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 snow between on-site measurements (open symbols) and Equation (1) with m = 5 (solid lines) or m = 6 (dotted lines) for ice Ih (r0 = 138 pm, γ = 0.208 J m−2). Upper left: old snow (saltire) by C. M. Keeler (1969), dry, fine-grained snow (dot) and dry depth hoar (down-pointing triangle) by C. M. Keeler & W. F. Weeks (1967), initial hard slab (cross), typical aged snow (circle), persistent soft snow (triangle) by M. Martinelli (1971), and naturally deposited snow by D. M. McClung (1979); upper right: naturally deposited snow by R. Perla (1969) and R. A. Sommerfeld (1974) and a slab of avalanche snow by S. L. Mccabe & F. W. Smith (1978) and H. Conway & J. Abrahamson (1984); bottom: dry rounded grains (open circle), slightly moist rounded grains (open diamond), multilayer specimens (saltire), faceted grains (open square), faceted and rounded grains (squared plus), newly fallen snow (cross), and partly settled grains (open triangle) by J. B. Jamieson & C. D. Johnston (1990).
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 snow between laboratory measurements (symbols) and Equation (1) with m = 5 (solid lines) or m = 6 (dotted lines) for ice Ih (r0 = 138 pm, γ = 0.208 J m−2). Upper left: fine-grained old snow (squares) by H. Narita (1980, 1984), metropolitan snow (diamond) by H. Bader et al. (1951), and age-hardened snow by A. Upadhyay et al. (2007); upper right: compacted snow by H. Narita (1987); lower left: finely grained fresh snow (circles) by T. Theile (2010) and snow of rounded grains (square) by P. Hagenmuller et al. (2014); lower right: snowpack by C. P. Borstad & D. M. McClung (2011).
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 aerogels between MD simulations (symbols) and Equation (1) with m = 8 (solid lines) for amorphous silica (r0 = 81 pm, γ = 0.243 J m−2). Upper left: simulation with the VKRE potential by J. S. Rivas Murillo et al. (2010); upper right and middle left: simulation with the VKRE potential by S. P. Patil et al. (2017); middle right: simulation with the VKRE potential by S. P. Patil et al. (2020); bottom: simulation with the BKS potential by W. Gonçalves et al. (2018) and Equation (1) with γ = 1.375 J m−2 (dotted line) expected from the Wolf BKS potential.
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 aerogels between laboratory experiments (symbols) and Equation (1) with m = 8 (solid lines) for amorphous silica (r = 81 pm, γ = 0.243 J m−2). Upper left: silica aerogels and xerogels under the Brazilian disk tests (filled circles) by T. Woignier & J. Phalippou (1988) and J. C. H. Wong et al. (2014); upper right: silica aerogels hydrolyzed under acidic (open triangles), neutral (filled squares), and basic conditions (filled circles) and densified by sintering (open circles) measured in a three-point bending technique by T. Woignier & J. Phalippou (1988), T. Woignier et al. (1998, 2015), and A. H. Alaoui et al. (2000); lower left: silica aerogels and xerogels with ϕ = 0.13 ± 0.02 inclusive of three-point bending data by L. Duffours et al. (1994); lower right: silica aerogels measured in a three-point bending technique by D. J. Boday & D. A. Loy (2015).
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 crystalline water ice between MD simulations (symbols) and Equation (1) with m = 5 (solid line) for ice Ih (r0 = 138 pm, γ = 0.208 J m−2). The coarse-grained model of water (mW) potential (circle) by P. Cao et al. (2018) and the extended simple point charge (SPC/E) potential (cross) by Y. Y. Chen et al. (2021) and P. Wei et al. (2022). Also plotted are Equation (1) with γ = 0.163 J m−2 expected from the SPC/E potential and γ = 0.151 J m−2 from the mW potential.
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 LISA detection rate estimated using 10,000 realizations of the MBH population. Upper: the number of observed binaries (with SNR >10) per year per unit redshift (left) / log MBH (right). In each panel, the yellow/blue solid curves represent the results from Circ/Ecc, respectively. The blue dashed curve shows the predicted inspiral sources from the Ecc. We do not plot the inspiral sources for the Circ since it has a negligible number of inspiral sources (less than 10−3 yr−1). In the upper left frame, the vertical dotted line represents the peak of redshift distribution: zpeak = 1.9 for Circ (yellow) and zpeak = 0.80 (blue) for Ecc. Bottom: the fraction between the number of detectable sources in Circ and Ecc. We mark the level of NEcc = NCirc with the black dashed 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: The galaxies hosting detectable sources at z = 0.8. The top contour plots compare the properties of host galaxies of detectable LISA sources that merge within 0.8 < z < 0.9 (red contours) and the galaxies hosting no mergers (gray contours). Each contour set plots the 1σ/2σ/3σ regions, enclosing 68%/95%/99.7% of the population. Top left: the MBH mass vs. galaxy stellar mass (MBH − Mgal). Top middle: the galaxy star formation rate vs. galaxy stellar mass (SFR − Mgal). Note that we remove the galaxies with zero star formation rate to plot this distribution. Top right: the MBH mass vs. the stellar mass ratio between the host galaxy and host friends-of-friends (FoF) halo (MBH − Mgal/MFoF). For the galaxies hosting detectable sources, we plot the mass of the remnant MBH as MBH, and for the nonmerger galaxies, we plot the mass of the central MBH. We randomly select a sample consisting of six detectable sources, which are marked by the diamonds in the contour plots. In the second and third rows, we plot the stellar density field for the FoF halo for the selected mergers. The location of the remnant MBH is marked by the arrows with corresponding colors. In each frame, the circle represents the virial radius of the halo.
