adsabs/AstroCLIMB huggingface dataset:
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: Detection limits of ALMA, ngVLA, Chandra (0.5–6 keV), and Athena (0.5–10 keV). The ACIS and WFI are considered as the detectors of Chandra and Athena, respectively. The right X-ray-luminosity axis is adjusted to the left one by considering ﹩\nu {L}_{\nu ,\mathrm{mm}}^{\mathrm{peak}}/{L}_{14-150}\sim {10}^{-4.6}﹩, which was found for AGNs with ﹩{\alpha }_{\mathrm{mm}}-{\alpha }_{\mathrm{mm}}^{{\rm{e}}}\gt 0.3﹩, and L 2−10/L 14−150 = 0.55, where a typical cutoff power-law model is assumed (i.e., Γ = 1.8 and E cut = 200 keV). Sensitivities for the exposure of 1 hr are calculated at redshifts indicated as circles, and solid lines are shown to tie the data points. Likewise, for the exposure of 100 hr, dashed lines are drawn to indicate its limits, calculated at the same redshifts. For the ALMA and ngVLA observations, we consider 5σ detections. A poor sensitivity of ALMA at z ∼ 0.2–0.3, appearing as a flare, is because of severe atmospheric absorption. The limits of Chandra (black) and Athena (purple) are calculated so that ≈100 counts can be obtained to infer X-ray luminosities. For the calculation, we simulated X-ray spectra of an obscured cutoff power-law model with Γ = 1.8, E cut = 200 keV, and N H = 1024 cm−2. In addition, the case of N H = 1024.5 cm−2 for Athena is plotted at z > 1 by a dotted line.
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: Top: scatter plot for the mm-wave emission and the maximum energy carried by the X-ray outflow for the 14 AGNs for which the maximum energies were estimated in either Tombesi et al. (2012) or Gofford et al. (2015). An AGN with an upper limit is shown as a black circle, and the AGN NGC 4395 is located outside in the lower-left direction. A regression line is indicated by the black dashed line. Bottom: scatter plot for the mm-wave emission and the energy carried by the outflow traced with [O III] emission for 18 AGNs. The outflow data are from Rojas et al. (2020). No significant correlation is found, and due to this, the regression line is drawn in white.
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: Correlations between the mm-wave and 14–150 keV luminosities for type-1 AGN and type-2 AGN subsamples, indicated in orange and blue. Orange and blue dashed lines indicate regression lines obtained for the type-1 and type-2 subsamples, respectively. We mention the reason why a smaller intrinsic scatter (σ scat) is obtained for type-2 AGNs in spite of the apparently larger scatter of their data point. The intrinsic scatter is derived by subtracting the scatter due to uncertainties in data points, and as a large fraction of type-2 AGNs have large uncertainty in their luminosities as shown, a much smaller intrinsic scatter than the apparent one can be obtained.
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption:  Mm-wave and X-ray luminosities of the sources with ﹩\mathrm{log}{\lambda }_{\mathrm{Edd}}\lt -2﹩ and the predictions of the ADAF model of Pesce et al. (2021). Black points connected by a dotted line represent the cases with ﹩\mathrm{log}{\lambda }_{\mathrm{Edd}}=-3.25﹩ for different black hole masses of ﹩\mathrm{log}({M}_{\mathrm{BH}}/{M}_{\odot })=6.5,7.5,8.5﹩, and 9.5 (from lower to higher luminosities). In the same way, the orange and blue points accompanied by lines indicate the cases of ﹩\mathrm{log}{\lambda }_{\mathrm{Edd}}=-2.75﹩ and −2.25, respectively.
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: Top: theoretically expected mm-wave luminosity as a function of magnetic-field strength. Bottom: scatter plot of the mm-wave luminosity vs. the X-ray photon index for three subsamples divided by Eddington-ratio bins of ﹩\mathrm{log}{\lambda }_{\mathrm{Edd}}\geqslant -1.30﹩ (HEdd), ﹩-1.30\gt \mathrm{log}{\lambda }_{\mathrm{Edd}}\geqslant -1.85﹩ (MEdd), and ﹩\mathrm{log}{\lambda }_{\mathrm{Edd}}\lt -1.85﹩ (LEdd). No correlation is found for any of the subsamples.
