adsabs/AstroCLIMB huggingface dataset:
Paper: The Radio Halo in PLCKESZ G171.94–40.65: Beacon of Merging Activity
Authors: R. Santra, R. Kale, S. Giacintucci, D. R. Wik, T. Venturi, D. Dallacasa, R. Cassano, G. Brunetti, D. C. Joshi
Figure caption: The radial profile of the radio surface brightness is shown. Each of the circles (different colors at different frequencies) denotes the azimuthally averaged radio surface brightness values, within the annular regions. The error bars represent the error on the mean. The dashed line shows the two-dimensional model fitted to the radio surface brightness profile.
Paper: The Radio Halo in PLCKESZ G171.94–40.65: Beacon of Merging Activity
Authors: R. Santra, R. Kale, S. Giacintucci, D. R. Wik, T. Venturi, D. Dallacasa, R. Cassano, G. Brunetti, D. C. Joshi
Figure caption: A Chandra image (in color) of PLCK171 in the 0.5−4.0 keV band is shown, smoothed with a Gaussian FWHM of 5″. The X-ray image is background-subtracted, divided by the exposure map, and the point source removed. The radio emission at 400 MHz is overlaid as yellow contours. The contours level starts from 3σ rms×[1, 2, 4..], where σ rms = 60 μJy beam−1.
Paper: Spatially Resolved Comparison of SFRs from UV and Hα in GASP Gas-stripped Galaxies
Authors: Neven Tomičić, Ariel Werle, Benedetta Vulcani, Alessandro Ignesti, Alessia Moretti, Anna Wolter, Koshy George, Bianca M. Poggianti, Marco Gullieuszik
Figure caption: The Monte Carlo simulation of a scatter in ΔSFR values due to variation in the SFR prescriptions and assumption of attenuation curve for UV tracer (see Equation (5)). The presented cases are where the following parameters are varying: (1) both η and A UV (left-hand panel), (2) only η parameters and the 0.44 x CCM curve (J. A. Cardelli et al. 1989) for UV is assumed (middle panel), and (3) the η parameters are set and the attenuation curve for UV varies between 0.44 x CCM and 1 x CCM (right-hand panel). We show median value with the 25th and 85th percentile (horizontal lines) for the disk (circles) and tails (triangles), dense-gas (blue colors) and DIG (red and orange colors) dominated spaxels in JO201, JO60, JW100, JW39, and JO194 (from top to bottom of point clusters).
Paper: Spatially Resolved Comparison of SFRs from UV and Hα in GASP Gas-stripped Galaxies
Authors: Neven Tomičić, Ariel Werle, Benedetta Vulcani, Alessandro Ignesti, Alessia Moretti, Anna Wolter, Koshy George, Bianca M. Poggianti, Marco Gullieuszik
Figure caption: Distribution of the number of spaxels characterized by a different ﹩{\rm{\Delta }}\mathrm{log}[{\rm{O}}{\rm{I}}]/{\rm{H}}\alpha ﹩ in the galaxy regions, characterized by Hα only, and Hα + FUV. The number of spaxels is on the y-axis, normalized by pixel numbers. Hα-only areas are presented with filled orange histograms, Hα + FUV areas in the disks (tails) with empty histograms with blue (red) edges, respectively. ﹩{\rm{\Delta }}\mathrm{log}[{\rm{O}}{\rm{I}}]/{\rm{H}}\alpha ﹩ value is defined as an offset in ﹩{\mathrm{log}}_{10}[{\rm{O}}{\rm{I}}]/{\rm{H}}\alpha ﹩ from the star-forming line in the BPT-[O I] diagram by N. Tomičić et al. (2021a). Positive and negative ﹩{\rm{\Delta }}\mathrm{log}[{\rm{O}}{\rm{I}}]/{\rm{H}}\alpha ﹩ values indicate that the gas was predominantly ionized by the SF and non-SF processes, respectively. In the panels, we also list the number of pixels in those areas. The black vertical line indicates value ﹩{\mathrm{log}}_{10}[{\rm{O}}{\rm\small{I}}]/{\rm{H}}\alpha =0﹩ and separates SF from non-SF spaxels.
