adsabs/AstroCLIMB huggingface dataset:
Paper: Early Results from GLASS–JWST. XXI. Rapid Asembly of a Galaxy at z = 6.23 Revealed by Its C/O Abundance
Authors: Tucker Jones, Ryan Sanders, Yuguang Chen, Xin Wang, Takahiro Morishita, Guido Roberts-Borsani, Tommaso Treu, Alan Dressler, Emiliano Merlin, Diego Paris, Paola Santini, Pietro Bergamini, A. Henry, Erin Huntzinger, Themiya Nanayakkara, Kristan Boyett, Marusa Bradac, Gabriel Brammer, Antonello Calabró, Karl Glazebrook, Kathryn Grasha, Sara Mascia, Laura Pentericci, Michele Trenti, Benedetta Vulcani
Figure caption: Results of spectral energy distribution (SED) fitting with a non-parametric star formation history (for details see Morishita et al. 2019). Left: the SED fit accurately reproduces the HST and JWST photometry (red points; open diamonds and gray spectrum show the best-fit model results), including strong emission line contributions in the F356W and F444W filters. The filter bandpasses are shown with colored shading below. Right: total stellar mass formed as a function of lookback time, based on the SED fit. The mass shown here is corrected for lensing magnification μ = 2.59 (equivalent to 0.4 dex; we do not propagate the ∼1% formal uncertainty in μ here). The ≳100 Myr timescale for increased C/O from asymptotic giant branch (AGB) stars is indicated with a red arrow, corresponding to stars formed at z ≳ 7 in this case. C/O abundance of this galaxy indicates enrichment dominated by core-collapse supernovae (SNe), with a majority of the stars formed within ≲100 Myr of the observed epoch, consistent with the best-fit mass-weighted age from SED fitting.
Paper: Early Results from GLASS–JWST. XXI. Rapid Asembly of a Galaxy at z = 6.23 Revealed by Its C/O Abundance
Authors: Tucker Jones, Ryan Sanders, Yuguang Chen, Xin Wang, Takahiro Morishita, Guido Roberts-Borsani, Tommaso Treu, Alan Dressler, Emiliano Merlin, Diego Paris, Paola Santini, Pietro Bergamini, A. Henry, Erin Huntzinger, Themiya Nanayakkara, Kristan Boyett, Marusa Bradac, Gabriel Brammer, Antonello Calabró, Karl Glazebrook, Kathryn Grasha, Sara Mascia, Laura Pentericci, Michele Trenti, Benedetta Vulcani
Figure caption: 2D and 1D spectra of rest-frame UV emission lines in velocity space. Vertical dashed lines in the 1D panels show expected line centers for the C III] and C IV doublets, relative to the best-fit redshift of optical [O III] and Hβ. The velocity origin in each panel corresponds to the bluer line. Best-fit line profiles (Section 2.2) are shown in red. The C III] redshift is consistent with the optical lines and rest-UV O III], while C IV emission is redshifted by ∼170 km s−1. This C IV velocity offset can be plausibly explained by resonant scattering in a galactic outflow.
Paper: JWST Peers into the Class I Protostar TMC1A: Atomic Jet and Spatially Resolved Dissociative Shock Region
Authors: D. Harsono, P. Bjerkeli, J. P. Ramsey, K. M. Pontoppidan, L. E. Kristensen, J. K. Jørgensen, H. Calcutt, Z-Y. Li, A. Plunkett
Figure caption: (a.) JWST 2 μm continuum map is shown in color. A linear scale between 0.5% and 99% of the intensity distribution is used. We have overlaid the HST F160W and ALMA 230 GHz continuum maps on top of the 2 μm map to orient our results with respect to previous observations. The contours are chosen to highlight the features of the HST image and the location of the millimeter dust disk. (b.) The integrated H I Paα map is shown by the black contour lines on top of the 2 μm map. Contours from 95% to 98% of the intensity distribution are used. ALMA observations of the blue- and redshifted rotational transition of 12CO (J = 2 − 1) are shown by the blue and red contours, respectively. The 12CO J = 2 − 1 line is only showing velocities >1.5 km s−1 from systemic. The contours are chosen to highlight the orientation of the 12CO J = 2 − 1 gas. (c.) A comparison between [Fe II] 1.644 μm, He I λ10835, and 12CO J = 2 − 1 line emission. The integrated [Fe II] line is shown in the background in green with a linear scale spanning between 60% and 99% of the intensity distribution. The He I map is shown by the brown contours with levels from 95% to 97% of the intensity distribution. (d.) A comparison between the [Fe II] 1.644 μm, O I λ1.12, and 12CO J = 2 − 1 lines. The contours of O I (in brown) are also showing the brightest components (95%–97% of the intensity distribution). (e.) The integrated [Fe II] map is overlaid on top of the integrated H2 2.12 μm map. The H2 map is drawn with colors spanning from 5σ up to the peak intensity. The green contours show [Fe II] but only the brightest pixels in the map (>96% of the intensity distribution). The center of the millimeter dust disk is indicated by the star. In each panel, a 50 au scale bar is show in the bottom left.
