adsabs/AstroCLIMB huggingface dataset:
Paper: ALMA Spectral Survey of an Eruptive Young Star, V883 Ori (ASSAY). II. Freshly Sublimated Complex Organic Molecules in the Keplerian Disk
Authors: Jae-Hong Jeong, Jeong-Eun Lee, Seonjae Lee, Giseon Baek, Ji-Hyun Kang, Seokho Lee, Chul-Hwan Kim, Hyeong-Sik Yun, Yuri Aikawa, Gregory J. Herczeg, Doug Johnstone, Lucas Cieza
Figure caption: Examples of iterative LTE line-fitting results on a molecule that emits mostly optically thin lines (13CH3OH), and several optically thick lines (CH3OCHO). The zeroth iteration indicates the fitting result when using the isolated lines without optical depth consideration. The remaining iterations show the results of the fitting using optically thin (τν,line < 0.7), isolated lines extracted from the results of the previous iteration. The numbers under data points are the number of isolated molecular lines used in the LTE fitting in that iteration. The number in the upper right of each figure is the column density obtained as the final result of this method, which is also drawn as a blue horizontal dashed line.
Paper: ALMA Spectral Survey of an Eruptive Young Star, V883 Ori (ASSAY). II. Freshly Sublimated Complex Organic Molecules in the Keplerian Disk
Authors: Jae-Hong Jeong, Jeong-Eun Lee, Seonjae Lee, Giseon Baek, Ji-Hyun Kang, Seokho Lee, Chul-Hwan Kim, Hyeong-Sik Yun, Yuri Aikawa, Gregory J. Herczeg, Doug Johnstone, Lucas Cieza
Figure caption: Example rotation diagrams for optically thin (13CH3OH, left panel) and thick (CH3OCHO, center and right panels) molecules. On the right panel, the gray data points are lines with relatively high Aij, and those with color are lines with relatively low Aij. The red dashed line on the right panel is the result of a linear fit using only lines with low Aij (colored points), while the gray dashed line shows the result when we use all lines (gray + colored points). This gray dashed line corresponds to the red dashed line in the middle panel, which shows the fitting to all data points.
Paper: ALMA Spectral Survey of an Eruptive Young Star, V883 Ori (ASSAY). II. Freshly Sublimated Complex Organic Molecules in the Keplerian Disk
Authors: Jae-Hong Jeong, Jeong-Eun Lee, Seonjae Lee, Giseon Baek, Ji-Hyun Kang, Seokho Lee, Chul-Hwan Kim, Hyeong-Sik Yun, Yuri Aikawa, Gregory J. Herczeg, Doug Johnstone, Lucas Cieza
Figure caption: Comparison of the column density of COMs relative to methanol between V883 Ori & IRAS 16293-2422B (left panel, based on Table 5), and V883 Ori & Comet 67P/Churyumov-Gerasimenko (right panel). The comet data represent relative bulk compositions of species with the same mass, and are taken from M. Schuhmann et al. (2019) and Rubin et al. (2019). For the nondetected molecules in V883 Ori, the upper limits are induced from the 3σ levels. The line representing 1:1 is indicated by a gray dashed line. The lines representing 3 times and 10 times are shown as gray solid lines with dark and light gray shaded areas, respectively.
Paper: ALMA Spectral Survey of an Eruptive Young Star, V883 Ori (ASSAY). II. Freshly Sublimated Complex Organic Molecules in the Keplerian Disk
Authors: Jae-Hong Jeong, Jeong-Eun Lee, Seonjae Lee, Giseon Baek, Ji-Hyun Kang, Seokho Lee, Chul-Hwan Kim, Hyeong-Sik Yun, Yuri Aikawa, Gregory J. Herczeg, Doug Johnstone, Lucas Cieza
Figure caption: The estimated column density results from 2019 V883 Ori (J.-E. Lee et al. 2019) compared to those derived in this work (Table 1, y-axis of Figure 6). The data points are from the Supplementary Table 1 by J.-E. Lee et al. (2019). The gray dashed line represents the one-to-one line. The lines representing 3 times and 10 times difference from the one-to-one values are shown as solid gray lines with dark and light gray shaded areas, respectively.