Paper: Spatially Resolved Comparison of SFRs from UV and Hα in GASP Gas-stripped Galaxies
Authors: Neven Tomičić, Ariel Werle, Benedetta Vulcani, Alessandro Ignesti, Alessia Moretti, Anna Wolter, Koshy George, Bianca M. Poggianti, Marco Gullieuszik
Figure caption: The model of SF and UV (blue dots) and Hα (red–orange–yellow lines) emission that it produces. The diagrams show the observed tracers (left-hand panel) and the measured ΔSFR (right-hand panel) as a function of time. The SFR of the model is constant at t<0 Myr, and stops at t = 0 Myr. We also added a separate Hα emission of DIG (as a percentage of the Hα emission from the SF process), which is not affected by the drop in SFR, to mimic the existence of DIG that might not be fully ionized by SF process. We show a different intensity of DIG, from 0% up to 70% of Hα from the SF process, as Hα lines with a different shade of red color in the figure.
Paper: Spatially Resolved Comparison of SFRs from UV and Hα in GASP Gas-stripped Galaxies
Authors: Neven Tomičić, Ariel Werle, Benedetta Vulcani, Alessandro Ignesti, Alessia Moretti, Anna Wolter, Koshy George, Bianca M. Poggianti, Marco Gullieuszik
Figure caption:                       ﹩{\rm{\Delta }}\mathrm{SFR}={\mathrm{log}}_{10}\mathrm{SFR}(\mathrm{FUV})-{\mathrm{log}}_{10}\mathrm{SFR}({\rm{H}}\alpha )﹩ for pixel-by-pixel values (y-axis) as a function of galactocentric distance (left-hand and center panels, x-axis). We present data for the disks (tails) in the left-hand(center) panels, respectively. The histogram of the ΔSFR (normalized units) is in the right-hand panels. We define the dense-gas-dominated pixels with C DIG < = 0.5 (dark blue for disks, and light blue for tails) and the DIG-dominated pixels with C DIG > = 0.7 (red for disks and orange for tails). The UV attenuation values are estimated as 0.44 of the extinction values using the J. A. Cardelli et al. (1989) extinction curve (CCM).
Paper: Spatially Resolved Comparison of SFRs from UV and Hα in GASP Gas-stripped Galaxies
Authors: Neven Tomičić, Ariel Werle, Benedetta Vulcani, Alessandro Ignesti, Alessia Moretti, Anna Wolter, Koshy George, Bianca M. Poggianti, Marco Gullieuszik
Figure caption: Empirically estimated SFR prescriptions η for FUV (first and second panels), NUV (third and fourth panels) and Hα (fifth panel), for the disks and the tails. We show pixel-by-pixel comparison as histograms (except the case for Hα), and integrated values as single data points. We also indicate the prescriptions from the literature (R. C. Kennicutt & N. J. Evans 2012) by the vertical, dashed line.
Paper: Spatially Resolved Comparison of SFRs from UV and Hα in GASP Gas-stripped Galaxies
Authors: Neven Tomičić, Ariel Werle, Benedetta Vulcani, Alessandro Ignesti, Alessia Moretti, Anna Wolter, Koshy George, Bianca M. Poggianti, Marco Gullieuszik
Figure caption: Coverage of the optical and UV tracers (FUV on top and NUV on bottom) for the galaxies. The SNR threshold used for the tracers is SNR > = 4.
Paper: Spatially Resolved Comparison of SFRs from UV and Hα in GASP Gas-stripped Galaxies
Authors: Neven Tomičić, Ariel Werle, Benedetta Vulcani, Alessandro Ignesti, Alessia Moretti, Anna Wolter, Koshy George, Bianca M. Poggianti, Marco Gullieuszik
Figure caption: Same as Figure 4 but for NUV tracer.
Paper: Spatially Resolved Comparison of SFRs from UV and Hα in GASP Gas-stripped Galaxies
Authors: Neven Tomičić, Ariel Werle, Benedetta Vulcani, Alessandro Ignesti, Alessia Moretti, Anna Wolter, Koshy George, Bianca M. Poggianti, Marco Gullieuszik
Figure caption: Same as Figure 1 for JW39 and JO194. In the case of these galaxies, we observed only FUV emission.