Paper: A Model for Confined Solar Eruptions Including External Reconnection
Authors: Jun Chen, Xin Cheng, Bernhard Kliem, MingDe Ding
Figure caption: Time–distance plot of U  z (0, 0, z) for the run Quadrupole2. Plus signs mark the position of the magnetic rope axis. A dotted line, where B  x  = 0, traces the motion of the apex of the upper (quasi-)separator.
Paper: JWST Peers into the Class I Protostar TMC1A: Atomic Jet and Spatially Resolved Dissociative Shock Region
Authors: D. Harsono, P. Bjerkeli, J. P. Ramsey, K. M. Pontoppidan, L. E. Kristensen, J. K. Jørgensen, H. Calcutt, Z-Y. Li, A. Plunkett
Figure caption: Top: normalized spectrum of TMC1A. The spectrum has been normalized with a global continuum fit constructed with polynomials of degrees 5 to 7. Transitions of H I, He I, O I, and Fe II with high A  ij  values are indicated by the vertical colored lines above the spectrum. Bottom: zoom-in spectra of the brightest H I lines and the He I λ10835 line. The spectral resolution is Δv ∼ 100–150 km s−1.
Paper: JWST Peers into the Class I Protostar TMC1A: Atomic Jet and Spatially Resolved Dissociative Shock Region
Authors: D. Harsono, P. Bjerkeli, J. P. Ramsey, K. M. Pontoppidan, L. E. Kristensen, J. K. Jørgensen, H. Calcutt, Z-Y. Li, A. Plunkett
Figure caption: NIRSpec spectrum extracted from the central 0.″3 spaxels. The spectral energy distribution of TMC1A from other observations is shown in the inset along with the NIRSpec data in blue. The photometric data points (black) are from Kristensen et al. (2012; which include points from Skrutskie et al. 2006; Di Francesco et al. 2008; Evans et al. 2009; Karska et al. 2013; Green et al. 2013). The Herschel PACS observations of Green et al. (2013) are shown in orange. The SPITZER IRS spectrum (pink; Lahuis et al. 2010) is overlaid. The extracted NIRSpec spectrum is available as data-behind-the-figure.(The data used to create this figure are available.)
Paper: JWST Peers into the Class I Protostar TMC1A: Atomic Jet and Spatially Resolved Dissociative Shock Region
Authors: D. Harsono, P. Bjerkeli, J. P. Ramsey, K. M. Pontoppidan, L. E. Kristensen, J. K. Jørgensen, H. Calcutt, Z-Y. Li, A. Plunkett
Figure caption: Cartoon of TMC1A’s physical structure. The three major components that are traced by the hot gas lines are accretion onto the protostar, the jet, and the illuminated cavity wall. The disk and the cold wind as traced with ALMA are also indicated.
Paper: JWST Peers into the Class I Protostar TMC1A: Atomic Jet and Spatially Resolved Dissociative Shock Region
Authors: D. Harsono, P. Bjerkeli, J. P. Ramsey, K. M. Pontoppidan, L. E. Kristensen, J. K. Jørgensen, H. Calcutt, Z-Y. Li, A. Plunkett
Figure caption: Left: original positions of the images. Right: aligned images after correcting for proper motion.
