adsabs/AstroCLIMB huggingface dataset:
Paper: Optical and Radio Analysis of Systematically Classified Broad-lined Type Ic Supernovae from the Zwicky Transient Facility
Authors: Gokul P. Srinivasaragavan, Sheng Yang, Shreya Anand, Jesper Sollerman, Anna Y. Q. Ho, Alessandra Corsi, S. Bradley Cenko, Daniel Perley, Steve Schulze, Marquice Sanchez-Fleming, Jack Pope, Nikhil Sarin, Conor Omand, Kaustav K. Das, Christoffer Fremling, Igor Andreoni, Rachel Bruch, Kevin B. Burdge, Kishalay De, Avishay Gal-Yam, Anjasha Gangopadhyay, Matthew J. Graham, Jacob E. Jencson, Viraj Karambelkar, Mansi M. Kasliwal, S. R. Kulkarni, Julia Martikainen, Yashvi S. Sharma, Anastasios Tzanidakis, Lin Yan, Yuhan Yao, Eric C. Bellm, Steven L. Groom, Frank J. Masci, Guy Nir, Josiah Purdum, Roger Smith, Niharika Sravan
Figure caption: Spectral sequences of SN 2019moc, SN 2019oqp, and SN 2019pgo.
Paper: AGN STORM 2. X. The Origin of the Interband Continuum Delays in Mrk 817 
Authors: Hagai Netzer, Michael R. Goad, Aaron J. Barth, Edward M. Cackett, Keith Horne, Chen Hu, Erin Kara, Kirk T. Korista, Gerard A. Kriss, Collin Lewin, John Montano, Nahum Arav, Ehud Behar, Michael S. Brotherton, Doron Chelouche, Gisella De Rosa, Elena Dalla Bontà, Maryam Dehghanian, Gary J. Ferland, Carina Fian, Yasaman Homayouni, Dragana Ilić, Shai Kaspi, Andjelka B. Kovačević, Hermine Landt, Luka Č. Popović, Thaisa Storchi-Bergmann, Jian-Min Wang, Fatima Zaidouni
Figure caption: The measured delay (ICCF centroid) as a function of the DC fractional contribution to the total light (Disk+DC) for a face-on thin ring with a radius of 10 light days. The output signal is the sum of the input signal (driving light curve) and responding signal, such that the responding signal contributes a fraction of the total light in the range 0–1. The measured delay is taken to be the centroid of the cross-correlation function determined from cross-correlating the driving and responding signals (see the text for details). The dashed horizontal line indicates the delay of the DC component only (=10 days). The diagonal line indicates linearity—the measured delay is directly proportional to the fractional contribution of the DC component to the total light. Results are shown for two instances of the driving continuum light curve: the F(1144 Å) light curve for Mrk 817 (red) and a damped random walk, T dur = 500 days, and damping timescale, T char = 40 days (blue).
Paper: AGN STORM 2. X. The Origin of the Interband Continuum Delays in Mrk 817 
Authors: Hagai Netzer, Michael R. Goad, Aaron J. Barth, Edward M. Cackett, Keith Horne, Chen Hu, Erin Kara, Kirk T. Korista, Gerard A. Kriss, Collin Lewin, John Montano, Nahum Arav, Ehud Behar, Michael S. Brotherton, Doron Chelouche, Gisella De Rosa, Elena Dalla Bontà, Maryam Dehghanian, Gary J. Ferland, Carina Fian, Yasaman Homayouni, Dragana Ilić, Shai Kaspi, Andjelka B. Kovačević, Hermine Landt, Luka Č. Popović, Thaisa Storchi-Bergmann, Jian-Min Wang, Fatima Zaidouni
Figure caption: Calculated spectra of three BLR models considered in this paper with C(R out) = 0.2. The inner and outer boundaries are marked inside the figure. Note the significant differences in the emission-line widths reflecting the different distances from the central BH. In particular, in Model 1 (green line), significant velocity broadening makes line emission hard to discern.
