adsabs/AstroCLIMB huggingface dataset:
Paper: The Cavity of 3CR 196.1: Hα Emission Spatially Associated with an X-Ray Cavity
Authors: A. Jimenez-Gallardo, E. Sani, F. Ricci, C. Mazzucchelli, B. Balmaverde, F. Massaro, A. Capetti, W. R. Forman, R. P. Kraft, G. Venturi, M. Gendron-Marsolais, M. A. Prieto, A. Marconi, H. A. Peña-Herazo, S. A. Baum, C. P. O'Dea, L. Lovisari, R. Gilli, E. Torresi, A. Paggi, V. Missaglia, G. R. Tremblay, B. J. Wilkes
Figure caption: Fit to the spectrum extracted from region b (i.e., a 1 arcsec2 region, as shown in the right panel of Figure 1) using one Hα + [N II]λ6584 at the rest frame (yellow) and another one redshifted by ∼21 Å. The uncertainties in the spectrum are shown in gray. The spectra in region b (see right panel of Figure 1) cannot be reproduced using a single triplet.
Paper: The Cavity of 3CR 196.1: Hα Emission Spatially Associated with an X-Ray Cavity
Authors: A. Jimenez-Gallardo, E. Sani, F. Ricci, C. Mazzucchelli, B. Balmaverde, F. Massaro, A. Capetti, W. R. Forman, R. P. Kraft, G. Venturi, M. Gendron-Marsolais, M. A. Prieto, A. Marconi, H. A. Peña-Herazo, S. A. Baum, C. P. O'Dea, L. Lovisari, R. Gilli, E. Torresi, A. Paggi, V. Missaglia, G. R. Tremblay, B. J. Wilkes
Figure caption: Flux (left), velocity (middle), and velocity dispersion (right) maps with 8.4 GHz VLA (black) and exposure-corrected 0.7-2 keV Chandra (blue) contours overlaid for the Hβ, [O III]λ λ4960, 5008, [O I]λ6300, Hα, [N II]λ λ6548, 6584, and [S II]λ λ6718, 6733 emission lines. MUSE images have a pixel size of 0.4 arcsec/pixel. 8.4 GHz VLA contours were drawn at 5, 20, and 50 times the rms level of the background. Chandra contours were smoothed with a 1.5″ Gaussian kernel radius and drawn in blue at 0.25  ·   10−15 erg cm−2 s−1. Flux maps have units of 10−17 erg cm−2  s−1, while velocity and velocity dispersion maps have units of km s−1.
Paper: The Cavity of 3CR 196.1: Hα Emission Spatially Associated with an X-Ray Cavity
Authors: A. Jimenez-Gallardo, E. Sani, F. Ricci, C. Mazzucchelli, B. Balmaverde, F. Massaro, A. Capetti, W. R. Forman, R. P. Kraft, G. Venturi, M. Gendron-Marsolais, M. A. Prieto, A. Marconi, H. A. Peña-Herazo, S. A. Baum, C. P. O'Dea, L. Lovisari, R. Gilli, E. Torresi, A. Paggi, V. Missaglia, G. R. Tremblay, B. J. Wilkes
Figure caption:  r-band Pan-STARRS image with MUSE 4800–6800 Å (red) and MUSE Hα + [N II]λ6584 (blue) contours overlaid. Sources SRC1 to SRC4 were used to compute the shift applied, while sources SRC5 to SRC8 allowed us to verify the registration. MUSE images have a pixel size of 0.″2. 4800–6800 Å contours were drawn at 20, 50, and 200 times the rms level of the background. Hα+[N II]λ6584 contours were drawn at 5, 10, 20, 50, and 100 times the rms level of the background. We found a good alignment between the Pan-STARRS and the MUSE emission applying a shift o 3.″1 (i.e., ∼10 kpc).
Paper: Luminous Supernovae: Unveiling a Population between Superluminous and Normal Core-collapse Supernovae
Authors: Sebastian Gomez, Edo Berger, Matt Nicholl, Peter K. Blanchard, Griffin Hosseinzadeh
Figure caption: Representative spectra for all the Gold and Silver LSNe that have spectra available within ±10 days of peak, sorted by color and spectral features. We find that LSNe appear to form a continuous distribution, from blue SLSN-like spectra to red SN Ic-like spectra. Individual references for each spectrum are listed in Appendix A.
