adsabs/AstroCLIMB huggingface dataset:
Paper: Sunyaev–Zeldovich Signals from L* Galaxies: Observations, Analytics, and Simulations
Authors: Yossi Oren, Amiel Sternberg, Christopher F. McKee, Yakov Faerman, Shy Genel
Figure caption: Stellar mass, M *, vs. virial mass, M vir (the SMHM relation). The gray dots are the TNG100 results for all halos at redshift z = 0. The gray curve shows the TNG100 medians and standard deviations. The blue curve is the observationally based B. P. Moster et al. (2010) SMHM relation. The red dotted curve shows the relation used by P+13. The yellow dot is for the MW.
Paper: Sunyaev–Zeldovich Signals from L* Galaxies: Observations, Analytics, and Simulations
Authors: Yossi Oren, Amiel Sternberg, Christopher F. McKee, Yakov Faerman, Shy Genel
Figure caption:                       B+22 stack data and error bars (blue), normalized by a stack mass of M vir,12 = 2.75, in comparison to the three models, FSM20 (yellow), FSM20-maximal (purple), and FSM17 (turquoise). The FSM17 model includes the O VI component (see text). The FSM models are unaffected by the renormalization since for these M vir,12 = 1. The green dashed curves show our best-fitting PLM for the B+22 data.
Paper: Sunyaev–Zeldovich Signals from L* Galaxies: Observations, Analytics, and Simulations
Authors: Yossi Oren, Amiel Sternberg, Christopher F. McKee, Yakov Faerman, Shy Genel
Figure caption: The dimensionless integrals, ﹩{I}_{y,{a}_{P,\mathrm{th}}}(b)﹩ (left panel), ﹩{I}_{Y,{a}_{P,\mathrm{th}}}(b)﹩ (middle panel), and the ratio ﹩Y/{Y}_{\perp }\equiv 1/{I}_{Y,{a}_{P,\mathrm{th}}}(b)﹩ (right panel). These integrals are defined by Equations (16) and (23) respectively. Curves are shown for the pressure power-law index a  P,th ranging from 0 to 2.5. In the right panel, the gray lines indicate the values of ﹩1/{I}_{Y,{a}_{P,\mathrm{th}}}﹩ at impact parameter b = 0.5. In the left panel, the three points are the values of ﹩{I}_{y,{a}_{P,\mathrm{th}}}﹩ for b → 0, as given by Equation (A5) in Appendix A.
Paper: Sunyaev–Zeldovich Signals from L* Galaxies: Observations, Analytics, and Simulations
Authors: Yossi Oren, Amiel Sternberg, Christopher F. McKee, Yakov Faerman, Shy Genel
Figure caption: TNG100 results (black curve) for b 500 ≡ R 500/R vir vs. M vir for redshift z = 0 halos. Error bars are 1σ. The dashed blue curve is for NFW halos with (median) cosmological concentration parameters (see text).
Paper: Narrow [O III] Emission Lines as a Potential Proxy for the Evolutionary Stage of Quasars
Authors: Zhi-fu Chen, Zhe-Geng Chen, Xing-long Peng, Wei-rong Huang
Figure caption: (a) The equivalent width of the core component of the [O III] λ5007 evolved with radio spectral shape. The large ﹩{\alpha }_{3000}^{144}﹩ indicates the quasar living in the early evolutionary stage, and the small ﹩{\alpha }_{3000}^{144}﹩ indicates the evolved quasar. The Spearman’s correlation coefficient is r = −0.489. Red squares show the median values in distinct ﹩{\alpha }_{3000}^{144}﹩ bins with the error bars representing standard deviations. The red solid line is the best linear fitting to the red squares: ﹩{\rm{Log}}\,{W}_{\mathrm{core}}^{[{\rm{O}}\,{\rm\small{III}}]\lambda 5007}\propto (-0.244\pm 0.102)\times {\rm{Log}}\,{\alpha }_{3000}^{144}﹩. (b) The relationship between continuum luminosity at 5100 Å and ﹩{\alpha }_{3000}^{144}﹩. The Spearman’s correlation coefficient is r = 0.060. (c) The relationship between [O III] λ5007 luminosity of the core component and ﹩{\alpha }_{3000}^{144}﹩. The Spearman’s correlation coefficient is r = −0.309.