Paper: AGN STORM 2. X. The Origin of the Interband Continuum Delays in Mrk 817 
Authors: Hagai Netzer, Michael R. Goad, Aaron J. Barth, Edward M. Cackett, Keith Horne, Chen Hu, Erin Kara, Kirk T. Korista, Gerard A. Kriss, Collin Lewin, John Montano, Nahum Arav, Ehud Behar, Michael S. Brotherton, Doron Chelouche, Gisella De Rosa, Elena Dalla Bontà, Maryam Dehghanian, Gary J. Ferland, Carina Fian, Yasaman Homayouni, Dragana Ilić, Shai Kaspi, Andjelka B. Kovačević, Hermine Landt, Luka Č. Popović, Thaisa Storchi-Bergmann, Jian-Min Wang, Fatima Zaidouni
Figure caption: A comparison of two COS-STIS spectra obtained during periods of high (v75, HJD = 2459322) and low (v30, HJD = 2459421) 1144 Å flux levels. The magenta curve shows the difference between the two spectra. The similarity of the spectra at long wavelengths compared with a factor of ≈2 difference in the 1144 Å flux suggests a significant change in the shape of the SED between the two epochs.
Paper: AGN STORM 2. X. The Origin of the Interband Continuum Delays in Mrk 817 
Authors: Hagai Netzer, Michael R. Goad, Aaron J. Barth, Edward M. Cackett, Keith Horne, Chen Hu, Erin Kara, Kirk T. Korista, Gerard A. Kriss, Collin Lewin, John Montano, Nahum Arav, Ehud Behar, Michael S. Brotherton, Doron Chelouche, Gisella De Rosa, Elena Dalla Bontà, Maryam Dehghanian, Gary J. Ferland, Carina Fian, Yasaman Homayouni, Dragana Ilić, Shai Kaspi, Andjelka B. Kovačević, Hermine Landt, Luka Č. Popović, Thaisa Storchi-Bergmann, Jian-Min Wang, Fatima Zaidouni
Figure caption: Comparison of the COS-STIS spectrum with an empirical model (green line) made of two components: Model 3 from Figure 3 (red line) and the Fe II template based on the UV observations of J. E. Mejía-Restrepo et al. (2016; magenta line).
Paper: AGN STORM 2. X. The Origin of the Interband Continuum Delays in Mrk 817 
Authors: Hagai Netzer, Michael R. Goad, Aaron J. Barth, Edward M. Cackett, Keith Horne, Chen Hu, Erin Kara, Kirk T. Korista, Gerard A. Kriss, Collin Lewin, John Montano, Nahum Arav, Ehud Behar, Michael S. Brotherton, Doron Chelouche, Gisella De Rosa, Elena Dalla Bontà, Maryam Dehghanian, Gary J. Ferland, Carina Fian, Yasaman Homayouni, Dragana Ilić, Shai Kaspi, Andjelka B. Kovačević, Hermine Landt, Luka Č. Popović, Thaisa Storchi-Bergmann, Jian-Min Wang, Fatima Zaidouni
Figure caption: Assumed continuum SED (in black) for Mrk 817 constructed from a thin disk and a power-law X-ray source normalized to the luminosity during the first 100 days of the campaign. The disk inclination to the line of sight is given by ﹩\cos i=0.75﹩. The blue line is a COS-STIS spectrum obtained on the HJD marked in the figure. More details are provided in the text.
Paper: AGN STORM 2. X. The Origin of the Interband Continuum Delays in Mrk 817 
Authors: Hagai Netzer, Michael R. Goad, Aaron J. Barth, Edward M. Cackett, Keith Horne, Chen Hu, Erin Kara, Kirk T. Korista, Gerard A. Kriss, Collin Lewin, John Montano, Nahum Arav, Ehud Behar, Michael S. Brotherton, Doron Chelouche, Gisella De Rosa, Elena Dalla Bontà, Maryam Dehghanian, Gary J. Ferland, Carina Fian, Yasaman Homayouni, Dragana Ilić, Shai Kaspi, Andjelka B. Kovačević, Hermine Landt, Luka Č. Popović, Thaisa Storchi-Bergmann, Jian-Min Wang, Fatima Zaidouni
Figure caption: The 1D response function (or TF) for the 7995 Å continuum band, for our model BLR viewed at line-of-sight inclination ﹩\cos (i)=0.75﹩. The response function has been normalized to the unit area. Inset: the 1D response function for the 7995 Å continuum band arising from the DW (Model 1) viewed at the same inclination.
Paper: AGN STORM 2. X. The Origin of the Interband Continuum Delays in Mrk 817 
Authors: Hagai Netzer, Michael R. Goad, Aaron J. Barth, Edward M. Cackett, Keith Horne, Chen Hu, Erin Kara, Kirk T. Korista, Gerard A. Kriss, Collin Lewin, John Montano, Nahum Arav, Ehud Behar, Michael S. Brotherton, Doron Chelouche, Gisella De Rosa, Elena Dalla Bontà, Maryam Dehghanian, Gary J. Ferland, Carina Fian, Yasaman Homayouni, Dragana Ilić, Shai Kaspi, Andjelka B. Kovačević, Hermine Landt, Luka Č. Popović, Thaisa Storchi-Bergmann, Jian-Min Wang, Fatima Zaidouni
Figure caption: MERs as a function of wavelength for the three BLR models shown in Figure 3.
