adsabs/AstroCLIMB huggingface dataset:
Paper: Analysis of the Intranight Variability of BL Lacertae during Its 2020 August Flare 
Authors: A. Agarwal, B. Mihov, V. Agrawal, S. Zola, Aykut Özdönmez, Ergün Ege, L. Slavcheva-Mihova, D. E. Reichart, D. B. Caton, Avik Kumar Das
Figure caption: LCs in BVRI bands from 2020 July 11 to September 14. The LCs are ordered as indicated in the top panel; RI-band LCs are shifted by the corresponding offsets for display purposes. The blue dashed lines are the fits used to determine the shape of the smooth component for the corresponding nights—see Section 4.2 for the description of the BRI-band LCs around JD = 2,459,088 and of the R-band LC around JD = 2,459,104.
Paper: Analysis of the Intranight Variability of BL Lacertae during Its 2020 August Flare 
Authors: A. Agarwal, B. Mihov, V. Agrawal, S. Zola, Aykut Özdönmez, Ergün Ege, L. Slavcheva-Mihova, D. E. Reichart, D. B. Caton, Avik Kumar Das
Figure caption: Optical (R band; red circles) and the “quick-look” γ-ray (0.1–300 GeV band; black stepped curve) LCs from 2020 July 11 to September 14. The R-band flux is in units of millijansky, while the γ-ray flux is in units of 10−7 photons s−1 cm−2.
Paper: Analysis of the Intranight Variability of BL Lacertae during Its 2020 August Flare 
Authors: A. Agarwal, B. Mihov, V. Agrawal, S. Zola, Aykut Özdönmez, Ergün Ege, L. Slavcheva-Mihova, D. E. Reichart, D. B. Caton, Avik Kumar Das
Figure caption: Combined BVRI-band LCs for the nights of intranight flaring activity. In each plot, the LCs are ordered from bottom to top as follows: B band—blue; V band—green; R band—red; I band—magenta. The (V)RI-band LCs are shifted for display purposes downward by the corresponding offsets indicated in the plots. The (composite) fitting functions, used to detrend the corresponding LCs, are overplotted (black solid lines); the alternative fitting functions are plotted as black dashed lines (see text). For the sake of clarity, (i) if a few data points are available for a given band, then its LC is not shown, and (ii) only the portion of the LC used in the decomposition is shown.
Paper: Analysis of the Intranight Variability of BL Lacertae during Its 2020 August Flare 
Authors: A. Agarwal, B. Mihov, V. Agrawal, S. Zola, Aykut Özdönmez, Ergün Ege, L. Slavcheva-Mihova, D. E. Reichart, D. B. Caton, Avik Kumar Das
Figure caption: Dependence of the spectral index on the R-band flux. The blue circles are the spectral indices calculated using the VRI bands, while the red squares are the spectral indices calculated using the BVRI ones. The error bars reflect the variability amplitude in the cases when the intranight monitoring data are included in the spectral index calculation (see text).
Paper: Analysis of the Intranight Variability of BL Lacertae during Its 2020 August Flare 
Authors: A. Agarwal, B. Mihov, V. Agrawal, S. Zola, Aykut Özdönmez, Ergün Ege, L. Slavcheva-Mihova, D. E. Reichart, D. B. Caton, Avik Kumar Das
Figure caption: WWZ of the nightly binned and cut R-band LC (see text). Left panel: the colored WWZ power in the time–period plane. Right panel: the time-averaged WWZ power as a function of the period. The colored dashed curves represent the corresponding local significance contours.
Paper: Analysis of the Intranight Variability of BL Lacertae during Its 2020 August Flare 
Authors: A. Agarwal, B. Mihov, V. Agrawal, S. Zola, Aykut Özdönmez, Ergün Ege, L. Slavcheva-Mihova, D. E. Reichart, D. B. Caton, Avik Kumar Das
Figure caption: SED for the individual nights. Note the scatter in the B-band fluxes (see text).
