adsabs/AstroCLIMB huggingface dataset:
Paper: Revisiting ϵ Eridani with NEID: Identifying New Activity-sensitive Lines in a Young K Dwarf Star
Authors: Sarah Jiang, Arpita Roy, Samuel Halverson, Chad F. Bender, Carlos Selgas, O. Justin Otor, Suvrath Mahadevan, Guđmundur Stefánsson, Ryan C. Terrien, Christian Schwab
Figure caption: Results of our analysis of the Wise line list using our partially automated method and NEID ϵ Eri spectra. In these graphs, the ∣τ∣ and ∣ρ∣ values are for the correlation between line core flux/depth and S-index. (a) ∣τ∣ values for each line in the Wise line list calculated by Wise et al. (2018; “W18”) plotted against the ∣τ∣ values we calculated for the same lines using NEID data of ϵ Eri. The 1:1 line is marked in blue, and our threshold for correlation in ∣τ∣ is marked in gray. Five lines did not meet our threshold for correlation in ∣τ∣. (b) Both our and W18's ∣τ∣ values for each line in the Wise line list, organized by wavelength. Our threshold for correlation in ∣τ∣ is marked in gray. (c) Both our and W18's ∣τ∣ values and our ∣ρ∣ values (W18 did not calculate ∣ρ∣) for each line in the Wise line list, organized by line number in descending order of ∣τ∣ values calculated by W18, and the corresponding histograms. Our thresholds for correlation in ∣τ∣ and ∣ρ∣ respectively are marked in gray. In addition to the lines that did not meet our threshold for correlation in ∣τ∣, one line was found to meet our threshold for correlation in ∣τ∣, but not ∣ρ∣. The corresponding histograms show the ∣τ∣ and ∣ρ∣ values we calculated for correlations between line depth and S-index for the Wise line list. ∣ρ∣ values are consistently higher than corresponding ∣τ∣ values for the same line.
Paper: Revisiting ϵ Eridani with NEID: Identifying New Activity-sensitive Lines in a Young K Dwarf Star
Authors: Sarah Jiang, Arpita Roy, Samuel Halverson, Chad F. Bender, Carlos Selgas, O. Justin Otor, Suvrath Mahadevan, Guđmundur Stefánsson, Ryan C. Terrien, Christian Schwab
Figure caption: Examples of the visual criteria we used to prune our line lists. We determine whether or not to remove a line based on whether the Gaussian fit appears to accurately fit and measure a line’s parameters, and if the correlations appear to exhibit a significant outlier that skews the correlation. (a) An example of a “good” line that we do not remove, since the Gaussian fit appears to match the line within its wings. (b) An example of a noisy line such that the Gaussian fit does not accurately fit the line. (c) An example of a blended line with multiple peaks in the fitting window, such that the Gaussian fit does not accurately fit the line. (d) An example of a line whose plot correlating line depth with the S-index exhibits a significant outlier that skews the best-fit line.
Paper: Revisiting ϵ Eridani with NEID: Identifying New Activity-sensitive Lines in a Young K Dwarf Star
Authors: Sarah Jiang, Arpita Roy, Samuel Halverson, Chad F. Bender, Carlos Selgas, O. Justin Otor, Suvrath Mahadevan, Guđmundur Stefánsson, Ryan C. Terrien, Christian Schwab
Figure caption: Venn diagram of our seven line lists and the number of lines in each list. All numbers/line lists are exclusive; i.e., we found nine lines correlated with the S-index in all three parameters (depth, FWHM, and integrated flux), 55 lines correlated with the S-index in depth and FWHM only, 79 lines correlated with the S-index in depth and integrated flux only, six lines correlated with the S-index in FWHM and integrated flux only, and 167, 131, 44 lines respectively correlated with the S-index in depth, FWHM, or integrated flux only.
Paper: Revisiting ϵ Eridani with NEID: Identifying New Activity-sensitive Lines in a Young K Dwarf Star
Authors: Sarah Jiang, Arpita Roy, Samuel Halverson, Chad F. Bender, Carlos Selgas, O. Justin Otor, Suvrath Mahadevan, Guđmundur Stefánsson, Ryan C. Terrien, Christian Schwab
Figure caption: Ranges of each of our seven line lists over the full NEID wavelength range (3800–9300 Å). The wavelengths of the lines in each line list are generally uniformly distributed blueward of ∼6500 Å, with a notable gap between 6500-9000 Å populated by only a couple of lines.
