adsabs/AstroCLIMB huggingface dataset:
Paper: The Dusty Red Supergiant Progenitor and the Local Environment of the Type II SN 2023ixf in M101
Authors: Zexi Niu, Ning-Chen Sun, Justyn R. Maund, Yu Zhang, Ruining Zhao, Jifeng Liu
Figure caption: (a) Observed SED (black data points) and the best-fitting model with C-rich dust (colored solid lines) for the progenitor of SN 2023ixf. The vertical error bars reflect their 3σ photometric uncertainties and the horizontal error bars are the rms bandwidths. Only 3σ detection limits in Spitzer/IRAC [5.8] and [8.0] bands are displayed (inverted triangles), and those in the other bands are not very constraining on the progenitor’s SED. The 2σ detection limit in [8.0] band is shown in gray. The dashed, dotted, and dotted–dashed lines correspond to the attenuated RSG radiation, dust emission, and dust-scattered radiation, respectively. The yellow, red, and blue colors correspond to effective temperatures of T eff = 3400, 3700, and 4000 K for the RSG progenitor. Detailed model parameters are listed in Table 3. (b) Same as (a) but for the O-rich dust model. Notice that the prominent silicate bumps of T eff = 3700 and 4000 K models almost exceed the [8.0] detection limit. (c) The progenitor of SN 2023ixf on the Hertzsprung–Russell diagram. The diamonds and stars demonstrate models with O-rich and C-rich dust, respectively. They are colored in the same way as (a)–(b). Overlaid black/gray lines are the PARSEC stellar evolutionary tracks for different initial masses.
Paper: The Dusty Red Supergiant Progenitor and the Local Environment of the Type II SN 2023ixf in M101
Authors: Zexi Niu, Ning-Chen Sun, Justyn R. Maund, Yu Zhang, Ruining Zhao, Jifeng Liu
Figure caption: (a), (b) Color–magnitude diagrams of resolved stellar populations within 150 pc from SN 2023ixf (orange data points). The error bars reflect their 1σ photometric uncertainties. The dashed lines show the 50% detection limits, and the gray-shaded regions show where ≤68% of the artificial stars can be successfully recovered. Model stellar populations with three age components are fitted to the data, and the (blue, green, and red) thin lines are stellar isochrones from 100 random realizations according to the stellar log-age and extinction distributions of the model populations. The arrows in the upper-left corners are total (Galactic + internal) reddening vectors for a standard extinction law with R  V  = 3.1. (c) The star formation history in the vicinity of SN 2023ixf from 100 random realizations; the heights of the peaks are scaled to correspond to the weighting of each star formation epoch.
Paper: The Dusty Red Supergiant Progenitor and the Local Environment of the Type II SN 2023ixf in M101
Authors: Zexi Niu, Ning-Chen Sun, Justyn R. Maund, Yu Zhang, Ruining Zhao, Jifeng Liu
Figure caption: (a) Continuum-subtracted spectrum of the nearby H II region to the north of SN 2023ixf (Figure 1). The gray-shaded wavelength ranges are enlarged in panels (b) and (c), where the red and blue lines display the total and single Gaussian fits to the nebular emission lines, respectively.
Paper: The Dusty Red Supergiant Progenitor and the Local Environment of the Type II SN 2023ixf in M101
Authors: Zexi Niu, Ning-Chen Sun, Justyn R. Maund, Yu Zhang, Ruining Zhao, Jifeng Liu
Figure caption: Light and color curves of the progenitor of SN 2023ixf. The dotted horizontal lines are the phase-weighted averages and the light-shaded regions reflect the typical photometric uncertainties.
Paper: Low- and High-energy Neutrinos from SN 2023ixf in M101
Authors: Dafne Guetta, Aurora Langella, Silvia Gagliardini, Massimo Della Valle
Figure caption: Number of expected IBD events in Super-Kamiokande as a function of distance for supernovae based on different models. The number of events is calculated considering the fiducial volume (FV) of the detector (22.5 kton). The black dashed lines correspond to “typical” distances within the Milky Way and in the Local Group up to M101, the host galaxy of SN 2023ixf.
Paper: Low- and High-energy Neutrinos from SN 2023ixf in M101
Authors: Dafne Guetta, Aurora Langella, Silvia Gagliardini, Massimo Della Valle
Figure caption: Super-Kamiokande detection efficiency as a function of the positron energy. Taken from Ricciardi et al. (2022).
