adsabs/AstroCLIMB huggingface dataset:
Paper: An Optically Discovered Outburst from XTE J1859+226
Authors: Eric C. Bellm, Yuankun Wang, Jan van Roestel, Rebecca A. Phillipson, Michael W. Coughlin, John A. Tomsick, Steven L. Groom, Brian Healy, Josiah Purdum, Ben Rusholme, Jesper Sollerman, Peter Bealo, Stefano Lora, Eddy Muyllaert, Ivo Peretto, Erik J. Schwendeman
Figure caption: ZTF forced photometry light curve of XTE J1859+226 in quiescence in g (blue) and r (orange) bands. We plot both single-epoch measurements (points) and error-weighted coadditions over 100 days (points with horizontal error bars). Detections with S/N greater than 3 are marked with circles, and 5σ upper limits with triangles. We exclude the outburst interval (gray region).
Paper: An Optically Discovered Outburst from XTE J1859+226
Authors: Eric C. Bellm, Yuankun Wang, Jan van Roestel, Rebecca A. Phillipson, Michael W. Coughlin, John A. Tomsick, Steven L. Groom, Brian Healy, Josiah Purdum, Ben Rusholme, Jesper Sollerman, Peter Bealo, Stefano Lora, Eddy Muyllaert, Ivo Peretto, Erik J. Schwendeman
Figure caption: Swift-XRT hardness–intensity diagram. Lines connect consecutive measurements; the earliest measurements are the brightest (see Figure 1). Dashed lines show the hardness–intensity values produced by absorbed power-law spectra with n H = 3.1 × 1021 atoms cm−2 and spectral indices Γ from 1.25 to 2.25 (top labels).
Paper: Left Ringing: Betelgeuse Illuminates the Connection between Convective Outbursts, Mode Switching, and Mass Ejection in Red Supergiants
Authors: Morgan MacLeod, Andrea Antoni, Caroline D. Huang, Andrea Dupree, Abraham Loeb
Figure caption: Histograms of time between successive photometric minima (top panel) or radial velocity maxima (lower panel). Minima and maxima are identified with a 60 days window function that suppresses short-timescale measurement noise and local extrema.
Paper: An Optically Discovered Outburst from XTE J1859+226
Authors: Eric C. Bellm, Yuankun Wang, Jan van Roestel, Rebecca A. Phillipson, Michael W. Coughlin, John A. Tomsick, Steven L. Groom, Brian Healy, Josiah Purdum, Ben Rusholme, Jesper Sollerman, Peter Bealo, Stefano Lora, Eddy Muyllaert, Ivo Peretto, Erik J. Schwendeman
Figure caption: Absorbed power-law fit to Swift and NuSTAR spectra.
Paper: CLASSY VII Lyα Profiles: The Structure and Kinematics of Neutral Gas and Implications for LyC Escape in Reionization-era Analogs 
Authors: Weida Hu, Crystal L. Martin, Max Gronke, Simon Gazagnes, Matthew Hayes, John Chisholm, Timothy Heckman, Matilde Mingozzi, Namrata Roy, Peter Senchyna, Xinfeng Xu, Danielle A. Berg, Bethan L. James, Daniel P. Stark, Karla Z. Arellano-Córdova, Alaina Henry, Anne E. Jaskot, Nimisha Kumari, Kaelee S. Parker, Claudia Scarlata, Aida Wofford, Ricardo O. Amorín, Naunet Leonhardes-Barboza, Jarle Brinchmann, Cody Carr, Alessandra Aloisi
Figure caption: Reduced χ 2 values of best-fit Lyα profiles derived by the first attempt of profile fitting (using total stellar continuum and Gaussian redshift prior) and the second attempt of profile fitting (using residual stellar continuum and Gaussian redshift prior). We notice that, except for one object (J0944-0038), the fitting results for objects with DLA are significantly improved if adopting the residual continua, which are corrected for the DLA covering fraction (1 − f  c ). For objects without DLA, the corrected continuum equals to the total stellar continuum. Thus, the reduced χ 2 does not change. We note the reduced χ 2 of some galaxies (J0944+3442, J1044+0353, J1144+4012, J1148+2546, J1416+1223) are much smaller than unity. This might be due to their error spectra being overestimated (comparing to their flux fluctuation, see Figure 3).
