adsabs/AstroCLIMB huggingface dataset:
Paper: Tensile Strength of Dust, Pebbles, and Planetesimals: A Simple Mathematical Formula from Aggregates to Monoliths Based on an Extension of an Elastic Theory for Particle Assemblies to Molecular Networks
Authors: Hiroshi Kimura, ヒロシ キムラ, Takayuki Hirai, Takaya Okamoto, Akiko M. Nakamura, Eiichiro Kokubo, Yuki Yoshida, Fumi Yoshida, Peng K. Hong, Koji Wada, Hiroki Senshu, Tomoko Arai, Sota Arakawa, Toshihiko Kadono, Masanori Kobayashi, Ko Ishibashi, Hiroshi Akitaya, Manabu Yamada, Osamu Okudaira, Takafumi Matsui
Figure caption: A comparison of tensile strength for diamond (DIA) between MD simulations (symbols) and Equation (1) with m = 6 (solid line) for nonporous (ϕ = 1.0) diamond (r = 77 pm, γ = 9.30 J m−2). Left: simulation results of monocrystalline diamond with the REBO potential (open circle) by O. A. Shenderova et al. (2000) and Q. Lu et al. (2008), the EDIP potential (open square) by Q. Lu et al. (2008), and the ReaxFF potential (open triangle) by B. D. Jensen et al. (2015). Also plotted are Equation (1) with γ = 4.31 J m−2 (dashed–dotted line) for the Tersoff potential, γ111 = 5.35 J m−2 (dotted line) for the REBO potential, γ111 = 1.26 J m−2 (dashed line) for the EDIP potential, and γ100 = 19.17 J m−2 (dashed–double-dotted line) for the ReaxFF potential; right: simulation results of polycrystalline diamond with the Tersoff potential by Z. D. Sha et al. (2011) and C. Huang et al. (2018).
Paper: Tensile Strength of Dust, Pebbles, and Planetesimals: A Simple Mathematical Formula from Aggregates to Monoliths Based on an Extension of an Elastic Theory for Particle Assemblies to Molecular Networks
Authors: Hiroshi Kimura, ヒロシ キムラ, Takayuki Hirai, Takaya Okamoto, Akiko M. Nakamura, Eiichiro Kokubo, Yuki Yoshida, Fumi Yoshida, Peng K. Hong, Koji Wada, Hiroki Senshu, Tomoko Arai, Sota Arakawa, Toshihiko Kadono, Masanori Kobayashi, Ko Ishibashi, Hiroshi Akitaya, Manabu Yamada, Osamu Okudaira, Takafumi Matsui
Figure caption: A comparison of tensile strength for nonporous (ϕ = 1.0) quartz group between MD simulations (crosses) and Equation (1) with m = 8 (solid line) for nonporous (ϕ = 1.0) crystalline quartz (r = 81 pm, γ = 2.13 J m−2). Upper left: the BMHB potential by T. F. Soules (1985), R. Ochoa et al. (1991), and T. P. Swiler et al. (1995); upper right: simulation results of the BKS potential by E. C. C. M. Silva et al. (2006) and F. Molaei & H. Siavoshi (2020); middle left: simulation results of the PMMCS potential by A. Pedone et al. (2008); middle right: simulation results of the VKRE potential by J. Zhang (2018); lower left: the ReaxFF potential by C. Zhang et al. (2023); lower right: the Tersoff potential by J. Guo & L. Ma (2019) and W. Sun et al. (2020b).
Paper: Gravitational Wave Decoupling in Retrograde Circumbinary Disks
Authors: David O'Neill, Christopher Tiede, Daniel J. D'Orazio, Zoltán Haiman, Andrew MacFadyen
Figure caption: Azimuthally averaged surface densities for retrograde disks (red) and prograde disks (blue) at three different stages during the inspiral (solid, dashed, and dotted). The x-axis units have been scaled to the current orbital separation of the binary (gray vertical lines). On each panel, we print the nominal decoupling semimajor axis adc (see Equation (10) with ξ = 0.6).
