adsabs/AstroCLIMB huggingface dataset:
Paper: New Coronae and Stellar Associations Revealed by a Clustering Analysis of the Solar Neighborhood
Authors: Leslie Moranta, Jonathan Gagné, Dominic Couture, Jacqueline K. Faherty
Figure caption: Properties of the input sample considered here, constructed from Gaia EDR3 entries with full kinematics. The input sample is identified with red dots in the upper-left color–magnitude diagram figure, and with black dots in all other panels. Our sample is heavily affected by the selection criteria for radial velocity measurements in Gaia DR2 (4 < G RVS < 13, 3550 < T eff < 6900, corresponding to spectral types F2–M2) because Gaia EDR3 does not include additional radial velocity measurements. The distribution of colors versus distance reflects a combination of these selection cuts with the initial mass function that peaks at early M spectral types. The overdensities that are visible by eye in the XY and UV distributions were identified.
Paper: New Coronae and Stellar Associations Revealed by a Clustering Analysis of the Solar Neighborhood
Authors: Leslie Moranta, Jonathan Gagné, Dominic Couture, Jacqueline K. Faherty
Figure caption: Galactic positions and space velocities of Crius 170 that we have identified as a putative extension of Theia 786. Members of Theia 786 and MELANGE–1 with UVW velocities located within 3 km s−1 from the median bulk velocity of Crius 170 are marked with colored symbols, and the single Crius 170 member with outlier velocities is marked with an orange cross. Both Crius 170 and Theia 786 are also likely related with MELANGE–1, as noted by Tofflemire et al. (2021). Theia 94 seems unrelated but causes slight contamination due to its similar space velocities and Galactic positions. The position and velocity of the Sun are marked with a black crosshair, when inside the figure range.
Paper: New Coronae and Stellar Associations Revealed by a Clustering Analysis of the Solar Neighborhood
Authors: Leslie Moranta, Jonathan Gagné, Dominic Couture, Jacqueline K. Faherty
Figure caption: Gaia EDR3 color–magnitude diagram for Crius 155 members, compared with the empirical sequences of Gagné et al. (2021) and the older open clusters NGC 752 and Ruprecht 147. The low-mass members of Crius 155 are consistent with the 100 Myr old sequence, but also with both older open clusters. The absence of a main-sequence turn-off of the most massive members of Crius 155 suggests a maximum age intermediate between NGC 752 and Ruprecht 147 (1.2–3 Gyr; Cantat-Gaudin et al. 2020).
Paper: New Coronae and Stellar Associations Revealed by a Clustering Analysis of the Solar Neighborhood
Authors: Leslie Moranta, Jonathan Gagné, Dominic Couture, Jacqueline K. Faherty
Figure caption: Median XY Galactic positions of the new candidate associations presented in this work (large, red stars), compared with other known associations in the literature (color-coded by age). Open symbols indicate “candidate” associations that have not yet been fully characterized, such as most of the Kounkel & Covey (2019) Theia groups. All new candidate associations are older than ≈ 100 Myr, and some of then are located well within 100 pc from the Sun.
Paper: New Coronae and Stellar Associations Revealed by a Clustering Analysis of the Solar Neighborhood
Authors: Leslie Moranta, Jonathan Gagné, Dominic Couture, Jacqueline K. Faherty
Figure caption: Corner plot of the median absolute deviations for the Z Galactic coordinate and the U-, V-, and W-space velocities of the 241 Crius groups identified here. Red dashed lines correspond to the selection criteria described in Section 3.
Paper: New Coronae and Stellar Associations Revealed by a Clustering Analysis of the Solar Neighborhood
Authors: Leslie Moranta, Jonathan Gagné, Dominic Couture, Jacqueline K. Faherty
Figure caption: Median XY Galactic positions of all 241 Crius groups recovered here, compared with the distribution of Theia groups from Kounkel & Covey (2019). The clustering analysis presented here allowed us to recover groups much closer to the Sun, filling in the region within ≲100 pc from the Sun, because of its use of UVW-space velocities to prevent projection effects from artificially spreading out the members of nearby associations.
Paper: New Coronae and Stellar Associations Revealed by a Clustering Analysis of the Solar Neighborhood
Authors: Leslie Moranta, Jonathan Gagné, Dominic Couture, Jacqueline K. Faherty
Figure caption: In our investigations of known associations possibly related with Crius 87, we have identified a previously unrecognized, likely corona of the UPK 612 open cluster (Cantat-Gaudin et al. 2020) contained in Theia 216 of Kounkel & Covey (2019). Crius 87 appeared as a candidate extension of this corona toward the Sun at a first glance, given its consistent Z-coordinate, location in the XY-plane, and similar kinematics. However, its median kinematics are discrepant by 8.5 km s−1, enough to call into question whether Crius 87 is related to UPK 612 at all.