Paper: Early Results from GLASS–JWST. XXI. Rapid Asembly of a Galaxy at z = 6.23 Revealed by Its C/O Abundance
Authors: Tucker Jones, Ryan Sanders, Yuguang Chen, Xin Wang, Takahiro Morishita, Guido Roberts-Borsani, Tommaso Treu, Alan Dressler, Emiliano Merlin, Diego Paris, Paola Santini, Pietro Bergamini, A. Henry, Erin Huntzinger, Themiya Nanayakkara, Kristan Boyett, Marusa Bradac, Gabriel Brammer, Antonello Calabró, Karl Glazebrook, Kathryn Grasha, Sara Mascia, Laura Pentericci, Michele Trenti, Benedetta Vulcani
Figure caption: Overview of the spectroscopic data. The top left panel shows JWST/NIRCam imaging (F115W/F200W/F444W = blue/green/red) in a 2″ × 2″ field centered on the target galaxy, with the position of the NIRSpec slitlet indicated by the rectangle. The other panels show regions of the spectra around the main emission lines used in this work with best-fit profiles shown in red (see Section 2.2 for details). Residuals around each line are shown in blue, offset vertically for clarity. All key lines used in this work are clearly detected, with ≳7σ significance for the rest-UV O III] and C III] doublets and 5.2σ for the C IV doublet. Residuals are generally consistent with the noise level in the spectra, except for [O III] λ λ4959,5007 which is discussed in Section 2.2.
Paper: The Kelvin–Helmholtz Instability at the Boundary of Relativistic Magnetized Jets
Authors: Anthony Chow, Jordy Davelaar, Michael E. Rowan, Lorenzo Sironi
Figure caption: A 3D schematic diagram of the boundary of the relativistic jet. The boundary (gray color) is located in the x − z plane. Above and below the boundary are the magnetically dominated cold jet and the unmagnetized gas-pressure-supported ambient wind, respectively.  q  ∥ is the projection of the wavevector  q  onto the boundary. The jet is at rest and the wind has a relative shear speed of  v . The magnetic field in the jet is  B . θ is the angle between  q  ∥ and  v , while ψ is the angle between  B  and  q  ∥.
Paper: The Kelvin–Helmholtz Instability at the Boundary of Relativistic Magnetized Jets
Authors: Anthony Chow, Jordy Davelaar, Michael E. Rowan, Lorenzo Sironi
Figure caption: Dependence of the instability growth rate ﹩\mathrm{Im}(\phi )﹩ on θ and M  e , for two choices of v A and two choices of ﹩\cos \psi ﹩, as indicated in the plots. The left and right columns represent the numerical and analytical solutions, respectively. For ﹩\cos \psi =0﹩, the maximum growth rate of the analytical solution is capped at its numerical counterpart to avoid the divergence at M  e  = 1. In all the panels, ﹩\mathrm{Im}(\phi )﹩ is then normalized to its maximum value, which is quoted in the panels themselves. The vertical dotted lines show the analytical upper bound on M  e  when ﹩\cos \psi =1﹩; see Equation (26). The vertical solid white lines indicate M  e  = 1.
Paper: The Kelvin–Helmholtz Instability at the Boundary of Relativistic Magnetized Jets
Authors: Anthony Chow, Jordy Davelaar, Michael E. Rowan, Lorenzo Sironi
Figure caption: Dependence of the maximum instability growth rate ﹩\mathrm{Im}(\phi )﹩ on ﹩\cos {\rm{\Omega }}﹩ and M ≡ v/v A, for two choices of v A, as indicated in the plots. The maximum value of ﹩\mathrm{Im}(\phi )﹩ is taken across all values of ﹩\cos \theta \in [0,1]﹩ for each ﹩(M,\cos {\rm{\Omega }})﹩ pair. The left and right columns represent the numerical and analytical solutions, respectively. In all the panels, ﹩\mathrm{Im}(\phi )﹩ is then normalized to its maximum value, which is quoted in the panels themselves. The white lines indicate ﹩M=\cos {\rm{\Omega }}﹩ and M = 1/v A.