Paper: AGN STORM 2. X. The Origin of the Interband Continuum Delays in Mrk 817 
Authors: Hagai Netzer, Michael R. Goad, Aaron J. Barth, Edward M. Cackett, Keith Horne, Chen Hu, Erin Kara, Kirk T. Korista, Gerard A. Kriss, Collin Lewin, John Montano, Nahum Arav, Ehud Behar, Michael S. Brotherton, Doron Chelouche, Gisella De Rosa, Elena Dalla Bontà, Maryam Dehghanian, Gary J. Ferland, Carina Fian, Yasaman Homayouni, Dragana Ilić, Shai Kaspi, Andjelka B. Kovačević, Hermine Landt, Luka Č. Popović, Thaisa Storchi-Bergmann, Jian-Min Wang, Fatima Zaidouni
Figure caption: Computed continuum lags for the three models shown in Figure 3, assuming f lag = 0.9 for Model 1 and f lag = 0.5 for the other two models (see the text for the justification). The large differences in lags mostly reflect the different MERs of the models.
Paper: Luminosity Evolution of the Hot Gas in Normal Galaxies from the Near Universe to z = 0.5
Authors: Dong-Woo Kim, Giuseppina Fabbiano
Figure caption: Same as Figure 13 (left), but with L X,GAS determined with Method A (left) and Method B (right) in Section 4. The two steep lines indicate ﹩{{L}}_{{\rm{X}},\mathrm{GAS}}\sim {{{M}}_{\mathrm{STAR}}}^{6}﹩ (red) and ﹩{{L}}_{{\rm{X}},\mathrm{GAS}}\sim {{{M}}_{\mathrm{STAR}}}^{4.5}﹩ (blue). The flatter green line indicates ﹩{{L}}_{{\rm{X}},\mathrm{GAS}}\sim {{{M}}_{\mathrm{STAR}}}^{1.5}﹩. The thick transparent gray line indicates the stacking result from Anderson et al. (2015). The green and magenta points represent average values in the M STAR range used by Anderson et al. (2015). See the text for the details.
Paper: Luminosity Evolution of the Hot Gas in Normal Galaxies from the Near Universe to z = 0.5
Authors: Dong-Woo Kim, Giuseppina Fabbiano
Figure caption:  L X in the S band (left) and in the H band (right) plotted against M STAR. The K-correction for the APEC (left) and PL model (right) is applied. Each data point is color-coded by z (see color scale on the right side of the Figure). The red solid and dashed lines indicate the expected L X,LMXB and L X,HMXB at z = 0, respectively. The green solid and dashed lines indicate the expected L X,LMXB and L X,HMXB at z = 0.6, respectively.
Paper: Luminosity Evolution of the Hot Gas in Normal Galaxies from the Near Universe to z = 0.5
Authors: Dong-Woo Kim, Giuseppina Fabbiano
Figure caption: Histograms of L X,GAS(S) to L X(S). In Method A, L X,GAS(S) = L X(S)–(L X, LMXB(S) + L X,LMXB(S)) and in Method B, L X,GAS(S) = L X(S)–L X,PL(S).
Paper: Luminosity Evolution of the Hot Gas in Normal Galaxies from the Near Universe to z = 0.5
Authors: Dong-Woo Kim, Giuseppina Fabbiano
Figure caption: The same as the right panel of Figure 11, except the assumed photon index is (left) 1.2 and (right) 1.6.
Paper: Luminosity Evolution of the Hot Gas in Normal Galaxies from the Near Universe to z = 0.5
Authors: Dong-Woo Kim, Giuseppina Fabbiano
Figure caption: The same as the right panels of Figures 10 and 11, but only with red galaxies (g − r > 0.7).
Paper: Luminosity Evolution of the Hot Gas in Normal Galaxies from the Near Universe to z = 0.5
Authors: Dong-Woo Kim, Giuseppina Fabbiano
Figure caption:  g − r histogram of our sample. The boundary of red and blue subsamples is set at g − r = 0.7.
Paper: Luminosity Evolution of the Hot Gas in Normal Galaxies from the Near Universe to z = 0.5
Authors: Dong-Woo Kim, Giuseppina Fabbiano
Figure caption: The same as Figure A2, but only with blue galaxies (g − r < 0.7).