Paper: Asking Fast Radio Bursts for More than Reionization History
Authors: Abinash Kumar Shaw, Raghunath Ghara, Paz Beniamini, Saleem Zaroubi, Pawan Kumar
Figure caption: Left: asymmetrical ﹩\tanh (z)﹩ ionization histories. Different colors represent three ionization histories corresponding to the simulated toy models. Right: mean DM estimates and 1σ fluctuations. Colors represent different reionization histories as shown in the left panel. Solid lines and the shaded regions are the average DM and corresponding 1σ errors estimated over all grid points available in the simulation volume. Dashed lines correspond to the DM estimated using the mean ionization fraction directly in Equation (3). Three vertical lines mark the redshift of mid-reionization.
Paper: Asking Fast Radio Bursts for More than Reionization History
Authors: Abinash Kumar Shaw, Raghunath Ghara, Paz Beniamini, Saleem Zaroubi, Pawan Kumar
Figure caption: Top: the ratio ﹩{\sigma }_{{\rm{DM}}}/{\overline{{\rm{DM}}}}_{{\rm{EoR}}}﹩ as a function of redshift z. The three different line styles correspond to the three reionization histories. Bottom: the redshift derivative of ﹩{\overline{{\rm{DM}}}}_{{\rm{EoR}}}(z)﹩. The green lines show the fluctuating estimates, whereas the orange lines are after a Gaussian smoothing.
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 the detectable mergers (with SNR > 10) in the Ecc. Left: ratio of total merger mass (M1 + M2) to the total black hole mass in the host galaxies. Middle: MBH Bolometric luminosity Lbol. Right: black hole Eddington ratio fedd. In each frame, the gray histogram represents the distribution of all the mergers across the redshift and mass range. The solid black (red) curves show the MBHs involving mergers with Mtot > 106 M⊙ (Mtot > 108 M⊙). The dashed histograms correspond to the mergers occurring at high redshift (z ≥ 2) with Mtot > 106M⊙ (black dashed) or Mtot > 108M⊙ (red dashed).
Paper: Asking Fast Radio Bursts for More than Reionization History
Authors: Abinash Kumar Shaw, Raghunath Ghara, Paz Beniamini, Saleem Zaroubi, Pawan Kumar
Figure caption: Image slice from the LC box of the fiducial EoR toy model. Both axes are in comoving units, with the axis labeled x being the LoS axis. The bubble radius is 10 grid units (≈12 Mpc). Black and white regions are, respectively, completely ionized and completely neutral. Reionization progresses from right to left in this box.
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: Same with Figure 10, but for the host galaxies of detectable mergers occur within 1.5 < z < 1.6.
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: Same as Figure 8, but the detection rate is plotted as a function of the mass ratio q = M2/M1. The black dotted curve in the upper panel represents all the merger sources in ASTRID.
Paper: Evidence for a Hot Galactic Halo around the Andromeda Galaxy Using Fast Radio Bursts along Two Sightlines
Authors: Reshma Anna-Thomas, Casey J. Law, Eric W. Koch, Alexa C. Gordon, Kritti Sharma, Benjamin F. Williams, Nickolas M. Pingel, Sarah Burke-Spolaor, Zhuo Chen, Jordan Stanley, Calvin Dear, Frank Verdi, J. Xavier Prochaska, Geoffrey C. Bower, Laura Chomiuk, Liam Connor, Paul B. Demorest, Wen-Fai Fong, Anya Nugent, Fabian Walter
Figure caption: The probability distribution of all different DM components. The left panel corresponds to FRB 20230930A and the right panel to FRB 20230506C. The blue line shows the PDF of the observed DM. The indigo dotted line represents the MW disk contribution, while the dashed–dotted line represents the MW halo. The green dashed line corresponds to the host DM distribution, the red line to the IGM distribution, and the black line to M31. In the left panel, the dark blue dashed vertical line marks the median of the DMM31 distribution, with the shaded region indicating the 90% CI. In the right panel, the orange dashed vertical line marks the median, and the shaded region likewise denotes the 90% CI.