Paper: Luminous Supernovae: Unveiling a Population between Superluminous and Normal Core-collapse Supernovae
Authors: Sebastian Gomez, Edo Berger, Matt Nicholl, Peter K. Blanchard, Griffin Hosseinzadeh
Figure caption: Light curves of all the Gold and Silver LSNe in our sample. The individual data points are r-band magnitudes of the SNe, and the lines are the corresponding best-fit models described in Section 3. The shaded regions represent the 1σ, 2σ, and 3σ intervals for typical light curves of SLSNe (blue) and SNe Ic (red) obtained from averaging their light-curve models.
Paper: The Host Galaxies of Hybrid Morphology Radio Sources
Authors: Andra Stroe, Victoria Catlett, Jeremy J. Harwood, Tessa Vernstrom, Beatriz Mingo
Figure caption: The Kauffmann et al. (2003) and Kewley et al. (2001) lines separate star-forming galaxies, composites, and AGN in the BPT diagram (Baldwin et al. 1981). The high [O III]/Hb narrow-line ratios securely classify J1348+286, J1313+507, and J1315+516 as Seyferts, even in the absence of [N II]/Hα coverage. Given their high redshift of z > 1, none of the four required emission lines are covered for J1206+503 and J1154+513. The contours represent 10,000 sources sampled from SDSS DR7 (Abazajian et al. 2009).
Paper: The Host Galaxies of Hybrid Morphology Radio Sources
Authors: Andra Stroe, Victoria Catlett, Jeremy J. Harwood, Tessa Vernstrom, Beatriz Mingo
Figure caption: The five HyMoRS in our sample. The background images are Pan-STARRS RGB composites (using g, r, i filters), with overlaid L-band VLA contours at σ rms × 2 n . Each image shows the host galaxy (zoomed-in section) with an FR I–like plume on one side and an FR II jet, hotspot, and lobe on the other.
Paper: The Host Galaxies of Hybrid Morphology Radio Sources
Authors: Andra Stroe, Victoria Catlett, Jeremy J. Harwood, Tessa Vernstrom, Beatriz Mingo
Figure caption: WISE W1–W2 vs. W2–W3 color–color plot, including the Mingo et al. (2016, 2022) lines that separate elliptical, spiral, and starburst galaxies, and active galactic nuclei (AGN). The four sources with secure WISE measurements are securely located in the AGN quadrant of this plot, where the bulk of FR IIs reside (Mingo et al. 2022).
Paper: The Host Galaxies of Hybrid Morphology Radio Sources
Authors: Andra Stroe, Victoria Catlett, Jeremy J. Harwood, Tessa Vernstrom, Beatriz Mingo
Figure caption: HyMoRS spectra with a selection of emission lines marked (gray vertical lines). Gaussian emission line fits are overplotted in the purple lines. All of our sources have prominent narrow and broad emission lines typical of Type 2 AGN and quasars, with [O II] emission suggesting significant SFRs. The line luminosities and velocity FWHMs are listed in Tables 2 and 3, respectively.
Paper: Successive Interacting Coronal Mass Ejections: How to Create a Perfect Storm
Authors: G. J. Koehn, R. T. Desai, E. E. Davies, R. J. Forsyth, J. P. Eastwood, S. Poedts
Figure caption: Magnetic field lines of (a) the initialized spheromak and (b) after 60 minutes of evolution, in static heliospheric conditions representative of conditions 0.1 au. The color is proportional to the normalized magnetic field magnitude.
Paper: Successive Interacting Coronal Mass Ejections: How to Create a Perfect Storm
Authors: G. J. Koehn, R. T. Desai, E. E. Davies, R. J. Forsyth, J. P. Eastwood, S. Poedts
Figure caption: Density profile and magnetic field lines (red) in the steady-state heliosphere from (a) the equatorial plane and (b) showing both the meridional and equatorial planes.
Paper: Temperature Structures Associated with Different Components of the Atmospheric Circulation on Tidally Locked Exoplanets
Authors: Neil T. Lewis, Mark Hammond
Figure caption: Geopotential height anomaly z − z0 (contours) and horizontal velocity (quivers) at p = 480 hPa for each GCM simulation. For each simulation, full fields are shown in the top row. The next three rows show the zonal-mean rotational circulation, eddy-rotational circulation, and divergent circulation. Note that the circulation in the P = ∞ day simulation has no rotational component. For reference, z 0∣ p=480 hPa = 5805, 5822, 5863, and 5889 m, for the P = 4, 8, 16, and ∞  day simulations, respectively.