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: Scatter plots of the spectral index for the 14–150 keV luminosity, the black hole mass, the bolometric luminosity, the Eddington ratio, the radio-to-mm-wave luminosity ratio, and the IR(host-galaxy)-to-mm-wave luminosity ratio. In each panel, a p-value (P cor) and a Pearson’s correlation coefficient (ρ P) are indicated within a box. No correlations are found.
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: Scatter plot of the index derived from ∼230 and 100 GHz data vs. that from 100 and 22 GHz data. The dashed line indicates the one-to-one relationship.
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: Scatter plot of the ratio between the mm-wave and host-galaxy IR luminosities vs. the excess 500 μm emission, whose values are taken from Shimizu et al. (2017). AGNs with upper limits are shown as a black circle.
Paper: BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100–200 pc
Authors: Taiki Kawamuro, Claudio Ricci, Masatoshi Imanishi, Richard F. Mushotzky, Takuma Izumi, Federica Ricci, Franz E. Bauer, Michael J. Koss, Benny Trakhtenbrot, Kohei Ichikawa, Alejandra F. Rojas, Krista Lynne Smith, Taro Shimizu, Kyuseok Oh, Jakob S. den Brok, Shunsuke Baba, Mislav Baloković, Chin-Shin Chang, Darshan Kakkad, Ryan W. Pfeifle, George C. Privon, Matthew J. Temple, Yoshihiro Ueda, Fiona Harrison, Meredith C. Powell, Daniel Stern, Meg Urry, David B. Sanders
Figure caption: Histogram of the logarithmic ratio between the peak mm-wave flux density and the one predicted by extrapolating the host-galaxy SED model. Sources with upper and lower limits are indicated in orange and gray, respectively.
Paper: Lepto-hadronic Jet-disk Model for the Multiwavelength SED of M87
Authors: Margot Boughelilba, Anita Reimer, Lukas Merten
Figure caption: Left panels: global core emission (red line), composed of the jet emission (cyan dashed curve) and the ADAF emission (blue dotted curve), for a proton spectral index p p = 1.7 and maximum proton energy ﹩{E}_{{\rm{p}},\max }=6\times {10}^{9}\,\mathrm{GeV}﹩ (top panel) and ﹩{E}_{{\rm{p}},\max }={10}^{10}﹩ GeV (bottom panel), for a magnetic field of 10 G. Right panels: corresponding integrated light curve for energies E > 350 GeV (red lines). The gray straight line represents the estimated level of flux with no variability in EHT MWL Science Working Group et al. (2021).
Paper: Lepto-hadronic Jet-disk Model for the Multiwavelength SED of M87
Authors: Margot Boughelilba, Anita Reimer, Lukas Merten
Figure caption: Left panels: Global core emission (red line), composed of the jet emission (cyan dashed curve) and the ADAF emission (blue dotted curve), for a proton spectral index p p = 1.7 and maximum proton energy ﹩{E}_{{\rm{p}},\max }=7\times {10}^{9}\,\mathrm{GeV}﹩ (top panel) and ﹩{E}_{{\rm{p}},\max }={10}^{10}﹩ GeV (bottom panel), for a magnetic field of 50 G. Right panels: Corresponding integrated light curve for energies E > 350 GeV (red lines). The gray straight line represents the estimated level of flux with no variability in EHT MWL Science Working Group et al. (2021).
Paper: Lepto-hadronic Jet-disk Model for the Multiwavelength SED of M87
Authors: Margot Boughelilba, Anita Reimer, Lukas Merten
Figure caption: SED from the ADAF component. The model with the best-fitting parameters in Table 1 with M BH = 6.5 × 109 M ⊙ is given by the red line. The gray area represents the variation of this model for the range of mass M BH = (6.5 ± 0.7) × 109 M ⊙.
Paper: Lepto-hadronic Jet-disk Model for the Multiwavelength SED of M87
Authors: Margot Boughelilba, Anita Reimer, Lukas Merten
Figure caption: Same as Figure 5, but for a proton spectral index p p = 2 and maximum proton energy ﹩{E}_{{\rm{p}},\max }=8\times {10}^{9}\,\mathrm{GeV}﹩ (top panel) and ﹩{E}_{{\rm{p}},\max }={10}^{10}﹩ GeV (bottom panel).
Paper: Lepto-hadronic Jet-disk Model for the Multiwavelength SED of M87
Authors: Margot Boughelilba, Anita Reimer, Lukas Merten
Figure caption: Same as Figure 3, but for a proton spectral index p p = 1.85 and maximum proton energy ﹩{E}_{{\rm{p}},\max }=7\times {10}^{9}\,\mathrm{GeV}﹩ (top panel) and ﹩{E}_{{\rm{p}},\max }={10}^{10}﹩ GeV (bottom panel).