Paper: Evidence for a Hot Galactic Halo around the Andromeda Galaxy Using Fast Radio Bursts along Two Sightlines
Authors: Reshma Anna-Thomas, Casey J. Law, Eric W. Koch, Alexa C. Gordon, Kritti Sharma, Benjamin F. Williams, Nickolas M. Pingel, Sarah Burke-Spolaor, Zhuo Chen, Jordan Stanley, Calvin Dear, Frank Verdi, J. Xavier Prochaska, Geoffrey C. Bower, Laura Chomiuk, Liam Connor, Paul B. Demorest, Wen-Fai Fong, Anya Nugent, Fabian Walter
Figure caption: (a) The Keck R-band image of the host galaxy of FRB 20230506C. The 5σ realfast localization region is shown in green. (b) The blue region and (c) the red region of Keck LRIS spectrum of the host galaxy of FRB 20230506C. The redder spectrum had a poor subtraction of telluric features, but we limit our analysis to the features labeled with dashed lines.
Paper: Evidence for a Hot Galactic Halo around the Andromeda Galaxy Using Fast Radio Bursts along Two Sightlines
Authors: Reshma Anna-Thomas, Casey J. Law, Eric W. Koch, Alexa C. Gordon, Kritti Sharma, Benjamin F. Williams, Nickolas M. Pingel, Sarah Burke-Spolaor, Zhuo Chen, Jordan Stanley, Calvin Dear, Frank Verdi, J. Xavier Prochaska, Geoffrey C. Bower, Laura Chomiuk, Liam Connor, Paul B. Demorest, Wen-Fai Fong, Anya Nugent, Fabian Walter
Figure caption: The map of H II regions and planetary nebula of M31 with respect to the FRB lines of sight. The region zoomed around FRB 20230930A is shown in the inset. The size of the H II regions and planetary nebulae circles are scaled by their actual size. The catalog is adapted from M. Azimlu et al. (2011).
Paper: Evidence for a Hot Galactic Halo around the Andromeda Galaxy Using Fast Radio Bursts along Two Sightlines
Authors: Reshma Anna-Thomas, Casey J. Law, Eric W. Koch, Alexa C. Gordon, Kritti Sharma, Benjamin F. Williams, Nickolas M. Pingel, Sarah Burke-Spolaor, Zhuo Chen, Jordan Stanley, Calvin Dear, Frank Verdi, J. Xavier Prochaska, Geoffrey C. Bower, Laura Chomiuk, Liam Connor, Paul B. Demorest, Wen-Fai Fong, Anya Nugent, Fabian Walter
Figure caption: (a) The HST/WCS image of the host galaxy of FRB 20230930A. The 5σ realfast localization region is shown in green. (b) The DBSP spectrum of the host galaxy of FRB 20230930A.
Paper: Evidence for a Hot Galactic Halo around the Andromeda Galaxy Using Fast Radio Bursts along Two Sightlines
Authors: Reshma Anna-Thomas, Casey J. Law, Eric W. Koch, Alexa C. Gordon, Kritti Sharma, Benjamin F. Williams, Nickolas M. Pingel, Sarah Burke-Spolaor, Zhuo Chen, Jordan Stanley, Calvin Dear, Frank Verdi, J. Xavier Prochaska, Geoffrey C. Bower, Laura Chomiuk, Liam Connor, Paul B. Demorest, Wen-Fai Fong, Anya Nugent, Fabian Walter
Figure caption: The geometry of M31’s disk with respect to the FRB 20230930A’s line of sight. The DM from M31’s disk is calculated by integrating the electron density ne(R, z) along this line of sight.
Paper: Evidence for a Hot Galactic Halo around the Andromeda Galaxy Using Fast Radio Bursts along Two Sightlines
Authors: Reshma Anna-Thomas, Casey J. Law, Eric W. Koch, Alexa C. Gordon, Kritti Sharma, Benjamin F. Williams, Nickolas M. Pingel, Sarah Burke-Spolaor, Zhuo Chen, Jordan Stanley, Calvin Dear, Frank Verdi, J. Xavier Prochaska, Geoffrey C. Bower, Laura Chomiuk, Liam Connor, Paul B. Demorest, Wen-Fai Fong, Anya Nugent, Fabian Walter
Figure caption: Dynamic spectrogram (bottom) and frequency-averaged time profile (top) of the realfast bursts, dedispersed at their detection DM. The data have 10 ms time resolution and 1 MHz frequency resolution; note that channels between 1490 MHz and 1690 MHz were not recorded by the realfast system.