Paper: The Kelvin–Helmholtz Instability at the Boundary of Relativistic Magnetized Jets
Authors: Anthony Chow, Jordy Davelaar, Michael E. Rowan, Lorenzo Sironi
Figure caption: Dependence of the instability growth rate ﹩\mathrm{Im}(\phi )﹩ on ψ and M  e , for two choices of v A as indicated in the plots. We fix ﹩\cos \theta =1﹩. See the caption to Figure 2 for further details.
Paper: The Kelvin–Helmholtz Instability at the Boundary of Relativistic Magnetized Jets
Authors: Anthony Chow, Jordy Davelaar, Michael E. Rowan, Lorenzo Sironi
Figure caption: Dependence of the instability growth rate Im (ϕ) on ﹩\cos \theta ﹩ for two choices of v A and a fixed value of ﹩\cos \psi =0﹩ in the singular case M  e  = 1. The solid lines represent the numerical solutions, while the dashed lines represent the analytical solutions obtained by Puiseux series expansion in the main text.
Paper: The Kelvin–Helmholtz Instability at the Boundary of Relativistic Magnetized Jets
Authors: Anthony Chow, Jordy Davelaar, Michael E. Rowan, Lorenzo Sironi
Figure caption: Dependence of the instability growth rate Im (ϕ) on ﹩\cos \psi ﹩ for two choices of v A and a fixed value of ﹩\cos \theta =1﹩ in the singular case M  e  = 1. The solid lines represent the numerical solutions, while the dashed lines represent the analytical solutions obtained by Puiseux series expansion in the main text.
Paper: A Comprehensive Simulation of Solar Wind Formation from the Solar Interior: Significant Cross-field Energy Transport by Interchange Reconnection near the Sun
Authors: Haruhisa Iijima, Takuma Matsumoto, Hideyuki Hotta, Shinsuke Imada
Figure caption: Overview of the simulated solar atmosphere. (a)–(b) Radial velocity field and radial magnetic field (normalized by its horizontal average), respectively, on an xr-plane at y = 0, where r = z + R ⊙. (c)–(e) Radial velocity field, proton number density, and radial magnetic field measured on an xy-plane at r = 29R ⊙, respectively. In each panel, the point value at (x, y) = (0, 0) is shown as a solid black line, and the gray-shaded region represents the range of the maximum and minimum values on the same xy-plane. (f) Differential emission measure at T = 1 MK observed from the top of the simulation box. (g) Radial magnetic field in the solar photosphere (at the optical depth unity). In panels (a), (b), (f), and (g), all variables are measured at time = 29 hr.
Paper: A Comprehensive Simulation of Solar Wind Formation from the Solar Interior: Significant Cross-field Energy Transport by Interchange Reconnection near the Sun
Authors: Haruhisa Iijima, Takuma Matsumoto, Hideyuki Hotta, Shinsuke Imada
Figure caption: Time variations in the solar atmosphere with magnetic activity near the surface. (a) rms of the radial magnetic field in a horizontal plane at z = 2 Mm (base of the corona, solid black line) and z = 40 Mm (middle corona, dashed red line). (b), (c) Horizontal average of the plasma temperature and radial magnetic energy flux, respectively, measured at z = 40 Mm. (d) Horizontal average of the radial velocity field at r = 29R ⊙. (e)–(g) Dependencies of the coronal temperature, coronal magnetic energy flux, and solar wind speed, respectively, on the rms of the magnetic field at z = 2 Mm. The shaded region in panels (b)–(d) is possibly affected by the initial condition and is thus excluded from the scatterplots (e)–(g) and other analyses.
Paper: A Comprehensive Simulation of Solar Wind Formation from the Solar Interior: Significant Cross-field Energy Transport by Interchange Reconnection near the Sun
Authors: Haruhisa Iijima, Takuma Matsumoto, Hideyuki Hotta, Shinsuke Imada
Figure caption: Magnetic and thermodynamic structures in the low corona. (a) Three-dimensional structure of the magnetic field lines. The line color indicates the plasma temperature. Horizontal slices of the radial magnetic field at z = 2 Mm and plasma temperature at z = 20 Mm are also shown. (b) Horizontal slices of (left) the plasma temperature T, (middle) the vertical velocity V  z , and (right) the magnitude of current density ﹩\left|{\rm{\nabla }}\times {\boldsymbol{B}}\right|﹩ at different heights. The thin solid lines indicate the boundary between the open and closed magnetic regions. Most of the field lines are open at z = 40 Mm.
