adsabs/AstroCLIMB huggingface dataset:
Paper: Far-side Active Regions Based on Helioseismic and EUV Measurements: A New Data Set for Heliospheric Machine Learning Advancements
Authors: Amr Hamada, Kiran Jain, Charles Lindsey, Mitchell Creelman, Niles Oien
Figure caption: Comparison of the GONG AR mean phase shift with (a) the EUV AR mean intensity and (b) with the corresponding minimum phase shift. The color refers to the AR area.
Paper: MHD Modeling of a Geoeffective Interplanetary Coronal Mass Ejection with the Magnetic Topology Informed by In Situ Observations
Authors: Elena Provornikova, Viacheslav G. Merkin, Angelos Vourlidas, Anna Malanushenko, Sarah E. Gibson, Eric Winter, Charles N. Arge
Figure caption: Summary of key imaging observations of the 2010 April 3 CME. (a) SOHO/Extreme Ultraviolet Imaging Telescope 195 Å channel running-difference image showing the source region and the extent of the post-CME arcade; (b) composite of STA/EUVI-195 Å and COR1 running-difference images showing the shape and direction of the CME in the inner corona; (c) base difference COR2-B and COR2-A snapshots showing the CME expanding northward toward the ecliptic in the middle corona; (d), (e) HI1-A and HI1-B running-difference snapshots showing that the northern part of the CME has crossed the ecliptic plan and the formation of a wave ahead of the CME.
Paper: Are There Black Hole Symbiotic X-Ray Binaries?
Authors: Zhu-Ling Deng, Xiang-Dong Li
Figure caption: Distributions of BH SyXBs in the companion mass vs. orbital period, BH mass vs. orbital period, eccentricity vs. orbital period, and X-ray luminosity vs. orbital period diagrams (from left to right) in the SNC0.25Vesc1Racc (upper panels) and SND0.25Vesc1Racc (lower panels) models. The cross and star represent Gaia BH1 and Gaia BH2 (K. El-Badry et al. 2023b, 2023a), respectively.
Paper: Are There Black Hole Symbiotic X-Ray Binaries?
Authors: Zhu-Ling Deng, Xiang-Dong Li
Figure caption: The characteristic radii R ISCO, R m (red), R CIRC (blue), and R ADAF (yellow) for BH (left) and NS (right) SyXBs. We adopt the BH mass of 10 M ☉, NS mass of 1.4 M ☉, companion mass of 2 M ☉, and radius of 10 R ☉, orbital separation of 200 R ☉, and NS surface magnetic field of 1012 G. The accretion rates are set to be 10−12 M ⊙  yr−1 and 10−10 M ⊙  yr−1 for comparison.
Paper: Are There Black Hole Symbiotic X-Ray Binaries?
Authors: Zhu-Ling Deng, Xiang-Dong Li
Figure caption: Distribution of companion masses and orbital periods for BH (left) and NS (right) SyXBs in different SN models. In all models we adopt v w = 0.25 v esc and δ = 1. The cross and star represent Gaia BH1 and Gaia BH2 (K. El-Badry et al. 2023b, 2023a), respectively. The black dots represent NS SyXBs with the companion mass and orbital period measured (data taken from N. Masetti et al. 2002; K. H. Hinkle et al. 2006; E. Nespoli et al. 2010; N. Masetti et al. 2011; Nagarajan et al. 2024).
Paper: Are There Black Hole Symbiotic X-Ray Binaries?
Authors: Zhu-Ling Deng, Xiang-Dong Li
Figure caption: Similar to Figure 2 but for detectable BH SyXBs.
Paper: Are There Black Hole Symbiotic X-Ray Binaries?
Authors: Zhu-Ling Deng, Xiang-Dong Li
Figure caption: The left and right panels display the lifetime PDFs for BH and NS SyXBs, respectively. The green and red bars represent the total and detectable lifetimes of the SyXBs, respectively.