Paper: ALMA Spectral Survey of an Eruptive Young Star, V883 Ori (ASSAY). II. Freshly Sublimated Complex Organic Molecules in the Keplerian Disk
Authors: Jae-Hong Jeong, Jeong-Eun Lee, Seonjae Lee, Giseon Baek, Ji-Hyun Kang, Seokho Lee, Chul-Hwan Kim, Hyeong-Sik Yun, Yuri Aikawa, Gregory J. Herczeg, Doug Johnstone, Lucas Cieza
Figure caption: 12C/13C isotopic ratios. The column density results using isolated lines of τν,line smaller than 0.7 (Table 1) and using isolated lines of all τν,line are plotted respectively. The dashed lines represent the average 12C/13C values, and the shaded areas show the 1σ error range for the average values.
Paper: ALMA Spectral Survey of an Eruptive Young Star, V883 Ori (ASSAY). II. Freshly Sublimated Complex Organic Molecules in the Keplerian Disk
Authors: Jae-Hong Jeong, Jeong-Eun Lee, Seonjae Lee, Giseon Baek, Ji-Hyun Kang, Seokho Lee, Chul-Hwan Kim, Hyeong-Sik Yun, Yuri Aikawa, Gregory J. Herczeg, Doug Johnstone, Lucas Cieza
Figure caption: Comparison of column densities derived from the iterative LTE line fitting (Table 1) and from the rotation diagrams (Table 4). The 1:1 reference line is depicted as a gray dashed line. Additionally, the gray solid lines, accompanied by dark and light gray shaded regions, represent 3 times and 10 times the reference value.
Paper: ALMA Spectral Survey of an Eruptive Young Star, V883 Ori (ASSAY). II. Freshly Sublimated Complex Organic Molecules in the Keplerian Disk
Authors: Jae-Hong Jeong, Jeong-Eun Lee, Seonjae Lee, Giseon Baek, Ji-Hyun Kang, Seokho Lee, Chul-Hwan Kim, Hyeong-Sik Yun, Yuri Aikawa, Gregory J. Herczeg, Doug Johnstone, Lucas Cieza
Figure caption: Bar plot for the (relative) column densities of all the COMs detected in V883 Ori. The column density values are from Table 1. COMs are sorted by increasing the value of mass, and the same color indicates isotopologues of the same species. The error bars are the uncertainties in the column densities, not the relative column densities.
Paper: ALMA Spectral Survey of an Eruptive Young Star, V883 Ori (ASSAY). II. Freshly Sublimated Complex Organic Molecules in the Keplerian Disk
Authors: Jae-Hong Jeong, Jeong-Eun Lee, Seonjae Lee, Giseon Baek, Ji-Hyun Kang, Seokho Lee, Chul-Hwan Kim, Hyeong-Sik Yun, Yuri Aikawa, Gregory J. Herczeg, Doug Johnstone, Lucas Cieza
Figure caption: LTE line-fitted model spectra when using isolated molecular lines of all line optical depths (upper panel of this figure, and x-axis of Figure 6), and when using isolated lines of τν,line < 0.7 (lower panel of this figure, and y-axis of Figure 6). Both panels show the same spectral window. Black solid lines represent the combined spectra of the model spectra for each species, and the individual model spectra are shown as various line colors and styles. The red solid lines indicate residual between the observed data and the model. The gray dashed/dotted horizontal lines represent the 1σ/3σ levels of the observed spectrum. Also, the blue shaded areas on the lower panel indicate lines excluded during the LTE line fitting because their modeled optical depths exceeded 0.7. This frequency region is the same as the frequency region in the lower panel of Figure 2.
Paper: ALMA Spectral Survey of an Eruptive Young Star, V883 Ori (ASSAY). II. Freshly Sublimated Complex Organic Molecules in the Keplerian Disk
Authors: Jae-Hong Jeong, Jeong-Eun Lee, Seonjae Lee, Giseon Baek, Ji-Hyun Kang, Seokho Lee, Chul-Hwan Kim, Hyeong-Sik Yun, Yuri Aikawa, Gregory J. Herczeg, Doug Johnstone, Lucas Cieza
Figure caption: Rotation temperature (left) and column density (right) maps of 13CH3OH (top) and CH3CN (bottom). Only pixels with fitted temperatures between 100 and 400 K are drawn.