Paper: A Comprehensive Simulation of Solar Wind Formation from the Solar Interior: Significant Cross-field Energy Transport by Interchange Reconnection near the Sun
Authors: Haruhisa Iijima, Takuma Matsumoto, Hideyuki Hotta, Shinsuke Imada
Figure caption: Strong energy transport from the closed coronal loops into the solar wind. (a) Vertical profile of the horizontally averaged magnetic energy flux (black dotted line). Energy fluxes in the open (solid red line) and closed (dashed blue line) field regions are also shown. (b) Gain and loss of the magnetic energy flux per unit mass (roughly corresponding to the cooling and heating rates of plasma, respectively) in the open field region. Thick and thin light lines show the vertically low-pass filtered and unfiltered data, respectively.
Paper: A Comprehensive Simulation of Solar Wind Formation from the Solar Interior: Significant Cross-field Energy Transport by Interchange Reconnection near the Sun
Authors: Haruhisa Iijima, Takuma Matsumoto, Hideyuki Hotta, Shinsuke Imada
Figure caption: Schematic illustration of energy transport in the solar corona. Field-aligned transport supplies half of the total energy input in the open field region. The remaining half comes from the closed field region through the interactions between open and closed magnetic field lines.
Paper: Constraints on the Intergalactic Magnetic Field Using Fermi-LAT and H.E.S.S. Blazar Observations
Authors: F. Aharonian, J. Aschersleben, M. Backes, V. Barbosa Martins, R. Batzofin, Y. Becherini, D. Berge, B. Bi, M. Bouyahiaoui, M. Breuhaus, R. Brose, F. Brun, B. Bruno, T. Bulik, C. Burger-Scheidlin, T. Bylund, S. Caroff, S. Casanova, J. Celic, M. Cerruti, T. Chand, S. Chandra, A. Chen, J. Chibueze, O. Chibueze, G. Cotter, M. de Bony, K. Egberts, J.-P. Ernenwein, G. Fichet de Clairfontaine, M. Filipovic, G. Fontaine, M. Füssling, S. Funk, S. Gabici, S. Ghafourizadeh, G. Giavitto, D. Glawion, J. F. Glicenstein, P. Goswami, M.-H. Grondin, L. Haerer, T. L. Holch, M. Holler, D. Horns, M. Jamrozy, F. Jankowsky, V. Joshi, I. Jung-Richardt, E. Kasai, K. Katarzyński, R. Khatoon, B. Khélifi, W. Kluźniak, Nu. Komin, K. Kosack, D. Kostunin, R. G. Lang, S. Le Stum, F. Leitl, A. Lemière, J.-P. Lenain, F. Leuschner, T. Lohse, A. Luashvili, I. Lypova, J. Mackey, D. Malyshev, D. Malyshev, V. Marandon, P. Marchegiani, A. Marcowith, G. Martí-Devesa, R. Marx, M. Meyer, A. Mitchell, R. Moderski, L. Mohrmann, A. Montanari, E. Moulin, J. Muller, T. Murach, K. Nakashima, J. Niemiec, S. Ohm, L. Olivera-Nieto, E. de Ona Wilhelmi, S. Panny, M. Panter, R. D. Parsons, G. Peron, D. A. Prokhorov, H. Prokoph, G. Pühlhofer, M. Punch, A. Quirrenbach, P. Reichherzer, A. Reimer, O. Reimer, B. Reville, F. Rieger, G. Rowell, B. Rudak, E. Ruiz-Velasco, V. Sahakian, D. A. Sanchez, M. Sasaki, F. Schüssler, H. M. Schutte, U. Schwanke, J. N. S. Shapopi, H. Sol, S. Spencer, S. Steinmassl, H. Suzuki, T. Takahashi, T. Tanaka, A. M. Taylor, R. Terrier, C. Thorpe-Morgan, M. Tsirou, N. Tsuji, Y. Uchiyama, C. van Eldik, J. Veh, C. Venter, S. J. Wagner, R. White, A. Wierzcholska, Yu Wun Wong, M. Zacharias, D. Zargaryan, A. A. Zdziarski, S. Zouari, N. Żywucka, M. Meyer
Figure caption: Best-fit spectra assuming a point-source model in addition to the halo flux templates for a combined LAT and H.E.S.S. analysis. An activity time of ﹩{t}_{\max }={10}^{7}\,﹩ yr is assumed for all sources. The columns show different field strengths B ∈ [10−16, 10−15, 10−14] G, and each source is shown in one row. A coherence length of 1 Mpc is assumed throughout, together with the EBL model of Domínguez et al. (2011). Blue and red markers and lines show the point-source spectra measured with the LAT and H.E.S.S., respectively.
