adsabs/AstroCLIMB huggingface dataset:
Paper: Hamilton Echelle Spectrograph Observations of Solar Analog Field Stars: Lithium Abundance and Activity
Authors: Dan Lubin, Bradford P. Holden, Camille Stock, Carl Melis, David Tytler
Figure caption: Illustration of ranking the subsample having effective temperatures within ±200 K of solar. (a) Sum of the age and lithium abundance ranks as a function of isochrone expectation age. (b) Activity as a function of the sum of the age and lithium ranks. The blue line is a linear fit with correlation coefficient R = 0.550. In both panels the Sun’s values are shown as an orange dot.
Paper: Hamilton Echelle Spectrograph Observations of Solar Analog Field Stars: Lithium Abundance and Activity
Authors: Dan Lubin, Bradford P. Holden, Camille Stock, Carl Melis, David Tytler
Figure caption: Retrieved Lithium abundance vs. our retrieved projected rotational velocity for all 211 program stars. As in Figure 3, open triangles are upper limits to log N(Li).
Paper: Lunar Farside Samples Returned by Chang’E-6 Mission: Significance for Understanding the South Pole-Aitken Basin Stratigraphic History
Authors: Xing Wang, James W. Head, Wenhao Zhao, Yuan Chen, Qin Zhou, Jiaming Zhu, Bo Wu, Jianjun Liu, Chunlai Li
Figure caption: CE-6 landing site in the southern mare plain of the Apollo basin within the SPA basin. (a) shows the thorium distribution across the SPA basin (D. J. Lawrence et al. 2003). The red dashed lines are the boundaries of the SPA compositional zones proposed by D. P. Moriarty & C. M. Pieters (2018), and the black dashed lines represent the elliptical structure of the SPA basin (I. Garrick-Bethell & M. T. Zuber 2009). The white solid lines outline the locations and the ring systems of the Apollo basin, the Schrödinger basin and the Orientale basin (IR = Inner Rook ring, OR = Outer Rook ring, CD = Cordillera ring; J. W. Head 1974), respectively. The box in deep blue indicates the previous candidate CE-6 landing area (X. Zeng et al. 2023) and the red star is the final landing site. The green crosses are the locations of the olivine outcrops within the SPA basin identified by S. Yamamoto et al. (2012). The mare boundaries are from D. M. Nelson et al. (2014). Orthographic projection centered at the center of SPA basin (191.1°E, 53.2°S; I. Garrick-Bethell & M. T. Zuber 2009) is applied in (a). (b) The zoom-in CE-2 digital orthophoto model (DOM) image (C. Li et al. 2018) for the CE-6 landing area, which was previously divided into three subregions (F, L, and B). The image is in equirectangular projection. (c) A panoramic image of the landing site taken by a camera onboard the CE-6 lander before scoop sampling.
Paper: Lunar Farside Samples Returned by Chang’E-6 Mission: Significance for Understanding the South Pole-Aitken Basin Stratigraphic History
Authors: Xing Wang, James W. Head, Wenhao Zhao, Yuan Chen, Qin Zhou, Jiaming Zhu, Bo Wu, Jianjun Liu, Chunlai Li
Figure caption: Basic characteristics of the Apollo basin. (a) is the CE-2 DOM image for the Apollo basin (C. Li et al. 2018). The locations of the Apollo peak ring and rim are from M. A. Ivanov et al. (2018). (b) Topographic map from SLDEM2015 (M. K. Barker et al. 2016). (c) Spectral classification based on the M3 data, see Section 2.2 for details. (d) Thorium distribution around the Apollo basin (D. J. Lawrence et al. 2003). (e) Variations in crustal thickness around Apollo (M. A. Wieczorek et al. 2013). (f) The difference of normalized brightness temperature between noon and dawn (dTB) derived from the CE-2 37 GHz microwave data by Z. Meng et al. (2019). The above panels are in stereographic projection centered at the center of the Apollo basin (36.09°S, 208.52°E; D. M. H. Baker et al. 2011).