Paper: Temperature Structures Associated with Different Components of the Atmospheric Circulation on Tidally Locked Exoplanets
Authors: Neil T. Lewis, Mark Hammond
Figure caption: Geopotential height anomaly z − z 0(p) (contours) and velocity (u, ω; quivers) in the longitude–pressure plane, averaged between ±40° latitude, shown for each GCM simulation. The top row shows the full circulation. Contributions to the full circulation from the eddy-rotational and divergent components are shown in the next two rows. Data is averaged over the tropics only in order to show the baroclinic structure of the eddy-rotational wind.
Paper: A Large (≈ 1 pc) Contracting Envelope Around the Prestellar Core L1544 
Authors: Elena Redaelli, Ana Chacón-Tanarro, Paola Caselli, Mario Tafalla, Jaime E. Pineda, Silvia Spezzano, Olli Sipilä
Figure caption: Maps of the best-fit values obtained with the two-step fitting procedure with the Hill5 model implemented in PYSPECKIT. The panels refer to V lsr (top-left), V infall (top-right), σ V (bottom left), and ﹩{T}_{\mathrm{ex}}^{\mathrm{peak}}﹩ (bottom-right). The solid contours show the H2 column density, as in Figure 1 (note however that the maps have been zoomed in). In the bottom-right panel, the beam size and scalebar are also shown.
Paper: A Large (≈ 1 pc) Contracting Envelope Around the Prestellar Core L1544 
Authors: Elena Redaelli, Ana Chacón-Tanarro, Paola Caselli, Mario Tafalla, Jaime E. Pineda, Silvia Spezzano, Olli Sipilä
Figure caption: Histogram of the distribution of the difference between the centroid velocity of C18O and HCO+, as obtained with the single Gaussian and the Hill5 fit, respectively, in km s−1. The vertical solid line is the mean of the distribution, while the shaded gray area shows the 3σ interval around it.
Paper: A Large (≈ 1 pc) Contracting Envelope Around the Prestellar Core L1544 
Authors: Elena Redaelli, Ana Chacón-Tanarro, Paola Caselli, Mario Tafalla, Jaime E. Pineda, Silvia Spezzano, Olli Sipilä
Figure caption: Left panel: the observed (1–0) spectrum of C18O is shown in black, overlaid to the synthetic line profiles obtained with MOLLIE using different values for the external visual extinction: A V = 2 mag and A V = 5 mag are shown in blue and red, respectively. Right panel: same as in the left one, but for the (2–1) line.
Paper: A Large (≈ 1 pc) Contracting Envelope Around the Prestellar Core L1544 
Authors: Elena Redaelli, Ana Chacón-Tanarro, Paola Caselli, Mario Tafalla, Jaime E. Pineda, Silvia Spezzano, Olli Sipilä
Figure caption: Abundance profiles obtained for HC18O+ with our chemical code, at t = 1 Myr. The red, solid curve shows the model where a lower external visual extinction is implemented (A V = 2 mag), while the higher value A V = 5 mag is used to produce the dashed green line. The two profiles have been extended in the simulated envelope.
Paper: A Large (≈ 1 pc) Contracting Envelope Around the Prestellar Core L1544 
Authors: Elena Redaelli, Ana Chacón-Tanarro, Paola Caselli, Mario Tafalla, Jaime E. Pineda, Silvia Spezzano, Olli Sipilä
Figure caption: The central panel shows a zoom-in of the infall velocity map shown in Figure 11. The small panels show a selection of spectra at different positions (black histograms), with overlaid the best-fit solution found with the Hill5 model (red curves). The best-fit parameters are reported in the top-right corners. The bottom subpanels show the residuals of each fit.
Paper: A Large (≈ 1 pc) Contracting Envelope Around the Prestellar Core L1544 
Authors: Elena Redaelli, Ana Chacón-Tanarro, Paola Caselli, Mario Tafalla, Jaime E. Pineda, Silvia Spezzano, Olli Sipilä
Figure caption: Black histograms are the HCO+ spectra at the positions shown with black crosses in Figure 1, while red histograms show the corresponding C18O (2–1) spectra. The panel with the blue asterisk represents the spectrum at a millimeter dust peak. The data are the same as shown in Figure 2, but this time the intensity axis is unscaled and shows the observed values.