Paper: Revisiting ϵ Eridani with NEID: Identifying New Activity-sensitive Lines in a Young K Dwarf Star
Authors: Sarah Jiang, Arpita Roy, Samuel Halverson, Chad F. Bender, Carlos Selgas, O. Justin Otor, Suvrath Mahadevan, Guđmundur Stefánsson, Ryan C. Terrien, Christian Schwab
Figure caption: Correlations between line depth, FWHM, and integrated flux and S-index for each of the five lines that we found to be strongly correlated with the S-index in all three of our measured line parameters, which also appear in the line list published by Wise et al. (2018). While Wise et al. (2018) found these lines to be correlated with the S-index in line core flux (analogous to line depth), we further confirmed these lines are also sensitive to activity in other parameters (FWHM and integrated flux).
Paper: Revisiting ϵ Eridani with NEID: Identifying New Activity-sensitive Lines in a Young K Dwarf Star
Authors: Sarah Jiang, Arpita Roy, Samuel Halverson, Chad F. Bender, Carlos Selgas, O. Justin Otor, Suvrath Mahadevan, Guđmundur Stefánsson, Ryan C. Terrien, Christian Schwab
Figure caption: Two lines that we found to be correlated with the S-index in all three of our line parameters and that have known blends within ± 3 km s−1 of the line center according to the Vienna Atomic Line Database (VALD). The positions and depths of the lines extracted from VALD are shown in red.
Paper: Revisiting ϵ Eridani with NEID: Identifying New Activity-sensitive Lines in a Young K Dwarf Star
Authors: Sarah Jiang, Arpita Roy, Samuel Halverson, Chad F. Bender, Carlos Selgas, O. Justin Otor, Suvrath Mahadevan, Guđmundur Stefánsson, Ryan C. Terrien, Christian Schwab
Figure caption: Correlations between line depth, FWHM, and integrated flux and S-index for each of the four lines that we found to be strongly correlated with the S-index in all three of our measured line parameters, which do not also appear in the line list published by Wise et al. (2018). These lines are newly identified activity-sensitive lines that trace activity in several different line features.
Paper: Revisiting ϵ Eridani with NEID: Identifying New Activity-sensitive Lines in a Young K Dwarf Star
Authors: Sarah Jiang, Arpita Roy, Samuel Halverson, Chad F. Bender, Carlos Selgas, O. Justin Otor, Suvrath Mahadevan, Guđmundur Stefánsson, Ryan C. Terrien, Christian Schwab
Figure caption: Time series of the measured RVs and S-indices and corresponding periodograms for each NEID observation used in our analysis. In the RV time series, we subtract the systematic RV of ϵ Eri, 16.49 km s−1, and plot the Δ RVs. Both periodograms display a peak at ∼11 days, the rotational period of the star (Howard & Fulton 2016; Mawet et al. 2019).
Paper: Bayesian Analysis for Remote Biosignature Identification on exoEarths (BARBIE). II. Using Grid-based Nested Sampling in Coronagraphy Observation Simulations for O2 and O3 
Authors: Natasha Latouf, Avi M. Mandell, Geronimo L. Villanueva, Michael D. Himes, Michael Dane Moore, Nicholas Susemiehl, Jaime Crouse, Shawn Domagal-Goldman, Giada Arney, Vincent Kofman, Amber V. Young
Figure caption: In all panels, the shortest bandpass center at which one can achieve a strong detection for O2 or a strong or weak detection for O3 are shown in purple triangles, dark purple diamonds, and light pink dots respectively. The strong detection range for H2O is presented in pink squares, to provide context for dual or triple-molecule detection. The range between the shortest and longest bandpass center at which detection is possible is filled in. We present the range for a strong detection S/N is on the y-axis, and the bandpass centers are on the x-axis. Note that the last bandpass center for strong detection is shaded out to the long edge of the bandpass, to maintain the ability to directly compare the panels.
