adsabs/AstroCLIMB huggingface dataset:
Paper: Implementation of Aerosol Mie Scattering in POSEIDON with Application to the Hot Jupiter HD 189733 b’s Transmission, Emission, and Reflected Light Spectrum
Authors: Elijah Mullens, Nikole K. Lewis, Ryan J. MacDonald
Figure caption: Same as Figure 9, but highlighting the retrieval results when including sulfide, soot, and haze aerosols. Top panel: retrieval results for sulfide aerosol species, namely manganese sulfide (MnS, purple) and sodium sulfide (Na2S, green). Middle panel: retrieval results for disequilibrium aerosols, namely flame soot (Soot, black) and Titan tholins (Tholins, gold). MnS has an absorption feature in the longest wavelengths, 23–30 μm. We note that the longer-wavelength data used is from a sulfide extrapolation, not laboratory data. Na2S has no significant absorption in the 0.2–30 μm range. Soot is featureless save a small feature in the shortest wavelengths (0.2–0.3 μm). Tholins have a large feature from 5 to 8 μm with continuum opacity from 9 to 30 μm. All four cloud species retrieve properties consistent with silicates (high-altitude, thin, low-density slab composed of submicron sized particles). Bottom panels: same as Figure 5.
Paper: Implementation of Aerosol Mie Scattering in POSEIDON with Application to the Hot Jupiter HD 189733 b’s Transmission, Emission, and Reflected Light Spectrum
Authors: Elijah Mullens, Nikole K. Lewis, Ryan J. MacDonald
Figure caption: Top panel: resulting transmission spectra from atmospheric retrievals assuming different aerosol models (median spectra and 1σ regions; from top to bottom: slab models, fuzzy deck models, and uniform X models). We find that the fuzzy deck larger prior (purple, thick line) results in the best fit that can fit the short-wavelength slope without imparting a strong silicate feature in the longest infrared wavelengths. The modified fuzzy deck is statistically consistent with the slab model (black, thick line). All uniform mixing ratios retrieve nearly identical spectra that cannot fit the slope (pink, thick line). Bottom panels: retrieved aerosol properties for the slab and modified fuzzy deck models. Left panel: shaded region represents vertical extent of slab in log-pressure space, with the dotted vertical line representing the mixing ratio of the aerosol in that region. A low-density, high-altitude, thin slab was retrieved. Right panel: gray shaded region represents vertical extent of opaque deck in log-pressure space, with the solid line representing the mixing ratio of the aerosol above the deck. The fuzzy deck larger prior retrieves an opaque deck at 0.01 bars, with an aerosol volume mixing ratio that rises from −16 to −10 to the top of the atmosphere. A full list of retrieved parameters can be seen in Table 6.
Paper: Implementation of Aerosol Mie Scattering in POSEIDON with Application to the Hot Jupiter HD 189733 b’s Transmission, Emission, and Reflected Light Spectrum
Authors: Elijah Mullens, Nikole K. Lewis, Ryan J. MacDonald
Figure caption: Updated Na cross section in POSEIDON. The retrievals in this paper use a sub-Voigt line wing prescription for all lines, based on the wing fit from J.-L. Baudino et al. (2015) for the Na and K resonance doublets.
Paper: Implementation of Aerosol Mie Scattering in POSEIDON with Application to the Hot Jupiter HD 189733 b’s Transmission, Emission, and Reflected Light Spectrum
Authors: Elijah Mullens, Nikole K. Lewis, Ryan J. MacDonald
Figure caption: The effect of aerosol properties and species on the resultant emission and reflection spectra. For all models, we test enstatite (MgSiO3), quartz (SiO2, both crystalline and amorphous), and manganese sulfide (MnS). Unless specified, the cloud-top pressure is at 0.1 bars and extends to 100 bars, is composed of submicron particle sizes, and has a fractional cloud coverage of 0.5. Each row displayed a zoom in on the HST data, the full spectra, and the geometric albedo up to to 5 μm. The first two rows display the effect of increasing the aerosol abundance to −15 and −10, with a general increase in reflected light, especially for MgSiO3 and amorphous SiO2. The third row displays the effect of increasing the cloud fraction to 1, which washes out the water absorption features and amplifies the reflected light. The fourth row utilizes the results from our transmission retrievals and initialized a high-altitude, low-density slab which results in a smooth reflection signal with no alkali absorption features. The fifth and sixth rows display the effect of particle size by utilizing 1 μm sized particles, with half and full cloud coverage. Larger particles dominate the reflection spectra, and impart strong scattering features in longer wavelengths, even when the atmospheric thermal structure contributing to those wavelengths is isothermal. In row six we display that thermal scattering imparts the features in long wavelengths by turning it off.