Paper: Low- and High-energy Neutrinos from SN 2023ixf in M101
Authors: Dafne Guetta, Aurora Langella, Silvia Gagliardini, Massimo Della Valle
Figure caption: Kinetic energy of the jet E = 1051 erg. The figure shows the muon and antimuon neutrino number in the IceCube telescope, as a function of the baryon loading f  p  for different sets of the parameters t jet = 102, 103, 104 s, and Γ = 1, 100.
Paper: Low- and High-energy Neutrinos from SN 2023ixf in M101
Authors: Dafne Guetta, Aurora Langella, Silvia Gagliardini, Massimo Della Valle
Figure caption: Number of expected IBD events in Hyper-Kamiokande as a function of distance for supernovae based on different models. The number of events is calculated considering the FV of the detector (220 kton). The black dashed lines correspond to “typical” distances within the Milky Way and in the Local Group up to M101, the host galaxy of SN 2023ixf.
Paper: The Mass–Metallicity Relation of Dwarf Galaxies at Cosmic Noon from JWST Observations
Authors: Mingyu Li, 明宇 李, Zheng Cai, Fuyan Bian, Xiaojing Lin, Zihao Li, Yunjing Wu, Fengwu Sun, Shiwu Zhang, Emmet Golden-Marx, Zechang Sun, Siwei Zou, Xiaohui Fan, Eiichi Egami, Stephane Charlot, Gustavo Bruzual, Jacopo Chevallard
Figure caption: The mass–metallicity relation (MZR) for dwarf galaxies at z ≃ 2 (blue) and z ≃ 3 (red). The unfilled squares and hexagons denote individual galaxies at z ≃ 2 and ≃3 respectively. The large blue squares and red hexagons mark the results based on stacked spectra. The error bar in the lower left corner displays the median uncertainty of the individual galaxies. The best-fit results are denoted by the colored dashed lines, with their 1σ uncertainties in the shaded region. The MOSDEF stacked results (Sanders et al. 2021) are marked as black triangles, and Henry et al. (2021) stacked results are marked as black crosses. The MOSDEF best-fit result and the extrapolation to the low-mass end are in solid and dashed lines.
Paper: The Mass–Metallicity Relation of Dwarf Galaxies at Cosmic Noon from JWST Observations
Authors: Mingyu Li, 明宇 李, Zheng Cai, Fuyan Bian, Xiaojing Lin, Zihao Li, Yunjing Wu, Fengwu Sun, Shiwu Zhang, Emmet Golden-Marx, Zechang Sun, Siwei Zou, Xiaohui Fan, Eiichi Egami, Stephane Charlot, Gustavo Bruzual, Jacopo Chevallard
Figure caption: Projection of the fundamental metallicity relation (FMR) as O/H vs. ﹩{\mu }_{{\alpha }_{\mathrm{best}}}=\mathrm{log}(M/{M}_{\odot })-{\alpha }_{\mathrm{best}}\times \mathrm{log}(\mathrm{SFR}/{M}_{\odot }\,{\mathrm{yr}}^{-1})﹩. The coefficient α best = 0.60, minimizes the scatter of the O/H for our sample. The solid black line shows the best linear fit from Equation (4), and the gray-shaded region shows the 1σ uncertainty. The unfilled squares and hexagons represent individual galaxies at z ≃ 2 and z ≃ 3 respectively, and the large colored ones show the stacked results. The black triangles denote the MOSDEF stacked results from Sanders et al. (2021), and the black dotted–dashed line marks their best fit. The error bar in the lower right corner displays the median uncertainty of the individual galaxies.