Paper: Evidence for a Hot Galactic Halo around the Andromeda Galaxy Using Fast Radio Bursts along Two Sightlines
Authors: Reshma Anna-Thomas, Casey J. Law, Eric W. Koch, Alexa C. Gordon, Kritti Sharma, Benjamin F. Williams, Nickolas M. Pingel, Sarah Burke-Spolaor, Zhuo Chen, Jordan Stanley, Calvin Dear, Frank Verdi, J. Xavier Prochaska, Geoffrey C. Bower, Laura Chomiuk, Liam Connor, Paul B. Demorest, Wen-Fai Fong, Anya Nugent, Fabian Walter
Figure caption: The DMM31,halo estimated from FRB 20230930A. The total DMM31 is shown in black, with the DMM31,disk in blue and the DMM31,halo in green. The dashed green line marks the median of the DMM31,halo PDF for FRB 20230930A, and the shaded region indicates the 90% CI.
Paper: Evidence for a Hot Galactic Halo around the Andromeda Galaxy Using Fast Radio Bursts along Two Sightlines
Authors: Reshma Anna-Thomas, Casey J. Law, Eric W. Koch, Alexa C. Gordon, Kritti Sharma, Benjamin F. Williams, Nickolas M. Pingel, Sarah Burke-Spolaor, Zhuo Chen, Jordan Stanley, Calvin Dear, Frank Verdi, J. Xavier Prochaska, Geoffrey C. Bower, Laura Chomiuk, Liam Connor, Paul B. Demorest, Wen-Fai Fong, Anya Nugent, Fabian Walter
Figure caption: The DM predicted from the mNFW profile of M31’s halo for a given impact parameter from the center of the halo (gray). The DMM31,halo measured from the two FRBs are also shown. The FRB measurements are centered on the median and extend to the 90% CIs.
Paper: Evidence for a Hot Galactic Halo around the Andromeda Galaxy Using Fast Radio Bursts along Two Sightlines
Authors: Reshma Anna-Thomas, Casey J. Law, Eric W. Koch, Alexa C. Gordon, Kritti Sharma, Benjamin F. Williams, Nickolas M. Pingel, Sarah Burke-Spolaor, Zhuo Chen, Jordan Stanley, Calvin Dear, Frank Verdi, J. Xavier Prochaska, Geoffrey C. Bower, Laura Chomiuk, Liam Connor, Paul B. Demorest, Wen-Fai Fong, Anya Nugent, Fabian Walter
Figure caption: The dirty and clean maps of the realfast localization of the bursts. FRB 20230930A and FRB 20230506C B2 were observed in VLA A-configuration, and the FRB 20230506C B1 was observed in VLA B-configuration.
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: The left column presents the flux distribution for the H2 0–0 S(1), S(2), S(3), S(4), and S(5) emission lines normalized by the maximum flux value for NGC 5506. The black contours overlaid on the H2 0–0 S(1) line map present the distribution of ALMA CO(3–2) intensity distribution (S. García-Burillo et al. 2021); contours range from 10−1.35 to 10−0.3 Jy (0.35 dex steps). The solid black line overlaid on the H2 0–0 S(2) line map indicates the orientation of the disk (PA = 90°), and the dotted black lines indicate the edges of the ionization bicone (PA = 22°, ΩOut = 80°). The tan dashed contours overlaid on the H2 0–0 S(5) flux map represent the [Fe II]5.34μm intensity distribution; contours range from 10−6.25 to 10−5.25 Jy (0.5 dex steps). The associated velocity fields for both the primary and secondary fit components are presented in the right two panels. The center column presents the 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: The top panels present NGC 3081 relative population levels estimated for the full set of rotational and rovibrational emission. The left panel presents the best-fit non-LTE radiative transfer model. The right panel depicts two shock scenarios which provide a reasonably good fit to the population level estimates. In this figure, the modeled ν = 2–1 transition lines have been included although no measurements above the 3σ S/N threshold are available. The bottom panels present NGC 5506 relative population levels estimated for the full set of rotational and rovibrational emission. The left panel presents the best-fit non-LTE radiative transfer model. The right panel depicts two shock scenarios which provide a reasonably good fit to the population level estimates.
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: Total flux distribution (normalized by the maximum flux value) and kinematics for NGC 3081 (top panels) and NGC 5506 (bottom panels) derived from [Fe II]5.34μm emission. The left column presents the normalized flux distribution, the center column depicts the associated velocity field, and the right column depicts the associated velocity dispersion. Overlaid on the flux distribution are the 8.46 GHz radio intensity contour lines. For NGC 3081, the contour intervals (NRAO/VLA Archive Survey: https://archive.nrao.edu/) range from 10−4.5 to 10−4.0 Jy Beam−1 in 0.25 dex steps. For NGC 5506, the contour intervals (H. Schmitt et al. 2001) range from 10−4.5 to 10−2.5 Jy Beam−1 in 0.5 dex steps. Dashed lines overlaid on the dispersion map of NGC 5506 indicate a wider opening angle of Ω = 140°.