Paper: Bayesian Analysis for Remote Biosignature Identification on exoEarths (BARBIE). II. Using Grid-based Nested Sampling in Coronagraphy Observation Simulations for O2 and O3 
Authors: Natasha Latouf, Avi M. Mandell, Geronimo L. Villanueva, Michael D. Himes, Michael Dane Moore, Nicholas Susemiehl, Jaime Crouse, Shawn Domagal-Goldman, Giada Arney, Vincent Kofman, Amber V. Young
Figure caption: Shown above are the regions of single, dual, and triple-molecular detection as a function of the wavelength. wavelength is presented on the x-axis, and S/N is presented on the y-axis. The hatched regions symbolize regions with single molecule detection, shaded regions symbolize only the overlapping areas between dual molecular strong detection zones, and the black-outlined shaded regions symbolize the overlapping areas between triple-molecular strong detection. We present the 10% O2 PAL and 105% O3 PAL case in the first row, the 50% O2 PAL and 110% O3 PAL case in the second row, and the 100% O2 PAL and 100% O3 PAL case in the last row. For all cases, we present a 20%, 30%, and 40% bandpass width.
Paper: Bayesian Analysis for Remote Biosignature Identification on exoEarths (BARBIE). II. Using Grid-based Nested Sampling in Coronagraphy Observation Simulations for O2 and O3 
Authors: Natasha Latouf, Avi M. Mandell, Geronimo L. Villanueva, Michael D. Himes, Michael Dane Moore, Nicholas Susemiehl, Jaime Crouse, Shawn Domagal-Goldman, Giada Arney, Vincent Kofman, Amber V. Young
Figure caption: Lowest S/N values for strong detection of the 0.74 μm O2 feature as a function of the O2 abundance. We note that although the 0.1% and 1% modern O2 abundances (i.e., mid-Proterozoic abundances) are in our study, they are not presented on the plot. We denote these abundances with a pink arrow. The VMR values are on the x-axis, with S/N on the y-axis. Strong detection is shown in purple squares, weak detection is shown in pink dots, and the modern abundance range is highlighted with a light pink strip.
Paper: Bayesian Analysis for Remote Biosignature Identification on exoEarths (BARBIE). II. Using Grid-based Nested Sampling in Coronagraphy Observation Simulations for O2 and O3 
Authors: Natasha Latouf, Avi M. Mandell, Geronimo L. Villanueva, Michael D. Himes, Michael Dane Moore, Nicholas Susemiehl, Jaime Crouse, Shawn Domagal-Goldman, Giada Arney, Vincent Kofman, Amber V. Young
Figure caption: Lowest S/N values for strong detection of the 0.63 μm O3 feature as a function of the O3 abundance. The VMR values are on the x-axis, with S/N on the y-axis. Strong detection is shown in purple squares, weak detection is shown in pink dots, and the modern abundance range is highlighted with a light pink strip.
Paper: Bayesian Analysis for Remote Biosignature Identification on exoEarths (BARBIE). II. Using Grid-based Nested Sampling in Coronagraphy Observation Simulations for O2 and O3 
Authors: Natasha Latouf, Avi M. Mandell, Geronimo L. Villanueva, Michael D. Himes, Michael Dane Moore, Nicholas Susemiehl, Jaime Crouse, Shawn Domagal-Goldman, Giada Arney, Vincent Kofman, Amber V. Young
Figure caption: The shortest bandpass centers at which one can achieve a strong detection for O2 or O3 at varying present atmospheric levels (PALs) for a specific S/N are shown with purple triangles and dark purple diamonds, respectively. The range between the shortest and longest bandpass center at which detection is possible is filled in. The strong detection range for H2O is presented in pink squared to provide context to the results.
Paper: Bayesian Analysis for Remote Biosignature Identification on exoEarths (BARBIE). II. Using Grid-based Nested Sampling in Coronagraphy Observation Simulations for O2 and O3 
Authors: Natasha Latouf, Avi M. Mandell, Geronimo L. Villanueva, Michael D. Himes, Michael Dane Moore, Nicholas Susemiehl, Jaime Crouse, Shawn Domagal-Goldman, Giada Arney, Vincent Kofman, Amber V. Young
Figure caption: Spectra with varied O3 abundances. We feature the highest abundance (3 × 10−6), the midpoint abundance (1.5 × 10−6), and the lowest abundance in the study (7 × 10−7; modern Earth), respectively. All spectra are binned at R = 140. We also present a 20% and 40% bandpass range width, in light gray and light blue respectively.
Paper: Galaxy Morphological Classification of the Legacy Surveys with Deformable Convolutional Neural Networks
Authors: Shoulin Wei, 守林 卫, Wei Lu, 伟 陆, Wei Dai, 伟 戴, Bo Liang, 波 梁, Longfei Hao, 龙飞 郝, Zhijian Zhang, 志坚 张, Xiaoli Zhang, 晓丽 张
Figure caption: Visualizing features learned by our method with t-SNE. Images A–E are samples of outliers.