Paper: Tensile Strength of Dust, Pebbles, and Planetesimals: A Simple Mathematical Formula from Aggregates to Monoliths Based on an Extension of an Elastic Theory for Particle Assemblies to Molecular Networks
Authors: Hiroshi Kimura, ヒロシ キムラ, Takayuki Hirai, Takaya Okamoto, Akiko M. Nakamura, Eiichiro Kokubo, Yuki Yoshida, Fumi Yoshida, Peng K. Hong, Koji Wada, Hiroki Senshu, Tomoko Arai, Sota Arakawa, Toshihiko Kadono, Masanori Kobayashi, Ko Ishibashi, Hiroshi Akitaya, Manabu Yamada, Osamu Okudaira, Takafumi Matsui
Figure caption: A comparison of tensile strength for interstellar silicate and graphite grains (shaded area) assumed in the classical model of the interstellar extinction curve and Equation (1) with m = 8 (dotted line) for amorphous silica (r0 = 81 pm, γ = 0.243 J m−2) and m = 6 (solid line) for graphite (r0 = 73.15 pm, γ = 4.17 J m−2) as a function of grain radius.
Paper: Tensile Strength of Dust, Pebbles, and Planetesimals: A Simple Mathematical Formula from Aggregates to Monoliths Based on an Extension of an Elastic Theory for Particle Assemblies to Molecular Networks
Authors: Hiroshi Kimura, ヒロシ キムラ, Takayuki Hirai, Takaya Okamoto, Akiko M. Nakamura, Eiichiro Kokubo, Yuki Yoshida, Fumi Yoshida, Peng K. Hong, Koji Wada, Hiroki Senshu, Tomoko Arai, Sota Arakawa, Toshihiko Kadono, Masanori Kobayashi, Ko Ishibashi, Hiroshi Akitaya, Manabu Yamada, Osamu Okudaira, Takafumi Matsui
Figure caption: A comparison of tensile strength for glassy carbon between laboratory experiments (symbols) and Equation (1) with m = 6 (solid line) for graphite (r = 73.15 pm, γ = 4.17 J m−2). Left: uniaxial tension tests by W. V. Kotlensky & D. B. Fischbach (1965), W. V. Kotlensky & H. E. Martens (1965), and T. C. Peng (1979); right: uniaxial tension tests by K. Kawamura & G. M. Jenkins (1972) and three-point bending tests by R. E. Bullock & J. L. Kaae (1979), as well as Equation (1) with ϕ = 0.71 (dotted line).
Paper: Tensile Strength of Dust, Pebbles, and Planetesimals: A Simple Mathematical Formula from Aggregates to Monoliths Based on an Extension of an Elastic Theory for Particle Assemblies to Molecular Networks
Authors: Hiroshi Kimura, ヒロシ キムラ, Takayuki Hirai, Takaya Okamoto, Akiko M. Nakamura, Eiichiro Kokubo, Yuki Yoshida, Fumi Yoshida, Peng K. Hong, Koji Wada, Hiroki Senshu, Tomoko Arai, Sota Arakawa, Toshihiko Kadono, Masanori Kobayashi, Ko Ishibashi, Hiroshi Akitaya, Manabu Yamada, Osamu Okudaira, Takafumi Matsui
Figure caption: A comparison of tensile strength for silica glass between laboratory experiments (symbols) and Equation (1) with m = 8 (solid lines) for nonporous (ϕ = 1.0) amorphous silica (r = 81 pm, γ = 0.243 J m−2). Left: J. Luo et al. (2016); right: nonporous samples by J. E. Ritter & C. L. Sherburne (1970, 1971; saltire) and porous samples by D. Kićević et al. (1996; open triangle), as well as Equation (1) with ϕ = 0.876 (dotted line).
Paper: Gravitational Waves from Massive Black Hole Mergers in ASTRID: Predictions for LISA
Authors: Bonny Y. Wang, 玥 汪, Yihao Zhou, 亦豪 周, William Chen, Nianyi Chen, Tiziana Di Matteo, Rupert Croft, Simeon Bird, Yueying Ni
Figure caption: Waveforms for three binaries of different mass and orbital eccentricity e0 during the 4 yr before the coalescence. The strain is calculated for z = 1, and the mass and the initial e0 are labeled on the upper right corner. In each panel, the black dotted line is the LISA instrument sensitivity curve with the galactic binary background. The thick black curve shows the strain assuming initial e0 = 0. The thin blue curves track the strain at different evolution times. The lines of constant time are shaded from light to dark for early to late evolution. On each blue curve, the circle, square, triangle, and diamond markers represent the evolution of individual harmonics: n = 2, 10, 50, and 100, respectively. The thick green curve plots the frequency having the highest strain fpeak for the eccentric waveforms during the evolution.