Paper: High-precision Nuclear Chronometer for the Cosmos
Authors: X. H. Wu, 鑫辉 吴, P. W. Zhao, 鹏巍 赵, S. Q. Zhang, 双全 张, J. Meng, 杰 孟
Figure caption: Ages estimated by the Th-U-X chronometer with different sets of nuclear physics inputs and for different stars. (a) Ages of the metal-poor J2038-0023 star estimated by the Th-U-X chronometer with nuclear physics inputs based on mass tables, WS4, DZ28, FRDM2012, and HFB24. The shadow region represents the uncertainty of estimated ages, and the black line represents the central values. (b) Ages of different metal-poor stars, i.e., CS31082-001, BD17°3248, HE1523-0901, J2038-0023, CS29497-004, and J0954+5246, estimated by the Th-U-X chronometer. The lengths of the rectangles represent the uncertainties from the theoretical simulations of initial elemental abundances, and the error bars stand for the uncertainties from the observations of present elemental abundances. The gray band shows the cosmic age of 13.8 Gyr with the uncertainty from the studies of microwave background radiation (Aghanim et al. 2020), and the pink band shows the age of 11.4 Gyr with the uncertainty from the recent gravitational lenses measurement (Jee et al. 2019).
Paper: High-precision Nuclear Chronometer for the Cosmos
Authors: X. H. Wu, 鑫辉 吴, P. W. Zhao, 鹏巍 赵, S. Q. Zhang, 双全 张, J. Meng, 杰 孟
Figure caption: Chemical abundances from the r-process simulations with different astrophysical conditions, i.e., Y  e  and S final, in comparison with the observed abundances of the metal-poor star J2038-0023 (Placco et al. 2017). The nuclear physics inputs are based on the WS4 mass model (Wang et al. 2014). (a) Fix the electron abundance Y  e  = 0.45 and vary the entropy S final from 275 to 400. The results with S final < 290 are shown with dashed lines. (b) Fix S final = 300 and vary Y  e  from 0.40 to 0.48. The results with Y  e  > 0.465 are shown with dashed lines.
Paper: High-precision Nuclear Chronometer for the Cosmos
Authors: X. H. Wu, 鑫辉 吴, P. W. Zhao, 鹏巍 赵, S. Q. Zhang, 双全 张, J. Meng, 杰 孟
Figure caption: Chemical abundances from the r-process simulations based on different nuclear physics inputs with fixed electron abundance Y  e  = 0.45, in comparison with the observed abundances of the metal-poor star J2038-0023. (a) Fix the entropy S final = 300. (b) The entropy S final is determined respectively for each set of nuclear physics inputs by the synchronization requirement of Th/X, U/X, and Th/U chronometers.
Paper: High-precision Nuclear Chronometer for the Cosmos
Authors: X. H. Wu, 鑫辉 吴, P. W. Zhao, 鹏巍 赵, S. Q. Zhang, 双全 张, J. Meng, 杰 孟
Figure caption: Estimated ages of the metal-poor star J2038-0023 with the Th/U chronometer under different astrophysical conditions (Y  e , S final) are represented by different squares with colors standing for the values. The ages after synchronizing the Th/X, U/X, and Th/U chronometers, i.e., the ages estimated by the Th-U-X chronometer, are highlighted with open black boxes. Gray squares stand for the excluded astrophysical conditions.
Paper: High-precision Nuclear Chronometer for the Cosmos
Authors: X. H. Wu, 鑫辉 吴, P. W. Zhao, 鹏巍 赵, S. Q. Zhang, 双全 张, J. Meng, 杰 孟
Figure caption: Ages of the metal-poor star J2038-0023 estimated by the Th/X, U/X, and Th/U chronometers with a fixed electron abundance Y  e  = 0.45 as functions of the entropy S final. The synchronization is achieved when the stellar ages estimated by the three chronometers are consistent.