Paper: Implementation of Aerosol Mie Scattering in POSEIDON with Application to the Hot Jupiter HD 189733 b’s Transmission, Emission, and Reflected Light Spectrum
Authors: Elijah Mullens, Nikole K. Lewis, Ryan J. MacDonald
Figure caption: Spectral and pressure contribution of the clear emission + reflection retrieval displayed in Figure 9. Top panels: spectral contribution of detected species, with the emission spectrum broadcasted into brightness temperature. Bottom panels: pressure and photometric contribution function for the total spectrum, as well as specific chemical species. Each pressure contribution function (left-hand panels) is normalized with darker regions representing the pressure regions where the opacity of that species is contributing to the spectrum. The photometric contribution (right-hand panels) shows which wavelengths are the most important for which pressure regions and species. The pressure and photometric contribution functions show that a bulk of the spectrum is forming in the 10–0.1 bar region, where the temperature gradient is.
Paper: Implementation of Aerosol Mie Scattering in POSEIDON with Application to the Hot Jupiter HD 189733 b’s Transmission, Emission, and Reflected Light Spectrum
Authors: Elijah Mullens, Nikole K. Lewis, Ryan J. MacDonald
Figure caption: Spectral contribution of highest evidence transmission retrieval, the MnS spectrum (black) displayed in Figure 6, sulfides. H2 + He continuum opacity (gray) provides a baseline to the spectrum. MnS (magenta) dominates the opacity 0.2–0.6 μm via Mie scattering and has an absorption feature at the longest wavelengths, 23–30 μm. Na (hot pink) has a weak absorption feature at 0.60 μm. K (purple) has an absorption feature at 0.76 μm. H2O (blue) dominates the spectrum in a series of absorption features in the infrared. H2S (cyan) broadens a few water features, and has a significant feature at 14 μm. CO2 (red) has an absorption feature at 4.5 μm. CO (orange), CH4 (yellow), and NH3 (pink) do not contribute to the spectrum.
Paper: Implementation of Aerosol Mie Scattering in POSEIDON with Application to the Hot Jupiter HD 189733 b’s Transmission, Emission, and Reflected Light Spectrum
Authors: Elijah Mullens, Nikole K. Lewis, Ryan J. MacDonald
Figure caption: Zoom in on the highest evidence aerosol (TiO2) from Section 3.5, which only fit the HST transmission data. TiO2 is able to near perfectly fit the slope. TiO2 hold significance due to being commonly invoked as a “seed” particle by which other volatiles condense onto.
Paper: Implementation of Aerosol Mie Scattering in POSEIDON with Application to the Hot Jupiter HD 189733 b’s Transmission, Emission, and Reflected Light Spectrum
Authors: Elijah Mullens, Nikole K. Lewis, Ryan J. MacDonald
Figure caption: The effect of removing CO from the median (black) and best-fit (magenta) retrieved atmospheric properties of the Guillot dayside (top panels) and Guillot dayside (larger prior) (bottom panels) retrievals (no CO, dark orange). The best-fit retrieval for both cases has high CO abundances. CO imparts only a slight feature in the data (around 5 μm where it widens the CO2 feature at 4.5 μm). The retrieval utilizes CO to increase the mean molecular weight of the atmosphere, decreasing the scale height, and allowing flux to escape from deeper in the atmosphere. This effect can be seen especially in the 0.8–2 μm region of the dayside Guillot (larger prior) retrieval. Spectra are plotted at R = 500.