Paper: Analysis of the Intranight Variability of BL Lacertae during Its 2020 August Flare 
Authors: A. Agarwal, B. Mihov, V. Agrawal, S. Zola, Aykut Özdönmez, Ergün Ege, L. Slavcheva-Mihova, D. E. Reichart, D. B. Caton, Avik Kumar Das
Figure caption: SFs built using the corrected LCs. For MWL LCs, only R-band (or I-band) SFs are shown. The SPL function fits are overplotted with a red line.
Paper: Analysis of the Intranight Variability of BL Lacertae during Its 2020 August Flare 
Authors: A. Agarwal, B. Mihov, V. Agrawal, S. Zola, Aykut Özdönmez, Ergün Ege, L. Slavcheva-Mihova, D. E. Reichart, D. B. Caton, Avik Kumar Das
Figure caption: CMDs built using the noncorrected LCs that show INV. The fitted power-law models are overplotted.
Paper: Analysis of the Intranight Variability of BL Lacertae during Its 2020 August Flare 
Authors: A. Agarwal, B. Mihov, V. Agrawal, S. Zola, Aykut Özdönmez, Ergün Ege, L. Slavcheva-Mihova, D. E. Reichart, D. B. Caton, Avik Kumar Das
Figure caption: Time lag of the BVI-band variations (with respect to the R-band ones) against the frequency of the corresponding bands (squares). The black solid curve is fit for this frequency dependence. The black plus signs mark the randomized lag values, while the green lines are the fits to each set of randomized time lags (see text). We show the 3σ error bars for the sake of comparison with the randomized lag values.
Paper: Analysis of the Intranight Variability of BL Lacertae during Its 2020 August Flare 
Authors: A. Agarwal, B. Mihov, V. Agrawal, S. Zola, Aykut Özdönmez, Ergün Ege, L. Slavcheva-Mihova, D. E. Reichart, D. B. Caton, Avik Kumar Das
Figure caption: Comparison of the timescales obtained after the decomposition of the LCs detrended using two alternative fitting functions. The symbols denote the bands as follows: B—blue diamonds; V—green triangles; R—red circles; I—magenta squares. The timescales along the x-axis are those adopted by us for the further analysis. The dotted line is the line of exact correspondence. The solid line is the line corresponding to the clipped mean difference between the timescales of 1.4 minutes.
Paper: Analysis of the Intranight Variability of BL Lacertae during Its 2020 August Flare 
Authors: A. Agarwal, B. Mihov, V. Agrawal, S. Zola, Aykut Özdönmez, Ergün Ege, L. Slavcheva-Mihova, D. E. Reichart, D. B. Caton, Avik Kumar Das
Figure caption: Results from the cross-correlation analysis of the corrected MWL LCs. In each plot the left panel shows the DCF (black lines) and its uncertainties (green shaded area). The red solid and dashed lines indicate the significance levels of 99% and 95%, respectively, while the red dotted line indicates the zero correlation. The right panel in each plot shows the corresponding CCCD.
Paper: Analysis of the Intranight Variability of BL Lacertae during Its 2020 August Flare 
Authors: A. Agarwal, B. Mihov, V. Agrawal, S. Zola, Aykut Özdönmez, Ergün Ege, L. Slavcheva-Mihova, D. E. Reichart, D. B. Caton, Avik Kumar Das
Figure caption: Same as Figure 11, but for the R-band-only LCs.
Paper: Analysis of the Intranight Variability of BL Lacertae during Its 2020 August Flare 
Authors: A. Agarwal, B. Mihov, V. Agrawal, S. Zola, Aykut Özdönmez, Ergün Ege, L. Slavcheva-Mihova, D. E. Reichart, D. B. Caton, Avik Kumar Das
Figure caption: Plot of the I-band decay timescales against the B-band (blue diamonds) and R-band (red circles) ones. The dotted line is the line of exact correspondence.