Paper: Galaxy Morphological Classification of the Legacy Surveys with Deformable Convolutional Neural Networks
Authors: Shoulin Wei, 守林 卫, Wei Lu, 伟 陆, Wei Dai, 伟 戴, Bo Liang, 波 梁, Longfei Hao, 龙飞 郝, Zhijian Zhang, 志坚 张, Xiaoli Zhang, 晓丽 张
Figure caption: Confusion matrices of testing results, where the x-axis corresponds to the predicted label from the network and the y-axis to the visually assigned label. Diagonal elements of the matrix represent the number of correctly classified images for each class, while off-diagonal elements represent misclassifications.
Paper: Galaxy Morphological Classification of the Legacy Surveys with Deformable Convolutional Neural Networks
Authors: Shoulin Wei, 守林 卫, Wei Lu, 伟 陆, Wei Dai, 伟 戴, Bo Liang, 波 梁, Longfei Hao, 龙飞 郝, Zhijian Zhang, 志坚 张, Xiaoli Zhang, 晓丽 张
Figure caption: Schematic diagram depicting calculation process of LAM.
Paper: Galaxy Morphological Classification of the Legacy Surveys with Deformable Convolutional Neural Networks
Authors: Shoulin Wei, 守林 卫, Wei Lu, 伟 陆, Wei Dai, 伟 戴, Bo Liang, 波 梁, Longfei Hao, 龙飞 郝, Zhijian Zhang, 志坚 张, Xiaoli Zhang, 晓丽 张
Figure caption: Samples of Spiral galaxies from the presented catalog. All images are displayed on the same scale. Coordinate and probability of being a Spiral is labeled at the left corner of each image.
Paper: Galaxy Morphological Classification of the Legacy Surveys with Deformable Convolutional Neural Networks
Authors: Shoulin Wei, 守林 卫, Wei Lu, 伟 陆, Wei Dai, 伟 戴, Bo Liang, 波 梁, Longfei Hao, 龙飞 郝, Zhijian Zhang, 志坚 张, Xiaoli Zhang, 晓丽 张
Figure caption: Accuracy of training and validation along with epochs.
Paper: Galaxy Morphological Classification of the Legacy Surveys with Deformable Convolutional Neural Networks
Authors: Shoulin Wei, 守林 卫, Wei Lu, 伟 陆, Wei Dai, 伟 戴, Bo Liang, 波 梁, Longfei Hao, 龙飞 郝, Zhijian Zhang, 志坚 张, Xiaoli Zhang, 晓丽 张
Figure caption: The overall architecture of the proposed network.
Paper: Transient Corotating Clumps around Adolescent Low-mass Stars from Four Years of TESS
Authors: Luke G. Bouma, Rahul Jayaraman, Saul Rappaport, Luisa M. Rebull, Lynne A. Hillenbrand, Joshua N. Winn, Alexandre David-Uraz, Gáspár Á. Bakos
Figure caption: River plots of the LP 12-502 light curve, showing (clockwise from top left) Sectors 18–19, 25–26, 53, and 58–59. A two-harmonic sinusoid has been subtracted to highlight the sharp dips. A fixed period and phase are adopted for all sectors; the dips across all observations are bounded by ϕ ∈ [ − 0.35, 0.35]. In Sectors 25–26 (cycles 248–315), periods are visible at the fundamental period of 18.5611 hr, as well as at faster (ϕ≈0–0.07) and slower (ϕ≈0.25–0.27) relative periods based on the presence of blue dips with distinct slopes. Multiple simultaneous periods are also visible in Sector 53 (cycles 1234–1263) and Sectors 58–59 (cycles 1411–1479). White chunks denote missing data. The state-changes noted with red markers in Figure 7 occur in cycles 261, 309, and 1241.