Paper: MHD Modeling of a Geoeffective Interplanetary Coronal Mass Ejection with the Magnetic Topology Informed by In Situ Observations
Authors: Elena Provornikova, Viacheslav G. Merkin, Angelos Vourlidas, Anna Malanushenko, Sarah E. Gibson, Eric Winter, Charles N. Arge
Figure caption: Boundary conditions for the solar wind background at the start of the GAMERA simulation. The radial component of the magnetic field (a) and radial velocity (b), obtained from WSA-ADAPT output for CR 2095, as well as number density (c) and temperature (d), calculated as described in Section 3.2, are shown as functions of latitude and longitude at a fixed radial distance, r in = 21.5 R  S . The white contours in panels (a), (c), and (d) and the black contour in panel (b) mark the location of the heliospheric current sheet defined as the B  r  = 0 isosurface. Color scales for the density and temperature are inverted, so the faster wind is always brighter, and the slower wind is always darker. Yellow and white circles on the B  r  map (panel (a)) show in-ecliptic and southern directions of CME propagation, respectively.
Paper: MHD Modeling of a Geoeffective Interplanetary Coronal Mass Ejection with the Magnetic Topology Informed by In Situ Observations
Authors: Elena Provornikova, Viacheslav G. Merkin, Angelos Vourlidas, Anna Malanushenko, Sarah E. Gibson, Eric Winter, Charles N. Arge
Figure caption: Transformation of a spheromak resulting in a tethered flux rope CME configuration used to simulate the 2010 April 3 event. Panels (A), (B), and (C) show the view with the axis of symmetry in the out-of-plane direction. Panels (D), (E), and (F) show the view with the axis of symmetry in the plane and pointing up. Panels (A) and (D) show the initial spheromak. Panels (B) and (E) show the part of the spheromak that is transformed into a tethered flux rope after applying a radial stretching transformation. Panels (C) and (F) show the resulting tethered flux rope configuration (topmorph parameter ϒ = 2.5).
Paper: MHD Modeling of a Geoeffective Interplanetary Coronal Mass Ejection with the Magnetic Topology Informed by In Situ Observations
Authors: Elena Provornikova, Viacheslav G. Merkin, Angelos Vourlidas, Anna Malanushenko, Sarah E. Gibson, Eric Winter, Charles N. Arge
Figure caption: Time-dependent GAMERA inner boundary conditions during the emergence of the Gibson–Low CME flux rope at 21.5 R  S . From top to bottom, panels show radial B  r , polar B  θ , and azimuthal B  ϕ  magnetic field components, radial velocity V  r  and number density n. Columns show increasing time in hours after the emergence started at the inner boundary 21.5 R  S .
Paper: MHD Modeling of a Geoeffective Interplanetary Coronal Mass Ejection with the Magnetic Topology Informed by In Situ Observations
Authors: Elena Provornikova, Viacheslav G. Merkin, Angelos Vourlidas, Anna Malanushenko, Sarah E. Gibson, Eric Winter, Charles N. Arge
Figure caption: Time series of plasma speed, number density, magnetic field magnitude, and three magnetic field components. Blue curves show hourly ACE in situ observations, Orange curves show values extracted from GAMERA simulations at Earth in Case 1 with the ecliptic CME propagation, Green curves show values extracted from GAMERA simulation in Case 2 with the southern CME propagation. Vertical lines—from left to right—mark the arrival of the CME shock, and the start and end of the CME magnetic ejecta.
Paper: MHD Modeling of a Geoeffective Interplanetary Coronal Mass Ejection with the Magnetic Topology Informed by In Situ Observations
Authors: Elena Provornikova, Viacheslav G. Merkin, Angelos Vourlidas, Anna Malanushenko, Sarah E. Gibson, Eric Winter, Charles N. Arge
Figure caption: GAMERA solution for the solar wind background in the inner heliosphere at 21.5–215 R  S  for CR 2095. The solar wind speed V and scaled solar wind density ﹩D=n{(r/{r}_{\mathrm{in}})}^{2}﹩ are shown in the ecliptic (A, C) and meridional (B, D) planes. The sphere in the center shows the inner boundary at 21.5 R  S , with the color showing the B  r  component of the coronal magnetic field. The arrows show two propagation directions of the simulated CMEs: in-ecliptic (yellow) and 15° to the south from the ecliptic (white).
