adsabs/AstroCLIMB huggingface dataset:
Paper: Detecting Molecular Hydrogen (H2) Emission at Cosmic Dawn
Authors: Madisen Johnson, Blakesley Burkhart, Francesco D'Eugenio, Sandro Tacchella, Roberto Maiolino, Shmuel Bialy, Jacques Le Bourlot, Evelyne Roueff, Franck Le Petit, Emeric Bron, Hervé Abgrall, Erica Nelson, Shyam Menon, Matthew E. Orr
Figure caption: H2 emissivity spatial repartition in a small range of wavelength (measured in the local rest frame). The model predicts a strong and rather uniform emissivity leading to the continuum part of the fluorescence spectrum in region 1 (lower part of the map). In region 2 (upper part of the map), only emission lines remain.
Paper: Detecting Molecular Hydrogen (H2) Emission at Cosmic Dawn
Authors: Madisen Johnson, Blakesley Burkhart, Francesco D'Eugenio, Sandro Tacchella, Roberto Maiolino, Shmuel Bialy, Jacques Le Bourlot, Evelyne Roueff, Franck Le Petit, Emeric Bron, Hervé Abgrall, Erica Nelson, Shyam Menon, Matthew E. Orr
Figure caption: Comparison of the inverse-variance stacked H2 fluorescent emission feature with our high-redshift Meudon model, which has been shifted by 0.18 nm or 340 km s−1 (blue line). This displays the unique profile of the potential detection, which could indicate the presence of molecular outflows.
Paper: Detecting Molecular Hydrogen (H2) Emission at Cosmic Dawn
Authors: Madisen Johnson, Blakesley Burkhart, Francesco D'Eugenio, Sandro Tacchella, Roberto Maiolino, Shmuel Bialy, Jacques Le Bourlot, Evelyne Roueff, Franck Le Petit, Emeric Bron, Hervé Abgrall, Erica Nelson, Shyam Menon, Matthew E. Orr
Figure caption: Temperature (red line) and density (blue line) profiles of the illuminated cloud in our Meudon PDR model. The profiles showcase two distinct regions: a hot and diffuse outer envelope, which transitions to a cooler and denser region deeper into the cloud.
Paper: Detecting Molecular Hydrogen (H2) Emission at Cosmic Dawn
Authors: Madisen Johnson, Blakesley Burkhart, Francesco D'Eugenio, Sandro Tacchella, Roberto Maiolino, Shmuel Bialy, Jacques Le Bourlot, Evelyne Roueff, Franck Le Petit, Emeric Bron, Hervé Abgrall, Erica Nelson, Shyam Menon, Matthew E. Orr
Figure caption: H and H2 profiles of the illuminated cloud and its two distinct regions. The outer envelope composed of fully atomic gas, and the inner region contains a significant amount of warm H2 gas.
Paper: Detecting Molecular Hydrogen (H2) Emission at Cosmic Dawn
Authors: Madisen Johnson, Blakesley Burkhart, Francesco D'Eugenio, Sandro Tacchella, Roberto Maiolino, Shmuel Bialy, Jacques Le Bourlot, Evelyne Roueff, Franck Le Petit, Emeric Bron, Hervé Abgrall, Erica Nelson, Shyam Menon, Matthew E. Orr
Figure caption: Effective formation rate coefficient of H2.
Paper: Detecting Molecular Hydrogen (H2) Emission at Cosmic Dawn
Authors: Madisen Johnson, Blakesley Burkhart, Francesco D'Eugenio, Sandro Tacchella, Roberto Maiolino, Shmuel Bialy, Jacques Le Bourlot, Evelyne Roueff, Franck Le Petit, Emeric Bron, Hervé Abgrall, Erica Nelson, Shyam Menon, Matthew E. Orr
Figure caption: Inverse-variance stacked spectrum (top row) and the SNR (bottom row) of all JWST JADES galaxies with redshifts z ≥ 7, investigating the tentative detections of C IV, H2 Fluorescence, He II, O III], and C III].