Paper: CLASSY VII Lyα Profiles: The Structure and Kinematics of Neutral Gas and Implications for LyC Escape in Reionization-era Analogs 
Authors: Weida Hu, Crystal L. Martin, Max Gronke, Simon Gazagnes, Matthew Hayes, John Chisholm, Timothy Heckman, Matilde Mingozzi, Namrata Roy, Peter Senchyna, Xinfeng Xu, Danielle A. Berg, Bethan L. James, Daniel P. Stark, Karla Z. Arellano-Córdova, Alaina Henry, Anne E. Jaskot, Nimisha Kumari, Kaelee S. Parker, Claudia Scarlata, Aida Wofford, Ricardo O. Amorín, Naunet Leonhardes-Barboza, Jarle Brinchmann, Cody Carr, Alessandra Aloisi
Figure caption: O I absorption profiles (blue) of CLASSY sample. The orange lines indicate best-fit Gaussian profiles. The first two rows show O I absorption profiles of galaxies without DLA system. The third row shows those O I profiles that might overlap with geocoronal O I emission, and the rest shows others. The shaded regions show the wavelength range (1302.2–1307.5 Å) that might be contaminated by geocoronal O I emission lines. An example of geocoronal O I line can be seen in the spectrum of J1525+0757, as shown in the online component of Figure 2. The O I absorption lines of 2 galaxies (J0405-3648 and J1225+6109) overlap with geocoronal O I line; thus, we adopt their C II velocities as DLA velocities. The vertical dashed lines indicate the zero velocity. Asterisks mark galaxies that show a pure DLA system with no Lyα emission.
Paper: CLASSY VII Lyα Profiles: The Structure and Kinematics of Neutral Gas and Implications for LyC Escape in Reionization-era Analogs 
Authors: Weida Hu, Crystal L. Martin, Max Gronke, Simon Gazagnes, Matthew Hayes, John Chisholm, Timothy Heckman, Matilde Mingozzi, Namrata Roy, Peter Senchyna, Xinfeng Xu, Danielle A. Berg, Bethan L. James, Daniel P. Stark, Karla Z. Arellano-Córdova, Alaina Henry, Anne E. Jaskot, Nimisha Kumari, Kaelee S. Parker, Claudia Scarlata, Aida Wofford, Ricardo O. Amorín, Naunet Leonhardes-Barboza, Jarle Brinchmann, Cody Carr, Alessandra Aloisi
Figure caption: Best-fit Lyα spectra (red) for 29 CLASSY galaxies using the residual stellar continuum and a Tophat redshift prior with a width of ±48 km s−1 (third attempt). The spectra are normalized by the peak flux, and the orange dashed lines indicate the continuum level for each object. We use the green lines to show the residual and manually shift it by −0.1 for better illustration. The gray dashed lines indicate the zero level of the residual.
Paper: CLASSY VII Lyα Profiles: The Structure and Kinematics of Neutral Gas and Implications for LyC Escape in Reionization-era Analogs 
Authors: Weida Hu, Crystal L. Martin, Max Gronke, Simon Gazagnes, Matthew Hayes, John Chisholm, Timothy Heckman, Matilde Mingozzi, Namrata Roy, Peter Senchyna, Xinfeng Xu, Danielle A. Berg, Bethan L. James, Daniel P. Stark, Karla Z. Arellano-Córdova, Alaina Henry, Anne E. Jaskot, Nimisha Kumari, Kaelee S. Parker, Claudia Scarlata, Aida Wofford, Ricardo O. Amorín, Naunet Leonhardes-Barboza, Jarle Brinchmann, Cody Carr, Alessandra Aloisi
Figure caption: Redshift difference between tlac redshift z tlac and spectroscopic redshift z spec. The black circles indicate the results of the second attempt of profile fitting with a Gaussian prior with σ = 120 km s−1 for redshift (unconstrained fitting). The red circles indicate the results of the third attempt of profile fitting with a Tophat prior with a width of ±44 km s−1 for redshift (constrained fitting).