Paper: New Coronae and Stellar Associations Revealed by a Clustering Analysis of the Solar Neighborhood
Authors: Leslie Moranta, Jonathan Gagné, Dominic Couture, Jacqueline K. Faherty
Figure caption: Galactic positions and space velocities of Crius 156 and Crius 171, which correspond to the Platais 3 and Alessi 9 associations, respectively. These associations have been, respectively, associated with Theia 787 and Theia 598 by Kounkel & Covey (2019). The tentative spatial extensions of both associations toward the Sun show systematically discrepant UVW velocities, which may indicate that they are simply caused by contamination. Both Crius 156/Theia 787 and Crius 171/Theia 598 are spatially much more extended than the core of their respective associations, and likely correspond to their extended coronae, which had not been previously discussed in the literature to the extent of our knowledge.
Paper: New Coronae and Stellar Associations Revealed by a Clustering Analysis of the Solar Neighborhood
Authors: Leslie Moranta, Jonathan Gagné, Dominic Couture, Jacqueline K. Faherty
Figure caption: The NGC 2451A open cluster with its corona identified by Meingast et al. (2019). The spatial position and kinematics of Crius 178 are consistent with it extending the corona slightly toward nearby distances, which was probably not recovered by previous studies because of projection effects. The elongated distribution of NGC 2451A members in UV-space is due to larger parallax measurement errors compared with proper motion and heliocentric radial velocity measurement errors in Gaia EDR3, which is typical of young associations and open clusters beyond 100 pc.
Paper: New Coronae and Stellar Associations Revealed by a Clustering Analysis of the Solar Neighborhood
Authors: Leslie Moranta, Jonathan Gagné, Dominic Couture, Jacqueline K. Faherty
Figure caption: Galactic positions and space velocities of Crius 172, which we associate with a likely front-facing tidal tail to the poorly characterized Group 51 of Oh et al. (2017). Theia 218 may correspond to a farther tidal tail behind Group 51 given its consistent space velocities and spatial location.
Paper: New Coronae and Stellar Associations Revealed by a Clustering Analysis of the Solar Neighborhood
Authors: Leslie Moranta, Jonathan Gagné, Dominic Couture, Jacqueline K. Faherty
Figure caption: Galactic positions and space velocities of Crius 217 and Theia 214 of Kounkel & Covey (2019), which likely correspond to an extensive corona around the newly discovered RSG 2 open cluster (Röser et al. 2016).
Paper: The ALMA Survey of 70 μm Dark High-mass Clumps in Early Stages (ASHES). VII. Chemistry of Embedded Dense Cores
Authors: Shanghuo Li, Patricio Sanhueza, Xing Lu, Chang Won Lee, Qizhou Zhang, Stefano Bovino, Giovanni Sabatini, Tie Liu, Kee-Tae Kim, Kaho Morii, Daniel Tafoya, Ken'ichi Tatematsu, Takeshi Sakai, Junzhi Wang, Fei Li, Andrea Silva, Natsuko Izumi, David Allingham
Figure caption:                         The velocity-integrated intensity maps of the N2D+, DCO+, DCN, C18O, CH3OH, and H2CO emission lines toward G14.49. The unit of the colorbar is Jy beam−1 km s−1. The fuchsia pluses and yellow, white, and green asterisks indicate prestellar candidates (category 1), outflow cores (category 2), warm cores (category 3), and outflow + warm cores (category 4). The white dashed line shows 30% of the sensitivity level of the mosaic in the ALMA continuum image. The blue and red arrows in the bottom right panel indicate the directions of the blueshifted and redshifted CO outflow lobes (see Paper II), respectively. The gray contours in each panel show the 1.3 mm continuum emission. The contour levels are (3, 6) × σ, with σ = 0.115 mJy beam−1. The beam sizes of the line emissions and scale bars are shown in the lower left and right corners of each panel, respectively. The remaining sources are presented in Appendix A (see Figures 10–14).