Paper: ODIN: Identifying Protoclusters and Cosmic Filaments Traced by Lyα-emitting Galaxies
Authors: Vandana Ramakrishnan, Kyoung-Soo Lee, Maria Celeste Artale, Eric Gawiser, Yujin Yang, Changbom Park, Yi-Kuan Chiang, Robin Ciardullo, Arjun Dey, Caryl Gronwall, Lucia Guaita, Ho Seong Hwang, Sang Hyeok Im, Woong-Seob Jeong, Seongjae Kim, Ankit Kumar, Jaehyun Lee, Seong-Kook Lee, Byeongha Moon, Nelson Padilla, Alexandra Pope, Roxana Popescu, Akriti Singh, Hyunmi Song, Paulina Troncoso, Francisco Valdes, Ann Zabludoff
Figure caption: Left: Gaussian smoothed (GS) LAE surface density map. Black, green, white, and cyan contours indicate LAE overdensities of 2σ, 3σ, 4σ, and 5σ significance respectively; the corresponding values of (1 + δ LAE) are marked on the color bar. The three largest overdensity complexes are highlighted in red. Right: VT-based density map. White contours indicate overdensities of 3σ significance. The LSS revealed by the surface density maps is highly clumpy and irregular. Nonspherical/irregular overdensities are better delineated at fixed significance in the VT map than in the GS map. The clover shape of the surface density maps arises from the HSC-SSP data, which consists of four Deep and one central UltraDeep pointing in the COSMOS field.
Paper: Implementation of Aerosol Mie Scattering in POSEIDON with Application to the Hot Jupiter HD 189733 b’s Transmission, Emission, and Reflected Light Spectrum
Authors: Elijah Mullens, Nikole K. Lewis, Ryan J. MacDonald
Figure caption: Log optical depth (log τ) of each aerosol model explored in the transmission suite of retrievals (Section 3) overlaid on a wavelength (in microns) vs. log-pressure (in bars) plot. Forward models were generated with the median retrieved aerosol properties found in Table 5. The gray cloud model (top panel) displays the infinite opacity deck and parameterized haze. Each aerosol model (bottom panels) displays the retrieved pressure region spanned by the aerosol slab, as well as opacity contributions in the short-wavelength scattering region (0.2–1 μm) and infrared absorption (1–30 μm). Color bar is normalized to τ = 1 and τ = 1 × 10–5.
Paper: ODIN: Identifying Protoclusters and Cosmic Filaments Traced by Lyα-emitting Galaxies
Authors: Vandana Ramakrishnan, Kyoung-Soo Lee, Maria Celeste Artale, Eric Gawiser, Yujin Yang, Changbom Park, Yi-Kuan Chiang, Robin Ciardullo, Arjun Dey, Caryl Gronwall, Lucia Guaita, Ho Seong Hwang, Sang Hyeok Im, Woong-Seob Jeong, Seongjae Kim, Ankit Kumar, Jaehyun Lee, Seong-Kook Lee, Byeongha Moon, Nelson Padilla, Alexandra Pope, Roxana Popescu, Akriti Singh, Hyunmi Song, Paulina Troncoso, Francisco Valdes, Ann Zabludoff
Figure caption: Positions of the observed ODIN LAEs (left panel, see text in Section 2.1) and the mock LAEs from a randomly chosen slice of TNG300 (right panel, see text in Section 2.2). In the left panel, the holes left by bright stars are shown by red circles.
Paper: ODIN: Identifying Protoclusters and Cosmic Filaments Traced by Lyα-emitting Galaxies
Authors: Vandana Ramakrishnan, Kyoung-Soo Lee, Maria Celeste Artale, Eric Gawiser, Yujin Yang, Changbom Park, Yi-Kuan Chiang, Robin Ciardullo, Arjun Dey, Caryl Gronwall, Lucia Guaita, Ho Seong Hwang, Sang Hyeok Im, Woong-Seob Jeong, Seongjae Kim, Ankit Kumar, Jaehyun Lee, Seong-Kook Lee, Byeongha Moon, Nelson Padilla, Alexandra Pope, Roxana Popescu, Akriti Singh, Hyunmi Song, Paulina Troncoso, Francisco Valdes, Ann Zabludoff
Figure caption:  M  z=0 values estimated from Equation (6) compared to the true values for the progenitors of the 30 most massive clusters in the TNG300 box. The left panel (blue points) indicates the masses estimated from the 2D projection of the LAE overdensity corresponding to the protocluster, with the LAEs matched in number density to observations. The dashed line indicates a one-to-one relation between estimated and true descendant masses, while the solid line indicates a relation of M est,z=0 = 0.35M 200,z=0. Highlighted points show cases where the protocluster was merged with another, more massive object by the detection. The right panel (red points) indicates the masses estimated from the 3D positions of the cluster members (see Section 5.2 for more details). Shaded regions indicate the range of the 1σ and 2σ scatter of the estimated masses. While the 2D mass estimate is subject to considerable scatter, primarily arising from the loss of information in the z-direction, it correlates well with the true descendant mass.