Paper: Sunyaev–Zeldovich Signals from L* Galaxies: Observations, Analytics, and Simulations
Authors: Yossi Oren, Amiel Sternberg, Christopher F. McKee, Yakov Faerman, Shy Genel
Figure caption: Top panel: Pressure profiles used by D+23 (blue), J. C. Hill et al. (2018; orange), and our PLM with a  P,th = 2.03 (green). Each pressure curve is normalized such that it provides a best-fitting Compton y(b) curve for the B+22 data. Lower panel: B+22 Compton-y data (blue points), and best-fitting y profiles, as functions of impact parameter b = r ⊥/R vir, computed using the pressure curves in the upper panel. The red curve is the B+22 truncated-β-model.
Paper: Narrow [O III] Emission Lines as a Potential Proxy for the Evolutionary Stage of Quasars
Authors: Zhi-fu Chen, Zhe-Geng Chen, Xing-long Peng, Wei-rong Huang
Figure caption: The distribution of ﹩{\alpha }_{3000}^{144}﹩. The black thin line is for the quasars with detected [O III] emission lines, and the red thick line is for the quasars without detected [O III] emission lines. The Kolmogorov–Smirnov test yields a probability P < 10−6.
Paper: Narrow [O III] Emission Lines as a Potential Proxy for the Evolutionary Stage of Quasars
Authors: Zhi-fu Chen, Zhe-Geng Chen, Xing-long Peng, Wei-rong Huang
Figure caption: (a) The redshift distribution of quasars in our final sample. (b) The relationship between ﹩{\alpha }_{3000}^{144}﹩ and redshifts. The Spearman’s correlation coefficient is r = −0.008.
Paper: Variations in the Inferred Cosmic-Ray Spectral Index as Measured by Neutron Monitors in Antarctica
Authors: Pradiphat Muangha, David Ruffolo, Alejandro Sáiz, Chanoknan Banglieng, Paul Evenson, Surujhdeo Seunarine, Suyeon Oh, Jongil Jung, Marc L. Duldig, John E. Humble
Figure caption: Wavelet power as a function of period and time from 2015 March to 2023 September for daily values of (a) SP C as a measure of the cosmic-ray flux at ∼10 GV, (b) SP L as a measure of the cosmic-ray spectral index at ∼10 GV, and solar wind parameters: (c) speed, (d) magnetic field magnitude B, and (e) B  x  − B  y  as a measure of the magnetic sector structure. The horizontal black dashed lines in each panel represent the periods of 27 and 13.5 days. The white dashed line near the edge corresponds to the 95% confidence level of the wavelet analysis. The color bar indicates the power of a period range from low to high power (blue to red). B  x  − B  y  is the solar wind parameter that best matches the SP C and L wavelet power, with dominant periodicity at the ≈27 day solar rotation period, only during times near solar maximum, and little power at the 13.5 day harmonic. We conclude that the magnetic sector structure is the key determinant of the 27 day variation in the GCR spectrum at ∼10 GV. The solar wind speed also makes a nearly rigidity-independent contribution to the variation in C, or the cosmic-ray flux, as evidenced by an occasional 13.5 day periodicity in those quantities but not in L.
Paper: Variations in the Inferred Cosmic-Ray Spectral Index as Measured by Neutron Monitors in Antarctica
Authors: Pradiphat Muangha, David Ruffolo, Alejandro Sáiz, Chanoknan Banglieng, Paul Evenson, Surujhdeo Seunarine, Suyeon Oh, Jongil Jung, Marc L. Duldig, John E. Humble
Figure caption: Left: cross-wavelet spectrum between SP C and solar wind parameters from 2015 March to 2023 September: (a) solar wind speed; (c) B; and (e) B  x  − B  y . Right: cross-wavelet spectrum between SP L and solar wind parameters: (b) solar wind speed; (d) B; and (f) B  x  − B  y . The horizontal white dashed lines in each panel represent the periods of 27 and 13.5 days. Where the magnitude exceeds 20% of the maximum magnitude, the phase difference between the two quantities is indicated by the direction of an arrow, with zero phase difference indicated by an arrow to the right.