Paper: SAGAbg. II. The Low-mass Star-forming Sequence Evolves Significantly between 0.05 < z < 0.21
Authors: Erin Kado-Fong, Marla Geha, Yao-Yuan Mao, Mithi A. C. de los Reyes, Risa H. Wechsler, Benjamin Weiner, Yasmeen Asali, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Yunchong Wang
Figure caption: In each panel, we show the redshift evolution of the mean SFR at fixed stellar mass as inferred from SAGAbg-A. The bold curve shows our estimate of the mean SFR of a galaxy of the specified stellar mass given our power-law fit to the SFS as a function of redshift; the curve is solid in the redshift range where the average retrogressed galaxy remains above the nominal magnitude limit of the SAGA spectra, and becomes dashed for model predictions below this limit. In the left column, we show the SFS evolution at ﹩{\mathrm{log}}_{10}({M}_{\star }/{M}_{\odot })﹩ = 8.5 (bold curve with blue outlines); the right column shows the same for ﹩{\mathrm{log}}_{10}({M}_{\star }/{M}_{\odot })﹩ = 9.5 (bold curve with orange outlines). The shaded regions around the bold curve in each panel show the 16th to 84th percentile confidence interval on our estimate of the mean SFR(M ⋆). To account for differences in the absolute normalization of the SFS, we show the redshift evolution of the SFS relative to its mean value at z = 0.0175, as shown by the dotted gray vertical line. We compare the results from the SAGAbg-A sample to results from the observational literature (J. S. Speagle et al. 2014; S. K. Leslie et al. 2020; J. E. Thorne et al. 2021; J. Leja et al. 2022; P. Popesso et al. 2023) at top and the theoretical literature at bottom (P. Behroozi et al. 2019; R. Dave et al. 2019; D. Nelson et al. 2019; Y. Wang et al. 2024). Observational fits that we have extrapolated beyond the original work’s sample domain in stellar mass are shown as dashed curves; fits that are extrapolated in both stellar mass and redshift are shown as dotted curves.
Paper: SAGAbg. II. The Low-mass Star-forming Sequence Evolves Significantly between 0.05 < z < 0.21
Authors: Erin Kado-Fong, Marla Geha, Yao-Yuan Mao, Mithi A. C. de los Reyes, Risa H. Wechsler, Benjamin Weiner, Yasmeen Asali, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Yunchong Wang
Figure caption: A comparison between our model SFS (blue) and other results from the observational literature at matched redshift. Our best-fit SFS is shown as a dashed curve where the average retrogressed galaxy is expected to be m  r  > 21, the approximate spectroscopic targeting limit of SAGA. We show the best-fit intrinsic scatter of the SAGAbg-A SFS as a blue-shaded region; the parameter estimates of Equation (8) are given for the SAGAbg-A SFS in each panel. As a visual reference, we also show the z < 0.035 SFS fit for the SAGAbg-A in each panel as the dotted blue line. We also show fits from the observational literature (J. S. Speagle et al. 2014; L. J. M. Davies et al. 2016; C. Hahn et al. 2019; A. K. Leroy et al. 2019; S. K. Leslie et al. 2020; J. Leja et al. 2022; D. A. Dale et al. 2023). Extrapolated fits to SFS fits made at higher redshifts are shown by dotted–dashed curves, and SFS fits to only the z ≈ 0 Universe are shown as dashed curves. All other SFS comparisons are shown as solid curves.
Paper: SAGAbg. II. The Low-mass Star-forming Sequence Evolves Significantly between 0.05 < z < 0.21
Authors: Erin Kado-Fong, Marla Geha, Yao-Yuan Mao, Mithi A. C. de los Reyes, Risa H. Wechsler, Benjamin Weiner, Yasmeen Asali, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Yunchong Wang
Figure caption: A comparison between the SFS that we estimate for our reference sample (z < 0.035, blue solid line), the local SFSs of the Local Volume Legacy Survey (red, D. A. Dale et al. 2023), the z = 0 Multiwavelength Galaxy Survey (gray, A. K. Leroy et al. 2019), and the SAGA satellites (dashed blue line, M. Geha et al. 2024). The upper panel shows the distribution over the stellar mass of each sample. The main panel shows the best-fit SFS of each sample, as well as individual points of the SAGAbg-A sample at z < 0.035. The horizontal line shows our approximate SFR detection limit at z = 0.035. Each SFS is shown for the central 90% stellar mass range of its respective sample in the main panel. The bottom panel shows the logarithm of the ratio between each comparison SFS and the SFS derived from SAGAbg-A.
