adsabs/AstroCLIMB huggingface dataset:
Paper: Interpreting Mass and Radius Measurements of Neutron Stars with Dark Matter Halos
Authors: Shafayat Shawqi, Sharon M. Morsink
Figure caption: Effects of different BM EOSs on the M  T (R  B ) curves of compact (left) and diffuse (right) halos with f  χ  = 0.05. Cartoon MR constraints for two fictitious DANSs are shown for illustrative purposes. Left: for both BM EOSs, the curve of M  T (R  B ) vs. R  B  (red dots) is almost identical to the M  T  vs. R  B  curve for the DANSs (orange curves), due to the tiny amounts of DM in the cloud. The orange shaded region depicts a cartoon 1σ confidence region for a gravitational self-lensing observation of a fictitious DANS by a telescope such as NICER. For the BM EOS NL3ωρL55, both a pure baryonic EOS and a DM EOS are supported by the observations of DANS(3). The pure BM EOS SLy5 is supported by the observations, but the corresponding DM EOS is ruled out. Right: for both BM EOSs, the curve of M  T (R  B ) vs. R  B  (red dots) is almost identical to the MR curve for the purely baryonic NS with no DM content (solid black curves). The green shaded region depicts a cartoon 1σ confidence region for a dynamical NS mass measurement of a different DANS, DANS(1). The orange shaded region depicts a cartoon 1σ gravitational-lensing MR posterior for DANS(1), obtained using a mass prior using the dynamical mass measurement. The red shaded region depicts an example of a different 1σ posterior obtained using an adjusted mass prior that tests for nonzero values of f  χ . For more details on the interpretation of this DANS, see Section 5.3.
Paper: Interpreting Mass and Radius Measurements of Neutron Stars with Dark Matter Halos
Authors: Shafayat Shawqi, Sharon M. Morsink
Figure caption: Effect of increasing DM fraction f  χ  on MR curves for diffuse halos. These schematic diagrams show how to interpret the validity of diffuse halo MR curves when only a dynamical mass measurement of an NS (left) or only a gravitational self-lensing MR constraint is available (right). The blue dashed curves correspond to M  T  for DM mass fractions f  χ  = 0.05, 0.1, and 0.2 (where higher mass corresponds to larger values of f  χ ). Left panel: the green shaded region depicts a cartoon 1σ confidence region of dynamical mass measurement of DANS(1). The dynamical mass measurement supports a BM EOS if an M  T  curve (blue dashed lines) intersects the range of measured masses. The dynamical mass measurement of DANS(1) supports the EOS NL3ωρL55 for any value of f  χ , while EOS SLy5 is only supported if the value of f  χ  is large enough. Right panel: the orange shaded region depicts a cartoon 1σ NICER confidence region for a different NS MR measurement. The observation supports EOS NL3ωρL55 with any value of f  χ  since the M  T (R  B ) vs. R  B  curves (red dots) for varying f  χ  are identical for diffuse halos. The observation rules out EOS SLy5 for any diffuse halo and any value of f  χ .
Paper: Interpreting Mass and Radius Measurements of Neutron Stars with Dark Matter Halos
Authors: Shafayat Shawqi, Sharon M. Morsink
Figure caption: Density and mass distributions for DANSs with varying DM particle mass m  χ , self-interaction parameter y = 0, DM fraction f  χ  = 0.05, and baryonic EOS NL3ωρL55. Top left: baryonic (dashed–dotted) and DM (solid or dashed) energy densities as a function of radial distance from the center of M  T  = 1.4 M ⊙ DANS models. Top right: baryonic (dashed–dotted) energy densities for the same DANS models. Energy densities of M  T  = 1.33 M ⊙ (black dashed–dotted) and M  T  = 1.4 M ⊙ (black dotted) pure baryonic NSs are also plotted for comparison. Bottom left: enclosed DM mass as a function of radial distance. Black dots show the location of the baryonic surface of the DANS. The mass fraction of DM in the cloud is shown in the legend. Bottom right: enclosed BM mass as a function of radial distance in the region close to the baryonic surface.
Paper: Interpreting Mass and Radius Measurements of Neutron Stars with Dark Matter Halos
Authors: Shafayat Shawqi, Sharon M. Morsink
Figure caption: Mass vs. baryonic radius curves for baryonic EOS NL3ωρL55 and different DM models with f  χ  = 0.05. Solid and dashed curves refer to stars with DM cores and halos, respectively. Left: total gravitational mass as a function of R  B . Right: total gravitational mass enclosed within R  B , ﹩{M}_{T}\left({R}_{B}\right)﹩, for the same DANS models. Green shaded regions show the MR constraints from one analysis of NICER data for PSR J0030+0451 (T. E. Riley et al. 2019).