Paper: Photospheric Hot Spots at Solar Coronal Loop Footpoints Revealed by Hyperspectral Imaging Observations
Authors: L. P. Chitta, M. van Noort, H. N. Smitha, E. R. Priest, L. H. M. Rouppe van der Voort
Figure caption: Magnetic signal of hot spots. Integrated MiHI Stokes V/I signal derived for the 29 hot spots whose lifetimes are at least 20 s. The field of view (2″ × 2″) is centered on the hot-spot pixel, when the event reaches its peak intensity in the red wing (location marked by the red-blue cross hair). The overlaid red and blue curves are the Stokes V/I signal along the respective colored cross-hair section, over the extent of the field of view. All the line plots have the same scale, with minimum and maximum, respectively, set to 0 and 1.6 in the Stokes V/I units. See Section 2 and Appendix D for details.
Paper: Photospheric Hot Spots at Solar Coronal Loop Footpoints Revealed by Hyperspectral Imaging Observations
Authors: L. P. Chitta, M. van Noort, H. N. Smitha, E. R. Priest, L. H. M. Rouppe van der Voort
Figure caption: Hα line bisectors. The three curves show the line bisectors derived for the average Hα line profile corresponding to the three distinct features as labeled (red: hot spots, green: network, magenta: quiet Sun). See Appendix C for details.
Paper: New Measurements of the Lyα Forest Continuum and Effective Optical Depth with LyCAN and DESI Y1 Data
Authors: Wynne Turner, Paul Martini, Naim Göksel Karaçaylı, J. Aguilar, S. Ahlen, D. Brooks, T. Claybaugh, A. de la Macorra, A. Dey, P. Doel, K. Fanning, J . E. Forero-Romero, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, G. Gutierrez, J. Guy, H. K. Herrera-Alcantar, K. Honscheid, S. Juneau, T. Kisner, A. Kremin, A. Lambert, M. Landriau, L. Le Guillou, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, C. Poppett, F. Prada, M. Rezaie, G. Rossi, E. Sanchez, E. F. Schlafly, D. Schlegel, Michael F. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: Distribution of coefficients obtained from fitting six NMF components to the 1230–1600 Å region of 10,000 DESI Y1 (gray points and black contours) and 48 COS quasar spectra (large blue and red points). The six components were derived from COS observations, where c  i  indicates the coefficient associated with component i. The red points mark the 10 COS objects with the lowest likelihood (<10−10) of being described by the GMM representation of the DESI distribution. These 10 quasar spectra (red points) were removed as unrepresentative of DESI quasars. The remaining 38 (blue points) were retained for the analysis.
Paper: Photospheric Hot Spots at Solar Coronal Loop Footpoints Revealed by Hyperspectral Imaging Observations
Authors: L. P. Chitta, M. van Noort, H. N. Smitha, E. R. Priest, L. H. M. Rouppe van der Voort
Figure caption: Forward synthesis of Hα hot spots profiles. The black hatched region covers the entire range of the intensity profiles of all the 161 hot spots, retrieved during their brightness peak. The red-colored curves are the synthesized Hα line profiles obtained by randomly varying the temperature of the input atmosphere. The magenta curve is the quiet-Sun Hα line profile, shown here for reference. See Section 3.2 and Appendix B for details.
Paper: New Measurements of the Lyα Forest Continuum and Effective Optical Depth with LyCAN and DESI Y1 Data
Authors: Wynne Turner, Paul Martini, Naim Göksel Karaçaylı, J. Aguilar, S. Ahlen, D. Brooks, T. Claybaugh, A. de la Macorra, A. Dey, P. Doel, K. Fanning, J . E. Forero-Romero, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, G. Gutierrez, J. Guy, H. K. Herrera-Alcantar, K. Honscheid, S. Juneau, T. Kisner, A. Kremin, A. Lambert, M. Landriau, L. Le Guillou, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, C. Poppett, F. Prada, M. Rezaie, G. Rossi, E. Sanchez, E. F. Schlafly, D. Schlegel, Michael F. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: HST/COS quasar spectrum and the smooth representation from LineTools. The original COS spectrum is in gray and the continuum fit is in blue. The continuum includes the extrapolation to 1040 Å (see Section 3.1).
