between 0.1 and 0.9. The color opacity of each pixel is proportional to this probability.
Paper: Identifying Physical Structures in Our Galaxy with Gaussian Mixture Models: An Unsupervised Machine Learning Technique
Authors: M. Tiwari, R. Kievit, S. Kabanovic, L. Bonne, F. Falasca, C. Guevara, R. Higgins, M. Justen, R. Karim, Ü. Kavak, C. Pabst, M. W. Pound, N. Schneider, R. Simon, J. Stutzki, M. Wolfire, A. G. G. M. Tielens
Figure caption: Domain map of RCW 120 displaying the identified clusters with the mean normalization technique. The other hyperparameters were same as those given in Table 1.
Paper: Mass Ratio Distribution of Hierarchical Triple Systems from the LAMOST-MRS Survey
Authors: Tongyu He, Jiangdan Li, Xuefei Chen, Rong-jia Yang, Lin Xiao, Zhanwen Han
Figure caption: Illustration of a triple system’s CCF. In the bottom panel, we display the spectrum of a normalized triple-star system (S/N = 20). The effective temperatures of the three components are T eff1 = 6400, T eff2 = 6000, and T eff3 = 5600 K. In the bottom panel, we present the generated CCF: A 1 = 0.53, V 1 = −131; A 2 = 0.48, V 2 = 134; and A 3 = 0.41, V 3 = 19 km s−1. The mass ratios are q in = 0.96 and q out  = 0.441.
Paper: Mass Ratio Distribution of Hierarchical Triple Systems from the LAMOST-MRS Survey
Authors: Tongyu He, Jiangdan Li, Xuefei Chen, Rong-jia Yang, Lin Xiao, Zhanwen Han
Figure caption: Cumulative q in and q out distribution of triple systems of different spectral types. The q in distributions are shown in panels (a) and (b), and the bias-corrected q in distributions and fits are shown in panel (b). The q out distributions are shown in panels (c) and (d), and the bias-corrected q out distributions and fits are shown in panel (d).
Paper: Mass Ratio Distribution of Hierarchical Triple Systems from the LAMOST-MRS Survey
Authors: Tongyu He, Jiangdan Li, Xuefei Chen, Rong-jia Yang, Lin Xiao, Zhanwen Han
Figure caption: Relationship between A 2/A 1 and q in, as well as the relationship between A 3/(A 1 + A 2) and q out. The blue dashed line indicates the result at 6400 K, the red solid line indicates the relationship at 5600 K, and the black dashed line indicates the result at 8000 K.
Paper: Mass Ratio Distribution of Hierarchical Triple Systems from the LAMOST-MRS Survey
Authors: Tongyu He, Jiangdan Li, Xuefei Chen, Rong-jia Yang, Lin Xiao, Zhanwen Han
Figure caption: Detection efficiency vs. mass ratio, q out and q in, of STs. The color scale on the right side represents the detection efficiency.
Paper: Mass Ratio Distribution of Hierarchical Triple Systems from the LAMOST-MRS Survey
Authors: Tongyu He, Jiangdan Li, Xuefei Chen, Rong-jia Yang, Lin Xiao, Zhanwen Han
Figure caption: Color–magnitude graph of 67 ST candidates (black dots) determined from LAMOST DR7 data (blue dots). The x-axis shows the color difference between G BP and G RP, and the y-axis displays the absolute value of M  G . All photometric data are from Gaia DR3, and our samples were chosen between the two lines according to their position on the diagram.
Paper: Mass Ratio Distribution of Hierarchical Triple Systems from the LAMOST-MRS Survey
Authors: Tongyu He, Jiangdan Li, Xuefei Chen, Rong-jia Yang, Lin Xiao, Zhanwen Han
Figure caption: The distribution of inner binaries (red squares, black circles, and blue triangles) in triple systems of types A, F, and G are shown in panels (a) and (b); the bias-corrected q in distributions and fits are shown in panel (b). Panels (c) and (d) show the distribution of outer binaries in triple systems in our sample; panel (d) shows the bias-corrected q out distributions and fits. In order to clearly show the error bars, we have shifted the mass ratio distribution of A-type stars to the left by 0.1 and that of G-type stars to the right by 0.1.
Paper: Mass Ratio Distribution of Hierarchical Triple Systems from the LAMOST-MRS Survey
Authors: Tongyu He, Jiangdan Li, Xuefei Chen, Rong-jia Yang, Lin Xiao, Zhanwen Han
Figure caption: Distribution of the number of ΔVs between any two components in the ST spectra.
Paper: Mass Ratio Distribution of Hierarchical Triple Systems from the LAMOST-MRS Survey
Authors: Tongyu He, Jiangdan Li, Xuefei Chen, Rong-jia Yang, Lin Xiao, Zhanwen Han
Figure caption: The CCFs and derivatives of one ST candidate (S/N = 20). All selected ranges of CCFs and smoothed derivatives are shown as black solid lines, while the original CCFs and derivatives are shown as gray dashed lines. Each candidate’s thresholds are shown as red horizontal lines, and their RVs are shown as black vertical lines.