Paper: CLASSY VII Lyα Profiles: The Structure and Kinematics of Neutral Gas and Implications for LyC Escape in Reionization-era Analogs 
Authors: Weida Hu, Crystal L. Martin, Max Gronke, Simon Gazagnes, Matthew Hayes, John Chisholm, Timothy Heckman, Matilde Mingozzi, Namrata Roy, Peter Senchyna, Xinfeng Xu, Danielle A. Berg, Bethan L. James, Daniel P. Stark, Karla Z. Arellano-Córdova, Alaina Henry, Anne E. Jaskot, Nimisha Kumari, Kaelee S. Parker, Claudia Scarlata, Aida Wofford, Ricardo O. Amorín, Naunet Leonhardes-Barboza, Jarle Brinchmann, Cody Carr, Alessandra Aloisi
Figure caption: The DLA covering fraction vs. the angular UV half-light radius. A covering fraction of 0 indicates no DLA. We color-coded the circles based on their spectroscopic redshift, thereby identifying variations in the physical scale of the aperture. We also use the blue and green vertical dashed lines to indicate the unvignetted radius (0.″4) and the total radius (1.″25) for the COS aperture. Roughly a half of higher-redshift galaxies (z > 0.1) show significant DLA system. This fraction increases to the lower-redshift sample, which tends to have a larger UV size (in arcsec) due to the projection effect.
Paper: CLASSY VII Lyα Profiles: The Structure and Kinematics of Neutral Gas and Implications for LyC Escape in Reionization-era Analogs 
Authors: Weida Hu, Crystal L. Martin, Max Gronke, Simon Gazagnes, Matthew Hayes, John Chisholm, Timothy Heckman, Matilde Mingozzi, Namrata Roy, Peter Senchyna, Xinfeng Xu, Danielle A. Berg, Bethan L. James, Daniel P. Stark, Karla Z. Arellano-Córdova, Alaina Henry, Anne E. Jaskot, Nimisha Kumari, Kaelee S. Parker, Claudia Scarlata, Aida Wofford, Ricardo O. Amorín, Naunet Leonhardes-Barboza, Jarle Brinchmann, Cody Carr, Alessandra Aloisi
Figure caption: Reduced χ 2 values of best-fit Lyα profiles derived by the second attempt (using the residual continuum and a Gaussian redshift prior) and the third attempt (using the residual continuum and a Tophat redshift prior). The second attempt adopts a Gaussian probability distribution with σ of 120 km s−1 as prior, and the third attempt adopts a Tophat probability distribution with a width of ±48 km s−1 as prior.
Paper: CLASSY VII Lyα Profiles: The Structure and Kinematics of Neutral Gas and Implications for LyC Escape in Reionization-era Analogs 
Authors: Weida Hu, Crystal L. Martin, Max Gronke, Simon Gazagnes, Matthew Hayes, John Chisholm, Timothy Heckman, Matilde Mingozzi, Namrata Roy, Peter Senchyna, Xinfeng Xu, Danielle A. Berg, Bethan L. James, Daniel P. Stark, Karla Z. Arellano-Córdova, Alaina Henry, Anne E. Jaskot, Nimisha Kumari, Kaelee S. Parker, Claudia Scarlata, Aida Wofford, Ricardo O. Amorín, Naunet Leonhardes-Barboza, Jarle Brinchmann, Cody Carr, Alessandra Aloisi
Figure caption: The Lyα spectra (black) and error spectra (gray) after subtracting the continuum and DLA of 34 CLASSY galaxies. We use green shades to show the masked geocoronal Lyα and O I emission lines. The continuum-subtracted spectra are normalized by peak flux. The total Lyα fluxes are measured by integrating fluxes within the wavelength range where Lyα emission lines meet zero flux.
Paper: CLASSY VII Lyα Profiles: The Structure and Kinematics of Neutral Gas and Implications for LyC Escape in Reionization-era Analogs 
Authors: Weida Hu, Crystal L. Martin, Max Gronke, Simon Gazagnes, Matthew Hayes, John Chisholm, Timothy Heckman, Matilde Mingozzi, Namrata Roy, Peter Senchyna, Xinfeng Xu, Danielle A. Berg, Bethan L. James, Daniel P. Stark, Karla Z. Arellano-Córdova, Alaina Henry, Anne E. Jaskot, Nimisha Kumari, Kaelee S. Parker, Claudia Scarlata, Aida Wofford, Ricardo O. Amorín, Naunet Leonhardes-Barboza, Jarle Brinchmann, Cody Carr, Alessandra Aloisi
Figure caption: DLA covering fraction vs. O I covering fraction. We mark those O I covering fractions that are possibly contaminated by geocoronal O I emission line (at 1302.2–1307.5 Å) as open circles. Excluding those points, the observed correlation suggests O I covering fraction probe H I covering fraction.