Paper: Potential Atmospheric Compositions of TRAPPIST-1 c Constrained by JWST/MIRI Observations at 15 μm
Authors: Andrew P. Lincowski, Victoria S. Meadows, Sebastian Zieba, Laura Kreidberg, Caroline Morley, Michaël Gillon, Franck Selsis, Eric Agol, Emeline Bolmont, Elsa Ducrot, Renyu Hu, Daniel D. B. Koll, Xintong Lyu, Avi Mandell, Gabrielle Suissa, Patrick Tamburo
Figure caption: Brightness temperature spectra for the dayside hemisphere of all modeled environments, with points corresponding to the model spectra convolved to the F1500W filter band over the band’s wavelength extent (horizontal error bars show the FWHM of the filter band). We also plot lines for 340 K (blackbody, no atmosphere, full heat redistribution) and 430 K (blackbody, no atmosphere, no heat redistribution), along with the data point measured by Zieba et al. (2023), which has a brightness temperature equivalent to 380 ± 31 K. Top: Venus-like modeled environments. Middle: steam environments. Bottom: O2-dominated environments. The Venuses are between 2.6σ and 3.1σ from the measured eclipse depth, and the steam atmospheres are within 1.7σ–1.8σ of the measured eclipse depth. The clear-sky Venuses all exhibit similar CO2 bands between 0.1 and 10 bars. The steam environments spanning 0.1–3 bars are nearly identical across the MIR spectrum. The O2-dominated environments, with varying amounts of CO2, exhibit the largest range in their spectra, and those of ≥1 bar also exhibit strong ozone features. For reference, the F1500W brightness temperature value from Zieba et al. (2023) for their best-fit desiccated O2–CO2 atmosphere is 395 K, and their best-fit bare rock surface is 420 K.
Paper: Potential Atmospheric Compositions of TRAPPIST-1 c Constrained by JWST/MIRI Observations at 15 μm
Authors: Andrew P. Lincowski, Victoria S. Meadows, Sebastian Zieba, Laura Kreidberg, Caroline Morley, Michaël Gillon, Franck Selsis, Eric Agol, Emeline Bolmont, Elsa Ducrot, Renyu Hu, Daniel D. B. Koll, Xintong Lyu, Avi Mandell, Gabrielle Suissa, Patrick Tamburo
Figure caption: Dayside hemisphere temperature structures for all modeled atmospheres: Venus-like (left panel), steam (middle panel), and O2–CO2 (right panel). For our modeled atmospheres, we have used a thicker line to show the layers over which the 15 μm band reached an optical depth of 1 (indicating the effective emission layer) for each model atmosphere. The dots indicate the lowest layer probed in the 15 μm band. In the right panel, we also include two example temperature–pressure profiles from Zieba et al. (2023) for 0.1 and 1 bar O2-dominated atmospheres, each with 100 ppm CO2. A wide variety of temperature profiles are possible for TRAPPIST-1 c under different atmospheric compositions. Although surface temperatures differ widely, note the similarities in emission temperatures/pressures probed for similar atmospheric compositions.
Paper: Potential Atmospheric Compositions of TRAPPIST-1 c Constrained by JWST/MIRI Observations at 15 μm
Authors: Andrew P. Lincowski, Victoria S. Meadows, Sebastian Zieba, Laura Kreidberg, Caroline Morley, Michaël Gillon, Franck Selsis, Eric Agol, Emeline Bolmont, Elsa Ducrot, Renyu Hu, Daniel D. B. Koll, Xintong Lyu, Avi Mandell, Gabrielle Suissa, Patrick Tamburo
Figure caption: Brightness temperature spectra for the dayside hemisphere of selected modeled environments for TRAPPIST-1 c with JWST with points corresponding to the model spectra convolved to the F1500W filter band over the FWHM of the band’s wavelength extent (horizontal error bars). We also show the data point measured by Zieba et al. (2023), along with lines corresponding to blackbody temperatures for the dayside with zero heat redistribution (dark gray dashed) and a blackbody with perfect heat redistribution (light gray dashed). The best-fit atmospheres are the 0.1 bar, O2-dominated atmospheres at 0.5σ–1.0σ from the measured eclipse depth.
Paper: Potential Atmospheric Compositions of TRAPPIST-1 c Constrained by JWST/MIRI Observations at 15 μm
Authors: Andrew P. Lincowski, Victoria S. Meadows, Sebastian Zieba, Laura Kreidberg, Caroline Morley, Michaël Gillon, Franck Selsis, Eric Agol, Emeline Bolmont, Elsa Ducrot, Renyu Hu, Daniel D. B. Koll, Xintong Lyu, Avi Mandell, Gabrielle Suissa, Patrick Tamburo
Figure caption: Global mixing ratio profiles for modeled steam (1 bar) and O2 atmospheres. The H2O and CO2 maintain evenly mixed profiles for each case. Ozone and CO are photochemically generated. As discussed in the main text, some of the cases do have CO outgassing, as seen here in the profiles.