Paper: Constraints on the Intergalactic Magnetic Field Using Fermi-LAT and H.E.S.S. Blazar Observations
Authors: F. Aharonian, J. Aschersleben, M. Backes, V. Barbosa Martins, R. Batzofin, Y. Becherini, D. Berge, B. Bi, M. Bouyahiaoui, M. Breuhaus, R. Brose, F. Brun, B. Bruno, T. Bulik, C. Burger-Scheidlin, T. Bylund, S. Caroff, S. Casanova, J. Celic, M. Cerruti, T. Chand, S. Chandra, A. Chen, J. Chibueze, O. Chibueze, G. Cotter, M. de Bony, K. Egberts, J.-P. Ernenwein, G. Fichet de Clairfontaine, M. Filipovic, G. Fontaine, M. Füssling, S. Funk, S. Gabici, S. Ghafourizadeh, G. Giavitto, D. Glawion, J. F. Glicenstein, P. Goswami, M.-H. Grondin, L. Haerer, T. L. Holch, M. Holler, D. Horns, M. Jamrozy, F. Jankowsky, V. Joshi, I. Jung-Richardt, E. Kasai, K. Katarzyński, R. Khatoon, B. Khélifi, W. Kluźniak, Nu. Komin, K. Kosack, D. Kostunin, R. G. Lang, S. Le Stum, F. Leitl, A. Lemière, J.-P. Lenain, F. Leuschner, T. Lohse, A. Luashvili, I. Lypova, J. Mackey, D. Malyshev, D. Malyshev, V. Marandon, P. Marchegiani, A. Marcowith, G. Martí-Devesa, R. Marx, M. Meyer, A. Mitchell, R. Moderski, L. Mohrmann, A. Montanari, E. Moulin, J. Muller, T. Murach, K. Nakashima, J. Niemiec, S. Ohm, L. Olivera-Nieto, E. de Ona Wilhelmi, S. Panny, M. Panter, R. D. Parsons, G. Peron, D. A. Prokhorov, H. Prokoph, G. Pühlhofer, M. Punch, A. Quirrenbach, P. Reichherzer, A. Reimer, O. Reimer, B. Reville, F. Rieger, G. Rowell, B. Rudak, E. Ruiz-Velasco, V. Sahakian, D. A. Sanchez, M. Sasaki, F. Schüssler, H. M. Schutte, U. Schwanke, J. N. S. Shapopi, H. Sol, S. Spencer, S. Steinmassl, H. Suzuki, T. Takahashi, T. Tanaka, A. M. Taylor, R. Terrier, C. Thorpe-Morgan, M. Tsirou, N. Tsuji, Y. Uchiyama, C. van Eldik, J. Veh, C. Venter, S. J. Wagner, R. White, A. Wierzcholska, Yu Wun Wong, M. Zacharias, D. Zargaryan, A. A. Zdziarski, S. Zouari, N. Żywucka, M. Meyer
Figure caption: The IGMF parameter space probed with gamma-ray instruments. Lower limits at 95% confidence level on the IGMF derived from the combined Fermi-LAT and H.E.S.S. analysis for different assumed blazar activity times are shown as orange filled and hatched regions. A scaling of the limits with the coherence length as ﹩{{\ell }}_{B}^{-1/2}﹩ is assumed. Exclusion regions from H.E.S.S., MAGIC, and VERITAS are shown as gray filled regions (Aleksić et al. 2010; H.E.S.S. Collaboration et al. 2014; Archambault et al. 2017). The CTA could exclude field strengths below the dashed gray line (Abdalla et al. 2021). The dark-gray line shows combined Fermi-LAT and IACT lower limits for ﹩{t}_{\max }=10\,﹩ yr (Ackermann et al. 2018). Light-gray shaded regions are disfavored by theory. Blue lines and regions indicate theoretically favored regions for the generation of the IGMF during either electro-weak phase transitions (EWPT) or QCD phase transitions (QCDPT), by Galactic winds or induced by cosmic-ray (CR) streaming (see Durrer & Neronov 2013, and references therein).