Paper: Morphology of 35 Repeating Fast Radio Burst Sources at Microsecond Time Scales with CHIME/FRB
Authors: Alice P. Curtin, Ketan R. Sand, Ziggy Pleunis, Naman Jain, Victoria Kaspi, Daniele Michilli, Emmanuel Fonseca, Kaitlyn Shin, Kenzie Nimmo, Charanjot Brar, Fengqiu Adam Dong, Gwendolyn M. Eadie, B. M. Gaensler, Antonio Herrera-Martin, Adaeze L. Ibik, Ronniy C. Joseph, Jane Kaczmarek, Calvin Leung, Robert Main, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Cherry Ng, Ayush Pandhi, Aaron B. Pearlman, Masoud Rafiei-Ravandi, Mawson W. Sammons, Paul Scholz, Kendrick Smith, Ingrid Stairs
Figure caption: Band-averaged fluence (calculated over the entire CHIME/FRB bandwidth), CHIME/FRB frequency range, and DM for FRB 20181119A as a function of time. Error bars for fluence and DM are shown at the 99% confidence level. The time resolution at which the burst is analyzed is shown by the color of the points. The lowest time resolution is 0.655 ms, while the highest is 2.56 μs. For this source, all bursts were analyzed at a time resolution of 0.655 ms, so no variation is seen in the color. We note that the uncertainties for bursts studied at a time resolution of 0.655 ms may be underestimated due to the inability to discern structure at such a low time resolution. For the DM, we show the inverse-variance weighted average as a red line. Bursts for which we could not calculate an optimal structure-maximized DM, and hence for which a by-eye DM was estimated, are shown as crosses. By-eye DMs were only estimated to within ∼0.5 pc cm−3.
Paper: Morphology of 35 Repeating Fast Radio Burst Sources at Microsecond Time Scales with CHIME/FRB
Authors: Alice P. Curtin, Ketan R. Sand, Ziggy Pleunis, Naman Jain, Victoria Kaspi, Daniele Michilli, Emmanuel Fonseca, Kaitlyn Shin, Kenzie Nimmo, Charanjot Brar, Fengqiu Adam Dong, Gwendolyn M. Eadie, B. M. Gaensler, Antonio Herrera-Martin, Adaeze L. Ibik, Ronniy C. Joseph, Jane Kaczmarek, Calvin Leung, Robert Main, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Cherry Ng, Ayush Pandhi, Aaron B. Pearlman, Masoud Rafiei-Ravandi, Mawson W. Sammons, Paul Scholz, Kendrick Smith, Ingrid Stairs
Figure caption: Top-left panel: sub-burst width distribution for repeating and thus-far nonrepeating FRBs. We limit the two samples to only include bursts studied at a time resolution ≤0.16 ms. Top-right panel: the same as the left panel except for the sub-burst width normalized by the total burst duration. Middle-left panel: wait time distribution for repeating and thus-far nonrepeating FRBs. The wait time is defined as the difference in arrival time between subsequent sub-bursts for a given FRB. The sample is limited to bursts that were analyzed at time resolutions equal to or less than 0.16 ms. Middle-right panel: the same as the left panel except for the duration-normalized wait time. Each wait time is normalized by the total duration of that given burst. Bottom panel: number of sub-burst components for repeating and thus-far nonrepeating FRBs. We limit the two samples to only include bursts studied at a time resolution ≤0.16 ms.