Paper: Lepto-hadronic Jet-disk Model for the Multiwavelength SED of M87
Authors: Margot Boughelilba, Anita Reimer, Lukas Merten
Figure caption: Energy density of the targets fields in the jet’s frame at 1011 Hz (red) and 1018 Hz (blue). The solid and dashed lines represent the contribution from the jet and the accretion flow, respectively.
Paper: Lepto-hadronic Jet-disk Model for the Multiwavelength SED of M87
Authors: Margot Boughelilba, Anita Reimer, Lukas Merten
Figure caption: Predicted electron and muon neutrino spectra, for the models with B = 10 G.
Paper: MaNGA 8313-1901: Gas Accretion Observed in a Blue Compact Dwarf Galaxy?
Authors: Mengting Ju, 梦婷 居, Jun Yin, 君 尹, Rongrong Liu, 蓉蓉 刘, Lei Hao, 蕾 郝, Zhengyi Shao, 正义 邵, Shuai Feng, 帅 冯, Rogério Riffel, Chenxu Liu, 辰旭 刘, David V. Stark, Shiyin Shen, 世银 沈, Eduardo Telles, José G. Fernández-Trincado, Junfeng Wang, 俊峰 王, Haiguang Xu, 海光 徐, Dmitry Bizyaev, Yu Rong, 昱 容
Figure caption: Two-dimensional surface brightness modeling of the host galaxy of MaNGA 8313-1901 with GALFIT. The leftmost panel shows the observed g-band image of BASS with a pixel size of 0.″06 and a PSF FWHM of 1.″68. The black box is defined to be the fitting area of the host galaxy. The gray box with a size of ∼3″ × 6″ and centered at the peak of Hα flux in the NE clump is the region we fit to obtain the morphological parameters of the NE clump with a size of ∼3″ × 6″. The best-fitted 2D model of the host galaxy given by GALFIT and the host-subtracted residual image are shown in the second and third panels. The color scale is the same for all images, and ranges from −0.25–20 nanomaggies arcsecond−2. The two gray dashed lines show the major (northeast–southwest direction) and the minor (northwest–southeast direction) axes. In the left three panels, the red solid circle indicates our definition of the NE clump region with a radius of 1.″71. The orange dashed circle with a radius of 1″ shows our definition of the SW clump (Section 3.2). The rightmost panel shows the surface brightness profiles of the host galaxy (black), the NE clump (red), and the scaled PSF model (yellow). The dots with error bars demonstrate the observed data, and the lines stand for the 1D profiles of the best-fit GALFIT model. The two bottom subpanels of the rightmost panel are the residual (μ data − μ model) profiles of the surface brightness of the host galaxy (black) and the NE clump (red), respectively.
Paper: MaNGA 8313-1901: Gas Accretion Observed in a Blue Compact Dwarf Galaxy?
Authors: Mengting Ju, 梦婷 居, Jun Yin, 君 尹, Rongrong Liu, 蓉蓉 刘, Lei Hao, 蕾 郝, Zhengyi Shao, 正义 邵, Shuai Feng, 帅 冯, Rogério Riffel, Chenxu Liu, 辰旭 刘, David V. Stark, Shiyin Shen, 世银 沈, Eduardo Telles, José G. Fernández-Trincado, Junfeng Wang, 俊峰 王, Haiguang Xu, 海光 徐, Dmitry Bizyaev, Yu Rong, 昱 容
Figure caption: Left: the radial distribution of metallicity for every MaNGA spaxel. Middle: the offset metallicity radial distribution. The radius is defined as the distance to the spaxel with the highest Hα flux in the NE clump. There are two branches in this panel, well separated by the green dashed line. Right: the g-band image from the MaNGA survey. The red circle is the NE clump region, and the orange dashed circle shows the SW clump region. The black line is a dividing line of spaxels located between the two branches shown in the middle panel. The red, orange, and black data points in the left panel and the middle panel represent the spaxels in the NE clump, the spaxels in the SW clump, and all other remaining spaxels in the right panel, respectively.
Paper: MaNGA 8313-1901: Gas Accretion Observed in a Blue Compact Dwarf Galaxy?