Paper: Potential Atmospheric Compositions of TRAPPIST-1 c Constrained by JWST/MIRI Observations at 15 μm
Authors: Andrew P. Lincowski, Victoria S. Meadows, Sebastian Zieba, Laura Kreidberg, Caroline Morley, Michaël Gillon, Franck Selsis, Eric Agol, Emeline Bolmont, Elsa Ducrot, Renyu Hu, Daniel D. B. Koll, Xintong Lyu, Avi Mandell, Gabrielle Suissa, Patrick Tamburo
Figure caption: Global mixing ratio profiles for modeled Venus-like atmospheres. Here we show the clear and cloudy 10 bar cases. The lower-pressure clear-sky cases are similar to the 10 bar case.
Paper: Potential Atmospheric Compositions of TRAPPIST-1 c Constrained by JWST/MIRI Observations at 15 μm
Authors: Andrew P. Lincowski, Victoria S. Meadows, Sebastian Zieba, Laura Kreidberg, Caroline Morley, Michaël Gillon, Franck Selsis, Eric Agol, Emeline Bolmont, Elsa Ducrot, Renyu Hu, Daniel D. B. Koll, Xintong Lyu, Avi Mandell, Gabrielle Suissa, Patrick Tamburo
Figure caption: Phase curves of THAI benchmark cases ben1 and ben2 with VPL Climate (black lines) and ExoCAM (blue lines). These phase curves demonstrate good agreement between the 3D GCM and two-column models, indicating the day–night advection functions appropriately in VPL Climate.
Paper: Constraints on the Intergalactic Magnetic Field Strength from γ-Ray Observations of GRB 221009A
Authors: Yi-Yun Huang, Cui-Yuan Dai, Hai-Ming Zhang, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: Comparison between the expected flux of the echo emission and the observed data by Fermi-LAT in the analytic approach. The SEDs of the echo emission are averaged over the observation time 4000 s–3 days (top panel), 3–30 days (middle panel), and 1–8 months (bottom panel). The dashed and solid lines represent the cases assuming a maximum energy of 7 TeV and 15 TeV, respectively. The black points denote the Fermi-LAT detection, while the black arrows denote the upper limits.
Paper: Constraints on the Intergalactic Magnetic Field Strength from γ-Ray Observations of GRB 221009A
Authors: Yi-Yun Huang, Cui-Yuan Dai, Hai-Ming Zhang, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: Comparison between the expected flux of the echo emission and the observed data by Fermi-LAT in Monte Carlo simulation. The dashed lines represent the echo emission using the standard flux of the EBL model of Saldana-Lopez et al. (2021), while the color bands represent the echo emission considering the uncertainties in the EBL intensity.
Paper: Constraints on the Intergalactic Magnetic Field Strength from γ-Ray Observations of GRB 221009A
Authors: Yi-Yun Huang, Cui-Yuan Dai, Hai-Ming Zhang, Ruo-Yu Liu, Xiang-Yu Wang
Figure caption: Comparison between the expected flux of the echo emission and the observed data by Fermi-LAT in the time interval of T 0 + 0.2 − T 0 + 0.8 day, during which the 397 GeV photon was detected.
Paper: The Q Branch Cooling Anomaly Can Be Explained by Mergers of White Dwarfs and Subgiant Stars
Authors: Ken J. Shen, Simon Blouin, Katelyn Breivik
Figure caption: Mass fractions vs. enclosed mass within a merger remnant initially consisting of a 1.0 M ⊙ C/O core with a 0.2 M ⊙ envelope composed of 95% helium and 5% 14N, by mass. Panel (a) shows the composition when the shell helium-burning luminosity has decreased to 1 L ⊙. Panel (b) shows profiles after the merger remnant has cooled to a core temperature of 1.5 × 107 K, 5 × 108 yr after the time shown in panel (a).
Paper: The Q Branch Cooling Anomaly Can Be Explained by Mergers of White Dwarfs and Subgiant Stars
Authors: Ken J. Shen, Simon Blouin, Katelyn Breivik
Figure caption: Mass-loss rate vs. the mass of an initially 2 M ⊙ subgiant in a binary with a 1 M ⊙ WD at an initial separation of 5 R ⊙. Mass transfer is assumed to be fully nonconservative, with 30% of the angular momentum in the ejected mass coming from the binary orbit.
