adsabs/AstroCLIMB huggingface dataset:
Paper: The Ophiuchus DIsk Survey Employing ALMA (ODISEA): Complete Size Distributions for the 100 Brightest Disks across Multiplicity and Spectral Energy Distribution Classes
Authors: Anuroop Dasgupta, Lucas A. Cieza, Camilo González-Ruilova, Trisha Bhowmik, Prachi Chavan, Grace Batalla-Falcon, Gregory Herczeg, Dary Ruiz-Rodriguez, Jonathan P. Williams, Anibal Sierra, Simon Casassus, Octavio Guilera, Sebastian Pérez, Santiago Orcajo, P.H. Nogueira, A.S Hales, J.M. Miley, Fernando R. Rannou, Alice Zurlo
Figure caption: A comparison of the profile obtained from Frank to the Gaussian fit from imfit for two sources. For well-resolved sources, imfit reproduces well the intensity profile. For very small sources, imfit might underestimate their size and Frank sizes should be preferred.
Paper: The Ophiuchus DIsk Survey Employing ALMA (ODISEA): Complete Size Distributions for the 100 Brightest Disks across Multiplicity and Spectral Energy Distribution Classes
Authors: Anuroop Dasgupta, Lucas A. Cieza, Camilo González-Ruilova, Trisha Bhowmik, Prachi Chavan, Grace Batalla-Falcon, Gregory Herczeg, Dary Ruiz-Rodriguez, Jonathan P. Williams, Anibal Sierra, Simon Casassus, Octavio Guilera, Sebastian Pérez, Santiago Orcajo, P.H. Nogueira, A.S Hales, J.M. Miley, Fernando R. Rannou, Alice Zurlo
Figure caption: Histograms of the size distribution of embedded targets (Class I and flat-spectrum sources) and Class II objects (left panels). The top and middle panels correspond to Gaussian size measurements, including and excluding close binaries. The bottom panel shows the size distribution for the 80 disks with Frank profiles (only available for nonbinary disks). The corresponding cumulative distributions are shown on the right panels. Results of the K-S tests show that the distributions of different SED classes are statistically indistinguishable from each other.
Paper: Exclusion of a Direct Progenitor Detection for the Type Ic SN 2017ein Based on Late-time Observations
Authors: Yi-Han Zhao, Ning-Chen Sun, Junjie Wu, Zexi Niu, Xinyi Hong, Yinhan Huang, Justyn R. Maund, Qiang Xi, Danfeng Xiang, Jifeng Liu
Figure caption: F336W–F555W vs. F555W–F814W color–color diagrams for Source A (red circle) and model stars (bottom panel, solid lines) and star clusters (top panel, solid lines). The arrows in the upper-left corner show the reddening vector under a standard extinction law with RV = 3.1.
Paper: Exclusion of a Direct Progenitor Detection for the Type Ic SN 2017ein Based on Late-time Observations
Authors: Yi-Han Zhao, Ning-Chen Sun, Junjie Wu, Zexi Niu, Xinyi Hong, Yinhan Huang, Justyn R. Maund, Qiang Xi, Danfeng Xiang, Jifeng Liu
Figure caption: Brightness and color evolution of Source A at different epochs. The preexplosion magnitudes measured by K18, X19, and VD18 are also plotted for comparison. The dashed lines represent the inverse-variance-weighted averages of the preexplosion and the last epoch, and the green-shaded bands indicate the errors. All the magnitudes have been corrected for systematic bias between the different epochs.
Paper: Exclusion of a Direct Progenitor Detection for the Type Ic SN 2017ein Based on Late-time Observations
Authors: Yi-Han Zhao, Ning-Chen Sun, Junjie Wu, Zexi Niu, Xinyi Hong, Yinhan Huang, Justyn R. Maund, Qiang Xi, Danfeng Xiang, Jifeng Liu
Figure caption: Pre- and postexplosion HST images of the site of SN 2017ein (F336W is not included here). The SN position is denoted by the white crosshair. Each image has a size of ∼160 × 160 pc and is oriented with north up and east to the left.
Paper: Exclusion of a Direct Progenitor Detection for the Type Ic SN 2017ein Based on Late-time Observations
Authors: Yi-Han Zhao, Ning-Chen Sun, Junjie Wu, Zexi Niu, Xinyi Hong, Yinhan Huang, Justyn R. Maund, Qiang Xi, Danfeng Xiang, Jifeng Liu
Figure caption: Comparison of photometry as reported by DOLPHOT for observations at different epochs. The black dashed line shows the one-to-one relation, while the orange dashed–dotted line corresponds to systematic shifts as calculated by inverse-variance-weighted averages.