Paper: Transient Corotating Clumps around Adolescent Low-mass Stars from Four Years of TESS
Authors: Luke G. Bouma, Rahul Jayaraman, Saul Rappaport, Luisa M. Rebull, Lynne A. Hillenbrand, Joshua N. Winn, Alexandre David-Uraz, Gáspár Á. Bakos
Figure caption: Evolution of CPV light curves over 2 yr. Out of the 50 CPVs in Figure 4, 32 had 2 minute cadence TESS data available for a baseline of at least 2 yr; the 27 brightest are shown here due to space constraints. Each panel shows one sector of TESS data, and is phased to its deepest minimum in flux. Each panel’s title shows the TIC identifier and period in hours. Text insets show the TESS sector numbers, which generally span 2 yr, or at least 1000 cycles. The vertical scale is fixed across sectors to clarify shape changes. Gray circles are raw 2 minute data; colored circles bin to 300 points per cycle.
Paper: Transient Corotating Clumps around Adolescent Low-mass Stars from Four Years of TESS
Authors: Luke G. Bouma, Rahul Jayaraman, Saul Rappaport, Luisa M. Rebull, Lynne A. Hillenbrand, Joshua N. Winn, Alexandre David-Uraz, Gáspár Á. Bakos
Figure caption: The magnetic B star connection. σ Ori E and HD 345439 (top row) are magnetic B stars with predominantly dipolar magnetic fields known to host circumstellar plasma tori. HD 37776 and HD 64740 (middle row) are analogous magnetic B stars with field topologies potentially dominated by high order multipoles. The bottom row compares the latter systems against the best-matching CPV light curves, selected by eye from Figure 4. CPVs have light curves that are visually similar to the topologically complex magnetic B stars. Stellar masses rounded to one significant figure are given in the lower right of each panel; the star, TESS sector, and period are listed in each subtitle.
Paper: Transient Corotating Clumps around Adolescent Low-mass Stars from Four Years of TESS
Authors: Luke G. Bouma, Rahul Jayaraman, Saul Rappaport, Luisa M. Rebull, Lynne A. Hillenbrand, Joshua N. Winn, Alexandre David-Uraz, Gáspár Á. Bakos
Figure caption: Evolution of LP 12-502 (P=18.5611 hr) at fixed period and epoch over 3 yr. Each panel shows one (averaged) TESS orbit; small text denotes relative cycle number. There are 200 binned black points per cycle. The TESS pointing law dictates the large time gaps between cycles 64–248, 315–1233, and 1264–1410; larger gaps tend to yield larger shape changes. The dips usually evolve over tens to hundreds of cycles. However, cycles 1233–1264 show a dip that switched from a depth and duration of 3% and 3 hr to 0.3% and 1 hr over less than one cycle (see Figure 7).
Paper: Transient Corotating Clumps around Adolescent Low-mass Stars from Four Years of TESS
Authors: Luke G. Bouma, Rahul Jayaraman, Saul Rappaport, Luisa M. Rebull, Lynne A. Hillenbrand, Joshua N. Winn, Alexandre David-Uraz, Gáspár Á. Bakos
Figure caption: LP 12-502 (TIC 402980664) light curve, where each time segment represents one TESS orbit. Data were acquired in Sectors 18–19, 25–26, 53, and 57–58. Flares are drawn in gray. The light curve is binned to 15 minute intervals so that there are 96 points per day, and each point is connected by a line. Data gaps have nothing plotted. The red vertical lines highlight apparently instantaneous state-changes in the shape of the dip pattern.
Paper: Transient Corotating Clumps around Adolescent Low-mass Stars from Four Years of TESS
Authors: Luke G. Bouma, Rahul Jayaraman, Saul Rappaport, Luisa M. Rebull, Lynne A. Hillenbrand, Joshua N. Winn, Alexandre David-Uraz, Gáspár Á. Bakos
Figure caption: Light-curve evolution of TIC 300651846. All available 2 minute cadence data as of 2023 August 11 are shown. Cycles 0 to 622 span TESS Sectors 32–39 (2020 November–2021 June); cycles 2296–2676 span Sectors 61–65 (2023 January–June). We assumed a 8.254 hr period and a fixed reference epoch (BTJD 2174.127) for both panels. Light-curve segments are split based on the presence of gaps longer than three hours. Cycle numbers are listed in the lower right of each light-curve segment.
Paper: Transient Corotating Clumps around Adolescent Low-mass Stars from Four Years of TESS
Authors: Luke G. Bouma, Rahul Jayaraman, Saul Rappaport, Luisa M. Rebull, Lynne A. Hillenbrand, Joshua N. Winn, Alexandre David-Uraz, Gáspár Á. Bakos
Figure caption: Spectral age and activity diagnostics for three CPVs. Wavelengths are in air; the continuum normalization is relative to the entire order. The Hα emission strength classifies the stars as weak-lined T Tauris. The lithium detection for TIC 146539195 is consistent with its mass and β Pic membership; the nondetections for LP 12-502 (TIC 402980664) and TIC 264599508 are consistent with the ≈42 Myr age implied by their membership in the Columba moving group.