Authors: Mengting Ju, 梦婷 居, Jun Yin, 君 尹, Rongrong Liu, 蓉蓉 刘, Lei Hao, 蕾 郝, Zhengyi Shao, 正义 邵, Shuai Feng, 帅 冯, Rogério Riffel, Chenxu Liu, 辰旭 刘, David V. Stark, Shiyin Shen, 世银 沈, Eduardo Telles, José G. Fernández-Trincado, Junfeng Wang, 俊峰 王, Haiguang Xu, 海光 徐, Dmitry Bizyaev, Yu Rong, 昱 容
Figure caption: The top-left panel shows the SDSS gri composite image, which covers 15″ × 15″ in size and corresponds to 7.56 kpc × 7.56 kpc at its distance. The magenta hexagon shows the coverage of the MaNGA bundle in this field. The red solid circle and the orange dashed circle are the locations of the NE clump and the SW clump, defined in Sections 3.1 and 3.2, respectively. In the top-right panel, the spectra of three spaxels indicated as red, black, and orange crosses in the top-left panel are shown as the red, black, and orange solid lines, respectively. Bottom left: the dust-corrected flux map of the Hα emission line. Bottom right: the equivalent width (EW) map of the Hα emission line. The major and minor axes are shown as dashed gray lines. The position angle is adopted from the NASA-Sloan Atlas catalog.
Paper: MaNGA 8313-1901: Gas Accretion Observed in a Blue Compact Dwarf Galaxy?
Authors: Mengting Ju, 梦婷 居, Jun Yin, 君 尹, Rongrong Liu, 蓉蓉 刘, Lei Hao, 蕾 郝, Zhengyi Shao, 正义 邵, Shuai Feng, 帅 冯, Rogério Riffel, Chenxu Liu, 辰旭 刘, David V. Stark, Shiyin Shen, 世银 沈, Eduardo Telles, José G. Fernández-Trincado, Junfeng Wang, 俊峰 王, Haiguang Xu, 海光 徐, Dmitry Bizyaev, Yu Rong, 昱 容
Figure caption: The SFR map (the left panel) and the metallicity map (the middle panel) with the metallicities measured via the O3N2 method. The error map of the metallicity measurements is shown in the right panel. The red circle indicates the NE clump region, and the orange dashed circle shows the SW clump region.
Paper: MaNGA 8313-1901: Gas Accretion Observed in a Blue Compact Dwarf Galaxy?
Authors: Mengting Ju, 梦婷 居, Jun Yin, 君 尹, Rongrong Liu, 蓉蓉 刘, Lei Hao, 蕾 郝, Zhengyi Shao, 正义 邵, Shuai Feng, 帅 冯, Rogério Riffel, Chenxu Liu, 辰旭 刘, David V. Stark, Shiyin Shen, 世银 沈, Eduardo Telles, José G. Fernández-Trincado, Junfeng Wang, 俊峰 王, Haiguang Xu, 海光 徐, Dmitry Bizyaev, Yu Rong, 昱 容
Figure caption: The maps of the light-weighted stellar age (the left panel) and the mass-weighted stellar age (the right panel).
Paper: The Propagation of Coherent Waves Across Multiple Solar Magnetic Pores
Authors: S. D. T. Grant, D. B. Jess, M. Stangalini, S. Jafarzadeh, V. Fedun, G. Verth, P. H. Keys, S. P. Rajaguru, H. Uitenbroek, C. D. MacBride, W. Bate, C. A. Gilchrist-Millar
Figure caption: The upper panel displays a typical IBIS line-core (8542.03 Å) image of the pores in true heliocentric coordinates. The time-averaged perimeters of the established pore boundaries across the bisector range are contoured in the same color scheme as Figure 1. The lower panel shows the average line-core line-of-sight velocity of the same region, where a positive value is a plasma downflow (i.e., redshift), with the time-averaged pore perimeters at the line core contoured in black.
Paper: The Propagation of Coherent Waves Across Multiple Solar Magnetic Pores
Authors: S. D. T. Grant, D. B. Jess, M. Stangalini, S. Jafarzadeh, V. Fedun, G. Verth, P. H. Keys, S. P. Rajaguru, H. Uitenbroek, C. D. MacBride, W. Bate, C. A. Gilchrist-Millar
Figure caption: Left panel: Response function of the Ca II 8542 Å spectral line to temperature perturbations in a magnetic atmosphere, with a Ca II 8542 Å reference profile plotted in white. Upper right panel: Cumulative response function with the height, measured at the wavelengths corresponding to each line depth, which are colored according to the legend on the right. Lower right panel: Cumulative distribution function of each bisector response function, with the same color key as above.