Paper: Solar–Stellar Connection: X-Ray Flares to Energetic (E > 10 MeV) Particle Events
Authors: S. W. Kahler, A. G. Ling
Figure caption: Peak flare temperature Tm  vs. log Fp for SEP events (including 13 GLEs; red plus signs) and DH type II bursts with no SEP events (diamonds). Events shown with turquoise circles are associated with neither SEP events nor type II bursts. Lines are quadratic fits to each distribution, showing lower Tm  values for SEP-associated events (SEP/Type II). The median peak flare temperature values of the No SEP, No Type II and SEP or Type II populations are indicated by the cyan and black horizontal dashed lines, respectively, and similarly for the log peak X-ray and vertical dashed lines. Not all X-ray flares had associated Tm  values.
Paper: Solar–Stellar Connection: X-Ray Flares to Energetic (E > 10 MeV) Particle Events
Authors: S. W. Kahler, A. G. Ling
Figure caption: Log decay times C2 vs. log Fp for SEP events, including eight GLEs (red plus signs) and DH type II bursts (diamonds). The non-SEP events (turquoise) are separated statistically from the SEP events. Not all the X-ray flares had associated C2 values. The median log decay time C2 values of the No SEP, No Type II and SEP or Type II populations are indicated by the cyan and black horizontal dashed lines, respectively, and similarly for the log peak X-ray and vertical dashed lines.
Paper: Solar–Stellar Connection: X-Ray Flares to Energetic (E > 10 MeV) Particle Events
Authors: S. W. Kahler, A. G. Ling
Figure caption: Log rise time TR vs. log Fp for SEP events, including 15 GLEs (red plus signs) and DH type II bursts (diamonds). Median values of the 390 non-SEP events shown in turquoise are clearly separated statistically from those of the 195 SEP and type II burst events. The median log rise time values of the No SEP, No Type II and SEP or Type II populations are indicated by the cyan and black horizontal dashed lines, respectively, and similarly for the log peak X-ray and vertical dashed lines.
Paper: Complex Organic Molecules in a Very Young Hot Corino, HOPS 373SW
Authors: Jeong-Eun Lee, Giseon Baek, Seokho Lee, Jae-Hong Jeong, Chul-Hwan Kim, Yuri Aikawa, Gregory J. Herczeg, Doug Johnstone, John J. Tobin
Figure caption: Comparison of COM abundances with other hot corinos and disks. The abundances toward HOPS 373SW and other sources (Table 6) are on the x- and y-axis, respectively. Some abundances from the literature are rescaled to be consistent with our assumption of 12C/13C = 60. The diagonal lines denote equal abundances (solid) and abundance factors of 3 (dashed) and 10 (dotted) above or below those in HOPS 373SW.
Paper: Complex Organic Molecules in a Very Young Hot Corino, HOPS 373SW
Authors: Jeong-Eun Lee, Giseon Baek, Seokho Lee, Jae-Hong Jeong, Chul-Hwan Kim, Yuri Aikawa, Gregory J. Herczeg, Doug Johnstone, John J. Tobin
Figure caption: Column density ratios of CH2DOH/CH3OH (upper panel) and CHD2OH/CH2DOH (lower panel). Filled and open symbols indicate single-dish and interferometric observations, respectively. Except for HOPS 373SW, the data have been obtained from the literature: L1521E, B68, L694-2, and H-MM1 from Lin et al. (2023); L1544 from Chacón-Tanarro et al. (2019); HH 212 from Lee et al. (2019a); IRAS 16293A and IRAS 16293B from Jørgensen et al. (2018), Manigand et al. (2019), and Drozdovskaya et al. (2022); NGC 1333–IRAS 2A and NGC 1333–IRAS 4A from Taquet et al. (2019); L483 from Agundez et al. (2019); SVS 13 from Bianchi et al. (2017); V883 Ori from Lee et al. (2019b); and 67P/C-G from Drozdovskaya et al. (2021).
Paper: Solar–Stellar Connection: X-Ray Flares to Energetic (E > 10 MeV) Particle Events
Authors: S. W. Kahler, A. G. Ling
Figure caption: Numbers of SEP events and DH type II bursts in five solar source longitude bins of equal widths. There are 105 total SEP events, of which eight have no associated type II bursts (red), and 90 DH type II bursts with no associated SEP events (orange), for a total of 195 combined events (blue) used in this work.