Paper: New Measurements of the Lyα Forest Continuum and Effective Optical Depth with LyCAN and DESI Y1 Data
Authors: Wynne Turner, Paul Martini, Naim Göksel Karaçaylı, J. Aguilar, S. Ahlen, D. Brooks, T. Claybaugh, A. de la Macorra, A. Dey, P. Doel, K. Fanning, J . E. Forero-Romero, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, G. Gutierrez, J. Guy, H. K. Herrera-Alcantar, K. Honscheid, S. Juneau, T. Kisner, A. Kremin, A. Lambert, M. Landriau, L. Le Guillou, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, C. Poppett, F. Prada, M. Rezaie, G. Rossi, E. Sanchez, E. F. Schlafly, D. Schlegel, Michael F. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: Redshift distribution of the HST/COS objects. The blue distribution is the original sample of 48 objects, while the orange distribution shows the final sample of 38 objects after outlier removal (see Section 3.1).
Paper: New Measurements of the Lyα Forest Continuum and Effective Optical Depth with LyCAN and DESI Y1 Data
Authors: Wynne Turner, Paul Martini, Naim Göksel Karaçaylı, J. Aguilar, S. Ahlen, D. Brooks, T. Claybaugh, A. de la Macorra, A. Dey, P. Doel, K. Fanning, J . E. Forero-Romero, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, G. Gutierrez, J. Guy, H. K. Herrera-Alcantar, K. Honscheid, S. Juneau, T. Kisner, A. Kremin, A. Lambert, M. Landriau, L. Le Guillou, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, C. Poppett, F. Prada, M. Rezaie, G. Rossi, E. Sanchez, E. F. Schlafly, D. Schlegel, Michael F. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: Reduced χ 2 for NMF models with a number of components ranging from 2 to 20. These components were derived from our initial sample of 48 COS continua. We used models with six components throughout this paper.
Paper: New Measurements of the Lyα Forest Continuum and Effective Optical Depth with LyCAN and DESI Y1 Data
Authors: Wynne Turner, Paul Martini, Naim Göksel Karaçaylı, J. Aguilar, S. Ahlen, D. Brooks, T. Claybaugh, A. de la Macorra, A. Dey, P. Doel, K. Fanning, J . E. Forero-Romero, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, G. Gutierrez, J. Guy, H. K. Herrera-Alcantar, K. Honscheid, S. Juneau, T. Kisner, A. Kremin, A. Lambert, M. Landriau, L. Le Guillou, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, C. Poppett, F. Prada, M. Rezaie, G. Rossi, E. Sanchez, E. F. Schlafly, D. Schlegel, Michael F. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: The mean spectra for our four classes of COS continua from the GMM representation of the NMF coefficients.
Paper: A JWST MIRI MRS View of the η Tel Debris Disk and Its Brown Dwarf Companion
Authors: Yiwei Chai, Christine H. Chen, Kadin Worthen, Alexis Li, Antranik A. Sefilian, William Balmer, Dean C. Hines, David R. Law, B. A. Sargent, Mark Wyatt, Cicero X. Lu, Marshall D. Perrin, Isabel Rebollido, Emily Rickman, G. C. Sloan
Figure caption: MIRI MRS spectrum of η Tel A, overplotted onto a T eff = 9700 K, ﹩\mathrm{log}(g)=4.0﹩ photosphere model (T. Mittal et al. 2015). The Spitzer IRS spectrum (C. H. Chen et al. 2014) is shown in orange, along with MIPS photometry (L. M. Rebull et al. 2008). We include our atmosphere model for η Tel B (see Section 5.1) to show that the flux contribution from the companion does not significantly impact the spectrum of the disk, even with the larger Spitzer aperture. The data set used to create this figure is available for download from the online journal.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: A JWST MIRI MRS View of the η Tel Debris Disk and Its Brown Dwarf Companion
Authors: Yiwei Chai, Christine H. Chen, Kadin Worthen, Alexis Li, Antranik A. Sefilian, William Balmer, Dean C. Hines, David R. Law, B. A. Sargent, Mark Wyatt, Cicero X. Lu, Marshall D. Perrin, Isabel Rebollido, Emily Rickman, G. C. Sloan
Figure caption: The same wavelength slice shown in Figure 1 after PSF subtraction using N Car, in which the PSF has been scaled to the peak flux of the η Tel slice. The image is log-scaled, so the blacked-out values within the FOV indicate regions of slight oversubtraction. Astronomical objects are labeled: (a) the spatially resolved component of the η Tel A debris disk; (b) η Tel B; (c) background galaxy 2CX0 J192251.5-542530; and (d) an unknown feature (see Section 3.3).