Paper: The Propagation of Coherent Waves Across Multiple Solar Magnetic Pores
Authors: S. D. T. Grant, D. B. Jess, M. Stangalini, S. Jafarzadeh, V. Fedun, G. Verth, P. H. Keys, S. P. Rajaguru, H. Uitenbroek, C. D. MacBride, W. Bate, C. A. Gilchrist-Millar
Figure caption: Histograms of the phase differences between coherent oscillations within pixels of adjacent pores. The dashed black line represents a phase lag of zero degrees. The histogram of P1–P2 is in green, P2–P3 in red, P3–P4 in blue, P4–P5 in yellow, while the comparison between P2 and a quiet-Sun region is displayed in gray.
Paper: The Propagation of Coherent Waves Across Multiple Solar Magnetic Pores
Authors: S. D. T. Grant, D. B. Jess, M. Stangalini, S. Jafarzadeh, V. Fedun, G. Verth, P. H. Keys, S. P. Rajaguru, H. Uitenbroek, C. D. MacBride, W. Bate, C. A. Gilchrist-Millar
Figure caption: Normalized cross power spectrum from the wavelet analysis between the average intensity emission of P3 and reference magnetic feature. Contoured regions represent the values above the 95% confidence interval, with the phase angle between the time series represented by arrows (a 0° phase lag is represented by an arrow pointing right, 180° by a left arrow, and 90° and −90° by up and down arrows, respectively). The cone of influence is represented by the hashed region.
Paper: The Propagation of Coherent Waves Across Multiple Solar Magnetic Pores
Authors: S. D. T. Grant, D. B. Jess, M. Stangalini, S. Jafarzadeh, V. Fedun, G. Verth, P. H. Keys, S. P. Rajaguru, H. Uitenbroek, C. D. MacBride, W. Bate, C. A. Gilchrist-Millar
Figure caption: Both panels depict the phase differences for the average (Eulerian) intensities between pores P3 and P4 in different regions of the optical spectrum. The top panel highlights phases associated with the photospheric 4170 Å continuum channel, while the bottom panel documents the phases associated with the chromospheric line core of the Ca II 8542 Å spectral line. The red crosses indicate coherent frequencies above the 95% confidence threshold, with a blue dashed line in each panel showing the location of zero degrees, indicative of “in-phase” oscillations.
Paper: The Propagation of Coherent Waves Across Multiple Solar Magnetic Pores
Authors: S. D. T. Grant, D. B. Jess, M. Stangalini, S. Jafarzadeh, V. Fedun, G. Verth, P. H. Keys, S. P. Rajaguru, H. Uitenbroek, C. D. MacBride, W. Bate, C. A. Gilchrist-Millar
Figure caption: Energy spectral density of the spatially averaged bisector velocities from pore P3, plotted in a color scheme represented in the legend above, where the unit corresponds to the percentage line depth of the Ca II 8542 Å line.
Paper: The Propagation of Coherent Waves Across Multiple Solar Magnetic Pores
Authors: S. D. T. Grant, D. B. Jess, M. Stangalini, S. Jafarzadeh, V. Fedun, G. Verth, P. H. Keys, S. P. Rajaguru, H. Uitenbroek, C. D. MacBride, W. Bate, C. A. Gilchrist-Millar
Figure caption: Response function of the Ca II 8542 Å spectral line to a 1 km s−1 velocity perturbation in a magnetic atmosphere, with a Ca II 8542 Å reference profile plotted in black. Positive (red) values refer to an intensity brightening as a result of the perturbation, with negative (blue) values referring to a reduction in intensity.
Paper: The Propagation of Coherent Waves Across Multiple Solar Magnetic Pores
Authors: S. D. T. Grant, D. B. Jess, M. Stangalini, S. Jafarzadeh, V. Fedun, G. Verth, P. H. Keys, S. P. Rajaguru, H. Uitenbroek, C. D. MacBride, W. Bate, C. A. Gilchrist-Millar
Figure caption: Top panel: Average LOS velocity for P3 at each percentage line depth, with standard deviations plotted for each measurement. Bottom panels: Histograms of the LOS velocities of the pixels contained within the P3 contour spanning the full height range of measurements. The left panel (blue bars) represents the velocities at 50% line depth, while the right panel (red bars) displays the line-core velocities calculated at a 100% line depth.