Paper: Morphology of 35 Repeating Fast Radio Burst Sources at Microsecond Time Scales with CHIME/FRB
Authors: Alice P. Curtin, Ketan R. Sand, Ziggy Pleunis, Naman Jain, Victoria Kaspi, Daniele Michilli, Emmanuel Fonseca, Kaitlyn Shin, Kenzie Nimmo, Charanjot Brar, Fengqiu Adam Dong, Gwendolyn M. Eadie, B. M. Gaensler, Antonio Herrera-Martin, Adaeze L. Ibik, Ronniy C. Joseph, Jane Kaczmarek, Calvin Leung, Robert Main, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Cherry Ng, Ayush Pandhi, Aaron B. Pearlman, Masoud Rafiei-Ravandi, Mawson W. Sammons, Paul Scholz, Kendrick Smith, Ingrid Stairs
Figure caption: Left panel: scattering vs. extragalactic (+halo) DM for repeaters and nonrepeaters. For DM, we subtract the Galactic component as determined using NE2001. Downward arrows represent upper limits on scattering timescales. For repeating FRBs, this is assumed to be the width of the narrowest sub-burst for that event. For nonrepeating FRB parameter descriptions, see K. R. Sand et al. (2024). Right panel: cumulative distribution function (CDF) for scattering for repeating and thus-far nonrepeating FRBs using the Kaplan–Meier method for left-censored data.
Paper: Morphology of 35 Repeating Fast Radio Burst Sources at Microsecond Time Scales with CHIME/FRB
Authors: Alice P. Curtin, Ketan R. Sand, Ziggy Pleunis, Naman Jain, Victoria Kaspi, Daniele Michilli, Emmanuel Fonseca, Kaitlyn Shin, Kenzie Nimmo, Charanjot Brar, Fengqiu Adam Dong, Gwendolyn M. Eadie, B. M. Gaensler, Antonio Herrera-Martin, Adaeze L. Ibik, Ronniy C. Joseph, Jane Kaczmarek, Calvin Leung, Robert Main, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Cherry Ng, Ayush Pandhi, Aaron B. Pearlman, Masoud Rafiei-Ravandi, Mawson W. Sammons, Paul Scholz, Kendrick Smith, Ingrid Stairs
Figure caption: Left panel: band-averaged spectral fluence distribution for repeating and thus-far nonrepeating FRBs over the entire 400 MHz CHIME/FRB bandwidth. As repeating FRBs have a different threshold for triggering the complex raw voltages than nonrepeaters at CHIME/FRB, we limit the sample to bursts (repeating and nonrepeating) whose detection S/N > 20. We also only include bursts for which the full CHIME/FRB band was recorded. Right panel: the same as left panel except for a band-limited spectral fluence calculation in which the spectral fluence is only determined over the frequency channels that contain emission from the source.
Paper: Morphology of 35 Repeating Fast Radio Burst Sources at Microsecond Time Scales with CHIME/FRB
Authors: Alice P. Curtin, Ketan R. Sand, Ziggy Pleunis, Naman Jain, Victoria Kaspi, Daniele Michilli, Emmanuel Fonseca, Kaitlyn Shin, Kenzie Nimmo, Charanjot Brar, Fengqiu Adam Dong, Gwendolyn M. Eadie, B. M. Gaensler, Antonio Herrera-Martin, Adaeze L. Ibik, Ronniy C. Joseph, Jane Kaczmarek, Calvin Leung, Robert Main, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Cherry Ng, Ayush Pandhi, Aaron B. Pearlman, Masoud Rafiei-Ravandi, Mawson W. Sammons, Paul Scholz, Kendrick Smith, Ingrid Stairs
Figure caption: Bandwidth vs. total duration for repeating and thus-far nonrepeating FRBs. Bursts for which the full bandwidth was not available are indicated with arrows. Additionally, bursts for which the bandwidth is 400 MHz are again lower limits, as this is solely set by the frequency range of CHIME. The normalized histograms and the CDFs only include bursts for which the full bandwidth was recorded.