Paper: Interpreting Mass and Radius Measurements of Neutron Stars with Dark Matter Halos
Authors: Shafayat Shawqi, Sharon M. Morsink
Figure caption: Density and mass distributions for DANSs with a varying DM self-interaction parameter y and constant m  χ  = 1 GeV, f  χ  = 0.05, and baryonic EOS NL3ωρL55. Descriptions of symbols and line styles are the same as for Figure 1.
Paper: Almost All Carbon/Oxygen White Dwarfs Can Host Double Detonations
Authors: Ken J. Shen, Samuel J. Boos, Dean M. Townsley
Figure caption: Profiles vs. distance behind the shock front of a steady-state detonation. The upstream unburned fuel has equal mass fractions of 4He and 12C and a density of 1.6 × 105 g cm−3. The top panel shows mass fractions of selected isotopes, and the bottom panel shows the sound speed and rest-frame fluid velocity (in units of 104 km s−1) and the energy generation rate normalized to the maximum value, ﹩\epsilon /{\epsilon }_{\max }﹩. The dotted line shows the location where the rest-frame fluid velocity is equal to the sound speed.
Paper: Almost All Carbon/Oxygen White Dwarfs Can Host Double Detonations
Authors: Ken J. Shen, Samuel J. Boos, Dean M. Townsley
Figure caption: Resolution study for a detonation with the same initial conditions as for the calculation shown in Figure 4. The detonation velocity in units of 104 km s−1 is shown in blue, and the sonic length scale in kilometers is shown in orange. The green dotted line is 3 times the minimum cell size in kilometers.
Paper: Almost All Carbon/Oxygen White Dwarfs Can Host Double Detonations
Authors: Ken J. Shen, Samuel J. Boos, Dean M. Townsley
Figure caption: Various length scales vs. the density of the transition layer for the WD models discussed in Section 2. The pressure scale height is shown in blue, with each mass as labeled. The orange line shows the sonic length scale assuming equal mass fractions of 4He and 12C, and the purple line shows the length scale between the shock and the location of maximal energy generation.
Paper: Almost All Carbon/Oxygen White Dwarfs Can Host Double Detonations
Authors: Ken J. Shen, Samuel J. Boos, Dean M. Townsley
Figure caption: Temperatures (colors) and helium mass fractions (green contours) for six snapshots of a 0.5 M ⊙ double detonation simulation. Helium mass fraction contours increase linearly from a value of 0.1 to 0.9 from dark to light.
Paper: Almost All Carbon/Oxygen White Dwarfs Can Host Double Detonations
Authors: Ken J. Shen, Samuel J. Boos, Dean M. Townsley
Figure caption: Length scales vs. added mass for 1.0 (top panel) and 1.1 M ⊙ (bottom panel) WDs. The pressure scale heights at the transition radius are shown as blue lines, and the orange lines demarcate the sonic length scale at the transition radius’s density. Crosses and circles represent 3 times the minimum cell size for simulations with failed and successful detonations, respectively.
Paper: Almost All Carbon/Oxygen White Dwarfs Can Host Double Detonations
Authors: Ken J. Shen, Samuel J. Boos, Dean M. Townsley
Figure caption: Various length scales vs. total WD mass. The blue line shows the pressure scale height measured at the transition layer. The sonic length scale of a detonation powered by helium/carbon fuel at the transition layer density is shown in orange. Crosses and circles show 3 times the minimum cell size for two-dimensional simulations with failed and successful detonations, respectively.
Paper: Almost All Carbon/Oxygen White Dwarfs Can Host Double Detonations
Authors: Ken J. Shen, Samuel J. Boos, Dean M. Townsley
Figure caption: Total mass of 4He (M He,tot) and mass above the transition layer (M He,transition) vs. WD mass.