Paper: SAGAbg. II. The Low-mass Star-forming Sequence Evolves Significantly between 0.05 < z < 0.21
Authors: Erin Kado-Fong, Marla Geha, Yao-Yuan Mao, Mithi A. C. de los Reyes, Risa H. Wechsler, Benjamin Weiner, Yasmeen Asali, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Yunchong Wang
Figure caption: A comparison between the observable retrogressed model predictions (the expected distribution of our median posterior model estimate as would be observable after the SAGA Survey selection function, red contours) and observed SAGA background sample (purple scatter)as a function of redshift in the M ⋆–SFR plane. Here, we also show the SFS as measured from the LVL Survey by D. A. Dale et al. (2023; black line) as a comparison to the z = 0 SFS.
Paper: The Study of Jet Formation Mechanism in Fermi Blazars
Authors: Shangchun Xie, Zhihao Ouyang, Jingyu Wu, Hubing Xiao, Shaohua Zhang, Yongyun Chen, Zhijian Luo, Junhui Fan
Figure caption: The correlation between jet power and accretion rate. The red dots and line stand for the data points and corresponding linear regression of FSRQs; the blue dots and line stand for the data points and corresponding linear regression of BL Lacs. The solid black line represents the linear regression for all blazars in this diagram. The blue and red crosses are the standard deviation error for BL Lac and FSRQ, respectively.
Paper: SAGAbg. II. The Low-mass Star-forming Sequence Evolves Significantly between 0.05 < z < 0.21
Authors: Erin Kado-Fong, Marla Geha, Yao-Yuan Mao, Mithi A. C. de los Reyes, Risa H. Wechsler, Benjamin Weiner, Yasmeen Asali, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Yunchong Wang
Figure caption: Left: redshift vs. the physical change in average SFR for our fiducial model (red), an exponentially declining τ model (blue), and a constant SFH (brown). Our best-fit τ produces a relationship between SFR and lookback time that is statistically indistinguishable from our fiducial linear model. Right: for each model, we show the difference in the median stellar mass (top) and SFR (bottom) between the observed SAGAbg-A sample and observable retrogressed model prediction. We define ﹩{\rm{\Delta }}{\mathrm{log}}_{10}{ \mathcal X }﹩ to be ﹩{\rm{\Delta }}{\mathrm{log}}_{10}{ \mathcal X }\equiv {\mathrm{log}}_{10}{{ \mathcal X }}_{\mathrm{obs}}-{\mathrm{log}}_{10}{{ \mathcal X }}_{\mathrm{model}}﹩ for some observed property ﹩{ \mathcal X }﹩ of the galaxy sample. For our nonfiducial models, we underlay the fiducial model performance as unfilled red error bars.
Paper: SAGAbg. II. The Low-mass Star-forming Sequence Evolves Significantly between 0.05 < z < 0.21
Authors: Erin Kado-Fong, Marla Geha, Yao-Yuan Mao, Mithi A. C. de los Reyes, Risa H. Wechsler, Benjamin Weiner, Yasmeen Asali, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Yunchong Wang
Figure caption: The distribution of the SAGAbg-A sample as a function of stellar mass and Hα-derived SFR. The clear evolution of the sample in the M ⋆–SFR space is a combination of the physical evolution of the galaxy population with redshift and redshift-dependent selection effects. We show the joint distribution in the main panel and the projected distribution over stellar mass and SFR at the top and right, respectively, in gray. In the main panel, we additionally show the median value of the sample as a function of redshift; Gaussian kernel density estimates of these projected distributions are shown at the top and at the right with the same colors. We note that the normalization of the kernel density estimates are chosen to maximize the visibility of the density estimate, and are not reflective of the number of galaxies in each redshift bin.
Paper: SAGAbg. II. The Low-mass Star-forming Sequence Evolves Significantly between 0.05 < z < 0.21
Authors: Erin Kado-Fong, Marla Geha, Yao-Yuan Mao, Mithi A. C. de los Reyes, Risa H. Wechsler, Benjamin Weiner, Yasmeen Asali, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Yunchong Wang
Figure caption: The SAGAbg-A SFS in the same redshift bins considered in Figure 4 without imposing our observability criteria. The retrogressed sample is shown in gray, while the best-fit power law and running median are shown in blue (where the error bars indicate the 16th and 84th percentiles). The best-fit parameters of Equation (8) are again given for each redshift bin.