Paper: Morphology of 35 Repeating Fast Radio Burst Sources at Microsecond Time Scales with CHIME/FRB
Authors: Alice P. Curtin, Ketan R. Sand, Ziggy Pleunis, Naman Jain, Victoria Kaspi, Daniele Michilli, Emmanuel Fonseca, Kaitlyn Shin, Kenzie Nimmo, Charanjot Brar, Fengqiu Adam Dong, Gwendolyn M. Eadie, B. M. Gaensler, Antonio Herrera-Martin, Adaeze L. Ibik, Ronniy C. Joseph, Jane Kaczmarek, Calvin Leung, Robert Main, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Cherry Ng, Ayush Pandhi, Aaron B. Pearlman, Masoud Rafiei-Ravandi, Mawson W. Sammons, Paul Scholz, Kendrick Smith, Ingrid Stairs
Figure caption: The same as Figure 7 except for FRB 20190208A. As FRB 20190208A has at least one burst with a measured scattering timescale, we also include the scattering timescale. For bursts for which there was no by-eye visible scattering timescale, we determine an upper limit on the scattering timescale as equivalent to the reported width of the narrowest sub-burst.
Paper: Morphology of 35 Repeating Fast Radio Burst Sources at Microsecond Time Scales with CHIME/FRB
Authors: Alice P. Curtin, Ketan R. Sand, Ziggy Pleunis, Naman Jain, Victoria Kaspi, Daniele Michilli, Emmanuel Fonseca, Kaitlyn Shin, Kenzie Nimmo, Charanjot Brar, Fengqiu Adam Dong, Gwendolyn M. Eadie, B. M. Gaensler, Antonio Herrera-Martin, Adaeze L. Ibik, Ronniy C. Joseph, Jane Kaczmarek, Calvin Leung, Robert Main, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Cherry Ng, Ayush Pandhi, Aaron B. Pearlman, Masoud Rafiei-Ravandi, Mawson W. Sammons, Paul Scholz, Kendrick Smith, Ingrid Stairs
Figure caption: Sub-burst width vs. total burst duration for all repeating and nonrepeating bursts studied at time resolutions ≤0.16 ms. We do not include bursts for which there is only one component. The gray shaded region indicates an unphysical phase space where the sub-burst width would be larger than the total burst duration.
Paper: Morphology of 35 Repeating Fast Radio Burst Sources at Microsecond Time Scales with CHIME/FRB
Authors: Alice P. Curtin, Ketan R. Sand, Ziggy Pleunis, Naman Jain, Victoria Kaspi, Daniele Michilli, Emmanuel Fonseca, Kaitlyn Shin, Kenzie Nimmo, Charanjot Brar, Fengqiu Adam Dong, Gwendolyn M. Eadie, B. M. Gaensler, Antonio Herrera-Martin, Adaeze L. Ibik, Ronniy C. Joseph, Jane Kaczmarek, Calvin Leung, Robert Main, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Cherry Ng, Ayush Pandhi, Aaron B. Pearlman, Masoud Rafiei-Ravandi, Mawson W. Sammons, Paul Scholz, Kendrick Smith, Ingrid Stairs
Figure caption: The same as Figure 8 except for FRB 20190303A. We do not include an extreme outlier burst for which the fluence was 351 Jy ms on 2021 June 6.
Paper: Morphology of 35 Repeating Fast Radio Burst Sources at Microsecond Time Scales with CHIME/FRB
Authors: Alice P. Curtin, Ketan R. Sand, Ziggy Pleunis, Naman Jain, Victoria Kaspi, Daniele Michilli, Emmanuel Fonseca, Kaitlyn Shin, Kenzie Nimmo, Charanjot Brar, Fengqiu Adam Dong, Gwendolyn M. Eadie, B. M. Gaensler, Antonio Herrera-Martin, Adaeze L. Ibik, Ronniy C. Joseph, Jane Kaczmarek, Calvin Leung, Robert Main, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Cherry Ng, Ayush Pandhi, Aaron B. Pearlman, Masoud Rafiei-Ravandi, Mawson W. Sammons, Paul Scholz, Kendrick Smith, Ingrid Stairs
Figure caption: The same as Figure 8 except for FRB 20190417A.