Paper: ODIN: Identifying Protoclusters and Cosmic Filaments Traced by Lyα-emitting Galaxies
Authors: Vandana Ramakrishnan, Kyoung-Soo Lee, Maria Celeste Artale, Eric Gawiser, Yujin Yang, Changbom Park, Yi-Kuan Chiang, Robin Ciardullo, Arjun Dey, Caryl Gronwall, Lucia Guaita, Ho Seong Hwang, Sang Hyeok Im, Woong-Seob Jeong, Seongjae Kim, Ankit Kumar, Jaehyun Lee, Seong-Kook Lee, Byeongha Moon, Nelson Padilla, Alexandra Pope, Roxana Popescu, Akriti Singh, Hyunmi Song, Paulina Troncoso, Francisco Valdes, Ann Zabludoff
Figure caption: Top left: the dark matter distribution for a randomly selected slice, centered on a protocluster with descendant mass log (M 200/M ⊙) = 15.18 (red cross; group ID = 0 within the z = 0 TNG300 simulation box). Top right: the filaments (pink lines) extracted by DisPerSE for this slice are based on the mock LAE positions, which are shown by black dots. This network is comparable to the cosmic web selected with ODIN data. Bottom: the filaments extracted by DisPerSE for the same slice using the 3D positions of the slice galaxies with 107 M ⊙ < M * < 1012 M ⊙, with varying persistence thresholds. The filaments are color-coded by their separation from the center of the slice along the line-of-sight direction. At large distances from the slice center, the filaments are truncated by the slice boundaries. The number of such truncated filaments reduces at higher persistence thresholds.
Paper: ODIN: Identifying Protoclusters and Cosmic Filaments Traced by Lyα-emitting Galaxies
Authors: Vandana Ramakrishnan, Kyoung-Soo Lee, Maria Celeste Artale, Eric Gawiser, Yujin Yang, Changbom Park, Yi-Kuan Chiang, Robin Ciardullo, Arjun Dey, Caryl Gronwall, Lucia Guaita, Ho Seong Hwang, Sang Hyeok Im, Woong-Seob Jeong, Seongjae Kim, Ankit Kumar, Jaehyun Lee, Seong-Kook Lee, Byeongha Moon, Nelson Padilla, Alexandra Pope, Roxana Popescu, Akriti Singh, Hyunmi Song, Paulina Troncoso, Francisco Valdes, Ann Zabludoff
Figure caption: Left: an example comparison of the 2D and 3D skeletons, illustrating how d 2d→3d  and d 3d→2d  are measured. Right: comparison of the 2D and 3D skeleton using the separation of the segments, d 2d→3d  (top) and d 3d→2d  (bottom). The separations are calculated across all 90 slices of 80 cMpc thickness from the z = 3 TNG300 simulation. In the majority of cases, both d 2d→3d  and d 3d→2d  are less than 5 cMpc, regardless of the specific persistence threshold.
Paper: ODIN: Identifying Protoclusters and Cosmic Filaments Traced by Lyα-emitting Galaxies
Authors: Vandana Ramakrishnan, Kyoung-Soo Lee, Maria Celeste Artale, Eric Gawiser, Yujin Yang, Changbom Park, Yi-Kuan Chiang, Robin Ciardullo, Arjun Dey, Caryl Gronwall, Lucia Guaita, Ho Seong Hwang, Sang Hyeok Im, Woong-Seob Jeong, Seongjae Kim, Ankit Kumar, Jaehyun Lee, Seong-Kook Lee, Byeongha Moon, Nelson Padilla, Alexandra Pope, Roxana Popescu, Akriti Singh, Hyunmi Song, Paulina Troncoso, Francisco Valdes, Ann Zabludoff
Figure caption: Protoclusters selected from the GS map (top left), VT map (top right), with HDBSCAN (bottom left) and filaments identified with DisPerSE with a persistence threshold of 2σ (bottom right) overlaid on the VT map. The red dashed region in the bottom left panel highlights a structure that is missed by the VT and GS maps but is detected with HDBSCAN. The filaments correspond to regions of moderate (∼2σ–3σ) overdensity, and connect protoclusters together.