Paper: MHD Modeling of a Geoeffective Interplanetary Coronal Mass Ejection with the Magnetic Topology Informed by In Situ Observations
Authors: Elena Provornikova, Viacheslav G. Merkin, Angelos Vourlidas, Anna Malanushenko, Sarah E. Gibson, Eric Winter, Charles N. Arge
Figure caption: Distorted structure of the heliospheric magnetic field as the CME with an internal flux rope with a large region of negative B  z  propagates to 1 au. Snapshots in time starting from the emergence of the CME at 21.5 R  S  are shown. Field lines traced from the area of emergence at the inner boundary and an equatorial slice are color-coded with the B  z  value. The GAMERA inner boundary sphere is color-coded with the B  r  value. The isosurface at temperature T = 0.5 MK ahead of the CME shows the CME’s sheath. GL model parameters are given in Table 1, Case 1.
Paper: MHD Modeling of a Geoeffective Interplanetary Coronal Mass Ejection with the Magnetic Topology Informed by In Situ Observations
Authors: Elena Provornikova, Viacheslav G. Merkin, Angelos Vourlidas, Anna Malanushenko, Sarah E. Gibson, Eric Winter, Charles N. Arge
Figure caption: (a) Radial velocity V  r , (b) scaled number density ﹩n{(r/{r}_{0})}^{2}﹩, (c) scaled magnetic field magnitude ﹩B{(r/{r}_{0})}^{2}﹩, and magnetic field components (d) B  z , (e) ﹩{B}_{r}{(r/{r}_{0})}^{2}﹩, and (f) B  ϕ  in the equatorial slice of a 3D simulation at t = 36 hr after the CME began to emerge. GL model parameters for the CME are given in Table 1 with the direction of propagation in the solar equatorial plane (Case 1).
Paper: MHD Modeling of a Geoeffective Interplanetary Coronal Mass Ejection with the Magnetic Topology Informed by In Situ Observations
Authors: Elena Provornikova, Viacheslav G. Merkin, Angelos Vourlidas, Anna Malanushenko, Sarah E. Gibson, Eric Winter, Charles N. Arge
Figure caption: From top to bottom: comparison of the solar wind radial velocity, radial magnetic field component, number density, and temperature extracted along the ACE trajectory during the 27 days period in the GAMERA simulation of the inner heliosphere (orange curves) with the ACE in situ measurements (blue curves). Both the in situ ACE data and GAMERA simulation output are taken at a 1 hr cadence. This GAMERA simulation of the solar wind background does not include a CME yet.
Paper: MHD Modeling of a Geoeffective Interplanetary Coronal Mass Ejection with the Magnetic Topology Informed by In Situ Observations
Authors: Elena Provornikova, Viacheslav G. Merkin, Angelos Vourlidas, Anna Malanushenko, Sarah E. Gibson, Eric Winter, Charles N. Arge
Figure caption: CME magnetic field lines at t = 19 hr after the start of emergence. Field lines are traced from the area of emergence and colored by B  z  (red–blue). The sphere at 21.5 R  S  shows B  r  (red–gray) in a CME and solar wind background.
Paper: MHD Modeling of a Geoeffective Interplanetary Coronal Mass Ejection with the Magnetic Topology Informed by In Situ Observations
Authors: Elena Provornikova, Viacheslav G. Merkin, Angelos Vourlidas, Anna Malanushenko, Sarah E. Gibson, Eric Winter, Charles N. Arge
Figure caption: Time series of the magnetic field strength and three magnetic field components, B  x , B  y , and B  z , from CME simulations with four different Gibson–Low magnetic topologies: flux rope (solid orange), toroidal spheromak (dashed pink), tethered spheromak (dashed purple), sheared arcade (dashed gray). The blue solid curve shows ACE magnetic field measurements.
Paper: Fe/O Variations Relative to Source Longitude and Heliospheric Current Sheet in Large Solar Energetic Particle Events
Authors: Jinhye Park, Radoslav Bucik, Hyun-Jin Jeong, Yong-Jae Moon
Figure caption: From the top to the bottom panels, (a) AIHMI-PFSS, (b) HMI-PFSS, and (c) GONG-PFSS extrapolations for the 2013 April 11 event. The red, blue, and yellow crosses represent the magnetic footpoints of STEREO-A, B, and Earth at 2.5R ⊙, respectively. The red, blue, and yellow dots mark the photospheric footpoints of STEREO-A, B, and Earth, respectively. The blue lines are the polarity inversion lines. The green and red indicate positive and negative open magnetic fields, respectively. The source region is enclosed by a white square.