Paper: Gravitational Waves from Massive Black Hole Mergers in ASTRID: Predictions for LISA
Authors: Bonny Y. Wang, 玥 汪, Yihao Zhou, 亦豪 周, William Chen, Nianyi Chen, Tiziana Di Matteo, Rupert Croft, Simeon Bird, Yueying Ni
Figure caption: Examples of MBH mergers with a circular orbit (e = 0.09; upper panel) and a highly eccentric orbit (e = 0.95; lower panel) in ASTRID at z = 0.8. The plots on the left display the separation Δr between the two merging black holes as a function of time, with pink and blue crosses marking the last three pairs of rapo and rperi used to calculate the eccentricity values. The plots on the right show the corresponding orbital trajectories of the secondary black hole relative to the primary black hole’s position. The black and red dots mark the locations of the primary black hole (BH1) and the secondary black hole (BH2) before the merger.
Paper: Gravitational Waves from Massive Black Hole Mergers in ASTRID: Predictions for LISA
Authors: Bonny Y. Wang, 玥 汪, Yihao Zhou, 亦豪 周, William Chen, Nianyi Chen, Tiziana Di Matteo, Rupert Croft, Simeon Bird, Yueying Ni
Figure caption: Parameter space of MBH mass and redshift explored by LISA. The left panel plots the two-dimensional distribution of the redshift and the total mass of merging MBHs Mtot. The right panel shows the distribution of the mass of the primary MBH M1 and the secondary MBH M2. The underlying blue color gradient represents the differential number of detected mergers during the LISA 4 yr observation for Ecc: ﹩dN/(d{\mathrm{log}}M\,dz\,dt)\times {\rm{4yr}}﹩ for the left panel and ﹩dN/(d{\mathrm{log}}{M}_{1}\,d{\mathrm{log}}{M}_{2}\,dt)\times {\rm{4yr}}﹩ for the right panel. The black and red contours correspond to the detected MBH merger population for Ecc and Circ, respectively.
Paper: Gravitational Waves from Massive Black Hole Mergers in ASTRID: Predictions for LISA
Authors: Bonny Y. Wang, 玥 汪, Yihao Zhou, 亦豪 周, William Chen, Nianyi Chen, Tiziana Di Matteo, Rupert Croft, Simeon Bird, Yueying Ni
Figure caption: Strain and frequency distribution for the mergers in ASTRID. The left frame is for Circ and the right panel is for Ecc. For each MBH merger, the plotted frequency and strain correspond to the evolution time point and harmonic mode that makes the largest contribution to SNR within 4 yr before the coalescence. For the Circ, the harmonic mode is always n = 2. We color the distribution based on the redshift and the number of events, as shown by the right colorbar: the high(low) redshifts are represented by the blue(red) colors, and the darkness corresponds to the regions with very few events. The redshift is averaged over the merger population in each pixel.
Paper: Gravitational Waves from Massive Black Hole Mergers in ASTRID: Predictions for LISA
Authors: Bonny Y. Wang, 玥 汪, Yihao Zhou, 亦豪 周, William Chen, Nianyi Chen, Tiziana Di Matteo, Rupert Croft, Simeon Bird, Yueying Ni
Figure caption: Probability density function (PDF) of merger orbit eccentricities e0 measured based on Equation (1). Left: PDF for mergers at different redshifts. Solid curves represent the distribution from the ASTRID merger population, and dotted curves show the fitted β distribution (Equation (9)) for the redshifts with the corresponding color. Right: PDF for mergers with different total MBH masses.