Paper: Constraints on the Intergalactic Magnetic Field Using Fermi-LAT and H.E.S.S. Blazar Observations
Authors: F. Aharonian, J. Aschersleben, M. Backes, V. Barbosa Martins, R. Batzofin, Y. Becherini, D. Berge, B. Bi, M. Bouyahiaoui, M. Breuhaus, R. Brose, F. Brun, B. Bruno, T. Bulik, C. Burger-Scheidlin, T. Bylund, S. Caroff, S. Casanova, J. Celic, M. Cerruti, T. Chand, S. Chandra, A. Chen, J. Chibueze, O. Chibueze, G. Cotter, M. de Bony, K. Egberts, J.-P. Ernenwein, G. Fichet de Clairfontaine, M. Filipovic, G. Fontaine, M. Füssling, S. Funk, S. Gabici, S. Ghafourizadeh, G. Giavitto, D. Glawion, J. F. Glicenstein, P. Goswami, M.-H. Grondin, L. Haerer, T. L. Holch, M. Holler, D. Horns, M. Jamrozy, F. Jankowsky, V. Joshi, I. Jung-Richardt, E. Kasai, K. Katarzyński, R. Khatoon, B. Khélifi, W. Kluźniak, Nu. Komin, K. Kosack, D. Kostunin, R. G. Lang, S. Le Stum, F. Leitl, A. Lemière, J.-P. Lenain, F. Leuschner, T. Lohse, A. Luashvili, I. Lypova, J. Mackey, D. Malyshev, D. Malyshev, V. Marandon, P. Marchegiani, A. Marcowith, G. Martí-Devesa, R. Marx, M. Meyer, A. Mitchell, R. Moderski, L. Mohrmann, A. Montanari, E. Moulin, J. Muller, T. Murach, K. Nakashima, J. Niemiec, S. Ohm, L. Olivera-Nieto, E. de Ona Wilhelmi, S. Panny, M. Panter, R. D. Parsons, G. Peron, D. A. Prokhorov, H. Prokoph, G. Pühlhofer, M. Punch, A. Quirrenbach, P. Reichherzer, A. Reimer, O. Reimer, B. Reville, F. Rieger, G. Rowell, B. Rudak, E. Ruiz-Velasco, V. Sahakian, D. A. Sanchez, M. Sasaki, F. Schüssler, H. M. Schutte, U. Schwanke, J. N. S. Shapopi, H. Sol, S. Spencer, S. Steinmassl, H. Suzuki, T. Takahashi, T. Tanaka, A. M. Taylor, R. Terrier, C. Thorpe-Morgan, M. Tsirou, N. Tsuji, Y. Uchiyama, C. van Eldik, J. Veh, C. Venter, S. J. Wagner, R. White, A. Wierzcholska, Yu Wun Wong, M. Zacharias, D. Zargaryan, A. A. Zdziarski, S. Zouari, N. Żywucka, M. Meyer
Figure caption: Observed LAT and H.E.S.S. spectra of 1ES 0229+200 (blue and red markers and lines, respectively), together with the total best-fit spectrum (orange solid band, including uncertainties) for a point-source model of the primary gamma-ray flux (dashed orange line) and the halo flux (dashed–dotted orange line). Spectral points are shown as upper limits if the detection significance is below 2σ. The same values for t max and B are assumed as in Figure 2.