Paper: Broad-line Region Characterization in Dozens of Active Galactic Nuclei Using Small-aperture Telescopes
Authors: Catalina Sobrino Figaredo, Doron Chelouche, Martin Haas, Michael Ramolla, Shai Kaspi, Swayamtrupta Panda, Martin W. Ochmann, Shay Zucker, Rolf Chini, Malte A. Probst, Wolfram Kollatschny, Miguel Murphy
Figure caption: Left: correlation between the B band and NB680 light curves for MRK 841. The correlation coefficient (Re) is shown at the top and the corresponding value for α is at the bottom. The value for the peak delay with its respective α value is marked with an orange star. The range for calculating the centroid is colored with a blue area, and the corresponding lag is marked with a light-blue star. The centroid calculation is performed within a range defined as ≥0.8 times the peak Re value, akin to the conventional method of RM. Right: the upper two panels illustrate the implementation of the flux-randomization (FR) algorithm for error estimation. The peak value is highlighted in orange, while the centroid is depicted in blue, with the final values labeled. The lower panel presents the histogram for the maximal correlation values, denoted as ﹩{R}_{{\rm{e}},\max }﹩. The result obtained via the FR method (Re, FR) is shown in orange, with a value that approximates 0.95. In contrast, the resulting histogram for the time-permuted version (Re, TP) is displayed in red, yielding an average value of approximately 0.4. This indicates a high level of confidence in the results (see the text).
Paper: Broad-line Region Characterization in Dozens of Active Galactic Nuclei Using Small-aperture Telescopes
Authors: Catalina Sobrino Figaredo, Doron Chelouche, Martin Haas, Michael Ramolla, Shai Kaspi, Swayamtrupta Panda, Martin W. Ochmann, Shay Zucker, Rolf Chini, Malte A. Probst, Wolfram Kollatschny, Miguel Murphy
Figure caption: Normalized spectrum of Mrk 841 at z = 0.03642. The normalized transmission for the different photometric filters is overplotted. The continuum signal is traced in this work by the broad bands, while the Hα line is covered by the NB680 filter. The significantly different relative contributions of emission lines to the broad and narrow bands allows for PRM analysis. Note that partial coverage of the emission line may occur for specific targets (see also Appendix E).
Paper: Broad-line Region Characterization in Dozens of Active Galactic Nuclei Using Small-aperture Telescopes
Authors: Catalina Sobrino Figaredo, Doron Chelouche, Martin Haas, Michael Ramolla, Shai Kaspi, Swayamtrupta Panda, Martin W. Ochmann, Shay Zucker, Rolf Chini, Malte A. Probst, Wolfram Kollatschny, Miguel Murphy
Figure caption: Photometric light curves for Mrk 841. The first deep minimum for the NB680 band appears to be delayed by 20 days with respect to the adjacent broadband data due to the significant contribution of the broad Hα line to the flux in the narrow band. Moreover, the continuum (B or V) shows a strong rise between 50 and 75 days, whereas in NB680, the rise is shallower, indicating that the Hα line may still be declining. As the contribution of the Hα line to the band is only partial, direct cross-correlation techniques are inadequate to recover the time delay associated with the line, and bivariate correlation analyses methods (Equation (1)) are more suitable.
Paper: Broad-line Region Characterization in Dozens of Active Galactic Nuclei Using Small-aperture Telescopes
Authors: Catalina Sobrino Figaredo, Doron Chelouche, Martin Haas, Michael Ramolla, Shai Kaspi, Swayamtrupta Panda, Martin W. Ochmann, Shay Zucker, Rolf Chini, Malte A. Probst, Wolfram Kollatschny, Miguel Murphy
Figure caption: An example of host galaxy subtraction and flux interpolation at 5100 Å for Mrk 841. Black circles represent the median total flux, with errors reflecting the median of all errors. Host galaxy values derived from the FVG method are shown as red squares, where error bars indicate the range of intersection between AGN and host slopes. Host subtracted fluxes trace the nuclear emission, and are depicted in blue. A power-law fit of the form fν ∝ λβ is illustrated by a solid line. The final host-subtracted value from this fit is denoted by a cyan star, accompanied by its corresponding flux label.
Paper: Broad-line Region Characterization in Dozens of Active Galactic Nuclei Using Small-aperture Telescopes
Authors: Catalina Sobrino Figaredo, Doron Chelouche, Martin Haas, Michael Ramolla, Shai Kaspi, Swayamtrupta Panda, Martin W. Ochmann, Shay Zucker, Rolf Chini, Malte A. Probst, Wolfram Kollatschny, Miguel Murphy
Figure caption: Ratio Re, FR/Re, TP against Re, FR (see Section 3.1.2 for details), with color coded according to the confidence level and size indicating the quality of the continuum and NB light curve (being larger for better quality of the light curve, based on the η-value). Criteria of Re, FR ≥ 0.6 and ratio Re, FR/Re, TP ≥ 1.7 are marked with vertical and horizontal lines, respectively. Good delay candidates are highlighted with a black edge.