Paper: Exclusion of a Direct Progenitor Detection for the Type Ic SN 2017ein Based on Late-time Observations
Authors: Yi-Han Zhao, Ning-Chen Sun, Junjie Wu, Zexi Niu, Xinyi Hong, Yinhan Huang, Justyn R. Maund, Qiang Xi, Danfeng Xiang, Jifeng Liu
Figure caption: Histograms of magnitude differences with respect to the epoch of t = 3.8 yr. The solid lines are Gaussian fit curves, and the dashed lines represent the means of the Gaussian fit. Normalization has been applied to each graph.
Paper: Discovery of Metal-poor and Distant Pre–Main Sequence Candidates in WLM with JWST
Authors: Venu M. Kalari, Ricardo Salinas, Morten Andersen, Guido De Marchi, Monica Rubio, Jorick S. Vink, Hans Zinnecker
Figure caption: F150W image of the cluster. The dashed red circle (radius of 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩1) encircles the region studied here. PMS candidates are labeled following the identification given in Table 1.
Paper: Discovery of Metal-poor and Distant Pre–Main Sequence Candidates in WLM with JWST
Authors: Venu M. Kalari, Ricardo Salinas, Morten Andersen, Guido De Marchi, Monica Rubio, Jorick S. Vink, Hans Zinnecker
Figure caption: WLM r/g/b image where r = 24 μm, g = Hα, and b is the optical V-band image. The red circle marks the cluster. North is up and east is to the left. Green squares mark the location of CO cores from M. Rubio et al. (2015). The dashed white lines represent the footprint covered by D. R. Weisz et al. (2023).
Paper: Stellar Streams Reveal the Mass Loss of Globular Clusters
Authors: Yingtian Chen, Hui Li, Oleg Y. Gnedin
Figure caption: Left panel: CFHT data in the extinction-corrected g − r color vs. r magnitude diagram. The CMD mask for Pal 5 is shown as gray solid curves. Top right panel: selected Pal 5 stream stars in the great circle frame. We compute the background surface density in the outskirt regions with ﹩|{\hat{\phi }}_{2}|\gt 0\mathop{.}\limits^{^\circ }5﹩ (indicated by gray curves). The Pal 5 cluster is shown as the star symbol. Bottom right panel: surface density of the Pal 5 stream with the background subtracted. We use Gaussian kernel density estimation with a 0﹩\mathop{.}\limits^{^\circ }﹩1 bandwidth to estimate the density.
Paper: Stellar Streams Reveal the Mass Loss of Globular Clusters
Authors: Yingtian Chen, Hui Li, Oleg Y. Gnedin
Figure caption: Mass-loss rate (left panel) and mean correction factor (as in Equation (6), right panel) of 12 GCs derived from different MF slopes α. For each GC, we plot the range around the central value with Δα = ±0.3, which is used in this work as the dispersion of α.
Paper: NGDEEP: The Star Formation and Ionization Properties of Galaxies at 1.7 < z < 3.4
Authors: Lu Shen, Casey Papovich, Jasleen Matharu, Nor Pirzkal, Weida Hu, Danielle A. Berg, Micaela B. Bagley, Bren E. Backhaus, Nikko J. Cleri, Mark Dickinson, Steven L. Finkelstein, Nimish P. Hathi, Marc Huertas-Company, Taylor A. Hutchison, Mauro Giavalisco, Norman A. Grogin, Anne E. Jaskot, Intae Jung, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Jennifer M. Lotz, Pablo G. Pérez-González, Barry Rothberg, Raymond C. Simons, Brittany N. Vanderhoof, L. Y. Aaron Yung
Figure caption: Left panels: the relation between the O32 ratio and Hβ EW (top) and Hα EW (bottom) for galaxies in the NGDEEP final sample and low-SNR sample with Hβ and Hα SNR > 5, respectively. Individual galaxies are color-coded by stellar mass. The median O32 values are shown for galaxies at 1.7 < z < 2.5 and 2.5⩽z < 3.4 as black orange-filled and purple-filled dots, respectively. The best fit for galaxies in the final sample with M * > 108.4  M ⊙ is shown as the solid black line and extended to the low EW region as the dashed black line. Right panels: comparison with galaxy samples at different redshift ranges. Median O32 ratios are shown for galaxies at z ∼ 4.5–9.5 from CEERS and JADES (C. P. Papovich et al. 2025, in preparation, open magenta diamonds), galaxies at z ∼ 5.6–9 measured from composite spectra (W. Hu et al. 2024, red star), CLEAR galaxies at z ∼ 1.1–2.3 (open orange squares), z ∼ 0 SDSS galaxies (brown crosses), blueberry galaxies (filled blue triangles), green pea galaxies (filled green triangles). The SDSS sample is shown in black as the 2D histogram. The relations from N. A. Reddy et al. (2018) using MOSDEF galaxies at z ∼ 2.3 are shown as purple lines. The same median values and fits from the NGDEEP final sample are shown, identical to those in the left panel. The NGDEEP sample shows tight EW–O32 relations. A clear evolutionary trend is seen as higher redshift galaxies having higher sSFR and O32.