Paper: Variations in the Inferred Cosmic-Ray Spectral Index as Measured by Neutron Monitors in Antarctica
Authors: Pradiphat Muangha, David Ruffolo, Alejandro Sáiz, Chanoknan Banglieng, Paul Evenson, Surujhdeo Seunarine, Suyeon Oh, Jongil Jung, Marc L. Duldig, John E. Humble
Figure caption: Daily raw leader fraction L of the SP NM during a time period with software changes, 2018 March through 2019 October. The daily L values were extracted from (a) computer 1 (PC1) and (b) computer 2 (PC2). L values from each of three counter tubes are indicated by the colored lines. (c) SP pressure in hPa. The vertical lines indicate the times when the data acquisition software was changed.
Paper: Variations in the Inferred Cosmic-Ray Spectral Index as Measured by Neutron Monitors in Antarctica
Authors: Pradiphat Muangha, David Ruffolo, Alejandro Sáiz, Chanoknan Banglieng, Paul Evenson, Surujhdeo Seunarine, Suyeon Oh, Jongil Jung, Marc L. Duldig, John E. Humble
Figure caption: (a) Daily raw leader fraction L of JB NM during a time period with changes in software and physical configuration, 2018 November through 2021 April, indicated by a colored trace for each counter tube. (b) JB atmospheric pressure in hPa. The vertical lines indicate the times of the software or configuration changes.
Paper: Variations in the Inferred Cosmic-Ray Spectral Index as Measured by Neutron Monitors in Antarctica
Authors: Pradiphat Muangha, David Ruffolo, Alejandro Sáiz, Chanoknan Banglieng, Paul Evenson, Surujhdeo Seunarine, Suyeon Oh, Jongil Jung, Marc L. Duldig, John E. Humble
Figure caption: (a) Daily raw leader fraction L of MA NM during a time period with changes in software, 2020 October through 2022 December, indicated by a colored trace for each counter tube. (b) MA atmospheric pressure in hPa. The vertical lines indicate the times of the software changes.
Paper: Precise Measurements of TeV Halos around Geminga and Monogem Pulsars with HAWC
Authors: A. Albert, R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, A. Bernal, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, U. Cotti, J. Cotzomi, S. Coutiño de León, E. de la Fuente, D. Depaoli, N. Di Lalla, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, M. Durocher, J. C. Díaz-Vélez, K. Engel, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, J. A. García-González, F. Garfias, H. Goksu, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, S. Hernández-Cadena, I. Herzog, P. Hüntemeyer, D. Huang, F. Hueyotl-Zahuantitla, A. Iriarte, V. Joshi, S. Kaufmann, D. Kieda, A. Lara, W. H. Lee, J. Lee, H. León Vargas, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Montes, J. A. Morales-Soto, E. Moreno, M. Mostafá, A. Nayerhoda, L. Nellen, R. Noriega-Papaqui, L. Olivera-Nieto, N. Omodei, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, H. Salazar, D. Salazar-Gallegos, A. Sandoval, M. Schneider, G. Schwefer, J. Serna-Franco, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Urea-Mena, E. Varela, L. Villaseñor, X. Wang, I. J. Watson, E. Willox, H. Wu, S. Yun-Cárcamo, H. Zhou, C. de León, M. Di Mauro
Figure caption: Spectral fit of Geminga (left) and Monogem (right). The darker bands show the statistical uncertainties, while the lighter band shows the systematic uncertainties. The fits for power-law and log parabola are shown for the same diffusion coefficient obtained from best-fit results. For energies where source is not significantly detected, we show a 90% confidence level upper limit.