Paper: Lunar Farside Samples Returned by Chang’E-6 Mission: Significance for Understanding the South Pole-Aitken Basin Stratigraphic History
Authors: Xing Wang, James W. Head, Wenhao Zhao, Yuan Chen, Qin Zhou, Jiaming Zhu, Bo Wu, Jianjun Liu, Chunlai Li
Figure caption: Distribution of foreign ejecta in the CE-6 landing area. (a) Grayscale stretched CE-2 DOM image (C. Li et al. 2018). The red star marks the final location of the CE-6 landing site. Some amounts of impact rays with higher albedo relative to surroundings can be observed. The arrows indicate some ejecta rays extending further from the Chaffee S ejecta blanket, and the white dashedes outline some ejecta rays from other sources in the near east–west direction. (b) and (c) display the iron (M. Lemelin et al. 2015) and titanium (H. Sato et al. 2017) abundance in the CE-6 landing area, respectively. In addition to the ejecta blanket of the Chaffee S, the bright ejecta rays originated from other sources also exhibit clear decreases in in iron and titanium abundances.
Paper: New Moons of Uranus and Neptune from Ultradeep Pencil-beam Surveys
Authors: Scott S. Sheppard, David J. Tholen, Marina Brozovic, Robert Jacobson, Chadwick A. Trujillo, Patryk Sofia Lykawka, Mike Alexandersen
Figure caption: The cumulative size distribution for the various well-determined outer irregular satellite dynamical families around the giant planets. Most dynamical satellite families have a few large to medium members and many more smaller members. A typical steep collisional size distribution is apparent for satellites smaller than about 5 km in size, whereas larger satellites have a much shallower distribution. The dotted line shows the canonical J. Dohnanyi (1972) asteroid collisional power-law index of q = −2.5, which fits the satellites smaller than 5 km well. This indicates the smallest known satellites are consistent with a collisional origin.
Paper: New Moons of Uranus and Neptune from Ultradeep Pencil-beam Surveys
Authors: Scott S. Sheppard, David J. Tholen, Marina Brozovic, Robert Jacobson, Chadwick A. Trujillo, Patryk Sofia Lykawka, Mike Alexandersen
Figure caption: Representation of Kozai–Lidov dynamics for Neptune satellites Sao, Neso, and the newly found S/2021 N1. The top panels show osculating (﹩{\rm{ecos}}(\omega )﹩ and ﹩{\rm{esin}}(\omega )﹩), while the bottom panels show the osculating argument of pericenter (ω) for 10,000 yr of orbit integration. The argument of pericenter librates around 90°. The reference plane for inclination is the orbital plane of Neptune around the Sun with the mean pole of R.A. = 273.°46 and decl. = 67.°71. The mean pole is estimated from the de441 planetary ephemeris.
Paper: New Moons of Uranus and Neptune from Ultradeep Pencil-beam Surveys
Authors: Scott S. Sheppard, David J. Tholen, Marina Brozovic, Robert Jacobson, Chadwick A. Trujillo, Patryk Sofia Lykawka, Mike Alexandersen
Figure caption: Caliban group of satellites. The newly discovered satellite S/2023 U1 (in orange) completely overlaps in phase space with Stephano. We investigated how close they can approach to each other within 30,000 yr of orbit integration: Stephano and S/2023 U1 could have about a 22,000 km encounter around 5176 AD.
Paper: New Moons of Uranus and Neptune from Ultradeep Pencil-beam Surveys
Authors: Scott S. Sheppard, David J. Tholen, Marina Brozovic, Robert Jacobson, Chadwick A. Trujillo, Patryk Sofia Lykawka, Mike Alexandersen
Figure caption: Orbital phase space for the irregular satellites of Uranus. Black dots show the osculating semimajor axis multiplied by the sines and cosines of the osculating inclination, while the colored outlines show the pericenter-to-apocenter variation, 2ae, for a duration of 10,000 yr. The reference plane for inclinations is the ecliptic. The Hill radius for Uranus is 0.47 au. The newly discovered satellite S/2023 U1 (in orange) completely overlaps in phase space with Stephano.