Paper: Broad-line Region Characterization in Dozens of Active Galactic Nuclei Using Small-aperture Telescopes
Authors: Catalina Sobrino Figaredo, Doron Chelouche, Martin Haas, Michael Ramolla, Shai Kaspi, Swayamtrupta Panda, Martin W. Ochmann, Shay Zucker, Rolf Chini, Malte A. Probst, Wolfram Kollatschny, Miguel Murphy
Figure caption: An example of a continuum-subtracted FAST spectrum of Mrk 841 showing the broad Hα emission line and the narrow [S II] and [N II] lines. A best-fit model to the data is shown in red, which consists of broad- and narrow-line components (green curves). The FWHM of the broad component is used for BH mass estimations.
Paper: Broad-line Region Characterization in Dozens of Active Galactic Nuclei Using Small-aperture Telescopes
Authors: Catalina Sobrino Figaredo, Doron Chelouche, Martin Haas, Michael Ramolla, Shai Kaspi, Swayamtrupta Panda, Martin W. Ochmann, Shay Zucker, Rolf Chini, Malte A. Probst, Wolfram Kollatschny, Miguel Murphy
Figure caption: An example of a flux–flux diagram for Mrk 841 exhibiting variability behavior that is consistent with a linear trend between the B and the V bands (plus symbols). A linear fit (blue line) intersects the galaxy-colors wedge (Y. Sakata et al. 2010; gray area) at the host-galaxy flux levels within the aperture (red star), and should be subtracted to reveal the net AGN flux (see the text).
Paper: Broad-line Region Characterization in Dozens of Active Galactic Nuclei Using Small-aperture Telescopes
Authors: Catalina Sobrino Figaredo, Doron Chelouche, Martin Haas, Michael Ramolla, Shai Kaspi, Swayamtrupta Panda, Martin W. Ochmann, Shay Zucker, Rolf Chini, Malte A. Probst, Wolfram Kollatschny, Miguel Murphy
Figure caption: Hα rBLR–L diagram. Cyan circles show the results obtained in this work for sources with reliable delays and host-subtracted luminosities (orange stars denote sources for which host subtraction was not successful and the total luminosity is shown instead). Gray diamonds, stars, pluses, and crosses represent previous results from S. Kaspi et al. (2000), M. C. Bentz et al. (2010), Y. Shen et al. (2024), and H. Cho et al. (2023), respectively. The result for NGC 4395 from H. Cho et al. (2021) is marked with a circle and labeled, as well as 3C273 at the high-luminosity end. Th gray shaded area represents the best linear fit with the value K = 1.51 ± 0.05 and γ = 0.57 ± 0.05 (see the text). The inset shows the distribution of the difference between the RM delays and the expected value from the best fit. The total scatter for the relation is σ = 0.32 dex, which is also shown as the light-gray area around the best fit in the main panel.
Paper: Broad-line Region Characterization in Dozens of Active Galactic Nuclei Using Small-aperture Telescopes
Authors: Catalina Sobrino Figaredo, Doron Chelouche, Martin Haas, Michael Ramolla, Shai Kaspi, Swayamtrupta Panda, Martin W. Ochmann, Shay Zucker, Rolf Chini, Malte A. Probst, Wolfram Kollatschny, Miguel Murphy
Figure caption: The BLR size–luminosity relation for the Hα line color coded by the dimensionless accretion rate, ﹩\dot{{\mathscr{M}}}﹩ (see the text), as estimated by RFe (see Equation (7) and note that the method, while maintaining monotonicity, likely overestimates the highest accretion rates by a large factor). There is a tendency for highly accreting sources to lie below the population mean, which is in agreement with studies based on the Hβ line. The size of the symbols corresponds to the value of ﹩\dot{{\mathscr{M}}}﹩ (in log units), as deduced by Equation (6) (see the text for an inherent bias with this method). The blue shaded area represents the best fit for our sample with luminosities >1.5 × 1043 erg s−1.