Paper: Lyman Continuum Emission from Spectroscopically Confirmed Lyα Emitters at z ∼ 3.1
Authors: Yuchen Liu, Linhua Jiang, Rogier A. Windhorst, Yucheng Guo, Zhen-Ya Zheng
Figure caption: LAEs used in this work. The upper panel shows the V-band magnitudes and redshifts of the LAEs. The symbols indicate all LAEs in SXDS. The dashed line is our selection criterion of V = 26.2 mag. Galaxies brighter than V = 26.2 mag (in blue) are used in this work. The red crosses represent the galaxies that are rejected due to the contamination from their neighbors in the U J band. The lower panel shows the detection limits of f esc for the individual LyC galaxies and stacked galaxies assuming an average IGM absorption and an average dust attenuation (see details in Section 3).
Paper: Lyman Continuum Emission from Spectroscopically Confirmed Lyα Emitters at z ∼ 3.1
Authors: Yuchen Liu, Linhua Jiang, Rogier A. Windhorst, Yucheng Guo, Zhen-Ya Zheng
Figure caption: Filter transmission curves and a typical spectrum for type A stars. The red curve shows the transmission curve of the U J filter, which is compared with the SDSS u filter in blue. The Subaru V filter is used to estimate the nonionizing flux. The transmission curves have included the CCD response curves. The dashed line represents a typical A5 star spectrum. The vertical lines indicate the Lyman limit and Lyα emission at z = 3.1, respectively.
Paper: Lyman Continuum Emission from Spectroscopically Confirmed Lyα Emitters at z ∼ 3.1
Authors: Yuchen Liu, Linhua Jiang, Rogier A. Windhorst, Yucheng Guo, Zhen-Ya Zheng
Figure caption: The combined U J-band image in the SXDS field. The dots represent spectroscopically confirmed LAEs at z ≈ 3.1. The color bar indicates redshifts.
Paper: Lyman Continuum Emission from Spectroscopically Confirmed Lyα Emitters at z ∼ 3.1
Authors: Yuchen Liu, Linhua Jiang, Rogier A. Windhorst, Yucheng Guo, Zhen-Ya Zheng
Figure caption: The SDSS color–color diagram of bright point sources in the SXDS field. The red rectangle is the selection area for type A stars. The color bar indicates the U J magnitude.
Paper: NICER Observations of Thermonuclear Bursts from 4U 1728-34: Detection of Oscillations prior to the Onset of Two Bursts
Authors: Z. Funda Bostancı, Tuğba Boztepe, Tolga Güver, Tod E. Strohmayer, Yuri Cavecchi, Ersin Göğüş, Diego Altamirano, Peter Bult, Deepto Chakrabarty, Sebastien Guillot, Gaurava K. Jaisawal, Christian Malacaria, Giulio C. Mancuso, Andrea Sanna, Jean H. Swank
Figure caption: Time evolution of spectral parameters for bursts 1–4, 6, and 7. Red symbols show the results of the f  a  method when applicable and black symbols show the results for constant background emission. In each panel, we show, from top to bottom, bolometric flux (in units of 10−9 erg s−1 cm−2), temperature (keV), blackbody normalization (﹩{R}_{\mathrm{km}}^{2}/{D}_{10\,\mathrm{kpc}}^{2}﹩), f  a , and finally the fit statistic.
Paper: NICER Observations of Thermonuclear Bursts from 4U 1728-34: Detection of Oscillations prior to the Onset of Two Bursts
Authors: Z. Funda Bostancı, Tuğba Boztepe, Tolga Güver, Tod E. Strohmayer, Yuri Cavecchi, Ersin Göğüş, Diego Altamirano, Peter Bult, Deepto Chakrabarty, Sebastien Guillot, Gaurava K. Jaisawal, Christian Malacaria, Giulio C. Mancuso, Andrea Sanna, Jean H. Swank
Figure caption: Histogram of the χ 2 values with or without the application of the f  a  parameter. Only in a very small fraction of the cases is the use of f  a  statistically required.
Paper: NICER Observations of Thermonuclear Bursts from 4U 1728-34: Detection of Oscillations prior to the Onset of Two Bursts
Authors: Z. Funda Bostancı, Tuğba Boztepe, Tolga Güver, Tod E. Strohmayer, Yuri Cavecchi, Ersin Göğüş, Diego Altamirano, Peter Bult, Deepto Chakrabarty, Sebastien Guillot, Gaurava K. Jaisawal, Christian Malacaria, Giulio C. Mancuso, Andrea Sanna, Jean H. Swank
Figure caption: Same as Figure 2 for bursts 8–11.
Paper: NICER Observations of Thermonuclear Bursts from 4U 1728-34: Detection of Oscillations prior to the Onset of Two Bursts
Authors: Z. Funda Bostancı, Tuğba Boztepe, Tolga Güver, Tod E. Strohmayer, Yuri Cavecchi, Ersin Göğüş, Diego Altamirano, Peter Bult, Deepto Chakrabarty, Sebastien Guillot, Gaurava K. Jaisawal, Christian Malacaria, Giulio C. Mancuso, Andrea Sanna, Jean H. Swank
Figure caption: Hardness–intensity diagram showing all NICER observations of 4U 1728−34 from 2017 to 2019. Observations in which an X-ray burst was detected are indicated by red filled circles.