Paper: Dust Rings and Cavities in the Protoplanetary Disks around HD 163296 and DoAr 44
Authors: Harrison Leiendecker, Hannah Jang-Condell, Neal J. Turner, Adam D. Myers
Figure caption: Top: dust surface density of the best-fitting model to the ALMA observation of DoAr 44. The three separate ring components are depicted as dashed lines. Middle: surface brightness of ALMA observation with shaded errors and the model at 1.3 mm. Bottom: surface brightness of the SPHERE observation, with shaded errors shown at 10× magnification (in order to be seen) and the model in H band. An additional model with a coronagraphic response function similar to the SPHERE data is also shown. The SPHERE data are not flux-calibrated, so they have been scaled to the same maximum value as our model with the coronagraphic response. Dimmer regions of the SPHERE observation have been excluded from this azimuthal average.
Paper: Dust Rings and Cavities in the Protoplanetary Disks around HD 163296 and DoAr 44
Authors: Harrison Leiendecker, Hannah Jang-Condell, Neal J. Turner, Adam D. Myers
Figure caption: Contour plots of model χ 2 values for the parameters of the inner ring of HD 163296. Contours are plotted for 1σ (purple), 2σ (blue), and 3σ (green) deviations from the best fit. The best fit is marked with a red cross in each plot. For each contour plot, the best-fit value was used for the unplotted parameter. Panels (a) and (b) show little correlated error between those variables, but there is a significant degeneracy in panel (c) between the ring width and surface density.
Paper: Dust Rings and Cavities in the Protoplanetary Disks around HD 163296 and DoAr 44
Authors: Harrison Leiendecker, Hannah Jang-Condell, Neal J. Turner, Adam D. Myers
Figure caption: Selected contours from χ 2 fitting that demonstrate correlation of Σ d,2 vs. (a) Σ d,3, (b) Σ d,1, and (c) σ 3. Contours are plotted for 1σ (purple), 2σ (blue), and 3σ (green) deviations from the best fit. The best fit is marked with a red cross in each plot. For each contour, the unused ring parameters are set to their best-fit values. Each contour shows some degeneracy between the variables, but it is most clearly demonstrated in panel (c).
Paper: Dust Rings and Cavities in the Protoplanetary Disks around HD 163296 and DoAr 44
Authors: Harrison Leiendecker, Hannah Jang-Condell, Neal J. Turner, Adam D. Myers
Figure caption: Left and middle: mass limits on the possible planets at 50 and 85 au, respectively, around HD 163296 as a function of the viscosity parameter α. Right: a lower mass limit on planet masses in DoAr 44 that would be massive enough to create the observed cavity. The dashed line at 1.6 M J represents a tentative upper limit for a putative optically thick CPD.
Paper: Dust Rings and Cavities in the Protoplanetary Disks around HD 163296 and DoAr 44
Authors: Harrison Leiendecker, Hannah Jang-Condell, Neal J. Turner, Adam D. Myers
Figure caption: Surface brightness of the thermal emission from (a) the 1.3 mm ALMA image of DoAr 44 (Cieza et al. 2021) and (b) the synthetic 1.3 mm data from our best-fitting model. An ellipse marks the beam size in the upper right of the ALMA observation. The approximate stellar location is marked by a red circle. Modeling the ring-skirt morphology as three overlaid Gaussian rings gives a good replica of the ALMA observation.
Paper: Dust Rings and Cavities in the Protoplanetary Disks around HD 163296 and DoAr 44
Authors: Harrison Leiendecker, Hannah Jang-Condell, Neal J. Turner, Adam D. Myers
Figure caption: Top: temperature map of the best-fitting model to the ALMA observation of DoAr 44. The scattering surface of the disk is displayed in red. Labeled isotherms are shown with dashed white lines. As with Figure 5, there is a significantly low density region in the upper left corner for which the temperature cannot be properly calculated using our model assumptions. Bottom: midplane temperature of the model. There is a subtle increase in temperature around the model’s peak surface density at the bright middle ring.
Paper: Dust Rings and Cavities in the Protoplanetary Disks around HD 163296 and DoAr 44
Authors: Harrison Leiendecker, Hannah Jang-Condell, Neal J. Turner, Adam D. Myers
Figure caption: (a) H-band SPHERE image of DoAr 44 (Avenhaus et al. 2018) and (b) synthetic data of scattered light from our best-fitting model. The surface brightness of the SPHERE data has been normalized since the data are not absolute-flux-calibrated. The 0.″1 SPHERE coronagraph (shown in gray) is displayed on both the H-band observation and the synthetic data. The approximate stellar location is marked by a red circle. The scattered light of both the disk and the best-fit model peaks inside of the cavity in thermal emission.