Paper: Broad-line Region Characterization in Dozens of Active Galactic Nuclei Using Small-aperture Telescopes
Authors: Catalina Sobrino Figaredo, Doron Chelouche, Martin Haas, Michael Ramolla, Shai Kaspi, Swayamtrupta Panda, Martin W. Ochmann, Shay Zucker, Rolf Chini, Malte A. Probst, Wolfram Kollatschny, Miguel Murphy
Figure caption: Multiepoch BV flux–flux diagrams for the objects 3C 120 (left), HE 1136-2304 (middle), and WPVS 48 (right). The FVGs are constructed by the combination of different observation campaigns. Fluxes are plotted as crosses, and the different colors refer to different observing years. The bisector fit for the AGN slope is plotted as blue lines, and the BV and BR host slope from Y. Sakata et al. (2010) is shown as a colored gray area. The red star marks the intersection between AGN and host slope and represents the assumed host value for the object.
Paper: Broad-line Region Characterization in Dozens of Active Galactic Nuclei Using Small-aperture Telescopes
Authors: Catalina Sobrino Figaredo, Doron Chelouche, Martin Haas, Michael Ramolla, Shai Kaspi, Swayamtrupta Panda, Martin W. Ochmann, Shay Zucker, Rolf Chini, Malte A. Probst, Wolfram Kollatschny, Miguel Murphy
Figure caption: Recovered time delay τpeak versus the assumed value for αecho. The results obtained with this new formalism are shown in orange, while the results obtained directly with the ICCF method are shown in blue. Left panel: results for uniform light curves with Nrmtot = 100 days and noise of 1%. Right panel: the same but for nonuniform light curves.
Paper: Broad-line Region Characterization in Dozens of Active Galactic Nuclei Using Small-aperture Telescopes
Authors: Catalina Sobrino Figaredo, Doron Chelouche, Martin Haas, Michael Ramolla, Shai Kaspi, Swayamtrupta Panda, Martin W. Ochmann, Shay Zucker, Rolf Chini, Malte A. Probst, Wolfram Kollatschny, Miguel Murphy
Figure caption: Observation and selection sample: η-values for NB light curves versus the continuum band light curves. Values are color coded based on Fvar (left) and cadence (right) of the continuum. Objects marked with a black edge mark the final selected light curves for the RM analysis. The same process was done for Fvar and cadence of the NB band (not shown).
Paper: Broad-line Region Characterization in Dozens of Active Galactic Nuclei Using Small-aperture Telescopes
Authors: Catalina Sobrino Figaredo, Doron Chelouche, Martin Haas, Michael Ramolla, Shai Kaspi, Swayamtrupta Panda, Martin W. Ochmann, Shay Zucker, Rolf Chini, Malte A. Probst, Wolfram Kollatschny, Miguel Murphy
Figure caption: The BLR size–luminosity relation for multiepoch sources. The results for our objects are shown with different colors, connected with lines and labeled. Values for single-epoch results for Hα from the literature are also shown (same as Figure 10). The tight clustering of the measurements per object indicates the stability of our PRM approach. The modest luminosity variations of the sources preclude a detailed analysis of the intrinsic size–luminosity relation.
Paper: Broad-line Region Characterization in Dozens of Active Galactic Nuclei Using Small-aperture Telescopes
Authors: Catalina Sobrino Figaredo, Doron Chelouche, Martin Haas, Michael Ramolla, Shai Kaspi, Swayamtrupta Panda, Martin W. Ochmann, Shay Zucker, Rolf Chini, Malte A. Probst, Wolfram Kollatschny, Miguel Murphy
Figure caption: Left panel: 100 day simulated continuum light curve with an exponent β = −2 in blue and simulated echo light curve with α = 0.6 and τ = 10 days in red. Right panel: the correlation coefficient Re is shown in the upper panel, and its corresponding α-value is shown in the bottom panel. The peak delay τpeak and αpeak are marked with an orange star and labeled.
Paper: Broad-line Region Characterization in Dozens of Active Galactic Nuclei Using Small-aperture Telescopes
Authors: Catalina Sobrino Figaredo, Doron Chelouche, Martin Haas, Michael Ramolla, Shai Kaspi, Swayamtrupta Panda, Martin W. Ochmann, Shay Zucker, Rolf Chini, Malte A. Probst, Wolfram Kollatschny, Miguel Murphy
Figure caption: Comparison between BH masses estimated in this work and previously reported BH masses (after adjusting for the same 〈f〉 factor; see the text). The resulting scatter is at the 0.3 dex level, which is typical in similar studies.