Paper: New Moons of Uranus and Neptune from Ultradeep Pencil-beam Surveys
Authors: Scott S. Sheppard, David J. Tholen, Marina Brozovic, Robert Jacobson, Chadwick A. Trujillo, Patryk Sofia Lykawka, Mike Alexandersen
Figure caption: Same as Figure 9 but for the Sao group of Neptune satellites. Sao is in Kozai–Lidov resonance with its argument of pericenter oscillating around 90°, but other dynamical group members Laomedeia and S/2002 N5 are not in this resonance.
Paper: New Moons of Uranus and Neptune from Ultradeep Pencil-beam Surveys
Authors: Scott S. Sheppard, David J. Tholen, Marina Brozovic, Robert Jacobson, Chadwick A. Trujillo, Patryk Sofia Lykawka, Mike Alexandersen
Figure caption: Orbital phase space for the irregular satellites of Neptune. Black dots show the osculating semimajor axis multiplied by the sines and cosines of the osculating inclination, while the colored outlines show the pericenter-to-apocenter variation, 2ae, for a duration of 10,000 yr. The reference plane for inclinations is the ecliptic. The Hill radius for Neptune is 0.77 au.
Paper: New Moons of Uranus and Neptune from Ultradeep Pencil-beam Surveys
Authors: Scott S. Sheppard, David J. Tholen, Marina Brozovic, Robert Jacobson, Chadwick A. Trujillo, Patryk Sofia Lykawka, Mike Alexandersen
Figure caption: Same as Figure 9 but for the Neso group of Neptune satellites. Neso and the newly found satellite S/2021 N1 are in Kozai–Lidov resonance with their argument of pericenter oscillating around 90°, but Psamathe is not in this resonance.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). III. Understanding the DTARPS-S Candidate Transiting Planet Catalogs
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Period–radius diagrams for three wide-field surveys. Top left: KOIs in gray symbols with Confirmed Planets in red (NASA Exoplanet Archive 2022b). Top right: TOIs in gray symbols with Confirmed Planets in red. These samples cover the entire celestial sphere. Bottom: DTARPS-S Candidate Catalog (blue) and Galactic Plane list (gold) from Paper II. The Kepler Neptune desert, highlighted in yellow, is bounded by the dashed lines defined by T. Mazeh et al. (2016).
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). III. Understanding the DTARPS-S Candidate Transiting Planet Catalogs
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Detailed view of the period–radius diagram. The left panel shows only the Confirmed Planets from the NASA Exoplanet Archive (light-gray points). The right panel adds the Confirmed Planets and DTARPS-S candidates and Galactic Plane objects. The symbol of each point represents whether it is a Confirmed Planet (circle), previously identified planet candidate (square), or a newly identified candidate (triangle). The Neptune desert, highlighted in yellow, is bounded by the dashed lines defined by T. Mazeh et al. (2016).
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). III. Understanding the DTARPS-S Candidate Transiting Planet Catalogs
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Neptune-desert region in period–radius space for the M20 candidates (left) and the TOI list objects (right). The candidates identified in M20 are plotted in orange and the Confirmed Planets and planet candidates from the TOI list are plotted in gray. DTARPS-S candidates are colored by their disposition level. The symbol of each point represents whether it is a Confirmed Planet (circle), previously identified planet candidate (square), or a newly identified candidate (triangle).
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). III. Understanding the DTARPS-S Candidate Transiting Planet Catalogs
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Insolation flux relative to Earth for the DTARPS-S candidates. The light-gray points represent Confirmed Planets from the NASA Exoplanet Archive’s Planetary systems table. The disposition of the DTARPS-S candidates is indicated by the color of each point and the symbol represents whether the DTARPS-S candidate is a Confirmed Planet (circle), previously identified planet candidate (square), or a newly identified candidate (triangle). The boundary for Jovian-planet inflation (145 S ⊕) is marked with an orange dashed line, and the boundary for photoevaporative mass loss in Neptunes (650 S ⊕) is marked with the red dotted line.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). III. Understanding the DTARPS-S Candidate Transiting Planet Catalogs
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Period of Confirmed Planets and DTARPS-S candidates as a function of effective temperature of the host star. The gray points in the background are the rotation periods for the Kepler stars and the red shaded area indicates the average stellar-rotation period with 1σ error bars around the red line measured by M. B. Nielsen et al. (2013). The entire region is shown in the left plot, and the right plot shows the candidates with periods P < 5 days (most of which are in the hot-Neptune desert) with error bars on their stellar-host temperatures. The DTARPS-S candidate symbols represent previously Confirmed Planets (circle), previously identified planet candidates (square), and new planetary candidates (triangle).