Paper: Gravitational Wave Decoupling in Retrograde Circumbinary Disks
Authors: David O'Neill, Christopher Tiede, Daniel J. D'Orazio, Zoltán Haiman, Andrew MacFadyen
Figure caption: The ratio of prograde to retrograde cavity closing timescales (or disk rebrightening), following merger. These timescales are based on the cavity semimajor axes at decoupling (given in Figure 8).
Paper: Gravitational Waves from Massive Black Hole Mergers in ASTRID: Predictions for LISA
Authors: Bonny Y. Wang, 玥 汪, Yihao Zhou, 亦豪 周, William Chen, Nianyi Chen, Tiziana Di Matteo, Rupert Croft, Simeon Bird, Yueying Ni
Figure caption: The MBH population in ASTRID at different redshifts. Upper: the black hole mass function in terms of comoving number density (dex−1 h3 Mpc−3). Lower: the ratio between the number of the MBH involved in mergers and the total MBH.
Paper: Asking Fast Radio Bursts for More than Reionization History
Authors: Abinash Kumar Shaw, Raghunath Ghara, Paz Beniamini, Saleem Zaroubi, Pawan Kumar
Figure caption: Variation of ﹩\langle \overline{{\rm{DM}}}({z}_{{\rm{mid}}})\rangle ﹩ and the marginalized ﹩\langle {\overline{{\rm{DM}}}}_{{\rm{margin}}}\rangle ﹩ as a function of total number of FRBs ﹩{N}_{{\rm{FRB}}}^{{\rm{tot}}}﹩ observed during the EoR. Top row: this shows the ensemble-averaged ﹩\overline{{\rm{DM}}}({z}_{{\rm{mid}}})﹩ and its standard deviation as a function of ﹩{N}_{{\rm{FRB}}}^{{\rm{tot}}}﹩ for the three reionization histories. Bottom row: this shows the ensemble mean of ﹩{\overline{{\rm{DM}}}}_{{\rm{margin}}}﹩, marginalized ﹩\overline{{\rm{DM}}}﹩ over the EoR redshift range, as a function of ﹩{N}_{{\rm{FRB}}}^{{\rm{tot}}}﹩ for the three different reionization histories. Solid lines here are the ensemble mean, and shaded regions correspond to 3σ cosmic variances, which are estimated, for every choice of ﹩{N}_{{\rm{FRB}}}^{{\rm{tot}}}﹩, using 1000 independent ensembles of FRB distributions in the IGM during EoR. The left, middle, and right columns correspond to the optimistic, moderate, and pessimistic scenarios, respectively, as described in the text.
Paper: Asking Fast Radio Bursts for More than Reionization History
Authors: Abinash Kumar Shaw, Raghunath Ghara, Paz Beniamini, Saleem Zaroubi, Pawan Kumar
Figure caption: Cumulative redshift distribution of observable FRBs. The orange solid line shows the cumulative distribution of the FRB abundance computed following the model in P. Beniamini et al. (2021). The green shaded region here demarcates the redshift range (6 ≤ z ≤ 15) used in this work.
Paper: Asking Fast Radio Bursts for More than Reionization History
Authors: Abinash Kumar Shaw, Raghunath Ghara, Paz Beniamini, Saleem Zaroubi, Pawan Kumar
Figure caption: Density distribution of ∂2Ξ/∂z∂δθ. This plot is similar to Figure 4, but for the realistic EoR simulations. The three different panels correspond to the three different reionization histories as labeled. However, this is obtained from a realistic simulation of EoR LCs, which does not have a fixed bubble size.
Paper: Asking Fast Radio Bursts for More than Reionization History
Authors: Abinash Kumar Shaw, Raghunath Ghara, Paz Beniamini, Saleem Zaroubi, Pawan Kumar
Figure caption: The ratio ﹩{\sigma }_{{\rm{DM}}}/{\overline{{\rm{DM}}}}_{{\rm{EoR}}}﹩ as a function of z. The ratios are computed using the estimates from the three realistic GRIZZLY simulations.