Paper: Unravelling the Asphericities in the Explosion and Multifaceted Circumstellar Matter of SN 2023ixf
Authors: Avinash Singh, Rishabh Singh Teja, Takashi J. Moriya, Keiichi Maeda, Koji S Kawabata, Masaomi Tanaka, Ryo Imazawa, Tatsuya Nakaoka, Anjasha Gangopadhyay, Masayuki Yamanaka, Vishwajeet Swain, D. K. Sahu, G. C. Anupama, Brajesh Kumar, Ramya M. Anche, Yasuo Sano, A. Raj, V. K. Agnihotri, Varun Bhalerao, D. Bisht, M. S. Bisht, K. Belwal, S. K. Chakrabarti, Mitsugu Fujii, Takahiro Nagayama, Katsura Matsumoto, Taisei Hamada, Miho Kawabata, Amit Kumar, Ravi Kumar, Brian K. Malkan, Paul Smith, Yuta Sakagami, Kenta Taguchi, Nozomu Tominaga, Arata Watanabe
Figure caption: Panel (A): Pseudobolometric light curves of SN 2023ixf computed in multiple wavelength bins. Panel (B): Temporal evolution of UV and NIR flux fraction in SN 2023ixf. Panel (C): Temperature and radius evolution of SN 2023ixf estimated from blackbody fits to the UVOIR data (0.16–2.35 μm). The radius of the line-forming region, i.e., the photospheric radius estimated from Fe II, is overplotted.
Paper: Unravelling the Asphericities in the Explosion and Multifaceted Circumstellar Matter of SN 2023ixf
Authors: Avinash Singh, Rishabh Singh Teja, Takashi J. Moriya, Keiichi Maeda, Koji S Kawabata, Masaomi Tanaka, Ryo Imazawa, Tatsuya Nakaoka, Anjasha Gangopadhyay, Masayuki Yamanaka, Vishwajeet Swain, D. K. Sahu, G. C. Anupama, Brajesh Kumar, Ramya M. Anche, Yasuo Sano, A. Raj, V. K. Agnihotri, Varun Bhalerao, D. Bisht, M. S. Bisht, K. Belwal, S. K. Chakrabarti, Mitsugu Fujii, Takahiro Nagayama, Katsura Matsumoto, Taisei Hamada, Miho Kawabata, Amit Kumar, Ravi Kumar, Brian K. Malkan, Paul Smith, Yuta Sakagami, Kenta Taguchi, Nozomu Tominaga, Arata Watanabe
Figure caption: Multiwavelength photometry of SN 2023ixf spanning UV, optical, and NIR wavelengths. Template subtraction was performed only in the UV bands (UVW2, UVM2, and UVW1) due to non-negligible contamination. The left-hand panel provides a close-up of the initial rise across all bands, annotated as blue peak and red shoulder, and the subsequent red peak.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Unravelling the Asphericities in the Explosion and Multifaceted Circumstellar Matter of SN 2023ixf
Authors: Avinash Singh, Rishabh Singh Teja, Takashi J. Moriya, Keiichi Maeda, Koji S Kawabata, Masaomi Tanaka, Ryo Imazawa, Tatsuya Nakaoka, Anjasha Gangopadhyay, Masayuki Yamanaka, Vishwajeet Swain, D. K. Sahu, G. C. Anupama, Brajesh Kumar, Ramya M. Anche, Yasuo Sano, A. Raj, V. K. Agnihotri, Varun Bhalerao, D. Bisht, M. S. Bisht, K. Belwal, S. K. Chakrabarti, Mitsugu Fujii, Takahiro Nagayama, Katsura Matsumoto, Taisei Hamada, Miho Kawabata, Amit Kumar, Ravi Kumar, Brian K. Malkan, Paul Smith, Yuta Sakagami, Kenta Taguchi, Nozomu Tominaga, Arata Watanabe
Figure caption: Comparison of absolute magnitude light curves (in AB-mag) of SN 2023ixf in UVW2 and V bands along with the UVW1 − V color evolution compared to other SNe II showing CSM interaction signatures.
Paper: Unravelling the Asphericities in the Explosion and Multifaceted Circumstellar Matter of SN 2023ixf
Authors: Avinash Singh, Rishabh Singh Teja, Takashi J. Moriya, Keiichi Maeda, Koji S Kawabata, Masaomi Tanaka, Ryo Imazawa, Tatsuya Nakaoka, Anjasha Gangopadhyay, Masayuki Yamanaka, Vishwajeet Swain, D. K. Sahu, G. C. Anupama, Brajesh Kumar, Ramya M. Anche, Yasuo Sano, A. Raj, V. K. Agnihotri, Varun Bhalerao, D. Bisht, M. S. Bisht, K. Belwal, S. K. Chakrabarti, Mitsugu Fujii, Takahiro Nagayama, Katsura Matsumoto, Taisei Hamada, Miho Kawabata, Amit Kumar, Ravi Kumar, Brian K. Malkan, Paul Smith, Yuta Sakagami, Kenta Taguchi, Nozomu Tominaga, Arata Watanabe
Figure caption: Color composite image (RGB) of the host galaxy M 101 using ﹩r^{\prime} ﹩ (red), ﹩g^{\prime} ﹩ (green), and ﹩u^{\prime} ﹩ (blue) acquired from 2 m HCT. SN 2023ixf and the nearby Giant H II region NGC 5461 are labeled.