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). III. Understanding the DTARPS-S Candidate Transiting Planet Catalogs
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Histogram of the effective temperature of the stellar hosts for newly identified DTARPS-S candidates compared to the TOI hosts from the TOI list (3000 K < T eff < 7000 K). The DTARPS-S objects are split by disposition. The TOI counts are divided by 2.5 for convenient visualization.
Paper: The Breakthrough Listen Search for Intelligent Life: Galactic Center Search for Scintillated Technosignatures
Authors: Bryan Brzycki, Andrew P. V. Siemion, Imke de Pater, Carmen Choza, Steve Croft, Vishal Gajjar, Jamie Drew, Brian C. Lacki, Danny C. Price, Sofia Z. Sheikh
Figure caption: Transmitter rate vs. EIRP for this study and previous radio technosignature searches. EIRP limits for this study at various distances for the GP targets and GC targets are plotted in blue and green, respectively. The EIRP limits for sources up to 8.5 kpc are marked in black. For each distance, we extend EIRP limits up to the right, corresponding to the maximum drift rate of 10 Hz s−1 searched in this study, for which β ≈ 0.11. Note that while this study and C. Choza et al. (2023) use S/N = 33 to correct for the offset factor in turboSETI, we choose not to alter the results from any earlier studies that may have been affected by this.
Paper: The Breakthrough Listen Search for Intelligent Life: Galactic Center Search for Scintillated Technosignatures
Authors: Bryan Brzycki, Andrew P. V. Siemion, Imke de Pater, Carmen Choza, Steve Croft, Vishal Gajjar, Jamie Drew, Brian C. Lacki, Danny C. Price, Sofia Z. Sheikh
Figure caption: Ranking estimates for all hits in detected events as a function of frequency, with rankings on a logarithmic scale. For comparison, synthetic ranking distributions are shown on the right panel for timescales of 10, 30, and 100 s.
Paper: The Breakthrough Listen Search for Intelligent Life: Galactic Center Search for Scintillated Technosignatures
Authors: Bryan Brzycki, Andrew P. V. Siemion, Imke de Pater, Carmen Choza, Steve Croft, Vishal Gajjar, Jamie Drew, Brian C. Lacki, Danny C. Price, Sofia Z. Sheikh
Figure caption: Corner plots comparing distributions of diagnostic statistics for three synthetic injected signal data sets, corresponding to each Δt  d  ∈ {10 s, 30 s, 100 s}. Each data set has N = 105 samples. Plots on the diagonal show the marginal distributions for each statistic. Off-diagonal plots show 2D contours for the joint distribution of each pair of statistics.
Paper: The Breakthrough Listen Search for Intelligent Life: Galactic Center Search for Scintillated Technosignatures
Authors: Bryan Brzycki, Andrew P. V. Siemion, Imke de Pater, Carmen Choza, Steve Croft, Vishal Gajjar, Jamie Drew, Brian C. Lacki, Danny C. Price, Sofia Z. Sheikh
Figure caption: Extended plots of adjacent cadences for the highest-quality candidates that passed the directional filter.
Paper: The Breakthrough Listen Search for Intelligent Life: Galactic Center Search for Scintillated Technosignatures
Authors: Bryan Brzycki, Andrew P. V. Siemion, Imke de Pater, Carmen Choza, Steve Croft, Vishal Gajjar, Jamie Drew, Brian C. Lacki, Danny C. Price, Sofia Z. Sheikh
Figure caption: Confusion matrix comparing true scintillation timescales with timescales predicted by the coarse maximum likelihood procedure described in Section 4.4. Each data set is composed of 105 synthetic signals.