Paper: Dust Rings and Cavities in the Protoplanetary Disks around HD 163296 and DoAr 44
Authors: Harrison Leiendecker, Hannah Jang-Condell, Neal J. Turner, Adam D. Myers
Figure caption: Azimuthal variation of the normalized surface brightness of the bright ring around DoAr 44 observed with ALMA. The figure formatting is the same as in Figure 6.
Paper: Dust Rings and Cavities in the Protoplanetary Disks around HD 163296 and DoAr 44
Authors: Harrison Leiendecker, Hannah Jang-Condell, Neal J. Turner, Adam D. Myers
Figure caption: Same as Figure 8, but for the outer ring parameters.
Paper: Creating the Radius Gap without Mass Loss
Authors: Eve J. Lee, Amalia Karalis, Daniel P. Thorngren
Figure caption: Radius–total mass distribution in contour lines for the primordial population (orange) and for the photoevaporated population (green) for different f dep, both evolved to 3 Gyr. We plot the data from the NASA Exoplanet Archive (2021) (for mass measurement from radial velocity (circles) and from transit timing variation (triangles) with lighter colors denoting those with larger percentage error. The data points are filtered to those with measurement errors within 30%, orbital periods less than 500 days, masses less than 30M ⊕, and radius less than 10R ⊕. The two triangles of mass ∼4–6 M ⊕ and radius ∼10R ⊕ are Kepler-51c and d, which are known super-puffs that require special formation channels including gas accretion beyond ∼1 au (e.g., Lee & Chiang 2016).
Paper: Observed Rate Variations in Superflaring G-type Stars
Authors: James Crowley, Michael S. Wheatland, Kai Yang
Figure caption: Top: excerpt of light curve of TIC 364588501 of the first identified block of high flaring rate on the star, showing the relative flux (blue), quiescent luminosity model (orange), flares (crosses), and identified periods using minima from the model (blue lines). The star initially has complicated oscillations; however, starting with the fifth manually identified cycle (red; cycle 62 overall) the rotational modulation shows a more regular pattern. Bottom: adjusted phase map and phase distribution for the whole first block of high flaring rate, using the identified periods as above. The phase distribution is split between flares before cycle 5 (blue) and after cycle 5 (orange).
Paper: Deflection of O2 + Ion Flow by Magnetic Fields in the Martian Ionosphere
Authors: Shibang Li, Haoyu Lu, Jinbin Cao, Jun Cui, Chenling Zhou, James A. Wild, Guokan Li, Yun Li
Figure caption: Dayside ﹩{{\rm{O}}}_{2}^{+}﹩ ion velocity vector (black anchor) overlapped on isomagnetic lines (gray) of the Martian crustal field in the horizontal plane at 350 km, resulting from simulation with the G110 crustal field model.
Paper: Observed Rate Variations in Superflaring G-type Stars
Authors: James Crowley, Michael S. Wheatland, Kai Yang
Figure caption: Left: FFDs for the three rate-variable stars which were fitted using a simple power-law model, shown in log–log plots. Power-law fits are shown in black, with the uncertainty in the index shown in gray. Uncertainties in the bolometric energies of each flare are calculated following Günther et al. (2020). Uncertainties in the count of each point are given by Poissonian counting errors following Gehrels (1986). The distributions for each star have been given arbitrary vertical offsets, to avoid overlapping. Right: same, for the four rate-variable stars which were fitted using a simple power-law model with an energy threshold. Flares included in the fit are shown as darker circles. For each panel, the vertical axis represents the cumulative number of events with a larger energy, shown with a log scaling.
Paper: Deflection of O2 + Ion Flow by Magnetic Fields in the Martian Ionosphere
Authors: Shibang Li, Haoyu Lu, Jinbin Cao, Jun Cui, Chenling Zhou, James A. Wild, Guokan Li, Yun Li
Figure caption: Distributions of variables resulting from simulation with the G110 crustal field model at 350 km. The variation of (a) eastward velocity (U  φ ), (b) magnetic field inclination angle, (c) eastward total electromagnetic forces (F  φ , red line), and Hall electric force (green line) along latitude at longitude of 180°.