Paper: Transient Corotating Clumps around Adolescent Low-mass Stars from Four Years of TESS
Authors: Luke G. Bouma, Rahul Jayaraman, Saul Rappaport, Luisa M. Rebull, Lynne A. Hillenbrand, Joshua N. Winn, Alexandre David-Uraz, Gáspár Á. Bakos
Figure caption: Brightnesses and distances of our CPVs compared against previous work. “K2 literature” corresponds to Stauffer et al. (2017), Stauffer et al. (2018b). “TESS literature” corresponds to Zhan et al. (2019), Stauffer et al. (2021), Günther et al. (2022), and Popinchalk et al. (2023). “CPVs” and “candidates” are as in Figure 5; though, for visual clarity, unresolved binaries are not highlighted. PTFO 8-8695, a CPV at a distance of ≈350 pc, is not shown.
Paper: Transient Corotating Clumps around Adolescent Low-mass Stars from Four Years of TESS
Authors: Luke G. Bouma, Rahul Jayaraman, Saul Rappaport, Luisa M. Rebull, Lynne A. Hillenbrand, Joshua N. Winn, Alexandre David-Uraz, Gáspár Á. Bakos
Figure caption: River plots of TIC 300651846. This is an alternative visualization of the data in Figure 11. All available 2 minute cadence data as of 2023 August 11 are shown. Cycles 0–622 span TESS Sectors 32–39 (2020 November–2021 June); cycles 2296–2676 span Sectors 61–65 (2023 January–June). We assumed P = 8.254 hr, and t 0=2174.127 [BTJD]. Note that the two panels have slightly different color scales.
Paper: High-resolution, Mid-infrared Color Temperature Mapping of the Central 10″ of the Galaxy
Authors: Cuc K. Dinh, Anna Ciurlo, Mark R. Morris, Rainer Schödel, Andrea Ghez, Tuan Do
Figure caption: Comparison of the Bullet feature as observed in the 3.8 μm band (upper left), 8.6 μm band (upper right), color temperature map (lower left), and optical depth map at 3.8 μm (lower right). We find that the color temperature of the Bullet is lowest at the head and increases in temperature with increasing distance along its tail. The proper motion of the Bullet shows it to be moving parallel to its length with the head at the leading edge (Zhao & Goss 1998).
Paper: High-resolution, Mid-infrared Color Temperature Mapping of the Central 10″ of the Galaxy
Authors: Cuc K. Dinh, Anna Ciurlo, Mark R. Morris, Rainer Schödel, Andrea Ghez, Tuan Do
Figure caption: Locations of currently known infrared-excess sources and G objects compared to the identified cold sources within the vicinity. Cool sources ID5 4, 55, and 65 are located beyond this region. The so-called Sgr A* ridge is superimposed near Sgr A* on the line of sight and not actually within its vicinity in 3D (but see also Peißker et al. 2020).
Paper: High-resolution, Mid-infrared Color Temperature Mapping of the Central 10″ of the Galaxy
Authors: Cuc K. Dinh, Anna Ciurlo, Mark R. Morris, Rainer Schödel, Andrea Ghez, Tuan Do
Figure caption: Comparison of the IRS 13N complex as observed at 3.6 μm (upper left), the 8.6 μm band (upper right), color temperature (lower left), and optical depth at 3.8 μm (lower right). Known K-band stars and their proper motion are marked in the L′ map (Jia et al. 2019). Cool features ID 55 and ID 39 have been marked in the PAH map.
Paper: High-resolution, Mid-infrared Color Temperature Mapping of the Central 10″ of the Galaxy
Authors: Cuc K. Dinh, Anna Ciurlo, Mark R. Morris, Rainer Schödel, Andrea Ghez, Tuan Do
Figure caption: Comparison of the Strand as observed in the 3 3.6 μm band (upper left), 8.6 μm band (upper right), color temperature map (lower left), and optical depth map at 3.8 μm (lower right). The strand is manifested in the color temperature map as a linear depression. The color temperature map indicates the possible presence of a secondary feature (Strand 2) parallel to the Strand.