Paper: Revisiting the Supermassive Black Hole Mass of NGC 7052 Using High Spatial Resolution Molecular Gas Observed with ALMA
Authors: Hai N. Ngo, Dieu D. Nguyen, Tinh Q. T. Le, Khue N. H. Ho, Tien H. T. Ho, Elena Gallo, Kristina Nyland, Masatoshi Imanishi, Kouichiro Nakanishi, Que T. Le, Fabio Pacucci, Eden Girma
Figure caption: Upper-row panels: The PVDs compare our ALMA observations of the 12CO(2−1) emission (orange-filled contours) with different KINMS models (blue contours), which assumed the gas distribution with the SKYSAMPLER tool. These models are extracted along the galaxy’s major axis at a PA of Γ = 63﹩\mathop{.}\limits^{\unicode{x000b0}}﹩9 and correspond to three different central SMBH masses: a model without a BH (left), the best-fitting SMBH from this study (center), and an overly large SMBH (right). The SMBH mass and M/LF814W for each case are indicated in the top-right corner of each panel. The black dashed lines mark the dynamical center, defined as the peak of the 1.3 mm continuum emission (Section 2.1). The intersection of these lines represents the systemic velocity (vsys) of the galaxy, shown on the velocity scale to the right. Lower-row panels: The same KINMS models, which assumed the gas surface brightness distribution with an analytically axisymmetric function as the sum of two center-offset Gaussians.
Paper: Revisiting the Supermassive Black Hole Mass of NGC 7052 Using High Spatial Resolution Molecular Gas Observed with ALMA
Authors: Hai N. Ngo, Dieu D. Nguyen, Tinh Q. T. Le, Khue N. H. Ho, Tien H. T. Ho, Elena Gallo, Kristina Nyland, Masatoshi Imanishi, Kouichiro Nakanishi, Que T. Le, Fabio Pacucci, Eden Girma
Figure caption: The corner plot shows the posterior distributions obtained after removing the initial 20% of the post-burn-in phase from a total of 105 MCMC iterations using the KINMS model, which assumed the gas distribution with the SKYSAMPLER tool. The top 1D histograms display the marginalized posterior distributions for each parameter, along with their 1σ uncertainties (see text for details). The lower panels present 2D scatter plots of parameter pairs, where colors indicate CLs, ranging from 1σ (white) to 3σ (blue), with black representing CLs below 3σ. Detailed results are listed in Table 5.
Paper: Revisiting the Supermassive Black Hole Mass of NGC 7052 Using High Spatial Resolution Molecular Gas Observed with ALMA
Authors: Hai N. Ngo, Dieu D. Nguyen, Tinh Q. T. Le, Khue N. H. Ho, Tien H. T. Ho, Elena Gallo, Kristina Nyland, Masatoshi Imanishi, Kouichiro Nakanishi, Que T. Le, Fabio Pacucci, Eden Girma
Figure caption: The first-moment residual map (data-model) was derived by subtracting the intensity-weighted mean velocity field of the best-fit KINMS models from the observed data. The differences are ≲15 km s−1 (or ≲4%) for the best-fitting KINMS model with SKYSAMPLER and ≲40 km s−1 (or ≲10%) for the best-fitting KINMS model with an axisymmetric function, indicating good agreement between the data and the assumed models, and showing the absence of noncircular motions within the 12CO(2−1)-CND of NGC 7052.
Paper: Revisiting the Supermassive Black Hole Mass of NGC 7052 Using High Spatial Resolution Molecular Gas Observed with ALMA
Authors: Hai N. Ngo, Dieu D. Nguyen, Tinh Q. T. Le, Khue N. H. Ho, Tien H. T. Ho, Elena Gallo, Kristina Nyland, Masatoshi Imanishi, Kouichiro Nakanishi, Que T. Le, Fabio Pacucci, Eden Girma
Figure caption: PVDs along the major axis of the best-fitting KINMS models using the SKYSAMPLER tool to describe the 12CO(2−1) gas surface brightness distribution, shown for models with linear (left) and Gaussian (right) M/LF814W(r) profiles.