Paper: The ALMA Survey of 70 μm Dark High-mass Clumps in Early Stages (ASHES). VII. Chemistry of Embedded Dense Cores
Authors: Shanghuo Li, Patricio Sanhueza, Xing Lu, Chang Won Lee, Qizhou Zhang, Stefano Bovino, Giovanni Sabatini, Tie Liu, Kee-Tae Kim, Kaho Morii, Daniel Tafoya, Ken'ichi Tatematsu, Takeshi Sakai, Junzhi Wang, Fei Li, Andrea Silva, Natsuko Izumi, David Allingham
Figure caption: Top row: plots of ﹩{N}_{{{\rm{H}}}_{2}}﹩ vs. ﹩{N}_{{{\rm{N}}}_{2}{{\rm{D}}}^{+}}﹩, ﹩{N}_{{{\rm{N}}}_{2}{{\rm{D}}}^{+}}/{N}_{{{\rm{H}}}_{2}\mathrm{CO}}﹩, and ﹩{N}_{{{\rm{N}}}_{2}{{\rm{D}}}^{+}}/{N}_{{\mathrm{CH}}_{3}\mathrm{OH}}﹩. Bottom row: plots of ﹩{T}_{{\mathrm{NH}}_{3}}﹩ vs. ﹩{X}_{{{\rm{N}}}_{2}{{\rm{D}}}^{+}}﹩, ﹩{N}_{{{\rm{N}}}_{2}{{\rm{D}}}^{+}}/{N}_{{{\rm{H}}}_{2}\mathrm{CO}}﹩, and ﹩{N}_{{{\rm{N}}}_{2}{{\rm{D}}}^{+}}/{N}_{{\mathrm{CH}}_{3}\mathrm{OH}}﹩. The correlation coefficients derived from Spearman’s rank correlation test are given in the text in each panel. The black cross shows the typical uncertainty in each panel.
Paper: The ALMA Survey of 70 μm Dark High-mass Clumps in Early Stages (ASHES). VII. Chemistry of Embedded Dense Cores
Authors: Shanghuo Li, Patricio Sanhueza, Xing Lu, Chang Won Lee, Qizhou Zhang, Stefano Bovino, Giovanni Sabatini, Tie Liu, Kee-Tae Kim, Kaho Morii, Daniel Tafoya, Ken'ichi Tatematsu, Takeshi Sakai, Junzhi Wang, Fei Li, Andrea Silva, Natsuko Izumi, David Allingham
Figure caption: Violin plots of the peak intensity I and observed velocity dispersion σ obs distributions for each line. The shape of each distribution shows the probability density of the data, smoothed by a kernel density estimator. The last panel shows the H2CO peak intensity distributions of each category of dense cores. The blue horizontal bars from the top to bottom of each violin plot represent the maximum, mean, and minimum values, respectively.
Paper: The ALMA Survey of 70 μm Dark High-mass Clumps in Early Stages (ASHES). VII. Chemistry of Embedded Dense Cores
Authors: Shanghuo Li, Patricio Sanhueza, Xing Lu, Chang Won Lee, Qizhou Zhang, Stefano Bovino, Giovanni Sabatini, Tie Liu, Kee-Tae Kim, Kaho Morii, Daniel Tafoya, Ken'ichi Tatematsu, Takeshi Sakai, Junzhi Wang, Fei Li, Andrea Silva, Natsuko Izumi, David Allingham
Figure caption: Integrated intensity correlation matrix, showing cross correlations for each pair of molecules. The correlation coefficients are described in the text. The “+” symbols mean that correlation coefficients cannot be derived, either due to lack of detection or the spatially overlapped emitting area being smaller than one beam in size. The colors indicate the number of beam areas of the spatially overlapping emitting regions. Larger numbers of beam areas have more robust derived correlation coefficients than smaller ones.
Paper: The ALMA Survey of 70 μm Dark High-mass Clumps in Early Stages (ASHES). VII. Chemistry of Embedded Dense Cores
Authors: Shanghuo Li, Patricio Sanhueza, Xing Lu, Chang Won Lee, Qizhou Zhang, Stefano Bovino, Giovanni Sabatini, Tie Liu, Kee-Tae Kim, Kaho Morii, Daniel Tafoya, Ken'ichi Tatematsu, Takeshi Sakai, Junzhi Wang, Fei Li, Andrea Silva, Natsuko Izumi, David Allingham
Figure caption: Left column: histograms of the molecular column densities for the prestellar and protostellar cores. Right column: histograms of the molecular abundances for the prestellar and protostellar cores. The black dashed vertical lines indicate the median values of the parameters.