Paper: Fe/O Variations Relative to Source Longitude and Heliospheric Current Sheet in Large Solar Energetic Particle Events
Authors: Jinhye Park, Radoslav Bucik, Hyun-Jin Jeong, Yong-Jae Moon
Figure caption: The full-Sun running difference image on the event of 2013 April 11 at maximum of the X-ray flare, which is a composite of STEREO-B/EUVI 195 Å, SDO/AIA 193 Å, and STEREO-A/EUVI 195 Å images. The black cross is the source region of the SEP event. The red, blue, and yellow crosses represent the magnetic footpoints of STEREO-A, B, and Earth at 2.5R ⊙, respectively.
Paper: Fe/O Variations Relative to Source Longitude and Heliospheric Current Sheet in Large Solar Energetic Particle Events
Authors: Jinhye Park, Radoslav Bucik, Hyun-Jin Jeong, Yong-Jae Moon
Figure caption: Fe, O, and proton fluxes for the event of 2013 April 11. The dashed line represents the flare peak flux time at 07:16 UT on April 11, detected by GOES. In the first and third panels, the period during which Fe/O ratios were obtained is indicated by dashed–dotted lines. In the third and fourth panels, the IP detected by WIND at 22:13 UT on April 13 is represented by a dotted line.
Paper: Fe/O Variations Relative to Source Longitude and Heliospheric Current Sheet in Large Solar Energetic Particle Events
Authors: Jinhye Park, Radoslav Bucik, Hyun-Jin Jeong, Yong-Jae Moon
Figure caption: The orbital positions of STEREO-A and B relative to the Earth and Sun from 2010 to 2014.
Paper: Fe/O Variations Relative to Source Longitude and Heliospheric Current Sheet in Large Solar Energetic Particle Events
Authors: Jinhye Park, Radoslav Bucik, Hyun-Jin Jeong, Yong-Jae Moon
Figure caption: Fe/O ratio vs. longitudinal separation angle where (a) the events are observed by three spacecraft, (b) the events are observed by two spacecraft, and (c) the event is observed by one spacecraft. The Fe/O ratios observed by STEREO-A, B, and ACE are shown by the red triangles, the blue squares, and the yellow circles, respectively. The filled circles are for the same polarity group, and the unfilled circles are for the opposite group. The dashed lines connect three Fe/O ratios and two Fe/O ratios, respectively, from a single event observed on different spacecraft.
Paper: MHD Modeling of a Geoeffective Interplanetary Coronal Mass Ejection with the Magnetic Topology Informed by In Situ Observations
Authors: Elena Provornikova, Viacheslav G. Merkin, Angelos Vourlidas, Anna Malanushenko, Sarah E. Gibson, Eric Winter, Charles N. Arge
Figure caption: Magnetic topologies of the Gibson–Low CME model for different values of the “topmorph” parameter: (a) toroidal spheromak ϒ = 5.45; (b) tethered spheromak ϒ = 3.5; (c) flux rope ϒ = 2.5; (d) sheared arcade ϒ = 1.5. The front of each magnetic configuration is at r = 20 R  S . A small sphere at r = 1 R  S  shows the Sun's surface.
Paper: MHD Modeling of a Geoeffective Interplanetary Coronal Mass Ejection with the Magnetic Topology Informed by In Situ Observations
Authors: Elena Provornikova, Viacheslav G. Merkin, Angelos Vourlidas, Anna Malanushenko, Sarah E. Gibson, Eric Winter, Charles N. Arge
Figure caption: Comparison of the ACE data (blue), GAMERA simulation of the solar wind background (purple) and GAMERA–GL simulation with the propagating CME (orange). Top: speed relative to the solar wind background speed just before the CME; bottom: radial component of the magnetic field.
Paper: The Environments of Green Pea Galaxies. II. The Hα Dot Sample
Authors: Brooke Kimsey-Miller, Samantha W. Brunker, John J. Salzer
Figure caption: We illustrate the photometric redshift cuts for the Hα Dot GP redshift survey sample selection for Hα Dot 136. We use SDSS to create a catalog of galaxies brighter than g = 21 and within 30′ our Hα Dot GP. Circles represent galaxies with a photometric redshift only, while the triangles represent galaxies that have a spectroscopic redshift. The black circles and triangles represent targets within 10′ of the Hα Dot GP. We separate the SDSS catalog into a bright and faint list, represented by the red vertical line at g = 20.5. The red and blue horizontal lines indicate the photometric redshift cuts (see text). We include black and gray circles within the red lines, and black circles between the red and blue lines for our spectroscopic redshift survey. Galaxies outside these criteria are not selected because they are not near Hα Dot 136 in redshift. The left image shows the selection for our study. In the right image, we show that a large number of spectroscopic redshifts have been added to the redshift range occupied by the Hα Dot GP. We plot the objects with a spectroscopic redshift measured by this study as pink triangles.