Paper: Solar–Stellar Connection: X-Ray Flares to Energetic (E > 10 MeV) Particle Events
Authors: S. W. Kahler, A. G. Ling
Figure caption: Log duration times TD vs. Fp for SEP events, including 15 GLEs (red plus signs) and DH type II bursts (diamonds). The 390 non-SEP events (turquoise) are clearly separated statistically from the 195 SEP and type II burst events. The median log duration time values of the No SEP, No Type II and SEP or Type II populations are indicated by the cyan and black horizontal dashed lines, respectively, similarly for the log peak X-ray and vertical dashed lines.
Paper: Solar–Stellar Connection: X-Ray Flares to Energetic (E > 10 MeV) Particle Events
Authors: S. W. Kahler, A. G. Ling
Figure caption: Log of timescale versus peak temperature for medians of flares with no SEP or type II event (black) and for flares with SEP events or type II bursts (red) for three X-ray flare timescales. The best separation is that of the C2 timescale.
Paper: Negative Lags on the Viscous Timescale in Quasar Photometry and Prospects for Detecting More with LSST
Authors: Amy Secunda, Jenny E. Greene, Yan-Fei Jiang, 燕飞 姜, Philippe Z. Yao, Abderahmen Zoghbi
Figure caption: The time lags as a function of frequency between two evenly sampled, daily cadence light curves found using the phase of their complex cross-spectrum and Equation (15). The input long (short) lags are −50 (7) and −130 (9) days in the top and bottom panels, respectively. Distributions shown in orange have been reprocessed with only a long lag. The ratio between the amplitudes of the long and short lag for the light curves with distributions shown in green, light blue, and pink, are 0.2, 0.1, and 0.01, respectively. The dashed horizontal lines show the input lags and zero, and the vertical gray lines show the wrapping frequencies.
Paper: Negative Lags on the Viscous Timescale in Quasar Photometry and Prospects for Detecting More with LSST
Authors: Amy Secunda, Jenny E. Greene, Yan-Fei Jiang, 燕飞 姜, Philippe Z. Yao, Abderahmen Zoghbi
Figure caption: Distribution of the long lags recovered by JAVELIN (top panel) and the maximum-likelihood method (bottom panel) for 100 mock light curves with input lags of −50 and 7 days (top panel). The dashed vertical line shows the input long lag. The green and light blue distributions are for mock light curves with the baseline v2.0 LSST cadence for the u and y band and g and z band, respectively. The distributions shown in pink are for light curves with the baseline g- and z-band cadence plus an LCO observation taken roughly every 10 days in each LSST observing gap. These LCO observations amount to around 18 observations in each gap, or per year, for a total of around 180 observations.
Paper: Negative Lags on the Viscous Timescale in Quasar Photometry and Prospects for Detecting More with LSST
Authors: Amy Secunda, Jenny E. Greene, Yan-Fei Jiang, 燕飞 姜, Philippe Z. Yao, Abderahmen Zoghbi
Figure caption: The distribution of the short lags detected by JAVELIN (top panel) and the maximum-likelihood method (bottom panel) for 100 mock long season cadence LSST light curves with different amplitude ratios (shown in the legend). In the top panel, we zoom in on the portion of the distribution between 0 and 20 days to better show the accuracy of the short lag when detected. The input short lag, shown as the vertical dashed line, is 7 days.
Paper: Negative Lags on the Viscous Timescale in Quasar Photometry and Prospects for Detecting More with LSST
Authors: Amy Secunda, Jenny E. Greene, Yan-Fei Jiang, 燕飞 姜, Philippe Z. Yao, Abderahmen Zoghbi
Figure caption: The distributions of the long lags detected by JAVELIN (top panel) and the maximum-likelihood method (bottom panel) for 100 mock long season cadence LSST light curves with an input long lag of −50 days (shown as a dashed black line). Distributions shown in blue are for light curves that also have a short lag of 7 days. The legends show the ratio of the amplitude of the long lag to the amplitude of the short lag for each blue distribution.
Paper: Negative Lags on the Viscous Timescale in Quasar Photometry and Prospects for Detecting More with LSST
Authors: Amy Secunda, Jenny E. Greene, Yan-Fei Jiang, 燕飞 姜, Philippe Z. Yao, Abderahmen Zoghbi
Figure caption: The distributions of the long lags recovered by JAVELIN (top panel) and the maximum-likelihood method (bottom panel) for 100 light curves with input lags of −50 and 7 days. The green and orange distributions are for mock light curves with the long season and baseline v2.0 LSST cadences, respectively, for the u and y band. The dashed vertical line shows the input long lag.