Paper: Forecasts for Helium Reionization Detection with Fast Radio Bursts in the Era of Square Kilometre Array
Authors: Jun-Jie Wei, Chong-Yu Gao
Figure caption: Sensitivity of the cosmic DMIGM(z) function to He II reionization. A sudden He II reionization is assumed to occur at redshift ﹩{z}_{\mathrm{re}}=3,4﹩, and 6. The inset illustrates a zoomed-in view of the separation among different model curves.
Paper: A Model for Flux Rope Formation and Disconnection in Pseudostreamer Coronal Mass Ejections
Authors: P. F. Wyper, B. J. Lynch, C. R. DeVore, P. Kumar, S. K. Antiochos, L. K. S. Daldorff
Figure caption: (a) Free magnetic (E  m , blue) and kinetic (E  k , red) energies. Gray: Time profile of the driving (scaled to fit on the plot). Blue shading highlights the flux rope disconnection period. (b) Average number of turns within the flux rope (〈T  w 〉, black) and the decay index at the flux rope axis (n, red). (c) Flux rope flux (ΦFR, black) and cumulative interchange-reconnected flux (Φint, red), normalized by the total closed-field flux (Φtot). (d) Rates of change of these normalized fluxes (same color scheme). Green: Normalized closed-field reconnection rate obtained by calculating the swept-over flare-ribbon flux (see text for details). HFT = hyperbolic flux tube; FR = flux rope.
Paper: A Model for Flux Rope Formation and Disconnection in Pseudostreamer Coronal Mass Ejections
Authors: P. F. Wyper, B. J. Lynch, C. R. DeVore, P. Kumar, S. K. Antiochos, L. K. S. Daldorff
Figure caption: Flux ropes formed following the second phase of interchange reconnection at t = 12 hr 30 minutes. Light blue/cyan shows the flux tube with the twist of the original rope. Other twisted flux tubes are formed from plasmoids ejected as part of the bursty interchange reconnection process. (a) Close-in view of the flux ropes; note that the yellow field lines showing the original rope foot points are now closed. (b) Farther-out view showing how the flux ropes wrap into the CME structure. (c) Cut showing the large-scale rotation of the field lines.
Paper: A Model for Flux Rope Formation and Disconnection in Pseudostreamer Coronal Mass Ejections
Authors: P. F. Wyper, B. J. Lynch, C. R. DeVore, P. Kumar, S. K. Antiochos, L. K. S. Daldorff
Figure caption: (a) Shading shows v  r  in the plane ϕ = 0 at t = 9 hr 35 minutes. The white line shows the path along which the CME front speed is calculated. The red arrow shows the position of the front at this time. The purple field line shows the flux rope axis. The blue arrow shows the highest point of this field line. (b) Radial positions of the front (red) and the highest point of the axis field line (blue). (c) Radial speeds: V front (red), V axis (blue).
Paper: A Model for Flux Rope Formation and Disconnection in Pseudostreamer Coronal Mass Ejections
Authors: P. F. Wyper, B. J. Lynch, C. R. DeVore, P. Kumar, S. K. Antiochos, L. K. S. Daldorff
Figure caption:  ρ (left), v  r  (middle), and v  ϕ  (right) in a cut (ϕ = 6°) through the CME at different times.
Paper: A Model for Flux Rope Formation and Disconnection in Pseudostreamer Coronal Mass Ejections
Authors: P. F. Wyper, B. J. Lynch, C. R. DeVore, P. Kumar, S. K. Antiochos, L. K. S. Daldorff
Figure caption: Second stage of CME flux rope disconnection. The top panels show field lines extending into the CME traced from the surface. The bottom panels show a close-up view (from the side) of the same field lines at the same time showing the re-closing of the yellow field lines and the shift in the CME flux rope foot points to the cyan field lines.