Paper: The ALMA Survey of 70 μm Dark High-mass Clumps in Early Stages (ASHES). VII. Chemistry of Embedded Dense Cores
Authors: Shanghuo Li, Patricio Sanhueza, Xing Lu, Chang Won Lee, Qizhou Zhang, Stefano Bovino, Giovanni Sabatini, Tie Liu, Kee-Tae Kim, Kaho Morii, Daniel Tafoya, Ken'ichi Tatematsu, Takeshi Sakai, Junzhi Wang, Fei Li, Andrea Silva, Natsuko Izumi, David Allingham
Figure caption: Histograms of the number and detection rate distributions of detected lines for: each evolutionary category of cores (a); prestellar vs. protostellar cores (b); prestellar cores only (c); and protostellar cores only (d).
Paper: The ALMA Survey of 70 μm Dark High-mass Clumps in Early Stages (ASHES). VII. Chemistry of Embedded Dense Cores
Authors: Shanghuo Li, Patricio Sanhueza, Xing Lu, Chang Won Lee, Qizhou Zhang, Stefano Bovino, Giovanni Sabatini, Tie Liu, Kee-Tae Kim, Kaho Morii, Daniel Tafoya, Ken'ichi Tatematsu, Takeshi Sakai, Junzhi Wang, Fei Li, Andrea Silva, Natsuko Izumi, David Allingham
Figure caption: The column density ratio of DCO+ to N2D+ vs. the core-averaged volume density ﹩{n}_{{{\rm{H}}}_{2}}﹩ and temperature ﹩{T}_{{\mathrm{NH}}_{3}}﹩.
Paper: The ALMA Survey of 70 μm Dark High-mass Clumps in Early Stages (ASHES). VII. Chemistry of Embedded Dense Cores
Authors: Shanghuo Li, Patricio Sanhueza, Xing Lu, Chang Won Lee, Qizhou Zhang, Stefano Bovino, Giovanni Sabatini, Tie Liu, Kee-Tae Kim, Kaho Morii, Daniel Tafoya, Ken'ichi Tatematsu, Takeshi Sakai, Junzhi Wang, Fei Li, Andrea Silva, Natsuko Izumi, David Allingham
Figure caption: The same as Figure 7, but for DCO+.
Paper: The ALMA Survey of 70 μm Dark High-mass Clumps in Early Stages (ASHES). VII. Chemistry of Embedded Dense Cores
Authors: Shanghuo Li, Patricio Sanhueza, Xing Lu, Chang Won Lee, Qizhou Zhang, Stefano Bovino, Giovanni Sabatini, Tie Liu, Kee-Tae Kim, Kaho Morii, Daniel Tafoya, Ken'ichi Tatematsu, Takeshi Sakai, Junzhi Wang, Fei Li, Andrea Silva, Natsuko Izumi, David Allingham
Figure caption: Examples of core-averaged spectra of C18O, DCO+, N2D+, H2CO, CH3OH, and SiO for core #7 in G14.49.
Paper: The ALMA Survey of 70 μm Dark High-mass Clumps in Early Stages (ASHES). VII. Chemistry of Embedded Dense Cores
Authors: Shanghuo Li, Patricio Sanhueza, Xing Lu, Chang Won Lee, Qizhou Zhang, Stefano Bovino, Giovanni Sabatini, Tie Liu, Kee-Tae Kim, Kaho Morii, Daniel Tafoya, Ken'ichi Tatematsu, Takeshi Sakai, Junzhi Wang, Fei Li, Andrea Silva, Natsuko Izumi, David Allingham
Figure caption: Velocity-integrated intensity maps of the N2D+, DCO+, DCN, C18O, CH3OH, and H2CO emission lines toward G10.99. The fuchsia pluses and the yellow, white, and green asterisk symbols indicate prestellar candidates (category 1), outflow cores (category 2), warm cores (category 3), and outflow + warm cores (category 4). The dashed white line shows 30% of the sensitivity level of the mosaic in the ALMA continuum image. The blue and red arrows in middle right panel indicate the directions of the blueshifted and redshifted CO outflow lobes (see Paper II), respectively. The gray contours in each panel shows the 1.3 mm continuum emission. The contour levels are (3, 6) ×  σ, with σ = 0.115 mJy beam−1. The beam size is shown in the lower left corner of each panel.