Paper: The Breakthrough Listen Search for Intelligent Life: Galactic Center Search for Scintillated Technosignatures
Authors: Bryan Brzycki, Andrew P. V. Siemion, Imke de Pater, Carmen Choza, Steve Croft, Vishal Gajjar, Jamie Drew, Brian C. Lacki, Danny C. Price, Sofia Z. Sheikh
Figure caption: Histogram of diagnostic statistics of detected hits in each NGP observation.
Paper: The Breakthrough Listen Search for Intelligent Life: Galactic Center Search for Scintillated Technosignatures
Authors: Bryan Brzycki, Andrew P. V. Siemion, Imke de Pater, Carmen Choza, Steve Croft, Vishal Gajjar, Jamie Drew, Brian C. Lacki, Danny C. Price, Sofia Z. Sheikh
Figure caption: Histogram of frequencies of detected hits in each NGP observation.
Paper: The Breakthrough Listen Search for Intelligent Life: Galactic Center Search for Scintillated Technosignatures
Authors: Bryan Brzycki, Andrew P. V. Siemion, Imke de Pater, Carmen Choza, Steve Croft, Vishal Gajjar, Jamie Drew, Brian C. Lacki, Danny C. Price, Sofia Z. Sheikh
Figure caption: Examples of signals found from the de-Doppler search that passed the algorithmic event filter and ranked highly on the scintillation analysis.
Paper: The Breakthrough Listen Search for Intelligent Life: Galactic Center Search for Scintillated Technosignatures
Authors: Bryan Brzycki, Andrew P. V. Siemion, Imke de Pater, Carmen Choza, Steve Croft, Vishal Gajjar, Jamie Drew, Brian C. Lacki, Danny C. Price, Sofia Z. Sheikh
Figure caption: Histograms of drift rates and S/Ns of detected hits in each NGP observation.
Paper: Demography of Stellar Radio Population within 500 pc: A VLASS-Gaia DR3 Study
Authors: D. Ayanabha, Mayank Narang, Manoj Puravankara, B. Shridharan, H. Tyagi, Bihan Banerjee, Prasanta K. Nayak, Arun Surya
Figure caption: Cutouts (CIRADA cutout service) of epoch 1 (top panel) and 2 (bottom panel) observations of one source from each of the three different categories: confirmed radio sources (Gaia DR3 3192038390381997056) in the left panel, candidate radio sources (ASAS J203622+1215.3) in the middle panel, and candidate transients or highly variable sources (ST Cae) in the right panel. Contours are drawn at the 3σ, 4σ, 5σ, and 7σ levels, where σ is local rms noise. The synthesized beam at FWHM of the fitted component is shown in the lower left corner of the images. The same color scale is used for both epochs to highlight the variability in source signal and local noise. The red star shows the epoch-corrected Gaia DR3 positions, and the yellow marker shows the VLASS coordinate as reported in the QL catalog.
Paper: Demography of Stellar Radio Population within 500 pc: A VLASS-Gaia DR3 Study
Authors: D. Ayanabha, Mayank Narang, Manoj Puravankara, B. Shridharan, H. Tyagi, Bihan Banerjee, Prasanta K. Nayak, Arun Surya
Figure caption: The offset between proper-motion-propagated Gaia DR3 position for the eruptive variable G272-61B and the VLASS component in epochs 1 and 2 is shown in panels (a) and (b), respectively. The red star and lime filled circle represent the Gaia DR3 position of G272-61B corrected to corresponding VLASS mean epochs and exact observed epochs, respectively. The yellow filled circle shows the VLASS 1.2 and 2.2 cataloged positions in the respective images. Contours are drawn at the 3σ, 4σ, 5σ, and 7σ levels, with σ being the local rms noise. The synthesized beam is shown as the black ellipse.