Paper: Precise Measurements of TeV Halos around Geminga and Monogem Pulsars with HAWC
Authors: A. Albert, R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, A. Bernal, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, U. Cotti, J. Cotzomi, S. Coutiño de León, E. de la Fuente, D. Depaoli, N. Di Lalla, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, M. Durocher, J. C. Díaz-Vélez, K. Engel, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, J. A. García-González, F. Garfias, H. Goksu, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, S. Hernández-Cadena, I. Herzog, P. Hüntemeyer, D. Huang, F. Hueyotl-Zahuantitla, A. Iriarte, V. Joshi, S. Kaufmann, D. Kieda, A. Lara, W. H. Lee, J. Lee, H. León Vargas, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Montes, J. A. Morales-Soto, E. Moreno, M. Mostafá, A. Nayerhoda, L. Nellen, R. Noriega-Papaqui, L. Olivera-Nieto, N. Omodei, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, H. Salazar, D. Salazar-Gallegos, A. Sandoval, M. Schneider, G. Schwefer, J. Serna-Franco, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Urea-Mena, E. Varela, L. Villaseñor, X. Wang, I. J. Watson, E. Willox, H. Wu, S. Yun-Cárcamo, H. Zhou, C. de León, M. Di Mauro
Figure caption: Surface brightness profiles of multi-TeV γ-ray emission in units of TeV cm−2 s−1 deg−2 as a function of distance for Geminga (left panel) and Monogem (right panel) for energy range of 5.4 to 68 TeV. The green color band shows the individual emission and the blue band shows the excess emission from its neighboring source.
Paper: Precise Measurements of TeV Halos around Geminga and Monogem Pulsars with HAWC
Authors: A. Albert, R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, A. Bernal, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, U. Cotti, J. Cotzomi, S. Coutiño de León, E. de la Fuente, D. Depaoli, N. Di Lalla, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, M. Durocher, J. C. Díaz-Vélez, K. Engel, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, J. A. García-González, F. Garfias, H. Goksu, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, S. Hernández-Cadena, I. Herzog, P. Hüntemeyer, D. Huang, F. Hueyotl-Zahuantitla, A. Iriarte, V. Joshi, S. Kaufmann, D. Kieda, A. Lara, W. H. Lee, J. Lee, H. León Vargas, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Montes, J. A. Morales-Soto, E. Moreno, M. Mostafá, A. Nayerhoda, L. Nellen, R. Noriega-Papaqui, L. Olivera-Nieto, N. Omodei, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, H. Salazar, D. Salazar-Gallegos, A. Sandoval, M. Schneider, G. Schwefer, J. Serna-Franco, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Urea-Mena, E. Varela, L. Villaseñor, X. Wang, I. J. Watson, E. Willox, H. Wu, S. Yun-Cárcamo, H. Zhou, C. de León, M. Di Mauro
Figure caption: Left: HAWC significance map region, for reconstructed energies between 1 TeV and 316 TeV. Right: Model map assuming best-fit parameters in analysis. The map is in equatorial coordinates. The significance is calculated by assuming a 1° disk for each pixel with a power-law spectral shape of α  γ  = −2.25. The contours show the 5σ, 7σ, and 10σ levels. Source outside the ROI is the supernova remnant IC 443. The white circle illustrates the ROI in both figures.
Paper: Precise Measurements of TeV Halos around Geminga and Monogem Pulsars with HAWC
Authors: A. Albert, R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, A. Bernal, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, U. Cotti, J. Cotzomi, S. Coutiño de León, E. de la Fuente, D. Depaoli, N. Di Lalla, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, M. Durocher, J. C. Díaz-Vélez, K. Engel, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, J. A. García-González, F. Garfias, H. Goksu, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, S. Hernández-Cadena, I. Herzog, P. Hüntemeyer, D. Huang, F. Hueyotl-Zahuantitla, A. Iriarte, V. Joshi, S. Kaufmann, D. Kieda, A. Lara, W. H. Lee, J. Lee, H. León Vargas, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Montes, J. A. Morales-Soto, E. Moreno, M. Mostafá, A. Nayerhoda, L. Nellen, R. Noriega-Papaqui, L. Olivera-Nieto, N. Omodei, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, H. Salazar, D. Salazar-Gallegos, A. Sandoval, M. Schneider, G. Schwefer, J. Serna-Franco, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Urea-Mena, E. Varela, L. Villaseñor, X. Wang, I. J. Watson, E. Willox, H. Wu, S. Yun-Cárcamo, H. Zhou, C. de León, M. Di Mauro
Figure caption: Example of intensity maps of the Geminga ICS γ-ray emission at energies of 10 TeV (left), 25 TeV (middle), and 63 TeV (right). The diffusion coefficient assumed is D 0 = 1.3 × 1026 cm2 s−1 and α  e  = 1.8 for a region of 15° × 15° around the pulsar.