Paper: NGDEEP: The Star Formation and Ionization Properties of Galaxies at 1.7 < z < 3.4
Authors: Lu Shen, Casey Papovich, Jasleen Matharu, Nor Pirzkal, Weida Hu, Danielle A. Berg, Micaela B. Bagley, Bren E. Backhaus, Nikko J. Cleri, Mark Dickinson, Steven L. Finkelstein, Nimish P. Hathi, Marc Huertas-Company, Taylor A. Hutchison, Mauro Giavalisco, Norman A. Grogin, Anne E. Jaskot, Intae Jung, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Jennifer M. Lotz, Pablo G. Pérez-González, Barry Rothberg, Raymond C. Simons, Brittany N. Vanderhoof, L. Y. Aaron Yung
Figure caption: The distribution of O32 and ionizing photon production rate Q (top) and ionizing production efficiency ξ ion (bottom) for the NGDEEP final sample with Hα or Hβ SNR > 5 detections, color-coded by stellar mass. The median values and best fits for the NGDEEP O32 galaxies with Hα or Hβ detection (without mass cut) are shown as black dots and solid black lines, and 1σ total scatter is shown as the gray regions. Results from the Spearman rank test are shown as well. The median values of galaxies at z = 2.7–6.3 from N. A. Reddy et al. (2023a) are shown as filled blue squares in the top panel. The median values of galaxies at z ∼ 4.5–9.5 from CEERS and JADES (C. P. Papovich et al. 2025, in preparation) are shown in open magenta diamonds. Both Q and ξ ion show correlations with O32.
Paper: NGDEEP: The Star Formation and Ionization Properties of Galaxies at 1.7 < z < 3.4
Authors: Lu Shen, Casey Papovich, Jasleen Matharu, Nor Pirzkal, Weida Hu, Danielle A. Berg, Micaela B. Bagley, Bren E. Backhaus, Nikko J. Cleri, Mark Dickinson, Steven L. Finkelstein, Nimish P. Hathi, Marc Huertas-Company, Taylor A. Hutchison, Mauro Giavalisco, Norman A. Grogin, Anne E. Jaskot, Intae Jung, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Jennifer M. Lotz, Pablo G. Pérez-González, Barry Rothberg, Raymond C. Simons, Brittany N. Vanderhoof, L. Y. Aaron Yung
Figure caption: Top: histogram of Hα/Hβ emission line ratios for the NGDEEP final sample with Hα and Hβ SNR > 5. The vertical orange solid line indicates the median Hα/Hβ ratio, while the dashed lines represent the 16th and 84th percentiles. The vertical black line marks the theoretical minimum value of 2.86 in the absence of dust for Case B recombination. Bottom: comparison of the color excesses derived for the stellar continuum from SED fitting and that for the ionized gas calculated from Hα/Hβ. The E(B − V)gas is computed assuming the J. A. Cardelli et al. (1989) extinction curve with Rv = 3.1. The median stellar-to-gas attenuation ratio for galaxies with Hα/Hβ  > 2.86 is marked by an orange star. The black solid line shows the relation E(B − V)star = 0.44 × E(B − V)gas from D. Calzetti et al. (2000). The gray dashed line shows the one-to-one relation between E(B − V)star and E(B − V)gas.