Paper: Excitation of Molecular Hydrogen in Seyferts: NGC 5506 and NGC 3081
Authors: Daniel E. Delaney, Erin K. S. Hicks, Lulu Zhang, Chris Packham, Ric Davies, Miguel Pereira Santaella, Enrica Bellocchi, Nancy A. Levenson, Steph Campbell, David J. Rosario, Houda Haidar, Cristina Ramos Almeida, Anelise Audibert, Claudio Ricci, Laura Hermosa Muñoz, Francoise Combes, Almudena Alonso-Herrero, Santiago García-Burillo, Federico Esposito, Ismael García-Bernete, Taro Shimizu, Martin Ward, Omaira Gonzalez Martin, Alvaro Labiano, Enrique Lopez-Rodriguez, Dimitra Rigopoulou, Marko Stalevski, Sebastian F. Hönig, Donaji Esparza-Arredondo, Takuma Izumi, Lindsay Fuller, Daniel Rouan
Figure caption: Flux distribution and kinematics for NGC 3081 [Ne V]14.322μm emission. The left column presents the primary/rotational component for the two-component fit, and the right column presents the secondary/outflowing fit component.
Paper: Excitation of Molecular Hydrogen in Seyferts: NGC 5506 and NGC 3081
Authors: Daniel E. Delaney, Erin K. S. Hicks, Lulu Zhang, Chris Packham, Ric Davies, Miguel Pereira Santaella, Enrica Bellocchi, Nancy A. Levenson, Steph Campbell, David J. Rosario, Houda Haidar, Cristina Ramos Almeida, Anelise Audibert, Claudio Ricci, Laura Hermosa Muñoz, Francoise Combes, Almudena Alonso-Herrero, Santiago García-Burillo, Federico Esposito, Ismael García-Bernete, Taro Shimizu, Martin Ward, Omaira Gonzalez Martin, Alvaro Labiano, Enrique Lopez-Rodriguez, Dimitra Rigopoulou, Marko Stalevski, Sebastian F. Hönig, Donaji Esparza-Arredondo, Takuma Izumi, Lindsay Fuller, Daniel Rouan
Figure caption: Flux distribution and kinematics for NGC 5506 H2 0–0 S(6) emission. The left column presents the primary/rotational component for the two-component fit, and the right column presents the secondary/outflowing fit component.
Paper: Excitation of Molecular Hydrogen in Seyferts: NGC 5506 and NGC 3081
Authors: Daniel E. Delaney, Erin K. S. Hicks, Lulu Zhang, Chris Packham, Ric Davies, Miguel Pereira Santaella, Enrica Bellocchi, Nancy A. Levenson, Steph Campbell, David J. Rosario, Houda Haidar, Cristina Ramos Almeida, Anelise Audibert, Claudio Ricci, Laura Hermosa Muñoz, Francoise Combes, Almudena Alonso-Herrero, Santiago García-Burillo, Federico Esposito, Ismael García-Bernete, Taro Shimizu, Martin Ward, Omaira Gonzalez Martin, Alvaro Labiano, Enrique Lopez-Rodriguez, Dimitra Rigopoulou, Marko Stalevski, Sebastian F. Hönig, Donaji Esparza-Arredondo, Takuma Izumi, Lindsay Fuller, Daniel Rouan
Figure caption: Flux distribution and kinematics for NGC 5506 H2 0–0 S(1) emission. The left column presents the primary/rotational component for the two-component fit, and the right column presents the secondary/outflowing fit component.
Paper: Excitation of Molecular Hydrogen in Seyferts: NGC 5506 and NGC 3081
Authors: Daniel E. Delaney, Erin K. S. Hicks, Lulu Zhang, Chris Packham, Ric Davies, Miguel Pereira Santaella, Enrica Bellocchi, Nancy A. Levenson, Steph Campbell, David J. Rosario, Houda Haidar, Cristina Ramos Almeida, Anelise Audibert, Claudio Ricci, Laura Hermosa Muñoz, Francoise Combes, Almudena Alonso-Herrero, Santiago García-Burillo, Federico Esposito, Ismael García-Bernete, Taro Shimizu, Martin Ward, Omaira Gonzalez Martin, Alvaro Labiano, Enrique Lopez-Rodriguez, Dimitra Rigopoulou, Marko Stalevski, Sebastian F. Hönig, Donaji Esparza-Arredondo, Takuma Izumi, Lindsay Fuller, Daniel Rouan
Figure caption: Flux distribution and kinematics for NGC 5506 H2 0–0 S(2) emission. The left column presents the primary/rotational component for the two-component fit, and the right column presents the secondary/outflowing fit component.