Paper: The ALMA Survey of 70 μm Dark High-mass Clumps in Early Stages (ASHES). VII. Chemistry of Embedded Dense Cores
Authors: Shanghuo Li, Patricio Sanhueza, Xing Lu, Chang Won Lee, Qizhou Zhang, Stefano Bovino, Giovanni Sabatini, Tie Liu, Kee-Tae Kim, Kaho Morii, Daniel Tafoya, Ken'ichi Tatematsu, Takeshi Sakai, Junzhi Wang, Fei Li, Andrea Silva, Natsuko Izumi, David Allingham
Figure caption:                         The same as Figure 10, but for different sources.
Paper: Collisional Growth Efficiency of Dust Aggregates and Its Independence of the Strength of Interparticle Rolling Friction
Authors: Sota Arakawa, Hidekazu Tanaka, Eiichiro Kokubo
Figure caption: Dependence of E dis,tot on ﹩{{B}_{\mathrm{off}}}^{2}﹩ and v col. Here we set ξ crit = 0.8  nm. The dashed line is the initial kinetic energy, N tot E kin,1, which is given by Equation (8).
Paper: Collisional Growth Efficiency of Dust Aggregates and Its Independence of the Strength of Interparticle Rolling Friction
Authors: Sota Arakawa, Hidekazu Tanaka, Eiichiro Kokubo
Figure caption: Same as Figure 5 but with ﹩{{B}_{\mathrm{off}}}^{2}=6/12﹩.
Paper: Collisional Growth Efficiency of Dust Aggregates and Its Independence of the Strength of Interparticle Rolling Friction
Authors: Sota Arakawa, Hidekazu Tanaka, Eiichiro Kokubo
Figure caption: Same as Figure 5 but with ﹩{{B}_{\mathrm{off}}}^{2}=9/12﹩.
Paper: Solar-cycle-related Variation of Differential Rotation of the Chromosphere
Authors: Miao Wan, Peng-xin Gao
Figure caption: Top panel: parameter A (black solid line) when the latitudinal distribution of the yearly rotation rate is fitted by the general expression of differential rotation: ﹩\omega (\phi )=A\,+\,B{\sin }^{2}\phi ﹩. The red solid line represents the linear fitting of parameter A. Middle panel: parameter B (the black solid line) of the solar differential rotation at each year of the considered time frame. The red solid line represents the linear fitting of parameter B. Bottom panel: the yearly mean sunspot number (black solid line) in the considered time frame. The red solid line represents the linear fitting of the yearly mean sunspot number. In all panels, the black vertical dashed/solid lines indicate the minimum/maximum years of solar cycles.
Paper: Solar-cycle-related Variation of Differential Rotation of the Chromosphere
Authors: Miao Wan, Peng-xin Gao
Figure caption: Top panel: variation of the asymmetry coefficient of the chromospheric rotation rate with time is shown as the black solid line, with its trend indicated by the red line. Bottom panel: variation of the normalized asymmetry index of the hemispheric sunspot area with time is shown as the black solid line, with its trend indicated by the red line. In all panels, the black vertical dashed/solid lines indicate the minimum/maximum years of solar cycles.
Paper: Solar-cycle-related Variation of Differential Rotation of the Chromosphere
Authors: Miao Wan, Peng-xin Gao
Figure caption: Autocorrelation coefficient (CC) of the Ca II K line time series at a certain latitude in a certain year, varying with its relative phase shift. The four panels correspond to four time series whose latitudes are shown at the top of each panel. The dashed vertical line in each panel represents the local maximum CC, and the abscissa value is the Carrington synodic rotation period (CR).
Paper: Solar-cycle-related Variation of Differential Rotation of the Chromosphere
Authors: Miao Wan, Peng-xin Gao
Figure caption: Isopleth lines (black solid lines) of rotation rates. The corresponding rotation rates are 13.3, 13.1, 12.9, and 12.7 (deg/day) from low latitude to high latitude. The vertical dashed/solid lines indicate the minimum/maximum years of solar cycles.
Paper: Solar-cycle-related Variation of Differential Rotation of the Chromosphere
Authors: Miao Wan, Peng-xin Gao
Figure caption: Top/bottom panels: the mean value of the parameter B (the black line) depending on the phase of the solar cycle relative to the minimum/maximum years of the nearest solar cycle, and their corresponding standard errors (blue lines)
Paper: Solar-cycle-related Variation of Differential Rotation of the Chromosphere
Authors: Miao Wan, Peng-xin Gao
Figure caption: Correlation coefficient (asterisks) when the latitudinal distribution of the yearly rotation rate within ± 40° latitudes belt is fitted by the standard formula of solar differential rotation. The vertical dashed/solid lines show the minimum/maximum years of solar cycles.