Paper: NGDEEP: The Star Formation and Ionization Properties of Galaxies at 1.7 < z < 3.4
Authors: Lu Shen, Casey Papovich, Jasleen Matharu, Nor Pirzkal, Weida Hu, Danielle A. Berg, Micaela B. Bagley, Bren E. Backhaus, Nikko J. Cleri, Mark Dickinson, Steven L. Finkelstein, Nimish P. Hathi, Marc Huertas-Company, Taylor A. Hutchison, Mauro Giavalisco, Norman A. Grogin, Anne E. Jaskot, Intae Jung, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Jennifer M. Lotz, Pablo G. Pérez-González, Barry Rothberg, Raymond C. Simons, Brittany N. Vanderhoof, L. Y. Aaron Yung
Figure caption: Comparison of the SED-derived instantaneous SFR (top), and the SFR averaged over 10 Myr (middle) and average over 100 Myr (bottom) and Hα- and Hβ-derived SFR for NGDEEP full sample with Hα and Hβ SNR > 5, respectively. In each panel, the solid orange line shows the best-fitted line using THE LINMIX package (B. C. Kelly 2007) using SFRHα  and SFRHβ  (if SFRHα  is not available). The black dashed line is the one-to-one relation. The median offset between SFRSED and SFRHα  (SFRHβ ) is presented in each panel.
Paper: NGDEEP: The Star Formation and Ionization Properties of Galaxies at 1.7 < z < 3.4
Authors: Lu Shen, Casey Papovich, Jasleen Matharu, Nor Pirzkal, Weida Hu, Danielle A. Berg, Micaela B. Bagley, Bren E. Backhaus, Nikko J. Cleri, Mark Dickinson, Steven L. Finkelstein, Nimish P. Hathi, Marc Huertas-Company, Taylor A. Hutchison, Mauro Giavalisco, Norman A. Grogin, Anne E. Jaskot, Intae Jung, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Jennifer M. Lotz, Pablo G. Pérez-González, Barry Rothberg, Raymond C. Simons, Brittany N. Vanderhoof, L. Y. Aaron Yung
Figure caption: The distribution of ionization parameter (q, top) and metallicity (12+log(O/H), bottom) as a function of O32. Galaxies with all four emission lines >5σ and with three lines ([O II], [O III], and Hβ) >5σ are shown in orange and green, respectively. The orange solid lines show a linear fit to the NGDEEP galaxies with all four emission line detection. The top panel shows the relations from CLEAR galaxies (C. Papovich et al. 2022; black dashed line) and a sample of z ∼ 2.3 SFGs from A. L. Strom et al. (2018; purple dashed line). The bottom panel shows the relation derived from a sample of z ∼ 2–9 galaxies from R. L. Sanders et al. (2024; black dashed line). While O32 correlates with both the ionization parameter and metallicity, the relationship between O32 and the ionization parameter is more pronounced.
Paper: NGDEEP: The Star Formation and Ionization Properties of Galaxies at 1.7 < z < 3.4
Authors: Lu Shen, Casey Papovich, Jasleen Matharu, Nor Pirzkal, Weida Hu, Danielle A. Berg, Micaela B. Bagley, Bren E. Backhaus, Nikko J. Cleri, Mark Dickinson, Steven L. Finkelstein, Nimish P. Hathi, Marc Huertas-Company, Taylor A. Hutchison, Mauro Giavalisco, Norman A. Grogin, Anne E. Jaskot, Intae Jung, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Jennifer M. Lotz, Pablo G. Pérez-González, Barry Rothberg, Raymond C. Simons, Brittany N. Vanderhoof, L. Y. Aaron Yung
Figure caption: The distribution of the O32 ratio and ΣSFR values for the NGDEEP final sample using effective radius measured from the HST F060W (top) and JWST F090W images (bottom). The data points are color-coded by sSFR. For galaxies identified with more than one component, we use the effective radius of the brightest clump. Such galaxies are marked with open black diamonds. In both panels, the median values of galaxies at z = 2.7–6.3 from N. A. Reddy et al. (2023a) are shown as filled blue squares, and the fit for MOSDEF galaxies at z ∼ 2–4 (N. A. Reddy et al. 2023b) are shown as a blue dotted line. The SFR surface density may contribute to affecting O32, but with a considerable scatter and sensitivity to the bandpass used for size measurements.