Paper: Analysis of the Intranight Variability of BL Lacertae during Its 2020 August Flare 
Authors: A. Agarwal, B. Mihov, V. Agrawal, S. Zola, Aykut Özdönmez, Ergün Ege, L. Slavcheva-Mihova, D. E. Reichart, D. B. Caton, Avik Kumar Das
Figure caption: Distribution of the decay timescales jointly for all bands.
Paper: Analysis of the Intranight Variability of BL Lacertae during Its 2020 August Flare 
Authors: A. Agarwal, B. Mihov, V. Agrawal, S. Zola, Aykut Özdönmez, Ergün Ege, L. Slavcheva-Mihova, D. E. Reichart, D. B. Caton, Avik Kumar Das
Figure caption: Distribution of the flare durations jointly for all bands.
Paper: Analysis of the Intranight Variability of BL Lacertae during Its 2020 August Flare 
Authors: A. Agarwal, B. Mihov, V. Agrawal, S. Zola, Aykut Özdönmez, Ergün Ege, L. Slavcheva-Mihova, D. E. Reichart, D. B. Caton, Avik Kumar Das
Figure caption: Distribution of the minimal magnetic field strengths.
Paper: Analysis of the Intranight Variability of BL Lacertae during Its 2020 August Flare 
Authors: A. Agarwal, B. Mihov, V. Agrawal, S. Zola, Aykut Özdönmez, Ergün Ege, L. Slavcheva-Mihova, D. E. Reichart, D. B. Caton, Avik Kumar Das
Figure caption: Distribution of the maximal electron Lorentz factors.
Paper: Analysis of the Intranight Variability of BL Lacertae during Its 2020 August Flare 
Authors: A. Agarwal, B. Mihov, V. Agrawal, S. Zola, Aykut Özdönmez, Ergün Ege, L. Slavcheva-Mihova, D. E. Reichart, D. B. Caton, Avik Kumar Das
Figure caption: Decomposition of the corrected MWL LCs. In each plot, we indicate the evening date, the value of t 0, the bands plotted, and the corresponding offsets used for display purposes. The bands are coded as follows: B—blue; V—green; R—red; I—magenta. The blue dashed lines are the individual flares to which the LC is decomposed, while the black solid line is the model LC. The error bars are not shown for the sake of clarity.
Paper: Analysis of the Intranight Variability of BL Lacertae during Its 2020 August Flare 
Authors: A. Agarwal, B. Mihov, V. Agrawal, S. Zola, Aykut Özdönmez, Ergün Ege, L. Slavcheva-Mihova, D. E. Reichart, D. B. Caton, Avik Kumar Das
Figure caption: Distribution of the maximal radii.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: An example of a hard X-ray-to-radio SED and best-fitting models for a stage D merger, NGC 34 (ID01). Upper panel: observed wavelength vs. flux density. Lower panel: rest-frame frequency vs. luminosity. The bottom panels show the residuals in the UV-to-radio bands. The individual curves show the SED models of nonthermal radio emission (pink dashed), attenuated stellar emission (blue dashed–dotted), nebular emission (gray), dust emission (red), AGN torus (green), escaped AGN disk (cyan), polar dust (orange), absorption-corrected AGN X-ray emission (blue dotted), the X-ray emission from AGN scattering and X-ray binaries (light green), and X-ray thermal emission (light purple). Purple and red circles represent the observed and model flux densities, respectively. Red crosses in the X-ray band denote the NuSTAR spectra analyzed by Yamada et al. (2021). The results for all targets are given in Figure E1–E10.