Paper: A Model for Flux Rope Formation and Disconnection in Pseudostreamer Coronal Mass Ejections
Authors: P. F. Wyper, B. J. Lynch, C. R. DeVore, P. Kumar, S. K. Antiochos, L. K. S. Daldorff
Figure caption: Flux rope disconnection in the jet simulation. (a) Isosurface of normalized current density (J/c = 1.2 G) shaded by the radial component (J  r /c). (b)–(d) Field line evolution showing the flux rope disconnection.
Paper: Characterizing the Molecular Gas in Infrared Bright Galaxies with CARMA
Authors: Katherine Alatalo, Andreea O. Petric, Lauranne Lanz, Kate Rowlands, Vivian U, Kirsten L. Larson, Lee Armus, Loreto Barcos-Muñoz, Aaron S. Evans, Jin Koda, Yuanze Luo, Anne M. Medling, Kristina E. Nyland, Justin A. Otter, Pallavi Patil, Fernando Peñaloza, Diane Salim, David B. Sanders, Elizaveta Sazonova, Maya Skarbinski, Yiqing Song, Ezequiel Treister, C. Meg Urry
Figure caption: The gas-to-dust ratio for all CARMA GOALS sources labeled based on their merger classification from A. O. Petric et al. (2018): red squares for “m”/mergers, orange hexagons for “em”/early-mergers, and blue circles for “nm”/nonmergers. With the left-hand plot using the standard Milky Way conversion factor (α = 4). The range of gas-to-dust ratios for normal star-forming galaxies from K. M. Sandstrom et al. (2013) is shaded in gray. If we assume that L CO-to-M(H2) conversion is not consistent with a Milky Way conversion and use the conversion from R. Herrero-Illana et al. (2019), we find that the measured gas-to-dust ratios in our sources are much more consistent with the range found in normal galaxies. The plot on the right-hand side uses the α CO determined for GOALS sources in R. Herrero-Illana et al. (2019).
Paper: Characterizing the Molecular Gas in Infrared Bright Galaxies with CARMA
Authors: Katherine Alatalo, Andreea O. Petric, Lauranne Lanz, Kate Rowlands, Vivian U, Kirsten L. Larson, Lee Armus, Loreto Barcos-Muñoz, Aaron S. Evans, Jin Koda, Yuanze Luo, Anne M. Medling, Kristina E. Nyland, Justin A. Otter, Pallavi Patil, Fernando Peñaloza, Diane Salim, David B. Sanders, Elizaveta Sazonova, Maya Skarbinski, Yiqing Song, Ezequiel Treister, C. Meg Urry
Figure caption: The Schmidt–Kennicutt relation (R.C. Kennicutt 1998) for the CARMA GOALS sample (color-coded by gas-to-dust ratio), with comparisons to normal star-forming galaxies (black triangles; R.C. Kennicutt 1998 and black circles; D. B. Fisher et al. 2013), bulges (gray circles; D. B. Fisher et al. 2013), early-type galaxies (teal squares; T. A. Davis et al. 2014), Hickson Compact Group galaxies (blue hexagons; K. Alatalo et al. 2015a), high-redshift galaxies (gray diamonds; R. Genzel et al. 2010), and radio galaxies (black squares; P. Ogle et al. 2010). The diagonal lines represent the 10× and 100× deviations from the average relation. All SFRs have been normalized to the Chabrier initial mass function (G. Chabrier 2003).
Paper: Characterizing the Molecular Gas in Infrared Bright Galaxies with CARMA
Authors: Katherine Alatalo, Andreea O. Petric, Lauranne Lanz, Kate Rowlands, Vivian U, Kirsten L. Larson, Lee Armus, Loreto Barcos-Muñoz, Aaron S. Evans, Jin Koda, Yuanze Luo, Anne M. Medling, Kristina E. Nyland, Justin A. Otter, Pallavi Patil, Fernando Peñaloza, Diane Salim, David B. Sanders, Elizaveta Sazonova, Maya Skarbinski, Yiqing Song, Ezequiel Treister, C. Meg Urry
Figure caption: The moment0 maps of CO(1–0) of the 28 CARMA GOALS galaxies overlaid atop the three-color Spitzer 3.6–4.5–8.0 μm image. The white bar in the lower left-hand corner demarcates 10″ in each field. The beam is shown in the lower right-hand corner in white. The red-hued portions of the Spitzer map show the locations of the PAH emission, which matches the positions of the molecular gas quite well.