Paper: Revisiting the Supermassive Black Hole Mass of NGC 7052 Using High Spatial Resolution Molecular Gas Observed with ALMA
Authors: Hai N. Ngo, Dieu D. Nguyen, Tinh Q. T. Le, Khue N. H. Ho, Tien H. T. Ho, Elena Gallo, Kristina Nyland, Masatoshi Imanishi, Kouichiro Nakanishi, Que T. Le, Fabio Pacucci, Eden Girma
Figure caption: Same as Figure 14 but the KINMS model assumed the gas surface brightness as the sum of two center-offset Gaussians.
Paper: Revisiting the Supermassive Black Hole Mass of NGC 7052 Using High Spatial Resolution Molecular Gas Observed with ALMA
Authors: Hai N. Ngo, Dieu D. Nguyen, Tinh Q. T. Le, Khue N. H. Ho, Tien H. T. Ho, Elena Gallo, Kristina Nyland, Masatoshi Imanishi, Kouichiro Nakanishi, Que T. Le, Fabio Pacucci, Eden Girma
Figure caption: The PVD along the major axis of models consist of an SMBH mass of MBH=3.9 × 108 M⊙ derived from ionized gas by R. P. van der Marel & F. C. van den Bosch (1998) with a constant M/LF814W.
Paper: Revisiting the Supermassive Black Hole Mass of NGC 7052 Using High Spatial Resolution Molecular Gas Observed with ALMA
Authors: Hai N. Ngo, Dieu D. Nguyen, Tinh Q. T. Le, Khue N. H. Ho, Tien H. T. Ho, Elena Gallo, Kristina Nyland, Masatoshi Imanishi, Kouichiro Nakanishi, Que T. Le, Fabio Pacucci, Eden Girma
Figure caption: The PVD extracted along the CND’s major axis (elongated along the orientation of PA Γ = 63﹩\mathop{.}\limits^{\unicode{x000b0}}﹩8 + 90°) with a systemic velocity vsys = 4610 km s−1. The best-fitting KINMS model using the SKYSAMPLER tool to describe the gas distribution is overlaid on the top as the blued contours.
Paper: Revisiting the Supermassive Black Hole Mass of NGC 7052 Using High Spatial Resolution Molecular Gas Observed with ALMA
Authors: Hai N. Ngo, Dieu D. Nguyen, Tinh Q. T. Le, Khue N. H. Ho, Tien H. T. Ho, Elena Gallo, Kristina Nyland, Masatoshi Imanishi, Kouichiro Nakanishi, Que T. Le, Fabio Pacucci, Eden Girma
Figure caption: Overlay of our ALMA 12CO(2−1) integrated spectrum (black), which is shown in panel (E) of Figure 3, with our best-fitting KINMS models (red).
Paper: Revisiting the Supermassive Black Hole Mass of NGC 7052 Using High Spatial Resolution Molecular Gas Observed with ALMA
Authors: Hai N. Ngo, Dieu D. Nguyen, Tinh Q. T. Le, Khue N. H. Ho, Tien H. T. Ho, Elena Gallo, Kristina Nyland, Masatoshi Imanishi, Kouichiro Nakanishi, Que T. Le, Fabio Pacucci, Eden Girma
Figure caption: Enclosed mass of NGC 7052 (black solid line) as a function of radius, showing the contributions of all mass components: MBH, stars, and ISM (i.e., gas and dust).