Paper: A JWST MIRI MRS View of the η Tel Debris Disk and Its Brown Dwarf Companion
Authors: Yiwei Chai, Christine H. Chen, Kadin Worthen, Alexis Li, Antranik A. Sefilian, William Balmer, Dean C. Hines, David R. Law, B. A. Sargent, Mark Wyatt, Cicero X. Lu, Marshall D. Perrin, Isabel Rebollido, Emily Rickman, G. C. Sloan
Figure caption: An example slice from the calibrated subband 3A data cube output by Stage 3 of the JWST pipeline, shown with a logarithmic scaling. Note that the six-point PSF dominates most of the FOV. Blacked-out NaN values within the FOV indicate areas of slight oversubtraction due to the pipeline background subtraction.
Paper: Modeling the X-Ray Emission of the Boomerang Nebula and Implication for Its Potential Ultrahigh-energy Gamma-Ray Emission
Authors: Xiao-Bin Chen, Xuan-Han Liang, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: Left panel: the fitting result of the radial profiles of X-ray surface brightness and photon index for the convection-only scenario. The optimal fitting values for MCMC are: η  B  = 0.015,  η  e  = 0.046,  α = 2.001,  β = 0.231,  ϵ = 0.91. The red line represents the PWN electron component, the green dashed–dotted line represents the SNR electron component, and the blue solid line with 1σ error band (gray) is the sum of the two. Cyan and magenta data points are from Chandra and XMM-Newton, respectively, taken from C. Ge et al. (2021). Displayed statistical and system errors, with a system error of 10% and indicated in black, due to calibration uncertainties of instruments (G. Schellenberger et al. 2015). Right panel: local electron spectra at different radii for the convection-dominated scenario.
Paper: Modeling the X-Ray Emission of the Boomerang Nebula and Implication for Its Potential Ultrahigh-energy Gamma-Ray Emission
Authors: Xiao-Bin Chen, Xuan-Han Liang, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: Left panel: the fitting result of the radial profiles of X-ray surface brightness and photon index for convection–diffusion scenario. The optimal fitting values for MCMC are: η  B  = 8.458 × 10−3,  η  e  = 0.0246,  α = 1.692,  β = 0.2836,  ϵ = 0.570. Right panel: local electron spectra at different radii for the convection–diffusion scenario. Legend same as Figure 2.
Paper: Modeling the X-Ray Emission of the Boomerang Nebula and Implication for Its Potential Ultrahigh-energy Gamma-Ray Emission
Authors: Xiao-Bin Chen, Xuan-Han Liang, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: X-ray Images of the Boomerang Nebula. The central-colored part is the combination of the X-ray observation from Chandra and XMM-Newton (C. Ge et al. 2021). The green circle has a radius of 100″ centered at the position of PSR J2229+6114. The two cyan arcs mark the approximate boundary between the head (900″) and the tail (1800″) of the SNR in the X-ray band. The white curve outlines the 1.4 GHz radio continuum of the SNR (S. Pineault & G. Joncas 2000). The region roughly represented by a quarter of a solid circle extending to the southwest direction is the focus of our model.
Paper: Modeling the X-Ray Emission of the Boomerang Nebula and Implication for Its Potential Ultrahigh-energy Gamma-Ray Emission
Authors: Xiao-Bin Chen, Xuan-Han Liang, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: The multiwavelength spectral energy distribution of PWN Boomerang for three scenarios. The green line represents a circular area with a radius of 100″ around the pulsar, and the orange line depicts a southwest extension structure stretching 900″, with the width of each line indicating the allowed error range of 1σ. The blue, cyan, and magenta TeV data points are from MAGIC (MAGIC Collaboration et al. 2023), ASγ (ASγ Collaboration et al. 2021), and LHAASO (LHAASO Collaboration et al. 2021), respectively. The brown butterfly plot is from HAWC (A. Albert et al. 2020).
Paper: Modeling the X-Ray Emission of the Boomerang Nebula and Implication for Its Potential Ultrahigh-energy Gamma-Ray Emission
Authors: Xiao-Bin Chen, Xuan-Han Liang, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: Left panel: the fitting result of the radial profiles of X-ray surface brightness and photon index for Diffusion-dominated scenario. The optimal fitting values for MCMC are: η  B  = 0.0223,  η  e  = 0.0117,  α = 1.476,  β = 0.3146,  ϵ = 0.1893. Right panel: local electron spectra at different radii for the diffusion-dominated scenario. Legend same as Figure 2.