Paper: The Q Branch Cooling Anomaly Can Be Explained by Mergers of White Dwarfs and Subgiant Stars
Authors: Ken J. Shen, Simon Blouin, Katelyn Breivik
Figure caption: C/O/Mg phase diagram. The liquidus (orange) and solidus (blue) are connected by green lines that represent the composition difference between the coexisting liquid and solid phases. C/O mixtures with traces of magnesium are found close to the right axis. Note that number fractions are used in this figure.
Paper: The Q Branch Cooling Anomaly Can Be Explained by Mergers of White Dwarfs and Subgiant Stars
Authors: Ken J. Shen, Simon Blouin, Katelyn Breivik
Figure caption: The radius of an initially 2 M ⊙ subgiant in a binary with a 1 M ⊙ WD at an initial separation of 5 R ⊙. The initial radius evolution, shown as a black line, corresponds to the binary calculation shown in Figure 1. After this phase, mass is removed at a constant rate of 10−6  M ⊙ yr−1, resulting in the red line. The blue dotted line shows the donor’s Roche lobe radius, assuming all of the angular momentum required for ejection comes from the binary orbit.
Paper: The Q Branch Cooling Anomaly Can Be Explained by Mergers of White Dwarfs and Subgiant Stars
Authors: Ken J. Shen, Simon Blouin, Katelyn Breivik
Figure caption: Mass fractions vs. enclosed mass within a 1.0 M ⊙ C/O WD. Panel (a) shows the composition when the shell helium-burning luminosity has decreased to 1 L ⊙. Panel (b) shows profiles when the WD’s core temperature has cooled to 107 K, 6 × 108 yr after the time shown in panel (a).
Paper: X-Ray Detection of the Galaxy’s Missing Baryons in the Circumgalactic Medium of L* Galaxies
Authors: Fabrizio Nicastro, Y. Krongold, T. Fang, F. Fraternali, S. Mathur, S. Bianchi, A. De Rosa, E. Piconcelli, L. Zappacosta, M. Bischetti, C. Feruglio, A. Gupta, Z. Zhou
Figure caption: The 1σ (orange), 2σ (green), and 3σ (violet) confidence-level contours of the LLS frame O VII Kα line EW and centroid hinted at in the individual XMM-Newton RGS  and Chandra LETG  spectra of our three targets. Colored shaded areas are the EW-λ confidence levels for the best-fitting line parameters of the three LLSs in the RGS spectrum of PG 1407+265 (left panel) and the simultaneous RGS+LETG spectra of PKS 0405−123 (middle panel) and PG 1116+215 (right panel). Solid and dashed curves in the middle and right panels are the confidence-level best-fitting line parameters in the individual RGS and LETG spectra of PKS 0405−123 and PG 1116+215, respectively. Horizontal error bars are the 1σ uncertainties on the X-ray halo line centroids, evaluated as the Gaussian-equivalent standard deviations of the distributions of Figure 9 in Appendix C.
Paper: X-Ray Detection of the Galaxy’s Missing Baryons in the Circumgalactic Medium of L* Galaxies
Authors: Fabrizio Nicastro, Y. Krongold, T. Fang, F. Fraternali, S. Mathur, S. Bianchi, A. De Rosa, E. Piconcelli, L. Zappacosta, M. Bischetti, C. Feruglio, A. Gupta, Z. Zhou
Figure caption: The O VII Kα+Kβ line EW-position confidence-level contours, up to the highest closed contour level, in the simultaneous fit to the five X-ray spectra of our X-ray halo sample. The three panels refer to the three different fitting methods described in the text, and for each method, the statistical significance of the highest closed contour is labeled for both one and two interesting parameters.