Paper: Long-term Study of the 2020 Magnetar-like Outburst of the Young Pulsar PSR J1846-0258 in Kes 75
Authors: R. Sathyaprakash, N. Rea, F. Coti Zelati, A. Borghese, M. Pilia, M. Trudu, M. Burgay, R. Turolla, S. Zane, P. Esposito, S. Mereghetti, S. Campana, D. Götz, A. Y. Ibrahim, G. L. Israel, A. Possenti, A. Tiengo
Figure caption: Top panel: evolution of the pulsed flux (in the 1–12 keV energy range) covering the periods before (left blue-shaded region), during (red-shaded region), and after (right green-shaded region) the 2020 August outburst of PSR J1846−0258. The solid black line denotes the epoch when the Swift Burst Alert Telescope (BAT) and Fermi Gamma-ray Burst Monitor (GBM) both confirmed the detection of a short (<100 ms) burst from the source, while the dashed black line indicates a slightly earlier period during which a spin-up glitch/irregularity was found to occur with respect to the pre-outburst spin evolution. The pulsed flux was computed using phase-resolved spectroscopy after deriving the spin parameters ν and ﹩\dot{\nu }﹩ via the tempo-derived phase-coherent timing approach (see Section 3.1) and Gaussian process regression (GPR; see Section 3.2). Middle panel: evolution in the spin frequency relative to the pre-outburst timing solution (i.e., before MJD 59,026) Δν derived from computing the derivative of the best-fit Gaussian process model to the timing residuals. Bottom panel: evolution in the frequency derivative ﹩\dot{\nu }﹩. For all three panels, the errors are quoted at the 1σ confidence level.
Paper: Long-term Study of the 2020 Magnetar-like Outburst of the Young Pulsar PSR J1846-0258 in Kes 75
Authors: R. Sathyaprakash, N. Rea, F. Coti Zelati, A. Borghese, M. Pilia, M. Trudu, M. Burgay, R. Turolla, S. Zane, P. Esposito, S. Mereghetti, S. Campana, D. Götz, A. Y. Ibrahim, G. L. Israel, A. Possenti, A. Tiengo
Figure caption: Comparison between the values of the spin frequency Δν (relative to the pre-outburst timing model; left) and the spin-down rate ﹩\dot{\nu }﹩ (right) obtained in our study through phase-coherent timing (black points) and Gaussian process regression (GPR). We also show the values reported by C.-P. Hu et al. (2023, solid blue line).(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Long-term Study of the 2020 Magnetar-like Outburst of the Young Pulsar PSR J1846-0258 in Kes 75
Authors: R. Sathyaprakash, N. Rea, F. Coti Zelati, A. Borghese, M. Pilia, M. Trudu, M. Burgay, R. Turolla, S. Zane, P. Esposito, S. Mereghetti, S. Campana, D. Götz, A. Y. Ibrahim, G. L. Israel, A. Possenti, A. Tiengo
Figure caption: Energy-resolved pulse profiles from the three post-outburst XMM-Newton observations, with the red solid line displaying the best-fit sinusoidal model (with at most two harmonic components). The number of phase bins for each profile was chosen based on the total number of counts available. Observational dates are indicated in the top panel of each plot.
Paper: Long-term Study of the 2020 Magnetar-like Outburst of the Young Pulsar PSR J1846-0258 in Kes 75
Authors: R. Sathyaprakash, N. Rea, F. Coti Zelati, A. Borghese, M. Pilia, M. Trudu, M. Burgay, R. Turolla, S. Zane, P. Esposito, S. Mereghetti, S. Campana, D. Götz, A. Y. Ibrahim, G. L. Israel, A. Possenti, A. Tiengo
Figure caption: Stacked NICER (blue), NuSTAR (magenta), and Swift (red) pulse profiles for the periods before (MJD 58,352–58,996), during (MJD 59,055–59,085, MJD 59,087–59,122, and MJD 59,125–59,171) and after (MJD 59,281–59,435) the 2020 outburst of PSR J1846–0258. The pulse profiles were combined over the observational epochs indicated at the top of each profile in the energy ranges of 1–12 keV (for NICER), 3–79 keV (for NuSTAR), and 1–10 keV for Swift.
Paper: Long-term Study of the 2020 Magnetar-like Outburst of the Young Pulsar PSR J1846-0258 in Kes 75
Authors: R. Sathyaprakash, N. Rea, F. Coti Zelati, A. Borghese, M. Pilia, M. Trudu, M. Burgay, R. Turolla, S. Zane, P. Esposito, S. Mereghetti, S. Campana, D. Götz, A. Y. Ibrahim, G. L. Israel, A. Possenti, A. Tiengo
Figure caption: The XMM-Newton EPIC-pn image of the field containing the high-B pulsar PSR J1846−0258, its PWN, and the spatially resolved SNR Kes 75. The circular black solid line indicates the extraction region used for the phase-resolved spectral analysis of the source.