Paper: Broad-line Region Characterization in Dozens of Active Galactic Nuclei Using Small-aperture Telescopes
Authors: Catalina Sobrino Figaredo, Doron Chelouche, Martin Haas, Michael Ramolla, Shai Kaspi, Swayamtrupta Panda, Martin W. Ochmann, Shay Zucker, Rolf Chini, Malte A. Probst, Wolfram Kollatschny, Miguel Murphy
Figure caption: Maximal value reached by the correlation coefficient Re for different kind of simulation settings. Left panel: simulated light curves with a total duration Ntot = 100 days and uniform sampling, τecho = 10 days (cyan) and τ = 30 days (orange). Right panel: for Ntot = 100 days and nonuniform sampling, τecho = 10 days (cyan) and τ = 30 days (orange).
Paper: Broad-line Region Characterization in Dozens of Active Galactic Nuclei Using Small-aperture Telescopes
Authors: Catalina Sobrino Figaredo, Doron Chelouche, Martin Haas, Michael Ramolla, Shai Kaspi, Swayamtrupta Panda, Martin W. Ochmann, Shay Zucker, Rolf Chini, Malte A. Probst, Wolfram Kollatschny, Miguel Murphy
Figure caption: Recovered time delay as a function of the assumed value for αecho. The left panel displays results obtained with an additional continuum delay of 10% of the line delay, while the right panel presents results for a continuum delay of 15% of the line delay. Blue circles represent results for a cadence of 2 days, and orange squares indicate a cadence of 4 days. The dashed black horizontal line marks the assumed τline, while the dotted gray line indicates a 10% deviation toward lower values.
Paper: Broad-line Region Characterization in Dozens of Active Galactic Nuclei Using Small-aperture Telescopes
Authors: Catalina Sobrino Figaredo, Doron Chelouche, Martin Haas, Michael Ramolla, Shai Kaspi, Swayamtrupta Panda, Martin W. Ochmann, Shay Zucker, Rolf Chini, Malte A. Probst, Wolfram Kollatschny, Miguel Murphy
Figure caption: Iron-template and multicomponent Hβ model fit to the optical spectrum of Mrk 841 (top) and RXS J17414+2304 (bottom). The fit includes a model for the host, where applicable. The derived fluxes for the iron blend and Hβ are then used to calculate their ratio, RFe, which may be used to estimate the mass-accretion rate (Section 4.4.2).
Paper: Broad-line Region Characterization in Dozens of Active Galactic Nuclei Using Small-aperture Telescopes
Authors: Catalina Sobrino Figaredo, Doron Chelouche, Martin Haas, Michael Ramolla, Shai Kaspi, Swayamtrupta Panda, Martin W. Ochmann, Shay Zucker, Rolf Chini, Malte A. Probst, Wolfram Kollatschny, Miguel Murphy
Figure caption: Statistics for the recovered time delay (left) and α (right) with a continuum delay (τcont = 1.5 days) set at 15% of the assumed line delay (τline = 10.5 days). Results are presented for three different assumed values of α: 0.3 in green, 0.4 in orange, and 0.8 in cyan.
Paper: Broad-line Region Characterization in Dozens of Active Galactic Nuclei Using Small-aperture Telescopes
Authors: Catalina Sobrino Figaredo, Doron Chelouche, Martin Haas, Michael Ramolla, Shai Kaspi, Swayamtrupta Panda, Martin W. Ochmann, Shay Zucker, Rolf Chini, Malte A. Probst, Wolfram Kollatschny, Miguel Murphy
Figure caption: Left panel: peak values versus centroid values obtained from our formalism. Right panel: peak-lag values versus lags derived from JAVELIN’s software. A one-to-one ratio is depicted in both plots.
Paper: Broad-line Region Characterization in Dozens of Active Galactic Nuclei Using Small-aperture Telescopes
Authors: Catalina Sobrino Figaredo, Doron Chelouche, Martin Haas, Michael Ramolla, Shai Kaspi, Swayamtrupta Panda, Martin W. Ochmann, Shay Zucker, Rolf Chini, Malte A. Probst, Wolfram Kollatschny, Miguel Murphy
Figure caption: Recovered αpeak versus assumed αecho values for different noise values and uniform sampling (left panel) and nonuniform sampling (right panel).