Paper: X-Ray Detection of the Galaxy’s Missing Baryons in the Circumgalactic Medium of L* Galaxies
Authors: Fabrizio Nicastro, Y. Krongold, T. Fang, F. Fraternali, S. Mathur, S. Bianchi, A. De Rosa, E. Piconcelli, L. Zappacosta, M. Bischetti, C. Feruglio, A. Gupta, Z. Zhou
Figure caption: Raw Chandra LETG  and XMM-Newton RGS  data of the targets of the X-ray halo in each X-ray–LLS frame 18–24 Å wavelength range (vertical error bars). In each panel, the solid lines are the best-fitting continuum plus Gaussian absorption models for methods A (orange), B (green), and C (cyan), folded through their instrumental responses. The complex and prominent structures visible in the RGS spectra are instrumental features due to bad pixels in the dispersion detectors. The black rectangles mark the region containing the O VII Kα and Kβ transitions.
Paper: Atmospheric Reconnaissance of TRAPPIST-1 b with JWST/NIRISS: Evidence for Strong Stellar Contamination in the Transmission Spectra
Authors: Olivia Lim, Björn Benneke, René Doyon, Ryan J. MacDonald, Caroline Piaulet, Étienne Artigau, Louis-Philippe Coulombe, Michael Radica, Alexandrine L'Heureux, Loïc Albert, Benjamin V. Rackham, Julien de Wit, Salma Salhi, Pierre-Alexis Roy, Laura Flagg, Marylou Fournier-Tondreau, Jake Taylor, Neil J. Cook, David Lafrenière, Nicolas B. Cowan, Lisa Kaltenegger, Jason F. Rowe, Néstor Espinoza, Lisa Dang, Antoine Darveau-Bernier
Figure caption: Comparison between the median out-of-transit SOSS spectrum of visit 2 (black) to PHOENIX ACES models (Husser et al. 2013; colored curves in panel (a)), and SPHINX models (Iyer et al. 2023; Iyer 2023; colored curves in panel (b)), normalized to match the SOSS observations in the J band. The blue curves are the models at the effective temperature and surface gravity of TRAPPIST-1 adopted from the literature (Agol et al. 2021; values rounded to T eff = 2600 K and ﹩\mathrm{log}g=5.0﹩). In panel (a), the orange curve is a linear combination of three PHOENIX models, where the weight, surface gravity, and temperature of each model are taken from the stellar-contamination model fit to the transit spectrum of visit 2 (Section 5.1). The green curves are the models that yielded the best fit between the observed SOSS spectrum and the PHOENIX or SPHINX model spectrum (T eff = 2600 K and ﹩\mathrm{log}(g)=3.5﹩ for PHOENIX, T eff = 2500 K and ﹩\mathrm{log}(g)=4.0﹩ for SPHINX). For the PHOENIX models, we scanned effective temperatures between 2300 and 2800 K with 100 K increments, and ﹩\mathrm{log}(g)﹩ values between 2.5 and 5.5 with 0.5 dex increments. For the SPHINX models, we scanned effective temperatures between 2400 and 2700 K with 100 K increments, and ﹩\mathrm{log}(g)﹩ values between 4.0 and 5.5 with 0.5 dex increments.
Paper: Atmospheric Reconnaissance of TRAPPIST-1 b with JWST/NIRISS: Evidence for Strong Stellar Contamination in the Transmission Spectra
Authors: Olivia Lim, Björn Benneke, René Doyon, Ryan J. MacDonald, Caroline Piaulet, Étienne Artigau, Louis-Philippe Coulombe, Michael Radica, Alexandrine L'Heureux, Loïc Albert, Benjamin V. Rackham, Julien de Wit, Salma Salhi, Pierre-Alexis Roy, Laura Flagg, Marylou Fournier-Tondreau, Jake Taylor, Neil J. Cook, David Lafrenière, Nicolas B. Cowan, Lisa Kaltenegger, Jason F. Rowe, Néstor Espinoza, Lisa Dang, Antoine Darveau-Bernier
Figure caption: Reduction and spectral extraction of two SOSS spectral orders with the NAMELESS pipeline. (a) Last group of the tenth integration of visit 1, after superbias subtraction and nonlinearity correction. (b) Detector image of the tenth integration after ramp fitting of the 18 groups comprising each integration. (c) Frame after bad pixel and outlier correction, as well as background subtraction. (d) Frame after correction of the 1/f noise. The center (full line) and edges (dashed lines) of the fixed aperture boxes used to extract the first (red) and second (blue) spectral orders are shown. (e) Extracted spectra of the first (red) and second (blue) spectral orders. The sharp rise in the spectrum of the second order when going to lower spectral pixels is caused by the overlap with the first order.