Paper: Precise Measurements of TeV Halos around Geminga and Monogem Pulsars with HAWC
Authors: A. Albert, R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, A. Bernal, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, U. Cotti, J. Cotzomi, S. Coutiño de León, E. de la Fuente, D. Depaoli, N. Di Lalla, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, M. Durocher, J. C. Díaz-Vélez, K. Engel, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, J. A. García-González, F. Garfias, H. Goksu, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, S. Hernández-Cadena, I. Herzog, P. Hüntemeyer, D. Huang, F. Hueyotl-Zahuantitla, A. Iriarte, V. Joshi, S. Kaufmann, D. Kieda, A. Lara, W. H. Lee, J. Lee, H. León Vargas, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Montes, J. A. Morales-Soto, E. Moreno, M. Mostafá, A. Nayerhoda, L. Nellen, R. Noriega-Papaqui, L. Olivera-Nieto, N. Omodei, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, H. Salazar, D. Salazar-Gallegos, A. Sandoval, M. Schneider, G. Schwefer, J. Serna-Franco, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Urea-Mena, E. Varela, L. Villaseñor, X. Wang, I. J. Watson, E. Willox, H. Wu, S. Yun-Cárcamo, H. Zhou, C. de León, M. Di Mauro
Figure caption: Left panel: significance map after subtraction of the best-fit model from HAWC data. The significance map is calculated assuming a point-source morphology to prevent any pixel correlation, which occurs for an extended source assumption. The white circle represents the ROI shown in Figure 2. Right panel: significance histogram of residuals within the ROI.
Paper: Precise Measurements of TeV Halos around Geminga and Monogem Pulsars with HAWC
Authors: A. Albert, R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, A. Bernal, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, U. Cotti, J. Cotzomi, S. Coutiño de León, E. de la Fuente, D. Depaoli, N. Di Lalla, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, M. Durocher, J. C. Díaz-Vélez, K. Engel, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, J. A. García-González, F. Garfias, H. Goksu, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, S. Hernández-Cadena, I. Herzog, P. Hüntemeyer, D. Huang, F. Hueyotl-Zahuantitla, A. Iriarte, V. Joshi, S. Kaufmann, D. Kieda, A. Lara, W. H. Lee, J. Lee, H. León Vargas, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Montes, J. A. Morales-Soto, E. Moreno, M. Mostafá, A. Nayerhoda, L. Nellen, R. Noriega-Papaqui, L. Olivera-Nieto, N. Omodei, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, H. Salazar, D. Salazar-Gallegos, A. Sandoval, M. Schneider, G. Schwefer, J. Serna-Franco, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Urea-Mena, E. Varela, L. Villaseñor, X. Wang, I. J. Watson, E. Willox, H. Wu, S. Yun-Cárcamo, H. Zhou, C. de León, M. Di Mauro
Figure caption: Significance maps of data (top) and model (bottom) for the Geminga region for three energy bands: 1–17 TeV (left), 17–31 TeV (center), and 31–316 TeV (right). The maps are generated with a spatial shape model of 1.°5 disk and the best-fit spectra from Table 1.