Paper: ODIN: Identifying Protoclusters and Cosmic Filaments Traced by Lyα-emitting Galaxies
Authors: Vandana Ramakrishnan, Kyoung-Soo Lee, Maria Celeste Artale, Eric Gawiser, Yujin Yang, Changbom Park, Yi-Kuan Chiang, Robin Ciardullo, Arjun Dey, Caryl Gronwall, Lucia Guaita, Ho Seong Hwang, Sang Hyeok Im, Woong-Seob Jeong, Seongjae Kim, Ankit Kumar, Jaehyun Lee, Seong-Kook Lee, Byeongha Moon, Nelson Padilla, Alexandra Pope, Roxana Popescu, Akriti Singh, Hyunmi Song, Paulina Troncoso, Francisco Valdes, Ann Zabludoff
Figure caption: Left: LAE surface density distribution of the TNG300 slices, in comparison to that of the observed LAEs. The red line shows the median distribution across all 90 slices while the shaded region shows the spread. The observed and simulated LAE distributions are very similar, particularly at the high end, which represents massive structures. Middle and right: area and median LAE overdensity (δ LAE) for the protocluster candidates detected in the 90 TNG300 slices compared to those of the observationally detected protocluster candidates. Blue/red vertical lines indicate the median value for the ODIN data/TNG300. The properties of the structures are similar in the observations and simulation.
Paper: ODIN: Identifying Protoclusters and Cosmic Filaments Traced by Lyα-emitting Galaxies
Authors: Vandana Ramakrishnan, Kyoung-Soo Lee, Maria Celeste Artale, Eric Gawiser, Yujin Yang, Changbom Park, Yi-Kuan Chiang, Robin Ciardullo, Arjun Dey, Caryl Gronwall, Lucia Guaita, Ho Seong Hwang, Sang Hyeok Im, Woong-Seob Jeong, Seongjae Kim, Ankit Kumar, Jaehyun Lee, Seong-Kook Lee, Byeongha Moon, Nelson Padilla, Alexandra Pope, Roxana Popescu, Akriti Singh, Hyunmi Song, Paulina Troncoso, Francisco Valdes, Ann Zabludoff
Figure caption: VT-based surface density map of our observed LAEs vs. that of a 80 cMpc thick slice of the TNG300 simulation box at z = 3. The positions of individual LAEs/mock LAEs are shown in Figure 1. Red lines in the top panels represent filaments selected with DisPerSE with a persistence threshold of 2σ. The cyan cross in the top right panel indicates the position of the massive protocluster on which the slice is centered (group ID = 13 at z = 0), while yellow crosses show the other massive protoclusters in the same volume (group IDs = 1, 2, 7, 11, 23 at z = 0). Green crosses show the progenitors of less massive clusters within the slice. Some overdensity complexes (A1, B1, C1; A2, B2, C2) are highlighted and zoomed in on the bottom panels. The two maps show visible similarities.
Paper: ODIN: Identifying Protoclusters and Cosmic Filaments Traced by Lyα-emitting Galaxies
Authors: Vandana Ramakrishnan, Kyoung-Soo Lee, Maria Celeste Artale, Eric Gawiser, Yujin Yang, Changbom Park, Yi-Kuan Chiang, Robin Ciardullo, Arjun Dey, Caryl Gronwall, Lucia Guaita, Ho Seong Hwang, Sang Hyeok Im, Woong-Seob Jeong, Seongjae Kim, Ankit Kumar, Jaehyun Lee, Seong-Kook Lee, Byeongha Moon, Nelson Padilla, Alexandra Pope, Roxana Popescu, Akriti Singh, Hyunmi Song, Paulina Troncoso, Francisco Valdes, Ann Zabludoff
Figure caption: Protocluster candidates selected from the GS map (top row), the VT map (middle), and with HDBSCAN (bottom). Red crosses indicate the geometric centers of the selected overdensities. Yellow swathes indicate the extent of the protoclusters in the upper two rows. In the bottom row, colored points indicate LAEs classified as belonging to a cluster by HDBSCAN, enclosed by an ellipse for clarity, while gray points are classified as noise.