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: Left panel: histogram of the fraction of sources that show some signature of the presence of polar dust emission for AGNs with a merger stage. Each signature derived from the high-resolution images (e.g., Asmus 2019) and interferometry (e.g., López-Gonzaga & Jaffe 2016; López-Gonzaga et al. 2016) in the mid-IR band (blue), and UV-to-IR SED decomposition with CLUMPY (black) and with SKIRTOR (red), are color coded. The green histograms illustrate the fraction of AGNs with one or more signs of polar dust emission (green). Right panel: Venn diagram of sources with/without signs of polar dust emission. The number of sources for the individual categories and merger stages are illustrated in parentheses.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: A schematic picture of the AGN structure assumed in the updated CLUMPY model. The central black circle and blue bar represent the SMBH and accretion disk, respectively. The brown circles show the clumps of torus, whose structure is constrained by the X-ray spectroscopy with XCLUMPY. The light-brown annular sector illustrates the polar dust. The green arrays mark torus-reflected emission. The blue thick (solid and dotted) arrays are the AGN disk emission, while the blue thin array is the escaped disk emission via the clump gaps. These emissions are attenuated by the polar dust, marked as dashed lines. The orange arrow shows the dust reradiation from the polar dust. The symbols “σ” and “i” mean the torus angular width and inclination angle, respectively.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: The differences in M *, SFR, L torus, L polar, and L AGN,int derived from the UV-to-IR SED analysis by using the combined photometry of the total system and separated photometry of the individual galaxies for 13 resolved pairs. The diamonds and the uncertainties denote the averaged values and 1σ dispersions, respectively.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: Histogram of ΔBIC (= BICwoAGN − BICwAGN) for the 72 individual targets in our sample. The black solid line shows the threshold of ΔBIC = 6 as the significant difference (posterior probability above 95%) in the two fits, i.e., with and without adding an AGN (torus and polar dust) component. The red histogram shows the number of hard X-ray-detected AGNs and three newly identified AGN candidates. The blue histogram is the number of other sources, i.e., starburst-dominant sources or hard X-ray-undetected sources.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: Left panel: averaged values of logarithmic M * compared with the different merger stages. Right panel: averaged values of logarithmic SFR compared with the merger stages.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: Histogram of the reduced χ 2 derived from the UV-to-IR SED decomposition for the 72 individual targets in our sample.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: Left panel: logarithmic stellar mass in M ⊙ vs. logarithmic SFR in M ⊙ yr−1. The blue circles, green triangles, orange diamonds, red stars, and purple triangles represent the sources in stages A, B (early mergers), C, D (late mergers), and N (nonmergers) U/LIRGs, respectively. The gray diamonds illustrate the PG QSOs at z < 0.1, whose SFRs are estimated by UV-to-IR SED decomposition (Lyu et al. 2017). The black dotted curve and cyan area denote the MS and 1σ uncertain reported by Speagle et al. (2014), while the dashed solid curve and shading represent those reported by Saintonge et al. (2016). The green dotted line is the MS among z < 0.1 SDSS galaxies (Elbaz et al. 2007). Right panel: the same as the left but for sources classified as AGNs in U/LIRGs (red stars), starburst-dominant or hard X-ray–nondetected sources in U/LIRGs (gray circles), and PG QSOs (gray diamonds).