Paper: NGDEEP: The Star Formation and Ionization Properties of Galaxies at 1.7 < z < 3.4
Authors: Lu Shen, Casey Papovich, Jasleen Matharu, Nor Pirzkal, Weida Hu, Danielle A. Berg, Micaela B. Bagley, Bren E. Backhaus, Nikko J. Cleri, Mark Dickinson, Steven L. Finkelstein, Nimish P. Hathi, Marc Huertas-Company, Taylor A. Hutchison, Mauro Giavalisco, Norman A. Grogin, Anne E. Jaskot, Intae Jung, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Jennifer M. Lotz, Pablo G. Pérez-González, Barry Rothberg, Raymond C. Simons, Brittany N. Vanderhoof, L. Y. Aaron Yung
Figure caption: Top: 1D spectrum of two galaxies with log(O32) > 0.75 and IZI-derived E(B − V) ≃ 0. Each panel shows the NIRISS grism data (black dots) along with the best-fit spectrum (red line). Important emission lines are marked by vertical gray dashed lines. Bottom: the corner plot of ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})﹩, ﹩\mathrm{log}(q)﹩, and E(B − V) from IZI for the same galaxies as the top panel. The median and associated uncertainties are displayed on the top of the histograms.
Paper: NGDEEP: The Star Formation and Ionization Properties of Galaxies at 1.7 < z < 3.4
Authors: Lu Shen, Casey Papovich, Jasleen Matharu, Nor Pirzkal, Weida Hu, Danielle A. Berg, Micaela B. Bagley, Bren E. Backhaus, Nikko J. Cleri, Mark Dickinson, Steven L. Finkelstein, Nimish P. Hathi, Marc Huertas-Company, Taylor A. Hutchison, Mauro Giavalisco, Norman A. Grogin, Anne E. Jaskot, Intae Jung, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Jennifer M. Lotz, Pablo G. Pérez-González, Barry Rothberg, Raymond C. Simons, Brittany N. Vanderhoof, L. Y. Aaron Yung
Figure caption: Left: the difference between nebular reddening E(B − V)gas derived using the Balmer decrement (BD) and stellar reddening E(B − V)star from SED fitting as a function of SFRHα  for SFGs at z ∼ 2 with detections of both Hα and Hβ SNR > 5. The orange solid line shows the best fit, with the shaded region indicating the 1σ uncertainties. The dashed black line shows the relation from R. L. Sanders et al. (2021). Right: SFRHα  vs. SFRSED,10 Myr. The solid black line shows the one-to-one relation.
Paper: NGDEEP: The Star Formation and Ionization Properties of Galaxies at 1.7 < z < 3.4
Authors: Lu Shen, Casey Papovich, Jasleen Matharu, Nor Pirzkal, Weida Hu, Danielle A. Berg, Micaela B. Bagley, Bren E. Backhaus, Nikko J. Cleri, Mark Dickinson, Steven L. Finkelstein, Nimish P. Hathi, Marc Huertas-Company, Taylor A. Hutchison, Mauro Giavalisco, Norman A. Grogin, Anne E. Jaskot, Intae Jung, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Jennifer M. Lotz, Pablo G. Pérez-González, Barry Rothberg, Raymond C. Simons, Brittany N. Vanderhoof, L. Y. Aaron Yung
Figure caption: Median fraction of galaxies with [O III] or [O II] detection above our 5σ emission line flux limit from downscaling galaxies as orange and purple solid lines. The fraction distributions of 100 bootstrapping iterations are shown as faint lines. Our empirically derived 80% mass-completeness limits are indicated by vertical dashed lines, and the 16th to 80th percentiles are shown as shaded regions.
Paper: Time-resolved Hubble Space Telescope UV Observations of an X-Ray Quasiperiodic Eruption Source
Authors: T. Wevers, M. Guolo, S. Lockwood, A. Mummery, D. R. Pasham, R. Arcodia
Figure caption: Image and lightcurves of eRO-QPE2. The top left panel shows an FUV image of the eRO-QPE2 host galaxy, while the top right panel shows a zoom-in of the white box (0﹩\mathop{.}\limits^{\unicode{x02033}}﹩75 on a side), indicating the 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩122 aperture used to perform the photometry of the nucleus. The middle panels show the X-ray lightcurves overlaid with the HST on-source periods in orange. Gray data points indicate quiescence, while blue/red/green point indicate eruption rise/peak/decay, respectively. The bottom panels show the FUV measurements made on the per-orbit stacked images with 1σ uncertainties. No statistically significant variability is evident, regardless of whether the X-ray QPE is active or not.