Paper: Excitation of Molecular Hydrogen in Seyferts: NGC 5506 and NGC 3081
Authors: Daniel E. Delaney, Erin K. S. Hicks, Lulu Zhang, Chris Packham, Ric Davies, Miguel Pereira Santaella, Enrica Bellocchi, Nancy A. Levenson, Steph Campbell, David J. Rosario, Houda Haidar, Cristina Ramos Almeida, Anelise Audibert, Claudio Ricci, Laura Hermosa Muñoz, Francoise Combes, Almudena Alonso-Herrero, Santiago García-Burillo, Federico Esposito, Ismael García-Bernete, Taro Shimizu, Martin Ward, Omaira Gonzalez Martin, Alvaro Labiano, Enrique Lopez-Rodriguez, Dimitra Rigopoulou, Marko Stalevski, Sebastian F. Hönig, Donaji Esparza-Arredondo, Takuma Izumi, Lindsay Fuller, Daniel Rouan
Figure caption: Flux distribution and kinematics for NGC 5506 H2 0–0 S(3) emission. The left column presents the primary/rotational component for the two-component fit, and the right column presents the secondary/outflowing fit component.
Paper: Excitation of Molecular Hydrogen in Seyferts: NGC 5506 and NGC 3081
Authors: Daniel E. Delaney, Erin K. S. Hicks, Lulu Zhang, Chris Packham, Ric Davies, Miguel Pereira Santaella, Enrica Bellocchi, Nancy A. Levenson, Steph Campbell, David J. Rosario, Houda Haidar, Cristina Ramos Almeida, Anelise Audibert, Claudio Ricci, Laura Hermosa Muñoz, Francoise Combes, Almudena Alonso-Herrero, Santiago García-Burillo, Federico Esposito, Ismael García-Bernete, Taro Shimizu, Martin Ward, Omaira Gonzalez Martin, Alvaro Labiano, Enrique Lopez-Rodriguez, Dimitra Rigopoulou, Marko Stalevski, Sebastian F. Hönig, Donaji Esparza-Arredondo, Takuma Izumi, Lindsay Fuller, Daniel Rouan
Figure caption: Flux distribution and kinematics for NGC 5506 H2 0–0 S(5) emission. The left column presents the primary/rotational component for the two-component fit, and the right column presents the secondary/outflowing fit component.
Paper: Excitation of Molecular Hydrogen in Seyferts: NGC 5506 and NGC 3081
Authors: Daniel E. Delaney, Erin K. S. Hicks, Lulu Zhang, Chris Packham, Ric Davies, Miguel Pereira Santaella, Enrica Bellocchi, Nancy A. Levenson, Steph Campbell, David J. Rosario, Houda Haidar, Cristina Ramos Almeida, Anelise Audibert, Claudio Ricci, Laura Hermosa Muñoz, Francoise Combes, Almudena Alonso-Herrero, Santiago García-Burillo, Federico Esposito, Ismael García-Bernete, Taro Shimizu, Martin Ward, Omaira Gonzalez Martin, Alvaro Labiano, Enrique Lopez-Rodriguez, Dimitra Rigopoulou, Marko Stalevski, Sebastian F. Hönig, Donaji Esparza-Arredondo, Takuma Izumi, Lindsay Fuller, Daniel Rouan
Figure caption: Flux distribution and kinematics for NGC 5506 H2 0–0 S(7) emission. The left column presents the primary/rotational component for the two-component fit, and the right column presents the secondary/outflowing fit component.