Paper: Characterizing the Molecular Gas in Infrared Bright Galaxies with CARMA
Authors: Katherine Alatalo, Andreea O. Petric, Lauranne Lanz, Kate Rowlands, Vivian U, Kirsten L. Larson, Lee Armus, Loreto Barcos-Muñoz, Aaron S. Evans, Jin Koda, Yuanze Luo, Anne M. Medling, Kristina E. Nyland, Justin A. Otter, Pallavi Patil, Fernando Peñaloza, Diane Salim, David B. Sanders, Elizaveta Sazonova, Maya Skarbinski, Yiqing Song, Ezequiel Treister, C. Meg Urry
Figure caption: The molecular gas fraction for all the CARMA GOALs sources, labeled based on their merger classification from A. O. Petric et al. (2018): red squares for “m”/mergers, orange hexagons for “em”/early-mergers, and blue circles for “nm”/nonmergers. There is a noticeable trend that higher SFRs also contain higher molecular gas fractions.
Paper: Characterizing the Molecular Gas in Infrared Bright Galaxies with CARMA
Authors: Katherine Alatalo, Andreea O. Petric, Lauranne Lanz, Kate Rowlands, Vivian U, Kirsten L. Larson, Lee Armus, Loreto Barcos-Muñoz, Aaron S. Evans, Jin Koda, Yuanze Luo, Anne M. Medling, Kristina E. Nyland, Justin A. Otter, Pallavi Patil, Fernando Peñaloza, Diane Salim, David B. Sanders, Elizaveta Sazonova, Maya Skarbinski, Yiqing Song, Ezequiel Treister, C. Meg Urry
Figure caption: PV diagrams of double sources, including UGC 02369 (top row), CGCG 468-002 (second row), VV 250 (third row), CGCG 142-034 (fourth row), and NGC 6670 (bottom row). The correlator edge is seen in UGC 02369N, and it is likely that some of the flux is missing from that source.
Paper: Characterizing the Molecular Gas in Infrared Bright Galaxies with CARMA
Authors: Katherine Alatalo, Andreea O. Petric, Lauranne Lanz, Kate Rowlands, Vivian U, Kirsten L. Larson, Lee Armus, Loreto Barcos-Muñoz, Aaron S. Evans, Jin Koda, Yuanze Luo, Anne M. Medling, Kristina E. Nyland, Justin A. Otter, Pallavi Patil, Fernando Peñaloza, Diane Salim, David B. Sanders, Elizaveta Sazonova, Maya Skarbinski, Yiqing Song, Ezequiel Treister, C. Meg Urry
Figure caption: PV diagrams for the CARMA GOALS sample
Paper:  MEDEA: A New Model for Emulating Radio Antenna Beam Patterns for 21 cm Cosmology and Antenna Design Studies
Authors: Joshua J. Hibbard, Bang D. Nhan, David Rapetti, Jack O. Burns
Figure caption: The first five Cryo-coefficients’ power plotted as a function of beam hyperparameter for each antenna case study and at three representative frequencies. The different colors label the different coefficients k  l , while the filled circles represent the low band, the plus signs the mid-band, and the filled triangles the high-band frequency beams; the exact frequencies represented are shown in the legend for each antenna case. The black-filled stars correspond to the points in the set K  T  that are tested for interpolation, while the solid lines are quintic splines fit to the input sets K  I−1, which do not contain the test set of coefficients.
Paper:  MEDEA: A New Model for Emulating Radio Antenna Beam Patterns for 21 cm Cosmology and Antenna Design Studies
Authors: Joshua J. Hibbard, Bang D. Nhan, David Rapetti, Jack O. Burns
Figure caption: Polar plots of the non-normalized linear gains for the analytically and numerically simulated beam patterns. The analytical dipole at its mid-band frequency is shown in the top panel as a function of hyperparameter h. The middle panel shows the patch antenna at 84 MHz and the bottom shows the ROLSES dipole at 15 MHz. Both of the latter two beams are simulated numerically in CST for different values of the lunar regolith dielectric constant, ϵ, with darker colors denoting lower values and lighter colors higher values. The left column of each panel shows the E-plane cut, while the right column shows the H-plane cut. Note that the ROLSES dipole is highly nonlinear in dielectric space, due to the fact that the antenna design is not optimized for the 1–30 MHz band. We only show the bottom half (θ ≤ 90°) of the polar plots.