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: Rest-frame 6 μm luminosity contributed from AGNs vs. unabsorbed (absorption-corrected) rest-frame 2–10 keV luminosity for AGNs in various IR-luminous galaxies. The cyan triangle indicates an ELIRG at z ∼ 2 (Toba et al. 2021b). The yellow circles represent WISSH quasars at z ∼ 2–4 (Martocchia et al. 2017; Zappacosta et al. 2020). The pink circles indicate mid-IR-luminous quasars at z ∼ 1–3 in the GOODS–Herschel fields (Del Moro et al. 2016) while the pink diamonds show extremely red quasars at z ∼ 2–3 (Goulding et al. 2018b). The pink and red squares mark BL DOGs at z ∼ 1 (Zou et al. 2020) and IR-bright/hot DOGs at z ∼ 1–3 (Ricci et al. 2017a; Vito et al. 2018; Zappacosta et al. 2018; Toba et al. 2020b), respectively. Their colors (cyan, yellow, pink, and red) are largely categorized by the typical N H of these populations (see the text). The other symbols are the same as in Figure 8. The green dashed and blue dotted lines illustrate the linear relations using a sample drawn from the eROSITA Final Equatorial Depth Survey (Toba et al. 2022a) and the Bright Ultra-hard XMM-Newton Survey (Mateos et al. 2015), respectively. The black solid curve denotes the 2D polynomial relations from Stern (2015). The red dashed–dotted line and the pink shaded area are the best-fitting relation and its 1σ dispersion among stage C–D mergers and the high-z IR-luminous sources, respectively.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: Top panels: logarithmic SFR vs. α radio (left) and fraction of AGN luminosity in the IR band vs. α radio (right), excluding sources whose α radio is fixed at 0.5. Sources with f AGN = 0.0 mean U/LIRGs which do not have AGNs. The dashed line is the median low-frequency (<5 GHz) α radio among the U/LIRGs reported by Murphy (2013). Bottom panels: logarithmic SFR vs. q IR (left) and fraction of AGN luminosity in the IR band vs. q IR (right). The dashed line is the averaged value reported by Bell (2003), and the dotted gray line illustrates the threshold for radio-excess (q IR < 1.64) as a tracer of AGNs (Yun et al. 2001; U et al. 2012). The large symbols are the same as in Figure 8, while small crosses denote sources where α radio = 0.5 is assumed in the radio fitting.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: Top panel: rest-frame wavelength vs. flux density normalized to the K s band. Bottom panel: rest-frame frequency vs. luminosity normalized to the K s band. The dotted green curve shows the averaged SEDs for sources whose X-ray spectra above ≳1 keV are not obtained in stage A–B (early) mergers. The solid curves represent the averaged SEDs for the hard X-ray-detected AGNs in stage A–B (early mergers; blue) and stage C–D (late mergers; red). The dashed curves are the same as those used for the soft X-ray-detected galaxies among the starburst-dominant or hard X-ray-nondetected sources. The values in parentheses show the number of sources. These SED templates are available in Table 5.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: Top panel: rest-frame wavelength vs. flux density normalized to the K s band for the hard X-ray-detected AGNs. Bottom panel: the same but for the soft X-ray-detected galaxies among the starburst-dominant and hard X-ray-nondetected sources. The solid curves represent the averaged SEDs for the sources in stage A (blue), stage B (green), stage C (orange), stage D (red), and stage N (purple) U/LIRGs. The values in parentheses show the number of sources. The light-colored curves show the SEDs for individual sources.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: WISE color–color diagram. AGN selection wedges are illustrated as the areas within the dotted gray (Jarrett et al. 2011), dashed–dotted gray (Mateos et al. 2012), and black dashed (Blecha et al. 2018) boxes, and the pink shaded area presented in this work. The large symbols are the same as in Figure 8, while the small circles illustrate sources where f AGN = 0.0 (starburst-dominant or hard X-ray-nondetected sources).
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: Left panel: logarithmic SFR vs. logarithmic radio luminosity at 1.4 GHz. The black dashed line is obtained by the empirical radio-far-IR relation in star-forming galaxies in Kennicutt (1998), assuming a Chabrier IMF (see Bonzini et al. 2015). Right panel: fraction of AGN luminosity in the IR band (f AGN) vs. radio-excess parameter (q excess). The sources with f AGN = 0.0 mean U/LIRGs which do not have AGNs. The black solid curve shows the threshold of radio-excess sources at z ≈ 0.0 (Delvecchio et al. 2017). The symbols are the same as in Figure 9.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: Enlarged picture of the IR (1–600 μm) wavelength of the left panel in Figure 14 (rest-frame wavelength vs. flux density normalized to the K s band). The stars and squares mark the photometry of WISE and other IR instruments (2MASS, AKARI, and Herschel) for the AGN in IRAS F08572+3915.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: WISE W1 – W2 color as a function of SFR (left) and the fraction of AGN luminosity in the IR band (right). The dashed lines illustrate the W1 − W2 > 0.5 threshold (Satyapal et al. 2014).