Paper: Fe/O Variations Relative to Source Longitude and Heliospheric Current Sheet in Large Solar Energetic Particle Events
Authors: Jinhye Park, Radoslav Bucik, Hyun-Jin Jeong, Yong-Jae Moon
Figure caption: Fe/O ratio vs. longitudinal separation angle where (a) all data, (b) the same polarity group, and (c) the opposite polarity group. The Fe/O ratios observed by STEREO-A, B, and ACE are shown by the red triangles, the blue squares, and the yellow circles. The dashed–dotted line represents the maximum value reached by the polynomial fit. The three dotted lines from top to bottom represent typical Fe/O ratio of ISEP, LSEP, and IP events, respectively. The error bars represent 1σ uncertainty.
Paper: Fe/O Variations Relative to Source Longitude and Heliospheric Current Sheet in Large Solar Energetic Particle Events
Authors: Jinhye Park, Radoslav Bucik, Hyun-Jin Jeong, Yong-Jae Moon
Figure caption: Fe/O ratio vs. absolute longitudinal separation angle. The yellow circles are the events of the same polarity group, and the blue circles are the events of the opposite polarity group. The three dotted lines from top to bottom represent typical Fe/O ratios of ISEP, LSEP, and IP events, respectively. The error bars represent 1σ uncertainty. In the figure, cc is the correlation coefficient and p is the p-value.
Paper: The Environments of Green Pea Galaxies. II. The Hα Dot Sample
Authors: Brooke Kimsey-Miller, Samantha W. Brunker, John J. Salzer
Figure caption: An example of a pencil-beam diagram for Hα Dot 136. The left image (a) shows the tangent projection of R.A. vs. the distance to the galaxies, while the right image (b) shows the tangent projection of decl. The top, middle, and bottom plots show 500, 200, and 60 Mpc, respectively, extended on either side of the central Hα Dot GP, which is plotted as the central red dot. The black points are the measured spectroscopic redshifts obtained by this study and the gray points are from SDSS.
Paper: Fe/O Variations Relative to Source Longitude and Heliospheric Current Sheet in Large Solar Energetic Particle Events
Authors: Jinhye Park, Radoslav Bucik, Hyun-Jin Jeong, Yong-Jae Moon
Figure caption: The number of events, mean, median, and maximum of Fe/O ratios for six ranges. The black squares, red circles, and blue circles represent all the events, the events in the same polarity group, and those in the opposite polarity group, respectively. R1 is ∣θ∣ < 25°, R2 is 25° ≤ ∣θ∣ < 50°, R3 is 50° ≤ ∣θ∣ < 75°, R4 is 75° ≤ ∣θ∣ < 100°, R5 is 100° ≤ ∣θ∣ < 125°, and R6 is 125° ≤ ∣θ∣ < 180°.
Paper: The Environments of Green Pea Galaxies. II. The Hα Dot Sample
Authors: Brooke Kimsey-Miller, Samantha W. Brunker, John J. Salzer
Figure caption: We select 20 Hα Dot GPs from GP-like Hα Dots by using the C. Cardamone et al. (2009) color–color selection. We extend the C. Cardamone et al. (2009) r − i ≤ −0.2 criterion to −0.1, drawn as a dashed line. Objects to the left of the dashed line are considered GPs.
Paper: The Environments of Green Pea Galaxies. II. The Hα Dot Sample
Authors: Brooke Kimsey-Miller, Samantha W. Brunker, John J. Salzer
Figure caption: We determine the completeness of each field as a function of g-band magnitude. The fraction is the number of galaxies with a spectroscopic redshift over the number of galaxies that made the photometric redshift cuts. The completeness for the field is shown as a horizontal dashed red line and reported in Table 2.
Paper: Fe/O Variations Relative to Source Longitude and Heliospheric Current Sheet in Large Solar Energetic Particle Events
Authors: Jinhye Park, Radoslav Bucik, Hyun-Jin Jeong, Yong-Jae Moon
Figure caption: The number of events for the same polarity group (yellow bar) and the opposite polarity group (blue bar) based on IP, LSEP, and ISEP event ratios.