Paper: Pearls on a String: Dark and Bright Galaxies on a Strikingly Straight and Narrow Filament
Authors: M. Arabsalmani, S. Roychowdhury, B. Schneider, V. Springel, E. Le Floc'h, F. Bournaud, A. Burkert, J.-C. Cuillandre, P.-A. Duc, E. Emsellem, D. Galárraga-Espinosa, E. Pian, F. Renaud, M. A. Zwaan
Figure caption: Left: 6∘ × 6∘ image, centered at the position of 2MASX J11093966-–1235116 (G3), showing galaxies with measured spectroscopic redshift listed in SIMBAD. We have also added LEDA 951348 (G4) with its redshift measured from the H I 21 cm emission line. The gray dashed box marks the frame of the right panel. Right: 2∘ × 2∘ image, showing the eight galaxies (G1–G8) along the narrow filament (see Table 1 for galaxy properties). The gray dashed line shows the best-fit straight line to the positions of the eight galaxies. In both panels, the color of the points represents the redshift values of the galaxies following the representative color bars above the panels. The dotted–dashed blue circle (centered at the position of 2MASX J11093966–1235116, G3) marks the JVLA HPBW for the H I 21 cm emission line observations we present in this Letter.
Paper: Pearls on a String: Dark and Bright Galaxies on a Strikingly Straight and Narrow Filament
Authors: M. Arabsalmani, S. Roychowdhury, B. Schneider, V. Springel, E. Le Floc'h, F. Bournaud, A. Burkert, J.-C. Cuillandre, P.-A. Duc, E. Emsellem, D. Galárraga-Espinosa, E. Pian, F. Renaud, M. A. Zwaan
Figure caption: Each row presents a source listed in Table 2. Left: Total intensity map of H I 21 cm emission line in color, overlaid with contours of H I 21 cm emission line. The outermost contour marks the 3σ level of emission in a single channel with a velocity width of 34 km s−1 (equivalent to the H I column densities provided in Table 2). Each subsequent contour is in multiples of ﹩\sqrt{2}﹩. Middle: The r-band CFHT image, overlaid with the 3σ contour of H I 21 cm emission line. The detected optical sources are marked with their identification numbers and circles. For sources marked with red color, association with the filament is ruled out based on photometric redshift measurements. For the sources marked with yellow color (listed in Table 5), z = 0.037 is not ruled out. Right: The intensity-weighted velocity map of H I 21 cm emission line in color, overlaid with the 3σ contour of H I 21 cm emission line. The size of the images in all panels are 50″× 50″except for S12 where the image sizes are 100″ × 100″. The synthesized beam of JVLA observations is shown in the bottom left corners of the maps.
Paper: Pearls on a String: Dark and Bright Galaxies on a Strikingly Straight and Narrow Filament
Authors: M. Arabsalmani, S. Roychowdhury, B. Schneider, V. Springel, E. Le Floc'h, F. Bournaud, A. Burkert, J.-C. Cuillandre, P.-A. Duc, E. Emsellem, D. Galárraga-Espinosa, E. Pian, F. Renaud, M. A. Zwaan
Figure caption: Left: the perpendicular (on-sky) distance to the filament axis, δ, vs. the distance along the filament axis from a reference point on the line, l. We have chosen G1 as the reference point, which is located at l = 0 (hence, G8 is located at l = 4.99 Mpc, the length of the filament). The filament axis is presented with the dashed line in the right panel of Figure 1. Right: the radial velocity with respect to zmed = 0.0368 (the median, and also the average, redshift of the eight galaxies on the filament), v, vs. l. The pink and blue points represent the eight galaxies and the 11 H I sources, respectively, in both panels.
Paper: Pearls on a String: Dark and Bright Galaxies on a Strikingly Straight and Narrow Filament
Authors: M. Arabsalmani, S. Roychowdhury, B. Schneider, V. Springel, E. Le Floc'h, F. Bournaud, A. Burkert, J.-C. Cuillandre, P.-A. Duc, E. Emsellem, D. Galárraga-Espinosa, E. Pian, F. Renaud, M. A. Zwaan
Figure caption: Three examples for 2° × 2° fields in the full-sky galaxy light cone of the MillenniumTNG simulation, selected to contain galaxies with similar masses and redshifts as observed and to exhibit a similarly long and narrow filamentary distribution. We measure the thinness of the galaxy distribution through a quantity T defined as the ratio between the averaged perpendicular distances (green) between galaxies and the ridgeline of their filament (blue) and the length of the extension of the galaxy distribution in the filament direction. The histogram in the bottom right panel shows the distribution of this quantity for the 1017 fields we have with matching galaxy number density. For our observed galaxy distribution, the value of the thinness parameter is Tobs = 0.035 (vertical dashed line). About 4% of the fields have an equal or lower value for T, implying that the configuration we have discovered is rare in ΛCDM, but not exceptionally so.