Paper: Superluminal Proper Motion in the X-Ray Jet of Centaurus A
Authors: David Bogensberger, Jon M Miller, Richard Mushotzky, W. N. Brandt, Elias Kammoun, Abderahmen Zoghbi, Ehud Behar
Figure caption: Adaptively smoothed, logarithmically scaled, background-subtracted false-color image of the combined Chandra observations of Cen A used in this work. The red, green, and blue colors represent the three energy bands: 0.3–1.0 keV, 1.0–3.0 keV, and 3.0–10.0 keV, respectively. The individual images were aligned according to the method described in Section 4. Two blue lines are the first-order HETGS grating arms from one of the observations. In this and the following images, the brightness is scaled by the number of counts per pixel in the merged image. The field of view of this image is 2.′87 × 2.′46, which corresponds to 3.17 kpc × 2.72 kpc at 3.8 Mpc. The nucleus is located at R.A. = 13h25m27.ˢ6, decl. = −43°01′0.″88.
Paper: Superluminal Proper Motion in the X-Ray Jet of Centaurus A
Authors: David Bogensberger, Jon M Miller, Richard Mushotzky, W. N. Brandt, Elias Kammoun, Abderahmen Zoghbi, Ehud Behar
Figure caption: Gaussian-smoothed, background-subtracted images of groups of observations, and the difference image of C1, C2, and the jet region between them and the jet knots AX1A and AX1C. The colors were chosen relative to the background brightness. The difference image is calculated between the first and last groups, scaled by the number of background-subtracted source counts in these two images. Blue regions indicate parts of the image that were brighter in the first group, and red regions are parts that were brighter in the fourth group. All images depict the energy band 0.8−3.0 keV and have a field of view of 6.″0 × 6.″0, which corresponds to 110 pc × 110 pc. A color bar is provided for the total and difference images. The color bars for the other panels are adjusted by the number of background-subtracted counts in this region. C1 has coordinates of R.A. = 13h25m28.ˢ0, decl. = −43°01′05.″7. C2 has coordinates of R.A. = 13h25m28.ˢ1, decl. = −43°01′06.″7.
Paper: Superluminal Proper Motion in the X-Ray Jet of Centaurus A
Authors: David Bogensberger, Jon M Miller, Richard Mushotzky, W. N. Brandt, Elias Kammoun, Abderahmen Zoghbi, Ehud Behar
Figure caption: The X-ray jet, with labeled jet knots. The image is of the 0.8−3.0 keV energy band and has been adaptively smoothed, logarithmically scaled, and background subtracted. It is the merged image from all Chandra observations of Cen A used in this work. The labels of the individual jet knots are adapted from those used by M. J. Hardcastle et al. (2007) and B. Snios et al. (2019b), but with slight modifications. The two potential new candidate jet knots have been labeled as C1 and C2. X1 refers to a possible XRB located at a distance from the nucleus similar to that of C1 and C2, and it is compared with them in Section 5. The depicted region is identical to that of Figure 2.
Paper: Superluminal Proper Motion in the X-Ray Jet of Centaurus A
Authors: David Bogensberger, Jon M Miller, Richard Mushotzky, W. N. Brandt, Elias Kammoun, Abderahmen Zoghbi, Ehud Behar
Figure caption: Images of the jet in the four groups of observations. On the left are adaptively smoothed, logarithmically scaled, background-subtracted images of the jet in the 0.8−3.0 keV energy band. On the right are the difference images of each group, compared to the total image. The two images being compared were scaled by the number of background-subtracted counts in the jet. Red depicts regions that are brighter in that group of observations than in the rest of the observations. Blue shows regions that are fainter in that group. The pileup at the nucleus generates weird structures, including an apparent hole, but these are not real. The field of view of this figure is 1.′79 × 1.′41, corresponding to 1.98 kpc × 1.56 kpc. A color bar is included for the fourth group. The color bars for the other panels are similar but with a range adjusted by the number of background-subtracted counts in the jet.
Paper: Superluminal Proper Motion in the X-Ray Jet of Centaurus A
Authors: David Bogensberger, Jon M Miller, Richard Mushotzky, W. N. Brandt, Elias Kammoun, Abderahmen Zoghbi, Ehud Behar
Figure caption: The 35 selected aligning point sources, as well as the regions around them, that are used in the optimal alignment of the 34 images. This figure depicts the same region as in Figure 1, for the 0.2−10 keV energy band.