Paper: MC-BLOS: Automated Software for Determining the Line-of-sight Component of Magnetic Fields Associated with Molecular Clouds 
Authors: Mehrnoosh Tahani, John Ming Ngo, Jennifer Glover, Ryan Clairmont, Gabriel M. Zarazua, René Plume
Figure caption: Flowchart showing the steps in determining direction (assuming stability trend, i.e., find optimal reference points, is set to True). The process starts with setting an extinction threshold (AV,th) to identify potential OFF points and proceeds through several filtering steps. The software identifies OFF points with low extinction values, removes anomalous points (those too close to high-extinction regions or with unusual RM values), and performs stability trend analysis to determine the number of reference points. If quadrant selection is enabled, the software further ensures adequate sampling from different regions around the cloud by selecting a minimum number of points from each quadrant. Finally, depending on the chosen weighting scheme, RMref is calculated either as a simple average or with quadrant-based weighting of the selected reference points. This RMref value is then subtracted from each ON point’s RM to determine the cloud’s contribution to rotation measure (RMMC) and consequently the direction of BLOS at each point. Rectangular boxes represent processes, diamond shapes indicate decision points, and arrows show the flow direction.
Paper: MC-BLOS: Automated Software for Determining the Line-of-sight Component of Magnetic Fields Associated with Molecular Clouds 
Authors: Mehrnoosh Tahani, John Ming Ngo, Jennifer Glover, Ryan Clairmont, Gabriel M. Zarazua, René Plume
Figure caption: Illustration of the quadrant division and anomalous (rejected) reference points for the Perseus Molecular Cloud. The background color image shows the extinction map of the region. The cloud is divided into four quadrants (separated by blue and red lines) to ensure thorough sampling around the cloud when selecting reference points. Green circles mark anomalous (rejected) potential OFF points, with points 63 and 76 identified as being too close to high-extinction regions based on the default input parameters. No anomalous reference RM values (statistical outliers) were found in this case. This quadrant division approach allows the software to ensure that each region around the cloud contributes equally to the determination of RMref when the quadrant weighting option is enabled, preventing bias that might arise from uneven sampling.
Paper: MC-BLOS: Automated Software for Determining the Line-of-sight Component of Magnetic Fields Associated with Molecular Clouds 
Authors: Mehrnoosh Tahani, John Ming Ngo, Jennifer Glover, Ryan Clairmont, Gabriel M. Zarazua, René Plume
Figure caption: Stability trend analysis for the Perseus cloud, showing how the calculated BLOS (y-axis) changes as increasing numbers of reference points (x-axis) are used in the analysis. Each colored line represents a different ON point in the data set. The software calculates BLOS for each point by incrementally including more reference points (sorted by extinction from lowest to highest). Initially, with few reference points, the BLOS values show significant fluctuations. As more reference points are added, the values tend to stabilize around a certain number, indicating that a sufficient number of reference points has been reached to reliably estimate the Galactic contribution to the rotation measure. This analysis helps determine an optimal number of reference points to use—to provide a stable RMref value while preserving as many points as possible as ON points.
Paper: MC-BLOS: Automated Software for Determining the Line-of-sight Component of Magnetic Fields Associated with Molecular Clouds 
Authors: Mehrnoosh Tahani, John Ming Ngo, Jennifer Glover, Ryan Clairmont, Gabriel M. Zarazua, René Plume
Figure caption: Flowchart illustrating the steps in determining the strength of BLOS. The process follows two parallel initial steps: (1) retrieving chemical evolution results using cloud-specific input parameters (cosmic-ray ionization rate IRCR, UV ionization rate IRUV, temperature T, and density n), and (2) finding the extinction value (AV) or column density at each RMON point. The software then divides the cloud into layers reaching half the total extinction (﹩{A}_{V,{\rm{M}}{\rm{C}}}/2﹩, assuming cloud symmetry), and determines the electron abundance (Xe,i) in each layer. The electron column density for each layer (Ne,i) is calculated using Xe,i and the extinction in that layer. Finally, the total electron column density is determined by summing the contributions from all layers and multiplying by 2 to account for the symmetrical back half of the cloud. The ellipse and rectangles represent starting point and processes, respectively.