Paper: Solar-cycle-related Variation of Differential Rotation of the Chromosphere
Authors: Miao Wan, Peng-xin Gao
Figure caption: Time–latitude distribution diagram of Ca II K normalized intensity during the period of 1915 August 10 to 1985 July 7 (CR827—CR1764). The two horizontal white dashed lines indicate the latitudes of ± 40°, and the vertical white dashed lines show the minimum epochs of solar cycles.
Paper: Solar-cycle-related Variation of Differential Rotation of the Chromosphere
Authors: Miao Wan, Peng-xin Gao
Figure caption: The latitudinal distribution of the yearly rotation rate given by the general expression of differential rotation. The unit shown on the color bar is deg/day. The white vertical dashed/solid lines indicate the minimum/maximum years of solar cycles, respectively.
Paper: Evidence That Shocks Destroy Small PAH Molecules in Low-luminosity Active Galactic Nuclei
Authors: Lulu Zhang, Luis C. Ho, Aigen Li
Figure caption: Spatially resolved diagnostics of PAH band ratios 6.2 μm/7.7 μm and 11.3 μm/7.7 μm for spaxels in galaxies classified as (a) SFGs and (b) AGNs, color coded according to the [Ne III]/[Ne II] line ratios. In panel (a), the three black stars, from left to right, give the median PAH band ratios for SFG spaxels that cover the range ﹩\mathrm{log}\ [\mathrm{Ne}\,{\rm\small{III}}]/[\mathrm{Ne}\,{\rm\small{II}}]\lt -0.7﹩, ﹩-0.7\lt \mathrm{log}\ [\mathrm{Ne}\,{\rm\small{III}}]/[\mathrm{Ne}\,{\rm\small{II}}]\lt -0.5﹩, and ﹩\mathrm{log}\ [\mathrm{Ne}\,{\rm\small{III}}]/[\mathrm{Ne}\,{\rm\small{II}}]\gt -0.5﹩. In panel (b), the points with a black dot denote the central-most spaxel of the AGN. The black crosses represent model predictions by Draine & Li (2001) for neutral (top sequence) and ionized (bottom sequence) PAHs, as well as PAHs of different sizes, with increasing number of C atoms (N C) from right to left. Typical error bars of the PAH band ratios are marked in the top-right of each panel.
Paper: Evidence That Shocks Destroy Small PAH Molecules in Low-luminosity Active Galactic Nuclei
Authors: Lulu Zhang, Luis C. Ho, Aigen Li
Figure caption: Correlation between integrated PAH luminosity and extinction-corrected FUV luminosity for spaxels in galaxies classified as (a) SFGs and (b) AGNs. The data points are color coded according to [Ne III]/[Ne II]. In panel (b), the points with a black dot pertain to the central-most spaxel of the AGN. The dashed line is the best-fit linear regression for the SFG spaxels (Equation (1)).
Paper: Evidence That Shocks Destroy Small PAH Molecules in Low-luminosity Active Galactic Nuclei
Authors: Lulu Zhang, Luis C. Ho, Aigen Li
Figure caption: Illustration of coverage of IRS mapping-mode observations of M 51, overlaid on GALEX FUV image as the background. The black and white rectangles delineate the central region with complete SL+LL and SH+LH spectra, respectively, with the black star marking the center. The inset in the top-right corner is a zoom-in of the central ﹩2^{\prime} \times 2^{\prime} ﹩ region that shows the distribution of resolved 10″  × 10″ spaxels within the black rectangle that has complete SL+LL spectra, color coded (from orange to yellow) according to the flux of the IRS spectra integrated over 5–20 μm.
Paper: Evidence That Shocks Destroy Small PAH Molecules in Low-luminosity Active Galactic Nuclei
Authors: Lulu Zhang, Luis C. Ho, Aigen Li
Figure caption: Integrated residual PAH spectra for the central regions of (a) SFGs and (b) AGNs, obtained by summing the residual PAH spectra of all the spaxels within the corresponding central region and normalized by the flux density at 7.7 μm. The residual PAH spectrum is produced by subtracting the best-fit continuum components from the observed spectrum. The main PAH features are marked in panel (a). Panel (c) shows the composite residual PAH spectra for regions from SFGs (blue) and AGNs (red). Panel (d) illustrates an example of the decomposition of individual PAH features from the residual spectrum (gray line) using Drude profiles (dashed curves), which combine to produce the total model (red curve).