Paper: ODIN: Identifying Protoclusters and Cosmic Filaments Traced by Lyα-emitting Galaxies
Authors: Vandana Ramakrishnan, Kyoung-Soo Lee, Maria Celeste Artale, Eric Gawiser, Yujin Yang, Changbom Park, Yi-Kuan Chiang, Robin Ciardullo, Arjun Dey, Caryl Gronwall, Lucia Guaita, Ho Seong Hwang, Sang Hyeok Im, Woong-Seob Jeong, Seongjae Kim, Ankit Kumar, Jaehyun Lee, Seong-Kook Lee, Byeongha Moon, Nelson Padilla, Alexandra Pope, Roxana Popescu, Akriti Singh, Hyunmi Song, Paulina Troncoso, Francisco Valdes, Ann Zabludoff
Figure caption: Number of candidates and contamination fraction for protoclusters selected from the VT map (top) and GS map (bottom), for different density thresholds and minimum areas. The density threshold is expressed in units of Nσ above the field surface density. White stars indicate the detection settings adopted for this work. While the VT map suffers from higher contamination than the GS map, it also detects far more candidates.
Paper: ODIN: Identifying Protoclusters and Cosmic Filaments Traced by Lyα-emitting Galaxies
Authors: Vandana Ramakrishnan, Kyoung-Soo Lee, Maria Celeste Artale, Eric Gawiser, Yujin Yang, Changbom Park, Yi-Kuan Chiang, Robin Ciardullo, Arjun Dey, Caryl Gronwall, Lucia Guaita, Ho Seong Hwang, Sang Hyeok Im, Woong-Seob Jeong, Seongjae Kim, Ankit Kumar, Jaehyun Lee, Seong-Kook Lee, Byeongha Moon, Nelson Padilla, Alexandra Pope, Roxana Popescu, Akriti Singh, Hyunmi Song, Paulina Troncoso, Francisco Valdes, Ann Zabludoff
Figure caption: Left: distribution of dark matter in a randomly chosen TNG300 slice. Middle: the filament network identified with DisPerSE, using 0.1% of the dark matter particles and with a persistence threshold of 6σ. Right: the filament network identified with DisPerSE using galaxies (red), again with a persistence threshold of 6σ, overlaid on that traced by dark matter. Although the former is less detailed than the latter, there is excellent correspondence between the two.
Paper: ODIN: Identifying Protoclusters and Cosmic Filaments Traced by Lyα-emitting Galaxies
Authors: Vandana Ramakrishnan, Kyoung-Soo Lee, Maria Celeste Artale, Eric Gawiser, Yujin Yang, Changbom Park, Yi-Kuan Chiang, Robin Ciardullo, Arjun Dey, Caryl Gronwall, Lucia Guaita, Ho Seong Hwang, Sang Hyeok Im, Woong-Seob Jeong, Seongjae Kim, Ankit Kumar, Jaehyun Lee, Seong-Kook Lee, Byeongha Moon, Nelson Padilla, Alexandra Pope, Roxana Popescu, Akriti Singh, Hyunmi Song, Paulina Troncoso, Francisco Valdes, Ann Zabludoff
Figure caption: Top: the fraction of 2D filament segments with a match with the 3D skeleton (detected with various persistence thresholds), as a function of the LAE surface density at the position of the filament segment. Regardless of the persistence threshold used to select the 3D skeleton, the fraction of matched 2D segments increases with increasing surface density. Bottom: d 3d→2d  as a function of the (2D) LAE surface density for the 5σ threshold 3D skeleton; the other two skeletons give virtually identical results. The solid line indicates the median value while the shaded region indicates the spread as measured from the 16–84 percentile scatter.
Paper: ODIN: Identifying Protoclusters and Cosmic Filaments Traced by Lyα-emitting Galaxies
Authors: Vandana Ramakrishnan, Kyoung-Soo Lee, Maria Celeste Artale, Eric Gawiser, Yujin Yang, Changbom Park, Yi-Kuan Chiang, Robin Ciardullo, Arjun Dey, Caryl Gronwall, Lucia Guaita, Ho Seong Hwang, Sang Hyeok Im, Woong-Seob Jeong, Seongjae Kim, Ankit Kumar, Jaehyun Lee, Seong-Kook Lee, Byeongha Moon, Nelson Padilla, Alexandra Pope, Roxana Popescu, Akriti Singh, Hyunmi Song, Paulina Troncoso, Francisco Valdes, Ann Zabludoff
Figure caption: Average area of the structures detected by HDBSCAN, for various combinations of the Kth nearest neighbor used to measure density (min_samples) and minimum number of points to constitute a cluster (min_cluster_size). The expected area of a protocluster is ∼100– 200 cMpc2; areas much larger than this suggest that multiple structures are being blended together by the algorithm.