Paper: Excitation of Molecular Hydrogen in Seyferts: NGC 5506 and NGC 3081
Authors: Daniel E. Delaney, Erin K. S. Hicks, Lulu Zhang, Chris Packham, Ric Davies, Miguel Pereira Santaella, Enrica Bellocchi, Nancy A. Levenson, Steph Campbell, David J. Rosario, Houda Haidar, Cristina Ramos Almeida, Anelise Audibert, Claudio Ricci, Laura Hermosa Muñoz, Francoise Combes, Almudena Alonso-Herrero, Santiago García-Burillo, Federico Esposito, Ismael García-Bernete, Taro Shimizu, Martin Ward, Omaira Gonzalez Martin, Alvaro Labiano, Enrique Lopez-Rodriguez, Dimitra Rigopoulou, Marko Stalevski, Sebastian F. Hönig, Donaji Esparza-Arredondo, Takuma Izumi, Lindsay Fuller, Daniel Rouan
Figure caption: Flux distribution and kinematics for NGC 5506 H2 0–0 S(4) emission. The left column presents the primary/rotational component for the two-component fit, and the right column presents the secondary/outflowing fit component.
Paper: Excitation of Molecular Hydrogen in Seyferts: NGC 5506 and NGC 3081
Authors: Daniel E. Delaney, Erin K. S. Hicks, Lulu Zhang, Chris Packham, Ric Davies, Miguel Pereira Santaella, Enrica Bellocchi, Nancy A. Levenson, Steph Campbell, David J. Rosario, Houda Haidar, Cristina Ramos Almeida, Anelise Audibert, Claudio Ricci, Laura Hermosa Muñoz, Francoise Combes, Almudena Alonso-Herrero, Santiago García-Burillo, Federico Esposito, Ismael García-Bernete, Taro Shimizu, Martin Ward, Omaira Gonzalez Martin, Alvaro Labiano, Enrique Lopez-Rodriguez, Dimitra Rigopoulou, Marko Stalevski, Sebastian F. Hönig, Donaji Esparza-Arredondo, Takuma Izumi, Lindsay Fuller, Daniel Rouan
Figure caption: Flux distribution and kinematics for NGC 5506 H2 0–0 S(8) emission. The left column presents the primary/rotational component for the two-component fit, and the right column presents the secondary/outflowing fit component.
Paper: Excitation of Molecular Hydrogen in Seyferts: NGC 5506 and NGC 3081
Authors: Daniel E. Delaney, Erin K. S. Hicks, Lulu Zhang, Chris Packham, Ric Davies, Miguel Pereira Santaella, Enrica Bellocchi, Nancy A. Levenson, Steph Campbell, David J. Rosario, Houda Haidar, Cristina Ramos Almeida, Anelise Audibert, Claudio Ricci, Laura Hermosa Muñoz, Francoise Combes, Almudena Alonso-Herrero, Santiago García-Burillo, Federico Esposito, Ismael García-Bernete, Taro Shimizu, Martin Ward, Omaira Gonzalez Martin, Alvaro Labiano, Enrique Lopez-Rodriguez, Dimitra Rigopoulou, Marko Stalevski, Sebastian F. Hönig, Donaji Esparza-Arredondo, Takuma Izumi, Lindsay Fuller, Daniel Rouan
Figure caption: Flux distribution and kinematics for NGC 5506 [Ne V]14.322μm emission. The left column presents the primary/rotational component for the two-component fit, and the right column presents the secondary/outflowing fit component.
Paper: Excitation of Molecular Hydrogen in Seyferts: NGC 5506 and NGC 3081
Authors: Daniel E. Delaney, Erin K. S. Hicks, Lulu Zhang, Chris Packham, Ric Davies, Miguel Pereira Santaella, Enrica Bellocchi, Nancy A. Levenson, Steph Campbell, David J. Rosario, Houda Haidar, Cristina Ramos Almeida, Anelise Audibert, Claudio Ricci, Laura Hermosa Muñoz, Francoise Combes, Almudena Alonso-Herrero, Santiago García-Burillo, Federico Esposito, Ismael García-Bernete, Taro Shimizu, Martin Ward, Omaira Gonzalez Martin, Alvaro Labiano, Enrique Lopez-Rodriguez, Dimitra Rigopoulou, Marko Stalevski, Sebastian F. Hönig, Donaji Esparza-Arredondo, Takuma Izumi, Lindsay Fuller, Daniel Rouan
Figure caption: Flux distribution and kinematics for NGC 5506 [Ne II]12.814μm emission. The left column presents the primary/rotational component for the two-component fit, and the right column presents the secondary/outflowing fit component.