Paper: The Environments of Green Pea Galaxies. II. The Hα Dot Sample
Authors: Brooke Kimsey-Miller, Samantha W. Brunker, John J. Salzer
Figure caption: Top: a pencil-beam diagram near the GP, extended 150 Mpc on either side. Middle: the cylindrical density, corrected for depth and incompleteness, is plotted vs. the distance to the midpoint of the cylinder, as the cylinder is moved along the pencil-beam diagram. The red vertical line is the location of the GP. The cylindrical density centered on the GP is provided as text within the plot. Bottom left: the spherical-shell density analysis, corrected for depth and incompleteness, is shown for each spherical shell, centered on the GP. Bottom right: a histogram of the distance to the NNs within 200 Mpc of the GP, but excluding the GP, is shown. The distance to the NN of the GP is presented as a red vertical line and as annotated text (3.69 Mpc). Also shown is an isolation statistic (e.g., 37% of galaxies within the Hα Dot 136 field are less isolated than the GP.) We utilize all plots to qualitatively classify the environment of Hα Dot 136 as extremely isolated/low density (EI/LD).
Paper: The Environments of Green Pea Galaxies. II. The Hα Dot Sample
Authors: Brooke Kimsey-Miller, Samantha W. Brunker, John J. Salzer
Figure caption: The environment analysis of Hα Dot 83 by utilizing a redshift-position diagram and three density estimators. Descriptions of the plots are found in Figure 5. The environment is classified as extremely isolated/low density (EI/LD).
Paper: The Environments of Green Pea Galaxies. II. The Hα Dot Sample
Authors: Brooke Kimsey-Miller, Samantha W. Brunker, John J. Salzer
Figure caption: The environment analysis of Hα Dot 72 by utilizing a redshift-position diagram and three density estimators. Descriptions of the plots are found in Figure 5. The environment is classified as extremely isolated/low density (EI/LD).
Paper: The Environments of Green Pea Galaxies. II. The Hα Dot Sample
Authors: Brooke Kimsey-Miller, Samantha W. Brunker, John J. Salzer
Figure caption: The environment analysis of Hα Dot 57 by utilizing a redshift-position diagram and three density estimators. Descriptions of the plots are found in Figure 5. The environment is classified as low density (LD).
Paper: The Environments of Green Pea Galaxies. II. The Hα Dot Sample
Authors: Brooke Kimsey-Miller, Samantha W. Brunker, John J. Salzer
Figure caption: The environment analysis of Hα Dot 19 by utilizing a redshift-position diagram and three density estimators. Descriptions of the plots are found in Figure 5. The environment is classified as extremely isolated (EI).
Paper: The Environments of Green Pea Galaxies. II. The Hα Dot Sample
Authors: Brooke Kimsey-Miller, Samantha W. Brunker, John J. Salzer
Figure caption: The environment analysis of Hα Dot 22 by utilizing a redshift-position diagram and three density estimators. Descriptions of the plots are found in Figure 5. The environment is classified as extremely isolated (EI).
Paper: The Environments of Green Pea Galaxies. II. The Hα Dot Sample
Authors: Brooke Kimsey-Miller, Samantha W. Brunker, John J. Salzer
Figure caption: The environment analysis of Hα Dot 65 by utilizing a redshift-position diagram and three density estimators. Descriptions of the plots are found in Figure 5. The environment is classified as extremely isolated (EI).
Paper: The Environments of Green Pea Galaxies. II. The Hα Dot Sample
Authors: Brooke Kimsey-Miller, Samantha W. Brunker, John J. Salzer
Figure caption: The environment analysis of Hα Dot 55 by utilizing a redshift-position diagram and three density estimators. Descriptions of the plots are found in Figure 5. The environment is classified as extremely isolated (EI).
Paper: The Environments of Green Pea Galaxies. II. The Hα Dot Sample
Authors: Brooke Kimsey-Miller, Samantha W. Brunker, John J. Salzer
Figure caption: The environment analysis of Hα Dot 37 by utilizing a redshift-position diagram and three density estimators. Descriptions of the plots are found in Figure 5. The environment is classified as extremely isolated (EI).