Paper: Demography of Stellar Radio Population within 500 pc: A VLASS-Gaia DR3 Study
Authors: D. Ayanabha, Mayank Narang, Manoj Puravankara, B. Shridharan, H. Tyagi, Bihan Banerjee, Prasanta K. Nayak, Arun Surya
Figure caption: Distribution of all the confirmed and candidate sources on the sky. This color map on a Molleweide projection shows the source density per resolution, and red circles are the source coordinates.
Paper: The Detectability of CH4/CO2/CO and N2O Biosignatures Through Reflection Spectroscopy of Terrestrial Exoplanets
Authors: Armen Tokadjian, Renyu Hu, Mario Damiano
Figure caption: Flux contrast ratio of an Archean Earth-like planet with CO/CH4 = 10 as a function of wavelength. The input forward model is shown by the red circles, and the retrieval result is overlain and separated by molecule to show the individual molecular contributions.
Paper: The Detectability of CH4/CO2/CO and N2O Biosignatures Through Reflection Spectroscopy of Terrestrial Exoplanets
Authors: Armen Tokadjian, Renyu Hu, Mario Damiano
Figure caption: Posterior solution curves for the mixing ratios of CH4 (left-hand panel) and CO2 (right-hand panel) for the same case shown in Figure 1. The dashed vertical lines represent the input value to the forward model, which agree well with the posterior results.
Paper: The Detectability of CH4/CO2/CO and N2O Biosignatures Through Reflection Spectroscopy of Terrestrial Exoplanets
Authors: Armen Tokadjian, Renyu Hu, Mario Damiano
Figure caption: Posterior solution curves for the abundance of CH4 for long wavelength cutoff of 1.60 μm (pink), 1.70 μm (green), and 1.80 μm (blue). The dashed vertical line is the input value of CH4. The full wavelength range results in the best constraint on CH4. The middle and short wavelength cutoff results show a bias toward higher amounts of CH4 due to the different types of atmospheres retrieved in these cases (see text). Nevertheless, all three cases show a good constraint on CH4.
Paper: The Detectability of CH4/CO2/CO and N2O Biosignatures Through Reflection Spectroscopy of Terrestrial Exoplanets
Authors: Armen Tokadjian, Renyu Hu, Mario Damiano
Figure caption: Posterior solution curves for the abundance of CO for CO/CH4 ratios of 1, 5, and 10, corresponding to CO VMR’s of 0.01 (pink), 0.05 (green), and 0.1 (blue), respectively. The dashed vertical lines represent the input values of CO, color coded to the corresponding histogram. For small ratios, the CO distribution is wide, signifying a nondetection. For moderate and high ratios, a peak appears for large CO abundance, which is degenerate with N2. Thus, with the current retrieval setup, it will be challenging to constrain CO abundance in an Archean-Earth scenario.
Paper: The Detectability of CH4/CO2/CO and N2O Biosignatures Through Reflection Spectroscopy of Terrestrial Exoplanets
Authors: Armen Tokadjian, Renyu Hu, Mario Damiano
Figure caption: Posterior solution curves for the mixing ratios of N2O for long wavelength cutoffs at 1.8 μm (blue), 1.4 μm (green), and 1.2 μm (pink). The dashed vertical line is the input value where Log(VMR﹩{}_{{{\rm{N}}}_{2}{\rm{O}}})=-3﹩. A long wavelength cutoff of 1.8 μm and 1.4 μm results in constrained and fairly accurate posteriors, whereas a 1.2 μm cutoff leads to a nondetection of N2O.
Paper: The Detectability of CH4/CO2/CO and N2O Biosignatures Through Reflection Spectroscopy of Terrestrial Exoplanets
Authors: Armen Tokadjian, Renyu Hu, Mario Damiano
Figure caption: Same as Figure 6, but for an input Log(VMR﹩{}_{{{\rm{N}}}_{2}{\rm{O}}})=-4﹩. For each of the long wavelength cutoffs considered here, we obtain a wide posterior distribution for mixing ratio of N2O, but the case of 1.8 μm cutoff results in a slight peak that is biased toward higher amounts of N2O.