Paper: Negative Lags on the Viscous Timescale in Quasar Photometry and Prospects for Detecting More with LSST
Authors: Amy Secunda, Jenny E. Greene, Yan-Fei Jiang, 燕飞 姜, Philippe Z. Yao, Abderahmen Zoghbi
Figure caption: The fractional error of the median of the distribution of long lags recovered by JAVELIN (points) and the Fourier method (diamonds) for 100 mock long season cadence LSST light curves as a function of the ratio of the amplitude of the long lag to the amplitude of the short lag for input long lags of −50, −130, and −400 days in blue, purple, and orange, respectively. The error bars represent the fractional error of one standard deviation for each distribution, and the horizontal dashed line shows zero. A slight scatter is added in the x-direction to make the individual points easier to view.
Paper: Negative Lags on the Viscous Timescale in Quasar Photometry and Prospects for Detecting More with LSST
Authors: Amy Secunda, Jenny E. Greene, Yan-Fei Jiang, 燕飞 姜, Philippe Z. Yao, Abderahmen Zoghbi
Figure caption: The distribution of the long lags detected by JAVELIN for 100 mock long season cadence LSST light curves with input long lags of −50, −130, and −400 days (shown as dashed black lines) in the top, center, and bottom panels, respectively.
Paper: Negative Lags on the Viscous Timescale in Quasar Photometry and Prospects for Detecting More with LSST
Authors: Amy Secunda, Jenny E. Greene, Yan-Fei Jiang, 燕飞 姜, Philippe Z. Yao, Abderahmen Zoghbi
Figure caption: The distribution of long lags recovered by the maximum-likelihood method for 100 mock long season cadence LSST light curves with input long lags (shown as dashed black lines) of −50 days (top panel) and −130 days (bottom panel).
Paper: Negative Lags on the Viscous Timescale in Quasar Photometry and Prospects for Detecting More with LSST
Authors: Amy Secunda, Jenny E. Greene, Yan-Fei Jiang, 燕飞 姜, Philippe Z. Yao, Abderahmen Zoghbi
Figure caption: The distribution of the inverse of the time between each observation in the LSST long season cadence.
Paper: Transition Probabilities of Near-infrared Ce III Lines from Stellar Spectra: Applications to Kilonovae
Authors: Nanae Domoto, Jae-Joon Lee, Masaomi Tanaka, Ho-Gyu Lee, Wako Aoki, Miho N. Ishigaki, Shinya Wanajo, Daiji Kato, Kenta Hotokezaka
Figure caption: The IGRINS spectra around the Ce III lines of the selected stars. Black and gray lines show the spectra for the objects used as the final sample and for the excluded objects, respectively (see the text). The positions of the three Ce III lines that we focus on are indicated by thick orange lines (Table 1), while that of another Ce III line is also indicated by a thin orange line (see Section 2). Al I and Si I lines that may contaminate the Ce III lines are labeled in blue. Other lines are also shown in gray.
Paper: Transition Probabilities of Near-infrared Ce III Lines from Stellar Spectra: Applications to Kilonovae
Authors: Nanae Domoto, Jae-Joon Lee, Masaomi Tanaka, Ho-Gyu Lee, Wako Aoki, Miho N. Ishigaki, Shinya Wanajo, Daiji Kato, Kenta Hotokezaka
Figure caption: Astrophysical gf-values of the Ce III lines derived from four stellar spectra (blue dots), and their average (red dots). Each panel shows the results of each transition as shown in the legend. Black diamonds show the theoretical gf-values (T20: Tanaka et al. 2020; WR98: Wyart & Palmeri 1998; B02: Biémont et al. 2002, see Table 1; CG21: Carvajal Gallego et al. 2021). Error bars indicate the estimated systematic uncertainties (see Section 4.3 and Table 4).
Paper: Deep Search for Molecular Oxygen in TW Hya
Authors: Becky J. Williams, L. Ilsedore Cleeves, Christian Eistrup, Jon P. Ramsey
Figure caption: Upper limits on O2 in TW Hya as a function of temperature. The shaded region shows typical temperatures in TW Hya (see Bergin & Cleeves 2018), the light blue and dark blue open triangles show the upper limits on O2 abundance within 120 au and 260 au, respectively. Values for solar oxygen abundance (Asplund et al. 2009) and other known oxygen-carrying species are shown along the right axis. For dust, we assumed a value of 1.4 × 10−4 from Whittet (2010). From top to bottom, the remaining values used are from Ripple et al. (2013), van Dishoeck et al. (2013), Favre et al. (2013), and Zhang et al. (2013).