Paper: Long-term Study of the 2020 Magnetar-like Outburst of the Young Pulsar PSR J1846-0258 in Kes 75
Authors: R. Sathyaprakash, N. Rea, F. Coti Zelati, A. Borghese, M. Pilia, M. Trudu, M. Burgay, R. Turolla, S. Zane, P. Esposito, S. Mereghetti, S. Campana, D. Götz, A. Y. Ibrahim, G. L. Israel, A. Possenti, A. Tiengo
Figure caption: Pulsed flux as a function of energy for the three post-outburst XMM-Newton observations.
Paper: KBSS-InCLOSE. I. Design and First Results from the Inner Circumgalactic Medium of QSO Line-of-sight Emitting Galaxies at z ∼ 2–3 
Authors: Evan Haze Nuñez, Charles C. Steidel, Evan N. Kirby, Gwen C. Rudie, Nikolaus Z. Prusinski, Yuguang Chen, Zhuyun Zhuang, Allison L. Strom, Dawn K. Erb, Max Pettini, Louise Welsh, David S. N. Rupke, Ryan J. Cooke
Figure caption: Rest-FUV and rest-optical images of the QSO sightlines. Left column:Keck/KCWI pseudobroadband (3500–5500 Å) images before and after (middle column) QSO subtraction; the images are on the same scale and stretch, showcasing the effectiveness of the subtraction (see Section 2.1.1). The gray contours in the postsubtracted images show constant Lyα surface brightness (vLyα  ∼ ±1000 km s−1; discussed in Section 4.1). Right column: HST images of the QSO sightlines. Objects at a similar redshift have the same color and are summarized in Section 2.1.4. Top row: The small red circle shows QSO Q2343, the large blue circle shows galaxy Q2343-G1, the Lyα contours show 0.35, 0.06, 0.01, 0.0012 ﹩\times {10}^{-17}\,\mathrm{erg}\,{{\rm{s}}}^{-1}\,{\mathrm{cm}}^{-2}\,{{\rm{arcsec}}}^{-2}﹩ for the galaxy, and the HST-IR/WFC3 F160W image shows all objects at higher resolution. Bottom row: The red circle shows QSO Q2233, the large orange circle shows galaxy Q2233-N1, the Lyα contours show 0.06, 0.04, 0.02, 0.002 ﹩\times {10}^{-17}\,\mathrm{erg}\,{{\rm{s}}}^{-1}\,{\mathrm{cm}}^{-2}\,{{\rm{arcsec}}}^{-2}﹩ for the galaxy, and the HST/WFPC2 F702W image shows all objects at higher resolution. Both galaxies lie at small impact parameter b ∼  20 kpc (see Table 2). More than 15 new galaxies were discovered from the KCWI cubes. N is up, and E is left.
Paper: Long-term Study of the 2020 Magnetar-like Outburst of the Young Pulsar PSR J1846-0258 in Kes 75
Authors: R. Sathyaprakash, N. Rea, F. Coti Zelati, A. Borghese, M. Pilia, M. Trudu, M. Burgay, R. Turolla, S. Zane, P. Esposito, S. Mereghetti, S. Campana, D. Götz, A. Y. Ibrahim, G. L. Israel, A. Possenti, A. Tiengo
Figure caption: Top panel: absorbed (N H = (5.5 ± 0.3) × 1022 cm−2) unfolded (deconvolved) pulsed energy spectra of PSR J1846−0258 in the aftermath of the 2020 outburst using NICER, NuSTAR, and XMM-Newton observations (see text). For display purposes, the NICER spectra were separated into seven groups, where in each group the spectra were stacked using the addspec tool (for the observation date ranges indicated in the legend). Similarly, the three XMM-Newton spectra were also combined. However, for spectral fitting we used the original spectra for each observation (see Table 1). Each spectrum was fit with an absorbed blackbody plus power-law model with the column density tied between the different observations. The results clearly demonstrate the gradual fading of the thermal component (below 10 keV) during the outburst, while the power-law component (above 8 keV) remains unchanged. The detailed best-fit parameters are reported in Table 1. The residuals of the best-fit model are also shown in the bottom panel of the figure.